FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Steele, A
McCubbin, FM
Fries, M
Kater, L
Boctor, NZ
Fogel, ML
Conrad, PG
Glamoclija, M
Spencer, M
Morrow, AL
Hammond, MR
Zare, RN
Vicenzi, EP
Siljestrom, S
Bowden, R
Herd, CDK
Mysen, BO
Shirey, SB
Amundsen, HEF
Treiman, AH
Bullock, ES
Jull, AJT
AF Steele, A.
McCubbin, F. M.
Fries, M.
Kater, L.
Boctor, N. Z.
Fogel, M. L.
Conrad, P. G.
Glamoclija, M.
Spencer, M.
Morrow, A. L.
Hammond, M. R.
Zare, R. N.
Vicenzi, E. P.
Siljestrom, S.
Bowden, R.
Herd, C. D. K.
Mysen, B. O.
Shirey, S. B.
Amundsen, H. E. F.
Treiman, A. H.
Bullock, E. S.
Jull, A. J. T.
TI A Reduced Organic Carbon Component in Martian Basalts
SO SCIENCE
LA English
DT Article
ID ALLAN HILLS 84001; POLYCYCLIC AROMATIC-HYDROCARBONS; METEORITE ALH84001;
ISOTOPIC EVIDENCE; OXYGEN FUGACITY; MARS; ORIGIN; MANTLE; GRAPHITE;
IMPACT
AB The source and nature of carbon on Mars have been a subject of intense speculation. We report the results of confocal Raman imaging spectroscopy on 11 martian meteorites, spanning about 4.2 billion years of martian history. Ten of the meteorites contain abiotic macromolecular carbon (MMC) phases detected in association with small oxide grains included within high-temperature minerals. Polycyclic aromatic hydrocarbons were detected along with MMC phases in Dar al Gani 476. The association of organic carbon within magmatic minerals indicates that martian magmas favored precipitation of reduced carbon species during crystallization. The ubiquitous distribution of abiotic organic carbon in martian igneous rocks is important for understanding the martian carbon cycle and has implications for future missions to detect possible past martian life.
C1 [Steele, A.; McCubbin, F. M.; Boctor, N. Z.; Fogel, M. L.; Glamoclija, M.; Bowden, R.; Mysen, B. O.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[McCubbin, F. M.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Fries, M.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Kater, L.] Witec GmbH, D-89081 Ulm, Germany.
[Conrad, P. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Spencer, M.; Morrow, A. L.; Hammond, M. R.; Zare, R. N.] Stanford Univ, Dept Chem, Stanford, CA 94305 USA.
[Vicenzi, E. P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
[Siljestrom, S.] Stockholm Univ, Dept Geol Sci, S-10691 Stockholm, Sweden.
[Siljestrom, S.] SP Tech Res Inst Sweden, Dept Chem & Mat, S-50115 Boras, Sweden.
[Herd, C. D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
[Shirey, S. B.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Amundsen, H. E. F.] Earth Explorat Serv, N-0364 Oslo, Norway.
[Amundsen, H. E. F.] Planetary Explorat Serv, N-0364 Oslo, Norway.
[Treiman, A. H.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Bullock, E. S.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA.
[Jull, A. J. T.] Univ Arizona, Tucson, AZ 85721 USA.
RP Steele, A (reprint author), Carnegie Inst Sci, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA.
EM asteele@ciw.edu
RI Steele, Andrew/A-3573-2013; McCubbin, Francis/D-1698-2009; Fogel,
Marilyn/M-2395-2015
OI Fogel, Marilyn/0000-0002-1176-3818
FU NASA Astrobiology Science and Technology for Exploring Planets
[NNX09AB74G]; NASA Mars Fundamental Research Program [NNX08AN61G]; W. M.
Keck Foundation [2007-6-29]; NASA Astrobiology Institute [NNA09DA81A];
Carnegie Institution of Washington; NASA Cosmochemistry [NNX11AG76G];
Natural Science and Engineering Research Council of Canada [261740]
FX This work was funded by NASA Astrobiology Science and Technology for
Exploring Planets (NNX09AB74G to A. S., P. G. C., A. H. T., and M. L.
F.), NASA Mars Fundamental Research Program (NNX08AN61G to A. S.), the
W. M. Keck Foundation (2007-6-29 to M. L. F. and A. S.), NASA
Astrobiology Institute (NNA09DA81A to A. S., S. B. S., N.Z.B., B.O.M.,
and M. L. F.), and the Carnegie Institution of Washington. F. M. M.
acknowledges financial support from NASA Cosmochemistry (NNX11AG76G to
F. M. M.). A. S. thanks J. Strope for identification of suitable
meteorite samples, C. Agee (University of New Mexico) for the Tissint
sample, and L. Welzenbach, T. Gooding, and T. Rose for their assistance
in thin-sectioning the meteorites and the use of the Scanning Electron
Microscope in the Department of Mineral Sciences, National Museum of
Natural History, Smithsonian Institution, Washington, DC. C. D. K. H.
thanks D. Hnatyshin for assistance with oxygen fugacity calculations.
This work was supported by Natural Science and Engineering Research
Council of Canada grant 261740 "The Geology of Mars from Studies of
Martian Meteorites" to C. D. K. H. L2MS, 14C, and
additional Raman data have been included in the supplementary materials.
NR 38
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PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JUL 13
PY 2012
VL 337
IS 6091
BP 212
EP 215
DI 10.1126/science.1220715
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 973AN
UT WOS:000306323500053
PM 22628557
ER
PT J
AU Koskelo, AI
Fisher, TR
Utz, RM
Jordan, TE
AF Koskelo, Antti I.
Fisher, Thomas R.
Utz, Ryan M.
Jordan, Thomas E.
TI A new precipitation-based method of baseflow separation and event
identification for small watersheds (< 50 km(2))
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Baseflow separation; Precipitation; Quickflow; Hydrochemical; UKIH;
Hydrograph
ID CHOPTANK RIVER-BASIN; RECESSION ANALYSIS; CHESAPEAKE BAY; STREAMFLOW;
HYDROCHEMISTRY; CATCHMENT; FOREST
AB Baseflow separation methods are often impractical, require expensive materials and time-consuming methods, and/or are not designed for individual events in small watersheds. To provide a simple baseflow separation method for small watersheds, we describe a new precipitation-based technique known as the Sliding Average with Rain Record (SARR). The SARR uses rainfall data to justify each separation of the hydrograph. SARR has several advantages such as: it shows better consistency with the precipitation and discharge records, it is easier and more practical to implement, and it includes a method of event identification based on precipitation and quickflow response. SARR was derived from the United Kingdom Institute of Hydrology (UKIH) method with several key modifications to adapt it for small watersheds (<50 km(2)). We tested SARR on watersheds in the Choptank Basin on the Delmarva Peninsula (US Mid-Atlantic region) and compared the results with the UKIH method at the annual scale and the hydrochemical method at the individual event scale. Annually, SARR calculated a baseflow index that was similar to 10% higher than the UKIH method due to the finer time step of SARR (1 d) compared to UKIH (5 d). At the watershed scale, hydric soils were an important driver of the annual baseflow index likely due to increased groundwater retention in hydric areas. At the event scale, SARR calculated less baseflow than the hydrochemical method, again because of the differences in time step (hourly for hydrochemical) and different definitions of baseflow. Both SARR and hydrochemical baseflow increased with event size, suggesting that baseflow contributions are more important during larger storms. To make SARR easy to implement, we have written a MatLab program to automate the calculations which requires only daily rainfall and daily flow data as inputs. (c) 2012 Elsevier B.V. All rights reserved.
C1 [Koskelo, Antti I.; Fisher, Thomas R.] Univ Maryland, Ctr Environm Sci, Horn Point Lab, Cambridge, MD 21613 USA.
[Utz, Ryan M.] Univ Maryland, Ctr Environm Sci, Appalachian Lab, Frostburg, MD 21532 USA.
[Jordan, Thomas E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Koskelo, AI (reprint author), EA Engn Sci & Technol Inc, 15 Loveton Circle, Sparks, MD 21152 USA.
EM akoskelo@hpl.umces.edu; fisher@umces.edu; rutz@al.umces.edu;
jordanth@si.edu
FU USDA CSREES Program; USDA CEAP Program; NSF Ecosystem Studies Program
FX This research was supported by the USDA CSREES Program, USDA CEAP
Program, and NSF Ecosystem Studies Program. We acknowledge the field
assistance of Dave Whitall (NOAA), Peter Downey (USDA), Anne Gustafson
(HPL UMCES), and Rebecca Fox (HPL UMCES). Keith Eshleman (AL UMCES)
provided helpful comments on an earlier draft of this manuscript.
NR 33
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
J9 J HYDROL
JI J. Hydrol.
PD JUL 11
PY 2012
VL 450
BP 267
EP 278
DI 10.1016/j.jhydrol.2012.04.055
PG 12
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 973GU
UT WOS:000306349000026
ER
PT J
AU Dohrmann, M
Gocke, C
Reed, J
Janussen, D
AF Dohrmann, Martin
Goecke, Christian
Reed, John
Janussen, Dorte
TI Integrative taxonomy justifies a new genus, Nodastrella gen. nov., for
North Atlantic "Rossella" species (Porifera: Hexactinellida:
Rossellidae)
SO ZOOTAXA
LA English
DT Article
DE Asconema; cold-water coral reefs; glass sponges; molecular systematics;
new genus; North Atlantic Ocean; Rossella nodastrella
ID GLASS SPONGES PORIFERA; PHYLOGENY; EVOLUTION; BOOTSTRAP; SYSTEMATICS;
CONFIDENCE; MODELS; RATES
AB Molecular systematic studies have indicated that the hexactinellid sponge species Rossella nodastrella Topsent (Lyssacinosida, Rossellidae), previously only known from the NE Atlantic, is only distantly related to its congeners, which are restricted to the Southern Ocean, representing the only case thus far reported of a diphyletic genus in the class Hexactinellida. Here we describe new material of "Rossella" nodastrella from cold-water coral reefs in the NW Atlantic (Florida). Morphological comparison with the holotype from the Azores and specimens recently reported from off Ireland reveal at least two distinct species, which we corroborate with molecular data. Because the diphyletic nature of "Rossella" is further supported with inclusion of the new specimens in the molecular phylogeny, we erect a new genus, Nodastrella gen. nov., for these two species. The Irish specimens are synonymized with our new species Nodastrella asconemaoida sp. nov. Subtle morphological and molecular differences between the E and W Atlantic specimens are for the time being ascribed to intraspecific geographic variation, but indicate that Nodastrella might contain more (sub) species, pending investigation of additional specimens, especially from intermediate locations.
C1 [Dohrmann, Martin] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Goecke, Christian; Janussen, Dorte] Forsch Inst, D-60325 Frankfurt, Germany.
[Goecke, Christian; Janussen, Dorte] Nat Museum Senckenberg, D-60325 Frankfurt, Germany.
[Reed, John] Florida Atlantic Univ, Oceanog Inst, Harbor Branch, Ft Pierce, FL 34946 USA.
RP Dohrmann, M (reprint author), Feldbergstr 6, D-55118 Mainz, Germany.
EM mdohrma@gmail.com; Dorte.Janussen@senckenberg.de; Jreed12@hboi.fau.edu;
Christian.Goecke@senckenberg.de
FU DFG [JA 1063/14-2]; SYNTHESYS project [GB-TAF-885]; European Community;
Postdoctoral Fellowship of the Smithsonian Institution; NSF Porifera
Tree of Life project
FX We thank R. van Soest for important discussions and for providing us
with a specimen identified by him as R. nodastrella from Rockall Bank,
Ireland, and K. R. Tabachnick for important discussions on the taxonomy
of Rossella. Technicians H. Szmutka and T. Bollinger are thanked for
skeletal measurements and SEM documentation. We further thank Lauren van
Thiel for preparing the initial spicule slides of USNM 1150045 and USNM
1150046, K. Haen for providing the sample of HBOI 5-VIII-05-1-004 to MD,
S. Pomponi for Fig. 4, S. Vargas for providing DJ and CG with a sample
of the A. mitsukurii specimen used in Dohrmann et al. (2008, 2012), and
O. Voigt for suggestions on bleach protocols. Gert Worheide is
acknowledged for providing access to computational resources at the
Molecular Geo- & Palaeobiology Lab at LMU Munich. DJ thanks the DFG for
financing projects of the study on Antarctic sponges (JA 1063/14-2), and
for getting access to the Rossella types in the NHM London, supported by
SYNTHESYS project GB-TAF-885 (financed by European Community Research
Infrastructure Action under the FP7 Integrating Activities Programme).
MD was supported by a Postdoctoral Fellowship of the Smithsonian
Institution and further acknowledges Allen G. Collins for providing
additional funding through the NSF Porifera Tree of Life project
(www.portol.org). Allen G. Collins and 2 anonymous reviewers are thanked
for helpful comments on earlier versions of this manuscript.
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U2 9
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 JUL 10
PY 2012
IS 3383
BP 1
EP 13
PG 13
WC Zoology
SC Zoology
GA 970XQ
UT WOS:000306166000001
ER
PT J
AU Bogdan, A
Forman, WR
Zhuravleva, I
Mihos, JC
Kraft, RP
Harding, P
Guo, Q
Li, ZY
Churazov, E
Vikhlinin, A
Nulsen, PEJ
Schindler, S
Jones, C
AF Bogdan, Akos
Forman, William R.
Zhuravleva, Irina
Mihos, J. Christopher
Kraft, Ralph P.
Harding, Paul
Guo, Qi
Li, Zhiyuan
Churazov, Eugene
Vikhlinin, Alexey
Nulsen, Paul E. J.
Schindler, Sabine
Jones, Christine
TI EXPLORING THE UNUSUALLY HIGH BLACK-HOLE-TO-BULGE MASS RATIOS IN NGC 4342
AND NGC 4291: THE ASYNCHRONOUS GROWTH OF BULGES AND BLACK HOLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: bulges; galaxies: elliptical and lenticular, cD; galaxies:
evolution; galaxies: individual (NGC 4291, NGC 4342); X-rays: galaxies;
X-rays: ISM
ID EARLY-TYPE GALAXIES; DARK-MATTER HALOES; ACTIVE GALACTIC NUCLEI; DIGITAL
SKY SURVEY; HOST GALAXIES; VIRGO-CLUSTER; FUNDAMENTAL RELATION; SCALING
RELATIONS; STELLAR MASS; LIGHT
AB We study two nearby early-type galaxies, NGC 4342 and NGC 4291, that host unusually massive black holes relative to their low stellar mass. The observed black-hole-to-bulge mass ratios of NGC 4342 and NGC 4291 are 6.9(-2.3)(+3.8)% and 1.9% +/- 0.6%, respectively, which significantly exceed the typical observed ratio of similar to 0.2%. As a consequence of the exceedingly large black-hole-to-bulge mass ratios, NGC 4342 and NGC 4291 are approximate to 5.1 sigma and approximate to 3.4 sigma outliers from the M-center dot-M-bulge scaling relation, respectively. In this paper, we explore the origin of the unusually high black-hole-to-bulge mass ratio. Based on Chandra X-ray observations of the hot gas content of NGC 4342 and NGC 4291, we compute gravitating mass profiles, and conclude that both galaxies reside in massive dark matter halos, which extend well beyond the stellar light. The presence of dark matter halos around NGC 4342 and NGC 4291 and a deep optical image of the environment of NGC 4342 indicate that tidal stripping, in which greater than or similar to 90% of the stellar mass was lost, cannot explain the observed high black-hole-to-bulge mass ratios. Therefore, we conclude that these galaxies formed with low stellar masses, implying that the bulge and black hole did not grow in tandem. We also find that the black hole mass correlates well with the properties of the dark matter halo, suggesting that dark matter halos may play a major role in regulating the growth of the supermassive black holes.
C1 [Bogdan, Akos; Forman, William R.; Kraft, Ralph P.; Li, Zhiyuan; Vikhlinin, Alexey; Nulsen, Paul E. J.; Jones, Christine] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Zhuravleva, Irina; Churazov, Eugene] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Mihos, J. Christopher; Harding, Paul] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA.
[Guo, Qi] Chinese Acad Sci, Partner Grp, Max Planck Inst Astrophys, Natl Astron Observ, Beijing 100012, Peoples R China.
[Guo, Qi] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Schindler, Sabine] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
RP Bogdan, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM abogdan@cfa.harvard.edu
RI Churazov, Eugene/A-7783-2013;
OI Mihos, Chris/0000-0002-7089-8616; Nulsen, Paul/0000-0003-0297-4493
FU National Aeronautics and Space Administration [NAS8-03060]; National
Science Foundation [AST-0607526, AST-0707793, AST-1108964]; NASA through
Chandra X-ray Center [PF1-120081]; Smithsonian Institution; National
basic research program of China (973 program) [2009CB24901]; CAS; NSFC
[11143005]; Max Planck Society
FX We thank the anonymous referee for constructive comments. A.B. and W. R.
F. are grateful to Debora Sijacki, Mark Vogelsberger, Frank van den
Bosch, Kevin Schawinski, and Charlie Conroy for helpful discussions and
to Hans Bohringer for his valuable contribution to the Chandra proposal.
This research has made use of Chandra data provided by the Chandra X-ray
Center. The publication makes use of software provided by the Chandra
X-ray Center (CXC) in the application package CIAO. 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. A.B. acknowledges support provided by NASA
through Einstein Postdoctoral Fellowship grant number PF1-120081 awarded
by the Chandra X-ray Center, which is operated by the Smithsonian
Astrophysical Observatory for NASA under contract NAS8-03060. W. F. and
C.J. acknowledge support from the Smithsonian Institution. G. Q.
acknowledges support from the National basic research program of China
(973 program under Grant No. 2009CB24901), the Young Researcher Grant of
National Astronomical Observatories, CAS, the NSFC grants program (No.
11143005), and the Partner Group program of the Max Planck Society.
J.C.M. appreciates support from the NSF through grants AST-0607526,
AST-0707793, and AST-1108964.
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
VL 753
IS 2
AR 140
DI 10.1088/0004-637X/753/2/140
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700047
ER
PT J
AU Bowler, BP
Liu, MC
Shkolnik, EL
Dupuy, TJ
Cieza, LA
Kraus, AL
Tamura, M
AF Bowler, Brendan P.
Liu, Michael C.
Shkolnik, Evgenya L.
Dupuy, Trent J.
Cieza, Lucas A.
Kraus, Adam L.
Tamura, Motohide
TI PLANETS AROUND LOW-MASS STARS (PALMS). I. A SUBSTELLAR COMPANION TO THE
YOUNG M DWARF 1RXS J235133.3+312720
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; stars: individual (1RXS J235133.3+312720); stars: low-mass
ID ALL-SKY SURVEY; EXTRASOLAR GIANT PLANETS; PICTORIS MOVING GROUP;
SOLAR-TYPE STARS; X-RAY-EMISSION; AB-DORADUS-C; ACTIVITY-ROTATION
RELATIONSHIP; ANGULAR-MOMENTUM EVOLUTION; COLOR-MAGNITUDE DIAGRAMS;
TW-HYDRAE ASSOCIATION
AB We report the discovery of a brown dwarf companion to the young M dwarf 1RXS J235133.3+312720 as part of a high contrast imaging search for planets around nearby young low-mass stars with Keck-II/NIRC2 and Subaru/HiCIAO. The 2 ''.4 (similar to 120AU) pair is confirmed to be comoving from two epochs of high-resolution imaging. Follow-up low- and moderate-resolution near-infrared spectroscopy of 1RXS J2351+3127 B with IRTF/SpeX and Keck-II/OSIRIS reveals a spectral type of L0(-1)(+2). The M2 primary star 1RXS J2351+3127 A exhibits X-ray and UV activity levels comparable to young moving group members with ages of similar to 10-100 Myr. UVW kinematics based the measured radial velocity of the primary and the system's photometric distance (50 +/- 10 pc) indicate it is likely a member of the similar to 50-150 Myr AB Dor moving group. The near-infrared spectrum of 1RXS J2351+3127 B does not exhibit obvious signs of youth, but its H-band morphology shows subtle hints of intermediate surface gravity. The spectrum is also an excellent match to the similar to 200 MyrM9 brown dwarf LP 944-20. Assuming an age of 50-150 Myr, evolutionary models imply a mass of 32 +/- 6 M-Jup for the companion, making 1RXS J2351+3127 B the second lowest-mass member of the AB Dor moving group after the L4 companion CD-35 2722 B and one of the few benchmark brown dwarfs known at young ages.
C1 [Bowler, Brendan P.; Liu, Michael C.; Cieza, Lucas A.; Kraus, Adam L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Shkolnik, Evgenya L.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Tamura, Motohide] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
RP Bowler, BP (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM bpbowler@ifa.hawaii.edu
FU NASA [NNX11AC31G, NAS 5-26555]; NSF [AST09-09222]; NASA through STScI
[51257.01]; MEXT; W. M. Keck Foundation
FX We thank the referee for helpful comments, Joshua Schlieder for early
access to his kinematic analysis of 1RXS J2351+3127 A, Katelyn Allers
for helpful discussions about young brown dwarfs, Eric Nielsen for the
background track predictions, and Carolin Liefke for providing us with
the NEXXUS 2 catalog. It is a pleasure to thank the support astronomers
and telescope operators at Keck and IRTF who helped make this work
possible: Marc Kassis, Heather Hershley, Jim Lyke, Hien Tran, and John
Rayner. B. P. B. and M. C. L. have been supported by NASA grant
NNX11AC31G and NSF grant AST09-09222. T.J.D. A. L. K. have been
supported by NASA through Hubble Fellowship grants 51257.01 and 51257.01
awarded by STScI, which is operated by AURA, Inc., for NASA under
contract NAS 5-26555. M. T. is supported by Grant-In-Aid for Science
Research in a Priority Area from MEXT. We utilized data products from
the Two Micron All Sky Survey, which is a joint project of the
University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by the National
Aeronautics and Space Administration and the National Science
Foundation. NASA's Astrophysics Data System Bibliographic Services
together with the VizieR catalogue access tool and SIMBAD database
operated at CDS, Strasbourg, France, were invaluable resources for this
work. Finally, mahalo nui loa to the kama'aina of Hawai'i for their
support of Keck and the Mauna Kea observatories. We are grateful to
conduct observations from this mountain.; Some of the data presented
herein were obtained at the W. M. Keck Observatory, which is operated as
a scientific partnership among the California Institute of Technology,
the University of California, and the National Aeronautics and Space
Administration. The Observatory was made possible by the generous
financial support of the W. M. Keck Foundation.
NR 143
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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 JUL 10
PY 2012
VL 753
IS 2
AR 142
DI 10.1088/0004-637X/753/2/142
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700049
ER
PT J
AU Brodwin, M
Gonzalez, AH
Stanford, SA
Plagge, T
Marrone, DP
Carlstrom, JE
Dey, A
Eisenhardt, PR
Fedeli, C
Gettings, D
Jannuzi, BT
Joy, M
Leitch, EM
Mancone, C
Snyder, GF
Stern, D
Zeimann, G
AF Brodwin, M.
Gonzalez, A. H.
Stanford, S. A.
Plagge, T.
Marrone, D. P.
Carlstrom, J. E.
Dey, A.
Eisenhardt, P. R.
Fedeli, C.
Gettings, D.
Jannuzi, B. T.
Joy, M.
Leitch, E. M.
Mancone, C.
Snyder, G. F.
Stern, D.
Zeimann, G.
TI IDCS J1426.5+3508: SUNYAEV-ZEL'DOVICH MEASUREMENT OF A MASSIVE
INFRARED-SELECTED CLUSTER AT z=1.75
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; galaxies:
clusters: individual (IDCS J1426.5+3508); galaxies: clusters:
intracluster medium; galaxies: evolution
ID SOUTH-POLE TELESCOPE; LUMINOUS GALAXY CLUSTER; IRAC SHALLOW SURVEY;
WIDE-FIELD SURVEY; GREATER-THAN 1; COSMOLOGY; SAMPLE; EVOLUTION;
DISCOVERY; ARRAY
AB We report 31 GHz CARMA observations of IDCS J1426.5+3508, an infrared-selected galaxy cluster at z = 1.75. A Sunyaev-Zel'dovich (SZ) decrement is detected toward this cluster, indicating a total mass of M-200,M-m = (4.3 +/- 1.1) x 10(14) M-circle dot in agreement with the approximate X-ray mass of similar to 5 x 10(14) M-circle dot. IDCS J1426.5+3508 is by far the most distant cluster yet detected via the SZ effect, and the most massive z >= 1.4 galaxy cluster found to date. Despite the mere similar to 1% probability of finding it in the 8.82 deg(2) IRAC Distant Cluster Survey, IDCS J1426.5+3508 is not completely unexpected in Lambda CDM once the area of large, existing surveys is considered. IDCS J1426.5+3508 is, however, among the rarest, most extreme clusters ever discovered and indeed is an evolutionary precursor to the most massive known clusters at all redshifts. We discuss how imminent, highly sensitive SZ experiments will complement infrared techniques for statistical studies of the formation of the most massive galaxy clusters in the z > 1.5 universe, including potential precursors to IDCS J1426.5+3508.
