FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Scudder, JM Ellison, SL Momjian, E Rosenberg, JL Torrey, P Patton, DR Fertig, D Mendel, JT AF Scudder, Jillian M. Ellison, Sara L. Momjian, Emmanuel Rosenberg, Jessica L. Torrey, Paul Patton, David R. Fertig, Derek Mendel, J. Trevor TI Galaxy pairs in the Sloan Digital Sky Survey - X. Does gas content alter star formation rate enhancement in galaxy interactions? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: interactions; galaxies: starburst; galaxies: star formation; radio lines: galaxies ID ACTIVE GALACTIC NUCLEI; FAST ALPHA SURVEY; MERGING DISK GALAXIES; MASSIVE GALAXIES; METALLICITY EVOLUTION; FORMATION EFFICIENCY; NGC-2782 ARP-215; MERGER GALAXIES; MAJOR MERGERS; MINOR MERGERS AB New spectral line observations, obtained with the Jansky Very Large Array (VLA), of a sample of 34 galaxies in 17 close pairs are presented in this paper. The sample of galaxy pairs is selected to contain galaxies in close, major interactions (i.e. projected separations <30 h(70)(-1) kpc, and mass ratios less extreme than 4: 1), while still having a sufficiently large angular separation that the VLA can spatially resolve both galaxies in the pair. Of the 34 galaxies, 17 are detected at > 3 sigma. We compare the H I gas fraction of the galaxies with the triggered star formation present in that galaxy. When compared to the star formation rates (SFRs) of non-pair galaxies matched in mass, redshift, and local environment, we find that the star formation enhancement is weakly positively correlated (similar to 2.5 sigma) with HI gas fraction. In order to help understand the physical mechanisms driving this weak correlation, we also present results from a small suite of binary galaxy merger simulations with varying gas fractions. The simulated galaxies indicate that larger initial gas fractions are associated with lower levels of interaction-triggered star formation (relative to an identical galaxy in isolation), but also show that high gas fraction galaxies have higher absolute SFRs prior to an interaction. We show that when interaction-driven SFR enhancements are calculated relative to a galaxy with an average gas fraction for its stellar mass, the relationship between SFR and initial gas fraction dominates over the SFR enhancements driven by the interaction. Simulated galaxy interactions that are matched in stellar mass but not in gas fraction, like our VLA sample, yield the same general positive correlation between SFR enhancement and gas fraction that we observe. C1 [Scudder, Jillian M.; Ellison, Sara L.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Scudder, Jillian M.] Univ Sussex, Dept Phys & Astron, Astron Ctr, Brighton BN1 9QH, E Sussex, England. [Momjian, Emmanuel] NRAO, Domenici Sci Operat Ctr, Socorro, NM 87801 USA. [Rosenberg, Jessica L.; Fertig, Derek] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Torrey, Paul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Torrey, Paul] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. [Torrey, Paul] CALTECH, TAPIR, Pasadena, CA 91125 USA. [Patton, David R.] Trent Univ, Dept Phys & Astron, Peterborough, ON K9J 7B8, Canada. [Mendel, J. Trevor] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Scudder, JM (reprint author), Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. EM j.scudder@sussex.ac.uk OI Scudder, Jillian/0000-0002-8798-3972; Torrey, Paul/0000-0002-5653-0786 FU NSERC; NSF [AST-000167932]; George Mason University Presidential Fellowship; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX SLE and DRP acknowledge the receipt of an NSERC Discovery grant which funded this research. DF and JLR acknowledge NSF grant AST-000167932 and George Mason University Presidential Fellowship for support of this work.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. 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 79 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 JUN 1 PY 2015 VL 449 IS 4 BP 3719 EP 3740 DI 10.1093/mnras/stv588 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000034 ER PT J AU D'Ai, A Di Salvo, T Iaria, R Garcia, JA Sanna, A Pintore, F Riggio, A Burderi, L Bozzo, E Dauser, T Matranga, M Galiano, CG Robba, NR AF D'Ai, A. Di Salvo, T. Iaria, R. Garcia, J. A. Sanna, A. Pintore, F. Riggio, A. Burderi, L. Bozzo, E. Dauser, T. Matranga, M. Galiano, C. G. Robba, N. R. TI GRO J1744-28: an intermediate B-field pulsar in a low-mass X-ray binary SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line: formation; line: identification; stars: individual: GRO J1744-28; X-rays: binaries; X-rays: general ID ACCRETING MILLISECOND PULSAR; BURSTING PULSAR; NEUTRON-STAR; XMM-NEWTON; IGR J17480-2446; MAGNETIC-FIELD; BLACK-HOLE; EVOLUTIONARY HISTORY; BULK COMPTONIZATION; TIMING-EXPLORER AB The bursting pulsar, GRO J1744-28, went again in outburst after similar to 18 yr of quiescence in 2014 mid-January. We studied the broad-band, persistent, X-ray spectrum using X-ray data from a XMM-Newton observation, performed almost at the peak of the outburst, and from a close INTEGRAL observation, performed 3 d later, thus covering the 1.3-70.0 keV band. The spectrum shows a complex continuum shape that cannot be modelled with standard high-mass X-ray pulsar models, nor by two-components models. We observe broad-band and peaked residuals from 4 to 15 keV, and we propose a self-consistent interpretation of these residuals, assuming they are produced by cyclotron absorption features and by a moderately smeared, highly ionized, reflection component. We identify the cyclotron fundamental at similar to 4.7 keV, with hints for two possible harmonics at similar to 10.4 and similar to 15.8 keV. The position of the cyclotron fundamental allows an estimate for the pulsar magnetic field of (5.27 +/- 0.06) x 10(11) G, if the feature is produced at its surface. From the dynamical and relativistic smearing of the disc reflected component, we obtain a lower limit estimate for the truncated accretion disc inner radius (greater than or similar to 100 R-g) and for the inclination angle (18 degrees-48 degrees). We also detect the presence of a softer thermal component that we associate with the emission from an accretion disc truncated at a distance from the pulsar of 50-115 R-g. From these estimates, we derive the magnetospheric radius for disc accretion to be similar to 0.2 times the classical Alfven radius for radial accretion. C1 [D'Ai, A.; Sanna, A.; Pintore, F.; Riggio, A.; Burderi, L.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, Italy. [Di Salvo, T.; Iaria, R.; Matranga, M.; Galiano, C. G.; Robba, N. R.] Univ Palermo, Dipartimento Fis & Chim, I-90123 Palermo, Italy. [Garcia, J. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bozzo, E.] ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Dauser, T.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. RP D'Ai, A (reprint author), Univ Cagliari, Dipartimento Fis, SP Monserrato Sestu KM 0-7, I-09042 Monserrato, Italy. EM antonino.dai@dsf.unica.it RI Iaria, Rosario/F-2520-2012; Di Salvo, Tiziana/F-3973-2012; Riggio, Alessandro/D-3174-2012; OI Iaria, Rosario/0000-0003-2882-0927; Di Salvo, Tiziana/0000-0002-3220-6375; Burderi, Luciano/0000-0001-5458-891X; Riggio, Alessandro/0000-0002-6145-9224; Sanna, Andrea/0000-0002-0118-2649 FU Fondo Finalizzato alla Ricerca (FFR) [2012-ATE-0390]; Sardinia Regional Government FX The High-Energy Astrophysics Group of Palermo acknowledges support from the Fondo Finalizzato alla Ricerca (FFR) 2012/13, project no. 2012-ATE-0390, founded by the University of Palermo.; AR gratefully acknowledges the Sardinia Regional Government for the financial support (P. O. R. Sardegna F.S.E. Operational Programme of the Autonomous Region of Sardinia, European Social Fund 2007-2013 - Axis IV Human Resources, Objective l.3, Line of Activity l.3.1). NR 66 TC 7 Z9 7 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2015 VL 449 IS 4 BP 4288 EP 4303 DI 10.1093/mnras/stv531 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000070 ER PT J AU Tokovinin, A Latham, DW Mason, BD AF Tokovinin, Andrei Latham, David W. Mason, Brian D. TI THE UNUSUAL QUADRUPLE SYSTEM HD 91962 WITH A "PLANETARY" ARCHITECTURE SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general ID SPECKLE INTERFEROMETRY; RADIAL-VELOCITIES; MULTIPLE STARS; PHOTOMETRY; COMPONENTS; EVOLUTION; BINARIES; SOAR AB The young nearby solar-type star HD 91962 is a rare quadruple system where three companions revolve around the main component with periods of 170.3 days, 8.85 years, and 205 years. The two outer orbits are nearly co-planar, and all orbits have small eccentricities. We refine the visual orbit of the outer pair and determine the combined spectro-interferometric orbit of the middle 8.8 year pair and the spectroscopic orbit of the inner binary. The middle and inner orbits are likely locked in a 1: 19 resonance, and the ratio of the outer and middle periods is similar to 23. The masses of all components are estimated (inside-out: 1.14, 0.32, 0.64, 0.64 solar mass). The dynamical parallax is 27.4 +/- 0.6 mas. We speculate that this multiple system originated from collapse of an isolated core and that the companions migrated in a dissipative disk. Other multiple systems with similar features (co-planarity, small eccentricity, and period ratio around 20) are known. C1 [Tokovinin, Andrei] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mason, Brian D.] US Naval Observ, Washington, DC 20392 USA. RP Tokovinin, A (reprint author), Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile. EM atokovinin@ctio.noao.edu; dlatham@cfa.harvard.edu; bdm@usno.navy.mil OI Tokovinin, Andrei/0000-0002-2084-0782; Latham, David/0000-0001-9911-7388 NR 22 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2015 VL 149 IS 6 AR 195 DI 10.1088/0004-6256/149/6/195 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ1NN UT WOS:000355250400018 ER PT J AU Bader, E Jung, K Kalko, EKV Page, RA Rodriguez, R Sattler, T AF Bader, Elias Jung, Kirsten Kalko, Elisabeth K. V. Page, Rachel A. Rodriguez, Raul Sattler, Thomas TI Mobility explains the response of aerial insectivorous bats to anthropogenic habitat change in the Neotropics SO BIOLOGICAL CONSERVATION LA English DT Article DE Panama; Vulnerability; Wing morphology; Acoustic monitoring; Occupancy; Detectability ID EXTINCTION RISK; AGRICULTURAL INTENSIFICATION; ACOUSTIC IDENTIFICATION; COMMUNITY STRUCTURE; ECHOLOCATION CALLS; FOREST FRAGMENTS; LAND-USE; URBANIZATION; CHIROPTERA; LANDSCAPE AB Habitat loss due to anthropogenic activities is a critical threat to biodiversity. Understanding which factors determine species persistence in degraded environments is essential for conservation management. Here, we investigated how aerial insectivorous bats in the Neotropics, an ecologically important, but understudied group of vertebrates, are affected by deforestation and urbanization. We conducted a standardized acoustic survey in four habitat types in 14 areas across Panama (500 km x 260 km), a scale hitherto unprecedented for the Neotropics, and assessed occupancy in 13 aerial insectivorous bat species, accounting for species- and habitat-specific detectability. In addition, we used wing measures to derive a proxy for flight efficiency and flight speed, as an indication of species-specific mobility. Results show that detectability does not only vary strongly among species but also, within a species, depending on the habitat: for nine species intra-specific detectability varied >10%. Model estimates for occupancy revealed that aerial insectivorous bats are highly heterogeneous in their response to deforestation and urbanization. Canopy height and canopy cover predicted occupancy best for most species. Relating occupancy to mobility we found that less mobile species with broad wings (high wing loading and low aspect ratio) decrease occupancy in deforested and urban areas, while more mobile species with narrow wings increase in these habitats. We suggest that this pattern applies also to species not analyzed in this study. Our study exemplifies how morphological information can help define conservation priorities when information on occurrence and distribution is limited. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Bader, Elias] Univ Zurich, Inst Evolutionary Biol & Environm Studies, CH-8057 Zurich, Switzerland. [Bader, Elias; Kalko, Elisabeth K. V.; Page, Rachel A.; Rodriguez, Raul; Sattler, Thomas] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Kalko, Elisabeth K. V.; Sattler, Thomas] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Rodriguez, Raul] Univ Ind Santander, Lab Ecol, Bucaramanga, Colombia. RP Bader, E (reprint author), Swiss Fed Res Inst WSL, Zurcherstr 111, CH-8903 Birmensdorf, Switzerland. EM ebader@gmx.ch; kirsten.jung@uni-ulm.de; pager@si.edu; rrodriguezuis@gmail.com; thomas.sattler@vogelwarte.ch FU Swiss Academy of Natural Sciences SCNAT; Swiss National Science Foundation (SNSF) FX Swiss Academy of Natural Sciences SCNAT: Funding of travel expenses.; Swiss National Science Foundation (SNSF): Research project of last author, in which this study was included. NR 79 TC 4 Z9 4 U1 11 U2 66 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 JUN PY 2015 VL 186 BP 97 EP 106 DI 10.1016/j.biocon.2015.02.028 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CI8ZX UT WOS:000355061300012 ER PT J AU Wang, F McShea, WJ Wang, DJ Li, S AF Wang, Fang McShea, William J. Wang, Dajun Li, Sheng TI Shared resources between giant panda and sympatric wild and domestic mammals SO BIOLOGICAL CONSERVATION LA English DT Article DE Species co-occurrence; Inter-species interaction; Grazing control; Camera-trapping; Occupancy model; Bayesian model ID SPECIES COOCCURRENCE PATTERNS; NATURE-RESERVE; SPATIAL-DISTRIBUTION; CONSERVATION PLANS; HABITAT SELECTION; SICHUAN PROVINCE; PREDATOR CONTROL; CHINA; LANDSCAPE; BEARS AB Interactions between sympatric species may negatively affect a species' fitness, and complicate management of species assemblages in protected areas. An example of the need to quantify the strength and direction of the species interactions is giant panda conservation in newly established reserves. Although the habitat requirements of giant panda have been broadly studied, the degree of its interactions with sympatric large mammals remains unclear. In this paper, we systematically surveyed for species occurrence in the southwestern China during 2008-2013, to better understand the interactions between giant panda and four sympatric large mammal species. We constructed species-specific occupancy models based on camera-trapping data using both environmental and detection variables. We then used the important predictor variables for each species to construct pairwise species co-occurrence models following a Bayesian framework. Our analysis detected significant habitat overlap between giant panda and its sympatric species. However, there was no evidence of native species limiting the distribution of giant pandas despite their extensive use of the same forests. The only evidence for negative interactions was between the distributions of giant panda and domestic cattle within bamboo forest, the primary habitat of giant pandas. The co-occurrence model has value for any conservation planning that benefits from knowledge of inter-species interactions. Our study suggests that, in southwestern China, strict grazing control of domestic cattle in protected areas is warranted until the nature of its interactions with native large mammals can be determined. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Wang, Fang; McShea, William J.] Natl Zool Pk, Conservat Ecol Ctr, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Wang, Dajun; Li, Sheng] Peking Univ, Sch Life Sci, Beijing 100871, Peoples R China. RP Li, S (reprint author), Peking Univ, Sch Life Sci, 5 Yiheyuan RD, Beijing 100871, Peoples R China. EM shengli@pku.edu.cn FU Friends of National Zoo (FONZ); World Wildlife Foundation (WWF); Conservation International (CI); The Nature Conservancy (TNC); Ocean Park Conservation Fund Hong Kong (OPCFHK) FX We thank the staff of Changqing Nature Reserve, Wanglang Nature Reserve, Wolong Nature Reserve, Tangjiahe Nature Reserve, Laohegou Nature Reserve, Huangbaiyuan Nature Reserve, Niuweihe Nature Reserve, and Xiaohegou Nature Reserve for their assistance to the field work. The Sichuan Forestry Department and the Shaanxi Forestry Department helped us in logistical details and permit applications. We thank Dr. J. Hardin Waddle and Dr. Qing Zhao for their assistance in data analysis. The field survey was funded by Friends of National Zoo (FONZ), World Wildlife Foundation (WWF), Conservation International (CI), The Nature Conservancy (TNC) and Ocean Park Conservation Fund Hong Kong (OPCFHK). NR 70 TC 3 Z9 3 U1 4 U2 44 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 JUN PY 2015 VL 186 BP 319 EP 325 DI 10.1016/j.biocon.2015.03.032 PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CI8ZX UT WOS:000355061300036 ER PT J AU Hong, T AF Hong, Terry TI The Way Things Were SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2015 VL 140 IS 10 BP 96 EP 96 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA CJ3MK UT WOS:000355387900115 ER PT J AU Smith, GD Murillo-Garcia, OE Hostetler, JA Mearns, R Rollie, C Newton, I McGrady, MJ Oli, MK AF Smith, George D. Murillo-Garcia, Oscar E. Hostetler, Jeffrey A. Mearns, Richard Rollie, Chris Newton, Ian McGrady, Michael J. Oli, Madan K. TI Demography of population recovery: survival and fidelity of peregrine falcons at various stages of population recovery SO OECOLOGIA LA English DT Article DE Age-specific survival; Burnham model; Density dependence; Falco peregrinus; Fidelity ID CLIMATIC VARIATION; DENSITY; DYNAMICS; ANIMALS; CALIFORNIA; DISPERSAL AB Factors influencing vital demographic rates and population dynamics can vary across phases of population growth. We studied factors influencing survival and fidelity of peregrine falcons in south Scotland-north England at two stages of population growth: when the population was recovering from pesticide-related declines and density was low, and when it had largely recovered from pesticide effects and density was high. Fidelity was higher for: adults and subadults than for juveniles, females than for males, and juveniles and adults during the low-density than during the high-density study period. Survival was age specific, with lower survival for juveniles than for older birds (juveniles, 0.600 +/- A SE 0.063; subadults, 0.811 +/- A 0.058; adults, 0.810 +/- A 0.034). Furthermore, there was some evidence that survival was generally lower for all age classes during the low-density period than during the high-density period, possibly due to a chronic, persistent effect of organochlorine pesticides as the population recovered. Evidence for a density-dependent effect on survival was weak, but a negative effect of density on fidelity of juveniles (dispersing age class) during the recovery phase suggests density-dependent dispersal when the population was increasing. Our results show how population density can influence demographic parameters differently and how such influences can vary across phases of population growth. C1 [Smith, George D.] Scottish Raptor Study Grp, Kirknewton EH27 8BS, West Lothian, Scotland. [Murillo-Garcia, Oscar E.; Oli, Madan K.] Univ Florida, Sch Nat Resources & Environm, Gainesville, FL 32611 USA. [Murillo-Garcia, Oscar E.; Oli, Madan K.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Hostetler, Jeffrey A.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA. [Mearns, Richard] Conansknowe, Dumfries DG1 1SX, Scotland. [Rollie, Chris] Royal Soc Protect Birds, Dumfries & Galloway Off, Crossmichael DG7 3AP, Castle Douglas, Scotland. [Newton, Ian] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England. [McGrady, Michael J.] Int Avian Res, A-3500 Krems, Austria. RP Oli, MK (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, 110 Newins Ziegler Hall, Gainesville, FL 32611 USA. EM olim@ufl.edu RI Hostetler, Jeffrey/A-3345-2011 OI Hostetler, Jeffrey/0000-0003-3669-1758 FU International Avian Research, Austria; Natural Research, UK; Fulbright Colombia Program; Universidad del Valle; University of Florida FX We thank International Avian Research, Austria, and Natural Research, UK for financial support. G. Carse and R. Roxburgh collected much of the field data in the early years. We are grateful to J. Clarke and the BTO for providing the recovery data. The large amount of voluntary fieldwork provided annually by members of the Scottish Raptor Study Groups that covered the study area was vital to the study. Fulbright Colombia Program, Universidad del Valle, and University of Florida provided financial support for graduate studies of Oscar Murillo-Garcia. We are greatly indebted to J. D. Nichols for providing much needed guidance in data analysis and to J. D. Nichols, S. K. Robinson and J. M. Ponciano for many helpful comments. NR 44 TC 1 Z9 1 U1 2 U2 37 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 JUN PY 2015 VL 178 IS 2 BP 391 EP 401 DI 10.1007/s00442-014-3168-3 PG 11 WC Ecology SC Environmental Sciences & Ecology GA CI6VF UT WOS:000354900700008 PM 25627408 ER PT J AU France, CAM Giaccai, JA Doney, CR AF France, Christine A. M. Giaccai, Jennifer A. Doney, Charlotte R. TI The effects of Paraloid B-72 and Butvar B-98 treatment and organic solvent removal on delta C-13, delta N-15, and delta O-18 values of collagen and hydroxyapatite in a modern bone SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE stable isotopes; bone; Paraloid; Butvar ID OXYGEN-ISOTOPE COMPOSITIONS; STABLE-ISOTOPES; ARCHAEOLOGICAL BONE; TROPHIC RELATIONSHIPS; DIAGENETIC ALTERATION; PHOSPHATE; NITROGEN; CARBONATE; RECONSTRUCTION; PHYSIOLOGY AB Stable isotopes in bones are a powerful tool for diet, provenance, climate, and physiological reconstructions, but necessarily require well-preserved specimens unaltered by postmortem diagenesis or conservation practices. This study examines the effects of Paraloid B-72 and Butvar B-98, two common consolidants used in field and museum conservation, on C-13, N-15, and O-18 values from bone collagen and hydroxyapatite. The effects of solvent removal (100% acetone, 100% ethanol, 9:1 acetone:xylenes, 9:1 ethanol:xylenes) and drying methods (ambient air, vacuum, oven drying at 80 degrees C) were also examined to determine if bones treated with these consolidants can successfully be cleaned and used for stable isotope analyses. Results show that introduction of Paraloid B-72 or Butvar B-98 in 100% acetone or 100% ethanol, respectively, with subsequent removal by the same solvents and drying at 80 degrees C facilitates the most successful removal of consolidants and solvents. The C-13 values in collagen, N-15 in collagen, O-18 in hydroxyapatite phosphate, and C-13 in hydroxyapatite structural carbonate were unaltered by treatments with Paraloid or Butvar and subsequent solvent removal. The O-18 in hydroxyapatite structural carbonate showed nonsystematic variability when bones were treated with Paraloid and Butvar, which is hypothesized to be a result of hydroxyl exchange when bones are exposed to consolidants in solution. It is therefore recommended that O-18 in hydroxyapatite structural carbonate should not be used in stable isotope studies if bones have been treated with Paraloid or Butvar. Am J Phys Anthropol 157:330-338, 2015. (c) 2015 Wiley Periodicals, Inc. C1 [France, Christine A. M.; Doney, Charlotte R.] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. [Giaccai, Jennifer A.] Smithsonian Inst, Freer Gallery Art, Washington, DC 20013 USA. RP France, CAM (reprint author), Smithsonian Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM francec@si.edu FU Smithsonian Institution FX Grant sponsor: Smithsonian Institution. NR 57 TC 0 Z9 0 U1 1 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD JUN PY 2015 VL 157 IS 2 BP 330 EP 338 DI 10.1002/ajpa.22697 PG 9 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CI4OU UT WOS:000354731600013 PM 25639211 ER PT J AU Farine, DR AF Farine, Damien R. TI Proximity as a proxy for interactions: issues of scale in social network analysis SO ANIMAL BEHAVIOUR LA English DT Editorial Material DE association; interaction; interspecific; mixed-species flocking; social network analysis; thornbill ID ORGANIZATION; ASSOCIATION; PREDICT; EVOLUTION; BEHAVIOR C1 [Farine, Damien R.] Univ Oxford, Dept Zool, Edward Grey Inst Field Ornithol, Oxford OX1 3PS, England. [Farine, Damien R.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Farine, Damien R.] Smithsonian Trop Res Inst, Ancon, Panama. 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 OI Farine, Damien/0000-0003-2208-7613 NR 31 TC 15 Z9 15 U1 8 U2 29 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 JUN PY 2015 VL 104 BP E1 EP E5 DI 10.1016/j.anbehav.2014.11.019 PG 5 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA CI5PX UT WOS:000354811800003 ER PT J AU Pitt, WC Sugihara, RT Berentsen, AR AF Pitt, William C. Sugihara, Robert T. Berentsen, Are R. TI Effect of travel distance, home range, and bait on the management of small Indian mongooses, Herpestes auropunctatus SO BIOLOGICAL INVASIONS LA English DT Article DE Bait attractiveness; Control; Foraging distance; Hawaii; Management ID CARNIVORA-VIVERRIDAE; ANTHROPOGENIC FOOD; ORAL TOXICITY; RAIN-FOREST; WEST-INDIES; JAVANICUS; MAMMALS; ISLAND; AMINOPROPIOPHENONE; VACCINATION AB Selection of preferred baits to attract mongooses to traps and other control devices is paramount in the effective management and control of this invasive predatory mammal. We examined the attractiveness of selected food items as baits to free-ranging mongooses in field trials at two different habitats on the island of Hawaii. We utilized radio telemetry to calculate mongoose home range and population density estimates. We implanted microchips to remotely identify and record visitations by mongooses to the candidate baits and investigated bait visitation rates, bait attraction distances, and bait discovery times. Mongooses in this study foraged over a wide area and readily investigated the various novel food baits, with fish, beef and egg-baited stations eliciting higher first and revisits over multiple days. We radio collared 34 mongooses. Overall mean home range estimates were 21.9 and 28.8 ha and did not differ between the two study sites (F = 2.12, p = 0.156), although overall male mongooses had larger home ranges than females (F = 22.92, df = 1, p < 0.0001). Extensive overlapping home ranges were recorded among individual mongooses, regardless of gender. Male mongooses were attracted from a greater distance to selected baits as compared to females (F = 15.80, df = 1, p = 0.0004) although females visited more bait stations than males at each site (F = 11.26, df = 1, p = 0.002 and F = 6.90, df = 1, p = 0.017). Baits were usually discovered within 24-30 h of exposure. Based on time to first bait discovery, no differences were found among percent of food stations visited among bait types at either site (F = 0.93, df = 4, p = 0.463 and F = 0.40, df = 3, p = 0.756). The results of this study provide insights on mongoose foraging ecology in Hawaii and the attractiveness of food baits used in developing effective control strategies in detecting and trapping mongooses in newly established areas as well as reducing or eradicating populations in native species habitat impacted by mongooses. C1 [Pitt, William C.; Sugihara, Robert T.] USDA, Anim & Plant Hlth Inspect Serv, Wildlife Serv, Natl Wildlife Res Ctr,Hawaii Field Stn, Hilo, HI 96720 USA. [Berentsen, Are R.] USDA, Anim & Plant Hlth Inspect Serv, Wildlife Serv, Natl Wildlife Res Ctr, Hilo, HI 96720 USA. RP Pitt, WC (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. EM pittw@si.edu FU U. S. Fish and Wildlife Service, Pacific Islands Fish and Wildlife Office FX We are grateful for the support and assistance provided by the U. S. Fish and Wildlife Service, Pacific Islands Fish and Wildlife Office. Capture, handling and marking of mongooses was performed with approval of the National Wildlife Research Center's Institutional Animal Care and Use Committee February 25, 2005 under QA-1255. We thank Michael W. Fall and Catherine E. Swift for assistance with literature review and manuscript preparation. Special thanks to two anonymous reviewers for helpful and insightful comments on an earlier draft of this manuscript. NR 52 TC 3 Z9 3 U1 9 U2 28 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 EI 1573-1464 J9 BIOL INVASIONS JI Biol. Invasions PD JUN PY 2015 VL 17 IS 6 BP 1743 EP 1759 DI 10.1007/s10530-014-0831-x PG 17 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CH9RJ UT WOS:000354373500014 ER PT J AU Crayn, DM Winter, K Schulte, K Smith, JAC AF Crayn, Darren M. Winter, Klaus Schulte, Katharina Smith, J. Andrew C. TI Photosynthetic pathways in Bromeliaceae: phylogenetic and ecological significance of CAM and C-3 based on carbon isotope ratios for 1893 species SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE adaptive radiation; ecophysiology; epiphytism; Neotropics; photosynthesis ID CRASSULACEAN ACID METABOLISM; NATURAL TROPICAL CONDITIONS; NDHF SEQUENCE DATA; DARK CO2 FIXATION; L SPANISH MOSS; VASCULAR EPIPHYTES; HISTORICAL BIOGEOGRAPHY; BROMELIOIDEAE BROMELIACEAE; TILLANDSIA-USNEOIDES; ADAPTIVE RADIATION AB A comprehensive analysis of photosynthetic pathways in relation to phylogeny and elevational distribution was conducted in Bromeliaceae, an ecologically diverse Neotropical family containing large numbers of both terrestrial and epiphytic species. Tissue carbon isotope ratio (C-13) was used to determine the occurrence of crassulacean acid metabolism (CAM) and C-3 photosynthesis in 1893 species, representing 57% of species and all 56 genera in the family. The frequency of C-13 values showed a strongly bimodal distribution: 1074 species (57%) had values more negative than -20 parts per thousand (mode=-26.7 parts per thousand), typical of predominantly daytime carbon fixation via the C-3 pathway, whereas 819 species (43%) possessed values less negative than -20 parts per thousand (mode=-13.3 parts per thousand), indicative of predominantly nocturnal fixation of carbon via the CAM pathway. Amongst the six almost exclusively terrestrial subfamilies in Bromeliaceae, Brocchinioideae, Lindmanioideae and Navioideae consisted entirely of C-3 species, with CAM species being restricted to Hechtioideae (all species of Hechtia tested), Pitcairnioideae (all species belonging to a xeric clade comprising Deuterocohnia, Dyckia and Encholirium) and Puyoideae (21% of Puya spp.). Of the other two subfamilies, in the overwhelmingly epiphytic (plus lithophytic) Tillandsioideae, 28% of species possessed CAM photosynthesis, all restricted to the derived genus Tillandsia and tending towards the more extreme epiphytic atmospheric' life-form. In Bromelioideae, with comparable numbers of terrestrial and epiphytic species, 90% of taxa showed CAM; included in these are the first records of CAM photosynthesis in Androlepis, Canistropsis, Deinacanthon, Disteganthus, Edmundoa, Eduandrea, Hohenbergiopsis, Lymania, Pseudananas, Ronnbergia and Ursulaea. With respect to elevational gradients, the greatest number of C-3 bromeliad species were found at mid-elevations between 500 and 1500m, whereas the frequency of CAM species declined monotonically with increasing elevation. However, in Puya, at least ten CAM species have been recorded at elevations >3000m, showing that CAM photosynthesis is not necessarily incompatible with low temperatures. This survey identifies five major origins of CAM photosynthesis at a higher taxonomic level in Bromeliaceae, but future phylogenetic work is likely to reveal a more fine-scale pattern of gains and losses of this trait, especially in ecologically diverse and widely distributed genera such as Tillandsia and Puya.(c) 2015 The Linnean Society of London, Botanical Journal of the Linnean Society, 2015, 178, 169-221. C1 [Crayn, Darren M.; Schulte, Katharina] James Cook Univ, Australian Trop Herbarium, Smithfield, Qld 4878, Australia. [Crayn, Darren M.] James Cook Univ, Ctr Trop Environm Sustainabil Sci, Smithfield, Qld 4878, Australia. [Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Schulte, Katharina] James Cook Univ, Ctr Trop Biodivers & Climate Change, Townsville, Qld 4814, Australia. [Smith, J. Andrew C.] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. RP Smith, JAC (reprint author), Univ Oxford, Dept Plant Sci, S Parks Rd, Oxford OX1 3RB, England. EM andrew.smith@plants.ox.ac.uk RI Research ID, CTBCC /O-3564-2014; James Cook University, TESS/B-8171-2012; Crayn, Darren/A-7386-2011 OI Crayn, Darren/0000-0001-6614-4216 FU Andrew W. Mellon Foundation grants through the Smithsonian Tropical Research Institute FX This paper is dedicated to the memory of Harry E. Luther (1952-2012), who was the foremost authority on the taxonomy and cultivation of Bromeliaceae since Lyman B. Smith. Harry facilitated this and much other bromeliad research through his Directorship of the Mulford B. Foster Bromeliad Identification Center at Marie Selby Botanical Gardens. We thank E. Leme (Rio de Janeiro, Brazil) and the Directors of the HB, K, MO, NY, OXF, SEL, SP, US and VEN herbaria, and the Marie Selby Botanical Gardens (Sarasota, FL, USA), for access to their collections, and R. Duno (VEN), S. A. Harris (OXF), B. K. Holst (SEL), the late H. E. Luther (SEL), the late D. Philcox (K), J. C. Solomon (MO), M. G. L. Wanderley (SP), S. Wookey (NY), S. Marner, E. Medina, E. Olivares, L. Peters and L. Pond for assistance and/or advice during collecting visits. L. Giles (Duke University, NC, USA) performed the isotope analyses. The following are also thanked for helpful discussions: M. H. J. Barfuss, L. Cernusak, J. R. Grant, H. Griffiths, F. A. Harper, R. Horres, J. A. M. Holtum, H. S. J. Lee, A. R. G. Plackett, the late W. Rauh, and G. Zizka. Two anonymous reviewers are acknowledged for comments that improved the manuscript. This research was supported by Andrew W. Mellon Foundation grants through the Smithsonian Tropical Research Institute to JACS and KW. NR 153 TC 16 Z9 16 U1 7 U2 44 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4074 EI 1095-8339 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD JUN PY 2015 VL 178 IS 2 BP 169 EP 221 DI 10.1111/boj.12275 PG 53 WC Plant Sciences SC Plant Sciences GA CI4OE UT WOS:000354729600001 ER PT J AU Pelletier, J Busch, J Potvin, C AF Pelletier, Johanne Busch, Jonah Potvin, Catherine TI Addressing uncertainty upstream or downstream of accounting for emissions reductions from deforestation and forest degradation SO CLIMATIC CHANGE LA English DT Article ID LAND CHANGE; REDD+; CONSERVATIVENESS; ACCURACY; BENEFITS; AREA AB Uncertainty in emissions and emission changes estimates constitutes an unresolved issue for a future international climate agreement. Uncertainty can be addressed 'upstream' through improvements in the technologies or techniques used to measure, report, and verify (MRV) emission reductions, or 'downstream' through the application of discount factors to more uncertain reductions. In the context of Reducing Emissions from Deforestation and forest Degradation (REDD+), we look at the effects of upstream interventions on reductions in uncertainty, using data from Panama. We also test five downstream proposals for discounting uncertainty of the potential credits received for reducing emissions. We compare the potential compensation received for these emission reductions to the cost of alternative upstream investments in forest monitoring capabilities. First, we find that upstream improvements can noticeably reduce the overall uncertainty in emission reductions. Furthermore, the costs of upstream investments in improved forest monitoring are relatively low compared to the potential benefits from carbon payments; they would allow the country to receive higher financial compensation from more certain emission reductions. When uncertainty is discounted downstream, we find that the degree of conservativeness applied downstream has a major influence on both overall creditable emission reductions and on incentives for upstream forest monitoring improvements. Of the five downstream approaches that we analyze, only the Conservativeness Approach and the Risk Charge Approach provided consistent financial incentives to reduce uncertainty upstream. We recommend specifying the use of one of these two approaches if REDD+ emission reductions are to be traded for emission reductions from other sectors. C1 [Pelletier, Johanne] Woods Hole Res Ctr, Falmouth, MA 02540 USA. [Busch, Jonah] Ctr Global Dev, Washington, DC 20036 USA. [Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Potvin, Catherine] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Pelletier, J (reprint author), Woods Hole Res Ctr, 149 Woods Hole Rd, Falmouth, MA 02540 USA. EM jpelletier@whrc.org RI Pelletier, Johanne/E-3156-2016 OI Pelletier, Johanne/0000-0001-8161-6410 NR 40 TC 4 Z9 4 U1 2 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-0009 EI 1573-1480 J9 CLIMATIC CHANGE JI Clim. Change PD JUN PY 2015 VL 130 IS 4 BP 635 EP 648 DI 10.1007/s10584-015-1352-z PG 14 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CI4GD UT WOS:000354705200012 ER PT J AU Ubelaker, DH Thomas, C Olson, JE AF Ubelaker, Douglas H. Thomas, Christian Olson, Jacqueline E. TI The impact of age at death on the lag time of radiocarbon values in human bone SO FORENSIC SCIENCE INTERNATIONAL LA English DT Review DE Forensic science; Radiocarbon; Bone; Lag time ID ARTIFICIAL RADIOCARBON; TURNOVER; C-14; SKELETAL AB Analysis of modern bomb-pulse radiocarbon in human bone offers data needed to interpret the postmortem interval in skeletonized human remains recovered from forensic contexts. Radiocarbon analysis of different tissues with distinct rates of remodeling allows proper placement of the values on the modern bomb-curve. However, the lag time between the date of intercept on the curve and the actual death date is largely affected by the age at death. Published data on radiocarbon analysis of individuals of known age at death and death dates indicate that this lag time increases with age until about 60 years. The lag time documented for each decade of life can be used to compensate for this age-related factor and increase the accuracy of interpretation of the death date. While this method could be greatly improved by original research with a larger sample size, this study provides an adequate point from which to launch further investigations into the subject. Published by Elsevier Ireland Ltd. C1 [Ubelaker, Douglas H.; Thomas, Christian; Olson, Jacqueline E.] Smithsonian Inst, NMNH, Dept Anthropol, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, NMNH, Dept Anthropol, MRC 112, Washington, DC 20560 USA. EM ubelaked@si.edu NR 16 TC 0 Z9 0 U1 9 U2 22 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0379-0738 EI 1872-6283 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD JUN PY 2015 VL 251 BP 56 EP 60 DI 10.1016/j.forsciint.2015.03.024 PG 5 WC Medicine, Legal SC Legal Medicine GA CH6DI UT WOS:000354125900012 PM 25863698 ER PT J AU Galache, JL Beeson, CL McLeod, KK Elvis, M AF Galache, J. L. Beeson, C. L. McLeod, K. K. Elvis, M. TI The need for speed in Near-Earth Asteroid characterization SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Asteroids; Asteroids' rotation; Near-Earth Objects; Orbit determination; Near-Earth Asteroids ID 101955 BENNU; OBJECTS; CHELYABINSK; POPULATION; MAGNITUDES; LIGHTCURVE; ROTATION; SYSTEM; ALBEDO; HAZARD AB We have used Minor Planet Center (MPG) data and tools to explore the discovery circumstances and properties of the currently known population of over 10,000 NEAs, and to quantify the challenges for follow-up from ground-based optical telescopes. The increasing rate of discovery has grown to similar to 1000/year as surveys have become more sensitive, by 1 mag every similar to 7.5 years. However, discoveries of large (H <= 22) NEAs have remained stable at similar to 365/year over the past decade, at which rate the 2005 Congressional mandate to find 90% of 140 m NEAs will not be met before 2030 (at least a decade late). Meanwhile, characterization is falling farther behind: Fewer than 10% of NEAs are well characterized in terms of size, rotation periods, and spectral composition, and at the current rates of follow-up it will take about a century to determine them even for the known population. Over 60% of NEAs have an orbital uncertainty parameter, U >= 4, making reacquisition more than a year following discovery difficult; for H > 22 this fraction is over 90%. We argue that rapid follow-up will be essential to characterize newly discovered NEAs. Most new NEAs are found within 0.5 mag of their peak brightness and fade quickly, typically by 0.5/3.5/5 mag after 1/4/6 weeks. About 80% have synodic periods of <3 years that would bring them close to Earth several times per decade. However follow-up observations on subsequent apparitions will be difficult or impossible for the bulk of new discoveries, as these will be smaller (H > 22) NEAs that tend to return 100 x fainter. We show that for characterization to keep pace with discovery would require: quick (within days) visible spectroscopy with a dedicated >2 m telescope; long-arc (months) astrometry, to be used also for phase curves, with a >= 4 m telescope; and fast-cadence (< min) light curves obtained rapidly (within days) with a >= 4 m telescope. For the already-known large (H <= 22) NEAs that tend to return to similar brightness, subsequent-apparition spectroscopy, astrometry, and photometry could be done with 1-2 m telescopes. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Galache, J. L.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA. [Beeson, C. L.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Beeson, C. L.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [McLeod, K. K.] Wellesley Coll, Whitin Observ, Wellesley, MA 02481 USA. RP Galache, JL (reprint author), Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, 60 Garden St, Cambridge, MA 02138 USA. EM jlgalache@cfa.harvard.edu; charlie.beeson@sky.com; kmcleod@wellesley.edu; melvis@cfa.harvard.edu FU NASA [NNX12AE89G] FX We thank both T. Spahr and G. Williams (MPC) for answering numerous questions, and the anonymous referees for keeping us honest and improving this paper through their inquisitiveness. C. Beeson thanks M. Trichas and J. Connolly for their guidance with Python coding; D. Polishook for an insight into NEA spectroscopy; and EE. DeMeo and RP. Binzel for crucial information with regard to spectroscopy. J.L. Galache was funded by NASA Grant NNX12AE89G. This research has made use of data and/or services provided by the International Astronomical Union's Minor Planet Center. NR 43 TC 3 Z9 3 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JUN PY 2015 VL 111 BP 155 EP 166 DI 10.1016/j.pss.2015.04.004 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8XJ UT WOS:000355054700014 ER PT J AU Lapinski, W Walther, P Tschapka, M AF Lapinski, Witold Walther, Paul Tschapka, Marco TI Morphology reflects microhabitat preferences in an assemblage of neotropical wandering spiders SO ZOOMORPHOLOGY LA English DT Article DE Ancylometes; Costa Rica; Ctenus; Cupiennius; Phoneutria; Trechalea ID HABITAT USE; ARANEAE; ATTACHMENT; PERFORMANCE; PISAURIDAE; LOCOMOTION; REVISION; ADHESION AB Coexistence is thought to be based mainly on interspecific differences in the use of limiting resources and habitat choice, both being associated with specific traits. We studied morphological parameters within an assemblage of large wandering spider species in Costa Rica subdivided into three subguilds: (1) semi-aquatic species, (2) forestground dwellers and (3) vegetation dwellers. We hypothesized that the observed differences between the spider species in microhabitat preferences and abilities to adhere to smooth surfaces should be associated with corresponding morphological traits. The leg scopulation patterns were surprisingly complex and reflected the ecological preferences of the spiders. We found that the scopulation patterns and the ratio of tarsus to leg length (T/L) appeared to be most important: the poor adhesion abilities of the semi-aquatic species were reflected by the absence of tarsal claw tufts, and these species also showed the highest T/L ratio. The forest-ground dwellers had smaller claw tufts relative to body mass than the vegetation dwellers that consistently showed the best adhesion performance. This study presents the first family-spanning ecomorphological analysis of an assemblage of large tropical wandering spiders. C1 [Lapinski, Witold; Tschapka, Marco] Univ Ulm, Evolutionary Ecol & Conservat Genom, D-89069 Ulm, Germany. [Walther, Paul] Univ Ulm, Electron Microscopy Dept, D-89069 Ulm, Germany. [Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. RP Lapinski, W (reprint author), Univ Ulm, Evolutionary Ecol & Conservat Genom, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM witold.lapinski@uni-ulm.de NR 34 TC 3 Z9 3 U1 0 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0720-213X EI 1432-234X J9 ZOOMORPHOLOGY JI Zoomorphology PD JUN PY 2015 VL 134 IS 2 BP 219 EP 236 DI 10.1007/s00435-015-0257-8 PG 18 WC Anatomy & Morphology; Zoology SC Anatomy & Morphology; Zoology GA CI0DH UT WOS:000354405600005 ER PT J AU Xia, SW Chen, J Schaefer, D Detto, M AF Xia, Shang-Wen Chen, Jin Schaefer, Doug Detto, Matteo TI Scale-dependent soil macronutrient heterogeneity reveals effects of litterfall in a tropical rainforest SO PLANT AND SOIL LA English DT Article DE Litterfall properties; Plant-soil feedback; Soil spatial heterogeneity; Topography; Wavelet analysis; Xishuangbanna ID SPATIAL HETEROGENEITY; SOUTHERN TAIWAN; LEAF-LITTER; COSTA-RICA; PATTERNS; NUTRIENTS; MANIPULATION; TOPOGRAPHY; NITROGEN; CHINA AB Aims Soil spatial heterogeneity is an important factor partitioning environmental niches and facilitating species coexistence, especially in tropical rainforests. However, fine-scale spatial variability of soil macronutrients and its causative factors are not well understood. We investigate this fine-scale variability and how it relates to environmental factors. Methods We conducted intensive soil sampling (361 samples) in a 1 ha plot in a tropical rainforest in Southwest China to investigate patterns of spatial heterogeneity in soil acidity and macronutrients and explored how the soil properties were influenced by topography and litterfall using a scale-wise wavelet analysis. Results Topography showed great variability at larger scales (>25 m) compared to litterfall properties, which peaked at about 25 m. Soil pH showed variation at large scales and was significantly correlated with topography, whereas soil total nitrogen, ammonium nitrogen, available phosphorus, and potassium showed variation at finer scales and were significantly correlated with litterfall chemical fluxes. A dominant species of canopy tree was non-randomly distributed in high litterfall input sites. Conclusions This study shows that fine-scale spatial variability of soil macronutrients is strongly influenced by litterfall chemical fluxes, highlighting the importance of biotic factors for understanding fine-scale patterns of soil heterogeneity in tropical rainforests. C1 [Xia, Shang-Wen; Chen, Jin; Schaefer, Doug] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Xishuangbanna 666303, Peoples R China. [Xia, Shang-Wen] Univ Chinese Acad Sci, Kunming Coll Life Sci, Beijing 100049, Peoples R China. [Detto, Matteo] Smithsonian Trop Res Inst, Ancon, Panama. RP Chen, J (reprint author), Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Xishuangbanna 666303, Peoples R China. EM cj@xtbg.org.cn NR 64 TC 4 Z9 4 U1 6 U2 30 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X EI 1573-5036 J9 PLANT SOIL JI Plant Soil PD JUN PY 2015 VL 391 IS 1-2 BP 51 EP 61 DI 10.1007/s11104-015-2402-z PG 11 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA CH7DZ UT WOS:000354197100004 ER PT J AU Rossman, AY Adams, GC Cannon, PF Castlebury, LA Crous, PW Gryzenhout, M Jaklitsch, WM Mejia, LC Stoykov, D Udayanga, D Voglmayr, H Walker, DM AF Rossman, Amy Y. Adams, Gerard C. Cannon, Paul F. Castlebury, Lisa A. Crous, Pedro W. Gryzenhout, Marieka Jaklitsch, Walter M. Mejia, Luis C. Stoykov, Dmitar Udayanga, Dhanushka Voglmayr, Hermann Walker, Donald M. TI Recommendations of generic names in Diaporthales competing for protection or use SO IMA FUNGUS LA English DT Article DE Article 59; Ascomycetes; Fungi; nomenclature; one fungus-one name; pleomorphic fungi; taxonomy; unit nomenclature AB In advancing to one name for fungi, this paper treats generic names competing for use in the order Diaporthales (Ascomycota, Sordariomycetes) and makes a recommendation for the use or protection of one generic name among synonymous names that may be either sexually or asexually typified. A table is presented that summarizes these recommendations. Among the genera most commonly encountered in this order, Cytospora is recommended over Valsa and Diaporthe over Phomopsis. New combinations are introduced for the oldest epithet of important species in the recommended genus. These include Amphiporthe tiliae, Coryneum lanciforme, Cytospora brevispora, C. ceratosperma, C. cinereostroma, C. eugeniae, C. fallax, C. myrtagena, Diaporthe amaranthophila, D. annonacearum, D. bougainvilleicola, D. caricae- papayae, D. cocoina, D. cucurbitae, D. juniperivora, D. leptostromiformis, D. pterophila, D. theae, D. vitimegaspora, Mastigosporella georgiana, Pilidiella angustispora, P. calamicola, P. pseudogranati, P. stromatica, and P. terminaliae. C1 [Rossman, Amy Y.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Adams, Gerard C.] Univ Nebraska, Dept Plant Pathol, Lincoln, NE 68503 USA. [Cannon, Paul F.] Royal Bot Gardens, Surrey TW9 3AB, England. [Castlebury, Lisa A.; Udayanga, Dhanushka] USDA ARS, Systemat Mycol & Microbiol Lab, Beltsville, MD 20705 USA. [Crous, Pedro W.] CBS KNAW Fungal Biodivers Inst, NL-3584 CT Utrecht, Netherlands. [Gryzenhout, Marieka] Univ Free State, Dept Plant Sci, ZA-9300 Bloemfontein, South Africa. [Jaklitsch, Walter M.] Univ Vienna, Dept Bot & Biodivers Res, Div Systemat & Evolutionary Bot, A-1030 Vienna, Austria. [Jaklitsch, Walter M.] BOKU Univ Nat Resources & Life Sci, Dept Forest & Soil Sci, Inst Forest Entomol Forest Pathol & Forest, A-1190 Vienna, Austria. [Mejia, Luis C.] Inst Sci Res & High Technol Serv INDICASAT AIP, Ctr Cellular & Mol Biol Dis, Panama City, Panama. [Mejia, Luis C.] Smithsonian Trop Res Inst, Balboa, Panama. [Stoykov, Dmitar] Bulgarian Acad Sci, Inst Biodivers & Ecosyst Res, Dept Plant & Fungal Divers & Resources, Sofia 113, Bulgaria. [Voglmayr, Hermann] Univ Vienna, Dept Bot & Biodivers Res, Div Systemat & Evolutionary Bot, A-1030 Vienna, Austria. [Walker, Donald M.] Findlay Univ, Dept Nat Sci, Findlay, OH 45840 USA. RP Rossman, AY (reprint author), Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. EM amydianer@yahoo.com FU Austrian Science Fund (FWF) [P27645-B16] FX Hermann Voglmayr acknowledges financial support by the Austrian Science Fund (FWF; project P27645-B16). NR 64 TC 16 Z9 16 U1 2 U2 6 PU INT MYCOLOGICAL ASSOC PI BERKELEY PA C/O J TAYLOR, DEPT PLANT & MICROBIAL BIOLOGY, BERKELEY, CA 94720 USA SN 2210-6340 EI 2210-6359 J9 IMA FUNGUS JI IMA Fungus PD JUN PY 2015 VL 6 IS 1 BP 145 EP 154 DI 10.5598/imafungus.2015.06.01.09 PG 10 WC Mycology SC Mycology GA V46UL UT WOS:000209909000021 PM 26203420 ER PT J AU Dittus, WPJ Gunathilake, KAS AF Dittus, Wolfgang P. J. Gunathilake, K. A. Sunil TI Validating skinfold thickness as a proxy to estimate total body fat in wild toque macaques (Macaca sinica) using the mass of dissected adipose tissue SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE wild primates; measuring adiposity; fat mass index; lean fatness; body composition ID FEMALE RHESUS-MONKEYS; PRIMATE POPULATION; NATURAL-POPULATION; CYNOMOLGUS MONKEYS; JAPANESE MACAQUES; NONHUMAN-PRIMATES; SEXUAL-DIMORPHISM; BABOONS PAPIO; OLIVE BABOONS; OBESITY AB Skinfold thickness (SFT) has been used often in non-human primates and humans as a proxy to estimate fatness (% body fat). We intended to validate the relation between SFT (in recently deceased specimens) and the mass of adipose tissue as determined from dissection of fresh carcasses of wild toque macaques (Macaca sinica). In adult male and female toque macaques body composition is normally 2% adipose tissue. Calipers for measuring SFT were suitable for measuring only some subcutaneous deposits of adipose tissue but were not suitable for measuring large fat deposits within the body cavity or minor intermuscular ones. The anatomical distribution of 13 different adipose deposits, in different body regions (subcutaneous, intra-abdominal and intermuscular) and their proportional size differences, were consistent in this species (as in other primates), though varying in total mass among individuals. These consistent allometric relationships were fundamental for estimating fatness of different body regions based on SFT. The best fit statistically significant correlations and regressions with the known masses of dissectible adipose tissue were evident between the SFT means of the seven sites measured, as well as with a single point on the abdomen anterior to the umbilicus. SFT related to total fat mass and intra-abdominal fat mass in curvilinear regressions and to subcutaneous fat mass in a linear relationship. To adjust for differences in body size among individuals, and to circumvent intangible variations in total body mass allocated, for example to the gastro-intestinal contents, dissected fat mass was estimated per unit body size (length of crown-rump)(3). SFT had greater coefficients of correlation and regressions with this Fat Mass Index (g/dm(3)) than with Percent Body Fat. Am. J. Primatol. 77:618-632, 2015. (c) 2015 Wiley Periodicals, Inc. C1 [Dittus, Wolfgang P. J.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC 20008 USA. [Dittus, Wolfgang P. J.] Natl Inst Fundamental Studies, Kandy, Sri Lanka. [Dittus, Wolfgang P. J.; Gunathilake, K. A. Sunil] Assoc Conservat Primate Divers, Polonnaruwa, Sri Lanka. RP Dittus, WPJ (reprint author), Smithsonian Primate Res Stn, New Town, New Town 51000, Polonnarwua, Sri Lanka. EM wdittus@gmail.com FU US National Science Foundation; Earthwatch Institute FX We thank Sumith Dissanayake, Nilantha Kodithuwakku, Kanchan Liyanage, Nadeera Weerasinghe for assistance in the field; Nirmala Basnayake and Chandra Handunge for office support; C.B. Dissanayake, the Director of the National Institute of Fundamental Studies (Sri Lanka) for research permits and John Seidensticker, Head of the Conservation Ecology Center, Smithsonian Conservation Biology Institute, National Zoological Park for administrative support. The manuscript benefited from comments by the editors, Donald Dunbar and Paul Garber, five anonymous reviewers, as well as by James Cheverud, Emma Crookenden, Clare Mosley, Michael Mosley and Rohan Pethiyagoda. Research was supported by the US National Science Foundation and the Earthwatch Institute. The methods of field observation and measurement comply with all laws and principles for the ethical treatment of research subjects of the National Institute of Fundamental Studies (Sri Lanka), the Smithsonian Conservation Biology Institute (USA) and American Society of Primatologists. NR 86 TC 0 Z9 0 U1 1 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD JUN PY 2015 VL 77 IS 6 BP 618 EP 632 DI 10.1002/ajp.22385 PG 15 WC Zoology SC Zoology GA CH9TS UT WOS:000354379900003 PM 25715692 ER PT J AU Gomez, CE Paul, VJ Ritson-Williams, R Muehllehner, N Langdon, C Sanchez, JA AF Gomez, C. E. Paul, V. J. Ritson-Williams, R. Muehllehner, N. Langdon, C. Sanchez, J. A. TI Responses of the tropical gorgonian coral Eunicea fusca to ocean acidification conditions SO CORAL REEFS LA English DT Article DE Ocean acidification; Carbonate saturation state; Tropical gorgonian; Caribbean; Calcein ID LEPTOGORGIA-VIRGULATA LAMARCK; MEDITERRANEAN RED CORAL; COMMUNITY STRUCTURE; CARBON-DIOXIDE; CALCIFICATION; GROWTH; REEFS; OCTOCORALLIA; SEAWATER; CALCIUM AB Ocean acidification can have negative repercussions from the organism to ecosystem levels. Octocorals deposit high-magnesium calcite in their skeletons, and according to different models, they could be more susceptible to the depletion of carbonate ions than either calcite or aragonite-depositing organisms. This study investigated the response of the gorgonian coral Eunicea fusca to a range of CO2 concentrations from 285 to 4,568 ppm (pH range 8.1-7.1) over a 4-week period. Gorgonian growth and calcification were measured at each level of CO2 as linear extension rate and percent change in buoyant weight and calcein incorporation in individual sclerites, respectively. There was a significant negative relationship for calcification and CO2 concentration that was well explained by a linear model regression analysis for both buoyant weight and calcein staining. In general, growth and calcification did not stop in any of the concentrations of pCO(2); however, some of the octocoral fragments experienced negative calcification at undersaturated levels of calcium carbonate (> 4,500 ppm) suggesting possible dissolution effects. These results highlight the susceptibility of the gorgonian coral E. fusca to elevated levels of carbon dioxide but suggest that E. fusca could still survive well in mid-term ocean acidification conditions expected by the end of this century, which provides important information on the effects of ocean acidification on the dynamics of coral reef communities. Gorgonian corals can be expected to diversify and thrive in the Atlantic-Eastern Pacific; as scleractinian corals decline, it is likely to expect a shift in these reef communities from scleractinian coral dominated to octocoral/soft coral dominated under a "business as usual" scenario of CO2 emissions. C1 [Gomez, C. E.; Sanchez, J. A.] Univ Los Andes, Lab Biol Mol Marina BIOMMAR, Dept Ciencias Biol, Fac Ciencias, Bogota, Colombia. [Gomez, C. E.; Paul, V. J.; Ritson-Williams, R.] Smithsonian Marine Stn, Ft Pierce, FL USA. [Gomez, C. E.] Temple Univ, Dept Biol, Philadelphia, PA 19122 USA. [Muehllehner, N.; Langdon, C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Marine Biol & Ecol, Miami, FL 33149 USA. RP Sanchez, JA (reprint author), Univ Los Andes, Lab Biol Mol Marina BIOMMAR, Dept Ciencias Biol, Fac Ciencias, Carrera 1E 18A 10, Bogota, Colombia. EM juansanc@uniandes.edu.co RI Johnson, Selena/K-3541-2013; OI Sanchez, Juan Armando/0000-0001-7149-8369 FU Smithsonian Institution Scholarly Studies Program; Smithsonian Marine Station at Fort Pierce (SMSFP); Coral and Climate Change Laboratory (RSMAS-University of Miami); Facultad de Ciencias, Universidad de los Andes; COLCIENCIAS [1204-521-28867] FX The Smithsonian Institution Scholarly Studies Program and the Smithsonian Marine Station at Fort Pierce (SMSFP) through the Hunterdon Oceanographic Endowment funded this study. Additional support was received from the Coral and Climate Change Laboratory (RSMAS-University of Miami) for use of the CO2 system as well as Facultad de Ciencias, Universidad de los Andes and COLCIENCIAS (1204-521-28867). We greatly appreciate the collaboration of SMSFP staff, H. Reichardt, J. Piraino, S. Reed. Special thanks to S. Gunasekera, M. Boyle, J. Craft and W. Hoffman (SMSFP) and C. Mor and R. Okasaki (University of Miami). We thank Simon Davy and two anonymous reviewers for their constructive comments that greatly improved this manuscript. This is contribution #968 of the SMSFP. NR 66 TC 2 Z9 2 U1 4 U2 63 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 JUN PY 2015 VL 34 IS 2 BP 451 EP 460 DI 10.1007/s00338-014-1241-3 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CH7BC UT WOS:000354189600008 ER PT J AU Teitelbaum, CS Fagan, WF Fleming, CH Dressler, G Calabrese, JM Leimgruber, P Mueller, T AF Teitelbaum, Claire S. Fagan, William F. Fleming, Chris H. Dressler, Gunnar Calabrese, Justin M. Leimgruber, Peter Mueller, Thomas TI How far to go? Determinants of migration distance in land mammals SO ECOLOGY LETTERS LA English DT Article DE Foraging resources; land migrations; mammalian herbivores; migration distance; normalised difference vegetation index; scaling relationships; ungulates ID DIFFERENCE VEGETATION INDEX; HOME RANGE SIZE; MONGOLIAN GAZELLES; MOVEMENT PATTERNS; TIME-SERIES; ROE DEER; NDVI; MODELS; PRODUCTIVITY; TERRESTRIAL AB Animal migration is a global phenomenon, but few studies have examined the substantial within- and between-species variation in migration distances. We built a global database of 94 land migrations of large mammalian herbivore populations ranging from 10 to 1638km. We examined how resource availability, spatial scale of resource variability and body size affect migration distance among populations. Resource availability measured as normalised difference vegetation index had a strong negative effect, predicting a tenfold difference in migration distances between low- and high-resource areas and explaining 23% of the variation in migration distances. We found a weak, positive effect of the spatial scale of resource variability but no effect of body size. Resource-poor environments are known to increase the size of mammalian home ranges and territories. Here, we demonstrate that for migratory populations as well, animals living in resource-poor environments travel farther to fulfil their resource needs. C1 [Teitelbaum, Claire S.; Mueller, Thomas] Senckenberg Gesell Nat Forsch, Senckenberg Biodivers & Climate Res Ctr, D-60325 Frankfurt, Germany. [Teitelbaum, Claire S.; Mueller, Thomas] Goethe Univ Frankfurt, Dept Biol Sci, D-60438 Frankfurt, Germany. [Teitelbaum, Claire S.; Fagan, William F.; Dressler, Gunnar; Mueller, Thomas] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Fleming, Chris H.; Calabrese, Justin M.; Leimgruber, Peter; Mueller, Thomas] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Teitelbaum, CS (reprint author), Senckenberg Gesell Nat Forsch, Senckenberg Biodivers & Climate Res Ctr, Senckenberganlage 25, D-60325 Frankfurt, Germany. EM claire.teitelbaum@gmail.com RI Calabrese, Justin/B-9131-2012; Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 NR 48 TC 6 Z9 6 U1 12 U2 75 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 JUN PY 2015 VL 18 IS 6 BP 545 EP 552 DI 10.1111/ele.12435 PG 8 WC Ecology SC Environmental Sciences & Ecology GA CH9SH UT WOS:000354376100006 PM 25865946 ER PT J AU Bohlman, SA AF Bohlman, Stephanie A. TI Species Diversity of Canopy Versus Understory Trees in a Neotropical Forest: Implications for Forest Structure, Function and Monitoring SO ECOSYSTEMS LA English DT Article DE species diversity; forest canopy; forest dynamics; crown layers; forest structure; stereophotographs; remote sensing; tropical forest ID TROPICAL RAIN-FORESTS; BARRO-COLORADO ISLAND; HABITAT ASSOCIATIONS; RADIATION REGIME; SPATIAL-PATTERNS; MORTALITY-RATES; MODELING BRF; PANAMA; DYNAMICS; GROWTH AB Species composition and diversity of the canopy layer of tropical forests have rarely been described, yet they are important to many aspects of ecosystem structure and function. Species composition was compared among canopy trees (defined as sun-exposed crowns), understory trees, trees a parts per thousand yen10-cm diameter at breast height (DBH), and the tree community as a whole in a Neotropical moist forest. High-resolution stereophotographs were used to map all individual canopy tree crowns in 8.6 ha of a 50-ha forest dynamics plot on Barro Colorado Island (BCI), Panama. The canopy was found to have high species diversity in relation to the understory and the whole forest. Only 5% of the stems were found in the canopy, but it contained 70% of the species. Diversity, standardized by stem count, for the canopy (a parts per thousand 135 species per 1000 trees) was higher than that of the forest as a whole (a parts per thousand 108 species per 1000 trees), and species composition was different between the two communities. Although only 50% of trees a parts per thousand yen10-cm DBH, the typical size range used in many forest inventories, were in the canopy, the species diversity and composition of the canopy and trees a parts per thousand yen10-cm DBH were nearly identical. The percentage of gap species in the canopy increased with tree size, providing evidence of the dynamic nature of the BCI forest. To the degree that tree function, such as carbon uptake and transpiration, vary among species, the rarified species richness of the canopy will generate high functional diversity at local-to-landscape scales. C1 [Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Bohlman, Stephanie A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Bohlman, SA (reprint author), Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. EM sbohlman@ufl.edu FU National Science Foundation; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Small World Institute Fund FX Richard Grotefendt of Grotefendt Photogrammetric Services took and processed the stereo photographs and assisted with crown digitizing. Andrew Hida provided much of the field work for the stereo photographs. The stereo photograph collection, field-truthing and analysis were supported under a NASA Earth Systems Science Fellowship and Center for Tropical Forest Science (CTFS) research grant. The BCI forest dynamics research project was made possible by the National Science Foundation grants to Stephen P. Hubbell, and supports 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 over 100 people from 10 countries over the last two decades. The plot project is part of CTFS, a global network of large-scale demographic tree plots. NR 72 TC 1 Z9 1 U1 6 U2 45 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-9840 EI 1435-0629 J9 ECOSYSTEMS JI Ecosystems PD JUN PY 2015 VL 18 IS 4 BP 658 EP 670 DI 10.1007/s10021-015-9854-0 PG 13 WC Ecology SC Environmental Sciences & Ecology GA CH6DM UT WOS:000354126300008 ER PT J AU Maire, V Wright, IJ Prentice, IC Batjes, NH Bhaskar, R van Bodegom, PM Cornwell, WK Ellsworth, D Niinemets, U Ordonez, A Reich, PB Santiago, LS AF Maire, Vincent Wright, Ian J. Prentice, I. Colin Batjes, Niels H. Bhaskar, Radika van Bodegom, Peter M. Cornwell, Will K. Ellsworth, David Niinemets, Uelo Ordonez, Alejandro Reich, Peter B. Santiago, Louis S. TI Global effects of soil and climate on leaf photosynthetic traits and rates SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Least-cost theory of photosynthesis; nitrogen; phosphorus; photosynthesis; plant functional traits; soil fertility; soil pH; stomatal conductance ID ECONOMICS SPECTRUM; NITROGEN; NUTRIENT; WATER; VARIABILITY; PHOSPHORUS; CARBON; PRECIPITATION; TEMPERATURE; PATTERNS AB AimThe influence of soil properties on photosynthetic traits in higher plants is poorly quantified in comparison with that of climate. We address this situation by quantifying the unique and joint contributions to global leaf-trait variation from soils and climate. LocationTerrestrial ecosystems world-wide. MethodsUsing a trait dataset comprising 1509 species from 288 sites, with climate and soil data derived from global datasets, we quantified the effects of 20 soil and 26 climate variables on light-saturated photosynthetic rate (A(area)), stomatal conductance (g(s)), leaf nitrogen and phosphorus (N-area and P-area) and specific leaf area (SLA) using mixed regression models and multivariate analyses. ResultsSoil variables were stronger predictors of leaf traits than climatic variables, except for SLA. On average, N-area, P-area and A(area) increased and SLA decreased with increasing soil pH and with increasing site aridity. g(s) declined and P-area increased with soil available P (P-avail). N-area was unrelated to total soil N. Joint effects of soil and climate dominated over their unique effects on N-area and P-area, while unique effects of soils dominated for A(area) and g(s). Path analysis indicated that variation in A(area) reflected the combined independent influences of N-area and g(s), the former promoted by high pH and aridity and the latter by low P-avail. Main conclusionsThree environmental variables were key for explaining variation in leaf traits: soil pH and P-avail, and the climatic moisture index (the ratio of precipitation to potential evapotranspiration). Although the reliability of global soil datasets lags behind that of climate datasets, our results nonetheless provide compelling evidence that both can be jointly used in broad-scale analyses, and that effects uniquely attributable to soil properties are important determinants of leaf photosynthetic traits and rates. A significant future challenge is to better disentangle the covarying physiological, ecological and evolutionary mechanisms that underpin trait-environment relationships. C1 [Maire, Vincent; Wright, Ian J.; Prentice, I. Colin] Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. [Prentice, I. Colin] Univ London Imperial Coll Sci Technol & Med, AXA Chair Biosphere & Climate Impacts Grand Chall, Ascot SL57PY, Berks, England. [Prentice, I. Colin] Univ London Imperial Coll Sci Technol & Med, Grantham Inst Climate Change & Environm, Dept Life Sci, Ascot SL57PY, Berks, England. [Batjes, Niels H.] ISRIC World Soil Informat, NL-6700 AJ Wageningen, Netherlands. [Bhaskar, Radika] Brown Univ, Environm Change Initiat, Providence, RI 02912 USA. [van Bodegom, Peter M.] Leiden Univ, Inst Environm Sci, NL-2333 CC Leiden, Netherlands. [Cornwell, Will K.] Vrije Univ Amsterdam, Inst Ecol Sci, Dept Syst Ecol, NL-1081 HV Amsterdam, Netherlands. [Cornwell, Will K.] Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. [Ellsworth, David; Reich, Peter B.] Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2751, Australia. [Niinemets, Uelo] Estonian Univ Life Sci, Inst Agr & Environm Sci, EE-51014 Tartu, Estonia. [Ordonez, Alejandro] Aarhus Univ, Dept Biosci, Aarhus, Denmark. [Reich, Peter B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Santiago, Louis S.] Univ Calif Riverside, Bot & Plant Sci Dept, Riverside, CA 92521 USA. [Santiago, Louis S.] Smithsonian Trop Res Inst, Panama City, Panama. RP Maire, V (reprint author), Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. EM vmaire24@gmail.com RI Batjes, Niels/F-7195-2010; Wright, Ian/G-4979-2012; van Bodegom, Peter/N-8150-2015; Santiago, Louis/E-3185-2016; Niinemets, Ulo/A-3816-2008; OI Batjes, Niels/0000-0003-2367-3067; Wright, Ian/0000-0001-8338-9143; van Bodegom, Peter/0000-0003-0771-4500; Santiago, Louis/0000-0001-5994-6122; Niinemets, Ulo/0000-0002-3078-2192; Cornwell, Will/0000-0003-4080-4073; Ordonez, Alejandro/0000-0003-2873-4551 FU ARC [DP120103600, FT100100910]; Macquarie University FX We thank the many data contributors, including Claudia Keitel, Fernando Valladares and Margaret Barbour; Allyson Eller, Sean Gleason, Pedro Peres-Neto, Mark Westoby and the Wright lab for stimulating discussions; and Bjorn Reu and one anonymous referee who challenged us to clarify our analytical approach. The research was supported by ARC grants DP120103600 to I.C.P. and I.J.W. and FT100100910 to I.J.W., and by funding from Macquarie University. This paper is a contribution to the AXA Chair Programme in Biosphere and Climate Impacts and the Imperial College initiative on Grand Challenges in Ecosystems and the Environment. NR 50 TC 22 Z9 22 U1 21 U2 141 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 JUN PY 2015 VL 24 IS 6 BP 706 EP 717 DI 10.1111/geb.12296 PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA CH6BV UT WOS:000354121600010 ER PT J AU Tanpradit, N Comizzoli, P Srisuwatanasagul, S Chatdarong, K AF Tanpradit, Nae Comizzoli, Pierre Srisuwatanasagul, Sayamon Chatdarong, Kaywalee TI Positive impact of sucrose supplementation during slow freezing of cat ovarian tissues on cellular viability, follicle morphology, and DNA integrity SO THERIOGENOLOGY LA English DT Article DE Domestic cat; Connexin 43; Cryopreservation; Ovarian tissue; Vitrification; Sucrose ID CRYOPROTECTIVE AGENTS; PRIMORDIAL FOLLICLES; VASCULAR PEDICLE; GAP-JUNCTIONS; HUMAN OOCYTES; WILD FELIDS; IN-SITU; CRYOPRESERVATION; PRESERVATION; CORTEX AB The objectives of the study were to (1) examine and optimize the impact of sucrose during slow freezing and (2) compare the results of two freezing methods (slow freezing and vitrification) on cellular viability (germinal and stromal cells), follicle morphology, DNA integrity, and gap junction protein expression (connexin 43 [Cx 43]). Different sucrose supplementations (0, 0.1, and 0.3 M) in standard freezing medium were compared before and after slow freezing. Ovarian tissue slow frozen using 0.1- (4.0 +/- 0.4) or 0.3-M sucrose (3.9 +/- 0.5) yielded better follicular viability (number of positive follicles per 0.0625 mm(2)) than the group without sucrose (1.9 +/- 0.2; P < 0.05). Morphologically normal primordial follicles were higher in the sucrose-treated groups (0.1 M, 47.4% and 0.3 M, 43.5%) than the group without sucrose (0 M, 33.8%; P < 0.05). Moreover, less apoptotic primordial follicles were found in both sucrose groups (0.1 M, 1.2% and 0.3 M, 1.9%) than the group without sucrose (7.7%; P < 0.05). However, their Cx 43 expression showed no difference among the groups of different sucrose concentrations. In terms of the freezing methods used, vitrified ovarian tissues had fewer viable follicles (3.2 +/- 0.6) than the slow-freezing method (4.6 +/- 0.6; P < 0.05). In addition, the slow freezing resulted in more postthawed morphologically normal primordial follicles (38.8% vs. 28.3%, P < 0.05) and less apoptotic primordial follicles (3.8% vs. 8.9%, P < 0.05) than vitrification. The Cx 43 expression showed no difference between slow freezing and vitrification. The present study reported the positive effects of sucrose supplementation and slow-freezing method on the follicular viability, follicular histologic appearances of follicles, and apoptosis of the follicles and stromal cells in cat ovarian tissues. (C) 2015 Elsevier Inc. All rights reserved. C1 [Tanpradit, Nae; Chatdarong, Kaywalee] Chulalongkorn Univ, Fac Vet Sci, Dept Obstet Gynaecol & Reprod, Bangkok, Thailand. [Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Species Survival, Washington, DC USA. [Srisuwatanasagul, Sayamon] Chulalongkorn Univ, Fac Vet Sci, Dept Anat, Bangkok, Thailand. RP Chatdarong, K (reprint author), Chulalongkorn Univ, Fac Vet Sci, Dept Obstet Gynaecol & Reprod, Bangkok, Thailand. EM kaywalee.c@chula.ac.th OI Chatdarong, Kaywalee/0000-0002-9470-8426 FU Royal Golden Jubilee Ph.D. Program [PHD/0199/2552]; 90th Anniversary of Chulalongkorn University Fund (Ratchadaphiseksomphot Endowment Fund); Research Unit of Obstetrics and Reproduction in Animals, Chulalongkorn University FX Financial support for a part of this work was provided by the Royal Golden Jubilee Ph.D. Program (PHD/0199/2552), the 90th Anniversary of Chulalongkorn University Fund (Ratchadaphiseksomphot Endowment Fund), and Research Unit of Obstetrics and Reproduction in Animals, Chulalongkorn University. The authors would like to thank Division of Obstetrics, Gynaecology and Reproduction, Small Animal Teaching Hospital, Faculty of Veterinary Science, Chulalongkorn University; the Veterinary Public Health Division of the Bangkok Metropolitan Administration, Thailand, for providing cat ovaries; Asst. Prof. Dr Sukanya Manee-in for her technical assistance on immunohistochemical assessment; and Assc. Prof. Dr Padet Tummaruk for helping with statistical analysis. NR 50 TC 5 Z9 7 U1 1 U2 9 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 JUN PY 2015 VL 83 IS 9 BP 1553 EP 1561 DI 10.1016/j.theriogenology.2015.01.035 PG 9 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA CH3LE UT WOS:000353931400022 PM 25747194 ER PT J AU Dohm, JM Hare, TM Robbins, SJ Williams, JP Soare, RJ El-Maarry, MR Conway, SJ Buczkowski, DL Kargel, JS Banks, ME Fairen, AG Schulze-Makuch, D Komatsu, G Miyamoto, H Anderson, RC Davila, AF Mahaney, WC Fink, W Cleaves, KJ Yan, J Hynek, B Maruyama, S AF Dohm, J. M. Hare, T. M. Robbins, S. J. Williams, J. -P. Soare, R. J. El-Maarry, M. R. Conway, S. J. Buczkowski, D. L. Kargel, J. S. Banks, M. E. Fairen, A. G. Schulze-Makuch, D. Komatsu, G. Miyamoto, H. Anderson, R. C. Davila, A. F. Mahaney, W. C. Fink, W. Cleaves, K. J. Yan, J. Hynek, B. Maruyama, S. TI Geological and hydrological histories of the Argyre province, Mars SO ICARUS LA English DT Article DE Mars; Geological processes; Astrobiology; Tectonics ID SURFACE GROUND ICE; MAGNETIC-FIELD; ANTARCTIC PALEOSOLS; VALLES MARINERIS; NORTHERN PLAINS; CLIMATE-CHANGE; SLOPE STREAKS; IMPACT BASIN; EVOLUTION; SYSTEM AB The geologic history of the multi-ringed Argyre impact basin and surroundings has been reconstructed on the basis of geologic mapping and relative-age dating of rock materials and structures. The impact formed a primary basin, rim materials, and a complex basement structural fabric including faults and valleys that are radial and concentric about the primary basin, as well as structurally-controlled local basins. Since its formation, the basin has been a regional catchment for volatiles and sedimentary materials as well as a dominant influence on the flow of surface ice, debris flows, and groundwater through and over its basement structures. The basin is interpreted to have been occupied by lakes, including a possible Mediterranean-sized sea that formed in the aftermath of the Argyre impact event The hypothesized lakes froze and diminished through time, though liquid water may have remained beneath the ice cover and sedimentation may have continued for some time. At its deepest, the main Argyre lake may have taken more than a hundred thousand years to freeze to the bottom even absent any heat source besides the Sun, but with impact-induced hydrothermal heat, geothermal heat flow due to long-lived radioactivities in early martian history, and concentration of solutes in sub-ice brine, liquid water may have persisted beneath thick ice for many millions of years. Existence of an ice-covered sea perhaps was long enough for life to originate and evolve with gradually colder and more hypersaline conditions. The Argyre rock materials, diverse in origin and emplacement mechanisms, have been modified by impact, magmatic, eolian, fluvial, lacustrine, glacial, periglacial, alluvial, colluvial, and tectonic processes. Post-impact adjustment of part of the impact-generated basement structural fabric such as concentric faults is apparent. Distinct basin-stratigraphic units are interpreted to be linked to large-scale geologic activity far from the basin, including growth of the Tharsis magmatic-tectonic complex and the growth into southern middle latitudes of south polar ice sheets. Along with the migration of surface and sub-surface volatiles towards the central part of the primaiy basin, the substantial difference in elevation with respect to the surrounding highlands and Tharsis and the Thaumasia highlands result in the trapping of atmospheric volatiles within the basin in the form of fog and regional or local precipitation, even today. In addition, the impact event caused long-term (millions of years) hydrothermal activity, as well as deep-seated basement structures that have tapped the internal heat of Mars, as conduits, for far greater time, possibly even today. This possibility is raised by the observation of putative open-system pingos and nearby gullies that occur in linear depressions with accompanying systems of faults and fractures. Long-term water and heat energy enrichment, complemented by the interaction of the nutrient-enriched primordial crustal and mantle materials favorable to life excavated to the surface and near-surface environs through the Argyre impact event, has not only resulted in distinct geomorphology, but also makes the Argyre basin a potential site of exceptional astrobiological significance. (C) 2015 Elsevier Inc. All rights reserved. C1 [Dohm, J. M.; Miyamoto, H.] Univ Tokyo, Univ Museum, Bunkyo Ku, Tokyo 1130033, Japan. [Hare, T. M.] US Geol Survey, Flagstaff, AZ 86001 USA. [Robbins, S. J.] SW Res Inst, Boulder, CO 80302 USA. [Williams, J. -P.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Soare, R. J.] Dawson Coll, Dept Geog, Montreal, PQ H3Z 1A4, Canada. [El-Maarry, M. R.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Conway, S. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Buczkowski, D. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Kargel, J. S.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Banks, M. E.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Banks, M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Fairen, A. G.] Ctr Astrobiol, Dept Planetol & Habitabil, Madrid 28850, Spain. [Fairen, A. G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Schulze-Makuch, D.] Tech Univ Berlin, Ctr Astron & Astrophys, D-10623 Berlin, Germany. [Komatsu, G.] Univ Annunzio, Int Res Sch Planetary Sci, I-65421 Pescara, Italy. [Anderson, R. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Davila, A. F.] SETI Inst, Mountain View, CA 94043 USA. [Mahaney, W. C.] Quaternary Surveys, Thornhill, ON L4J 1J4, Canada. [Fink, W.] Univ Arizona, Dept Elect & Comp Engn, Coll Engn, Tucson, AZ 85721 USA. [Cleaves, K. J.; Maruyama, S.] Tokyo Inst Technol, Earth Life Sci Inst, Tokyo 1528551, Japan. [Cleaves, K. J.] Inst Adv Study, Princeton, NJ 08540 USA. [Yan, J.] Natl Astron Observ Japan, RISE Project Off, Oshu 0230861, Japan. [Hynek, B.] Univ Colorado, Lab Atmospher & Space Phys & Geol Sci, Boulder, CO 80309 USA. RP Dohm, JM (reprint author), Univ Tokyo, Univ Museum, Bunkyo Ku, Hongo 7-3-1, Tokyo 1130033, Japan. EM jmd@um.u-tokyo.ac.jp RI Williams, Jean-Pierre/C-3531-2009; Komatsu, Goro/I-7822-2012; Miyamoto, Hideaki/B-9666-2008; Maruyama, Shigenori/C-8288-2009; OI Williams, Jean-Pierre/0000-0003-4163-2760; Komatsu, Goro/0000-0003-4155-108X; Conway, Susan/0000-0002-0577-2312; EL-MAARRY, MOHAMED RAMY/0000-0002-8262-0320; Hare, Trent/0000-0001-8842-389X; Schulze-Makuch, Dirk/0000-0002-1923-9746; Cleaves, Henderson/0000-0003-4101-0654 FU National Aeronautics and Space Administration (NASA) Planetary Geology & Geophysics Program; Tokyo Dome Corporation; European Research Council under the European Union's Seventh Framework Programme (FP7), ERC [307496] FX J.M. Dohm was supported by the National Aeronautics and Space Administration (NASA) Planetary Geology & Geophysics Program. Professors Dohm and Miyamoto express their gratitude to the Tokyo Dome Corporation for their support of the TeNQ exhibit and the branch of Space Exploration Education & Discovery, the University Museum, the University of Tokyo. Work by A.G. Fairen was supported by the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013), ERC Grant agreement No. 307496. We are grateful for the thoughtful reviews by T. Ohman and an anonymous reviewer which ultimately resulted in an improved manuscript. NR 195 TC 9 Z9 9 U1 3 U2 42 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 JUN PY 2015 VL 253 BP 66 EP 98 DI 10.1016/j.icarus.2015.02.017 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH1BD UT WOS:000353755200007 ER PT J AU Pfaller, JB Alfaro-Shigueto, J Giffoni, B Ishihara, T Mangel, JC Peckham, SH Bjorndal, KA Baeza, JA AF Pfaller, Joseph B. Alfaro-Shigueto, Joanna Giffoni, Bruno Ishihara, Takashi Mangel, Jeffrey C. Peckham, S. Hoyt Bjorndal, Karen A. Antonio Baeza, J. TI Social monogamy in the crab Planes major, a facultative symbiont of loggerhead sea turtles (vol 461, pg 124, 2014) SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Correction C1 [Pfaller, Joseph B.; Bjorndal, Karen A.] Univ Florida, Archie Carr Ctr Sea Turtle Res, Gainesville, FL 32611 USA. [Pfaller, Joseph B.; Bjorndal, Karen A.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Pfaller, Joseph B.] Caretta Res Project, Savannah, GA 31412 USA. [Alfaro-Shigueto, Joanna; Mangel, Jeffrey C.] ProDelphinus, Lima 18, Peru. [Alfaro-Shigueto, Joanna; Mangel, Jeffrey C.] Univ Exeter, Ctr Ecol & Conservat, Penryn TR10 9EZ, Cornwall, England. [Giffoni, Bruno] Fundacao Pro TAMAR, BR-11680000 Ubatuba, SP, Brazil. [Ishihara, Takashi] Sea Turtle Assoc Japan, Osaka, Japan. [Ishihara, Takashi] Suma Aqualife Pk, Kobe, Hyogo, Japan. [Peckham, S. Hoyt] Stanford Univ, Ctr Ocean Solut, Stanford, CA 94305 USA. [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, Fac Ciencias Mar, Dept Biol Marina, Coquimbo, Chile. RP Pfaller, JB (reprint author), Univ Florida, Archie Carr Ctr Sea Turtle Res, 220 Bartram Hall, Gainesville, FL 32611 USA. EM jpfaller@ufl.edu; jas_26@yahoo.com; bruno@tamar.org.br; ishihara@umigame.org; jeffrey_mangel@yahoo.com; hoyt@propeninsula.org; bjorndal@ufl.edu; baeza.antonio@gmail.com NR 1 TC 0 Z9 0 U1 1 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD JUN PY 2015 VL 467 BP 121 EP 121 DI 10.1016/j.jembe.2015.03.001 PG 1 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA CH0WR UT WOS:000353743600016 ER PT J AU Kim, C Deng, T Wen, J Nie, ZL Sun, H AF Kim, Changkyun Deng, Tao Wen, Jun Nie, Ze-Long Sun, Hang TI Systematics, biogeography, and character evolution of Deutzia (Hydrangeaceae) inferred from nuclear and chloroplast DNA sequences SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Biogeography; Character evolution; Dating analysis; Deutzia; Molecular phylogeny; Infrageneric classification ID QINGHAI-TIBETAN PLATEAU; PHYLOGENETIC ANALYSIS; NORTHERN-HEMISPHERE; COMPARATIVE ANATOMY; MORPHOLOGICAL DATA; EARLY MIOCENE; RBCL; DIVERSIFICATION; SAXIFRAGACEAE; CORNALES AB The genus Deutzia (Hydrangeaceae), containing ca. 60 species circumscribed in three sections, is disjunctly distributed in eastern Asia and Central America (Mexico). Although the genus is well delimited, its subdivisions into sections and series have not been the subject of an explicit test of monophyly based on molecular data. A comprehensive examination of the evolutionary relationships within the genus is thus still lacking. We present a fossil-calibrated, molecular phylogeny of Deutzia based on two nuclear ribosomal DNA (ITS and 26S) and three chloroplast DNA regions (matK, rbcL, and trnL-F intergenic spacer). Within this framework, we examine character evolution in petal arrangement, filament shape, and the number of stamens, and infer the ancestral area and biogeographic history of the genus. Our molecular phylogeny suggests that Deutzia is monophyletic. Two major clades are recovered: one composed of the species of sect. Neodeutzia from Mexico, and the other containing all remaining Deutzia species of sections Mesodeutzia and Deutzia from SW China and Northeast Asia. The latter two Asian sections were each revealed to be polyphyletic. The induplicate petals, 2-dentate filaments, and polystemonous androecia are inferred to be ancestral character states. Biogeographic reconstructions suggest a Northeast Asian origin for the genus and subsequent spread to Mexico during the Oligocene and to SW China during the Miocene. Based on our results, a new infrageneric classification of Deutzia inferred from molecular phylogeny is required. We propose to merge sections Mesodeutzia and Deutzia to ensure the monophyly at the sectional level. Cooling trends during the Oligocene resulted in isolation, separating eastern Asian and Mexican taxa, while the warm period during the middle Miocene stimulated the diversification from Northeast Asia to SW China. The uplift in the Qinghai-Tibetan Plateau and monsoon regimes are important in promoting high species diversification of Deutzia in SW China. (C) 2015 Elsevier Inc. All rights reserved. C1 [Kim, Changkyun; Deng, Tao; Nie, Ze-Long; Sun, Hang] Chinese Acad Sci, Kunming Inst Bot, Key Lab Plant Biodivers & Biogeog East Asia, Kunming 650204, Yunnan, Peoples R China. [Deng, Tao] Yunnan Univ, Sch Life Sci, Kunming 650091, Peoples R China. [Deng, Tao] Univ Chinese Acad Sci, Beijing 100039, Peoples R China. [Wen, Jun] Smithsonian Inst, MRC 166, Dept Bot, Washington, DC 20013 USA. RP Sun, H (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Plant Biodivers & Biogeog East Asia, 132 Lanhei Rd, Kunming 650204, Yunnan, Peoples R China. EM hsun@mail.kib.ac.cn FU Chinese Academy of Sciences [XDB03030112]; Hundred Talents Program of the Chinese Academy of Sciences [2011312D11022]; Yunnan Natural Science Foundation; National Natural Science Foundation of China [U1136601, 31129001]; CAS/SAFEA International Partnership Program for Creative Research Teams; Key Laboratory of Biodiversity and Biogeography, Kunming Institute of Botany, CAS [Y0205111L1] FX The authors thank the following people and institutions that helped with field collections or provision of plant material: D.E. Boufford (Harvard University), H.-K. Choi and Y.I. Ryu (Ajou University), D.G. Zhang and Y. Chen (Jishou University), J.W. Zhang, X. Li, Y. Niu, Q, Wang, and B. Yang (Kunming Institute of Botany), Ajou University (AJOU), New York Botanical Garden (NY), Institute of Botany, Chinese Academy of Sciences (PE), and the US National Herbarium of Smithsonian Institution (US). This work was supported by grants from the research program for "Strategic Priority Research Program (B)" of the Chinese Academy of Sciences (Grant no. XDB03030112), Hundred Talents Program of the Chinese Academy of Sciences (2011312D11022), Yunnan Natural Science Foundation and National Natural Science Foundation of China (No. U1136601 and No. 31129001), and the CAS/SAFEA International Partnership Program for Creative Research Teams to H. Sun and Postdoctoral Scholar, Key Laboratory of Biodiversity and Biogeography, Kunming Institute of Botany, CAS (No. Y0205111L1) to C. Kim. NR 80 TC 0 Z9 1 U1 9 U2 30 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 JUN PY 2015 VL 87 BP 91 EP 104 DI 10.1016/j.ympev.2015.03.002 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CG5XH UT WOS:000353368700008 PM 25776523 ER PT J AU Hammer, TJ Van Bael, SA AF Hammer, Tobin J. Van Bael, Sunshine A. TI An endophyte-rich diet increases ant predation on a specialist herbivorous insect SO ECOLOGICAL ENTOMOLOGY LA English DT Article DE Acromis sparsa; Azteca lacrymosa; endophytic fungi; insect herbivory; Merremia umbellata; multitrophic interactions ID TROPICAL FUNGAL ENDOPHYTES; LARVAL TORTOISE BEETLE; MYCORRHIZAL FUNGI; SHIELD DEFENSE; TALL FESCUE; PLANT; GRASSES; FOLIAR; PARASITOIDS; COMMUNITIES AB 1. All plants form symbioses with microfungi, known as endophytes, which live within plant tissues. Numerous studies have documented endophyte-herbivore antagonism in grass systems, but plant-endophyte-insect interactions are highly variable for forbs and woody plants. 2. The net effect of endophytes on insect herbivory may be modified by their interactions with higher trophic levels, such as predators. Including these multitrophic dynamics may explain some of the variability among endophyte studies of non-grass plants, which are currently based exclusively on bitrophic studies. 3. The abundance of natural foliar endophytes in a Neotropical vine was manipulated and beetles were fed high or low endophyte diets. Experimental assays assessed whether dietary endophyte load affected beetle growth, leaf consumption, and susceptibility to ant predation. 4. Beetles feeding on high- versus low-endophyte plants had almost identical growth and leaf consumption rates. 5. In a field bioassay, however, it was discovered that feeding on an endophyte-rich diet increased a beetle's odds of capture by predatory ants nine-fold. 6. Endophytes could thus provide an indirect, enemy-mediated form of plant defence that operates even against specialist herbivores. We argue that a multitrophic approach is necessary to untangle the potentially diverse types of endophyte defence among plants. C1 [Hammer, Tobin J.] Univ Colorado, Cooperat Inst Res Environm Sci, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Hammer, Tobin J.; Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Apartado, Panama. [Van Bael, Sunshine A.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. RP Van Bael, SA (reprint author), Tulane Univ, 6823 St Charles Ave,Boggs Suite 400, New Orleans, LA 70118 USA. EM svanbael@tulane.edu FU STRI short-term fellowship; [NSF-DEB-0949602] FX We would like to thank the staff of the Smithsonian Tropical Research Institute (STRI) for logistical support, and F. Vencl and D. Windsor for invaluable advice on study design. We also gratefully acknowledge A. Trillo and W. Wagoner for their assistance with beetle collection and husbandry. M. Grant gave feedback on statistical analyses, and P. Mason and two anonymous reviewers provided helpful comments on an earlier version of the manuscript. Funding sources included a STRI short-term fellowship to TJH and NSF-DEB-0949602 to SAV. Permission to do this research was granted by the Environmental authority (ANAM) of Panama. NR 50 TC 0 Z9 0 U1 7 U2 52 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6946 EI 1365-2311 J9 ECOL ENTOMOL JI Ecol. Entomol. PD JUN PY 2015 VL 40 IS 3 BP 316 EP 321 DI 10.1111/een.12186 PG 6 WC Entomology SC Entomology GA CF8GM UT WOS:000352794200014 ER PT J AU Cheng, RC Kuntner, M AF Cheng, Ren-Chung Kuntner, Matjaz TI Disentangling the Size and Shape Components of Sexual Dimorphism SO EVOLUTIONARY BIOLOGY LA English DT Review DE Sexual shape dimorphism; Sexual size dimorphism; Abdominal shape; Sexual selection; Intraspecific niche divergence; Spiders ID BODY SHAPE; GEOMETRIC MORPHOMETRICS; MECHANICAL-PROPERTIES; PHYLOGENETIC ANALYSIS; PODARCIS LIZARDS; WEB DECORATIONS; SPIDERS ARANEAE; BILL SIZE; EVOLUTION; SELECTION AB Many organisms are sexually dimorphic, reflecting sex-specific selection pressures. But although sexual dimorphism may consist of different variables from size to shape and physiology, most research emphasizes a single aspect of sexual dimorphism, notably size, without specifying its components and their relationship. Among terrestrial animals, spiders exhibit most extreme sex-specific differences in size and abdominal shape, and therefore represent ideal models to address this question. Here, we dissect sexual dimorphism in spiders at two phylogenetic hierarchical levels. At the species level, we employ comparative phylogenetic tests to explore the association between sexual shape dimorphism (SShD) and sexual size dimorphism (SSD) in the orbweb clade Argiopinae. At the genus level, we then explore such patterns on a phylogeny of orb weavers (Araneoidea). Female argiopines had more diverse abdominal morphotypes than the males and the abdominal shape evolution was only poorly correlated between the sexes. Phylogenetic and comparative data suggested that evolution of SShD in argiopines was related to geographic history, but that sexually shape monomorphic cases arose through selection for male size, perhaps acting against fecundity selection. While in argiopines there was no clear association between SShD and SSD, we detected a significant correlation in all orb weavers at the genus level. The shape and the size components of sexual dimorphism may thus respond independently to selection pressures, but at certain phylogenetic levels SSD may be a prerequisite for SShD. Research on other animal groups is needed to establish whether the here detected patterns on spiders are general. C1 [Cheng, Ren-Chung; Kuntner, Matjaz] Biol Inst ZRC SAZU, Evolutionary Zool Lab, 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, Washington, DC 20560 USA. RP Cheng, RC (reprint author), Biol Inst ZRC SAZU, Evolutionary Zool Lab, Ljubljana, Slovenia. EM bolasargiope@gmail.com; kuntner@gmail.com FU Slovenian Research Agency [P1-10236] FX We thank 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, M. Gregoric., G. Uhl, E. A. Yagmur, M. A. Herberstein, and J. N. Huang for their help with material for size measurement and molecular work. We also thank C. P. Liao for helping on statistics and EZ Lab members for various support: N. Vidergar, T. Lokovsek and S. Kralj-Fiser. Our paper was independently reviewed by Axios Review, and we thank Tim Vines, Matthew Symonds and three anonymous reviewers for their feedback. This work was supported by the Slovenian Research Agency (P1-10236 to MK and a Young Researcher fellowship to RCC). NR 77 TC 6 Z9 6 U1 11 U2 51 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0071-3260 EI 1934-2845 J9 EVOL BIOL JI Evol. Biol. PD JUN PY 2015 VL 42 IS 2 BP 223 EP 234 DI 10.1007/s11692-015-9313-z PG 12 WC Evolutionary Biology SC Evolutionary Biology GA CF8OE UT WOS:000352820600010 ER PT J AU Villarreal-Trevino, C Vasquez, GM Lopez-Sifuentes, VM Escobedo-Vargas, K Huayanay-Repetto, A Linton, YM Flores-Mendoza, C Lescano, AG Stell, FM AF Villarreal-Trevino, Cuauhtemoc Vasquez, Gissella M. Lopez-Sifuentes, Victor M. Escobedo-Vargas, Karin Huayanay-Repetto, Anibal Linton, Yvonne-Marie Flores-Mendoza, Carmen Lescano, Andres G. Stell, Frederick M. TI Establishment of a free-mating, long-standing and highly productive laboratory colony of Anopheles darlingi from the Peruvian Amazon SO MALARIA JOURNAL LA English DT Article DE Anopheles darlingi; Colony establishment; Natural copulation induction; Larval rearing; Amazon basin; Peru; Malaria vector ID NEOTROPICAL MALARIA VECTOR; PLASMODIUM-VIVAX; BODY-SIZE; BRAZIL; COLONIZATION; TRANSMISSION; CULICIDAE; FECUNDITY; DIPTERA; AREA AB Background: Anopheles darlingi is the main malaria vector in the Amazon region and is among the most efficient malaria vectors worldwide. However, due to the lack of a well-established laboratory colony, key control-relevant aspects of the bionomics, behaviour, genetics, and vector-parasite relationships of An. darlingi remain unknown. Here, biological parameters that had been successful in initiating other Anopheles colonies were optimized and improved for An. darlingi, with the aim of establish a free-mating, stable, and highly productive laboratory colony. Methods: Wild An. darlingi adult females were field collected from Zungarococha, Loreto Department, Peru (03 degrees 49' 32.40 '' S, 73 degrees 21'00.08 '' W), and taken to the NAMRU-6 Insectary in Iquitos where F-1 offspring were produced and reared. Natural copulation was successfully induced in F1 adults under a thermoperiod of 30 +/- 1 degrees C during the day and 25 +/- 1 degrees C at night, and with a 30-min LED light stimulation period at dusk. Oviposition success was enhanced using egg-laying containers with a dark-coloured surface. Larval feeding regimes were standardized for optimal larval development. Optimized copulation induction methods were used to facilitate mating in An. darlingi until the F-10 generation. No copulation induction assistance was needed in subsequent generations. Results: In 19 generations, the An. darlingi colony produced a total of 763,775 eggs; 441,124 larvae; 248,041 pupae; and 231,591 adults. A mean of 0.56 sexual encounters/female/cage (n = 36 cages) was recorded across the first ten generations (F-1-F-10). A mean insemination rate of 54.7 % (n = 5,907 females) ranging from 43.6 % (F-2) to 66.6 % (F-10) was recorded across nine generations (F-2-F-10). Free-mating was casually observed in the F-8 generation, and subsequently confirmed in the F-9 and F-10 generations; comparable insemination rates and egg laying between stimulated (51.6 %, 12.9 eggs/female), and non-stimulated (52.3 %, 11.2 eggs/female) females were recorded. The time from egg to adult development ranged from 10 to 20 days. Moreover, the colony was relocated to a new laboratory within Iquitos in the F-14 generation without any noted changes in its productivity. By March 2015, the An. darlingi colony has been successfully reared to the F-26 generation. Conclusions: This constitutes the first report of a free-mating, highly productive, and long-standing An. darlingi laboratory colony established through natural copulation induction, which will support critical malaria research. This rearing methodology may be a transferable, cost-effective alternative to labour-intensive forced mating practices widely used in maintaining other Anopheles colonies. C1 [Villarreal-Trevino, Cuauhtemoc] US Naval Med Res Unit 6 NAMRU 6, Dept Entomol, Bellavista, Callao, Peru. [Vasquez, Gissella M.; Lopez-Sifuentes, Victor M.; Escobedo-Vargas, Karin; Huayanay-Repetto, Anibal; Flores-Mendoza, Carmen; Stell, Frederick M.] US Naval Med Res Unit 6, Dept Entomol, Bellavista, Callao, Peru. [Linton, Yvonne-Marie] Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, Suitland, MD USA. [Linton, Yvonne-Marie] Walter Reed Army Inst Res, Silver Spring, MD USA. [Linton, Yvonne-Marie] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Lescano, Andres G.] US Naval Med Res Unit 6, Dept Parasitol, Bellavista, Callao, Peru. RP Vasquez, GM (reprint author), US Naval Med Res Unit 6 NAMRU 6, Dept Entomol, Bellavista, Callao, Peru. EM gissella.vasquez@med.navy.mil RI Lescano, Andres/B-8479-2008 OI Lescano, Andres/0000-0001-9779-633X FU Contrato de Acceso Marco a Recursos Geneticos [0017-2014-MINAGRI-DGFFS/DGEFFS]; Global Emerging Infections Surveillance and Response System (AFHSC/GEIS) of the U.S. Department of Defense sustainment funding award; Consejo Nacional de Ciencia y Tecnologia (CONACYT) Mexico [CB2008-105806-M]; Fogarty International Center of the U.S. National Institutes of Health [2D43 TW007393-06]; National Research Council (NRC) Research Associate Program FX We would like to thank the Ministerio de Agricultura y Riego de Peru, Direccion General Forestal y de Fauna Silvestre, and the Direccion de Salud, Gobierno Regional de Loreto for permission to conduct these studies: Anopheles darlingi collections in Loreto were conducted under the auspices of Resolucion Directoral No. 0406-2013-MINAGRI-DGFFS/DGEFFS; An. darlingi molecular identification was conducted under the auspices of Contrato de Acceso Marco a Recursos Geneticos No. 0017-2014-MINAGRI-DGFFS/DGEFFS. We would like to thank Fanny Castro, Geidin Chavez, Hugo Jaba, Luz Romero, Miguel Vasquez, and Alex Vasquez for technical support. Additionally, we would like to thank Dr. Craig Stoops for providing helpful comments on the manuscript. Financial support was provided by the Global Emerging Infections Surveillance and Response System (AFHSC/GEIS) of the U.S. Department of Defense sustainment funding award (FMS, GMV), the Consejo Nacional de Ciencia y Tecnologia (CONACYT) Mexico, grant CB2008-105806-M (CVT), and by the training grant 2D43 TW007393-06 awarded to NAMRU-6 by the Fogarty International Center of the U.S. National Institutes of Health. YML was supported by the National Research Council (NRC) Research Associate Program. NR 40 TC 3 Z9 3 U1 1 U2 2 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1475-2875 J9 MALARIA J JI Malar. J. PD MAY 30 PY 2015 VL 14 AR 227 DI 10.1186/s12936-015-0733-0 PG 12 WC Infectious Diseases; Parasitology; Tropical Medicine SC Infectious Diseases; Parasitology; Tropical Medicine GA CK4UZ UT WOS:000356220100001 PM 26024853 ER PT J AU Loi, ST Murphy, T Cairns, IH Menk, FW Waters, CL Erickson, PJ Trott, CM Hurley-Walker, N Morgan, J Lenc, E Offringa, AR Bell, ME Ekers, RD Gaensler, BM Lonsdale, CJ Feng, L Hancock, PJ Kaplan, DL Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Wayth, RB Webster, RL Williams, A Williams, CL AF Loi, Shyeh Tjing Murphy, Tara Cairns, Iver H. Menk, Frederick W. Waters, Colin L. Erickson, Philip J. Trott, Cathryn M. Hurley-Walker, Natasha Morgan, John Lenc, Emil Offringa, Andre R. Bell, Martin E. Ekers, Ronald D. Gaensler, B. M. Lonsdale, Colin J. Feng, Lu Hancock, Paul J. Kaplan, David L. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Tingay, S. J. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. TI Real-time imaging of density ducts between the plasmasphere and ionosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Murchison Widefield Array; radio telescope; field aligned; whistler duct; ionosphere ID VLA RADIO INTERFEROMETER; ELECTRIC-FIELDS; IRREGULARITIES; PROPAGATION; SIGNALS; CLUSTER; ARRAY AB Ionization of the Earth's atmosphere by sunlight forms a complex, multilayered plasma environment within the Earth's magnetosphere, the innermost layers being the ionosphere and plasmasphere. The plasmasphere is believed to be embedded with cylindrical density structures (ducts) aligned along the Earth's magnetic field, but direct evidence for these remains scarce. Here we report the first direct wide-angle observation of an extensive array of field-aligned ducts bridging the upper ionosphere and inner plasmasphere, using a novel ground-based imaging technique. We establish their heights and motions by feature tracking and parallax analysis. The structures are strikingly organized, appearing as regularly spaced, alternating tubes of overdensities and underdensities strongly aligned with the Earth's magnetic field. These findings represent the first direct visual evidence for the existence of such structures. C1 [Loi, Shyeh Tjing; Murphy, Tara; Cairns, Iver H.; Lenc, Emil; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Loi, Shyeh Tjing; Murphy, Tara; Trott, Cathryn M.; Lenc, Emil; Offringa, Andre R.; Bell, Martin E.; Gaensler, B. M.; Hancock, Paul J.; Briggs, F.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys, Redfern, NSW, Australia. [Menk, Frederick W.; Waters, Colin L.] Univ Newcastle, Sch Math & Phys Sci, Callaghan, NSW 2308, Australia. [Erickson, Philip J.; Lonsdale, Colin J.; Cappallo, R. J.; McWhirter, S. R.] MIT Haystack Observ, Westford, MA USA. [Trott, Cathryn M.; Hurley-Walker, Natasha; Morgan, John; Hancock, Paul J.; Ord, S. M.; Tingay, S. J.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA, Australia. [Offringa, Andre R.; Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. [Offringa, Andre R.] Netherlands Inst Radio Astron, Dwingeloo, Netherlands. [Bell, Martin E.; Ekers, Ronald D.; Mitchell, D. A.] CSIRO Astron & Space Sci, Epping, NSW, Australia. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada. [Feng, Lu; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI USA. [Bernardi, G.] Square Kilometre Array South Africa, Cape Town, South Africa. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune, Maharashtra, India. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. RP Loi, ST (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. EM sloi5113@uni.sydney.edu.au RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Deshpande, Avinash/D-4868-2012; Hurley-Walker, Natasha/B-9520-2013; Subrahmanyan, Ravi/D-4889-2012; Udayashankar , N/D-4901-2012; OI Hancock, Paul/0000-0002-4203-2946; Wayth, Randall/0000-0002-6995-4131; Lenc, Emil/0000-0002-9994-1593; Trott, Cathryn/0000-0001-6324-1766; Hurley-Walker, Natasha/0000-0002-5119-4808; Loi, Shyeh Tjing/0000-0002-6528-4548; Murphy, Tara/0000-0002-2686-438X; Cairns, Iver/0000-0001-6978-9765; Gaensler, Bryan/0000-0002-3382-9558 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884, AST-1412421]; 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 from the New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington from the IBM; Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; Western Australian State government FX The data supporting this paper are available upon request submitted via email to the corresponding author at sloi5113@uni.sydney.edu.au. This scientific work makes use of the Murchison Radio-astronomy Observatory, 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, AST-0908884, and AST-1412421), 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. We thank D. B. Melrose for discussions regarding physical interpretations. NR 39 TC 14 Z9 14 U1 1 U2 8 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 MAY 28 PY 2015 VL 42 IS 10 BP 3707 EP 3714 DI 10.1002/2015GL063699 PG 8 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300011 ER PT J AU Watters, TR Selvans, MM Banks, ME Hauck, SA Becker, KJ Robinson, MS AF Watters, Thomas R. Selvans, Michelle M. Banks, Maria E. Hauck, Steven A., II Becker, Kris J. Robinson, Mark S. TI Distribution of large-scale contractional tectonic landforms on Mercury: Implications for the origin of global stresses SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Mercury; tectonics; thrust fault; stress ID LOBATE SCARPS; TERRESTRIAL PLANETS; WRINKLE RIDGES; MESSENGER; EVOLUTION; TOPOGRAPHY; HEMISPHERE; MANTLE; FAULTS; BASIN AB The surface of Mercury is dominated by contractional tectonic landforms that are evidence of global-scale crustal deformation. Using MESSENGER orbital high-incidence angle imaging and topographic data, large-scale lobate thrust fault scarps have been mapped globally. The spatial distribution and areal density of the contractional landforms are not uniform; concentrations occur in longitudinal bands and between the north and south hemispheres. Their orientations are generally north-south at low latitude to midlatitude and east-west at high latitudes. The spatial distribution and distribution of orientations of these large-scale contractional features suggest that planet-wide contraction due to interior cooling cannot be the sole source of global stresses. The nonrandom orientations are best explained by a combination of stresses from global contraction and tidal despinning combined with an equator-to-pole variation in lithospheric thickness, while the nonuniform areal density of the contractional features may indicate the influence of mantle downwelling or heterogeneities in lithospheric strength. C1 [Watters, Thomas R.; Selvans, Michelle M.; Banks, Maria E.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Hauck, Steven A., II] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. [Becker, Kris J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Robinson, Mark S.] Arizona State Univ Tempe, Sch Earth & Space Explorat, Flagstaff, AZ USA. RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM watterst@si.edu OI Hauck, Steven/0000-0001-8245-146X FU NASA [NNX07AR60G] FX We thank W.B. McKinnon and an anonymous reviewer for helpful comments that greatly improved the manuscript. We also thank S.C. Solomon, P.K. Byrne, and C. Klimczak for helpful suggestion on an early manuscript. We are grateful to the MESSENGER engineers and technical support personnel at Johns Hopkins University Applied Physics Laboratory. This work is also supported by NASA grant NNX07AR60G. Data used to produce the results of this paper can be obtained upon request from the first author. NR 45 TC 3 Z9 3 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 28 PY 2015 VL 42 IS 10 BP 3755 EP 3763 DI 10.1002/2015GL063570 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300017 ER PT J AU Myers, CG Oster, JL Sharp, WD Bennartz, R Kelley, NP Covey, AK Breitenbach, SFM AF Myers, Christopher G. Oster, Jessica L. Sharp, Warren D. Bennartz, Ralf Kelley, Neil P. Covey, Aaron K. Breitenbach, Sebastian F. M. TI Northeast Indian stalagmite records Pacific decadal climate change: Implications for moisture transport and drought in India SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE speleothem; oxygen isotopes; El Nino; Indian monsoon; PDO; NPGO ID EL-NINO; SUMMER MONSOON; ENSO; RAINFALL; FAILURE; OCEAN; WATER AB Two types of El Nino events are distinguished by sea surface temperature (SST) anomalies centered in the central or eastern equatorial Pacific. The Central Pacific El Nino events (CP-El Nino) are more highly correlated with weakening of the central Indian Summer Monsoon and linked to decadal Pacific climate variability. We present a 50year, subannually resolved speleothem O-18 record from northeast India that exhibits a significant correlation with northern Pacific decadal variability and central equatorial Pacific SSTs. Accordingly, we suggest that O-18 time series in similar northeast Indian speleothems are effective tools for investigating preinstrumental changes in Pacific climate, including changes in El Nino dynamics. In contrast to central India, rainfall amounts in northeast India are relatively unaffected by El Nino. However, back trajectory analysis indicates that during CP-El Nino events moisture transport distance to northeast India is reduced, suggesting that variations in moisture transport primarily control O-18 in the region. C1 [Myers, Christopher G.; Oster, Jessica L.; Bennartz, Ralf; Covey, Aaron K.] Vanderbilt Univ, Dept Earth & Environm Sci, Nashville, TN 37235 USA. [Sharp, Warren D.] Berkeley Geochronol Ctr, Berkeley, CA USA. [Kelley, Neil P.