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
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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
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U1 0
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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
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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
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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
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U1 0
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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
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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
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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
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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
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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
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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
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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.
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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.
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JI Mon. Not. Roy. Astron. Soc.
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VL 449
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DI 10.1093/mnras/stv451
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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.
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JI Mon. Not. Roy. Astron. Soc.
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VL 449
IS 3
BP 2685
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DI 10.1093/mnras/stv480
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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.
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JI Mon. Not. Roy. Astron. Soc.
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VL 449
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DI 10.1093/mnras/stv372
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SC Astronomy & Astrophysics
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UT WOS:000355337800055
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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
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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
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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).
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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
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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
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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
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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
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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
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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).
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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
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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.
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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.
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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.
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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
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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.
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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.
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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
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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.
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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.
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JI Astrophys. J.
PD MAY 1
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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.
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JI Astrophys. J.
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DI 10.1088/0004-637X/804/1/49
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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.
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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.
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JI Astrophys. J.
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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).
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JI Astrophys. J.
PD MAY 1
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SC Astronomy & Astrophysics
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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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2015
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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.
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JI Astrophys. J.
PD MAY 1
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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
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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
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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.
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PU IOP PUBLISHING LTD
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
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PU IOP PUBLISHING LTD
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
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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
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U1 0
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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
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U1 0
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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
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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
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U1 0
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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.
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JI Astron. J.
PD MAY
PY 2015
VL 149
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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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
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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
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
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DI 10.1088/0004-6256/149/5/177
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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
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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
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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
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U1 0
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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
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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
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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
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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
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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
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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
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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
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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.
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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.
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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.
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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.
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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
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PU IOP PUBLISHING LTD
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
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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
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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
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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
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U2 2
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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