C1 [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Brodwin, M.; Snyder, G. F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
[Gonzalez, A. H.; Fedeli, C.; Gettings, D.; Mancone, C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Stanford, S. A.; Zeimann, G.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Plagge, T.; Carlstrom, J. E.; Leitch, E. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Plagge, T.; Carlstrom, J. E.; Leitch, E. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
[Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Eisenhardt, P. R.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Joy, M.] NASA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Brodwin, M (reprint author), Univ Missouri, Dept Phys & Astron, 5110 Rockhill Rd, Kansas City, MO 64110 USA.
OI Marrone, Daniel/0000-0002-2367-1080
FU National Science Foundation [AST-0838187, PHY-0114422]; CARMA; NASA;
NASA by JPL/Caltech; Smithsonian Astrophysical Observatory; NASA
[G09-0150A, NAS 5-26555]; NASA through Space Telescope Science Institute
[11663, 12203]; W. M. Keck Foundation; U.S. Department of Energy
[W-7405-ENG-48]; CARMA construction; [SV4-74018, A31]
FX Support for CARMA construction was derived from the states of
California, Illinois, and Maryland, the James S. McDonnell Foundation,
the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L.
Norris Foundation, the University of Chicago, the Associates of the
California Institute of Technology, and the National Science Foundation.
Ongoing CARMA development and operations are supported by the National
Science Foundation under a cooperative agreement, and by the CARMA
partner universities. The work at Chicago is supported by NSF grants
AST-0838187 and PHY-0114422.; This work is based in part on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. Support for this work was provided by NASA through
an award issued by JPL/Caltech. This work is based in part on
observations obtained with the Chandra X-Ray Observatory (Chandra),
under contract SV4-74018, A31 with the Smithsonian Astrophysical
Observatory, which operates Chandra for NASA. Support for this research
was provided by the NASA grant G09-0150A. Support for HST programs 11663
and 12203 were 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 the NASA contract NAS 5-26555.
This work is based in part on data obtained at the W. M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
the National Aeronautics and Space Administration. The Observatory was
made possible by the generous financial support of the W. M. Keck
Foundation. This work makes use of image data from the NOAO
DeepWide-Field Survey (NDWFS) as distributed by the NOAO Science
Archive. NOAO is operated by the Association of Universities for
Research in Astronomy (AURA), Inc., under a cooperative agreement with
the National Science Foundation.; We thank the anonymous referee for
suggestions that improved the manuscript, Bradford Benson for helpful
discussions, F. Will High and Keith Vanderlinde for providing published
SPT masses in a digital form, Matt Ashby for creating the IRAC catalogs
for SDWFS, Michael Brown for combining the NDWFS with SDWFS catalogs,
Alexey Vikhlinin for advice on the analysis of the Chandra data, and
Daniel Holz for providing his predictions in an electronic format. This
paper would not have been possible without the efforts of the support
staffs of CARMA, the Keck Observatory, the Spitzer Space Telescope, the
Hubble Space Telescope, and the Chandra X-Ray Observatory. Support for
M.B. was provided by the W. M. Keck Foundation. A.H.G. acknowledges
support from the National Science Foundation performed under the
auspices of the U.S. Department of Energy under Contract No.
W-7405-ENG-48.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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PT J
AU Drout, MR
Soderberg, AM
Gal-Yam, A
Cenko, SB
Fox, DB
Leonard, DC
Sand, DJ
Moon, DS
Arcavi, I
Green, Y
AF Drout, Maria R.
Soderberg, Alicia M.
Gal-Yam, Avishay
Cenko, S. Bradley
Fox, Derek B.
Leonard, Douglas C.
Sand, David J.
Moon, Dae-Sik
Arcavi, Iair
Green, Yoav
TI THE FIRST SYSTEMATIC STUDY OF TYPE Ibc SUPERNOVA MULTI-BAND LIGHT CURVES
(vol 741, pg 97, 2011)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Drout, Maria R.; Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Drout, Maria R.] Univ Cambridge Churchhill Coll, Cambridge CB3 0DS, England.
[Gal-Yam, Avishay; Arcavi, Iair; Green, Yoav] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Cenko, S. Bradley] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fox, Derek B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Sand, David J.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Sand, David J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Moon, Dae-Sik] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Drout, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA.
RI Green, Yoav/L-5874-2015
OI Green, Yoav/0000-0002-0809-6575
NR 1
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700087
ER
PT J
AU Fu, H
Jullo, E
Cooray, A
Bussmann, RS
Ivison, RJ
Perez-Fournon, I
Djorgovski, SG
Scoville, N
Yan, L
Riechers, DA
Aguirre, J
Auld, R
Baes, M
Baker, AJ
Bradford, M
Cava, A
Clements, DL
Dannerbauer, H
Dariush, A
De Zotti, G
Dole, H
Dunne, L
Dye, S
Eales, S
Frayer, D
Gavazzi, R
Gurwell, M
Harris, AI
Herranz, D
Hopwood, R
Hoyos, C
Ibar, E
Jarvis, MJ
Kim, S
Leeuw, L
Lupu, R
Maddox, S
Martinez-Navajas, P
Michalowski, MJ
Negrello, M
Omont, A
Rosenman, M
Scott, D
Serjeant, S
Smail, I
Swinbank, AM
Valiante, E
Verma, A
Vieira, J
Wardlow, JL
van der Werf, P
AF Fu, Hai
Jullo, E.
Cooray, A.
Bussmann, R. S.
Ivison, R. J.
Perez-Fournon, I.
Djorgovski, S. G.
Scoville, N.
Yan, L.
Riechers, D. A.
Aguirre, J.
Auld, R.
Baes, M.
Baker, A. J.
Bradford, M.
Cava, A.
Clements, D. L.
Dannerbauer, H.
Dariush, A.
De Zotti, G.
Dole, H.
Dunne, L.
Dye, S.
Eales, S.
Frayer, D.
Gavazzi, R.
Gurwell, M.
Harris, A. I.
Herranz, D.
Hopwood, R.
Hoyos, C.
Ibar, E.
Jarvis, M. J.
Kim, S.
Leeuw, L.
Lupu, R.
Maddox, S.
Martinez-Navajas, P.
Michalowski, M. J.
Negrello, M.
Omont, A.
Rosenman, M.
Scott, D.
Serjeant, S.
Smail, I.
Swinbank, A. M.
Valiante, E.
Verma, A.
Vieira, J.
Wardlow, J. L.
van der Werf, P.
TI A COMPREHENSIVE VIEW OF A STRONGLY LENSED PLANCK-ASSOCIATED
SUBMILLIMETER GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: formation; galaxies: individual (HATLAS J114637.9-001132);
galaxies: interactions
ID SCIENCE DEMONSTRATION PHASE; STAR-FORMATION LAW; DIGITAL SKY SURVEY;
HERSCHEL-ATLAS; MOLECULAR GAS; HIGH-REDSHIFT; EXTRAGALACTIC SOURCES;
INTERSTELLAR-MEDIUM; CONVERSION FACTOR; MAJOR MERGERS
AB We present high-resolution maps of stars, dust, and molecular gas in a strongly lensed submillimeter galaxy (SMG) at z = 3.259. HATLAS J114637.9-001132 is selected from the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS) as a strong lens candidate mainly based on its unusually high 500 mu m flux density (similar to 300 mJy). It is the only high-redshift Planck detection in the 130 deg(2) H-ATLAS Phase-I area. Keck Adaptive Optics images reveal a quadruply imaged galaxy in the K band while the Submillimeter Array and the Jansky Very Large Array show doubly imaged 880 mu m and CO(1 -> 0) sources, indicating differentiated distributions of the various components in the galaxy. In the source plane, the stars reside in three major kpc-scale clumps extended over similar to 1.6 kpc, the dust in a compact (similar to 1 kpc) region similar to 3 kpc north of the stars, and the cold molecular gas in an extended (similar to 7 kpc) disk similar to 5 kpc northeast of the stars. The emissions from the stars, dust, and gas are magnified by similar to 17, similar to 8, and similar to 7 times, respectively, by four lensing galaxies at z similar to 1. Intrinsically, the lensed galaxy is a warm (T-dust similar to 40-65 K), hyperluminous (L-IR similar to 1.7 x 10(13) L-circle dot; star formation rate (SFR) similar to 2000 M-circle dot similar to yr(-1)), gas-rich (M-gas/M-baryon similar to 70%), young (M-stellar/SFR similar to 20 Myr), and short-lived (M-gas/SFR similar to 40 Myr) starburst. With physical properties similar to unlensed z > 2 SMGs, HATLAS J114637.9-001132 offers a detailed view of a typical SMG through a powerful cosmic microscope.
C1 [Fu, Hai; Cooray, A.; Kim, S.; Wardlow, J. L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Jullo, E.] Observ Astrophys Marseille Provence, F-13388 Marseille, France.
[Bussmann, R. S.; Gurwell, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Perez-Fournon, I.; Martinez-Navajas, P.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Perez-Fournon, I.; Martinez-Navajas, P.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Djorgovski, S. G.; Scoville, N.; Yan, L.; Riechers, D. A.; Bradford, M.; Vieira, J.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Djorgovski, S. G.] King Abdulaziz Univ, Jeddah 21413, Saudi Arabia.
[Aguirre, J.; Lupu, R.; Rosenman, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Auld, R.; Eales, S.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Cava, A.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain.
[Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Dannerbauer, H.] Univ Vienna, Inst Astron, A-1160 Vienna, Austria.
[Dannerbauer, H.] Univ Paris Diderot, Irfu SAp, CEA Saclay, Lab AIM Paris Saclay,CEA DSM CNRS, F-91191 Gif Sur Yvette, France.
[Dariush, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England.
[De Zotti, G.; Negrello, M.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[De Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Dole, H.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Dole, H.] CNRS, UMR 8617, F-91405 Orsay, France.
[Frayer, D.] NRAO, Green Bank, WV 24944 USA.
[Dunne, L.; Dye, S.; Hoyos, C.; Maddox, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Gavazzi, R.; Omont, A.] Univ Paris 06, Inst Astrophys Paris, UMR 7095, CNRS, F-75014 Paris, France.
[Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Herranz, D.] Inst Fis Cantabria CSIC UC, E-39005 Santander, Spain.
[Jarvis, M. J.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
[Leeuw, L.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Leeuw, L.] SETI Inst, Mountain View, CA 94043 USA.
[Michalowski, M. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Negrello, M.; Serjeant, S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Smail, I.; Swinbank, A. M.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England.
[Verma, A.] Univ Oxford, Oxford OX1 3RH, England.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Fu, H (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
EM haif@uci.edu
RI Baes, Maarten/I-6985-2013; Smail, Ian/M-5161-2013; Herranz,
Diego/K-9143-2014; Lupu, Roxana/P-9060-2014; Wardlow, Julie/C-9903-2015;
Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017;
OI De Hoyos Fernandez De Cordova, Carlos/0000-0003-3120-6856; Dye,
Simon/0000-0002-1318-8343; Scott, Douglas/0000-0002-6878-9840; Baes,
Maarten/0000-0002-3930-2757; Smail, Ian/0000-0003-3037-257X; Herranz,
Diego/0000-0003-4540-1417; Lupu, Roxana/0000-0003-3444-5908; Wardlow,
Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Cava,
Antonio/0000-0002-4821-1275; De Zotti, Gianfranco/0000-0003-2868-2595;
Maddox, Stephen/0000-0001-5549-195X
FU NSF [AST-0645427, AST-0909182]; Spanish grants [ESP2007-65812-C02-02,
AYA2010-21697-C05-04]; ASI/INAF [I/072/09/0]; MIUR; W.M. Keck
Foundation; NASA Herschel Science Center/JPL; ESA Member States; NASA
FX We thank the anonymous referee for comments that helped improve the
paper. H. F., A. C., J.L.W., and S. K. acknowledge support from NSF
CAREER AST-0645427. I. P. F. is supported by the Spanish grants
ESP2007-65812-C02-02 and AYA2010-21697-C05-04. S. G. D. acknowledges
partial support from the NSF grant AST-0909182. G.D.Z. and M.N.
acknowledge support from ASI/INAF agreement I/072/09/0 ("Planck LFI
Activity of Phase E2") and from MIUR through the PRIN 2009. Some of the
data presented herein were obtained at the W. M. Keck Observatory, which
is operated as a scientific partnership among the California Institute
of Technology, the University of California, and the National
Aeronautics and Space Administration. The Observatory was made possible
by the generous financial support of the W.M. Keck Foundation. The
authors wish to recognize and acknowledge the very significant cultural
role and reverence that the summit of Mauna Kea has always had within
the indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. The
Herschel-ATLAS is a project with Herschel, which is an ESA space
observatory with science instruments provided by European-led Principal
Investigator consortia and with important participation from NASA. The
H-ATLAS Web site is http://www.h-atlas.org/. The US participants
acknowledge support from the NASA Herschel Science Center/JPL. Partly
based on observations obtained with Planck (http://www.esa.int/Planck),
an ESA science mission with instruments and contributions directly
funded by ESA Member States, NASA, and Canada. 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
William Herschel Telescope is operated on the island of La Palma by the
Issac Newton Group in the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofisica de Canarias.
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JI Astrophys. J.
PD JUL 10
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SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700041
ER
PT J
AU Gonzalez, AH
Stanford, SA
Brodwin, M
Fedeli, C
Dey, A
Eisenhardt, PRM
Mancone, C
Stern, D
Zeimann, G
AF Gonzalez, Anthony H.
Stanford, S. Adam
Brodwin, Mark
Fedeli, Cosimo
Dey, Arjun
Eisenhardt, Peter R. M.
Mancone, Conor
Stern, Daniel
Zeimann, Greg
TI IDCS J1426.5+3508: COSMOLOGICAL IMPLICATIONS OF A MASSIVE, STRONG
LENSING CLUSTER AT z=1.75
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; cosmology: observations; galaxies: clusters:
individual (IDCS J1426.5+3508); gravitational lensing: strong
ID GIANT-ARC STATISTICS; DARK-MATTER HALOES; GALAXY CLUSTERS;
CROSS-SECTIONS; UNIVERSE; FIELD; POPULATION; POTENTIALS; SIMULATION;
DEPENDENCE
AB The galaxy cluster IDCS J1426.5+3508 at z = 1.75 is the most massive galaxy cluster yet discovered at z > 1.4 and the first cluster at this epoch for which the Sunyaev-Zel'Dovich effect has been observed. In this paper, we report on the discovery with Hubble Space Telescope imaging of a giant arc associated with this cluster. The curvature of the arc suggests that the lensing mass is nearly coincident with the brightest cluster galaxy, and the color is consistent with the arc being a star-forming galaxy. We compare the constraint on M-200 based upon strong lensing with Sunyaev-Zel'Dovich results, finding that the two are consistent if the redshift of the arc is z greater than or similar to 3. Finally, we explore the cosmological implications of this system, considering the likelihood of the existence of a strongly lensing galaxy cluster at this epoch in a Lambda CDM universe. While the existence of the cluster itself can potentially be accommodated if one considers the entire volume covered at this redshift by all current high-redshift cluster surveys, the existence of this strongly lensed galaxy greatly exacerbates the long-standing giant arc problem. For standard Lambda CDM structure formation and observed background field galaxy counts this lens system should not exist. Specifically, there should be no giant arcs in the entire sky as bright in F814W as the observed arc for clusters at z >= 1.75, and only similar to 0.3 as bright in F160W as the observed arc. If we relax the redshift constraint to consider all clusters at z >= 1.5, the expected number of giant arcs rises to similar to 15 in F160W, but the number of giant arcs of this brightness in F814W remains zero. These arc statistic results are independent of the mass of IDCS J1426.5+3508. We consider possible explanations for this discrepancy.
C1 [Gonzalez, Anthony H.; Fedeli, Cosimo; Mancone, Conor] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Stanford, S. Adam; Zeimann, Greg] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. Adam] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Brodwin, Mark] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA.
[Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Eisenhardt, Peter R. M.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gonzalez, AH (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
FU Nancy Levenson; NASA through HST GO programs [11663, 12203]; National
Science Foundation [AST-0708490]; U.S. Department of Energy
[W-7405-ENG-48]; NOAO; NASA
FX The authors thank the anonymous referee for suggestions that improved
the quality of this paper. We are also grateful to the Gemini
Observatory for allocating Director's Discretionary time to obtain a
redshift for the giant arc. We appreciate the support provided by Nancy
Levenson and the rest of the Gemini staff for this project. Gemini
Observatory is operated by the Association of Universities for Research
in Astronomy, Inc., under a cooperative agreement with the NSF on behalf
of the Gemini partnership: the National Science Foundation (United
States), the Science and Technology Facilities Council (United Kingdom),
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). This work is based in part on data obtained at
the W. M. Keck Observatory, which is operated as a scientific
partnership among the California Institute of Technology, the University
of California, and the National Aeronautics and Space Administration.
Support for this research was provided by NASA through HST GO programs
11663 and 12203. A.H.G. thanks Marusa Bradac for a useful discussion
about the arc, and also acknowledges support from the National Science
Foundation through the grant AST-0708490. The work by S.A.S. at LLNL was
performed under the auspices of the U.S. Department of Energy under
Contract No. W-7405-ENG-48, and support for M.B. was provided by the W.
M. Keck Foundation. The work of P.R.M.E. and D.S. was carried out at Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. The research activities of A.D. are supported by
NOAO, which is operated by the Association of Universities for Research
in Astronomy (AURA) under a cooperative agreement with the National
Science Foundation.
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SN 0004-637X
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JI Astrophys. J.
PD JUL 10
PY 2012
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DI 10.1088/0004-637X/753/2/163
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700070
ER
PT J
AU Gu, WM
AF Gu, Wei-Min
TI RADIATION PRESSURE-SUPPORTED ACCRETION DISKS: VERTICAL STRUCTURE, ENERGY
ADVECTION, AND CONVECTIVE STABILITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; convection;
hydrodynamics; instabilities
ID BLACK-HOLE; DOMINATED ACCRETION; MAGNETOHYDRODYNAMIC SIMULATIONS;
EDDINGTON LUMINOSITY; GAS-PRESSURE; SLIM; THICK; DISSIPATION; OUTFLOWS;
MODELS
AB By taking into account the local energy balance per unit volume between the viscous heating and the advective cooling plus the radiative cooling, we investigate the vertical structure of radiation pressure-supported accretion disks in spherical coordinates. Our solutions show that the photosphere of the disk is close to the polar axis and therefore the disk seems to be extremely thick. However, the density profile implies that most of the accreted matter exists in a moderate range around the equatorial plane. We show that the well-known polytropic relation between the pressure and the density is unsuitable for describing the vertical structure of radiation pressure-supported disks. More importantly, we find that the energy advection is significant even for slightly sub-Eddington accretion disks. We argue that the non-negligible advection may help us understand why the standard thin disk model is likely to be inaccurate above similar to 0.3 Eddington luminosity, which was found by some works on black hole spin measurement. Furthermore, the solutions satisfy the Solberg-Hoiland conditions, which indicate the disk to be convectively stable. In addition, we discuss the possible link between our disk model and ultraluminous X-ray sources.
C1 [Gu, Wei-Min] Xiamen Univ, Dept Phys, Xiamen 361005, Fujian, Peoples R China.
[Gu, Wei-Min] Xiamen Univ, Inst Theoret Phys & Astrophys, Xiamen 361005, Fujian, Peoples R China.
[Gu, Wei-Min] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gu, WM (reprint author), Xiamen Univ, Dept Phys, Xiamen 361005, Fujian, Peoples R China.
EM guwm@xmu.edu.cn
RI Gu, WM/G-3984-2010
FU National Natural Science Foundation of China [11073015, 10833002];
National Basic Research Program (973 Program) of China [2009CB824800];
China Scholarship Council [2009835057]
FX The author is particularly grateful to Ramesh Narayan for constructive
suggestions and beneficial discussions. The author also thanks Ivan
Hubeny, Da-Bin Lin, Aleksander Sadowski, Lijun Gou, Yucong Zhu, and
Shan-Shan Weng for helpful discussions, and the referee for providing
useful comments to improve the paper. This work was supported by the
National Natural Science Foundation of China under grants 11073015 and
10833002, the National Basic Research Program (973 Program) of China
under grant 2009CB824800, and the scholarship from China Scholarship
Council under grant 2009835057.
NR 32
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
VL 753
IS 2
AR 118
DI 10.1088/0004-637X/753/2/118
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700025
ER
PT J
AU Guarcello, MG
Caramazza, M
Micela, G
Sciortino, S
Drake, JJ
Prisinzano, L
AF Guarcello, M. G.
Caramazza, M.
Micela, G.
Sciortino, S.
Drake, J. J.
Prisinzano, L.
TI CHANDRA/ACIS-I STUDY OF THE X-RAY PROPERTIES OF THE NGC 6611 AND M16
STELLAR POPULATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE open clusters and associations: individual (NGC 6611 and M16); stars:
coronae; stars: massive; stars: pre-main sequence; X-rays: stars
ID PRE-MAIN-SEQUENCE; ORION-NEBULA-CLUSTER; EMISSION-LINE DIAGNOSTICS;
INTERMEDIATE-MASS STARS; VLT-FLAMES SURVEY; EAGLE-NEBULA; YOUNG STELLAR;
OB STARS; SPATIAL-DISTRIBUTION; CIRCUMSTELLAR DISKS
AB Mechanisms regulating the origin of X-rays in young stellar objects and the correlation with their evolutionary stage are under debate. Studies of the X-ray properties in young clusters allow us to understand these mechanisms. One ideal target for this analysis is the Eagle Nebula (M16), with its central cluster NGC 6611. At 1750 pc from the Sun, it harbors 93 OB stars, together with a population of low-mass stars from embedded protostars to disk-less Class III objects, with age <= 3Myr. We study an archival 78 ks Chandra/ACIS-I observation of NGC 6611 and two new 80 ks observations of the outer region of M16, one centered on the Column V and the other on a region of the molecular cloud with ongoing star formation. We detect 1755 point sources with 1183 candidate cluster members (219 disk-bearing and 964 disk-less). We study the global X-ray properties of M16 and compare them with those of the Orion Nebula Cluster. We also compare the level of X-ray emission of Class II and Class III stars and analyze the X-ray spectral properties of OB stars. Our study supports the lower level of X-ray activity for the disk-bearing stars with respect to the disk-less members. The X-ray luminosity function (XLF) of M16 is similar to that of Orion, supporting the universality of the XLF in young clusters. Eighty-five percent of the O stars of NGC 6611 have been detected in X-rays. With only one possible exception, they show soft spectra with no hard components, indicating that mechanisms for the production of hard X-ray emission in O stars are not operating in NGC 6611.
C1 [Guarcello, M. G.; Drake, J. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Caramazza, M.; Micela, G.; Sciortino, S.; Prisinzano, L.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy.
RP Guarcello, MG (reprint author), Smithsonian Astrophys Observ, MS-67,60 Garden St, Cambridge, MA 02138 USA.
OI Prisinzano, Loredana/0000-0002-8893-2210; Micela,
Giuseppina/0000-0002-9900-4751
FU Chandra Grant [GO0-11040X]; NASA [NAS8-39073]; PRIN-INAF
FX We thank the anonymous referee for useful comments and suggestions. This
work is based on observations performed with Chandra/ACIS-I. M. G. G.
was supported by Chandra Grant GO0-11040X. J. J. D. was supported by the
NASA contract NAS8-39073 to the Chandra X-ray Center and thanks the
Director, H. Tananbaum, for continuing advice and support. G.M., S.S.,
M.C., and L.P. were supported by the contract PRIN-INAF 2009.
NR 76
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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 JUL 10
PY 2012
VL 753
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AR 117
DI 10.1088/0004-637X/753/2/117
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700024
ER
PT J
AU Meisner, AM
Frebel, A
Juric, M
Finkbeiner, DP
AF Meisner, Aaron M.
Frebel, Anna
Juric, Mario
Finkbeiner, Douglas P.