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Breitenbach, Sebastian F. M.] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England. RP Oster, JL (reprint author), Vanderbilt Univ, Dept Earth & Environm Sci, 221 Kirkland Hall, Nashville, TN 37235 USA. EM jessica.l.oster@vanderbilt.edu RI Breitenbach, Sebastian/C-2529-2014; OI Oster, Jessica/0000-0002-1780-2435 FU BanglaPIRE project [NSF OISE-0968354]; Vanderbilt International Office; Cave Research Foundation; Geological Society of America; Schweizer National Fond (SNF), Sinergia grant [CRSI22 132646/1] FX Kaplan SST V2 data provided by the NOAA/OAR/ESRL PSD from http://www.esrl.noaa.gov/psd/. Data from this study will be archived at the NOAA National Climatic Data Center (http://www.ncdc.noaa.gov/data-access/paleoclimatology-data). This work was supported through the BanglaPIRE project (NSF OISE-0968354), an award from the Vanderbilt International Office to JLO and SFMB, and awards from the Cave Research Foundation and the Geological Society of America to CGM. SFMB received financial support from the Schweizer National Fond (SNF), Sinergia grant CRSI22 132646/1. We thank Steven Goodbred, Gregory Diengdoh, and Brian Kharpran Daly for support during fieldwork, David Furbish and Tyler Doane for assistance with wavelets, and two anonymous reviewers for constructive comments. NR 36 TC 4 Z9 4 U1 5 U2 12 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 MAY 28 PY 2015 VL 42 IS 10 BP 4124 EP 4132 DI 10.1002/2015GL063826 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CL0KJ UT WOS:000356631300062 ER PT J AU Shen, G Stancil, PC Wang, JG McCann, JF McLaughlin, BM AF Shen, G. Stancil, P. C. Wang, J. G. McCann, J. F. McLaughlin, B. M. TI Radiative charge transfer in cold and ultracold sulphur atoms colliding with protons SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE ultracold collisions; radiative loss; rate coefficients ID COLLISIONS; SH+; ASSOCIATION; ABSORPTION; CHEMISTRY; IONS; H+ AB Radiative decay processes at cold and ultra cold temperatures for sulfur atoms colliding with protons are investigated. The MOLPRO quantum chemistry suite of codes was used to obtain accurate potential energies and transition dipole moments, as a function of internuclear distance, between low-lying states of the SH+ molecular cation. A multi-reference configuration-interaction approximation together with the Davidson correction is used to determine the potential energy curves and transition dipole moments, between the states of interest, where the molecular orbitals are obtained from state-averaged multi-configuration-self-consistent field calculations. The collision problem is solved approximately using an optical potential method to obtain radiative loss, and a fully two-channel quantum approach for radiative charge transfer. Cross sections and rate coefficients are determined for the first time for temperatures ranging from 10 mu K up to 10 000 K. Results are obtained for all isotopes of sulfur, colliding with H+ and D+ ions and comparison is made to a number of other collision systems. C1 [Shen, G.; Stancil, P. C.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Shen, G.; Stancil, P. C.] Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. [Shen, G.; Wang, J. G.] Inst Appl Phys & Computat Math, Beijing 100088, Peoples R China. [McCann, J. F.; McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA. RP Shen, G (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. EM stancil@physast.uga.edu; b.mclaughlin@qub.ac.uk FU NASA [NNX09AC46G]; Queen's University Belfast; US National Science Foundation FX GS acknowledges travel support by the International Cooperation and Exchange Foundation of CAEP. PCS acknowledges support from NASA grant NNX09AC46G. The hospitality of the University of Georgia at Athens is gratefully acknowledged by B MMcL during recent research visits. B MMcL also thanks Queen's University Belfast for the award of a Visiting Research Fellowship (VRF). PCS and BMMcL thank the US National Science Foundation under the visitors program through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics. Grants of computational time at the National Energy Research Scientific Computing Center in Oakland, CA, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany are gratefully acknowledged. NR 35 TC 2 Z9 2 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAY 28 PY 2015 VL 48 IS 10 AR 105203 DI 10.1088/0953-4075/48/10/105203 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CG5KD UT WOS:000353329500009 ER PT J AU Testa, P Saar, SH Drake, JJ AF Testa, Paola Saar, Steven H. Drake, Jeremy J. TI Stellar activity and coronal heating: an overview of recent results SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Review DE solar corona; magnetic activity; X-ray activity; chromospheric activity; solar-stellar connection ID X-RAY-EMISSION; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; ACTIVITY-ROTATION RELATIONSHIP; SCALE MAGNETIC TOPOLOGIES; CA-II EMISSION; NON-WKB MODELS; COOL STARS; M-DWARFS; DIFFERENTIAL ROTATION AB Observations of the coronae of the Sun and of solar-like stars provide complementary information to advance our understanding of stellar magnetic activity, and of the processes leading to the heating of their outer atmospheres. While solar observations allow us to study the corona at high spatial and temporal resolution, the study of stellar coronae allows us to probe stellar activity over a wide range of ages and stellar parameters. Stellar studies therefore provide us with additional tools for understanding coronal heating processes, as well as the long-term evolution of solar X-ray activity. We discuss how recent studies of stellar magnetic fields and coronae contribute to our understanding of the phenomenon of activity and coronal heating in late-type stars. C1 [Testa, Paola; Saar, Steven H.; Drake, Jeremy J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Testa, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ptesta@cfa.harvard.edu FU NASA [NNX10AF29G, NNM07AB07C]; Chandra grant [GO1-12036X]; Lockheed-Martin [SP02H1701R] FX This work was supported by NASA under grant no. NNX10AF29G, contract no. NNM07AB07C, to the Smithsonian Astrophysical Observatory, Chandra grant no. GO1-12036X and contract SP02H1701R from Lockheed-Martin to S.A.O. NR 161 TC 3 Z9 3 U1 0 U2 0 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 MAY 28 PY 2015 VL 373 IS 2042 AR UNSP 20140259 DI 10.1098/rsta.2014.0259 PG 21 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG5BL UT WOS:000353304600003 ER PT J AU Siebert, S Goetz, FE Church, SH Bhattacharyya, P Zapata, F Haddock, SHD Dunn, CW AF Siebert, Stefan Goetz, Freya E. Church, Samuel H. Bhattacharyya, Pathikrit Zapata, Felipe Haddock, Steven H. D. Dunn, Casey W. TI Stem cells in Nanomia bijuga (Siphonophora), a colonial animal with localized growth zones SO EVODEVO LA English DT Article DE Siphonophora; Nanomia bijuga; Growth zone; Interstitial stem cell; i-cell ID PHYSONECTID SIPHONOPHORES; INTERSTITIAL-CELLS; HYDRA-ATTENUATA; SOMATIC-CELLS; GERM-LINE; DIFFERENTIATION; CNIDARIAN; HYDROZOA; HYDRACTINIA; EVOLUTION AB Background: Siphonophores (Hydrozoa) have unparalleled colony-level complexity, precision of colony organization, and functional specialization between zooids (i.e., the units that make up colonies). Previous work has shown that, unlike other colonial animals, most growth in siphonophores is restricted to one or two well-defined growth zones that are the sites of both elongation and zooid budding. It remained unknown, however, how this unique colony growth and development is realized at the cellular level. Results: To understand the colony-level growth and development of siphonophores at the cellular level, we characterize the distribution of proliferating cells and interstitial stem cells (i-cells) in the siphonophore Nanomia bijuga. Within the colony, we find evidence that i-cells are present at the tip of the horn, the structure within the growth zone that gives rise to new zooids. Co-localized gene expression of vasa-1, pl10, piwi, nanos-1, and nanos-2 suggests that i-cells persist in the youngest zooid buds and that i-cells become progressively restricted to specific regions within the zooids until they are mostly absent from the oldest zooids. The examined genes remain expressed in gametogenic regions. No evidence for i-cells is found in the stem between maturing zooids. Domains of high cell proliferation include regions where the examined genes are expressed, but also include some areas in which the examined genes were not expressed such as the stem within the growth zones. Cell proliferation in regions devoid of vasa-1, pl10, piwi, nanos-1, and nanos-2 expression indicates the presence of mitotically active epithelial cell lineages and, potentially, progenitor cell populations. Conclusions: We provide the first evidence for i-cells in a siphonophore. Our findings suggest maintenance of i-cell populations at the sites of growth zones and that these sites are the main source of i-cells. This restriction of stem cells to particular regions in the colony, in combination with localized budding and spatial patterning during pro-bud subdivision, may play a major role in facilitating the precision of siphonophore growth. Spatially restricted maintenance of i-cells in mature zooids and absence of i-cells along the stem may explain the reduced developmental plasticity in older parts of the colony. C1 [Siebert, Stefan; Church, Samuel H.; Bhattacharyya, Pathikrit; Zapata, Felipe; Dunn, Casey W.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Goetz, Freya E.] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20004 USA. [Haddock, Steven H. D.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. RP Siebert, S (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, 80 Waterman St Box GW, Providence, RI 02912 USA. EM stefan_siebert@brown.edu OI Zapata, Felipe/0000-0002-9386-0573; Dunn, Casey/0000-0003-0628-5150 FU NSF EPSCoR [EPS1004057]; State of Rhode Island; US National Science Foundation [1256695]; David and Lucile Packard Foundation; US National Science Foundation (Alan T. Waterman Award) FX We thank Leo W. Buss and Uri Frank for critical feedback on a preprint version of the manuscript. SS and CWD thank Claudia Mills for informing us about high abundances of Nanomia bijuga at Friday Harbor Labs (FHL), San Juan Island, WA, and Billie Swalla for hosting SS at her lab. We thank members of the Dunn lab for discussion and feedback on the manuscript, in particular Catriona Munro. We also thank the MBARI crews and ROV pilots for collection of N. bijuga specimens. Computational work was conducted at the Center for Computation and Visualization, Brown University, supported in part by the NSF EPSCoR EPS1004057 and the State of Rhode Island. This research was supported by the US National Science Foundation (grant 1256695 and the Alan T. Waterman Award) and by the David and Lucile Packard Foundation. NR 60 TC 3 Z9 3 U1 1 U2 11 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 MAY 27 PY 2015 VL 6 AR 22 DI 10.1186/s13227-015-0018-2 PG 18 WC Evolutionary Biology; Developmental Biology SC Evolutionary Biology; Developmental Biology GA CK7MD UT WOS:000356415600001 PM 26090088 ER PT J AU Doorenweerd, C Van Nieukerken, EJ Sohn, JC Labandeira, CC AF Doorenweerd, Camiel Van Nieukerken, Erik J. Sohn, Jae-Cheon Labandeira, Conrad C. TI A revised checklist of Nepticulidae fossils (Lepidoptera) indicates an Early Cretaceous origin SO ZOOTAXA LA English DT Article DE Baltic Amber; Calibration points; Dakota Formation; Evolutionary history; Extinction; Fossil record; Larvae; Leaf mining; Plant hosts; Stigmella; Stigmellites ID PLANT-INSECT ASSOCIATIONS; LEAF MINES; EOCENE; BUTTERFLIES; MOTHS; AGE; DIVERSIFICATION; WASHINGTON; AUSTRALIA; HERBIVORY AB With phylogenetic knowledge of Lepidoptera rapidly increasing, catalysed by increasingly powerful molecular techniques, the demand for fossil calibration points to estimate an evolutionary time frame for the order is becoming an increasingly pressing issue. The family Nepticulidae is a species rich, basal branch within the phylogeny of the Lepidoptera, characterized by larval leaf-mining habits, and thereby represents a potentially important lineage whose evolutionary history can be established more thoroughly with the potential use of fossil calibration points. Using our experience with extant global Nepticulidae, we discuss a list of characters that may be used to assign fossil leaf mines to Nepticulidae, and suggest useful methods for classifying relevant fossil material. We present a checklist of 79 records of Nepticulidae representing adult and leaf-mine fossils mentioned in literature, often with multiple exemplars constituting a single record. We provide our interpretation of these fossils. Two species now are included in the collective generic name Stigmellites: Stigmellites resupinata (Krassilov, 2008) comb. nov. (from Ophiheliconoma) and Stigmellites almeidae (Martins-Neto, 1989) comb. nov. (from Nepticula). Eleven records are for the first time attributed to Nepticulidae. After discarding several dubious records, including one possibly placing the family at a latest Jurassic position, we conclude that the oldest fossils likely attributable to Nepticulidae are several exemplars representing a variety of species from the Dakota Formation (USA). The relevant strata containing these earliest fossils are now dated at 102 Ma (million years ago) in age, corresponding to the latest Albian Stage of the Early Cretaceous. Integration of all records in the checklist shows that a continuous presence of nepticulid-like leaf mines preserved as compression-impression fossils and by amber entombment of adults have a fossil record extending to the latest Early Cretaceous. C1 [Doorenweerd, Camiel; Van Nieukerken, Erik J.] Nat Biodivers Ctr, Dept Terr Zool, Leiden, Netherlands. [Doorenweerd, Camiel] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, Amsterdam, Netherlands. [Sohn, Jae-Cheon; Labandeira, Conrad C.] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA. [Sohn, Jae-Cheon; Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. RP Doorenweerd, C (reprint author), Nat Biodivers Ctr, Dept Terr Zool, Leiden, Netherlands. EM camiel.doorenweerd@naturalis.nl NR 127 TC 4 Z9 4 U1 3 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 27 PY 2015 VL 3963 IS 3 BP 295 EP 334 PG 40 WC Zoology SC Zoology GA CJ1RS UT WOS:000355262600002 PM 26249403 ER PT J AU Smacchia, P Knap, M Demler, E Silva, A AF Smacchia, Pietro Knap, Michael Demler, Eugene Silva, Alessandro TI Exploring dynamical phase transitions and prethermalization with quantum noise of excitations SO PHYSICAL REVIEW B LA English DT Article ID MOTT INSULATOR; THERMALIZATION; QUENCHES AB Dynamical phase transitions can occur in isolated quantum systems that are brought out of equilibrium by sudden parameter changes. We discuss the characterization of such dynamical phase transitions based on the statistics of produced excitations. We consider both the O(N) model in the large-N limit and a spin model with long-range interactions and show that the dynamical criticality of their prethermal steady states manifests most dramatically not in the average number of excitations but in their higher moments. We argue that the growth of defect fluctuations carries unique signatures of the dynamical criticality, irrespective of the precise details of the model. Our theoretical results should be relevant to quantum quench experiments with ultracold bosonic atoms in optical lattices. C1 [Smacchia, Pietro; Silva, Alessandro] SISSA, Int Sch Adv Studies, I-34136 Trieste, Italy. [Smacchia, Pietro] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Knap, Michael; Demler, Eugene] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, Michael] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Silva, Alessandro] Abdus Salam Int Ctr Theoret Phys, I-34100 Trieste, Italy. RP Smacchia, P (reprint author), SISSA, Int Sch Adv Studies, Via Bonomea 265, I-34136 Trieste, Italy. RI Knap, Michael/H-3344-2011; Silva, Alessandro/B-6928-2012 OI Knap, Michael/0000-0002-7093-9502; Silva, Alessandro/0000-0002-5668-7134 FU Harvard-MIT CUA; ARO-MURI Quism program; ARO-MURI on Atomtronics; Austrian Science Fund (FWF) [J 3361-N20] FX We thank G. Biroli, A. Gambassi, and A. Polkovnikov for useful discussions. The authors acknowledge support from Harvard-MIT CUA, the ARO-MURI Quism program, ARO-MURI on Atomtronics, as well as the Austrian Science Fund (FWF), Project No. J 3361-N20. NR 30 TC 18 Z9 18 U1 1 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD MAY 26 PY 2015 VL 91 IS 20 AR 205136 DI 10.1103/PhysRevB.91.205136 PG 9 WC Physics, Condensed Matter SC Physics GA CI9LM UT WOS:000355091600012 ER PT J AU Fernandez-Marin, H Nash, DR Higginbotham, S Estrada, C van Zweden, JS d'Ettorre, P Wcislo, WT Boomsma, JJ AF Fernandez-Marin, Hermogenes Nash, David R. Higginbotham, Sarah Estrada, Catalina van Zweden, Jelle S. d'Ettorre, Patrizia Wcislo, William T. Boomsma, Jacobus J. TI Functional role of phenylacetic acid from metapleural gland secretions in controlling fungal pathogens in evolutionarily derived leaf-cutting ants SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE mutualism; symbiosis; Attini; Escovopsis; actinomycetes; entomopathogens ID GROWING ANTS; ANTIFUNGAL ACTIVITY; SYMBIOSIS; WORKERS; GARDEN; SIZE; AGRICULTURE; SPECIFICITY; FORMICIDAE; MANAGEMENT AB Fungus-farming ant colonies vary four to five orders of magnitude in size. They employ compounds from actinomycete bacteria and exocrine glands as antimicrobial agents. Atta colonies have millions of ants and are particularly relevant for understanding hygienic strategies as they have abandoned their ancestors' prime dependence on antibiotic-based biological control in favour of using metapleural gland (MG) chemical secretions. Atta MGs are unique in synthesizing large quantities of phenylacetic acid (PAA), a known but little investigated antimicrobial agent. We show that particularly the smallest workers greatly reduce germination rates of Escovopsis and Metarhizium spores after actively applying PAA to experimental infection targets in garden fragments and transferring the spores to the ants' infrabuccal cavities. In vitro assays further indicated that Escovopsis strains isolated from evolutionarily derived leaf-cutting ants are less sensitive to PAA than strains from phylogenetically more basal fungus-farming ants, consistent with the dynamics of an evolutionary arms race between virulence and control for Escovopsis, but not Metarhizium. Atta ants form larger colonies with more extreme caste differentiation relative to other attines, in societies characterized by an almost complete absence of reproductive conflicts. We hypothesize that these changes are associated with unique evolutionary innovations in chemical pest management that appear robust against selection pressure for resistance by specialized mycopathogens. C1 [Fernandez-Marin, Hermogenes] Inst Invest Cient & Serv Alta Tecnol, Ctr Biodiversidad & Descubrimiento Drogas, Ciudad Del Saber, Clayton, Panama. [Fernandez-Marin, Hermogenes; Nash, David R.; van Zweden, Jelle S.; d'Ettorre, Patrizia; Boomsma, Jacobus J.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. [Fernandez-Marin, Hermogenes; Higginbotham, Sarah; Estrada, Catalina; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [van Zweden, Jelle S.] Univ Leuven, Inst Zool, Lab Socioecol & Social Evolut, B-3000 Leuven, Belgium. [d'Ettorre, Patrizia] Univ Paris 13, Sorbonne Paris Cite, LEEC, F-93430 Villetaneuse, France. RP Fernandez-Marin, H (reprint author), Inst Invest Cient & Serv Alta Tecnol, Ctr Biodiversidad & Descubrimiento Drogas, Edificio 219, Ciudad Del Saber, Clayton, Panama. EM hfernandez@indicasat.org.pa; jjboomsma@bio.ku.dk RI Nash, David/B-2916-2009; Boomsma, Jacobus/M-2785-2014 OI Nash, David/0000-0002-0462-6794; Boomsma, Jacobus/0000-0002-3598-1609 FU STRI Tupper Postdoctoral fellowship; SNI; SENACYT [09-038]; Danish Natural Research Foundation [DNRF57]; STRI FX Funding was provided by a STRI Tupper Postdoctoral fellowship, and a postdoctoral fellowship, SNI and Collaboration grant no. 09-038 from SENACYT to H.F.M., the Danish Natural Research Foundation (grant no. DNRF57 to J.J.B.) and STRI general research funds to W.T.W. NR 60 TC 5 Z9 5 U1 2 U2 35 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 MAY 22 PY 2015 VL 282 IS 1807 AR 20150212 DI 10.1098/rspb.2015.0212 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CM1SK UT WOS:000357460400005 PM 25925100 ER PT J AU Guarnizo, CE Paz, A Munoz-Ortiz, A Flechas, SV Mendez-Narvaez, J Crawford, AJ AF Guarnizo, Carlos E. Paz, Andrea Munoz-Ortiz, Astrid Flechas, Sandra V. Mendez-Narvaez, Javier Crawford, Andrew J. TI DNA Barcoding Survey of Anurans across the Eastern Cordillera of Colombia and the Impact of the Andes on Cryptic Diversity SO PLOS ONE LA English DT Article ID GENETIC DIFFERENTIATION; MOLECULAR PHYLOGENETICS; SPECIES RICHNESS; EVOLUTIONARY DIFFERENTIATION; AMPHIBIAN DIVERSITY; MAXIMUM-LIKELIHOOD; AMAZONIAN FROGS; MANTELLID FROGS; CLIMATE-CHANGE; BODY-SIZE AB Colombia hosts the second highest amphibian species diversity on Earth, yet its fauna remains poorly studied, especially using molecular genetic techniques. We present the results of the first wide-scale DNA barcoding survey of anurans of Colombia, focusing on a transect across the Eastern Cordillera. We surveyed 10 sites between the Magdalena Valley to the west and the eastern foothills of the Eastern Cordillera, sequencing portions of the mitochondrial 16S ribosomal RNA and cytochrome oxidase subunit 1 (CO1) genes for 235 individuals from 52 nominal species. We applied two barcode algorithms, Automatic Barcode Gap Discovery and Refined Single Linkage Analysis, to estimate the number of clusters or "unconfirmed candidate species" supported by DNA barcode data. Our survey included similar to 7% of the anuran species known from Colombia. While barcoding algorithms differed slightly in the number of clusters identified, between three and ten nominal species may be obscuring candidate species (in some cases, more than one cryptic species per nominal species). Our data suggest that the high elevations of the Eastern Cordillera and the low elevations of the Chicamocha canyon acted as geographic barriers in at least seven nominal species, promoting strong genetic divergences between populations associated with the Eastern Cordillera. C1 [Guarnizo, Carlos E.] Univ Brasilia, Dept Zool, BR-70910900 Brasilia, DF, Brazil. [Paz, Andrea; Munoz-Ortiz, Astrid; Flechas, Sandra V.; Mendez-Narvaez, Javier; Crawford, Andrew J.] Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia. [Munoz-Ortiz, Astrid] La Salle Univ, Dept Basic Sci, Bogota, Colombia. [Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City, Panama. RP Guarnizo, CE (reprint author), Univ Brasilia, Dept Zool, BR-70910900 Brasilia, DF, Brazil. EM carlosguarnizo@gmail.com RI Guarnizo, Carlos/A-6383-2011; OI Guarnizo, Carlos/0000-0001-7324-1241; Crawford, Andrew J./0000-0003-3153-6898; Paz, Andrea/0000-0001-6484-1210 FU Ecopetrol [156-09] FX Field and laboratory work were financed by grant number 156-09 from Ecopetrol. The funder had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 97 TC 3 Z9 3 U1 3 U2 14 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 MAY 22 PY 2015 VL 10 IS 5 AR e0127312 DI 10.1371/journal.pone.0127312 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI7GR UT WOS:000354931700049 PM 26000447 ER PT J AU Sabin, L Hull, CLH Plambeck, RL Zijlstra, AA Vazquez, R Navarro, SG Guillen, PF AF Sabin, L. Hull, C. L. H. Plambeck, R. L. Zijlstra, A. A. Vazquez, R. Navarro, S. G. Guillen, P. F. TI Millimetre polarization of the protoplanetary nebula OH 231.8+4.2: a follow-up study with CARMA SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Magnetic fields; polarization; stars: AGB and post-AGB; stars: individual: OH 231.8+4.2 ID MAGNETIC-FIELDS; PLANETARY-NEBULAE; MOLECULAR CLOUDS; CENTRAL STARS; EVOLVED STAR; ENVELOPES; EMISSION; SEARCH; LINES; CORES AB In order to investigate the characteristics and influence of the magnetic field in evolved stars, we performed a follow-up investigation of our previous submillimetre analysis of the protoplanetary nebula (PPN) OH231.8+4.2, this time at 1.3mmwith the CARMA(Combined Array for Research in Millimeter-wave Astronomy) facility in polarization mode for the purpose of a multiscale analysis. OH 231.8+4.2 was observed at similar to 2.5 arcsec resolution, and we detected polarized emission above the 3s threshold (with a mean polarization fraction of 3.5 per cent). The polarization map indicates an overall organized magnetic field within the nebula. The main finding in this paper is the presence of a structure mostly compatible with an ordered toroidal component that is aligned with the PPN's dark lane. We also present some alternative magnetic field configuration to explain the structure observed. These data complete our previous SMA submillimetre data for a better investigation and understanding of the magnetic field structure in OH 231.8+4.2. C1 [Sabin, L.; Navarro, S. G.] Univ Guadalajara, Dept Fis, Inst Astron & Meteorol, CUCEI, Guadalajara, Mexico. [Sabin, L.] Inst Estudios Avanzados Baja Calif AC, Ensenada 22800, BC, Mexico. [Hull, C. L. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Plambeck, R. L.] Univ Calif Berkeley, Astron Dept, Berkeley, CA 94720 USA. [Plambeck, R. L.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Zijlstra, A. A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Vazquez, R.; Guillen, P. F.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, BC, Mexico. RP Sabin, L (reprint author), Univ Guadalajara, Dept Fis, Inst Astron & Meteorol, CUCEI, Ave Vallarta 2602, Guadalajara, Mexico. EM laurence.sabin@gmail.com RI Vazquez, Roberto/L-3613-2016 OI Vazquez, Roberto/0000-0002-3279-9764 FU CONACYT [CB-2011-01-0168078]; University of Guadalajara (Mexico) [PIFI-2014]; NSF Graduate Fellowship; Ford Foundation Dissertation Fellowship; PAPIIT-DGAPA-UNAM [107914]; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; state of California; state of Illinois; state of Maryland; National Science Foundation; NASA [NAS 5-26555] FX We would like to thank the referee for his/her valuable comments which helped us improve the quality of this paper. LS is supported by the CONACYT grant CB-2011-01-0168078 and this research was also partially supported by the PIFI-2014 programme from the University of Guadalajara (Mexico). CLHH acknowledges support from an NSF Graduate Fellowship and from a Ford Foundation Dissertation Fellowship. RV is supported by PAPIIT-DGAPA-UNAM grant 107914. LS also thank Marco Gomez for his help. 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 also made use of the SIMBAD data base, operated at CDS, Strasbourg, France and the NASA's Astrophysics Data System. We acknowledge the use of observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. NR 30 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2015 VL 449 IS 3 BP 2368 EP 2373 DI 10.1093/mnras/stv461 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800012 ER PT J AU De Silva, GM Freeman, KC Bland-Hawthorn, J Martell, S de Boer, EW Asplund, M Keller, S Sharma, S Zucker, DB Zwitter, T Anguiano, B Bacigalupo, C Bayliss, D Beavis, MA Bergemann, M Campbell, S Cannon, R Carollo, D Casagrande, L Casey, AR Da Costa, G D'Orazi, V Dotter, A Duong, L Heger, A Ireland, MJ Kafle, PR Kos, J Lattanzio, J Lewis, GF Lin, J Lind, K Munari, U Nataf, DM O'Toole, S Parker, Q Reid, W Schlesinger, KJ Sheinis, A Simpson, JD Stello, D Ting, YS Traven, G Watson, F Wittenmyer, R Yong, D Zerjal, M AF De Silva, G. M. Freeman, K. C. Bland-Hawthorn, J. Martell, S. de Boer, E. Wylie Asplund, M. Keller, S. Sharma, S. Zucker, D. B. Zwitter, T. Anguiano, B. Bacigalupo, C. Bayliss, D. Beavis, M. A. Bergemann, M. Campbell, S. Cannon, R. Carollo, D. Casagrande, L. Casey, A. R. Da Costa, G. D'Orazi, V. Dotter, A. Duong, L. Heger, A. Ireland, M. J. Kafle, P. R. Kos, J. Lattanzio, J. Lewis, G. F. Lin, J. Lind, K. Munari, U. Nataf, D. M. O'Toole, S. Parker, Q. Reid, W. Schlesinger, K. J. Sheinis, A. Simpson, J. D. Stello, D. Ting, Y. -S. Traven, G. Watson, F. Wittenmyer, R. Yong, D. Zerjal, M. TI The GALAH survey: scientific motivation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxy: stellar content ID WAY STELLAR HALO; OLD OPEN CLUSTERS; RED GIANT BRANCH; MILKY-WAY; GALACTIC HALO; CHEMICAL EVOLUTION; THICK DISK; GLOBULAR-CLUSTERS; ELEMENTAL ABUNDANCE; SOLAR NEIGHBORHOOD AB The Galactic Archaeology with HERMES (GALAH) survey is a large high-resolution spectroscopic survey using the newly commissioned High Efficiency and Resolution Multi-Element Spectrograph (HERMES) on the Anglo-Australian Telescope. The HERMES spectrograph provides high-resolution (R similar to 28 000) spectra in four passbands for 392 stars simultaneously over a 2 deg field of view. The goal of the survey is to unravel the formation and evolutionary history of the Milky Way, using fossil remnants of ancient star formation events which have been disrupted and are now dispersed throughout the Galaxy. Chemical tagging seeks to identify such dispersed remnants solely from their common and unique chemical signatures; these groups are unidentifiable from their spatial, photometric or kinematic properties. To carry out chemical tagging, the GALAH survey will acquire spectra for a million stars down to V similar to 14. The HERMES spectra of FGK stars contain absorption lines from 29 elements including light proton-capture elements, alpha-elements, odd-Z elements, iron-peak elements and n-capture elements from the light and heavy s-process and the r-process. This paper describes the motivation and planned execution of the GALAH survey, and presents some results on the first-light performance of HERMES. C1 [De Silva, G. M.; Cannon, R.; O'Toole, S.; Sheinis, A.; Watson, F.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [De Silva, G. M.; Bland-Hawthorn, J.; Sharma, S.; Lewis, G. F.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Freeman, K. C.; de Boer, E. Wylie; Asplund, M.; Keller, S.; Bayliss, D.; Casagrande, L.; Da Costa, G.; Dotter, A.; Duong, L.; Ireland, M. J.; Lin, J.; Nataf, D. M.; Schlesinger, K. J.; Yong, D.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Martell, S.; Wittenmyer, R.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Zucker, D. B.; Anguiano, B.; Bacigalupo, C.; Carollo, D.; D'Orazi, V.; Parker, Q.; Reid, W.; Simpson, J. D.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Zucker, D. B.; Anguiano, B.; Bacigalupo, C.; Carollo, D.; Parker, Q.; Reid, W.; Simpson, J. D.] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia. [Zwitter, T.; Kos, J.; Traven, G.; Zerjal, M.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia. [Beavis, M. A.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Bergemann, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Campbell, S.; Heger, A.; Lattanzio, J.] Monash Univ, Sch Math Sci, Monash Ctr Astrophys, Clayton, Vic 3800, Australia. [Casey, A. R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [D'Orazi, V.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Heger, A.] Michigan State Univ, Joint Inst Nucl Astrophys, E Lansing, MI 48824 USA. [Heger, A.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kafle, P. R.] Univ Western Australia, ICRAR, Nedlands, WA 6009, Australia. [Lind, K.] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden. [Munari, U.] Astron Observ Padova, INAF, I-36012 Asiago, VI, Italy. [Ting, Y. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP De Silva, GM (reprint author), Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. EM gayandhi.desilva@aao.gov.au RI D'Orazi, Valentina/N-5230-2015; OI D'Orazi, Valentina/0000-0002-2662-3762; Kafle, Prajwal Raj/0000-0002-3625-9546; Ting, Yuan-Sen/0000-0001-5082-9536; Casey, Andrew/0000-0003-0174-0564; Lattanzio, John/0000-0003-2952-859X; Simpson, Jeffrey/0000-0002-8165-2507 FU Australian Research Council (ARC) [DP1095368, DP120101815, DP120101237, DP120104562, FS110200035, FL110100012]; ARC Future Fellowship [FT120100363]; ARC [FL110100012]; ARC DECRA [DE140100598]; National Aeronautics and Space Administration; National Science Foundation FX This research has been supported in part by the Australian Research Council (ARC) funding schemes (grant numbers DP1095368, DP120101815, DP120101237, DP120104562, FS110200035 and FL110100012). AH was supported by an ARC Future Fellowship grant FT120100363. DMN was supported by the ARC grant FL110100012. SLM was supported by the ARC DECRA grant DE140100598. 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 140 TC 65 Z9 65 U1 1 U2 7 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 MAY 21 PY 2015 VL 449 IS 3 BP 2604 EP 2617 DI 10.1093/mnras/stv327 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800032 ER PT J AU Bate, MR Keto, ER AF Bate, Matthew R. Keto, Eric R. TI Combining radiative transfer and diffuse interstellar medium physics to model star formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; hydrodynamics; radiative transfer; methods: numerical; stars: formation; ISM: general ID INITIAL MASS FUNCTION; SMOOTHED PARTICLE HYDRODYNAMICS; FLUX-LIMITED DIFFUSION; MOLECULAR CLOUD CORE; STELLAR DENSITIES; JEANS MASS; GAS CLOUDS; PROTOSTELLAR CORES; THERMAL STRUCTURE; FORMING CLOUDS AB We present a method for modelling star-forming clouds that combines two different models of the thermal evolution of the interstellar medium (ISM). In the combined model, where the densities are low enough that at least some part of the spectrum is optically thin, a model of the thermodynamics of the diffuse ISM is more significant in setting the temperatures. Where the densities are high enough to be optically thick across the spectrum, a model of flux-limited diffusion is more appropriate. Previous methods either model the low-density ISM and ignore the thermal behaviour at high densities (e.g. inside collapsing molecular cloud cores), or model the thermal behaviour near protostars but assume a fixed background temperature (e.g. approximate to 10 K) on large scales. Our new method treats both regimes. It also captures the different thermal evolution of the gas, dust, and radiation separately. We compare our results with those from the literature, and investigate the dependence of the thermal behaviour of the gas on the various model parameters. This new method should allow us to model the ISM across a wide range of densities and, thus, develop a more complete and consistent understanding of the role of thermodynamics in the star formation process. C1 [Bate, Matthew R.] Univ Exeter, Sch Phys & Astron, Exeter EX4 4QL, Devon, England. [Keto, Eric R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02420 USA. [Keto, Eric R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Bate, MR (reprint author), Univ Exeter, Sch Phys & Astron, Stocker Rd, Exeter EX4 4QL, Devon, England. EM mbate@astro.ex.ac.uk FU European Research Council under the European Community [339248]; STFC; Large Facilities Capital Fund of BIS; University of Exeter FX We thank Paul Clark for constructive criticism that helped improve the method, and the anonymous referee whose comments helped us improve the manuscript. This work was supported by the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013 grant ggreement no. 339248). The calculations for this paper were performed on the University of Exeter Supercomputer, a DiRAC Facility jointly funded by STFC, the Large Facilities Capital Fund of BIS, and the University of Exeter, and on the Complexity DiRAC Facility jointly funded by STFC and the Large Facilities Capital Fund of BIS. NR 96 TC 4 Z9 4 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 MAY 21 PY 2015 VL 449 IS 3 BP 2643 EP 2667 DI 10.1093/mnras/stv451 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800035 ER PT J AU Zelati, FC Rea, N Papitto, A Vigano, D Pons, JA Turolla, R Esposito, P Haggard, D Baganoff, FK Ponti, G Israel, GL Campana, S Torres, DF Tiengo, A Mereghetti, S Perna, R Zane, S Mignani, RP Possenti, A Stella, L AF Zelati, F. Coti Rea, N. Papitto, A. Vigano, D. Pons, J. A. Turolla, R. Esposito, P. Haggard, D. Baganoff, F. K. Ponti, G. Israel, G. L. Campana, S. Torres, D. F. Tiengo, A. Mereghetti, S. Perna, R. Zane, S. Mignani, R. P. Possenti, A. Stella, L. TI The X-ray outburst of the Galactic Centre magnetar SGR J1745-2900 during the first 1.5 year SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: magnetars; Galaxy: centre; X-rays: individual: SGR J1745-2900 ID SAGITTARIUS-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; XMM-NEWTON OBSERVATIONS; PHOTON IMAGING CAMERA; QUARK-NOVA REMNANTS; SOFT GAMMA REPEATER; FIELD MAGNETAR; NEUTRON-STARS; 3XMM J185246.6+003317; TRANSIENT MAGNETAR AB In 2013 April a new magnetar, SGR 1745-2900, was discovered as it entered an outburst, at only 2.4 arcsec angular distance from the supermassive black hole at the centre of the Milky Way, Sagittarius A*. SGR 1745-2900 has a surface dipolar magnetic field of similar to 2 x 10(14) G, and it is the neutron star closest to a black hole ever observed. The new source was detected both in the radio and X-ray bands, with a peak X-ray luminosity L-X similar to 5 x 10(35) erg s(-1). Here we report on the long-term Chandra (25 observations) and XMM-Newton (eight observations) X-ray monitoring campaign of SGR 1745-2900 from the onset of the outburst in 2013 April until 2014 September. This unprecedented data set allows us to refine the timing properties of the source, as well as to study the outburst spectral evolution as a function of time and rotational phase. Our timing analysis confirms the increase in the spin period derivative by a factor of similar to 2 around 2013 June, and reveals that a further increase occurred between 2013 October 30 and 2014 February 21. We find that the period derivative changed from 6.6 x 10(-12) to 3.3 x 10(-11) s s(-1) in 1.5 yr. On the other hand, this magnetar shows a slow flux decay compared to other magnetars and a rather inefficient surface cooling. In particular, starquake-induced crustal cooling models alone have difficulty in explaining the high luminosity of the source for the first similar to 200 d of its outburst, and additional heating of the star surface from currents flowing in a twisted magnetic bundle is probably playing an important role in the outburst evolution. C1 [Zelati, F. Coti] Univ Insubria, I-22100 Como, Italy. [Zelati, F. Coti; Rea, N.] Univ Amsterdam, Anton Pannekoek Inst Astron, NL-1090 GE Amsterdam, Netherlands. [Zelati, F. Coti; Campana, S.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Rea, N.; Papitto, A.; Vigano, D.; Torres, D. F.] CSIC IEEC, Inst Space Sci ICE, E-08193 Barcelona, Spain. [Pons, J. A.] Univ Alacant, Dept Fis Aplicada, E-03080 Alacant, Spain. [Turolla, R.] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy. [Turolla, R.; Zane, S.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Esposito, P.; Tiengo, A.; Mereghetti, S.; Mignani, R. P.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Esposito, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Haggard, D.] Amherst Coll, Dept Phys & Astron, Amherst, MA 01002 USA. [Baganoff, F. K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Ponti, G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Israel, G. L.; Stella, L.] Osserv Astron Roma, INAF, I-00040 Rome, Italy. [Torres, D. F.] ICREA, E-08010 Barcelona, Spain. [Tiengo, A.] Ist Univ Studi Super, I-27100 Pavia, Italy. [Tiengo, A.] Ist Nazl Fis Nucl, Sez Pavia, I-27100 Pavia, Italy. [Perna, R.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Mignani, R. P.] Univ Zielona Gora, Kepler Inst Astron, PL-65265 Zielona Gora, Poland. [Possenti, A.] Osservatorio Astron Cagliari, INAF, I-09047 Cagliari, Italy. RP Zelati, FC (reprint author), Univ Insubria, Via Valleggio 11, I-22100 Como, Italy. EM francesco.cotizelati@brera.inaf.it RI PONS, JOSE/D-4687-2012; Rea, Nanda/I-2853-2015; Torres, Diego/O-9422-2016; OI MEREGHETTI, SANDRO/0000-0003-3259-7801; Esposito, Paolo/0000-0003-4849-5092; PONS, JOSE/0000-0003-1018-8126; Rea, Nanda/0000-0003-2177-6388; Torres, Diego/0000-0002-1522-9065; Tiengo, Andrea/0000-0002-6038-1090 FU NWO Vidi Grant; European COST Action [MP1304]; Juan de la Cierva fellowship; Fulbright Research Scholar grant; Chandra X-ray Observatory (CXO) Award [GO3-14121X]; NASA [NAS8-03060]; NASA Swift grant [NNX14AC30G]; EU [FP-PEOPLE-2012-IEF- 331095]; Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft-und Raumfahrt (BMWI/DLR) [FKZ 50 OR 1408]; Max Planck Society; Chandra grants - SAO [G03-13068A, G04-15068X]; European Commission [267251]; ESA Member States; NASA; [AYA2012-39303]; [SGR2014-1073]; [AYA 2013-42184-P] FX FCZ and NR are supported by an NWO Vidi Grant (PI: Rea) and by the European COST Action MP1304 (NewCOMPSTAR). NR, AP, DV, and DFT acknowledge support by grants AYA2012-39303 and SGR2014-1073. AP is supported by a Juan de la Cierva fellowship. JAP acknowledges support by grant AYA 2013-42184-P. PE acknowledges a Fulbright Research Scholar grant administered by the US-Italy Fulbright Commission and is grateful to the Harvard-Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. DH acknowledges support from Chandra X-ray Observatory (CXO) Award Number GO3-14121X, operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060, and also by NASA Swift grant NNX14AC30G. GP acknowledges support via an EU Marie Curie Intra-European fellowship under contract no. FP-PEOPLE-2012-IEF- 331095 and the Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft-und Raumfahrt (BMWI/DLR, FKZ 50 OR 1408) and the Max Planck Society. RP acknowledges partial support by Chandra grants (awarded by SAO) G03-13068A and G04-15068X. RPM acknowledges funding from the European Commission Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 267251. FCZ acknowledges CSIC-IEEC for very kind hospitality during part of the work and Geoffrey Bower for helpful discussions. The scientific results reported in this paper are based on observations obtained with the Chandra X-ray Observatory and XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO, and of softwares and tools 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. NR 62 TC 13 Z9 13 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 MAY 21 PY 2015 VL 449 IS 3 BP 2685 EP 2699 DI 10.1093/mnras/stv480 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800037 ER PT J AU Gullberg, B De Breuck, C Vieira, JD Weiss, A Aguirre, JE Aravena, M Bethermin, M Bradford, CM Bothwell, MS Carlstrom, JE Chapman, SC Fassnacht, CD Gonzalez, AH Greve, TR Hezaveh, Y Holzapfel, WL Husband, K Ma, J Malkan, M Marrone, DP Menten, K Murphy, EJ Reichardt, CL Spilker, JS Stark, AA Strandet, M Welikala, N AF Gullberg, B. De Breuck, C. Vieira, J. D. Weiss, A. Aguirre, J. E. Aravena, M. Bethermin, M. Bradford, C. M. Bothwell, M. S. Carlstrom, J. E. Chapman, S. C. Fassnacht, C. D. Gonzalez, A. H. Greve, T. R. Hezaveh, Y. Holzapfel, W. L. Husband, K. Ma, J. Malkan, M. Marrone, D. P. Menten, K. Murphy, E. J. Reichardt, C. L. Spilker, J. S. Stark, A. A. Strandet, M. Welikala, N. TI The nature of the [C II] emission in dusty star-forming galaxies from the SPT survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high-redshift; galaxies: ISM; galaxies: starburst; infrared: galaxies; submillimetre: galaxies ID 158 MU-M; ULTRALUMINOUS INFRARED GALAXIES; SOUTH-POLE TELESCOPE; LUMINOUS SUBMILLIMETER GALAXIES; SPACE-OBSERVATORY MEASUREMENTS; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; MICRON LINE DEFICIT; HUBBLE DEEP FIELD; SIMILAR-TO 1-2 AB We present [C II] observations of 20 strongly lensed dusty star-forming galaxies at 2.1 < z < 5.7 using Atacama Pathfinder EXperiment and Herschel. The sources were selected on their 1.4 mm flux (S-1.4mm > 20 mJy) from the South Pole Telescope (SPT) survey, with far-infrared (FIR) luminosities determined from extensive photometric data. The [CII] line is robustly detected in 17 sources, all but one being spectrally resolved. 11 out of 20 sources observed in [C II] also have low-J CO detections from Australia Telescope Compact Array. A comparison with mid-and high-J CO lines from Atacama Large Millimeter/submillimeter Array reveals consistent [C II] and CO velocity profiles, suggesting that there is little differential lensing between these species. The [C II], low-J CO and FIR data allow us to constrain the properties of the interstellar medium. We find [C II] to CO(1-0) luminosity ratios in the SPT sample of 5200 +/- 1800, with significantly less scatter than in other samples. This line ratio can be best described by a medium of [C II] and CO emitting gas with a higher [C II] than CO excitation temperature, high CO optical depth tau(CO)(1-0) >> 1, and low to moderate [CII] optical depth tau[C II] less than or similar to 1. The geometric structure of photodissociation regions allows for such conditions. C1 [Gullberg, B.; De Breuck, C.; Bethermin, M.] European So Observ, D-85748 Garching, Germany. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Weiss, A.; Menten, K.; Strandet, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA. [Aravena, M.] European So Observ, Santiago 19, Chile. [Aravena, M.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. [Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bothwell, M. S.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HA, England. [Carlstrom, J. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Chapman, S. C.] Dalhousie Univ, Halifax, NS B3H 4R2, Canada. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Gonzalez, A. H.; Ma, J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hezaveh, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Holzapfel, W. L.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Husband, K.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Marrone, D. P.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murphy, E. J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Welikala, N.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Gullberg, B (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM bgullber@eso.org RI Holzapfel, William/I-4836-2015; OI Marrone, Daniel/0000-0002-2367-1080; De Breuck, Carlos/0000-0002-6637-3315; Stark, Antony/0000-0002-2718-9996 FU National Aeronautics and Space Administration; Commonwealth of Australia; US National Science Foundation [AST-1312950]; National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947] FX This publication is based on data acquired with the APEX. APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00957.S, ADS/JAO.ALMA#2011.0.00958.S and ADS/JAO. ALMA#2012.1.00844.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 Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System Bibliographic Services; This material is based on work supported by the US National Science Foundation under grant no. AST-1312950. The SPT is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. NR 126 TC 18 Z9 18 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 MAY 21 PY 2015 VL 449 IS 3 BP 2883 EP 2900 DI 10.1093/mnras/stv372 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TP UT WOS:000355337800055 ER PT J AU Butler, MJ Tan, JC Van Loo, S AF Butler, Michael J. Tan, Jonathan C. Van Loo, Sven TI KILOPARSEC-SCALE SIMULATIONS OF STAR FORMATION IN DISK GALAXIES. III. STRUCTURE AND DYNAMICS OF FILAMENTS AND CLUMPS IN GIANT MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; galaxies: star clusters: general; ISM: clouds; ISM: structure; methods: numerical; stars: formation ID INFRARED DARK CLOUDS; MILKY-WAY; GRAVITATIONAL-INSTABILITY; GAS; I.; TURBULENCE; CLUSTERS; GRAVITY; CORES; RESOLUTION AB We present hydrodynamic simulations of self-gravitating dense gas in a galactic disk, exploring scales ranging from 1 kpc down to similar to 0.1 pc. Our primary goal is to understand how dense filaments form in giant molecular clouds (GMCs). These structures, often observed as infrared dark clouds (IRDCs) in the Galactic plane, are thought to be the precursors to massive stars and star clusters, so their formation may be the rate-limiting step controlling global star formation rates in galactic systems as described by the Kennicutt-Schmidt relation. Our study follows on from Van Loo et al., which carried out simulations to 0.5 pc resolution and examined global aspects of the formation of dense gas clumps and the resulting star formation rate. Here, using our higher resolution, we examine the detailed structural, kinematic, and dynamical properties of dense filaments and clumps, including mass surface density (Sigma) probability distribution functions, filament mass per unit length and its dispersion, lateral Sigma profiles, filament fragmentation, filament velocity gradients and infall, and degree of filament and clump virialization. Where possible, these properties are compared to observations of IRDCs. By many metrics, especially too large mass fractions of high Sigma > 1 g cm(-2) material, too high mass per unit length dispersion due to dense clump formation, too high velocity gradients, and too high velocity dispersion for a given mass per unit length, the simulated filaments differ from observed IRDCs. We thus conclude that IRDCs do not form from global fast collapse of GMCs. Rather, we expect that IRDC formation and collapse are slowed significantly by the influence of dynamically important magnetic fields, which may thus play a crucial role in regulating galactic star formation rates. C1 [Butler, Michael J.] Univ Zurich, Inst Computat Sci, CH-8049 Zurich, Switzerland. [Tan, Jonathan C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Tan, Jonathan C.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. [Van Loo, Sven] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Van Loo, Sven] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Butler, MJ (reprint author), Univ Zurich, Inst Computat Sci, CH-8049 Zurich, Switzerland. FU STAR-FORM Sinergia project - Swiss National Science Foundation; Theory Postdoctoral Fellowship from UF Department of Astronomy and College of Liberal Arts and Sciences; SMA Postdoctoral Fellowship of the Smithsonian Astrophysical Observatory; NSF CAREER grant [AST-0645412]; NASA Astrophysics Theory and Fundamental Physics grant [ATP09-0094]; NASA Astrophysics Data Analysis Program [ADAP10-0110]; University of Florida Research Computing; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center FX We thank Paola Caselli and Sam Falle for useful discussions, and Elizabeth Tasker for providing the initial conditions of our simulations. M.J.B. acknowledges support from the STAR-FORM Sinergia project funded by the Swiss National Science Foundation. S.v.L. acknowledges support from the Theory Postdoctoral Fellowship from UF Department of Astronomy and College of Liberal Arts and Sciences and from the SMA Postdoctoral Fellowship of the Smithsonian Astrophysical Observatory. J.C.T. acknowledges support from NSF CAREER grant AST-0645412; NASA Astrophysics Theory and Fundamental Physics grant ATP09-0094; NASA Astrophysics Data Analysis Program ADAP10-0110. Resources supporting this work were provided by the University of Florida Research Computing and the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 54 TC 4 Z9 4 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 MAY 20 PY 2015 VL 805 IS 1 AR 1 DI 10.1088/0004-637X/805/1/1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300001 ER PT J AU Canovas, H Schreiber, MR Caceres, C Menard, F Pinte, C Mathews, GS Cieza, L Casassus, S Hales, A Williams, JP Roman, P Hardy, A AF Canovas, H. Schreiber, M. R. Caceres, C. Menard, F. Pinte, C. Mathews, G. S. Cieza, L. Casassus, S. Hales, A. Williams, J. P. Roman, P. Hardy, A. TI GAS INSIDE THE 97 AU CAVITY AROUND THE TRANSITION DISK Sz 91 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planet-disk interactions; protoplanetary disks; stars: individual (Sz 91); stars: variables: T Tauri, Herbig Ae/Be ID SPITZER C2D SURVEY; T-TAURI STARS; PROTOPLANETARY DISKS; SUBMILLIMETER ARRAY; CIRCUMSTELLAR DISKS; RADIATIVE-TRANSFER; MULTIPLE PLANETS; DUST EMISSION; MASS STARS; INNER HOLE AB We present ALMA (Cycle 0) band. 6 and band. 3 observations of the transition disk Sz 91. The disk inclination and position angle are determined to be i - 49.5 +/- 3.5 degrees and PA - 18.2 +/- 3.5 and the dusty and gaseous disk are detected up to similar to 220 and similar to 400 AU from the star, respectively. Most importantly, our continuum observations indicate that the cavity size in the millimeter-sized dust distribution must be similar to 97 AU in radius, the largest cavity observed around a T Tauri star. Our data clearly confirm. the presence of (CO)-C-12 (2-1) well inside the dust cavity. Based on these observational constraints we developed a disk model that simultaneously accounts for the (CO)-C-12 and continuum observations (i.e., gaseous and dusty disk). According to our model, most of the millimeter emission comes from a ring located between 97 and 140 AU. We also find that the dust cavity is divided into an innermost region largely depleted of dust particles ranging from the dust sublimation radius up to 85 AU, and a second, moderately dust-depleted region, extending from 85 to 97 AU. The extremely large size of the dust cavity, the presence of gas and small dust particles within the cavity, and the accretion rate of Sz 91 are consistent with the formation of multiple (giant) planets. C1 [Canovas, H.; Schreiber, M. R.; Caceres, C.; Hardy, A.] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile. [Menard, F.; Pinte, C.] CNRS INSU, UMI 3386, UMI FCA, Paris, France. [Menard, F.; Pinte, C.; Casassus, S.] Univ Chile, Dept Astron, Santiago, Chile. [Mathews, G. S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Mathews, G. S.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA. [Cieza, L.] Univ Diego Portales, Fac Ingn, Santiago, Chile. [Hales, A.] Joint ALMA Observ, Atacama Large Millimeter Submillimeter Array, Santiago 7630355, Chile. [Williams, J. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roman, P.] Univ Chile, Ctr Math Modeling, Santiago, Chile. RP Canovas, H (reprint author), Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile. EM hector.canovas@dfa.uv.cl RI Casassus, Simon/I-8609-2016; Caceres, Claudio/Q-6297-2016; OI Roman, Pablo/0000-0002-7105-9371; Canovas, Hector/0000-0001-7668-8022; Williams, Jonathan/0000-0001-5058-695X FU Millenium Science Initiative, Chilean Ministry of Economy, Nucleus [RC130007]; ALMA/CONICYT [31100025, 31130027]; CONICYT-FONDECYT [3140592, 1140109]; FONDECYT [1141269, 1130949, 3140634]; European Commission [PERG06-GA-2009-256513]; Agence Nationale pour la Recherche (ANR) of France [ANR-2010-JCJC-0504-01]; ALMA-CONICYT [31120009, 31120006]; NSF [AST-1208911]; NASA [NNX15AC92G]; National Aeronautics and Space Administration; National Science Foundation FX The authors thank the anonymous referee for providing very constructive comments, which significantly helped to improve the paper. We are grateful to the ALMA staff. This research was funded by the Millenium Science Initiative, Chilean Ministry of Economy, Nucleus RC130007. H.C. and C.C. are grateful for support from ALMA/CONICYT (grants 31100025 and 31130027). C.C. also acknowledges support from CONICYT-FONDECYT grant 3140592. M.R.S. acknowledges support from FONDECYT (grant 1141269). C.P. acknowledges funding from the European Commission's 7th Framework Program (contract PERG06-GA-2009-256513) and Agence Nationale pour la Recherche (ANR) of France (contract ANR-2010-JCJC-0504-01). L.C. was supported by ALMA-CONICYT grant number 31120009 and CONICYT-FONDECYT grant number 1140109. S.C. acknowledges support from FONDECYT grant 1130949. J.P.W. acknowledges support from NSF grant AST-1208911 and NASA grant NNX15AC92G. P.R. acknowledges support from ALMA-CONICYT 31120006 and FONDECYT grant 3140634. 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 paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00733.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 62 TC 17 Z9 17 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 MAY 20 PY 2015 VL 805 IS 1 AR 21 DI 10.1088/0004-637X/805/1/21 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300021 ER PT J AU Crites, AT Henning, JW Ade, PAR Aird, KA Austermann, JE Beall, JA Bender, AN Benson, BA Bleem, LE Carlstrom, JE Chang, CL Chiang, HC Cho, HM Citron, R Crawford, TM De Haan, T Dobbs, MA Everett, W Gallicchio, J Gao, J George, EM Gilbert, A Halverson, NW Hanson, D Harrington, N Hilton, GC Holder, GP Holzapfel, WL Hoover, S Hou, Z Hrubes, JD Huang, N Hubmayr, J Irwin, KD Keisler, R Knox, L Lee, AT Leitch, EM Li, D Liang, C Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Mocanu, L Montroy, TE Natoli, T Nibarger, JP Novosad, V Padin, S Pryke, C Reichardt, CL Ruhl, JE Saliwanchik, BR Sayre, JT Schaffer, KK Smecher, G Stark, AA Story, KT Tucker, C Vanderlinde, K Vieira, JD Wang, G Whitehorn, N Yefremenko, V Zahn, O AF Crites, A. T. Henning, J. W. Ade, P. A. R. Aird, K. A. Austermann, J. E. Beall, J. A. Bender, A. N. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Chiang, H. C. Cho, H-M. Citron, R. Crawford, T. M. De Haan, T. Dobbs, M. A. Everett, W. Gallicchio, J. Gao, J. George, E. M. Gilbert, A. Halverson, N. W. Hanson, D. Harrington, N. Hilton, G. C. Holder, G. P. Holzapfel, W. L. Hoover, S. Hou, Z. Hrubes, J. D. Huang, N. Hubmayr, J. Irwin, K. D. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Li, D. Liang, C. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Montroy, T. E. Natoli, T. Nibarger, J. P. Novosad, V. Padin, S. Pryke, C. Reichardt, C. L. Ruhl, J. E. Saliwanchik, B. R. Sayre, J. T. Schaffer, K. K. Smecher, G. Stark, A. A. Story, K. T. Tucker, C. Vanderlinde, K. Vieira, J. D. Wang, G. Whitehorn, N. Yefremenko, V. Zahn, O. TI MEASUREMENTS OF E-MODE POLARIZATION AND TEMPERATURE-E-MODE CORRELATION IN THE COSMIC MICROWAVE BACKGROUND FROM 100 SQUARE DEGREES OF SPTPOL DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; polarization ID SOUTH-POLE TELESCOPE; SZ SURVEY; POWER SPECTRUM; HIGH-FREQUENCY; RADIO-SOURCES; ANISOTROPIES; DEG(2); QUAD; CONSTRAINTS; COMPUTATION AB We present measurements of E-mode polarization and temperature-E-mode correlation in the cosmic microwave background using data from the first season of observations with SPTpol, the polarization-sensitive receiver currently installed on the South Pole Telescope (SPT). The observations used in this work cover 100 deg(2) of sky with arcminute resolution at 150 GHz. We report the E-mode angular auto-power spectrum (EE) and the temperature-E-mode angular cross-power spectrum (TE) over the multipole range 500 < l <= 5000. These power spectra improve on previous measurements in the high-l (small-scale) regime. We fit the combination of the SPTpol power spectra, data from Planck, and previous SPT measurements with a six-parameter Lambda CDM cosmological model. We find that the best-fit parameters are consistent with previous results. The improvement in high-l sensitivity over previous measurements leads to a significant improvement in the limit on polarized point-source power: after masking sources brighter than 50 mJy in unpolarized flux at 150 GHz, we find a 95% confidence upper limit on unclustered point-source power in the EE spectrum of D-l = l (l + 1) Cl/2 pi < 0.40 mu K-2 at l = 3000, indicating that future EE measurements will not be limited by power from unclustered point sources in the multipole range l < 3600, and possibly much higher in l. C1 [Crites, A. T.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Meyer, S. S.; Padin, S.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Crites, A. T.; Henning, J. W.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Citron, R.; Crawford, T. M.; Gallicchio, J.; Hoover, S.; Hou, Z.; Leitch, E. M.; Meyer, S. S.; Mocanu, L.; Padin, S.; Schaffer, K. K.; Story, K. T.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Crites, A. T.] CALTECH, Pasadena, CA 91125 USA. [Henning, J. W.; Austermann, J. E.; Everett, W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Ade, P. A. R.] Cardiff Univ, Cardiff CF10 3XQ, S Glam, Wales. [Aird, K. A.; Liang, C.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Beall, J. A.; Gao, J.; Hilton, G. C.; Nibarger, J. P.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Bender, A. N.; Hanson, D.; Holder, G. P.; Smecher, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Mehl, J.; Yefremenko, V.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Meyer, S. S.; Natoli, T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Durban, South Africa. [Cho, H-M.; Irwin, K. D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Dobbs, M. A.] CIFAR Program Cosmol & Grav, Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada. [George, E. M.; Harrington, N.; Holzapfel, W. L.; Huang, N.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Irwin, K. D.; Keisler, R.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Keisler, R.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Novosad, V.] Argonne Natl Lab, Div Mat Sci, Argonne, IL 60439 USA. [Pryke, C.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Smecher, G.] Three Speed Log Inc, Vancouver, BC V6A 2J8, Canada. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP Crites, AT (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM acrites@caltech.edu RI Holzapfel, William/I-4836-2015; Novosad, V /J-4843-2015; OI CRAWFORD, THOMAS/0000-0001-9000-5013; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU Natural Sciences and Engineering Research Council of Canada; Canadian Institute for Advanced Research; Canada Research Chairs program; National Science Foundation [PLR-1248097, AST-1402161]; NSF Physics Frontier Center grant [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation [947]; Fermi Research Alliance, LLC [De-AC02-07CH11359]; US Department of Energy; NSF [AST0956135]; UChicago Argonne, LLC, Operator of Argonne National Laboratory (Argonne); Argonne, US Department of Energy Office of Science Laboratory [DE-AC02-06CH11357]; Argonne Center for Nanoscale Materials FX We thank Joshua Schiffrin for help with the mode-mode coupling kernel calculation. We also thank Wayne Hu and Aurien Benoit-Levy for help implementing the super-sample lensing covariance. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and Canada Research Chairs program. The South Pole Telescope program is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant GBMF#947 to the University of Chicago. J.W.H. is supported by the National Science Foundation under Award No. AST-1402161. B.B. is supported by the Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the US Department of Energy. The CU Boulder group acknowledges support from NSF AST-0956135. This work is also supported by the US Department of Energy. Work at Argonne National Lab is supported by UChicago Argonne, LLC, Operator of Argonne National Laboratory (Argonne). Argonne, a US Department of Energy Office of Science Laboratory, is operated under Contract No. DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. The data analysis pipeline uses the scientific python stack (Jones et al. 2001; Hunter 2007; van der Walt et al. 2011) and the HDF5 file format (The HDF Group 1997). NR 56 TC 14 Z9 14 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 MAY 20 PY 2015 VL 805 IS 1 AR 36 DI 10.1088/0004-637X/805/1/36 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300036 ER PT J AU Frisch, PC Andersson, BG Berdyugin, A Piirola, V Funsten, HO Magalhaes, AM Seriacopi, DB McComas, DJ Schwadron, NA Slavin, JD Wiktorowicz, SJ AF Frisch, P. C. Andersson, B-G Berdyugin, A. Piirola, V. Funsten, H. O. Magalhaes, A. M. Seriacopi, D. B. McComas, D. J. Schwadron, N. A. Slavin, J. D. Wiktorowicz, S. J. TI EVIDENCE FOR AN INTERSTELLAR DUST FILAMENT IN THE OUTER HELIOSHEATH SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: magnetic fields; polarization; Sun: heliosphere ID BOUNDARY-EXPLORER RIBBON; IBEX-LO OBSERVATIONS; NEUTRAL ATOM FLUX; PICK-UP IONS; 1ST 5 YEARS; MAGNETIC-FIELD; SOLAR-SYSTEM; VOYAGER 1; HELIOPAUSE; GRAINS AB A recently discovered filament of polarized starlight that traces a coherent magnetic field is shown to have several properties that are consistent with an origin in the outer heliosheath of the heliosphere: (1) the magnetic field that provides the best fit to the polarization position angles is directed toward l = 357 degrees.3, b = 17 degrees.0 (+/- 11 degrees.2); this direction is within 6 degrees.7 +/- 11 degrees.2 of the observed upwind direction of the flow of interstellar neutral helium gas through the heliosphere. (2) The magnetic field is ordered; the component of the variation of the polarization position angles that can be attributed to magnetic turbulence is +/- 9 degrees.6. (3) The axis of the elongated filament can be approximated by a line that defines an angle of 80 degrees +/- 14 degrees with the plane that is formed by the interstellar magnetic field (ISMF) vector and the vector of the inflowing neutral gas (the BV plane). We propose that this polarization feature arises from aligned interstellar dust grains in the outer heliosheath where the interstellar plasma and magnetic field are deflected around the heliosphere. This interpretation suggests that the polarization is seen where stream lines of the flow and the draped ISMF lines are approximately parallel to each other and perpendicular to the sightline. An ordered magnetic field is required so that grain alignment is not disrupted during the interaction. The filament location is consistent with dust plumes previously predicted to form around the heliosphere. The proposed outer heliosheath location of the polarizing grains can be tested with three-dimensional models that track torques on asymmetric dust grains as they propagate through the heliosheath plasma, and using these models to evaluate grain alignment and the asymmetric extinction of the grains. C1 [Frisch, P. C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Andersson, B-G] USRA, SOFIA, San Francisco, CA USA. [Berdyugin, A.; Piirola, V.] Univ Turku, Finnish Ctr Astron ESO, SF-20500 Turku, Finland. [Funsten, H. O.] Los Alamos Natl Lab, Los Alamos, NM USA. [Magalhaes, A. M.; Seriacopi, D. B.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508 Sao Paulo, Brazil. [McComas, D. J.] SW Res Inst, San Antonio, TX USA. [Schwadron, N. A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Slavin, J. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wiktorowicz, S. J.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [McComas, D. J.] Univ Texas San Antonio, San Antonio, TX USA. RP Frisch, PC (reprint author), Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. OI Andersson, B-G/0000-0001-6717-0686; Funsten, Herbert/0000-0002-6817-1039; Slavin, Jonathan/0000-0002-7597-6935 FU NASA Explorer program; European Research Council Advanced Grant HotMol [ERC-2011-AdG 291659] FX This research has been partly supported by the NASA Explorer program through support for the IBEX mission, and by the European Research Council Advanced Grant HotMol (ERC-2011-AdG 291659). NR 75 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 MAY 20 PY 2015 VL 805 IS 1 AR 60 DI 10.1088/0004-637X/805/1/60 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300060 ER PT J AU Hlavacek-Larrondo, J McDonald, M Benson, BA Forman, WR Allen, SW Bleem, LE Ashby, MLN Bocquet, S Brodwin, M Dietrich, JP Jones, C Liu, J Reichardt, CL Saliwanchik, BR Saro, A Schrabback, T Song, J Stalder, B Vikhlinin, A Zenteno, A AF Hlavacek-Larrondo, J. McDonald, M. Benson, B. A. Forman, W. R. Allen, S. W. Bleem, L. E. Ashby, M. L. N. Bocquet, S. Brodwin, M. Dietrich, J. P. Jones, C. Liu, J. Reichardt, C. L. Saliwanchik, B. R. Saro, A. Schrabback, T. Song, J. Stalder, B. Vikhlinin, A. Zenteno, A. TI X-RAY CAVITIES IN A SAMPLE OF 83 SPT-SELECTED CLUSTERS OF GALAXIES: TRACING THE EVOLUTION OF AGN FEEDBACK IN CLUSTERS OF GALAXIES OUT TO z=1.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: clusters: general; galaxies: jets; X-rays: galaxies: clusters ID DEEP CHANDRA OBSERVATION; ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; POLE TELESCOPE SURVEY; HEATING HOT ATMOSPHERES; RADIO IMAGING SURVEY; 720 SQUARE DEGREES; ELLIPTIC GALAXIES; JET POWER; COOL-CORE AB X-ray cavities are key tracers of mechanical (or radio mode) heating arising from the active galactic nuclei (AGNs) in brightest cluster galaxies (BCGs). We report on a survey for X-ray cavities in 83 massive, high-redshift (0.4 < z < 1.2) clusters of galaxies selected by their Sunyaev-Zel'dovich signature in the South Pole Telescope data. Based on Chandra X-ray images, we find a total of six clusters having symmetric pairs of surface brightness depressions consistent with the picture of radio jets inflating X-ray cavities in the intracluster medium (ICM). The majority of these detections are of relatively low significance and require deeper follow-up data in order to be confirmed. Further, this search will miss small (<10 kpc) X-ray cavities that are unresolved by Chandra at high (z greater than or similar to 5) redshift. Despite these limitations, our results suggest that the power generated by AGN feedback in BCGs has remained unchanged for over half of the age of the universe (>7 Gyr at z similar to 0.8). On average, the detected X-ray cavities have powers of (0.8-5) x 10(45) erg s(-1), enthalpies of (3-6) x 10(59) erg, and radii of similar to 17 kpc. Integrating over 7 Gyr, we find that the supermassive black holes in BCGs may have accreted 10(8) to several 10(9) M-circle dot of material to power these outflows. This level of accretion indicates that significant supermassive black hole growth may occur not only at early times, in the quasar era, but at late times as well. We also find that X-ray cavities at high redshift may inject an excess heat of 0.1-1.0 keV per particle into the hot ICM above and beyond the energy needed to offset cooling. Although this result needs to be confirmed, we note that the magnitude of excess heating is similar to the energy needed to preheat clusters, break self-similarity, and explain the excess entropy in hot atmospheres. C1 [Hlavacek-Larrondo, J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Hlavacek-Larrondo, J.; Allen, S. W.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Hlavacek-Larrondo, J.; Allen, S. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Benson, B. A.; Bleem, L. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Bleem, L. E.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Benson, B. A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Forman, W. R.; Ashby, M. L. N.; Jones, C.; Stalder, B.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Bleem, L. E.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Bleem, L. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bocquet, S.; Dietrich, J. P.; Liu, J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bocquet, S.; Dietrich, J. P.; Liu, J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Saliwanchik, B. R.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Schrabback, T.] Argelander Inst Astron, D-53121 Bonn, Germany. [Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Song, J.] Korea Astron & Space Sci Inst, Taejon, South Korea. [Stalder, B.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Zenteno, A.] Cerro Tololo Interamer Observ, La Serena, Chile. RP Hlavacek-Larrondo, J (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM juliehl@astro.umontreal.ca OI Dietrich, Jorg/0000-0002-8134-9591; Reichardt, Christian/0000-0003-2226-9169; Bocquet, Sebastian/0000-0002-4900-805X; Forman, William/0000-0002-9478-1682 FU NASA [PF2-130094]; NSERC; Canada Research Chair programs; FRQNT; National Science Foundation [ANT-0638937, PLR-1248097]; NSF Physics Frontier Center grant [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF grant [AST-1009012, AST-1009649, MRI-0723073]; U.S. Department of Energy [DE-AC02-06CH11357, DE-AC02-76SF00515]; NASA through Chandra X-ray Observatory Center [12800071, 12800088, 13800883] FX J.H.L. is supported by NASA through the Einstein Fellowship Program, grant number PF2-130094, NSERC through the discovery grant and Canada Research Chair programs, as well as FRQNT. Partial support is also provided by the National Science Foundation through grants ANT-0638937 and PLR-1248097, 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. This work was supported in part by the U.S. Department of Energy contract numbers DE-AC02-06CH11357 and DE-AC02-76SF00515. NR 84 TC 13 Z9 13 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 35 DI 10.1088/0004-637X/805/1/35 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300035 ER PT J AU Kong, S Lada, CJ Lada, EA Roman-Zuniga, C Bieging, JH Lombardi, M Forbrich, J Alves, JF AF Kong, S. Lada, C. J. Lada, E. A. Roman-Zuniga, C. Bieging, J. H. Lombardi, M. Forbrich, J. Alves, J. F. TI THE RELATIONSHIP BETWEEN THE DUST AND GAS-PHASE CO ACROSS THE CALIFORNIA MOLECULAR CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: abundances; ISM: clouds; stars: formation ID CO-TO-H-2 CONVERSION FACTOR; INTER-STELLAR CLOUDS; X-FACTOR; STAR-FORMATION; DARK CLOUD; EXTINCTION MAPS; CARBON-MONOXIDE; PIPE NEBULA; IC 5146; EMISSION AB We present results of an extinction-CO line survey of the southeastern part of the California molecular cloud (CMC). Deep, wide-field, near-infrared images were used to construct a sensitive, relatively high resolution (similar to 0.5 arcmin) (NICEST) extinction map of the region. The same region was also surveyed in the (CO)-C-12(2-1), (CO)-C-13(2-1), and (CO)-O-18(2-1) emission lines at the same angular resolution. These data were used to investigate the relation between the molecular gas, traced by CO emission lines, and the dust column density, traced by extinction, on spatial scales of 0.04 pc across the cloud. We found strong spatial variations in the abundances of (CO)-C-13 and (CO)-O-18 that were correlated with variations in gas temperature, consistent with temperature-dependent CO depletion/ desorption on dust grains. The (CO)-C-13-to-(CO)-O-18 abundance ratio was found to increase with decreasing extinction, suggesting selective photodissociation of (CO)-O-18 by the ambient UV radiation field. The effect is particularly pronounced in the vicinity of an embedded cluster where the UV radiation appears to have penetrated deeply (i.e., A(V) less than or similar to 15 mag) into the cloud. We derived the cloud-averaged X-factor to be < X-CO > = 2.53 x 10(20) cm(2)(K km s(-1))(-1), a value somewhat higher than the Milky Way average. On sub-parsec scales we find there is no single empirical value of the (CO)-C-12 X-factor that can characterize the molecular gas in cold (T-k less than or similar to 15 K) cloud regions, with X-CO infinity A(V)(0.74) for A(V) greater than or similar to 3 mag. However, in regions containing relatively hot (Tex greater than or similar to 25 K) molecular gas we find a clear correlation between W((CO)-C-12) and A(V) over a large (3 less than or similar to A(V) less than or similar to 25 mag) range of extinction. This results in a constant X-CO = 1.5 x 10(20) cm(-2)(K km s(-1))(-1) for the hot gas, a lower value than either the average for the CMC or the Milky Way. Overall we find an (inverse) correlation between X-CO and T-ex in the cloud with X-CO infinity T-ex(-0.7). This correlation suggests that the global X-factor of a giant molecular cloud may depend on the relative amounts of hot gas contained within the cloud. C1 [Kong, S.; Lada, E. A.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roman-Zuniga, C.] Univ Nacl Autonoma Mexico, Inst Astron, Unidad Acad Ensenada, Ensenada 22860, Baja California, Mexico. [Bieging, J. H.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Lombardi, M.] Univ Milan, Dept Phys, I-20122 Milan, Italy. [Forbrich, J.; Alves, J. F.] Univ Vienna, Vienna, Austria. RP Kong, S (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM skong@astro.ufl.edu RI Roman-Zuniga, Carlos/F-6602-2016; OI Roman-Zuniga, Carlos/0000-0001-8600-4798; LOMBARDI, MARCO/0000-0002-3336-4965; Kong, Shuo/0000-0002-8469-2029; Alves, Joao/0000-0002-4355-0921 FU CONACYT project, Mexico [CB2010-152160]; National Science Foundation [AST-1140030] FX We thank Kelsey Jorgenson for assistance with acquiring the CO observations and acknowledge useful discussions with Karin Oberg. Suggestions from an anonymous referee led to numerous improvements in the paper. Carlos Roman acknowledges support from CONACYT project CB2010-152160, Mexico. This research is based in part on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). The Heinrich Hertz Submillimeter Telescope is operated by the Arizona Radio Observatory, which is part of the Steward Observatory at the University of Arizona. This work was supported in part by National Science Foundation grant AST-1140030 to the University of Arizona. NR 52 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 58 DI 10.1088/0004-637X/805/1/58 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300058 ER PT J AU Pillitteri, I Maggio, A Micela, G Sciortino, S Wolk, SJ Matsakos, T AF Pillitteri, I. Maggio, A. Micela, G. Sciortino, S. Wolk, S. J. Matsakos, T. TI FUV VARIABILITY OF HD 189733. IS THE STAR ACCRETING MATERIAL FROM ITS HOT JUPITER? SO ASTROPHYSICAL JOURNAL LA English DT Article DE planet-star interactions; planetary systems; stars: activity; stars: chromospheres ID STELLAR ACTIVITY ENHANCEMENT; FRAGMENTS FALLING BACK; X-RAY ACTIVITY; I LYMAN-ALPHA; HOST STARS; ATMOSPHERIC ESCAPE; GIANT PLANETS; CHROMOSPHERIC ACTIVITY; PHOTOSPHERIC ACTIVITY; MAGNETIC INTERACTION AB Hot Jupiters are subject to strong irradiation from their host stars and, as a consequence, they do evaporate. They can also interact with the parent stars by means of tides and magnetic fields. Both phenomena have strong implications for the evolution of these systems. Here we present time-resolved spectroscopy of HD 189733 observed with the Cosmic Origins Spectrograph on board. Hubble Space Telescope (HST). The star has been observed during five consecutive HST orbits, starting at a secondary transit of the planet (phi similar to 0.50-0.63). Two main episodes of variability of ion lines of Si, C, N, and O are detected, with an increase of line fluxes. The Si IV. lines show the highest degree of variability. The far-ultraviolet variability is a signature of enhanced activity in phase with the planet motion, occurring after the planet egress, as already observed three times in X-rays. With the support of MHD simulations, we propose the following interpretation: a stream of gas evaporating from the planet is actively and almost steadily accreting onto the stellar surface, impacting at 70 degrees-90 degrees ahead of the subplanetary point. C1 [Pillitteri, I.; Maggio, A.; Micela, G.; Sciortino, S.] INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matsakos, T.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Pillitteri, I (reprint author), INAF, Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. EM pilli@astropa.inaf.it RI Maggio, Antonio/P-5700-2015; Pillitteri, Ignazio/L-1549-2016; OI Maggio, Antonio/0000-0001-5154-6108; Pillitteri, Ignazio/0000-0003-4948-6550; Micela, Giuseppina/0000-0002-9900-4751; Matsakos, Titos/0000-0003-0447-2147 FU European Union Seventh Framework Programme (FP7) under Astronomy Fellowships in Italy (AstroFIt) [267251]; NASA ATP grant [NNX13AH56G]; NASA [NAS 5-26555]; NASA through a grant from the Space Telescope Science Institute [12984] FX I.P. is grateful to H. M. Gunther for the help and the discussion of the results. I.P. acknowledges financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251 Astronomy Fellowships in Italy (AstroFIt). T.M. was supported in part by NASA ATP grant NNX13AH56G. The simulation was carried out with resources provided by the University of Chicago Research Computing Center. This work is 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 #12984. Support for program #12984 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. NR 54 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 52 DI 10.1088/0004-637X/805/1/52 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300052 ER PT J AU Tetarenko, AJ Sivakoff, GR Miller-Jones, JCA Curran, PA Russell, TD Coulson, IM Heinz, S Maitra, D Markoff, SB Migliari, S Petitpas, GR Rupen, MP Rushton, AP Russell, DM Sarazin, CL AF Tetarenko, A. J. Sivakoff, G. R. Miller-Jones, J. C. A. Curran, P. A. Russell, T. D. Coulson, I. M. Heinz, S. Maitra, D. Markoff, S. B. Migliari, S. Petitpas, G. R. Rupen, M. P. Rushton, A. P. Russell, D. M. Sarazin, C. L. TI SUB-mm JET PROPERTIES OF THE X-RAY BINARY SWIFT J1745-26 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; ISM: jets and outflows; radio continuum: stars; stars: individual (Swift J1745-26); submillimeter: stars; X-rays: binaries ID BLACK-HOLE CANDIDATE; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTION; SGR-A-ASTERISK; GX 339-4; COMPACT JET; SAGITTARIUS-A; RELATIVISTIC JETS; RADIO-EMISSION; MULTIWAVELENGTH OBSERVATIONS AB We present the results of our observations of the early stages of the 2012-2013 outburst of the transient black hole X-ray binary (BHXRB), Swift J1745-26, with the Very Large Array, Submillimeter Array, and James Clerk Maxwell telescope (SCUBA-2). Our data mark the first multiple-band mm and sub-mm observations of a BHXRB. During our observations the system was in the hard accretion state producing a steady, compact jet. The unique combination of radio and mm/sub-mm data allows us to directly measure the spectral indices in and between the radio and mm/sub-mm regimes, including the first mm/sub-mm spectral index measured for a BHXRB. Spectral fitting revealed that both the mm (230 GHz) and sub-mm (350 GHz) measurements are consistent with extrapolations of an inverted power law from contemporaneous radio data (1-30 GHz). This indicates that, as standard jet models predict, a power law extending up to mm/sub-mm frequencies can adequately describe the spectrum, and suggests that the mechanism driving spectral inversion could be responsible for the high mm/sub-mm fluxes (compared to radio fluxes) observed in outbursting BHXRBs. While this power law is also consistent with contemporaneous optical data, the optical data could arise from either jet emission with a jet spectral break frequency of nu(break) greater than or similar to 1x10(14) Hz or the combination of jet emission with a lower jet spectral break frequency of nu(break) greater than or similar to 2x10(11) Hz and accretion disk emission. Our analysis solidifies the importance of the mm/sub-mm regime in bridging the crucial gap between radio and IR frequencies in the jet spectrum, and justifies the need to explore this regime further. C1 [Tetarenko, A. J.; Sivakoff, G. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Miller-Jones, J. C. A.; Curran, P. A.; Russell, T. D.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Coulson, I. M.] Joint Astron Ctr, Hilo, HI 96720 USA. [Heinz, S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Maitra, D.] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA. [Markoff, S. B.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Migliari, S.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Migliari, S.] Univ Barcelona, Inst Cosm Sci, E-08028 Barcelona, Spain. [Migliari, S.] ESAC ESA, XMM Newton Sci Operat Ctr, E-28691 Madrid, Spain. [Petitpas, G. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rupen, M. P.] Natl Res Council Canada, Herzberg Astron & Astrophys, Penticton, BC V2A 6J9, Canada. [Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Rushton, A. P.] Univ Oxford, Dept Phys, Astrophys, Oxford OX1 3RH, England. [Rushton, A. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Russell, D. M.] NYU Abu Dhabi, Abu Dhabi, U Arab Emirates. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Tetarenko, AJ (reprint author), Univ Alberta, Dept Phys, CCIS 4-181, Edmonton, AB T6G 2E1, Canada. EM tetarenk@ualberta.ca RI Miller-Jones, James/B-2411-2013; Sivakoff, Gregory/G-9602-2011; OI Russell, Thomas/0000-0001-6958-8891; Miller-Jones, James/0000-0003-3124-2814; Russell, Thomas/0000-0002-7930-2276; Sivakoff, Gregory/0000-0001-6682-916X; Heinz, Sebastian/0000-0002-8433-8652; Russell, David/0000-0002-3500-631X FU NSERC; Australian Research Council [DP120102393]; Spanish Ministerio de Economia y Competitividad; European Social Funds through a Ramon y Cajal Fellowship; Spanish Ministerio de Ciencia e Innovacion [AYA2013-47447-C03-1-P]; Smithsonian Institution; Academia Sinica; Canada Foundation for Innovation FX A.J.T. would like to thank Erik Rosolowsky for sharing his extensive knowledge of MCMC and Craig Heinke for helpful discussions. A.J.T. and G.R.S. are supported by an NSERC Discovery Grant. This work was supported by Australian Research Council grant DP120102393. This work was supported by the Spanish Ministerio de Economia y Competitividad and European Social Funds through a Ramon y Cajal Fellowship (S. M.) and the Spanish Ministerio de Ciencia e Innovacion (S. M.; grant AYA2013-47447-C03-1-P). 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 James Clerk Maxwell Telescope has historically been operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada and the Netherlands Organisation for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 89 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2015 VL 805 IS 1 AR 30 DI 10.1088/0004-637X/805/1/30 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300030 ER PT J AU Zhu, W Udalski, A Gould, A Dominik, M Bozza, V Han, C Yee, JC Novati, SC Beichman, CA Carey, S Poleski, R Skowron, J Kozlowski, S Mroz, P Pietrukowicz, P Pietrzynski, G Szymanski, MK Soszynski, I Ulaczyk, K Wyrzykowski, L Gaudi, BS Pogge, RW DePoy, DL Jung, YK Choi, JY Hwang, KH Shin, IG Park, H Jeong, J AF Zhu, Wei Udalski, A. Gould, A. Dominik, M. Bozza, V. Han, C. Yee, J. C. Novati, S. Calchi Beichman, C. A. Carey, S. Poleski, R. Skowron, J. Kozlowski, S. Mroz, P. Pietrukowicz, P. Pietrzynski, G. Szymanski, M. K. Soszynski, I. Ulaczyk, K. Wyrzykowski, L. Gaudi, B. S. Pogge, R. W. DePoy, D. L. Jung, Y. K. Choi, J. -Y. Hwang, K. -H. Shin, I. -G. Park, H. Jeong, J. CA OGLE Collaboration FUN Collaboration TI SPITZER AS A MICROLENS PARALLAX SATELLITE: MASS AND DISTANCE MEASUREMENTS OF BINARY LENS SYSTEM OGLE-2014-BLG-1050L SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; gravitational lensing: micro ID GALACTIC BULGE; ISOLATED STAR; HOST STAR; OGLE-III; EVENTS; MAGNIFICATION; DWARF; PREDICTIONS; DISCOVERY; MOTIONS AB We report the first mass and distance measurements of a caustic-crossing binary system OGLE-2014-BLG-1050 L using the space-based microlens parallax method. Spitzer captured the second caustic. crossing of the event, which occurred similar to 10 days before that seen from Earth. Due to the coincidence that the source-lens relative motion was almost parallel to the direction of the binary-lens axis, the fourfold degeneracy, which was known before only to occur in single-lens events, persists in this case, leading to either a lower-mass (0.2 and 0.07 M-circle dot) binary at similar to 1.1 kpc or a higher-mass (0.9 and 0.35 M-circle dot) binary at similar to 3.5 kpc. However, the latter solution is strongly preferred for reasons including blending and lensing probability. OGLE-2014-BLG-1050 L demonstrates the power of microlens parallax in probing stellar and substellar binaries. C1 [Zhu, Wei; Gould, A.; Poleski, R.; Gaudi, B. S.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Udalski, A.; Poleski, R.; Skowron, J.; Kozlowski, S.; Mroz, P.; Pietrukowicz, P.; Pietrzynski, G.; Szymanski, M. K.; Soszynski, I.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Dominik, M.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Bozza, V.; Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy. [Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Han, C.; Jung, Y. K.; Choi, J. -Y.; Hwang, K. -H.; Shin, I. -G.; Park, H.; Jeong, J.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Novati, S. Calchi; Beichman, C. A.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Novati, S. Calchi] IIASS, I-84019 Vietri Sul Mare, SA, Italy. [Carey, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. RP Zhu, W (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. RI Skowron, Jan/M-5186-2014; Kozlowski, Szymon/G-4799-2013; OI Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X; ZHU, WEI/0000-0003-4027-4711 FU NSF [AST 1103471]; JPL [1500811]; NASA [NNX12AB99G]; Creative Research Initiative Program of the National Research Foundation of Korea [2009-0081561]; NASA through the Sagan Fellowship Program; European Research Council under the European Community's Seventh Framework Programme (FP7)/ERC [246678] FX Work by W.Z., A.G., and B.S.G. was supported by NSF grant AST 1103471. Work by J.C.Y., A.G., and S.C. was supported by JPL grant 1500811. A.G., B.S.G., and R.W.P. were supported by NASA grant NNX12AB99G. Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Work by C.A.B. was carried out in part at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration. 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 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. NR 56 TC 17 Z9 17 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 MAY 20 PY 2015 VL 805 IS 1 AR 8 DI 10.1088/0004-637X/805/1/8 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8BA UT WOS:000354991300008 ER PT J AU Hsiang, AY Field, DJ Webster, TH Behlke, ADB Davis, MB Racicot, RA Gauthier, JA AF Hsiang, Allison Y. Field, Daniel J. Webster, Timothy H. Behlke, Adam D. B. Davis, Matthew B. Racicot, Rachel A. Gauthier, Jacques A. TI The origin of snakes: revealing the ecology, behavior, and evolutionary history of early snakes using genomics, phenomics, and the fossil record SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Serpentes; Phylogeny; Ancestral state reconstruction; Divergence time estimation; Combined analysis; Fossil tip-dating ID INDEPENDENT CONTRASTS; GEOGRAPHIC RANGE; MASS EXTINCTION; BODY-SIZE; PHYLOGENY; INFERENCE; RADIATION; TAXA; LIFE; TREE AB Background: The highly derived morphology and astounding diversity of snakes has long inspired debate regarding the ecological and evolutionary origin of both the snake total-group (Pan-Serpentes) and crown snakes (Serpentes). Although speculation abounds on the ecology, behavior, and provenance of the earliest snakes, a rigorous, clade-wide analysis of snake origins has yet to be attempted, in part due to a dearth of adequate paleontological data on early stem snakes. Here, we present the first comprehensive analytical reconstruction of the ancestor of crown snakes and the ancestor of the snake total-group, as inferred using multiple methods of ancestral state reconstruction. We use a combined-data approach that includes new information from the fossil record on extinct crown snakes, new data on the anatomy of the stem snakes Najash rionegrina, Dinilysia patagonica, and Coniophis precedens, and a deeper understanding of the distribution of phenotypic apomorphies among the major clades of fossil and Recent snakes. Additionally, we infer time-calibrated phylogenies using both new 'tip-dating' and traditional node-based approaches, providing new insights on temporal patterns in the early evolutionary history of snakes. Results: Comprehensive ancestral state reconstructions reveal that both the ancestor of crown snakes and the ancestor of total-group snakes were nocturnal, widely foraging, non-constricting stealth hunters. They likely consumed soft-bodied vertebrate and invertebrate prey that was subequal to head size, and occupied terrestrial settings in warm, well-watered, and well-vegetated environments. The snake total-group - approximated by the Coniophis node - is inferred to have originated on land during the middle Early Cretaceous (similar to 128.5 Ma), with the crown-group following about 20 million years later, during the Albian stage. Our inferred divergence dates provide strong evidence for a major radiation of henophidian snake diversity in the wake of the Cretaceous-Paleogene (K-Pg) mass extinction, clarifying the pattern and timing of the extant snake radiation. Although the snake crown-group most likely arose on the supercontinent of Gondwana, our results suggest the possibility that the snake total-group originated on Laurasia. Conclusions: Our study provides new insights into when, where, and how snakes originated, and presents the most complete picture of the early evolution of snakes to date. More broadly, we demonstrate the striking influence of including fossils and phenotypic data in combined analyses aimed at both phylogenetic topology inference and ancestral state reconstruction. C1 [Hsiang, Allison Y.; Field, Daniel J.; Behlke, Adam D. B.; Davis, Matthew B.; Racicot, Rachel A.; Gauthier, Jacques A.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA. [Field, Daniel J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Webster, Timothy H.] Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. [Gauthier, Jacques A.] Yale Univ, Yale Peabody Museum Nat Hist, New Haven, CT 06520 USA. RP Hsiang, AY (reprint author), Yale Univ, Dept Geol & Geophys, POB 6666, New Haven, CT 06520 USA. EM allison.hsiang@yale.edu OI Webster, Timothy/0000-0003-1174-2395; Field, Daniel/0000-0002-1786-0352 NR 92 TC 29 Z9 29 U1 25 U2 80 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD MAY 20 PY 2015 VL 15 AR UNSP 87 DI 10.1186/s12862-015-0358-5 PG 22 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA CI6AK UT WOS:000354840800001 PM 25989795 ER PT J AU Ronquist, F Nieves-Aldrey, JL Buffington, ML Liu, ZW Liljeblad, J Nylander, JAA AF Ronquist, Fredrik Nieves-Aldrey, Jose-Luis Buffington, Matthew L. Liu, Zhiwei Liljeblad, Johan Nylander, Johan A. A. TI Phylogeny, Evolution and Classification of Gall Wasps: The Plot Thickens SO PLOS ONE LA English DT Article ID AUSTRALIAN THRASORINAE HYMENOPTERA; FIGITIDAE HYMENOPTERA; GALLWASPS HYMENOPTERA; OAK GALLWASPS; CYNIPIDAE; CYNIPOIDEA; GENUS; REVISION; SUBFAMILY; INQUILINE AB Gall wasps (Cynipidae) represent the most spectacular radiation of gall-inducing insects. In addition to true gall formers, gall wasps also include phytophagous inquilines, which live inside the galls induced by gall wasps or other insects. Here we present the first comprehensive molecular and total-evidence analyses of higher-level gall wasp relationships. We studied more than 100 taxa representing a rich selection of outgroups and the majority of described cynipid genera outside the diverse oak gall wasps (Cynipini), which were more sparsely sampled. About 5 kb of nucleotide data from one mitochondrial (COI) and four nuclear (28S, LWRh, EF1alpha F1, and EF1alpha F2) markers were analyzed separately and in combination with morphological and life-history data. According to previous morphology-based studies, gall wasps evolved in the Northern Hemisphere and were initially herb gallers. Inquilines originated once from gall inducers that lost the ability to initiate galls. Our results, albeit not conclusive, suggest a different scenario. The first gall wasps were more likely associated with woody host plants, and there must have been multiple origins of gall inducers, inquilines or both. One possibility is that gall inducers arose independently from inquilines in several lineages. Except for these surprising results, our analyses are largely consistent with previous studies. They confirm that gall wasps are conservative in their host-plant preferences, and that herb-galling lineages have radiated repeatedly onto the same set of unrelated host plants. We propose a revised classification of the family into twelve tribes, which are strongly supported as monophyletic across independent datasets. Four are new: Aulacideini, Phanacidini, Diastrophini and Ceroptresini. We present a key to the tribes and discuss their morphological and biological diversity. Until the relationships among the tribes are resolved, the origin and early evolution of gall wasps will remain elusive. C1 [Ronquist, Fredrik; Nylander, Johan A. A.] Swedish Museum Nat Hist, Dept Bioinformat & Genet, S-10405 Stockholm, Sweden. [Nieves-Aldrey, Jose-Luis] CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolut, E-28006 Madrid, Spain. [Buffington, Matthew L.] USDA, Smithsonian Inst, Systemat Entomol Lab, Washington, DC 20250 USA. [Liu, Zhiwei] Eastern Illinois Univ, Dept Biol Sci, Charleston, IL 61920 USA. [Liljeblad, Johan] Swedish Univ Agr Sci, Swedish Species Informat Ctr, Uppsala, Sweden. [Nylander, Johan A. A.] Linkoping Univ, Bioinformat Infrastruct Life Sci, Linkoping, Sweden. RP Ronquist, F (reprint author), Swedish Museum Nat Hist, Dept Bioinformat & Genet, S-10405 Stockholm, Sweden. EM fredrik.ronquist@nrm.se RI Ronquist, Fredrik/Q-2013-2015 FU Swedish Research Council [20115622]; Spanish Ministry of Science and Innovation [CGL-2009-10111, CGL-2010-15786]; Kalbfleisch Fellowship, American Museum of Natural History; Boyd Scholarship, The Field Museum; National Science Foundation [1K12 Gm00708]; (HymAToL), National Science Foundation [DEB-0337220] FX This work received support from: 20115622, Swedish Research Council (http://vr.se): FR. CGL-2009-10111 and CGL-2010-15786, Spanish Ministry of Science and Innovation (http://www.idi.mineco.gob.es): JLNA. Kalbfleisch Fellowship, American Museum of Natural History (http://www.amnh.org): ZL. Boyd Scholarship, The Field Museum (http://www.fieldmuseum.org): ZL. Training Grant #1K12 Gm00708, National Science Foundation (http://www.nsf.gov): ZL. DEB-0337220 (HymAToL), National Science Foundation (http://www.nsf.gov): FR MB. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 60 TC 8 Z9 11 U1 4 U2 34 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 MAY 20 PY 2015 VL 10 IS 5 AR e0123301 DI 10.1371/journal.pone.0123301 PG 40 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI7CV UT WOS:000354921400009 PM 25993346 ER PT J AU Braiding, C Burton, MG Blackwell, R Gluck, C Hawkes, J Kulesa, C Maxted, N Rebolledo, D Rowell, G Stark, A Tothill, N Urquhart, JS Voisin, F Walsh, AJ de Wilt, P Wong, GF AF Braiding, Catherine Burton, M. G. Blackwell, R. Glueck, C. Hawkes, J. Kulesa, C. Maxted, N. Rebolledo, D. Rowell, G. Stark, A. Tothill, N. Urquhart, J. S. Voisin, F. Walsh, A. J. de Wilt, P. Wong, G. F. TI The Mopra Southern Galactic Plane CO Survey - Data Release 1 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE Galaxy: kinematics and dynamics; Galaxy: structure; ISM: clouds; ISM: molecules; radio lines: ISM surveys ID CHERENKOV TELESCOPE ARRAY; MILKY-WAY; MOLECULAR CLOUD; DESIGN; GALAXY; FIELD; VIEW AB We present observations of the first 10 degrees of longitude in the Mopra CO survey of the southern Galactic plane, covering Galactic longitude l = 320- 330 degrees and latitude b=+/- 0.5 degrees, and l = 327- 330 degrees, b= +0.5-1.0 degrees. These data have been taken at 35-arcsec spatial resolution and 0.1 km s(-1) spectral resolution, providing an unprecedented view of the molecular clouds and gas of the southern Galactic plane in the 109-115 GHz J = 1-0 transitions of (CO)-C-12, (CO)-C-13, (CO)-O-18, and (CO)-O-17. Together with information about the noise statistics from the Mopra telescope, these data can be retrieved from the Mopra CO website and the CSIRO-ATNF data archive. C1 [Braiding, Catherine; Burton, M. G.; Rebolledo, D.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Blackwell, R.; Hawkes, J.; Rowell, G.; Voisin, F.; de Wilt, P.] Univ Adelaide, Sch Phys Sci, Dept Phys, Adelaide, SA 5005, Australia. [Glueck, C.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Kulesa, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Maxted, N.] Univ Montpellier 2, Lab Univers & Particules Montpellier, F-34000 Montpellier, France. [Rebolledo, D.] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Stark, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tothill, N.; Wong, G. F.] Univ Western Sydney, Sch Comp Engn & Math, Penrith, NSW 2751, Australia. [Urquhart, J. S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Walsh, A. J.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Wong, G. F.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. RP Braiding, C (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. EM catherine.braiding@gmail.com RI Walsh, Andrew/B-5627-2013; OI Walsh, Andrew/0000-0001-9506-0855; Maxted, Nigel/0000-0003-2762-8378; Rowell, Gavin/0000-0002-9516-1581; Stark, Antony/0000-0002-2718-9996 FU Australian Research Council (ARC); ARC [DP120101585] FX The Mopra radio telescope is currently part of the Australia Telescope National Facility. Operations support was provided by the University of New South Wales and the University of Adelaide. Many staff of the ATNF have contributed to the success of the remote operations at Mopra. We particularly wish to acknowledge the contributions of David Brodrick, Philip Edwards, Brett Hiscock, Balt Indermuehle, and Peter Mirtschin. The University of New South Wales Digital Filter Bank used for the observations with the Mopra Telescope (the UNSW-MOPS) was provided with support from the Australian Research Council (ARC). We also acknowledge ARC support through Discovery Project DP120101585. NR 24 TC 3 Z9 3 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD MAY 20 PY 2015 VL 32 AR e020 DI 10.1017/pasa.2015.20 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6NL UT WOS:000354876500003 ER PT J AU Schmidt, R Lemeshko, M AF Schmidt, Richard Lemeshko, Mikhail TI Rotation of Quantum Impurities in the Presence of a Many-Body Environment SO PHYSICAL REVIEW LETTERS LA English DT Article ID HELIUM DROPLETS; OPTICAL LATTICE; LIQUID-HELIUM; MOLECULES; SPECTRUM; POLARON; PHYSICS; HE-4 AB We develop a microscopic theory describing a quantum impurity whose rotational degree of freedom is coupled to a many-particle bath. We approach the problem by introducing the concept of an "angulon"-a quantum rotor dressed by a quantum field-and reveal its quasiparticle properties using a combination of variational and diagrammatic techniques. Our theory predicts renormalization of the impurity rotational structure, such as that observed in experiments with molecules in superfluid helium droplets, in terms of a rotational Lamb shift induced by the many-particle environment. Furthermore, we discover a rich many-body-induced fine structure, emerging in rotational spectra due to a redistribution of angular momentum within the quantum many-body system. C1 [Schmidt, Richard] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Schmidt, Richard] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Lemeshko, Mikhail] IST Austria Inst Sci & Technol Austria, A-3400 Klosterneuburg, Austria. RP Schmidt, R (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St, Cambridge, MA 02138 USA. EM richard.schmidt@cfa.harvard.edu; mikhail.lemeshko@ist.ac.at FU NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University; Smithsonian Astrophysical Observatory FX We are grateful to Eugene Demler, Sarang Gopalakrishnan, Michael Knap, Vasili Kharchenko, Markus Oberthaler, Seth Rittenhouse, Robert Seiringer, and Zhenhua Yu for the fruitful discussions. R. S. is grateful for the hospitality during his stay at the Institute for Advanced Study at Tsinghua University. The work was supported by the NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and the Smithsonian Astrophysical Observatory. NR 43 TC 10 Z9 10 U1 2 U2 8 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 MAY 18 PY 2015 VL 114 IS 20 AR 203001 DI 10.1103/PhysRevLett.114.203001 PG 6 WC Physics, Multidisciplinary SC Physics GA CI7UI UT WOS:000354969900003 PM 26047225 ER PT J AU Brogan, WR Relyea, RA AF Brogan, William R., III Relyea, Rick A. TI Submerged Macrophytes Mitigate Direct and Indirect Insecticide Effects in Freshwater Communities SO PLOS ONE LA English DT Article ID MALATHIONS ACUTE TOXICITY; HABITAT COMPLEXITY; PERTURBATION EXPERIMENTS; ZOOPLANKTON COMMUNITIES; AMPHIBIAN COMMUNITIES; AQUATIC MACROPHYTES; PREDATOR IDENTITY; HYLA-SQUIRELLA; PLANTS REDUCE; FROGS AB Understanding how ecological interactions mitigate the impacts of perturbations such as pesticides in biological communities is an important basic and applied question for ecologists. In aquatic ecosystems, new evidence from microcosm experiments suggests that submerged macrophytes can buffer cladocerans from pulse exposures to the widely used insecticide malathion, and that mitigation increases with macrophyte density. However, whether these results scale up to more complex aquatic communities where ecological interactions such as competition can alter toxicity is unknown. Further, macrophyte abilities to mitigate different insecticide exposure scenarios (i.e. single versus repeated pulses) have never been tested. To address these gaps, we performed a factorial mesocosm experiment examining the influence of four macrophyte treatments (0, 10, 50, or 100 Elodea Canadensis shoots planted per mesocosm) crossed with three malathion exposure scenarios (no insecticide, single pulse, repeated pulses) on aquatic communities containing zooplankton, phytoplankton, periphyton, two snail species, and larval amphibians. In the absence of macrophytes, single malathion pulses caused short-term declines in cladoceran abundance followed by their rapid recovery, which precluded any indirect effects (i.e. trophic cascades). However, repeated malathion pulses caused cladoceran extinctions, resulting in persistent phytoplankton blooms and reduced abundance of one snail species. In contrast, with macrophytes present, even at low density, malathion had no effect on any taxa. We also discovered novel effects of macrophytes on the benthic food web. In the two highest macrophyte treatments, we observed trends of reduced periphyton biomass, decreased abundance of one snail species, and decreased amphibian time to and mass at metamorphosis. To our knowledge, this is the first evidence of negative submerged macrophyte effects on amphibians, a taxa of global conservation concern. Our findings suggest that facilitating macrophytes could be an important strategy for buffering freshwater communities from insecticides, though consideration of their impacts on animal species is necessary. C1 [Brogan, William R., III] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Relyea, Rick A.] Rensselaer Polytech Inst, Troy, NY 12180 USA. RP Brogan, WR (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM wbrogan@gmail.com FU Sigma Xi [G20090315100640]; Society for Wetland Scientists; L.K. Darbaker Award (University of Pittsburgh); National Science Foundation [NSF DEB 05-18250] FX WRBIII funded this research in part from: 1. Sigma Xi Grants-in-aid-of-research: Funding #: G20090315100640, website - https://www.sigmaxi.org/programs/grants-in-aid, 2. Society for Wetland Scientists: Funding #: N/A, website - http://www.sws.org/, 3. L.K. Darbaker Award (University of Pittsburgh): Funding #: N/A, website - http://biology.pitt.edu/facilities/pymatuning/research-grants. RAR funded this research in part from: National Science Foundation: Funding #: NSF DEB 05-18250, website - http://www.nsf.gov/. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 65 TC 0 Z9 0 U1 3 U2 37 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 15 PY 2015 VL 10 IS 5 AR UNSP e0126677 DI 10.1371/journal.pone.0126677 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI7AU UT WOS:000354916100089 PM 25978686 ER PT J AU Graham, L Graff, TG Yingst, RA ten Kate, IL Russell, P AF Graham, Lee Graff, Trevor G. Yingst, R. Aileen ten Kate, Inge L. Russell, Patrick TI 2012 Moon Mars Analog Mission Activities on Mauna Kea, Hawai'i SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Geology; Moon; Mars; Rover ID GROUND-PENETRATING RADAR; MOSSBAUER SPECTROMETER AB Rover-based 2012 Moon and Mars Analog Mission Activities (MMAMA) scientific investigations were completed at Mauna Kea, Hawaii. Scientific investigations, scientific input, and science operations constraints were tested in the context of an existing project and protocols for the field activities designed to help NASA achieve the Vision for Space Exploration. Four separate science investigations were integrated in a Martian analog environment with initial science operations planned based on a model similar to the operations control of the Mars Exploration Rovers (MER). However, evolution of the operations process occurred during the initial planning sessions and as the analog mission progressed. We review here the overall program of the investigation into the origin of the valley including preliminary sensor data results, an applicable methodology for developing an optimum science input based on productive engineering, and science trades and the science operations approach for an investigation into the valley on the upper slopes of Mauna Kea identified as "Apollo Valley". Published by Elsevier Ltd. on behalf of COSPAR. C1 [Graham, Lee] NASA, Lyndon B Johnson Space Ctr, Explorat Integrat & Sci, Houston, TX 77058 USA. [Graff, Trevor G.] NASA, Lyndon B Johnson Space Ctr, Dept Sci, JACOBS, Houston, TX 77058 USA. [Yingst, R. Aileen] Planetary Sci Inst, Tucson, AZ 85719 USA. [ten Kate, Inge L.] Univ Utrecht, Dept Earth Sci, NL-3584 CD Utrecht, Netherlands. [Russell, Patrick] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. RP Graham, L (reprint author), NASA, Lyndon B Johnson Space Ctr, Explorat Integrat & Sci, Mail Code X14,2101 NASA Pkwy, Houston, TX 77058 USA. EM lee.d.graham@nasa.gov NR 14 TC 4 Z9 4 U1 4 U2 9 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD MAY 15 PY 2015 VL 55 IS 10 BP 2405 EP 2413 DI 10.1016/j.asr.2015.01.024 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA CH0ZC UT WOS:000353749900003 ER PT J AU French, RA Bina, CR Robinson, MS Watters, TR AF French, Renee A. Bina, Craig R. Robinson, Mark S. Watters, Thomas R. TI Small-scale lunar graben: Distribution, dimensions, and formation processes SO ICARUS LA English DT Article DE Moon; Tectonics; Moon, surface; Geological processes ID RECONNAISSANCE ORBITER CAMERA; CANYONLANDS-NATIONAL-PARK; NORMAL FAULTS; IMPACT CRATERS; STRUCTURAL-ANALYSIS; MAGMATIC EVOLUTION; MESSENGER FLYBY; CALORIS BASIN; MOON; MERCURY AB The Lunar Reconnaissance Orbiter Camera (LROC) is the first instrument to provide widespread coverage with a range of incidence angles at the resolution required to detect small-scale landforms. A sample (n = 238) of globally distributed, small-scale graben average 26 m wide and 179 m long. When dividing the population into those located within mare and highland regions, we observe that graben located within mare tend to be narrower, shorter, and more irregularly spaced than those in highland terrane. For graben associated with contractional landforms, those in mare are smaller in width and length than those in highlands; the same is true for graben independent of contractional landforms. Assuming a simple geometry, widths of mare graben associated with scarps or ridges are used to estimate the minimum depth range to a mechanical discontinuity (e.g., base of the regolith) resulting in values of similar to 4-48 m. These values are similar to the ranges estimated for regolith thickness from previous workers using Apollo 14 seismic data (3.9-8.5 m), crater counting techniques (8-33 m), crater morphology techniques (2.5-9 m), and crater blockiness (8-31 m). Widths of highland graben yield minimum depths of faulting of 209-296 m. While this range agrees well with models for regolith production (an older surface will have thicker regolith), this estimate likely does not represent the thickness of a mechanical unit due to the fragmented nature of the highland crust (it does not provide a defining boundary between bedrock and regolith). Spacing of mare graben not associated with contractional landforms is used to estimate maximum local mare unit thickness for two graben groups: 190 m for Posidonius and 296 m for Vitello. Maximum graben ages range from late Eratosthenian to early Copernican based on superposed and crosscut crater ages with a group of graben deforming ejecta from Copernicus crater. Data presented here provide further evidence of a globally distributed, young, small-scale graben population that has formed as a result of localized extension either from flexural bending or dilation due to contractional faulting or volcanic uplift, indicating a significant level of recent geologic activity. (C) 2015 Elsevier Inc. All rights reserved. C1 [French, Renee A.; Bina, Craig R.] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL 60208 USA. [Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP French, RA (reprint author), Northwestern Univ, Dept Earth & Planetary Sci, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM renee@earth.northwestern.edu OI Bina, Craig/0000-0001-5946-3737 FU NASA Lunar Reconnaissance Orbiter project; Department of Earth and Planetary Sciences at Northwestern University FX This work was supported by the NASA Lunar Reconnaissance Orbiter project and the Department of Earth and Planetary Sciences at Northwestern University. The authors would like to thank the LROC team for their hard work in data acquisition, distribution, and support, as well as the groups at Arizona State University and University of Arizona for processing NAC stereo pairs into digital elevation models. The authors would like to thank Brett Denevi for her thoughtful and constructive comments. NR 76 TC 2 Z9 2 U1 1 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAY 15 PY 2015 VL 252 BP 95 EP 106 DI 10.1016/j.icarus.2014.12.031 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE8TW UT WOS:000352118000006 ER PT J AU Yao, JL Kula, RR Wharton, RA Chen, JH AF Yao, Junli Kula, Robert R. Wharton, Robert A. Chen, Jiahua TI Four new species of Tanycarpa (Hymenoptera, Braconidae, Alysiinae) from the Palaearctic Region and new records of species from China SO ZOOTAXA LA English DT Article DE Alysiini; Asia; identification; key; range extension; taxonomy ID REVISION AB Four new species of Tanycarpa (Hymenoptera, Braconidae, Alysiinae), T. gymnonotum Yao sp. n., T. similis Yao sp. n., T. areolata Yao sp. n., and T. lineata Yao sp. n., are described from the Palaearctic Region of China, and T. chors Belokobylskij is newly recorded from China. Significant range extensions are given for T. bicolor (Nees von Esenbeck), T. gracilicornis (Nees von Esenbeck), and T. mitis Stelfox. A key to the Palaearctic species of Tanycarpa is provided. C1 [Yao, Junli; Chen, Jiahua] Fujian Agr & Forestry Univ, Beneficial Insects Inst, Fuzhou 350002, Fujian, Peoples R China. [Kula, Robert R.] ARS, Systemat Entomol Lab, Beltsville Agr Res Ctr, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Wharton, Robert A.] Texas A&M Univ, Dept Entomol, College Stn, TX 77843 USA. RP Chen, JH (reprint author), Fujian Agr & Forestry Univ, Beneficial Insects Inst, Fuzhou 350002, Fujian, Peoples R China. EM yao.junli.china@gmail.com; Robert.Kula@ars.usda.gov; rawbaw2@tamu.edu; JhChen34@163.com FU Specialized Research Fund for the Doctoral Program in Colleges and Universities for the project Systemic Studies on Alysiinae of China [20113515110003] FX The images in this paper were acquired by the first author with the help of Andrew Ly and Danielle Restuccia while the first author was visiting Texas A&M University. We thank Dr. Dicky Yu for providing many references. Mention of trade names or commercial products in this publication is solely for the purpose of providing specific information and does not imply recommendation or endorsement by the USDA. USDA is an equal opportunity provider and employer. This research was supported by the Specialized Research Fund for the Doctoral Program in Colleges and Universities (2011) for the project Systemic Studies on Alysiinae of China (code: 20113515110003). NR 30 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 MAY 14 PY 2015 VL 3957 IS 2 BP 169 EP 187 PG 19 WC Zoology SC Zoology GA CI8BV UT WOS:000354993400002 PM 26249064 ER PT J AU Kuprewicz, EK AF Kuprewicz, Erin K. TI Scatter Hoarding of Seeds Confers Survival Advantages and Disadvantages to Large-Seeded Tropical Plants at Different Life Stages SO PLOS ONE LA English DT Article ID NEOTROPICAL RAIN-FOREST; DIPTERYX-PANAMENSIS; PREDATION; TREE; DISPERSAL; RODENTS; PALM; RECRUITMENT; DYNAMICS; PANAMA AB Scatter hoarding of seeds by animals contributes significantly to forest-level processes, including plant recruitment and forest community composition. However, the potential positive and negative effects of caching on seed survival, germination success, and seedling survival have rarely been assessed through experimental studies. Here, I tested the hypothesis that seed burial mimicking caches made by scatter hoarding Central American agoutis (Dasyprocta punctate) enhances seed survival, germination, and growth by protecting seeds from seed predators and providing favorable microhabitats for germination. In a series of experiments, I used simulated agouti seed caches to assess how hoarding affects seed predation by ground-dwelling invertebrates and vertebrates for four plant species. I tracked germination and seedling growth of intact and beetle-infested seeds and, using exclosures, monitored the effects of mammals on seedling survival through time. All experiments were conducted over three years in a lowland wet forest in Costa Rica. The majority of hoarded palm seeds escaped predation by both invertebrates and vertebrates while exposed seeds suffered high levels of infestation and removal. Hoarding had no effect on infestation rates of D. panamensis, but burial negatively affected germination success by preventing endocarp dehiscence. Non-infested palm seeds had higher germination success and produced larger seedlings than infested seeds. Seedlings of A. alatum and I. deltoidea suffered high mortality by seed-eating mammals. Hoarding protected most seeds from predators and enhanced germination success (except for D. panamensis) and seedling growth, although mammals killed many seedlings of two plant species; all seedling deaths were due to seed removal from the plant base. Using experimental caches, this study shows that scatter hoarding is beneficial to most seeds and may positively affect plant propagation in tropical forests, although tradeoffs in seed survival do exist. C1 [Kuprewicz, Erin K.] Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. RP Kuprewicz, EK (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. EM erinkuprewicz@gmail.com FU Organization for Tropical Studies; University of Miami FX Funding for this project was provided by the Organization for Tropical Studies, http://ots.ac.cr/ (Emily P. Foster Fund and Rowe Family Fellowship) and the University of Miami, http://www.miami.edu/ (Curtis Plant Sciences Scholarship, Kushlan Fund, and Center for Latin American Studies Doctoral Research Fellowship). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 46 TC 1 Z9 1 U1 2 U2 13 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 MAY 13 PY 2015 VL 10 IS 5 AR e0124932 DI 10.1371/journal.pone.0124932 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI1ZP UT WOS:000354544200057 PM 25970832 ER PT J AU Larabee, FJ Suarez, AV AF Larabee, Fredrick J. Suarez, Andrew V. TI Mandible-Powered Escape Jumps in Trap-Jaw Ants Increase Survival Rates during Predator-Prey Encounters SO PLOS ONE LA English DT Article ID ODONTOMACHUS; NEUROPTERA; FORMICIDAE; MYRMELEON; FLORIDA; LARVAE; KEY; DIVERSIFICATION; HYMENOPTERA; PERFORMANCE AB Animals use a variety of escape mechanisms to increase the probability of surviving predatory attacks. Antipredator defenses can be elaborate, making their evolutionary origin unclear. Trap-jaw ants are known for their rapid and powerful predatory mandible strikes, and some species have been observed to direct those strikes at the substrate, thereby launching themselves into the air away from a potential threat. This potential escape mechanism has never been examined in a natural context. We studied the use of mandible-powered jumping in Odontomachus brunneus during their interactions with a common ant predator: pit-building antlions. We observed that while trap-jaw ant workers escaped from antlion pits by running in about half of interactions, in 15% of interactions they escaped by mandible-powered jumping. To test whether escape jumps improved individual survival, we experimentally prevented workers from jumping and measured their escape rate. Workers with unrestrained mandibles escaped from antlion pits significantly more frequently than workers with restrained mandibles. Our results indicate that some trap-jaw ant species can use mandible-powered jumps to escape from common predators. These results also provide a charismatic example of evolutionary co-option, where a trait that evolved for one function (predation) has been co-opted for another (defense). C1 [Larabee, Fredrick J.; Suarez, Andrew V.] Univ Illinois, Dept Entomol, Urbana, IL 61801 USA. [Larabee, Fredrick J.] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Suarez, Andrew V.] Univ Illinois, Dept Anim Biol, Urbana, IL 61801 USA. RP Larabee, FJ (reprint author), Univ Illinois, Dept Entomol, Urbana, IL 61801 USA. EM larabee@life.illinois.edu FU American Museum of Natural History; Society of Integrative and Comparative Biology; National Science Foundation [1407279]; National Geographic Committee for Research and Exploration [9481-14] FX Theodore Roosevelt Memorial Grant from the American Museum of Natural History was awarded to FJL (http://www.amnh.org/our-research/richard-gilder-graduate-school/academi cs-and-research/fellowship-and-grant-opportunities/research-grants-and-s tudent-exchange-fellowships); Libbie Hyman Memorial Grant from the Society of Integrative and Comparative Biology was awarded to FJL (http://sicb.org/grants/hyman/); Doctoral Dissertation Improvement Grant (Award Number 1407279) from the National Science Foundation was awarded to FJL (http://www.nsf.gov/); and National Geographic Committee for Research and Exploration (Award Number 9481-14) was awarded to AVS (http://www.nationalgeographic.com/explorers/grants-programs/cre-applica tion/). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 32 TC 2 Z9 2 U1 5 U2 20 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 13 PY 2015 VL 10 IS 5 AR e0124871 DI 10.1371/journal.pone.0124871 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI1ZP UT WOS:000354544200054 PM 25970637 ER PT J AU Rodrigues, FD Mathis, WN Hauser, M AF Rodrigues Junior, Francisco De Assis Mathis, Wayne Nielsen Hauser, Martin TI Argentine Hydrellia Robineau-Desvoidy (Diptera, Ephydridae): new species and key to identification SO ZOOTAXA LA English DT Article DE Hydrellia egeriae sp nov.; Leafminer; Shore-fly; New World; Neotropical Region AB Hydrellia egeriae sp. nov., a new species of Hydrellia from Campana (34 14' 04 S, 58 52' 32 W) and Hurlingham (3435' 14 S, 5838' 27 W), Buenos Aires province, Argentina is described. A key to the Argentine Hydrellia species is presented. C1 [Rodrigues Junior, Francisco De Assis] Univ Fed Rio de Janeiro, Museu Nacl, Dept Entomol, BR-20940040 Rio De Janeiro, Brazil. [Mathis, Wayne Nielsen] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Hauser, Martin] Calif Dept Food & Agr, Plant Pest Diagnost Ctr, Sacramento, CA 95832 USA. RP Rodrigues, FD (reprint author), Univ Fed Rio de Janeiro, Museu Nacl, Dept Entomol, Quinta Boa Vista S-N, BR-20940040 Rio De Janeiro, Brazil. EM rodriguesjuniorfa@gmail.com NR 8 TC 0 Z9 0 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 13 PY 2015 VL 3957 IS 1 BP 131 EP 136 PG 6 WC Zoology SC Zoology GA CI8BU UT WOS:000354993300011 ER PT J AU Mocz, P Succi, S AF Mocz, Philip Succi, Sauro TI Numerical solution of the nonlinear Schrodinger equation using smoothed-particle hydrodynamics SO PHYSICAL REVIEW E LA English DT Article ID BOSE-EINSTEIN CONDENSATION; GROUND-STATE SOLUTION; LATTICE-GAS; ATOMIC GAS; DARK; WAVE; COMPUTATION; SIMULATION; FLOWS; HEAT AB We formulate a smoothed-particle hydrodynamics numerical method, traditionally used for the Euler equations for fluid dynamics in the context of astrophysical simulations, to solve the nonlinear Schrodinger equation in the Madelung formulation. The probability density of the wave function is discretized into moving particles, whose properties are smoothed by a kernel function. The traditional fluid pressure is replaced by a quantum pressure tensor, for which a robust discretization is found. We demonstrate our numerical method on a variety of numerical test problems involving the simple harmonic oscillator, soliton-soliton collision, Bose-Einstein condensates, collapsing singularities, and dark matter halos governed by the Gross-Pitaevskii-Poisson equation. Our method is conservative, applicable to unbounded domains, and is automatically adaptive in its resolution, making it well suited to study problems with collapsing solutions. C1 [Mocz, Philip] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Succi, Sauro] CNR, Ist Applicaz Calcolo, I-00161 Rome, Italy. [Succi, Sauro] Harvard Univ, Sch Engn & Appl Sci, Inst Appl Computat Sci, Cambridge, MA 02138 USA. RP Mocz, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmocz@cfa.harvard.edu; succi@iac.cnr.it RI Succi, Sauro/E-4606-2015; OI Succi, Sauro/0000-0002-3070-3079; Mocz, Philip/0000-0001-6631-2566 FU National Science Foundation [DGE-1144152] FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144152 (P.M.). P.M. would like to thank D. Marsh and X. Guo for careful reading of the manuscript, and H.Y. Schive for valuable discussions. NR 42 TC 7 Z9 7 U1 3 U2 10 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 EI 1550-2376 J9 PHYS REV E JI Phys. Rev. E PD MAY 13 PY 2015 VL 91 IS 5 AR 053304 DI 10.1103/PhysRevE.91.053304 PG 9 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA CI2BZ UT WOS:000354551000009 PM 26066276 ER PT J AU Cranmer, SR Asgari-Targhi, M Miralles, MP Raymond, JC Strachan, L Tian, H Woolsey, LN AF Cranmer, Steven R. Asgari-Targhi, Mahboubeh Miralles, Mari Paz Raymond, John C. Strachan, Leonard Tian, Hui Woolsey, Lauren N. TI The role of turbulence in coronal heating and solar wind expansion SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Review DE heliosphere; plasma physics; solar atmosphere; solar corona; solar wind; turbulence ID ALFVEN-WAVE TURBULENCE; PHOTOSPHERIC MAGNETIC-FIELD; EJECTION CURRENT SHEET; MAGNETOHYDRODYNAMIC TURBULENCE; TRANSITION REGION; LOW-FREQUENCY; MHD TURBULENCE; INTERCHANGE RECONNECTION; HYDROMAGNETIC TURBULENCE; INTERPLANETARY MEDIUM AB Plasma in the Sun's hot corona expands into the heliosphere as a supersonic and highly magnetized solar wind. This paper provides an overview of our current understanding of how the corona is heated and how the solar wind is accelerated. Recent models of magnetohydrodynamic turbulence have progressed to the point of successfully predicting many observed properties of this complex, multi-scale system. However, it is not clear whether the heating in open-field regions comes mainly from the dissipation of turbulent fluctuations that are launched from the solar surface, or whether the chaotic 'magnetic carpet' in the low corona energizes the system via magnetic reconnection. To help pin down the physics, we also review some key observational results fromultraviolet spectroscopy of the collisionless outer corona. C1 [Cranmer, Steven R.; Asgari-Targhi, Mahboubeh; Miralles, Mari Paz; Raymond, John C.; Strachan, Leonard; Tian, Hui; Woolsey, Lauren N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cranmer, Steven R.] Univ Colorado, Dept Astrophys & Planetary Sci, Lab Atmospher & Space Phys, Boulder, CO USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu FU NASA [NNX-10-AC11G, NNX-14-AG99G, NX-06-AG95G, NNX-09-AH22G, NNX-10-AQ58G]; NSF SHINE program [AGS-1259519] FX S.R.C.'s work was supported by NASA grant nos. NNX-10-AC11G and NNX-14-AG99G, and NSF SHINE program grant no. AGS-1259519. M.P.M.'s work was supported by NASA grant nos. NNX-06-AG95G, NNX-09-AH22G and NNX-10-AQ58G. The SOHO mission is a project of international cooperation between NASA and ESA. NR 148 TC 14 Z9 14 U1 1 U2 19 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 MAY 13 PY 2015 VL 373 IS 2041 AR 20140148 DI 10.1098/rsta.2014.0148 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG5BK UT WOS:000353304500005 ER PT J AU Freidl, GS Binger, T Muller, MA de Bruin, E van Beek, J Corman, VM Rasche, A Drexler, JF Sylverken, A Oppong, SK Adu-Sarkodie, Y Tschapka, M Cottontail, VM Drosten, C Koopmans, M AF Freidl, Gudrun Stephanie Binger, Tabea Mueller, Marcel Alexander de Bruin, Erwin van Beek, Janko Corman, Victor Max Rasche, Andrea Drexler, Jan Felix Sylverken, Augustina Oppong, Samuel K. Adu-Sarkodie, Yaw Tschapka, Marco Cottontail, Veronika M. Drosten, Christian Koopmans, Marion TI Serological Evidence of Influenza A Viruses in Frugivorous Bats from Africa SO PLOS ONE LA English DT Article ID INFECTIOUS-DISEASES; WILDLIFE; ECOLOGY; ASSAYS AB Bats are likely natural hosts for a range of zoonotic viruses such as Marburg, Ebola, Rabies, as well as for various Corona-and Paramyxoviruses. In 2009/10, researchers discovered RNA of two novel influenza virus subtypes - H17N10 and H18N11 - in Central and South American fruit bats. The identification of bats as possible additional reservoir for influenza A viruses raises questions about the role of this mammalian taxon in influenza A virus ecology and possible public health relevance. As molecular testing can be limited by a short time window in which the virus is present, serological testing provides information about past infections and virus spread in populations after the virus has been cleared. This study aimed at screening available sera from 100 free-ranging, frugivorous bats (Eidolon helvum) sampled in 2009/10 in Ghana, for the presence of antibodies against the complete panel of influenza A haemagglutinin (HA) types ranging from H1 to H18 by means of a protein microarray platform. This technique enables simultaneous serological testing against multiple recombinant HA-types in 5 mu l of serum. Preliminary results indicate serological evidence against avian influenza subtype H9 in about 30% of the animals screened, with low-level cross-reactivity to phylogenetically closely related subtypes H8 and H12. To our knowledge, this is the first report of serological evidence of influenza A viruses other than H17 and H18 in bats. As avian influenza subtype H9 is associated with human infections, the implications of our findings from a public health context remain to be investigated. C1 [Freidl, Gudrun Stephanie; de Bruin, Erwin; van Beek, Janko; Koopmans, Marion] Natl Inst Publ Hlth & Environm, Ctr Infect Dis Res Diagnost & Screening, Dept Virol, NL-3720 BA Bilthoven, Netherlands. [Freidl, Gudrun Stephanie; de Bruin, Erwin; van Beek, Janko; Koopmans, Marion] Erasmus MC, Virosci Dept, Rotterdam, Netherlands. [Binger, Tabea; Mueller, Marcel Alexander; Corman, Victor Max; Rasche, Andrea; Drexler, Jan Felix; Drosten, Christian] Univ Bonn, Med Ctr, Inst Virol, Bonn, Germany. [Sylverken, Augustina; Oppong, Samuel K.; Adu-Sarkodie, Yaw] Kumasi Ctr Collaborat Res Trop Med, Kumasi, Ghana. [Oppong, Samuel K.; Adu-Sarkodie, Yaw] Kwame Nkrumah Univ Sci & Technol, Kumasi, Ghana. [Tschapka, Marco; Cottontail, Veronika M.] Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, D-89069 Ulm, Germany. [Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. RP Freidl, GS (reprint author), Natl Inst Publ Hlth & Environm, Ctr Infect Dis Res Diagnost & Screening, Dept Virol, NL-3720 BA Bilthoven, Netherlands. EM gudrun.freidl@rivm.nl OI Mueller, Marcel/0000-0003-2242-5117; Corman, Victor Max/0000-0002-3605-0136 FU European Commission [278976] FX This project was funded by the European Commission's FP7 program under the umbrella of the Antigone project - ANTIcipating the Global onset of Novel Epidemics (project number 278976, http://antigonefp7.eu/). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 25 TC 3 Z9 4 U1 2 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 MAY 12 PY 2015 VL 10 IS 5 AR e0127035 DI 10.1371/journal.pone.0127035 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CI1ZI UT WOS:000354543500088 PM 25965069 ER PT J AU Leslie, HM Basurto, X Nenadovic, M Sievanen, L Cavanaugh, KC Cota-Nieto, JJ Erisman, BE Finkbeiner, E Hinojosa-Arango, G Moreno-Baez, M Nagavarapu, S Reddy, SMW Sanchez-Rodriguez, A Siegel, K Ulibarria-Valenzuela, JJ Weaver, AH Aburto-Oropeza, O AF Leslie, Heather M. Basurto, Xavier Nenadovic, Mateja Sievanen, Leila Cavanaugh, Kyle C. Jose Cota-Nieto, Juan Erisman, Brad E. Finkbeiner, Elena Hinojosa-Arango, Gustavo Moreno-Baez, Marcia Nagavarapu, Sriniketh Reddy, Sheila M. W. Sanchez-Rodriguez, Alexandra Siegel, Katherine Juan Ulibarria-Valenzuela, Jose Hudson Weaver, Amy Aburto-Oropeza, Octavio TI Operationalizing the social-ecological systems framework to assess sustainability SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE coupled natural and human systems; marine; governance; small-scale fisheries; conservation science ID SMALL-SCALE FISHERIES; BIODIVERSITY CONSERVATION; COMMONS; GOVERNANCE AB Environmental governance is more effective when the scales of ecological processes are well matched with the human institutions charged with managing human-environment interactions. The social-ecological systems (SESs) framework provides guidance on how to assess the social and ecological dimensions that contribute to sustainable resource use and management, but rarely if ever has been operationalized for multiple localities in a spatially explicit, quantitative manner. Here, we use the case of small-scale fisheries in Baja California Sur, Mexico, to identify distinct SES regions and test key aspects of coupled SESs theory. Regions that exhibit greater potential for social-ecological sustainability in one dimension do not necessarily exhibit it in others, highlighting the importance of integrative, coupled system analyses when implementing spatial planning and other ecosystem-based strategies. C1 [Leslie, Heather M.; Sievanen, Leila; Cavanaugh, Kyle C.; Reddy, Sheila M. W.; Siegel, Katherine] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Leslie, Heather M.; Sievanen, Leila; Cavanaugh, Kyle C.; Nagavarapu, Sriniketh; Reddy, Sheila M. W.; Siegel, Katherine] Brown Univ, Inst Brown Environm & Soc, Providence, RI 02912 USA. [Basurto, Xavier; Nenadovic, Mateja] Duke Univ, Marine Lab, Nicholas Sch Environm, Beaufort, NC 28516 USA. [Sievanen, Leila] Pacific Islands Fisheries Sci Ctr, Joint Inst Marine & Atmospher Res, Honolulu, HI 96818 USA. [Cavanaugh, Kyle C.] Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA. [Jose Cota-Nieto, Juan; Hinojosa-Arango, Gustavo; Moreno-Baez, Marcia; Sanchez-Rodriguez, Alexandra] Ctr Biodiversidad Marina & Conservac AC, La Paz 23090, Bcs, Mexico. [Erisman, Brad E.; Moreno-Baez, Marcia; Aburto-Oropeza, Octavio] Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. [Finkbeiner, Elena] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. [Nagavarapu, Sriniketh] Brown Univ, Dept Econ, Providence, RI 02912 USA. [Reddy, Sheila M. W.] Nature Conservancy, Cent Sci Div, Durham, NC 27701 USA. [Juan Ulibarria-Valenzuela, Jose] Fondo Protecc Recursos Marinos, La Paz 23090, Bcs, Mexico. [Hudson Weaver, Amy] Soc Hist Nat Niparaja AC, La Paz 23020, Bcs, Mexico. RP Leslie, HM (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. EM heather.m.leslie@gmail.com; xavier.basurto@duke.edu OI Leslie, Heather/0000-0003-4512-9417 FU US National Science Foundation [GEO 1114964]; David and Lucile Packard Foundation; Brown University's Environmental Change Initiative; Voss Environmental Fellowship Program; Walton Family Foundation; World Wildlife Fund Fuller Fellowship Program FX We appreciate the thoughtful and constructive comments provided by S. Levin, M. Ballestreros, and two anonymous reviewers on earlier versions of this manuscript, and we thank our community partners, who have contributed to our individual and collaborative activities in the region. Funding was provided by the US National Science Foundation (GEO 1114964, to H.M.L., S.N., S.M.W.R., and O.A.-O.), The David and Lucile Packard Foundation (H.M.L., O.A.-O., B.E.E., and M.M.-B.), Brown University's Environmental Change Initiative (H.M.L., L.S., S.N., and S.M.W.R.), Voss Environmental Fellowship Program (K.S.), The Walton Family Foundation (X.B., O.A.-O., B.E.E., M.M.-B., and M.N.), and the World Wildlife Fund Fuller Fellowship Program (M.N.). NR 27 TC 23 Z9 23 U1 9 U2 60 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 MAY 12 PY 2015 VL 112 IS 19 BP 5979 EP 5984 DI 10.1073/pnas.1414640112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH9XS UT WOS:000354390600049 PM 25918372 ER PT J AU Bacon, CD Silvestro, D Jaramillo, C Smith, BT Chakrabarty, P Antonelli, A AF Bacon, Christine D. Silvestro, Daniele Jaramillo, Carlos Smith, Brian Tilston Chakrabarty, Prosanta Antonelli, Alexandre TI Biological evidence supports an early and complex emergence of the Isthmus of Panama SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE biogeography; evolution; neotropics; fossil; migration ID AMERICAN BIOTIC INTERCHANGE; NORTHWESTERN SOUTH-AMERICA; WESTERN PANAMA; NORTH-AMERICA; MIOCENE; COLLISION; HISTORY; CLOSURE; ARC; EVOLUTION AB The linking of North and South America by the Isthmus of Panama had major impacts on global climate, oceanic and atmospheric currents, and biodiversity, yet the timing of this critical event remains contentious. The Isthmus is traditionally understood to have fully closed by ca. 3.5 million years ago (Ma), and this date has been used as a benchmark for oceanographic, climatic, and evolutionary research, but recent evidence suggests a more complex geological formation. Here, we analyze both molecular and fossil data to evaluate the tempo of biotic exchange across the Americas in light of geological evidence. We demonstrate significant waves of dispersal of terrestrial organisms at approximately ca. 20 and 6 Ma and corresponding events separating marine organisms in the Atlantic and Pacific oceans at ca. 23 and 7 Ma. The direction of dispersal and their rates were symmetrical until the last ca. 6 Ma, when northern migration of South American lineages increased significantly. Variability among taxa in their timing of dispersal or vicariance across the Isthmus is not explained by the ecological factors tested in these analyses, including biome type, dispersal ability, and elevation preference. Migration was therefore not generally regulated by intrinsic traits but more likely reflects the presence of emergent terrain several millions of years earlier than commonly assumed. These results indicate that the dramatic biotic turnover associated with the Great American Biotic Interchange was a long and complex process that began as early as the Oligocene-Miocene transition. C1 [Bacon, Christine D.; Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Bacon, Christine D.; Silvestro, Daniele; Antonelli, Alexandre] Univ Gothenburg, Dept Biol & Environm Sci, SE-41319 Gothenburg, Sweden. [Silvestro, Daniele] Univ Lausanne, Dept Ecol & Evolut, CH-1015 Lausanne, Switzerland. [Silvestro, Daniele] Swiss Inst Bioinformat, CH-1015 Lausanne, Switzerland. [Smith, Brian Tilston] Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA. [Smith, Brian Tilston; Chakrabarty, Prosanta] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Antonelli, Alexandre] Gothenburg Bot Garden, SE-41319 Gothenburg, Sweden. RP Bacon, CD (reprint author), Smithsonian Trop Res Inst, Balboa 084303092, Panama. EM christinedbacon@gmail.com RI Chakrabarty, Prosanta/E-3307-2010; Antonelli, Alexandre/A-5353-2011 OI Silvestro, Daniele/0000-0003-0100-0961; Antonelli, Alexandre/0000-0003-1842-9297 FU Smithsonian Institution; Wenner-Gren and Carl Tryggers foundations; Autoridad del Canal de Panama; National Science Foundation [EAR 0824299, OISE/EAR/DRL 0966884, DEB 0916695, DEB 1354149]; National Geographic Society; Swedish Research Council [B0569601]; European Research Council under European Union [331024]; Mark Tupper Smithsonian Fellowship, Ricardo Perez S.A. FX We thank Fernando Alda, Eldridge Bermingham, Juan David Carillo, Anthony Coates, David Dilcher, John Klicka, Harilaos Lessios, Camilo Montes, Andres Mora, Geovanni Romero, Pierre Sepulchre, and The Panama Canal Project-Partnerships in International Research and Education participants for discussions. We are grateful to the Paleobiology Database team for reviewing and databasing the fossil data used in this study. Data analyses were run at the high-performance computing center Vital-IT of the Swiss Institute of Bioinformatics (Lausanne, Switzerland). Financial support was provided by a postdoctoral research fellowship from the Smithsonian Institution (to C.D.B.); the Wenner-Gren and Carl Tryggers foundations (D.S.); the Autoridad del Canal de Panama, the Mark Tupper Smithsonian Fellowship, Ricardo Perez S.A., National Science Foundation Grants EAR 0824299 and OISE/EAR/DRL 0966884, and the National Geographic Society (to C.J.); National Science Foundation Grants DEB 0916695 and DEB 1354149 (to P.C.); and Swedish Research Council Grant B0569601 and European Research Council Grant 331024 under European Union's Seventh Framework Programme FP/2007-2013 (to A.A.). NR 39 TC 72 Z9 75 U1 10 U2 70 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 MAY 12 PY 2015 VL 112 IS 19 BP 6110 EP 6115 DI 10.1073/pnas.1423853112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH9XS UT WOS:000354390600071 PM 25918375 ER PT J AU Peris, CS Vrtilek, SD Steiner, JF Vrtilek, JM Wu, JF McClintock, JE Longa-Pena, P Steeghs, D Callanan, P Ho, LC Orosz, JA Reynolds, MT AF Peris, Charith S. Vrtilek, Saeqa D. Steiner, James F. Vrtilek, Jan M. Wu, Jianfeng McClintock, Jeffrey E. Longa-Pena, Penelope Steeghs, Danny Callanan, Paul Ho, Luis C. Orosz, Jerome A. Reynolds, Mark T. TI Tomography of X-ray Nova Muscae 1991: evidence for ongoing mass transfer and stream-disc overflow SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; stars: individual: Nova Muscae 1991; X-rays: binaries ID BLACK-HOLE; DOPPLER TOMOGRAPHY; ACCRETION DISC; A0620-00; SPECTROSCOPY; SIMULATIONS; QUIESCENCE; BINARIES AB We present a spectroscopic analysis of the black hole binary NovaMuscae 1991 in quiescence using data obtained in 2009 with Magellan Echelette on the Magellan Clay telescope and in 2010 with IMACS on the Magellan Baade telescope at the Las Campanas Observatory. Emission from the disc is observed in H alpha, H beta and Ca II (lambda 8662). A prominent hotspot is observed in the Doppler maps of all three emission lines. The existence of this spot establishes ongoing mass transfer from the donor star in 2009-2010 and, given its absence in the 1993-1995 observations, demonstrates the presence of a variable hotspot in the system. We find the radial distance to the hotspot from the black hole to be consistent with the circularization radius. Our tomograms are suggestive of stream-disc overflow in the system. We also detect possible Ca II (lambda 8662) absorption from the donor star. C1 [Peris, Charith S.; Vrtilek, Saeqa D.; Steiner, James F.; Vrtilek, Jan M.; Wu, Jianfeng; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peris, Charith S.] Northeastern Univ, Dept Phys, Boston, MA 02115 USA. [Longa-Pena, Penelope; Steeghs, Danny] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Callanan, Paul] Univ Coll Cork, Dept Phys, Cork, Ireland. [Ho, Luis C.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Ho, Luis C.] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Reynolds, Mark T.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Peris, CS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cperis@cfa.harvard.edu FU NASA Hubble Fellowship [HST-HF-51315.01]; Kavli Foundation; Peking University; Chinese Academy of Science [XDB09030102] FX We gratefully acknowledge the use of the MOLLY software package written by Tom Marsh. We would like to thank Jorge Casares for sharing his data on Nova Muscae with us. We would also like to thank the referee for helpful comments. JFS has been supported by NASA Hubble Fellowship grant HST-HF-51315.01. LCH acknowledges support from the Kavli Foundation, Peking University, and the Chinese Academy of Science through grant no. XDB09030102 (Emergence of Cosmological Structures) from the Strategic Priority Research Program. NR 32 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 MAY 11 PY 2015 VL 449 IS 2 BP 1584 EP 1592 DI 10.1093/mnras/stv407 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TN UT WOS:000355337500034 ER PT J AU Collinson, JS Ward, MJ Done, C Landt, H Elvis, M McDowell, JC AF Collinson, James S. Ward, Martin J. Done, Chris Landt, Hermine Elvis, Martin McDowell, Jonathan C. TI Reaching the peak of the quasar spectral energy distribution - I. Observations and models SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; galaxies: active; galaxies: high-redshift; quasars: supermassive black holes ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; DIGITAL SKY SURVEY; EMISSION-LINE PROPERTIES; XMM-NEWTON OBSERVATIONS; X-RAY EXCESS; SEYFERT-GALAXIES; DATA RELEASE; OPTICAL-SPECTRA; 1H 0707-495 AB We perform a spectral analysis of a sample of 11 medium redshift (1.5 less than or similar to z less than or similar to 2.2) quasars. Our sample all have optical spectra from the SDSS, infrared spectra from GNIRS and TripleSpec, and X-ray spectra from XMM-Newton. We first analyse the Balmer broad emission line profiles which are shifted into the IR spectra to constrain black hole masses. Then we fit an energy-conserving, three component accretion model of the broad-band spectral energy distribution (SED) to our multiwavelength data. 5 out of the 11 quasars show evidence of an SED peak, allowing us to constrain their bolometric luminosity from these models and estimate their mass accretion rates. Based on our limited sample, we suggest that estimating bolometric luminosities from L-5100 angstrom and L2-10 keV may be unreliable, as has been also noted for a low-redshift, X-ray selected active galactic nucleus sample. C1 [Collinson, James S.; Ward, Martin J.; Done, Chris; Landt, Hermine] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Elvis, Martin; McDowell, Jonathan C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Collinson, JS (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM j.s.collinson@durham.ac.uk RI done, chris/D-4605-2016 OI done, chris/0000-0002-1065-7239 FU STFC FX JSC would like to acknowledge the support of an STFC studentship, and also useful advice from Charles Finn, Emma Gardner, Chichuan Jin and Sarah Hutton. NR 70 TC 7 Z9 7 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 MAY 11 PY 2015 VL 449 IS 2 BP 2174 EP 2193 DI 10.1093/mnras/stv362 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2TN UT WOS:000355337500083 ER PT J AU Diaz, MC Thacker, RW Redmond, NE Perez, T Collins, AG AF Diaz, Maria C. Thacker, Robert W. Redmond, Niamh E. Perez, Thierry Collins, Allen G. TI Vansoestia caribensis gen. nov., sp nov.: first report of the family Ianthellidae (Verongida, Demospongiae) in the Caribbean SO ZOOTAXA LA English DT Article DE Ianthella; Anomoianthella; sponges; cortex; synapomorphy; clade ID SPONGES; REVISION AB A thin fiber-less sponge from Caribbean reefs (Bocas del Toro, Panama) with close genetic affinities (based on 18S and 28S nuclear ribosomal RNA gene sequences) to large fan-shaped fiber-bearing sponges (Ianthella and Anomoianthella) from the Indo-Pacific Ocean is here presented. We describe its overall external morphology, histological features, and ultrastructure. Its genetic distance from the only previously known fiber-less verongid genus, Hexadella, prompted the need to erect a new genus to classify this species. This novel species constitutes the first record for a member of the family Ianthellidae in the Caribbean. The characterization of the family Ianthellidae (sensu Cook and Bergquist, 2000) is here modified by: i) highlighting the cavernous nature of the choanosome, with many lacunae and channels reported for all genera included in the family; ii) extending the family distribution to the Caribbean; and iii) adding a fourth genus to the group of verongids with eurypylous chambers. The possession of a cellularized cortex (10-300 mu m in thickness) is here proposed as a potential synapomorphic character of the Ianthella-Anomoianthella-Vansoestia clade. The main issues regarding the suprageneric classification of verongids are discussed. C1 [Diaz, Maria C.] Museo Marino, Nueva Esparta, Venezuela. [Diaz, Maria C.] NOVA SEU, Oceanog Ctr, Dania, FL 33004 USA. [Thacker, Robert W.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Redmond, Niamh E.; Collins, Allen G.] Smithsonian Inst, NMNH, Washington, DC 20560 USA. [Redmond, Niamh E.; Collins, Allen G.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Perez, Thierry] Inst Mediterraneen Biodivers & Ecol Marine & Cont, CNRS, UMR 7263, F-13007 Marseille, France. [Collins, Allen G.] NOAA, Natl Systemat Lab, Fisheries Serv, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC USA. RP Diaz, MC (reprint author), Museo Marino, Blvd Boca Rio, Nueva Esparta, Venezuela. EM taxochica@gmail.com FU US National Science Foundation, Division of Environmental Biology to the Porifera Tree of Life project [0829763, 0829783, 0829791, 0829986]; University of Alabama at Birmingham (UAB) Center for AIDS Research - US National Institutes of Health [P30 AI027767] FX This work was supported by grants from the US National Science Foundation, Division of Environmental Biology to the Porifera Tree of Life project [grant numbers 0829763, 0829783, 0829791, and 0829986]. This research was also supported by the University of Alabama at Birmingham (UAB) Center for AIDS Research, funded by the US National Institutes of Health [programP30 AI027767]. Dr. Chris Freeman, Kenan Matterson, Dr. Rachel Collin, and the staff of the Smithsonian Tropical Research Institute's Bocas del Toro Research Station provided field assistance. Dr. Susan Laramore assisted on the Histological Lab, at HBOI-FAU, and Sandrine Chenesseau kindly realized cytological sections at IMBE, Marseille. Dr. Eduardo Hajdu (Museu Nacional, UFRJ, Brazil) for editorial comments. NR 20 TC 1 Z9 1 U1 0 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 11 PY 2015 VL 3956 IS 3 BP 403 EP 412 PG 10 WC Zoology SC Zoology GA CI8BO UT WOS:000354992700005 PM 26248926 ER PT J AU Chesser, RT AF Chesser, R. Terry TI A further note on the scientific name of Bullocks' Oriole SO ZOOTAXA LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. RP Chesser, RT (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, POB 37012, Washington, DC 20013 USA. EM chessert@si.edu NR 2 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 11 PY 2015 VL 3956 IS 3 BP 444 EP 444 PG 1 WC Zoology SC Zoology GA CI8BO UT WOS:000354992700009 PM 26248930 ER PT J AU Chan, CK Lee, TE Gopalakrishnan, S AF Chan, Ching-Kit Lee, Tony E. Gopalakrishnan, Sarang TI Limit-cycle phase in driven-dissipative spin systems SO PHYSICAL REVIEW A LA English DT Article ID ION QUANTUM SIMULATOR AB We explore the phase diagram of interacting spin-1/2 systems in the presence of anisotropic interactions, spontaneous decay, and driving. We find a rich phase diagram featuring a limit-cycle phase in which the magnetization oscillates in time. We analyze the spatiotemporal fluctuations of this limit-cycle phase based on a Gaussian-Floquet analysis. Spatial fluctuations destroy long-range limit-cycle ordering for dimension d <= 2, as a time-dependent generalization of the Mermin-Wagner theorem. This result can be interpreted in terms of a spatiotemporal Goldstone mode corresponding to phase fluctuations of the limit cycle. We also demonstrate that the limit-cycle phase exhibits an asymmetric power spectrum measurable in fluorescence experiments. C1 [Chan, Ching-Kit; Lee, Tony E.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Chan, Ching-Kit; Lee, Tony E.; Gopalakrishnan, Sarang] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Chan, CK (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. FU NSF; Croucher Foundation FX We thank Lukas Sieberer for drawing our attention to Ref. [42]. This work was supported by the NSF through a grant to ITAMP. C.K.C. acknowledges support from the Croucher Foundation. NR 43 TC 9 Z9 9 U1 0 U2 5 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 MAY 11 PY 2015 VL 91 IS 5 AR 051601 DI 10.1103/PhysRevA.91.051601 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CH9IP UT WOS:000354349500001 ER PT J AU Banados, E Venemans, BP Morganson, E Hodge, J Decarli, R Walter, F Stern, D Schlafly, E Farina, EP Greiner, J Chambers, KC Fan, X Rix, HW Burgett, WS Draper, PW Flewelling, J Kaiser, N Metcalfe, N Morgan, JS Tonry, JL Wainscoat, RJ AF Banados, E. Venemans, B. P. Morganson, E. Hodge, J. Decarli, R. Walter, F. Stern, D. Schlafly, E. Farina, E. P. Greiner, J. Chambers, K. C. Fan, X. Rix, H-W Burgett, W. S. Draper, P. W. Flewelling, J. Kaiser, N. Metcalfe, N. Morgan, J. S. Tonry, J. L. Wainscoat, R. J. TI CONSTRAINING THE RADIO-LOUD FRACTION OF QUASARS AT z > 5.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; quasars: general ID DIGITAL SKY SURVEY; SIMILAR-TO 6; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; OPTICALLY SELECTED QUASARS; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; LUMINOSITY FUNCTION; HIGH-REDSHIFT; Z-SIMILAR-TO-6 QUASARS; HIGH-RESOLUTION AB Radio-loud active galactic nuclei at z similar to 2-4 are typically located in dense environments and their host galaxies are among the most massive systems at those redshifts, providing key insights for galaxy evolution. Finding radio-loud quasars at the highest accessible redshifts (z similar to 6) is important to the study of their properties and environments at even earlier cosmic time. They could also serve as background sources for radio surveys intended to study the intergalactic medium beyond the epoch of reionization in HI 21 cm absorption. Currently, only five radio-loud (R= f(v,5) (GHz)/f(v,4400) (angstrom) > 10) quasars are known at z similar to 6. In this paper we search for 5.5 less than or similar to z less than or similar to 7.2 quasars by cross-matching the optical Panoramic Survey Telescope & Rapid Response System 1 and radio Faint Images of the Radio Sky at Twenty cm surveys. The radio information allows identification of quasars missed by typical color-based selections. While we find no good 6.4 less than or similar to z less than or similar to 7.2 quasar candidates at the sensitivities of these surveys, we discover two new radio-loud quasars at z similar to 6. Furthermore, we identify two additional z similar to 6 radio-loud quasars that were not previously known to be radio-loud, nearly doubling the current z similar to 6 sample. We show the importance of having infrared photometry for z > 5.5 quasars to robustly classify them as radio-quiet or radioloud. Based on this, we reclassify the quasar J0203+0012 (z = 5.72), previously considered radio-loud, to be radio-quiet. Using the available data in the literature, we constrain the radio-loud fraction of quasars at z similar to 6, using the Kaplan-Meier estimator, to be 8.1(-3.2)(+5.0)%. This result is consistent with there being no evolution of the radio-loud fraction with redshift, in contrast to what has been suggested by some studies at lower redshifts. C1 [Banados, E.; Venemans, B. P.; Decarli, R.; Walter, F.; Schlafly, E.; Farina, E. P.; Rix, H-W] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Morganson, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hodge, J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Chambers, K. C.; Burgett, W. S.; Flewelling, J.; Kaiser, N.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Fan, X.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Draper, P. W.; Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Banados, E (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM banados@mpia.de OI Farina, Emanuele Paolo/0000-0002-6822-2254; Banados, Eduardo/0000-0002-2931-7824; Chambers, Kenneth /0000-0001-6965-7789; Schlafly, Edward Ford/0000-0002-3569-7421 FU ERC grant "Cosmic Dawn"; National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877]; NSF [AST-9987045]; NSF Telescope System Instrumentation Program (TSIP); Ohio Board of Regents; Ohio State University Office of Research; DFG [HA 1850/28-1]; National Aeronautics and Space Administration FX We thank the anonymous referee for providing excellent suggestions and comments that improved the manuscript. E. B. thanks the IMPRS for Astronomy & Cosmic Physics at the University of Heidelberg. E. P. F. and B. P. V. acknowledge funding through the ERC grant "Cosmic Dawn." We thank F. Ardila, M. Balokovic J. Larson, E. Manjavacas, M. Maseda, T. Minear, A. Place, S. Schmidl, and C. Steinhardt for their important participation in some of our follow-up observations. 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, Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. This work is based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programs ID 092.A-0150, 093.A-0863, and 093.A-0574. The LBT is an international collaboration among institutions in the United States, Italy and Germany. The LBT Corporation partners are: The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University; The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota and University of Virginia. This paper used data obtained with the MODS spectrographs built with funding from NSF grant AST-9987045 and the NSF Telescope System Instrumentation Program (TSIP), with additional funds from the Ohio Board of Regents and the Ohio State University Office of Research. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). 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. We used the Milliquas Quasar Catalog to cross match our candidates with known quasars (http://quasars.org/milliquas.htm; Flesch 2015) This research made use of Astropy, a community-developed core Python package for Astronomy (Robitaille & Tollerud 2013; http://www.astropy.org). We used the python package Lifelines (Davidson-Pilon 2015) https://github.com/camdavidsonpilon/lifelines) to perform the Kaplan-Meier estimates. This publication made use of TOPCAT (Taylor et al. 2005, http://www.starlink.ac.uk/topcat). The plots in this publication were produced using Matplotlib (Hunter 2007, http://www.matplotlib.org). NR 101 TC 9 Z9 9 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 MAY 10 PY 2015 VL 804 IS 2 AR 118 DI 10.1088/0004-637X/804/2/118 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000040 ER PT J AU Lunnan, R Chornock, R Berger, E Rest, A Fong, W Scolnic, D Jones, DO Soderberg, AM Challis, PM Drout, MR Foley, RJ Huber, ME Kirshner, RP Leibler, C Marion, GH McCrum, M Milisavljevic, D Narayan, G Sanders, NE Smartt, SJ Smith, KW Tonry, JL Burgett, WS Chambers, KC Flewelling, H Kudritzki, RP Wainscoat, RJ Waters, C AF Lunnan, R. Chornock, R. Berger, E. Rest, A. Fong, W. Scolnic, D. Jones, D. O. Soderberg, A. M. Challis, P. M. Drout, M. R. Foley, R. J. Huber, M. E. Kirshner, R. P. Leibler, C. Marion, G. H. McCrum, M. Milisavljevic, D. Narayan, G. Sanders, N. E. Smartt, S. J. Smith, K. W. Tonry, J. L. Burgett, W. S. Chambers, K. C. Flewelling, H. Kudritzki, R. -P. Wainscoat, R. J. Waters, C. TI ZOOMING IN ON THE PROGENITORS OF SUPERLUMINOUS SUPERNOVAE WITH THE HST SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: star formation; supernovae: general ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURSTS; PAIR-INSTABILITY SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; HOST GALAXIES; LIGHT CURVES; LUMINOUS SUPERNOVAE; IC SUPERNOVAE; IIN SUPERNOVA; ULTRALUMINOUS SUPERNOVAE AB We present Hubble Space Telescope (HST) rest-frame ultraviolet imaging of the host galaxies of 16 hydrogen-poor superluminous supernovae (SLSNe), including 11 events from the Pan-STARRS Medium Deep Survey. Taking advantage of the superb angular resolution of HST, we characterize the galaxies' morphological properties, sizes, and star formation rate (SFR) densities. We determine the supernova (SN) locations within the host galaxies through precise astrometric matching and measure physical and host-normalized offsets as well as the SN positions within the cumulative distribution of UV light pixel brightness. We find that the host galaxies of H-poor SLSNe are irregular, compact dwarf galaxies, with a median half-light radius of just 0.9 kpc. The UV-derived SFR densities are high ([Sigma(SFR)] similar or equal to 0.1M(circle dot) yr(-1) kpc(-1)), suggesting that SLSNe form in overdense environments. Their locations trace the UV light of their host galaxies, with a distribution intermediate between that of long-duration gamma-ray bursts (LGRBs; which are strongly clustered on the brightest regions of their hosts) and a uniform distribution (characteristic of normal core-collapse SNe), though cannot be statistically distinguished from either with the current sample size. Taken together, this strengthens the picture that SLSN progenitors require different conditions than those of ordinary core-collapse SNe to form and that they explode in broadly similar galaxies as do LGRBs. If the tendency for SLSNe to be less clustered on the brightest regions than are LGRBs is confirmed by a larger sample, this would indicate a different, potentially lower-mass progenitor for SLSNe than LRGBs. C1 [Lunnan, R.; Chornock, R.; Berger, E.; Fong, W.; Soderberg, A. M.; Challis, P. M.; Drout, M. R.; Foley, R. J.; Kirshner, R. P.; Leibler, C.; Marion, G. H.; Milisavljevic, D.; Narayan, G.; Sanders, N. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chornock, R.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Clippinger Lab 251B, Athens, OH 45701 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fong, W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Scolnic, D.; Jones, D. O.] Johns Hopkins Univ, Dept Phys & Astron, 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. [Huber, M. E.; Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Flewelling, H.; Kudritzki, R. -P.; Wainscoat, R. J.; Waters, C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Leibler, C.] UCSC, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [McCrum, M.; Smartt, S. J.; Smith, K. W.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Lunnan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rlunnan@cfa.harvard.edu OI Lunnan, Ragnhild/0000-0001-9454-4639; Narayan, Gautham/0000-0001-6022-0484; Chambers, Kenneth /0000-0001-6965-7789; Flewelling, Heather/0000-0002-1050-4056 FU NASA through Space Telescope Science Institute [GO-12529, GO-13022, GO-13326]; NASA [NAS5-26555]; National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877, AST1211196]; European Research Council under European Union's Seventh Framework Programme (FP7)/ERC [291222] FX We thank the anonymous referee for helpful comments that improved the clarity of the paper. Support for program numbers GO-12529, GO-13022, and GO-13326 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. 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). This paper includes data based on observations made with the NASA/ESA Hubble Space Telescope and 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). S.J.S. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. [291222]. R.P.K. acknowledges support from the National Science foundation through AST1211196. NR 82 TC 17 Z9 17 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2015 VL 804 IS 2 AR 90 DI 10.1088/0004-7X/804/2/90 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000012 ER PT J AU Miyaji, T Hasinger, G Salvato, M Brusa, M Cappelluti, N Civano, F Puccetti, S Elvis, M Brunner, H Fotopoulou, S Ueda, Y Griffiths, RE Koekemoer, AM Akiyama, M Comastri, A Gilli, R Lanzuisi, G Merloni, A Vignali, C AF Miyaji, T. Hasinger, G. Salvato, M. Brusa, M. Cappelluti, N. Civano, F. Puccetti, S. Elvis, M. Brunner, H. Fotopoulou, S. Ueda, Y. Griffiths, R. E. Koekemoer, A. M. Akiyama, M. Comastri, A. Gilli, R. Lanzuisi, G. Merloni, A. Vignali, C. TI DETAILED SHAPE AND EVOLUTIONARY BEHAVIOR OF THE X-RAY LUMINOSITY FUNCTION OF ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: luminosity function, mass function; quasars: general; X-rays: galaxies ID WIDE-FIELD SURVEY; MEDIUM SENSITIVITY SURVEY; SUPERMASSIVE BLACK-HOLES; HALO OCCUPATION DISTRIBUTION; SPATIAL CORRELATION-FUNCTION; NEWTON SERENDIPITOUS SURVEY; CROSS-CORRELATION FUNCTION; DEEP ROSAT SURVEY; LARGE SKY SURVEY; LOG S-RELATIONS AB We construct the rest-frame 2-10 keV intrinsic X-ray luminosity function (XLF) of active galactic nuclei (AGNs) from a combination of X-ray surveys from the all-sky Swift BAT survey to the Chandra Deep Field. South. We use similar to 3200 AGNs in our analysis, which covers six orders of magnitude in flux. The inclusion of XMM and Chandra COSMOS data has allowed us to investigate the detailed behavior of the XLF and evolution. In deriving our XLF, we take into account realistic AGN spectrum templates, absorption corrections, and probability. density distributions in photometric redshift. We present an analytical expression for the overall behavior of the XLF in terms of the luminosity-dependent density evolution, smoothed two-power-law expressions in 11 redshift shells, three-segment power-law expression of the number density evolution in four luminosity classes, and binned XLF. We observe a sudden flattening of the low luminosity end slope of the XLF slope at z greater than or similar to 0.6. Detailed structures of the AGN downsizing have also been revealed, where the number density curves have two clear breaks at all luminosity classes above log L-X > 43. The two-break structure is suggestive of two-phase AGN evolution, consisting of major merger triggering and secular processes. C1 [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron Sede Ensenada, Ensenada 22860, Baja California, Mexico. [Miyaji, T.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Salvato, M.; Brusa, M.; Brunner, H.; Merloni, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Brusa, M.; Vignali, C.] Univ Bologna, DIFA Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Brusa, M.; Cappelluti, N.; Comastri, A.; Gilli, R.; Lanzuisi, G.; Vignali, C.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Civano, F.] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, F.; Elvis, M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Fotopoulou, S.] Univ Geneva, CH-1290 Versoix, Switzerland. [Ueda, Y.] Kyoto Univ, Fac Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Griffiths, R. E.] Univ Hawaii, Phys & Astron, Hilo, HI 96720 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Akiyama, M.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. RP Miyaji, T (reprint author), POB 439027, San Ysidro, CA 92143 USA. EM miyaji@astrosen.unam.mx; hasinger@ifa.hawaii.edu RI Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; Vignali, Cristian/J-4974-2012; OI Koekemoer, Anton/0000-0002-6610-2048; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Vignali, Cristian/0000-0002-8853-9611; Fotopoulou, Sotiria/0000-0002-9686-254X; Cappelluti, Nico/0000-0002-1697-186X; Lanzuisi, Giorgio/0000-0001-9094-0984; Puccetti, Simonetta/0000-0002-2734-7835; Hasinger, Guenther/0000-0002-0797-0646; Miyaji, Takamitsu/0000-0002-7562-485X FU UNAM-DGAPA Grant [PAPIIT IN104113]; CONACyT [179662]; FP7 Career Integration Grant "eEASy" [CIG 321913]; INAF [PRIN-INAF-2011, PRIN-INAF-2012]; Ministry of Education, Culture, Sports, Science and Technology of Japan (MEXT) [26400228] FX This work is supported by UNAM-DGAPA Grant PAPIIT IN104113 and CONACyT Grant Cientifica Basica 179662 (to T.M.). Also acknowledged are the FP7 Career Integration Grant "eEASy" CIG 321913 (to M.B.), financial support from INAF under Contracts PRIN-INAF-2011 and PRIN-INAF-2012 (to N.C., A.C., and R.G.), and the Grant-in-Aid for Scientific Research 26400228 (to Y.U.) from the Ministry of Education, Culture, Sports, Science and Technology of Japan (MEXT). We gratefully acknowledge the contributions of the entire COSMOS collaboration, consisting of more than 100 scientists. More information about the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. The authors thank Len Cowie and his collaborators for allowing us to use their unpublished spectroscopic redshifts and Murray Brightman for his advice on CTK AGNs. NR 115 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 MAY 10 PY 2015 VL 804 IS 2 AR 104 DI 10.1088/0004-637X/804/2/104 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000026 ER PT J AU Rivers, E Risaliti, G Walton, DJ Harrison, F Arevalo, P Baur, FE Boggs, SE Brenneman, LW Brightman, M Christensen, FE Craig, WW Furst, F Hailey, CJ Hickox, RC Marinucci, A Reeves, J Stern, D Zhang, WW AF Rivers, E. Risaliti, G. Walton, D. J. Harrison, F. Arevalo, P. Baur, F. E. Boggs, S. E. Brenneman, L. W. Brightman, M. Christensen, F. E. Craig, W. W. Fuerst, F. Hailey, C. J. Hickox, R. C. Marinucci, A. Reeves, J. Stern, D. Zhang, W. W. TI THE MULTI-LAYER VARIABLE ABSORBERS IN NGC 1365 REVEALED BY XMM-NEWTON AND NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 1365); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL VARIABILITY; ACCRETION DISK; ABSORPTION; WIND; SUZAKU; AGN AB Between 2012 July and 2013 February, NuSTAR and XMM-Newton performed four long-look joint observations of the type 1.8 Seyfert, NGC 1365. We have analyzed the variable absorption seen in these observations in order to characterize the geometry of the absorbing material. Two of the observations caught NGC 1365 in an unusually low absorption state, revealing complexity in the multi-layer absorber that had previously been hidden. We find the need for three distinct zones of neutral absorption in addition to the two zones of ionized absorption and the Compton-thick torus previously seen in this source. The most prominent absorber is likely associated with broad-line region clouds with column densities of around similar to 10(23) cm(-2) and a highly clumpy nature as evidenced by an occultation event in 2013 February. We also find evidence of a patchy absorber with a variable column around similar to 10(22) cm(-2) and a line-of-sight covering fraction of 0.3-0.9, which responds directly to the intrinsic source flux, possibly due to a wind geometry. A full-covering, constant absorber with a low column density of similar to 1 x 10(22) cm(-2) is also present, though the location of this low density haze is unknown. C1 [Rivers, E.; Walton, D. J.; Harrison, F.; Brightman, M.; Fuerst, F.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.; Brenneman, L. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Baur, F. E.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 22, Chile. [Baur, 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. [Christensen, F. E.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [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. [Marinucci, A.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Reeves, J.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rivers, E (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Risaliti, Guido/0000-0002-3556-977X FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; NASA/GSFC; NASA/IPAC; NASA FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. 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 work has also made use of HEASARC online services, supported by NASA/GSFC, and the NASA/IPAC Extragalactic Database, operated by JPL/California Institute of Technology under contract with NASA. This work also made use of data from the XMM-Newton observatory. NR 31 TC 5 Z9 5 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 MAY 10 PY 2015 VL 804 IS 2 AR 107 DI 10.1088/0004-637X/804/2/107 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000029 ER PT J AU Yuan, F Gan, ZM Narayan, R Sadowski, A Bu, DF Bai, XN AF Yuan, Feng Gan, Zhaoming Narayan, Ramesh Sadowski, Aleksander Bu, Defu Bai, Xue-Ning TI NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: jets; hydrodynamics ID ADVECTION-DOMINATED ACCRETION; ACTIVE GALACTIC NUCLEI; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; SPINNING BLACK-HOLE; SAGITTARIUS-A; 2-DIMENSIONAL MODELS; ELLIPTIC GALAXIES; MASS OUTFLOWS; 2 DIMENSIONS; FEEDBACK AB Previous MHD simulations have shown that wind must exist in black hole hot accretion flows. In this paper, we continue our study by investigating the detailed properties of wind and the mechanism of wind production. For this aim, we make use of a 3D general relativistic MHD simulation of hot accretion flows around a Schwarzschild black hole. To distinguish real wind from turbulent outflows, we track the trajectories of the virtual Lagrangian particles from simulation data. We find two types of real outflows, i.e., a jet and a wind. The mass flux of wind is very significant, and its radial profile can be described by (M) over dot(wind) approximate to (M) over dot(BH) (r/20 r(s)), with (M) over dot(BH) being the mass accretion rate at the black hole horizon and r(s) being the Schwarzschild radius. The poloidal wind speed almost remains constant once they are produced, but the flux-weighted wind speed roughly follows v(p,wind) (r) approximate to 0.25v(k) (r), with v(k)(r) being the Keplerian speed at radius r. The mass flux of the. jet is much lower, but the speed is much higher, v(p, jet) similar to (0.3-0.4)c. Consequently, both the energy and momentum fluxes of the wind are much larger than those of the jet. The wind is produced and accelerated primarily by the combination of centrifugal force and magnetic pressure gradient, while the jet is mainly accelerated by the magnetic pressure gradient. Finally, we find that the wind production efficiency is an element of(wind) equivalent to (E) over dot(wind)/(M) over dot(BH)c(2) similar to 1/1000 2 is in good agreement with the value required from large-scale galaxy simulations with active galactic nucleus feedback. C1 [Yuan, Feng; Gan, Zhaoming; Bu, Defu] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Narayan, Ramesh; Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sadowski, Aleksander] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Yuan, F (reprint author), Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China. EM fyuan@shao.ac.cn; zmgan@shao.ac.cn; narayan@cfa.harvard.edu; asadowsk@mit.edu; dfbu@shao.ac.cn; xbai@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU National Basic Research Program of China (973 Program) [2014CB845800]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of CAS [XDB09000000]; NSF of China [11103059, 11103061, 11121062, 11133005]; NSF [AST1312651, TG-AST080026N]; NASA [NNX14AB47G, NAS8-03060, NAS 5-26555]; NASA through Einstein Postdoctotral Fellowship - Chandra X-ray Center [PF4-150126]; NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51301.001-A]; NASA via the High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center; SHAO Super Computing Platform FX F.Y. thanks Jim Stone for the valuable discussions. F.Y., Z.G., and D.B. were supported in part by the National Basic Research Program of China (973 Program, grant 2014CB845800), the Strategic Priority Research Program "The Emergence of Cosmological Structures" of CAS (grant XDB09000000), and NSF of China (grants 11103059, 11103061, 11121062, and 11133005). R.N. was supported in part by NSF grant AST1312651 and NASA grant NNX14AB47G. A.S. acknowledges support for this work by NASA through Einstein Postdoctotral Fellowship number PF4-150126 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. X.B. is supported by NASA through Hubble Fellowship grant HST-HF2-51301.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The authors acknowledge computational support from NSF via XSEDE resources (grant TG-AST080026N), from NASA via the High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, and from SHAO Super Computing Platform. NR 60 TC 27 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 MAY 10 PY 2015 VL 804 IS 2 AR 101 DI 10.1088/0004-637X/804/2/101 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000023 ER PT J AU Zhang, B David, LP Jones, C Andrade-Santos, F O'Sullivan, E Dahle, H Nulsen, PEJ Clarke, TE Pointecouteau, E Pratt, GW Arnaud, M Vrtilek, JM Ji, L van Weeren, RJ Kraft, RP Kong, X AF Zhang, B. David, L. P. Jones, C. Andrade-Santos, F. O'Sullivan, E. Dahle, H. Nulsen, P. E. J. Clarke, T. E. Pointecouteau, E. Pratt, G. W. Arnaud, M. Vrtilek, J. M. Ji, L. van Weeren, R. J. Kraft, R. P. Kong, X. TI CHANDRA AND XMM-NEWTON OBSERVATIONS OF THE MERGING CLUSTER OF GALAXIES PLCK G036.7+14.9 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: individual (PLCK G036.7+14.9); X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; INTERACTION CROSS-SECTION; DIGITAL SKY SURVEY; X-RAY-CLUSTERS; COOLING FLOWS; DARK-MATTER; COSMOLOGICAL SIMULATIONS; TEMPERATURE PROFILES; REPRESENTATIVE SAMPLE; THERMAL CONDUCTION AB We present Chandra and XMM-Newton observations of PLCK G036.7+14.9 from the Chandra-Planck Legacy Program. The high resolution X-ray observations reveal two close (similar to 72" - 193 kpc in projection) subclusters, G036N and G036S, which were not resolved by previous ROSAT, optical, or recent Planck observations. We perform detailed imaging and spectral analyses and use a simplified model to study the kinematics of this system. The basic picture is that PLCK G036.7+14.9 is undergoing a major merger (mass ratio close to unity) between the two massive subclusters, with the merger largely along the line of sight (similar to 80 degrees between the merger axis and the plane of the sky from the simplified model) and probably at an early stage (less than similar to 0.4-0.7 Gyr since the merger began). G036N hosts a small (similar to 27 kpc), moderate cool core (cooling time t(cool) similar to 2.6-4.7Gyr), while G036S has at most a very weak cool core (t(cool) similar to 5.7-10.3Gyr) in the central similar to 40 kpc region. The difference in core cooling times is unlikely to be caused by the ongoing merger disrupting a pre-existing cool core in G036S. G036N also hosts an unresolved radio source in the center, which may be heating the gas if the radio source is extended. The total mass of the whole cluster determined from XMM-Newton is similar to(5.9-8.0) x 10(14) M-circle dot, and is similar to(6.7-9.9) x 10(14) M-circle dot from Chandra. The Planck derived mass,similar to(5.1-6.0) x 10(14) M-circle dot, is higher than the X-ray measured mass of either subcluster, but is lower than the X-ray measured mass of the whole cluster, due to the fact that Planck does not resolve PLCK G036.7+14.9 into subclusters and interprets it as a single cluster. This mass discrepancy could induce significant bias to the mass function if such previously unresolved systems are common in the Planck cluster sample. High resolution X-ray observations are necessary to identify the fraction of such systems and correct such a bias for the purpose of precision cosmological studies. C1 [Zhang, B.; Kong, X.] Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. [Zhang, B.; Kong, X.] Chinese Acad Sci, Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China. [Zhang, B.; David, L. P.; Jones, C.; Andrade-Santos, F.; O'Sullivan, E.; Nulsen, P. E. J.; Vrtilek, J. M.; van Weeren, R. J.; Kraft, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dahle, H.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Clarke, T. E.] Naval Res Lab, Washington, DC 20375 USA. [Pointecouteau, E.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Pointecouteau, E.] CNRS, IRAP, F-31028 Toulouse 4, France. [Pratt, G. W.; Arnaud, M.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,IRFU,Serv Astrophys,CEA DSM, F-91191 Gif Sur Yvette, France. [Ji, L.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. RP Zhang, B (reprint author), Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China. EM zhb006@mail.ustc.edu.cn; xkong@ustc.edu.cn OI O'Sullivan, Ewan/0000-0002-5671-6900; Nulsen, Paul/0000-0003-0297-4493; van Weeren, Reinout/0000-0002-0587-1660 FU China Scholarship Council; NASA [GO2-13146X]; Chandra X-ray Center; 100 Talents program of the Chinese Academy of Sciences (CAS); Key Laboratory of Dark Matter and Space Astronomy of CAS; National Natural Science Foundation of China (NSFC) [11225315, 1320101002, 11433005, 11421303]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; Specialized Research Fund for the Doctoral Program of Higher Education (SRFDP) [20123402110037]; Chinese National 973 Fundamental Science Programs (973 program) [2015CB857004]; ESA Member States; NASA; National Aeronautics Space Administration (NASA) [NAS8-03060]; SAO predoctoral fellowship program FX We thank Nabila Aghanim, Iacopo Bartalucci, James G. Bartlett, Hans Bohringer, Stefano Borgani, Shea Brown, Gayoung Chon, Eugene Churazov, Jessica Democles, Daniel Eisenstein, Chiara Ferrari, William Forman, Simona Giacintucci, Charles Lawrence, Marceau Limousin, Giulia Macario, Douspis Marian, Pasquale Mazzotta, Jean-Baptiste Melin, Stephen S. Murray, Elena Pierpaoli, Rashid A. Sunyaev, and Alexey Vikhlinin for reading an early version of the manuscript and Harald Ebeling for communications on PLCK G036.7+14.9. We thank the referee for useful comments and suggestions. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory (ObsID 15098), which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of the National Aeronautics Space Administration (NASA) under contract NAS8-03060, and XMM-Newton (ObsID 0692931901), an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We also present results based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain of the Instituto de Astrofisica de Canarias. B.Z. acknowledges the SAO predoctoral fellowship program and financial support from China Scholarship Council. L.P.D. is supported in part by NASA grant GO2-13146X. C.J. acknowledges support from the Chandra X-ray Center. L.J. is supported by the 100 Talents program of the Chinese Academy of Sciences (CAS) and the Key Laboratory of Dark Matter and Space Astronomy of CAS. X.K. is supported by the National Natural Science Foundation of China (NSFC, Nos. 11225315, 1320101002, 11433005, and 11421303), the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (No. XDB09000000), the Specialized Research Fund for the Doctoral Program of Higher Education (SRFDP, No. 20123402110037), and the Chinese National 973 Fundamental Science Programs (973 program) (2015CB857004). NR 92 TC 1 Z9 1 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 MAY 10 PY 2015 VL 804 IS 2 AR 129 DI 10.1088/0004-637X/804/2/129 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000051 ER PT J AU Zhang, QZ Wang, K Lu, X Jimenez-Serra, I AF Zhang, Qizhou Wang, Ke Lu, Xing Jimenez-Serra, Izaskun TI FRAGMENTATION OF MOLECULAR CLUMPS AND FORMATION OF A PROTOCLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (IRDC G28.34+0.06); ISM: jets and outflows; ISM: kinematics and dynamics; stars: formation ID INFRARED-DARK CLOUDS; MASSIVE-STAR-FORMATION; LARGE ARRAY OBSERVATIONS; DUST CONTINUUM EMISSION; MAGNETIC-FIELDS; FORMING REGION; PROTOSTELLAR CANDIDATES; DYNAMICAL COLLAPSE; INITIAL CONDITIONS; MILKY-WAY AB Sufficiently massive clumps of molecular gas collapse under self-gravity and fragment to spawn a cluster of stars that have a range of masses. We investigate observationally the early stages of formation of a stellar cluster in a massive filamentary infrared dark cloud, G28.34+0.06 P1, in the 1.3 mm continuum and spectral line emission using the Atacama Large Millimeter/Submillimeter Array. Sensitive continuum data reveal further fragmentation in five dusty cores at a resolution of several 10(3) AU. Spectral line emission from (CO)-O-18, CH3OH, (CS)-C-13, H2CO, and N2D+ is detected for the first time toward these dense cores. We found that three cores are chemically more evolved as compared with the other two; interestingly, though, all of them are associated with collimated outflows as suggested by evidence from the CO, SiO, CH3OH, H2CO, and SO emission. The parsec-scale kinematics in NH3 exhibit velocity gradients along the filament, consistent with accretion flows toward the clumps and cores. The moderate luminosity and the chemical signatures indicate that the five cores harbor low-to intermediate-mass protostars that likely become massive ones at the end of the accretion. Despite the fact that the mass limit reached by the 1 sigma dust continuum sensitivity is 30 times lower than the thermal Jeans mass, there is a lack of a distributed low-mass protostellar population in the clump. Our observations indicate that in a protocluster, low-mass stars form at a later stage after the birth of more massive protostars. C1 [Zhang, Qizhou; Lu, Xing] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Ke; Jimenez-Serra, Izaskun] European So Observ, D-85748 Garching, Germany. [Lu, Xing] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. RP Zhang, QZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM qzhang@cfa.harvard.edu OI Wang, Ke/0000-0002-7237-3856; Zhang, Qizhou/0000-0003-2384-6589 FU National Science Foundation of China [11328301]; ESO fellowship; Smithsonian Predoctoral Fellowship; People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7) Uunder REA [PIIF-GA-2011-301538]; NASA FX We thank P. C. Myers for enlightening discussions. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the ALMA data. ALMA is a partnership of ESO (representing its member states), NFS (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research is partly supported by the National Science Foundation of China under Grant 11328301. K.W. acknowledges support from the ESO fellowship. X.L. acknowledges the support of the Smithsonian Predoctoral Fellowship. I.J.-S. acknowledges funding received from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7/2007-2013) under REA grant agreement PIIF-GA-2011-301538. 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. NR 114 TC 17 Z9 17 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 MAY 10 PY 2015 VL 804 IS 2 AR 141 DI 10.1088/0004-637X/804/2/141 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI6WR UT WOS:000354905000063 ER PT J AU Genel, S Fall, SM Hernquist, L Vogelsberger, M Snyder, GF Rodriguez-Gomez, V Sijacki, D Springel, V AF Genel, Shy Fall, S. Michael Hernquist, Lars Vogelsberger, Mark Snyder, Gregory F. Rodriguez-Gomez, Vicente Sijacki, Debora Springel, Volker TI GALACTIC ANGULAR MOMENTUM IN THE ILLUSTRIS SIMULATION: FEEDBACK AND THE HUBBLE SEQUENCE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: formation; galaxies: fundamental parameters; galaxies: kinematics and dynamics; galaxies: structure; hydrodynamics; methods: numerical ID MOVING-MESH COSMOLOGY; DISC GALAXY FORMATION; STELLAR FEEDBACK; MATTER; DARK; ORIGIN; MODEL; GAS; EVOLUTION; UNIVERSE AB We study the stellar angular momentum of thousands of galaxies in the Illustris cosmological simulation, which captures gravitational and gas dynamics within galaxies, as well as feedback from stars and black holes. We find that the angular momentum of the simulated galaxies matches observations well, and in particular two distinct relations are found for late-type versus early-type galaxies. The relation for late-type galaxies corresponds to the value expected from full conservation of the specific angular momentum generated by cosmological tidal torques. The relation for early-type galaxies corresponds to retention of only similar to 30% of that, but we find that those early-type galaxies with low angular momentum at z = 0 nevertheless reside at high redshift on the late-type relation. Some of them abruptly lose angular momentum during major mergers. To gain further insight, we explore the scaling relations in simulations where the galaxy formation physics is modified with respect to the fiducial model. We find that galactic winds with high mass-loading factors are essential for obtaining the high angular momentum relation typical for late-type galaxies, while active galactic nucleus feedback largely operates in the opposite direction. Hence, feedback controls the stellar angular momentum of galaxies, and appears to be instrumental for establishing the Hubble sequence. C1 [Genel, Shy] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Genel, Shy; Hernquist, Lars; Rodriguez-Gomez, Vicente] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fall, S. Michael; Snyder, Gregory F.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Vogelsberger, Mark] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sijacki, Debora] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Springel, Volker] Heidelberg Inst Theoret Studies, Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany. RP Genel, S (reprint author), Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. EM shygenelastro@gmail.com OI Rodriguez-Gomez, Vicente/0000-0002-9495-0079; Genel, Shy/0000-0002-3185-1540; Springel, Volker/0000-0001-5976-4599 FU XSEDE project [TG-AST110016]; Leibniz Computing Centre, Germany [pr85je]; CURIE supercomputer at CEA/France, PRACE project [RA0844]; FAS Science Division Research Computing Group at Harvard University; NASA through Hubble Fellowship [HST-HF2-51341.001 A]; NASA [NAS5-26555, NNX12AC67G]; NSF [PHY11-25915, PHYS-1066293, AST-1312095]; HST [HST-AR-12856.01 A, HST-AR-13887.004 A]; NASA through grants from STScI; DFG Research Centre [SFB-881, A1]; European Research Council under ERC-StG [EXAGAL-308037] FX We thank Avishai Dekel and Jolanta Krzyszkowska for useful discussions, Jennifer Lotz for providing us her code for calculating galaxy morphologies, and Dylan Nelson for comments on an early draft. We also thank the anonymous referee for helpful comments. Simulations were run at the Texas Advanced Computing Center as part of XSEDE project TG-AST110016, the Leibniz Computing Centre, Germany, as part of project pr85je, on the CURIE supercomputer at CEA/France as part of PRACE project RA0844, and on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. S.G. acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51341.001 A awarded by the STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. S.M.F. appreciates the hospitality of the Kavli Institute for Theoretical Physics and the Aspen Center for Physics, which are supported in part by NSF grants PHY11-25915 and PHYS-1066293 respectively. G.S. acknowledges support from HST grants HST-AR-12856.01 A and HST-AR-13887.004 A, provided by NASA through grants from STScI. 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 grant EXAGAL-308037. L.H. acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. NR 51 TC 21 Z9 21 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 MAY 10 PY 2015 VL 804 IS 2 AR L40 DI 10.1088/2041-8205/804/2/L40 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH8NN UT WOS:000354293200014 ER PT J AU Sterrenburg, FAS Tiffany, MA Hinz, F Herwig, WE Hargraves, PE AF Sterrenburg, Frithjof A. S. Tiffany, Mary Ann Hinz, Friedel Herwig, Wulf E. Hargraves, Paul E. TI Seven new species expand the morphological spectrum of Haslea. A comparison with Gyrosigma and Pleurosigma (Bacillariophyta) SO PHYTOTAXA LA English DT Article ID VALVE MORPHOGENESIS; SP-NOV; DIATOMS AB Seven new Haslea species demonstrate that the genus has evolved a richer morphological repertoire than so far reported. H. feriarum sp. nov. has a valve contour suggesting an Amphora; H. staurosigmoidea sp. nov. has a sigmoid valve with a pseudostauros; H. tsukamotoi sp. nov. and the closely similar H. meteorou sp. nov. possess uniquely shaped external central raphe endings and a fully sideways-tilted internal raphe system; H. clevei sp. nov. and H. avium sp. nov. also have central raphe ending shapes not yet described in the genus; H. amicorum shows interrupted longitudinal fissures besides the continuous fissures characteristic of Haslea. A survey of the Haslea species described, for differentiation of our taxa, led to two conclusions: 1) the data in the protologue of H. indica Desikachary & Prema are spurious and 2) "Navicula" duerrenbergiana Hustedt is here transferred to the genus Haslea. The basic Haslea morphology is a sandwich-type valve, with a grate-like inner layer (here called basal layer) and an outer layer (here called tegumental layer) perforated by continuous longitudinal fissures. These two layers are shored by upright longitudinal "bulkheads", here called saepes, seen to be perforated in the valves that permitted their observation. This morphology is closely similar to that of Gyrosigma (and Pleurosigma). The great variety of central external raphe ending patterns in Haslea, Gyrosigma and Pleurosigma is shown and discussed. C1 [Tiffany, Mary Ann] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Hinz, Friedel] Helmholtz Zentrum Polar & Meeresforsch, Alfred Wegener Inst, Friedrich Hustedt Zentrum Diatomeenforsch, D-27570 Bremerhaven, Germany. [Hargraves, Paul E.] Florida Atlantic Univ, Harbor Branch, Oceanog Inst, Ft Pierce, FL USA. [Hargraves, Paul E.] Smithsonian Inst, Marine Stn, Ft Pierce, FL USA. RP Sterrenburg, FAS (reprint author), Stn Sweg 158, Heiloo, Netherlands. EM fass@wxs.nl; mtiffany24@yahoo.com; Friedel.Hinz@awi.de; WEHerwig@arcor.de; Hargravespe@gmail.com NR 22 TC 3 Z9 3 U1 1 U2 4 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 MAY 8 PY 2015 VL 207 IS 2 BP 143 EP 162 PG 20 WC Plant Sciences SC Plant Sciences GA CI8AE UT WOS:000354988800001 ER PT J AU Fernandes, IO Souza, JLP Fernandez, CF Delabie, JHC Schultz, TR AF Fernandes, Itanna O. Souza, Jorge L. P. Fernando Fernandez, C. Delabie, Jacques H. C. Schultz, Ted R. TI A new species of Simopelta (Hymenoptera: Formicidae: Ponerinae) from Brazil and Costa Rica SO ZOOTAXA LA English DT Article DE blind ant; Rio Madeira; hydroelectric plant; cryptobiotic; Simopelta jeckylli AB The genus Simopelta consists of 21 described species restricted to Central America and South America. The present study describes a new cryptobiotic species, Simopelta anomma sp. nov.. The new species is blind, possesses a 3-segmented antennal club, and has the midtibia with several stout setae, a combination of characters unique within the genus. Moreover, some traits of this species require broadening the definition of the genus. The discovery of Simopelta anomma sp. nov. suggests that many undiscovered species, some of which may be important for understanding ant evolution, remain hidden below ground in Neotropical rainforests. C1 [Fernandes, Itanna O.; Souza, Jorge L. P.] INPA, CBio, BR-69011970 Manaus, AM, Brazil. [Fernandes, Itanna O.; Schultz, Ted R.] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomology, Washington, DC 20013 USA. [Souza, Jorge L. P.] Ctr Estudos Integrados Biodiversidade Amazoni CEN, BR-69080971 Manaus, AM, Brazil. [Fernando Fernandez, C.] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. [Delabie, Jacques H. C.] Univ Estadual Santa Cruz, Ctr Pesquisas Cacau CEPEC, CEPLAC, Lab Mirmecol, BR-45600000 Ilheus, BA, Brazil. RP Fernandes, IO (reprint author), INPA, CBio, Av Andre Araujo 2936,CP 2223, BR-69011970 Manaus, AM, Brazil. EM itanna.fernandes@gmail.com; FernandesI@si.edu RI Souza, Jorge/L-5154-2013 OI Souza, Jorge/0000-0003-4574-8111 FU INPA; Smithsonian Institution (NMNH); FAPEAM; CBio; Pro-equipamentos project CAPES/DCEN - MCT; Pronex program FAPESB-CNPq [PNX 011/2009]; Wildlife Conservation Program of Santo Antonio Energia; CAPES/CNPq/PDSE; CNPq; CNPq/FAPEAM; NSF; Smithsonian CGPS FX The first author (IOF) kindly acknowledges support from INPA, the Smithsonian Institution (NMNH), FAPEAM, CBio (for logistics), the Pro-equipamentos project CAPES / DCEN - MCT, and the Pronex program FAPESB-CNPq PNX 011/2009. We thank INPA for supporting the visit of the third author to INPA in Manaus. The authors acknowledge their grants from CAPES/CNPq/PDSE (IOF), CNPq (JHCD), CNPq/FAPEAM (JLPS), and NSF and the Smithsonian CGPS (TRS). The authors also thank to Dr. John T. Longino to encourage this publication and the anonymous reviewers. This study was supported by the Wildlife Conservation Program of Santo Antonio Energia, the company responsible for building and operating the SAE Hydroelectric Plant. The authors kindly acknowledge the help of Paulo V. Cruz with Photoshop, of Adriano H.C. Oliveira for help with fieldwork and sampling in Santo Antonio, and of Jeffrey Sosa-Calvo and Roberto F. Guerrero for valuable discussions and suggestions. NR 20 TC 1 Z9 1 U1 0 U2 7 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 MAY 8 PY 2015 VL 3956 IS 2 BP 295 EP 300 PG 6 WC Zoology SC Zoology GA CH9DG UT WOS:000354335600010 PM 26248921 ER PT J AU Christian, P Loeb, A AF Christian, Pierre Loeb, Abraham TI Probing the spacetime around supermassive black holes with ejected plasma blobs SO PHYSICAL REVIEW D LA English DT Article ID GALACTIC-CENTER; STELLAR ORBITS; A-ASTERISK; PULSARS; M87; JET; TELESCOPE; DISTANCE; BASE; MASS AB Millimeter-wavelength very-long-baseline-interferometry observations of the supermassive black holes in Sgr A* and M87 by the Event Horizon Telescope could potentially trace the dynamics of ejected plasma blobs in real time. We demonstrate that the trajectory and tidal stretching of these blobs can be used to test general relativity and set new constraints on the mass and spin of these black holes. C1 [Christian, Pierre; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Christian, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [AST-1312034] FX This work was supported in part by NSF Grant No. AST-1312034. NR 29 TC 4 Z9 4 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD MAY 8 PY 2015 VL 91 IS 10 AR 101301 DI 10.1103/PhysRevD.91.101301 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CH7YB UT WOS:000354251500001 ER PT J AU Fey, C Kurz, M Schmelcher, P Rittenhouse, ST Sadeghpour, HR AF Fey, C. Kurz, M. Schmelcher, P. Rittenhouse, S. T. Sadeghpour, H. R. TI A comparative analysis of binding in ultralong-range Rydberg molecules SO NEW JOURNAL OF PHYSICS LA English DT Article DE Rydberg molecules; permanent dipole moment; ultracold atoms and molecules; diagnonalization; regularization of delta function potential ID COLLISIONS; DIMERS; STATES; ATOMS AB We perform a comparative analysis of different computational approaches employed to explore the electronic structure of ultralong-range Rydberg molecules. Employing the Fermi pseudopotential approach, where the interaction is approximated by an s-wave bare delta function potential, one encounters a non-convergent behavior in basis set diagonalization. Nevertheless, the energy shifts within the first order perturbation theory coincide with those obtained by an alternative approach relying on Green's function calculation with the quantum defect theory. A pseudopotential that yields exactly the results obtained with the quantum defect theory, i.e. beyond first order perturbation theory, is the regularized delta function potential. The origin of the discrepancies between the different approaches is analytically explained. C1 [Fey, C.; Kurz, M.; Schmelcher, P.] Univ Hamburg, Zentrum Opt Quantentechnol, D-22761 Hamburg, Germany. [Schmelcher, P.] Hamburg Ctr Ultrafast Imaging, D-22761 Hamburg, Germany. [Rittenhouse, S. T.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Fey, C (reprint author), Univ Hamburg, Zentrum Opt Quantentechnol, Luruper Chaussee 149, D-22761 Hamburg, Germany. EM hrs@cfa.havard.edu RI Schmelcher, Peter/D-9592-2014 OI Schmelcher, Peter/0000-0002-2637-0937 FU Studienstiftung des deutschen Volkes FX The authors thank CH Greene and W Li for fruitful discussions. CF gratefully acknowledges a scholarship by the Studienstiftung des deutschen Volkes. NR 31 TC 5 Z9 5 U1 4 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD MAY 7 PY 2015 VL 17 AR 055010 DI 10.1088/1367-2630/17/5/055010 PG 6 WC Physics, Multidisciplinary SC Physics GA CJ1XE UT WOS:000355277600006 ER PT J AU Dutta, T Sharma, S Maldonado, JE Panwar, HS Seidensticker, J AF Dutta, Trishna Sharma, Sandeep Maldonado, Jesus E. Panwar, Hemendra Singh Seidensticker, John TI Genetic Variation, Structure, and Gene Flow in a Sloth Bear (Melursus ursinus) Meta-Population in the Satpura-Maikal Landscape of Central India SO PLOS ONE LA English DT Article ID COMPUTER-PROGRAM; MADHYA-PRADESH; BROWN BEARS; BLACK BEAR; INDIVIDUAL IDENTIFICATION; MULTILOCUS GENOTYPES; RECENT MIGRATION; PANTHERA-PARDUS; ERROR RATES; FRAGMENTATION AB Sloth bears (Melursus ursinus) are endemic to the Indian subcontinent. As a result of continued habitat loss and degradation over the past century, sloth bear populations have been in steady decline and now exist only in isolated or fragmented habitat across the entire range. We investigated the genetic connectivity of the sloth bear meta-population in five tiger reserves in the Satpura-Maikal landscape of central India. We used noninvasively collected fecal and hair samples to obtain genotypic information using a panel of seven polymorphic loci. Out of 194 field collected samples, we identified 55 individuals in this meta-population. We found that thismeta-population has moderate genetic variation, and is subdivided into two genetic clusters. Further, we identified five first-generationmigrants and signatures of contemporary gene flow. We found evidence of sloth bears in the corridor between the Kanha and Pench Tiger Reserves, and our results suggest that habitat connectivity and corridors play an important role inmaintaining gene flow in this meta-population. These corridors face several anthropogenic and infrastructure development threats that have the potential to sever ongoing gene flow, if policies to protect them are not put into action immediately. C1 [Dutta, Trishna; Sharma, Sandeep; Maldonado, Jesus E.; Seidensticker, John] Smithsonian Conservat Biol Inst, Washington, DC 20560 USA. [Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. [Panwar, Hemendra Singh] Peace Inst Charitable Trust, Delhi, India. RP Dutta, T (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20560 USA. EM trishnad@gmail.com FU International Bear Association (IBA); Smithsonian Conservation Biology Institute (SCBI); Friends of the National Zoo (FONZ); Kathryn Fuller Science for Nature Fund of the World Wildlife Fund (WWF) FX This project was funded by the International Bear Association (IBA), Smithsonian Conservation Biology Institute (SCBI), Friends of the National Zoo (FONZ), and Kathryn Fuller Science for Nature Fund of the World Wildlife Fund (WWF). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 72 TC 3 Z9 3 U1 2 U2 27 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 MAY 6 PY 2015 VL 10 IS 5 AR UNSP e0123384 DI 10.1371/journal.pone.0123384 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH5BQ UT WOS:000354049700013 PM 25945939 ER PT J AU Mettke-Hofmann, C Hamel, PB Hofmann, G Zenzal, TJ Pellegrini, A Malpass, J Garfinkel, M Schiff, N Greenberg, R AF Mettke-Hofmann, Claudia Hamel, Paul B. Hofmann, Gerhard Zenzal, Theodore J., Jr. Pellegrini, Anne Malpass, Jennifer Garfinkel, Megan Schiff, Nathan Greenberg, Russell TI Competition and Habitat Quality Influence Age and Sex Distribution in Wintering Rusty Blackbirds SO PLOS ONE LA English DT Article ID MISSISSIPPI ALLUVIAL VALLEY; IDEAL FREE DISTRIBUTION; MIGRATORY BIRD; BODY CONDITION; BOTTOMLAND HARDWOODS; NONBREEDING SEASON; RIPARIAN FORESTS; DIFFERENT WIDTHS; FOOD RESOURCES; CLIMATE-CHANGE AB Bird habitat quality is often inferred from species abundance measures during the breeding and non-breeding season and used for conservation management decisions. However, during the non-breeding season age and sex classes often occupy different habitats which suggest a need for more habitat-specific data. Rusty Blackbird (Euphagus carolinus) is a forested wetland specialist wintering in bottomland hardwood forests in the south-eastern U.S. and belongs to the most steeply declining songbirds in the U.S. Little information is available to support priority birds such as the Rusty Blackbird wintering in this threatened habitat. We assessed age and sex distribution and body condition of Rusty Blackbirds among the three major habitats used by this species in the Lower Mississippi Alluvial Valley and also measured food availability. Overall, pecan groves had the highest biomass mainly driven by the amount of nuts. Invertebrate biomass was highest in forests but contributed only a small percentage to overall biomass. Age and sex classes were unevenly distributed among habitats with adult males primarily occupying pecan groves containing the highest nut biomass, females being found in forests which had the lowest nut biomass and young males primarily staying in forest fragments along creeks which had intermediate nut biomass. Males were in better body condition than females and were in slightly better condition in pecan groves. The results suggest that adult males occupy the highest quality habitat and may competitively exclude the other age and sex classes. C1 [Mettke-Hofmann, Claudia] Liverpool John Moores Univ, Sch Nat Sci & Psychol, Liverpool L3 5UX, Merseyside, England. [Hamel, Paul B.; Schiff, Nathan] US Forest Serv, Stoneville, MS USA. [Hofmann, Gerhard] Tamar Grove, Moreton, Merseyside, England. [Zenzal, Theodore J., Jr.] Univ So Mississippi, Dept Biol Sci, Hattiesburg, MS 39406 USA. [Pellegrini, Anne] SWCA Environm Consultants, Flagstaff, AZ USA. [Malpass, Jennifer] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Garfinkel, Megan] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA. [Mettke-Hofmann, Claudia; Greenberg, Russell] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Mettke-Hofmann, C (reprint author), Liverpool John Moores Univ, Sch Nat Sci & Psychol, Liverpool L3 5UX, Merseyside, England. EM C.C.Mettke-Hofmann@ljmu.ac.uk FU U.S. Fish and Wildlife Service; Canadian Wildlife Service, Friends of the National Zoo, USA; Max Planck Institute for Ornithology, Andechs, Germany; German Ethological Society, Germany; Society for Tropical Ornithology, Germany; Arthur-von-Gwinner Foundation, Austria FX Assistants, travel and material were supported by the U.S. Fish and Wildlife Service (SMA grant, Quick Response Programme, Challenge Cost Share grant granted to the International Rusty Blackbird Technical Group). CM-H received support by the Canadian Wildlife Service, Friends of the National Zoo, USA, the Max Planck Institute for Ornithology, Andechs, Germany, the German Ethological Society, the Society for Tropical Ornithology, Germany, and the Arthur-von-Gwinner Foundation, Austria. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. SWCA Environmental Consultants provided support in the form of salaries for authors AP, but did not have any additional role in the study design, data collection and analysis, decision to publish, or preparation of the manuscript. The specific roles of these authors are articulated in the 'author contributions' section. NR 64 TC 2 Z9 2 U1 4 U2 18 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 MAY 6 PY 2015 VL 10 IS 5 AR e0123775 DI 10.1371/journal.pone.0123775 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH5BQ UT WOS:000354049700021 PM 25946335 ER PT J AU Winston, ME Herz, H AF Winston, Max E. Herz, Hubert TI Unpaved roads alter foraging patterns of the leafcutter ant Atta colombica SO STUDIES ON NEOTROPICAL FAUNA AND ENVIRONMENT LA English DT Article DE disturbance; human impact; optimal foraging; foraging trails; tropical moist forest ID LEAF-CUTTING ANTS; ATLANTIC FOREST; PLANT-SELECTION; CUTTER ANT; EDGE; HERBIVORY; COLONIES; CEPHALOTES; TRANSPORT; TRAILS AB Leaf cutting ants are dominant herbivores and influential ecosystem engineers in the Neotropics. It has been suggested that habitat disturbances alter the architecture of foraging trail systems for colonies in their vicinity; however, the evidence remains scarce. In this study we investigated the effect of unpaved roads dissecting tropical lowland forest habitat on the structure of leafcutter foraging trail systems and foraging effort. We mapped trail systems for 16 mature Atta colombica colonies located at different distances from unpaved roads. Our results suggest exploitation of unpaved roads by leafcutters provides favorable foraging conditions, causing significant differences in foraging trail structure. C1 [Winston, Max E.] Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. [Winston, Max E.] Field Museum Nat Hist, Dept Sci & Educ, Chicago, IL 60605 USA. [Winston, Max E.; Herz, Hubert] Smithsonian Trop Res Inst, Balboa, Panama. [Herz, Hubert] Univ Kaiserslautern, Dept Plant Ecol & Systemat, D-67663 Kaiserslautern, Germany. RP Winston, ME (reprint author), Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA. EM mewinsto@uchicago.edu FU Princeton Environmental Institute; Ecology and Evolutionary Biology Department at Princeton University; Secretaria Nacional de Ciencia y Technologia e Innovacionde la Republica de Panama (SENACYT) [COL 08-067] FX We thank the Princeton Environmental Institute and the Ecology and Evolutionary Biology Department at Princeton University for research funding for M.E.W. and the Secretaria Nacional de Ciencia y Technologia e Innovacionde la Republica de Panama (SENACYT) for a grant to H.H. [grant no. COL 08-067]. The Smithsonian Tropical Research Institute (STRI) provided logistic support, and thanks are due especially to J.S. Wright for his help. We thank S. Grossberg, P. Cowgill, B. Rubin and A. Olsen for programming tutorials, and helping us transform the data into the format necessary for spatial analyses. Lastly, we thank J. Mitchell and C. Moreau, advisor to M.E.W., for their comments on the manuscript. NR 36 TC 0 Z9 0 U1 6 U2 18 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0165-0521 EI 1744-5140 J9 STUD NEOTROP FAUNA E JI Stud. Neotrop. Fauna Environ. PD MAY 4 PY 2015 VL 50 IS 2 BP 57 EP 64 DI 10.1080/01650521.2015.1020702 PG 8 WC Zoology SC Zoology GA CO9JS UT WOS:000359492200001 ER PT J AU Valenzuela-Toro, AM Gutstein, CS Suarez, ME Otero, R Pyenson, ND AF Valenzuela-Toro, Ana M. Gutstein, Carolina S. Suarez, Mario E. Otero, Rodrigo Pyenson, Nicholas D. TI Elephant seal (Mirounga sp.) from the Pleistocene of the Antofagasta Region, northern Chile SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID SOUTH-AFRICA; FOSSIL CALIBRATIONS; MARINE MAMMALS; PACIFIC-OCEAN; LATE NEOGENE; ANCIENT DNA; EVOLUTION; BIOGEOGRAPHY; PHYLOGENY; CARNIVORA AB The genus Mirounga is the largest living member of the Phocidae family (true seals) and includes two species: M. angustirostris and M. leonina. These species exhibit a noticeable antitropical distribution in the Northern and Southern hemispheres, respectively. The evolutionary history of elephant seals, especially in regard to establishing this antitropical pattern, is poorly known. Nearly all fossils of the genus are isolated remains from the Pleistocene of California (M. angustirostris) and South Africa (M. leonina). Here, we describe new fossil material of Mirounga sp. (incomplete maxilla, dentary, and humerus), from the middle to late Pleistocene of Antofagasta Region, northern Chile. This material constitutes the first fossil occurrence of this species in South America and suggests that during part of the Pleistocene, phocids coexisted with otariids along the eastern edge of the South Pacific Ocean, which contrasts with the current biogeographic pattern in this ocean basin, providing new information about the structure of the pinniped community during the Pleistocene of South America. C1 [Valenzuela-Toro, Ana M.] Univ Chile, Fac Ciencias, Lab Ecofisiol, Santiago, Chile. [Valenzuela-Toro, Ana M.; Gutstein, Carolina S.; Suarez, Mario E.; Otero, Rodrigo] Univ Chile, Fac Ciencias, Dept Biol, Red Paleontol U Chile,Lab Ontogenia & Filogenia, Santiago, Chile. [Gutstein, Carolina S.; Pyenson, Nicholas D.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA. RP Valenzuela-Toro, AM (reprint author), Univ Chile, Fac Ciencias, Lab Ecofisiol, Las Palmeras 3425, Santiago, Chile. EM avalenzuela.toro@gmail.com; sgcarolina@gmail.com; marioesuarezp@gmail.com; paracrioceras@gmail.com; pyensonn@si.edu OI Gutstein, Carolina/0000-0002-0823-2434 FU CONICYT-PCHA/Magister Nacional [2013-221320410]; National Geographic Society Committee on Research Exploration [9391-13]; National Museum of Natural History Small Grant Award; NMNH Office of the Director; Smithsonian Institution's Remington Kellogg Fund; NGS CRE grant [8903-11]; U-REDES (Universidad de Chile) [Domeyko II UR-C12/1]; Sociedad GNL Mejillones FX A.V.T. was funded by CONICYT-PCHA/Magister Nacional/2013-221320410 and for Young Explorer Grant (9391-13) from National Geographic Society Committee on Research Exploration to A.V.T. Additional funding for this work comes from a National Museum of Natural History Small Grant Award, discretionary funding from NMNH Office of the Director, the Smithsonian Institution's Remington Kellogg Fund, a NGS CRE grant (8903-11) to N.D.P, and by U-REDES (Domeyko II UR-C12/1, Universidad de Chile) to the rest of the authors. Excavations were financed by Sociedad GNL Mejillones. We would like to thank C. Loch (University of Otago, Dunedin, New Zealand) for providing information about dentition of Elephant seals. We also thank S. Fuentes Tamblay (Museo Paleontologico de Caldera) and S. Soto Acuna (Museo Nacional de Historia Natural, Santiago, Chile) for the preparation and photography, respectively. Also, R. E. Yury-Yanez (Universidad de Chile) and D. Rubilar-Rogers (Museo Nacional de Historia Natural, Santiago, Chile) provided comments and suggestions that improved a preliminary version of the manuscript. We appreciate the useful and detailed comments from the editor Erich Fitzgerald, as well as those from R.W. Boessenecker and an anonymous reviewer, which substantially improved the manuscript. NR 85 TC 2 Z9 2 U1 3 U2 8 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD MAY 4 PY 2015 VL 35 IS 3 DI 10.1080/02724634.2014.918883 PG 7 WC Paleontology SC Paleontology GA CJ7MO UT WOS:000355679900012 ER PT J AU Vogl, AW Lillie, MA Piscitelli, MA Goldbogen, JA Pyenson, ND Shadwick, RE AF Vogl, A. Wayne Lillie, Margo A. Piscitelli, Marina A. Goldbogen, Jeremy A. Pyenson, Nicholas D. Shadwick, Robert E. TI Stretchy nerves are an essential component of the extreme feeding mechanism of rorqual whales SO CURRENT BIOLOGY LA English DT Letter ID PERIPHERAL-NERVE; FIN WHALES; EXTENSIBILITY; CONDUCTION; INJURY C1 [Vogl, A. Wayne] Univ British Columbia, Fac Med, Dept Cellular & Physiol Sci, Vancouver, BC V6T 1Z3, Canada. [Lillie, Margo A.; Piscitelli, Marina A.; Shadwick, Robert E.] Univ British Columbia, Fac Sci, Dept Zool, Vancouver, BC V6T 1Z4, Canada. [Goldbogen, Jeremy A.] Stanford Univ, Dept Biol, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. [Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Vogl, AW (reprint author), Univ British Columbia, Fac Med, Dept Cellular & Physiol Sci, Vancouver, BC V6T 1Z3, Canada. EM vogl@mail.ubc.ca NR 10 TC 6 Z9 6 U1 0 U2 12 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 MAY 4 PY 2015 VL 25 IS 9 BP R360 EP R361 PG 2 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA CH4JE UT WOS:000353999000007 PM 25942546 ER PT J AU Zhang, M Lee, TE Sadeghpour, HR AF Zhang, M. Lee, Tony E. Sadeghpour, H. R. TI Transport of quantum excitations via local and nonlocal fluctuations SO PHYSICAL REVIEW A LA English DT Article ID STOCHASTIC RESONANCE; PROPAGATION; DYNAMICS; SYSTEMS; ABSENCE AB In quantum systems, one usually seeks to minimize dephasing noise and disorder. The efficiency of transport in a quantum system is usually degraded by the presence of noise and disorder. However, it has been shown that the combination of the two can lead to significantly more efficiency than each by itself. Here, we consider how the addition of nonlocal noise, in the form of incoherent hopping, affects the transport efficiency. We show that incoherent hopping introduces additional local extrema in the efficiency function and investigate how the transport dynamics crosses over from a quantum random walk to a classical random walk. C1 [Zhang, M.; Lee, Tony E.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Zhang, M.] Beijing Normal Univ, Dept Phys, Beijing 100875, Peoples R China. [Lee, Tony E.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Zhang, M (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RI Zhang, Mei/F-1252-2015 OI Zhang, Mei/0000-0002-9728-9001 FU NSF; National Natural Science Foundation of China [11174040]; State Scholarship Fund of China FX This work was supported by the NSF through a grant to ITAMP. M.Z. is partially supported by National Natural Science Foundation of China under Grant No. 11174040 and also acknowledges the State Scholarship Fund of China for additional financial aid and ITAMP for generous hospitality. NR 18 TC 0 Z9 0 U1 2 U2 6 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 MAY 4 PY 2015 VL 91 IS 5 AR 052101 DI 10.1103/PhysRevA.91.052101 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CH1GC UT WOS:000353768200001 ER PT J AU Basset, Y AF Basset, Yves TI Long-term monitoring of tropical arthropods and DNA barcoding SO GENOME LA English DT Meeting Abstract C1 [Basset, Yves] Smithsonian Trop Res Inst, Panama City, Panama. EM bassety@si.edu RI Basset, Yves/B-6642-2014 NR 0 TC 0 Z9 0 U1 0 U2 0 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0831-2796 EI 1480-3321 J9 GENOME JI Genome PD MAY PY 2015 VL 58 IS 5 BP 193 EP 193 PG 1 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA CQ8MF UT WOS:000360861200031 ER PT J AU Garcia-Robledo, C Kress, WJ Erwin, TL AF Garcia-Robledo, Carlos Kress, W. John Erwin, Terry L. TI Reconstructing interactions among plants, insect herbivores, and phoretic mites using DNA barcodes: modeling SO GENOME LA English DT Meeting Abstract C1 [Garcia-Robledo, Carlos] Inst Ecol, Xalapa Enriquez 91070, Ver, Mexico. [Garcia-Robledo, Carlos; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Erwin, Terry L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. EM carlos.garcia@inecol.mx NR 0 TC 0 Z9 0 U1 3 U2 5 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0831-2796 EI 1480-3321 J9 GENOME JI Genome PD MAY PY 2015 VL 58 IS 5 BP 218 EP 218 PG 1 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA CQ8MF UT WOS:000360861200124 ER PT J AU Hausmann, A Miller, SE Prosser, S AF Hausmann, Axel Miller, Scott E. Prosser, Sean TI Calibrating the taxonomy of a megadiverse family on BOLD: 2700 geometrid moth types barcoded (Geometridae, Lepidoptera) SO GENOME LA English DT Meeting Abstract C1 [Hausmann, Axel] Bavarian State Collect Zool, D-81247 Munich, Germany. [Miller, Scott E.] Smithsonian Inst, Washington, DC 20013 USA. [Prosser, Sean] Univ Guelph, Biodivers Inst Ontario, Canadian Ctr DNA Barcoding, Guelph, ON N1G 2W1, Canada. EM Axel.Hausmann@zsm.mwn.de NR 0 TC 0 Z9 0 U1 3 U2 3 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0831-2796 EI 1480-3321 J9 GENOME JI Genome PD MAY PY 2015 VL 58 IS 5 BP 225 EP 225 PG 1 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA CQ8MF UT WOS:000360861200152 ER PT J AU Knowlton, N Leray, M AF Knowlton, Nancy Leray, Matthieu TI Censusing marine life in the 21st Century SO GENOME LA English DT Meeting Abstract C1 [Knowlton, Nancy; Leray, Matthieu] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM knowlton@si.edu NR 0 TC 0 Z9 0 U1 4 U2 10 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0831-2796 EI 1480-3321 J9 GENOME JI Genome PD MAY PY 2015 VL 58 IS 5 BP 238 EP 238 PG 1 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA CQ8MF UT WOS:000360861200201 ER PT J AU Kress, WJ Jones, FA Swenson, NG Erickson, DL AF Kress, W. John Jones, F. Andrew Swenson, Nathan G. Erickson, David L. TI Tracking evolutionary diversity and phylogenetic structure across global forest dynamics plots using plant DNA barcodes SO GENOME LA English DT Meeting Abstract C1 [Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Jones, F. Andrew] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Swenson, Nathan G.] Univ Maryland, Dept Plant Biol, College Pk, MD 20742 USA. [Erickson, David L.] US FDA, Beltsville, MD USA. EM kressj@si.edu NR 0 TC 0 Z9 0 U1 1 U2 4 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0831-2796 EI 1480-3321 J9 GENOME JI Genome PD MAY PY 2015 VL 58 IS 5 BP 239 EP 239 PG 1 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA CQ8MF UT WOS:000360861200205 ER PT J AU Moura, CJ Santos, RS Lessios, H Collins, A AF Moura, Carlos J. Santos, Ricardo S. Lessios, Harilaos Collins, Allen TI Large-scale DNA barcoding of marine hydroids of the superfamily Plumularioidea (Cnidaria: Hydrozoa) SO GENOME LA English DT Meeting Abstract C1 [Moura, Carlos J.; Santos, Ricardo S.] Univ Acores, Ctr IMAR, Univ Azores, IMAR MARE IMAR,Inst MAR, P-9901862 Horta, Portugal. [Moura, Carlos J.; Santos, Ricardo S.] NMNH Smithsonian Inst, Washington, DC USA. [Lessios, Harilaos] Smithsonian Trop Res Inst, Smithsonian Inst, Panama City Pl, Panama. [Collins, Allen] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. EM carlos.moura@mail.com RI Santos, Ricardo/B-3960-2008 OI Santos, Ricardo/0000-0002-2536-1369 NR 0 TC 0 Z9 0 U1 3 U2 4 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0831-2796 EI 1480-3321 J9 GENOME JI Genome PD MAY PY 2015 VL 58 IS 5 BP 259 EP 259 PG 1 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA CQ8MF UT WOS:000360861200278 ER PT J AU Prosser, S deWaard, J Miller, S Hebert, PDN AF Prosser, Sean deWaard, Jeremy Miller, Scott Hebert, Paul D. N. TI DNA barcodes from century-old type specimens using next-generation sequencing SO GENOME LA English DT Meeting Abstract C1 [Prosser, Sean; deWaard, Jeremy; Hebert, Paul D. N.] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Miller, Scott] Smithsonian Inst, Washington, DC 20560 USA. EM sprosser@uoguelph.ca RI Hebert, Paul/C-4161-2013; deWaard, Jeremy/G-8112-2014 OI Hebert, Paul/0000-0002-3081-6700; NR 0 TC 0 Z9 0 U1 0 U2 3 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0831-2796 EI 1480-3321 J9 GENOME JI Genome PD MAY PY 2015 VL 58 IS 5 BP 267 EP 268 PG 2 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA CQ8MF UT WOS:000360861200312 ER PT J AU Schindel, DE Trizna, MG AF Schindel, David E. Trizna, Michael G. TI The Barcode of Wildlife Project, Part 1: a systemic barcoding initiative to protect endangered species SO GENOME LA English DT Meeting Abstract C1 [Schindel, David E.; Trizna, Michael G.] Smithsonian Inst, Consortium Barcode Life, Washington, DC 20560 USA. EM schindeld@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0831-2796 EI 1480-3321 J9 GENOME JI Genome PD MAY PY 2015 VL 58 IS 5 BP 277 EP 277 PG 1 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA CQ8MF UT WOS:000360861200347 ER PT J AU Temeles, EJ AF Temeles, Ethan J. TI Bathing Beauty SO NATURAL HISTORY LA English DT Editorial Material C1 [Temeles, Ethan J.] Amherst Coll, Biol, Amherst, MA 01002 USA. [Temeles, Ethan J.] Amherst Coll, Dept Environm Studies, Amherst, MA 01002 USA. [Temeles, Ethan J.] Smithsonian Inst, Washington, DC 20560 USA. RP Temeles, EJ (reprint author), Amherst Coll, Biol, Amherst, MA 01002 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU NATURAL HISTORY MAGAZINE PI NEW YORK PA 36 WEST 25TH STREET, FIFTH FLOOR, NEW YORK, NY 10010 USA SN 0028-0712 J9 NAT HIST JI Nat. Hist. PD MAY PY 2015 VL 123 IS 4 BP 48 EP 48 PG 1 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CO1DN UT WOS:000358893200015 ER PT J AU Kurster, M Trifonov, T Reffert, S Kostogryz, NM Rodler, F AF Kuerster, Martin Trifonov, Trifon Reffert, Sabine Kostogryz, Nadiia M. Rodler, Florian TI Disentangling 2:1 resonant radial velocity orbits from eccentric ones and a case study for HD 27894 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE celestial mechanics; planetary systems; techniques: radial velocities; stars: individual: HD 27894 ID EXTRA-SOLAR PLANETS; COOL STARS; SYSTEMS; COMPANIONS; MIGRATION; PAIR AB Context. In radial velocity (RV) observations, a pair of extrasolar planets near a 2:1 orbital resonance can be misinterpreted as a single eccentric planet, if data are sparse and measurement precision insufficient to distinguish between these models. Aims. Using the Exoplanet Orbit Database (EOD), we determine the fraction of alleged single-planet RV detected systems for which a 2:1 resonant pair of planets is also a viable model and address the question of how the models can be disentangled. Methods. By simulation we quantified the mismatch arising from applying the wrong model. Model alternatives are illustrated using the supposed single-planet system HD 27894 for which we also study the dynamical stability of near-2:1 resonant solutions. Results. Using EOD values of the data scatter around the fitted single-planet Keplerians, we find that for 74% of the 254 putative single-planet systems, a 2:1 resonant pair cannot be excluded as a viable model, since the error due to the wrong model is smaller than the scatter. For 187 EOD stars chi(2)-probabilities can be used to reject the Keplerian models with a confidence of 95% for 54% of the stars and with 99.9% for 39% of the stars. For HD 27894 a considerable fit improvement is obtained when adding a low-mass planet near half the orbital period of the known Jovian planet. Dynamical analysis demonstrates that this system is stable when both planets are initially placed on circular orbits. For fully Keplerian orbits a stable system is only obtained if the eccentricity of the inner planet is constrained to <0.3. Conclusions. A large part of the allegedly RV detected single-planet systems should be scrutinized in order to determine the fraction of systems containing near-2:1 resonant pairs of planets. Knowing the abundance of such systems will allow us to revise the eccentricity distribution for extrasolar planets and provide direct constraints for planetary system formation. C1 [Kuerster, Martin; Rodler, Florian] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Trifonov, Trifon] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China. [Reffert, Sabine] Heidelberg Univ, Zentrum Astron, D-69117 Heidelberg, Germany. [Kostogryz, Nadiia M.