TI THE METALLICITY OF THE MONOCEROS STREAM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: interactions; Galaxy: evolution; Galaxy:
stellar content; Galaxy: structure; stars: abundances
ID SAGITTARIUS DWARF GALAXY; MILKY-WAY TOMOGRAPHY; DIGITAL SKY SURVEY;
ANTICENTER STELLAR STRUCTURE; CANIS-MAJOR; GIANT BRANCH; SURVEY VIEW;
STARS; HALO; KINEMATICS
AB We present low-resolution MMT Hectospec spectroscopy of 594 candidate Monoceros stream member stars. Based on strong color-magnitude diagram overdensities, we targeted three fields within the stream's footprint, with 178 degrees <= l <= 203 degrees and -25 degrees <= b <= 25 degrees. By comparing the measured iron abundances with those expected from smooth Galactic components alone, we measure, for the first time, the spectroscopic metallicity distribution function for Monoceros. We find the stream to be chemically distinct from both the thick disk and halo, with [Fe/H] = -1, and do not detect a trend in the stream's metallicity with Galactic longitude. Passing from b = +25 degrees to b = -25 degrees, the median Monoceros metallicity trends upward by 0.1 dex, though uncertainties in modeling sample contamination by the disk and halo make this a marginal detection. In each field, we find Monoceros to have an intrinsic [Fe/H] dispersion of 0.10-0.22 dex. From the Ca II K line, we measure [Ca/Fe] for a subsample of metal-poor program stars with -1.1 < [Fe/H] < -0.5. In two of three fields, we find calcium deficiencies qualitatively similar to previously reported [Ti/Fe] underabundances in Monoceros and the Sagittarius tidal stream. Further, using 90 spectra of thick disk stars in the Monoceros pointings with b approximate to +/-25 degrees, we detect a 0.22 dex north/south metallicity asymmetry coincident with known stellar density asymmetry at R-GC approximate to 12 kpc and vertical bar Z vertical bar approximate to 1.7 kpc. Our median Monoceros [Fe/H] = -1.0 and its relatively low dispersion naturally fit the expectation for an appropriately luminous M-V similar to -13 dwarf galaxy progenitor.
C1 [Meisner, Aaron M.; Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Meisner, Aaron M.; Frebel, Anna; Juric, Mario; Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Meisner, AM (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.
EM ameisner@fas.harvard.edu; afrebel@mit.edu; mjuric@cfa.harvard.edu;
dfinkbeiner@cfa.harvard.edu
OI Meisner, Aaron/0000-0002-1125-7384
FU National Defense Science & Engineering Graduate fellowship; Clay
Fellowship; NASA [HF-51255.01-A, NAS 5-26555]; Space Telescope Science
Institute
FX We warmly thank Nelson Caldwell for his advice on MMT observations,
Hectospec details, and queue scheduling, as well as Evan Kirby and John
Norris for fruitful discussions. We furthermore thank the queue
observers and the SAO Telescope Data Center for reducing the data. This
research made extensive use of the Vienna Atomic Line Database (VALD).
A.M.M. is supported by a National Defense Science & Engineering Graduate
fellowship. A.F. is supported by a Clay Fellowship administered by the
Smithsonian Astrophysical Observatory. M.J. acknowledges support by NASA
through Hubble Fellowship grant No. HF-51255.01-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under the
contract NAS 5-26555.
NR 40
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
VL 753
IS 2
AR 116
DI 10.1088/0004-637X/753/2/116
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700023
ER
PT J
AU Morales-Calderon, M
Stauffer, JR
Stassun, KG
Vrba, FJ
Prato, L
Hillenbrand, LA
Terebey, S
Covey, KR
Rebull, LM
Terndrup, DM
Gutermuth, R
Song, I
Plavchan, P
Carpenter, JM
Marchis, F
Garcia, EV
Margheim, S
Luhman, KL
Angione, J
Irwin, JM
AF Morales-Calderon, M.
Stauffer, J. R.
Stassun, K. G.
Vrba, F. J.
Prato, L.
Hillenbrand, L. A.
Terebey, S.
Covey, K. R.
Rebull, L. M.
Terndrup, D. M.
Gutermuth, R.
Song, I.
Plavchan, P.
Carpenter, J. M.
Marchis, F.
Garcia, E. V.
Margheim, S.
Luhman, K. L.
Angione, J.
Irwin, J. M.
TI YSOVAR: SIX PRE-MAIN-SEQUENCE ECLIPSING BINARIES IN THE ORION NEBULA
CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; open clusters and associations: individual (Orion);
stars: pre-main sequence; stars: variables: general
ID LOW-MASS STARS; SPITZER-SPACE-TELESCOPE; UPPER CENTAURUS-LUPUS; YOUNG
BROWN DWARFS; X-RAY OBSERVATIONS; KECK-II-TELESCOPE; SPECTROSCOPIC
BINARY; 2MASS J05352184-0546085; ECHELLE SPECTROGRAPH; EVOLUTIONARY
TRACKS
AB Eclipsing binaries (EBs) provide critical laboratories for empirically testing predictions of theoretical models of stellar structure and evolution. Pre-main-sequence (PMS) EBs are particularly valuable, both due to their rarity and the highly dynamic nature of PMS evolution, such that a dense grid of PMS EBs is required to properly calibrate theoretical PMS models. Analyzing multi-epoch, multi-color light curves for similar to 2400 candidate Orion Nebula Cluster (ONC) members from our Warm Spitzer Exploration Science Program YSOVAR, we have identified 12 stars whose light curves show eclipse features. Four of these 12 EBs are previously known. Supplementing our light curves with follow-up optical and near-infrared spectroscopy, we establish two of the candidates as likely field EBs lying behind the ONC. We confirm the remaining six candidate systems, however, as newly identified ONC PMS EBs. These systems increase the number of known PMS EBs by over 50% and include the highest mass (theta(1) Ori E, for which we provide a complete set of well-determined parameters including component masses of 2.807 and 2.797 M-circle dot) and longest-period (ISOY J053505.71-052354.1, P similar to 20 days) PMS EBs currently known. In two cases (theta(1) Ori E and ISOY J053526.88-044730.7), enough photometric and spectroscopic data exist to attempt an orbit solution and derive the system parameters. For the remaining systems, we combine our data with literature information to provide a preliminary characterization sufficient to guide follow-up investigations of these rare, benchmark systems.
C1 [Morales-Calderon, M.; Stauffer, J. R.; Rebull, L. M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Morales-Calderon, M.] Ctr Astrobiol INTA CSIC, E-28691 Villanueva De La Canada, Spain.
[Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Stassun, K. G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Stassun, K. G.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Vrba, F. J.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA.
[Prato, L.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Hillenbrand, L. A.; Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Terebey, S.; Angione, J.] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA.
[Covey, K. R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Terndrup, D. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Terndrup, D. M.] Natl Sci Fdn, Arlington, VA 22230 USA.
[Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Song, I.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
[Plavchan, P.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Marchis, F.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA.
[Margheim, S.] So Operat Ctr, Gemini Observ, La Serena, Chile.
[Luhman, K. L.] So Operat Ctr, Gemini Observ, La Serena, Chile.
[Luhman, K. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Irwin, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Morales-Calderon, M (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM mariamc@cab.inta-csic.es
RI Marchis, Franck/H-3971-2012; Morales-Calderon, Maria/C-8384-2017;
OI Morales-Calderon, Maria/0000-0001-9526-9499; Rebull,
Luisa/0000-0001-6381-515X; Covey, Kevin/0000-0001-6914-7797
FU NASA through JPL/Caltech; National Aeronautics and Space Administration;
National Science Foundation [AST-0544588, AST-1009136]; Pennsylvania
State University; Eberly College of Science; Pennsylvania Space Grant
Consortium; Gemini Observatory, Argentina; Gemini Observatory,
Australia; Gemini Observatory, Brazil; Gemini Observatory, Canada;
Gemini Observatory, Chile; Gemini Observatory, United Kingdom; Gemini
Observatory, United States of America
FX We are grateful to the anonymous referee for a helpful report. This work
is based in part on observations made with the Spitzer Space Telescope,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology under a contract with NASA. Support for this work was
provided by NASA through an award issued by JPL/Caltech. This research
has made use of the NASA Exoplanet Archive, which is operated by the
California Institute of Technology, under contract with the National
Aeronautics and Space Administration under the Exoplanet Exploration
Program. K.L. was supported by grant AST-0544588 and L.P. by grant
AST-1009136 from the National Science Foundation. The Center for
Exoplanets and Habitable Worlds is supported by the Pennsylvania State
University, the Eberly College of Science, and the Pennsylvania Space
Grant Consortium. S.M. was supported by the Gemini Observatory, which is
operated by the Association of Universities for Research in Astronomy,
Inc., on behalf of the international Gemini partnership of Argentina,
Australia, Brazil, Canada, Chile, the United Kingdom, and the United
States of America.
NR 73
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
VL 753
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AR 149
DI 10.1088/0004-637X/753/2/149
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700056
ER
PT J
AU Munoz-Jaramillo, A
Sheeley, NR
Zhang, J
DeLuca, EE
AF Munoz-Jaramillo, Andres
Sheeley, Neil R., Jr.
Zhang, Jie
DeLuca, Edward E.
TI CALIBRATING 100 YEARS OF POLAR FACULAE MEASUREMENTS: IMPLICATIONS FOR
THE EVOLUTION OF THE HELIOSPHERIC MAGNETIC FIELD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar-terrestrial relations; Sun: activity; Sun: dynamo; Sun: faculae,
plages; Sun: surface magnetism
ID CYCLE 23; SOLAR; FLUX
AB Although the Sun's polar magnetic fields are thought to provide important clues for understanding the 11 year sunspot cycle, including the observed variations of its amplitude and period, the current database of high-quality polar field measurements spans relatively few sunspot cycles. In this paper, we address this deficiency by consolidating Mount Wilson Observatory polar faculae data from four data reduction campaigns, validating it through a comparison with facular data counted automatically from Michelson Doppler Imager (MDI) intensitygrams, and calibrating it against polar field measurements taken by the Wilcox Solar Observatory and average polar field and total polar flux calculated using MDI line-of-sight magnetograms. Our results show that the consolidated polar facular measurements are in excellent agreement with both polar field and polar flux estimates, making them an ideal proxy to study the evolution of the polar magnetic field. Additionally, we combine this database with sunspot area measurements to study the role of the polar magnetic flux in the evolution of the heliospheric magnetic field (HMF). We find that there is a strong correlation between HMF and polar flux at solar minimum and that, taken together, polar flux and sunspot area are better at explaining the evolution of the HMF during the last century than sunspot area alone.
C1 [Munoz-Jaramillo, Andres; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Munoz-Jaramillo, Andres] Univ Corp Atmospher Res, Boulder, CO 80307 USA.
[Munoz-Jaramillo, Andres] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Sheeley, Neil R., Jr.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Zhang, Jie] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA.
RP Munoz-Jaramillo, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM amunoz@cfa.harvard.edu; neil.sheeley@nrl.navy.mil; jzhang7@gmu.edu;
edeluca@cfa.harvard.edu
RI DeLuca, Edward/L-7534-2013;
OI DeLuca, Edward/0000-0001-7416-2895; Munoz-Jaramillo,
Andres/0000-0002-4716-0840
FU NASA [NNX07AO72G]; University of Utah; Office of Naval Research;
Lockheed Martin [SP02H1701R]; NSF [ATM-0748003]
FX We are grateful to Steve Cranmer for the original suggestion which led
to this collaboration, Georgios Cintzoglou for his invaluable help with
the automatic detection algorithm, the anonymous referee for feedback
which helped improved the quality of this paper, Aad Vanballegooijen and
Yi-Ming Wang for useful discussions, Mike Lockwood and Leif Svalgaard
for sharing their HMF data and discussing their usage with us, Laura
Balmaceda and Sami Solanki for sharing their sunspot database with us,
and Jeneen Sommers for her invaluable help in acquiring MDI
intensitygram and LOS magnetogram data. This research is supported by
the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program,
administered by the UCAR Visiting Scientist Programs and has made
extensive use of SAO/NASA's Astrophysics Data System. The computations
required for this work were performed using the resources of the
Harvard-Smithsonian Center for Astrophysics-we thank Jonathan
Sattelberger and Alisdair Davey for much appreciated technical support.
Wilcox Solar Observatory data used in this study were obtained via the
Web site http://wso.stanford.edu at 2011:11:7 courtesy of J. Todd
Hoeksema. The Wilcox Solar Observatory is currently supported by NASA.
The MDI instrument is part of SOHO, which is a project of international
cooperation between ESA and NASA. OMNI data were obtained from the Space
Physics Data Facility at NASA's Goddard Space flight center
http://omniweb.gsfc.nasa.gov/. Andres Munoz-Jaramillo is very grateful
to David Kieda for his support and sponsorship at the University of
Utah. Neil R. Sheeley is grateful to Roger K. Ulrich (UCLA) for
permission to examine the historical collection of Mount Wilson white
light images, and to his colleagues J. E. Boyden and S. Padilla for help
during the most recent data reduction campaign. At NRL, financial
support was provided by NASA and the Office of Naval Research. Ed DeLuca
was supported by contract SP02H1701R from Lockheed Martin to SAO. Jie
Zhang is supported by NSF Grant ATM-0748003 and NASA Grant NNX07AO72G.
NR 29
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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 JUL 10
PY 2012
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IS 2
AR 146
DI 10.1088/0004-637X/753/2/146
PG 14
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SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700053
ER
PT J
AU Nyland, K
Marvil, J
Wrobel, JM
Young, LM
Zauderer, BA
AF Nyland, Kristina
Marvil, Josh
Wrobel, J. M.
Young, Lisa M.
Zauderer, B. Ashley
TI THE INTERMEDIATE-MASS BLACK HOLE CANDIDATE IN THE CENTER OF NGC 404: NEW
EVIDENCE FROM RADIO CONTINUUM OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: dwarf; galaxies: individual (NGC 404);
galaxies: nuclei; galaxies: star formation; radio continuum: galaxies
ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; DWARF STARBURST GALAXY;
GLOBULAR-CLUSTER G1; X-RAY-PROPERTIES; FUNDAMENTAL PLANE; STAR-CLUSTERS;
LINER GALAXIES; CENTRAL ENGINE; HENIZE 2-10
AB We present the results of deep, high-resolution, 5 GHz Expanded Very Large Array (EVLA) observations of the nearby, dwarf lenticular galaxy and intermediate-mass black hole candidate (M-BH similar to 4.5 x 10(5) M-circle dot), NGC 404. For the first time, radio emission at frequencies above 1.4 GHz has been detected in this galaxy. We found a modestly resolved source in the NGC 404 nucleus with a total radio luminosity of 7.6 +/- 0.7 x 10(17) W Hz(-1) at 5 GHz and a spectral index from 5 to 7.45 GHz of alpha = -0.88 +/- 0.30. NGC 404 is only the third central intermediate-mass black hole candidate detected in the radio regime with subarcsecond resolution. The position of the radio source is consistent with the optical center of the galaxy and the location of a known, hard X-ray point source (L-X similar to 1.2 x 10(37) erg s(-1)). The faint radio and X-ray emission could conceivably be produced by an X-ray binary, star formation, a supernova remnant, or a low-luminosity active galactic nucleus powered by an intermediate-mass black hole. In light of our new EVLA observations, we find that the most likely scenario is an accreting intermediate-mass black hole, with other explanations being either incompatible with the observed X-ray and/or radio luminosities or statistically unlikely.
C1 [Nyland, Kristina; Marvil, Josh; Young, Lisa M.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Nyland, Kristina; Marvil, Josh; Wrobel, J. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Zauderer, B. Ashley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Nyland, K (reprint author), New Mexico Inst Min & Technol, Dept Phys, 801 Leroy Pl, Socorro, NM 87801 USA.
EM knyland@nmt.edu
FU NRAO; NSF [1109803]
FX We thank the anonymous referee for helpful suggestions that have
improved the clarity and strength of this work. We also thank Anil Seth
for helpful comments and for providing us with coordinate
frame-corrected Hubble Legacy Archive images. The National Radio
Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
This research was partially funded by the NRAO Graduate Summer Student
Research Assistantship Program. We would also like to acknowledge
funding support from NSF grant 1109803.
NR 72
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
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IS 2
AR 103
DI 10.1088/0004-637X/753/2/103
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700010
ER
PT J
AU Offner, SSR
Robitaille, TP
Hansen, CE
McKee, CF
Klein, RI
AF Offner, Stella S. R.
Robitaille, Thomas P.
Hansen, Charles E.
McKee, Christopher F.
Klein, Richard I.
TI OBSERVING SIMULATED PROTOSTARS WITH OUTFLOWS: HOW ACCURATE ARE
PROTOSTELLAR PROPERTIES INFERRED FROM SEDs?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; polarization; radiative transfer; stars: formation;
stars: low-mass; stars: pre-main sequence; stars: winds, outflows
ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; MASS
STAR-FORMATION; SELF-GRAVITATIONAL HYDRODYNAMICS; ADAPTIVE MESH
REFINEMENT; RADIATIVE-TRANSFER; TURBULENT FRAGMENTATION; ACCRETION;
EVOLUTION; OPHIUCHUS
AB The properties of unresolved protostars and their local environment are frequently inferred from spectral energy distributions (SEDs) using radiative transfer modeling. In this paper, we use synthetic observations of realistic star formation simulations to evaluate the accuracy of properties inferred from fitting model SEDs to observations. We use ORION, an adaptive mesh refinement (AMR) three-dimensional gravito-radiation-hydrodynamics code, to simulate low-mass star formation in a turbulent molecular cloud including the effects of protostellar outflows. To obtain the dust temperature distribution and SEDs of the forming protostars, we post-process the simulations using HYPERION, a state-of-the-art Monte Carlo radiative transfer code. We find that the ORION and HYPERION dust temperatures typically agree within a factor of two. We compare synthetic SEDs of embedded protostars for a range of evolutionary times, simulation resolutions, aperture sizes, and viewing angles. We demonstrate that complex, asymmetric gas morphology leads to a variety of classifications for individual objects as a function of viewing angle. We derive best-fit source parameters for each SED through comparison with a pre-computed grid of radiative transfer models. While the SED models correctly identify the evolutionary stage of the synthetic sources as embedded protostars, we show that the disk and stellar parameters can be very discrepant from the simulated values, which is expected since the disk and central source are obscured by the protostellar envelope. Parameters such as the stellar accretion rate, stellar mass, and disk mass show better agreement, but can still deviate significantly, and the agreement may in some cases be artificially good due to the limited range of parameters in the set of model SEDs. Lack of correlation between the model and simulation properties in many individual instances cautions against overinterpreting properties inferred from SEDs for unresolved protostellar sources.
C1 [Offner, Stella S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Robitaille, Thomas P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Hansen, Charles E.; McKee, Christopher F.; Klein, Richard I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[McKee, Christopher F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Klein, Richard I.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
RP Offner, SSR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM soffner@cfa.harvard.edu
OI Robitaille, Thomas/0000-0002-8642-1329
FU NSF [AST-0901055, AST-0908553]; NASA; ATFP [NNX09AK31G]; U.S. Department
of Energy at LLNL [DE-AC52-07NA]; Office of Science of the U.S.
Department of Energy [DE-AC02-05CH11231]
FX The authors thank the anonymous referee for constructive suggestions and
Andrew Cunningham for helpful discussions of protostellar outflows. This
research has been supported by the NSF through grants AST-0901055
(S.S.R.O.) and AST-0908553 (C.F.M. and R.I.K.), by NASA through the
Spitzer Space Telescope Fellowship Program (T.P.R.) and ATFP grant
NNX09AK31G (R.I.K., C.F.M.), and by the U.S. Department of Energy at
LLNL under contract DE-AC52-07NA (R.I.K.). The ORION simulations were
performed on resources managed by the National Energy Research
Scientific Computing Center, which is supported by the Office of Science
of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.
The HYPERION calculations and other data analysis were performed on the
Odyssey cluster, which is supported by the Harvard FAS Sciences Division
Research Computing Group. Figure 2 was rendered using yt (Turk et al.
2011).
NR 61
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
VL 753
IS 2
AR 98
DI 10.1088/0004-637X/753/2/98
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700005
ER
PT J
AU Pe'er, A
Markoff, S
AF Pe'er, Asaf
Markoff, Sera
TI X-RAY EMISSION FROM TRANSIENT JET MODEL IN BLACK HOLE BINARIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radiation mechanisms: non-thermal; stars: winds, outflows; X-rays:
binaries; X-rays: bursts; X-rays: individual (XTE J1118+480)
ID BROAD-BAND SPECTRUM; NOVA XTE J1118+480; SGR-A-ASTERISK;
PARTICLE-ACCELERATION; HARD STATE; GRB 970508; MULTIWAVELENGTH
OBSERVATIONS; SYNCHROTRON EMISSION; ASTROPHYSICAL SHOCKS; RELATIVISTIC
JETS
AB While the non-thermal radio through at least near-infrared emission in the hard state in X-ray binaries (XRBs) is known to originate in jets, the source of the non-thermal X-ray component is still uncertain. We introduce a new model for this emission, which takes into account the transient nature of outflows, and show that it can explain the observed properties of the X-ray spectrum. Rapid radiative cooling of the electrons naturally accounts for the break often seen below around 10 keV, and for the canonical spectral slope F-nu alpha nu(-1/2) observed below the break. We derive the constraints set by the data for both synchrotron- and Compton-dominated models. We show that for the synchrotron-dominated case, the jet should be launched at radii comparable to the inner radius of the disk (similar to few 100 r(s) for the 2000 outburst of XTE J1118+480), with typical magnetic field B greater than or similar to 10(6) G. We discuss the consequences of our results for the possible connection between the inflow and outflow in the hard state of XRBs.
C1 [Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Markoff, Sera] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
RP Pe'er, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Netherlands Organization for Scientific Research (NWO); European
Community [ITN 215212]
FX We thank Dipankar Maitra, Shmulik Balberg, Ramesh Narayan, Jorn Wilms,
and Piergiorgio Casella for useful discussions and comments. A special
thank for Dipankar Maitra for providing us with the reduced data from
the 2000 outburst of XTE J1118+480 (from Hynes et al. 2000). S. M. is
grateful for support from a Netherlands Organization for Scientific
Research (NWO) Vidi Fellowship, and the European Community's Seventh
Framework Programme (FP7/2007-2013) under grant agreement number ITN
215212, "Black Hole Universe."
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
VL 753
IS 2
AR 177
DI 10.1088/0004-637X/753/2/177
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700084
ER
PT J
AU Shen, Y
Liu, X
AF Shen, Yue
Liu, Xin
TI COMPARING SINGLE-EPOCH VIRIAL BLACK HOLE MASS ESTIMATORS FOR LUMINOUS
QUASARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: active; quasars: general
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; BROAD-LINE REGION; AGN
MONITORING PROJECT; HOST-GALAXY STARLIGHT; HIGH-REDSHIFT QUASARS; SURVEY
DATA RELEASE-3; EMISSION-LINE; EDDINGTON RATIO; ASTRONOMICAL DATA
AB Single-epoch virial black hole (BH) mass estimators utilizing broad emission lines have been routinely applied to high-redshift quasars to estimate their BH masses. Depending on the redshift, different line estimators (H alpha, H beta, MgII lambda 2798, CIV lambda 1549) are often used with optical/near-infrared spectroscopy. Here, we use a homogeneous sample of 60 intermediate-redshift (z similar to 1.5-2.2) Sloan Digital Sky Survey quasars with optical and near-infrared spectra covering CIV through H alpha to investigate the consistency between different single-epoch virial BH mass estimators. We critically compare rest-frame UV line estimators (CIV lambda 1549, CIII] lambda 1908, and MgII lambda 2798) with optical estimators (H beta and H alpha) in terms of correlations between line widths and between continuum/line luminosities, for the high-luminosity regime (L-5100 > 10(45.4) erg s(-1)) probed by our sample. The continuum luminosities of L-1350 and L-3000, and the broad-line luminosities are well correlated with L5100, reflecting the homogeneity of quasar spectra in the rest-frame UV-optical, among which L-1350 and the line luminosities for CIV and CIII] have the largest scatter in the correlation with L-5100. We found that the MgII FWHM correlates well with the FWHMs of the Balmer lines and that the MgII line estimator can be calibrated to yield consistent virial mass estimates with those based on the H beta/H alpha estimators, thus extending earlier results on less luminous objects. The CIV FWHM is poorly correlated with the Balmer line FWHMs, and the scatter between the CIV and H beta FWHMs consists of an irreducible part (similar to 0.12 dex), and a part that correlates with the blueshift of the CIV centroid relative to that of H beta, similar to earlier studies comparing CIV with MgII. The CIII] FWHM is found to correlate with the CIV FWHM, and hence is also poorly correlated with the H beta FWHM. While the CIV and CIII] lines can be calibrated to yield consistent virial mass estimates as H beta on average, the scatter is substantially larger than MgII, and the usage of CIV/CIII] FWHM in the mass estimators does not improve the agreement with the H beta estimator. We discuss controversial claims in the literature on the correlation between CIV and H beta FWHMs, and suggest that the reported correlation is either a result based on small samples or only valid for low-luminosity objects.
C1 [Shen, Yue; Liu, Xin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Shen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA.
FU Smithsonian Astrophysical Observatory; NASA through Chandra X-ray Center
[PF0-110076]; NASA [NAS8-03060]; Alfred P. Sloan Foundation; National
Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho;
Max Planck Society; Higher Education Funding Council for England
FX We thank the anonymous referee for constructive comments that led to
improvement of the manuscript, and Michael Strauss, Benny Trakhtenbrot,
Roberto Assef, Kelly Denney, Chris Kochanek, Brad Peterson, and Jenny
Greene for insightful comments on the draft. We also thank Brandon
Kelly, Jenny Greene, and Gordon Richards for useful discussions during
the course of the work, Rob Simcoe for help with the FIRE data reduction
pipeline, and Michael Crushing for help with the TripleSpec data
reduction pipeline. Y.S. acknowledges support from the Smithsonian
Astrophysical Observatory through a Clay Postdoctoral Fellowship.