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. [Kostogryz, Nadiia M.] NAS Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. [Rodler, Florian] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurster, M (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM kuerster@mpia-hd.mpg.de; trifonov@hku.hk; sreffert@lsw.uni-heidelberg.de; kostogryz@kis.uni-freiburg.de; flo@mpia.de FU European Research Council [ERC-2011-AdG 291659]; Alexander von Humboldt foundation FX We thank the anonymous referee for useful suggestions. N.M.K. ackowledges support by the European Research Council Advanced Grant HotMol (ERC-2011-AdG 291659). F.R. acknowledges financial support from the Alexander von Humboldt foundation. NR 34 TC 2 Z9 2 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 MAY PY 2015 VL 577 AR A103 DI 10.1051/0004-6361/201525872 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM0CN UT WOS:000357345900055 ER PT J AU Vlemmings, WHT Ramstedt, S O'Gorman, E Humphreys, EML Wittkowski, M Baudry, A Karovska, M AF Vlemmings, W. H. T. Ramstedt, S. O'Gorman, E. Humphreys, E. M. L. Wittkowski, M. Baudry, A. Karovska, M. TI Resolving the stellar activity of the Mira AB binary with ALMA SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: atmospheres; binaries: close; stars: individual: Mira AB ID O-CETI; INTERFEROMETRIC OBSERVATIONS; RADIO PHOTOSPHERES; VARIABLE-STARS; ATMOSPHERE; IMAGES; SYSTEM AB Aims. We present the size, shape, and flux densities at millimeter continuum wavelengths, based on ALMA science verification observations in Band 3 (similar to 94.6 GHz) and Band 6 (similar to 228.7 GHz), from the binary Mira A (o Ceti) and Mira B. Methods. The Mira AB system was observed with ALMA at a spatial resolution down to similar to 25 mas. The extended atmosphere of Mira A and the wind around Mira B sources were resolved, and we derived the sizes of Mira A and of the ionized region around Mira B. The spectral indices within Band 3 (between 89-100 GHz) and between Bands 3 and 6 were also derived. Results. The spectral index of Mira A is found to change from 1.71 +/- 0.05 within Band 3 to 1.54 +/- 0.04 between Bands 3 and 6. The spectral index of Mira B is 1.3 +/- 0.2 in Band 3, in good agreement with measurements at longer wavelengths; however, it rises to 1.72 +/- 0.11 between the bands. For the first time, the extended atmosphere of a star is resolved at these frequencies, and for Mira A the diameter is similar to 3.8 x 3.2 AU in Band 3 (with brightness temperature T-b similar to 5300 K) and similar to 4.0 x 3.6 AU in Band 6 (T-b similar to 2500 K). Additionally, a bright hotspot similar to 0.4 AU, with T-b similar to 10 000 K, is found on the stellar disk of Mira A. The size of the ionized region around the accretion disk of Mira B is found to be similar to 2.4 AU. Conclusions. The emission around Mira B is consistent with emission from a partially ionized wind of gravitationally bound material from Mira A close to the accretion disk of Mira B. The Mira A atmosphere does not fully match predictions with brightness temperatures in Band 3 significantly higher than expected, potentially owing to shock heating. The hotspot is very likely due to magnetic activity and could be related to the previously observed X-ray flare of Mira A. C1 [Vlemmings, W. H. T.; O'Gorman, E.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Ramstedt, S.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Humphreys, E. M. L.; Wittkowski, M.] ESO, D-85748 Garching, Germany. [Baudry, A.] Univ Bordeaux 1, LAB, UMR 5804, F-33270 Floirac, France. [Baudry, A.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Karovska, M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Vlemmings, WHT (reprint author), Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. EM wouter.vlemmings@chalmers.se OI /0000-0002-2700-9916; Wittkowski, Markus/0000-0002-7952-9550 FU Marie Curie Career Integration Grant [321691]; Swedish Research Council (VR); European Research Council through ERC consolidator grant [614264] FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00014.SV. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research is supported by Marie Curie Career Integration Grant 321691, the Swedish Research Council (VR), and the European Research Council through ERC consolidator grant 614264. NR 20 TC 8 Z9 8 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 MAY PY 2015 VL 577 AR L4 DI 10.1051/0004-6361/201526186 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM0CN UT WOS:000357345900105 ER PT J AU Ryabchikova, T Piskunov, N Kurucz, RL Stempels, HC Heiter, U Pakhomov, Y Barklem, PS AF Ryabchikova, T. Piskunov, N. Kurucz, R. L. Stempels, H. C. Heiter, U. Pakhomov, Yu Barklem, P. S. TI A major upgrade of the VALD database SO PHYSICA SCRIPTA LA English DT Article DE data bases; atomic and molecular data; astrophysics ID LINE-DATA-BASE; TRANSITION-PROBABILITIES; TIO; SPECTROSCOPY; SYSTEM AB Vienna atomic line database (VALD) is a collection of critically evaluated laboratory parameters for individual atomic transitions, complemented by theoretical calculations. VALD is actively used by astronomers for stellar spectroscopic studies-model atmosphere calculations, atmospheric parameter determinations, abundance analysis etc. The two first VALD releases contained parameters for atomic transitions only. In a major upgrade of VALD-VALD3, publically available from spring 2014, atomic data was complemented with parameters of molecular lines. The diatomic molecules C-2, CH, CN, CO, OH, MgH, SiH, TiO are now included. For each transition VALD provides species name, wavelength, energy, quantum number J and Lande-factor of the lower and upper levels, radiative, Stark and van der Waals damping factors and a full description of electronic configurarion and term information of both levels. Compared to the previous versions we have revised and verify all of the existing data and added new measurements and calculations for transitions in the range between 20 angstrom and 200 microns. All transitions were complemented with term designations in a consistent way and electron configurations when available. All data were checked for consistency: listed wavelength versus Ritz, selection rules etc. A new bibliographic system keeps track of literature references for each parameter in a given transition throughout the merging process so that every selected data entry can be traced to the original source. The query language and the extraction tools can now handle various units, vacuum and air wavelengths. In the upgrade process we had an intensive interaction with data producers, which was very helpful for improving the quality of the VALD content. C1 [Ryabchikova, T.; Pakhomov, Yu] Russian Acad Sci, Inst Astron, Moscow V71, Russia. [Piskunov, N.; Stempels, H. C.; Heiter, U.; Barklem, P. S.] Uppsala Univ, Dept Astron & Space Phys, Uppsala, Sweden. [Kurucz, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Ryabchikova, T (reprint author), Russian Acad Sci, Inst Astron, Moscow V71, Russia. EM ryabchik@inasan.ru RI Pakhomov, Yury/B-5172-2014 FU Basic Research Program of the Russian Academy of Sciences 'Non-stationary phenomena in the Universe'; EU FP7 infrastructure grant 'Virtual Atomic and Molecular Data Center'; 'Swedish Science Infrastructure Council (RFI)' 'VALD database' FX This work was supported by the Basic Research Program of the Russian Academy of Sciences 'Non-stationary phenomena in the Universe' (TR), the EU FP7 infrastructure grant 'Virtual Atomic and Molecular Data Center' and the 'Swedish Science Infrastructure Council (RFI)' 'VALD database' NR 24 TC 32 Z9 33 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0031-8949 EI 1402-4896 J9 PHYS SCRIPTA JI Phys. Scr. PD MAY PY 2015 VL 90 IS 5 AR 054005 DI 10.1088/0031-8949/90/5/054005 PG 4 WC Physics, Multidisciplinary SC Physics GA CK8OX UT WOS:000356498700006 ER PT J AU Diaz-Montilla, AE Gonzalez, R Solis, MA Saldamando-Benjumea, CI AF Diaz-Montilla, A. E. Gonzalez, Ranulfo Solis, M. Alma Saldamando-Benjumea, C. I. TI Evidence of Sexual Selection in Neoleucinodes elegantalis (Lepidoptera: Crambidae): Correlation of Female Moth Genitalia and Solanaceae Host Fruit Size SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE selection; biotype; genitalia; Solanaceae; fruit ID MECHANICAL REPRODUCTIVE ISOLATION; GENETIC DIFFERENTIATION; PLANT ASSOCIATION; COLOMBIA; BORER; MORPHOLOGY; SPECIATION; NOCTUIDAE; PARAGUAY; INSECTS AB Neoleucinodes elegantalis (Guenee) (Lepidoptera: Crambidae) is a major pest of fruits in the family Solanaceae in the Western Hemisphere. The objectives of this study were to determine whether life zone or host plant explained morphological variation in females, and if so, if there was evidence of sexual selection driving diversification in this species. We collected larvae feeding on cultivated (Capsicum annuum L., Solanum betaceum Cavanilles, Solanum lycopersicum Lamarck, Solanum melongena L., and Solanum quitoense Lamarck) and wild species (Solanum atropurpureum Schrank, Solanum acerifolium Dunal, Solanum crinitum Lamarck, and Solanum hirtum Vahl) of Solanceae in Colombia. The genitalia traits of 547 reared females were measured and correlations with host plant fruit size were estimated. Six female genitalia morphological characters, apophysis posterioris, apophysis anterioris, ostium bursae, ductus bursae length, corpus bursae, and the seventh abdominal segment were measured. Principal component analysis and cluster analysis classified individuals based on female morphological similarity and clustered them into four main groups according to host plant: 1) S. aceriflolium; 2) S. quitoense, S. lycopersicum, C. annuum and S. hirtum; 3) S. atroporpureum; 4) S. melongena, S. crinitum and S. betaceum. In this unique study, we found that variation in female genitalia size is directly correlated with the size of its host fruit, which suggests a mechanism for reproductive isolation and divergence of the four host races. Ours is one of the first studies that shows female genitalia morphology is correlated with species of host plants and represents a valuable contribution to the study of sexual selection in the evolution of insects. C1 [Diaz-Montilla, A. E.] Corp Colombiana Invest Agr CORPOICA, Ctr Invest Selva, Rionegro, Antioquia, Colombia. [Gonzalez, Ranulfo] Univ Valle, Dept Biol, Cali, Colombia. [Solis, M. Alma] USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Saldamando-Benjumea, C. I.] Univ Nacl Colombia Medellin, Dept Biociencias, Fac Ciencias, Medellin, Antioquia, Colombia. RP Diaz-Montilla, AE (reprint author), Corp Colombiana Invest Agr CORPOICA, Ctr Invest Selva, Rionegro, Antioquia, Colombia. EM anaelizabethd@gmail.com FU Ministerio de Agricultura y Desarrollo Rural de Colombia [PN25100033] FX Many thanks to Dr. Cesar Cardona (deceased) from Centro Internacional de Agricultura Tropical, International Center for Tropical Agriculture CIAT and to Dr. Argemiro Dominguez for statistics analysis. This project was funded by Ministerio de Agricultura y Desarrollo Rural de Colombia Project number PN25100033. NR 60 TC 2 Z9 2 U1 3 U2 10 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0013-8746 EI 1938-2901 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD MAY PY 2015 VL 108 IS 3 BP 272 EP 281 DI 10.1093/aesa/sav011 PG 10 WC Entomology SC Entomology GA CL6NQ UT WOS:000357084200008 ER PT J AU Jenner, FE Hauri, EH Bullock, ES Konig, S Arculus, RJ Mavrogenes, JA Mikkelson, N Goddard, C AF Jenner, Frances E. Hauri, Erik H. Bullock, Emma S. Koenig, Stephan Arculus, Richard J. Mavrogenes, John A. Mikkelson, Nicole Goddard, Charlotte TI The competing effects of sulfide saturation versus degassing on the behavior of the chalcophile elements during the differentiation of hydrous melts SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE sulfide; magma mixing; chalcophile; mid-ocean ridge basalt; convergent margin; degassing ID VALU-FA-RIDGE; HIGHLY SIDEROPHILE ELEMENTS; EASTERN MANUS BASIN; SOUTHERN LAU BASIN; BACK-ARC BASIN; OXIDATION-STATE; ORE-DEPOSITS; SUBDUCTION ZONE; OXYGEN FUGACITY; SILICATE MELTS AB There is a lack of consensus regarding the roles of sulfide saturation versus volatile degassing on the partitioning of Cu and Ag during differentiation and eruption of convergent margin magmas. Because of their oxidized character, volatile-rich magmas from the Eastern Manus Back-arc Basin (EMBB) only reach sulfide saturation following magnetite-driven reduction of the melt: the so-called magnetite crisis. If sulfide saturation typically precedes volatile saturation, the magnetite crisis will limit the proportion of Cu and Ag that can partition from the melt into an exsolving volatile-rich phase, which may contribute to the sporadic occurrence of magmatic-hydrothermal ore deposits at convergent margins. However, it is unclear whether the magnetite crisis is a common or rare event during differentiation of volatile-rich magmas. We report major and trace element data for submarine volcanic glasses from the Tonga arc-proximal Valu Fa Ridge (VFR; SW Pacific). Cu-Se-Ag systematics of samples erupting at the southern VFR suggest magnetite fractionation-triggered sulfide saturation. The similarity in chalcophile element systematics of the southern VFR and EMBB samples is unlikely to be coincidental, and may indicate that the magnetite crisis is a common event during differentiation of hydrous melts. However, unlike many convergent margin magmas, it is unlikely that the evolving VFR and EMBB were saturated in a S-bearing volatile phase prior to magnetite fractionation. Hence, the metal-depleting magnetite crisis may be restricted to back-arc basin magmas that do not degas volatiles prior to magnetite fractionation and potentially convergent margin magmas fractionating at high pressures in the continental crust. C1 [Jenner, Frances E.] Open Univ, Dept Environm Earth & Ecosyst, Milton Keynes MK7 6AA, Bucks, England. [Jenner, Frances E.; Hauri, Erik H.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Bullock, Emma S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Koenig, Stephan] Univ Tubingen, Isotopengeochem, Tubingen, Germany. [Arculus, Richard J.; Mavrogenes, John A.; Mikkelson, Nicole] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia. [Goddard, Charlotte] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. RP Jenner, FE (reprint author), Open Univ, Dept Environm Earth & Ecosyst, Milton Keynes MK7 6AA, Bucks, England. EM frances.jenner@open.ac.uk FU Australian Research Council; Deep Carbon Observatory; DTM FX Major and trace element data for samples from the VFR are presented in supporting information. We thank the officers, crew, and coscientific staff of the RV Southern Surveyor 02/2003 Tonga-Eastern Lau Vents Expedition for their effort in retrieving samples from the Valu Fa Ridge that were analyzed as part of this study. The postvoyage analytical costs for analyses undertaken at the RSES were supported by an Australian Research Council Discovery Grant to Richard Arculus and John Mavrogenes. Frances Jenner and Erik Hauri acknowledge funding from the Deep Carbon Observatory and the DTM for analyses undertaken at the DTM. We thank Jianhua Wang, Tim Mock, and Charlotte Allen for expert maintenance and assistance in the DTM SIMS lab and LA-ICPMS facility at the RSES, ANU, respectively. Ed Mathez, Sune Nielsen, and an anonymous reviewer are thanked for taking the time to review our manuscript and for their constructive criticism that improved the clarity of the text. Jannes Blichert-Toft is thanked for the editorial handing of our manuscript and constructive criticism throughout the submission process. NR 90 TC 4 Z9 4 U1 7 U2 26 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD MAY PY 2015 VL 16 IS 5 BP 1490 EP 1507 DI 10.1002/2014GC005670 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CL1NG UT WOS:000356710000015 ER PT J AU West, CF Jarvis, KN AF West, C. F. Jarvis, K. N. TI Osteometric Variation in Domestic Dogs (Canis familiaris) from the Kodiak Archipelago, Alaska SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE Alaska; domestic dog; Kodiak; North Pacific; osteometry; zooarchaeology ID SEXUAL DIMORPHISM; AGE CALIBRATION; BONE AB The research presented here is a re-examination of domestic dog (Canis familiaris) remains from the Uyak site on Kodiak Island, Alaska. Previous analyses suggest there were two breeds of dog represented in this archaeological assemblage, primarily on the basis of dog cranial size. Here, we use a series of metric and nonmetric traits to test the argument that these breeds' actually represent a population of male and female dogs. On the basis of the results presented here, we argue the metric and nonmetric data produced by this study suggest that the dogs in this sample are male and female specimens, rather than two distinct breeds. The Uyak assemblage is the largest collection of domestic dog from Kodiak, and these results have the potential to contribute to our understanding of human-dog relationships in the archipelago. Copyright (c) 2012 John Wiley & Sons, Ltd. C1 [West, C. F.] Univ Maine, Dept Anthropol, Orono Smithsonian Inst, Orono, ME 04469 USA. [West, C. F.] Univ Maine, Climate Change Inst, Orono Smithsonian Inst, Orono, ME 04469 USA. [Jarvis, K. N.] George Washington Univ, Dept Anthropol, Washington, DC USA. RP West, CF (reprint author), Univ Maine, Dept Anthropol, Orono, ME 04469 USA. EM catherine.west@umit.maine.edu FU Smithsonian Institution's Office of Fellowships; NMNH Program on Human Ecology and Archaeobiology FX Thanks first to the Alutiiq Museum and Archaeological Repository in Kodiak, Alaska, which has graciously acknowledged the value of further study of the Uyak collections. Thanks to Susan Crockford and Amy Steffian for advice and direction on this project. We acknowledge the Anthropology and Mammalogy Departments at the National Museum of Natural History, Smithsonian Institution, for permission to study the Uyak fauna, the Smithsonian Institution's Office of Fellowships for their financial support, and Torben Rick and Melinda Zeder in the NMNH Program on Human Ecology and Archaeobiology for their guidance. The accelerator mass spectrometry dates were provided by the National Ocean Sciences Accelerator Mass Spectrometry facility with funding from the NMNH Program on Human Ecology and Archaeobiology. NR 43 TC 1 Z9 1 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1047-482X EI 1099-1212 J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD MAY-JUN PY 2015 VL 25 IS 3 BP 289 EP 298 DI 10.1002/oa.2293 PG 10 WC Anthropology; Archaeology SC Anthropology; Archaeology GA CK7DU UT WOS:000356392300004 ER PT J AU France, CAM Owsley, DW AF France, C. A. M. Owsley, D. W. TI Stable Carbon and Oxygen Isotope Spacing Between Bone and Tooth Collagen and Hydroxyapatite in Human Archaeological Remains SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE bone; carbon isotopes; collagen; hydroxyapatite; human; oxygen isotopes; tooth ID NATURAL-ABUNDANCE DELTA-N-15; DIAGENETIC EVOLUTION; C-13/C-12 RATIOS; LA-BREA; NITROGEN; DIET; PHOSPHATE; APATITE; N-15; FRACTIONATION AB Spacing between stable isotope values in bones and teeth is a valuable tool for examining dietary influences and diagenesis. This study examines carbon and oxygen isotope values from collagen and hydroxyapatite (structural carbonate and phosphate) in archaeological human bones and teeth to derive species-specific correlation equations and isotope spacing values. The C-13(collagen) and C-13(structural) (carbonate) in bone and dentin collagen show a strong correlation (R = 0.87, 0.90, respectively) with an average C-13(carb-coll) spacing of 5.4 parts per thousand. The consistency of this isotope spacing with other large mammals and in humans with both low and high protein intake (as indicated by enriched N-15 values) suggests a similar allocation of protein-derived carbon and whole diet-derived carbon to collagen and structural carbonates, respectively, as other terrestrial mammals regardless of absolute meat intake. The O-18(structural carbonate) and O-18(phosphate) show the strongest correlation in enamel (R = 0.65), weaker correlations in dentin (R = 0.59) and bone (R = 0.35), with an average O-18(carb-phos) of 7.8 parts per thousand. This isotope spacing is slightly lower than previously reported for large mammals and limited available data for humans. The results potentially indicate species-specific fractionations and differing access to body water and blood-dissolved inorganic carbonates in the presence of collagen formation. The use of correlation between O-18(structural carbonate) and O-18(phosphate) to determine diagenetic state is not recommended. The strength of this correlation observed in bones and teeth is variable and alternate indicators of diagenetic state (i.e. C:N ratios of collagen) provide more robust and independent evidence of isotope preservation despite presence/absence of a strong isotope correlation. Published 2012. This article is a U.S. Government work and is in the public domain in the USA. C1 [France, C. A. M.] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. [Owsley, D. W.] Smithsonian Natl Museum Nat Hist, Washington, DC USA. RP France, CAM (reprint author), Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. EM francec@si.edu NR 78 TC 3 Z9 3 U1 4 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1047-482X EI 1099-1212 J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD MAY-JUN PY 2015 VL 25 IS 3 BP 299 EP 312 DI 10.1002/oa.2300 PG 14 WC Anthropology; Archaeology SC Anthropology; Archaeology GA CK7DU UT WOS:000356392300005 ER PT J AU Waters, LE Andrews, BJ Lange, RA AF Waters, Laura E. Andrews, Benjamin J. Lange, Rebecca A. TI Rapid Crystallization of Plagioclase Phenocrysts in Silicic Melts during Fluid-saturated Ascent: Phase Equilibrium and Decompression Experiments SO JOURNAL OF PETROLOGY LA English DT Article DE experimental petrology; rhyolite; plagioclase; water; equilibria ID MOUNT-ST-HELENS; DEGASSING-INDUCED CRYSTALLIZATION; MAGMA STORAGE-CONDITIONS; EXPERIMENTAL CONSTRAINTS; DRIVEN CRYSTALLIZATION; HILLS VOLCANO; KINETICS; GROWTH; DIFFUSION; RHYOLITE AB Three crystal-poor obsidian samples (one dacite, 67 wt % SiO2; two rhyolites, 73 and 75 wt % SiO2), which erupted effusively from monogenetic vents, contain sparse (<2%) plagioclase phenocrysts that span a remarkably wide and continuous range in composition (<= 30 mol % An). Many, but not all, of the plagioclase crystals display diffusion-limited growth textures (e.g. swallow-tails, skeletal, vermiform). Hypotheses to explain the paradox of a wide compositional range despite a low abundance of plagioclase include (1) incorporation of xenocrysts and/or magma mingling, (2) slow crystallization of plagioclase driven by slow cooling in a magma chamber, (3) slow crystallization of plagioclase followed by a resorption (e.g. heating) event, and (4) crystallization driven by rapid degassing (i.e. loss of melt H2O) +/- rapid cooling during ascent. To test these hypotheses, a series of phase equilibrium experiments were conducted under pure-H2O fluid-saturated conditions in a cold-seal pressure vessel between 30 and 300 MPa and 750 and 950 degrees C. The results show that the plagioclase population in each obsidian sample could have grown from their respective melts, with the exception of a single calcic core (An(60-63)) in one sample. The results additionally rule out slow cooling in a magma chamber, because this would lead to equilibrium abundances of plagioclase (<= 20%), which are far higher than what is observed in the samples (<2%). Nor can resorption (i.e. heating) explain the low abundance of plagioclase, because this would eliminate the more sodic plagioclase crystals and hence the wide compositional range of plagioclase that is observed. The most viable hypothesis is that the sparse plagioclase phenocrysts grew relatively rapidly during magma ascent to the surface; this is consistent with the results of isothermal (850 degrees C) continuous decompression experiments (2.9, 1.0, 0.8, and 0.1 MPa h(-1)), under pure-H2O fluid-saturated conditions, which were performed on one of the rhyolites (MLV-36; 73 wt % SiO2) and quenched at P-H2O = 89, 58 and 40 MPa. The four decompression rates correspond to degassing rates of 1.6, 0.56, 0.45 and 0.06 wt % H2O per day. Decompressions >= 1.0 MPa (P-H2O) h(-1), initiated above the liquidus, quenched to 100% glass at all final P-H2O. Decompressions at 0.8 MPa (P-H2O) h(-1), also initiated above the liquidus, led to plagioclase crystals nearly five times larger than those grown in runs decompressed at the same rate, but initiated just below the plagioclase-in curve. It is the kinetic hindrance to nucleation that permits crystal growth to be concentrated on relatively few crystals, leading to larger crystals. Plagioclase growth rates from these experiments show that the largest phenocrysts (similar to 1 mm) in the MLV-36 obsidian could have grown in <42 h. A cooling rate of similar to 1.2 degrees C h(-1) closely matches both the increase in melt viscosity with time and the effective undercooling with time that occurs during the 0.8 MPa(P-H2O) h(-1) decompression over the first 50 h. The combined results point to crystallization of sparse plagioclase driven by relatively rapid rates of degassing +/- cooling during ascent to the surface of melts that were initially above their liquidus. The obsidian samples must have been efficiently segregated as nearly 100% liquids from their respective source regions at H2O-fluid undersaturated conditions to attain a degree of superheating upon ascent before reaching fluid saturation. C1 [Waters, Laura E.; Lange, Rebecca A.] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA. [Andrews, Benjamin J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. RP Waters, LE (reprint author), Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA. EM lewaters@umich.edu FU National Science Foundation [EAR-12503685, EAR-9911352]; University of Michigan FX This experimental study was supported by the National Science Foundation (EAR-12503685 and EAR-9911352), along with discretionary funds from the University of Michigan. NR 43 TC 4 Z9 4 U1 6 U2 17 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-3530 EI 1460-2415 J9 J PETROL JI J. Petrol. PD MAY PY 2015 VL 56 IS 5 BP 981 EP 1006 DI 10.1093/petrology/egv025 PG 26 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CL1SD UT WOS:000356723700006 ER PT J AU Jiang, JC Bambi, C Steiner, JF AF Jiang, Jiachen Bambi, Cosimo Steiner, James F. TI Using iron line reverberation and spectroscopy to distinguish Kerr and non-Kerr black holes SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE modified gravity; astrophysical black holes; X-rays ID ACTIVE GALACTIC NUCLEI; X-RAY REFLECTION; RELATIVISTIC GRAVITATIONAL COLLAPSE; NONBARYONIC COMPACT OBJECT; K-ALPHA LINE; ACCRETION DISKS; NONSPHERICAL PERTURBATIONS; SPIN MEASUREMENTS; EVENT HORIZON; HAIR THEOREM AB The iron K alpha line commonly observed in the X-ray spectrum of both stellar-mass and supermassive black hole candidates is produced by the illumination of a cold accretion disk by a hot corona. In this framework, the activation of a new flaring region in the hot corona imprints a time variation on the iron line spectrum. Future X-ray facilities with high time resolution and large effective areas may be able to measure the so-called 2-dimensional transfer function; that is, the iron line profile detected by a distant observer as a function of time in response to an instantaneous flare from the X-ray primary source. This work is a preliminary study to determine if and how such a technique can provide more information about the spacetime geometry around the compact object than the already possible measurements of the time-integrated iron line profile. Within our simplified model, we find that a measurement of iron line reverberation can improve constraints appreciably given a sufficiently strong signal, though that most of the information is present in the time-integrated spectrum. Our aim is to test the Kerr metric. We find that current X-ray facilities and data are unable to provide strong tests of the Kerr nature of supermassive black hole candidates. We consider an optimistic case of 10(5) iron line photons from a next-generation data set. With such data, the reverberation model improves upon the spectral constraint by an order of magnitude. C1 [Jiang, Jiachen; Bambi, Cosimo] Fudan Univ, Ctr Field Theory & Particle Phys, Shanghai 200433, Peoples R China. [Jiang, Jiachen; Bambi, Cosimo] Fudan Univ, Dept Phys, Shanghai 200433, Peoples R China. [Steiner, James F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bambi, C (reprint author), Fudan Univ, Ctr Field Theory & Particle Phys, 220 Handan Rd, Shanghai 200433, Peoples R China. EM jcjiang12@fudan.edu.cn; bambi@fudan.edu.cn; jsteiner@cfa.harvard.edu FU NSFC [11305038]; Shanghai Municipal Education Commission grant for Innovative Programs [14ZZ001]; Thousand Young Talents Program; Fudan University; NASA Hubble Fellowship grant [HST-HF-51315.01] FX We would like to thank Gary Hinshaw for useful comments and suggestions. JJ and CB were supported by the NSFC grant No. 11305038, the Shanghai Municipal Education Commission grant for Innovative Programs No. 14ZZ001, the Thousand Young Talents Program, and Fudan University. JFS was supported by the NASA Hubble Fellowship grant HST-HF-51315.01. NR 97 TC 18 Z9 18 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD MAY PY 2015 IS 5 AR 025 DI 10.1088/1475-7516/2015/05/025 PG 27 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CJ9AN UT WOS:000355794800025 ER PT J AU Deutsch, JI AF Deutsch, James I. TI Zanis Lipke Memorial SO PUBLIC HISTORIAN LA English DT Art Exhibit Review C1 Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, JI (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD MAY PY 2015 VL 37 IS 2 BP 163 EP 167 PG 5 WC History SC History GA CJ8SJ UT WOS:000355773500026 ER PT J AU Bougeois, L Williams, B Halfar, J Konar, B Adey, W Kronz, A Wortmann, UG AF Bougeois, Laurie Williams, Branwen Halfar, Jochen Konar, Brenda Adey, Walter Kronz, Andreas Wortmann, Ulrich G. TI Does the coralline alga Leptophytum foecundum (Kjellman) capture paleoenvironmental variability in the Arctic Ocean? SO ARCTIC ANTARCTIC AND ALPINE RESEARCH LA English DT Article ID MG/CA RATIOS; BERING-SEA; RED ALGAE; RESOLUTION; TEMPERATURE; GROWTH; PROXY; CALIBRATION; RHODOPHYTA; ISLANDICA AB Records of high resolution climate variability in the past are essential to understanding the climate change observed today. This is particularly true for Arctic regions, which are rapidly warming. Prior to instrumental data, proxy records can be extracted from high-latitude climate archives to provide critical records of past Arctic climate variability. Here, we investigate the feasibility of extracting records of climate and environmental variability from the skeleton of the crustose coralline alga Leptophytum foecundum from offshore the Sagavanirktok River in the Beaufort Sea. Although this alga forms an annually banded skeleton, age chronologies were established with difficulty due to the large uncalcified reproductive structures relative to low annual growth rates. Average measurements of skeletal Mg content, delta O-18(alga) values, and delta C-13(alga) values were consistent among the analyzed specimens, but time series of these parameters only significantly correlated between two of the collected specimens for delta O-18(alga). No clear trends in environmental variability explained the patterns in the skeletal geochemistry over time. This suggests that ambient seawater combined with freshwater from the Sagavanirktok River drives the geochemistry of L. foecundum at this site. Thus, coralline algal specimens located near variable sources of low-salinity waters are not ideal organisms to use as proxy archives. C1 [Bougeois, Laurie; Williams, Branwen; Halfar, Jochen] Univ Toronto, Dept Chem & Phys Sci, Mississauga, ON L5L 1C6, Canada. [Bougeois, Laurie] Univ Rennes 1, CNRS, UMR 6118, Geosci Rennes, F-35000 Rennes, France. [Bougeois, Laurie] Univ Paris 06, CNRS, UMR 7193, Inst Sci Terre Paris, F-75005 Paris, France. [Konar, Brenda] Univ Alaska Fairbanks, Inst Marine Sci, Fairbanks, AK 99775 USA. [Adey, Walter] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Kronz, Andreas] Univ Gottingen, Geowissensch Zentrum, D-37077 Gottingen, Germany. [Wortmann, Ulrich G.] Univ Toronto, Dept Earth Sci, Toronto, ON M5S 3B1, Canada. RP Williams, B (reprint author), Scripps Coll, Pitzer Coll, Claremont Mckenna Coll, M Keck Sci Dept, 925 North Mills Ave, Claremont, CA 91711 USA. EM bwilliams@kecksci.claremont.edu FU Natural Science and Engineering Research Council (Canada) Discovery Grant FX Mathew Schellekens provided the data for Sag River. Hong Li assisted with the isotope analyses at the Geology Department at University of Toronto. Sophie Padie and Phoebe Chan provided assistance with data interpretation and statistical analyses. Analyses and visualizations of Beaufort Sea SST used in this paper were produced with the Giovanni online data system, developed and maintained by the U.S. National Aeronautics and Space Administration (NASA) Goddard Earth Sciences Data and Information Services Center (GES DISC). Funding was provided by a Natural Science and Engineering Research Council (Canada) Discovery Grant to Halfar. NR 70 TC 0 Z9 0 U1 1 U2 7 PU INST ARCTIC ALPINE RES PI BOULDER PA UNIV COLORADO, BOULDER, CO 80309 USA SN 1523-0430 EI 1938-4246 J9 ARCT ANTARCT ALP RES JI Arct. Antarct. Alp. Res. PD MAY PY 2015 VL 47 IS 2 BP 375 EP 387 DI 10.1657/AAAR0014-061 PG 13 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA CJ6TS UT WOS:000355627500018 ER PT J AU Tonra, CM Both, C Marra, PP AF Tonra, Christopher M. Both, Christiaan Marra, Peter P. TI Incorporating site and year-specific deuterium ratios (H-2) from precipitation into geographic assignments of a migratory bird SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID STABLE-ISOTOPES; LONG-TERM; CONNECTIVITY; HYDROGEN; ORIGIN; TRACKING; GEOLOCATORS; DELTA-H-2; FEATHERS; SONGBIRD AB The study of migratory connectivity is rapidly growing in ornithology, as is the technology used to measure it. While use of extrinsic markers, such as archival tags, is becoming more prevalent, for many small species the best tool available for tracking birds remains intrinsic markers, such as stable-hydrogen isotope ratios (H-2). Many researchers have raised concerns that spatial and temporal environmental variation introduces a large amount of error into isotope-based assignments, limiting their utility. Here, using feathers, we sought to address these issues in developing H-2 base maps for assigning pied flycatchers Ficedula hypoleuca of known origin to 15 sites across the breeding range (approx. 4 020 800 km(2)). We evaluated the effects of including random site variation and year-specific precipitation H-2 (H-2(P)) maps on assignments, compared to using mean annual growing season H-2(p) and no site effects. We found a positive correlation between feather H-2 (H-2(F)) and mean annual H-2(P,) resulting from large scale geographic variation. Repeatability of feather H-2 for individuals sampled in multiple years was strong overall, but variable among populations. Annual variation in H-2(P) explained 21% of within individual variation in H-2(F). Neither year- nor site-specific methods improved assignment precision or accuracy. All three methods assigned flycatchers of unknown origin captured at an African overwintering site to similar breeding areas. However, methods using long-term means of H-2(p) assigned birds more precisely than year-specific methods. Our results suggest that annual variation in this system is primarily a result of food web or individual level processes and that random site effects are not strong enough to drastically impact accuracy. We conclude that improvements in isotope based geographic assignments will rely on the addition of prior information, such as relative abundance in a Bayesian framework, or additional intrinsic markers. C1 [Tonra, Christopher M.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC 20013 USA. [Tonra, Christopher M.; Marra, Peter P.] Ohio State Univ, Terr Wildlife Ecol Lab, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Both, Christiaan] Univ Groningen, Anim Ecol Grp, Ctr Ecol & Evolutionary Studies, Groningen, Netherlands. RP Tonra, CM (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC 20013 USA. EM tonra.1@osu.edu RI Tonra, Christopher/B-1620-2013; Both, Christiaan/E-6459-2011 FU Smithsonian Post-doctoral Fellowship; VIDI-grant of the Dutch Research Council (NWO) FX We wish to thank the numerous biologists and projects who contributed feathers for this study Alexandr Artemyev, Antero Jarvinen, Erik Nyholm, Eugen Belskii, Helen Lampe, Herwig Zang, Indrik Krams, Jaime Potti, Malcolm Burgess, Paivi Sirkia, Pierre-Alain Ravussin, Raivo Mand, Stanislav Bures, Toni Laaksonen, Vladimir Grinkov, Wolfgang Winkel. This work was partially supported by a Smithsonian Post-doctoral Fellowship awarded to CMT and a VIDI-grant of the Dutch Research Council (NWO) to CB. For assistance in the laboratory we thank Leah Culp, Nora Diggs, and Christine France. Clark Rushing, Michael Hallworth, and Colin Studds provided valuable input on analysis and comments on an earlier version of this manuscript. NR 41 TC 1 Z9 1 U1 4 U2 22 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0908-8857 EI 1600-048X J9 J AVIAN BIOL JI J. Avian Biol. PD MAY PY 2015 VL 46 IS 3 BP 266 EP 274 DI 10.1111/jav.00553 PG 9 WC Ornithology SC Zoology GA CJ6RX UT WOS:000355622400005 ER PT J AU Rodriguez-Gomez, V Genel, S Vogelsberger, M Sijacki, D Pillepich, A Sales, LV Torrey, P Snyder, G Nelson, D Springel, V Ma, CP Hernquist, L AF Rodriguez-Gomez, Vicente Genel, Shy Vogelsberger, Mark Sijacki, Debora Pillepich, Annalisa Sales, Laura V. Torrey, Paul Snyder, Greg Nelson, Dylan Springel, Volker Ma, Chung-Pei Hernquist, Lars TI The merger rate of galaxies in the Illustris simulation: a comparison with observations and semi-empirical models SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: interactions; cosmology: theory ID SIMILAR-TO 1; DARK-MATTER HALOES; SMOOTHED PARTICLE HYDRODYNAMICS; GOODS NICMOS SURVEY; MASSIVE GALAXIES; MOVING MESH; LAMBDA-CDM; ENVIRONMENTAL DEPENDENCE; COSMOLOGICAL SIMULATIONS; SEMIANALYTIC MODEL AB We have constructed merger trees for galaxies in the Illustris simulation by directly tracking the baryonic content of subhaloes. These merger trees are used to calculate the galaxy-galaxy merger rate as a function of descendant stellar mass, progenitor stellar mass ratio, and redshift. We demonstrate that the most appropriate definition for the mass ratio of a galaxy-galaxy merger consists in taking both progenitor masses at the time when the secondary progenitor reaches its maximum stellar mass. Additionally, we avoid effects from 'orphaned' galaxies by allowing some objects to 'skip' a snapshot when finding a descendant, and by only considering mergers which show a well-defined 'infall' moment. Adopting these definitions, we obtain well-converged predictions for the galaxy-galaxy merger rate with the following main features, which are qualitatively similar to the halo-halo merger rate except for the last one: a strong correlation with redshift that evolves as similar to(1 + z)(2.4-2.8), a power law with respect to mass ratio, and an increasing dependence on descendant stellar mass, which steepens significantly for descendant stellar masses greater than similar to 2 x 10(11) M-circle dot. These trends are consistent with observational constraints for medium-sized galaxies (M-* greater than or similar to 10(10) M-circle dot), but in tension with some recent observations of the close pair fraction for massive galaxies (M-* greater than or similar to 10(11) M-circle dot), which report a nearly constant or decreasing evolution with redshift. Finally, we provide a fitting function for the galaxy-galaxy merger rate which is accurate over a wide range of stellar masses, progenitor mass ratios, and redshifts. C1 [Rodriguez-Gomez, Vicente; Genel, Shy; Pillepich, Annalisa; Sales, Laura V.; Nelson, Dylan; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Genel, Shy] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Vogelsberger, Mark; Torrey, Paul] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Sijacki, Debora] Kavli Inst Cosmol, Cambridge, England. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sales, Laura V.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Torrey, Paul] CALTECH, TAPIR, Pasadena, CA 91125 USA. [Snyder, Greg] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany. [Ma, Chung-Pei] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Rodriguez-Gomez, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vrodriguez-gomez@cfa.harvard.edu OI Torrey, Paul/0000-0002-5653-0786; Rodriguez-Gomez, Vicente/0000-0002-9495-0079 FU European Research Council through ERC-StG grant [EXAGAL-308037]; NASA [NNX12AC67G]; NSF [AST-1312095] FX We are grateful to Asa Bluck, Gurtina Besla, Sarah Wellons, and Joshua Suresh for useful comments and discussions. We also thank Laura Blecha for carefully reading the manuscript. VS acknowledges support by the European Research Council through ERC-StG grant EXAGAL-308037. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. NR 69 TC 34 Z9 34 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 MAY 1 PY 2015 VL 449 IS 1 BP 49 EP 64 DI 10.1093/mnras/stv264 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2WO UT WOS:000355345600005 ER PT J AU Price, DC Smirnov, OM AF Price, D. C. Smirnov, O. M. TI Generalized formalisms of the radio interferometer measurement equation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: interferometric; techniques: polarimetric ID FLUX-DENSITY SCALE; STOKES PARAMETERS; SELF-CALIBRATION; POLARIMETRY; MATRIX AB The radio interferometer measurement equation (RIME) is a matrix-based mathematical model that describes the response of a radio interferometer. The Jones calculus it employs is not suitable for describing the analogue components of a telescope. This is because it does not consider the effect of impedance mismatches between components. This paper aims to highlight the limitations of Jones calculus, and suggests some alternative methods that are more applicable. We reformulate the RIME with a different basis that includes magnetic and mixed coherency statistics. We present a microwave network inspired 2N-port version of the RIME, and a tensor formalism based upon the electromagnetic tensor from special relativity. We elucidate the limitations of the Jones-matrix-based RIME for describing analogue components. We show how measured scattering parameters of analogue components can be used in a 2N-port version of the RIME. In addition, we show how motion at relativistic speed affects the observed flux. We present reformulations of the RIME that correctly account for magnetic field coherency. These reformulations extend the standard formulation, highlight its limitations, and may have applications in space-based interferometry and precise absolute calibration experiments. C1 [Price, D. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01243 USA. [Smirnov, O. M.] Rhodes Univ, Det Phys & Elect, ZA-6140 Grahamstown, South Africa. [Smirnov, O. M.] SKA South Africa, ZA-7405 Pinelands, South Africa. RP Price, DC (reprint author), Harvard Smithsonian Ctr Astrophys, MS42,60 Garden St, Cambridge, MA 01243 USA. EM dprice@cfa.harvard.edu FU South African Research Chairs Initiative of the Department of Science and Technology; National Research Foundation; NSF [AST-1106054, AST-1106059, AST-1106045, AST-1105949] FX We would like to thank Stef Salvini, Ian Heywood, and Mike Jones for their comments, Tobias Carozzi for his valuable insight, and the late Steve Rawlings for his advice in the seminal stages of this paper. OMS's research is supported by the South African Research Chairs Initiative of the Department of Science and Technology and National Research Foundation. This work has made use of LWA1 outrigger dipoles made available by the LEDA project, funded by NSF under grants AST-1106054, AST-1106059, AST-1106045, and AST-1105949. NR 34 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2015 VL 449 IS 1 BP 107 EP 118 DI 10.1093/mnras/stv137 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2WO UT WOS:000355345600010 ER PT J AU Wellons, S Torrey, P Ma, CP Rodriguez-Gomez, V Vogelsberger, M Kriek, M van Dokkum, P Nelson, E Genel, S Pillepich, A Springel, V Sijacki, D Snyder, G Nelson, D Sales, L Hernquist, L AF Wellons, Sarah Torrey, Paul Ma, Chung-Pei Rodriguez-Gomez, Vicente Vogelsberger, Mark Kriek, Mariska van Dokkum, Pieter Nelson, Erica Genel, Shy Pillepich, Annalisa Springel, Volker Sijacki, Debora Snyder, Gregory Nelson, Dylan Sales, Laura Hernquist, Lars TI The formation of massive, compact galaxies at z=2 in the Illustris simulation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; galaxies: high-redshift ID SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; INSIDE-OUT GROWTH; FIELD CAMERA 3; QUIESCENT GALAXIES; SIZE EVOLUTION; STAR-FORMATION; MOVING-MESH; COSMOLOGICAL SIMULATIONS; EXTRA LIGHT AB Massive, quiescent galaxies at high redshift have been found to be considerably more compact than galaxies of similar mass in the local universe. How these compact galaxies formed has yet to be determined, though several progenitor populations have been proposed. Here we investigate the formation processes and quantify the assembly histories of such galaxies in Illustris, a suite of hydrodynamical cosmological simulations encompassing a sufficiently large volume to include rare objects, while simultaneously resolving the internal structure of galaxies. We select massive (similar to 10(11) M-circle dot) and compact (stellar half-mass radius <2 kpc) galaxies from the simulation at z = 2. Within the Illustris suite, we find that these quantities are not perfectly converged, but are reasonably reliable for our purposes. The resulting population is composed primarily of quiescent galaxies, but we also find several star-forming compact galaxies. The simulated compact galaxies are similar to observed galaxies in star formation activity and appearance. We follow their evolution at high redshift in the simulation and find that there are multiple pathways to form these compact galaxies, dominated by two mechanisms: (i) intense, centrally concentrated starbursts generally triggered by gas-rich major mergers between z similar to 2-4, reducing the galaxies' half-mass radii by a factor of a few to below 2 kpc, and (ii) assembly at very early times when the universe was much denser; the galaxies formed compact and remained so until z similar to 2. C1 [Wellons, Sarah; Rodriguez-Gomez, Vicente; Genel, Shy; Pillepich, Annalisa; Nelson, Dylan; Sales, Laura; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Torrey, Paul; Vogelsberger, Mark] MIT, Cambridge, MA 02139 USA. [Torrey, Paul] CALTECH, TAPIR, Pasadena, CA 91125 USA. [Ma, Chung-Pei; Kriek, Mariska] Univ Calif Berkeley, Berkeley, CA 94720 USA. [van Dokkum, Pieter; Nelson, Erica] Yale Univ, New Haven, CT 06511 USA. [Genel, Shy] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, ARI, Zentrum Astron, D-69120 Heidelberg, Germany. [Sijacki, Debora] Kavli Inst Cosmol, Cambridge, England. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Snyder, Gregory] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Wellons, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM swellons@cfa.harvard.edu OI Torrey, Paul/0000-0002-5653-0786; Rodriguez-Gomez, Vicente/0000-0002-9495-0079 FU National Science Foundation [DGE1144152]; NASA [NNX12AC67G]; NSF [AST-1312095] FX SW is supported by the National Science Foundation Graduate Research Fellowship under grant number DGE1144152. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. We thank Pascal Oesch for helpful discussions and guidance on generating the mock observations presented in this paper. NR 83 TC 39 Z9 39 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 MAY 1 PY 2015 VL 449 IS 1 BP 361 EP 372 DI 10.1093/mnras/stv303 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2WO UT WOS:000355345600026 ER PT J AU Gafton, E Tejeda, E Guillochon, J Korobkin, O Rosswog, S AF Gafton, E. Tejeda, E. Guillochon, J. Korobkin, O. Rosswog, S. TI Relativistic effects on tidal disruption kicks of solitary stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; hydrodynamics; relativistic processes; methods: numerical; galaxies: nuclei ID MASSIVE BLACK-HOLE; HYPERVELOCITY STAR; GALACTIC-CENTER; ECCENTRIC ORBITS; BINARIES; EVOLUTION; NUCLEI; GALAXY; RATES AB Solitary stars that wander too close to their galactic centres can become tidally disrupted, if the tidal forces due to the supermassive black hole residing there overcome the self-gravity of the star. If the star is only partially disrupted, so that a fraction survives as a self-bound object, this remaining core will experience a net gain in specific orbital energy, which translates into a velocity 'kick' of up to similar to 10(3) km s(-1). In this paper, we present the result of smoothed particle hydrodynamics simulations of such partial disruptions, and analyse the velocity kick imparted on the surviving core. We compare gamma = 5/3 and gamma = 4/3 polytropes disrupted in both a Newtonian potential, and a generalized potential that reproduces most relativistic effects around a Schwarzschild black hole either exactly or to excellent precision. For the Newtonian case, we confirm the results of previous studies that the kick velocity of the surviving core is virtually independent of the ratio of the black hole to stellar mass, and is a function of the impact parameter beta alone, reaching at most the escape velocity of the original star. For a given beta, relativistic effects become increasingly important for larger black holemasses. In particular, we find that the kick velocity increases with the black hole mass, making larger kicks more common than in the Newtonian case, as low-beta encounters are statistically more likely than high-beta encounters. The analysis of the tidal tensor for the generalized potential shows that our results are robust lower limits on the true relativistic kick velocities, and are generally in very good agreement with the exact results. C1 [Gafton, E.; Tejeda, E.; Korobkin, O.; Rosswog, S.] Stockholm Univ, AlbaNova, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Guillochon, J.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Gafton, E (reprint author), Stockholm Univ, AlbaNova, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. EM emanuel.gafton@astro.su.se OI Gafton, Emanuel/0000-0003-0781-6638; Guillochon, James/0000-0002-9809-8215; Korobkin, Oleg/0000-0003-4156-5342 FU Swedish Research Council (VR) [621-2012-4870] FX The simulations of this paper were in part performed on the facilities of the Hochstleistungsrechenzentrum Nord (HLRN) in Hannover, and at the PDC Centre for High Performance Computing (PDC-HPC) in Stockholm. We thank John Miller for the careful reading of the manuscript, and we acknowledge useful discussions on the topic of the paper with Enrico Ramirez-Ruiz. In addition, we thank the referee, Tamara Bogdanovic, for insightful comments and very helpful suggestions. The work of SR has been supported by the Swedish Research Council (VR) under grant 621-2012-4870. NR 34 TC 3 Z9 3 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 MAY 1 PY 2015 VL 449 IS 1 BP 771 EP 780 DI 10.1093/mnras/stv350 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2WO UT WOS:000355345600056 ER PT J AU Najera, F Brown, J Wildt, DE Virolle, L Kongprom, U Revuelta, L Goodrowe-Beck, K AF Najera, Fernando Brown, Janine Wildt, David E. Virolle, Laurie Kongprom, Urarikha Revuelta, Luis Goodrowe-Beck, Karen TI Body mass dynamics in hand reared clouded leopard (Neofelis nebulosa) cubs from birth to weaning SO ZOO BIOLOGY LA English DT Article DE clouded leopard; growth rate; hand rearing; Neofelis nebulosa ID LITTER SIZE; KITTENS AB To study the dynamics of body mass changes in hand reared clouded leopards, we analyzed 3,697 weight data points during the first 3 months of life in 49 cubs from 24 zoo-born litters from 2003 through 2012. All cubs were fed the same formula mixture after a similar weaning protocol. The hand rearing process was divided into three periods based on feeding protocols: Stage 1: formula only (Days 1-28; Day 0=day of birth); Stage 2, formula supplemented with protein (e.g., turkey baby food; Days 29-42); Stage 3, formula in decreasing amounts supplemented with meat (chicken and/or beef; Days 43-90). Weights at birth were 11.2% higher (P<0.001) for males (n=29) than females (n=20). Daily weight gain was slowest (P<0.05) during Stage 1 when cubs were fed straight formula only and fastest during Stage 3 when provided a mixture of formula and meat. Mean growth rate (+/- SD) during hand rearing differed (P<0.05) by gender, being 34.6 +/- 1.4g/day for male and 30.0 +/- 1.2g/day for female cubs. Eighteen cubs (37%) exhibited mild to severe diarrhea during the study; however, palliative treatment resulted in similar (P>0.05) growth and weaning weights compared to healthy counterparts. These are the first data documenting, on a large scale, the growth patterns for zoo born, hand reared clouded leopard cubs. Findings are valuable as an aid in managing this rare species, including for helping identify early onset of medical issues and further determining key factors regulating the first 3 months of development. Zoo Biol. 34:239-243, 2015. (c) 2015 Wiley Periodicals Inc. C1 [Najera, Fernando; Kongprom, Urarikha] Khao Kheow Open Zoo, Sriracha, Chonburi, Thailand. [Najera, Fernando; Revuelta, Luis] Univ Complutense Madrid, Vet Coll, E-28040 Madrid, Spain. [Brown, Janine; Wildt, David E.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA USA. [Virolle, Laurie] Alfort Natl Vet Sch, Maisons Alfort, France. [Goodrowe-Beck, Karen] Point Defiance Zoo & Aquarium, Tacoma, WA USA. RP Najera, F (reprint author), Univ Complutense Madrid, Fac Vet Med, Avda Ciudad Uni S-N, E-28040 Madrid, Spain. EM fernanaj@ucm.es RI Revuelta, Luis/F-8764-2011 OI Revuelta, Luis/0000-0002-4935-3013 NR 24 TC 0 Z9 0 U1 4 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 EI 1098-2361 J9 ZOO BIOL JI Zoo Biol. PD MAY-JUN PY 2015 VL 34 IS 3 BP 239 EP 243 DI 10.1002/zoo.21206 PG 5 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA CK0FF UT WOS:000355880200006 PM 25716685 ER PT J AU Augustine, L Watkins, B AF Augustine, Lauren Watkins, Barbara TI Age, fertility and reproductive behavior in cuban crocodiles, Crocodylus rhombifer, at the smithsonian's national zoological park SO ZOO BIOLOGY LA English DT Article ID AMERICAN CROCODILE; NESTING ECOLOGY; ALLIGATOR-MISSISSIPPIENSIS; ENVIRONMENTAL ENRICHMENT; TEMPERATURE; REPTILES; BIOLOGY; SUCCESS; BELIZE AB The Smithsonian's National Zoological Park (NZP) has a long history with Cuban crocodiles, Crocodylus rhombifer, beginning in 1900's when the first animals arrived at the NZP. Today, the Zoo has two breeding groups of C. rhombifer and has observed and analyzed reproductive behavior and fertility rates over the last three years. Fertility rates were determined initially by observing the formation of an opaque band that forms on the shell of a fertile egg, called banding. The fertility rates by banding were later compared to the observation made after opening the eggs to verify fertility. In addition to tracking fertility, nesting and agonistic behavior were also observed. Several notable observations were documented over the same period. These included a male predating a nesting female's eggs, increased aggression between two females housed together, the continued development of a partially banded egg, and the discovery of 19 additional egg shells post oviposition by both females in the enclosure. Here we discuss the nest phenology, fertility and behavior of the five exhibited C. rhombifer at the Smithsonian's National Zoological Park over a 3-year period. Zoo Biol. 34:278-284, 2015. (c) 2015 Wiley Periodicals Inc. C1 [Augustine, Lauren; Watkins, Barbara] Smithsonian Natl Zool Pk, Washington, DC 20008 USA. RP Augustine, L (reprint author), Smithsonian Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM Augustinel@si.edu NR 45 TC 0 Z9 0 U1 6 U2 28 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 EI 1098-2361 J9 ZOO BIOL JI Zoo Biol. PD MAY-JUN PY 2015 VL 34 IS 3 BP 278 EP 284 DI 10.1002/zoo.21204 PG 7 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA CK0FF UT WOS:000355880200011 PM 25716550 ER PT J AU Bykov, AM Churazov, EM Ferrari, C Forman, WR Kaastra, JS Klein, U Markevitch, M de Plaa, J AF Bykov, A. M. Churazov, E. M. Ferrari, C. Forman, W. R. Kaastra, J. S. Klein, U. Markevitch, M. de Plaa, J. TI Structures and Components in Galaxy Clusters: Observations and Models SO SPACE SCIENCE REVIEWS LA English DT Review DE Clusters of galaxies; Radiation mechanisms: non-thermal; Radio continuum; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; DIFFUSIVE SHOCK ACCELERATION; X-RAY-LINES; MAGNETIC-FIELD AMPLIFICATION; XMM-NEWTON OBSERVATIONS; MASSIVE BLACK-HOLES; COOLING FLOWS; PERSEUS CLUSTER; RESONANT SCATTERING; ELLIPTIC GALAXIES AB Clusters of galaxies are the largest gravitationally bounded structures in the Universe dominated by dark matter. We review the observational appearance and physical models of plasma structures in clusters of galaxies. Bubbles of relativistic plasma which are inflated by supermassive black holes of AGNs, cooling and heating of the gas, large scale plasma shocks, cold fronts, non-thermal halos and relics are observed in clusters. These constituents are reflecting both the formation history and the dynamical properties of clusters of galaxies. We discuss X-ray spectroscopy as a tool to study the metal enrichment in clusters and fine spectroscopy of Fe X-ray lines as a powerful diagnostics of both the turbulent plasma motions and the energetics of the non-thermal electron populations. The knowledge of the complex dynamical and feedback processes is necessary to understand the energy and matter balance as well as to constrain the role of the non-thermal components of clusters. C1 [Bykov, A. M.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Bykov, A. M.] St Petersburg State Politecn Univ, St Petersburg, Russia. [Bykov, A. M.] Int Space Sci Inst, Bern, Switzerland. [Churazov, E. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E. M.] Space Res Inst IKI, Moscow 117997, Russia. [Ferrari, C.] Univ Nice Sophia Antipolis, Lab Lagrange, Observ Cote Azur, CNRS,UMR7293, F-06300 Nice, France. [Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaastra, J. S.; de Plaa, J.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Klein, U.] Univ Bonn, Argelander Inst Astron, Bonn, Germany. [Markevitch, M.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Bykov, AM (reprint author), AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. EM byk@astro.ioffe.ru; churazov@mpa-garching.mpg.de; chiara.ferrari@oca.eu; forman@cfa.harvard.edu; j.kaastra@sron.nl; uklein@astro.uni-bonn.de; maxim.markevitch@nasa.gov; J.de.Plaa@sron.nl RI Bykov, Andrei/E-3131-2014; Churazov, Eugene/A-7783-2013; OI Forman, William/0000-0002-9478-1682 FU NASA [NASA-03060]; Chandra HRC project; Chandra archive grant [AR1-12007X]; NASA observing grant [GO2-13005X]; NWO (the Netherlands Organization for Scientific Research) FX We would like to thank the referee for useful comments and the ISSI staff for providing an inspiring atmosphere favorable for intense discussions. We thank Hiroki Akamatsu for providing us with Fig. 21 before publication. W. Forman acknowledges support from NASA contract NASA-03060 that funds the Chandra HRC project, the Chandra archive grant AR1-12007X, and the NASA observing grant GO2-13005X. SRON is financially supported by NWO (the Netherlands Organization for Scientific Research). NR 202 TC 3 Z9 3 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD MAY PY 2015 VL 188 IS 1-4 BP 141 EP 185 DI 10.1007/s11214-014-0129-4 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ0FO UT WOS:000355151400005 ER PT J AU Slane, P Bykov, A Ellison, DC Dubner, G Castro, D AF Slane, Patrick Bykov, Andrei Ellison, Donald C. Dubner, Gloria Castro, Daniel TI Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures SO SPACE SCIENCE REVIEWS LA English DT Review DE Supernova remnants; Molecular clouds; X-rays; Gamma-rays ID MHZ MASER EMISSION; BROAD-BAND EMISSION; FORMED DENSE SHELL; IC 443; COSMIC-RAYS; INTERSTELLAR-MEDIUM; NEUTRAL HYDROGEN; RX J1713.7-3946; POLARIZATION OBSERVATIONS; ACCELERATED PARTICLES AB The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and gamma-ray studies have established the presence of relativistic electrons and protons in some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the gamma-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and gamma-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy. C1 [Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bykov, Andrei] Ioffe Inst Phys & Technol, St Petersburg 194021, Russia. [Bykov, Andrei] St Petersburg State Polytech Univ, St Petersburg, Russia. [Ellison, Donald C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Dubner, Gloria] UBA CONICET, IAFE, RA-1428 Buenos Aires, DF, Argentina. [Castro, Daniel] MIT Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM slane@cfa.harvard.edu; byk@astro.ioffe.ru; don_ellison@ncsu.edu; gdubner@iafe.uba.ar; castro@mit.edu RI Bykov, Andrei/E-3131-2014 FU NASA [NAS8-03060]; RAS Presidium 21 program; OFN 15 program FX The authors would like to thank Tom Dame and Herman Lee for important discussions contributing to this paper. We also thank ISSI and its staff for supporting this effort and for creating a stimulating environment for the meeting at which this work was initiated. POS acknowledges support from NASA Contract NAS8-03060. AMB was supported in part by RAS Presidium 21 and OFN 15 programs. NR 127 TC 12 Z9 12 U1 1 U2 4 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 MAY PY 2015 VL 188 IS 1-4 BP 187 EP 210 DI 10.1007/s11214-014-0062-6 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ0FO UT WOS:000355151400006 ER PT J AU Brassington, NJ Zezas, A Ashby, MLN Lanz, L Smith, HA Willner, SP Klein, C AF Brassington, N. J. Zezas, A. Ashby, M. L. N. Lanz, L. Smith, Howard. A. Willner, S. P. Klein, C. TI THE SPITZER INTERACTING GALAXIES SURVEY: A MID-INFRARED ATLAS OF STAR FORMATION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: evolution; galaxies: interactions; stars: formation ID DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEUS; SWIRE-FIELD GALAXIES; FORMATION RATES; INFRARED GALAXIES; NEARBY GALAXIES; PECULIAR GALAXIES; SPACE-TELESCOPE; SPIRAL GALAXIES AB The Spitzer Interacting Galaxies Survey is a sample of 103 nearby galaxies in 48 systems, selected using association likelihoods and therefore free from disturbed morphology biases. All galaxies have been observed with Infrared Array Camera and MIPS 24 mu m bands from the Spitzer Space Telescope. This catalog presents the global flux densities and colors of all systems and correlations between the interacting systems and their specific star formation rate (sSFR). This sample contains a wide variety of galaxy interactions with systems ranging in mass, mass ratios, and gas-content as well as interaction strength. This study seeks to identify the process of triggering star formation in galaxy interactions, therefore, we focus on the non-active galactic nucleus spiral galaxies only. From this subset of 70 spiral galaxies we have determined that this sample has enhanced sSFR compared to a sample of non-interacting field galaxies. Through optical data we have classified each system by "interaction strength"; the strongly interacting (Stage 4) galaxies have higher sSFR values than the weakly (Stage 2) and moderately (Stage 3) interacting systems. However, the Stage 2 and 3 systems have statistically identical sSFR properties, despite the lack of optical interaction signatures exhibited by the Stage 2 galaxies. We suggest that the similarity of sSFR in these stages could be a consequence of some of these Stage 2 systems actually being post-perigalactic and having had sufficient time for their tidal features to fade to undetectable levels. This interpretation is consistent with the correlation of sSFR with separation, which we have determined to have little variation up to 100 kpc. C1 [Brassington, N. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Zezas, A.; Ashby, M. L. N.; Lanz, L.; Smith, Howard. A.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Lanz, L.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Klein, C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Brassington, NJ (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM n.brassington@herts.ac.uk RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Lanz, Lauranne/0000-0002-3249-8224 FU NASA [NNX10AD68G]; NASA JPL RSA [1369566, 717352] FX We would like to thank the referee for useful comments which have improved our paper. This work makes use of observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work is based in part on the IRAC post-BCD processing software "IRACproc" developed by Mike Schuster, Massimo Marengo, and Brian Patten at the Smithsonian Astrophysical Observatory. We acknowledge support in part from NASA grant NNX10AD68G, NASA JPL RSA 1369566, and NASA JPL RSA 717352. N.J.B. would like to thank the physics department at the University of Crete and IESL Foundation for Research and Technology for their hospitality during part of this work. NR 70 TC 4 Z9 4 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 MAY PY 2015 VL 218 IS 1 AR 6 DI 10.1088/0067-0049/218/1/6 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8DN UT WOS:000354999200006 ER PT J AU Kim, J Lee, JE Choi, M Bourke, TL Evans, NJ Di Francesco, J Cieza, LA Dunham, MM Kang, M AF Kim, Jungha Lee, Jeong-Eun Choi, Minho Bourke, Tyler L. Evans, Neal J., II Di Francesco, James Cieza, Lucas A. Dunham, Michael M. Kang, Miju TI INFRARED AND RADIO OBSERVATIONS OF A SMALL GROUP OF PROTOSTELLAR OBJECTS IN THE MOLECULAR CORE, L1251-C SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM: individual objects (L1251-C); ISM: jets and outflows; stars: formation; stars: protostars ID YOUNG STELLAR OBJECTS; NEARBY DENSE CORES; SPITZER C2D SURVEY; ARRAY CAMERA IRAC; SUBMILLIMETER ARRAY; STAR-FORMATION; SPACE-TELESCOPE; EMBEDDED SOURCE; WATER MASERS; SMALL CLOUDS AB We present a multi-wavelength observational study of a low-mass star-forming region, L1251-C, with observational results at wavelengths from the near-infrared to the millimeter. Spitzer Space Telescope observations confirmed that IRAS 22343+7501 is a small group of protostellar objects. The extended emission in the east-west direction with its intensity peak at the center of L1251A has been detected at 350 and 850 mu m with the Caltech Submillimeter Observatory and James Clerk Maxwell telescopes, tracing dense envelope material around L1251A. The single-dish data from the Korean VLBI Network and TRAO telescopes show inconsistencies between the intensity peaks of several molecular emission lines and that of the continuum emission, suggesting complex distributions of molecular abundances around L1251A. The Submillimeter Array interferometer data, however, show intensity peaks of CO 2-1 and (CO)-C-13 2-1 located at the position of IRS 1, which is both the brightest source in the Infrared Array Camera image and the weakest source in the 1.3 mm dust-continuum map. IRS 1 is the strongest candidate for the driving source of the newly detected compact CO 2-1 outflow. Over the entire region (14' x 14') of L125l-C, 3 Class I and 16 Class II sources have been detected, including three young stellar objects (YSOs) in L1251A. A comparison between the average projected distance among the 19 YSOs in L1251-C and that among the 3 YSOs in L1251A suggests that L1251-C is an example of low-mass cluster formation where protostellar objects form in a small group. C1 [Kim, Jungha; Lee, Jeong-Eun] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea. [Choi, Minho; Kang, Miju] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Bourke, Tyler L.] Jodrell Bank Observ, Sq Kilometre Array Org, Lower Withington SK11 9DL, Cheshire, England. [Lee, Jeong-Eun; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Di Francesco, James] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC, Canada. [Cieza, Lucas A.] Univ Diego Portales, Fac Ingn, Santiago, Chile. [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kim, J (reprint author), Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea. FU Basic Science Research Program through the National Research Foundation of Korea (NRF) - Ministry of Education of the Korean government [NRF-2012R1A1A2044689]; BK21 plus program through the National Research Foundation (NRF) - Ministry of Education of Korea; Korea Astronomy and Space Science Institute (KASI) grant - Korea government (MEST); National Science Foundation [0708158]; NASA [NNX13AE54G, 1224608, 1230782, 1407] FX Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608 and 1230782 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. This research was also supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education of the Korean government (grant No. NRF-2012R1A1A2044689). J.-E.L. is very grateful to the department of Astronomy, University of Texas at Austin for the hospitality provided to her from 2013 August to 2014 July. This work was supported by the BK21 plus program through the National Research Foundation (NRF) funded by the Ministry of Education of Korea. This work was also supported by the Korea Astronomy and Space Science Institute (KASI) grant funded by the Korea government (MEST). This research was supported in part by the National Science Foundation under grant No. 0708158, and by NASA under grant No. NNX13AE54G (T.L.B.). NR 46 TC 1 Z9 1 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 MAY PY 2015 VL 218 IS 1 AR 5 DI 10.1088/0067-0049/218/1/5 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8DN UT WOS:000354999200005 ER PT J AU Merello, M Evans, NJ Shirley, YL Rosolowsky, E Ginsburg, A Bally, J Battersby, C Dunham, MM AF Merello, Manuel Evans, Neal J., II Shirley, Yancy L. Rosolowsky, Erik Ginsburg, Adam Bally, John Battersby, Cara Dunham, Michael M. TI THE BOLOCAM GALACTIC PLANE SURVEY. XI. TEMPERATURES AND SUBSTRUCTURE OF GALACTIC CLUMPS BASED ON 350 mu M OBSERVATIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; dust, extinction; Galaxy: structure; stars: formation; submillimeter: ISM; surveys ID MASSIVE STAR-FORMATION; DUST CONTINUUM SOURCES; SOUTH MOLECULAR CLOUD; INFRARED DARK CLOUDS; FORMING REGIONS; OUTER GALAXY; HI-GAL; PHYSICAL CONDITIONS; DATA REDUCTION; SHARC-II AB We present 107 maps of continuum emission at 350 mu m from Galactic molecular clumps. Observed sources were mainly selected from the Bolocam Galactic Plane Survey (BGPS) catalog, with three additional maps covering star-forming regions in the outer Galaxy. The higher resolution of the SHARC-II images (8."5 beam) compared with the 1.1 mm images from BGPS (33"beam) allowed us to identify a large population of smaller substructures within the clumps. A catalog is presented for the 1386 sources extracted from the 350 mu m maps. The color temperature distribution of clumps based on the two wavelengths has a median of 13.3 K and mean of 16.3 +/- 0.4 K, assuming an opacity law index of 1.7. For the structures with good determination of color temperatures, the mean ratio of gas temperature, determined from NH3 observations, to dust color temperature is 0.88 and the median ratio is 0.76. About half the clumps have more than 2 substructures and 22 clumps have more than 10. The fraction of the mass in dense substructures seen at 350 mu m compared to the mass of their parental clump is similar to 0.19, and the surface densities of these substructures are, on average, 2.2 times those seen in the clumps identified at 1.1 mm. For a well-characterized sample, 88 structures (31%) exceed a surface density of 0.2 g cm(-2), and 18 (6%) exceed 1.0 g cm(-2), thresholds for massive star formation suggested by theorists. C1 [Merello, Manuel; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Merello, Manuel] Ist Astrofis & Planetol Spaziali INAF, I-00133 Rome, Italy. [Shirley, Yancy L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Rosolowsky, Erik] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Ginsburg, Adam] European So Observ, ESO Headquarters, D-95748 Garching, Germany. [Bally, John] Univ Colorado, CASA, Boulder, CO 80309 USA. [Battersby, Cara; Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Merello, M (reprint author), Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA. EM manuel@astro.as.utexas.edu FU National Science Foundation through NSF grant [AST-0708403]; NRAO; NSF [AST-9980846, AST-0206158, AST-1109116]; Fulbright Fellowship; ASI, Agenzia Spaziale Italiana [I/038/080/0, I/029/12/0]; national funding agency: CSA (Canada); national funding agency: NAOC (China); national funding agency: CEA (France); national funding agency: ASI (Italy); national funding agency: MCINN (Spain); national funding agency: Stockholm Observatory (Sweden); national funding agency: STFC (UK); national funding agency: NASA (USA); national funding agency: CNES (France); national funding agency: CNRS (France) FX We thank the anonymous referee for the helpful comments and suggestions that improve the clarity of this article. We would like to thank all the people involved in obtaining our observations including D. Dowell, students and researchers from the University of Texas, and staff from CSO. The BGPS project was supported in part by the National Science Foundation through NSF grant AST-0708403. The first observing runs for BGPS were supported by travel funds provided by NRAO. Support for the development of Bolocam was provided by NSF grants AST-9980846 and AST-0206158. N.J.E. and M.M. were supported by NSF grant AST-1109116. MM was also supported by a Fulbright Fellowship. This material is based upon work at the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (AST-0838261). Herschel Hi-GAL data processing, maps production and source catalogue generation from the Hi-GAL Team have been possible thanks to Contracts I/038/080/0 and I/029/12/0 from ASI, Agenzia Spaziale Italiana. Herschel in an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IAPS, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). NR 72 TC 6 Z9 6 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 MAY PY 2015 VL 218 IS 1 AR 1 DI 10.1088/0067-0049/218/1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8DN UT WOS:000354999200001 ER PT J AU Williams, BF Wold, B Haberl, F Garofali, K Blair, WP Gaetz, TJ Kuntz, KD Long, KS Pannuti, TG Pietsch, W Plucinsky, PP Winkler, PF AF Williams, Benjamin F. Wold, Brian Haberl, Frank Garofali, Kristen Blair, William P. Gaetz, Terrance J. Kuntz, K. D. Long, Knox S. Pannuti, Thomas G. Pietsch, Wolfgang Plucinsky, Paul P. Winkler, P. Frank TI A DEEP XMM-NEWTON SURVEY OF M33: POINT-SOURCE CATALOG, SOURCE DETECTION, AND CHARACTERIZATION OF OVERLAPPING FIELDS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: individual (M33); X-rays: binaries; X-rays: stars ID CHANDRA ACIS SURVEY; X-RAY SOURCES; PHOTON IMAGING CAMERA; SUPERNOVA-REMNANTS; BINARY POPULATION; GALAXY M33; CHASEM33; VARIABILITY; EMISSION; SPECTRA AB We have obtained a deep 8 field XMM-Newton mosaic of M33 covering the galaxy out to the D-25 isophote and beyond to a limiting 0.2-4.5 keV unabsorbed flux of 5 x 10(-16) erg cm(-2) s(-1) (L > 4 x 10(34) erg s(-1) at the distance of M33). These data allow complete coverage of the galaxy with high sensitivity to soft sources such as diffuse hot gas and supernova remnants (SNRs). Here, we describe the methods we used to identify and characterize 1296 point sources in the 8 fields. We compare our resulting source catalog to the literature, note variable sources, construct hardness ratios, classify soft sources, analyze the source density profile, and measure the X-ray luminosity function (XLF). As a result of the large effective area of XMM-Newton below 1 keV, the survey contains many new soft X-ray sources. The radial source density profile and XLF for the sources suggest that only similar to 15% of the 391 bright sources with L > 3.6 x 10(35) erg s(-1) are likely to be associated with M33, and more than a third of these are known SNRs. The log(N)-log(S) distribution, when corrected for background contamination, is a relatively flat power law with a differential index of 1.5, which suggests that many of the other M33 sources may be high-mass X-ray binaries. Finally, we note the discovery of an interesting new transient X-ray source, which we are unable to classify. C1 [Williams, Benjamin F.; Wold, Brian; Garofali, Kristen] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Haberl, Frank; Pietsch, Wolfgang] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Blair, William P.; Kuntz, K. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Gaetz, Terrance J.; Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Pannuti, Thomas G.] Morehead State Univ, Dept Earth & Space Sci, Ctr Space Sci, Morehead, KY 40351 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Williams, BF (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM ben@astro.washington.edu; fwh@mpe.mpg.de; kgarofali@gmail.com; wpb@pha.jhu.edu; gaetz@head.cfa.harvard.edu; kuntz@pha.jhu.edu; long@stsci.edu; t.pannuti@moreheadstate.edu; wnp@mpe.mpg.de; plucinsk@head.cfa.harvard.edu; winkler@middlebury.edu OI Haberl, Frank/0000-0002-0107-5237 FU NASA [NNX12AD42G, NNX12AI52G, NAS8-03060]; Chandra X-ray Center FX Support for this work was provided by NASA grants NNX12AD42G and NNX12AI52G. T.J.G. and P.P.P. acknowledge support under NASA contract NAS8-03060 with the Chandra X-ray Center. NR 44 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2015 VL 218 IS 1 AR 9 DI 10.1088/0067-0049/218/1/9 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CI8DN UT WOS:000354999200009 ER PT J AU Levin, LA Breitburg, DL AF Levin, Lisa A. Breitburg, Denise L. TI Linking coasts and seas to address ocean deoxygenation SO NATURE CLIMATE CHANGE LA English DT Editorial Material ID HYPOXIA; CONSEQUENCES; ECOSYSTEMS AB Accelerated oxygen loss in both coastal and open oceans is generating complex biological responses; future understanding and management will require holistic integration of currently fragmented oxygen observation and research programmes. C1 [Levin, Lisa A.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. [Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Levin, LA (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. EM llevin@ucsd.edu FU NSF [EAR-1234095, OCE-0927445, 1041062, OISE-1204866]; University of California Irvine; NOAA [NA10OAR4170060-R/CC-04]; NOAA-CSCOR [NA10NOS4780138, NA09NOS4780214] FX We acknowledge support for our deoxygenation research from NSF EAR-1234095, OCE-0927445 & 1041062, OISE-1204866 (sub-award from University of California Irvine) and NOAA award NA10OAR4170060-R/CC-04 to L.A.L., and NOAA-CSCOR awards NA10NOS4780138 and NA09NOS4780214 to D.L.B. We thank K. Gedan and L. Bopp for providing materials for figure production. NR 15 TC 3 Z9 4 U1 1 U2 27 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD MAY PY 2015 VL 5 IS 5 BP 401 EP 403 PG 4 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA CI6SO UT WOS:000354891900011 ER PT J AU Reudink, MW McKellar, AE Marini, KLD McArthur, SL Marra, PP Ratcliffe, LM AF Reudink, Matthew W. McKellar, Ann E. Marini, Kristen L. D. McArthur, Sarah L. Marra, Peter P. Ratcliffe, Laurene M. TI Inter-annual variation in American redstart (Setophaga ruticilla) plumage colour is associated with rainfall and temperature during moult: an 11-year study SO OECOLOGIA LA English DT Article DE Plumage; Carotenoid; Climate; Long-term; Moult; Colour change ID SEXUAL SELECTION; MIGRATORY BIRD; CAROTENOID CONTENT; MIGRANT SONGBIRD; FEMALE PLUMAGE; CLIMATE-CHANGE; FEATHER COLOR; EXPRESSION; SEASON; ORNAMENTATION AB Carotenoid-based colouration plays an important role in sexual signaling in animals as an honest indicator of individual quality during mate choice and competitive interactions. However, few studies have examined how natural variation in weather conditions influences inter-annual variation in the expression of ornamentation, potentially through affecting the dietary availability of carotenoids. In this study, we examine variation in the expression of carotenoid-based plumage colouration in relation to temperature and rainfall during the pre-moulting and moulting period over 11 years in a population of American redstarts, Setophaga ruticilla, breeding in eastern Canada. We used reflectance spectrometry of tail feathers collected from male and female redstarts to relate feather colour with weather conditions the previous breeding season during the months over which redstarts are likely to moult (June-September). At a population level, birds expressed feathers with higher red chroma and lower brightness in years following high July rainfall and low August temperature. The pattern was stronger in males, but was generally consistent across ages and sexes. Analyses of feathers from repeatedly captured birds indicated that the above patterns could be explained by individual change in feather colour. We suggest that higher rainfall during the moulting period may increase insect abundance and the availability of dietary carotenoids. This is among the first studies to show effects of weather conditions on a sexual signalling trait, which may have important consequences for sexual selection, mate choice, and the reliability of putative signals. C1 [Reudink, Matthew W.; Marini, Kristen L. D.; McArthur, Sarah L.] Thompson Rivers Univ, Dept Biol Sci, Kamloops, BC, Canada. [McKellar, Ann E.] Environm Canada, Saskatoon, SK, Canada. [Marra, Peter P.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC USA. [Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. RP Reudink, MW (reprint author), Thompson Rivers Univ, Dept Biol Sci, Kamloops, BC, Canada. EM mreudink@tru.ca FU National Science Foundation; Natural Sciences and Engineering Research Council of Canada FX We thank would like to thank the many field assistants, technicians, and students that worked on this population over the years. We also thank the editor and two anonymous reviewers for helpful comments and suggestions. Funding for this project was provided by the National Science Foundation (P.P.M) and Natural Sciences and Engineering Research Council of Canada Discovery Grants to L.M.R. and M.W.R. NR 56 TC 4 Z9 4 U1 7 U2 23 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 MAY PY 2015 VL 178 IS 1 BP 161 EP 173 DI 10.1007/s00442-014-3167-4 PG 13 WC Ecology SC Environmental Sciences & Ecology GA CI4MY UT WOS:000354725200014 PM 25433695 ER PT J AU Coats, DW Lynn, DH AF Coats, D. Wayne Lynn, Denis H. TI Obituary: John O. Corliss, February 23, 1922-December 21, 2014 SO PROTIST LA English DT Editorial Material ID CILIATED PROTOZOA; REVISED CLASSIFICATION; PHYLUM CILIOPHORA; PROTISTS; BIODIVERSITY; BIOSPHERE C1 [Coats, D. Wayne] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Lynn, Denis H.] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. RP Coats, DW (reprint author), 318 Bayard Rd, Lothian, MD 20711 USA. EM coatsw1@gmail.com RI Lynn, Denis/F-4939-2010 OI Lynn, Denis/0000-0002-1554-7792 NR 25 TC 0 Z9 0 U1 1 U2 2 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1434-4610 J9 PROTIST JI Protist PD MAY PY 2015 VL 166 IS 2 BP 173 EP 176 DI 10.1016/j.protis.2015.02.001 PG 4 WC Microbiology SC Microbiology GA CI8JJ UT WOS:000355018300001 PM 25768268 ER PT J AU Bogdan, A Vogelsberger, M Kraft, RP Hernquist, L Gilfanov, M Torrey, P Churazov, E Genel, S Forman, WR Murray, SS Vikhlinin, A Jones, C Bohringer, H AF Bogdan, Akos Vogelsberger, Mark Kraft, Ralph P. Hernquist, Lars Gilfanov, Marat Torrey, Paul Churazov, Eugene Genel, Shy Forman, William R. Murray, Stephen S. Vikhlinin, Alexey Jones, Christine Boehringer, Hans TI HOT GASEOUS CORONAE AROUND SPIRAL GALAXIES: PROBING THE ILLUSTRIS SIMULATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; galaxies: ISM; galaxies: spiral; X-rays: galaxies; X-rays: general; X-rays: ISM ID X-RAY-EMISSION; INCLINED DISC GALAXIES; COSMOLOGICAL SIMULATIONS; HYDRODYNAMICAL SIMULATIONS; FORMATION PHYSICS; CHANDRA SURVEY; MOVING MESH; GAS; HALOS; LUMINOSITY AB The presence of hot gaseous coronae around present-day massive spiral galaxies is a fundamental prediction of galaxy formation models. However, our observational knowledge remains scarce, since to date only four gaseous coronae have been detected around spirals with massive stellar bodies (greater than or similar to 2 x 10(11) M-circle dot). To explore the hot coronae around lower mass spiral galaxies, we utilized Chandra X-ray observations of a sample of eight normal spiral galaxies with stellar masses of (0.7 - 2.0) x 10(11) M-circle dot. Although statistically significant diffuse X-ray emission is not detected beyond the optical radii (similar to 20 kpc) of the galaxies, we derive 3 sigma limits on the characteristics of the coronae. These limits, complemented with previous detections of NGC 1961 and NGC 6753, are used to probe the Illustris Simulation. The observed 3 sigma upper limits on the X-ray luminosities and gas masses exceed or are at the upper end of the model predictions. For NGC 1961 and NGC 6753 the observed gas temperatures, metal abundances, and electron density profiles broadly agree with those predicted by Illustris. These results hint that the physics modules of Illustris are broadly consistent with the observed properties of hot coronae around spiral galaxies. However, one shortcoming of Illustris is that massive black holes, mostly residing in giant ellipticals, give rise to powerful radio-mode active galactic nucleus feedback, which results in under-luminous coronae for ellipticals. C1 [Bogdan, Akos; Kraft, Ralph P.; Hernquist, Lars; Genel, Shy; Forman, William R.; Murray, Stephen S.; Vikhlinin, Alexey; Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vogelsberger, Mark; Torrey, Paul] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. [Gilfanov, Marat; Churazov, Eugene] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Gilfanov, Marat; Churazov, Eugene] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Torrey, Paul] CALTECH, TAPIR, Pasadena, CA 91125 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Boehringer, Hans] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Bogdan, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abogdan@cfa.harvard.edu RI Churazov, Eugene/A-7783-2013; OI Torrey, Paul/0000-0002-5653-0786; Forman, William/0000-0002-9478-1682 FU NASA - CXC [NAS8-03060]; NASA [NNX12AC67G]; Smithsonian Institution; NSF [AST-1312095] FX We thank the anonymous referee for constructive comments. We thank Volker Springel, Debora Sijacki, and Dylan Nelson for helpful discussions. This research made use of software provided by the Chandra X-ray Center in the application packages CIAO. This work made use of the NASA/IPAC Extragalactic Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We acknowledge the use of the HyperLeda database (http://leda.univ-lyon1.fr). A.B. acknowledges support provided by NASA through Einstein Postdoctoral Fellowship awarded by the CXC, which is operated by the SAO for NASA under contract NAS8-03060. W.F. and C.J. acknowledge support from the Smithsonian Institution. L.H. acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. NR 41 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 MAY 1 PY 2015 VL 804 IS 1 AR 72 DI 10.1088/0004-637X/804/1/72 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500072 ER PT J AU Brown, WR Anderson, J Gnedin, OY Bond, HE Geller, MJ Kenyon, SJ AF Brown, Warren R. Anderson, Jay Gnedin, Oleg Y. Bond, Howard E. Geller, Margaret J. Kenyon, Scott J. TI PROPER MOTIONS AND TRAJECTORIES FOR 16 EXTREME RUNAWAY AND HYPERVELOCITY STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: kinematics and dynamics; Magellanic Clouds; stars: early-type; stars: kinematics and dynamics ID LARGE-MAGELLANIC-CLOUD; DYNAMICALLY EJECTED RUNAWAY; MILKY-WAY; GALACTIC HALO; RADIAL-VELOCITIES; IA SUPERNOVAE; BRANCH STARS; BLACK-HOLE; ORIGIN; MASS AB We measure proper motions with the Hubble Space Telescope for 16 extreme radial velocity stars, mostly unbound B stars in the Milky Way halo. Twelve of these stars have proper motions statistically consistent with zero, and thus have radial trajectories statistically consistent with a Galactic center "hypervelocity star" origin. The trajectory of HE 0437-5439 is consistent with both Milky Way and Large Magellanic Cloud origins. A Galactic center origin is excluded at 3 sigma confidence for two of the lowest radial velocity stars in our sample, however. These two stars are probable disk runaways and provide evidence for similar to 500 km s(-1) ejections from the disk. We also measure a significant proper motion for the unbound sdO star US 708. Its 1000 km s(-1) motion is in some tension with proposed supernova ejection models, but can be explained if US 708 was ejected from the stellar halo. In the future, we expect Gaia will better constrain the origin of these remarkable unbound stars. C1 [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Anderson, Jay; Bond, Howard E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gnedin, Oleg Y.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bond, Howard E.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X; Gnedin, Oleg/0000-0001-9852-9954 FU Alfred P. Sloan Foundation; U.S. Dept. of Energy; NASA from the Space Telescope Science Institute [GO-11589, GO-12503]; NASA [NAS 5-26555]; Smithsonian Institution FX We thank the referee for constructive scientific comments. This research makes use of SAO/NASA's Astrophysics Data System Bibliographic Services. This research makes use of the Sloan Digital Sky Survey, which is funded by the Alfred P. Sloan Foundation, the Participating Institutions, and the U.S. Dept. of Energy. H.E.B. acknowledges support by NASA through grants GO-11589 and GO-12503 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This work was supported in part by the Smithsonian Institution. NR 64 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 MAY 1 PY 2015 VL 804 IS 1 AR 49 DI 10.1088/0004-637X/804/1/49 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500049 ER PT J AU Desert, JM Charbonneau, D Torres, G Fressin, F Ballard, S Bryson, ST Knutson, HA Batalha, NM Borucki, WJ Brown, TM Deming, D Ford, EB Fortney, JJ Gilliland, RL Latham, DW Seager, S AF Desert, Jean-Michel Charbonneau, David Torres, Guillermo Fressin, Francois Ballard, Sarah Bryson, Stephen T. Knutson, Heather A. Batalha, Natalie M. Borucki, William J. Brown, Timothy M. Deming, Drake Ford, Eric B. Fortney, Jonathan J. Gilliland, Ronald L. Latham, David W. Seager, Sara TI LOW FALSE POSITIVE RATE OF KEPLER CANDIDATES ESTIMATED FROM A COMBINATION OF SPITZER AND FOLLOW-UP OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; eclipses; planetary systems; planets and satellites: detection; techniques: polarimetric ID TRANSIT TIMING VARIATIONS; SUN-LIKE STAR; INFRARED ARRAY CAMERA; MULTIPLE-PLANET SYSTEMS; EXOPLANET HD 189733B; CIRCLE-PLUS PLANET; HABITABLE-ZONE; SPACE-TELESCOPE; ECLIPSING BINARIES; EXTRASOLAR PLANET AB NASA's Kepler mission has provided several thousand transiting planet candidates during the 4 yr of its nominal mission, yet only a small subset of these candidates have been confirmed as true planets. Therefore, the most fundamental question about these candidates is the fraction of bona fide planets. Estimating the rate of false positives of the overall Kepler sample is necessary to derive the planet occurrence rate. We present the results from two large observational campaigns that were conducted with the Spitzer Space Telescope during the the Kepler mission. These observations are dedicated to estimating the false positive rate (FPR) among the Kepler candidates. We select a sub-sample of 51 candidates, spanning wide ranges in stellar, orbital, and planetary parameter space, and we observe their transits with Spitzer at 4.5 mu m. We use these observations to measures the candidate's transit depths and infrared magnitudes. An authentic planet produces an achromatic transit depth (neglecting the modest effect of limb darkening). Conversely a bandpass-dependent depth alerts us to the potential presence of a blending star that could be the source of the observed eclipse: a false positive scenario. For most of the candidates (85%), the transit depths measured with Kepler are consistent with the transit depths measured with Spitzer as expected for planetary objects, while we find that the most discrepant measurements are due to the presence of unresolved stars that dilute the photometry. The Spitzer constraints on their own yield FPRs between 5% and depending on the Kepler Objects of Interest. By considering the population of the Kepler field stars, and by combining follow-up observations (imaging) when available, we find that the overall FPR of our sample is low. The measured upper limit on the FPR of our sample is 8.8% at a confidence level of 3 sigma. This observational result, which uses the achromatic property of planetary transit signals that is not investigated by the Kepler observations, provides an independent indication that Kepler's FPR is low. C1 [Desert, Jean-Michel; Brown, Timothy M.] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Desert, Jean-Michel; Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Charbonneau, David; Torres, Guillermo; Fressin, Francois; Ballard, Sarah; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ballard, Sarah] Univ Washington, Seattle, WA 98195 USA. [Bryson, Stephen T.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Ford, Eric B.] Univ Florida, Gainesville, FL 32611 USA. [Ford, Eric B.; Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Seager, Sara] MIT, Cambridge, MA 02159 USA. RP Desert, JM (reprint author), Univ Colorado, CASA, Dept Astrophys & Planetary Sci, 389-UCB, Boulder, CO 80309 USA. EM desert@colorado.edu OI /0000-0001-6545-639X FU NASA's Science Mission Directorate; NASA; NASA Kepler Mission Participating Scientist Program [NNX09AB53G, NNX12AC77G, NNX12AC75G, NNX14AB83G]; John Templeton Foundation; National Aeronautics and Space Administration FX We thank the anonymous reviewer for the careful reading of our manuscript and the valuable comments. This work is based on observations made with Kepler, which was competitively selected as the 10th Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors would like to thank the many people who generously gave so much of their time to make this mission a success. This work is also 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. D.C. acknowledges support for this work from grants NNX09AB53G and NNX12AC77G, and G.T. acknowledges support from grants NNX12AC75G and NNX14AB83G, each from the NASA Kepler Mission Participating Scientist Program. D.C. acknowledges the support of a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. We would like to thank the Spitzer staff at IPAC and in particular Nancy Silbermann for scheduling the Spitzer observations of this program. J.-M.D. and S.B. acknowledge the Sagan Exoplanet Fellowship program supported by the National Aeronautics and Space Administration and administered by the NASA Exoplanet Science Institute (NExScI). We thank Samaya Nissanke for careful reading of the manuscript. NR 108 TC 15 Z9 15 U1 4 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 MAY 1 PY 2015 VL 804 IS 1 AR 59 DI 10.1088/0004-637X/804/1/59 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500059 ER PT J AU Field, G AF Field, George TI THE 2014 HENRY NORRIS RUSSELL LECTURE: A CAREER IN ASTRONOMY SO ASTROPHYSICAL JOURNAL LA English DT Article ID MAGNETIC-FIELDS; MOLECULAR CLOUDS; RELAXATION; TURBULENCE; HYDROGEN; DYNAMO; MODEL C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Field, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 38 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 MAY 1 PY 2015 VL 804 IS 1 AR 1 DI 10.1088/0004-637X/804/1/1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500001 ER PT J AU Gezari, S Jones, DO Sanders, NE Soderberg, AM Hung, T Heinis, S Smartt, SJ Rest, A Scolnic, D Chornock, R Berger, E Foley, RJ Huber, ME Price, P Stubbs, CW Riess, AG Kirshner, RP Smith, K Wood-Vasey, WM Schiminovich, D Martin, DC Burgett, WS Chambers, KC Flewelling, H Kaiser, N Tonry, JL Wainscoat, R AF Gezari, S. Jones, D. O. Sanders, N. E. Soderberg, A. M. Hung, T. Heinis, S. Smartt, S. J. Rest, A. Scolnic, D. Chornock, R. Berger, E. Foley, R. J. Huber, M. E. Price, P. Stubbs, C. W. Riess, A. G. Kirshner, R. P. Smith, K. Wood-Vasey, W. M. Schiminovich, D. Martin, D. C. Burgett, W. S. Chambers, K. C. Flewelling, H. Kaiser, N. Tonry, J. L. Wainscoat, R. TI GALEX DETECTION OF SHOCK BREAKOUT IN TYPE IIP SUPERNOVA PS1-13arp: IMPLICATIONS FOR THE PROGENITOR STAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: individual (PS1-13arp); surveys; ultraviolet: general ID CORE-COLLAPSE SUPERNOVAE; DIGITAL SKY SURVEY; X-RAY-EMISSION; RED SUPERGIANT; MASS-LOSS; ULTRALUMINOUS SUPERNOVAE; PAN-STARRS1 DISCOVERY; CIRCUMSTELLAR WIND; P SUPERNOVAE; LIGHT CURVES AB We present the GALEX detection of a UV burst at the time of explosion of an optically normal supernova (SN) IIP (PS1-13arp) from the Pan-STARRS1 survey at z = 0.1665. The temperature and luminosity of the UV burst match the theoretical predictions for shock breakout in a red supergiant (RSG), but with a duration a factor of similar to 50 longer than expected. We compare the NUV light curve of PS1-13arp to previous GALEX detections of SNe IIP and find clear distinctions that indicate that the UV emission is powered by shock breakout, and not by the subsequent cooling envelope emission previously detected in these systems. We interpret the similar to 1 day duration of the UV signal with a shock breakout in the wind of an RSG with a pre-explosion mass-loss rate of similar to 10(-3) M-circle dot yr(-1). This mass-loss rate is enough to prolong the duration of the shock breakout signal, but not enough to produce an excess in the optical plateau light curve or narrow emission lines powered by circumstellar interaction. This detection of nonstandard, potentially episodic high mass loss in an RSG SN progenitor has favorable consequences for the prospects of future wide-field UV surveys to detect shock breakout directly in these systems, and provide a sensitive probe of the pre-explosion conditions of SN progenitors. C1 [Gezari, S.; Hung, T.; Heinis, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Jones, D. O.; Riess, A. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Sanders, N. E.; Soderberg, A. M.; Berger, E.; Stubbs, C. W.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smartt, S. J.; Smith, K.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Scolnic, D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Chornock, R.] Ohio Univ, Athens, OH 45701 USA. [Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Huber, M. E.; Chambers, K. C.; Flewelling, H.; Kaiser, N.; Tonry, J. L.; Wainscoat, R.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Price, P.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Stubbs, C. W.; Kirshner, R. P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Astrophys & Cosmol Ctr, Pittsburgh Particle Phys, Pittsburgh, PA USA. [Schiminovich, D.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Martin, D. C.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Burgett, W. S.] GMTO Corp, Pasadena, CA 91101 USA. RP Gezari, S (reprint author), Univ Maryland, Dept Astron, Stadium Dr, College Pk, MD 20742 USA. EM suvi@astro.umd.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Chambers, Kenneth /0000-0001-6965-7789; Flewelling, Heather/0000-0002-1050-4056 FU program for the TOO program [GN-2013A-Q-32]; National Aeronautics and Space Administration [NNX08AR22G]; National Science Foundation [AST-1238877] FX S.G. thanks the Gemini Deputy Director for approving a change of program for the TOO program GN-2013A-Q-32 to observe PS1-13arp. 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). NR 70 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 MAY 1 PY 2015 VL 804 IS 1 AR 28 DI 10.1088/0004-637X/804/1/28 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500028 ER PT J AU Jeong, J Park, H Han, C Gould, A Udalski, A Szymanski, MK Pietrzynski, G Soszynski, I Poleski, R Ulaczyk, K Wyrzykowski, L Abe, F Bennett, DP Bond, IA Botzler, CS Freeman, M Fukui, A Fukunaga, D Itow, Y Koshimoto, N Masuda, K Matsubara, Y Muraki, Y Namba, S Ohnishi, K Rattenbury, NJ Saito, T Sullivan, DJ Sweatman, WL Sumi, T Suzuki, D Tristram, PJ Tsurumi, N Wada, K Yamai, N Yock, PCM Yonehara, A Albrow, MD Batista, V Beaulieu, JP Caldwell, JAR Cassan, A Cole, A Coutures, C Dieters, S Dominik, M Prester, DD Donatowicz, J Fouque, P Greenhill, J Hoffman, M Huber, M Jorgensen, UG Kane, SR Kubas, D Martin, R Marquette, JB Menzies, J Pitrou, C Pollard, K Sahu, KC Vinter, C Wambsganss, J Williams, A Allen, W Bolt, G Choi, JY Christie, GW DePoy, DL Drummond, J Gaudi, BS Hwang, KH Jung, YK Lee, CU Mallia, F Maoz, D Maury, A McCormick, J Monard, LAG Moorhouse, D Natusch, T Ofek, EO Park, BG Pogge, RW Santallo, R Shin, IG Thornley, G Yee, JC Bramich, DM Burgdorf, M Horne, K Hundertmark, M Kains, N Snodgrass, C Steele, I Street, R Tsapras, Y AF Jeong, J. Park, H. Han, C. Gould, A. Udalski, A. Szymanski, M. K. Pietrzynski, G. Soszynski, I. Poleski, R. Ulaczyk, K. Wyrzykowski, L. Abe, F. Bennett, D. P. Bond, I. A. Botzler, C. S. Freeman, M. Fukui, A. Fukunaga, D. Itow, Y. Koshimoto, N. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Rattenbury, N. J. Saito, To. Sullivan, D. J. Sweatman, W. L. Sumi, T. Suzuki, D. Tristram, P. J. Tsurumi, N. Wada, K. Yamai, N. Yock, P. C. M. Yonehara, A. Albrow, M. D. Batista, V. Beaulieu, J. -P. Caldwell, J. A. R. Cassan, A. Cole, A. Coutures, C. Dieters, S. Dominik, M. Prester, D. Dominis Donatowicz, J. Fouque, P. Greenhill, J. Hoffman, M. Huber, M. Jorgensen, U. G. Kane, S. R. Kubas, D. Martin, R. Marquette, J. -B. Menzies, J. Pitrou, C. Pollard, K. Sahu, K. C. Vinter, C. Wambsganss, J. Williams, A. Allen, W. Bolt, G. Choi, J. -Y. Christie, G. W. DePoy, D. L. Drummond, J. Gaudi, B. S. Hwang, K. -H. Jung, Y. K. Lee, C. -U. Mallia, F. Maoz, D. Maury, A. McCormick, J. Monard, L. A. G. Moorhouse, D. Natusch, T. Ofek, E. O. Park, B. -G. Pogge, R. W. Santallo, R. Shin, I. -G. Thornley, G. Yee, J. C. Bramich, D. M. Burgdorf, M. Horne, K. Hundertmark, M. Kains, N. Snodgrass, C. Steele, I. Street, R. Tsapras, Y. CA OGLE Collaboration MOA Collaboration PLANET Collaboration mFUN Collaboration RoboNet Collaboration TI REANALYSES OF ANOMALOUS GRAVITATIONAL MICROLENSING EVENTS IN THE OGLE-III EARLY WARNING SYSTEM DATABASE WITH COMBINED DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; gravitational lensing: micro ID BINARY LENSES; GALACTIC BULGE; EWS DATABASE; SEARCH; MASS; PERTURBATIONS; STELLAR; LIMITS; HALO AB We reanalyze microlensing events in the published list of anomalous events that were observed from the Optical Gravitational Lensing Experiment (OGLE) lensing survey conducted during the 2004-2008 period. In order to check the existence of possible degenerate solutions and extract extra information, we conduct analyses based on combined data from other survey and follow-up observation and consider higher-order effects. Among the analyzed events, we present analyses of eight events for which either new solutions are identified or additional information is obtained. We find that the previous binary-source interpretations of five events are better interpreted by binary-lens models. These events include OGLE-2006-BLG-238, OGLE-2007-BLG-159, OGLE-2007-BLG-491, OGLE-2008-BLG-143, and OGLE-2008-BLG-210. With additional data covering caustic crossings, we detect finite-source effects for six events including OGLE-2006-BLG-215, OGLE-2006-BLG-238, OGLE-2006-BLG-450, OGLE-2008-BLG-143, OGLE-2008-BLG-210, and OGLE-2008-BLG-513. Among them, we are able to measure the Einstein radii of three events for which multi-band data are available. These events are OGLE-2006-BLG-238, OGLE-2008-BLG-210, and OGLE-2008-BLG-513. For OGLE-2008-BLG-143, we detect higher-order effects induced by the changes of the observer's position caused by the orbital motion of the Earth around the Sun. In addition, we present degenerate solutions resulting from the known close/wide or ecliptic degeneracy. Finally, we note that the masses of the binary companions of the lenses of OGLE-2006-BLG-450 and OGLE-2008-BLG-210 are in the brown-dwarf regime. C1 [Jeong, J.; Park, H.; Han, C.; Choi, J. -Y.; Hwang, K. -H.; Jung, Y. K.; Shin, I. -G.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 361763, South Korea. [Gould, A.; Poleski, R.; Batista, V.; Pogge, R. W.; Yee, J. C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Udalski, A.; Szymanski, M. K.; Pietrzynski, G.; Soszynski, I.; Poleski, R.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Abe, F.; Fukunaga, D.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Sumi, T.; 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.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Auckland, New Zealand. [Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. [Koshimoto, N.; Namba, S.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Saito, To.; Gaudi, B. S.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. [Sullivan, D. J.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. [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. [Albrow, M. D.; Pollard, K.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Beaulieu, J. -P.; Cassan, A.; Coutures, C.; Dieters, S.; Kubas, D.; Marquette, J. -B.; Pitrou, C.] Univ Paris 06, CNRS UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Caldwell, J. A. R.; Cole, A.] McDonald Observ, Ft Davis, TX 79734 USA. [Dominik, M.; Horne, K.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Prester, D. Dominis] Univ Rijeka, Fac Arts & Sci, Dept Phys, Rijeka 51000, Croatia. [Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1040 Vienna, Austria. [Fouque, P.] Univ Toulouse, CNRS, UMR 5277, IRAP, F-31400 Toulouse, France. [Fouque, P.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Hoffman, M.] Univ Orange Free State, Fac Nat & Agr Sci, Dept Phys, ZA-9300 Bloemfontein, South Africa. [Huber, M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Jorgensen, U. G.; Vinter, C.; Hundertmark, M.] Niels Bohr Inst, Astron Observ, DK-2100 Copenhagen, Denmark. [Kane, S. R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia. [Menzies, J.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wambsganss, J.] Astron Rech Inst, D-69120 Heidelberg, Germany. [Allen, W.] Vintage Lane Observ, Blenheim, New Zealand. [Bolt, G.] Craigie Observ, Craigie, WA, Australia. [Christie, G. W.; Natusch, T.] Auckland Observ, Auckland, New Zealand. [DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Drummond, J.] Possum Observ, Patutahi, Gisbourne, New Zealand. [Lee, C. -U.; Park, B. -G.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Mallia, F.; Maury, A.] Campo Catino Austral Observ, San Pedro De Atacama, Chile. [Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Maoz, D.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. [McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand. [Monard, L. A. G.] Klein Karoo Observ, Calitzdorp, South Africa. [Monard, L. A. G.] Bronberg Observ, Pretoria, South Africa. [Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand. [Natusch, T.] AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand. [Ofek, E. O.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Santallo, R.] Southern Stars Observ, Faaa, Tahiti, Fr Polynesia. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bramich, D. M.; Kains, N.] European So Observ, D-85748 Garching, Germany. [Burgdorf, M.] Univ Hamburg, Meterol Inst, D-20146 Hamburg, Germany. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Steele, I.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Street, R.; Tsapras, Y.] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA. [Tsapras, Y.] Univ London, Sch Math Sci, Astron Unit, London E1 4NS, England. RP Han, C (reprint author), Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 361763, South Korea. RI Hundertmark, Markus/C-6190-2015; OI Dominik, Martin/0000-0002-3202-0343; Hundertmark, Markus/0000-0003-0961-5231; Cole, Andrew/0000-0003-0303-3855; Snodgrass, Colin/0000-0001-9328-2905 FU Creative Research Initiative Program of the National Research Foundation of Korea [2009-0081561]; European Research Council under the European Community's Seventh Framework Programme (FP7) / ERC [246678]; JSPS [JSPS23340044, JSPS24253004]; NSF [AST 110347]; NASA [NNX12AB99G]; NASA through the Sagan Fellowship Program; [JSPS18253002]; [JSPS20340052]; [NASA-NNX12AF54G]; [JPL-RSA 1453175]; [NSF AST-1211875] FX Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. 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. The MOA project is supported by the grants JSPS18253002 and JSPS20340052. T.S. acknowledges the financial support from the JSPS, JSPS23340044 and JSPS24253004. D.P.B. was supported by grants NASA-NNX12AF54G, JPL-RSA 1453175, and NSF AST-1211875. B.S.G. and A.G. were supported by NSF grant AST 110347. B.S.G., A.G., and R.P.G. were supported by NASA grant NNX12AB99G. 