Support for the work of X. L. was provided by NASA through Einstein
Postdoctoral Fellowship grant number PF0-110076 awarded by the Chandra
X-ray Center, which is operated by the Smithsonian Astrophysical
Observatory for NASA under contract NAS8-03060.; Funding for the SDSS
and SDSS-II has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, the U.S.
Department of Energy, the National Aeronautics and Space Administration,
the Japanese Monbukagakusho, the Max Planck Society, and the Higher
Education Funding Council for England. The SDSS Web site is
http://www.sdss.org/.
NR 88
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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 JUL 10
PY 2012
VL 753
IS 2
AR 125
DI 10.1088/0004-637X/753/2/125
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700032
ER
PT J
AU Stanford, SA
Brodwin, M
Gonzalez, AH
Zeimann, G
Stern, D
Dey, A
Eisenhardt, PR
Snyder, GF
Mancone, C
AF Stanford, S. A.
Brodwin, M.
Gonzalez, Anthony H.
Zeimann, Greg
Stern, Daniel
Dey, Arjun
Eisenhardt, P. R.
Snyder, Gregory F.
Mancone, C.
TI IDCS J1426.5+3508: DISCOVERY OF A MASSIVE, INFRARED-SELECTED GALAXY
CLUSTER AT z=1.75
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual; galaxies: distances and redshifts;
galaxies: evolution
ID IRAC SHALLOW SURVEY; WIDE-FIELD SURVEY; PROBE; DEEP; CONSTRAINTS;
EXTRACTION; RESOLUTION; SOFTWARE; XBOOTES; PROFILE
AB We report the discovery of an IR-selected massive galaxy cluster in the IRAC Deep Cluster Survey (IDCS). We present new data from the Hubble Space Telescope and the W. M. Keck Observatory that spectroscopically confirm IDCS J1426.5+3508 at z = 1.75. Moreover, the cluster is detected in archival Chandra data as an extended X-ray source, comprising 53 counts after the removal of point sources. We calculate an X-ray luminosity of L0.5-2 keV = (5.4 +/- 1.2) x 10(44) erg s(-1) within r = 60 arcsec (similar to 1 Mpc diameter), which implies M-200,M- Lx = (5.3 +/- 1.6) x 10(14) M-circle dot. IDCS J1426.5+3508 appears to be an exceptionally massive cluster for its redshift.
C1 [Stanford, S. A.; Zeimann, Greg] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Stanford, S. A.; Snyder, Gregory F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gonzalez, Anthony H.; Mancone, C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Stern, Daniel; Eisenhardt, P. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Stanford, SA (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA.
EM stanford@physics.ucdavis.edu
FU NASA [G09-0150A, NAS 5-26555]; National Science Foundation
[AST-0708490]; NASA by JPL/Caltech; NASA through a grant from the Space
Telescope Science Institute [11663, 12203]; W. M. Keck Foundation; U. S.
Department of Energy [W-7405-ENG-48]; [SV4-74018, A31]
FX This work is based in part on observations obtained with the Chandra
X-Ray Observatory (Chandra), under contract SV4-74018, A31 with the
Smithsonian Astrophysical Observatory which operates Chandra for NASA.
Support for this research was provided by the NASA grant G09-0150A.
A.H.G. acknowledges support from the National Science Foundation through
grant AST-0708490. This work is based in part on observations made with
the Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was provided by NASA through an award issued
by JPL/Caltech. Support for HST programs 11663 and 12203 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. Some of the data
presented here were obtained at the W. M. Keck Observatory, which is
operated as a scientific partnership among the California Institute of
Technology, the University of California, and the National Aeronautics
and Space Administration. The Observatory was made possible by the
generous financial support of the W. M. Keck Foundation. This work makes
use of image data from the NOAO Deep Wide-Field Survey (NDWFS) as
distributed by the NOAO Science Archive. NOAO is operated by the
Association of Universities for Research in Astronomy (AURA), Inc.,
under a cooperative agreement with the National Science Foundation.; We
thank Matt Ashby for creating the IRAC catalogs for SDWFS, Buell Jannuzi
for his work on the NDWFS, Michael Brown for combining the NDWFS with
SDWFS catalogs, Steve Murray and his XBootes team for obtaining the
Chandra data in the Bootes field, and Alexey Vihklinin for advice on the
analysis of the Chandra data. We also thank the referee for a report
which helped to improve the presentation and interpretation of the
results. This paper would not have been possible without the efforts of
the support staffs of the Keck Observatory, the Spitzer Space Telescope,
the Hubble Space Telescope, and the Chandra X-Ray Observatory. Support
for M. B. was provided by the W. M. Keck Foundation. The work by S.A.S.
at LLNL was performed under the auspices of the U. S. Department of
Energy under Contract No. W-7405-ENG-48.
NR 47
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
VL 753
IS 2
AR 164
DI 10.1088/0004-637X/753/2/164
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700071
ER
PT J
AU Yuan, Y
Neufeld, DA
Sonnentrucker, P
Melnick, GJ
Watson, DM
AF Yuan, Yuan
Neufeld, David A.
Sonnentrucker, Paule
Melnick, Gary J.
Watson, Dan M.
TI SPITZER OBSERVATIONS OF SHOCK-EXCITED HYDROGEN DEUTERIDE IN IC 443C, HH
7, AND HH 54: PROBING THE GAS-PHASE DEUTERIUM ABUNDANCE IN THE DENSE
INTERSTELLAR MEDIUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: abundances; ISM: clouds; ISM: molecules; molecular processes; shock
waves
ID MOLECULAR-HYDROGEN; GALACTIC DISK; HD MOLECULES; ROTATIONAL-EXCITATION;
BARYON DENSITY; HIGH-REDSHIFT; BASIC DATA; LINE; RATIO; IC-443
AB We present and analyze observations-carried out using the Infrared Spectrograph (IRS) on the Spitzer Space Telescope-of the R(3) and R(4) pure rotational lines of hydrogen deuteride (HD) detected from shock-heated material associated with the supernova remnant IC 443C and with the Herbig-Haro objects HH 7 and HH 54. Assuming a continuous temperature distribution for gas observed along the sight lines, we have constrained the gas density to be in the similar to 10(3)-10(4) cm(-3) range, using both spectroscopic data for H-2, HD, and CO from IRS and from the Infrared Space Observatory (ISO), as well as photometric data from Spitzer's Infrared Array Camera. The derived HD abundance relative to H-2 is quite sensitive to the assumed excitation conditions in the emitting gas. Assuming that HD accounts for all gas-phase deuterium in the emitting material, and using all the available spectroscopic data to constrain the excitation conditions, we obtained gas-phase deuterium abundances [D/H](gas) of 0.95(-0.27)(+0.54) x 10(-5) and 0.87(-0.27)(+0.31) x 10(-5) (statistical errors only) for IC 443C and HH 54, respectively. The uncertainties in the HD abundance are dominated by systematic effects related to the poorly known excitation conditions, and more accurate estimates of the HD abundance in shocked molecular clouds will require measurements of the emission in additional HD rotational transitions.
C1 [Yuan, Yuan; Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Sonnentrucker, Paule] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Watson, Dan M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
RP Yuan, Y (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
NR 55
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
VL 753
IS 2
AR 126
DI 10.1088/0004-637X/753/2/126
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700033
ER
PT J
AU Zappacosta, L
Nicastro, F
Krongold, Y
Maiolino, R
AF Zappacosta, L.
Nicastro, F.
Krongold, Y.
Maiolino, R.
TI AN X-RAY WHIM METAL ABSORBER FROM A Mpc-SCALE EMPTY REGION OF SPACE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (H 2356-309); intergalactic medium;
large-scale structure of universe; quasars: absorption lines;
techniques: spectroscopic; X-rays: galaxies: clusters
ID HOT INTERGALACTIC MEDIUM; BL LACERTAE OBJECTS; ABSORPTION-LINES;
SCULPTOR WALL; BARYONS; FILAMENT; GALAXIES; CLUSTERS; FOREST; MASS
AB We report a detection of an absorption line at similar to 44.8 angstrom in a > 500 ks Chandra HRC-S/LETG X-ray grating spectrum of the blazar H 2356-309. This line can be identified as intervening Cv-K alpha absorption, at z approximate to 0.112, produced by a warm (log T = 5.1 K) intergalactic absorber. The feature is significant at a 2.9 sigma level (accounting for the number of independent redshift trials). We estimate an equivalent hydrogen column density of log N-H = 19.05(Z/Z(circle dot))(-1) cm(-2). Unlike other previously reported FUV/X-ray metal detections of warm-hot intergalactic medium (WHIM), this C v absorber lies in a region with locally low galaxy density, at similar to 2.2 Mpc from the closest galaxy at that redshift, and therefore is unlikely to be associated with an extended galactic halo. We instead tentatively identify this absorber with an intervening WHIM filament possibly permeating a large-scale, 30 Mpc extended, structure of galaxies whose redshift centroid, within a cylinder of 7.5 Mpc radius centered on the line of sight to H 2356-309, is marginally consistent (at a 1.8 sigma level) with the redshift of the absorber.
C1 [Zappacosta, L.; Nicastro, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Nicastro, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Krongold, Y.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Maiolino, R.] Cavendish Lab, Astrophys Grp, Cambridge CB3 OHE, England.
RP Zappacosta, L (reprint author), INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
EM luca.zappacosta@oa-roma.inaf.it
OI Nicastro, Fabrizio/0000-0002-6896-1364
NR 27
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2012
VL 753
IS 2
AR 137
DI 10.1088/0004-637X/753/2/137
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 967MR
UT WOS:000305912700044
ER
PT J
AU Fletcher, RJ
Orrock, JL
Robertson, BA
AF Fletcher, Robert J., Jr.
Orrock, John L.
Robertson, Bruce A.
TI How the type of anthropogenic change alters the consequences of
ecological traps
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE attractive sink; evolutionary trap; habitat selection; maladaptation;
Price equation; rapid evolution
ID HABITAT SELECTION; UNDERVALUED RESOURCES; POPULATION-DYNAMICS;
EVOLUTIONARY TRAPS; QUANTITATIVE TRAIT; CLIMATE-CHANGE; CONSERVATION;
ENVIRONMENT; COVARIANCE; EXTINCTION
AB Understanding altered ecological and evolutionary dynamics in novel environments is vital for predicting species responses to rapid environmental change. One fundamental concept relevant to such dynamics is the ecological trap, which arises from rapid anthropogenic change and can facilitate extinction. Ecological traps occur when formerly adaptive habitat preferences become maladaptive because the cues individuals preferentially use in selecting habitats lead to lower fitness than other alternatives. While it has been emphasized that traps can arise from different types of anthropogenic change, the resulting consequences of these different types of traps remain unknown. Using a novel model framework that builds upon the Price equation from evolutionary genetics, we provide the first analysis that contrasts the ecological and evolutionary consequences of ecological traps arising from two general types of perturbations known to trigger traps. Our model suggests that traps arising from degradation of existing habitats are more likely to facilitate extinction than those arising from the addition of novel trap habitat. Importantly, our framework reveals the mechanisms of these outcomes and the substantial scope for persistence via rapid evolution that may buffer many populations from extinction, helping to resolve the paradox of continued persistence of many species in dramatically altered landscapes.
C1 [Fletcher, Robert J., Jr.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA.
[Orrock, John L.] Univ Wisconsin, Dept Zool, Madison, WI 53706 USA.
[Robertson, Bruce A.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA.
RP Fletcher, RJ (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, POB 110430,110 Newins Ziegler Hall, Gainesville, FL 32611 USA.
EM robert.fletcher@ufl.edu
OI Fletcher, Robert/0000-0003-1717-5707
FU USDA-NRI [2006-55101-17158]; PPL-Montana
FX R.J.F. was supported by grants from the USDA-NRI (no. 2006-55101-17158)
and PPL-Montana. M. Patten, C. W. Miller and anonymous reviewers
provided valuable comments on previous versions of this manuscript,
which improved the ideas presented here.
NR 47
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U1 5
U2 95
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
EI 1471-2954
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD JUL 7
PY 2012
VL 279
IS 1738
BP 2546
EP 2552
DI 10.1098/rspb.2012.0139
PG 7
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 947TF
UT WOS:000304453000008
PM 22378802
ER
PT J
AU Barkley, MP
Kurosu, TP
Chance, K
De Smedt, I
Van Roozendael, M
Arneth, A
Hagberg, D
Guenther, A
AF Barkley, Michael P.
Kurosu, Thomas P.
Chance, Kelly
De Smedt, Isabelle
Van Roozendael, Michel
Arneth, Almut
Hagberg, Daniel
Guenther, Alex
TI Assessing sources of uncertainty in formaldehyde air mass factors over
tropical South America: Implications for top-down isoprene emission
estimates
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; RETRIEVAL; MODEL; PHOTOOXIDATION;
SCIAMACHY; COLUMNS; SPACE; MEGAN; BAND; NM
AB We use a nested-grid version of the GEOS-Chem chemistry transport model, constrained by isoprene emissions from the Model of Emissions of Gases and Aerosols from Nature (MEGAN), and the Lund-Potsdam-Jena General Ecosystem Simulator (LPJ-GUESS) bottom-up inventories, to evaluate the impact that surface isoprene emissions have on formaldehyde (HCHO) air-mass factors (AMFs) and vertical column densities (VCDs) over tropical South America during 2006, as observed by the Scanning Imaging Absorption Spectrometer for Atmospheric Chartography (SCIAMACHY) and Ozone Monitoring Instrument (OMI). Although the large-scale seasonal variability of monthly mean HCHO VCDs is typically unaffected by the choice of bottom-up inventory, large relative differences of up to +/- 45% in the HCHO VCD can occur for individual regions and months, but typically most VCD differences are of order +/- 20%. These relative changes are comparable to those produced by other sources of uncertainty in the AMF including aerosols and surface albedo, but less than those from clouds. In a sensitivity test, we find that top-down annual isoprene emissions inferred from SCIAMACHY and OMI HCHO vertical columns can vary by as much as +/- 30-50% for each instrument respectively, depending on the region studied and the a priori isoprene emissions used. Our analysis suggests that the influence of the a priori isoprene emissions on HCHO AMFs and VCDs is therefore non-negligible and must be carefully considered when inferring top-down isoprene emissions estimates over this, or potentially any other, region.
C1 [Barkley, Michael P.] Univ Leicester, Dept Phys & Astron, EOS Grp, Leicester LE1 7RH, Leics, England.
[Kurosu, Thomas P.; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[De Smedt, Isabelle; Van Roozendael, Michel] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium.
[Arneth, Almut; Hagberg, Daniel] Lund Univ, Dept Phys Geog & Ecosyst Anal, Geobiosphere Sci Ctr, Lund, Sweden.
[Arneth, Almut] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Karlsruhe, Germany.
[Guenther, Alex] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
RP Barkley, MP (reprint author), Univ Leicester, Dept Phys & Astron, EOS Grp, Univ Rd, Leicester LE1 7RH, Leics, England.
EM mpb14@le.ac.uk
RI Arneth, Almut/B-2702-2013; Chem, GEOS/C-5595-2014;
OI Chance, Kelly/0000-0002-7339-7577
FU Natural Environment Research Council [NE/GE013810/2]; Swedish Research
Council Formas
FX This work was supported by the Natural Environment Research Council
(grant NE/GE013810/2). A. A. and D. H. acknowledge support from the
Swedish Research Council Formas.
NR 32
TC 13
Z9 13
U1 1
U2 32
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUL 6
PY 2012
VL 117
AR D13304
DI 10.1029/2011JD016827
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 971WX
UT WOS:000306237700002
ER
PT J
AU Toth, LT
Aronson, RB
Vollmer, SV
Hobbs, JW
Urrego, DH
Cheng, H
Enochs, IC
Combosch, DJ
van Woesik, R
Macintyre, IG
AF Toth, Lauren T.
Aronson, Richard B.
Vollmer, Steven V.
Hobbs, Jennifer W.
Urrego, Dunia H.
Cheng, Hai
Enochs, Ian C.
Combosch, David J.
van Woesik, Robert
Macintyre, Ian G.
TI ENSO Drove 2500-Year Collapse of Eastern Pacific Coral Reefs
SO SCIENCE
LA English
DT Article
ID NINO-SOUTHERN-OSCILLATION; EL-NINO; CLIMATE-CHANGE; TROPICAL PACIFIC;
OCEAN ACIDIFICATION; HOLOCENE; RECORD; GROWTH; SEA; DISTURBANCES
AB Cores of coral reef frameworks along an upwelling gradient in Panama show that reef ecosystems in the tropical eastern Pacific collapsed for 2500 years, representing as much as 40% of their history, beginning about 4000 years ago. The principal cause of this millennial-scale hiatus in reef growth was increased variability of the El Nino-Southern Oscillation (ENSO) and its coupling with the Intertropical Convergence Zone. The hiatus was a Pacific-wide phenomenon with an underlying climatology similar to probable scenarios for the next century. Global climate change is probably driving eastern Pacific reefs toward another regional collapse.
C1 [Toth, Lauren T.; Aronson, Richard B.; Hobbs, Jennifer W.; Urrego, Dunia H.; van Woesik, Robert] Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA.
[Aronson, Richard B.; Macintyre, Ian G.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Vollmer, Steven V.; Combosch, David J.] Northeastern Univ, Ctr Marine Sci, Nahant, MA 01908 USA.
[Urrego, Dunia H.] Univ Bordeaux 1, UMR CNRS EPOC 5805, F-33405 Talence, France.
[Cheng, Hai] Xi An Jiao Tong Univ, Inst Global Environm Change, Xian 710049, Peoples R China.
[Cheng, Hai] Univ Minnesota, Dept Geol & Geophys, Minneapolis, MN 55455 USA.
[Enochs, Ian C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Cooperat Inst Marine & Atmospher Sci, Miami, FL 33149 USA.
[Enochs, Ian C.] NOAA, Atlantic Oceanog & Meteorol Labs, Miami, FL 33149 USA.
RP Aronson, RB (reprint author), Florida Inst Technol, Dept Biol Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA.
EM raronson@fit.edu
RI Enochs, Ian/B-8051-2014; Chen, Hua/B-7664-2014;
OI Enochs, Ian/0000-0002-8867-0361; Chen, Hua/0000-0002-9493-6939;
Combosch, David/0000-0001-7004-7435
FU Smithsonian Institution; NSF; Florida Institute of Technology
FX We thank M. Bush, A. Correa-Metrio, P. Glynn, H. Lessios, D. Manzello,
W. Precht, and P. Reimer for advice and V. Brandtneris, L. Camilli, M.
Dardeau, K. Hendrickson, A. Lam, A. Moesinger, R. Muthukrishnan, E.
Ochoa, J. Reynolds, B. Valencia, and A. Velarde for assistance.
Supported by the Smithsonian Institution, NSF, and the Florida Institute
of Technology. This research was carried out under permits from the
Republic of Panama. Data are available online in NOAA's Paleoclimatology
database (www.ncdc.noaa.gov/paleo/).
NR 34
TC 44
Z9 45
U1 1
U2 80
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JUL 6
PY 2012
VL 337
IS 6090
BP 81
EP 84
DI 10.1126/science.1221168
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 969KC
UT WOS:000306053100048
PM 22767927
ER
PT J
AU Dasmahapatra, KK
Walters, JR
Briscoe, AD
Davey, JW
Whibley, A
Nadeau, NJ
Zimin, AV
Hughes, DST
Ferguson, LC
Martin, SH
Salazar, C
Lewis, JJ
Adler, S
Ahn, SJ
Baker, DA
Baxter, SW
Chamberlain, NL
Chauhan, R
Counterman, BA
Dalmay, T
Gilbert, LE
Gordon, K
Heckel, DG
Hines, HM
Hoff, KJ
Holland, PWH
Jacquin-Joly, E
Jiggins, FM
Jones, RT
Kapan, DD
Kersey, P
Lamas, G
Lawson, D
Mapleson, D
Maroja, LS
Martin, A
Moxon, S
Palmer, WJ
Papa, R
Papanicolaou, A
Pauchet, Y
Ray, DA
Rosser, N
Salzberg, SL
Supple, MA
Surridge, A
Tenger-Trolander, A
Vogel, H
Wilkinson, PA
Wilson, D
Yorke, JA
Yuan, FR
Balmuth, AL
Eland, C
Gharbi, K
Thomson, M
Gibbs, RA
Han, Y
Jayaseelan, JC
Kovar, C
Mathew, T
Muzny, DM
Ongeri, F
Pu, LL
Qu, JX
Thornton, RL
Worley, KC
Wu, YQ
Linares, M
Blaxter, ML
Ffrench-Constant, RH
Joron, M
Kronforst, MR
Mullen, SP
Reed, RD
Scherer, SE
Richards, S
Mallet, J
McMillan, WO
Jiggins, CD
AF Dasmahapatra, Kanchon K.
Walters, James R.
Briscoe, Adriana D.
Davey, John W.
Whibley, Annabel
Nadeau, Nicola J.
Zimin, Aleksey V.
Hughes, Daniel S. T.
Ferguson, Laura C.
Martin, Simon H.
Salazar, Camilo
Lewis, James J.
Adler, Sebastian
Ahn, Seung-Joon
Baker, Dean A.
Baxter, Simon W.
Chamberlain, Nicola L.
Chauhan, Ritika
Counterman, Brian A.
Dalmay, Tamas
Gilbert, Lawrence E.
Gordon, Karl
Heckel, David G.
Hines, Heather M.
Hoff, Katharina J.
Holland, Peter W. H.
Jacquin-Joly, Emmanuelle
Jiggins, Francis M.
Jones, Robert T.
Kapan, Durrell D.
Kersey, Paul
Lamas, Gerardo
Lawson, Daniel
Mapleson, Daniel
Maroja, Luana S.
Martin, Arnaud
Moxon, Simon
Palmer, William J.
Papa, Riccardo
Papanicolaou, Alexie
Pauchet, Yannick
Ray, David A.
Rosser, Neil
Salzberg, Steven L.
Supple, Megan A.
Surridge, Alison
Tenger-Trolander, Ayse
Vogel, Heiko
Wilkinson, Paul A.
Wilson, Derek
Yorke, James A.
Yuan, Furong
Balmuth, Alexi L.
Eland, Cathlene
Gharbi, Karim
Thomson, Marian
Gibbs, Richard A.
Han, Yi
Jayaseelan, Joy C.
Kovar, Christie
Mathew, Tittu
Muzny, Donna M.
Ongeri, Fiona
Pu, Ling-Ling
Qu, Jiaxin
Thornton, Rebecca L.
Worley, Kim C.
Wu, Yuan-Qing
Linares, Mauricio
Blaxter, Mark L.
Ffrench-Constant, Richard H.
Joron, Mathieu
Kronforst, Marcus R.
Mullen, Sean P.
Reed, Robert D.
Scherer, Steven E.
Richards, Stephen
Mallet, James
McMillan, W. Owen
Jiggins, Chris D.
CA Heliconius Genome Consortium
TI Butterfly genome reveals promiscuous exchange of mimicry adaptations
among species
SO NATURE
LA English
DT Article
ID HELICONIUS BUTTERFLIES; ADAPTIVE RADIATION; PATTERN MIMICRY;
BOMBYX-MORI; GENE FLOW; EVOLUTION; HYBRIDIZATION; SYNTENY; LEPIDOPTERA;
SPECIATION
AB The evolutionary importance of hybridization and introgression has long been debated(1). Hybrids are usually rare and unfit, but even infrequent hybridization can aid adaptation by transferring beneficial traits between species. Here we use genomic tools to investigate introgression in Heliconius, a rapidly radiating genus of neotropical butterflies widely used in studies of ecology, behaviour, mimicry and speciation(2-5). We sequenced the genome of Heliconius melpomene and compared it with other taxa to investigate chromosomal evolution in Lepidoptera and gene flow among multiple Heliconius species and races. Among 12,669 predicted genes, biologically important expansions of families of chemosensory and Hox genes are particularly noteworthy. Chromosomal organization has remained broadly conserved since the Cretaceous period, when butterflies split from the Bombyx (silkmoth) lineage. Using genomic resequencing, we show hybrid exchange of genes between three co-mimics, Heliconius melpomene, Heliconius timareta and Heliconius elevatus, especially at two genomic regions that control mimicry pattern. We infer that closely related Heliconius species exchange protective colour-pattern genes promiscuously, implying that hybridization has an important role in adaptive radiation.
C1 [Dasmahapatra, Kanchon K.; Rosser, Neil; Mallet, James] UCL, Dept Genet Evolut & Environm, London WC1E 6BT, England.
[Walters, James R.; Nadeau, Nicola J.; Martin, Simon H.; Salazar, Camilo; Baxter, Simon W.; Surridge, Alison; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England.
[Briscoe, Adriana D.; Lewis, James J.; Martin, Arnaud; Yuan, Furong; Reed, Robert D.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA.
[Davey, John W.; Blaxter, Mark L.] Univ Edinburgh, Inst Evolutionary Biol, Ashworth Labs, Edinburgh EH9 3JT, Midlothian, Scotland.
[Whibley, Annabel; Jones, Robert T.; Joron, Mathieu] Museum Natl Hist Nat, CNRS UMR 7205, F-75005 Paris, France.
[Zimin, Aleksey V.; Yorke, James A.] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA.
[Hughes, Daniel S. T.; Kersey, Paul; Lawson, Daniel; Wilson, Derek] European Bioinformat Inst, Hinxton CB10 1SD, England.
[Ferguson, Laura C.; Holland, Peter W. H.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England.
[Salazar, Camilo; McMillan, W. Owen; Jiggins, Chris D.] Smithsonian Trop Res Inst, Panama City, Panama.
[Adler, Sebastian; Hoff, Katharina J.] Ernst Moritz Arndt Univ Greifswald, Inst Math & Informat, D-17487 Greifswald, Germany.
[Ahn, Seung-Joon; Heckel, David G.; Pauchet, Yannick; Vogel, Heiko] Max Planck Inst Chem Biol, D-07745 Jena, Germany.
[Baker, Dean A.] Univ London Imperial Coll Sci Technol & Med, London SW7 2AZ, England.
[Chamberlain, Nicola L.; Tenger-Trolander, Ayse; Kronforst, Marcus R.] Harvard Univ, FAS Ctr Syst Biol, Cambridge, MA 02138 USA.
[Chauhan, Ritika; Ffrench-Constant, Richard H.] Univ Exeter, Sch Biosci, Ctr Ecol & Conservat, Penryn TR10 9EZ, England.
[Counterman, Brian A.] Mississippi State Univ, Dept Biol, Mississippi State, MS 39762 USA.
[Dalmay, Tamas] Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England.
[Gilbert, Lawrence E.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Gilbert, Lawrence E.] Univ Texas Austin, Brackenridge Field Lab, Austin, TX 78712 USA.
[Gordon, Karl; Papanicolaou, Alexie] CSIRO Ecosyst Sci, Black Mt Labs, Canberra, ACT 2601, Australia.
[Hines, Heather M.] N Carolina State Univ, Dept Genet, Raleigh, NC 27695 USA.
[Jacquin-Joly, Emmanuelle] Univ Paris 06, INRA, UMR A 1272, F-78026 Versailles, France.
[Jiggins, Francis M.; Palmer, William J.] Univ Cambridge, Dept Genet, Cambridge CB2 3EH, England.
[Kapan, Durrell D.] Calif Acad Sci, Dept Entomol, Ctr Comparat Genom, San Francisco, CA 94118 USA.
[Kapan, Durrell D.] Univ Hawaii Manoa, Pacific Biosci Res Ctr, Ctr Conservat & Res Training, Honolulu, HI 96822 USA.
[Lamas, Gerardo] Univ Nacl Mayor San Marcos, Museo Hist Nat, Lima 14, Peru.
[Mapleson, Daniel; Maroja, Luana S.] Univ E Anglia, Sch Comp Sci, Norwich NR4 7TJ, Norfolk, England.
[Maroja, Luana S.] Williams Coll, Dept Biol, Williamstown, MA 01267 USA.
[Moxon, Simon] Yale Univ, Sch Med, Dept Genet, New Haven, CT 06520 USA.
[Papa, Riccardo] Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA.
[Ray, David A.] Mississippi State Univ, Dept Biochem Mol Biol Entomol & Plant Pathol, Mississippi State, MS 39762 USA.
[Ray, David A.] Mississippi State Univ, Inst Genom Biocomp & Biotechnol, Mississippi State, MS 39759 USA.
[Salzberg, Steven L.] Johns Hopkins Univ, McKusick Nathans Inst Genet Med, Baltimore, MD 21205 USA.
[Supple, Megan A.] N Carolina State Univ, Biomath Program, Raleigh, NC 27695 USA.
[Wilkinson, Paul A.] Univ Bristol, Sch Biol Sci, Bristol BS8 1UG, Avon, England.
[Balmuth, Alexi L.; Eland, Cathlene; Gharbi, Karim; Thomson, Marian; Blaxter, Mark L.] Univ Edinburgh, Ashworth Labs, Edinburgh EH9 3JT, Midlothian, Scotland.
[Gibbs, Richard A.; Han, Yi; Jayaseelan, Joy C.; Kovar, Christie; Mathew, Tittu; Muzny, Donna M.; Ongeri, Fiona; Pu, Ling-Ling; Qu, Jiaxin; Thornton, Rebecca L.; Worley, Kim C.; Wu, Yuan-Qing; Scherer, Steven E.; Richards, Stephen] Baylor Coll Med, Human GenomeSequencing Ctr, Houston, TX 77030 USA.
[Linares, Mauricio] Univ Nacl Rosario, Fac Ciencias Nat & Matemat, Bogota, Colombia.
[Linares, Mauricio] Univ Los Andes, Inst Genet, Bogota, Colombia.
[Mullen, Sean P.] Boston Univ, Dept Biol, Boston, MA 02215 USA.
[Mallet, James] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
RP Mallet, J (reprint author), UCL, Dept Genet Evolut & Environm, Gower St, London WC1E 6BT, England.
EM jmallet@oeb.harvard.edu
RI JAYASEELAN, JOY CHRISTINA/F-9824-2015; Blaxter, Mark/B-4113-2010;
Linares, Mauricio/I-3509-2016; Salzberg, Steven/F-6162-2011; Gordon,
Karl/A-1976-2008; Moxon, Simon/A-5385-2010; mallet, james/B-5114-2008;
Briscoe, Adriana/E-8963-2010; GenePool, The/D-8812-2012; Joron,
Mathieu/C-9178-2009; Papanicolaou, Alexie/A-1618-2011; Jiggins,
Chris/B-9960-2008; Nadeau, Nicola/E-1149-2011; Davey, John/B-5075-2013;
Gharbi, Karim/C-5771-2012; Salazar, camilo/A-1647-2010; Heckel,
David/K-2138-2013
OI Lamas, Gerardo/0000-0002-3664-6730; Ahn, Seung-Joon/0000-0002-5980-106X;
Jiggins, Francis Michael/0000-0001-7470-8157; Holland,
Peter/0000-0003-1533-9376; Kersey, Paul/0000-0002-7054-800X; Pauchet,
Yannick/0000-0002-2918-8946; Dasmahapatra, Kanchon
Kumar/0000-0002-2840-7019; JAYASEELAN, JOY
CHRISTINA/0000-0002-7759-0139; Blaxter, Mark/0000-0003-2861-949X;
Linares, Mauricio/0000-0002-1021-0226; Salzberg,
Steven/0000-0002-8859-7432; Gordon, Karl/0000-0002-4371-0454;
ffrench-Constant, Richard/0000-0001-5385-9888; Lawson,
Daniel/0000-0001-7765-983X; Davey, John/0000-0002-1017-9775; Mallet,
James/0000-0002-3370-0367; Briscoe, Adriana/0000-0001-8514-4983; Joron,
Mathieu/0000-0003-1043-4147; Papanicolaou, Alexie/0000-0002-3635-6848;
Jiggins, Chris/0000-0002-7809-062X; Nadeau, Nicola/0000-0002-9319-921X;
Gharbi, Karim/0000-0003-1092-4488; Salazar, camilo/0000-0001-9217-6588;
Heckel, David/0000-0001-8991-2150
FU Leverhulme Trust; John Fell Fund; Christ Church College, Oxford; Royal
Society; NSF; NIH; CNRS; ERC; Banco de la Republica; COLCIENCAS; BBSRC
FX We thank the governments of Colombia, Peru and Panama for permission to
collect the butterflies. Sequencing was funded by contributions from
consortium members. We thank M. Abanto for assistance in raising the
inbred line. Individual laboratories were funded by the Leverhulme Trust
(C.D.J.), the John Fell Fund and Christ Church College, Oxford (L. C.
F.), The Royal Society (M.J., C.D.J.), the NSF (W.O.M., M. R. K., R. D.
R., S. M., A. D. B.), the NIH (M. R. K., S. L. S., J.A.Y.), the CNRS
(M.J.), the ERC (M.J., P. W. H. H.), the Banco de la Republica and
COLCIENCAS (M. L.) and the BBSRC (J.M., C.D.J., M.L.B. and R.H.f.-C.).
NR 27
TC 371
Z9 468
U1 29
U2 382
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUL 5
PY 2012
VL 487
IS 7405
BP 94
EP 98
DI 10.1038/nature11041
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 968LM
UT WOS:000305982900057
ER
PT J
AU Liertzer, M
Feist, J
Nagele, S
Burgdorfer, J
AF Liertzer, M.
Feist, J.
Nagele, S.
Burgdoerfer, J.
TI Multielectron Transitions Induced by Neutron Impact on Helium
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID DOUBLE PHOTOIONIZATION; EXCITATION-IONIZATION; MULTIPLE IONIZATION;
COMPTON-SCATTERING; CROSS-SECTIONS; PHOTON; ATOMS
AB We explore excitation and ionization by neutron impact as a novel tool for the investigation of electron-electron correlations in helium. We present single-and double-ionization spectra calculated in accurate numerical ab initio simulations for incoming neutrons with kinetic energies of up to 150 keV. The resulting electron spectra are found to be fundamentally different from photoionization or charged particle impact due to the intrinsic many-body character of the interaction. In particular, doubly excited resonances that are strongly suppressed in electron or photon impact become prominent. The ratio of double to single ionization is found to differ significantly from those of photon and charged-particle impact.
C1 [Liertzer, M.; Nagele, S.; Burgdoerfer, J.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria.
[Feist, J.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Liertzer, M (reprint author), Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria.
EM matthias.liertzer@tuwien.ac.at
RI Nagele, Stefan/E-6938-2011; Feist, Johannes/J-7394-2012
OI Nagele, Stefan/0000-0003-1213-0294; Feist, Johannes/0000-0002-7972-0646
FU FWF-Austria [SFB-041 VICOM, P23359-N16]; NSF; Vienna Science and
Technology Fund (WWTF) [MA09-030]; TACC [TG-PHY090031]
FX We thank B. deHarak for providing us with the data of the
e--He scattering measurements. S. N. and J. B. acknowledge
support by the FWF-Austria, SFB-041 VICOM, and P23359-N16. J. F.
acknowledges support from the NSF through a grant to ITAMP. M. L.
acknowledges funding by the Vienna Science and Technology Fund (WWTF)
through Project No. MA09-030. The computational results have been
achieved using the Vienna Scientific Cluster and NSF TeraGrid/XSEDE
resources provided by NICS and TACC under Grant No. TG-PHY090031.
NR 36
TC 4
Z9 4
U1 0
U2 13
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD JUL 2
PY 2012
VL 109
IS 1
AR 013201
DI 10.1103/PhysRevLett.109.013201
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 967GV
UT WOS:000305895700004
PM 23031102
ER
PT J
AU Kabat, AR
Hershler, R
Gonzalez-Guillen, A
AF Kabat, Alan R.
Hershler, Robert
Gonzalez-Guillen, Adrian
TI Resolution of taxonomic problems associated with the complex publication
history of the seminal Torre and Bartsch monograph on Cuban Urocoptidae
(Gastropoda, Pulmonata)
SO ZOOTAXA
LA English
DT Article
DE Urocoptoidea; land snails; Caribbean; biodiversity; taxonomy;
nomenclature
ID CERION
AB This paper clarifies the confusion relating to the publication of Carlos de la Torre & Paul Bartsch's taxonomic study of the Cuban Urocoptidae. This massive work, which described >500 new taxa, was completed in manuscript form in 1943, but was not published during the authors' lifetime. In 1972 Miguel Jaume and Alfredo de la Torre (a nephew of C. de la Torre) published a slightly modified version of a large portion of this manuscript in the Circulares del Museo y Biblioteca de Zoologa de la Habana, a mimeographed journal which is available for taxonomic purposes per ICZN Code Article 8. The 420 new taxa introduced in this paper were made available under the ICZN Code (even though many were differentiated only in identification keys) and should be attributed to C. de la Torre & Bartsch because the descriptions were copied from the 1943 manuscript and Jaume & A. de la Torre explicitly credited this work to the former two authors (per Article 50 of the 1964 edition of the ICZN Code). The 1972 paper does not delineate type material for most of the new species-group taxa; however the detailed information provided in the 1943 manuscript constitutes valid evidence of the type series per ICZN Code (1999) Article 72.2. The 1972 paper was republished by Jaume & A. de la Torre in 1976 in the Ciencias Biologicas of the Universidad de la Habana. In 1980 Jaume & A. de la Torre prepared a typescript describing the remaining new taxa from the 1943 manuscript, which was slated to be published in the Circulares; however we have not found any evidence that it was distributed or otherwise made available in a manner satisfying the ICZN Code criteria for availability. In 2008 Carolina de la Torre, grand-niece of C. de la Torre, published the entire 1943 manuscript in a book of more than 760 pages that was printed in Havana. The authorship of this book was credited to C. de la Torre & Bartsch. The book describes as new the taxa already treated in the 1972 paper as well as 130 additional taxa, which also should be attributed to C. de la Torre & Bartsch. We briefly discuss the disposition of the Cuban urocoptid material studied by C. de la Torre & Bartsch and the subsequent citations to their taxonomic study of this fauna.
C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Kabat, Alan R.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA.
RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012, Washington, DC 20013 USA.
EM alankabat@aol.com; hershlerr@si.edu; adrian.polymita@gmail.com
NR 50
TC 0
Z9 0
U1 2
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 JUL 2
PY 2012
IS 3362
BP 43
EP 53
PG 11
WC Zoology
SC Zoology
GA 967CB
UT WOS:000305882600002
ER
PT J
AU Shurakov, A
Seliverstov, S
Kaurova, N
Finkel, M
Voronov, B
Goltsman, G
AF Shurakov, Alexander
Seliverstov, Sergey
Kaurova, Natalia
Finkel, Matvey
Voronov, Boris
Goltsman, Gregory
TI Input Bandwidth of Hot Electron Bolometer With Spiral Antenna
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Hot electron bolometer (HEB); terahertz (THz) region; ultra wideband
antennas
AB We report the results of our study of the input bandwidth of hot electron bolometers (HEB) embedded into the planar log-spiral antenna. The sensitive element is made of the ultrathin superconducting NbN film patterned as a bridge at the feed of the antenna. The contacts between the antenna and a sensitive element are made from in situ deposited gold (i.e., deposited over NbN film without breaking vacuum), which gives high quality contacts and makes the response of the HEB at higher frequencies less affected by the RF loss. An accurate experimental spectroscopic procedure is demonstrated that leads to the confirmation of the wide (similar to 8 THz) bandwidth in this antenna coupled device.
C1 [Shurakov, Alexander; Kaurova, Natalia; Goltsman, Gregory] Moscow State Pedag Univ, Dept Phys & Informat Technol, Moscow 119435, Russia.
[Shurakov, Alexander] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Seliverstov, Sergey] Moscow State Pedag Univ, Radio Phys Lab, Moscow 119435, Russia.
[Finkel, Matvey] Moscow State Pedag Univ, Moscow 119435, Russia.
[Voronov, Boris] Moscow State Pedag Univ, Proc Lab, Moscow 119435, Russia.
RP Shurakov, A (reprint author), Moscow State Pedag Univ, Dept Phys & Informat Technol, Moscow 119435, Russia.
EM matveyf@yahoo.com
NR 13
TC 5
Z9 6
U1 0
U2 8
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD JUL
PY 2012
VL 2
IS 4
BP 400
EP 405
DI 10.1109/TTHZ.2012.2194852
PG 6
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AG
UT WOS:000318767400006
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI THE LATEST AND THE GREATEST
SO SMITHSONIAN
LA English
DT Editorial Material
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SMITHSONIAN ASSOC
PI WASHINGTON
PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA
SN 0037-7333
J9 SMITHSONIAN
JI Smithsonian
PD JUL-AUG
PY 2012
VL 43
IS 4
BP 8
EP 8
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 126SP
UT WOS:000317641800008
ER
PT J
AU Diogo, R
Richmond, BG
Wood, B
AF Diogo, Rui
Richmond, Brian G.
Wood, Bernard
TI Evolution and homologies of primate and modern human hand and forearm
muscles, with notes on thumb movements and tool use
SO JOURNAL OF HUMAN EVOLUTION
LA English
DT Article
DE Phylogenetic analysis; Morphology; Extensor pollicis brevis; Flexor
pollicis longus; Adductor pollicis accessorius
ID PALMAR INTEROSSEOUS MUSCLE; SOFT-TISSUE ANATOMY; FORELIMB MUSCULATURE;
FUNCTIONAL-ANATOMY; PHYLOGENY; ADAPTATIONS; MORPHOLOGY; TETRAPODS;
MIOCENE; MYOLOGY
AB In this paper, we explore how the results of a primate-wide higher-level phylogenetic analysis of muscle characters can improve our understanding of the evolution and homologies of the forearm and hand muscles of modern humans. Contrary to what is often suggested in the literature, none of the forearm and hand muscle structures usually present in modern humans are autapomorphic. All are found in one or more extant non-human primate taxa. What is unique is the particular combination of muscles. However, more muscles go to the thumb in modern humans than in almost all other primates, reinforcing the hypothesis that focal thumb movements probably played an important role in human evolution. What makes the modern human thumb myology special within the primate clade is not so much its intrinsic musculature but two extrinsic muscles, extensor pollicis brevis and flexor pollicis longus, that are otherwise only found in hylobatids. It is likely that these two forearm muscles play different functional roles in hylobatids and modern humans. In the former, the thumb is separated from elongated digits by a deep cleft and there is no pulp-to-pulp opposition, whereas modern humans exhibit powerful thumb flexion and greater manipulative abilities, such as those involved in the manufacture and use of tools. The functional and evolutionary significance of a third peculiar structure, the intrinsic hand structure that is often called the 'interosseous volaris primus of Henle' (and which we suggest is referred to as the musculus adductor pollicis accessorius) is still obscure. The presence of distinct contrahentes digitorum and intermetacarpales in adult chimpanzees is likely the result of prolonged or delayed development of the hand musculature of these apes. In relation to these structures, extant chimpanzees are more neotenic than modern humans. (c) 2012 Elsevier Ltd. All rights reserved.
C1 [Diogo, Rui] Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA.
[Richmond, Brian G.; Wood, Bernard] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA.
[Richmond, Brian G.; Wood, Bernard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA.
RP Diogo, R (reprint author), Howard Univ, Coll Med, Dept Anat, 520 W St NW, Washington, DC 20059 USA.
EM rui.diogo@howard.edu
OI Diogo, Rui/0000-0002-9008-1910
FU George Washington University (GW) Presidential Merit Fellowship; Howard
University; GW University Professorship in Human Origins; GW Provost; GW
Selective Excellence Program; National Science Foundation [BCS-0725122]
FX We thank R. Walsh and F. Slaby (Department of Anatomy, George Washington
University), R. Bernstein and S. McFarlin (Department of Anthropology,
George Washington University), N. Rybczynski (Canadian Museum of
Nature), H. Mays (Cincinnati Museum of Natural History), A. Aziz
(Department of Anatomy, Howard University), F. Pastor (Department of
Anatomy, University of Valladolid), A. Gorow, H. Fitch-Snyder and B.
Rideout (San Diego Zoo) and J. Fritz and J. Murphy (Primate Foundation
of Arizona) for kindly providing the non-primate and primate mammalian
specimens dissected during this project. RD was supported by a George
Washington University (GW) Presidential Merit Fellowship and by a Howard
University start-up package. BW by the GW University Professorship in
Human Origins, the GW Provost and the GW Selective Excellence Program,
and BGR by the National Science Foundation (BCS-0725122).
NR 132
TC 20
Z9 21
U1 11
U2 126
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0047-2484
J9 J HUM EVOL
JI J. Hum. Evol.
PD JUL
PY 2012
VL 63
IS 1
BP 64
EP 78
DI 10.1016/j.jhevol.2012.04.001
PG 15
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA 987NJ
UT WOS:000307423900003
PM 22640954
ER
PT J
AU Garcia-Robledo, C
Horvitz, CC
AF Garcia-Robledo, Carlos
Horvitz, Carol C.
TI Parent-offspring conflicts, "optimal bad motherhood" and the "mother
knows best" principles in insect herbivores colonizing novel host plants
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Exotic plants; feeding preference; larval and adult survival;
oviposition preference; parent and offspring performance
ID ROLLED-LEAF BEETLES; HISPINE BEETLES; PHYTOPHAGOUS INSECTS; NATURAL
ENEMIES; EVOLUTION; PERFORMANCE; PREFERENCE; CHRYSOMELIDAE; COMMUNITIES;
GINGERS
AB Specialization of insect herbivores to one or a few host plants stimulated the development of two hypotheses on how natural selection should shape oviposition preferences: The "mother knows best" principle suggests that females prefer to oviposit on hosts that increase offspring survival. The "optimal bad motherhood" principle predicts that females prefer to oviposit on hosts that increase their own longevity. In insects colonizing novel host plants, current theory predicts that initial preferences of insect herbivores should be maladaptive, leading to ecological traps. Ecological trap theory does not take into account the fact that insect lineages frequently switch hosts at both ecological and evolutionary time scales. Therefore, the behavior of insect herbivores facing novel hosts is also shaped by natural selection. Using a study system in which four Cephaloleia beetles are currently expanding their diets from native to exotic plants in the order Zingiberales, we determined if initial oviposition preferences are conservative, maladaptive, or follow the patterns predicted by the "mother knows best" or the "optimal badmotherhood" principles. Interactions with novel hosts generated parent-offspring conflicts. Larval survival was higher on native hosts. However, adult generally lived longer on novel hosts. In Cephaloleia beetles, oviposition preferences are usually associated with hosts that increase larval survival, female fecundity, and population growth. In most cases, Cephaloleia oviposition preferences follow the expectations of the "mothers knows best" principle.
C1 [Garcia-Robledo, Carlos; Horvitz, Carol C.] Univ Miami, Dept Biol, Coral Gables, FL 33124 USA.
RP Garcia-Robledo, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, POB 37012, Washington, DC 20013 USA.
EM garciac@si.edu
FU J. McLamore Fellowship - University of Miami; OTS (Organization for
Tropical Studies) - Donald and Beverly Stone; Christiane Fellowship;
Christopher Tyson Fellowship; Smithsonian Postdoctoral Fellowship;
National Geographic-Waitt Institute; Rubenstein Fellowship -
Encyclopedia of Life to C. Garcia-Robledo; Cooper Fellowship, College of
Arts and Sciences, University of Miami; National Institutes of Health,
National Institute of Aging [P01 AG022500-01]; NSF [DEB-0614457]
FX This research was funded by the J. McLamore Fellowship - University of
Miami, the OTS (Organization for Tropical Studies) - Donald and Beverly
Stone and the Christiane and Christopher Tyson Fellowships, the
Smithsonian Postdoctoral Fellowship, a National Geographic-Waitt
Institute grant and the Rubenstein Fellowship - Encyclopedia of Life to
C. Garcia-Robledo and the Cooper Fellowship, College of Arts and
Sciences, University of Miami, National Institutes of Health, National
Institute of Aging P01 AG022500-01 and NSF DEB-0614457 grants to C. C.
Horvitz.
NR 38
TC 11
Z9 11
U1 2
U2 45
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD JUL
PY 2012
VL 2
IS 7
BP 1446
EP 1457
DI 10.1002/ece3.267
PG 12
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA 055WK
UT WOS:000312448400011
PM 22957153
ER
PT J
AU Kroll, O
Hershler, R
Albrecht, C
Terrazas, EM
Apaza, R
Fuentealba, C
Wolff, C
Wilke, T
AF Kroll, Oliver
Hershler, Robert
Albrecht, Christian
Terrazas, Edmundo M.
Apaza, Roberto
Fuentealba, Carmen
Wolff, Christian
Wilke, Thomas
TI The endemic gastropod fauna of Lake Titicaca: correlation between
molecular evolution and hydrographic history
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Altiplano; Heleobia; molecular clock; phylogeography; species flock
ID MITOCHONDRIAL SEQUENCE DIVERSITY; PHYLOGENETIC-RELATIONSHIPS; SPECIES
FLOCK; HYDROLOGIC VARIATION; ANCIENT LAKES; CENTRAL ANDES; FRESH-WATER;
ALTIPLANO; HYDROBIIDAE; RISSOOIDEA
AB Lake Titicaca, situated in the Altiplano high plateau, is the only ancient lake in South America. This 2- to 3-My-old (where My ismillion years) water body has had a complex history that included at least five major hydrological phases during the Pleistocene. It is generally assumed that these physical events helped shape the evolutionary history of the lake's biota. Herein, we study an endemic species assemblage in Lake Titicaca, composed of members of the microgastropod genus Heleobia, to determine whether the lake has functioned as a reservoir of relic species or the site of local diversification, to evaluate congruence of the regional paleohydrology and the evolutionary history of this assemblage, and to assess whether the geographic distributions of endemic lineages are hierarchical. Our phylogenetic analyses indicate that the Titicaca/Altiplano Heleobia fauna (together with few extralimital taxa) forms a species flock. A molecular clock analysis suggests that the most recent common ancestor (MRCAs) of the Altiplano taxa evolved 0.53 (0.28-0.80) My ago and the MRCAs of the Altiplano taxa and their extralimital sister group 0.92 (0.46-1.52) My ago. The endemic species of Lake Titicaca are younger than the lake itself, implying primarily intralacustrine speciation. Moreover, the timing of evolutionary branching events and the ages of two precursors of Lake Titicaca, lakes Cabana and Ballivian, is congruent. Although Lake Titicaca appears to have been the principal site of speciation for the regional Heleobia fauna, the contemporary spatial patterns of endemism have been masked by immigration and/or emigration events of local riverine taxa, which we attribute to the unstable hydrographic history of the Altiplano. Thus, a hierarchical distribution of endemism is not evident, but instead there is a single genetic break between two regional clades. We also discuss our findings in relation to studies of other regional biota and suggest that salinity tolerance was the most likely limiting factor in the evolution of Altiplano species flocks.