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. NR 26 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2015 VL 804 IS 1 AR 38 DI 10.1088/0004-637X/804/1/38 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500038 ER PT J AU Liu, HB Galvan-Madrid, R Jimenez-Serra, I Roman-Zuniga, C Zhang, QZ Li, ZY Chen, HR AF Liu, Hauyu Baobab Galvan-Madrid, Roberto Jimenez-Serra, Izaskun Roman-Zuniga, Carlos Zhang, Qizhou Li, Zhiyun Chen, Huei-Ru TI ALMA RESOLVES THE SPIRALING ACCRETION FLOW IN THE LUMINOUS OB CLUSTER-FORMING REGION G33.92+0.11 SO ASTROPHYSICAL JOURNAL LA English DT Article DE evolution; ISM: individual objects (G33.92+0.11); stars: formation ID MASSIVE STAR-FORMATION; HOT MOLECULAR CORES; GRAVITATIONAL FRAGMENTATION; MAGNETIC-FIELD; FINITE SHEETS; HII-REGIONS; CLOUD; COLLAPSE; FILAMENT; CAMERA AB How rapidly collapsing parsec-scale massive molecular clumps feed high-mass stars and how they fragment to form OB clusters have been outstanding questions in the field of star formation. In this work, we report the resolved structures and kinematics of the approximately face-on, rotating massive molecular clump, G33.92+0.11. Our high-resolution Atacama Large Millimeter/submillimeter Array images show that the spiral arm-like gas overdensities form in the eccentric gas accretion streams. First, we resolved that the dominant part of the similar to 0.6 pc scale massive molecular clump (3.0(-1.4)(+2.8).10(3) M-circle dot) G33.92+0.11 A is tangled with several 0.5-1 pc size molecular arms spiraling around it, which may be connected further to exterior gas accretion streams. Within G33.92+0.11 A, we resolved the similar to 0.1 pc width gas mini-arms connecting to the two central massive (100-300 M-circle dot) molecular cores. The kinematics of arms and cores elucidate a coherent accretion flow continuing from large to small scales. We demonstrate that the large molecular arms are indeed the cradles of dense cores, which are likely current or future sites of high-mass star formation. Since these deeply embedded massive molecular clumps preferentially form the highest-mass stars in the clusters, we argue that dense cores fed by or formed within molecular arms play a key role in making the upper end of the stellar and core mass functions. C1 [Liu, Hauyu Baobab; Chen, Huei-Ru] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Galvan-Madrid, Roberto] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Jimenez-Serra, Izaskun] European So Observ, D-85748 Garching, Germany. [Roman-Zuniga, Carlos] UNAM, Inst Astron, Unidad Acad Ensenada, Ensenada 22860, Baja California, Mexico. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Li, Zhiyun] Dept Astron, Charlottesville, VA 22904 USA. [Chen, Huei-Ru] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan. [Chen, Huei-Ru] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan. RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM hyliu@asiaa.sinica.edu.tw RI Roman-Zuniga, Carlos/F-6602-2016; OI Roman-Zuniga, Carlos/0000-0001-8600-4798; Zhang, Qizhou/0000-0003-2384-6589 FU National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project [NCC5-626]; People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7) REA grant [PIIF-GA-2011-301538]; program CONACYT, Mexico [CB2010-152160]; MOST grant [103-2119-M-001-010-MY2] FX This paper makes use of the following ALMA data: ADS/JAO. ALMA 2012.1.00387.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. This material is based upon work at the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology. In the present paper, we discussed observations performed with the ESA Herschel Space Observatory (Pilbratt et al. 2010), in particular, employing Herschel's large telescope and powerful science payload to do photometry using the PACS (Poglitsch et al. 2010) and SPIRE (Griffin et al. 2010) instruments. Herschel is an ESA space observatory with science instruments provided by the European-led Principal Investigator consortia and with important participation from NASA. This research made use of Montage, funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. H.B.L. thanks Simon Radford and other CSO staff for assisting the operation of SHARC2. H.B.L. thanks ASIAA for supporting a series of related researches. I.J.-S. acknowledges funding from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7/2007-2013) under REA grant agreement No. PIIF-GA-2011-301538. C.R.Z. acknowledges support from program CONACYT CB2010-152160, Mexico. H.B.L. acknowledges funding under MOST grant number 103-2119-M-001-010-MY2. NR 52 TC 10 Z9 10 U1 2 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 MAY 1 PY 2015 VL 804 IS 1 AR 37 DI 10.1088/0004-637X/804/1/37 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500037 ER PT J AU Munoz-Jaramillo, A Senkpeil, RR Longcope, DW Tlatov, AG Pevtsov, AA Balmaceda, LA DeLuca, EE Martens, PCH AF Munoz-Jaramillo, Andres Senkpeil, Ryan R. Longcope, Dana W. Tlatov, Andrey G. Pevtsov, Alexei A. Balmaceda, Laura A. DeLuca, Edward E. Martens, Petrus C. H. TI THE MINIMUM OF SOLAR CYCLE 23: AS DEEP AS IT COULD BE? SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: magnetic fields; Sun: photosphere; sunspots ID SUNSPOT MAGNETIC-FIELDS; ACTIVE-REGIONS; STATISTICAL PROPERTIES; SIZE DISTRIBUTION; DYNAMO MODELS; TILT ANGLES; FLUX; DEPENDENCE; EMERGENCE; WIND AB In this work we introduce a new way of binning sunspot group data with the purpose of better understanding the impact of the solar cycle on sunspot properties and how this defined the characteristics of the extended minimum of cycle 23. Our approach assumes that the statistical properties of sunspots are completely determined by the strength of the underlying large-scale field and have no additional time dependencies. We use the amplitude of the cycle at any given moment (something we refer to as activity level) as a proxy for the strength of this deep-seated magnetic field. We find that the sunspot size distribution is composed of two populations: one population of groups and active regions and a second population of pores and ephemeral regions. When fits are performed at periods of different activity level, only the statistical properties of the former population, the active regions, are found to vary. Finally, we study the relative contribution of each component (small-scale versus large-scale) to solar magnetism. We find that when hemispheres are treated separately, almost every one of the past 12 solar minima reaches a point where the main contribution to magnetism comes from the small-scale component. However, due to asymmetries in cycle phase, this state is very rarely reached by both hemispheres at the same time. From this we infer that even though each hemisphere did reach the magnetic baseline, from a heliospheric point of view the minimum of cycle 23 was not as deep as it could have been. C1 [Munoz-Jaramillo, Andres; Longcope, Dana W.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Munoz-Jaramillo, Andres] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Munoz-Jaramillo, Andres] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Senkpeil, Ryan R.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Tlatov, Andrey G.] Pulkovo Observ, Kislovodsk Mt Astron Stn, Kislovodsk 357700, Russia. [Pevtsov, Alexei A.] Natl Solar Observ, Sunspot, NM 88349 USA. [Balmaceda, Laura A.] Consejo Nacl Invest Cient & Tecn, ICATE, Inst Astron Terr & Space Sci, San Juan, Argentina. [Balmaceda, Laura A.] Natl Inst Space Res INPE, Sao Jose Dos Campos, Brazil. [DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martens, Petrus C. H.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. RP Munoz-Jaramillo, A (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. EM munoz@solar.physics.montana.edu OI Balmaceda, Laura/0000-0003-1162-5498; Pevtsov, Alexei/0000-0003-0489-0920 FU NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program; Lockheed-Martin [SP02H1701R]; CfA Solar Physics REU program, NSF [AGS-1263241] FX We thank Karel Schrijver, Maria Navas Moreno, and an anonymous referee for useful discussions and suggestions. This research was supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs, contract SP02H1701R from Lockheed-Martin to the Smithsonian Astrophysical Observatory, and the CfA Solar Physics REU program, NSF grant number AGS-1263241. Andres Munoz-Jaramillo is very grateful to George Fisher and Stuart Bale for their support at the University of California, Berkeley, and Phil Scherrer for his support at Stanford University. The National Solar Observatory (NSO) is operated by the Association of Universities for Research in Astronomy, AURA Inc. under cooperative agreement with the National Science Foundation (NSF). NR 47 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2015 VL 804 IS 1 AR 68 DI 10.1088/0004-637X/804/1/68 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500068 ER PT J AU Novati, SC Gould, A Udalski, A Menzies, JW Bond, IA Shvartzvald, Y Street, RA Hundertmark, M Beichman, CA Yee, JC Carey, S Poleski, R Skowron, J Kozlowski, S Mroz, P Pietrukowicz, P Pietrzynski, G Szymanski, MK Soszynski, I Ulaczyk, K Wyrzykowski, L Albrow, M Beaulieu, JP Caldwell, JAR Cassan, A Coutures, C Danielski, C Prester, DD Donatowicz, J Loncaric, K McDougall, A Morales, JC Ranc, C Zhu, W Abe, F Barry, RK Bennett, DP Bhattacharya, A Fukunaga, D Inayama, K Koshimoto, N Namba, S Sumi, T Suzuki, D Tristram, PJ Wakiyama, Y Yonehara, A Maoz, D Kaspi, S Friedmann, M Bachelet, E Jaimes, RF Bramich, DM Tsapras, Y Horne, K Snodgrass, C Wambsganss, J Steele, IA Kains, N Bozza, V Dominik, M Jorgensen, UG Alsubai, KA Ciceri, S D'Ago, G Haugbolle, T Hessman, FV Hinse, TC Juncher, D Korhonen, H Mancini, L Popovas, A Rabus, M Rahvar, S Scarpetta, G Schmidt, RW Skottfelt, J Southworth, J Starkey, D Surdej, J Wertz, O Zarucki, M Gaudi, BS Pogge, RW De Poy, DL The OGLE Collaboration AF Novati, S. Calchi Gould, A. Udalski, A. Menzies, J. W. Bond, I. A. Shvartzvald, Y. Street, R. A. Hundertmark, M. Beichman, C. A. Yee, J. C. Carey, S. Poleski, R. Skowron, J. Kozlowski, S. Mroz, P. Pietrukowicz, P. Pietrzynski, G. Szymanski, M. K. Soszynski, I. Ulaczyk, K. Wyrzykowski, L. Albrow, M. Beaulieu, J. P. Caldwell, J. A. R. Cassan, A. Coutures, C. Danielski, C. Prester, D. Dominis Donatowicz, J. Loncaric, K. McDougall, A. Morales, J. C. Ranc, C. Zhu, W. Abe, F. Barry, R. K. Bennett, D. P. Bhattacharya, A. Fukunaga, D. Inayama, K. Koshimoto, N. Namba, S. Sumi, T. Suzuki, D. Tristram, P. J. Wakiyama, Y. Yonehara, A. Maoz, D. Kaspi, S. Friedmann, M. Bachelet, E. Jaimes, R. Figuera Bramich, D. M. Tsapras, Y. Horne, K. Snodgrass, C. Wambsganss, J. Steele, I. A. Kains, N. Bozza, V. Dominik, M. Jorgensen, U. G. Alsubai, K. A. Ciceri, S. D'Ago, G. Haugbolle, T. Hessman, F. V. Hinse, T. C. Juncher, D. Korhonen, H. Mancini, L. Popovas, A. Rabus, M. Rahvar, S. Scarpetta, G. Schmidt, R. W. Skottfelt, J. Southworth, J. Starkey, D. Surdej, J. Wertz, O. Zarucki, M. Gaudi, B. S. Pogge, R. W. De Poy, D. L. Collaboration, The O. G. L. E. CA The PLANET Collaboration The MOA Collaboration The Wise Grp The RoboNet Collaboration The MiNDSTEp Consortium The FUN Collaboration TI PATHWAY TO THE GALACTIC DISTRIBUTION OF PLANETS: COMBINED SPITZER AND GROUND-BASED MICROLENS PARALLAX MEASUREMENTS OF 21 SINGLE-LENS EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planetary systems; planets and satellites: dynamical evolution and stability ID SPACE-TELESCOPE; ISOLATED STAR; MASS; BULGE; COMPANIONS; PHOTOMETRY; FREQUENCY; NETWORK; SYSTEMS; MACHOS AB We present microlens parallax measurements for 21 (apparently) isolated lenses observed toward the Galactic bulge that were imaged simultaneously from Earth and Spitzer, which was similar to 1 AU west of Earth in projection. We combine these measurements with a kinematic model of the Galaxy to derive distance estimates for each lens, with error bars that are small compared to the Sun's galactocentric distance. The ensemble therefore yields a well-defined cumulative distribution of lens distances. In principle, it is possible to compare this distribution against a set of planets detected in the same experiment in order to measure the Galactic distribution of planets. Since these Spitzer observations yielded only one planet, this is not yet possible in practice. However, it will become possible as larger samples are accumulated. C1 [Novati, S. Calchi; Beichman, C. A.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Novati, S. Calchi; Bozza, V.; D'Ago, G.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy. [Novati, S. Calchi; Scarpetta, G.; Zarucki, M.] IIASS, I-84019 Vietri Sul Mare, SA, Italy. [Gould, A.; Poleski, R.; Zhu, W.; Gaudi, B. S.; Pogge, R. W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Udalski, A.; Poleski, R.; Skowron, J.; Kozlowski, S.; Mroz, P.; Pietrukowicz, P.; Pietrzynski, G.; Szymanski, M. K.; Soszynski, I.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Menzies, J. W.] S African Astron Observ, Observ 7935, Cape Town, South Africa. [Bond, I. A.] Massey Univ, North Shore Mail Ctr, Inst Nat & Math Sci, Auckland, New Zealand. [Shvartzvald, Y.; Maoz, D.; Kaspi, S.; Friedmann, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Street, R. A.; Tsapras, Y.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Hundertmark, M.; Jorgensen, U. G.; Haugbolle, T.; Juncher, D.; Korhonen, H.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Hundertmark, M.; Jaimes, R. Figuera; Horne, K.; Dominik, M.; Starkey, D.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carey, S.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Albrow, M.; McDougall, A.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Beaulieu, J. P.; Cassan, A.; Coutures, C.; Ranc, C.] UPMC, CNRS, Inst Astrophys, UMR 7095, F-75014 Paris, France. [Beaulieu, J. P.; Morales, J. C.] LESIA, Sect Meudon 5, Observ Paris, F-92195 Meudon, France. [Caldwell, J. A. R.] McDonald Observ, Ft Davis, TX 79734 USA. [Danielski, C.] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Prester, D. Dominis; Loncaric, K.] Univ Rijeka, Dept Phys, Rijeka 51000, Croatia. [Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1040 Vienna, Austria. [Abe, F.; Fukunaga, D.; Wakiyama, Y.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Barry, R. K.] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Bennett, D. P.; Bhattacharya, A.; Suzuki, D.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Inayama, K.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan. [Koshimoto, N.; Namba, S.; Sumi, T.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Tristram, P. J.] Mt John Univ Observ, Lake Tekapo, New Zealand. [Bachelet, E.; Bramich, D. M.; Alsubai, K. A.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar. [Jaimes, R. Figuera; Kains, N.] European So Observ, D-85748 Garching, Germany. [Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Snodgrass, C.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Wambsganss, J.; Schmidt, R. W.] Zentrum Astron Univ Heidelberg ZAH, Astron Rechen Inst, D-69120 Heidelberg, Germany. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Bozza, V.; D'Ago, G.; Scarpetta, G.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Ciceri, S.; Mancini, L.; Rabus, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hessman, F. V.] Univ Gottingen, Inst Astrophys, D-37073 Gottingen, Germany. [Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Korhonen, H.] Turku Univ, Finnish Ctr Astron ESO, FI-21500 Piikkio, Finland. [Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrophys, Santiago 22, Chile. [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Surdej, J.; Wertz, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Cointe Ougree, Belgium. [De Poy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. RP Novati, SC (reprint author), CALTECH, NASA Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA. RI Hundertmark, Markus/C-6190-2015; Ranc, Clement/B-1958-2016; Skowron, Jan/M-5186-2014; Korhonen, Heidi/E-3065-2016; Morales, Juan Carlos/H-5548-2015; D'Ago, Giuseppe/N-8318-2016; Kozlowski, Szymon/G-4799-2013; OI Snodgrass, Colin/0000-0001-9328-2905; Hundertmark, Markus/0000-0003-0961-5231; Ranc, Clement/0000-0003-2388-4534; Skowron, Jan/0000-0002-2335-1730; Korhonen, Heidi/0000-0003-0529-1161; Morales, Juan Carlos/0000-0003-0061-518X; D'Ago, Giuseppe/0000-0001-9697-7331; Kozlowski, Szymon/0000-0003-4084-880X; Dominik, Martin/0000-0002-3202-0343 FU JPL grant [1500811]; NSF [AST 1103471]; NASA [NNX12AB99G]; European Research Council under the European Community's Seventh Framework Programme (FP7)/ ERC grant [246678]; NASA through the Sagan Fellowship Program; University of Rijeka project [13.12.1.3.02]; Marsden Fund of the Royal Society of New Zealand [MAU1104]; I-CORE program of the Planning and Budgeting Committee; Israel Science Foundation [1829/12]; US-Israel Binational Science Foundation; Danish Natural Science Foundation (FNU); NPRP grants from the Qatar National Research Fund (a member of Qatar Foundation) [09-476-1-078, X-019-1-006]; Communaute francaise de Belgique-Actions de recherche concertees-Academie Wallonie-Europe; Villum Foundation; European Union Seventh Framework Programme (FP7) [268421]; [JSPS23103002]; [JSPS24253004]; [JSPS26247023]; [JSPS25103508]; [JSPS23340064] FX Work by C.A.B. was carried out in part at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Work by J.C.Y. A.G., and S.C. was supported by JPL grant 1500811. A.G. and B.S.G. were supported by NSF grant AST 1103471. A.G., B.S.G., and R. W.P. were supported by NASA grant NNX12AB99G. 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 J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Work by D.D.P. and K.L. was supported by the University of Rijeka project 13.12.1.3.02. Work by T.S. is supported by grants JSPS23103002, JSPS24253004, and JSPS26247023. Work by I.A.B. was supported by the Marsden Fund of the Royal Society of New Zealand, contract no. MAU1104. The MOA project is supported by the grant JSPS25103508 and 23340064. Work by D.M. is supported by the I-CORE program of the Planning and Budgeting Committee and the Israel Science Foundation, Grant 1829/12. D.M. and A.G. acknowledge support by the US-Israel Binational Science Foundation. The operation of the Danish 1.54 m telescope at ESO's La Silla Observatory is financed by a grant to U.G.J. from the Danish Natural Science Foundation (FNU). This publication was made possible by NPRP grants 09-476-1-078 and X-019-1-006 from the Qatar National Research Fund (a member of Qatar Foundation). O.W. (FNRS research fellow) and J. Surdej acknowledge support from the Communaute francaise de Belgique-Actions de recherche concertees-Academie Wallonie-Europe. M.H. acknowledges support from the Villum Foundation. C.S. received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 268421. 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. The research described in this publication was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 41 TC 17 Z9 17 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 MAY 1 PY 2015 VL 804 IS 1 AR 20 DI 10.1088/0004-637X/804/1/20 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500020 ER PT J AU Skowron, J Shin, IG Udalski, A Han, C Sumi, T Shvartzvald, Y Gould, A Prester, DD Street, RA Jorgensen, UG Bennett, DP Bozza, V Szymanski, MK Kubiak, M Pietrzynski, G Soszynski, I Poleski, R Kozlowski, S Pietrukowicz, P Ulaczyk, K Wyrzykowski, L Abe, F Bhattacharya, A Bond, IA Botzler, CS Freeman, M Fukui, A Fukunaga, D Itow, Y Ling, CH Koshimoto, N Masuda, K Matsubara, Y Muraki, Y Namba, S Ohnishi, K Philpott, LC Rattenbury, N Saito, T Sullivan, DJ Suzuki, D Tristram, PJ Yock, PCM Maoz, D Kaspi, S Friedmann, M Almeida, LA Batista, V Christie, G Choi, JY Depoy, DL Gaudi, BS Henderson, C Hwang, KH Jablonski, F Jung, YK Lee, CU McCormick, J Natusch, T Ngan, H Park, H Pogge, RW Yee, JC Albrow, MD Bachelet, E Beaulieu, JP Brillant, S Caldwell, JAR Cassan, A Cole, A Corrales, E Coutures, CH Dieters, S Donatowicz, J Fouque, P Greenhill, J Kains, N Kane, SR Kubas, D Marquette, JB Martin, R Menzies, J Pollard, KR Ranc, C Sahu, KC Wambsganss, J Williams, A Wouters, D Tsapras, Y Bramich, DM Horne, K Hundertmark, M Snodgrass, C Steele, IA Alsubai, KA Browne, P Burgdorf, MJ Novati, SC Dodds, P Dominik, M Dreizler, S Fang, XS Gu, CH Hardis Harpsoe, K Hessman, FV Hinse, TC Hornstrup, A Jessen-Hansen, J Kerins, E Liebig, C Lund, M Lundkvist, M Mancini, L Mathiasen, M Penny, MT Rahvar, S Ricci, D Scarpetta, G Skottfelt, J Southworth, J Surdej, J Tregloan-Reed, J Wertz, O AF Skowron, J. Shin, I. -G. Udalski, A. Han, C. Sumi, T. Shvartzvald, Y. Gould, A. Prester, D. Dominis Street, R. A. Jorgensen, U. G. Bennett, D. P. Bozza, V. Szymanski, M. K. Kubiak, M. Pietrzynski, G. Soszynski, I. Poleski, R. Kozlowski, S. Pietrukowicz, P. Ulaczyk, K. Wyrzykowski, L. Abe, F. Bhattacharya, A. Bond, I. A. Botzler, C. S. Freeman, M. Fukui, A. Fukunaga, D. Itow, Y. Ling, C. H. Koshimoto, N. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Philpott, L. C. Rattenbury, N. Saito, T. Sullivan, D. J. Suzuki, D. Tristram, P. J. Yock, P. C. M. Maoz, D. Kaspi, S. Friedmann, M. Almeida, L. A. Batista, V. Christie, G. Choi, J. -Y. Depoy, D. L. Gaudi, B. S. Henderson, C. Hwang, K. -H. Jablonski, F. Jung, Y. K. Lee, C. -U. McCormick, J. Natusch, T. Ngan, H. Park, H. Pogge, R. W. Yee, J. C. Albrow, M. D. Bachelet, E. Beaulieu, J. -P. Brillant, S. Caldwell, J. A. R. Cassan, A. Cole, A. Corrales, E. Coutures, C. H. Dieters, S. Donatowicz, J. Fouque, P. Greenhill, J. Kains, N. Kane, S. R. Kubas, D. Marquette, J. -B. Martin, R. Menzies, J. Pollard, K. R. Ranc, C. Sahu, K. C. Wambsganss, J. Williams, A. Wouters, D. Tsapras, Y. Bramich, D. M. Horne, K. Hundertmark, M. Snodgrass, C. Steele, I. A. Alsubai, K. A. Browne, P. Burgdorf, M. J. Novati, S. Calchi Dodds, P. Dominik, M. Dreizler, S. Fang, X. -S. Gu, C. -H. Hardis Harpsoe, K. Hessman, F. V. Hinse, T. C. Hornstrup, A. Jessen-Hansen, J. Kerins, E. Liebig, C. Lund, M. Lundkvist, M. Mancini, L. Mathiasen, M. Penny, M. T. Rahvar, S. Ricci, D. Scarpetta, G. Skottfelt, J. Southworth, J. Surdej, J. Tregloan-Reed, J. Wertz, O. CA OGLE Collaboration MOA Collaboration Wise Grp FUN Collaboration PLANET Collaboration RoboNet Collaboration MiNDSTEp Consortium TI OGLE-2011-BLG-0265Lb: A JOVIAN MICROLENSING PLANET ORBITING AN M DWARF SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planetary systems ID SURFACE BRIGHTNESS RELATIONS; GRAVITATIONAL BINARY-LENS; GALACTIC BULGE; MASS PLANET; OGLE-III; JUPITER/SATURN ANALOG; ANGULAR SIZES; GIANT PLANETS; SNOW LINE; STARS AB We report the discovery of a Jupiter-mass planet orbiting an M-dwarf star that gave rise to the microlensing event OGLE-2011-BLG-0265. Such a system is very rare among known planetary systems and thus the discovery is important for theoretical studies of planetary formation and evolution. High-cadence temporal coverage of the planetary signal, combined with extended observations throughout the event, allows us to accurately model the observed light curve. However, the final microlensing solution remains degenerate, yielding two possible configurations of the planet and the host star. In the case of the preferred solution, the mass of the planet is M-p = 0.9 +/- 0.3 M-J, and the planet is orbiting a star with a mass M = 0.22 +/- 0.06 M-circle dot. The second possible configuration (2 sigma away) consists of a planet with M-p = 0.6 +/- 0.3M(J) and host star with M = 0.14 +/- 0.06M(circle dot). The system is located in the Galactic disk 3-4 kpc toward the Galactic bulge. In both cases, with an orbit size of 1.5-2.0 AU, the planet is a "cold Jupiter"-located well beyond the "snow line" of the host star. Currently available data make the secure selection of the correct solution difficult, but there are prospects for lifting the degeneracy with additional follow-up observations in the future, when the lens and source star separate. C1 [Skowron, J.; Udalski, A.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Poleski, R.; Kozlowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Shin, I. -G.; Han, C.; Choi, J. -Y.; Hwang, K. -H.; Jung, Y. K.; Park, H.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea. [Sumi, T.; Koshimoto, N.; Namba, S.; Suzuki, D.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Shvartzvald, Y.; Maoz, D.; Kaspi, S.; Friedmann, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Gould, A.; Poleski, R.; Batista, V.; Gaudi, B. S.; Henderson, C.; Pogge, R. W.; Yee, J. C.; Penny, M. T.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Prester, D. Dominis] Univ Rijeka, Fac Arts & Sci, Dept Phys, Rijeka 51000, Croatia. [Street, R. A.; Tsapras, Y.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Jorgensen, U. G.; Hardis; Harpsoe, K.; Hinse, T. C.; Mathiasen, M.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Jorgensen, U. G.; Harpsoe, K.; Skottfelt, J.] Ctr Star & Planet Format, Geol Museum, DK-1350 Copenhagen, Denmark. [Bennett, D. P.; Bhattacharya, A.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, SA, Italy. [Bozza, V.; Scarpetta, G.] Ist Nazl Fis Nucl, Sezione Napoli, Italy. [Soszynski, I.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Abe, F.; Fukunaga, D.; Itow, Y.; Masuda, K.; Matsubara, Y.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Auckland, New Zealand. [Botzler, C. S.; Freeman, M.; Rattenbury, N.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1, New Zealand. [Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan. [Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Philpott, L. C.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada. [Saito, T.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan. [Sullivan, D. J.; Tristram, P. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Almeida, L. A.; Jablonski, F.] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Christie, G.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland 1023, New Zealand. [Depoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Lee, C. -U.; Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand. [Natusch, T.] AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Albrow, M. D.; Pollard, K. R.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand. [Bachelet, E.; Dieters, S.; Fouque, P.] Univ Toulouse, IRAP, UPS OMP, F-31400 Toulouse, France. [Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, C. H.; Kubas, D.; Marquette, J. -B.; Ranc, C.; Wouters, D.] UPMC, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Brillant, S.; Kubas, D.] European So Observ, Santiago 19001 19, Chile. [Caldwell, J. A. R.] McDonald Observ, Ft Davis, TX 79734 USA. [Cole, A.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria. [Fouque, P.] CFHT Corp, Kamuela, HI 96743 USA. [Kains, N.] European So Observ, D-85748 Garching, Germany. [Kains, N.; Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kane, S. R.; Novati, S. Calchi] CALTECH, Exoplanet Sci Inst, NASA, Pasadena, CA 91125 USA. [Martin, R.] Perth Observ, Perth, WA 6076, Australia. [Menzies, J.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Wambsganss, J.; Williams, A.] Zentrum Astron Univ Heidelberg ZAH, Astron Rech Inst, D-69120 Heidelberg, Germany. [Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar. [Horne, K.; Hundertmark, M.; Browne, P.; Dodds, P.; Dominik, M.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Hundertmark, M.; Dreizler, S.; Hessman, F. V.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Alsubai, K. A.] Qatar Fdn, Doha, Qatar. [Burgdorf, M. J.] HE Space Operat GmbH, D-28199 Bremen, Germany. [Novati, S. Calchi; Scarpetta, G.] IIASS, I-84019 Vietri Sul Mare Salerno, Italy. [Fang, X. -S.; Gu, C. -H.; Hornstrup, A.] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Natl Astron Observat Yunnan Observ, Kunming 650011, Peoples R China. [Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Kerins, E.; Penny, M. T.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Jessen-Hansen, J.; Lund, M.; Lundkvist, M.] Aarhus Univ, Dept Phys & Astron, Aarhus C, Denmark. [Lundkvist, M.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran. [Rahvar, S.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Ricci, D.] Ist Astrofis Spaziale & Fis Cosm, INAF, Bologna, Italy. [Ricci, D.] UNAM, Inst Astron, Ensenada 22800, Baja California, Mexico. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Tregloan-Reed, J.; Wertz, O.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Tregloan-Reed, J (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Hundertmark, Markus/C-6190-2015; Almeida, L./G-7188-2012; Ranc, Clement/B-1958-2016; Skowron, Jan/M-5186-2014; Kozlowski, Szymon/G-4799-2013; OI Snodgrass, Colin/0000-0001-9328-2905; Hundertmark, Markus/0000-0003-0961-5231; Ranc, Clement/0000-0003-2388-4534; Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X; Philpott, Lydia/0000-0002-5286-8528; Dominik, Martin/0000-0002-3202-0343; Cole, Andrew/0000-0003-0303-3855 FU European Research Council under the European Community's Seventh Framework Programme (FP7) / ERC [246678]; Polish Ministry of Science and Higher Education (MNiSW) through the program "Iuventus Plus" [IP2011 026771]; Creative Research Initiative Program of National Research Foundation of Korea [2009-0081561]; JSPS [24253004, JSPS23540339, JSPS19340058]; Distinguished University Fellowship from The Ohio State University and in part under contract with the California Institute of Technology (Caltech) - NASA through the Sagan Fellowship Program; NSF [AST 1103471]; NASA [NNX12AB99G]; European Union [268421]; Danish Natural Science Foundation (FNU); German Research Foundation (DFG); Communaute francaise de Belgique-Actions de recherche concertees-Academie universitaire Wallonie-Europe; Qatar National Research Fund (QNRF), Qatar Foundation [NPRP 09-476-1-078]; University of Rijeka Project [13.12.1.3.02]; I-CORE program of the Planning and Budgeting Committee; Israel Science Foundation [1829/12]; US-Israel Binational Science Foundation; [JSPS22403003]; [JSPS23340064]; [JSPS23340044]; [JSPS24253004] FX 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. This research was partly supported by the Polish Ministry of Science and Higher Education (MNiSW) through the program "Iuventus Plus" award No. IP2011 026771. Work by C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. The MOA experiment was supported by grants JSPS22403003 and JSPS23340064. T.S. acknowledges the support of JSPS 24253004. T.S. is supported by the grant JSPS23340044. Y.M. acknowledges support from JSPS grants JSPS23540339 and JSPS19340058. Work by J.C.Y. is supported in part by a Distinguished University Fellowship from The Ohio State University and in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. Work by A.G. and B.S.G was supported by NSF grant AST 1103471. Work by A.G., B.S.G., and RWP was supported by NASA grant NNX12AB99G. T.S. acknowledges support from the grants JSPS23340044 and JSPS24253004. C.S. received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 268421. This work is based in part on data collected by MiNDSTEp with the Danish 1.54 m telescope at the ESO La Silla Observatory. The Danish 1.54 m telescope is operated based on a grant from the Danish Natural Science Foundation (FNU). The MiNDSTEp monitoring campaign is powered by ARTEMiS (Automated Terrestrial Exoplanet Microlensing Search; Dominik et al. 2008, AN 329, 248). M.H. acknowledges support by the German Research Foundation (DFG). D.R. (boursier FRIA) and J.S. acknowledge support from the Communaute francaise de Belgique-Actions de recherche concertees-Academie universitaire Wallonie-Europe. K.A., D.M.B., M.D., K.H., M.H., C.L., C.S., R.A.S., and Y.T. are thankful to the Qatar National Research Fund (QNRF), member of Qatar Foundation, for support by grant NPRP 09-476-1-078. Work by D.D.P. was supported by the University of Rijeka Project 13.12.1.3.02. This research was supported by the I-CORE program of the Planning and Budgeting Committee and the Israel Science Foundation, grant 1829/12. D.M. and A.G. acknowledge support by the US-Israel Binational Science Foundation. NR 63 TC 11 Z9 11 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 MAY 1 PY 2015 VL 804 IS 1 AR 33 DI 10.1088/0004-637X/804/1/33 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500033 ER PT J AU Thyagarajan, N Jacobs, DC Bowman, JD Barry, N Beardsley, AP Bernardi, G Briggs, F Cappallo, RJ Carroll, P Corey, BE de Oliveira-Costa, A Dillon, JS Emrich, D Ewall-Wice, A Feng, L Goeke, R Greenhill, LJ Hazelton, BJ Hewitt, JN Hurley-Walker, N Johnston-Hollitt, M Kaplan, DL Kasper, JC Kim, HS Kittiwisit, P Kratzenberg, E Lenc, E Line, J Loeb, A Lonsdale, CJ Lynch, MJ McKinley, B McWhirter, SR Mitchell, DA Morales, MF Morgan, E Neben, AR Oberoi, D Offringa, AR Ord, SM Paul, S Pindor, B Pober, JC Prabu, T Procopio, P Riding, J Rogers, AEE Roshi, A Shankar, NU Sethi, SK Srivani, KS Subrahmanyan, R Sullivan, IS Tegmark, M Tingay, SJ Trott, CM Waterson, M Wayth, RB Webster, RL Whitney, AR Williams, A Williams, CL Wu, C Wyithe, JSB AF Thyagarajan, Nithyanandan Jacobs, Daniel C. Bowman, Judd D. Barry, N. Beardsley, A. P. Bernardi, G. Briggs, F. Cappallo, R. J. Carroll, P. Corey, B. E. de Oliveira-Costa, A. Dillon, Joshua S. Emrich, D. Ewall-Wice, A. Feng, L. Goeke, R. Greenhill, L. J. Hazelton, B. J. Hewitt, J. N. Hurley-Walker, N. Johnston-Hollitt, M. Kaplan, D. L. Kasper, J. C. Kim, Han-Seek Kittiwisit, P. Kratzenberg, E. Lenc, E. Line, J. Loeb, A. Lonsdale, C. J. Lynch, M. J. McKinley, B. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Neben, A. R. Oberoi, D. Offringa, A. R. Ord, S. M. Paul, Sourabh Pindor, B. Pober, J. C. Prabu, T. Procopio, P. Riding, J. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Sethi, Shiv K. Srivani, K. S. Subrahmanyan, R. Sullivan, I. S. Tegmark, M. Tingay, S. J. Trott, C. M. Waterson, M. Wayth, R. B. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. Wu, C. Wyithe, J. S. B. TI FOREGROUNDS IN WIDE-FIELD REDSHIFTED 21 cm POWER SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; large-scale structure of universe; methods: statistical; radio continuum: galaxies; techniques: interferometric ID MURCHISON WIDEFIELD ARRAY; RADIO IMAGING SURVEY; LOW-FREQUENCY; INTERGALACTIC MEDIUM; CENTIMETER TOMOGRAPHY; SOUTHERN SKY; DARK-AGES; BASE-LINE; 150 MHZ; REIONIZATION AB Detection of 21 cm emission of H I from the epoch of reionization, at redshifts z > 6, is limited primarily by foreground emission. We investigate the signatures of wide-field measurements and an all-sky foreground model using the delay spectrum technique that maps the measurements to foreground object locations through signal delays between antenna pairs. We demonstrate interferometric measurements are inherently sensitive to all scales, including the largest angular scales, owing to the nature of wide-field measurements. These wide-field effects are generic to all observations but antenna shapes impact their amplitudes substantially. A dish-shaped antenna yields the most desirable features from a foreground contamination viewpoint, relative to a dipole or a phased array. Comparing data from recent Murchison Widefield Array observations, we demonstrate that the foreground signatures that have the largest impact on the H I signal arise from power received far away from the primary field of view. We identify diffuse emission near the horizon as a significant contributing factor, even on wide antenna spacings that usually represent structures on small scales. For signals entering through the primary field of view, compact emission dominates the foreground contamination. These two mechanisms imprint a characteristic pitchfork signature on the "foreground wedge" in Fourier delay space. Based on these results, we propose that selective down-weighting of data based on antenna spacing and time can mitigate foreground contamination substantially by a factor of similar to 100 with negligible loss of sensitivity. C1 [Thyagarajan, Nithyanandan; Jacobs, Daniel C.; Bowman, Judd D.; Kittiwisit, P.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Barry, N.; Beardsley, A. P.; Hazelton, B. J.; Morales, M. F.; Pober, J. C.; Sullivan, I. S.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 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. [de Oliveira-Costa, A.; Ewall-Wice, A.; Feng, L.; Goeke, R.; Morgan, E.; Neben, A. R.; Tegmark, M.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hurley-Walker, N.; Ord, S. M.; Tingay, S. J.; Trott, C. M.; Waterson, M.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Kim, Han-Seek; Line, J.; McKinley, B.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Epping, NSW 1710, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Morales, M. F.; Paul, Sourabh; Shankar, N. Udaya; Sethi, Shiv K.; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA USA. [Wu, C.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. RP Thyagarajan, N (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM t_nithyanandan@asu.edu RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Sethi, Shiv/D-4893-2012; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Udayashankar , N/D-4901-2012 OI Pober, Jonathan/0000-0002-3492-0433; Lenc, Emil/0000-0002-9994-1593; Wyithe, Stuart/0000-0001-7956-9758; KIM, HANSIK/0000-0002-5507-5769; /0000-0002-0086-7363; Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; FU U.S. National Science Foundation (NSF) [AST-1109257]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1401708]; NSF Astronomy and Astrophysics Fellowship [AST-1302774]; NSF [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF grants) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (via grant from the New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University Research Grant); Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy; Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited, under contract to Curtin University; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Western Australian State government FX This work was supported by the U.S. National Science Foundation (NSF) through award AST-1109257. D.C.J. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1401708. J.C.P. is supported by an NSF Astronomy and Astrophysics Fellowship under award AST-1302774. This work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the NSF (awards: AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 59 TC 30 Z9 30 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 MAY 1 PY 2015 VL 804 IS 1 AR 14 DI 10.1088/0004-637X/804/1/14 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500014 ER PT J AU Vacca, WD Hamilton, RT Savage, M Shenoy, S Becklin, EE McLean, IS Logsdon, SE Marion, GH Ashok, NM Banerjee, DPK Evans, A Fox, OD Garnavich, P Gehrz, RD Greenhouse, M Helton, LA Kirshner, RP Shenoy, D Smith, N Spyromilio, J Starrfield, S Wooden, DH Woodward, CE AF Vacca, William D. Hamilton, Ryan T. Savage, Maureen Shenoy, Sachindev Becklin, E. E. McLean, Ian S. Logsdon, Sarah E. Marion, G. H. Ashok, N. M. Banerjee, D. P. K. Evans, A. Fox, O. D. Garnavich, P. Gehrz, R. D. Greenhouse, M. Helton, L. A. Kirshner, R. P. Shenoy, D. Smith, Nathan Spyromilio, J. Starrfield, S. Wooden, D. H. Woodward, C. E. TI OBSERVATIONS OF TYPE Ia SUPERNOVA 2014J WITH FLITECAM ON SOFIA SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; supernovae: general; supernovae: individual (SN 2014J) ID NEAR-INFRARED SPECTRA; SN 2014J; TELESCOPE FACILITY; M82; SPECTROGRAPH; ULTRAVIOLET; ASTRONOMY; BINARIES; MODELS; TIME AB We present medium-resolution near-infrared (NIR) spectra, covering 1.1-3.4 mu m, of the normal Type Ia supernova (SN Ia) SN 2014J in M82 obtained with the FLITECAM instrument on board Stratospheric Observatory for Infrared Astronomy (SOFIA) between 17 and 26 days after maximum B light. Our 2.8-3.4 mu m spectra may be the first similar to 3 mu m spectra of an SN Ia ever published. The spectra spanning the 1.5-2.7 mu m range are characterized by a strong emission feature at similar to 1.77 mu m with a FWHM of similar to 11,000-13,000 kms(-1). We compare the observed FLITECAM spectra to the recent non-LTE delayed detonation models of Dessart et al. and find that the models agree with the spectra remarkably well in the 1.5-2.7 mu m wavelength range. Based on this comparison we identify the similar to 1.77 mu m emission peak as a blend of permitted lines of Co II. Other features seen in the 2.0-2.5 mu m spectra are also identified as emission from permitted transitions of Co II. However, the models are not as successful at reproducing the spectra in the 1.1-1.4 mu m range or between 2.8 and 3.4 mu m. These observations demonstrate the promise of SOFIA, which allows access to wavelength regions inaccessible from the ground, and serve to draw attention to the usefulness of the regions between the standard ground-based NIR passbands for constraining SN models. C1 [Vacca, William D.; Hamilton, Ryan T.; Savage, Maureen; Shenoy, Sachindev; Becklin, E. E.; Helton, L. A.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [McLean, Ian S.; Logsdon, Sarah E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Marion, G. H.] Univ Texas Austin, Austin, TX 78712 USA. [Ashok, N. M.; Banerjee, D. P. K.] Phys Res Lab, Ahmadabad 380009, Gujarat, India. [Evans, A.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Fox, O. D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Garnavich, P.] Univ Notre Dame, Notre Dame, IN 46556 USA. [Gehrz, R. D.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Greenhouse, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shenoy, D.; Woodward, C. E.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Smith, Nathan] Steward Observ, Tucson, AZ 85719 USA. [Spyromilio, J.] European So Observ, D-85748 Garching, Germany. [Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Wooden, D. H.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Vacca, WD (reprint author), NASA, Ames Res Ctr, SOFIA USRA, Mail Stop N232-12, Moffett Field, CA 94035 USA. EM wvacca@sofia.usra.edu FU NSF; NASA; NASA [NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901]; SOFIA Cycle 2 GI Research Grant [75-0001, 75-0002, 02-0100]; NASA through USRA [08500-05] FX We would like to thank the USRA/DSI science and mission operations teams and the engineering and support staff at NASA Armstrong and Ames for their pivotal roles in making SOFIA a reality. We also thank Luc Dessart and Stephane Blondin for sharing their SN models with us. R.D.G. thanks R. G. Arendt, E. Dwek, and T. Temim for providing useful input during the formulation of the scientific case for the observing program as members of the DDT proposal team. Similarly, P.G. thanks P. Milne, E. Hsiao, M. Phillips, and N. Suntzeff for their contributions to the science case of the accepted DDT proposal. S.S. acknowledges support from NSF and NASA grants to ASU.; Based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. Financial support for R.T.H., R.D.G., and P.G. was provided in part by SOFIA Cycle 2 GI Research Grant #'s 75-0001, 75-0002, and 02-0100, respectively, issued by USRA, on behalf of NASA. I.S.M. and S.E.L. were supported by NASA through grant 08500-05 from USRA for the development of FLITECAM. NR 44 TC 5 Z9 5 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 MAY 1 PY 2015 VL 804 IS 1 AR 66 DI 10.1088/0004-637X/804/1/66 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH7BB UT WOS:000354189500066 ER PT J AU Rangel, TF Colwell, RK Graves, GR Fucikova, K Rahbek, C Diniz, JAF AF Rangel, Thiago F. Colwell, Robert K. Graves, Gary R. Fucikova, Karolina Rahbek, Carsten Diniz-Filho, Jose Alexandre F. TI Phylogenetic uncertainty revisited: Implications for ecological analyses SO EVOLUTION LA English DT Article DE Hummingbirds; sensitivity analysis; uncertainty quantification ID EVOLUTIONARY; HUMMINGBIRDS; SUPERTREE; PATTERNS; TREES; DIVERSIFICATION; ADAPTATION; INFERENCE; RICHNESS; MAMMALS AB Ecologists and biogeographers usually rely on a single phylogenetic tree to study evolutionary processes that affect macroecological patterns. This approach ignores the fact that each phylogenetic tree is a hypothesis about the evolutionary history of a clade, and cannot be directly observed in nature. Also, trees often leave out many extant species, or include missing species as polytomies because of a lack of information on the relationship among taxa. Still, researchers usually do not quantify the effects of phylogenetic uncertainty in ecological analyses. We propose here a novel analytical strategy to maximize the use of incomplete phylogenetic information, while simultaneously accounting for several sources of phylogenetic uncertainty that may distort statistical inferences about evolutionary processes. We illustrate the approach using a clade-wide analysis of the hummingbirds, evaluating how different sources of uncertainty affect several phylogenetic comparative analyses of trait evolution and biogeographic patterns. Although no statistical approximation can fully substitute for a complete and robust phylogeny, the method we describe and illustrate enables researchers to broaden the number of clades for which studies informed by evolutionary relationships are possible, while allowing the estimation and control of statistical error that arises from phylogenetic uncertainty. Software tools to carry out the necessary computations are offered. C1 [Rangel, Thiago F.; Colwell, Robert K.; Diniz-Filho, Jose Alexandre F.] Univ Fed Goias, Dept Ecol, BR-74001970 Goiania, Go, Brazil. [Colwell, Robert K.; Fucikova, Karolina] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Colwell, Robert K.] Univ Colorado, Museum Nat Hist, Boulder, CO 80309 USA. [Graves, Gary R.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Graves, Gary R.; Rahbek, Carsten] Univ Copenhagen, Ctr Macroecol Evolut & Climate, Dept Biol, DK-2100 Copenhagen O, Denmark. RP Rangel, TF (reprint author), Univ Fed Goias, Dept Ecol, CP 131, BR-74001970 Goiania, Go, Brazil. EM thiago.rangel@ufg.br RI Diniz-Filho, Jose Alexandre/D-9405-2013; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 OI Diniz-Filho, Jose Alexandre/0000-0002-0967-9684; FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [564718/2010-6]; National Science Foundation (USA) [DEB-0639979, DBI-0851245, DEB-1036448]; Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); Alexander Wetmore Fund of the Smithsonian Institution; Smoketree Trust; Danish National Research Foundation; Center for Macroecology, Evolution and Climate; CAPES; CNPq FX Several concepts in this article were inspired by the phylogenetics course (EEB5349), taught by Dr. P. Lewis, at the University of Connecticut. TFR is supported by Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq, 564718/2010-6). RKC was supported by the National Science Foundation (USA, DEB-0639979 and DBI-0851245) and by Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES). GRG thanks the Alexander Wetmore Fund of the Smithsonian Institution, the Smoketree Trust, the Danish National Research Foundation, and the Center for Macroecology, Evolution and Climate for support. CR acknowledges the Danish National Research Foundation for support to the Center for Macroecology, Evolution and Climate. KF was supported by the National Science Foundation (USA, DEB-1036448, awarded to L.A. Lewis and P.O. Lewis). JAFD-F has been continuously supported by CAPES and CNPq through several research grants. NR 56 TC 10 Z9 10 U1 1 U2 26 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 MAY PY 2015 VL 69 IS 5 BP 1301 EP 1312 DI 10.1111/evo.12644 PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CI2FT UT WOS:000354561600015 PM 25800868 ER PT J AU Villa, C Buckberry, J Cattaneo, C Frohlich, B Lynnerup, N AF Villa, Chiara Buckberry, Jo Cattaneo, Cristina Frohlich, Bruno Lynnerup, Niels TI Quantitative Analysis of the Morphological Changes of the Pubic Symphyseal Face and the Auricular Surface and Implications for Age at Death Estimation SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE forensic science; forensic anthropology; curvature; CT scans; surface scans; 3D models ID ADULT SKELETAL AGE; SUCHEY-BROOKS; COMPUTED-TOMOGRAPHY; REVISED METHOD; IDENTIFICATION; RELIABILITY; ILIUM AB Age estimation methods are often based on the age-related morphological changes of the auricular surface and the pubic bone. In this study, a mathematical approach to quantify these changes has been tested analyzing the curvature variation on 3D models from CT and laser scans. The sample consisted of the 24 Suchey-Brooks (SB) pubic bone casts, 19 auricular surfaces from the Buckberry and Chamberlain (BC) recording kit and 98 pelvic bones from the Terry Collection (Smithsonian Institution). Strong and moderate correlations between phases and curvature were found in SB casts ( 0.60-0.93) and BC recording kit ( 0.47-0.75), moderate and weak correlations in the Terry Collection bones (pubic bones: 0.29-0.51, auricular surfaces: 0.33-0.50) but associated with large individual variability and overlap of curvature values between adjacent decades. The new procedure, requiring no expert judgment from the operator, achieved similar correlations that can be found in the classic methods. C1 [Villa, Chiara; Lynnerup, Niels] Univ Copenhagen, Dept Forens Med, Lab Biol Anthropol, DK-2100 Copenhagen, Denmark. [Buckberry, Jo] Univ Bradford, Biol Anthropol Res Ctr, Archaeol Sci, Bradford BD7 1DP, W Yorkshire, England. [Cattaneo, Cristina] Univ Milan, Dept Human Morphol, Forens Anthropol & Odontol Lab, LABANOF, I-20133 Milan, Italy. [Frohlich, Bruno] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Villa, C (reprint author), Univ Copenhagen, Dept Forens Med, Frederik Vs Vej 11, DK-2100 Copenhagen, Denmark. EM chiara.villa@sund.ku.dk RI Cattaneo, Cristina/M-2671-2016; OI Cattaneo, Cristina/0000-0003-0086-029X; Villa, Chiara/0000-0002-9967-8131 NR 30 TC 1 Z9 1 U1 2 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1198 EI 1556-4029 J9 J FORENSIC SCI JI J. Forensic Sci. PD MAY PY 2015 VL 60 IS 3 BP 556 EP 565 DI 10.1111/1556-4029.12689 PG 10 WC Medicine, Legal SC Legal Medicine GA CH4HI UT WOS:000353994200002 PM 25613520 ER PT J AU Batygin, K Deck, KM Holman, MJ AF Batygin, Konstantin Deck, Katherine M. Holman, Matthew J. TI DYNAMICAL EVOLUTION OF MULTI-RESONANT SYSTEMS: THE CASE OF GJ 876 SO ASTRONOMICAL JOURNAL LA English DT Article DE celestial mechanics; planet-disk interactions; planets and satellites: dynamical evolution and stability ID MEAN MOTION RESONANCES; EXTRASOLAR PLANETARY SYSTEMS; TURBULENT PROTOPLANETARY DISCS; OUTER ASTEROID BELT; SOLAR-SYSTEM; GIANT PLANETS; ORBITAL EVOLUTION; FREQUENCY-ANALYSIS; MAGNETIZED DISKS; CHAOTIC BEHAVIOR AB The GJ 876 system was among the earliest multi-planetary detections outside of the Solar System, and has long been known to harbor a resonant pair of giant planets. Subsequent characterization of the system revealed the presence of an additional Neptune mass object on an external orbit, locked in a three body Laplace mean motion resonance with the previously known planets. While this system is currently the only known extrasolar example of a Laplace resonance, it differs from the Galilean satellites in that the orbital motion of the planets is known to be chaotic. In this work, we present a simple perturbative model that illuminates the origins of stochasticity inherent to this system and derive analytic estimates of the Lyapunov time as well as the chaotic diffusion coefficient. We then address the formation of the multi-resonant structure within a protoplanetary disk and show that modest turbulent forcing in addition to dissipative effects is required to reproduce the observed chaotic configuration. Accordingly, this work places important constraints on the typical formation environments of planetary systems and informs the attributes of representative orbital architectures that arise from extended disk-driven evolution. C1 [Batygin, Konstantin; Deck, Katherine M.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Batygin, K (reprint author), CALTECH, Div Geol & Planetary Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA. NR 135 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2015 VL 149 IS 5 AR 167 DI 10.1088/0004-6256/149/5/167 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH5HC UT WOS:000354065200018 ER PT J AU Debes, JH Kilic, M Tremblay, PE Lopez-Morales, M Anglada-Escude, G Napiwotzki, R Osip, D Weinberger, A AF Debes, John H. Kilic, Mukremin Tremblay, Pier-Emmanuel Lopez-Morales, Mercedes Anglada-Escude, Guillem Napiwotzki, Ralph Osip, David Weinberger, Alycia TI A NEW MERGING DOUBLE DEGENERATE BINARY IN THE SOLAR NEIGHBORHOOD SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: close; binaries: spectroscopic; stars: individual (WD 1242-105); white dwarfs ID DA WHITE-DWARFS; SPY PROJECT; SPECTROSCOPIC IDENTIFICATION; GRAVITATIONAL-RADIATION; MAGELLAN-TELESCOPES; SKY SURVEY; MASS; STARS; EVOLUTION; CATALOG AB Characterizing the local space density of double degenerate (DD) binary systems is a complementary approach to broad sky surveys of DDs to determine the expected rates of WD binary mergers, in particular those that may evolve into other observable phenomena such as extreme helium stars, Am CVn systems, and SNe Ia. However, there have been few such systems detected in local space. We report here the discovery that WD1242-105, a nearby bright WD, is a double-line spectroscopic binary consisting of two degenerate DA WDs of similar mass and temperature, despite it previously having been spectroscopically characterized as a single degenerate. Follow-up photometry, spectroscopy, and trigonometric parallax have been obtained in an effort to determine the fundamental parameters of each component of this system. The binary has a mass ratio of 0.7 and a trigonometric parallax of 25.5 mas, placing it at a distance of 39 pc. The system's total mass is 0.95 M-circle dot and has an orbital period of 2.85 hr, making it the strongest known gravitational wave source (log h = -20.78) in the mHz regime. Because of its orbital period and total mass, WD1242-105 is predicted to merge via gravitational radiation on a timescale of 740 Myr, which will most likely not result in a catastrophic explosion. C1 [Debes, John H.; Tremblay, Pier-Emmanuel] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kilic, Mukremin] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. [Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. [Anglada-Escude, Guillem] Univ London, Sch Math Sci, Astron Unit, London E1 4NS, England. [Napiwotzki, Ralph] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Osip, David] Carnegie Inst Sci, Observ, Las Campanas Observ, La Serena, Chile. [Weinberger, Alycia] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. RP Debes, JH (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. OI Anglada Escude, Guillem/0000-0002-3645-5977 FU NSF [AST-1312678]; NASA [NNX14AF65G, HF-51329.01]; Association of Universities for Research in Astronomy via the European Space Agency; Space Telescope Science Institute FX The authors would like to thank the numerous support staff and scientists at the Las Campanas Observatory, who make world-class observing routine by their high level of help and knowledge. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. M.K. gratefully acknowledges the support of the NSF and NASA under grants AST-1312678 and NNX14AF65G, respectively. J.H.D. acknowledges support through a contract to the Association of Universities for Research in Astronomy via the European Space Agency. P.-E.T. is supported by NASA through Hubble Fellowship grant #HF-51329.01 awarded by the Space Telescope Science Institute. NR 59 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2015 VL 149 IS 5 AR 176 DI 10.1088/0004-6256/149/5/176 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH5HC UT WOS:000354065200027 ER PT J AU Hartman, JD Bayliss, D Brahm, R Bakos, GA Mancini, L Jordan, A Penev, K Rabus, M Zhou, G Butler, RP Espinoza, N de Val-Borro, M Bhatti, W Csubry, Z Ciceri, S Henning, T Schmidt, B Arriagada, P Shectman, S Crane, J Thompson, I Suc, V Csak, B Tan, TG Noyes, RW Lazar, J Papp, I Sari, P AF Hartman, J. D. Bayliss, D. Brahm, R. Bakos, G. A. Mancini, L. Jordan, A. Penev, K. Rabus, M. Zhou, G. Butler, R. P. Espinoza, N. de Val-Borro, M. Bhatti, W. Csubry, Z. Ciceri, S. Henning, T. Schmidt, B. Arriagada, P. Shectman, S. Crane, J. Thompson, I. Suc, V. Csak, B. Tan, T. G. Noyes, R. W. Lazar, J. Papp, I. Sari, P. TI HATS-6b: A WARM SATURN TRANSITING AN EARLY M DWARF STAR, AND A SET OF EMPIRICAL RELATIONS FOR CHARACTERIZING K AND M DWARF PLANET HOSTS SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HATS-6); techniques: photometric; techniques: spectroscopic ID LOW-MASS STARS; SEQUENCE ECLIPSING BINARIES; LOWER MAIN-SEQUENCE; HOT JUPITER; LIGHT CURVES; ABSOLUTE DIMENSIONS; EVOLUTIONARY MODELS; EXTRASOLAR PLANETS; STELLAR EVOLUTION; ACCURATE MASSES AB We report the discovery by the HATSouth survey of HATS-6b, an extrasolar planet transiting a V = 15.2 mag, i = 13.7 mag M1V star with a mass of 0.57 M-circle dot and a radius of 0.57 R-circle dot HATS-6b has a period of P = 3.3253 d, mass of M-p = 0.32 M-J, radius of R-p = 1.00 R-J, and zero-albedo equilibrium temperature of T-eq = 712.8 +/- 5.1 K. HATS-6 is one of the lowest mass stars known to host a close-in gas giant planet, and its transits are among the deepest of any known transiting planet system. We discuss the follow-up opportunities afforded by this system, noting that despite the faintness of the host star, it is expected to have the highest K-band S/N transmission spectrum among known gas giant planets with T-eq < 750 K. In order to characterize the star we present a new set of empirical relations between the density, radius, mass, bolometric magnitude, and V-, J-, H-and K-band bolometric corrections for main sequence stars with M < 0.80 M-circle dot, or spectral types later than K5. These relations are calibrated using eclipsing binary components as well as members of resolved binary systems. We account for intrinsic scatter in the relations in a self-consistent manner. We show that from the transit-based stellar density alone it is possible to measure the mass and radius of a similar to 0.6 M-circle dot star to similar to 7 and similar to 2% precision, respectively. Incorporating additional information, such as the V - K color, or an absolute magnitude, allows the precision to be improved by up to a factor of two. C1 [Hartman, J. D.; Bakos, G. A.; Penev, K.; de Val-Borro, M.; Bhatti, W.; Csubry, Z.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bayliss, D.; Zhou, G.; Schmidt, B.] Australian Natl Univ, Canberra, ACT, Australia. [Brahm, R.; Jordan, A.; Rabus, M.; Espinoza, N.; Suc, V.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago, Chile. [Brahm, R.; Jordan, A.; Espinoza, N.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Mancini, L.; Rabus, M.; Ciceri, S.; Henning, T.; Csak, B.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Butler, R. P.; Arriagada, P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Shectman, S.; Crane, J.; Thompson, I.] Carnegie Inst Sci, Observ, Pasadena, CA 91101 USA. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Hartman, JD (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM jhartman@astro.princeton.edu RI Butler, Robert/B-1125-2009; OI Jordan, Andres/0000-0002-5389-3944; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287; Bakos, Gaspar/0000-0001-7204-6727; Tan, Thiam-Guan/0000-0001-5603-6895; Hartman, Joel/0000-0001-8732-6166 FU NSF MRI [NSF/AST-0723074]; NASA [NNX09AB29G, NNX12AH91H, NNX14AE87G, NNX13AQ62G]; FONDECYT "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative, Chilean Ministry of Economy [1130857, IC120009]; CONICYT-PCHA/Doctorado Nacional; "Millenium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy [IC120009]; BASAL CATA PFB-06; FONDECYT postdoctoral fellowship [3120097]; ARC Laureate Fellowship Grant [FL0992131]; Robert Martin Ayers Sciences Fund; SIMBAD database, operated at CDS, Strasbourg, France; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations have been supported by NASA grants NNX09AB29G and NNX12AH91H, and follow-up observations receive partial support from grant NSF/AST-1108686. J.H. acknowledges support from NASA grant NNX14AE87G. K.P. acknowledges support from NASA grant NNX13AQ62G. A.J. acknowledges support from FONDECYT project 1130857, BASAL CATA PFB-06, and project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative, Chilean Ministry of Economy. R.B. and N.E. are supported by CONICYT-PCHA/Doctorado Nacional. R.B. and N.E. acknowledge additional support from project IC120009 "Millenium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy. V.S. acknowledges support form BASAL CATA PFB-06. M.R. acknowledges support from FONDECYT postdoctoral fellowship 3120097. This work is based on observations made with ESO Telescopes at the La Silla Observatory. This paper also uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. We acknowledge the use of the AAVSO Photometric All-sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD database, operated at CDS, Strasbourg, France. Operations at the MPG 2.2 m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. The imaging system GROND has been built by the high-energy group of MPE in collaboration with the LSW Tautenburg and ESO. We thank Regis Lachaume for his technical assistance during the observations at the MPG 2.2 m Telescope. We thank Helmut Steinle and Jochen Greiner for supporting the GROND observations presented in this manuscript. We are grateful to P. Sackett for her help in the early phase of the HATSouth project. NR 93 TC 16 Z9 17 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2015 VL 149 IS 5 AR 166 DI 10.1088/0004-6256/149/5/166 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH5HC UT WOS:000354065200017 ER PT J AU Keel, WC Maksym, WP Bennert, VN Lintott, CJ Chojnowski, SD Moiseev, A Smirnova, A Schawinski, K Urry, CM Evans, DA Pancoast, A Scott, B Showley, C Flatland, K AF Keel, William C. Maksym, W. Peter Bennert, Vardha N. Lintott, Chris J. Chojnowski, S. Drew Moiseev, Alexei Smirnova, Aleksandrina Schawinski, Kevin Urry, C. Megan Evans, Daniel A. Pancoast, Anna Scott, Bryan Showley, Charles Flatland, Kelsi TI HST IMAGING OF FADING AGN CANDIDATES. I. HOST-GALAXY PROPERTIES AND ORIGIN OF THE EXTENDED GAS SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 5792, NGC 5252, UGC 7342, UGC 11185, Mkn 1498) galaxies: interactions; galaxies: Seyfert ID DIGITAL-SKY-SURVEY; IONIZATION-CONE STRUCTURES; EMISSION-LINE REGIONS; NGC 5252; ELLIPTIC GALAXIES; HANNYS VOORWERP; SEYFERT-GALAXIES; STAR-FORMATION; IC 2497; QUASAR AB We present narrow- and medium-band Hubble Space Telescope imaging, with additional supporting ground-based imaging, spectrophotometry, and Fabry-Perot interferometric data, for eight galaxies identified as hosting a fading active galactic nucleus (AGN). These are selected to have AGN-ionized gas projected > 10 kpc from the nucleus and energy budgets with a significant shortfall of ionizing radiation between the requirement to ionize the distant gas and the AGN as observed directly, indicating fading of the AGN on approximate to 50,000 yr timescales. This paper focuses on the host-galaxy properties and origin of the gas. In every galaxy, we identify evidence of ongoing or past interactions, including tidal tails, shells, and warped or chaotic dust structures; a similarly selected sample of obscured AGNs with extended ionized clouds shares this high incidence of disturbed morphologies. Several systems show multiple dust lanes in different orientations, broadly fit by differentially precessing disks of accreted material viewed similar to 1.5 Gyr after its initial arrival. The host systems are of early Hubble type; most show nearly pure de Vaucouleurs surface brightness profiles and Sersic indices appropriate for classical bulges, with one S0 and one SB0 galaxy. The gas has a systematically lower metallicity than the nuclei; three systems have abundances uniformly well below solar, consistent with an origin in tidally disrupted low-luminosity galaxies, while some systems have more nearly solar abundances (accompanied by such signatures as multiple Doppler components), which may suggest redistribution of gas by outflows within the host galaxies themselves. These aspects are consistent with a tidal origin for the extended gas in most systems, although the ionized gas and stellar tidal features do not always match closely. Unlike extended emission regions around many radio-loud AGNs, these clouds are kinematically dominated by rotation, in some cases in warped disks. Outflows can play important kinematic roles only in localized regions near some of the AGNs. We find only a few sets of young star clusters potentially triggered by AGN outflows. In UGC 7342 and UGC 11185, multiple luminous star clusters are seen just within the projected ionization cones, potentially marking star formation triggered by outflows. As in the discovery example, Hanny's Voorwerp/IC 2497, there are regions in these clouds where the lack of a strong correlation between Ha surface brightness and ionization parameter indicates that there is unresolved fine structure in the clouds. Together with thin coherent filaments spanning several kpc, persistence of these structures over their orbital lifetimes may require a role for magnetic confinement. Overall, we find that the sample of fading AGNs occur in interacting and merging systems, that the very extended ionized gas is composed of tidal debris rather than galactic winds, and that these host systems are bulge-dominated and show no strong evidence of triggered star formation in luminous clusters. C1 [Keel, William C.; Maksym, W. Peter] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Bennert, Vardha N.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA. [Lintott, Chris J.] Univ Oxford, Astrophys, Chicago, IL 60605 USA. [Chojnowski, S. Drew] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Moiseev, Alexei; Smirnova, Aleksandrina] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia. [Schawinski, Kevin] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Evans, Daniel A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pancoast, Anna] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Scott, Bryan; Showley, Charles; Flatland, Kelsi] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA. [Scott, Bryan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Showley, Charles] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. RP Keel, WC (reprint author), Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. EM wkeel@ua.edu; wpmaksym@ua.edu; vbennert@calpoly.edu; cjl@astro.ox.ac.uk; kevin.schawinski@phys.ethz.ch RI Moiseev, Alexey/H-9391-2013; OI Maksym, Walter/0000-0002-2203-7889; Schawinski, Kevin/0000-0001-5464-0888; Urry, Meg/0000-0002-0745-9792; Keel, William/0000-0002-6131-9539 FU NASA [HST-GO-12525.01-A, HST-GO-12525.01-B]; Active Processes in Galactic and Extragalactic Objects basic research programme of the Department of Physical Sciences of the RAS [OFN-17]; Ministry of Education and Science of the Russian Federation [N14.619.21.0004, RFMEFI61914X0004]; University of Alabama Research Stimulation Program; National Science Foundation (NSF) Research at Undergraduate Institutions (RUI) grant [AST-1312296]; Leverhulme Trust; STFC Science in Society Program; Dynasty Foundation; President of the Russian Federation [MD3623.2015.2]; NASA Einstein Fellowship at Yale; Swiss National Science Foundation [PP00P2 138979/1]; Jim Gray Research Fund from Microsoft; National Aeronautics and Space Administration FX This work was supported by NASA through STScI grants HST-GO-12525.01-A and -B. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). This research has made use of NASA's Astrophysics Data System 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. We thank Linda Dressel for advice on setting up the observations, especially reducing intrusive reflections. Giles Novak provided useful pointers on magnetic fields in the ISM. Identification of this galaxy sample was possible through the efforts of nearly 200 Galaxy Zoo volunteers; we are grateful for their contributions, and thank once more the list of participants in Keel et al. (2012a). This work was partly supported by the Active Processes in Galactic and Extragalactic Objects basic research programme of the Department of Physical Sciences of the RAS OFN-17. The observations obtained with the 6 m telescope of the SAO of the RAS were carried out with the financial support of the Ministry of Education and Science of the Russian Federation (contract no. N14.619.21.0004, the project RFMEFI61914X0004). W.P. Maksym is grateful for support by the University of Alabama Research Stimulation Program. V.N. Bennert acknowledges assistance from a National Science Foundation (NSF) Research at Undergraduate Institutions (RUI) grant AST-1312296. Note that findings and conclusions do not necessarily represent views of the NSF. C.J. Lintott acknowledges funding from The Leverhulme Trust and the STFC Science in Society Program. A. Moiseev is also grateful for the financial support of the Dynasty Foundation and a grant from the President of the Russian Federation (MD3623.2015.2). K. Schawinski was supported by a NASA Einstein Fellowship at Yale, and gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2 138979/1. Galaxy Zoo was made possible by funding from a Jim Gray Research Fund from Microsoft and The Leverhulme Trust. 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. NR 51 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2015 VL 149 IS 5 AR 155 DI 10.1088/0004-6256/149/5/155 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH5HC UT WOS:000354065200006 ER PT J AU Landoni, M Massaro, F Paggi, A D'Abrusco, R Milisavljevic, D Masetti, N Smith, HA Tosti, G Chomiuk, L Strader, J Cheung, CC AF Landoni, M. Massaro, F. Paggi, A. D'Abrusco, R. Milisavljevic, D. Masetti, N. Smith, H. A. Tosti, G. Chomiuk, L. Strader, J. Cheung, C. C. TI OPTICAL SPECTROSCOPIC OBSERVATIONS OF gamma-RAY BLAZAR CANDIDATES. III. THE 2013/2014 CAMPAIGN IN THE SOUTHERN HEMISPHERE SO ASTRONOMICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; BL LACERTAE OBJECTS; ALL-SKY SURVEY; FERMI UNASSOCIATED SOURCES; POINT-SOURCE CATALOG; RADIO PROPERTIES; DATA RELEASE; SAMPLE; COUNTERPARTS AB We report the results of our exploratory program carried out with the southern Astrophysical Research telescope aimed at associating counterparts and establishing the nature of the Fermi Unidentified gamma-ray Sources (UGSs). We selected the optical counterparts of six UGSs from the Fermi catalog on the basis of our recently discovered tight connection between infrared and gamma-ray emission found for the gamma-ray blazars detected by the Wide-Field Infrared Survey Explorer in its all-sky survey. We perform for the first time a spectroscopic study of the low-energy counterparts of the Fermi UGSs, in the optical band, confirming the blazar-like nature of the whole sample. We also present new spectroscopic observations of six active galaxies of uncertain type associated with Fermi sources which appear to be BL Lac objects. Finally, we report the spectra collected for six known gamma-ray blazars belonging to the Roma BZCAT that were obtained to establish their nature or better estimate their redshifts. Two interesting cases of high redshift and extremely luminous BL Lac objects (z >= 1.18 and z >= 1.02, based on the detection of Mg II intervening systems) are also discussed. C1 [Landoni, M.] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Landoni, M.] Ist Nazl Fis Nucl, Rome, Italy. [Landoni, M.; Paggi, A.; D'Abrusco, R.; Milisavljevic, D.; Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Massaro, F.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Massaro, F.] Univ Turin, Dipartmento Fis, I-10125 Turin, Italy. [Masetti, N.] Ist Astrofis Spaziale & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy. [Tosti, G.] Univ Perugia, Dipartmento Fis, I-06123 Perugia, Italy. [Chomiuk, L.; Strader, J.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Landoni, M (reprint author), Osserv Astron Brera, INAF, Via Emilio Bianchi 46, I-23807 Merate, Italy. EM marco.landoni@brera.inaf.it RI D'Abrusco, Raffaele/L-2767-2016; Massaro, Francesco/L-9102-2016; Paggi, Alessandro/C-1219-2017 OI D'Abrusco, Raffaele/0000-0003-3073-0605; Massaro, Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410 FU NASA [NNX12AO97G, NNX13AP20G, DPR S-15633-Y]; NASA/JPL grant RSAs [1369566, 1369556, 1369565]; ASI/INAF [I/005/12/0]; National Aeronautics and Space Administration; National Science Foundation FX This investigation is supported by the NASA grants NNX12AO97G and NNX13AP20G. H.A.S. acknowledges partial support from NASA/JPL grant RSAs 1369566, 1369556, and 1369565. The work by G. Tosti is supported by the ASI/INAF contract I/005/12/0 while work by C.C.C. at NRL is supported in part by NASA DPR S-15633-Y. We are grateful to Dr. S. Points for his help to schedule, prepare, and perform the SOAR observations. Part of this work is based on archival data, software, or online services provided by the ASI Science Data Center. This research has made use of data obtained from the high-energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA's Goddard Space Flight Center; the SIMBAD database operated at CDS, Strasbourg, France; and the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Molonglo Observatory site manager, Duncan Campbell-Wilson, and the staff, Jeff Webb, Michael White, and John Barry, are responsible for the smooth operation of Molonglo Observatory Synthesis Telescope (MOST) and the day-to-day observing programme of SUMSS. The SUMSS survey is dedicated to Michael Large whose expertise and vision made the project possible. MOST is operated by the School of Physics with the support of the Australian Research Council and the Science Foundation for Physics within the University of Sydney. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the USNOFS Image and Catalogue Archive operated by the United States Naval Observatory, Flagstaff Station (http://www.nofs.navy.mil/data/fchpix/). TOPCAT16 (Taylor 2005) for the preparation and manipulation of the tabular data and the images. NR 56 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2015 VL 149 IS 5 AR 163 DI 10.1088/0004-6256/149/5/163 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH5HC UT WOS:000354065200014 ER PT J AU Mainzer, A Grav, T Bauer, J Conrow, T Cutri, RM Dailey, J Fowler, J Giorgini, J Jarrett, T Masiero, J Spahr, T Statler, T Wright, EL AF Mainzer, A. Grav, T. Bauer, J. Conrow, T. Cutri, R. M. Dailey, J. Fowler, J. Giorgini, J. Jarrett, T. Masiero, J. Spahr, T. Statler, T. Wright, E. L. TI SURVEY SIMULATIONS OF A NEW NEAR-EARTH ASTEROID DETECTION SYSTEM SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: numerical; minor planets, asteroids: general; surveys; techniques: image processing; telescopes ID INFRARED-ASTRONOMICAL-SATELLITE; MIDCOURSE-SPACE-EXPERIMENT; MAIN BELT ASTEROIDS; THERMAL-MODEL CALIBRATION; MINOR PLANET SURVEY; ALL-SKY SURVEY; WISE/NEOWISE OBSERVATIONS; PHYSICAL-CHARACTERIZATION; SURVEY-EXPLORER; NEOWISE AB We have carried out simulations to predict the performance of a new space-based telescopic survey operating at thermal infrared wavelengths that seeks to discover and characterize a large fraction of the potentially hazardous near-Earth asteroid (NEA) population. Two potential architectures for the survey were considered: one located at the Earth-Sun L1 Lagrange point, and one in a Venus-trailing orbit. A sample cadence was formulated and tested, allowing for the self-follow-up necessary for objects discovered in the daytime sky on Earth. Synthetic populations of NEAs with sizes as small as 140 m in effective spherical diameter were simulated using recent determinations of their physical and orbital properties. Estimates of the instrumental sensitivity, integration times, and slew speeds were included for both architectures assuming the properties of newly developed large-format 10 mu m HgCdTe detector arrays capable of operating at similar to 35 K. Our simulation included the creation of a preliminary version of a moving object processing pipeline suitable for operating on the trial cadence. We tested this pipeline on a simulated sky populated with astrophysical sources such as stars and galaxies extrapolated from Spitzer Space Telescope and Wide-field Infrared Explorer data, the catalog of known minor planets (including Main Belt asteroids, comets, Jovian Trojans, planets, etc.), and the synthetic NEA model. Trial orbits were computed for simulated position-time pairs extracted from the synthetic surveys to verify that the tested cadence would result in orbits suitable for recovering objects at a later time. Our results indicate that the Earth-Sun L1 and Venus-trailing surveys achieve similar levels of integral completeness for potentially hazardous asteroids larger than 140 m; placing the telescope in an interior orbit does not yield an improvement in discovery rates. This work serves as a necessary first step for the detailed planning of a next-generation NEA survey. C1 [Mainzer, A.; Bauer, J.; Giorgini, J.; Masiero, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ USA. [Bauer, J.; Conrow, T.; Cutri, R. M.; Dailey, J.; Fowler, J.; Jarrett, T.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Jarrett, T.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA. [Statler, T.] Ohio Univ, Inst Astrophys, Athens, OH 45701 USA. [Statler, T.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Wright, E. L.] Univ Calif Los Angeles, Dept Astron & Astrophys, Los Angeles, CA USA. RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. OI Masiero, Joseph/0000-0003-2638-720X; Cutri, Roc/0000-0002-0077-2305 FU National Aeronautics and Space Administration FX 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, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. We thank the referee, Dr. Alan Harris of Pasadena, for helpful suggestions that greatly improved the manuscript. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This 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. NR 91 TC 5 Z9 5 U1 1 U2 10 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 MAY PY 2015 VL 149 IS 5 AR 172 DI 10.1088/0004-6256/149/5/172 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH5HC UT WOS:000354065200023 ER PT J AU Overbeek, JC Friel, ED Jacobson, HR Johnson, CI Pilachowski, CA Meszaros, S AF Overbeek, Jamie C. Friel, Eileen D. Jacobson, Heather R. Johnson, Christian I. Pilachowski, Catherine A. Meszaros, Szabolcs TI NGC 7789: AN OPEN CLUSTER CASE STUDY (vol 149, 15, 2015) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Overbeek, Jamie C.; Friel, Eileen D.; Pilachowski, Catherine A.; Meszaros, Szabolcs] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Jacobson, Heather R.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Johnson, Christian I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Overbeek, JC (reprint author), Indiana Univ, Dept Astron, Swain West 319,727 East 3rd St, Bloomington, IN 47405 USA. EM joverbee@indiana.edu RI Meszaros, Szabolcs/N-2287-2014 OI Meszaros, Szabolcs/0000-0001-8237-5209 NR 4 TC 0 Z9 0 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2015 VL 149 IS 5 AR 177 DI 10.1088/0004-6256/149/5/177 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH5HC UT WOS:000354065200028 ER PT J AU Ricci, F Massaro, F Landoni, M D'Abrusco, R Milisavljevic, D Stern, D Masetti, N Paggi, A Smith, HA Tosti, G AF Ricci, F. Massaro, F. Landoni, M. D'Abrusco, R. Milisavljevic, D. Stern, D. Masetti, N. Paggi, A. Smith, Howard A. Tosti, G. TI OPTICAL SPECTROSCOPIC OBSERVATIONS OF GAMMA-RAY BLAZAR CANDIDATES. IV. RESULTS OF THE 2014 FOLLOW-UP CAMPAIGN SO ASTRONOMICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; radiation mechanisms: non-thermal ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; ALL-SKY SURVEY; FERMI UNASSOCIATED SOURCES; SOURCE CATALOG; RADIO; COUNTERPARTS; SAMPLE; I. AB The extragalactic gamma-ray sky is dominated by the emission arising from blazars, one of the most peculiar classes of radio-loud active galaxies. Since the launch of Fermi several methods were developed to search for blazars as potential counterparts of unidentified gamma-ray sources (UGSs). To confirm the nature of the selected candidates, optical spectroscopic observations are necessary. In 2013 we started a spectroscopic campaign to investigate gamma-ray blazar candidates selected according to different procedures. The main goals of our campaign are: (1) to confirm the nature of these candidates, and (2) whenever possible, determine their redshifts. Optical spectroscopic observations will also permit us to verify the robustness of the proposed associations and check for the presence of possible source class contaminants to our counterpart selection. This paper reports the results of observations carried out in 2014 in the northern hemisphere with Kitt Peak National Observatory and in the southern hemisphere with the Southern Astrophysical Research telescopes. We also report three sources observed with the Magellan and Palomar telescopes. Our selection of blazar-like sources that could be potential counterparts of UGSs is based on their peculiar infrared colors and on their combination with radio observations both at high and low frequencies (i.e., above and below similar to 1 GHz) in publicly available large radio surveys. We present the optical spectra of 27 objects. We confirm the blazar-like nature of nine sources that appear to be potential low-energy counterparts of UGSs. Then we present new spectroscopic observations of 10 active galaxies of uncertain type associated with Fermi sources, classifying all of them as blazars. In addition, we present the spectra for five known gamma-ray blazars with uncertain redshift estimates and three BL Lac candidates that were observed during our campaign. We also report the case for WISE J173052.85-035247.2, candidate counterpart of the source 2FGL J1730.6-0353, which has no radio counterpart in the major radio surveys. We confirm that our selection of gamma-ray blazars candidates can successfully indentify low-energy counterparts to Fermi unassociated sources and allow us to discover new blazars. C1 [Ricci, F.] Univ Rome Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. [Ricci, F.; D'Abrusco, R.; Milisavljevic, D.; Paggi, A.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Massaro, F.] Univ Turin, Dipartmento Fis, I-10125 Turin, Italy. [Massaro, F.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Landoni, M.] Osservatorio Astronomico Brera, INAF, I-23807 Merate, Italy. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Masetti, N.] Ist Astrofis Spaziale & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy. [Tosti, G.] Univ Perugia, Dipartmento Fis, I-06123 Perugia, Italy. RP Ricci, F (reprint author), Univ Rome Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. EM riccif@fis.uniroma3.it RI D'Abrusco, Raffaele/L-2767-2016; Massaro, Francesco/L-9102-2016; Paggi, Alessandro/C-1219-2017; OI D'Abrusco, Raffaele/0000-0003-3073-0605; Massaro, Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410; Ricci, Federica/0000-0001-5742-5980 FU NASA [NNX12AO97G, NNX13AP20G]; MIUR [PRIN 2010-2011, INAF-PRIN 2011]; NASA/JPL grant RSAs [1369566, 1369556, 1369565]; ASI/INAF [I/005/12/0]; National Science Foundation; Australian Research Council; Science Foundation for Physics within the University of Sydney; NASA; NSF FX We are grateful to. D. Hammer and S. Points for their help scheduling, preparing, and performing the KPNO and the SOAR observations, respectively. We are grateful to F. La Franca for the fruitful discussions that significantly improved the paper. This investigation is supported by the NASA grants NNX12AO97G and NNX13AP20G. F. Ricci acknowledges the grants MIUR PRIN 2010-2011 and INAF-PRIN 2011. H. A. Smith acknowledges partial support from NASA/JPL grant RSAs 1369566, 1369556, and 1369565. The work by G. Tosti is supported by the ASI/INAF contract I/005/12/0. Part of this work is based on archival data, software or online services provided by the ASI Science Data Center. This research has made use of data obtained from the high-energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA's Goddard Space Flight Center; the SIMBAD database operated at CDS, Strasbourg, France; the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA. Part of this work is based on the NVSS (NRAO VLA Sky Survey): the National Radio Astronomy Observatory is operated by Associated Universities, Inc., under contract with the National Science Foundation and on the VLA low-frequency Sky Survey (VLSS). The Molonglo Observatory site manager, D. Campbell-Wilson, and the staff, J. Webb, M. White and J. Barry, are responsible for the smooth operation of Molonglo Observatory Synthesis Telescope (MOST) and the day-to-day observing programme of SUMSS. The SUMSS survey is dedicated to M. Large whose expertise and vision made the project possible. The MOST is operated by the School of Physics with the support of the Australian Research Council and the Science Foundation for Physics within the University of Sydney. 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 NASA. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and NSF. This research has made use of the USNOFS Image and Catalogue Archive operated by the United States Naval Observatory, Flagstaff Station. 15 Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, the U.S. Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions.; r 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 JointInstitute 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-PlanckInstitute 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. The WENSS project was a collaboration between the Netherlands Foundation for Research in Astronomy and the Leiden Observatory. We acknowledge the WENSS team consisted of G. de Bruyn, Y. Tang, R. Rengelink, G. Miley, H. Rottgering, M. Bremer, M. Bremer, W. Brouw, E. Raimond and D. Fullagar for the extensive work aimed at producing the WENSS catalog. TOPCAT16 (Taylor 2005) for the preparation and manipulation of the tabular data and the images. The Aladin Java applet17 was used to create the finding charts reported in this paper (Bonnarel et al. 2000). It can be started from the CDS (Strasbourg, France), from the CFA (Harvard, USA), from the ADAC (Tokyo, Japan), from the IUCAA (Pune, India), from the UKADC (Cambridge, UK), or from the CADC (Victoria, Canada). NR 62 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2015 VL 149 IS 5 AR 160 DI 10.1088/0004-6256/149/5/160 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH5HC UT WOS:000354065200011 ER PT J AU Heineman, KD Caballero, P Morris, A Velasquez, C Serrano, K Ramos, N Gonzalez, J Mayorga, L Corre, MD Dalling, JW AF Heineman, Katherine D. Caballero, Pedro Morris, Arturo Velasquez, Carmen Serrano, Kiria Ramos, Nelly Gonzalez, Jonathan Mayorga, Luis Corre, Marife D. Dalling, James W. TI Variation in Canopy Litterfall Along a Precipitation and Soil Fertility Gradient in a Panamanian Lower Montane Forest SO BIOTROPICA LA English DT Article DE ectomycorrhizal trees; environmental gradients; fertilization experiment; Fortuna Forest Reserve; nutrient limitation; tropical forest productivity; tropical forest seasonality; tropical montane forest ID NET PRIMARY PRODUCTION; TROPICAL RAIN-FORESTS; PRIMARY PRODUCTIVITY; NUTRIENT LIMITATION; SEEDLING SURVIVAL; NITROGEN; PHOSPHORUS; BIOMASS; GROWTH; CARBON AB Fertilization experiments in tropical forests have shown that litterfall increases in response to the addition of one or more soil nutrients. However, the relationship between soil nutrient availability and litterfall is poorly defined along natural soil fertility gradients, especially in tropical montane forests. Here, we measured litterfall for two years in five lower montane 1-ha plots spanning a soil fertility and precipitation gradient in lower montane forest at Fortuna, Panama. Litterfall was also measured in a concurrent nitrogen fertilization experiment at one site. Repeated-measures ANOVA was used to test for site (or treatment), year, and season effects on vegetative, reproductive and total litterfall. We predicted that total litterfall, and the ratio of reproductive to leaf litterfall, would increase with nutrient availability along the fertility gradient, and in response to nitrogen addition. We found that total annual litterfall varied substantially among 1-ha plots (4.78Mg/ha/yr to 7.96Mg/ha/yr), and all but the most aseasonal plot showed significant seasonality in litterfall. However, litterfall accumulation did not track soil nutrient availability; instead forest growing on relatively infertile soil, but dominated by an ectomycorrhizal tree species, had the highest total litterfall accumulation. In the fertilization plots, significantly more total litter fell in nitrogen addition relative to control plots, but this increase in response to nitrogen (13%) was small compared to variation observed among 1-ha plots. These results suggest that while litterfall at Fortuna is nutrient-limited, compositional and functional turnover along the fertility gradient obscure any direct relationship between soil resource availability and canopy productivity. Resumen Se demostro con experimentos de fertilizacion en bosques tropicales incrementos en la caida de hojarasca asociados con la adicion de nutrientes; empero, se desconoce la relacion entre la disponibilidad de nutrientes del suelo con la produccion de hojarasca en gradientes naturales de fertilidad del suelo, especialmente en bosques montanos tropicales. Medimos la produccion de hojarasca durante dos anos en cinco parcelas (1-ha) en bosques montanos bajos, sobre gradientes de fertilidad y precipitacion y en un experimento paralelo de fertilizacion de nitrogeno en la Reserva Forestal Fortuna, Panama. Predijimos incrementos de hojarasca total y reproductiva con la disponibilidad de nutrientes en el gradiente de fertilidad del suelo y en respuesta a la adicion de nitrogeno (13%). Encontramos que la hojarasca total varia sustancialmente entre parcelas (4.78 Mg/ha/yr hasta 7.96 Mg/ha/yr) y que en todas las parcelas, excepto la menos estacional, hay estacionalidad significativa en la cantidad de hojarasca; pero, la acumulacion de hojarasca no coincide con la disponibilidad de nutrientes en el suelo, porque el bosque sobre suelo poco fertil con dominio de una especie ectomicorricica, presento mayor acumulacion de hojarasca. Las parcelas con fertilizacion tenian significativamente mas hojarasca que las control; pero, el incremento en hojarasca en respuesta a la adicion de nitrogeno fue menor respecto a la variacion entre parcelas. Los resultados sugieren que mientras la produccion de hojarasca en Fortuna es limitada por nutrientes, la variacion en la composicion de especies a traves de gradientes de fertilidad ocultan cualquier relacion directa entre la disponibilidad de nutrientes del suelo y la productividad del dosel. C1 [Heineman, Katherine D.; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Heineman, Katherine D.; Dalling, James W.] Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. [Caballero, Pedro; Morris, Arturo; Velasquez, Carmen; Serrano, Kiria; Ramos, Nelly; Gonzalez, Jonathan; Mayorga, Luis] Univ Autonoma Chiriqui, Dept Biol, David, Panama. [Corre, Marife D.] Univ Gottingen, Soil Sci Trop & Subtrop Ecosyst, Busgen Inst, D-37077 Gottingen, Germany. [Dalling, James W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Heineman, KD (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. EM kheineman@life.illinois.edu FU Government of Panama's Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) [COLO08]; Robert Bosch Foundation (Germany); Deutsche Forschungsgemeinschaft (German Research Foundation) [Co 749/1-1] FX We thank the Government of Panama's Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) for providing financial support for this project through the international research collaboration grant COLO08. The NITROF experiment was funded by the Robert Bosch Foundation (Germany) and the Deutsche Forschungsgemeinschaft (German Research Foundation, Co 749/1-1). ENEL Greenpower and the Smithsonian Tropical Research Institute provided logistic support and housing at Fortuna and the Autoridad Nacional del Ambiente (ANAM) provided research permits to undertake the study. NR 45 TC 2 Z9 2 U1 9 U2 32 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 MAY PY 2015 VL 47 IS 3 BP 300 EP 309 DI 10.1111/btp.12214 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CH4GZ UT WOS:000353993300006 ER PT J AU Remo, JL AF Remo, John L. TI The dilemma of nuclear energy in space SO BULLETIN OF THE ATOMIC SCIENTISTS LA English DT Article DE asteroids; comets; Fermi paradox; near-Earth object; NEO; nuclear explosives ID METEORITE AB Nuclear energy, used in weapons as well as for electricity generation, has the potential to destroy life on Earth. But it also has the potential to save life as we know it. Currently, nuclear explosives are the only technology with the capability to deflect, on relatively short notice, a large asteroid fragment or comet headed for a collision with Earth. However, a number of international treaties prohibit the use of nuclear explosives in space. The peaceful and critically effective use of nuclear energy to prevent a civilization-threatening collision is at odds with its potential for inducing a catastrophic thermonuclear war on Earth. The author uses the Fermi paradoxif there are extraterrestrial civilizations in our galaxy, why haven't they communicated with us?to examine the dichotomy of whether nuclear explosives are a barrier or a path to long-term human survival. C1 [Remo, John L.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Remo, John L.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Remo, John L.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Remo, JL (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 15 TC 1 Z9 1 U1 0 U2 1 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 MAY-JUN PY 2015 VL 71 IS 3 BP 38 EP 45 DI 10.1177/0096340215581359 PG 8 WC International Relations; Social Issues SC International Relations; Social Issues GA CH4TC UT WOS:000354024800007 ER PT J AU Fleming, CH Fagan, WF Mueller, T Olson, KA Leimgruber, P Calabrese, JM AF Fleming, C. H. Fagan, W. F. Mueller, T. Olson, K. A. Leimgruber, P. Calabrese, J. M. TI Rigorous home range estimation with movement data: a new autocorrelated kernel density estimator SO ECOLOGY LA English DT Article DE autocorrelation; Brownian bridge; home range; kernel density; minimum convex polygon; Mongolian gazelle, Procapra gutturosa; tracking data; utilization distribution ID SQUARES CROSS-VALIDATION; ANIMAL MOVEMENTS; TELEMETRY DATA; SPACE USE; INDEPENDENCE; SCALE; SIZE; TIME AB Quantifying animals' home ranges is a key problem in ecology and has important conservation and wildlife management applications. Kernel density estimation (KDE) is a workhorse technique for range delineation problems that is both statistically efficient and nonparametric. KDE assumes that the data are independent and identically distributed (IID). However, animal tracking data, which are routinely used as inputs to KDEs, are inherently autocorrelated and violate this key assumption. As we demonstrate, using realistically autocorrelated data in conventional KDEs results in grossly underestimated home ranges. We further show that the performance of conventional KDEs actually degrades as data quality improves, because autocorrelation strength increases as movement paths become more finely resolved. To remedy these flaws with the traditional KDE method, we derive an autocorrelated KDE (AKDE) from first principles to use autocorrelated data, making it perfectly suited for movement data sets. We illustrate the vastly improved performance of AKDE using analytical arguments, relocation data from Mongolian gazelles, and simulations based upon the gazelle's observed movement process. By yielding better minimum area estimates for threatened wildlife populations, we believe that future widespread use of AKDE will have significant impact on ecology and conservation biology. C1 [Fleming, C. H.; Mueller, T.; Olson, K. A.; Leimgruber, P.; Calabrese, J. M.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Fleming, C. H.; Fagan, W. F.; Mueller, T.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Mueller, T.] Senckenberg Gesell Naturforsch, Biodivers & Climate Res Ctr, D-60325 Frankfurt, Germany. [Mueller, T.] Goethe Univ Frankfurt, Dept Biol Sci, D-60438 Frankfurt, Germany. RP Fleming, CH (reprint author), Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM flemingc@si.edu RI Calabrese, Justin/B-9131-2012; Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 FU U.S. National Science Foundation [ABI 1062411]; Robert Bosch Foundation; Smithsonian Institution FX The project was funded by the U.S. National Science Foundation ABI 1062411. T. Mueller was funded by the Robert Bosch Foundation. C. H. Fleming was funded by a Smithsonian Institution postdoctoral fellowship. NR 32 TC 13 Z9 13 U1 12 U2 77 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD MAY PY 2015 VL 96 IS 5 BP 1182 EP 1188 DI 10.1890/14-2010.1 PG 7 WC Ecology SC Environmental Sciences & Ecology GA CH6BB UT WOS:000354119300004 PM 26236833 ER PT J AU He, Q Altieri, AH Cui, BS AF He, Qiang Altieri, Andrew H. Cui, Baoshan TI Herbivory drives zonation of stress-tolerant marsh plants SO ECOLOGY LA English DT Article DE coastal wetlands; competition; consumer control; crab grazing; distribution patterns; plant interactions; Salicornia europaea; salinity and waterlogging; salt marsh; Suaeda salsa; Yellow River Delta National Nature Reserve, China ID ENGLAND SALT-MARSH; SPARTINA-ALTERNIFLORA; SALICORNIA-EUROPAEA; RELATIVE IMPORTANCE; COMMUNITY STRUCTURE; BIOTIC INTERACTIONS; SALINITY GRADIENT; PHYSICAL FACTORS; SUAEDA-SALSA; BRENT GEESE AB Ecological studies of plant distributions along environmental gradients, such as plant zonation in salt marshes, have primarily focused on abiotic stress and plant interactions (competition and facilitation). A decades-old paradigm is that the stressful and benign boundaries of salt marsh plants are determined by abiotic stress and competition, respectively. Although consumers have long been recognized as mediating algal and sessile animal zonation in the rocky intertidal, their role in generating plant zonation in salt marshes remains largely unexplored. We examined the zonation of two annual succulents, Salicornia europaea and Suaeda salsa, along an elevation gradient in a northern Chinese salt marsh, with and without manipulating the common herbivorous crab Helice tientsinensis. Salicornia occupies waterlogged, low-salinity habitats, whereas Suaeda dominates non-waterlogged, hypersaline habitats at higher elevations. We first conducted a pot experiment crossing salinity, waterlogging, and competition, followed by a field experiment with removal of competitors, and found that neither waterlogging nor salinity stress explained the absence of either species from the other's zone, while Suaeda competitively excluded Salicornia from the upper nonwater-logged zone. We then conducted field and lab herbivory experiments, which showed that Helice preferentially grazed Suaeda at waterlogged low elevations and that Helice grazing on Suaeda increased with waterlogging. These results reveal that while competition plays a role in the zonation by excluding Salicornia from the upper Suaeda zone, crab grazing limits the success of Suaeda in the lower Salicornia zone. These findings challenge the idea that plant interactions and abiotic stress are sufficient to explain marsh zonation in all cases, and highlight an overlooked role of consumers, a role potentially general across diverse intertidal ecosystems. Future models of plant distributions should consider how consumer pressure interacts with plant interactions and abiotic stress across environmental gradients. C1 [He, Qiang; Cui, Baoshan] Beijing Normal Univ, Sch Environm, State Key Lab Water Environm Simulat, Beijing 100875, Peoples R China. [Altieri, Andrew H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. 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 OI He, Qiang/0000-0001-6481-0924 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] FX M. D. Bertness and B. R. Silliman provided comments and edits. F. Meng, Y. Cai, and X. Shao provided field and lab assistance. Comments by the editor and two anonymous reviewers improved the manuscript. Funding was provided by National Key Basic Research Program of China (2013CB430406), China National Funds for Distinguished Young Scientists (51125035), and National Science Foundation for Innovative Research Group (51121003). NR 72 TC 7 Z9 7 U1 7 U2 75 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD MAY PY 2015 VL 96 IS 5 BP 1318 EP 1328 DI 10.1890/14-0937.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA CH6BB UT WOS:000354119300016 PM 26236845 ER PT J AU Cunning, R Vaughan, N Gillette, P Capo, TR Mate, JL Baker, AC AF Cunning, R. Vaughan, N. Gillette, P. Capo, T. R. Mate, J. L. Baker, A. C. TI Dynamic regulation of partner abundance mediates response of reef coral symbioses to environmental change SO ECOLOGY LA English DT Article DE benefits and costs; context dependence; coral; density dependence; dinoflagellates; mutualism; optimality model; Pocillopora damicorni; population dynamics; Symbiodinium; symbiosis ID SYMBIODINIUM-MICROADRIATICUM; INTERSPECIFIC INTERACTIONS; STYLOPHORA-PISTILLATA; ELEVATED-TEMPERATURE; OCEAN ACIDIFICATION; THERMALLY TOLERANT; ALGAL SYMBIONTS; POPULATION; ZOOXANTHELLAE; DENSITY AB Regulating partner abundance may allow symbiotic organisms to mediate interaction outcomes, facilitating adaptive responses to environmental change. To explore the capacity for adaptive regulation in an ecologically important endosymbiosis, we studied the population dynamics of symbiotic algae in reef-building corals under different abiotic contexts. We found high natural variability in symbiont abundance in corals across reefs, but this variability converged to different symbiont-specific abundances when colonies were maintained under constant conditions. When conditions changed seasonally, symbiont abundance readjusted to new equilibria. We explain these patterns using an a priori model of symbiotic costs and benefits to the coral host, which shows that the observed changes in symbiont abundance are consistent with the maximization of interaction benefit under different environmental conditions. These results indicate that, while regulating symbiont abundance helps hosts sustain maximum benefit in a dynamic environment, spatiotemporal variation in abiotic factors creates a broad range of symbiont abundances (and interaction outcomes) among corals that may account for observed natural variability in performance (e.g., growth rate) and stress tolerance (e.g., bleaching susceptibility). This cost or benefit framework provides a new perspective on the dynamic regulation of reef coral symbioses and illustrates that the dependence of interaction outcomes on biotic and abiotic contexts may be important in understanding how diverse mutualisms respond to environmental change. C1 [Cunning, R.; Vaughan, N.; Gillette, P.; Capo, T. R.; Baker, A. C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Dept Marine Biol & Ecol, Miami, FL 33149 USA. [Mate, J. L.] Smithsonian Trop Res Inst, Panama City, Panama. [Baker, A. C.] Marine Program, Wildlife Conservat Soc, Bronx, NY 10460 USA. RP Cunning, R (reprint author), Univ Hawaii, Hawaii Inst Marine Biol, POB 1346, Kaneohe, HI 96744 USA. EM ross.cunning@gmail.com FU NSF [OCE-0527184]; Pew Fellowship in Marine Conservation; University of Miami Fellowship; NSF Graduate Research Fellowship FX We thank the STRI Marine Environmental Science Program for temperature data, and the UMCRF staff for maintaining corals. R. Silverstein, P. Jones, X. Serrano, R. Winter, A. Palacio, P. Kushlan, Q. Devlin, and S. McIlroy provided helpful comments on the manuscript. Support was provided by NSF (OCE-0527184) and a Pew Fellowship in Marine Conservation to A. C. Baker. R. Cunning was supported by a University of Miami Fellowship and a NSF Graduate Research Fellowship. NR 60 TC 3 Z9 4 U1 7 U2 59 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 MAY PY 2015 VL 96 IS 5 BP 1411 EP 1420 DI 10.1890/14-0449.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CH6BB UT WOS:000354119300024 PM 26236853 ER PT J AU Munk, Y Yanoviak, SP Koehl, MAR Dudley, R AF Munk, Yonatan Yanoviak, Stephen P. Koehl, M. A. R. Dudley, Robert TI The descent of ant: field-measured performance of gliding ants SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Aerodynamics; Arboreal ants; Rainforest; Biomechanics; Particle filter ID DIRECTED AERIAL DESCENT; CEPHALOTES-ATRATUS; FLYING LIZARDS; CANOPY ANTS; PEA APHIDS; EVOLUTION; ORIGINS; MANEUVERABILITY; LOCOMOTION; BEHAVIOR AB Gliding ants avoid predatory attacks and potentially mortal consequences of dislodgement from rainforest canopy substrates by directing their aerial descent towards nearby tree trunks. The ecologically relevant measure of performance for gliding ants is the ratio of net horizontal to vertical distance traveled over the course of a gliding trajectory, or glide index. To study variation in glide index, we measured three-dimensional trajectories of Cephalotes atratus ants gliding in natural rainforest habitats. We determined that righting phase duration, glide angle, and path directness all significantly influence variation in glide index. Unsuccessful landing attempts result in the ant bouncing off its target and being forced to make a second landing attempt. Our results indicate that ants are not passive gliders and that they exert active control over the aerodynamic forces they experience during their descent, despite their apparent lack of specialized control surfaces. C1 [Munk, Yonatan] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Munk, Yonatan; Koehl, M. A. R.; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Yanoviak, Stephen P.] Univ Louisville, Dept Biol, Louisville, KY 40292 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Munk, Y (reprint author), Univ Washington, Dept Biol, Seattle, WA 98195 USA. EM yomunk@uw.edu FU National Science Foundation [IOS-0837866, IOS-0843120]; Virginia G. and Robert E. Gill Chair FX This research was supported by grants from the National Science Foundation (IOS-0837866 to R.D. and IOS-0843120 to S.P.Y.), and the Virginia G. and Robert E. Gill Chair to M.A.R.K. NR 33 TC 5 Z9 5 U1 1 U2 10 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 MAY PY 2015 VL 218 IS 9 BP 1393 EP 1401 DI 10.1242/jeb.106914 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CH5ZV UT WOS:000354115800020 PM 25788722 ER PT J AU Gregoric, M Kuntner, M Blackledge, TA AF Gregoric, M. Kuntner, M. Blackledge, T. A. TI Does body size predict foraging effort? Patterns of material investment in spider orb webs SO JOURNAL OF ZOOLOGY LA English DT Article DE foraging investment; allometry; phylogenetic allometry; behavioral plasticity; behavioral compensation; trade-off; Zygiella ID ZYGIELLA-X-NOTATA; BUILDING BEHAVIOR; WEAVING SPIDERS; ARANEAE-ARANEIDAE; PHENOTYPIC PLASTICITY; STATIC ALLOMETRY; METABOLIC-RATES; PREY VARIATION; BLACK-WIDOW; BARRIER WEB AB Body size affects almost all aspects of animals' resource use, and its scaling syntheses are well established in most biological fields. In contrast, how behavioral variation scales with body size is understudied. Understanding how body size influences behavior is important as behavior responds more readily to natural selection than many other traits, and foraging effort is a critical behavioral trait. Web spiders are good models for studying foraging effort because webs are physical records of behaviors. Variability in web architectures is well documented, but how spider size scales with foraging effort and web performance is virtually unknown. Here, we investigate behavioral allometry at three phylogenetic scales - broadly across orb-weaving spiders, among a recent radiation of species, and among individuals within species. Conducting a meta-analysis across a wide range of orb weavers, we investigate how foraging effort scales with body size by measuring effort as the volumes of the three silk gland secretions used for building orb webs. We show that volumes of web material scale negatively allometrically with body size, and suggest silk investment is an important limiting factor in evolution of web performance and body size. To assess whether such broad evolutionary trends exist at finer phylogenetic scales, we investigated how foraging effort scales with body size in a group of five closely related Zygiella s.l. species (Araneidae). We find that the general scaling pattern across orb weavers is only partially confirmed. Finally, we examine patterns among individuals within each of the Zygiella species. We find different patterns of silk use in relation to body size, and show that both web architecture and silk investment need to be quantified to estimate total foraging effort. In conclusion, we find support for the prediction that behavioral traits scale differently to body size at different phylogenetic scales and at the individual level. C1 [Gregoric, M.; Kuntner, M.] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. [Gregoric, M.; Blackledge, T. A.] Univ Akron, Dept Biol, Akron, OH 44325 USA. [Gregoric, M.; Blackledge, T. A.] Univ Akron, Integrated Biosci Program, Akron, OH 44325 USA. [Kuntner, M.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kuntner, M.] Hubei Univ, Coll Life Sci, Wuhan, Hubei, Peoples R China. RP Gregoric, M (reprint author), Univ Akron, Dept Biol, Akron, OH 44325 USA. EM matjaz.gregoric@gmail.com FU Slovenian Research Agency [P1-0236, J1-2063]; National Science Foundation FX We thank T. Knapic, L. Rozman and M. Turjak for their help in the field, and A. Sensenig for providing raw data of already published work. We thank T. Gondek, A. Sensenig and J. Duff for their laboratory and logistic help, and S. Kralj-Fiser and C.P. Liao for help in statistics, as well as two anonymous reviewers for helpful comments. This research was funded by the Slovenian Research Agency (grants P1-0236, J1-2063 to M.K.) and National Science Foundation ( grants to T.A.B.). NR 72 TC 1 Z9 1 U1 4 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0952-8369 EI 1469-7998 J9 J ZOOL JI J. Zool. PD MAY PY 2015 VL 296 IS 1 BP 67 EP 78 DI 10.1111/jzo.12219 PG 12 WC Zoology SC Zoology GA CH4WV UT WOS:000354034900009 ER PT J AU Marchand, THJ AF Marchand, Trevor H. J. TI 'IT'S IN OUR BLOOD': MALI'S GRIOTS AND MUSICAL ENSKILMENT SO AFRICA LA English DT Article AB Film review of Da Kali: the pledge of the art of the griot (2013, 86 minutes) and D Farala A Kan: something has been added (2013, 69 minutes). French and Bamanankan, with English subtitles. Directed by Lucy Duran, edited by Michele Banal, and made with assistance from Lassana Diabate. C1 [Marchand, Trevor H. J.] Univ London, Social Anthropol, SOAS, London WC1E 7HU, England. RP Marchand, THJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Mud Masons Mali, Washington, DC 20560 USA. EM tm6@soas.ac.uk NR 0 TC 0 Z9 0 U1 1 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0001-9720 EI 1750-0184 J9 AFRICA JI Africa PD MAY PY 2015 VL 85 IS 2 BP 356 EP 364 DI 10.1017/S0001972015000054 PG 9 WC Anthropology; Area Studies SC Anthropology; Area Studies GA CG7SJ UT WOS:000353505000008 ER PT J AU Schultz, TR Sosa-Calvo, J Brady, SG Lopes, CT Mueller, UG Bacci, M Vasconcelos, HL AF Schultz, Ted R. Sosa-Calvo, Jeffrey Brady, Sean G. Lopes, Caue T. Mueller, Ulrich G. Bacci, Mauricio, Jr. Vasconcelos, Heraldo L. TI The Most Relictual Fungus-Farming Ant Species Cultivates the Most Recently Evolved and Highly Domesticated Fungal Symbiont Species SO AMERICAN NATURALIST LA English DT Article DE Attini; coevolution; fungus-farming ants; Leucocoprineae; symbiosis ID LEAF-CUTTING ANTS; GROWING ANTS; PHYLOGENETIC ANALYSES; CUTTER ANTS; ATTINE ANT; BACTERIA; FORMICIDAE; COEVOLUTION; EVOLUTION; PSEUDONOCARDIA AB Fungus-farming (attine) ant agriculture is made up of five known agricultural systems characterized by remarkable symbiont fidelity in which five phylogenetic groups of ants faithfully cultivate five phylogenetic groups of fungi. Here we describe the first case of a lower-attine ant cultivating a higher-attine fungus based on our discovery of a Brazilian population of the relictual fungus-farming ant Apterostigma megacephala, known previously from four stray specimens from Peru and Colombia. We find that A. megacephala is the sole surviving representative of an ancient lineage that diverged similar to 39 million years ago, very early in the similar to 55-million-year evolution of fungus-farming ants. Contrary to all previously known patterns of ant-fungus symbiont fidelity, A. megacephala cultivates Leucoagaricus gongylophorus, a highly domesticated fungal cultivar that originated only 2-8 million years ago in the gardens of the highly derived and recently evolved (similar to 12 million years ago) leaf-cutting ants. Because no other lower fungus-farming ant is known to cultivate any of the higher-attine fungi, let alone the leaf-cutter fungus, A. megacephala may provide important clues about the biological mechanisms constraining the otherwise seemingly obligate ant-fungus associations that characterize attine ant agriculture. C1 [Schultz, Ted R.; Sosa-Calvo, Jeffrey; Brady, Sean G.