C1 [Kroll, Oliver; Albrecht, Christian; Wolff, Christian; Wilke, Thomas] Univ Giessen, Dept Anim Ecol & Systemat, D-35392 Giessen, Germany.
[Hershler, Robert] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Terrazas, Edmundo M.] Univ Nacl Altiplano, Fac Ciencias Biol, Puno, Peru.
[Apaza, Roberto] Univ Nacl Mayor San Marcos, Inst Ecol, La Paz, Bolivia.
[Fuentealba, Carmen] Univ Concepcion, Dept Zool, Concepcion, Chile.
RP Wilke, T (reprint author), Univ Giessen, Dept Anim Ecol & Systemat, Heinrich Buff Ring 26-32 IFZ, D-35392 Giessen, Germany.
EM tom.wilke@allzool.bio.uni-giessen.de
RI Wilke, Thomas/G-1517-2012
OI Wilke, Thomas/0000-0001-8263-7758
FU DAAD Center of Excellence in Marine Sciences (CEMarin) in Santa Marta,
Colombia; Deutsche Forschungsgemeinschaft (DFG) [WI 1902/8-1, AL
1076/3-1]
FX We would like to thank D. Aranibar and all employees of the Reserva
Nacional del Titicaca (RNT) for their hospitality and support. We are
very grateful to M. Bodon, U. Bossneck, S. Cianfanelli, G. M. Davis, A.
Falniowski, C. Gamarra, H. Girardi, K. Gonzales, E. Gutierrez, J.
Heller, E. Loro, W. Maldonado, E. Miranda, I. Niero, D. Pineda, M.
Szarowska, and B. Werding for providing valuable materials and for
supporting our fieldwork. We also thank S. Nachtigall for her help with
the DNA work as well as R. Schultheiss, M. Haase, and an anonymous
referee for their critical comments on a previous version of this paper.
H.-P. Liu kindly provided two unpublished Heleobia sequences for this
study. This study was inspired by the Diploma thesis of O. Kroll,
supervised by S. Richter. Partial support for the study came from the
DAAD Center of Excellence in Marine Sciences (CEMarin) in Santa Marta,
Colombia and from the Deutsche Forschungsgemeinschaft (DFG) grants WI
1902/8-1 and AL 1076/3-1.
NR 71
TC 16
Z9 16
U1 1
U2 23
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD JUL
PY 2012
VL 2
IS 7
BP 1517
EP 1530
DI 10.1002/ece3.280
PG 14
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA 055WK
UT WOS:000312448400017
PM 22957159
ER
PT J
AU Attasopa, K
Warrit, N
AF Attasopa, Korrawat
Warrit, Natapot
TI Redescription, subgeneric position and distribution of the Oriental
burrowing bee, Amegilla fimbriata (Hymenoptera: Apidae: Anthophorini)
SO PAN-PACIFIC ENTOMOLOGIST
LA English
DT Article
DE Amegilla fimbriata; Amegilla; Glossamegilla; burrowing bees; Thailand
ID CHLOROCYANEA; POLLINATION
AB Amegilla fimbriata (Smith, 1897) (Hymenoptera; Apidae; Anthophorini) is redescribed with detailed study of the male genitalia. Ambiguity concerning the subgeneric placement of A. fimbriata in the subgenus Glossamegilla is discussed. Lectotype of A. fimbriata is designated.
C1 [Attasopa, Korrawat; Warrit, Natapot] Chulalongkorn Univ, Fac Sci, Dept Biol, Ctr Excellence Entomol, Bangkok 10330, Thailand.
[Warrit, Natapot] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
RP Warrit, N (reprint author), Chulalongkorn Univ, Fac Sci, Dept Biol, Ctr Excellence Entomol, Bangkok 10330, Thailand.
EM Natapot.W@chula.ac.th
FU Chulalongkorn University; Thailand Research Fund (TRF) [MRG5380139]
FX We would like to thank two anonymous reviewers and Dr. Charles D.
Michener for providing insights and invaluable comments on the
manuscript; Dr. Deborah R. Smith for help editing the manuscript, the
staff at the Center of Excellence in Entomology, Chulalongkorn
University, particularly Sureerat Deowanish and Chariya Lekprayoon, for
providing research facilities; Yuvarin Boontop of the Ministry of
Agriculture (MA) for her courtesy during our visit to the MA National
Insect Collection. The authors also thank the following collection
managers and their institutions for kindly providing access to specimens
used in this study: Chariya Lekprayoon (NHMCU), Prachaval Sukumalanand
and Sawai Buranapanichpan (ACMU), Araya Jatisatienr (SCMU), Virot
Khipsuwon (KKU), and David G. Notton (NHM). The photographic equipment
was provided by the Animal Systematics Research Unit (ASRU), Department
of Biology, Chulalongkorn University, through assistance of Somsak
Panha, Chirasak Sutcharit, and Natdanai Likhitrakarn. This study was
funded by Grants for the Development of New Faculty Staff, Chulalongkorn
University, and in part by the Thailand Research Fund (TRF# MRG5380139)
to NW.
NR 19
TC 0
Z9 0
U1 1
U2 2
PU PACIFIC COAST ENTOMOL SOC
PI SAN FRANCISCO
PA C/O CALIFORNIA ACADEMY SCIENCES, 875 HOWARD STREET, SAN FRANCISCO, CA
94103-3009 USA
SN 0031-0603
J9 PAN-PAC ENTOMOL
JI Pan-Pacific Entomol.
PD JUL
PY 2012
VL 88
IS 3
BP 281
EP 291
PG 11
WC Entomology
SC Entomology
GA 053NA
UT WOS:000312278500001
ER
PT J
AU Flint, OS
AF Flint, Oliver S., Jr.
TI Two new Oecetis of the reticulata group from Micronesia (Trichoptera:
Leptoceridae)
SO PAN-PACIFIC ENTOMOLOGIST
LA English
DT Article
DE Trichoptera; Leptoceridae; Oecetis; Caddisfly; Pohnpei; Micronesia; new
species
AB Two new species of the reticulata group of the widespread genus Oecetis McLachlan 1877 are described front Pohnpei. Oecetis mackenziei, sp. nov., and O. squamifera, sp. nov., are the first species described from Micronesia after the poorly known Triaenodes esakii Tsuda 1941, known from Koror and Babelthuap, Palau. Figures are presented of the male and female genitalia of O mackenziei, and the male only of O. squamifera: wing photographs of males of both species are included.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
RP Flint, OS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 169, Washington, DC 20013 USA.
EM flinto@si.edu
NR 5
TC 0
Z9 0
U1 0
U2 2
PU PACIFIC COAST ENTOMOL SOC
PI SAN FRANCISCO
PA C/O CALIFORNIA ACADEMY SCIENCES, 875 HOWARD STREET, SAN FRANCISCO, CA
94103-3009 USA
SN 0031-0603
J9 PAN-PAC ENTOMOL
JI Pan-Pacific Entomol.
PD JUL
PY 2012
VL 88
IS 3
BP 299
EP 303
PG 5
WC Entomology
SC Entomology
GA 053NA
UT WOS:000312278500003
ER
PT J
AU Zahniser, JN
McKamey, SH
Dmitriev, DA
AF Zahniser, J. N.
McKamey, S. H.
Dmitriev, D. A.
TI Nomenclatural changes and notes in the Deltocephalinae (Hemiptera:
Cicadellidae)
SO PAN-PACIFIC ENTOMOLOGIST
LA English
DT Article
DE Membracoidea; homonym; synonym; nomen novum; nomen protectum; nomen
oblitum; new name; Drabescus; Osbornellus
ID GENUS; LEAFHOPPERS; NAMES
AB Nomenclatural changes and clarifications are provided for names in the leafhopper subfamily Deltocephalinae. The replacement names Cicadula vilbastei nom. nov., Eutettix harlani nom. nov.. Macrosteles raoi nom. nov., Maiestas chalami nom. nov., Maiestas viraktamathi nom. nov., Opsius emeljanovi nom. nov.. Paradorydium naudei nom. nov., Penthimia alba nom. nov., Penthimia evansi nom. nov., and Peuthimia walker nom. nov. are given for species-group homonyms. Four new synonyms are recognized for previous replacement names that are no longer valid. The status of Acinopterus angulatus Lawson nomen protectum is discussed. Paramacrosteles Dai, Li & Chen status reinstated is reinstated as valid on taxonomic grounds. Priority is clarified for two species of Deltocephalinae, five new combinations in Balclutha Kirkaldy are given, and two original spellings are fixed.
C1 [Zahniser, J. N.; Dmitriev, D. A.] Univ Illinois, Prairie Res Inst, Illinois Nat Hist Survey, Champaign, IL 61820 USA.
[McKamey, S. H.] USDA ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA.
RP Zahniser, JN (reprint author), Univ Illinois, Prairie Res Inst, Illinois Nat Hist Survey, 1816 S Oak St, Champaign, IL 61820 USA.
EM zahniser@illinois.edu; stuart.mckamey@ars.usda.gov;
dmitriev@inhs.illinois.edu
NR 35
TC 1
Z9 1
U1 0
U2 2
PU PACIFIC COAST ENTOMOL SOC
PI SAN FRANCISCO
PA C/O CALIFORNIA ACADEMY SCIENCES, 875 HOWARD STREET, SAN FRANCISCO, CA
94103-3009 USA
SN 0031-0603
EI 2162-0237
J9 PAN-PAC ENTOMOL
JI Pan-Pacific Entomol.
PD JUL
PY 2012
VL 88
IS 3
BP 356
EP 364
PG 9
WC Entomology
SC Entomology
GA 053NA
UT WOS:000312278500009
ER
PT J
AU Ballen, GA
Vari, RP
AF Ballen, Gustavo A.
Vari, Richard P.
TI Review of the Andean armored catfishes of the genus Dolichancistrus
Isbrucker (Siluriformes: Loricariidae)
SO NEOTROPICAL ICHTHYOLOGY
LA English
DT Review
DE Andes; Chaetostoma group; Chaetostomus setosus; Northwestern South
America
ID SUCKERMOUTH; VENEZUELA; HYPOSTOMINAE; RIVER
AB The loricariid catfish genus Dolichancistrus is reviewed and four species recognized. Species of Dolichancistrus are distinguished from each other by the degree of development of the pectoral-fin spine, the form of the distal margin of the pelvic fin, the relative size and form of the cheek plates, the pattern of odontodes along the margin of the snout, the presence versus absence of a buccal papilla at the premaxillary symphysis, and the relative lengths of the anal- versus pelvic-spines. Dolichancistrus atratoensis is known from the rio Atrato system and the rio Cubarrado on the Pacific versant of Colombia; D. carnegiei occurs in the eastern rio Magdalena basin in the departments of Boyaca and Santander, Colombia; D. cobrensis inhabits southern tributaries of the Lago Maracaibo basin in Colombia and Venezuela along with some highland rivers of the Cordillera de Merida in Venezuela draining into the rio Orinoco system; and D. fuesslii is known from the Andean piedmont portions of the rio Meta basin in the western rio Orinoco system. Pseudancistrus pediculatus is considered a junior synonym of Ancistrus fuesslii. Chaetostomus setosus previously assigned to Dolichancistrus, was found to lack features characteristic of its putative congeners and is rather more closely related to other members of Chaetostoma group. Consequently, the species is herein considered as incertae sedis within that group. Dolichancistrus is diagnosed, a key is provided to the members of the genus, and diagnoses and redescriptions are provided for all of the recognized species.
C1 [Ballen, Gustavo A.] Univ Nacl Colombia, Grp Cladist Profunda & Biogeog Hist, Inst Ciencias Nat, Bogota, Colombia.
[Vari, Richard P.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Ballen, GA (reprint author), Univ Nacl Colombia, Grp Cladist Profunda & Biogeog Hist, Inst Ciencias Nat, Apartado Aereo 7495, Bogota, Colombia.
EM gaballench@gmail.com; varir@si.edu
FU Office of the Associate Director of Research; Robert H. Gibbs Memorial
Fund at the National Museum of Natural History, Smithsonian Institution
FX Research associated with this project was supported by the Office of the
Associate Director of Research and the Robert H. Gibbs Memorial Fund at
the National Museum of Natural History, Smithsonian Institution. We
thank Mark Sabaj Perez and John Lundberg (ANSP), Jonathan Armbruster and
David Werneke (AUM), James Maclaine (BMNH), Carlos Ardila (CAR), David
Catania (CAS), Luz Fernanda Jimenez (CIUA), Francisco Villa (CZUT-IC),
Mary Anne Rogers (FMNH), Claudia Medina (IAvH-P), J. Ivan Mojica
(ICNMHN), Otto Castillo (MCNG), Brother Jose Espitia (MLS), Ernst
Mikschi and Helmut Wellendorf (NMW), Sven Kullander (NRM), and Sandra
Raredon (USNM) for the loan of specimens and other assistance. Gonzalo
Andrade and Julio Betancur (ICNMHN) provided access to photographic
equipment and Paola Trivino and Miguel Rodriguez provided assistance
during photographic sessions. T. Britt Griswold prepared Figure 4. John
D. Lynch (ICNMHN) is especially acknowledged for providing workspace and
access to equipment and library facilities in addition to invaluable
advice over the years to GAB. The paper benefitted from the comments of
Carl J. Ferraris Jr., John D. Lynch, and Donald C. Taphorn.
NR 56
TC 5
Z9 5
U1 1
U2 8
PU SOC BRASILEIRA ICTIOLOGIA
PI SAO PAULO
PA UNIV SAO PAULO, DEPT FISIOLOGIA-IB, RUA DO MATAO, TRAVESSA 14 N 321, SAO
PAULO, SP 05508-900, BRAZIL
SN 1679-6225
J9 NEOTROP ICHTHYOL
JI Neotrop. Ichthyol.
PD JUL-SEP
PY 2012
VL 10
IS 3
BP 499
EP 518
PG 20
WC Zoology
SC Zoology
GA 022HZ
UT WOS:000309950200003
ER
PT J
AU Bogan, S
Sidlauskas, B
Vari, RP
Agnolin, F
AF Bogan, Sergio
Sidlauskas, Brian
Vari, Richard P.
Agnolin, Federico
TI Arrhinolemur scalabrinii Ameghino, 1898, of the late Miocene - a
taxonomic journey from the Mammalia to the Anostomidae (Ostariophysi:
Characiformes)
SO NEOTROPICAL ICHTHYOLOGY
LA English
DT Article
DE Argentina; fossil; Leporinus; Osteology; Phylogeny
ID TELEOSTEI; BASIN
AB The fossil species Arrhinolemur scalabrinii, which was described from late Miocene deposits of Entre Rios, Argentina, is reevaluated. Whereas the species was originally placed in the Primates (Mammalia) and later made the unique member of the order Arrhinolemuroidea within the Mammalia, our analysis indicates that the specimen is rather a fish of the genus Leporinus, family Anostomidae (Characiformes). The species is redescribed, and the characters that support its new generic assignment are discussed.
C1 [Bogan, Sergio; Agnolin, Federico] Univ Maimonides, Fdn Hist Nat Felix Azara, Area Paleontol, Dept Ciencias Nat & Antropol, Buenos Aires, DF, Argentina.
[Sidlauskas, Brian] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA.
[Sidlauskas, Brian; Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
[Agnolin, Federico] Museo Argentino Ciencias Nat Bernardino Rivadavia, Lab Anat Comparada & Evoluc Vertebrados, Buenos Aires, DF, Argentina.
RP Bogan, S (reprint author), Univ Maimonides, Fdn Hist Nat Felix Azara, Area Paleontol, Dept Ciencias Nat & Antropol, CEBBAD Hidalgo 775 Piso 7 C1405BDB, Buenos Aires, DF, Argentina.
EM sergiobogan@yahoo.com.ar; brian.sidlauskas@oregonstate.edu; varir@si.edu
OI Sidlauskas, Brian/0000-0003-0597-4085
FU Adrian Giacchino (FHNFA)
FX We thank Fernando Novas for allowing us to study the material, and Mario
Sevilla and Sebastian Suarez for their help with tomographic images
taken at Maimonides University. Comments from Jose Birindelli (MZUSP)
and an anonymous reviewer helped to improve the manuscript. Adrian
Giacchino (FHNFA) kindly provided logistic and financial support.
NR 20
TC 4
Z9 4
U1 0
U2 3
PU SOC BRASILEIRA ICTIOLOGIA
PI SAO PAULO
PA UNIV SAO PAULO, DEPT FISIOLOGIA-IB, RUA DO MATAO, TRAVESSA 14 N 321, SAO
PAULO, SP 05508-900, BRAZIL
SN 1679-6225
J9 NEOTROP ICHTHYOL
JI Neotrop. Ichthyol.
PD JUL-SEP
PY 2012
VL 10
IS 3
BP 555
EP 560
PG 6
WC Zoology
SC Zoology
GA 022HZ
UT WOS:000309950200008
ER
PT J
AU Vaslet, A
France, C
Baldwin, CC
Feller, IC
AF Vaslet, Amandine
France, Christine
Baldwin, Carole C.
Feller, Ilka C.
TI Dietary habits of juveniles of the Mayan cichlid, Cichlasoma
urophthalmus, in mangrove ponds of an offshore islet in Belize, Central
America
SO NEOTROPICAL ICHTHYOLOGY
LA English
DT Article
DE Caribbean; Cichlidae; Diet; Seagrass beds; Stable isotopes
ID STABLE-ISOTOPE ANALYSES; AQUATIC FOOD WEBS; MIXING MODELS; FLORIDA;
FISHES; CARBON; DELTA-C-13; ASSUMPTIONS; ECOSYSTEMS; DEPENDENCE
AB Foraging habitats of juveniles of the Mayan cichlid, Cichlasoma urophthalmus (Gunther, 1862), were investigated in two mangrove ponds located in Twin Cays offshore islet in Belize: Sink Hole pond (SH) and Hidden Lake pond (HL). Sink Hole pond is a semiclosed body of water, whereas Hidden Lake pond is connected by a channel to adjacent seagrass beds that surround the islet. Gut contents of 21 juvenile C. urophthalmus (9.8-13.2 cm total length) were analyzed, and five prey taxa were identified. In both mangrove ponds, C. urophthalmus were opportunistic carnivores and consumed primarily crustaceans. Plant material and detritus present in gut contents were most likely ingested incidentally when the fish foraged on small invertebrates. Carbon isotopic values of fish specimens from the two ponds were similar (mean +/- SD of -19.2 +/- 0.4 parts per thousand in SH and -19.4 +/- 0.4 parts per thousand in HL), and were close to those of mangrove prey (mean +/- SD = -20.2 +/- 1.5 parts per thousand), suggesting that this fish species forages in this habitat. Mixing models showed a higher contribution of mangrove food sources to the fish diet than seagrass food sources. This study reveals that young Mayan cichlids, inhabiting two Belize mangrove ponds, are generalists and opportunistic carnivores that forage on mangrove food sources and do not appear to move to adjacent seagrass beds to complement their diets. Understanding trophic linkages between aquatic consumers and food resources may contribute to better management of threatened coastal ecosystems.
C1 [Vaslet, Amandine] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
[France, Christine] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA.
[Baldwin, Carole C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Vaslet, A (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM amandine.vaslet@gmail.com
OI Feller, Ilka/0000-0002-6391-1608
FU SMSFP Postdoctoral Fellowship; Smithsonian's Caribbean Coral Reef
Ecosystems Program [929]
FX The authors thank Valerie Paul, director of Smithsonian Marine Station
at Fort Pierce (SMSFP), and all the staff of SMSFP for their assistance
and logistic support in the field. The authors are grateful to Zach
Foltz, Woody Lee from SMSFP for their help in field collections. We
thank the Belize Fisheries Department for permission to collect in
mangroves. This research was funded by SMSFP Postdoctoral Fellowship to
Amandine Vas let. This paper is contribution number 889 from SMSFP and
contribution number 929 from Smithsonian's Caribbean Coral Reef
Ecosystems Program.
NR 42
TC 3
Z9 3
U1 0
U2 22
PU SOC BRASILEIRA ICTIOLOGIA
PI SAO PAULO
PA UNIV SAO PAULO, DEPT FISIOLOGIA-IB, RUA DO MATAO, TRAVESSA 14 N 321, SAO
PAULO, SP 05508-900, BRAZIL
SN 1679-6225
J9 NEOTROP ICHTHYOL
JI Neotrop. Ichthyol.
PD JUL-SEP
PY 2012
VL 10
IS 3
BP 667
EP 674
PG 8
WC Zoology
SC Zoology
GA 022HZ
UT WOS:000309950200021
ER
PT J
AU Dahl, C
Kiatik, I
Baisen, I
Bronikowski, E
Fleischer, RC
Rotzel, NC
Lock, J
Novotny, V
Narayan, E
Herol, JM
AF Dahl, Chris
Kiatik, Ismale
Baisen, Ismale
Bronikowski, Ed
Fleischer, Robert C.
Rotzel, Nancy C.
Lock, Justin
Novotny, Vojtech
Narayan, Edward
Herol, Jean-Marc
TI Batrachochytrium dendrobatidis not found in rainforest frogs along an
altitudinal gradient of Papua New Guinea
SO HERPETOLOGICAL JOURNAL
LA English
DT Article
DE altitude; amphibians; Batrachochytrium; dendrobatidis; chytridiomycosis;
Papua New Guinea
ID TIME TAQMAN PCR; AMPHIBIAN CHYTRIDIOMYCOSIS; WILD FROGS; DECLINES;
DISEASE; BIODIVERSITY; AUSTRALIA
AB Batrachochytrium dendrobatidis (Bd) is a fungal pathogen often responsible for amphibian declines worldwide. We report here survey on Bd in Papua New Guinea (PNG). The survey for Bd was conducted along a rainforest altitudinal gradient from Madang (50 m a.s.l.) to Mt. Wilhelm (3700 m a.s.l.). We swabbed 249 frogs of 63 native species at nine sites to quantify the number of Bd zoospore equivalents using real-time Syber Green Polymerase Chain Reaction (qPCR). We found no evidence for Bd. The lack of Bd may be due to 1) hot climate all year round inhibiting the spread of Bd in the entire lowland areas of PNG, 2) low number of non-native amphibian introductions to PNG such as Litho bales catesbeianus or Xenopus spp. or 3) the lack of invasive introductions by humans due to geographic isolation. While it is difficult to discern between these hypotheses, an effective quarantine should be devised to protect PNG from future disease outbreak. International assistance is needed in conservation education and research to assist the local scientists in monitoring and protecting these rich fauna from future Bd outbreaks.
C1 [Dahl, Chris; Narayan, Edward; Herol, Jean-Marc] Griffith Sch Environm, Environm Futures Ctr, Nathan, Qld, Australia.
[Dahl, Chris; Kiatik, Ismale; Baisen, Ismale] New Guinea Binatang Res Ctr, Madang, Papua N Guinea.
[Bronikowski, Ed] Smithsonian Inst, Washington, DC 20560 USA.
[Novotny, Vojtech] Univ S Bohemia, Ctr Biol, Czech Acad Sci, Ceske Budejovice, Czech Republic.
[Novotny, Vojtech] Univ S Bohemia, Fac Sci, Ceske Budejovice, Czech Republic.
[Fleischer, Robert C.; Rotzel, Nancy C.; Lock, Justin] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC USA.
RP Dahl, C (reprint author), Griffith Univ, Sch Environm, Environm Futures Ctr, Gold Coast Campus, Nathan, Qld 4222, Australia.
EM c.dahl@griffith.edu.au
RI Novotny, Vojtech/G-9434-2014; Narayan, Edward/E-8238-2016
OI Novotny, Vojtech/0000-0001-7918-8023; Narayan,
Edward/0000-0003-2719-0900
FU Association of Zoos and Aquariums; Conservation Endowment Fund [08-857];
Christensen Fund [2009-2729546]; PNG Mama Graun Conservation Trust Fund
[PC 10-3 -010]
FX The study was funded by the Association of Zoos and Aquariums;
Conservation Endowment Fund No. 08-857, The Christensen Fund
(2009-2729546) and PNG Mama Graun Conservation Trust Fund (PC 10-3
-010). We thank Scott Miller, Lauren He Igen for advice, Phil Shearman
and Jane Bryan for remote sensing data and the altitude study map on
Fig. 1, the New Guinea Binatang Research Center staff for logistical
support, the Bundi-Mt. Wilhelm landowners, and the field assistants for
the field work. Jim Murphy also commented on our manuscript.
NR 31
TC 3
Z9 3
U1 0
U2 7
PU BRITISH HERPETOL SOC
PI LONDON
PA C/O ZOOL SOC LONDON REGENTS PARK, LONDON NW1 4RY, ENGLAND
SN 0268-0130
J9 HERPETOL J
JI Herpetolog. J.
PD JUL
PY 2012
VL 22
IS 3
BP 183
EP 186
PG 4
WC Zoology
SC Zoology
GA 021NZ
UT WOS:000309893600008
ER
PT J
AU Ferraz, G
AF Ferraz, Goncalo
TI Twelve Guidelines for Biological Sampling in Environmental Licensing
Studies
SO NATUREZA & CONSERVACAO
LA English
DT Article
DE Environmental Licensing; Sampling; Monitoring Protocols; Management
ID PROGRESS; AMAZON
AB Environmental licensing is a decision-making process that requires scientific information and has far-reaching political and economic consequences. Sound science leads to informed decisions; unfocused science leaves an information void that is easily filled by power struggles. In the last few years, Brazil has seen a lively debate between two alternative approaches to the science behind environmental licensing: one centers on detailed methodological prescription with broadly defined goals; the other builds on the precise definition of questions that focus the scientific work and allows case-by-case flexibility in methodological choices. This essay offers twelve guidelines for pursuing the second approach, formulated around the key questions of why, what, and how to sample. These guidelines illustrate how it is possible to set scientific standards of operation without tying the hands of practitioners to omnibus protocols that may serve the purpose of accumulating data but won't necessarily produce knowledge to inform rational licensing decisions. The guidelines are formulated in the context of Brazilian environmental licensing, but they should apply wherever a regulatory agency needs to elicit scientific answers to urgent environmental questions.
C1 [Ferraz, Goncalo] Smithsonian Trop Res Inst, Inst Nacl Pesquisas Amazonia, Biol Dynam Forest Fragments Project, BR-69083000 Manaus, Amazonas, Brazil.
[Ferraz, Goncalo] Smithsonian Trop Res Inst, Balboa, Panama.
RP Ferraz, G (reprint author), Smithsonian Trop Res Inst, Inst Nacl Pesquisas Amazonia, Biol Dynam Forest Fragments Project, Av Andre Araujo 1753,CP 478, BR-69083000 Manaus, Amazonas, Brazil.
EM ferrazg@si.edu
NR 16
TC 4
Z9 5
U1 0
U2 6
PU ASSOC BRASILEIRA CIENCIA ECOLOGICA E CONSERVACAO
PI RIO DE JANEIRO
PA CAIXA POSTAL 68038, CIDADE UNIV, ILHA DO FUNDAO, RIO DE JANEIRO, RJ
00000, BRAZIL
SN 1679-0073
EI 2178-3675
J9 NAT CONSERVACAO
JI Nat. Conserv.
PD JUL
PY 2012
VL 10
IS 1
BP 20
EP 26
DI 10.4322/natcon.2012.004
PG 7
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA 990KH
UT WOS:000307628900004
ER
PT J
AU Ferrari, FD
AF Ferrari, Frank D.
TI ECDYSOZOANS, ARTICULATES, AND THE NEEDLE IN A HAYSTACK
SO CRUSTACEANA
LA English
DT Article
ID CLADE
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA.
RP Ferrari, FD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM ferrarif@si.edu
NR 13
TC 1
Z9 1
U1 0
U2 3
PU BRILL ACADEMIC PUBLISHERS
PI LEIDEN
PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS
SN 0011-216X
J9 CRUSTACEANA
JI Crustaceana
PD JUL
PY 2012
VL 85
IS 8
BP 1013
EP 1017
DI 10.1163/156854012X649531
PG 5
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 986DM
UT WOS:000307321100009
ER
PT J
AU Abreu, NM
Stanek, GL
Bullock, ES
AF Abreu, N. M.
Stanek, G. L.
Bullock, E. S.
TI EXOTIC MINERALS FOUND IN OPAQUE NODULES IN CR GRA 06100
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
C1 [Abreu, N. M.; Stanek, G. L.] Penn State Univ DuBois, Du Bois, PA USA.
[Bullock, E. S.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
EM abreu@psu.edu
NR 3
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A39
EP A39
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700006
ER
PT J
AU Corrigan, CM
Lunning, NG
AF Corrigan, C. M.
Lunning, N. G.
TI IDENTIFICATION OF IMPACT MELTED MATERIALS IN ORDINARY CHONDRITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
C1 [Corrigan, C. M.] Smithsonian Inst, NMNH, Washington, DC 20560 USA.
EM corriganc@si.edu
NR 22
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A109
EP A109
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700076
ER
PT J
AU Goreva, YS
McCoy, TJ
AF Goreva, Y. S.
McCoy, T. J.
TI USING TOF-SIMS FOR EVALUATION OF FLIGHT HARDWARE
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
C1 [Goreva, Y. S.; McCoy, T. J.] Smithsonian Inst, Dept Mineral Sci, NMNH, Washington, DC 20560 USA.
EM gorevay@si.edu
NR 5
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A158
EP A158
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700125
ER
PT J
AU Herd, CDK
Zhou, Q
Yin, Q
Wu, F
Li, X
Li, QL
McCoy, TJ
AF Herd, C. D. K.
Zhou, Q.
Yin, Q.
Wu, F.
Li, X.
Li, Q-L.
McCoy, T. J.
TI U-Pb Geochronology of Baddeleyite in Zagami by Gaussian Illumination
Probe SIMS.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
ID ISOTOPIC SYSTEMATICS
C1 [Herd, C. D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
[Zhou, Q.; Wu, F.; Li, X.; Li, Q-L.] Chinese Acad Sci, Inst Geol & Geophys, Beijing, Peoples R China.
[Yin, Q.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA.
[McCoy, T. J.] Smithsonian Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
EM herd@ualberta.ca
NR 7
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A178
EP A178
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700145
ER
PT J
AU McCoy, TJ
Beck, A
McSween, HY
Team, D
AF McCoy, T. J.
Beck, A.
McSween, H. Y., Jr.
Team, Dawn
TI DAWN, VESTA AND THE HED'S: THE EXPECTED, THE EXPLAINED, AND THE
SURPRISES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
C1 [McCoy, T. J.; Beck, A.] Smithsonian Inst, Washington, DC 20560 USA.
[McSween, H. Y., Jr.] Univ Tennessee, Knoxville, TN USA.
RI Beck, Andrew/J-7215-2015
OI Beck, Andrew/0000-0003-4455-2299
NR 10
TC 0
Z9 0
U1 0
U2 8
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A264
EP A264
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700231
ER
PT J
AU Mittlefehldt, DW
Beck, AW
Ammannito, E
Carsenty, U
De Sanctis, MC
Le Corre, L
McCoy, TJ
Reddy, V
Schroder, SE
AF Mittlefehldt, D. W.
Beck, A. W.
Ammannito, E.
Carsenty, U.
De Sanctis, M. C.
Le Corre, L.
McCoy, T. J.
Reddy, V.
Schroeder, S. E.
TI GEOLOGIC STRUCTURES IN CRATER WALLS ON VESTA.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
C1 [Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Beck, A. W.; McCoy, T. J.] Smithsonian Natl Museum Nat Hist, Washington, DC USA.
[Ammannito, E.; De Sanctis, M. C.] INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy.
[Carsenty, U.] DLR, Inst Planetary Res, Berlin, Germany.
[Le Corre, L.; Reddy, V.; Schroeder, S. E.] Max Planck Inst Sonnensyst Forsch, Katlenburg Lindau, Germany.
[Reddy, V.] Univ N Dakota, Grand Forks, ND 58201 USA.
EM david.w.mittlefehldt@nasa.gov
RI De Sanctis, Maria Cristina/G-5232-2013; Beck, Andrew/J-7215-2015
OI De Sanctis, Maria Cristina/0000-0002-3463-4437; Beck,
Andrew/0000-0003-4455-2299
NR 8
TC 0
Z9 0
U1 0
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A275
EP A275
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700242
ER
PT J
AU Prettyman, TH
Reedy, RC
Mittlefehldt, DW
Yamashita, N
Lawrence, DJ
Beck, AW
Feldman, WC
McCoy, TJ
McSween, HY
Toplis, MJ
Forni, O
Mizzon, H
Raymond, CA
Russell, CT
Polanskey, CA
Joy, SP
Mafi, J
AF Prettyman, T. H.
Reedy, R. C.
Mittlefehldt, D. W.
Yamashita, N.
Lawrence, D. J.
Beck, A. W.
Feldman, W. C.
McCoy, T. J.
McSween, H. Y.
Toplis, M. J.
Forni, O.
Mizzon, H.
Raymond, C. A.
Russell, C. T.
Polanskey, C. A.
Joy, S. P.
Mafi, J.
CA Dawn Sci Team
TI FOR A FEW HOWARDITES MORE: GRAND MAPS THE ELEMENTAL COMPOSITION OF VESTA
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
ID GAMMA-RAY; DAWN
C1 [Lawrence, D. J.] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA.
[Beck, A. W.; McCoy, T. J.] Smithsonian Inst, Washington, DC 20560 USA.
[McSween, H. Y.] Univ Tennessee, Knoxville, TN 37996 USA.
[Toplis, M. J.; Forni, O.; Mizzon, H.] Univ Toulouse, Toulouse, France.
[Russell, C. T.; Joy, S. P.; Mafi, J.] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
EM prettyman@psi.edu
RI Russell, Christopher/E-7745-2012; Beck, Andrew/J-7215-2015; Lawrence,
David/E-7463-2015
OI Russell, Christopher/0000-0003-1639-8298; Beck,
Andrew/0000-0003-4455-2299; Lawrence, David/0000-0002-7696-6667
NR 7
TC 0
Z9 0
U1 0
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A322
EP A322
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700289
ER
PT J
AU Weider, SZ
Nittler, LR
Starr, RD
Evans, LG
McCoy, TJ
Solomon, SC
AF Weider, Shoshana Z.
Nittler, Larry R.
Starr, Richard D.
Evans, Larry G.
McCoy, Timothy J.
Solomon, Sean C.
TI THE IRON CONTENT OF MERCURY'S SURFACE FROM MESSENGER X-RAY SPECTROMETRY.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
C1 [Weider, Shoshana Z.; Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA.
[McCoy, Timothy J.] Smithsonian Inst, Washington, DC 20013 USA.
EM sweider@ciw.edu
NR 7
TC 0
Z9 0
U1 0
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A403
EP A403
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700370
ER
PT J
AU Welzenbach, L
Corrigan, C
McCoy, T
Lunning, N
AF Welzenbach, L.
Corrigan, C.
McCoy, T.
Lunning, N.
TI ANTARCTIC METEORITES AT THE SMITHSONIAN INSTITUTION: PARTNERING WITH A
BIOREPOSITORY TO OPTIMIZE CURATION
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
C1 [Welzenbach, L.; Corrigan, C.; McCoy, T.; Lunning, N.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
EM welzenbl@si.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A407
EP A407
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700374
ER
PT J
AU Williams, CD
Wadhwa, M
Janney, PE
Hines, RR
Bullock, ES
MacPherson, GJ
AF Williams, C. D.
Wadhwa, M.
Janney, P. E.
Hines, R. R.
Bullock, E. S.
MacPherson, G. J.
TI Ti, Si and Mg Isotope Systematics of FUN CAI CMS-1.
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 75th Annual Meeting of the Meteoritical-Society
CY AUG 12-17, 2012
CL Cairns, AUSTRALIA
SP Meteorit Soc, Australian Natl Univ, Australian Sci Instruments, Barringer Crater Co, Cameca, Australian Govt, Dept Ind, Innovat Sci, Res & Tertiary Educ, IMCA, Japan Aerosp Explorat Agcy, Lunar & Planetary Inst, NASA, Planetary Studies Fdn, ThermoFisher Sci
ID METEORITES; ANOMALIES; TITANIUM; ALLENDE
C1 [Williams, C. D.; Wadhwa, M.; Janney, P. E.; Hines, R. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Bullock, E. S.; MacPherson, G. J.] Smithsonian Inst, Washington, DC 20560 USA.
EM cdwill10@asu.edu
RI Janney, Philip/K-2733-2013
OI Janney, Philip/0000-0001-5740-4266
NR 6
TC 0
Z9 0
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
SU 1
SI SI
BP A411
EP A411
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 987AV
UT WOS:000307389700378
ER
PT J
AU Richardson, DJ
Moser, WE
Richardson, KE
Hammond, CI
Lazo-Wasem, E
AF Richardson, Dennis J.
Moser, William E.
Richardson, Kristen E.
Hammond, Charlotte I.
Lazo-Wasem, Eric
TI New Host and Geographic Distribution Records for the Fish Leeches
Placobdella translucens (Sawyer and Shelley, 1976) and Myzobdella
reducta (Meyer, 1940) (Hirudinida)
SO COMPARATIVE PARASITOLOGY
LA English
DT Article
DE Placobdella translucens; Placobdella michiganensis; Placobdella phalera;
Myzobdella reducta; green sunfish; Lepomis cyanellus; pumpkinseed;
Lepomis gibbosus; Glossiphoniidae; Piscicolidae; Hirudinea; Annelida;
Nebraska
ID PISCICOLARIA-REDUCTA; FAMILY GLOSSIPHONIIDAE; WEST-VIRGINIA; WISCONSIN;
RHYNCHOBDELLIDA; REDESCRIPTION; PARASITES; ANNELIDA; LUGUBRIS; DARTER
AB The leeches Placobdella translucens (Sawyer and Shelley, 1976) and Myzobdella reducta (Meyer, 1940) are reported from Nebraska, U.S.A. for the first time. Individuals of M. reducta were collected from the caudal fins of 4 green sunfish (Lepomis cyanellus). A single pumpkinseed (Lepomis gibbosus) was infested with 2 individuals of P. translucens, constituting the first report of this species from a host. Placobdella translucens closely resembles Placobdella michiganensis (Sawyer. 1972) and Placobdella phalera (sensu Moore, 1906). In 1906, J. P. Moore established the most widely recognized concept of P. phalera when he "rather doubtfully referred" some material that he collected from Michigan to P. phalera (Graf, 1899). Placobdella phalera (Graf, 1899) was recently declared a junior synonym of Placobdella ornata. Given the similarities among the species, it is likely that at least some individuals previously identified as P. phalera (sensu Moore, 1906) represent P. translucens and/or P. michiganensis.
C1 [Richardson, Dennis J.; Richardson, Kristen E.; Hammond, Charlotte I.] Quinnipiac Univ, Hamden, CT 06518 USA.
[Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Suitland, MD 20746 USA.
[Lazo-Wasem, Eric] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA.
RP Richardson, DJ (reprint author), Quinnipiac Univ, 275 Mt Carmel Ave, Hamden, CT 06518 USA.
EM Dennis.Richardson@quinnipiac.edu; moserw@si.edu;
Kristen.Richardson@quinnipiac.edu; Charlotte.Hammond@quinnipiac.edu;
eric.lazo-wasem@yale.edu
FU School of Arts and Sciences, Quinnipiac University
FX Vince Kirby, Sr., graciously allowed access to the collecting site.
Katherine R. Richardson, Marjorie A. Richardson, Emma L. Richardson,
Benjamin Praeuner, and Susan A. Penas assisted in collecting fish.
Dwight and Nancy Praeuner provided logistic support. This study was
funded in part by a Grant-in-Aid Award (summer 2011) by The School of
Arts and Sciences, Quinnipiac University to D.J.R., and C.I.H. Tamara
Cook served as acting editor for this manuscript, arranging reviews and
exercising full editorial discretion, thereby allowing D.J.R. to
contribute to the Helminthological Society of Washington through
continued publication in Comparative Parasitology.
NR 54
TC 0
Z9 0
U1 2
U2 8
PU HELMINTHOLOGICAL SOC WASHINGTON
PI LAWRENCE
PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, ACCT# 141866, LAWRENCE, KS
66044 USA
SN 1525-2647
J9 COMP PARASITOL
JI Comp. Parasitol.
PD JUL
PY 2012
VL 79
IS 2
BP 293
EP 297
PG 5
WC Parasitology; Zoology
SC Parasitology; Zoology
GA 983OE
UT WOS:000307127800017
ER
PT J
AU Warrit, N
Michener, CD
Lekprayoon, C
AF Warrit, Natapot
Michener, Charles D.
Lekprayoon, Chariya
TI A REVIEW OF SMALL CARPENTER BEES OF THE GENUS CERATINA, SUBGENUS
CERATINIDIA, OF THAILAND (HYMENOPTERA, APIDAE)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Xylocopinae; locality records; Thailand; taxonomy; keys
AB Ten taxa of small carpenter bees belonging to subgenus Ceratinidia Cockerell and Porter, 1899, of the genus Ceratina Latreille, 1802, are recorded from Thailand. One new species, C. chiangmaiensis, is described. Ceratina lepida var. sutepensis Cockerell is elevated to full species status as C. sutepensis Cockerell. Ceratina lepida var. sublepida is synonymized under C. sutepensis. Lectotypes are designated for Ceratina cognata Smith, C. compacta Smith, and C. sutepensis Cockerell. Collecting records and brief taxonomic comments on Ceratinidia species in Thailand are presented, together with keys to the species.
C1 [Warrit, Natapot; Lekprayoon, Chariya] Chulalongkorn Univ, Fac Sci, Ctr Excellence Entomol, Dept Biol, Bangkok 10330, Thailand.
[Michener, Charles D.] Univ Kansas, Nat Hist Museum, Div Entomol, Lawrence, KS 66045 USA.
[Michener, Charles D.] Univ Kansas, Entomol Program, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA.
[Warrit, Natapot] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
RP Warrit, N (reprint author), Chulalongkorn Univ, Fac Sci, Ctr Excellence Entomol, Dept Biol, Bangkok 10330, Thailand.
EM michener@ku.edu; natapot.w@chula.ac.th
FU Biodiversity Research Training Program, Thailand [BRT-149006];
Hungerford Fund; Raymond Beamer Fellowship of the University of Kansas
Entomology Program, USA; Thailand Research Fund [TRfemale MRG5380139];
Grants for Development of New Faculty Staff, Chulalongkorn University,
Thailand
FX We thank the following people and their institutions for providing
specimens for study: Cornelius van Achterberg, John S. Ascher, George R.
Else, Michael S. Engel, Zachary H. Falin, David G. Furth, Tino
Gonsalves, Maureen Melo, Wojciech J. Pulawski, Jerome G. Rozen Jr., G.
Allan Samuelson, the late Roy R. Snelling, Prachaval Sukhumalanand, and
Yan-ru Wu. The research by CL and NW was largely supported from the
Biodiversity Research Training Program (BRT-149006), Thailand, and that
by NW, from the Hungerford Fund and the Raymond Beamer Fellowship of the
University of Kansas Entomology Program, USA, and the Thailand Research
Fund (TR female MRG5380139) and Grants for Development of New Faculty
Staff, Chulalongkorn University, Thailand.
NR 30
TC 0
Z9 1
U1 1
U2 11
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD JUL
PY 2012
VL 114
IS 3
BP 398
EP 416
DI 10.4289/0013-8797.114.3.398
PG 19
WC Entomology
SC Entomology
GA 988ZE
UT WOS:000307529200007
ER
PT J
AU Dobbs, MA
Lueker, M
Aird, KA
Bender, AN
Benson, BA
Bleem, LE
Carlstrom, JE
Chang, CL
Cho, HM
Clarke, J
Crawford, TM
Crites, AT
Flanigan, DI
de Haan, T
George, EM
Halverson, NW
Holzapfel, WL
Hrubes, JD
Johnson, BR
Joseph, J
Keisler, R
Kennedy, J
Kermish, Z
Lanting, TM
Lee, AT
Leitch, EM
Luong-Van, D
McMahon, JJ
Mehl, J
Meyer, SS
Montroy, TE
Padin, S
Plagge, T
Pryke, C
Richards, PL
Ruh, JE
Schaffer, KK
Schwan, D
Shirokoff, E
Spieler, HG
Staniszewski, Z
Stark, AA
Vanderlinde, K
Vieira, JD
Vu, C
Westbrook, B
Williamson, R
AF Dobbs, M. A.
Lueker, M.
Aird, K. A.
Bender, A. N.
Benson, B. A.
Bleem, L. E.
Carlstrom, J. E.
Chang, C. L.
Cho, H. -M.
Clarke, J.
Crawford, T. M.
Crites, A. T.
Flanigan, D. I.
de Haan, T.
George, E. M.
Halverson, N. W.
Holzapfel, W. L.
Hrubes, J. D.
Johnson, B. R.
Joseph, J.
Keisler, R.
Kennedy, J.
Kermish, Z.
Lanting, T. M.
Lee, A. T.
Leitch, E. M.
Luong-Van, D.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Montroy, T. E.
Padin, S.
Plagge, T.
Pryke, C.
Richards, P. L.
Ruh, J. E.
Schaffer, K. K.
Schwan, D.
Shirokoff, E.
Spieler, H. G.
Staniszewski, Z.
Stark, A. A.
Vanderlinde, K.
Vieira, J. D.
Vu, C.
Westbrook, B.
Williamson, R.
TI Frequency multiplexed superconducting quantum interference device
readout of large bolometer arrays for cosmic microwave background
measurements
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID SOUTH-POLE TELESCOPE; TRANSITION-EDGE SENSORS; X-RAY MICROCALORIMETERS;
APEX-SZ; GALAXY CLUSTERS; ELECTROTHERMAL FEEDBACK; SQUID MULTIPLEXERS;
CMB POLARIZATION; POWER SPECTRUM; MILLIMETER
AB A technological milestone for experiments employing transition edge sensor bolometers operating at sub-Kelvin temperature is the deployment of detector arrays with 100s-1000s of bolometers. One key technology for such arrays is readout multiplexing: the ability to read out many sensors simultaneously on the same set of wires. This paper describes a frequency-domain multiplexed readout system which has been developed for and deployed on the APEX-SZ and South Pole Telescope millimeter wavelength receivers. In this system, the detector array is divided into modules of seven detectors, and each bolometer within the module is biased with a unique similar to MHz sinusoidal carrier such that the individual bolometer signals are well separated in frequency space. The currents from all bolometers in a module are summed together and pre-amplified with superconducting quantum interference devices operating at 4 K. Room temperature electronics demodulate the carriers to recover the bolometer signals, which are digitized separately and stored to disk. This readout system contributes little noise relative to the detectors themselves, is remarkably insensitive to unwanted microphonic excitations, and provides a technology pathway to multiplexing larger numbers of sensors. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4737629]
C1 [Dobbs, M. A.; de Haan, T.; Kennedy, J.; Lanting, T. M.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Lueker, M.; Clarke, J.; Flanigan, D. I.; George, E. M.; Holzapfel, W. L.; Johnson, B. R.; Kermish, Z.; Lee, A. T.; Richards, P. L.; Schwan, D.; Shirokoff, E.; Westbrook, B.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.; Vieira, J. D.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
[Bender, A. N.; Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Bender, A. N.; Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Schaffer, K. K.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Padin, S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Cho, H. -M.] Natl Inst Stand & Technol, Boulder, CO 80305 USA.
[Clarke, J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Mat Sci, Berkeley, CA 94720 USA.
[Johnson, B. R.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Joseph, J.; Vu, C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Engn, Berkeley, CA 94720 USA.
[Lanting, T. M.] D Wave Syst, Burnaby, BC V5C 6G9, Canada.
[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.
[Montroy, T. E.; Ruh, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Montroy, T. E.; Ruh, J. E.; Staniszewski, Z.] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA.
[Pryke, C.] Univ Minnesota Twin Cities, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Dobbs, MA (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518
FU National Science Foundation (NSF) funds APEX-SZ [AST-0138348,
AST-0709497]; South Pole Telescope [ANT-0638937, ANT-0130612]; U.S.
Department of Energy (DOE) [DE-AC02-05CH11231]; Natural Sciences and
Engineering Research Council of Canada; Canadian Institute for Advanced
Research; Canadian Foundation for Innovation; Canada Research Chairs
program; Sloan Fellowship
FX The National Science Foundation (NSF) funds APEX-SZ through Grant Nos.
AST-0138348 and AST-0709497 and the South Pole Telescope through Grant
Nos. ANT-0638937 and ANT-0130612. Work at LBNL is supported by the U.S.
Department of Energy (DOE) under Contract No. DE-AC02-05CH11231. The
McGill team acknowledges funding from the Natural Sciences and
Engineering Research Council of Canada, Canadian Institute for Advanced
Research, and the Canadian Foundation for Innovation. M.D. acknowledges
support from the Canada Research Chairs program and a Sloan Fellowship.