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Sosa-Calvo, Jeffrey] Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. [Lopes, Caue T.; Vasconcelos, Heraldo L.] Univ Fed Uberlandia, Inst Biol, BR-38405320 Uberlandia, MG, Brazil. [Mueller, Ulrich G.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Bacci, Mauricio, Jr.] Univ Estadual Paulista, Ctr Estudos Insetos Sociais, BR-13506900 Sao Paulo, Brazil. RP Schultz, TR (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, NHB 169, Washington, DC 20560 USA. EM schultzt@si.edu; sossajef@si.edu FU National Science Foundation (NSF) [DEB-0949689]; National Museum of Natural History (NMNH); Smithsonian Institution Scholarly Studies Program; NMNH; Cosmos Club Foundation; NSF [DEB-0919519]; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) [2011/50226-0]; CNPq [311562/2012-4, 487639/2012-0] FX We are grateful to R. C. F. Brandao and R. Rosa da Silva for alerting us to the occurrence of Apterostigma megacephala in Carajas; to F. Drumond Martins and E. Esteves of Instituto Chico Mendes de Conservacao da Biodiversidade (ICMBio) at Floresta Nacional de Carajas for their help and guidance; and to E. Okonski for collections and research support. For permission to conduct field research, we thank the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq; Processo EXC 039/07; Portarias 267-359), the Instituto Brasileiro do Meio Ambiente e dos Recursos Naturais Renovaveis (IBAMA), and the ICMBio (permits 14789-1, 14789-2). T.R.S. and J.S.-C. were supported by National Science Foundation (NSF) grant DEB-0949689 and the National Museum of Natural History (NMNH) Small Grants program; T.R.S. by the Smithsonian Institution Scholarly Studies Program; J.S.-C. by an NMNH Peter Buck Predoctoral Fellowship and a Max and Vera Britton Environmental Science Award (Cosmos Club Foundation); U.G.M. by NSF DEB-0919519; and M.B. by Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP; 2011/50226-0) and CNPq (311562/2012-4 and 487639/2012-0). NR 86 TC 4 Z9 4 U1 16 U2 44 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 MAY PY 2015 VL 185 IS 5 BP 693 EP 703 DI 10.1086/680501 PG 11 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA CG7BH UT WOS:000353456600015 PM 25905511 ER PT J AU Sanna, A Menten, KM Carrasco-Gonzalez, C Reid, MJ Ellingsen, SP Brunthaler, A Moscadelli, L Cesaroni, R Krishnan, V AF Sanna, A. Menten, K. M. Carrasco-Gonzalez, C. Reid, M. J. Ellingsen, S. P. Brunthaler, A. Moscadelli, L. Cesaroni, R. Krishnan, V. TI THE ENVIRONMENT OF THE STRONGEST GALACTIC METHANOL MASER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: kinematics and dynamics; masers; stars: formation; stars: individual (G009.62+00.20); techniques: high angular resolution ID STAR-FORMING REGIONS; TRIGONOMETRIC PARALLAXES; PERIODIC VARIABILITY; COMPLEX G9.62+0.19; MASSIVE STARS; CORE; HOT; EMISSION; OUTFLOW; FLARES AB The high-mass star-forming site G009.62+00.20 E hosts the 6.7 GHz methanol maser source with the greatest flux density in the Galaxy which has been flaring periodically over the last 10 yr. We performed high-resolution astrometric measurements of the CH3OH, H2O, and OH maser emission and 7 mm continuum in the region. The radio continuum emission was resolved in two sources separated by 1300 AU. The CH3OH maser cloudlets are distributed along two north-south ridges of emission to the east and west of the strongest radio continuum component. This component likely pinpoints a massive young stellar object which heats up its dusty envelope, providing a constant IR pumping for the Class II CH3OH maser transitions. We suggest that the periodic maser activity may be accounted for by an independent, pulsating, IR radiation field provided by a bloated protostar in the vicinity of the brightest masers. We also report the discovery of an elliptical distribution of CH3OH maser emission in the region of periodic variability. C1 [Sanna, A.; Menten, K. M.; Carrasco-Gonzalez, C.; Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Carrasco-Gonzalez, C.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ellingsen, S. P.; Krishnan, V.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Moscadelli, L.; Cesaroni, R.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. RP Sanna, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM asanna@mpifr-bonn.mpg.de RI Ellingsen, Simon/J-7754-2014; OI Ellingsen, Simon/0000-0002-1363-5457; Moscadelli, Luca/0000-0002-8517-8881; Cesaroni, Riccardo/0000-0002-2430-5103 FU ERC Advanced Grant GLOSTAR [247078]; Commonwealth of Australia FX Comments from an anonymous referee are gratefully acknowledged. This work has been supported by the ERC Advanced Grant GLOSTAR under grant agreement No. 247078. 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 licence. The Australia Telescope Compact Array (/Parkes radio telescope/Mopra radio telescope/Long Baseline Array) is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The VLBA and JVLA are operated by the National Radio Astronomy Observatory (NRAO). The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 25 TC 4 Z9 4 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 1 PY 2015 VL 804 IS 1 AR L2 DI 10.1088/2041-8205/804/1/L2 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH1YK UT WOS:000353819400002 ER PT J AU van Dokkum, PG Romanowsky, AJ Abraham, R Brodie, JP Conroy, C Geha, M Merritt, A Villaume, A Zhang, JL AF van Dokkum, Pieter G. Romanowsky, Aaron J. Abraham, Roberto Brodie, Jean P. Conroy, Charlie Geha, Marla Merritt, Allison Villaume, Alexa Zhang, Jielai TI SPECTROSCOPIC CONFIRMATION OF THE EXISTENCE OF LARGE, DIFFUSE GALAXIES IN THE COMA CLUSTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: individual (Coma); galaxies: evolution; galaxies: structure ID SURFACE BRIGHTNESS GALAXIES; INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; DWARF GALAXIES; LOCAL GROUP; EVOLUTION; PROFILES; FEEDBACK; DENSITY; SYSTEMS AB We recently identified a population of low surface brightness objects in the field of the Z = 0.023 Coma cluster, using the Dragonfly Telephoto Array. Here we present Keck spectroscopy of one of the largest of these "ultradiffuse galaxies" (UDGs), confirming that it is a member of the cluster. The galaxy has prominent absorption features, including the Ca H+K lines and the G-band, and no detected emission lines. Its radial velocity of cz = 6280 +/- 120 km s(-1) is within the 1 sigma velocity dispersion of the Coma cluster. The galaxy has an effective radius of 4.3 +/- 0.3 kpc and a Sersic index of 0.89 +/- 0.06, as measured from Keck imaging. We find no indications of tidal tails or other distortions, at least out to a radius of similar to 2r(e). We show that UDGs are located in a previously sparsely populated region of the size magnitude plane of quiescent stellar systems, as they are similar to 6 mag fainter than normal early-type galaxies of the same size. It appears that the luminosity distribution of large quiescent galaxies is not continuous, although this could largely be due to selection effects. Dynamical measurements are needed to determine whether the dark matter halos of UDGs are similar to those of galaxies with the same luminosity or to those of galaxies with the same size. C1 [van Dokkum, Pieter G.; Geha, Marla; Merritt, Allison] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Romanowsky, Aaron J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Romanowsky, Aaron J.; Brodie, Jean P.; Villaume, Alexa] Univ Calif Observ, Santa Cruz, CA 95064 USA. [Abraham, Roberto; Zhang, Jielai] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Dokkum, PG (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA. OI Villaume, Alexa/0000-0003-1887-0621; Zhang, Jielai/0000-0001-5310-4186 FU NSF [AST-1312376, AST-1109878, AST-1211995]; Dunlap Institute; University of Toronto FX 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. We thank Nicola Pastorello for an independent check of the redshift measurement. Support from NSF grants AST-1312376, AST-1109878, and AST-1211995 is gratefully acknowledged. We also acknowledge the support of the Dunlap Institute, funded through an endowment established by the David Dunlap family and the University of Toronto. NR 34 TC 16 Z9 16 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 MAY 1 PY 2015 VL 804 IS 1 AR L26 DI 10.1088/2041-8205/804/1/L26 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CH1YK UT WOS:000353819400026 ER PT J AU Zuo, YJ Wen, J Ma, JS Zhou, SL AF Zuo, Yun-Juan Wen, Jun Ma, Jin-Shuang Zhou, Shi-Liang TI Evolutionary radiation of the Panax bipinnatifidus species complex (Araliaceae) in the Sino-Himalayan region of eastern Asia as inferred from AFLP analysis SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Article DE Araliaceae; evolutionary radiation; geographic isolation; Panax; Panax bipinnatifidus; Sino-Himalayan region ID QINGHAI-TIBETAN PLATEAU; MULTILOCUS GENOTYPE DATA; PHYLOGENETIC-RELATIONSHIPS; POPULATION-STRUCTURE; GENE FLOW; ASTERACEAE; DNA; NUCLEAR; PLANTS; SEQUENCES AB The Panax bipinnatifidus species complex (P. bipinnatifidus and its close relatives) in the Sino-Himalayan region has been taxonomically difficult. Evolutionary analyses using amplified fragment length polymorphism (AFLP) markers were carried out on 125 individuals representing 11 populations of the P. bipinnatifidus species complex and one population of P. stipuleanatus Tsai & Feng as an outgroup. The populations from the eastern Himalayan region, sampled from Nepal and eastern Tibet, formed two main groups in the neighbor-joining and split network analyses. The Pailong population (Tibet-PL) in eastern Tibet showed a highly distinct AFLP profile and was placed as the most basally branched group in the neighbor-joining tree. The remaining Himalayan populations showed three subgroups: the Nepal-HB and Nepal-HS subgroup, the Nepal HH subgroup, and the Tibet-BY subgroup. The three Himalayan subgroups had very limited gene flow among them and showed subtle morphological differences. The populations in eastern, central, and western China showed clear geographic patterns and can be sorted into several geographical groups. Each major group in the species complex has strong bootstrap support, but relationships among them are poorly resolved, which is consistent with a pattern of evolutionary radiation. The strong geographic grouping, high Nei's population differentiation index, and limited gene flow among populations in different regions support the importance of geographic isolation in the diversification of the P. bipinnatifidus species complex in the Sino-Himalayan region. C1 [Zuo, Yun-Juan; Ma, Jin-Shuang] Chinese Acad Sci, Shanghai Chenshan Bot Garden, Shanghai Chenshan Plant Sci Res Ctr, Shanghai 201602, Peoples R China. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. [Zhou, Shi-Liang] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. RP Zhou, SL (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. EM wenj@si.edu; slzhou@ibcas.ac.cn FU Institute of Botany, Chinese Academy of Sciences; National Natural Science Foundation of China [30370154]; John D. and Catherine T. MacArthur Foundation FX This work was supported by a collaborative grant from the Institute of Botany, Chinese Academy of Sciences, a National Natural Science Foundation of China grant (Grant No. 30370154) to S. L. Zhou, and the John D. and Catherine T. MacArthur Foundation to J. Wen. The authors are grateful to K. J. Malla, Z. L. Nie, Hang Sun, and Sugong Wu for their assistances during the sample collections. We also thank Professor Jian-Quan Liu for constructive comments. NR 57 TC 0 Z9 0 U1 3 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD MAY PY 2015 VL 53 IS 3 BP 210 EP 220 DI 10.1111/jse.12119 PG 11 WC Plant Sciences SC Plant Sciences GA CH4IO UT WOS:000353997400002 ER PT J AU Harris, AJ Lutz, S Acevedo, P Wen, J AF Harris, A. J. Lutz, Sue Acevedo, Pedro Wen, Jun TI The utility of the morphological variation of pollen for resolving the evolutionary history of Billia (subfam. Hippocastanoideae, Sapindaceae) SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Article DE Aesculus; Billia; buckeyes; Hippocastanaceae; Hippocastanoideae; horsechestnuts; pollen; Sapindaceae ID AESCULUS L.; DNA-SEQUENCES; BIOGEOGRAPHY; PHYLOGENY; ORIGIN; FAMILY; GENUS AB In this study, we examined the utility of pollen morphology for resolving questions about the evolutionary history of Billia, which is a poorly known genus of Neotropical trees. Billia has been traditionally circumscribed with two species and treated as sister to Aesculus L. However, the number of species in Billia is uncertain, because the genus exhibits abundant morphological diversity but little discontinuous variation. Therefore, Billia may be monotypic and highly polymorphic, or it may have two species with blurred boundaries due to incipient speciation and/or hybridization. Moreover, one recent molecular phylogenetic study shows Billia nested within Aesculus. Our work sought to address the following questions: (i) Are there discontinuities in the pollen of Billia that may suggest species boundaries? (ii) Does the pollen of Billia show evidence for inter-specific hybridization? (iii) Do the exine morphology and size of pollen in Billia differ from those in Aesculus? Our results from scanning electron microscopy showed that pollen exine morphology is not taxonomically informative in Billia but that there are significant differences in pollen size between red- and white-flowered individuals. Thus, our pollen data support the utility of flower color in Billia for species delimitation. Our assessments of pollen viability do not support hybridization in the genus, but cannot be used to rule it out. Finally, pollen exine morphology may lend some support to an evolutionary origin of Billia within eastern North American Aesculus. In contrast, data on pollen size suggest that Billia may belong in a topological position outside of Aesculus. C1 [Harris, A. J.] Oklahoma State Univ, Dept Bot, Phys Sci 301, Stillwater, OK 74074 USA. [Lutz, Sue; Acevedo, Pedro; Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. RP Harris, AJ (reprint author), Oklahoma State Univ, Dept Bot, Phys Sci 301, Stillwater, OK 74074 USA. EM aj.harris@okstate.edu NR 40 TC 2 Z9 2 U1 1 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD MAY PY 2015 VL 53 IS 3 BP 228 EP 238 DI 10.1111/jse.12130 PG 11 WC Plant Sciences SC Plant Sciences GA CH4IO UT WOS:000353997400004 ER PT J AU Lu, YJ Chen, C Wang, RH Egan, AN Fu, CX AF Lu, Yi-Jun Chen, Chuan Wang, Rui-Hong Egan, Ashley N. Fu, Cheng-Xin TI Effects of domestication on genetic diversity in Chimonanthus praecox: Evidence from chloroplast DNA and amplified fragment length polymorphism data SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Article DE AFLP; Chimonanthus praecox; cpDNA; domestication; geographic origin ID BARLEY HORDEUM-VULGARE; CULTIVATED RICE; CROP DOMESTICATION; ORYZA-RUFIPOGON; WILD RELATIVES; AFLP ANALYSIS; ORIGIN; PHYLOGEOGRAPHY; MARKERS; POPULATIONS AB Chimonanthus praecox (L.) Link is a widely cultivated endemic winter-flowering plant in China that has a long cultivation history. Genetic diversity and genetic structure were compared between wild and cultivated groups to reveal the geographic origin of the cultivated genotypes using chloroplast DNA (cpDNA) sequences and amplified fragment length polymorphism (AFLP) markers. Nine haplotypes were identified using three combined chloroplast fragments. Based on chloroplast data, the wild group showed greater genetic variation and genetic differentiation and a lower measure of gene flow compared to the cultivated group. The AFLP markers also supported this trend. More than 40% of the cpDNA haplotypes were shared between wild and cultivated groups, with shared haplotypes originating from multiple wild populations, suggesting multiple origins of cultivated plants. Moreover, principal coordinate analysis, UPGMA, and structure analysis of AFLP markers revealed that two wild populations clustered with most of the cultivated populations of Ch. praecox, suggesting that most of the cultivated populations mainly originated from these two populations. The combined cpDNA and AFLP results indicated that modern cultivated Ch. praecox experienced multiple events of origin involving two geographic origins, eastern China (Tianmu Mountain) and southwestern China (the border of Hunan-Guangxi-Sichuan-Guizhou). C1 [Lu, Yi-Jun; Wang, Rui-Hong; Fu, Cheng-Xin] Zhejiang Univ, Coll Life Sci, Key Lab Conservat Biol Endangered Wildlife, Minist Educ, Hangzhou 310058, Zhejiang, Peoples R China. [Lu, Yi-Jun; Chen, Chuan] Hangzhou Bot Garden, Hangzhou 310013, Zhejiang, Peoples R China. [Egan, Ashley N.] Smithsonian Inst, Dept Bot, Natl Museum Natl Hist, Washington, DC 20013 USA. RP Fu, CX (reprint author), Zhejiang Univ, Coll Life Sci, Key Lab Conservat Biol Endangered Wildlife, Minist Educ, Hangzhou 310058, Zhejiang, Peoples R China. EM cxfu@zju.edu.cn FU Hangzhou Municipal Bureau of Landscape and Cultural Relics [200801] FX We thank Dr. Jun Liu from China Jiliang University for providing assistance with experiments. This work was supported by grants from Hangzhou Municipal Bureau of Landscape and Cultural Relics (Grant No. 200801). NR 78 TC 0 Z9 0 U1 1 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD MAY PY 2015 VL 53 IS 3 BP 239 EP 251 DI 10.1111/jse.12134 PG 13 WC Plant Sciences SC Plant Sciences GA CH4IO UT WOS:000353997400005 ER PT J AU Finnegan, S Anderson, SC Harnik, PG Simpson, C Tittensor, DP Byrnes, JE Finkel, ZV Lindberg, DR Liow, LH Lockwood, R Lotze, HK McClain, CR McGuire, JL O'Dea, A Pandolfi, JM AF Finnegan, Seth Anderson, Sean C. Harnik, Paul G. Simpson, Carl Tittensor, Derek P. Byrnes, Jarrett E. Finkel, Zoe V. Lindberg, David R. Liow, Lee Hsiang Lockwood, Rowan Lotze, Heike K. McClain, Craig R. McGuire, Jenny L. O'Dea, Aaron Pandolfi, John M. TI Paleontological baselines for evaluating extinction risk in the modern oceans SO SCIENCE LA English DT Article ID MARINE BIODIVERSITY; LATITUDINAL GRADIENTS; SPECIES RICHNESS; GLOBAL PATTERNS; DIVERSITY; CONSERVATION; HOTSPOTS; VULNERABILITY; ASSEMBLAGES; ECOSYSTEMS AB Marine taxa are threatened by anthropogenic impacts, but knowledge of their extinction vulnerabilities is limited. The fossil record provides rich information on past extinctions that can help predict biotic responses. We show that over 23 million years, taxonomic membership and geographic range size consistently explain a large proportion of extinction risk variation in six major taxonomic groups. We assess intrinsic risk-extinction risk predicted by paleontologically calibrated models-for modern genera in these groups. Mapping the geographic distribution of these genera identifies coastal biogeographic provinces where fauna with high intrinsic risk are strongly affected by human activity or climate change. Such regions are disproportionately in the tropics, raising the possibility that these ecosystems may be particularly vulnerable to future extinctions. Intrinsic risk provides a prehuman baseline for considering current threats to marine biodiversity. C1 [Finnegan, Seth; Lindberg, David R.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Anderson, Sean C.] Simon Fraser Univ, Dept Biol Sci, Burnaby, BC V5A 1S6, Canada. [Harnik, Paul G.] Franklin & Marshall Coll, Dept Earth & Environm, Lancaster, PA 17604 USA. [Simpson, Carl] Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Tittensor, Derek P.] United Nations Environm Programme World Conservat, Cambridge CB3 0DL, England. [Tittensor, Derek P.] Microsoft Res, Sci Computat Lab, Cambridge CB1 2FB, England. [Tittensor, Derek P.; Lotze, Heike K.] Dalhousie Univ, Dept Biol, Halifax, NS B3H 4R2, Canada. [Byrnes, Jarrett E.] Univ Massachusetts, Dept Biol, Boston, MA 02125 USA. [Finkel, Zoe V.] Mt Allison Univ, Environm Sci Program, Sackville, NB E4L 1A5, Canada. [Liow, Lee Hsiang] Univ Oslo, Dept Biosci, Ctr Ecol & Evolutionary Synth, N-0316 Oslo, Norway. [Lockwood, Rowan] Coll William & Mary, Dept Geol, Williamsburg, VA 23187 USA. [McClain, Craig R.] Natl Evolutionary Synth Ctr, Durham, NC 27705 USA. [McGuire, Jenny L.] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. [O'Dea, Aaron] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Pandolfi, John M.] Univ Queensland, Sch Biol Sci, Australian Res Council, Ctr Excellence Coral Reef Studies, St Lucia, Qld 4072, Australia. RP Finnegan, S (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM sethf@berkeley.edu RI Liow, Lee Hsiang/E-3481-2010; McGuire, Jenny/G-8819-2011; Pandolfi, John/A-3121-2009; OI Liow, Lee Hsiang/0000-0002-3732-6069; McGuire, Jenny/0000-0002-0663-6902; Pandolfi, John/0000-0003-3047-6694; Byrnes, Jarrett/0000-0002-9791-9472; McClain, Craig/0000-0003-0574-428X FU National Evolutionary Synthesis Center (NSF) [EF-0905606]; Natural Sciences and Engineering Research Council of Canada; National System of Investigators of the National Secretariat for Science, Technology and Innovation of Panama; Australian Research Council Centre of Excellence for Coral Reef Studies; Deutsche Forschungsgemeinschaft [KI 806/7-1] FX This work is a product of the Determinants of Extinction in Ancient and Modern Seas Working Group supported by the National Evolutionary Synthesis Center (NSF grant EF-0905606). Additional support was provided by the Natural Sciences and Engineering Research Council of Canada (to H.K.L., S.C.A., and Z.V.F.); the National System of Investigators of the National Secretariat for Science, Technology and Innovation of Panama (to A.O.); the Australian Research Council Centre of Excellence for Coral Reef Studies (to J.M.P.); and the Deutsche Forschungsgemeinschaft (grant KI 806/7-1 to C.S.). We thank the contributors to the Paleobiology Database and to OBIS. We also thank four anonymous reviewers for insightful comments that substantially improved the quality of the manuscript. This article is Paleobiology Database contribution no. 227. All scripts and data used to conduct analyses are available at https://github.com/seananderson/paleobaselines NR 43 TC 18 Z9 18 U1 9 U2 39 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 MAY 1 PY 2015 VL 348 IS 6234 BP 567 EP 570 DI 10.1126/science.aaa6635 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH1JR UT WOS:000353778100040 PM 25931558 ER PT J AU Chirchir, H AF Chirchir, Habiba TI A Comparative Study of Trabecular Bone Mass Distribution in Cursorial and Non-Cursorial Limb Joints SO Anatomical Record-Advances in Integrative Anatomy and Evolutionary Biology LA English DT Article DE cursors; felids; cercopithecines; hominids; trabecular bone mass ID CHEETAH ACINONYX-JUBATUS; NATURAL PENDULAR PERIOD; ENERGETIC COST; TRADE-OFFS; LOCOMOTION; EVOLUTION; MAMMALS; WALKING; MORPHOLOGY; BEHAVIOR AB Skeletal design among cursorial animals is a compromise between a stable body that can withstand locomotor stress and a light design that is energetically inexpensive to grow, maintain, and move. Cursors have been hypothesized to reduce distal musculoskeletal mass to maintain a balance between safety and energetic cost due to an exponential increase in energetic demand observed during the oscillation of the distal limb. Additionally, experimental research shows that the cortical bone in distal limbs experiences higher strains and remodeling rates, apparently maintaining lower mass at the expense of a smaller safety factor. This study tests the hypothesis that the trabecular bone mass in the distal limb epiphyses of cursors is relatively lower than that in the proximal limb epiphyses to minimize the energetic cost of moving the limb. This study utilized peripheral quantitative computed tomography scanning to measure the trabecular mass in the lower and upper limb epiphyses of hominids, cercopithecines, and felids that are considered cursorial and non-cursorial. One-way ANOVA with Tukey post hoc corrections was used to test for significant differences in trabecular mass across limb epiphyses. The results indicate that overall, both cursors and non-cursors exhibit varied trabecular mass in limb epiphyses and, in certain instances, conform to a proximal-distal decrease in mass irrespective of cursoriality. Specifically, hominid and cercopithecine hind limb epiphyses exhibit a proximal-distal decrease in mass irrespective of cursorial adaptations. These results suggest that cursorial mammals employ other energy saving mechanisms to minimize energy costs during running. Anat Rec, 298:797-809, 2015. (c) 2014 Wiley Periodicals, Inc. C1 [Chirchir, Habiba] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA. [Chirchir, Habiba] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. RP Chirchir, H (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, 1000 Constitution Ave, Washington, DC 20013 USA. EM habibachirchir@gmail.com FU NSF IGERT [DGE-0801634]; Wenner-Gren Foundation Wadsworth Fellowship; Leakey Foundation Baldwin Fellowship FX Grant sponsor: NSF IGERT; Grant number: DGE-0801634;; Grant sponsor: Wenner-Gren Foundation Wadsworth Fellowship, Leakey Foundation Baldwin Fellowship. NR 76 TC 1 Z9 1 U1 4 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-8486 EI 1932-8494 J9 ANAT REC JI Anat. Rec. PD MAY PY 2015 VL 298 IS 5 BP 797 EP 809 DI 10.1002/ar.23090 PG 13 WC Anatomy & Morphology SC Anatomy & Morphology GA CG4FH UT WOS:000353238900003 PM 25403099 ER PT J AU de Silva, P Nutter, B Bernal, XE AF de Silva, Priyanka Nutter, Brian Bernal, Ximena E. TI Use of acoustic signals in mating in an eavesdropping frog-biting midge SO ANIMAL BEHAVIOUR LA English DT Article DE acoustic communication; Corethrellidae; Culicidae; flight tone; harmonic convergence; wing beat frequency ID CORETHRELLA DIPTERA; ANOPHELES-GAMBIAE; AEDES-AEGYPTI; CULICIDAE; MOSQUITO; MALES; CALLS; FIELD; COMMUNICATION; BEHAVIOR AB The sensory systems of organisms are shaped by selective pressures imposed by their performance in a variety of contexts. Female frog-biting midges use the mating calls of anurans to locate their host to obtain a blood meal. Although the use of sound in foraging is well documented in this group, it is unknown whether sound is used in other contexts. To investigate the ability to use sound in nonforaging contexts, we experimentally tested the prediction that frog-biting midges (Corethrella appendiculata) use sound in mating. We recorded their wing beats while swarming, in controlled tethered conditions and during different- and same-sex pair interactions. Our results show sexual differences in the acoustic properties of flight tones, with male midges having higher frequency wing beats than females. Wing beats of free-flying individuals were significantly higher in frequency than those recorded from tethered individuals, cautioning the interpretation of recordings obtained following this widely used technique. In addition, interacting, tethered opposite-sex pairs altered their flight tones to match their upper harmonics, converging at the third and fourth harmonic frequencies of males and females, respectively. In male-male interactions, however, the frequency of their wing beats diverged. Therefore, flight tones in frog-biting midges may function as courtship signals attracting conspecific females and deterring rival males. We discuss the use of sound in multiple contexts in these midges and potential factors leading to their ability to eavesdrop on anurans. (C) 2015 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [de Silva, Priyanka] Univ Peradeniya, Dept Zool, Peradeniya, Sri Lanka. [Nutter, Brian] Texas Tech Univ, Dept Elect & Comp Engn, Lubbock, TX 79409 USA. [Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Bernal, Ximena E.] Smithsonian Trop Res Inst, Balboa, Panama. RP Bernal, XE (reprint author), Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. EM depriyanka@pdn.ac.lk; brian.nutter@ttu.edu; xbernal@purdue.edu FU National Science Foundation [IOS-1258039/1433990] FX We are thankful to Lewis Held who provided guidance and equipment to anaesthetize frog-biting midges, and Bianca Rendon for her assistance when performing the recordings of tethered individuals. Art Borkent provided valuable comments on an earlier version of this manuscript. We thank Lauren Cator and one anonymous referee for their constructive comments that helped improve this manuscript. We are also grateful to Phil Lounibos and Erik Blosser, who kindly provided the specimens that allowed us to start our frog-biting midge colony. This work was supported by the National Science Foundation grant IOS-1258039/1433990 to X.E.B. NR 49 TC 1 Z9 1 U1 7 U2 23 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 MAY PY 2015 VL 103 BP 45 EP 51 DI 10.1016/j.anbehav.2015.02.002 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA CG6AU UT WOS:000353378200007 ER PT J AU Pitt, WC Berentsen, AR Shiels, AB Volker, SF Eisemann, JD Wegmann, AS Howald, GR AF Pitt, William C. Berentsen, Are R. Shiels, Aaron B. Volker, Steven F. Eisemann, John D. Wegmann, Alexander S. Howald, Gregg R. TI Non-target species mortality and the measurement of brodifacoum rodenticide residues after a rat (Rattus rattus) eradication on Palmyra Atoll, tropical Pacific SO BIOLOGICAL CONSERVATION LA English DT Article DE Aerial broadcast; Brodifacoum rodenticide; Invasive rodent eradication; Toxicant residue; Trophic level bioaccumulation; Tropical island forest ID AERIAL POISONING OPERATION; NEW-ZEALAND; INVASIVE RODENTS; BLACK RATS; ISLAND; INVERTEBRATES; IMPACTS; BIRDS; BAITS; ENVIRONMENT AB The use of rodenticides to control or eradicate invasive rats (Rattus spp.) for conservation purposes has rapidly grown in the past decades, especially on islands. The non-target consequences and the fate of toxicant residue from such rodent eradication operations have not been well explored. In a cooperative effort, we monitored the application of a rodenticide, 'Brodifacoum 25W: Conservation', during an attempt to eradicate Rattus rattus from Palmyra Atoll. In 2011, Brodifacoum 25W: Conservation was aerially broadcasted twice over the entire atoll (2.5 km(2)) at rates of 80 kg/ha and 75 kg/ha and a supplemental hand broadcast application (71.6 kg/ha) occurred three weeks after the second aerial application over a 10 ha area. We documented brodifacoum residues in soil, water, and biota, and documented mortality of non-target organisms. Some bait (14-19% of the target application rate) entered the marine environment to distances 7 m from the shore. After the application commenced, carcasses of 84 animals representing 15 species of birds, fish, reptiles and invertebrates were collected opportunistically as potential non-target mortalities. In addition, fish, reptiles, and invertebrates were systematically collected for residue analysis. Brodifacoum residues were detected in most (84.3%) of the animal samples analyzed. Although detection of residues in samples was anticipated, the extent and concentrations in many parts of the food web were greater than expected. Risk assessments should carefully consider application rates and entire food webs prior to operations using rodenticides. Published by Elsevier Ltd. C1 [Pitt, William C.; Shiels, Aaron B.] USDA APHIS, Wildlife Serv, Natl Wildlife Res Ctr, Hawaii Field Stn, Hilo, HI 96720 USA. [Berentsen, Are R.; Volker, Steven F.; Eisemann, John D.] USDA APHIS, Wildlife Serv, Natl Wildlife Res Ctr, Ft Collins, CO 80521 USA. [Wegmann, Alexander S.] Hawaii Program Off, Isl Conservat, Honolulu, HI 96850 USA. [Howald, Gregg R.] Isl Conservat, Vancouver, BC V6B 1H5, Canada. RP Pitt, WC (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM PittW@SI.edu; Are.R.Berentsen@aphis.usda.gov; Aaron.B.Shiels@aphis.usda.gov; Steven.F.Volker@aphis.usda.gov; John.D.Eisemann@aphis.usda.gov; Alex.Wegmann@islandconservation.org; Gregg.Howald@islandconservation.org FU IC; USFWS; TNC; USDA FX The authors wish to thank T. McAuliffe (USDA), K. Hayes (USDA), A. Meyer (USFWS), S. Hathaway (USGS) and A. Kristof (USFWS) for exceptional assistance in the field. We thank D. Griffin and D. Goldade for assistance with residue analysis and B. Kimball for editorial suggestions. This study was funded by IC, USFWS, TNC, and USDA. Author contributions: WCP and ARB conceptualized the project, collected, analyzed, and interpreted data, and wrote the paper; ABS wrote the paper; SFV collected data; JDE conceptualized the project. ASW and GRH assisted in the project design. NR 54 TC 9 Z9 9 U1 11 U2 40 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 MAY PY 2015 VL 185 SI SI BP 36 EP 46 DI 10.1016/j.biocon.2015.01.008 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CG2FH UT WOS:000353089800005 ER PT J AU Brusatte, SL Butler, RJ Barrett, PM Carrano, MT Evans, DC Lloyd, GT Mannion, PD Norell, MA Peppe, DJ Upchurch, P Williamson, TE AF Brusatte, Stephen L. Butler, Richard J. Barrett, Paul M. Carrano, Matthew T. Evans, David C. Lloyd, Graeme T. Mannion, Philip D. Norell, Mark A. Peppe, Daniel J. Upchurch, Paul Williamson, Thomas E. TI The extinction of the dinosaurs SO BIOLOGICAL REVIEWS LA English DT Review DE dinosaurs; end-Cretaceous; mass extinction; Cretaceous-Paleogene; extinctions; macroevolution; Chicxulub impact; Deccan Traps; global change; palaeontology ID CRETACEOUS-TERTIARY BOUNDARY; SAN-JUAN BASIN; HELL CREEK FORMATION; MASS EXTINCTION; PALEOGENE BOUNDARY; NEW-MEXICO; DECCAN VOLCANISM; NORTH-DAKOTA; GLOBAL CLIMATE; IMPACT EJECTA AB Non-avian dinosaurs went extinct 66 million years ago, geologically coincident with the impact of a large bolide (comet or asteroid) during an interval of massive volcanic eruptions and changes in temperature and sea level. There has long been fervent debate about how these events affected dinosaurs. We review a wealth of new data accumulated over the past two decades, provide updated and novel analyses of long-term dinosaur diversity trends during the latest Cretaceous, and discuss an emerging consensus on the extinction's tempo and causes. Little support exists for a global, long-term decline across non-avian dinosaur diversity prior to their extinction at the end of the Cretaceous. However, restructuring of latest Cretaceous dinosaur faunas in North America led to reduced diversity of large-bodied herbivores, perhaps making communities more susceptible to cascading extinctions. The abruptness of the dinosaur extinction suggests a key role for the bolide impact, although the coarseness of the fossil record makes testing the effects of Deccan volcanism difficult. C1 [Brusatte, Stephen L.] Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3JW, Midlothian, Scotland. [Butler, Richard J.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. [Barrett, Paul M.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England. [Carrano, Matthew T.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Evans, David C.] Royal Ontario Museum, Dept Nat Hist, Toronto, ON M5S 2C6, Canada. [Lloyd, Graeme T.] Univ Oxford, Dept Earth Sci, Oxford OX1 3AN, England. [Mannion, Philip D.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London SW7 2AZ, England. [Norell, Mark A.] Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. [Peppe, Daniel J.] Baylor Univ, Dept Geol, Waco, TX 76706 USA. [Upchurch, Paul] UCL, Dept Earth Sci, London WC1E 6BT, England. [Williamson, Thomas E.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. RP Brusatte, SL (reprint author), Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3JW, Midlothian, Scotland. EM Stephen.Brusatte@ed.ac.uk RI Upchurch, Paul/C-1654-2008; Barrett, Paul/A-2648-2010; Butler, Richard/A-5239-2011; Carrano, Matthew/C-7601-2011; OI Barrett, Paul/0000-0003-0412-3000; Butler, Richard/0000-0003-2136-7541; Carrano, Matthew/0000-0003-2129-1612; Williamson, Thomas/0000-0002-2856-9632; Brusatte, Stephen/0000-0001-7525-7319; Peppe, Daniel/0000-0003-4263-133X FU NSF [EAR-1325544, EAR-1325552]; Marie Curie Career Integration [EC 630652]; Imperial College Junior and Alexander von Humboldt Research Fellowships FX This work was funded by NSF EAR-1325544 (S.L.B., T.E.W.) and EAR-1325552 (D.J.P.), a Marie Curie Career Integration Grant EC 630652 (S.L.B.), and an Imperial College Junior and Alexander von Humboldt Research Fellowships (P.D.M.). We thank two anonymous referees for their helpful comments and A. Cooper and W. Foster for their editorial assistance. NR 119 TC 24 Z9 24 U1 40 U2 173 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1464-7931 EI 1469-185X J9 BIOL REV JI Biol. Rev. PD MAY PY 2015 VL 90 IS 2 BP 628 EP 642 DI 10.1111/brv.12128 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CF8NL UT WOS:000352818700014 PM 25065505 ER PT J AU Cavanaugh, KC Parker, JD Cook-Patton, SC Feller, IC Williams, AP Kellner, JR AF Cavanaugh, Kyle C. Parker, John D. Cook-Patton, Susan C. Feller, Ilka C. Williams, A. Park Kellner, James R. TI Integrating physiological threshold experiments with climate modeling to project mangrove species' range expansion SO GLOBAL CHANGE BIOLOGY LA English DT Article DE Avicennia germinans; climate change; ecological thresholds; freeze tolerance; Laguncularia racemosa; range expansion; Rhizophora mangle; species distribution modeling ID SEA-LEVEL RISE; UNITED-STATES; TERRESTRIAL ECOSYSTEMS; FREEZING TEMPERATURES; CHANGING CLIMATE; SALT-MARSHES; EVENTS; VEGETATION; ECOLOGY; FLORIDA AB Predictions of climate-related shifts in species ranges have largely been based on correlative models. Due to limitations of these models, there is a need for more integration of experimental approaches when studying impacts of climate change on species distributions. Here, we used controlled experiments to identify physiological thresholds that control poleward range limits of three species of mangroves found in North America. We found that all three species exhibited a threshold response to extreme cold, but freeze tolerance thresholds varied among species. From these experiments, we developed a climate metric, freeze degree days (FDD), which incorporates both the intensity and the frequency of freezes. When included in distribution models, FDD accurately predicted mangrove presence/absence. Using 28years of satellite imagery, we linked FDD to observed changes in mangrove abundance in Florida, further exemplifying the importance of extreme cold. We then used downscaled climate projections of FDD to project that these range limits will move northward by 2.2-3.2kmyr(-1) over the next 50years. C1 [Cavanaugh, Kyle C.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. [Cavanaugh, Kyle C.; Parker, John D.; Cook-Patton, Susan C.; Feller, Ilka C.] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Cavanaugh, Kyle C.; Kellner, James R.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Williams, A. Park] Colombia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Cavanaugh, KC (reprint author), Univ Calif Los Angeles, Dept Geog, 1255 Bunche Hall,Box 951524, Los Angeles, CA 90095 USA. EM kcavanaugh@geog.ucla.edu RI Williams, Park/B-8214-2016; Parker, John/F-9761-2010; OI Williams, Park/0000-0001-8176-8166; Parker, John/0000-0002-3632-7625; Feller, Ilka/0000-0002-6391-1608 FU NASA Climate and Biological Response Program [NNX11AO94G]; NSF Macrosystems Biology Program [EF 1065821, 1065098] FX Funding for this work was provided by the NASA Climate and Biological Response Program (NNX11AO94G) and the NSF Macrosystems Biology Program (EF 1065821 and 1065098). Thanks to Mike Lehmann and Lorae Simpson for field and laboratory assistance. NR 61 TC 9 Z9 10 U1 9 U2 71 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 MAY PY 2015 VL 21 IS 5 BP 1928 EP 1938 DI 10.1111/gcb.12843 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CG3ZX UT WOS:000353220500015 PM 25558057 ER PT J AU Marvin, DC Winter, K Burnham, RJ Schnitzer, SA AF Marvin, David C. Winter, Klaus Burnham, Robyn J. Schnitzer, Stefan A. TI No evidence that elevated CO2 gives tropical lianas an advantage over tropical trees SO GLOBAL CHANGE BIOLOGY LA English DT Article DE carbon cycle; global change; mixed-effects models; open-top chambers; Panama; seasonal drought; tropical forests ID BARRO-COLORADO ISLAND; LIQUIDAMBAR-STYRACIFLUA; FOREST SUCCESSION; AMAZONIAN BOLIVIA; FUNCTIONAL-GROUPS; CLIMBING PLANTS; TREEFALL GAPS; TERM CHANGES; BASAL AREA; GROWTH AB Recent studies indicate that lianas are increasing in size and abundance relative to trees in neotropical forests. As a result, forest dynamics and carbon balance may be altered through liana-induced suppression of tree growth and increases in tree mortality. Increasing atmospheric CO2 is hypothesized to be responsible for the increase in neotropical lianas, yet no study has directly compared the relative response of tropical lianas and trees to elevated CO2. We explicitly tested whether tropical lianas had a larger response to elevated CO2 than co-occurring tropical trees and whether seasonal drought alters the response of either growth form. In two experiments conducted in central Panama, one spanning both wet and dry seasons and one restricted to the dry season, we grew liana (n=12) and tree (n=10) species in open-top growth chambers maintained at ambient or twice-ambient CO2 levels. Seedlings of eight individuals (four lianas, four trees) were grown in the ground in each chamber for at least 3months during each season. We found that both liana and tree seedlings had a significant and positive response to elevated CO2 (in biomass, leaf area, leaf mass per area, and photosynthesis), but that the relative response to elevated CO2 for all variables was not significantly greater for lianas than trees regardless of the season. The lack of differences in the relative response between growth forms does not support the hypothesis that elevated CO2 is responsible for increasing liana size and abundance across the neotropics. C1 [Marvin, David C.; Burnham, Robyn J.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Winter, Klaus; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Schnitzer, Stefan A.] Univ Wisconsin, Sch Freshwater Sci, Milwaukee, WI 53201 USA. RP Marvin, DC (reprint author), Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA. EM dmarvin@carnegiescience.edu FU Smithsonian Tropical Research Institute Office of Academic Programs; University of Michigan Department of Ecology and Evolutionary Biology; University of Michigan Rackham Graduate School; National Science Foundation Graduate Research Fellowship Program; [NSF-DEB 0613666]; [NSF-DEB 0845071]; [NSF-DEB 1019436] FX Funding for this research was provided by the Smithsonian Tropical Research Institute Office of Academic Programs (DCM), the University of Michigan Department of Ecology and Evolutionary Biology (DCM), the University of Michigan Rackham Graduate School (DCM), and the National Science Foundation Graduate Research Fellowship Program (DCM), and NSF-DEB 0613666, NSF-DEB 0845071 and NSF-DEB 1019436 (to SAS). The University of Michigan Biosphere Atmosphere Research and Training (BART) programme, N. Tuchman, and S. Mangan provided material support. B. Turner, J. Wright, and S. Mangan gave helpful advice on study design and analysis. J. Aranda, A. Virgo, and M. Garcia provided technical and logistical support. We would like to thank A. Quebbeman, E. Morrison, J. Malcomb, J. Luciani, H. Stott, and J. Dunlap for assistance with the chamber array construction, experiment monitoring, and sample processing. I. Ibanez, C. Dick, and K. Bergen gave comments on the manuscript and earlier drafts. NR 69 TC 1 Z9 1 U1 8 U2 39 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 MAY PY 2015 VL 21 IS 5 BP 2055 EP 2069 DI 10.1111/gcb.12820 PG 15 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CG3ZX UT WOS:000353220500024 PM 25471795 ER PT J AU Woodman, N Stabile, FA AF Woodman, Neal Stabile, Frank A. TI Functional Skeletal Morphology and Its Implications for Locomotory Behavior Among Three Genera of Myosoricine Shrews (Mammalia: Eulipotyphla: Soricidae) SO JOURNAL OF MORPHOLOGY LA English DT Article DE anatomy; digging; fossorial; Insectivora; Soricomorpha; substrate use; terrestrial ID INTRINSIC HAND PROPORTIONS; FOSSORIAL ADAPTATIONS; MYOSOREX MAMMALIA; GENUS CRYPTOTIS; EVOLUTION; SCANDENTIA; DIVERSITY; DIVERSIFICATION; MARSUPIALS; TUPAIIDAE AB Myosoricinae is a small clade of shrews (Mammalia, Eulipotyphla, Soricidae) that is currently restricted to the African continent. Individual species have limited distributions that are often associated with higher elevations. Although the majority of species in the subfamily are considered ambulatory in their locomotory behavior, species of the myosoricine genus Surdisorex are known to be semifossorial. To better characterize variation in locomotory behaviors among myosoricines, we calculated 32 morphological indices from skeletal measurements from nine species representing all three genera that comprise the subfamily (i.e., Congosorex, Myosorex, Surdisorex) and compared them to indices calculated for two species with well-documented locomotory behaviors: the ambulatory talpid Uropsilus soricipes and the semifossorial talpid Neurotrichus gibbsii. We summarized the 22 most complete morphological variables by 1) calculating a mean percentile rank for each species and 2) using the first principal component from principal component analysis of the indices. The two methods yielded similar results and indicate grades of adaptations reflecting a range of potential locomotory behaviors from ambulatory to semifossorial that exceeds the range represented by the two talpids. Morphological variation reflecting grades of increased semifossoriality among myosoricine shrews is similar in many respects to that seen for soricines, but some features are unique to the Myosoricinae. J. Morphol. 276:550-563, 2015. (c) 2015 Wiley Periodicals, Inc. C1 [Woodman, Neal] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Dept Vertebrate Zool, Washington, DC 20013 USA. [Stabile, Frank A.] Coll New Jersey, Dept Biol, Ewing, NJ 08628 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, MRC 111,POB 37012, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 FU National Science Foundation [through the Natural History Research Experiences Program of the United States National Museum of Natural History (USNM)] FX Contract grant sponsor: National Science Foundation [through the Natural History Research Experiences Program of the United States National Museum of Natural History (USNM) (to F.A.S)]. NR 42 TC 4 Z9 4 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD MAY PY 2015 VL 276 IS 5 BP 550 EP 563 DI 10.1002/jmor.20365 PG 14 WC Anatomy & Morphology SC Anatomy & Morphology GA CG4DU UT WOS:000353234000007 PM 25678028 ER PT J AU Seidensticker, J AF Seidensticker, John TI The UN's Lone Ranger: Combating International Wildlife Crime. SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Book Review C1 [Seidensticker, John] Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP Seidensticker, J (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. EM seidenstickerj@si.edu NR 3 TC 0 Z9 0 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-541X EI 1937-2817 J9 J WILDLIFE MANAGE JI J. Wildl. Manage. PD MAY PY 2015 VL 79 IS 4 BP 691 EP 692 DI 10.1002/jwmg.864 PG 2 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA CG3YW UT WOS:000353217100018 ER PT J AU McGuire, KL D'Angelo, H Brearley, FQ Gedallovich, SM Babar, N Yang, N Gillikin, CM Gradoville, R Bateman, C Turner, BL Mansor, P Leff, JW Fierer, N AF McGuire, K. L. D'Angelo, H. Brearley, F. Q. Gedallovich, S. M. Babar, N. Yang, N. Gillikin, C. M. Gradoville, R. Bateman, C. Turner, B. L. Mansor, P. Leff, J. W. Fierer, N. TI Responses of Soil Fungi to Logging and Oil Palm Agriculture in Southeast Asian Tropical Forests SO MICROBIAL ECOLOGY LA English DT Article ID ECTOMYCORRHIZAL FUNGI; RAIN-FOREST; LITTER DECOMPOSITION; COMMUNITY STRUCTURE; LAND-USE; MOLECULAR-IDENTIFICATION; BACTERIAL COMMUNITIES; MICROBIAL COMMUNITIES; CARBON SEQUESTRATION; PENINSULAR MALAYSIA AB Human land use alters soil microbial composition and function in a variety of systems, although few comparable studies have been done in tropical forests and tropical agricultural production areas. Logging and the expansion of oil palm agriculture are two of the most significant drivers of tropical deforestation, and the latter is most prevalent in Southeast Asia. The aim of this study was to compare soil fungal communities from three sites in Malaysia that represent three of the most dominant land-use types in the Southeast Asia tropics: a primary forest, a regenerating forest that had been selectively logged 50 years previously, and a 25-year-old oil palm plantation. Soil cores were collected from three replicate plots at each site, and fungal communities were sequenced using the Illumina platform. Extracellular enzyme assays were assessed as a proxy for soil microbial function. We found that fungal communities were distinct across all sites, although fungal composition in the regenerating forest was more similar to the primary forest than either forest community was to the oil palm site. Ectomycorrhizal fungi, which are important associates of the dominant Dipterocarpaceae tree family in this region, were compositionally distinct across forests, but were nearly absent from oil palm soils. Extracellular enzyme assays indicated that the soil ecosystem in oil palm plantations experienced altered nutrient cycling dynamics, but there were few differences between regenerating and primary forest soils. Together, these results show that logging and the replacement of primary forest with oil palm plantations alter fungal community and function, although forests regenerating from logging had more similarities with primary forests in terms of fungal composition and nutrient cycling potential. Since oil palm agriculture is currently the mostly rapidly expanding equatorial crop and logging is pervasive across tropical ecosystems, these findings may have broad applicability. C1 [McGuire, K. L.; Gedallovich, S. M.; Babar, N.; Yang, N.; Gillikin, C. M.; Bateman, C.] Columbia Univ Barnard Coll, Dept Biol, New York, NY 10027 USA. [McGuire, K. L.; D'Angelo, H.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA. [Brearley, F. Q.] Manchester Metropolitan Univ, Sch Sci & Environm, Manchester M15 6BH, Lancs, England. [Gradoville, R.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Turner, B. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Mansor, P.] Forest Res Inst Malaysia, Kuala Lumpur, Malaysia. [Leff, J. W.; Fierer, N.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Fierer, N.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO USA. RP McGuire, KL (reprint author), Columbia Univ Barnard Coll, Dept Biol, 3009 Broadway, New York, NY 10027 USA. EM kmcguire@barnard.edu; hd2144@columbia.edu; f.q.brearley@mmu.ac.uk; turnerbl@si.edu; patahayah@frim.gov.my; leff.jonathan@gmail.com; noah.fierer@colorado.edu RI Turner, Benjamin/E-5940-2011; Gedapudi, Mahesh/L-8094-2013 OI Turner, Benjamin/0000-0002-6585-0722; FU National Science Foundation [DEB 1120011] FX We thank Lee Su See, Stuart Davies, and the Center for Tropical Forest Science (CTFS) for logistical support. Permits were granted by the Forestry Research Institute Malaysia (FRIM), the Economic Planning Unit of Malaysia, and the United States Department of Agriculture (USDA). Funding was provided by the National Science Foundation (DEB 1120011 to KM). We thank Jonathan Adams and one anonymous reviewer for useful feedback on previous versions of this manuscript. NR 105 TC 9 Z9 9 U1 10 U2 51 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0095-3628 EI 1432-184X J9 MICROB ECOL JI Microb. Ecol. PD MAY PY 2015 VL 69 IS 4 SI SI BP 733 EP 747 DI 10.1007/s00248-014-0468-4 PG 15 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA CG4YP UT WOS:000353295800002 PM 25149283 ER PT J AU Chapman, SC Bertoldi, F Smail, I Blain, AW Geach, JE Gurwell, M Ivison, RJ Petitpas, GR Reddy, N Steidel, CC AF Chapman, S. C. Bertoldi, F. Smail, Ian Blain, A. W. Geach, J. E. Gurwell, M. Ivison, R. J. Petitpas, G. R. Reddy, N. Steidel, C. C. TI A blind CO detection of a distant red galaxy in the HS1700+64 protocluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: molecules; galaxies: clusters: general; galaxies: high-redshift; galaxies: starburst ID STAR-FORMING GALAXIES; FORMATION-DENSITY RELATION; SIMILAR-TO 2; MOLECULAR GAS; SUBMILLIMETER GALAXIES; HIGH-REDSHIFT; CLUSTER; ULTRAVIOLET; POPULATION; REVERSAL AB We report the blind detection of (CO)-C-12 emission from a distant red galaxy, HS1700.DRG55. We have used the IRAM Plateau de Bure Interferometer WideX, with its 3.6 GHz of instantaneous dual-polarization bandwidth, to target (CO)-C-12(3-2) from galaxies lying in the protocluster at z = 2.300 in the field HS1700+64. If indeed this line in DRG55 is (CO)-C-12(3-2), its detection at 104.9 GHz indicates z(CO) = 2.296. None of the other eight known z similar to 2.30 protocluster galaxies lying within the primary beam (PB) are detected in (CO)-C-12, although the limits are similar to 2 x worse towards the edge of the PB where several lie. The optical/near-IR magnitudes of DRG55 (R-AB > 27, K-AB = 22.3) mean that optical spectroscopic redshifts are difficult with 10-m-class telescopes, but near-IR redshifts would be feasible. The 24-mu m-implied star formation rate (210 M-aS (TM) yr(-1)), stellar mass (similar to 10(11) M-aS (TM)) and (CO)-C-12 line luminosity (3.6 x 10(10) K km s(-1) pc(2)) are comparable to other normal (CO)-C-12-detected star-forming galaxies in the literature, although the galaxy is some similar to 2 mag (similar to 6 x) fainter in the rest-frame UV than (CO)-C-12-detected galaxies at z > 2. The detection of DRG55 in (CO)-C-12 complements three other (CO)-C-12 detected UV-bright galaxies in this protocluster from previous studies, and suggests that many optically faint galaxies in the protocluster may host substantial molecular gas reservoirs, and a full blind census of (CO)-C-12 in this overdense environment is warranted. C1 [Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Bertoldi, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Smail, Ian] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England. [Blain, A. W.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Geach, J. E.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Gurwell, M.; Petitpas, G. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Reddy, N.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Steidel, C. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RP Chapman, SC (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. EM scott.chapman@dal.ca RI Smail, Ian/M-5161-2013; Ivison, R./G-4450-2011 OI Smail, Ian/0000-0003-3037-257X; Ivison, R./0000-0001-5118-1313 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Smithsonian Institution; Academia Sinica; NSERC; CFI FX 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). 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. SC and IS acknowledge the Aspen Center for Physics where parts of this manuscript were written. SC acknowledges support from NSERC and CFI. NR 32 TC 3 Z9 3 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2015 VL 449 IS 1 BP L68 EP L72 DI 10.1093/mnrasl/slv010 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG8KA UT WOS:000353555000015 ER PT J AU Guo, H Zheng, Z Jing, YP Zehavi, I Li, C Weinberg, DH Skibba, RA Nichol, RC Rossi, G Sabiu, CG Schneider, DP McBride, CK AF Guo, Hong Zheng, Zheng Jing, Y. P. Zehavi, Idit Li, Cheng Weinberg, David H. Skibba, Ramin A. Nichol, Robert C. Rossi, Graziano Sabiu, Cristiano G. Schneider, Donald P. McBride, Cameron K. TI Modelling the redshift-space three-point correlation function in SDSS-III SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: distances and redshifts; galaxies: haloes; galaxies: statistics; cosmology: observations; cosmology: theory; large-scale structure of Universe ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; HALO OCCUPATION DISTRIBUTION; PAIRWISE VELOCITY DISPERSION; GALAXY CORRELATION-FUNCTION; LUMINOUS RED GALAXIES; LARGE-SCALE STRUCTURE; COLOR DEPENDENCE; BIAS; UNIVERSE AB We present the measurements of the redshift-space three-point correlation function (3PCF) for z similar to 0.5 luminous red galaxies of the CMASS sample in the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey Data Release 11. The 3PCF measurements are interpreted within the halo occupation distribution framework using high-resolution N-body simulations, and the model successfully reproduces the 3PCF on scales larger than 1 h(-1) Mpc. As with the case for the redshift-space two-point correlation functions, we find that the redshift-space 3PCF measurements also favour the inclusion of galaxy velocity bias in the model. In particular, the central galaxy in a halo is on average in motion with respect to the core of the halo. We discuss the potential of the small-scale 3PCF to tighten the constraints on the relation between galaxies and dark matter haloes and on the phase-space distribution of galaxies. C1 [Guo, Hong; Zheng, Zheng] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Jing, Y. P.] Shanghai Jiao Tong Univ, Dept Phys & Astron, Ctr Astron & Astrophys, Shanghai 200240, Peoples R China. [Jing, Y. P.] Shanghai Jiao Tong Univ, IFSA Collaborat Innovat Ctr, Shanghai 200240, Peoples R China. [Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Li, Cheng] Chinese Acad Sci, Shanghai Astron Observ, Max Planck Inst Astrophys, Partner Grp, Shanghai 200030, Peoples R China. [Li, Cheng] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Skibba, Ramin A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Nichol, Robert C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Rossi, Graziano] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea. [Rossi, Graziano] CEA, Ctr Saclay, Irfu, SPP, F-91191 Gif Sur Yvette, France. [Sabiu, Cristiano G.] Korea Inst Adv Study, Seoul 130722, South Korea. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Guo, H (reprint author), Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. EM hong.guo@utah.edu RI Guo, Hong/J-5797-2015; Jing, Yipeng/P-3678-2015 OI Guo, Hong/0000-0003-4936-8247; FU NSF [AST-1208891]; NSFC [11173045, 11233005, 11325314, 11320101002]; CAS [XDB09000000]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; [2015CB857000]; [NSFC-11320101002]; [11033006]; [11121062] FX We thank the anonymous referee for the helpful and constructive comments. ZZ was partially supported by NSF grant AST-1208891. YPJ is supported by grants (2015CB857000, NSFC-11320101002, 11033006, 11121062). CL acknowledges the support of NSFC (11173045, 11233005, 11325314, 11320101002) and the Strategic Priority Research Program 'The Emergence of Cosmological Structures' of CAS (Grant No. XDB09000000). We gratefully acknowledge the use of computing resources at Shanghai Astronomical Observatory, from the High Performance Computing Resource in the Core Facility for Advanced Research Computing at Case Western Reserve University and from the Centre for High Performance Computing at the University of Utah.; 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 46 TC 8 Z9 8 U1 4 U2 7 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 MAY 1 PY 2015 VL 449 IS 1 BP L95 EP L99 DI 10.1093/mnrasl/slv020 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG8KA UT WOS:000353555000021 ER PT J AU Field, DJ LeBlanc, A Gau, A Behlke, AD AF Field, Daniel J. LeBlanc, Aaron Gau, Adrienne Behlke, Adam D. TI PELAGIC NEONATAL FOSSILS SUPPORT VIVIPARITY AND PRECOCIAL LIFE HISTORY OF CRETACEOUS MOSASAURS SO PALAEONTOLOGY LA English DT Article DE mosasaur; viviparity; Niobrara; marine reptile; life history ID NORTH-AMERICA; SQUAMATA; EVOLUTION; REPTILIA; ATTACHMENT; ICHTHYORNIS; PLATECARPUS; MORPHOLOGY; PHYLOGENY; CLIDASTES AB Mosasaurs were large marine squamates that inhabited all of the world's oceans during the Late Cretaceous. Their success as apex predators has been attributed to their rapid acquisition of aquatic adaptations, which allowed them to become fully pelagic. However, little is known about the breeding biology of derived, flipper-bearing mosasaurs, as the record of neonatal mosasaur fossils is extremely sparse. Here, we report on the fragmentary cranial remains of two neonatal mosasaurs from the Niobrara Formation, referred to Clidastes sp. Comparison with other preliminary reports of neonatal mosasaurs reveals that these specimens are among the smallest individuals ever found and certainly represent the smallest known Clidastes specimens. The recovery of these extremely young specimens from a pelagic setting indicates that even neonatal mosasaurs occupied open oceanic habitats and were likely born in this setting. These data shed new light on the ecology of neonatal mosasaurs and illustrate the degree to which size-related taphonomic and collection biases have influenced our understanding of the early life history of these iconic marine reptiles. C1 [Field, Daniel J.; Gau, Adrienne; Behlke, Adam D.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06511 USA. [Field, Daniel J.] Smithsonian Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [LeBlanc, Aaron] Univ Toronto, Dept Ecol & Evolutionary Biol, Mississauga, ON L5L 1C6, Canada. RP Field, DJ (reprint author), Yale Univ, Dept Geol & Geophys, 210 Whitney Ave, New Haven, CT 06511 USA. EM daniel.field@yale.edu; aaron.leblanc@mail.utoronto.ca; adrien.gau@yale.edu; adam.behlke@yale.edu OI LeBlanc, Aaron/0000-0002-2497-1296; Field, Daniel/0000-0002-1786-0352 FU NSERC (CGS-D); Smithsonian Predoctoral Fellowship FX We are indebted to T. Ikejiri, M. Caldwell, J. Gauthier and R. Benson for critical comments that improved the quality of this manuscript. D. Brinkman and C. Norris (YPM) formally accessioned and deciphered the provenance of these specimens. J. Gauthier provided initial affirmation of our taxonomic diagnosis. We thank J. Csotonyi for the extraordinary artwork exhibited in Figure 4. DJF was supported by NSERC (CGS-D) and a Smithsonian Predoctoral Fellowship. NR 53 TC 6 Z9 6 U1 2 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0031-0239 EI 1475-4983 J9 PALAEONTOLOGY JI Paleontology PD MAY PY 2015 VL 58 IS 3 BP 401 EP 407 DI 10.1111/pala.12165 PG 7 WC Paleontology SC Paleontology GA CG6GZ UT WOS:000353398000002 ER PT J AU Mah, C Linse, K Copley, J Marsh, L Rogers, A Clague, D Foltz, D AF Mah, Christopher Linse, Katrin Copley, Jon Marsh, Leigh Rogers, Alex Clague, David Foltz, David TI Description of a new family, new genus, and two new species of deep-sea Forcipulatacea (Asteroidea), including the first known sea star from hydrothermal vent habitats SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Antarctica; deep sea; forcipulatacea; hydrothermal vent; North Pacific; pedicellariae ID GULF-OF-MEXICO; FUCA RIDGE; OPHIUROID ECHINODERMATA; MOLECULAR PHYLOGENY; GALAPAGOS RIFT; AXIAL SEAMOUNT; ATLANTIC-OCEAN; BIOLOGY; MORPHOLOGY; PEDICELLARIAE AB Based on a phylogenetic analysis of undescribed taxa within the Forcipulatacea, a new family of deep-sea forcipulatacean starfishes, Paulasteriidaefam.nov., is described from deep-sea settings. Paulasterias tylerigen.etsp.nov. was observed at recently documented hydrothermal vents on the East Scotia Ridge, Southern Ocean. A second species, Paulasterias mcclainigen.etsp.nov. was observed in deep-sea settings in the North Pacific, more distant from hydrothermal vents. Both species are multi-armed (with between six and eight arms), with a fleshy body wall, and a poorly developed or absent adoral carina. Here, we include discussions of pedicellariae morphology, feeding biology, and classification.(c) 2015 The Linnean Society of London C1 [Mah, Christopher] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Mah, Christopher; Foltz, David] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Linse, Katrin] British Antarctic Survey, Cambridge CB3 0ET, England. [Copley, Jon; Marsh, Leigh] Univ Southampton, Ocean & Earth Sci, Southampton SO14 3ZH, Hants, England. [Rogers, Alex] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Clague, David] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. RP Mah, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. EM brisinga@gmail.com RI Copley, Jonathan/I-7076-2012; OI Copley, Jonathan/0000-0003-3333-4325; Marsh, Leigh/0000-0002-4613-1538 FU UK NERC Consortium [NE/DO1249X/1]; NSF-Polar Programs Postdoctoral Fellowship [OPP-0631245]; LSU Faculty Research Grant; NSF [DEB-1036358] FX C. Mah is extremely grateful to Dr Craig McClain and Dr Dave Clague for their invitation to participate in the 2009 MBARI Pacific Northwest Expedition. C. Mah also thanks Lonny Lundsten, Linda Kuntz, the crew of the RV Western Flyer and other personnel at MBARI for their assistance. We extend thanks to the crew of RRS James Cook and the staff of the UK National Marine Facilities at NOC, especially the ROV Isis team, for logistic, technical, and shipboard support during JC42, as well the ChEsSo research programme, which was funded by UK NERC Consortium Grant (NE/DO1249X/1) under the lead of Professor Paul Tyler. We gratefully acknowledge Will Reid, who provided us with isotope data in advance of his paper (Reid et al., 2013). Special appreciation is extended to Bob Ford and Taylor Steed, Frederick Community College, and Scott Whitaker, NMNH SEM Lab, for their help with SEM logistics. For specimen cataloguing and logistics we thank Linda Ward and Paul Greenhall at the NMNH, and Miranda Lowe and Andrew Cabrinovic at the NHM. The original forcipulates sequence data set was collected with support by NSF-Polar Programs Postdoctoral Fellowship OPP-0631245 to C. Mah, and by an LSU Faculty Research Grant to D. Foltz. The new molecular work was funded in part by NSF award DEB-1036358 to D. Foltz and C. Mah. The manuscript benefitted from improvements provided by two anonymous reviewers. NR 66 TC 3 Z9 3 U1 4 U2 21 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 MAY PY 2015 VL 174 IS 1 BP 93 EP 113 DI 10.1111/zoj.12229 PG 21 WC Zoology SC Zoology GA CG6GU UT WOS:000353397200004 ER PT J AU Dutra, GM Jerep, FC Vari, RP de Santana, CD AF Dutra, Guilherme Moreira Jerep, Fernando C. Vari, Richard P. de Santana, Carlos David TI The pseudotympanum in the Gymnotiformes (Teleostei, Ostariophysi, Otophysi): homology and evolution of a previously unexplored system in Neotropical electric fishes SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE comparative anatomy; muscular reductions; phylogenetically informative characters ID PHYLOGENETIC-RELATIONSHIPS; CATFISHES SILURIFORMES; GAS BLADDER; HISTORICAL BIOGEOGRAPHY; CHARACIFORMES; CHARACIDAE; MORPHOLOGY; BASIN; GENUS; RHAMPHICHTHYIDAE AB The pseudotympanum, a reduction of the hypaxialis muscle in the body wall lateral to the anterior portion of the swim bladder, is unique to some members of the Otophysi, the largest clade of primarily freshwater fishes. Prior studies documented the presence of the pseudotympanum in a number of groups within the Characiformes, to a lesser extent in subunits of the Siluriformes, and in a few taxa of the Cypriniformes, but with only one record of the aperture in the Gymnotiformes - the Neotropical electric fishes. Surveys across the five families and c. two-thirds of the genera in the Gymnotiformes revealed the occurrence of a pseudotympanum in all examined taxa. Pronounced variation in the expanse and details of the morphology of the opening and its relationship to the anterior elements of the axial skeleton was documented amongst Neotropical electric fish. Details of pseudotympanal morphology in the different families of the Gymnotiformes are described and the variation evaluated within the context of the two alternative hypotheses of higher-level phylogenetic relationships within the order.(c) 2015 The Linnean Society of London C1 [Dutra, Guilherme Moreira] Setor Ictiol, Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [Jerep, Fernando C.; Vari, Richard P.; de Santana, Carlos David] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. [Jerep, Fernando C.] Univ Estadual Londrina, Museu Zool, Ctr Ciencias Biol, Dept Biol Anim & Vegetal, BR-86057970 Londrina, PR, Brazil. RP de Santana, CD (reprint author), Setor Ictiol, Museu Paraense Emilio Goeldi, Ave Magalhaes Barata 376,CP 399, BR-66040170 Belem, Para, Brazil. EM apteronotidae@ig.com.br RI Jerep, Fernando/F-5274-2015 FU Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [245310/2012-6]; National Museum of Natural History; Smithsonian Institution; Herbert R and Evelyn Axelrod Chair in Ichthyology at the National Museum of Natural History; CNPq/Ciencia Sem Fronteiras [245622/2012-8] FX We thank M. Sabaj Perez (ANSP); C. Uribe (IAvH); C. Lucena and Z. Lucena (MCP); W. Wosiacki (MPEG); L. Page and R. Robins (UF); and L. Malabarba (UFRGS) for the loan of specimens. S. Raredon (USNM) assisted with the photographs in Figures 1-3. G. M. D. 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). F. C. J. was funded by a fellowship provided by the National Museum of Natural History, Smithsonian Institution. Support for the project to F. C. J. and R. P. V. was received from the Herbert R and Evelyn Axelrod Chair in Ichthyology at the National Museum of Natural History. C. D. S. was supported by a postdoctoral fellowship from the CNPq/Ciencia Sem Fronteiras (245622/2012-8). C. Ferraris provided valuable suggestions for improvements to the paper. NR 67 TC 1 Z9 3 U1 2 U2 8 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 MAY PY 2015 VL 174 IS 1 BP 114 EP 129 DI 10.1111/zoj.12221 PG 16 WC Zoology SC Zoology GA CG6GU UT WOS:000353397200005 ER PT J AU Psorakis, I Voelkl, B Garroway, CJ Radersma, R Aplin, LM Crates, RA Culina, A Farine, DR Firth, JA Hinde, CA Kidd, LR Milligan, ND Roberts, SJ Verhelst, B Sheldon, BC AF Psorakis, Ioannis Voelkl, Bernhard Garroway, Colin J. Radersma, Reinder Aplin, Lucy M. Crates, Ross A. Culina, Antica Farine, Damien R. Firth, Josh A. Hinde, Camilla A. Kidd, Lindall R. Milligan, Nicole D. Roberts, Stephen J. Verhelst, Brecht Sheldon, Ben C. TI Inferring social structure from temporal data SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Social networks; Group detection; Flocks; Gathering events; Great tits ID NETWORKS; INDIVIDUALS; ASSOCIATION; BEHAVIOR; SYSTEMS AB Social network analysis has become a popular tool for characterising the social structure of populations. Animal social networks can be built either by observing individuals and defining links based on the occurrence of specific types of social interactions, or by linking individuals based on observations of physical proximity or group membership, given a certain behavioural activity. The latter approaches of discovering network structure require splitting the temporal observation stream into discrete events given an appropriate time resolution parameter. This process poses several non-trivial problems which have not received adequate attention so far. Here, using data from a study of passive integrated transponder (PIT)-tagged great tits Parus major, we discuss these problems, demonstrate how the choice of the extraction method and the temporal resolution parameter influence the appearance and properties of the retrieved network and suggest a modus operandi that minimises observer bias due to arbitrary parameter choice. Our results have important implications for all studies of social networks where associations are based on spatio-temporal proximity, and more generally for all studies where we seek to uncover the relationships amongst a population of individuals that are observed through a temporal data stream of appearance records. C1 [Psorakis, Ioannis; Roberts, Stephen J.] Univ Oxford, Dept Engn Sci, Oxford OX1 3PJ, England. [Psorakis, Ioannis] Thought Machine Ltd, London EC2 3HU, England. [Voelkl, Bernhard; Garroway, Colin J.; Radersma, Reinder; Aplin, Lucy M.; Crates, Ross A.; Culina, Antica; Farine, Damien R.; Firth, Josh A.; Hinde, Camilla A.; Kidd, Lindall R.; Milligan, Nicole D.; Verhelst, Brecht; Sheldon, Ben C.] Univ Oxford, Dept Zool, Edward Grey Inst, 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. [Hinde, Camilla A.] Wageningen Univ, Dept Anim Sci, NL-6700 AH Wageningen, Netherlands. RP Voelkl, B (reprint author), Univ Oxford, Dept Zool, Edward Grey Inst, S Parks Rd, Oxford OX1 3PS, England. EM bernhard.voelkl@zoo.ox.ac.uk RI Sheldon, Ben/A-8056-2010; Voelkl, Bernhard/D-1390-2009; OI Sheldon, Ben/0000-0002-5240-7828; Voelkl, Bernhard/0000-0001-5454-2508; Farine, Damien/0000-0003-2208-7613; Culina, Antica/0000-0003-2910-8085 FU ERC [AdG 250164]; Microsoft Research; Australian Postgraduate Award; International Alliance of Research Universities travel grant FX We thank J. Howe, T. Wilkin, S. Evans, A. Hinks and A. Grabowska for assistance in the field and three anonymous reviewers for valuable comments on the manuscript. This research was funded by an ERC grant to BCS (AdG 250164) and a Microsoft Research Grant to IP. LMA was also funded by an Australian Postgraduate Award and by an International Alliance of Research Universities travel grant. NR 28 TC 17 Z9 19 U1 3 U2 36 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 MAY PY 2015 VL 69 IS 5 BP 857 EP 866 DI 10.1007/s00265-015-1906-0 PG 10 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA CF7EI UT WOS:000352718600017 ER PT J AU Betancur-R, R Orti, G Pyron, RA AF Betancur-R, Ricardo Orti, Guillermo Pyron, Robert Alexander TI Fossil-based comparative analyses reveal ancient marine ancestry erased by extinction in ray-finned fishes SO ECOLOGY LETTERS LA English DT Article DE Actinopterygii; diversification; ecological transitions; marine and freshwaters; neontology; palaeontology; phylogenetic comparative methods; phylogeny; state dependent diversification ID PHYLOGENETIC ANALYSES; SPECIES RICHNESS; DIVERSIFICATION; EVOLUTION; TAXA; SPECIATION; RATES; TRANSITIONS; CHARACTERS; LIKELIHOOD AB The marine-freshwater boundary is a major biodiversity gradient and few groups have colonised both systems successfully. Fishes have transitioned between habitats repeatedly, diversifying in rivers, lakes and oceans over evolutionary time. However, their history of habitat colonisation and diversification is unclear based on available fossil and phylogenetic data. We estimate ancestral habitats and diversification and transition rates using a large-scale phylogeny of extant fish taxa and one containing a massive number of extinct species. Extant-only phylogenetic analyses indicate freshwater ancestry, but inclusion of fossils reveal strong evidence of marine ancestry in lineages now restricted to freshwaters. Diversification and colonisation dynamics vary asymmetrically between habitats, as marine lineages colonise and flourish in rivers more frequently than the reverse. Our study highlights the importance of including fossils in comparative analyses, showing that freshwaters have played a role as refuges for ancient fish lineages, a signal erased by extinction in extant-only phylogenies. C1 [Betancur-R, Ricardo] Univ Puerto Rico Rio Piedras, Dept Biol, San Juan, PR 00931 USA. [Betancur-R, Ricardo] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Orti, Guillermo; Pyron, Robert Alexander] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Betancur-R, R (reprint author), Univ Puerto Rico Rio Piedras, Dept Biol, POB 23360, San Juan, PR 00931 USA. EM betanri@fishphylogeny.org NR 49 TC 19 Z9 19 U1 3 U2 33 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 MAY PY 2015 VL 18 IS 5 BP 441 EP 450 DI 10.1111/ele.12423 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CF8GP UT WOS:000352794500003 PM 25808114 ER PT J AU Huber, B Whibley, A Poul, YL Navarro, N Martin, A Baxter, S Shah, A Gilles, B Wirth, T McMillan, WO Joron, M AF Huber, B. Whibley, A. Poul, Y. L. Navarro, N. Martin, A. Baxter, S. Shah, A. Gilles, B. Wirth, T. McMillan, W. O. Joron, M. TI Conservatism and novelty in the genetic architecture of adaptation in Heliconius butterflies SO HEREDITY LA English DT Article ID POPULATION GENOMICS; CONVERGENT EVOLUTION; PATTERN MIMICRY; WARNING COLOR; HYBRID ZONES; DIVERGENCE; MELPOMENE; SELECTION; SUPERGENE; PARALLELISM AB Understanding the genetic architecture of adaptive traits has been at the centre of modern evolutionary biology since Fisher; however, evaluating how the genetic architecture of ecologically important traits influences their diversification has been hampered by the scarcity of empirical data. Now, high-throughput genomics facilitates the detailed exploration of variation in the genome-to-phenotype map among closely related taxa. Here, we investigate the evolution of wing pattern diversity in Heliconius, a clade of neotropical butterflies that have undergone an adaptive radiation for wing-pattern mimicry and are influenced by distinct selection regimes. Using crosses between natural wing-pattern variants, we used genome-wide restriction site-associated DNA (RAD) genotyping, traditional linkage mapping and multivariate image analysis to study the evolution of the architecture of adaptive variation in two closely related species: Heliconius hecale and H. ismenius. We implemented a new morphometric procedure for the analysis of whole-wing pattern variation, which allows visualising spatial heatmaps of genotype-to-phenotype association for each quantitative trait locus separately. We used the H. melpomene reference genome to fine-map variation for each major wing-patterning region uncovered, evaluated the role of candidate genes and compared genetic architectures across the genus. Our results show that, although the loci responding to mimicry selection are highly conserved between species, their effect size and phenotypic action vary throughout the clade. Multilocus architecture is ancestral and maintained across species under directional selection, whereas the single-locus (supergene) inheritance controlling polymorphism in H. numata appears to have evolved only once. Nevertheless, the conservatism in the wing-patterning toolkit found throughout the genus does not appear to constrain phenotypic evolution towards local adaptive optima. C1 [Huber, B.; Whibley, A.; Poul, Y. L.; Shah, A.; Gilles, B.; Wirth, T.; Joron, M.] Museum Natl Hist Nat, UMR CNRS 7205, Inst Systemat Evolut & Biodivers, F-75231 Paris, France. [Huber, B.; Wirth, T.] EPHE, Lab Biol Integrat Populat, F-75006 Paris, France. [Huber, B.; Gilles, B.; McMillan, W. O.; Joron, M.] Smithsonian Trop Res Inst, Balboa, Panama. [Navarro, N.] Ecole Prat Hautes Etud, Lab PALEVO, Dijon, France. [Navarro, N.] Univ Bourgogne, UMR uB CNRS Biogeosci 6282, Dijon, France. [Martin, A.] Univ Calif Berkeley, Dept Mol & Cell Biol, Berkeley, CA 94720 USA. [Baxter, S.] Univ Adelaide, Sch Mol & Biomed Sci, Adelaide, SA, Australia. [Baxter, S.] Univ Cambridge, Dept Zool, Cambridge, England. [Shah, A.] Univ Bielefeld, Dept Anim Behav, D-33615 Bielefeld, Germany. RP Huber, B (reprint author), UMR 7205 CNRS EPHE MNHN UPMC, Museum Natl Hist Nat, Inst Systemat Evolut & Biodivers, 45 Rue Buffon,CP50, F-75005 Paris, France. EM babahuber@gmail.com; mathieu.joron@cefe.cnrs.fr RI Wirth, Thierry/B-4915-2008; Navarro, Nicolas/H-2364-2012; OI Navarro, Nicolas/0000-0001-5694-4201; Shah, Abhijeet/0000-0002-0467-4884; Martin, Arnaud/0000-0002-5980-2249 FU Smithsonian Tropical Research Institute short-term fellowship; CNRS ATIP grant; ERC grant (MimEvol); ANR grant (HybEvol) FX We thank Adriana Tapia, Andres Orellana, Cristobal Rios, Catherine Brunton, Moises Abanto, Elizabeth Evans, Nicola Nadeau and Patricio Salazar for help with butterfly collection and breeding; the Autoridad Nacional del Ambiente (Panama) for collection permits; Lise Frezal, The Gene Pool (Edinburgh Genomics), the BoEM lab (MNHN) and the SSM (MNHN) for assistance with molecular work; Marcus Kronforst for providing primers; John Davey, Kanchon Dasmahapatra, Manmohan Sharma and Robert Jones for assistance with sequence analysis and bioinformatics; Violaine Llaurens and Chris Jiggins for help and comments on the manuscript. We are most grateful to the three anonymous referees whose in-depth reviews improved this work. This work was funded by a Smithsonian Tropical Research Institute short-term fellowship to BH, AM and BG and by a CNRS ATIP grant, an ERC grant (MimEvol) and an ANR grant (HybEvol) to MJ. NR 57 TC 9 Z9 9 U1 3 U2 50 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0018-067X EI 1365-2540 J9 HEREDITY JI Heredity PD MAY PY 2015 VL 114 IS 5 SI SI BP 515 EP 524 DI 10.1038/hdy.2015.22 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CG1IU UT WOS:000353027100011 PM 25806542 ER PT J AU Helms, JA Kaspari, M AF Helms, J. A. Kaspari, M. TI Reproduction-dispersal tradeoffs in ant queens SO INSECTES SOCIAUX LA English DT Article DE Colony founding; Dispersal tradeoffs; Found or Fly; Mating flight; Reproductive strategy ID IN-FLIGHT MORPHOLOGY; SEED-HARVESTER ANTS; SOLENOPSIS-INVICTA; FIRE ANT; STORAGE PROTEINS; BROOD PRODUCTION; INSECT FLIGHT; HYMENOPTERA-FORMICIDAE; COLONY FOUNDATION; SIZE-DIMORPHISM AB Organisms often experience reproduction-dispersal tradeoffs mediated by body size. In ants (Hymenoptera: Formicidae) the Found or Fly (FoF) Hypothesis states that dispersing queens face an ecological tradeoff between colony founding and flight success mediated by abdominal nutrient loading. If expressed interspecifically, such a tradeoff implies biomechanical costs to more energetically demanding life history strategies. Claustrally founding queens, who carry the entire resource load necessary to fuel early colony growth, may incur flight costs. We characterized the flight morphology of 21 Neotropical species representing four major subfamilies, spanning four orders of magnitude in body mass and practicing several colony founding strategies. Flight morphologies were compared in a phylogenetic context to evaluate how they varied with body size and reproductive ecology. Consistent with FoF, claustral founders had 30 % lower flight muscle ratios (FMR) and trended toward higher abdomen drag than species in which founding queens feed. The two strategies did not differ in wing loading. Instead, claustral founders evolved larger wings, counteracting the effect of heavier abdomens. Heavy nutrient loads pushed several claustral species to theoretical limits of flight by lowering FMR to levels which cause flightlessness in other insects. Selection for higher nutrient loads related to colony founding is a possible mechanism for the recurrent evolution of flightlessness in ants. The importance and conflicting demands of nutrient storage and flight make ant queens ideal organisms for modeling reproduction-dispersal tradeoffs. By emphasizing the role of flight in ant biology, the FoF Hypothesis highlights this tradeoff and provides novel insights into ant evolution. C1 [Helms, J. A.; Kaspari, M.] Univ Oklahoma, Dept Biol, Norman, OK 73019 USA. [Kaspari, M.] Smithsonian Trop Res Inst, Balboa, Panama. RP Helms, JA (reprint author), Univ Oklahoma, Dept Biol, Norman, OK 73019 USA. EM jackson.a.helms-1@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 FU National Science Foundation [EF-1065844]; University of Oklahoma FX We thank the Republic of Panama, Barro Colorado Nature Monument and the Smithsonian Tropical Research Institute for allowing us to work on Barro Colorado Island. This project could not have succeeded without Rosemary Knapp who allowed us to use her lab. Adam Kay provided valuable advice. Jon Shik and two anonymous reviewers provided helpful comments that improved the manuscript. This work was supported by National Science Foundation grant EF-1065844 to MK. JAH is funded by a National Science Foundation Graduate Research Fellowship and a University of Oklahoma Alumni Fellowship. NR 92 TC 4 Z9 4 U1 3 U2 35 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD MAY PY 2015 VL 62 IS 2 BP 171 EP 181 DI 10.1007/s00040-015-0391-9 PG 11 WC Entomology SC Entomology GA CF7FQ UT WOS:000352722000009 ER PT J AU Leonard, JA den Tex, RJ Hawkins, MTR Munoz-Fuentes, V Thorington, R Maldonado, JE AF Leonard, Jennifer A. den Tex, Robert-Jan Hawkins, Melissa T. R. Munoz-Fuentes, Violeta Thorington, Richard Maldonado, Jesus E. TI Phylogeography of vertebrates on the Sunda Shelf: a multi-species comparison SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Comparative phylogeography; extinction; molecular dating; Pleistocene divergence; population divergence; priority effect; Sundaland ID LAST GLACIAL PERIOD; SOUTHEAST-ASIA; EVOLUTIONARY HISTORY; POPULATION DIVERGENCE; SHRIKE-BABBLERS; SPECIES LIMITS; RAIN-FORESTS; BIOGEOGRAPHY; DIVERSITY; PHYLOGENY AB Aim Pleistocene environmental fluctuations had well-characterized impacts on the patterns of within-species divergences and diversity in temperate habitats. Here we examine the impact the Pleistocene had on widely distributed forest vertebrates in a tropical system where the distribution of the habitat was affected by those fluctuations. LocationSundaland, tropical Southeast Asia. Methods We conducted a comparative phylogeographical analysis of 28 non-migratory, forest-dependent vertebrates, for which we constructed rooted, intraspecifc phylogenies based on mitochondrial DNA sequences of individuals from at least the three major landmasses in the area (Borneo, Sumatra and the Malay Peninsula) and compared them to hypothetical phylogenies based on independent geological data and climate models regarding connections and relationships between the major landmasses of Sundaland. Java was included where possible. We dated the phylogenies to determine whether patterns of differentiation were concordant across species. Results In most species, populations on the Malay Peninsula and Sumatra were most closely related, and sister to those from Borneo. The dates of these divergences, however, varied extensively between species. Borneo harbours multiple deeply divergent lineages of many species compared to the diversity within those species. Javan populations of several birds were most divergent relative to those from the rest of the Sunda Shelf. Main conclusions These results suggest a dynamic history, including recurrent population extinctions and replacements and a strong priority effect for local populations. The close relationship between populations in Sumatra and the Malay Peninsula supports the existence of forest on the exposed shelf during the Pleistocene at many different times, and suggests that proximity was more important than the presence of palaeorivers for dispersal of forest taxa between landmasses. C1 [Leonard, Jennifer A.; Hawkins, Melissa T. R.; Munoz-Fuentes, Violeta] Estn Biol Donana EBD CSIC, Conservat & Evolutionary Genet Grp, Seville 41092, Spain. [Leonard, Jennifer A.; den Tex, Robert-Jan; Munoz-Fuentes, Violeta] Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. [Hawkins, Melissa T. R.; Maldonado, Jesus E.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Hawkins, Melissa T. R.; Thorington, Richard; Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. RP Leonard, JA (reprint author), Estn Biol Donana EBD CSIC, Conservat & Evolutionary Genet Grp, Avda Amer Vespucio S-N, Seville 41092, Spain. EM jleonard@ebd.csic.es RI CSIC, EBD Donana/C-4157-2011; Leonard, Jennifer/A-7894-2010 OI CSIC, EBD Donana/0000-0003-4318-6602; Leonard, Jennifer/0000-0003-0291-7819 FU Spanish Research Council [CGL2010-21524]; Spanish Research Council/Consejo Superior de Investigaciones Cientificas (CSIC); EU Marie Curie Mobility and Training Programme FX Antonia Gorog is cordially thanked for invaluable help and rapidly making the cytb sequence data of Leopoldamys sabanus, Maxomys surifer and M. whiteheadi available for this study. We also thank Ines Sanchez-Donoso for her assistance with figure preparation. The Spanish Research Council supported this work (CGL2010-21524). V.M.F. was supported by the Spanish Research Council/Consejo Superior de Investigaciones Cientificas (CSIC) and the EU Marie Curie Mobility and Training Programme. NR 61 TC 8 Z9 8 U1 2 U2 23 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 MAY PY 2015 VL 42 IS 5 BP 871 EP 879 DI 10.1111/jbi.12465 PG 9 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA CF8GH UT WOS:000352793700006 ER PT J AU Lohan, KMP Hill-Spanik, KM Torchin, ME Strong, EE Fleischer, RC Ruiz, GM AF Lohan, Katrina M. Pagenkopp Hill-Spanik, Kristina M. Torchin, Mark E. Strong, Ellen E. Fleischer, Robert C. Ruiz, Gregory M. TI Molecular phylogenetics reveals first record and invasion of Saccostrea species in the Caribbean SO MARINE BIOLOGY LA English DT Article ID MULTIPLE SEQUENCE ALIGNMENT; MANGROVE OYSTERS CRASSOSTREA; MITOCHONDRIAL-DNA; HAPLOSPORIDIUM-NELSONI; SEA-CHESTS; OSTREIDAE; BIVALVIA; IDENTIFICATION; ECOSYSTEM; INVERTEBRATES AB Taxonomic uncertainty often limits our ability to resolve biogeographic patterns and discern biological invasions. Within the bivalve mollusks, this uncertainty is particularly acute for oysters, as the high degree of phenotypic plasticity of their shells creates taxonomic confusion. The integration of molecular data with shell morphology can differentiate species, providing new insights into biogeography, invasions, and ecology of this functionally important group. As an initial step in resolving the identities and current geographic distributions of oyster species, sequence data from the mitochondrial cytochrome oxidase I gene were combined with morphological criteria to confirm the identities of ten oyster species of Ostreidae, Isognomonidae, and Pteriidae, focusing on the Pacific and Caribbean coasts of Panama, since tropical biota have received the least study. The results indicate that Crassostrea virginica, previously only reported from this region along the Yucatan Peninsula and coast of Venezuela, also occurs in the Caribbean waters of Panama. We also document the first record for a species of Saccostrea, a genus native to the Pacific, suggesting an invasion by an unknown non-native Saccostrea species that is now widespread along the Caribbean from the Panama Canal west to Bocas del Toro. Sequences of the internal transcribed spacer region (ITS1) of the ribosomal gene complex (rDNA) did not reveal any hybridization. Considering the high connectivity of shipping and boating in Panama, Saccostrea sp. may have been introduced to the Caribbean by either recreational or commercial vessels, but the timing and potential ecological effects of this invasion remain unknown. C1 [Lohan, Katrina M. Pagenkopp; Hill-Spanik, Kristina M.; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Lohan, Katrina M. Pagenkopp; Hill-Spanik, Kristina M.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA. [Torchin, Mark E.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Strong, Ellen E.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Lohan, KMP (reprint author), Smithsonian Environm Res Ctr, Marine Invas Lab, POB 28, Edgewater, MD 21037 USA. EM lohank@si.edu OI Ruiz, Gregory/0000-0003-2499-441X; Lohan, Katrina/0000-0003-3885-7985 FU Smithsonian Institution Grand Challenges Grant; Smithsonian Institution MarineGEO Postdoctoral Fellowship FX We thank Gabriel Jacome and Plinio Gondola at the Smithsonian Bocas del Toro Marine Station for assistance and discussions on local bivalve species. Dr. Carmen Schloder assisted with field collections and obtaining permits. We thank Dr. Ilya Temkin (NOVA) for assistance with identifying members of the Isognomonidae and John Wilk (UIC) for sharing his data and confirming the identity of the second species of Isognomon. Dr. Mark Minton assisted with the creation of maps in ArcGIS. Nancy Rotzel McInerney provided lab logistical support at CCEG. A Smithsonian Institution Grand Challenges Grant funded this project. A Smithsonian Institution MarineGEO Postdoctoral Fellowship funded KM Pagenkopp Lohan. This is contribution number 2 from the Smithsonian's Tennenbaum Marine Observatories Network. NR 58 TC 2 Z9 2 U1 4 U2 16 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD MAY PY 2015 VL 162 IS 5 BP 957 EP 968 DI 10.1007/s00227-015-2637-5 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CF8IC UT WOS:000352798800005 ER PT J AU Faircloth, BC Branstetter, MG White, ND Brady, SG AF Faircloth, Brant C. Branstetter, Michael G. White, Noor D. Brady, Sean G. TI Target enrichment of ultraconserved elements from arthropods provides a genomic perspective on relationships among Hymenoptera SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE arthropods; baits; conserved sequence; Hymenoptera; probes; target enrichment; ultraconserved elements ID HONEYBEE APIS-MELLIFERA; DNA-SEQUENCING DATA; MOLECULAR-DATA; PHYLOGENETIC ANALYSES; SPECIES RICHNESS; SOCIAL INSECTS; SISTER GROUP; ANTS; EVOLUTION; DIVERSIFICATION AB Gaining a genomic perspective on phylogeny requires the collection of data from many putatively independent loci across the genome. Among insects, an increasingly common approach to collecting this class of data involves transcriptome sequencing, because few insects have high-quality genome sequences available; assembling new genomes remains a limiting factor; the transcribed portion of the genome is a reasonable, reduced subset of the genome to target; and the data collected from transcribed portions of the genome are similar in composition to the types of data with which biologists have traditionally worked (e.g. exons). However, molecular techniques requiring RNA as a template, including transcriptome sequencing, are limited to using very high-quality source materials, which are often unavailable from a large proportion of biologically important insect samples. Recent research suggests that DNA-based target enrichment of conserved genomic elements offers another path to collecting phylogenomic data across insect taxa, provided that conserved elements are present in and can be collected from insect genomes. Here, we identify a large set (n=1510) of ultraconserved elements (UCEs) shared among the insect order Hymenoptera. We used in silico analyses to show that these loci accurately reconstruct relationships among genome-enabled hymenoptera, and we designed a set of RNA baits (n=2749) for enriching these loci that researchers can use with DNA templates extracted from a variety of sources. We used our UCE bait set to enrich an average of 721 UCE loci from 30 hymenopteran taxa, and we used these UCE loci to reconstruct phylogenetic relationships spanning very old (220Ma) to very young (1Ma) divergences among hymenopteran lineages. In contrast to a recent study addressing hymenopteran phylogeny using transcriptome data, we found ants to be sister to all remaining aculeate lineages with complete support, although this result could be explained by factors such as taxon sampling. We discuss this approach and our results in the context of elucidating the evolutionary history of one of the most diverse and speciose animal orders. C1 [Faircloth, Brant C.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Faircloth, Brant C.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Branstetter, Michael G.; Brady, Sean G.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [White, Noor D.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [White, Noor D.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Faircloth, BC (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. EM brant@faircloth-lab.org OI White, Noor/0000-0002-9510-3744; Faircloth, Brant/0000-0002-1943-0217 FU Consortium for Understanding and Sustaining a Biodiverse Planet; Smithsonian Institution Buck Postdoctoral Fellowship; NSF [DEB-1354739, DEB-1354996]; Amazon Web Services Education Grant FX A Smithsonian Institution grant from the Consortium for Understanding and Sustaining a Biodiverse Planet (to SGB, BCF, and NDW) provided most of the funding for this project and support for NDW's participation. A Smithsonian Institution Buck Postdoctoral Fellowship and NSF grants DEB-1354739 and DEB-1354996 (project ADMAC) supported MGB. NSF DEB-1242260 (to BCF) and an Amazon Web Services Education Grant (to BCF) supported computational portions of this work. NSF EF-0431330 (to SGB) provided resources to obtain some specimens used in this study. This study was also supported in part by resources and technical expertise from the Georgia Advanced Computing Resource Center, a partnership between the University of Georgia's Office of the Vice President for Research and Office of the Vice President for Information Technology. NR 89 TC 31 Z9 31 U1 11 U2 52 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-098X EI 1755-0998 J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAY PY 2015 VL 15 IS 3 BP 489 EP 501 DI 10.1111/1755-0998.12328 PG 13 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA CF6FY UT WOS:000352653700004 PM 25207863 ER PT J AU Hwang, GC Post, JE Lee, Y AF Hwang, Gil Chan Post, Jeffrey E. Lee, Yongjae TI In situ high-pressure synchrotron X-ray powder diffraction study of tunnel manganese oxide minerals: hollandite, romanechite, and todorokite SO PHYSICS AND CHEMISTRY OF MINERALS LA English DT Article DE Manganese oxide; Hollandite; Romanechite; Todorokite; High pressure ID REFINEMENT; NATROLITES; ZEOLITES; BEHAVIOR; PHASE AB In situ high-pressure synchrotron X-ray powder diffraction study of three tunnel manganese oxide minerals (hollandite with 2 x 2 MnO6 octahedra tunnels, romanechite with 2 x 3 tunnels, and todorokite with 3 x 3 tunnels) was performed using a diamond anvil cell and nominally penetrating alcohol and water mixture as a pressure-transmitting medium up to similar to 8 GPa. Bulk moduli (B (0)) calculated using Murnaghan's equation of state are inversely proportional to the size of the tunnel, i.e., 134(4) GPa for hollandite (I2/m), 108(2) GPa for romanechite (C2/m), and 67(5) GPa for todorokite (P2/m). On the other hand, axial compressibilities show different elastic anisotropies depending on the size of the tunnel, i.e., (a/a (0)) = -0.00066(3) GPa(-1), (b/b (0)) = 0.00179(8) GPa(-1), (c/c (0)) = 0.00637(4) GPa(-1) [c > b > a] for hollandite; (a/a (0)) = 0.00485(4) GPa(-1), (b/b (0)) = 0.0016(1) GPa(-1), (c/c (0)) = 0.00199(8) GPa(-1) [a > c > b] for romanechite; and (a/a (0)) = 0.00826(9) GPa(-1), (b/b (0)) = 0.0054(1) GPa(-1), (c/c (0)) = 0.00081(8) GPa(-1) [a > b > c] for todorokite. Overall, the degree of tunnel distortion increases with increasing pressure and correlates with the size of the tunnel, which is evidenced by the gradual increases in the monoclinic beta angles up to 3 GPa of 0.62A degrees, 0.8A degrees, and 1.15A degrees in hollandite, romanechite, and todorokite, respectively. The compression of tunnel manganese oxides is related to the tunnel distortion and the size of the tunnel. C1 [Hwang, Gil Chan; Lee, Yongjae] Yonsei Univ, Dept Earth Syst Sci, Seoul 120749, South Korea. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Lee, Y (reprint author), Yonsei Univ, Dept Earth Syst Sci, Seoul 120749, South Korea. EM yongjaelee@yonsei.ac.kr RI Lee, Yongjae/K-6566-2016 FU Global Research Laboratory Program of the Korean Ministry of Science, ICT and Planning (MSIP); U.S. Department of Energy, Office of Basic Energy Sciences; Yonsei University [2014-12-0140]; NSF [EAR-0745374, EAR11-47728] FX This work was supported by the Global Research Laboratory Program of the Korean Ministry of Science, ICT and Planning (MSIP). Experiments using synchrotron were supported by Pohang Accelerator Laboratory in Korea through the abroad beamtime program of Synchrotron Radiation Facility Project under the MSIP and have been performed under the approval of the NSLS. Research carried out in part at the NSLS at BNL is supported by the U.S. Department of Energy, Office of Basic Energy Sciences. GCH thanks the support from the Yonsei University Research Fund of 2014-12-0140. JEP acknowledges funding by NSF grants EAR-0745374 and EAR11-47728. NR 22 TC 1 Z9 1 U1 4 U2 24 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0342-1791 EI 1432-2021 J9 PHYS CHEM MINER JI Phys. Chem. Miner. PD MAY PY 2015 VL 42 IS 5 BP 405 EP 411 DI 10.1007/s00269-014-0731-8 PG 7 WC Materials Science, Multidisciplinary; Mineralogy SC Materials Science; Mineralogy GA CF9RT UT WOS:000352904400007 ER PT J AU Huffer, D Oxenham, M AF Huffer, Damien Oxenham, Marc TI How Much Life do I Lose from the Plague? Educational Board Games as Teaching Tools in Archaeology and Ancient History Courses SO PUBLIC ARCHAEOLOGY LA English DT Article DE ancient history; archaeology; course design; educational board games; pedagogy AB This article describes the development, implementation, assessment, debriefing and outcomes, and potential uses of a university student-driven educational gaming project, as a major assessment item in an archaeology course entitled Ancient Medicine'. Discussion of these various aspects of the project is explored in the context of educational gaming theory and practice. We demonstrate that educational board games not only represent an effective method for students to retain and convey information in courses exploring the history and archaeology of medicine, but provide such a platform for undergraduate courses in general. Furthermore, we argue that they can present a cost-effective, fun and less time-/resource-intensive alternative to electronic or web-based projects, while still being an attractive addition to traditional classroom teaching methods. C1 [Huffer, Damien] Smithsonian Inst, Washington, DC 20560 USA. [Oxenham, Marc] Australian Natl Univ, Canberra, ACT 0200, Australia. RP Oxenham, M (reprint author), Australian Natl Univ, Sch Archaeol & Anthropol, AD Hope Bldg 14, Canberra, ACT 0200, Australia. EM hufferd@si.edu; Marc.Oxenham@anu.edu NR 18 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1465-5187 EI 1753-5530 J9 PUBLIC ARCHAEOL JI Public Archaeol. PD MAY PY 2015 VL 14 IS 2 BP 81 EP 91 DI 10.1080/14655187.2015.1112692 PG 11 WC Archaeology SC Archaeology GA DP6PY UT WOS:000378620900002 ER PT J AU Grosholz, ED Crafton, RE Fontana, RE Pasari, JR Williams, SL Zabin, CJ AF Grosholz, Edwin D. Crafton, R. Eliot Fontana, Rachel E. Pasari, Jae R. Williams, Susan L. Zabin, Chela J. TI Aquaculture as a vector for marine invasions in California SO BIOLOGICAL INVASIONS LA English DT Article DE Invasive; Marine; Aquaculture; Vector; Impacts; California ID BALLAST WATER; NORTH-AMERICA; UNITED-STATES; ECOSYSTEMS; MANAGEMENT; ESTUARINE; ECOLOGY AB Although ballast water and hull fouling are widely recognized as important vectors for marine invasions, the risk posed by commercial aquaculture remains poorly quantified. To understand the importance of aquaculture as an invasion vector in California, we conducted an analysis of both current and historical introductions of marine and estuarine species associated with aquaculture using a comprehensive database ('NEMESIS') and permitting records for species imported into California. Our results showed that 126 non-native species associated with commercial aquaculture have been reported from California waters and 106 of these have become established. The vast majority are unintentional introductions linked to historical importation practices of the aquaculture industry. To understand the consequences of these invasions, we reviewed the literature on the impacts of mollusk and algal species introduced into California via aquaculture. Of the few studies we found, the majority demonstrated negative impacts on native species. Finally and significantly, we found that changes in aquaculture importation practices over the past decade have resulted in most shellfish currently being imported as larvae or juveniles. Consequently, rates of unintentional introductions have been reduced. We cautiously conclude that current aquaculture importation in California represents a minor risk as a vector for introductions of NIS. C1 [Grosholz, Edwin D.; Zabin, Chela J.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Crafton, R. Eliot; Fontana, Rachel E.] Univ Calif Davis, Grad Grp Ecol, Davis, CA 95616 USA. [Fontana, Rachel E.; Pasari, Jae R.; Williams, Susan L.] Univ Calif Davis, Bodega Marine Lab, Bodega Bay, CA 94923 USA. [Fontana, Rachel E.; Pasari, Jae R.; Williams, Susan L.] Univ Calif Davis, Dept Ecol & Evolut, Bodega Bay, CA 94923 USA. [Fontana, Rachel E.] NOAA, Off Ocean & Atmospher Res, Silver Spring, MD 20910 USA. [Zabin, Chela J.] Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. RP Grosholz, ED (reprint author), Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. EM tedgrosholz@ucdavis.edu FU California Ocean Protection Council; California Ocean Science Trust FX We wish to thank the Smithsonian Environmental Research Center's Marine Invasions Research Laboratory and in particular G. Ruiz, B. Steves and P. Fofonoff, for facilitating access to the NEMESIS California database. We would also like to thank the many state and federal agency officials who volunteered their time and effort for our work including K. Holzer, J. Moore and K. Ramey. We also thank the Executive Director (S. McAfee) and staff of the Ocean Science Trust (R. Gentry, E. Kramer-Wilt) for facilitating the project and coordinating project investigators. This work was supported by the California Ocean Protection Council through Proposition 84 funds as well as additional support from the California Ocean Science Trust. NR 25 TC 5 Z9 5 U1 7 U2 40 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 EI 1573-1464 J9 BIOL INVASIONS JI Biol. Invasions PD MAY PY 2015 VL 17 IS 5 BP 1471 EP 1484 DI 10.1007/s10530-014-0808-9 PG 14 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CF3HK UT WOS:000352438800015 ER PT J AU Fehlauer-Ale, KH Winston, JE Tilbrook, KJ Nascimento, KB Vieira, LM AF Fehlauer-Ale, Karin H. Winston, Judith E. Tilbrook, Kevin J. Nascimento, Karine B. Vieira, Leandro M. TI Identifying monophyletic groups within Bugula sensu lato ( Bryozoa, Buguloidea) SO ZOOLOGICA SCRIPTA LA English DT Article ID MOLECULAR PHYLOGENY; CHEILOSTOMATA; PATTERNS; SHORELINE; SEQUENCES; TAXONOMY; NERITINA; BARCODE; KOREA; COAST AB Species in the genus Bugula are globally distributed. They are most abundant in tropical and temperate shallow waters, but representatives are found in polar regions. Seven species occur in the Arctic and one in the Antarctic and species are represented in continental shelf or greater depths as well. The main characters used to define the genus include bird's head pedunculate avicularia, erect colonies, embryos brooded in globular ooecia and branches comprising two or more series of zooids. Skeletal morphology has been the primary source of taxonomic information for many calcified bryozoan groups, including the Buguloidea. Several morphological characters, however, have been suggested to be homoplastic at distinct taxonomic levels, in the light of molecular phylogenies. Our purpose was to investigate the phylogenetic interrelationships of the genus Bugula, based on molecular phylogenetics and morphology. A Bayesian molecular phylogeny was constructed using original and previously published sequences of the mitochondrial genes cytochrome c oxidase subunit 1 (COI) and the large ribosomal RNA subunit (16S). Morphological characteristics from scanning electron and light microscopy were used to confirm the clades detected by the molecular phylogeny. Our results suggest that the genus is composed of four clades, for which we provide diagnoses: Bugula sensu stricto (30 species), Bugulina (24 species), Crisularia (23 species) and the monotypic Virididentula gen. n. Ten species could not be assigned to any of those genera, so they remain as genus incertae sedis. Our findings highlight the importance of using molecular phylogenies in association with morphological characters in systematic revisions of bryozoan taxa. C1 [Fehlauer-Ale, Karin H.] Univ Fed Parana, Ctr Estudos Mar, Lab Bentos, BR-83255976 Pontal Do Parana, PR, Brazil. [Fehlauer-Ale, Karin H.; Nascimento, Karine B.; Vieira, Leandro M.] Univ Sao Paulo, Ctr Biol Marinha, Lab Sistemat & Evolucao Bryozoa, BR-05588000 Sao Sebastiao, SP, Brazil. [Winston, Judith E.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Tilbrook, Kevin J.] Univ Oxford, Museum Nat Hist, Oxford OX1 3PW, England. [Vieira, Leandro M.] Univ Fed Pernambuco, Dept Zool, Ctr Ciencias Biol, BR-50670901 Recife, PE, Brazil. RP Fehlauer-Ale, KH (reprint author), Univ Fed Parana, Ctr Estudos Mar, Lab Bentos, Ave Beira Mar,Caixa Postal 61, BR-83255976 Pontal Do Parana, PR, Brazil. EM fehlauer.ale@gmail.com; judithewinston@gmail.com; kevin_j_tilbrook@yahoo.co.uk; kbnasc@gmail.com; leandromanzoni@hotmail.com RI Vieira, Leandro/B-7712-2011; Hoch Fehlauer Ale, Karin/D-6628-2011; OI Hoch Fehlauer Ale, Karin/0000-0002-6617-2062; Manzoni Vieira, Leandro/0000-0001-8661-8861 FU National Council for Scientific and Technological Development (CNPq) [151221/2013-8, 305608/2006-1, 474605/2013-2, 564945/2010-2 - 'BrBol']; Sao Paulo Research Foundation (FAPESP) [2009/08940-7, 2009/08941-3, 2012/24285-1] FX This is a contribution of the Center for Marine Studies, Federal University of Parana (CEM/UFPR), the Center for Marine Biology of the University of Sao Paulo (CEBIMar/USP) and the Center for Marine Biodiversity Research (NP-BioMar/USP). This research was partially supported by The National Council for Scientific and Technological Development (CNPq) (151221/2013-8, granted to Paulo C. Lana and Karin H. Fehlauer-Ale; 305608/2006-1, 474605/2013-2, granted to Leandro M. Vieira; 564945/2010-2 - 'BrBol', granted to Mariana C de Oliveira) and the Sao Paulo Research Foundation (FAPESP) (2009/08940-7, granted to Karin H Fehlauer-Ale; 2009/08941-3 to Alvaro E Migotto; 2012/24285-1, granted to Leandro M Vieira). Contribution no. 979 from the Smithsonian Marine Station, Fort Pierce, Florida. We wish to thank Alvaro E. Migotto (Center for Marine Biology of the University of Sao Paulo), Paulo C. Lana (Center for Marine Studies of the Federal University of Parana) and Tim Littlewood (Natural History Museum of London) for providing laboratory and office facilities. Several collaborators donated exemplars and/or helped with fieldwork, and we are very grateful to all of them: Alberto Lindner (Federal University of Santa Catarina), Andrea Waeschenbach (Natural History Museum of London), Arnaud Czaja (Imperial College of London), Dennis Gordon (National Institute of Water & Atmospheric Research), Javier Souto (University of Santiago de Compostela), Judith Fuchs (Marine Biological Association UK), Oscar Reverter-Gil (University of Santiago de Compostela) and Rosana M. da Rocha (Federal University of Parana). Andrew Ostrovsky provided helpful information on brood chamber structures included in this study. Three anonymous reviewers provided very helpful comments and suggestions on the manuscript. NR 113 TC 4 Z9 4 U1 1 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0300-3256 EI 1463-6409 J9 ZOOL SCR JI Zool. Scr. PD MAY PY 2015 VL 44 IS 3 BP 334 EP 347 DI 10.1111/zsc.12103 PG 14 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA CF5PG UT WOS:000352608600008 ER PT J AU Sues, HD Averianov, A AF Sues, Hans-Dieter Averianov, Alexander TI New material of Caenagnathasia martinsoni (Dinosauria: Theropoda: Oviraptorosauria) from the Bissekty Formation (Upper Cretaceous: Turonian) of Uzbekistan SO CRETACEOUS RESEARCH LA English DT Article DE Dinosauria; Theropoda; Oviraptorosauria; Caenagnathidae; Cretaceous; Uzbekistan ID OSTEOLOGY; ASIA AB The oviraptorosaurian theropod Caenagnathasia martinsoni is the least common dinosaur taxon in the Late Cretaceous (Turonian) vertebrate assemblage from the Bissekty Formation of the Kyzylkum Desert, Uzbekistan. The dentaries show numerous caenagnathid synapomorphies, including a fused dentary symphysis bearing distinct vascular grooves and associated foramina on its lingual surface, a lingual triturating shelf on the dentary, and extensive pneumatization of the dentary. Cervical and dorsal vertebrae attributed to C. martinsoni show a structure typical for Caenagnathoidea, whereas a referred partial femur is relatively plesiomorphic in having a large, finger-like anterior (lesser) trochanter separated from the greater trochanter. A referred synsacrum has only four vertebrae but may represent an immature individual. Caenagnathasia martinsoni is closely related to the clade comprising the North American Campanian-Maastrichtian caenagnathids. Published by Elsevier Ltd. C1 [Sues, Hans-Dieter] Natl Museum Nat Hist, Smithsonian Inst, 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, St Petersburg 199178, Russia. RP Sues, HD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, 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; 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 DJ. Ward. We thank P.R. Bell, Editor E. Koutsoukos, and an anonymous reviewer for helpful comments on a draft of the manuscript. The field work in 1997-2006 was funded by 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), and the Navoi Mining and Metallurgy Combinat. The laboratory research by AA is supported by the Russian Scientific Fund (14-14-00015). NR 32 TC 3 Z9 4 U1 0 U2 7 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 MAY PY 2015 VL 54 BP 50 EP 59 DI 10.1016/j.cretres.2014.12.001 PG 10 WC Geology; Paleontology SC Geology; Paleontology GA CE4KR UT WOS:000351800000005 ER PT J AU Wang, HQ Richardson, MI AF Wang, Huiqun Richardson, Mark I. TI The origin, evolution, and trajectory of large dust storms on Mars during Mars years 24-30 (1999-2011) SO ICARUS LA English DT Article DE Mars; Mars, atmosphere; Image processing ID GENERAL-CIRCULATION MODEL; NORTHERN-HEMISPHERE; GLOBAL SURVEYOR; ORBITER CAMERA; INTERANNUAL VARIABILITY; MARTIAN ATMOSPHERE; DYNAMICS; OPACITY; SURFACE; WAVES AB Mars Daily Global Maps (MDGM) derived from the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) and Mars Reconnaissance Orbiter (MRO) Mars Color Imager (MARCI) are used to study the distribution and evolution of large dust storms over the period from Mars years 24-30 (1999-2001). Large storms are defined here as discrete dust events visible in image sequences extending over at least 5 sols (Mars days) and where the dust covers areas beyond the origination region. A total of 65 large dust storms meeting these criteria are identified during the observational period and all are observed during the L-s = 135-30 degrees seasonal window. Dust storms originating in the northern and southern hemispheres appear to form two distinct families. All but two of the storms originating in the northern hemisphere are observed in two seasonal windows at L-s = 180-240 degrees and L-s = 305-350 degrees; while all but two of those originating in the southern hemisphere are observed during L-s = 135-245 degrees. None of the large dust storms originating in the northern hemisphere are observed to develop to global scale, but some of them develop into large regional storms with peak area >1 x 10(7) km(2) and duration on the order of several weeks. In comparison, large dust storms originating in the southern hemisphere are typically much smaller, except notably in the two cases that expanded to global scale (the 2001 and 2007 global storms). Distinct locations of preferred storm origination emerge from the dust storm image sequences, including Acidalia, Utopia, Arcadia and Hellas. A route (trajectory) 'graph' for the observed sequences is provided. The routes are highly asymmetric between the two hemispheres. In the south, for non-global dust storms, the main routes are primarily oriented eastwest, whereas in the north, the routes are primarily north-south and zonally-concentrated into meridional channels. In a few impressive cases, storms originating in the northern hemisphere are observed to "flush" through Acidalia and Utopia, across the equator, and then branch in the low- and mid-southern latitudes. The origin of the 2007 global dust storm is ambiguous from the imaging data. Immediately prior to the global storm, a dust storm sequence from Chryse is identified. This storm's connection to the explosive expansion observed to start from Noachis/ West Hellas is unclear due to image coverage. This paper further identifies and describes three different styles of dust storm development, which we refer to as "consecutive dust storms", "sequential activation" and "merging." The evolution of a given dust storm sequence can exhibit different combinations of these growth styles at different stages of development. Dust storm sequences can overlap in time, which makes them good candidate to grow into larger scale. (C) 2013 Elsevier Inc. All rights reserved. C1 [Wang, Huiqun] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Richardson, Mark I.] Ashima Res, Pasadena, CA 91101 USA. RP Wang, HQ (reprint author), MS 50,60 Garden St, Cambridge, MA 02138 USA. EM hwang@cfa.harvard.edu FU NASA's Mars Data Analysis program FX This paper is supported by NASA's Mars Data Analysis program. We thank Michael D. Smith for providing the gridded TES and THE-MIS data that are used in Fig. 9. We thank Michael D. Smith and Alexey Pankine for their reviews. NR 32 TC 22 Z9 22 U1 4 U2 16 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 MAY 1 PY 2015 VL 251 BP 112 EP 127 DI 10.1016/j.icarus.2013.10.033 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0FQ UT WOS:000351480300008 ER PT J AU Nelles, A Schellart, P Buitink, S Corstanje, A de Vries, KD Enriquez, JE Falcke, H Frieswijk, W Horandel, JR Scholten, O ter Veen, S Thoudam, S van den Akker, M Anderson, J Asgekar, A Bell, ME Bentum, MJ Bernardi, G Best, P Bregman, J Breitling, F Broderick, J Brouw, WN Bruggen, M Butcher, HR Ciardi, B Deller, A Duscha, S Eisloffel, J Fallows, RA Garrett, MA Gunst, AW Hassall, TE Heald, G Horneffer, A Iacobelli, M Juette, E Karastergiou, A Kondratiev, VI Kramer, M Kuniyoshi, M Kuper, G Maat, P Mann, G Mevius, M Norden, MJ Paas, H Pandey-Pommier, M Pietka, G Pizzo, R Polatidis, AG Reich, W Rottgering, H Scaife, AMM Schwarz, D Smirnov, O Stappers, BW Steinmetz, M Stewart, A Tagger, M Tang, Y Tasse, C Vermeulen, R Vocks, C van Weeren, RJ Wijnholds, SJ Wucknitz, O Yatawatta, S Zarka, P AF Nelles, A. Schellart, P. Buitink, S. Corstanje, A. de Vries, K. D. Enriquez, J. E. Falcke, H. Frieswijk, W. Hoerandel, J. R. Scholten, O. ter Veen, S. Thoudam, S. van den Akker, M. Anderson, J. Asgekar, A. Bell, M. E. Bentum, M. J. Bernardi, G. Best, P. Bregman, J. Breitling, F. Broderick, J. Brouw, W. N. Brueggen, M. Butcher, H. R. Ciardi, B. Deller, A. Duscha, S. Eisloeffel, J. Fallows, R. A. Garrett, M. A. Gunst, A. W. Hassall, T. E. Heald, G. Horneffer, A. Iacobelli, M. Juette, E. Karastergiou, A. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Kuper, G. Maat, P. Mann, G. Mevius, M. Norden, M. J. Paas, H. Pandey-Pommier, M. Pietka, G. Pizzo, R. Polatidis, A. G. Reich, W. Roettgering, H. Scaife, A. M. M. Schwarz, D. Smirnov, O. Stappers, B. W. Steinmetz, M. Stewart, A. Tagger, M. Tang, Y. Tasse, C. Vermeulen, R. Vocks, C. van Weeren, R. J. Wijnholds, S. J. Wucknitz, O. Yatawatta, S. Zarka, P. TI Measuring a Cherenkov ring in the radio emission from air showers at 110-190 MHz with LOFAR SO ASTROPARTICLE PHYSICS LA English DT Article DE Cosmic rays; Extensive air showers; Radio emission; LOFAR; Time-compression ID PULSES; RADIATION; ARRAY AB Measuring radio emission from air showers offers a novel way to determine properties of the primary cosmic rays such as their mass and energy. Theory predicts that relativistic time compression effects lead to a ring of amplified emission which starts to dominate the emission pattern for frequencies above similar to 100 MHz. In this article we present the first detailed measurements of this structure. Ring structures in the radio emission of air showers are measured with the LOFAR radio telescope in the frequency range of 110-190 MHz. These data are well described by CoREAS simulations. They clearly confirm the importance of including the index of refraction of air as a function of height. Furthermore, the presence of the Cherenkov ring offers the possibility for a geometrical measurement of the depth of shower maximum, which in turn depends on the mass of the primary particle. (C) 2014 Elsevier B.V. All rights reserved. C1 [Nelles, A.; Schellart, P.; Buitink, S.; Corstanje, A.; Enriquez, J. E.; Falcke, H.; Hoerandel, J. R.; ter Veen, S.; Thoudam, S.; van den Akker, M.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Nelles, A.; Falcke, H.; Hoerandel, J. R.] Nikhef, NL-1098 XG Amsterdam, Netherlands. [de Vries, K. D.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Falcke, H.; Frieswijk, W.; Asgekar, A.; Bentum, M. J.; Bregman, J.; Brouw, W. N.; Deller, A.; Duscha, S.; Fallows, R. A.; Garrett, M. A.; Gunst, A. W.; Heald, G.; Kondratiev, V. I.; Kuper, G.; Maat, P.; Mevius, M.; Norden, M. J.; Pizzo, R.; Polatidis, A. G.; Tang, Y.; Vermeulen, R.; Wijnholds, S. J.; Yatawatta, S.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Falcke, H.; Horneffer, A.; Kramer, M.; Kuniyoshi, M.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Scholten, O.] Univ Groningen, KVI, NL-9747 AA Groningen, Netherlands. [Anderson, J.; Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Asgekar, A.] Shell Technol Ctr, Bangalore, Karnataka, India. [Bell, M. E.] Univ Sydney, Sydney Inst Astron, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Broderick, J.; Hassall, T. E.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Brouw, W. N.; Mevius, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Brueggen, M.] 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.] Thuringer Landesstemwarte, D-07778 Tautenburg, Germany. [Garrett, M. A.; Iacobelli, M.; Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Hassall, T. E.; Kramer, M.; Stappers, B. W.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Juette, E.] Ruhr Univ Bochum, Inst Astron, D-44780 Bochum, Germany. [Karastergiou, A.; Stewart, A.] Univ Oxford, Oxford OX1 3RH, England. [Kondratiev, V. I.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [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. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Smirnov, O.] Rhodes Univ, Ctr Radio Astron Techn ET Technol RATT, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Afr, ZA-7405 Pinelands, South Africa. [Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45067 Orleans, France. [Tasse, C.; Zarka, P.] Observ Paris, LESIA, UMR CNRS 8109, F-92195 Meudon, France. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Nelles, A (reprint author), Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM a.nelles@astro.ru.nl RI Tagger, Michel/O-6615-2014; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Yatawatta, Sarod/E-6037-2013; OI Tagger, Michel/0000-0003-2962-3220; Kondratiev, Vladislav/0000-0001-8864-7471; Yatawatta, Sarod/0000-0001-5619-4017; Deller, Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660 FU Netherlands Research School for Astronomy (NOVA); Samenwerkingsverband Noord-Nederland (SNN); Foundation for Fundamental Research on Matter (FOM); Netherlands Organization for Scientific Research (NWO); VENI [639-041-130]; Advanced Grant of the European Research Council; European Union [227610] FX We thank both the internal and external reviewers for the fruitful discussions regarding this article. The LOFAR cosmic ray key science project very much acknowledges the scientific and technical support from ASTRON. Furthermore, we acknowledge financial support from the Netherlands Research School for Astronomy (NOVA), the Samenwerkingsverband Noord-Nederland (SNN), the Foundation for Fundamental Research on Matter (FOM) and the Netherlands Organization for Scientific Research (NWO), VENI Grant 639-041-130. We acknowledge funding from an Advanced Grant of the European Research Council under the European Union's Seventh Framework Program (FP/2007-2013)/ERC Grant Agreement no. 227610. NR 29 TC 14 Z9 14 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD MAY PY 2015 VL 65 BP 11 EP 21 DI 10.1016/j.astropartphys.2014.11.006 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CB6GK UT WOS:000349725300002 ER PT J AU Perez, K Hailey, CJ Bauer, FE Krivonos, RA Mori, K Baganoff, FK Barriere, NM Boggs, SE Christensen, FE Craig, WW Grefenstette, BW Grindlay, JE Harrison, FA Hong, J Madsen, KK Nynka, M Stern, D Tomsick, JA Wik, DR Zhang, S Zhang, WW Zoglauer, A AF Perez, Kerstin Hailey, Charles J. Bauer, Franz E. Krivonos, Roman A. Mori, Kaya Baganoff, Frederick K. Barriere, Nicolas M. Boggs, Steven E. Christensen, Finn E. Craig, William W. Grefenstette, Brian W. Grindlay, Jonathan E. Harrison, Fiona A. Hong, Jaesub Madsen, Kristin K. Nynka, Melania Stern, Daniel Tomsick, John A. Wik, Daniel R. Zhang, Shuo Zhang, William W. Zoglauer, Andreas TI Extended hard-X-ray emission in the inner few parsecs of the Galaxy SO NATURE LA English DT Article ID XMM-NEWTON OBSERVATIONS; SAGITTARIUS-A-EAST; GALACTIC-CENTER; BLACK-HOLE; MILLISECOND PULSARS; CANDIDATE; RIDGE; SGR; VARIABILITY; LUMINOSITY AB The Galactic Centre hosts a puzzling stellar population in its inner few parsecs, with a high abundance of surprisingly young, relatively massive stars bound within the deep potential well of the central supermassive black hole, Sagittarius A* (ref. 1). Previous studies suggest that the population of objects emitting soft X-rays (less than 10 kiloelectronvolts) within the surrounding hundreds of parsecs, as well as the population responsible for unresolved X-ray emission extending along the Galactic plane, is dominated by accreting white dwarf systems'. Observations of diffuse hardX-ray (more than 10 kiloelectronvolts) emission in the inner 10 parsecs, however, have been hampered by the limited spatial resolution of previous instruments. Here we report the presence of a distinct hard-X-ray component within the central 4 X 8 parsecs, as revealed by subarcminute-resolution images in the 20-40 kiloelectronvolt range. This emission is more sharply peaked towards the Galactic Centre than is the surface brightness of the soft-X-ray population'. This could indicate a significantly more massive population of accreting white dwarfs, large populations of lowmass X-ray binaries or millisecond pulsars, or particle outflows interacting with the surrounding radiation field, dense molecular material or magnetic fields. However, all these interpretations pose significant challenges to our understanding of stellar evolution, binary formation, and cosmic-ray production in the Galactic Centre. C1 [Perez, Kerstin; Hailey, Charles J.; Mori, Kaya; Nynka, Melania; Zhang, Shuo] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Perez, Kerstin] Haverford Coll, Haverford, PA 19041 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Krivonos, Roman A.; Barriere, Nicolas M.; Boggs, Steven E.; Craig, William W.; Tomsick, John A.; Zoglauer, Andreas] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 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 94551 USA. [Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Grindlay, Jonathan E.; Hong, Jaesub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wik, Daniel R.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Perez, K (reprint author), Columbia Univ, Columbia Astrophys Lab, 550 West 120th St,Room 1027, New York, NY 10027 USA. EM kperez1@haverford.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Madsen, Kristin/0000-0003-1252-4891; Krivonos, Roman/0000-0003-2737-5673 FU NASA [NNG08FD60C]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1141218, EMBIGGEN Anillo ACT1101]; Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009] FX This work was supported by NASA contract no. NNGO8FD60C, 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 NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We also than kA. Canipe, J. Dodaro, D. Hong and T.V.T. Luu for assistance with data preparation and analysis. F.E.B. acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile (FONDECYT 1141218 and EMBIGGEN Anillo ACT1101), and Project IC120009 "Millennium Institute of Astrophysics (MAS)" funded by the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo. NR 46 TC 15 Z9 15 U1 1 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 APR 30 PY 2015 VL 520 IS 7549 BP 646 EP U138 DI 10.1038/nature14353 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH0DQ UT WOS:000353689700043 PM 25925477 ER PT J AU Pukazhenthi, BS Nagashima, J Travis, AJ Costa, GM Escobar, EN Franca, LR Wildt, DE AF Pukazhenthi, Budhan S. Nagashima, Jennifer Travis, Alexander J. Costa, Guilherme M. Escobar, Enrique N. Franca, Luiz R. Wildt, David E. TI Slow Freezing, but Not Vitrification Supports Complete Spermatogenesis in Cryopreserved, Neonatal Sheep Testicular Xenografts SO PLOS ONE LA English DT Article ID TESTIS TISSUE; RECIPIENT MICE; SPERMATOGONIAL SURVIVAL; GENETIC MATERIAL; GONADAL TISSUES; MOUSE TESTES; SPERM; PORCINE; CELLS; TRANSPLANTATION AB The ability to spur growth of early stage gametic cells recovered from neonates could lead to significant advances in rescuing the genomes of rare genotypes or endangered species that die unexpectedly. The purpose of this study was to determine, for the first time, the ability of two substantially different cryopreservation approaches, slow freezing versus vitrification, to preserve testicular tissue of the neonatal sheep and subsequently allow initiation of spermatogenesis post-xenografting. Testis tissue from four lambs (3-5 wk old) was processed and then untreated or subjected to slow freezing or vitrification. Tissue pieces (fresh, n = 214; slow freezing, then thawing, n = 196; vitrification, then warming, n = 139) were placed subcutaneously under the dorsal skin of SCID mice and then grafts recovered and evaluated 17 wk later. Grafts from fresh and slow frozen tissue contained the most advanced stages of spermatogenesis, including normal tubule architecture with elongating spermatids in similar to 1% (fresh) and similar to 10% (slow frozen) of tubules. Fewer than 2% of seminiferous tubules advanced to the primary spermatocyte stage in xenografts derived from vitrified tissue. Results demonstrate that slow freezing of neonatal lamb testes was far superior to vitrification in preserving cellular integrity and function after xenografting, including allowing similar to 10% of tubules to retain the capacity to resume spermatogenesis and yield mature spermatozoa. Although a first for any ruminant species, findings also illustrate the importance of preemptive studies that examine cryo-sensitivity of testicular tissue before attempting this type of male fertility preservation on a large scale. C1 [Pukazhenthi, Budhan S.; Nagashima, Jennifer; Wildt, David E.] Ctr Species Survival, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Nagashima, Jennifer; Travis, Alexander J.] Cornell Univ, Coll Vet Med, Baker Inst Anim Hlth, Ithaca, NY 14853 USA. [Travis, Alexander J.] Cornell Univ, Atkinson Ctr Sustainable Future, Ithaca, NY USA. [Costa, Guilherme M.] Univ Fed Minas Gerais, Dept Morphol, Lab Cellular Biol, Belo Horizonte, MG, Brazil. [Escobar, Enrique N.] Univ Maryland Eastern Shore, Dept Agr Food & Resource Sci, Sch Agr & Nat Sci, Princess Anne, MD USA. RP Pukazhenthi, BS (reprint author), Ctr Species Survival, Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. EM pukazhenthib@si.edu RI Mattos Jardim Costa, Guilherme/A-7369-2016 OI Mattos Jardim Costa, Guilherme/0000-0002-2907-7760 FU Sichel Endowment Fund FX This study was supported with funding from the Sichel Endowment Fund. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 72 TC 6 Z9 7 U1 1 U2 8 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 29 PY 2015 VL 10 IS 4 AR e0123957 DI 10.1371/journal.pone.0123957 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH0LO UT WOS:000353711600064 PM 25923660 ER PT J AU Ruggiero, MA Gordon, DP Orrell, TM Bailly, N Bourgoin, T Brusca, RC Cavalier-Smith, T Guiry, MD Kirk, PM AF Ruggiero, Michael A. Gordon, Dennis P. Orrell, Thomas M. Bailly, Nicolas Bourgoin, Thierry Brusca, Richard C. Cavalier-Smith, Thomas Guiry, Michael D. Kirk, Paul M. TI A Higher Level Classification of All Living Organisms SO PLOS ONE LA English DT Article ID ANIMAL PHYLOGENY; EVOLUTIONARY HISTORY; GENE-SEQUENCES; EUKARYOTES; ACANTHOCEPHALA; DIVERSITY; ROTIFERA; LIFE; GNATHOSTOMULIDA; MICROGNATHOZOA AB We present a consensus classification of life to embrace the more than 1.6 million species already provided by more than 3,000 taxonomists' expert opinions in a unified and coherent, hierarchically ranked system known as the Catalogue of Life (CoL). The intent of this collaborative effort is to provide a hierarchical classification serving not only the needs of the CoL's database providers but also the diverse public-domain user community, most of whom are familiar with the Linnaean conceptual system of ordering taxon relationships. This classification is neither phylogenetic nor evolutionary but instead represents a consensus view that accommodates taxonomic choices and practical compromises among diverse expert opinions, public usages, and conflicting evidence about the boundaries between taxa and the ranks of major taxa, including kingdoms. Certain key issues, some not fully resolved, are addressed in particular. Beyond its immediate use as a management tool for the CoL and ITIS (Integrated Taxonomic Information System), it is immediately valuable as a reference for taxonomic and biodiversity research, as a tool for societal communication, and as a classificatory "backbone" for biodiversity databases, museum collections, libraries, and textbooks. Such a modern comprehensive hierarchy has not previously existed at this level of specificity. C1 [Ruggiero, Michael A.; Orrell, Thomas M.] Smithsonian Inst, Natl Museum Nat Hist, Integrated Taxon Informat Syst, Washington, DC 20560 USA. [Gordon, Dennis P.] Natl Inst Water & Atmospher Res, Wellington, New Zealand. [Bailly, Nicolas] WorldFish FIN, Los Banos, Philippines. [Bourgoin, Thierry] Univ Paris 04, Inst Systemat, UMR 7205 MNHN CNRS UPMC EPHE, Evolut,Biodiversite ISYEB,Museum Natl Hist Nat, F-75005 Paris, France. [Brusca, Richard C.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Cavalier-Smith, Thomas] Univ Oxford, Dept Zool, Oxford, England. [Guiry, Michael D.] Natl Univ Ireland, Ryan Inst, AlgaeBase Fdn & Irish Seaweed Res Grp, Galway, Ireland. [Kirk, Paul M.] Royal Bot Gardens, Mycol Sect, London, England. RP Ruggiero, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Integrated Taxon Informat Syst, Washington, DC 20560 USA. EM ruggierm@si.edu NR 99 TC 23 Z9 24 U1 23 U2 81 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 APR 29 PY 2015 VL 10 IS 4 AR e0119248 DI 10.1371/journal.pone.0119248 PG 60 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH0LO UT WOS:000353711600003 PM 25923521 ER PT J AU Velez-Juarbe, J Wood, AR De Gracia, C Hendy, AJW AF Velez-Juarbe, Jorge Wood, Aaron R. De Gracia, Carlos Hendy, Austin J. W. TI Evolutionary Patterns among Living and Fossil Kogiid Sperm Whales: Evidence from the Neogene of Central America SO PLOS ONE LA English DT Article ID LATE MIOCENE; SEXUAL SELECTION; MARINE MAMMALS; CETACEA; ODONTOCETI; BREVICEPS; PLIOCENE; PANAMA; PERU; PHYSETEROIDEA AB Kogiids are known by two living species, the pygmy and dwarf sperm whale (Kogia breviceps and K. sima). Both are relatively rare, and as their names suggest, they are closely related to the sperm whale, all being characterized by the presence of a spermaceti organ. However, this organ is much reduced in kogiids and may have become functionally different. Here we describe a fossil kogiid from the late Miocene of Panama and we explore the evolutionary history of the group with special attention to this evolutionary reduction. The fossil consists of cranial material from the late Tortonian (similar to 7.5 Ma) Pina facies of the Chagres Formation in Panama. Detailed comparison with other fossil and extant kogiids and the results of a phylogenetic analysis place the Panamanian kogiid, herein named Nanokogia isthmia gen. et sp. nov., as a taxon most closely related to Praekogia cedrosensis from the Messinian (similar to 6 Ma) of Baja California and to Kogia spp. Furthermore our results show that reduction of the spermaceti organ has occurred iteratively in kogiids, once in Thalassocetus antwerpiensis in the early-middle Miocene, and more recently in Kogia spp. Additionally, we estimate the divergence between extant species of Kogia at around the late Pliocene, later than previously predicted by molecular estimates. Finally, comparison of Nanokogia with the coeval Scaphokogia cochlearis from Peru shows that these two species display a greater morphological disparity between them than that observed between the extant members of the group. We hypothesize that this reflects differences in feeding ecologies of the two species, with Nanokogia being more similar to extant Kogia. Nanokogia shows that kogiids have been part of the Neotropical marine mammal communities at least since the late Miocene, and gives us insight into the evolutionary history and origins of one of the rarest groups of living whales. C1 [Velez-Juarbe, Jorge] Nat Hist Museum Los Angeles Cty, Dept Mammal, Los Angeles, CA 90007 USA. [Velez-Juarbe, Jorge] Calif State Univ Fullerton, Dept Geol Sci, John D Cooper Archaeol & Paleontol Ctr, Fullerton, CA 92634 USA. [Wood, Aaron R.] Iowa State Univ, Dept Geol & Atmospher Sci, Ames, IA USA. [De Gracia, Carlos] Smithsonian Trop Res Inst, Balboa, Panama. [Hendy, Austin J. W.] Nat Hist Museum Los Angeles Cty, Dept Invertebrate Paleontol, Los Angeles, CA USA. RP Velez-Juarbe, J (reprint author), Nat Hist Museum Los Angeles Cty, Dept Mammal, Los Angeles, CA 90007 USA. EM jvelezjuar@nhm.org OI De Gracia, Carlos/0000-0003-0637-3302 FU National Science Foundation Partnerships for International Research and Education [0966884]; National Science Foundation Earth Sciences Postdoctoral Fellowship [1249920]; Secretaria Nacional de Ciencia, Tecnologia en Innovacion [APY-NI10-016A] FX Funding for this project was provided by National Science Foundation Partnerships for International Research and Education grant #0966884 to JVJ, ARW, CDG, and AJWH; National Science Foundation Earth Sciences Postdoctoral Fellowship grant #1249920 to JVJ; and Secretaria Nacional de Ciencia, Tecnologia en Innovacion grant #APY-NI10-016A to CDG. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 62 TC 4 Z9 5 U1 1 U2 16 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 29 PY 2015 VL 10 IS 4 AR e0123909 DI 10.1371/journal.pone.0123909 PG 29 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH0LO UT WOS:000353711600060 PM 25923213 ER PT J AU Jay, JA Delgado, FJ Torres, JL Pritchard, ME Macedo, O Aguilar, V AF Jay, Jennifer A. Delgado, Francisco J. Luis Torres, Jose Pritchard, Matthew E. Macedo, Orlando Aguilar, Victor TI Deformation and seismicity near Sabancaya volcano, southern Peru, from 2002 to 2015 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Sabancaya volcano; volcano seismicity; volcano deformation; InSAR ID EARTHQUAKE SWARMS; CENTRAL ANDES; SPACE; STRESS; IMAGES; STATE AB We use interferometric synthetic aperture radar (InSAR) and local seismic data to investigate the cause of earthquake sequences near Sabancaya volcano in southern Peru from 2002 to 2014, with a particular focus on events leading up to the August 2014 phreatic eruption. InSAR-observed deformation associated with earthquake swarms in late 2002, February 2013, and July 2013 is modeled by fault slip, with no need for magmatic sources to explain the deformation. The majority of the seismicity is an expression of the regional tectonic system, which is characterized by E-W trending normal faults, but a link to the magmatic system is possible. The M-w 5.9 earthquake on 17 July 2013 occurred on a previously unmapped normal fault that continued to deform in the months following the earthquake. An increase in long period and hybrid seismicity and changes in fumarolic emissions in 2013-2014 culminating in the August 2014 eruption indicates the involvement of both tectonic and magmatic systems. C1 [Jay, Jennifer A.; Delgado, Francisco J.; Pritchard, Matthew E.] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY 14850 USA. [Jay, Jennifer A.] Smithsonian Inst, Washington, DC 20560 USA. [Luis Torres, Jose; Macedo, Orlando] Inst Geofis Peru, Observ Vulcanol Sur, Arequipa, Peru. [Aguilar, Victor] Univ Nacl San Agustin, Inst Geofis, Arequipa, Peru. RP Jay, JA (reprint author), Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY 14850 USA. EM jayj@si.edu RI Pritchard, Matthew/L-5892-2015; OI Pritchard, Matthew/0000-0003-3616-3373; Macedo, Orlando/0000-0002-9944-7990 FU NASA [NNX12AM24G]; Instituto Geofisico del Peru (IGP) Area de Vulcanologia [PP 068] FX Partial support from NASA Earth Science program grant NNX12AM24G. The French Institut de recherche pour le developpement (IRD) supplied five Guralp seismic stations which helped with the success of the seismic monitoring. The seismic study was financed by the PP 068, Meta 7 "Vigilancia Geofisica de Volcanes" of the Instituto Geofisico del Peru (IGP) Area de Vulcanologia. We thank H. Tavera for the review of focal mechanism calculations and R. Machacca, R. Chijcheapaza, and A. Ramos for their help in the field. We also thank Scott Henderson for assistance with InSAR data processing. TerraSAR-X data are available through agreement with the German Aerospace Center (DLR) and the Committee on Earth Observation Satellites Disaster Risk Management Volcano Pilot Observation Project, and ERS/Envisat data are available through the European Space Agency (ESA) Category 1 proposal 3194. ASTER data are provided by NASA Land Processes Distributed Active Archive Center (LP DAAC). Finally, we thank Paul Lundgren, Mike Poland, and an anonymous reviewer for their extremely helpful comments. NR 33 TC 2 Z9 2 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 28 PY 2015 VL 42 IS 8 BP 2780 EP 2788 DI 10.1002/2015GL063589 PG 9 WC Geosciences, Multidisciplinary SC Geology GA CI2FN UT WOS:000354560800028 ER PT J AU Lohbeck, M Lebrija-Trejos, E Martinez-Ramos, M Meave, JA Poorter, L Bongers, F AF Lohbeck, Madelon Lebrija-Trejos, Edwin Martinez-Ramos, Miguel Meave, Jorge A. Poorter, Lourens Bongers, Frans TI Functional Trait Strategies of Trees in Dry and Wet Tropical Forests Are Similar but Differ in Their Consequences for Succession SO PLOS ONE LA English DT Article ID PLANT ECONOMICS SPECTRUM; LEAF LIFE-SPANS; SEED SIZE; SECONDARY SUCCESSION; NEOTROPICAL FORESTS; SHADE-TOLERANCE; WOODY-PLANTS; TRADE-OFF; DROUGHT; DISPERSAL AB Global plant trait studies have revealed fundamental trade-offs in plant resource economics. We evaluated such trait trade-offs during secondary succession in two species-rich tropical ecosystems that contrast in precipitation: dry deciduous and wet evergreen forests of Mexico. Species turnover with succession in dry forest largely relates to increasing water availability and in wet forest to decreasing light availability. We hypothesized that while functional trait trade-offs are similar in the two forest systems, the successful plant strategies in these communities will be different, as contrasting filters affect species turnover. Research was carried out in 15 dry secondary forest sites (5-63 years after abandonment) and in 17 wet secondary forest sites (<1-25 years after abandonment). We used 11 functional traits measured on 132 species to make species-trait PCA biplots for dry and wet forest and compare trait trade-offs. We evaluated whether multivariate plant strategies changed during succession, by calculating a 'Community-Weighted Mean' plant strategy, based on species scores on the first two PCA-axes. Trait spectra reflected two main trade-off axes that were similar for dry and wet forest species: acquisitive versus conservative species, and drought avoiding species versus evergreen species with large animal-dispersed seeds. These trait associations were consistent when accounting for evolutionary history. Successional changes in the most successful plant strategies reflected different functional trait spectra depending on the forest type. In dry forest the community changed from having drought avoiding strategies early in succession to increased abundance of evergreen strategies with larger seeds late in succession. In wet forest the community changed from species having mainly acquisitive strategies to those with more conservative strategies during succession. These strategy changes were explained by increasing water availability during dry forest succession and increasing light scarcity during wet forest succession. Although similar trait spectra were observed among dry and wet secondary forest species, the consequences for succession were different resulting from contrasting environmental filters. C1 [Lohbeck, Madelon; Lebrija-Trejos, Edwin; Poorter, Lourens; Bongers, Frans] Wageningen Univ, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Lebrija-Trejos, Edwin] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Lohbeck, Madelon; Martinez-Ramos, Miguel] Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Morelia 58190, Michoacan, Mexico. [Lebrija-Trejos, Edwin; Meave, Jorge A.] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Ecol & Recursos Nat, Mexico City 04510, DF, Mexico. RP Lohbeck, M (reprint author), Wageningen Univ, Forest Ecol & Forest Management Grp, POB 47, NL-6700 AA Wageningen, Netherlands. EM madelon.lohbeck@wur.nl OI Meave, Jorge A./0000-0002-6241-8803 FU Wageningen University; Wageningen Research Center; NSF-LTREB [DEB-0639393, DEB 1147429]; SEMARNAT-CONACYT [2002-C01-0597]; SEP-CONACYT [CB-2005-01-51043, 2009-129740]; CONACYT; CONACYT-SEMARNAT [2002-C01-0267]; PAPIIT [IN216007]; SNI, Panama; SENACYT, Panama; Nucleo DiverSus project by Inter-American Institute for Global Change Research (IAI)CRN; SGP-CRA (National Science Foundation) [GEO-0452325, GEO-1138881]; [SEP CONACYT-2009-01-128136] FX Funding: ML and FB were supported by a research grant from Wageningen University and Research Center. FB and MMR were supported by NSF-LTREB DEB-0639393 and #DEB 1147429. MMR was supported by grants SEMARNAT-CONACYT 2002-C01-0597, SEP-CONACYT CB-2005-01-51043, SEP-CONACYT 2009-129740. ELT acknowledges support by CONACYT (personal scholarship), CONACYT-SEMARNAT (grant 2002-C01-0267), PAPIIT (grant IN216007) and SNI, SENACYT, Panama. JAM was supported by SEP CONACYT-2009-01-128136. LP was partly supported by the Nucleo DiverSus project, which was supported by the Inter-American Institute for Global Change Research (IAI)CRN 2015 and SGP-CRA2015 (through National Science Foundation grants GEO-0452325 and GEO-1138881). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 72 TC 5 Z9 5 U1 5 U2 55 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 APR 28 PY 2015 VL 10 IS 4 AR e0123741 DI 10.1371/journal.pone.0123741 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG9SE UT WOS:000353659400033 ER PT J AU Ballance, CP McLaughlin, BM AF Ballance, C. P. McLaughlin, B. M. TI Photoionization of the valence shells of the neutral tungsten atom SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE Dirac R-matrix; photoionization; tungsten ID R-MATRIX METHOD; ELECTRON-SCATTERING; PHOTOABSORPTION AB Results from large-scale theoretical cross section calculations for the total photoionization (PI) of the 4f, 5s, 5p and 6s orbitals of the neutral tungsten atom using the Dirac Coulomb R-matrix approximation (DARC: Dirac-atomic R-matrix codes) are presented. Comparisons are made with previous theoretical methods and prior experimental measurements. In previous experiments a time-resolved dual laser approach was employed for the photo-absorption of metal vapours and photo-absorption measurements on tungsten in a solid, using synchrotron radiation. The lowest ground state level of neutral tungsten is 5p(6) 5d(4)6s(2) D-J , with J = 0, and requires only a single dipole matrix for PI. To make a meaningful comparison with existing experimental measurements, we statistically average the large-scale theoretical PI cross sections from the levels associated with the ground state 5p(6)5d(4)6s(2)D(J) (J = 0, 1, 2, 3, 4) levels and the 5d(5)6s(7)S(3) excited metastable level. As the experiments have a self-evident metastable component in their ground state measurement, averaging over the initial levels allows for a more consistent and realistic comparison to be made. In the wider context, the absence of many detailed electron-impact excitation (EIE) experiments for tungsten and its multi-charged ion stages allows current PI measurements and theory to provide a road-map for future EIE, ionization and di-electronic cross section calculations by identifying the dominant resonance structure and features across an energy range of hundreds of eV. C1 [Ballance, C. P.] Auburn Univ, Dept Phys, Allison Lab 206, Auburn, AL 36849 USA. [McLaughlin, B. M.] Queens Univ Belfast, Ctr Theoret Atom Mol & Opt Phys, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Ballance, CP (reprint author), Auburn Univ, Dept Phys, Allison Lab 206, Auburn, AL 36849 USA. EM ballance@physics.auburn.edu; b.mclaughlin@qub.ac.uk FU NSF; NASA grants through Auburn University; US National Science Foundation; Office of Science of the US Department of Energy [DE-AC05-00OR22725] FX C P Ballance was supported by NSF and NASA grants through Auburn University. B M McLaughlin acknowledges support by the US National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, Queen's University Belfast for the award of a visiting research fellowship (VRF) and the hospitality of the University of Auburn during a research recent visit. The computational work was carried out at the National Energy Research Scientific Computing Center in Oakland, CA, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany. This research also used resources of the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC05-00OR22725. Helpful discussions with Professor E T Kennedy are gratefully acknowledged. NR 26 TC 4 Z9 4 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD APR 28 PY 2015 VL 48 IS 8 AR 085201 DI 10.1088/0953-4075/48/8/085201 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CE3WY UT WOS:000351762000004 ER PT J AU Jarvi, SI Pitt, WC Farias, ME Shiels, L Severino, MG Howe, KM Jacquier, SH Shiels, AB Amano, KK Luiz, BC Maher, DE Allison, ML Holtquist, ZC Scheibelhut, NT AF Jarvi, Susan I. Pitt, William C. Farias, Margaret E. Shiels, Laura Severino, Michael G. Howe, Kathleen M. Jacquier, Steven H. Shiels, Aaron B. Amano, Karis K. Luiz, Blaine C. Maher, Daisy E. Allison, Maureen L. Holtquist, Zachariah C. Scheibelhut, Neil T. TI Detection of Angiostrongylus cantonensis in the Blood and Peripheral Tissues of Wild Hawaiian Rats (Rattus rattus) by a Quantitative PCR (qPCR) Assay SO PLOS ONE LA English DT Article ID EOSINOPHILIC MENINGITIS; INFECTION; DIAGNOSIS; LUNGWORM AB The nematode Angiostrongylus cantonensis is a rat lungworm, a zoonotic pathogen that causes human eosinophilic meningitis and ocular angiostrongyliasis characteristic of rat lungworm (RLW) disease. Definitive diagnosis is made by finding and identifying A. cantonensis larvae in the cerebral spinal fluid or by using a custom immunological or molecular test. This study was conducted to determine if genomic DNA from A. cantonensis is detectable by qPCR in the blood or tissues of experimentally infected rats. F1 offspring from wild rats were subjected to experimental infection with RLW larvae isolated from slugs, then blood or tissue samples were collected over multiple time points. Blood samples were collected from 21 rats throughout the course of two trials (15 rats in Trial I, and 6 rats in Trial II). In addition to a control group, each trial had two treatment groups: the rats in the low dose (LD) group were infected by approximately 10 larvae and the rats in the high dose (HD) group were infected with approximately 50 larvae. In Trial I, parasite DNA was detected in cardiac bleed samples from five of five LD rats and five of five HD rats at six weeks post-infection (PI), and three of five LD rats and five of five HD rats from tail tissue. In Trial II, parasite DNA was detected in peripheral blood samples from one of two HD rats at 53 minutes PI, one of two LD rats at 1.5 hours PI, one of two HD rats at 18 hours PI, one of two LD rats at five weeks PI and two of two at six weeks PI, and two of two HD rats at weeks five and six PI. These data demonstrate that parasite DNA can be detected in peripheral blood at various time points throughout RLW infection in rats. C1 [Jarvi, Susan I.; Farias, Margaret E.; Shiels, Laura; Severino, Michael G.; Howe, Kathleen M.; Jacquier, Steven H.; Amano, Karis K.; Luiz, Blaine C.; Maher, Daisy E.; Allison, Maureen L.; Holtquist, Zachariah C.; Scheibelhut, Neil T.] Univ Hawaii, Coll Pharm, Dept Pharmaceut Sci, Hilo, HI 96720 USA. [Pitt, William C.; Shiels, Laura; Shiels, Aaron B.] Natl Wildlife Res Ctr, Hawaii Field Stn, USDA APHIS Wildlife Serv, Hilo, HI 96720 USA. [Pitt, William C.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Jarvi, SI (reprint author), Univ Hawaii, Coll Pharm, Dept Pharmaceut Sci, Hilo, HI 96720 USA. EM jarvi@hawaii.edu FU UHH Daniel K. Inouye College of Pharmacy; University of Hawaii at Hilo; United States Department of Agriculture-APHIS National Wildlife Research Center's National Wildlife Disease Program; University of Hawaii at Hilo Research Council; National Institute of General Medical Sciences, National Institutes of Health [P20GM 103466] FX This project was supported by the UHH Daniel K. Inouye College of Pharmacy, University of Hawaii at Hilo, United States Department of Agriculture-APHIS National Wildlife Research Center's National Wildlife Disease Program, University of Hawaii at Hilo Research Council, and a grant from the National Institute of General Medical Sciences, National Institutes of Health, award number: P20GM 103466. The content is solely the responsibility of the authors and do not necessarily represent the official views of the National Institutes of Health. The funders had no role in the study design, data collection and analysis, decision to publish or preparation of the manuscript. NR 30 TC 1 Z9 1 U1 4 U2 8 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 24 PY 2015 VL 10 IS 4 AR e0123064 DI 10.1371/journal.pone.0123064 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG6AH UT WOS:000353376800028 PM 25910229 ER PT J AU Schellart, P Trinh, TNG Buitink, S Corstanje, A Enriquez, JE Falcke, H Horandel, JR Nelles, A Rachen, JP Rossetto, L Scholten, O ter Veen, S Thoudam, S Ebert, U Koehn, C Rutjes, C Alexov, A Anderson, JM Avruch, IM Bentum, MJ Bernardi, G Best, P Bonafede, A Breitling, F Broderick, JW Bruggen, M Butcher, HR Ciardi, B de Geus, E de Vos, M Duscha, S Eisloffel, J Fallows, RA Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Heald, G Hessels, JWT Hoeft, M Holties, HA Juette, E Kondratiev, VI Kuniyoshi, M Kuper, G Mann, G McFadden, R McKay-Bukowski, D McKean, JP Mevius, M Moldon, J Norden, MJ Orru, E Paas, H Pandey-Pommier, M Pizzo, R Polatidis, AG Reich, W Rottgering, H Scaife, AMM Schwarz, DJ Serylak, M Smirnov, O Steinmetz, M Swinbank, J Tagger, M Tasse, C Toribio, MC van Weeren, RJ Vermeulen, R Vocks, C Wise, MW Wucknitz, O Zarka, P AF Schellart, P. Trinh, T. N. G. Buitink, S. Corstanje, A. Enriquez, J. E. Falcke, H. Horandel, J. R. Nelles, A. Rachen, J. P. Rossetto, L. Scholten, O. ter Veen, S. Thoudam, S. Ebert, U. Koehn, C. Rutjes, C. Alexov, A. Anderson, J. M. Avruch, I. M. Bentum, M. J. Bernardi, G. Best, P. Bonafede, A. Breitling, F. Broderick, J. W. Brueggen, M. Butcher, H. R. Ciardi, B. de Geus, E. de Vos, M. Duscha, S. Eisloeffel, J. Fallows, R. A. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Heald, G. Hessels, J. W. T. Hoeft, M. Holties, H. A. Juette, E. Kondratiev, V. I. Kuniyoshi, M. Kuper, G. Mann, G. McFadden, R. McKay-Bukowski, D. McKean, J. P. Mevius, M. Moldon, J. Norden, M. J. Orru, E. Paas, H. Pandey-Pommier, M. Pizzo, R. Polatidis, A. G. Reich, W. Rottgering, H. Scaife, A. M. M. Schwarz, D. J. Serylak, M. Smirnov, O. Steinmetz, M. Swinbank, J. Tagger, M. Tasse, C. Toribio, M. C. van Weeren, R. J. Vermeulen, R. Vocks, C. Wise, M. W. Wucknitz, O. Zarka, P. TI Probing Atmospheric Electric Fields in Thunderstorms through Radio Emission from Cosmic-Ray-Induced Air Showers SO PHYSICAL REVIEW LETTERS LA English DT Article ID LOFAR; SIMULATIONS; COREAS; ARRAY AB We present measurements of radio emission from cosmic ray air showers that took place during thunderstorms. The intensity and polarization patterns of these air showers are radically different from those measured during fair-weather conditions. With the use of a simple two-layer model for the atmospheric electric field, these patterns can be well reproduced by state-of-the-art simulation codes. This in turn provides a novel way to study atmospheric electric fields. C1 [Schellart, P.; Buitink, S.; Corstanje, A.; Enriquez, J. E.; Falcke, H.; Horandel, J. R.; Nelles, A.; Rachen, J. P.; Rossetto, L.; ter Veen, S.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Trinh, T. N. G.; Scholten, O.] Univ Groningen, KVI Ctr Adv Radiat Technol, NL-9700 AB Groningen, Netherlands. [Buitink, S.] Vrije Univ Brussel, Inst Astrophys, B-1050 Brussels, Belgium. [Falcke, H.; Horandel, J. R.] Nikhef, Sci Pk Amsterdam, NL-1098 XG Amsterdam, Netherlands. [Falcke, H.; ter Veen, S.; Bentum, M. J.; de Geus, E.; de Vos, M.; Duscha, S.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Heald, G.; Hessels, J. W. T.; Holties, H. A.; Kondratiev, V. I.; Kuper, G.; McFadden, R.; McKean, J. P.; Mevius, M.; Moldon, J.; Norden, M. J.; Orru, E.; Pizzo, R.; Polatidis, A. G.; Toribio, M. C.; Vermeulen, R.; Wise, M. W.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Falcke, H.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Scholten, O.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium. [Ebert, U.; Koehn, C.; Rutjes, C.] Ctr Math & Comp Sci, CWI, NL-1090 GB Amsterdam, Netherlands. [Ebert, U.] Eindhoven Univ Technol, TU e, NL-5600 MB Eindhoven, Netherlands. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Anderson, J. M.] Deutsch GeoForsch Zentrum GFZ, Helmholtz Zentrum Potsdam, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Avruch, I. M.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, I. M.; Heald, G.; McKean, J. P.; Mevius, M.] Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [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. [Brueggen, M.] Univ Hamburg, D-21029 Hamburg, Germany. [Bonafede, A.; Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Broderick, J. W.; Serylak, M.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Broderick, J. W.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [de Geus, E.] SmarterVis BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Garrett, M. A.; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Griessmeier, J.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France. [Griessmeier, J.] Univ Orleans, CNRS INSU, Stn Radioastron Nancay, Observ Paris,OSUC,USR 704, F-18330 Nancay, France. [Hessels, J. W. T.; Swinbank, J.; Wise, M. W.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [Juette, E.] Ruhr Univ Bochum, Inst Astron, D-44780 Bochum, Germany. [Kondratiev, V. I.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Kuniyoshi, M.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bukowski, D.] Rutherford Appleton Lab, STFC, Didcot OX11 0QX, Oxon, England. [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. J.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Smirnov, O.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Tasse, C.; Zarka, P.] Observ Paris, LESIA, UMR CNRS 8109, F-92195 Meudon, France. RP Schellart, P (reprint author), Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM P.Schellart@astro.ru.nl RI Ebert, Ute/C-4977-2008; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; OI Ebert, Ute/0000-0003-3891-6869; Kondratiev, Vladislav/0000-0001-8864-7471; Swinbank, John/0000-0001-9445-1846; van Weeren, Reinout/0000-0002-0587-1660 FU NOVA; SNN; FOM; NWO, VENI Grant [639-041-130]; European Research Council [227610]; FOM-project [12PR3041] FX The LOFAR key science project cosmic rays acknowledges financial support from NOVA, SNN, and FOM as well as from NWO, VENI Grant No. 639-041-130. We acknowledge funding from an Advanced Grant of the European Research Council (FP/2007-2013)/ERC Grant Agreement No. 227610. We also acknowledge funding from the FOM-project 12PR3041 "Cosmic Lightning". 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 foundation under a joint scientific policy. NR 22 TC 13 Z9 13 U1 0 U2 11 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 APR 24 PY 2015 VL 114 IS 16 AR 165001 DI 10.1103/PhysRevLett.114.165001 PG 5 WC Physics, Multidisciplinary SC Physics GA CG6ZY UT WOS:000353452900004 PM 25955053 ER PT J AU Chilingarian, I Zolotukhin, I AF Chilingarian, Igor Zolotukhin, Ivan TI Isolated compact elliptical galaxies: Stellar systems that ran away SO SCIENCE LA English DT Article ID DWARF GALAXIES; CLUSTERS; MASS; MERGER; STAR; DISCOVERY; REGIONS; SPACE; FIELD AB Compact elliptical galaxies form a rare class of stellar system (similar to 30 presently known) characterized by high stellar densities and small sizes and often harboring metal-rich stars. They were thought to form through tidal stripping of massive progenitors, until two isolated objects were discovered where massive galaxies performing the stripping could not be identified. By mining astronomical survey data, we have now found 195 compact elliptical galaxies in all types of environment. They all share similar dynamical and stellar population properties. Dynamical analysis for nonisolated galaxies demonstrates the feasibility of their ejection from host clusters and groups by three-body encounters, which is in agreement with numerical simulations. Hence, isolated compact elliptical and isolated quiescent dwarf galaxies are tidally stripped systems that ran away from their hosts. C1 [Chilingarian, Igor] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chilingarian, Igor; Zolotukhin, Ivan] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Zolotukhin, Ivan] Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. RP Chilingarian, I (reprint author), Smithsonian Astrophys Observ, 60 Garden St MS09, Cambridge, MA 02138 USA. EM igor.chilingarian@cfa.harvard.edu RI Chilingarian, Igor/N-5117-2016; OI Chilingarian, Igor/0000-0002-7924-3253; Zolotukhin, Ivan/0000-0002-5544-9476 FU Russian Science Foundation [14-22-00041]; M. V. Lomonosov Moscow State University Program of Development; NASA; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX The authors are greatful to F. Combes (Observatoire de Paris), I. Katkov (Sternberg Astronomical Institute), and M. Kurtz (Smithsonian Astrophysical Observatory) for useful discussions and critical reading of the manuscript. This result emerged from the tutorial run by the authors at the Astronomical Data Analysis Software and Systems conference in 2012. The authors acknowledge support by the Russian Science Foundation project 14-22-00041 "VOLGA-A View On the Life of GAlaxies.". The project used computational resourses funded by the M. V. Lomonosov Moscow State University Program of Development. This research has made use of Aladin developed by the Centre de Donnees Astronomiques de Strasbourg; TOPCAT and STILTS software packages developed by M. Taylor; "exploresdss" script by G. Mamon; the VizieR catalog access tool, CDS, Strasbourg, France; and the NASA/IPAC NED, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under 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, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is www.sdss.org. GALEX and SDSS databases used in our study are available via the CasJobs web-site http://skyserver.sdss.org/CasJobs. NR 32 TC 8 Z9 8 U1 0 U2 3 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 APR 24 PY 2015 VL 348 IS 6233 BP 418 EP 421 DI 10.1126/science.aaa3344 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG5NF UT WOS:000353338000029 PM 25908816 ER PT J AU Li, HB Yuen, KH Otto, F Leung, PK Sridharan, TK Zhang, QZ Liu, HY Tang, YW Qiu, KP AF Li, Hua-bai Yuen, Ka Ho Otto, Frank Leung, Po Kin Sridharan, T. K. Zhang, Qizhou Liu, Hauyu Tang, Ya-Wen Qiu, Keping TI Self-similar fragmentation regulated by magnetic fields in a region forming massive stars SO NATURE LA English DT Article ID NGC 6334 I; MOLECULAR CLOUDS; SUBMILLIMETER POLARIZATION; ZEEMAN OBSERVATIONS; FILAMENTARY CLOUDS; GOULD BELT; I(N); COLLAPSE; CORES; DUST AB Most molecular clouds are filamentary or elongated(1-3). For those forming low-mass stars (<8 solar masses), the competition between self-gravity and turbulent pressure along the dynamically dominant intercloud magnetic field (10 to 100 parsecs) shapes the clouds to be elongated either perpendicularly(4) or parallel(5) to the fields. A recent study(6) also suggested that on the scales of 0.1 to 0.01 parsecs, such fields are dynamically important within cloud cores forming massive stars (>8 solar masses). But whether the core fieldmorphologies are inherited from the intercloud medium or governed by cloud turbulence is unknown, as is the effect of magnetic fields on cloud fragmentation at scales of 10 to 0.1 parsecs(7-9). Here we report magnetic-field maps inferred from polarimetric observations of NGC6334, a region forming massive stars, on the 100 to 0.01 parsec scale. NGC6334 hosts young star-forming sites(10-12) where fields are not severely affected by stellar feedback, and their directions do not change much over the entire scale range. This means that the fields are dynamically important. The ordered fields lead to a self-similar gas fragmentation: at all scales, there exist elongated gas structures nearly perpendicular to the fields. Many gas elongations have density peaks near the ends, which symmetrically pinch the fields. The field strength is proportional to the 0.4th power of the density, which is an indication of anisotropic gas contractions along the field. We conclude that magnetic fields have a crucial role in the fragmentation of NGC6334. C1 [Li, Hua-bai; Yuen, Ka Ho; Otto, Frank; Leung, Po Kin] Chinese Univ Hong Kong, Dept Phys, Shatin, Hong Kong, Peoples R China. [Sridharan, T. K.; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Hauyu; Tang, Ya-Wen] Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Qiu, Keping] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. RP Li, HB (reprint author), Chinese Univ Hong Kong, Dept Phys, Shatin, Hong Kong, Peoples R China. EM hbli@phy.cuhk.edu.hk OI Zhang, Qizhou/0000-0003-2384-6589 FU Hong Kong Research Grants Council [ECS 24300314]; CUHK; Deutsche Forschungsgemeinschaft priority programme 1573 [46]; Smithsonian Institution; Academia Sinica FX We thank R. Blundell for the SMA Director's Discretionary Time that allowed the project to take off. We also thank the SPARO team led by G. Novak and the Hertz team led by R. Hildebrand. Discussions with Z.-Y. Li and the proofread by D. Wilmshurst and T.T. Wu improved the manuscript. The experiment was supported by the Hong Kong Research Grants Council, project ECS 24300314; by CUHK Direct Grant for Research 2013-2014, project 'Modelling Star Formation with GPU Computing'; and by the Deutsche Forschungsgemeinschaft priority programme 1573, project number 46. 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. NR 48 TC 14 Z9 14 U1 1 U2 16 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 APR 23 PY 2015 VL 520 IS 7548 BP 518 EP + DI 10.1038/nature14291 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG5LX UT WOS:000353334500037 PM 25822792 ER PT J AU Parker, IM Saunders, M Bontrager, M Weitz, AP Hendricks, R Magarey, R Suiter, K Gilbert, GS AF Parker, Ingrid M. Saunders, Megan Bontrager, Megan Weitz, Andrew P. Hendricks, Rebecca Magarey, Roger Suiter, Karl Gilbert, Gregory S. TI Phylogenetic structure and host abundance drive disease pressure in communities SO NATURE LA English DT Article ID INFECTIOUS-DISEASES; TROPICAL FOREST; PLANT-DISEASE; BIODIVERSITY; PATHOGENS; ECOLOGY; HERBIVORES; EMERGENCE; ESCAPE; SIGNAL AB Pathogens play an important part in shaping the structure and dynamics of natural communities, because species are not affected by them equally(1,2). A shared goal of ecology and epidemiology is to predict when a species is most vulnerable to disease. A leading hypothesis asserts that the impact of disease should increase with host abundance, producing a 'rare-species advantage'(3-5). However, the impact of a pathogen may be decoupled from host abundance, because most pathogens infect more than one species, leading to pathogen spillover onto closely related species(6,7). Here we show that the phylogenetic and ecological structure of the surrounding community can be important predictors of disease pressure. We found that the amount of tissue lost to disease increased with the relative abundance of a species across a grassland plant community, and that this rare-species advantage had an additional phylogenetic component: disease pressure was stronger on species with many close relatives. We used a global model of pathogen sharing as a function of relatedness between hosts, which provided a robust predictor of relative disease pressure at the local scale. In our grassland, the total amount of disease was most accurately explained not by the abundance of the focal host alone, but by the abundance of all species in the community weighted by their phylogenetic distance to the host. Furthermore, the model strongly predicted observed disease pressure for 44 novel host species we introduced experimentally to our study site, providing evidence for a mechanism to explain why phylogenetically rare species are more likely to become invasive when introduced(8,9). Our results demonstrate how the phylogenetic and ecological structure of communities can have a key role in disease dynamics, with implications for the maintenance of biodiversity, biotic resistance against introduced weeds, and the success of managed plants in agriculture and forestry. C1 [Parker, Ingrid M.; Bontrager, Megan; Weitz, Andrew P.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Parker, Ingrid M.; Gilbert, Gregory S.] Smithsonian Trop Res Inst, Balboa, Panama. [Saunders, Megan; Hendricks, Rebecca; Gilbert, Gregory S.] Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. [Magarey, Roger; Suiter, Karl] N Carolina State Univ, Ctr Integrated Pest Management, Raleigh, NC 27606 USA. RP Parker, IM (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. EM imparker@ucsc.edu FU National Science Foundation [DEB-0842059, DEB-1136626]; G.S.G. [14-8130-1472-CA]; US Department of Agriculture APHIS-PPQ-CPHST PERAL [14-8130-1472-CA] FX We thank C. Webb for development of the methods of phylogenetic ecology. We thank J. Velzy for greenhouse support and the many undergraduates and volunteers who helped with fieldwork and disease assessments from scanned leaves. Editorial comments were provided by M. Kilpatrick, B. Lyon, C. Fresquez, D. Gordon, S. Grove, S. Gulamhussein, J. Harrower, C. Ray, K. Ross and M. Shu; K. Tanner revised Fig. 1. This research was funded by National Science Foundation grants DEB-0842059 and DEB-1136626, and by a Cooperative Agreement 14-8130-1472-CA between G.S.G. and US Department of Agriculture APHIS-PPQ-CPHST PERAL funded from Section 10201 of the Farm Bill. NR 37 TC 32 Z9 32 U1 23 U2 119 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 APR 23 PY 2015 VL 520 IS 7548 BP 542 EP + DI 10.1038/nature14372 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG5LX UT WOS:000353334500043 PM 25903634 ER PT J AU Agarwal, K Gopalakrishnan, S Knap, M Muller, M Demler, E AF Agarwal, Kartiek Gopalakrishnan, Sarang Knap, Michael Mueller, Markus Demler, Eugene TI Anomalous Diffusion and Griffiths Effects Near the Many-Body Localization Transition SO PHYSICAL REVIEW LETTERS LA English DT Article ID METAL-INSULATOR-TRANSITION; ANDERSON LOCALIZATION; DISORDERED-SYSTEMS; OPTICAL LATTICE; CONDUCTION; IMPURITY; STATES; CHAIN; PHASE AB We explore the high-temperature dynamics of the disordered, one-dimensional XXZ model near the many-body localization (MBL) transition, focusing on the delocalized (i.e., "metallic") phase. In the vicinity of the transition, we find that this phase has the following properties: (i) local magnetization fluctuations relax subdiffusively; (ii) the ac conductivity vanishes near zero frequency as a power law; and (iii) the distribution of resistivities becomes increasingly broad at low frequencies, approaching a power law in the zero-frequency limit. We argue that these effects can be understood in a unified way if the metallic phase near the MBL transition is a quantum Griffiths phase. We establish scaling relations between the associated exponents, assuming a scaling form of the spin-diffusion propagator. A phenomenological classical resistor-capacitor model captures all the essential features. C1 [Agarwal, Kartiek; Gopalakrishnan, Sarang; Knap, Michael; Demler, Eugene] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, Michael] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Mueller, Markus] Abdus Salam Int Ctr Theoret Phys, I-34151 Trieste, Italy. [Mueller, Markus] Univ Basel, Dept Phys, CH-4056 Basel, Switzerland. RP Agarwal, K (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM agarwal@physics.harvard.edu RI Knap, Michael/H-3344-2011 OI Knap, Michael/0000-0002-7093-9502 FU Harvard Quantum Optics Center; Harvard-MIT CUA; ARO-MURI Quism program; ARO-MURI on Atomtronics; Austrian Science Fund (FWF) [J 3361-N20] FX The authors acknowledge discussions with D. Abanin, E. Altman, A. Amir, I. Bloch, I. Gornyi, D. Huse, L. Ioffe, I. Lerner, M. Lukin, I. Martin, A. Mirlin, R. Modak, A. Pal, A. Polkovnikov, and N. Yao. The authors acknowledge support from Harvard Quantum Optics Center, Harvard-MIT CUA, ARO-MURI Quism program, ARO-MURI on Atomtronics, as well as the Austrian Science Fund (FWF) Project No. J 3361-N20. M. M. acknowledges the hospitality of the University of Basel. NR 63 TC 66 Z9 66 U1 5 U2 20 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 APR 23 PY 2015 VL 114 IS 16 AR 160401 DI 10.1103/PhysRevLett.114.160401 PG 6 WC Physics, Multidisciplinary SC Physics GA CG5KI UT WOS:000353330000001 PM 25955037 ER PT J AU Freeman, CJ Baker, DM Easson, CG Thacker, RW AF Freeman, Christopher J. Baker, David M. Easson, Cole G. Thacker, Robert W. TI Shifts in sponge-microbe mutualisms across an experimental irradiance gradient SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Stable isotopes; Metabolism; Mutualism; Porifera; Symbiosis ID CORAL-ALGAE SYMBIOSIS; STABLE-ISOTOPE; MARINE SPONGES; CYANOBACTERIA SYMBIOSES; DIVERSITY; EVOLUTION; COMMUNITIES; ZOOXANTHELLAE; ECOLOGY; MICROORGANISMS AB To investigate how the interactions between the closely related sponge species Aplysina cauliformis and Aplysina fulva and their symbiotic microbial communities vary under changing environmental conditions, we conducted a manipulative shading experiment with treatments spanning a gradient of 6 irradiances. In A. cauliformis, there was a tight coupling of symbiont and host metabolism across treatments, and changes in growth rate were correlated more with shifts in symbiont delta C-13 and delta N-15 values than with shade treatment. In contrast, symbiont and host C metabolism were weakly coupled in A. fulva, and the growth of this species was not correlated with shifts in symbiont delta C-13 and delta N-15 values. In addition, although photosymbiont meta bolism was an important driver of shifts in holobiont C and N metabolism of both host species, host and photosymbiont C metabolism were only correlated in A. cauliformis. Thus, although both species host stable, abundant, and similar photosymbiont communities, each host forms a unique mutualism with its symbionts. These 2 host species may be on different evolutionary trajectories, potentially allowing each to exploit novel niche space in coral reef ecosystems. This study provides data in support of the hypothesis that these symbioses represent a dynamic balance of costs and benefits and provides evidence that, because these costs and benefits are highly species specific, not all species will respond similarly to environmental fluctuations. C1 [Freeman, Christopher J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Freeman, Christopher J.; Easson, Cole G.; Thacker, Robert W.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Baker, David M.] Univ Hong Kong, Sch Biol Sci, Swire Inst Marine Sci, Hong Kong, Hong Kong, Peoples R China. [Baker, David M.] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China. RP Freeman, CJ (reprint author), Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. EM freemanc@si.edu FU Smithsonian Tropical Research Short-Term Fellowship; US National Science Foundation [0726944, 0829986]; Smithsonian Institution Marine Science Network Postdoctoral Fellowship FX We thank R. Collin, G. Jacome, and P. Gondola at the Smithsonian Tropical Research Institute Bocas Research Station and M. Fogel and R. Bowden at the Geophysical Laboratory for their technical assistance and logistical support. K. Erickson provided field assistance. Financial support for this project came from a Smithsonian Tropical Research Short-Term Fellowship, a Sigma Xi Grants-in-Aid of Research to C.J.F., US National Science Foundation Grants 0726944 and 0829986 to R.W.T. and a Smithsonian Institution Marine Science Network Postdoctoral Fellowship awarded to D.M.B. NR 49 TC 3 Z9 3 U1 6 U2 26 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD APR 22 PY 2015 VL 526 BP 41 EP 53 DI 10.3354/meps11249 PG 13 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA CH9ZJ UT WOS:000354394900004 ER PT J AU Becker, MH Walke, JB Cikanek, S Savage, AE Mattheus, N Santiago, CN Minbiole, KPC Harris, RN Belden, LK Gratwicke, B AF Becker, Matthew H. Walke, Jenifer B. Cikanek, Shawna Savage, Anna E. Mattheus, Nichole Santiago, Celina N. Minbiole, Kevin P. C. Harris, Reid N. Belden, Lisa K. Gratwicke, Brian TI Composition of symbiotic bacteria predicts survival in Panamanian golden frogs infected with a lethal fungus SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE amphibians; probiotics; skin bacteria; disease; microbiome; chytrid fungus ID SALAMANDER PLETHODON-CINEREUS; BATRACHOCHYTRIUM-DENDROBATIDIS; CUTANEOUS BACTERIA; ANTIFUNGAL METABOLITES; 4-TOED SALAMANDERS; SKIN MICROBIOME; ATELOPUS-ZETEKI; CHYTRIDIOMYCOSIS; AMPHIBIANS; IMMUNITY AB Symbiotic microbes can dramatically impact host health and fitness, and recent research in a diversity of systems suggests that different symbiont community structures may result in distinct outcomes for the host. In amphibians, some symbiotic skin bacteria produce metabolites that inhibit the growth of Batrachochytrium dendrobatidis (Bd), a cutaneous fungal pathogen that has caused many amphibian population declines and extinctions. Treatment with beneficial bacteria (probiotics) prevents Bd infection in some amphibian species and creates optimism for conservation of species that are highly susceptible to chytridiomycosis, the disease caused by Bd. In a laboratory experiment, we used Bd-inhibitory bacteria from Bd-tolerant Panamanian amphibians in a probiotic development trial with Panamanian golden frogs, Atelopus zeteki, a species currently surviving only in captive assurance colonies. Approximately 30% of infected golden frogs survived Bd exposure by either clearing infection or maintaining low Bd loads, but this was not associated with probiotic treatment. Survival was instead related to initial composition of the skin bacterial community and metabolites present on the skin. These results suggest a strong link between the structure of these symbiotic microbial communities and amphibian host health in the face of Bd exposure and also suggest a new approach for developing amphibian probiotics. C1 [Becker, Matthew H.; Walke, Jenifer B.; Belden, Lisa K.] Virginia Tech, Dept Biol Sci, Blacksburg, VA USA. [Cikanek, Shawna] Kansas State Univ, Dept Clin Sci, Manhattan, KS 66506 USA. [Savage, Anna E.; Mattheus, Nichole] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC USA. [Gratwicke, Brian] Smithsonian Conservat Biol Inst, Ctr Species Survival, Natl Zool Pk, Washington, DC USA. [Santiago, Celina N.; Minbiole, Kevin P. C.] Villanova Univ, Dept Chem, Villanova, PA 19085 USA. [Harris, Reid N.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA. RP Becker, MH (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC USA. EM beckerm@si.edu RI Savage, Anna/D-8296-2015; OI Savage, Anna/0000-0002-4917-8358; Belden, Lisa/0000-0002-3514-3920 FU United States Fish and Wildlife Service Amphibians in Decline Fund; National Science Foundation [DEB-1136640, DEB-1136662]; Shared Earth Foundation; frog-friendly foundation FX This research was financially supported by the United States Fish and Wildlife Service Amphibians in Decline Fund, the National Science Foundation (DEB-1136640 and DEB-1136662), the Shared Earth Foundation and an anonymous frog-friendly foundation. NR 71 TC 12 Z9 12 U1 13 U2 91 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 APR 22 PY 2015 VL 282 IS 1805 AR 20142881 DI 10.1098/rspb.2014.2881 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CE3ZU UT WOS:000351770200011 ER PT J AU Chang, D Olenzek, AM Duda, TF AF Chang, Dan Olenzek, Amy M. Duda, Thomas F., Jr. TI Effects of geographical heterogeneity in species interactions on the evolution of venom genes SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE conotoxin; Conus; predator-prey interactions; selection; geographical variation ID NUCLEOTIDE SUBSTITUTIONS; INTRASPECIFIC VARIATION; POPULATION-STRUCTURE; STATISTICAL TESTS; MITOCHONDRIAL-DNA; TROPICAL PACIFIC; MARINE GASTROPOD; RAPID EVOLUTION; EASTER-ISLAND; CONUS-EBRAEUS AB Geographical heterogeneity in the composition of biotic interactions can create a mosaic of selection regimes that may drive the differentiation of phenotypes that operate at the interface of these interactions. Nonetheless, little is known about effects of these geographical mosaics on the evolution of genes encoding traits associated with species interactions. Predatory marine snails of the family Conidae use venom, a cocktail of conotoxins, to capture prey. We characterized patterns of geographical variation at five conotoxin genes of a vermivorous species, Conus ebraeus, at Hawaii, Guam and American Samoa, and evaluated how these patterns of variation are associated with geographical heterogeneity in prey utilization. All populations show distinct patterns of prey utilization. Three 'highly polymorphic' conotoxin genes showed significant geographical differences in allelic frequency, and appear to be affected by different modes of selection among populations. Two genes exhibited low levels of diversity and a general lack of differentiation among populations. Levels of diversity of 'highly polymorphic' genes exhibit a positive relationship with dietary breadth. The different patterns of evolution exhibited by conotoxin genes suggest that these genes play different roles in prey capture, and that some genes are more greatly affected by differences in predator-prey interactions than others. Moreover, differences in dietary breadth appear to have a greater influence on the differentiation of venoms than differences in the species of prey. C1 [Chang, Dan; Olenzek, Amy M.; Duda, Thomas F., Jr.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Chang, Dan; Olenzek, Amy M.; Duda, Thomas F., Jr.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Chang, Dan] Univ Michigan, Dept Stat, Ann Arbor, MI 48109 USA. [Duda, Thomas F., Jr.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Chang, D (reprint author), Univ Calif Santa Cruz, 1156 High St,Mail Stop EEBiol, Santa Cruz, CA 95064 USA. EM changdan@umich.edu FU NSF [IOS-0718379] FX This study was funded by an NSF grant (IOS-0718379) to T.F.D. NR 72 TC 3 Z9 3 U1 4 U2 13 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 APR 22 PY 2015 VL 282 IS 1805 AR 20141984 DI 10.1098/rspb.2014.1984 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CE3ZU UT WOS:000351770200003 ER PT J AU Harvey, MG Judy, CD Seeholzer, GF Maley, JM Graves, GR Brumfield, RT AF Harvey, Michael G. Judy, Caroline Duffie Seeholzer, Glenn F. Maley, James M. Graves, Gary R. Brumfield, Robb T. TI Similarity thresholds used in DNA sequence assembly from short reads can reduce the comparability of population histories across species SO PEERJ LA English DT Article DE Next-generation sequencing; Bioinformatics; Birds; Non-model species; Phylogeography; Population genetics ID DE-NOVO; GENETIC DIVERSITY; PHYLOGEOGRAPHY; GENOMICS; DELIMITATION; DIVERGENCE; SPECIATION; EVOLUTION; EXPANSION; MARKERS AB Comparing inferences among datasets generated using short read sequencing may provide insight into the concerted impacts of divergence, gene flow and selection across organisms, but comparisons are complicated by biases introduced during dataset assembly. Sequence similarity thresholds allow the de novo assembly of short reads into clusters of alleles representing different loci, but the resulting datasets are sensitive to both the similarity threshold used and to the variation naturally present in the organism under study. Thresholds that require high sequence similarity among reads for assembly (stringent thresholds) as well as highly variable species may result in datasets in which divergent alleles are lost or divided into separate loci ('over-splitting'), whereas liberal thresholds increase the risk of paralogous loci being combined into a single locus ('under-splitting'). Comparisons among datasets or species are therefore potentially biased if different similarity thresholds are applied or if the species differ in levels of within-lineage genetic variation. We examine the impact of a range of similarity thresholds on assembly of empirical short read datasets from populations of four different non-model bird lineages (species or species pairs) with different levels of genetic divergence. We find that, in all species, stringent similarity thresholds result in fewer alleles per locus than more liberal thresholds, which appears to be the result of high levels of over-splitting. The frequency of putative under-splitting, conversely, is low at all thresholds. Inferred genetic distances between individuals, gene tree depths, and estimates of the ancestral mutation-scaled effective population size (.) differ depending upon the similarity threshold applied. Relative differences in inferences across species differ even when the same threshold is applied, but may be dramatically different when datasets assembled under different thresholds are compared. These differences not only complicate comparisons across species, but also preclude the application of standard mutation rates for parameter calibration. We suggest some best practices for assembling short read data to maximize comparability, such as using more liberal thresholds and examining the impact of different thresholds on each dataset. C1 [Harvey, Michael G.; Judy, Caroline Duffie; Seeholzer, Glenn F.; Maley, James M.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Harvey, Michael G.; Judy, Caroline Duffie; Seeholzer, Glenn F.; Maley, James M.; Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Judy, Caroline Duffie; Graves, Gary R.] Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116, Smithsonian Inst, Washington, DC 20560 USA. [Maley, James M.] Occidental Coll, Moore Lab Zool, Los Angeles, CA 90041 USA. [Graves, Gary R.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, Copenhagen O, Denmark. RP Harvey, MG (reprint author), Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. EM mharve9@lsu.edu RI Brumfield, Robb/K-6108-2015; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 OI Brumfield, Robb/0000-0003-2307-0688; FU NSF Doctoral Dissertation Improvement [DEB-1210556, DEB-1110624] FX Funding was provided by NSF Doctoral Dissertation Improvement Grants to Michael G. Harvey (DEB-1210556) and James M. Maley (DEB-1110624). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 51 TC 11 Z9 11 U1 2 U2 29 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD APR 21 PY 2015 VL 3 AR e895 DI 10.7717/peerj.895 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CH2DU UT WOS:000353836500002 PM 25922792 ER PT J AU Hunt, G Hopkins, MJ Lidgard, S AF Hunt, Gene Hopkins, Melanie J. Lidgard, Scott TI Simple versus complex models of trait evolution and stasis as a response to environmental change SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE evolutionary mode; stasis; gradualism; punctuated equilibrium; climate change ID PHENOTYPIC EVOLUTION; RANDOM-WALKS; BODY-SIZE; PUNCTUATED EQUILIBRIA; STABILIZING SELECTION; CLIMATE-CHANGE; FOSSIL RECORD; TEMPO; RATES; SEA AB Previous analyses of evolutionary patterns, or modes, in fossil lineages have focused overwhelmingly on three simple models: stasis, random walks, and directional evolution. Here we use likelihood methods to fit an expanded set of evolutionary models to a large compilation of ancestor-descendant series of populations from the fossil record. In addition to the standard three models, we assess more complex models with punctuations and shifts from one evolutionary mode to another. As in previous studies, we find that stasis is common in the fossil record, as is a strict version of stasis that entails no real evolutionary changes. Incidence of directional evolution is relatively low (13%), but higher than in previous studies because our analytical approach can more sensitively detect noisy trends. Complex evolutionary models are often favored, overwhelmingly so for sequences comprising many samples. This finding is consistent with evolutionary dynamics that are, in reality, more complex than any of the models we consider. Furthermore, the timing of shifts in evolutionary dynamics varies among traits measured from the same series. Finally, we use our empirical collection of evolutionary sequences and a long and highly resolved proxy for global climate to inform simulations in which traits adaptively track temperature changes over time. When realistically calibrated, we find that this simple model can reproduce important aspects of our paleontological results. We conclude that observed paleontological patterns, including the prevalence of stasis, need not be inconsistent with adaptive evolution, even in the face of unstable physical environments. C1 [Hunt, Gene] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Hopkins, Melanie J.] Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. [Lidgard, Scott] Field Museum Nat Hist, Integrat Res Ctr, Chicago, IL 60605 USA. RP Hunt, G (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. EM hunte@si.edu NR 56 TC 13 Z9 13 U1 3 U2 30 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 APR 21 PY 2015 VL 112 IS 16 BP 4885 EP 4890 DI 10.1073/pnas.1403662111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG4FJ UT WOS:000353239100034 PM 25901309 ER PT J AU Slater, GJ AF Slater, Graham J. TI Iterative adaptive radiations of fossil canids show no evidence for diversity-dependent trait evolution SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE macroevolution; adaptive radiation; Canidae; phylogenetics; rates ID BODY-SIZE EVOLUTION; EARLY BURSTS; PHYLOGENETIC SYSTEMATICS; MORPHOLOGICAL DISPARITY; ECOLOGICAL OPPORTUNITY; STABILIZING SELECTION; ACTIVE TRENDS; COPES RULE; CARNIVORA; DIVERSIFICATION AB A long-standing hypothesis in adaptive radiation theory is that ecological opportunity constrains rates of phenotypic evolution, generating a burst of morphological disparity early in clade history. Empirical support for the early burst model is rare in comparative data, however. One possible reason for this lack of support is that most phylogenetic tests have focused on extant clades, neglecting information from fossil taxa. Here, I test for the expected signature of adaptive radiation using the outstanding 40-My fossil record of North American canids. Models implying time-and diversity-dependent rates of morphological evolution are strongly rejected for two ecologically important traits, body size and grinding area of the molar teeth. Instead, Ornstein-Uhlenbeck processes implying repeated, and sometimes rapid, attraction to distinct dietary adaptive peaks receive substantial support. Diversity-dependent rates of morphological evolution seem uncommon in clades, such as canids, that exhibit a pattern of replicated adaptive radiation. Instead, these clades might best be thought of as deterministic radiations in constrained Simpsonian subzones of a major adaptive zone. Support for adaptive peak models may be diagnostic of subzonal radiations. It remains to be seen whether early burst or ecological opportunity models can explain broader adaptive radiations, such as the evolution of higher taxa. C1 Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20001 USA. RP Slater, GJ (reprint author), Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20001 USA. EM slaterg@si.edu FU Peter Buck Post-Doctoral Fellowship at the National Museum of Natural History (Smithsonian Institution) FX I thank D. Jablonski and N. Shubin for inviting me to contribute this article, and D. Bohaska, J. Galkin, D. Lunde, and N. Pyenson for access to specimens. I am especially grateful to G. Hunt for much useful discussion of ideas, and to G. Hunt, J. Finarelli, and an anonymous reviewer for helpful comments and criticisms on earlier versions of the manuscript. This work was supported by a Peter Buck Post-Doctoral Fellowship at the National Museum of Natural History (Smithsonian Institution). NR 68 TC 19 Z9 19 U1 5 U2 31 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 APR 21 PY 2015 VL 112 IS 16 BP 4897 EP 4902 DI 10.1073/pnas.1403666111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG4FJ UT WOS:000353239100036 PM 25901311 ER PT J AU Douchin, D De Marco, O Frew, DJ Jacoby, GH Jasniewicz, G Fitzgerald, M Passy, JC Harmer, D Hillwig, T Moe, M AF Douchin, Dimitri De Marco, Orsola Frew, D. J. Jacoby, G. H. Jasniewicz, G. Fitzgerald, M. Passy, Jean-Claude Harmer, D. Hillwig, Todd Moe, Maxwell TI The binary fraction of planetary nebula central stars - II. A larger sample and improved technique for the infrared excess search SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; surveys; binaries: general; stars: evolution; stars: statistics; planetary nebulae: general ID DIGITAL SKY SURVEY; H-ALPHA SURVEY; BE-URSAE-MAJORIS; WHITE-DWARFS; TRIGONOMETRIC PARALLAXES; POPULATION SYNTHESIS; RADIAL-VELOCITY; GALACTIC PLANE; STELLAR LOCUS; LOTR 5 AB There is no conclusive explanation of why similar to 80 per cent of planetary nebulae (PNe) are non-spherical. In the Binary Hypothesis, a binary interaction is a preferred channel to form a non-spherical PN. A fundamental step to corroborate or disprove the Binary Hypothesis is to estimate the binary fraction of central stars of PNe (CSPNe) and compare it with a prediction based on the binary fraction of the progenitor, main-sequence population. In this paper, the second in a series, we search for spatially unresolved I-and J-band flux excess in an extended sample of 34 CSPN by a refined measurement technique with a better quantification of the uncertainties. The detection rate of I-(J-) band flux excess is 32 +/- 16 per cent (50 +/- 24 per cent). This result is very close to what was obtained in Paper I with a smaller sample. We account conservatively for unobserved cool companions down to brown dwarf luminosities, increasing these fractions to 40 +/- 20 per cent (62 +/- 30 per cent). This step is very sensitive to the adopted brightness limit of our survey. Accounting for visual companions increases the binary fraction to 46 +/- 23 per cent (71 +/- 34 per cent). These figures are lower than in Paper I. The error bars are better quantified, but still unacceptably large. Taken at face value, the current CSPN binary fraction is in line with the main-sequence progenitor population binary fraction. However, including white dwarfs companions could increase this fraction by as much as 13 (21) per cent points. C1 [Douchin, Dimitri; De Marco, Orsola; Frew, D. J.; Fitzgerald, M.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Douchin, Dimitri; De Marco, Orsola; Frew, D. J.; Fitzgerald, M.] Macquarie Univ, Astron Astrophys & Astrophoton Res Ctr, Sydney, NSW 2109, Australia. [Douchin, Dimitri; Jasniewicz, G.] Univ Montpellier 2, Lab Univers & Particules, F-34095 Montpellier 5, France. [Jacoby, G. H.] Giant Magellan Telescope, Pasadena, CA 91101 USA. [Jacoby, G. H.] Carnegie Observ, Pasadena, CA 91101 USA. [Passy, Jean-Claude] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P5C2, Canada. [Harmer, D.] Natl Opt Astron Observ, Kitt Peak Natl Observ, Tucson, AZ 85719 USA. [Hillwig, Todd] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA. [Moe, Maxwell] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Douchin, D (reprint author), Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. EM dimitri.douchin@mq.edu.au OI Hillwig, Todd/0000-0002-0816-1090; Frew, David/0000-0002-3108-5284 FU Australian Research Council via the Future Fellowship scheme [FT120100452]; 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 The authors thank the anonymous reviewer for his comments and suggestions. DD thanks Quentin Parker for his support during the writing of this paper and Ivan Bojicic for his help in using the Macquarie University GPN Database. OD acknowledges financial support from the Australian Research Council via the Future Fellowship scheme (FT120100452).; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 93 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 APR 21 PY 2015 VL 448 IS 4 BP 3132 EP 3155 DI 10.1093/mnras/stu2700 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0WF UT WOS:000351529500013 ER PT J AU Dincel, B Neuhauser, R Yerli, SK Ankay, A Tetzlaff, N Torres, G Mugrauer, M AF Dincel, B. Neuhaeuser, R. Yerli, S. K. Ankay, A. Tetzlaff, N. Torres, G. Mugrauer, M. TI Discovery of an OB runaway star inside SNR S147 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: early type; stars: individual: HD37424; pulsars: individual: PSR J0538+2817; ISM: individual objects: SNR G180.0-1.7 (S147); ISM: supernova remnants ID NOVA REMNANT S147; UNIVERSITY OBSERVATORY JENA; GALACTIC SUPERNOVA-REMNANTS; B-TYPE STARS; SPECTRAL CLASSIFICATION; PULSAR COMPANIONS; PROPER MOTIONS; PSR J0538+2817; RADIO PULSARS; NEUTRON-STARS AB We present first results of a long-term study: Searching for OB-type runaway stars inside supernova remnants (SNRs). We identified spectral types and measured radial velocities by optical spectroscopic observations and we found an early type runaway star inside SNR S147. HD 37424 is a B0.5V-type star with a peculiar velocity of 74 +/- 8 kms(-1). Tracing back the past trajectories via Monte Carlo simulations, we found that HD 37424 was located at the same position as the central compact object, PSR J0538+2817, 30 +/- 4 kyr ago. This position is only similar to 4 arcmin away from the geometrical centre of the SNR. So, we suggest that HD 37424 was the pre-supernova binary companion to the progenitor of the pulsar and the SNR. We found a distance of 1333(-112)(+103) pc to the SNR. The zero-age main sequence progenitor mass should be greater than 13 M-circle dot. The age is 30 +/- 4 kyr and the total visual absorption towards the centre is 1.28 +/- 0.06 mag. For different progenitor masses, we calculated the pre-supernova binary parameters. The Roche lobe radii suggest that it was an interacting binary in the late stages of the progenitor. C1 [Dincel, B.; Neuhaeuser, R.; Tetzlaff, N.; Mugrauer, M.] Inst Astrophys, D-07745 Jena, Germany. [Dincel, B.; Neuhaeuser, R.; Tetzlaff, N.; Mugrauer, M.] Univ Sternwarte Jena, D-07745 Jena, Germany. [Yerli, S. K.] Orta Dogu Teknik Univ, Dept Phys, TR-06531 Ankara, Turkey. [Ankay, A.] Bogazici Univ, Dept Phys, TR-34342 Istanbul, Turkey. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dincel, B (reprint author), Inst Astrophys, D-07745 Jena, Germany. EM baha.dincel@uni-jena.de RI Yerli, Sinan/D-1324-2010 FU DFG [SFB/TR-7, NE 515/53-1]; TUBITAK National Observatory [12ARTT150-267] FX This work was conceived by the late Oktay H. GUSEINOV (1938-2009). We acknowledge the leading role he had in all stages of this work and other related topics. His contribution to Galactic Astrophysics and his scholarship will be greatly missed. We thank Janos Schmidt and Christian Ginski for their observational support and Ronny Errmann for useful discussions. BD, NT and RN acknowledge support from DFG in the SFB/TR-7 Gravitational Wave Astronomy. This research has made use of ALADIN. We would like to thank the Calar Alto observatory staff for their help in our observations; and we would like to thank DFG in NE 515/53-1 for financial support for the Calar Alto observing run. We also thank TUBITAK National Observatory for their supports in using RTT-150 with project number 12ARTT150-267. NR 81 TC 2 Z9 2 U1 2 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 APR 21 PY 2015 VL 448 IS 4 BP 3196 EP 3205 DI 10.1093/mnras/stv124 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0WF UT WOS:000351529500016 ER PT J AU Britt, CT Maccarone, T Pretorius, ML Hynes, RI Jonker, PG Torres, MAP Knigge, C Johnson, CO Heinke, CB Steeghs, D Greiss, S Nelemans, G AF Britt, C. T. Maccarone, T. Pretorius, M. L. Hynes, R. I. Jonker, P. G. Torres, M. A. P. Knigge, C. Johnson, C. O. Heinke, C. B. Steeghs, D. Greiss, S. Nelemans, G. TI The relationship between X-ray luminosity and duty cycle for dwarf novae and their specific frequency in the inner Galaxy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars: dwarf novae; novae, cataclysmic variables ID GALACTIC BULGE SURVEY; CATACLYSMIC VARIABLE-STARS; Z-CAMELOPARDALIS; SPACE DENSITY; MILKY-WAY; ABSOLUTE MAGNITUDES; COMPACT BINARIES; U-GEMINORUM; SS-CYGNI; EVOLUTION AB We measure the duty cycles for an existing sample of well-observed, nearby dwarf novae (DNe) using data from American Association of Variable Star Observers, and present a quantitative empirical relation between the duty cycle of DNe outbursts and the X-ray luminosity of the system in quiescence. We have found that logDC = 0.63(+/- 0.21) x (log L-X(erg s(-1)) - 31.3) -0.95(+/- 0.1), where DC stands for duty cycle. We note that there is intrinsic scatter in this relation greater than what is expected from purely statistical errors. Using the DN X-ray luminosity functions from Pretorius & Knigge and Byckling et al., we compare this relation to the number of DNe in the Galactic Bulge Survey which were identified through optical outbursts during an 8-d-long monitoring campaign. We find a specific frequency of X-ray-bright (L-X greater than or similar to 10(31) erg s(-1)) cataclysmic variables (CVs) undergoing DNe outbursts in the direction of the Galactic bulge of 6.6 +/- 4.7 x 10(-5) M-circle dot(-1). Such a specific frequency would give a solar neighbourhood space density of long-period CVs of. = 5.6 +/- 3.9 x 10(-6) pc(-3). We advocate the use of specific frequency in future work, given that projects like Large Synoptic Survey Telescope will detect DNe well outside the distance range over which rho approximate to const. C1 [Britt, C. T.; Maccarone, T.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Pretorius, M. L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Hynes, R. I.; Johnson, C. O.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Jonker, P. G.; Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Torres, M. A. P.; Nelemans, G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Heinke, C. B.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Heinke, C. B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Steeghs, D.; Greiss, S.] Univ Warwick, Dept Phys, Astron & Astrophys, Coventry CV4 7AL, W Midlands, England. RP Britt, CT (reprint author), Texas Tech Univ, Dept Phys, Box 41051,Sci Bldg, Lubbock, TX 79409 USA. EM christopher.britt@ttu.edu RI Nelemans, Gijs/D-3177-2012 OI Nelemans, Gijs/0000-0002-0752-2974 FU NSERC; Ingenuity New Faculty Award; Alexander von Humboldt Fellowship FX COH is supported by NSERC, an Ingenuity New Faculty Award, and an Alexander von Humboldt Fellowship. This research has made use of NASA's Astrophysics Data System Bibliographic Services and of SAOImage DS9, developed by Smithsonian Astrophysical Observatory. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. We thank the referee, Koji Mukai, for his insightful comments improving the interpretation of this work. NR 66 TC 2 Z9 2 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 APR 21 PY 2015 VL 448 IS 4 BP 3455 EP 3462 DI 10.1093/mnras/stv256 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0WF UT WOS:000351529500040 ER PT J AU Zemunik, G Turner, BL Lambers, H Laliberte, E AF Zemunik, Graham Turner, Benjamin L. Lambers, Hans Laliberte, Etienne TI Diversity of plant nutrient-acquisition strategies increases during long-term ecosystem development SO NATURE PLANTS LA English DT Article ID 2-MILLION-YEAR DUNE CHRONOSEQUENCE; TEMPERATE RAIN-FOREST; SOIL CHRONOSEQUENCE; PHOSPHORUS LIMITATION; FUNCTIONAL DIVERSITY; ECONOMICS SPECTRUM; MULTIPLE TRAITS; RETROGRESSION; BIODIVERSITY; PEDOGENESIS AB Plant species diversity increases as soil phosphorus availability declines during long-term ecosystem development(1,2). The increase in plant species diversity is associated with a decline in above-ground functional diversity, because leaf traits converge on a high phosphorus-use efficiency strategy on old and infertile soils(3,4). In contrast, the response of below-ground traits that directly influence nutrient acquisition remains poorly understood(3,5); yet it might be key to understanding how soil fertility drives patterns of plant species diversity(1). Here we show a marked increase in the richness and diversity of plant nutrient-acquisition strategies with declining soil phosphorus availability during long-term ecosystem development in a global biodiversity hotspot. Almost all nutrient-acquisition strategies currently known were found in plants from the most infertile soils, despite these being some of the most phosphorus-impoverished soils on Earth. Mycorrhizal plants declined in relative abundance by >30%, although the decline was compensated by an increase in non-mycorrhizal, carboxylate-exuding species that 'mine' phosphorus from the soil using different strategies. Plant species richness within individual nutrient-acquisition strategies also increased dramatically, with the species richness of many strategies more than doubling between the youngest and oldest soils. These results reveal increasing functional diversity of below-ground traits related to nutrient acquisition during ecosystem development, suggesting that no single combination of traits, including those related to nutrient-acquisition strategies, is superior to all others at extremely low soil fertility. Furthermore, the increasing diversity of nutrient-acquisition strategies with declining soil fertility, despite functional convergence of above-ground traits(4,6), suggests that fundamentally different plant community assembly processes operate above-and below-ground. C1 [Zemunik, Graham; Turner, Benjamin L.; Lambers, Hans; Laliberte, Etienne] Univ Western Australia, Sch Plant Biol, Perth, WA 6009, Australia. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Laliberte, Etienne] Univ Montreal, Inst Rech Biol Vegetale, Montreal, PQ H1X 2B2, Canada. RP Zemunik, G (reprint author), Univ Western Australia, Sch Plant Biol, Perth, WA 6009, Australia. EM graham@graduate.uwa.edu.au RI Laliberte, Etienne/B-6855-2008; Turner, Benjamin/E-5940-2011; Lambers, Hans/A-1544-2008; OI Laliberte, Etienne/0000-0002-3167-2622; Turner, Benjamin/0000-0002-6585-0722; Lambers, Hans/0000-0002-4118-2272; Zemunik, Graham/0000-0002-6064-345X FU Paul Hasluck Bequest; UWA; DECRA [DE120100352]; Australian Research Council (ARC) [ARC DP0985685]; University, State and Commonwealth Governments FX G.Z. was supported by a scholarship from the Paul Hasluck Bequest administered by the Kwongan Foundation. We acknowledge the assistance of many people in conducting the flora surveys. Funding was provided by research awards from UWA and a DECRA (DE120100352) from the Australian Research Council (ARC) to E.L. H.L. was supported by the Australian Research Council (ARC DP0985685). We thank D. Agudo and A. Bielnicka for laboratory support. We acknowledge the Department of Parks and Wildlife (Western Australia) and the Shires of Dandaragan, and Coorow for permission to conduct research on land under their administration. We acknowledge the facilities, and the scientific and technical assistance of the Australian Microscopy & Microanalysis Research Facility at the Centre for Microscopy, Characterisation & Analysis, The University of Western Australia, a facility funded by the University, State and Commonwealth Governments. NR 30 TC 17 Z9 17 U1 12 U2 36 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2055-026X EI 2055-0278 J9 NAT PLANTS JI Nat. Plants PD APR 20 PY 2015 VL 1 IS 5 BP 1 EP 4 AR 15050 DI 10.1038/NPLANTS.2015.50 PG 4 WC Plant Sciences SC Plant Sciences GA CV6RP UT WOS:000364398300001 ER PT J AU Andrade-Santos, F Jones, C Forman, WR Murray, SS Kraft, RP Vikhlinin, A van Weeren, RJ Nulsen, PEJ David, LP Dawson, WA Arnaud, M Pointecouteau, E Pratt, GW Melin, JB AF Andrade-Santos, Felipe Jones, Christine Forman, William R. Murray, Stephen S. Kraft, Ralph P. Vikhlinin, Alexey van Weeren, Reinout J. Nulsen, Paul E. J. David, Laurence P. Dawson, William A. Arnaud, Monique Pointecouteau, Etienne Pratt, Gabriel W. Melin, Jean-Baptiste TI CHANDRA AND XMM-NEWTON OBSERVATIONS OF THE BIMODAL PLANCK SZ-DETECTED CLUSTER PLCKG345.40-39.34 (A3716) WITH HIGH AND LOW ENTROPY SUBCLUSTER CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (A3716); large-scale structure of universe; X-rays: galaxies: clusters ID RELAXED GALAXY CLUSTERS; REPRESENTATIVE SAMPLE; TEMPERATURE RELATION; STELLAR POPULATION; SURVEY DESIGN; COMA CLUSTER; JET POWER; EVOLUTION; MASS; GAS AB We present results from Chandra, XMM-Newton, and ROSAT observations of the Planck SZ-detected cluster A3716 (PLCKG345.40-39.34-G345). We show that G345 is, in fact, two subclusters separated on the sky by 400 kpc. We measure the subclusters' gas temperatures (similar to 2-3 keV), total (similar to 1-2 x 10(14) M-circle dot) and gas (similar to 1-2 x 10(13) M-circle dot) masses, gas mass fraction within r(500), entropy profiles, and X-ray luminosities (similar to 10(43) erg s(-1)). Using the gas density and temperature profiles for both subclusters, we show that there is good (0.8 sigma) agreement between the expected Sunyaev-Zel'dovich signal predicted from the X-ray data and that measured from the Planck mission, and better agreement within 0.6 sigma when we re-computed the Planck value assuming a two component cluster model, with relative amplitudes fixed based on the X-ray data. Dynamical analysis shows that the two galaxy subclusters are very likely (> 97% probability) gravitationally bound, and in the most likely scenario, the subclusters will undergo core passage in 500 +/- 200 Myr. The northern subcluster is centrally peaked and has a low entropy core, while the southern subcluster has a high central entropy. The high central entropy in the southern subcluster can be explained either by the mergers of several groups, as suggested by the presence of five giant ellipticals or by active galactic nucleus energy injection, as suggested by the presence of a strong radio source in one of its massive elliptical galaxies, or by a combination of both processes. C1 [Andrade-Santos, Felipe; Jones, Christine; Forman, William R.; Murray, Stephen S.; Kraft, Ralph P.; Vikhlinin, Alexey; van Weeren, Reinout J.; Nulsen, Paul E. J.; David, Laurence P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Dawson, William A.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Arnaud, Monique; Pratt, Gabriel W.] Univ Paris Diderot, IRFU Serv Astrophys CEA DSM CNRS, Lab AIM, CEA Saclay, F-91191 Gif Sur Yvette, France. [Pointecouteau, Etienne] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Pointecouteau, Etienne] CNRS, IRAP, F-31028 Toulouse 4, France. [Melin, Jean-Baptiste] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. RP Andrade-Santos, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM fsantos@cfa.harvard.edu OI Nulsen, Paul/0000-0003-0297-4493; van Weeren, Reinout/0000-0002-0587-1660; Forman, William/0000-0002-9478-1682 FU Chandra grant [G03-14131X]; Smithsonian Institution; NASA through Einstein Postdoctoral grant by Chandra X-Ray Center [PF2-130104]; NASA [NAS8-03060]; US DOE [DE-AC52-07NA27344]; French Agence Nationale de la Recherche [ANR-11-BD56-015] FX F.A.-S. acknowledges support from Chandra grant G03-14131X. C.J. and W.R.F. are supported by the Smithsonian Institution. R.J.W. is supported by NASA through the Einstein Postdoctoral grant PF2-130104 awarded by the Chandra X-Ray Center, which is operated by the Smithsonian Astro-physical Observatory for NASA under contract NAS8-03060. P.E.J.N., A.V., L.P.D., and R.P.K. were supported by NASA contract NAS8-03060. Part of this work performed under the auspices of the US DOE by LLNL under Contract DE-AC52-07NA27344. E.P., M.A. and G.W.P. acknowledge the support of the French Agence Nationale de la Recherche under grant ANR-11-BD56-015 We are also very grateful to the anonymous referee who helped to improve this work. NR 47 TC 2 Z9 2 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2015 VL 803 IS 2 AR 108 DI 10.1088/0004-637X/803/2/108 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG7YT UT WOS:000353524500059 ER PT J AU Dierickx, M Jimenez-Serra, I Rivilla, VM Zhang, Q AF Dierickx, M. Jimenez-Serra, I. Rivilla, V. M. Zhang, Q. TI SUBMILLIMETER ARRAY HIGH-ANGULAR RESOLUTION OBSERVATIONS OF THE MONOCEROS R2 STAR-FORMING CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Mon R2); ISM: jets and outflows; stars: formation ID YOUNG STELLAR OBJECTS; MASS PROTOSTELLAR CANDIDATES; OUTFLOW-DRIVEN TURBULENCE; GAS-PHASE H2O; H-II REGION; MOLECULAR OUTFLOWS; MON R2; CO OUTFLOWS; CLOUD CORE; HOT CORES AB We present the first high-angular resolution study of the MonR2 star-forming complex carried out with the Submillimeter Array at (sub-) millimeter wavelengths. We image the continuum and molecular line emission toward the young stellar objects in MonR2 at 0.85 and 1.3 mm, with resolutions ranging from 0.'' 5 to similar to 3 ''. While free-free emission dominates the IRS1 and IRS2 continuum, dust thermal emission prevails for IRS3 and IRS5, giving envelope masses of similar to 0.1-0.3 M-circle dot. IRS5 splits into at least two sub-arcsecond scale sources, IRS5B and the more massive IRS5A. Our (CO)-C-12(2-1) images reveal 11 previously unknown molecular outflows in the MonR2 clump. Comparing these outflows with known IR sources in the IRS5 and IRS3 subclusters allows for tentative identification of driving stars. Line images of molecular species such as CH3CN or CH3OH show that, besides IRS3 (a well-known hot molecular core), IRS5 is also a chemically active source in the region. The gas excitation temperature derived from CH3CN lines toward IRS5 is 144 +/- 15 K, indicating a deeply embedded protostar at the hot-core evolutionary stage. Spectral energy distribution fitting of IRS5 gives a mass of similar to 7 M-circle dot and a luminosity of 300 L-circle dot for the central source. The derived physical properties of the CO outflows suggest that they contribute to the turbulent support of the MonR2 complex and to the gas velocity dispersion in the clump's center. The detection of a large number of CO outflows widespread across the region supports the competitive accretion scenario as origin of the MonR2 star cluster. C1 [Dierickx, M.; Jimenez-Serra, I.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jimenez-Serra, I.] European So Observ, D-85748 Garching, Germany. [Jimenez-Serra, I.] UCL, Dept Phys & Astron, London NW1 2PS, England. [Rivilla, V. M.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain. [Rivilla, V. M.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. RP Dierickx, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mdierickx@cfa.harvard.edu; ijimenez@eso.org; ryvendel@gmail.com; qzhang@cfa.harvard.edu OI Dierickx, Marion/0000-0002-3519-8593; Zhang, Qizhou/0000-0003-2384-6589 FU People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7) under REA [PIIF-GA-2011-301538]; Spanish project [AYA2010-21697-C05-01] FX I.J.-S. acknowledges financial support from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7/2007-2013) under REA grant agreement number PIIF-GA-2011-301538. V.M.R. acknowledges financial support from the Spanish project AYA2010-21697-C05-01. NR 99 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 APR 20 PY 2015 VL 803 IS 2 AR 89 DI 10.1088/0004-637X/803/2/89 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG7YT UT WOS:000353524500041 ER PT J AU Hung, CL Rich, JA Yuan, TT Larson, KL Casey, CM Smith, HA Sanders, DB Kewley, LJ Hayward, CC AF Hung, Chao-Ling Rich, Jeffrey A. Yuan, Tiantian Larson, Kirsten L. Casey, Caitlin M. Smith, Howard A. Sanders, D. B. Kewley, Lisa J. Hayward, Christopher C. TI KINEMATIC CLASSIFICATIONS OF LOCAL INTERACTING GALAXIES: IMPLICATIONS FOR THE MERGER/DISK CLASSIFICATIONS AT HIGH-z SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: interactions; galaxies: kinematics and dynamics; galaxies: structure ID ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMING GALAXIES; INTEGRAL FIELD SPECTROSCOPY; H-ALPHA KINEMATICS; ULTRA DEEP FIELD; ON SPIRAL GALAXY; HIGH-REDSHIFT; SUBMILLIMETER GALAXIES; MAJOR MERGERS; GOALS SAMPLE AB The classification of galaxy mergers and isolated disks is key for understanding the relative importance of galaxy interactions and secular evolution during the assembly of galaxies. Galaxy kinematics as traced by emission lines have been used to suggest the existence of a significant population of high-z star-forming galaxies consistent with isolated rotating disks. However, recent studies have cautioned that post-coalescence mergers may also display disk-like kinematics. To further investigate the robustness of merger/disk classifications based on kinematic properties, we carry out a systematic classification of 24 local (U) LIRGs spanning a range of morphologies: from isolated spiral galaxies, ongoing interacting systems, to fully merged remnants. We artificially redshift the Wide Field Spectrograph observations of these local (U) LIRGs to z = 1.5 to make a realistic comparison with observations at high-z, and also to ensure that all galaxies have the same spatial sampling of similar to 900 pc. Using both kinemetry-based and visual classifications, we find that the reliability of kinematic classification shows a strong trend with the interaction stage of galaxies. Mergers with two nuclei and tidal tails have the most distinct kinematics compared to isolated disks, whereas a significant population of the interacting disks and merger remnants are indistinguishable from isolated disks. The high fraction of mergers displaying disk-like kinematics reflects the complexity of the dynamics during galaxy interactions. Additional merger indicators such as morphological properties traced by stars or molecular gas are required to further constrain the merger/disk classifications at high-z. C1 [Hung, Chao-Ling; Larson, Kirsten L.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hung, Chao-Ling; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rich, Jeffrey A.] Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Rich, Jeffrey A.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Yuan, Tiantian; Kewley, Lisa J.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Casey, Caitlin M.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Hayward, Christopher C.] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Hayward, Christopher C.] CALTECH, TAPIR, Pasadena, CA 91125 USA. RP Hung, CL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM clhung@ifa.hawaii.edu RI Hayward, Christopher/I-4756-2012; OI Hayward, Christopher/0000-0003-4073-3236; Rich, Jeffrey/0000-0002-5807-5078; Casey, Caitlin/0000-0002-0930-6466 FU NASA [NNX14AJ61G, NNX11AB02G, NNX12AI55G]; Smithsonian Predoctoral Fellowship program; McCue Fellowship through the University of California, Irvines Center for Cosmology; Klaus Tschira Foundation; Gordon and Betty Moore Foundation; U.S. Government [NAG W-2166] FX We thank the referee for the great effort with improving the paper. C.-L.H. thanks A. W. Mann for technical help with Figures 1 and 5. C.-L.H. wishes to acknowledge support from NASA grants NNX14AJ61G, NNX11AB02G, and the Smithsonian Predoctoral Fellowship program. K.L.L. and D.B.S. gratefully acknowledge support from NASA grant NNX11AB02G. C.M.C. acknowledges support from a McCue Fellowship through the University of California, Irvines Center for Cosmology. H.A.S. acknowledges partial support from NASA grants NNX14AJ61G and NNX12AI55G. C.C.H. is grateful to the Klaus Tschira Foundation and Gordon and Betty Moore Foundation for financial support. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. NR 95 TC 6 Z9 6 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 APR 20 PY 2015 VL 803 IS 2 AR 62 DI 10.1088/0004-637X/803/2/62 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG7YT UT WOS:000353524500014 ER PT J AU Lindner, RR Aguirre, P Baker, AJ Bond, JR Crichton, D Devlin, MJ Essinger-Hileman, T Gallardo, P Gralla, MB Hilton, M Hincks, AD Huffenberger, KM Hughes, JP Infante, L Lima, M Marriage, TA Menanteau, F Niemack, MD Page, LA Schmitt, BL Sehgal, N Sievers, JL Sifon, C Staggs, ST Swetz, D Weiss, A Wollack, EJ AF Lindner, Robert R. Aguirre, Paula Baker, Andrew J. Bond, J. Richard Crichton, Devin Devlin, Mark J. Essinger-Hileman, Thomas Gallardo, Patricio Gralla, Megan B. Hilton, Matt Hincks, Adam D. Huffenberger, Kevin M. Hughes, John P. Infante, Leopoldo Lima, Marcos Marriage, Tobias A. Menanteau, Felipe Niemack, Michael D. Page, Lyman A. Schmitt, Benjamin L. Sehgal, Neelima Sievers, J. L. Sifon, Cristobal Staggs, Suzanne T. Swetz, Daniel Weiss, Axel Wollack, Edward J. TI THE ATACAMA COSMOLOGY TELESCOPE: THE LABOCA/ACT SURVEY OF CLUSTERS AT ALL REDSHIFTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; cosmology: observations; submillimeter: galaxies; submillimeter: general ID DEEP FIELD-SOUTH; MASSIVE GALAXY CLUSTERS; X-RAY; SUBMILLIMETER GALAXIES; 1E 0657-56; EL GORDO; PHYSICAL-PROPERTIES; PECULIAR VELOCITY; SCALING RELATIONS; MERGING CLUSTER AB We present a multi-wavelength analysis of 11 Sunyaev-Zel'dovich effect (SZE)-selected galaxy clusters (10 with new data) from the Atacama Cosmology Telescope (ACT) southern survey. We have obtained new imaging from the Large APEX Bolometer Camera (345 GHz; LABOCA) on the Atacama Pathfinder EXperiment (APEX) telescope, the Australia Telescope Compact Array (2.1 GHz; ATCA), and the Spectral and Photometric Imaging Receiver (250, 350, and 500 mu m; SPIRE) on the Herschel Space Observatory. (24)Spatially resolved 345 GHz SZE increments with integrated signal-to-noise ratio (S/N) > 5 are found in six clusters. We compute 2.1 GHz number counts as a function of cluster-centric radius and find significant enhancements in the counts of bright sources at projected radii theta < theta(2500c). By extrapolating in frequency, we predict that the combined signals from 2.1 GHz-selected radio sources and 345 GHz-selected submillimeter galaxies (SMGs) contaminate the 148 GHz SZE decrement signal by similar to 5% and the 345 GHz SZE increment by similar to 18%. After removing radio source and SMG emission from the SZE signals, we use ACT, LABOCA, and (in some cases) new Herschel SPIRE imaging to place constraints on the clusters' peculiar velocities. The sample's average peculiar velocity relative to the cosmic microwave background is < v(p)> = 153 +/- 383 km s(-1). C1 [Lindner, Robert R.; Baker, Andrew J.; Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Lindner, Robert R.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Aguirre, Paula] Pontificia Univ Catolica Chile, Sch Engn, Santiago, Chile. [Bond, J. Richard] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Crichton, Devin; Essinger-Hileman, Thomas; Gralla, Megan B.; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Devlin, Mark J.; Schmitt, Benjamin L.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Gallardo, Patricio; Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Gallardo, Patricio] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Gralla, Megan B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hilton, Matt; Infante, Leopoldo; Sievers, J. L.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. [Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Huffenberger, Kevin M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Lima, Marcos] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, BR-01498 Sao Paulo, SP, Brazil. [Menanteau, Felipe] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Menanteau, Felipe] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Sehgal, Neelima] Dept Phys & Astron, Stony Brook, NY 11794 USA. [Sievers, J. L.] Univ KwaZulu Natal, Natl Inst Theoret Phys NITheP, ZA-4000 Durban, South Africa. [Sifon, Cristobal] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Swetz, Daniel] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Weiss, Axel] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lindner, RR (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. EM rlindner@astro.wisc.edu RI Lima, Marcos/E-8378-2010; Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Sievers, Jonathan/0000-0001-6903-5074; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sifon, Cristobal/0000-0002-8149-1352 FU U.S. National Science Foundation [AST-0955810, AST-0408698, AST-0965625, PHY-0855887, PHY-1214379, AST-0707731, PIRE-0507768, OISE-0530095]; National Aeronautics and Space Administration (NASA) [GO1-12008X, GO2-13156X]; NASA [NAS8-03060]; Programa de Astronomia de la Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI); CFI under the Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; FONDAP Center for Astrophysics [15010003]; BASAL CATA Center for Astrophysics and Associated Technologies; National Aeronautics and Space Administration (NASA) through JPL/Caltech; Herschel FX R.R.L. and A.J.B. acknowledge significant support for this work from the U.S. National Science Foundation through grant AST-0955810. J.P.H. acknowledges support from the National Aeronautics and Space Administration (NASA) through Chandra Awards numbered GO1-12008X and GO2-13156X issued to Rutgers University by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060, and through an award issued by JPL/Caltech in association with Herschel, which is a European Space Agency Cornerstone Mission with significant participation by NASA. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Programa de Astronomia de la Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). This work was supported by the U.S. National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, and PHY-0855887, PHY-1214379, AST-0707731, and PIRE-0507768 (award No. OISE-0530095). Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. Computations were performed on the GPC super-computer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund-Research Excellence, and the University of Toronto. We acknowledge support from the FONDAP Center for Astrophysics 15010003, BASAL CATA Center for Astrophysics and Associated Technologies. The authors thank the APEX staff for their help in carrying out the observations presented here, as well as Phil Edwards, Robin Wark, and Shane O'Sullivan for their assistance with the ATCA observations. We thank the anonymous referee for helpful feedback that has improved this manuscript. APEX is operated by the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. NR 89 TC 2 Z9 2 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 APR 20 PY 2015 VL 803 IS 2 AR 79 DI 10.1088/0004-637X/803/2/79 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG7YT UT WOS:000353524500031 ER PT J AU Naiman, JP Ramirez-Ruiz, E Debuhr, J Ma, CP AF Naiman, J. P. Ramirez-Ruiz, E. Debuhr, J. Ma, C. -P. TI THE ROLE OF NUCLEAR STAR CLUSTERS IN ENHANCING SUPERMASSIVE BLACK HOLE FEEDING RATES DURING GALAXY MERGERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: nuclei ID ACTIVE GALACTIC NUCLEI; MERGING DISC GALAXIES; BONDI-HOYLE ACCRETION; X-RAY; COSMOLOGICAL SIMULATIONS; SPACE-TELESCOPE; SPIRAL GALAXIES; GAS ACCRETION; STELLAR-SYSTEMS; DWARF GALAXIES AB During galaxy mergers the gas falls to the center, triggers star formation, and feeds the rapid growth of supermassive black holes (SMBHs). SMBHs respond to this fueling by supplying energy back to the ambient gas. Numerical studies suggest that this feedback is necessary to explain why the properties of SMBHs and the formation of bulges are closely related. This intimate link between the SMBH's mass and the large scale dynamics and luminosity of the host has proven to be a difficult issue to tackle with simulations due to the inability to resolve all the relevant length scales simultaneously. In this paper we simulate SMBH growth at high-resolution with FLASH, accounting for the gravitational focusing effects of nuclear star clusters (NSCs), which appear to be ubiquitous in galactic nuclei. In the simulations, the NSC core is resolved by a minimum cell size of about 0.001 pc or approximately 10(-3) of the cluster's radius. We discuss the conditions required for effective gas funneling to occur, which are mainly dominated by a relationship between NSC velocity dispersion and the local sound speed, and provide a sub-grid prescription for the augmentation of central SMBH accretion rates in the presence of NSCs. For the conditions expected to persist in the centers of merging galaxies, the resultant large central gas densities in NSCs should produce drastically enhanced embedded SMBH accretion rates-up to an order of magnitude increase can be achieved for gas properties resembling those in large-scale galaxy merger simulations. This will naturally result in faster black hole growth rates and higher luminosities than predicted by the commonly used Bondi-Hoyle-Lyttleton accretion formalism. C1 [Naiman, J. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ramirez-Ruiz, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Debuhr, J.] Indiana Univ, Ctr Res Extreme Scale Technol, Bloomington, IN 47404 USA. [Ma, C. -P.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Naiman, JP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU David and Lucile Packard Foundation; NSF [AST-0847563]; Simons Foundation; NASA [NNX11AI97G] FX We acknowledge helpful discussions with Doug Lin, Elena D'Onghia, Anil Seth, Morgan MacLeod and Lars Hernquist. We also thank the anonymous referee for constructive comments. Support was provided by the David and Lucile Packard Foundation and NSF grant AST-0847563, Simons Foundation and NASA grant NNX11AI97G. NR 71 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 APR 20 PY 2015 VL 803 IS 2 AR 81 DI 10.1088/0004-637X/803/2/81 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG7YT UT WOS:000353524500033 ER PT J AU Patnaude, DJ Lee, SH Slane, PO Badenes, C Heger, A Ellison, DC Nagataki, S AF Patnaude, Daniel J. Lee, Shiu-Hang Slane, Patrick O. Badenes, Carles Heger, Alexander Ellison, Donald C. Nagataki, Shigehiro TI ARE MODELS FOR CORE-COLLAPSE SUPERNOVA PROGENITORS CONSISTENT WITH THE PROPERTIES OF SUPERNOVA REMNANTS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: supernova remnants; stars: mass-loss; supernovae: general; X-rays: ISM ID X-RAY-EMISSION; DIFFUSIVE SHOCK ACCELERATION; MASSIVE STARS; IIN SUPERNOVAE; IA SUPERNOVA; CASSIOPEIA-A; NONEQUILIBRIUM IONIZATION; CIRCUMSTELLAR INTERACTION; SOLAR-METALLICITY; RX J1713.7-3946 AB The recent discovery that the Fe-K line luminosities and energy centroids observed in nearby supernova remnants are a strong discriminant of both progenitor type and circumstellar environment has implications for our understanding of supernova progenitor evolution. Using models for the chemical composition of core-collapse supernova (CCSN) ejecta, we model the dynamics and thermal X-ray emission from shocked ejecta and circumstellar material, modeled as an r(-2) wind, to ages of 3000 yr. We compare the X-ray spectra expected from these models to observations made with the Suzaku satellite. We also model the dynamics and X-ray emission from Type Ia progenitor models. We find a clear distinction in Fe-K line energy centroid between core-collapse and Type Ia models. The CCSN models predict higher Fe-K line centroid energies than the Type Ia models, in agreement with observations. We argue that the higher line centroids are a consequence of the increased densities found in the circumstellar environment created by the expansion of the slow-moving wind from the massive progenitors. C1 [Patnaude, Daniel J.; Slane, Patrick O.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Lee, Shiu-Hang] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [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. [Heger, Alexander] Monash Univ, Sch Math Sci, Monash Ctr Astrophys, Clayton, Vic 3800, Australia. [Ellison, Donald C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Nagataki, Shigehiro] RIKEN, Astrophys Big Bang Lab, Wako, Saitama 3510198, Japan. RP Patnaude, DJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. EM dpatnaude@cfa.harvard.edu; slee@astro.isas.jaxa.jp; pslane@cfa.harvard.edu; badenes@pitt.edu; alexander.heger@monash.edu; don_ellison@ncsu.edu; shigehiro.nagataki@riken.jp RI XRAY, SUZAKU/A-1808-2009; OI Badenes, Carles/0000-0003-3494-343X FU Smithsonian Institution's Competitive Grants for Science Program; NASA [NAS8-03060, NNX11AE03G]; Japan Society for the Promotion of Science [23340069, 24.02022, 25.03786, 25610056]; Australian Research Council [FT120100363]; [2503018] FX We thank R. Fesen and D. Milisavljevic for useful discussions during the preparation of this manuscript. Additionally, we thank the anonymous referee for several useful suggestions that we have incorporated into this paper. D.J.P. acknowledges support for this work through the Smithsonian Institution's Competitive Grants for Science Program. D.J.P. and P.O.S. also acknowledge support from NASA contract NAS8-03060. S.-H.L. acknowledges support from Grants-in-Aid for Foreign JSPS Fellow (No. 2503018). D.C.E. acknowledges support from NASA grant NNX11AE03G, and S.N. acknowledges support from the Japan Society for the Promotion of Science (Nos. 23340069, 24.02022, 25.03786, and 25610056). A.H. was supported by a Future Fellowship by the Australian Research Council (FT120100363). NR 67 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2015 VL 803 IS 2 AR 101 DI 10.1088/0004-637X/803/2/101 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG7YT UT WOS:000353524500052 ER PT J AU Polito, V Reeves, KK Del Zanna, G Golub, L Mason, HE AF Polito, V. Reeves, K. K. Del Zanna, G. Golub, L. Mason, H. E. TI JOINT HIGH TEMPERATURE OBSERVATION OF A SMALL C6.5 SOLAR FLARE WITH IRIS/EIS/AIA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: chromosphere; Sun: corona; Sun: flares; Sun: UV radiation; techniques: spectroscopic ID ULTRAVIOLET IMAGING SPECTROMETER; CORONAL DIAGNOSTIC SPECTROMETER; CHROMOSPHERIC EVAPORATION; MAGNETIC RECONNECTION; IMPULSIVE PHASE; ATOMIC DATABASE; EMISSION-LINES; ACTIVE-REGION; SDO AIA; HINODE AB We present the observation of a C6.5 class flare on 2014 February 3, obtained with the Interface Region Imaging Spectrograph (IRIS) and the EUV Imaging Spectrometer (EIS) on board HINODE. We follow the details of the impulsive phase with IRIS and the gradual decay phase with both IRIS and EIS. The IRIS Slit-Jaw Imager and Atmospheric Imaging Assembly (AIA) are used to precisely co-align the two sets of spectroscopic observations. Of particular interest is the Fe XXI 1354.08 angstrom spectral line, which is the highest temperature emission (similar to 10 MK) observed in the IRIS wavelength range. We show the evolution of the Fe XXI profiles during the impulsive phase of the flare at the same ribbon location with a 75 s temporal cadence. Totally blueshifted (similar to 82 km s(-1)) profiles are found at the very early phase of the flare and gradually decrease in about 6 minutes. This result is consistent with 1D model predictions during chromospheric evaporation in flares. The blueshifted components also exhibit large non-thermal broadening, which decreases simultaneously with the blueshifted velocity. After the evaporation first occurs, the Fe XXI intensity progressively moves from the footpoints to the top of the hot flare loops seen in the AIA 131 angstrom images, where the emission is observed to be at rest and thermal. Emission measure estimates from IRIS/EIS/AIA observations during the gradual phase show isothermal loop top structures cooling from about 13.5 to 12 MK with electron densities of the order of similar to 5-6 x 10(10) cm(-3). C1 [Polito, V.; Del Zanna, G.; Mason, H. E.] Univ Cambridge, CMS, DAMTP, Cambridge CB3 0WA, England. [Reeves, K. K.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. RP Polito, V (reprint author), Univ Cambridge, CMS, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England. FU Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract; Isaac Newton Studentship; Cambridge Trust; IRIS team at Harvard-Smithsonian Centre for Astrophysics; STFC; Lockheed-Martin [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). AIA data are courtesy of NASA/SDO and the respective science teams. CHIANTI is a collaborative project involving researchers at the universities of Cambridge (UK), George Mason, and Michigan (USA). V.P. ackowledge support from the Isaac Newton Studentship, the Cambridge Trust, and the IRIS team at Harvard-Smithsonian Centre for Astrophysics. H.E.M. and G.D.Z. acknowledge support from the STFC. L.G. and K.R. are supported by contract 8100002705 from Lockheed-Martin to SAO. NR 47 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 APR 20 PY 2015 VL 803 IS 2 AR 84 DI 10.1088/0004-637X/803/2/84 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG7YT UT WOS:000353524500036 ER PT J AU Quinn, SN White, TR Latham, DW Chaplin, WJ Handberg, R Huber, D Kipping, DM Payne, MJ Jiang, C Aguirre, VS Stello, D Sliski, DH Ciardi, DR Buchhave, LA Bedding, TR Davies, GR Hekker, S Kjeldsen, H Kuszlewicz, JS Everett, ME Howell, SB Basu, S Campante, TL Christensen-Dalsgaard, J Elsworth, YP Karoff, C Kawaler, SD Lund, MN Lundkvist, M Esquerdo, GA Calkins, ML Berlind, P AF Quinn, Samuel N. White, Timothy. R. Latham, David W. Chaplin, William J. Handberg, Rasmus Huber, Daniel Kipping, David M. Payne, Matthew J. Jiang, Chen Aguirre, Victor Silva Stello, Dennis Sliski, David H. Ciardi, David R. Buchhave, Lars A. Bedding, Timothy R. Davies, Guy R. Hekker, Saskia Kjeldsen, Hans Kuszlewicz, James S. Everett, Mark E. Howell, Steve B. Basu, Sarbani Campante, Tiago L. Christensen-Dalsgaard, Jorgen Elsworth, Yvonne P. Karoff, Christoffer Kawaler, Steven D. Lund, Mikkel N. Lundkvist, Mia Esquerdo, Gilbert A. Calkins, Michael L. Berlind, Perry TI KEPLER-432: A RED GIANT INTERACTING WITH ONE OF ITS TWO LONG-PERIOD GIANT PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE asteroseismology; planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: gaseous planets; planet-star interactions; stars: individual (Kepler-432) ID STELLAR EVOLUTION CODE; SOLAR-TYPE STARS; SPIN-ORBIT MISALIGNMENT; SUN-LIKE STAR; A-TYPE STARS; HOT-JUPITER; ECCENTRIC ORBIT; TRANSITING PLANETS; ASTEROSEISMIC ANALYSIS; BLEND SCENARIOS AB We report the discovery of Kepler-432b, a giant planet ( M-b = 5.41(-0.18)(+0.32) M-Jup R-b = 1.145(-0.039)(+0.036),R-Jup) transiting an evolved star (M-* = 1.32(-0.07)(+0.10) M-circle dot R-* 4.06(-0.08)(+0.12) R-circle dot) with an orbital period of Pb = 52.501129(-0.000053)(+0.000067) days. Radial velocities (RVs) reveal that Kepler-432b orbits its parent star with an eccentricity of e = 0.5134(-0.0089)(+0.0098) , which we also measure independently with asterodensity profiling (AP; e = 0.507(-0.114)(+0.039)), thereby confirming the validity of AP on this particular evolved star. The well-determined planetary properties and unusually large mass also make this planet an important benchmark for theoretical models of super-Jupiter formation. Long-term RV monitoring detected the presence of a non-transiting outer planet (Kepler-432c; = M-c sin i(c) = 2.43(-0.24)(+0.22) M-Jup, P-c = 406.2(-2.5)(+3.9) days), and adaptive optics imaging revealed a nearby (0.'' 87), faint companion (Kepler-432B) that is a physically bound M dwarf. The host star exhibits high signal-to-noise ratio asteroseismic oscillations, which enable precise measurements of the stellar mass, radius, and age. Analysis of the rotational splitting of the oscillation modes additionally reveals the stellar spin axis to be nearly edge-on, which suggests that the stellar spin is likely well aligned with the orbit of the transiting planet. Despite its long period, the obliquity of the 52.5 day orbit may have been shaped by star-planet interaction in a manner similar to hot Jupiter systems, and we present observational and theoretical evidence to support this scenario. Finally, as a short-period outlier among giant planets orbiting giant stars, study of Kepler-432b may help explain the distribution of massive planets orbiting giant stars interior to 1 AU. C1 [Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [White, Timothy. R.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Latham, David W.; Kipping, David M.; Payne, Matthew J.; Sliski, David H.; Buchhave, Lars A.; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chaplin, William J.; Handberg, Rasmus; Davies, Guy R.; Kuszlewicz, James S.; Campante, Tiago L.; Elsworth, Yvonne P.; Lund, Mikkel N.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.; Handberg, Rasmus; Huber, Daniel; Jiang, Chen; Aguirre, Victor Silva; Stello, Dennis; Bedding, Timothy R.; Davies, Guy R.; Hekker, Saskia; Kjeldsen, Hans; Kuszlewicz, James S.; Campante, Tiago L.; Christensen-Dalsgaard, Jorgen; Elsworth, Yvonne P.; Karoff, Christoffer; Lund, Mikkel N.; Lundkvist, Mia] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Huber, Daniel; Stello, Dennis; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Sliski, David H.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasdena, CA 91125 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Hekker, Saskia] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Karoff, Christoffer] Aarhus Univ, Dept Geosci, DK-8000 Aarhus C, Denmark. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kipping, David M.] NASA, Washington, DC USA. [Quinn, Samuel N.] NSF, Arlington, VA USA. RP Quinn, SN (reprint author), Georgia State Univ, Dept Phys & Astron, 25 Pk Pl Suite 605, Atlanta, GA 30303 USA. OI Davies, Guy/0000-0002-4290-7351; Lundkvist, Mia Sloth/0000-0002-8661-2571; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Karoff, Christoffer/0000-0003-2009-7965; Bedding, Tim/0000-0001-5222-4661; Handberg, Rasmus/0000-0001-8725-4502; Lund, Mikkel Norup/0000-0001-9214-5642 FU NSF Graduate Research Fellowship [DGE-1051030]; NASA's Kepler mission [NNX11AB99A]; Smithsonian Astrophysical Observatory; Australian Research Council [DEI40101364]; NASA [NNX14AB92G]; NASA Origins of Solar Systems Program [NNX13A124G]; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) - European Research Council [267864]; European Research Council under the European Community's Seventh Framework Programme [338251]; Robert Martin Ayers Sciences Fund; National Aeronautics and Space Administration; National Science Foundation; University of Massachusetts; Infrared Processing and Analysis Center/California Institute of Technology FX We thank Russel White and an anonymous referee for valuable discussion and feedback. S.N.Q. is supported by the NSF Graduate Research Fellowship, Grant DGE-1051030. D.W.L. acknowledges partial support from NASA's Kepler mission under Cooperative Agreement NNX11AB99A with the Smithsonian Astrophysical Observatory. D.H. acknowledges support by the Australian Research Council's Discovery Projects funding scheme (project number DEI40101364) and support by NASA under Grant NNX14AB92G issued through the Kepler Participating Scientist Program. M.J.P. gratefully acknowledges the NASA Origins of Solar Systems Program grant NNX13A124G. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no.: 267864). The research leading to the presented results has also received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no 338251 (StellarAges). 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 also made use of the APASS database, located at the AAVSO Web site. Funding for APASS has been provided by the Robert Martin Ayers Sciences Fund. NR 139 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 APR 20 PY 2015 VL 803 IS 2 AR 49 DI 10.1088/0004-637X/803/2/49 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG7YT UT WOS:000353524500001 ER PT J AU Gilbert, GS Briggs, HM Magarey, R AF Gilbert, Gregory S. Briggs, Heather M. Magarey, Roger TI The Impact of Plant Enemies Shows a Phylogenetic Signal SO PLOS ONE LA English DT Article ID TROPICAL FORESTS; HOST PHYLOGENY; TRAITS; TREE; HERBIVORES; TRANSMISSION; SPECIFICITY; SIMILARITY; COMPONENTS; RESISTANCE AB The host ranges of plant pathogens and herbivores are phylogenetically constrained, so that closely related plant species are more likely to share pests and pathogens. Here we conducted a reanalysis of data from published experimental studies to test whether the severity of host-enemy interactions follows a similar phylogenetic signal. The impact of herbivores and pathogens on their host plants declined steadily with phylogenetic distance from the most severely affected focal hosts. The steepness of this phylogenetic signal was similar to that previously measured for binary-response host ranges. Enemy behavior and development showed similar, but weaker phylogenetic signal, with oviposition and growth rates declining with evolutionary distance from optimal hosts. Phylogenetic distance is an informative surrogate for estimating the likely impacts of a pest or pathogen on potential plant hosts, and may be particularly useful in early assessing risk from emergent plant pests, where critical decisions must be made with incomplete host records. C1 [Gilbert, Gregory S.; Briggs, Heather M.] Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. [Gilbert, Gregory S.] Smithsonian Trop Res Inst, Balboa, Panama. [Magarey, Roger] N Carolina State Univ, Ctr Integrated Pest Management, Raleigh, NC 27695 USA. RP Gilbert, GS (reprint author), Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA. EM ggilbert@ucsc.edu FU NSF [DEB-0842059, DEB-1136626]; University of California Santa Cruz FX Funding for this work was provided by Cooperative Agreement between G. Gilbert and USDA-APHIS-PPQ-CPHST PERAL funded from Section 10201 of the Farm Bill, and by NSF grants DEB-0842059 and DEB-1136626 to G. Gilbert. Additional support was provided by the University of California Santa Cruz. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 46 TC 9 Z9 9 U1 2 U2 25 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 APR 20 PY 2015 VL 10 IS 4 AR UNSP e0123758 DI 10.1371/journal.pone.0123758 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG3XA UT WOS:000353211700054 PM 25893581 ER PT J AU Kelley, NP Pyenson, ND AF Kelley, Neil P. Pyenson, Nicholas D. TI Evolutionary innovation and ecology in marine tetrapods from the Triassic to the Anthropocene SO SCIENCE LA English DT Review ID SEA-SNAKES ELAPIDAE; CLIMATE-CHANGE; PACIFIC-OCEAN; AMBLYRHYNCHUS-CRISTATUS; CONVERGENT EVOLUTION; ENVIRONMENTAL-CHANGE; FOSSIL CALIBRATIONS; SPECIES-DIVERSITY; MIOCENE EPOCH; LIFE-HISTORY AB Many top consumers in today's oceans are marine tetrapods, a collection of lineages independently derived from terrestrial ancestors. The fossil record illuminates their transitions from land to sea, yet these initial invasions account for a small proportion of their evolutionary history. We review the history of marine invasions that drove major changes in anatomy, physiology, and ecology over more than 250 million years. Many innovations evolved convergently in multiple clades, whereas others are unique to individual lineages. The evolutionary arcs of these ecologically important clades are framed against the backdrop of mass extinctions and regime shifts in ocean ecosystems. Past and present human disruptions to marine tetrapods, with cascading impacts on marine ecosystems, underscore the need to link macroecology with evolutionary change. C1 [Kelley, Neil P.; Pyenson, Nicholas D.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Kelley, Neil P.] Vanderbilt Univ, Dept Earth & Environm Sci, Nashville, TN 37240 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Mammal & Paleontol, Seattle, WA 98195 USA. RP Kelley, NP (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. EM kelleynp@si.edu FU Smithsonian Institution Peter Buck Postdoctoral Fellowship; Smithsonian Institution National Museum of Natural History Small Grant Award; Remington Kellogg Fund; Basis Foundation FX We thank D. Erwin, J. Jackson, M. Carrano, J. Goldbogen, J. Parham, J. Velez-Juarbe, and J. Oster for helpful comments on previous versions of this paper, and three anonymous reviewers for helpful suggestions. D. Johnston provided the penguin photograph for Fig. 2. Supported by a Smithsonian Institution Peter Buck Postdoctoral Fellowship (N.P.K.), a Smithsonian Institution National Museum of Natural History Small Grant Award and the Remington Kellogg Fund (N.D.P.), and the Basis Foundation (N.D.P. and N.P.K.). NR 142 TC 9 Z9 9 U1 9 U2 29 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 APR 17 PY 2015 VL 348 IS 6232 AR aaa3716 DI 10.1126/science.aaa3716 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG0YC UT WOS:000352999000033 PM 25883362 ER PT J AU Kaminski, T Menten, KM Tylenda, R Hajduk, M Patel, NA Kraus, A AF Kaminski, Tomasz Menten, Karl M. Tylenda, Romuald Hajduk, Marcin Patel, Nimesh A. Kraus, Alexander TI Nuclear ashes and outflow in the eruptive star Nova Vul 1670 SO NATURE LA English DT Article ID CK-VUL; CLASSICAL NOVAE; SUBMILLIMETER; NEBULA; GRAINS; OLDEST; APEX; NUCLEOSYNTHESIS; SPECTROSCOPY; MILLIMETER AB CK Vulpeculae was observed in outburst in 1670-1672 (ref. 1), but no counterpart was seen until 1982, when a bipolar nebula was found at its location(1-3). Historically, CK Vul has been considered to be a nova (Nova Vul 1670), but its similarity to 'red transients', which are more luminous than classical novae and thought to be the results of stellar collisions(4), has re-opened the question of CK Vul's status5'6. Red transients cool to resemble late M-type stars, surrounded by circumstellar material rich in molecules and dust(7-9). No stellar source has been seen in CK Vul, though a radio continuum source was identified at the expansion centre of the nebula'. Here we report that CK Vul is surrounded by chemically rich molecular gas in the form of an outflow, as well as dust. The gas has peculiar isotopic ratios, revealing that CK Vul's composition was strongly enhanced by the nuclear ashes of hydrogen burning. The chemical composition cannot be reconciled with a nova or indeed any other known explosion. In addition, the mass of the surrounding gas is too large for a nova, though the conversion from observations of CO to a total mass is uncertain. We conclude that CK Vul is best explained as the remnant of a merger of two stars. C1 [Kaminski, Tomasz] European So Observ, Santiago, Chile. [Kaminski, Tomasz; Menten, Karl M.; Kraus, Alexander] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Tylenda, Romuald; Hajduk, Marcin] N Copernicus Astron Ctr, Dept Astrophys, PL-87100 Torun, Poland. [Patel, Nimesh A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kaminski, T (reprint author), European So Observ, Alonso de Cordova 3107, Santiago, Chile. EM tkaminsk@eso.org RI Hajduk, Marcin/C-9693-2014 NR 49 TC 12 Z9 13 U1 2 U2 7 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD APR 16 PY 2015 VL 520 IS 7547 BP 322 EP + DI 10.1038/nature14257 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG0RI UT WOS:000352974200032 PM 25799986 ER PT J AU Hayhurst, SE Engel, JD Walsh, T Gordon, S Murray, S Boedeker, N AF Hayhurst, Susan E. Engel, Jason D. Walsh, Timothy Gordon, Sebastian Murray, Suzan Boedeker, Nancy TI What Is Your Diagnosis? SO JAVMA-JOURNAL OF THE AMERICAN VETERINARY MEDICAL ASSOCIATION LA English DT Editorial Material C1 [Hayhurst, Susan E.; Engel, Jason D.; Walsh, Timothy; Gordon, Sebastian; Murray, Suzan; Boedeker, Nancy] Smithsonian Natl Zool Pk, Smithsonian Conservat Biol Inst, Dept Wildlife Hlth Sci, Washington, DC 20008 USA. RP Hayhurst, SE (reprint author), Mann Mem Vet Clin, POB 919, Kennebunk, ME 04043 USA. EM susan.hayhurst@gmail.com NR 2 TC 0 Z9 0 U1 0 U2 0 PU AMER VETERINARY MEDICAL ASSOC PI SCHAUMBURG PA 1931 N MEACHAM RD SUITE 100, SCHAUMBURG, IL 60173-4360 USA SN 0003-1488 EI 1943-569X J9 JAVMA-J AM VET MED A JI JAVMA-J. Am. Vet. Med. Assoc. PD APR 15 PY 2015 VL 246 IS 8 BP 839 EP 841 PG 3 WC Veterinary Sciences SC Veterinary Sciences GA CK0XW UT WOS:000355930000020 PM 25835164 ER PT J AU Cabi, E Soreng, RJ Cingay, B Karabacak, E AF Cabi, Evren Soreng, Robert John Cingay, Burcin Karabacak, Ersin TI A new species of Bellardiochloa, B-doganiana (Poaceae), from the Taurus Mountains of Turkey SO PHYTOTAXA LA English DT Article DE Grasses; Poeae; Poinae; Poa; Festuca AB Bellardiochloa doganiana, a new species from the Taurus Mountains of Turkey, is described and illustrated. It differs from the other four species of the genus in its basal tuft of short, stiff, terete, arched, pungent-tipped basal leaf-blades, conical panicles with numerous panicle branches and mostly 1 or 2 spikelets per branch, and pedicels as long as or longer than the spikelets. C1 [Cabi, Evren] Namik Kemal Univ, Fac Arts & Sci, Dept Biol, Tekirdag, Turkey. [Soreng, Robert John] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Cingay, Burcin] Nezahat Gokyigit Bot Garden, Istanbul, Turkey. [Karabacak, Ersin] Canakkale Onsekiz Mart Univ, Fac Arts & Sci, Dept Biol, Canakkale, Turkey. RP Cabi, E (reprint author), Namik Kemal Univ, Fac Arts & Sci, Dept Biol, Tekirdag, Turkey. EM ecabi@nku.edu.tr FU TUBITAK-KBAG [212T113]; TUBITAK-BIDEB FX Our gratitude is extended to Musa Dogan for his contributions to botanical taxonomy of Turkey and support for the Poa project; To Yildirim Akman for his introduction of R.J. Soreng to the flora of central Turkey and providing assistance in field work in conjunction with Osman Ketenoglu, Latif Kurt,Kerim Guney, and Umit Bingol for guidance and assistance in field work to R.J. Soreng in 1991 and 1993. To Lynn Gillespie for joint field work in Turkey in 2011. To Tugrul Koruklu, Ayse Mine Gencler Ozkan, Osman Tugay for access to the ANK, AEF, KNYA university herbaria, respectively in 2014. To TUBITAK-KBAG for support of Grant no. 212T113 and TUBITAK-BIDEB for support that made R.J. Soreng's visit possible to Namik Kemal University. NR 20 TC 0 Z9 0 U1 0 U2 2 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 APR 15 PY 2015 VL 205 IS 2 BP 123 EP 128 DI 10.11646/phytotaxa.205.2.6 PG 6 WC Plant Sciences SC Plant Sciences GA CG2RJ UT WOS:000353122000006 ER PT J AU Bulbert, MW Page, RA Bernal, XE AF Bulbert, Matthew W. Page, Rachel A. Bernal, Ximena E. TI Danger Comes from All Fronts: Predator-Dependent Escape Tactics of Tungara Frogs SO PLOS ONE LA English DT Article ID FLIGHT INITIATION DISTANCE; BAT PREDATION; ANTIPREDATOR BEHAVIOR; ECHOLOCATING BATS; TURNING BEHAVIOR; EVASIVE BEHAVIOR; PREY; STRATEGIES; BIRDS; TOADS AB The escape response of an organism is generally its last line of defense against a predator. Because the effectiveness of an escape varies with the approach behaviour of the predator, it should be advantageous for prey to alter their escape trajectories depending on the mode of predator attack. To test this hypothesis we examined the escape responses of a single prey species, the ground-dwelling tungara frog (Engystomops pustulosus), to disparate predators approaching from different spatial planes: a terrestrial predator (snake) and an aerial predator (bat). Tungara frogs showed consistently distinct escape responses when attacked by terrestrial versus aerial predators. The frogs fled away from the snake models (Median: 131 degrees). In stark contrast, the frogs moved toward the bat models (Median: 27 degrees); effectively undercutting the bat's flight path. Our results reveal that prey escape trajectories reflect the specificity of their predators' attacks. This study emphasizes the flexibility of strategies performed by prey to outcompete predators with diverse modes of attack. C1 [Bulbert, Matthew W.] Macquarie Univ, Dept Biol, Behav Ecol Grp, N Ryde, NSW 2109, Australia. [Bulbert, Matthew W.; Page, Rachel A.; Bernal, Ximena E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. RP Bulbert, MW (reprint author), Macquarie Univ, Dept Biol, Behav Ecol Grp, N Ryde, NSW 2109, Australia. EM matthew.bulbert@mq.edu.au FU Texas Tech University FX This work was partially supported by Texas Tech University funding to XEB. This research received no additional funding from any public, commercial or not-for-profit sectors. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 62 TC 3 Z9 3 U1 4 U2 21 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 15 PY 2015 VL 10 IS 4 AR e0120546 DI 10.1371/journal.pone.0120546 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG1EL UT WOS:000353015800011 PM 25874798 ER PT J AU Rinehart, LF Lucas, SG Tanner, L Nelson, WJ Elrick, SD Chaney, DS DiMichele, WA AF Rinehart, Larry F. Lucas, Spencer G. Tanner, Lawrence Nelson, W. John Elrick, Scott D. Chaney, Dan S. DiMichele, William A. TI Plant architecture and spatial structure of an early Permian woodland buried by flood waters, Sangre de Cristo Formation, New Mexico SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Permian; T-o assemblage; Fossil forest; Self thinning; Dicranophyllum ID TERTIARY METASEQUOIA FORESTS; GENERAL QUANTITATIVE THEORY; IN-SITU; PALEOZOIC CONIFERS; FOSSIL FORESTS; INNER-MONGOLIA; NEW-BRUNSWICK; ABO FORMATION; VOLCANIC ASH; USA AB Natural molds of 165 stems were found in life position in a 1 m-thick sandstone bed, lower Permian (Wolfcampian), Sangre de Cristo Formation, northern New Mexico. The sandstone represents a single flood event of a river sourced in the Ancestral Rocky Mountains. Most of the flood-buried plants survived and resumed growth. The stem affinities are uncertain, but they resemble coniferophytic gymnosperms, possibly dicranophylls. Stem diameters (N = 135) vary from 1 to 21 cm, with three strongly overlapping size classes. Modern forest studies predict a monotonically decreasing number (inverse square law) of individuals per size class as diameter increases. This is not seen for fossil stems <= 6 cm diameter, reflecting biases against preservation, exposure, and observation of smaller individuals. Stems >= 6 cm diameter obey the predicted inverse square law of diameter distribution. Height estimates calculated from diameter-to-height relationships of modern gymnosperms yielded heights varying from similar to 0.9 m to >8 m, mean of similar to 3 m. Mean stand density is approximately 2 stems/m(2) (20,000 stems/hectare) for all stems >1 cm diameter. For sterns >7.5 cm or >10 cm diameter, density is approximately 0.24 stems/m(2) (2400 stems/hectare) and 0.14 stems/m(2) (1400 stems/hectare). Stem spatial distribution is random (Poisson). Mean all-stem nearest-neighbor distance (NND) averages 36 cm. Mean NND between stems >7.5 cm and >10 cm diameter is approximately 1.02 m and 136 m. NND increases in approximate isometry with stem diameter, indicating conformation to the same spatial packing rules found in extant forests and other fossil forests of varying ages. Nearest-neighbor distance distribution passes statistical testing for normality, but with positive skew, as often seen in extant NND distributions. The size-frequency distribution of the stems is similar to those of Jurassic, early Tertiary, and extant woodlands; the early Permian woodland distribution line has the same slope, but differs in that the overall size range increases over time (Cope's rule). The early Permian woodland is self-thinning; its volume versus density relationship shows a self-thinning exponent between -1.25 and -1.5, within the range seen in some extant plant stands (-1.21 to -1.7). Published by Elsevier B.V. C1 [Rinehart, Larry F.; Lucas, Spencer G.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [Tanner, Lawrence] Le Moyne Coll, Dept Biol, Syracuse, NY 13214 USA. [Nelson, W. John; Elrick, Scott D.] Illinois State Geol Survey, Champaign, IL 61820 USA. [Chaney, Dan S.; DiMichele, William A.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP DiMichele, WA (reprint author), NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. EM dimichel@si.edu NR 83 TC 1 Z9 1 U1 4 U2 17 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 APR 15 PY 2015 VL 424 BP 91 EP 110 DI 10.1016/j.palaeo.2015.02.018 PG 20 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA CF1TQ UT WOS:000352331200008 ER PT J AU Alvarez-Filip, L Paddack, MJ Ben Collen Robertson, DR Cote, IM AF Alvarez-Filip, Lorenzo Paddack, Michelle J. Ben Collen Robertson, D. Ross Cote, Isabelle M. TI Simplification of Caribbean Reef-Fish Assemblages over Decades of Coral Reef Degradation SO PLOS ONE LA English DT Article ID REGION-WIDE DECLINES; LIVING PLANET INDEX; MONITORING CHANGE; SPARISOMA-VIRIDE; MARINE RESERVES; ADULT ABUNDANCE; CLIMATE-CHANGE; HABITAT LOSS; BIODIVERSITY; POPULATIONS AB Caribbean coral reefs are becoming structurally simpler, largely due to human impacts. The consequences of this trend for reef-associated communities are currently unclear, but expected to be profound. Here, we assess whether changes in fish assemblages have been non-random over several decades of declining reef structure. More specifically, we predicted that species that depend exclusively on coral reef habitat (i.e., habitat specialists) should be at a disadvantage compared to those that use a broader array of habitats (i.e., habitat generalists). Analysing 3727 abundance trends of 161 Caribbean reef-fishes, surveyed between 1980 and 2006, we found that the trends of habitat-generalists and habitat-specialists differed markedly. The abundance of specialists started to decline in the mid-1980s, reaching a low of similar to 60% of the 1980 baseline by the mid-1990s. Both the average and the variation in abundance of specialists have increased since the early 2000s, although the average is still well below the baseline level of 1980. This modest recovery occurred despite no clear evidence of a regional recovery in coral reef habitat quality in the Caribbean during the 2000s. In contrast, the abundance of generalist fishes remained relatively stable over the same three decades. Few specialist species are fished, thus their population declines are most likely linked to habitat degradation. These results mirror the observed trends of replacement of specialists by generalists, observed in terrestrial taxa across the globe. A significant challenge that arises from our findings is now to investigate if, and how, such community-level changes in fish populations affect ecosystem function. C1 [Alvarez-Filip, Lorenzo] Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Unidad Acad Sistemas Arrecifales, Puerto Morelos, Quintana Roo, Mexico. [Alvarez-Filip, Lorenzo; Paddack, Michelle J.; Cote, Isabelle M.] Simon Fraser Univ, Dept Biol Sci, Burnaby, BC V5A 1S6, Canada. [Paddack, Michelle J.] Santa Barbara City Coll, Dept Biol, Santa Barbara, CA 93109 USA. [Ben Collen] UCL, Ctr Biodivers & Environm Res, London WC1E 6BT, England. [Robertson, D. Ross] Smithsonian Trop Res Inst, Balboa, Panama. RP Alvarez-Filip, L (reprint author), Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Unidad Acad Sistemas Arrecifales, Puerto Morelos, Quintana Roo, Mexico. EM lorenzo@cmarl.unam.mx.com RI Collen, Ben/F-2543-2016; Alvarez-Filip, Lorenzo/C-9552-2011 OI Collen, Ben/0000-0003-2564-4243; Alvarez-Filip, Lorenzo/0000-0002-5726-7238 FU UK's Natural Environment Resource Council [NE/C004442/1]; Mexican Council of Science and Technology (CONACYT) [160230]; Natural Sciences and Engineering Council of Canada (NSERC); Rufford Foundation; NSERC; Smithsonian Tropical Research Institute FX Compilation of the original database by MJP was funded by the UK's Natural Environment Resource Council, NE/C004442/1. LA-F was supported by the Mexican Council of Science and Technology (CONACYT; 160230), and by the Natural Sciences and Engineering Council of Canada (NSERC). BC is supported by the Rufford Foundation, IMC is funded by a Discovery Grant from NSERC, and DRR is supported by 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 54 TC 4 Z9 5 U1 2 U2 42 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 APR 14 PY 2015 VL 10 IS 4 AR UNSP e0126004 DI 10.1371/journal.pone.0126004 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CG1EB UT WOS:000353014700078 PM 25875218 ER PT J AU Ho, IT Kudritzki, RP Kewley, LJ Zahid, HJ Dopita, MA Bresolin, F Rupke, DSN AF Ho, I-Ting Kudritzki, Rolf-Peter Kewley, Lisa J. Zahid, H. Jabran Dopita, Michael A. Bresolin, Fabio Rupke, David S. N. TI Metallicity gradients in local field star-forming galaxies: insights on inflows, outflows, and the coevolution of gas, stars and metals SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: formation; galaxies: ISM; galaxies: spiral ID DIGITAL SKY SURVEY; STELLAR POPULATION SYNTHESIS; H-II REGIONS; POTSDAM MULTIAPERTURE SPECTROPHOTOMETER; ULTRALUMINOUS INFRARED GALAXIES; GALACTIC CHEMICAL EVOLUTION; INITIAL MASS FUNCTION; WARM IONIZED MEDIUM; SPIRAL GALAXIES; ABUNDANCE GRADIENTS AB We present metallicity gradients in 49 local field star-forming galaxies. We derive gas-phase oxygen abundances using two widely adopted metallicity calibrations based on the [O-III]/H beta, [N-II]/H alpha, and [N-II]/[O-II] line ratios. The two derived metallicity gradients are usually in good agreement within +/- 0.14 dexR(25)(-1) (R-25 is the B-band iso-photoal radius), but the metallicity gradients can differ significantly when the ionization parameters change systematically with radius. We investigate the metallicity gradients as a function of stellar mass (8 < log (M-*/M-circle dot) < 11) and absolute B-band luminosity (-16 > M-B > -22). When the metallicity gradients are expressed in dex kpc(-1), we show that galaxies with lower mass and luminosity, on average, have steeper metallicity gradients. When the metallicity gradients are expressed in dexR(25)(-1), we find no correlation between the metallicity gradients, and stellar mass and luminosity. We provide a local benchmark metallicity gradient of field star-forming galaxies useful for comparison with studies at high redshifts. We investigate the origin of the local benchmark gradient using simple chemical evolution models and observed gas and stellar surface density profiles in nearby field spiral galaxies. Our models suggest that the local benchmark gradient is a direct result of the coevolution of gas and stellar disc under virtually closed-box chemical evolution when the stellar-to-gas mass ratio becomes high (>> 0.3). These models imply low current mass accretion rates (less than or similar to 0.3 x SFR), and low-mass outflow rates (less than or similar to 3 x SFR) in local field star-forming galaxies. C1 [Ho, I-Ting; Kudritzki, Rolf-Peter; Kewley, Lisa J.; Bresolin, Fabio] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kudritzki, Rolf-Peter] Univ Observ Munich, D-81679 Munich, Germany. [Kewley, Lisa J.; Dopita, Michael A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Zahid, H. Jabran] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dopita, Michael A.] King Abdulaziz Univ, Dept Astron, Jeddah 21413, Saudi Arabia. [Rupke, David S. N.] Rhodes Coll, Dept Phys, Memphis, TN 38112 USA. RP Ho, IT (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM itho@ifa.hawaii.edu RI Dopita, Michael/P-5413-2014 OI Dopita, Michael/0000-0003-0922-4986 FU Australian Research Council (ARC) [DP130103925]; King Abdulaziz University under HiCi programme; National Science Foundation [AST-1008798]; Time Assignment Committee at the Research School of Astronomy and Astrophysics of the Australian National University FX We thank the anonymous referee for constructive comments and suggestions. MAD and LJK acknowledge the support of the Australian Research Council (ARC) through Discovery project DP130103925. MAD also acknowledges financial support from King Abdulaziz University under the HiCi programme. RPK and FB were supported by the National Science Foundation under grant AST-1008798. We thank support from the Time Assignment Committee at the Research School of Astronomy and Astrophysics of the Australian National University. NR 160 TC 28 Z9 28 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 APR 11 PY 2015 VL 448 IS 3 BP 2030 EP 2054 DI 10.1093/mnras/stv067 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0PQ UT WOS:000351507000005 ER PT J AU Liu, J Mohr, J Saro, A Aird, KA Ashby, MLN Bautz, M Bayliss, M Benson, BA Bleem, LE Bocquet, S Brodwin, M Carlstrom, JE Chang, CL Chiu, I Cho, HM Clocchiatti, A Crawford, TM Crites, AT de Haan, T Desai, S Dietrich, JP Dobbs, MA Foley, RJ Gangkofner, D George, EM Gladders, MD Gonzalez, AH Halverson, NW Hennig, C Hlavacek-Larrondo, J Holder, GP Holzapfel, WL Hrubes, JD Jones, C Keisler, R Lee, AT Leitch, EM Lueker, M Luong-Van, D McDonald, M McMahon, JJ Meyer, SS Mocanu, L Murray, SS Padin, S Pryke, C Reichardt, CL Rest, A Ruel, J Ruhl, JE Saliwanchik, BR Sayre, JT Schaffer, KK Shirokoff, E Spieler, HG Stalder, B Staniszewski, Z Stark, AA Story, K Suhada, R Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Liu, J. Mohr, J. Saro, A. Aird, K. A. Ashby, M. L. N. Bautz, M. Bayliss, M. Benson, B. A. Bleem, L. E. Bocquet, S. Brodwin, M. Carlstrom, J. E. Chang, C. L. Chiu, I. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. de Haan, T. Desai, S. Dietrich, J. P. Dobbs, M. A. Foley, R. J. Gangkofner, D. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Hennig, C. Hlavacek-Larrondo, J. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Jones, C. Keisler, R. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McDonald, M. McMahon, J. J. Meyer, S. S. Mocanu, L. Murray, S. S. Padin, S. Pryke, C. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Saliwanchik, B. R. Sayre, J. T. Schaffer, K. K. Shirokoff, E. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Story, K. Suhada, R. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI Analysis of Sunyaev-Zel'dovich effect mass-observable relations using South Pole Telescope observations of an X-ray selected sample of low-mass galaxy clusters and groups SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium; cosmology: observations ID RADIO IMAGING SURVEY; 720 SQUARE DEGREES; SPT-SZ SURVEY; SCALING RELATIONS; COSMOLOGICAL CONSTRAINTS; PRECISION COSMOLOGY; INTRACLUSTER MEDIUM; OBSERVED GROWTH; HALO MASS; CATALOG AB We use microwave observations from the South Pole Telescope (SPT) to examine the Sunyaev-Zel'dovich effect (SZE) signatures of a sample of 46 X-ray selected groups and clusters drawn from similar to 6 deg(2) of the XMM-Newton Blanco Cosmology Survey. These systems extend to redshift z = 1.02 and probe the SZE signal to the lowest X-ray luminosities (>= 10(42) erg s(-1)) yet; these sample characteristics make this analysis complementary to previous studies. We develop an analysis tool, using X-ray luminosity as a mass proxy, to extract selection-bias-corrected constraints on the SZE significance and Y-500 mass relations. The former is in good agreement with an extrapolation of the relation obtained from high-mass clusters. However, the latter, at low masses, while in good agreement with the extrapolation from the high-mass SPT clusters, is in tension at 2.8 sigma with the Planck constraints, indicating the low-mass systems exhibit lower SZE signatures in the SPT data. We also present an analysis of potential sources of contamination. For the radio galaxy point source population, we find 18 of our systems have 843 MHz Sydney University Molonglo Sky Survey sources within 2 arcmin of the X-ray centre, and three of these are also detected at significance >4 by SPT. Of these three, two are associated with the group brightest cluster galaxies, and the third is likely an unassociated quasar candidate. We examine the impact of these point sources on our SZE scaling relation analyses and find no evidence of biases. We also examine the impact of dusty galaxies using constraints from the 220 GHz data. The stacked sample provides 2.8 sigma significant evidence of dusty galaxy flux, which would correspond to an average underestimate of the SPT Y-500 signal that is (17 +/- 9) per cent in this sample of low-mass systems. Finally, we explore the impact of future data from SPTpol and XMM-XXL, showing that it will lead to a factor of 4 to 5 tighter constraints on these SZE mass-observable relations. C1 [Liu, J.; Mohr, J.; Saro, A.; Bocquet, S.; Chiu, I.; Desai, S.; Dietrich, J. P.; Gangkofner, D.; Hennig, C.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Liu, J.; Mohr, J.; Saro, A.; Bocquet, S.; Chiu, I.; Clocchiatti, A.; Desai, S.; Dietrich, J. P.; Gangkofner, D.; Hennig, C.; Rest, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Ashby, M. L. N.; Bayliss, M.; Foley, R. J.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bayliss, M.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, 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.; Meyer, S. S.; Mocanu, L.; Padin, S.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; 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. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; 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. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Crites, A. T.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.; Williamson, R.] CALTECH, Dept Astron, 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.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Hlavacek-Larrondo, J.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [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 Liu, J (reprint author), Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany. EM jiayiliu@usm.uni-muenchen.de RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; CRAWFORD, THOMAS/0000-0001-9000-5013; Dietrich, Jorg/0000-0002-8134-9591; Stern, Corvin/0000-0003-4406-6127; Stark, Antony/0000-0002-2718-9996 FU DFG [TR33]; Cluster of Excellence 'Origin and Structure of the Universe'; National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; US Department of Energy; NSF [AST-1009012, DGE-1144152, AST-1009649, MRI-0723073]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs programme; Canadian Institute for Advanced Research FX We acknowledge the support of the DFG through TR33 'The Dark Universe' and the Cluster of Excellence 'Origin and Structure of the Universe'. Some calculations have been carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP). The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947. This work is also supported by the US Department of Energy. Galaxy cluster research at Harvard is supported by NSF grants AST-1009012 and DGE-1144152. 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 programme, and the Canadian Institute for Advanced Research. NR 61 TC 5 Z9 5 U1 1 U2 12 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 APR 11 PY 2015 VL 448 IS 3 BP 2085 EP 2099 DI 10.1093/mnras/stv080 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0PQ UT WOS:000351507000009 ER PT J AU de Gasperin, F Ogrean, GA van Weeren, RJ Dawson, WA Bruggen, M Bonafede, A Simionescu, A AF de Gasperin, F. Ogrean, G. A. van Weeren, R. J. Dawson, W. A. Brueggen, M. Bonafede, A. Simionescu, A. TI Abell 1033: birth of a radio phoenix SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: Abell 1033; large-scale structure of Universe; radio continuum: general; X-rays: galaxies: clusters ID GALAXY CLUSTER CATALOG; SHOCK-WAVES; SCALING RELATIONS; RICH CLUSTERS; DATA RELEASE; RELICS; ACCELERATION; REACCELERATION; ABUNDANCES; PARTICLES AB Extended steep-spectrum radio emission in a galaxy cluster is usually associated with a recent merger. However, given the complex scenario of galaxy cluster mergers, many of the discovered sources hardly fit into the strict boundaries of a precise taxonomy. This is especially true for radio phoenixes that do not have very well defined observational criteria. Radio phoenixes are aged radio galaxy lobes whose emission is reactivated by compression or other mechanisms. Here, we present the detection of a radio phoenix close to the moment of its formation. The source is located in Abell 1033, a peculiar galaxy cluster which underwent a recent merger. To support our claim, we present unpublished Westerbork Synthesis Radio Telescope and Chandra observations together with archival data from the Very Large Array and the Sloan Digital Sky Survey. We discover the presence of two subclusters displaced along the N-S direction. The two subclusters probably underwent a recent merger which is the cause of a moderately perturbed X-ray brightness distribution. A steep-spectrum extended radio source very close to an active galactic nucleus (AGN) is proposed to be a newly born radio phoenix: the AGN lobes have been displaced/compressed by shocks formed during the merger event. This scenario explains the source location, morphology, spectral index, and brightness. Finally, we show evidence of a density discontinuity close to the radio phoenix and discuss the consequences of its presence. C1 [de Gasperin, F.; Ogrean, G. A.; Brueggen, M.; Bonafede, A.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Ogrean, G. A.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dawson, W. A.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Simionescu, A.] Japan Aerosp Explorat Agcy, Sagamihara, Kanagawa 2298510, Japan. RP de Gasperin, F (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM fdg@hs.uni-hamburg.de OI van Weeren, Reinout/0000-0002-0587-1660 FU Deutsche Forschungsgemeinschaft [FOR 1254]; National Aeronautics and Space Administration (NASA) by Space Telescope Science Institute [HST-HF2-51345.001-A]; NASA [NAS5-26555, NAS8-03060]; NASA by Chandra X-ray Center [PF2-130104]; U.S. Department of Energy (DOE) by LLNL [DE-AC52-07NA27344]; Alfred P. Sloan Foundation; National Science Foundation; U.S. DOE Office of Science FX AB and MB acknowledge support by the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft: 'Magnetisation of interstellar and intergalactic media: the prospects of low-frequency radio observations'. GAO acknowledges support by the National Aeronautics and Space Administration (NASA) through a Hubble Fellowship grant HST-HF2-51345.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. RJW is supported by NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. Part of this work performed under the auspices of the U.S. Department of Energy (DOE) by LLNL under Contract DE-AC52-07NA27344.r Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. DOE Office of Science. The SDSS-III web site is http://www.sdss3.org. NR 49 TC 5 Z9 5 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 APR 11 PY 2015 VL 448 IS 3 BP 2197 EP 2209 DI 10.1093/mnras/stv129 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0PQ UT WOS:000351507000016 ER PT J AU Valenti, S Sand, D Stritzinger, M Howell, DA Arcavi, I McCully, C Childress, MJ Hsiao, EY Contreras, C Morrell, N Phillips, MM Gromadzki, M Kirshner, RP Marion, GH AF Valenti, S. Sand, D. Stritzinger, M. Howell, D. A. Arcavi, I. McCully, C. Childress, M. J. Hsiao, E. Y. Contreras, C. Morrell, N. Phillips, M. M. Gromadzki, M. Kirshner, R. P. Marion, G. H. TI Supernova 2013by: a Type IIL supernova with a IIP-like light-curve drop SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN 2013by ID PHOTOMETRY DATA RELEASE; PHYSICAL-PROPERTIES; IA SUPERNOVAE; NEBULAR PHASE; P SUPERNOVAE; PROJECT; TELESCOPE; SAMPLE; PROGENITOR; SPECTRA AB We present multiband ultraviolet and optical light curves, as well as visual-wavelength and near-infrared spectroscopy of the Type II linear (IIL) supernova (SN) 2013by. We show that SN 2013by and other SNe IIL in the literature, after their linear decline phase that start after maximum, have a sharp light-curve decline similar to that seen in SNe IIP. This light-curve feature has rarely been observed in other SNe IIL due to their relative rarity and the intrinsic faintness of this particular phase of the light curve. We suggest that the presence of this drop could be used as a physical parameter to distinguish between subclasses of SNe II, rather than their light-curve decline rate shortly after peak. Close inspection of the spectra of SN 2013by indicate asymmetric line profiles and signatures of high-velocity hydrogen. Late (similar to 90 d after explosion) near-infrared spectra of SN 2013by exhibit oxygen lines, indicating significant mixing within the ejecta. From the late-time light curve, we estimate that 0.029 M-circle dot of Ni-56 was synthesized during the explosion. It is also shown that the V-band light-curve slope is responsible for part of the scatter in the luminosity (V magnitude 50 d after explosion) versus Ni-56 relation. Our observations of SN 2013by and other SNe IIL through the onset of the nebular phase indicate that their progenitors are similar to those of SNe IIP. C1 [Valenti, S.; Howell, D. A.; Arcavi, I.; McCully, C.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Valenti, S.; Howell, D. A.; McCully, C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Sand, D.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Stritzinger, M.; Hsiao, E. Y.; Contreras, C.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Arcavi, I.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Childress, M. J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Childress, M. J.] Australian Natl Univ, ARC Ctr Excellence All Sky Astrophys CAASTRO, Canberra, ACT 2611, Australia. [Hsiao, E. Y.; Contreras, C.; Morrell, N.; Phillips, M. M.] Las Campanas Observ, Carnegie Observ, Colina El Pino, Chile. [Gromadzki, M.] Millennium Inst Astrophys, Santiago, Chile. [Gromadzki, M.] Univ Valparaiso, Inst Fis & Astron, Playa Ancha, Chile. [Kirshner, R. P.; Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marion, G. H.] Univ Texas Austin, Austin, TX 78712 USA. RP Valenti, S (reprint author), Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. EM svalenti@lcogt.net FU NSF [AST-0306969, AST-0908886, AST-0607438, AST-1008343]; Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant; ESO; Government of Chile; Ministry for the Economy, Development and Tourisms Programa Inicativa Cientifica Milenio [IC 12009]; Fondecyt [1120601] FX This material is based upon work supported by NSF under grants AST-0306969, AST-0908886, AST-0607438 and AST-1008343. MDS and the CSP gratefully acknowledge generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. MG acknowledges support from Joined Committee ESO and Government of Chile 2014 and the Ministry for the Economy, Development and Tourisms Programa Inicativa Cientifica Milenio through grant IC 12009, awarded to The Millennium Institute of Astrophysics (MAS) and Fondecyt Regular no. 1120601. We are grateful to Rubina Kotak who provided us spectra of SN 2002hh. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at LCO, Chile. 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 45 TC 14 Z9 14 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2015 VL 448 IS 3 BP 2608 EP 2616 DI 10.1093/mnras/stv208 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0PQ UT WOS:000351507000048 ER PT J AU Walker, MG Olszewski, EW Mateo, M AF Walker, Matthew G. Olszewski, Edward W. Mateo, Mario TI Bayesian analysis of resolved stellar spectra: application to MMT/Hectochelle observations of the Draco dwarf spheroidal SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: spectroscopic; galaxies: dwarf; galaxies: individual: Draco; galaxies: kinematics and dynamics; Local Group ID METAL-POOR STARS; TO-LIGHT RATIOS; URSA-MINOR; RADIAL-VELOCITIES; SATELLITE GALAXIES; LOCAL GROUP; MILKY; SPECTROSCOPY; SEXTANS; MMT AB We introduce a Bayesian method for fitting faint, resolved stellar spectra in order to obtain simultaneous estimates of redshift and stellar-atmospheric parameters. We apply the method to thousands of spectra - covering 5160-5280 angstrom at resolution R similar to 20 000 - that we have acquired with the MMT/Hectochelle fibre spectrograph for red giant and horizontal branch candidates along the line of sight to the Milky Way's dwarf spheroidal satellite in Draco. The observed stars subtend an area of similar to 4 deg(2), extending similar to 3 times beyond Draco's nominal 'tidal' radius. For each spectrum, we tabulate the first four moments - central value, variance, skewness and kurtosis - of posterior probability distribution functions representing estimates of the following physical parameters: line-of-sight velocity (v(los)), effective temperature (T-eff), surface gravity (log g) and metallicity ([Fe/H]). After rejecting low-quality measurements, we retain a new sample consisting of 2813 independent observations of 1565 unique stars, including 1879 observations for 631 stars with (as many as 13) repeat observations. Parameter estimates have median random errors of sigma(vlos) = 0.88 km s(-1), sigma(Teff) = 162 K, sigma(log g) = 0.37 dex and sigma([Fe/H]) = 0.20 dex. Our estimates of physical parameters distinguish similar to 470 likely Draco members from interlopers in the Galactic foreground. C1 [Walker, Matthew G.] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Walker, Matthew G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Olszewski, Edward W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Mateo, Mario] Univ Michigan, Ann Arbor, MI 48109 USA. RP Walker, MG (reprint author), Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. EM mgwalker@andrew.cmu.edu FU National Science Foundation [AST-1313045, AST-1412999, PHYS-1066293]; NSF [AST-0807498, AST-1313006, AST-0808043, AST-1312997] FX We acknowledge helpful discussions with Sergey Koposov, Alan McConnachie, Jorge Penarrubia, Nelson Caldwell, Evan Kirby and Alwin Mao. We further thank Evan Kirby for making available the velocities measured from Keck/DEIMOS spectra. We thank Andy Szentgyorgyi, Gabor Furesz and Dan Fabricant for building and maintaining Hectochelle. We thank the MMT and SAO staff, particularly Perry Berlind, Mike Calkins, Marc Lacasse, John McAfee, Ale Milone, Ricardo Ortiz, Dennis Smith, Bill Wyatt and all the observers who participated in the Hectochelle queue. Finally, we thank an anonymous referee for helpful suggestions. MGW is supported by National Science Foundation grants AST-1313045, AST-1412999 and in part by National Science Foundation Grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics, where portions of this work were completed. EO is supported by NSF grant AST-0807498 and AST-1313006. MM is supported by NSF grants AST-0808043 and AST-1312997.; Table 5 include g- and i-band magnitudes from the ninth data release of SDSS. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 46 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 APR 11 PY 2015 VL 448 IS 3 BP 2717 EP 2732 DI 10.1093/mnras/stv099 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0PQ UT WOS:000351507000056 ER PT J AU Rose, M Elvis, M Tadhunter, CN AF Rose, Marvin Elvis, Martin Tadhunter, Clive N. TI Coronal-Line Forest AGN: the best view of the inner edge of the AGN torus? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: emission lines; quasars: general; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; HIGH-IONIZATION LINES; SEYFERT-GALAXIES; SPECTRAL CLASSIFICATION; ENERGY-DISTRIBUTIONS; STARBURST GALAXIES; TIDAL DISRUPTION; HOST GALAXIES AB We introduce Coronal-Line Forest active galactic nuclei (CLiF AGN), AGN which have a rich spectrum of forbidden high-ionization lines (FHILs, e.g. [Fe VII], [Fe X] and [Ne V]), as well as relatively strong narrow (similar to 300 km s(-1)) H alpha emission when compared to the other Balmer transition lines. We find that the kinematics of the CLiF emitting region are similar to those of the forbidden low-ionization emission-line (FLIL) region. We compare emission line strengths of both FHILs and FLILs to CLOUDY photoionization results and find that the CLiF emitting region has higher densities (10(4.5) < n(H) < 10(7.5) cm(-3)) when compared to the FLIL emitting region (10(3.0) < n(H) < 10(4.5) cm(-3)). We use the photoionization results to calculate the CLiF regions radial distances (0.04 < R-CLiF < 32.5 pc) and find that they are comparable to the dust grain sublimation distances (0.10 < R-SUB < 4.3 pc). As a result, we suggest that the inner torus wall is the most likely location of the CLiF region, and the unusual strength of the FHILs is due to a specific viewing angle giving a maximal view of the far wall of the torus without the continuum being revealed. C1 [Rose, Marvin; Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tadhunter, Clive N.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. RP Rose, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mrose@cfa.harvard.edu FU NASA [NNX13AE88G]; National Aeronautics and Space Administration; National Science Foundation; Planetary Science Division of the National Aeronautics and Space Administration; Alfred P. Sloan Foundation; US Department of Energy Office of Science FX We gratefully acknowledge Eugene Avrett, Thaisa Storchi Bergmann and Hagai Netzer for their insightful discussions. This work was supported in part by NASA grant NNX13AE88G. We thank the referee for useful comments and suggestions which improved this work substantially. The authors acknowledge the data analysis facilities provided by the Starlink Project, which is run by CCLRC on behalf of PPARC. This publication makes use of data products from 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 publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. NR 54 TC 8 Z9 8 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 APR 11 PY 2015 VL 448 IS 3 BP 2900 EP 2920 DI 10.1093/mnras/stv113 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CE0PQ UT WOS:000351507000069 ER PT J AU Ben-Ami, S Hachinger, S Gal-Yam, A Mazzali, PA Filippenko, AV Horesh, A Matheson, T Modjaz, M Sauer, DN Silverman, JM Smith, N Yaron, O AF Ben-Ami, Sagi Hachinger, Stephan Gal-Yam, Avishay Mazzali, Paolo A. Filippenko, Alexei V. Horesh, Assaf Matheson, Thomas Modjaz, Maryam Sauer, Daniel N. Silverman, Jeffrey M. Smith, Nathan Yaron, Ofer TI ULTRAVIOLET SPECTROSCOPY OF TYPE IIB SUPERNOVAE: DIVERSITY AND THE IMPACT OF CIRCUMSTELLAR MATERIAL SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (Type IIb) ID CORE-COLLAPSE SUPERNOVAE; MASS-LOSS RATE; SN 1993J; SUPERGIANT PROGENITOR; LIGHT-CURVE; BINARY PROGENITOR; IA SUPERNOVAE; X-RAY; IB SUPERNOVAE; STELLAR WIND AB We present new Hubble Space Telescope (HST) multi-epoch ultraviolet (UV) spectra of the bright Type IIb SN 2013df, and undertake a comprehensive analysis of the set of four SNe IIb for which HST UV spectra are available (SN 1993J, SN 2001ig, SN 2011dh, and SN 2013df). We find strong diversity in both continuum levels and line features among these objects. We use radiative-transfer models that fit the optical part of the spectrum well, and find that in three of these four events we see a UV continuum flux excess, apparently unaffected by line absorption. We hypothesize that this emission originates above the photosphere, and is related to interaction with circumstellar material (CSM) located in close proximity to the SN progenitor. In contrast, the spectra of SN 2001ig are well fit by single-temperature models, display weak continuum and strong reverse-fluorescence features, and are similar to spectra of radioactive 56Ni-dominated SNe Ia. A comparison of the early shock-cooling components in the observed light curves with the UV continuum levels which we assume trace the strength of CSM interaction suggests that events with slower cooling have stronger CSM emission. The radio emission from events having a prominent UV excess is perhaps consistent with slower blast-wave velocities, as expected if the explosion shock was slowed down by the CSM that is also responsible for the strong UV, but this connection is currently speculative as it is based on only a few events. C1 [Ben-Ami, Sagi] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Ben-Ami, Sagi; Gal-Yam, Avishay; Horesh, Assaf; Yaron, Ofer] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Hachinger, Stephan; Mazzali, Paolo A.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Hachinger, Stephan] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Mazzali, Paolo A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Mazzali, Paolo A.] INAF Osservatorio Astronom, I-35122 Padua, Italy. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Modjaz, Maryam] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Sauer, Daniel N.] Stockholm Univ, Albanova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Ben-Ami, S (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM sbenami@cfa.harvard.edu RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Gal-Yam, Avishay/0000-0002-3653-5598; Sauer, Daniel/0000-0002-0317-5063 FU Minerva ARCHES award; NASA [PF0000, NAS8-03060]; Chandra X-ray Center; ISF; BSF; GIF; Minerva; FP7/ERC [307260]; Kimmel Investigator award; "Quantum-universe" I-core program of the planning and budgeting committee; Gary & Cynthia Bengier; Richard & Rhoda Goldman Fund; Sylvia & Jim Katzman Foundation; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916]; NASA/HST from the Space Telescope Science Institute [GO-13030]; Association of Universities for Research in Astronomy, Inc., under NASA [NAS 05-26555]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771] FX S.B. acknowledges support for this work by NASA through Einstein Postdoctoral Fellowship grant number PF0000 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. S.H. is supported by a Minerva ARCHES award. A.G. acknowledges support by grants from the ISF, BSF, GIF, Minerva, FP7/ERC grant # 307260, the "Quantum-universe" I-core program of the planning and budgeting committee and the ISF, and a Kimmel Investigator award. A.V.F. and his group at UC Berkeley have depended on generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Sylvia & Jim Katzman Foundation, the Christopher R. Redlich Fund, the TABASGO Foundation, NSF grant AST-1211916, and NASA/HST grant GO-13030 from the Space Telescope Science Institute (which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 05-26555). J.M.S is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. NR 80 TC 9 Z9 9 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 APR 10 PY 2015 VL 803 IS 1 AR 40 DI 10.1088/0004-637X/803/1/40 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG1EI UT WOS:000353015400040 ER PT J AU Imara, N AF Imara, N. TI RETHINKING A MYSTERIOUS MOLECULAR CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust; extinction; infrared: ISM; ISM: clouds; ISM: individual objects (G216-2.5 Rosette); radio lines: ISM ID YOUNG STELLAR OBJECTS; CO-TO-H-2 CONVERSION FACTOR; FAR-INFRARED LUMINOSITY; STAR-FORMATION RATES; COLUMN DENSITY; CLUSTER-FORMATION; MAGELLANIC-CLOUD; SPITZER SURVEY; IMAGING SURVEY; MILKY-WAY AB I present high-resolution column density maps of two molecular clouds (MCs) having strikingly different star formation rates. To better understand the unusual, massive G216-2.5, an MC with no massive star formation, the distribution of its molecular gas is compared to that of the Rosette MC. Far-infrared data from Herschel are used to derive N(H-2) maps of each cloud and are combined with ICO data to determine the CO-to-H-2 ratio, X-CO. In addition, the probability distribution functions (PDFs) and cumulative mass fractions of the clouds are compared. For G216-2.5, < N(H-2)> = 7.8 x 10(20) cm(-2) and < X-CO > = 2.2 x 10(20) cm(-2) (K km s(-1))(-1); for the Rosette, < N(H-2)> = 1.8 x 10(21) cm(-2) and < X-CO > = 2.8 x 10(20) cm(-2) (K km s(-1))(-1). The PDFs of both clouds are lognormal for extinctions below similar to 2 mag and both show departures from log-normality at high extinctions. Although it is the less-massive cloud, the Rosette has a higher fraction of its mass in the form of dense gas and contains 1389 M-circle dot of gas above the so-called extinction threshold for star formation, A(V) = 7.3 mag. The G216-2.5 cloud has 874 M-circle dot of dense gas above this threshold. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Imara, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nimara@cfa.harvard.edu FU Harvard-MIT FFL Postdoctoral Fellowship FX My work is supported by the Harvard-MIT FFL Postdoctoral Fellowship. I thank Sean Andrews, Charles Lada, and Tom Dame for their careful readings of earlier versions of this manuscript and for their helpful suggestions. Youngung Lee and Mark Heyer have my gratitude for providing the CO data sets. I also thank an anonymous referee for constructive comments that improved this paper. NR 47 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2015 VL 803 IS 1 AR 38 DI 10.1088/0004-637X/803/1/38 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG1EI UT WOS:000353015400038 ER PT J AU Krolewski, AG Eisenstein, DJ AF Krolewski, Alex G. Eisenstein, Daniel J. TI MEASURING THE LUMINOSITY AND VIRIAL BLACK HOLE MASS DEPENDENCE OF QUASAR-GALAXY CLUSTERING AT z similar to 0.8 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; large-scale structure of universe; quasars: general ID DIGITAL-SKY-SURVEY; DARK-MATTER HALOES; ACTIVE GALACTIC NUCLEI; QSO REDSHIFT SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; DATA RELEASE; SDSS-III; HOST GALAXIES; CROSS-CORRELATION; OCCUPATION DISTRIBUTION AB We study the dependence of quasar clustering on quasar luminosity and black hole mass by measuring the angular overdensity of photometrically selected galaxies imaged by the Wide-field Infrared Survey Explorer (WISE) about z similar to 0.8 quasars from SDSS. By measuring the quasar-galaxy cross-correlation function and using photometrically selected galaxies, we achieve a higher density of tracer objects and a more sensitive detection of clustering than measurements of the quasar autocorrelation function. We test models of quasar formation and evolution by measuring the luminosity dependence of clustering amplitude. We find a significant overdensity of WISE galaxies about z similar to 0.8 quasars at 0.2-6.4 h(-1) Mpc in projected comoving separation. We find no appreciable increase in clustering amplitude with quasar luminosity across a decade in luminosity, and a power-law fit between luminosity and clustering amplitude gives an exponent of -0.01 +/- 0.06 (1 sigma error). We also fail to find a significant relationship between clustering amplitude and black hole mass, although our dynamic range in true mass is suppressed due to the large uncertainties in virial black hole mass estimates. Our results indicate that a small range in host dark matter halo mass maps to a large range in quasar luminosity. C1 [Krolewski, Alex G.; Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krolewski, AG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM akrolewski@college.harvard.edu FU Harvard College Research Program; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; SDSS-III Collaboration; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We thank Doug Finkbeiner, Yue Shen, Adam Myers, Martin White, and Lars Hernquist for helpful comments and suggestions. We also thank Aaron Bray and Mario Juric for assistance with the SDSS imaging mask and the selection queries for the WISE and SDSS galaxies, respectively. A.G.K. acknowledges support from the Harvard College Research Program.; 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.; 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://sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 108 TC 2 Z9 2 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 APR 10 PY 2015 VL 803 IS 1 AR 4 DI 10.1088/0004-637X/803/1/4 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG1EI UT WOS:000353015400004 ER PT J AU Martinez-Sykora, J van der Voort, LR Carlsson, M De Pontieu, B Pereira, TMD Boerner, P Hurlburt, N Kleint, L Lemen, J Tarbell, TD Title, A Wuelser, JP Hansteen, VH Golub, L McKillop, S Reeves, KK Saar, S Testa, P Tian, H Jaeggli, S Kankelborg, C AF Martinez-Sykora, Juan van der Voort, Luc Rouppe Carlsson, Mats De Pontieu, Bart Pereira, Tiago M. D. Boerner, Paul Hurlburt, Neal Kleint, Lucia Lemen, James Tarbell, Ted D. Title, Alan Wuelser, Jean-Pierre Hansteen, Viggo H. Golub, Leon McKillop, Sean Reeves, Kathy K. Saar, Steven Testa, Paola Tian, Hui Jaeggli, Sarah Kankelborg, Charles TI INTERNETWORK CHROMOSPHERIC BRIGHT GRAINS OBSERVED WITH IRIS AND SST SO ASTROPHYSICAL JOURNAL LA English DT Article DE line: profiles; Sun: atmosphere; Sun: chromosphere; Sun: oscillations; Sun: transition region waves ID NONMAGNETIC SOLAR CHROMOSPHERE; HIGH-RESOLUTION OBSERVATIONS; TRANSITION REGION; SUMER OBSERVATIONS; IMAGE-RESTORATION; FINE-STRUCTURE; K LINES; MG II; ATMOSPHERE; TELESCOPE AB The Interface Region Imaging Spectrograph (IRIS) reveals small-scale rapid brightenings in the form of bright grains all over coronal holes and the quiet Sun. These bright grains are seen with the IRIS 1330, 1400, and 2796 angstrom slit-jaw filters. We combine coordinated observations with IRIS and from the ground with the Swedish 1 m Solar Telescope (SST) which allows us to have chromospheric (Ca II 8542 angstrom, Ca II H 3968 angstrom, Ha, and Mg II k 2796 angstrom) and transition region (C II 1334 angstrom, Si IV 1403 angstrom) spectral imaging, and single-wavelength Stokes maps in Fe I 6302 angstrom at high spatial (0.'' 33), temporal, and spectral resolution. We conclude that the IRIS slit-jaw grains are the counterpart of so-called acoustic grains, i.e., resulting from chromospheric acoustic waves in a nonmagnetic environment. We compare slit-jaw images (SJIs) with spectra from the IRIS spectrograph. We conclude that the grain intensity in the 2796 angstrom slit-jaw filter comes from both the Mg II k core and wings. The signal in the C II and Si IV lines is too weak to explain the presence of grains in the 1300 and 1400 angstrom SJIs and we conclude that the grain signal in these passbands comes mostly from the continuum. Although weak, the characteristic shock signatures of acoustic grains can often be detected in IRIS C II spectra. For some grains, a spectral signature can be found in IRIS Si IV. This suggests that upward propagating acoustic waves sometimes reach all the way up to the transition region. C1 [Martinez-Sykora, Juan; De Pontieu, Bart; Boerner, Paul; Hurlburt, Neal; Lemen, James; Tarbell, Ted D.; Title, Alan; Wuelser, Jean-Pierre; Hansteen, Viggo H.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Martinez-Sykora, Juan] Bay Area Environm Res Inst, Sonoma, CA USA. [van der Voort, Luc Rouppe; Carlsson, Mats; De Pontieu, Bart; Pereira, Tiago M. D.; Hansteen, Viggo H.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Kleint, Lucia] Univ Appl Sci & Arts Northwestern Switzerland, CH-5210 Windisch, Switzerland. [Golub, Leon; McKillop, Sean; Reeves, Kathy K.; Saar, Steven; Testa, Paola; Tian, Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jaeggli, Sarah; Kankelborg, Charles] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Martinez-Sykora, J (reprint author), Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. EM j.m.sykora@astro.uio.no OI De Pontieu, Bart/0000-0002-8370-952X; Rouppe van der Voort, Luc/0000-0003-2088-028X; Carlsson, Mats/0000-0001-9218-3139 FU NASA [NNM07AA01C, NNG09FA40C]; Research Council of Norway; European Research Council under the European Union's Seventh Framework Programme [291058] FX We gratefully acknowledge support by NASA grants NNX11AN98G and NNM12AB40P, and NASA contracts NNM07AA01C (Hinode) and NNG09FA40C (IRIS). This work has benefited from discussions at the International Space Science Institute (ISSI) meeting on "Heating of the magnetized chromosphere" from 2014 February 24-28 where many aspects of this paper were discussed with other colleagues. To analyze the data, we have used IDL and the Solar SoftWare library (SSW). The Swedish 1 m Solar Telescope is operated by the Institute for Solar Physics of the Royal Swedish Academy of Sciences in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research was supported by the Research Council of Norway and by the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 291058. Thanks are also due to Hakon Skogsrud, Eamon Scullion, and Ada Ortiz for performing the observations at the SST. NR 37 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2015 VL 803 IS 1 AR UNSP 44 DI 10.1088/0004-637X/803/1/44 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG1EI UT WOS:000353015400044 ER PT J AU Papovich, C Labbe, I Quadri, R Tilvi, V Behroozi, P Bell, EF Glazebrook, K Spitler, L Straatman, CMS Tran, KV Cowley, M Dave, R Dekel, A Dickinson, M Ferguson, HC Finkelstein, SL Gawiser, E Inami, H Faber, SM Kacprzak, GG Kawinwanichakij, L Kocevski, D Koekemoer, A Koo, DC Kurczynski, P Lotz, JM Lu, Y Lucas, RA McIntosh, D Mehrtens, N Mobasher, B Monson, A Morrison, G Nanayakkara, T Persson, SE Salmon, B Simons, R Tomczak, A van Dokkum, P Weiner, B Willner, SP AF Papovich, C. Labbe, I. Quadri, R. Tilvi, V. Behroozi, P. Bell, E. F. Glazebrook, K. Spitler, L. Straatman, C. M. S. Tran, K. -V. Cowley, M. Dave, R. Dekel, A. Dickinson, M. Ferguson, H. C. Finkelstein, S. L. Gawiser, E. Inami, H. Faber, S. M. Kacprzak, G. G. Kawinwanichakij, L. Kocevski, D. Koekemoer, A. Koo, D. C. Kurczynski, P. Lotz, J. M. Lu, Y. Lucas, R. A. McIntosh, D. Mehrtens, N. Mobasher, B. Monson, A. Morrison, G. Nanayakkara, T. Persson, S. E. Salmon, B. Simons, R. Tomczak, A. van Dokkum, P. Weiner, B. Willner, S. P. TI ZFOURGE/CANDELS: ON THE EVOLUTION OF M* GALAXY PROGENITORS FROM z=3 TO 0.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: structure ID STAR-FORMING GALAXIES; SIMILAR-TO 2; LYMAN-BREAK GALAXIES; STELLAR MASS FUNCTIONS; SPECTRAL ENERGY-DISTRIBUTIONS; EXTRAGALACTIC LEGACY SURVEY; ALPHA-EMITTING GALAXIES; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; ULTRA-DEEP FIELD AB Galaxies with stellar masses near M* contain the majority of stellar mass in the universe, and are therefore of special interest in the study of galaxy evolution. The Milky Way (MW) and Andromeda (M31) have present-day stellar masses near M*, at 5 x 10(10) M-circle dot (defined here to be MW-mass) and 10(11) M-circle dot (defined to be M31-mass). We study the typical progenitors of these galaxies using the FOURSTAR Galaxy Evolution Survey (ZFOURGE). ZFOURGE is a deep medium-band near-IR imaging survey, which is sensitive to the progenitors of these galaxies out to z similar to 3. We use abundance-matching techniques to identify the main progenitors of these galaxies at higher redshifts. We measure the evolution in the stellar mass, rest-frame colors, morphologies, far-IR luminosities, and star formation rates, combining our deep multiwavelength imaging with near-IR Hubble Space Telescope imaging from Cosmic Near-IR Deep Extragalactic Legacy Survey (CANDELS), and Spitzer and Herschel far-IR imaging from Great Observatories Origins Deep Survey-Herschel and CANDELS-Herschel. The typical MW-mass and M31-mass progenitors passed through the same evolution stages, evolving from blue, star-forming disk galaxies at the earliest stages to redder dust-obscured IR-luminous galaxies in intermediate stages and to red, more quiescent galaxies at their latest stages. The progenitors of the MW-mass galaxies reached each evolutionary stage at later times (lower redshifts) and with stellar masses that are a factor of two to three lower than the progenitors of the M31-mass galaxies. The process driving this evolution, including the suppression of star formation in present-day M* galaxies, requires an evolving stellar-mass/halo-mass ratio and/or evolving halo-mass threshold for quiescent galaxies. The effective size and SFRs imply that the baryonic cold-gas fractions drop as galaxies evolve from high redshift to z similar to 0 and are strongly anticorrelated with an increase in the Sersic index. Therefore, the growth of galaxy bulges in M* galaxies corresponds to a rapid decline in the galaxy gas fractions and/or a decrease in the star formation efficiency. C1 [Papovich, C.; Quadri, R.; Tilvi, V.; Tran, K. -V.; Kawinwanichakij, L.; Mehrtens, N.; Salmon, B.; Tomczak, A.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Papovich, C.; Quadri, R.; Tilvi, V.; Tran, K. -V.; Kawinwanichakij, L.; Mehrtens, N.; Salmon, B.; Tomczak, A.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Labbe, I.; Straatman, C. M. S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Behroozi, P.; Ferguson, H. C.; Koekemoer, A.; Lotz, J. M.; Lucas, R. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bell, E. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Glazebrook, K.; Kacprzak, G. G.; Nanayakkara, T.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Spitler, L.; Cowley, M.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Spitler, L.] Australian Astron Observ, Sydney, NSW 2113, Australia. [Dave, R.] Univ Western Cape, ZA-7535 Bellville, South Africa. [Dave, R.] South African Astron Observ, ZA-7925 Cape Town, South Africa. [Dave, R.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Dekel, A.] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel. [Dickinson, M.; Inami, H.] Natl Opt Astron Observ, Tucson, AZ 85721 USA. [Finkelstein, S. L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Gawiser, E.; Kurczynski, P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Faber, S. M.; Koo, D. C.] Univ Calif Santa Cruz, Univ Calif Observ Lick Observ, Santa Cruz, CA 95064 USA. [Kocevski, D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Lu, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [McIntosh, D.] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA. [Mobasher, B.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Morrison, G.; Persson, S. E.] Carnegie Observ, Pasadena, CA 91101 USA. [Morrison, G.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Morrison, G.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Simons, R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [van Dokkum, P.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Weiner, B.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Papovich, C (reprint author), Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. EM papovich@tamu.edu RI Glazebrook, Karl/N-3488-2015; OI Glazebrook, Karl/0000-0002-3254-9044; Nanayakkara, Themiya/0000-0003-2804-0648; Papovich, Casey/0000-0001-7503-8482; Cowley, Michael/0000-0002-4653-8637; Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873 FU National Science Foundation [AST-1009707, AST-0808133]; ERC [HIGHZ 227749]; NL-NWO Spinoza; NASA [NAS5-26555]; HST program [NAS5-26555, GO-12060]; NASA through a grant from the Space Telescope Science Institute [GO-12060]; National Collaborative Research Infrastructure Strategy of the Australian Federal Government; Texas AM University; George P. and Cynthia Woods Institute for Fundamental Physics and Astronomy FX We thank our other colleagues in CANDELS and ZFOURGE for their work and collaboration. We thank B. Moster for valuable input, and we thank the referee for a thorough report that improved the quality and clarity of this paper. This work is supported by the National Science Foundation through grants AST-1009707 and AST-0808133. I.L. acknowledges support from ERC HIGHZ 227749 and NL-NWO Spinoza. 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 supported in part by HST program number GO-12060. Support for Program number 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. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology. This work is based on observations made with the Herschel Space Observatory. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Australian access to the Magellan Telescopes was supported through the National Collaborative Research Infrastructure Strategy of the Australian Federal Government. We acknowledge generous support from the Texas A&M University and the George P. and Cynthia Woods Institute for Fundamental Physics and Astronomy. This paper is dedicated to the memory of Alma J. Broy and James W. Broy of Baltimore, Maryland. NR 158 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 APR 10 PY 2015 VL 803 IS 1 AR 26 DI 10.1088/0004-637X/803/1/26 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG1EI UT WOS:000353015400026 ER PT J AU Plunkett, AL Arce, HG Corder, SA Dunham, MM Garay, G Mardones, D AF Plunkett, Adele L. Arce, Hector G. Corder, Stuartt A. Dunham, Michael M. Garay, Guido Mardones, Diego TI ASSESSING MOLECULAR OUTFLOWS AND TURBULENCE IN THE PROTOSTELLAR CLUSTER SERPENS SOUTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Serpens South); ISM: jets and outflows; ISM: molecules; stars: formation; stars: protostars; techniques: interferometric ID YOUNG STELLAR OBJECTS; GOULD BELT SURVEY; J CO OBSERVATIONS; STAR EC 95; AQUILA RIFT; DRIVEN TURBULENCE; NGC 1333; EMBEDDED CLUSTERS; CARBON-MONOXIDE; MASS PROTOSTARS AB Molecular outflows driven by protostellar cluster members likely impact their surroundings and contribute to turbulence, affecting subsequent star formation. The very young Serpens South cluster consists of a particularly high density and fraction of protostars, yielding a relevant case study for protostellar outflows and their impact on the cluster environment. We combined CO J = 1-0 observations of this region using the Combined Array for Research in Millimeter-wave Astronomy and the Institut de Radioastronomie Millimetrique 30 m single-dish telescope. The combined map allows us to probe CO outflows within the central, most active region at size scales of 0.01-0.8 pc. We account for effects of line opacity and excitation temperature variations by incorporating (CO)-C-12 and (CO)-C-13 data for the J = 1 - 0 and J = 3 - 2 transitions (using Atacama Pathfinder Experiment and Caltech Submillimeter Observatory observations for the higher CO transitions), and we calculate mass, momentum, and energy of the molecular outflows in this region. The outflow mass-loss rate, force, and luminosity, compared with diagnostics of turbulence and gravity, suggest that outflows drive a sufficient amount of energy to sustain turbulence, but not enough energy to substantially counter the gravitational potential energy and disrupt the clump. Further, we compare Serpens South with the slightly more evolved cluster NGC 1333, and we propose an empirical scenario for outflow-cluster interaction at different evolutionary stages. C1 [Plunkett, Adele L.; Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Corder, Stuartt A.] Joint ALMA Observ, Santiago, Chile. [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Garay, Guido; Mardones, Diego] Univ Chile, Dept Astron, Santiago, Chile. RP Plunkett, AL (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. RI Mardones, Diego/I-5719-2016; Garay, Guido/H-8840-2013; OI Garay, Guido/0000-0003-1649-7958; Plunkett, Adele/0000-0002-9912-5705 FU National Science Foundation Graduate Research Fellowship [DGE-1122492]; NSF [AST-0845619]; Submillimeter Array through an SMA postdoctoral fellowship; CONICYT [PFB-06]; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; state of California; state of Illinois; state of Maryland; National Science Foundation [AST-0838261]; CARMA partner universities; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX We thank the anonymous referee for providing careful comments to improve the quality of the paper. We would like to thank Manuel Fernandez-Lopez and Jenny Hatchell for specific details and discussion of this region. A.L.P. acknowledges the Yale Graduate Writing Center Peer Review Group for constructive comments about this manuscript throughout the writing process. A.L.P. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1122492, and previously by the US Student Program of Fulbright Chile. H.G.A. receives funding from the NSF under grant AST-0845619. M.M.D. acknowledges support from the Submillimeter Array through an SMA postdoctoral fellowship. D.M. and G.G. acknowledge support from CONICYT project PFB-06. This publication is based on data acquired with the Combined Array for Research in Millimeter-wave Astronomy (CARMA), IRAM 30 m telescope, Atacama Pathfinder Experiment (APEX), and Caltech Submillimeter Observatory (CSO). Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The 30 m telescope, operated by the Institut de RadioAstronomie Millimtrique (IRAM), is funded by a partnership of INSU/CNRS (France), MPG (Germany), and IGN (Spain). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. The CSO is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (AST-0838261). The research presented here made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration, 2013). Facilities: CARMA, IRAM, APEX, CSO. NR 70 TC 9 Z9 9 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 APR 10 PY 2015 VL 803 IS 1 AR 22 DI 10.1088/0004-637X/803/1/22 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG1EI UT WOS:000353015400022 ER PT J AU Slavin, JD Dwek, E Jones, AP AF Slavin, Jonathan D. Dwek, Eli Jones, Anthony P. TI DESTRUCTION OF INTERSTELLAR DUST IN EVOLVING SUPERNOVA REMNANT SHOCK WAVES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: supernova remnants; ISM: abundances; shock waves ID MILKY-WAY; HOT GAS; SOLAR NEIGHBORHOOD; GRAIN DESTRUCTION; SIZE DISTRIBUTION; FILLING FACTOR; EVOLUTION; EMISSION; MODELS; EXTINCTION AB Supernova generated shock waves are responsible for most of the destruction of dust grains in the interstellar medium (ISM). Calculations of the dust destruction timescale have so far been carried out using plane parallel steady shocks, however, that approximation breaks down when the destruction timescale becomes longer than that for the evolution of the supernova remnant (SNR) shock. In this paper we present new calculations of grain destruction in evolving, radiative SNRs. To facilitate comparison with the previous study by Jones et al., we adopt the same dust properties as in that paper. We find that the efficiencies of grain destruction are most divergent from those for a steady shock when the thermal history of a shocked gas parcel in the SNR differs significantly from that behind a steady shock. This occurs in shocks with velocities greater than or similar to 200 km s(-1) for which the remnant is just beginning to go radiative. Assuming SNRs evolve in a warm phase dominated ISM, we find dust destruction timescales are increased by a factor of similar to 2 compared to those of Jones et al., who assumed a hot gas dominated ISM. Recent estimates of supernova rates and ISM mass lead to another factor of similar to 3 increase in the destruction timescales, resulting in a silicate grain destruction timescale of similar to 2-3 Gyr. These increases, while not able to resolve the problem of the discrepant timescales for silicate grain destruction and creation, are an important step toward understanding the origin and evolution of dust in the ISM. C1 [Slavin, Jonathan D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dwek, Eli] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Jones, Anthony P.] Univ Paris 11, CNRS, IAS, UMR 8617, F-91405 Orsay, France. RP Slavin, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jslavin@cfa.harvard.edu OI Slavin, Jonathan/0000-0002-7597-6935; Jones, Anthony/0000-0003-0577-6425 FU NASA Astrophysics Theory Program grant [NNX12AF84G]; NASA Astrophysical Data Analysis Program [ADAP13-0094] FX This research was supported by NASA Astrophysics Theory Program grant NNX12AF84G. ED acknowledges support by NASA Astrophysical Data Analysis Program ADAP13-0094. We thank John Raymond for providing the steady shock model calculations and our collaborator Xander Tielens for helpful discussions. We also wish to thank the developers of matplotlib, a python plotting library, which we used to produce all of the plots in this paper. NR 55 TC 16 Z9 16 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 APR 10 PY 2015 VL 803 IS 1 AR 7 DI 10.1088/0004-637X/803/1/7 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CG1EI UT WOS:000353015400007 ER PT J AU Rapson, VA Kastner, JH Andrews, SM Hines, DC Macintosh, B Millar-Blanchaer, M Tamura, M AF Rapson, Valerie A. Kastner, Joel H. Andrews, Sean M. Hines, Dean C. Macintosh, Bruce Millar-Blanchaer, Max Tamura, Motohide TI SCATTERED LIGHT FROM DUST IN THE CAVITY OF THE V4046 Sgr TRANSITION DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; polarization; stars: individual (V4046 Sgr); stars: pre-main sequence ID INDUCED GAP EDGES; TWIN YOUNG SUNS; PROTOPLANETARY DISK; CIRCUMSTELLAR DISKS; POLARIZED-LIGHT; ACCRETION; PLANETS; EVOLUTION; POLARIMETRY; SAGITTARII AB report the presence of scattered light from dust grains located in the giant planet formation region of the circumbinary disk orbiting the 20 Myr old close (-0.045 AU separation) binary system V4046 Sgr AB based on observations with the new Gemini Planet Imager (GPI) instrument. These GPI images probe to within 7 AU of the central binary with a linear spatial resolution of 3 AU, and are therefore capable of revealing the dust disk structure within a region corresponding to the giant planets in our solar system. GPI imaging reveals a relatively narrow (FWHM 10 AU) ring of polarized near-infrared flux whose brightness peaks at 14 AU. This 14 AU radius ring is surrounded by a fainter outer halo of scattered light extending to 45 AU, which coincides with previously detected millimeter-wave thermal dust emission. The presence of small grains that efficiently scatter starlight well inside the millimeter-wavelength disk cavity supports current models of planet formation which suggest that planet disk interactions can generate pressure traps that impose strong radial variations in the particle size distribution throughout the disk. C1 [Rapson, Valerie A.; Kastner, Joel H.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hines, Dean C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Macintosh, Bruce] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Millar-Blanchaer, Max] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M55 3H4, Canada. [Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Rapson, VA (reprint author), Rochester Inst Technol, Sch Phys & Astron, 1 Lomb Mem Dr, Rochester, NY 14623 USA. EM var5998@rit.edu FU National Science Foundation [AST-1108950] FX This work is based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the 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). Support is provided by the National Science Foundation grant AST-1108950 to R.I.T. NR 43 TC 10 Z9 10 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 APR 10 PY 2015 VL 803 IS 1 DI 10.1088/2041-8205/803/1/L10 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CF8NC UT WOS:000352817200010 ER PT J AU Zuluaga, JI Kipping, DM Sucerquia, M Alvarado, JA AF Zuluaga, Jorge I. Kipping, David M. Sucerquia, Mario Alvarado, Jaime A. TI A NOVEL METHOD FOR IDENTIFYING EXOPLANETARY RINGS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: analytical; occultations; planets and satellites: rings; techniques: photometric ID SUN-LIKE STAR; PLANETARY CANDIDATES; EXTRASOLAR PLANETS; DETECTABILITY; DISCOVERY; LINE AB The discovery of rings around extrasolar planets ("exorings") is one of the next breakthroughs in exoplanetary research. Previous studies have explored the feasibility of detecting exorings with present and future photometric sensitivities by seeking anomalous deviations in the residuals of a standard transit light curve fit, at the level of similar or equal to 100 ppm for Kronian rings. In this work, we explore two much larger observational consequences of exorings: (1) the significant increase in transit depth that may lead to the misclassification of ringed planetary candidates as false-positives and/or the underestimation of planetary density; and (2) the so-called "photo-ring" effect, a new asterodensity profiling effect, revealed by a comparison of the light curve derived stellar density to that measured with independent methods (e.g., asteroseismology). While these methods do not provide an unambiguous detection of exorings, we show that the large amplitude of these effects, combined with their relatively simple analytic description, makes them highly suited to large-scale surveys to identify candidate ringed planets worthy of more detailed investigation. Moreover, these methods lend themselves to ensemble analyses seeking to uncover evidence of a population of ringed planets. We describe the method in detail, develop the basic underlying formalism, and test it in the parameter space of rings and transit configuration. We discuss the prospects of using this method for the first systematic search of exoplanetary rings in the Kepler database and provide a basic computational code for implementing it. C1 [Zuluaga, Jorge I.; Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zuluaga, Jorge I.; Sucerquia, Mario; Alvarado, Jaime A.] Univ Antioquia, FACom Inst Fis FCEN, Medellin, Colombia. RP Zuluaga, JI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Vicerrectoria de Docencia de la Universidad de Antioquia, Estrategia de Sostenibilidad de la Universidad de Antioquia; Fulbright Commission, Colombia; Menzel fellowship; CODI/UdeA; Young Researchers program of the Vicerrectoria de Investigacion-UdeA FX J.I.Z. is supported by Vicerrectoria de Docencia de la Universidad de Antioquia, Estrategia de Sostenibilidad 2014-2015 de la Universidad de Antioquia and by the Fulbright Commission, Colombia. J.I.Z. thanks the Harvard-Smithsonian Center for Astrophysics for its hospitality while this work was carried out. D.M.K. is supported by the Menzel fellowship. M.S. is supported by CODI/UdeA and J.A.A. by the Young Researchers program of the Vicerrectoria de Investigacion-UdeA. We thank our refere, Jason Barnes, for comments and useful suggestions. NR 22 TC 7 Z9 7 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 APR 10 PY 2015 VL 803 IS 1 AR L14 DI 10.1088/2041-8205/803/1/L14 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CF8NC UT WOS:000352817200014 ER PT J AU Montes, C Cardona, A Jaramillo, C Pardo, A Silva, JC Valencia, V Ayala, C Perez-Angel, LC Rodriguez-Parra, LA Ramirez, V Nino, H AF Montes, C. Cardona, A. Jaramillo, C. Pardo, A. Silva, J. C. Valencia, V. Ayala, C. Perez-Angel, L. C. Rodriguez-Parra, L. A. Ramirez, V. Nino, H. TI Middle Miocene closure of the Central American Seaway SO SCIENCE LA English DT Article ID NORTHWESTERN SOUTH-AMERICA; MAGDALENA VALLEY BASIN; PANAMA IMPLICATIONS; TECTONIC EVOLUTION; COLOMBIAN ANDES; HISTORY; ARC; GEOCHRONOLOGY; MAGMATISM; COLLISION AB Uranium-lead geochronology in detrital zircons and provenance analyses in eight boreholes and two surface stratigraphic sections in the northern Andes provide insight into the time of closure of the Central American Seaway. The timing of this closure has been correlated with Plio-Pleistocene global oceanographic, atmospheric, and biotic events. We found that a uniquely Panamanian Eocene detrital zircon fingerprint is pronounced in middle Miocene fluvial and shallow marine strata cropping out in the northern Andes but is absent in underlying lower Miocene and Oligocene strata. We contend that this fingerprint demonstrates a fluvial connection, and therefore the absence of an intervening seaway, between the Panama arc and South America in middle Miocene times; the Central American Seaway had vanished by that time. C1 [Montes, C.; Perez-Angel, L. C.; Rodriguez-Parra, L. A.] Univ Los Andes, Bogota, Colombia. [Cardona, A.] Univ Nacl Colombia, Medellin, Colombia. [Jaramillo, C.] Smithsonian Trop Res Inst, Panama City, Panama. [Pardo, A.] Univ Caldas, Manizales, Colombia. [Silva, J. C.] Univ Houston, Houston, TX 77004 USA. [Valencia, V.] Washington State Univ, Pullman, WA 99164 USA. [Ayala, C.] Corp Geol Ares, Bogota, Colombia. [Ramirez, V.; Nino, H.] Ecopetrol, Bogota, Colombia. RP Montes, C (reprint author), Univ Los Andes, Bogota, Colombia. EM cmontes@uniandes.edu.co OI Montes, Camilo/0000-0002-3553-0787 FU Ecopetrol-ICP "Cronologia de la Deformacion en las Cuencas Subandinas"; Smithsonian Institution, Uniandes [P12. 160422.002/001]; Autoridad del Canal de Panama (ACP); Mark Tupper Fellowship; Ricardo Perez S.A.; NSF [EAR 0824299, OISE, EAR, DRL 0966884]; National Geographic Society FX Supported by Ecopetrol-ICP "Cronologia de la Deformacion en las Cuencas Subandinas," Smithsonian Institution, Uniandes P12. 160422.002/001, Autoridad del Canal de Panama (ACP), the Mark Tupper Fellowship, Ricardo Perez S.A.; NSF grant EAR 0824299 and OISE, EAR, DRL 0966884, Colciencias, and the National Geographic Society. We thank N. Hoyos, D. Villagomez, A. O'Dea, C. Bustamante, O. Montenegro, and C. Ojeda. All the data reported in this manuscript are presented in the main paper and in the supplementary materials. NR 30 TC 79 Z9 81 U1 10 U2 60 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 APR 10 PY 2015 VL 348 IS 6231 BP 226 EP 229 DI 10.1126/science.aaa2815 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CF5RD UT WOS:000352613700043 PM 25859042 ER PT J AU van Breugel, P Kindt, R Lilleso, JPB van Breugel, M AF van Breugel, Paulo Kindt, Roeland Lilleso, Jens-Peter Barnekow van Breugel, Michiel TI Environmental Gap Analysis to Prioritize Conservation Efforts in Eastern Africa SO PLOS ONE LA English DT Article ID PROTECTED-AREA NETWORK; GLOBAL LAND-COVER; BIODIVERSITY HOTSPOTS; SPECIES-DIVERSITY; CONSERVING BIODIVERSITY; METHODOLOGICAL APPROACH; BIOLOGICAL DIVERSITY; RESERVE SELECTION; ECOREGIONS; FOREST AB Countries in eastern Africa have set aside significant proportions of their land for protection. But are these areas representative of the diverse range of species and habitats found in the region? And do conservation efforts include areas where the state of biodiversity is likely to deteriorate without further interventions? Various studies have addressed these questions at global and continental scales. However, meaningful conservation decisions are required at finer geographical scales. To operate more effectively at the national level, finer scale baseline data on species and on higher levels of biological organization such as the eco-regions are required, among other factors. Here we adopted a recently developed high-resolution potential natural vegetation (PNV) map for eastern Africa as a baseline to more effectively identify conservation priorities. We examined how well different potential natural vegetations (PNVs) are represented in the protected area (PA) network of eastern Africa and used a multivariate environmental similarity index to evaluate biases in PA versus PNV coverage. We additionally overlaid data of anthropogenic factors that potentially influence the natural vegetation to assess the level of threat to different PNVs. Our results indicate substantial differences in the conservation status of PNVs. In addition, particular PNVs in which biodiversity protection and ecological functions are at risk due to human influences are revealed. The data and approach presented here provide a step forward in developing more transparent and better informed translation from global priorities to regional or national implementation in eastern Africa, and are valid for other geographic regions. C1 [van Breugel, Paulo; Lilleso, Jens-Peter Barnekow] Univ Copenhagen, Dept Geosci & Nat Resource Management, Forest Nat & Biomass, DK-1958 Frederiksberg C, Denmark. [van Breugel, Paulo; Kindt, Roeland] World Agroforestry Ctr, Nairobi, Kenya. [van Breugel, Michiel] Natl Univ Singapore, Dept Biol Sci, Yale NUS Coll, Singapore 138614, Singapore. [van Breugel, Michiel] Ciudad Panam, Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Panama City, Panama. [van Breugel, Michiel] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. RP van Breugel, P (reprint author), Univ Copenhagen, Dept Geosci & Nat Resource Management, Forest Nat & Biomass, Rolighedsvej 23, DK-1958 Frederiksberg C, Denmark. EM p.vanbreugel@gmail.com RI Lilleso, Jens-Peter Barnekow/F-4455-2015; OI Lilleso, Jens-Peter Barnekow/0000-0003-1418-3496; van Breugel, Paulo/0000-0001-9579-0831; Kindt, Roeland/0000-0002-7672-0712 FU Consultative Research Committee for Development Research (FFU) [10-095-LIFE] FX The research presented was funded by a grant from the Consultative Research Committee for Development Research (FFU) under project 10-095-LIFE. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 130 TC 1 Z9 1 U1 2 U2 18 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 APR 9 PY 2015 VL 10 IS 4 AR e0121444 DI 10.1371/journal.pone.0121444 PG 26 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CF5HQ UT WOS:000352588500020 PM 25855968 ER PT J AU Oberg, KI Guzman, VV Furuya, K Qi, CH Aikawa, Y Andrews, SM Loomis, R Wilner, DJ AF Oeberg, Karin I. Guzman, Viviana V. Furuya, Kenji Qi, Chunhua Aikawa, Yuri Andrews, Sean M. Loomis, Ryan Wilner, David J. TI The comet-like composition of a protoplanetary disk as revealed by complex cyanides SO NATURE LA English DT Article ID T-TAURI STARS; CO SNOW LINE; CHEMICAL-COMPOSITION; SOLAR NEBULA; X-RAY; CIRCUMSTELLAR DISKS; ORGANIC-MOLECULES; IMAGING SURVEY; AMINO-ACIDS; LOW-MASS AB Observations of comets and asteroids show that the solar nebula that spawned our planetary system was rich in water and organic molecules. Bombardment brought these organics to the young Earth's surface(1). Unlike asteroids, comets preserve a nearly pristine record of the solar nebula composition. The presence of cyanides in comets, including 0.01 per cent of methyl cyanide (CH3CN) with respect to water, is of special interest because of the importance of C-N bonds for abiotic amino acid synthesis(2). Comet-like compositions of simple and complex volatiles are found in protostars, and can readily be explained by a combination of gas-phase chemistry (to form, for example, HCN) and an active ice-phase chemistry on grain surfaces that advances complexity(3). Simple volatiles, including water and HCN, have been detected previously in solar nebula analogues, indicating that they survive disk formation or are re-formed in situ(4-7). It has hitherto been unclear whether the same holds for more complex organic molecules outside the solar nebula, given that recent observations show a marked change in the chemistry at the boundary between nascent envelopes and young disks due to accretion shocks(8). Here we report the detection of the complex cyanides CH3CN and