NR 75
TC 39
Z9 39
U1 1
U2 12
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD JUL
PY 2012
VL 83
IS 7
AR 073113
DI 10.1063/1.4737629
PG 24
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 988YR
UT WOS:000307527900014
PM 22852677
ER
PT J
AU des Etangs, AL
Bourrier, V
Wheatley, PJ
Dupuy, H
Ehrenreich, D
Vidal-Madjar, A
Hebrard, G
Ballester, GE
Desert, JM
Ferlet, R
Sing, DK
AF des Etangs, A. Lecavelier
Bourrier, V.
Wheatley, P. J.
Dupuy, H.
Ehrenreich, D.
Vidal-Madjar, A.
Hebrard, G.
Ballester, G. E.
Desert, J. -M.
Ferlet, R.
Sing, D. K.
TI Temporal variations in the evaporating atmosphere of the exoplanet HD
189733b
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE planetary systems; stars: individual: HD 189733; techniques:
spectroscopic; planets and satellites: atmospheres; stars: flare
ID EXTRASOLAR PLANET HD209458B; ENERGETIC NEUTRAL ATOMS; HOT JUPITERS;
X-RAY; LYMAN-ALPHA; MASS-LOSS; 209458B; HYDROGEN; ULTRAVIOLET;
HD-209458B
AB Atmospheric escape has been detected from the exoplanet HD 209458b through transit observations of the hydrogen Lyman-alpha line. Here we present spectrally resolved Lyman-alpha transit observations of the exoplanet HD 189733b at two different epochs. These HST/STIS observations show for the first time that there are significant temporal variations in the physical conditions of an evaporating planetary atmosphere. While atmospheric hydrogen is not detected in the first epoch observations, it is observed at the second epoch, producing a transit absorption depth of 14.4 +/- 3.6% between velocities of -230 to -140 km s(-1). Contrary to HD 209458b, these high velocities cannot arise from radiation pressure alone and require an additional acceleration mechanism, such as interactions with stellar wind protons. The observed absorption can be explained by an atmospheric escape rate of neutral hydrogen atoms of about 10(9) g s(-1), a stellar wind with a velocity of 190 kms(-1) and a temperature of similar to 10(5) K. An X-ray flare from the active star seen with Swift/XRT 8 h before the second-epoch observation supports the idea that the observed changes within the upper atmosphere of the planet can be caused by variations in the stellar wind properties, or by variations in the stellar energy input to the planetary escaping gas (or a mix of the two effects). These observations provide the first indication of interaction between the exoplanet's atmosphere and stellar variations.
C1 [des Etangs, A. Lecavelier; Bourrier, V.; Dupuy, H.; Vidal-Madjar, A.; Hebrard, G.; Ferlet, R.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[des Etangs, A. Lecavelier; Bourrier, V.; Dupuy, H.; Vidal-Madjar, A.; Hebrard, G.; Ferlet, R.] Univ Paris 06, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Ehrenreich, D.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, Grenoble, France.
[Ballester, G. E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sing, D. K.] Univ Exeter, Astrophys Grp, Sch Phys, Exeter EX4 4QL, Devon, England.
RP des Etangs, AL (reprint author), CNRS, UMR 7095, Inst Astrophys Paris, 98Bis Blvd Arago, F-75014 Paris, France.
EM lecaveli@iap.fr
OI Ehrenreich, David/0000-0001-9704-5405; Wheatley,
Peter/0000-0003-1452-2240; Sing, David /0000-0001-6050-7645
FU NASA [NAS 5-26555]; STScI [HST-GO-11673.01-A]; Fondation Simone et Cino
Del Duca
FX Based on observations made with the NASA/ESA Hubble Space Telescope,
obtained at the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-26555. This research has made use of data obtained
from NASA's Swift satellite. G. E. B. acknowledges financial support by
this program through STScI grant HST-GO-11673.01-A to the University of
Arizona. These observations are associated with program #11673. This
work has been supported by an award from the Fondation Simone et Cino
Del Duca.
NR 35
TC 65
Z9 65
U1 1
U2 4
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2012
VL 543
AR L4
DI 10.1051/0004-6361/201219363
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 976PQ
UT WOS:000306597200167
ER
PT J
AU Hassall, TE
Stappers, BW
Hessels, JWT
Kramer, M
Alexov, A
Anderson, K
Coenen, T
Karastergiou, A
Keane, EF
Kondratiev, VI
Lazaridis, K
van Leeuwen, J
Noutsos, A
Serylak, M
Sobey, C
Verbiest, JPW
Weltevrede, P
Zagkouris, K
Fender, R
Wijers, RAMJ
Bahren, L
Bell, ME
Broderick, JW
Corbel, S
Daw, EJ
Dhillon, VS
Eisloffel, J
Falcke, H
Griessmeier, JM
Jonker, P
Law, C
Markoff, S
Miller-Jones, JCA
Osten, R
Rol, E
Scaife, AMM
Scheers, B
Schellart, P
Spreeuw, H
Swinbank, J
ter Veen, S
Wise, MW
Wijnands, R
Wucknitz, O
Zarka, P
Asgekar, A
Bell, MR
Bentum, MJ
Bernardi, G
Best, P
Bonafede, A
Boonstra, AJ
Brentjens, M
Brouw, WN
Bruggen, M
Butcher, HR
Ciardi, B
Garrett, MA
Gerbers, M
Gunst, AW
van Haarlem, MP
Heald, G
Hoeft, M
Holties, H
de Jong, A
Koopmans, LVE
Kuniyoshi, M
Kuper, G
Loose, GM
Maat, P
Masters, J
McKean, JP
Meulman, H
Mevius, M
Munk, H
Noordam, JE
Orru, E
Paas, H
Pandey-Pommier, M
Pandey, VN
Pizzo, R
Polatidis, A
Reich, W
Rottgering, H
Sluman, J
Steinmetz, M
Sterks, CGM
Tagger, M
Tang, Y
Tasse, C
Vermeulen, R
van Weeren, RJ
Wijnholds, SJ
Yatawatta, S
AF Hassall, T. E.
Stappers, B. W.
Hessels, J. W. T.
Kramer, M.
Alexov, A.
Anderson, K.
Coenen, T.
Karastergiou, A.
Keane, E. F.
Kondratiev, V. I.
Lazaridis, K.
van Leeuwen, J.
Noutsos, A.
Serylak, M.
Sobey, C.
Verbiest, J. P. W.
Weltevrede, P.
Zagkouris, K.
Fender, R.
Wijers, R. A. M. J.
Bahren, L.
Bell, M. E.
Broderick, J. W.
Corbel, S.
Daw, E. J.
Dhillon, V. S.
Eisloeffel, J.
Falcke, H.
Griessmeier, J. -M.
Jonker, P.
Law, C.
Markoff, S.
Miller-Jones, J. C. A.
Osten, R.
Rol, E.
Scaife, A. M. M.
Scheers, B.
Schellart, P.
Spreeuw, H.
Swinbank, J.
ter Veen, S.
Wise, M. W.
Wijnands, R.
Wucknitz, O.
Zarka, P.
Asgekar, A.
Bell, M. R.
Bentum, M. J.
Bernardi, G.
Best, P.
Bonafede, A.
Boonstra, A. J.
Brentjens, M.
Brouw, W. N.
Brueggen, M.
Butcher, H. R.
Ciardi, B.
Garrett, M. A.
Gerbers, M.
Gunst, A. W.
van Haarlem, M. P.
Heald, G.
Hoeft, M.
Holties, H.
de Jong, A.
Koopmans, L. V. E.
Kuniyoshi, M.
Kuper, G.
Loose, G. M.
Maat, P.
Masters, J.
McKean, J. P.
Meulman, H.
Mevius, M.
Munk, H.
Noordam, J. E.
Orru, E.
Paas, H.
Pandey-Pommier, M.
Pandey, V. N.
Pizzo, R.
Polatidis, A.
Reich, W.
Rottgering, H.
Sluman, J.
Steinmetz, M.
Sterks, C. G. M.
Tagger, M.
Tang, Y.
Tasse, C.
Vermeulen, R.
van Weeren, R. J.
Wijnholds, S. J.
Yatawatta, S.
TI Wide-band simultaneous observations of pulsars: disentangling dispersion
measure and profile variations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE pulsars: general; ISM: general; magnetic fields; telescopes
ID ARRIVAL-TIME DELAY; EMPIRICAL-THEORY; RADIO-EMISSION; INTERSTELLAR
SCATTERING; SUPERDISPERSION DELAY; FREQUENCY-DEPENDENCE; SPECTRAL
BEHAVIOR; PULSES; REFRACTION; RADIATION
AB Dispersion in the interstellar medium is a well known phenomenon that follows a simple relationship, which has been used to predict the time delay of dispersed radio pulses since the late 1960s. We performed wide-band simultaneous observations of four pulsars with LOFAR (at 40-190 MHz), the 76-m Lovell Telescope (at 1400 MHz) and the Effelsberg 100-m Telescope (at 8000 MHz) to test the accuracy of the dispersion law over a broad frequency range. In this paper we present the results of these observations which show that the dispersion law is accurate to better than 1 part in 105 across our observing band. We use this fact to constrain some of the properties of the interstellar medium along the line-of-sight and use the lack of any aberration or retardation effects to determine upper limits on emission heights in the pulsar magnetosphere. We also discuss the effect of pulse profile evolution on our observations, and the implications that it could have for precision pulsar timing projects such as the detection of gravitational waves with pulsar timing arrays.
C1 [Hassall, T. E.; Stappers, B. W.; Kramer, M.; Weltevrede, P.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England.
[Hessels, J. W. T.; Kondratiev, V. I.; van Leeuwen, J.; Falcke, H.; Wise, M. W.; Asgekar, A.; Bentum, M. J.; Boonstra, A. J.; Brentjens, M.; Butcher, H. R.; Garrett, M. A.; Gerbers, M.; Gunst, A. W.; van Haarlem, M. P.; Heald, G.; Holties, H.; de Jong, A.; Kuper, G.; Loose, G. M.; Maat, P.; McKean, J. P.; Meulman, H.; Mevius, M.; Munk, H.; Noordam, J. E.; Paas, H.; Pandey, V. N.; Pizzo, R.; Polatidis, A.; Sluman, J.; Tang, Y.; Vermeulen, R.; van Weeren, R. J.; Wijnholds, S. J.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Hessels, J. W. T.; Alexov, A.; Anderson, K.; Coenen, T.; van Leeuwen, J.; Wijers, R. A. M. J.; Bahren, L.; Law, C.; Markoff, S.; Miller-Jones, J. C. A.; Rol, E.; Scheers, B.; Spreeuw, H.; Swinbank, J.; Wise, M. W.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Kramer, M.; Keane, E. F.; Lazaridis, K.; Noutsos, A.; Sobey, C.; Verbiest, J. P. W.; Falcke, H.; Kuniyoshi, M.; Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Karastergiou, A.; Zagkouris, K.] Univ Oxford, Oxford OX1 3RH, England.
[Serylak, M.] CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France.
[Serylak, M.; Griessmeier, J. -M.; Tagger, M.] CNRS, UMR 7328, LPC2E, F-45071 Orleans 02, France.
[Fender, R.; Bell, M. E.; Broderick, J. W.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Bell, M. E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Corbel, S.] Univ Paris 07, F-91191 Gif Sur Yvette, France.
[Corbel, S.] CEA Saclay, UMR AIM, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Corbel, S.] Inst Univ France, F-75005 Paris, France.
[Daw, E. J.; Dhillon, V. S.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
[Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany.
[Falcke, H.; Jonker, P.; Schellart, P.; ter Veen, S.; Orru, E.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Jonker, P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands.
[Jonker, P.; Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Law, C.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA USA.
[Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Osten, R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Scheers, B.] CWI, NL-1090 GB Amsterdam, Netherlands.
[Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Zarka, P.; Tasse, C.] UPMC, CNRS, Observ Paris, LESIA, F-92195 Meudon, France.
[Bell, M. R.; Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Bonafede, A.; Brueggen, M.] Jacobs Univ Bremen, D-28759 Bremen, Germany.
[Brouw, W. N.; Koopmans, L. V. E.; Yatawatta, S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia.
[Garrett, M. A.; Rottgering, H.; van Weeren, R. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Masters, J.] NRAO Headquarters, Charlottesville, VA 22903 USA.
[Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France.
[Steinmetz, M.] Leibniz Inst Fr Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Sterks, C. G. M.] Univ Groningen, CIT, NL-9700 AB Groningen, Netherlands.
RP Hassall, TE (reprint author), Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England.
EM tomehassall@gmail.com
RI Falcke, Heino/H-5262-2012; Yatawatta, Sarod/E-6037-2013; Miller-Jones,
James/B-2411-2013; Tagger, Michel/O-6615-2014; Ciardi,
Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015;
OI Falcke, Heino/0000-0002-2526-6724; Yatawatta, Sarod/0000-0001-5619-4017;
Wijers, Ralph/0000-0002-3101-1808; Miller-Jones,
James/0000-0003-3124-2814; Tagger, Michel/0000-0003-2962-3220;
Kondratiev, Vladislav/0000-0001-8864-7471; Swinbank,
John/0000-0001-9445-1846; van Weeren, Reinout/0000-0002-0587-1660
FU STFC studentship; Netherlands Research School for Astronomy
[NOVA3-NW3-2.3.1]; European Commission [FP7-PEOPLE-2007-4-3-IRG,
224838]; Leverhulme Trust; European Union [236394]; DFG (German Research
Foundation) within the framework of the Research Unit [FOR 1254]
FX We would like to thank Jim Cordes for his insight and useful
discussions, Christine Jordan for arranging the observations from
Jodrell Bank, and the anonymous referee for their insightful comments.
LOFAR, the LOw Frequency ARray designed and constructed by ASTRON, has
facilities in several countries, that are owned by various parties (each
with their own funding sources), and that are collectively operated by
the International LOFAR Telescope (ILT) foundation under a joint
scientific policy. This publication made use of observations taken with
the 100-m telescopes of the MPIfR (Max-Planck-Institut fur
Radioastronomie) at Effelsberg. Ben Stappers, Patrick Weltevrede and the
Lovell observations are supported through an STFC rolling grant. Tom
Hassall is the recipient of an STFC studentship. Jason Hessels is a Veni
Fellow of the Netherlands Foundation for Scientific Research. Joeri van
Leeuwen and Thijs Coenen are supported by the Netherlands Research
School for Astronomy (Grant NOVA3-NW3-2.3.1) and by the European
Commission (Grant FP7-PEOPLE-2007-4-3-IRG #224838). Aris Karastergiou is
grateful to the Leverhulme Trust for financial support. Joris Verbiest
is supported by the European Union under Marie Curie Intra-European
Fellowship 236394. Charlotte Sobey is supported by the DFG (German
Research Foundation) within the framework of the Research Unit FOR 1254,
Magnetisation of Interstellar and Intergalactic Media: The Prospects of
Low-Frequency Radio Observations.
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JI Astron. Astrophys.
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SC Astronomy & Astrophysics
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ER
PT J
AU Hatzes, AP
Zechmeister, M
Matthews, J
Kuschnig, R
Walker, GAH
Dollinger, M
Guenther, DB
Moffat, AFJ
Rucinski, SM
Sasselov, D
Weiss, WW
AF Hatzes, A. P.
Zechmeister, M.
Matthews, J.
Kuschnig, R.
Walker, G. A. H.
Doellinger, M.
Guenther, D. B.
Moffat, A. F. J.
Rucinski, S. M.
Sasselov, D.
Weiss, W. W.
TI The mass of the planet-hosting giant star beta Geminorum determined from
its p-mode oscillation spectrum
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: radial velocities; stars: individual: beta Geminorum; stars:
late-type
ID RADIAL-VELOCITY VARIATIONS; SOLAR-LIKE OSCILLATIONS; STELLAR
OSCILLATIONS; SPECTROSCOPIC SURVEY; EPSILON-OPHIUCHI; RED GIANTS;
ASTEROSEISMOLOGY; PULSATIONS; ISOCHRONES; PARAMETERS
AB Aims. Our aim is to use precise radial velocity measurements and photometric data to derive the frequency spacing of the p-mode oscillation spectrum of the planet-hosting star beta Gem. This spacing along with the interferometric radius for this star can then be used to derive an accurate stellar mass.
Methods. We use a long time series of over 60 h of precise stellar radial velocity measurements of beta Gem taken with an iodine absorption cell at the echelle spectrograph mounted on the 2 m Alfred Jensch Telescope. We also present complementary photometric data for this star taken with the MOST microsatellite spanning 3.6 d. A Fourier analysis is used to derive the frequencies that are present in each data set.
Results. The Fourier analysis of the radial velocity data reveals the presence of up to 17 significant pulsation modes in the frequency interval 10-250 mu Hz. Most of these fall on a grid of equally-spaced frequencies having a separation of 7.14 +/- 0.12 mu Hz. An analysis of 3.6 days of high precision photometry taken with the MOST space telescopes shows the presence of up to 16 modes, six of which are consistent with modes found in the spectral (radial velocity) data. This frequency spacing is consistent with high overtone radial pulsations; however, until the pulsation modes are identified we cannot be sure if some of these are nonradial modes or even mixed modes. The radial velocity frequency spacing along with angular diameter measurements of beta Gem via interferometry results in a stellar mass of M = 1.91 +/- 0.09 M-circle dot. This value confirms the intermediate mass of the star determined using stellar evolutionary tracks.
Conclusions. beta Gem is confirmed to be an intermediate mass star. Stellar pulsations in giant stars along with interferometric radius measurements can provide accurate determinations of the stellar mass of planet hosting giant stars. These can also be used to calibrate stellar evolutionary tracks.
C1 [Hatzes, A. P.; Doellinger, M.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Zechmeister, M.] Univ Gottingen, D-37077 Gottingen, Germany.
[Matthews, J.] Univ British Columbia, Dept Phys, Vancouver, BC V6T 1Z1, Canada.
[Kuschnig, R.; Weiss, W. W.] Univ Wien, Inst Astron, A-1180 Vienna, Austria.
[Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Observ Astron Mt Megant, Montreal, PQ H3C 3J7, Canada.
[Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
RP Hatzes, AP (reprint author), Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany.
EM artie@tls-tautenburg.de
FU Deutsche Forschungsgemeinschaft (DFG) [HA 3279/5-1, RE 1664/4-1]
FX We thank the referee for useful comments that improved the manuscript.
This research has made use of the SIMBAD data base operated at CDS,
Strasbourg, France. A. P. H. acknowledges grant HA 3279/5-1 from the
Deutsche Forschungsgemeinschaft (DFG). M.Z. acknowledges financial
support from DFG grant RE 1664/4-1.
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JI Astron. Astrophys.
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PY 2012
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SC Astronomy & Astrophysics
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UT WOS:000306597200098
ER
PT J
AU Menten, KM
Reid, MJ
Kaminski, T
Claussen, MJ
AF Menten, K. M.
Reid, M. J.
Kaminski, T.
Claussen, M. J.
TI The size, luminosity, and motion of the extreme carbon star IRC+10216
(CW Leonis)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrometry; proper motions; stars: AGB and post-AGB; stars: carbon; ISM:
kinematics and dynamics; radio continuum: stars
ID ASYMPTOTIC GIANT BRANCH; INFRARED OBJECT IRC&10216; MASS-LOSS HISTORY;
CIRCUMSTELLAR ENVELOPE; RADIO-CONTINUUM; LINE SURVEY; DUST SHELL; BOW
SHOCKS; EVOLUTION; MIRA
AB Very Large Array observations of the extreme carbon star IRC+10216 at 7 mm wavelength with 40 milli-arcsec resolution resolve the object's radio emission, which forms an almost round uniform disk of 83 milli-arcsec diameter, corresponding to 11 AU (for an assumed distance of 130 pc). We find a brightness temperature of 1630 K for the radio photosphere. Since the emission is optically thick, we can directly estimate IRC+10216's average luminosity, which is 8600 L-circle dot. This value is in excellent agreement with what is predicted from the period-luminosity relation for carbon-rich Miras. Assuming an effective temperature of 2750 K for IRC+10216, it implies an optical photospheric diameter of 3.8 AU. Our precise determination of IRC+10216's proper motion fits the picture presented by far-ultraviolet and far-infrared wavelength observations of its interaction region with the interstellar medium (its "astrosphere"): the star moves roughly in the direction expected from the morphology of the termination shock and its astrotail structures. Calculation of its three dimensional velocity and an analysis of the kinematics of its surrounding interstellar medium (ISM) suggest an appreciable relative velocity of 42 km s(-1), which is about half the value discussed in recent studies. This suggests a lower (time-averaged) mass loss rate and/or a higher ISM density than previously assumed.
C1 [Menten, K. M.; Kaminski, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Claussen, M. J.] Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA.
RP Menten, KM (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM kmenten@mpifr-bonn.mpg.de; reid@cfa.harvard.edu;
kaminski@mpifr-bonn.mpg.de; mclausse@nrao.edu
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J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
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PY 2012
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SC Astronomy & Astrophysics
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UT WOS:000306597200073
ER
PT J
AU Mortier, A
Santos, NC
Sozzetti, A
Mayor, M
Latham, D
Bonfils, X
Udry, S
AF Mortier, A.
Santos, N. C.
Sozzetti, A.
Mayor, M.
Latham, D.
Bonfils, X.
Udry, S.
TI The frequency of giant planets around metal-poor stars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques: radial velocities; planetary systems; planets and
satellites: formation; stars: abundances; stars: statistics
ID EXTRA-SOLAR PLANETS; HARPS SEARCH; STELLAR METALLICITY; DISK
INSTABILITY; WIDE ORBITS; K-GIANTS; MASS; DWARF; GAS; DETECTABILITY
AB Context. The discovery of about 700 extrasolar planets, so far, has lead to the first statistics concerning extrasolar planets. The presence of giant planets seems to depend on stellar metallicity and mass. For example, they are more frequent around metal-rich stars, with an exponential increase in planet occurrence rates with metallicity.
Aims. We analyzed two samples of metal-poor stars (-2.0 <= [Fe/H] <= 0.0) to see if giant planets are indeed rare around these objects. Radial velocity datasets were obtained with two different spectrographs (HARPS and HIRES). Detection limits for these data, expressed in minimum planetary mass and period, are calculated. These produce trustworthy numbers for the planet frequency.
Methods. A general Lomb-Scargle (GLS) periodogram analysis was used together with a bootstrapping method to produce the detection limits. Planet frequencies were calculated based on a binomial distribution function within metallicity bins.
Results. Almost all hot Jupiters and most giant planets should have been found in these data. Hot Jupiters around metal-poor stars have a frequency lower than 1.0% at one sigma. Giant planets with periods up to 1800 days, however, have a higher frequency of f(p) = 2.63(-0.8)(+2.5)%. Taking into account the different metallicities of the stars, we show that giant planets appear to be very frequent (f(p) = 4.48(-1.38)(+4.04)%) around stars with [Fe/H] > -0.7, while they are rare around stars with [Fe/H] <= -0.7 (<= 2.36% at one sigma).
Conclusions. Giant planet frequency is indeed a strong function of metallicity, even in the low-metallicity tail. However, the frequencies are most likely higher than previously thought.
C1 [Mortier, A.; Santos, N. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4150762 Oporto, Portugal.
[Sozzetti, A.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy.
[Mayor, M.; Udry, S.] Univ Geneva, Observ Genve, CH-1290 Sauverny, Switzerland.
[Latham, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bonfils, X.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France.
RP Mortier, A (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal.
EM amortier@astro.up.pt
RI Santos, Nuno/E-9957-2011;
OI Santos, Nuno/0000-0003-4422-2919; Sozzetti,
Alessandro/0000-0002-7504-365X; Bonfils, Xavier/0000-0001-9003-8894;
Mortier, Annelies/0000-0001-7254-4363
FU W. M. Keck Foundation; European Research Council/European Community
[239953]; Fundacao para a Ciencia e a Tecnologia (FCT); FCT/MCTES
(Portugal); POPH/FSE (EC); [PTDC/CTE-AST/098528/2008];
[PTDC/CTE-AST/09860/2008]
FX The data presented herein are based on observations collected at the La
Silla Parana Observatory, ESO (Chile) with the HARPS spectrograph at the
3.6-m telescope (ESO runs ID 72.C-0488, 082.C-0212, and 085.C-0063) and
at the W. M. Keck Observatory that is operated as a scientific
partnership among the California Institute of Technology, the University
of California and the National Aeronautics and Space Administration.
This Observatory was made possible by the generous financial support of
the W. M. Keck Foundation.; We thank the ananymous referee for his/her
useful comments. This work was supported by the European Research
Council/European Community under the FP7 through Starting Grant
agreement number 239953. N.C.S. also acknowledges the support from
Fundacao para a Ciencia e a Tecnologia (FCT) through program Ciencia
2007 funded by FCT/MCTES (Portugal) and POPH/FSE (EC), and in the form
of grants reference PTDC/CTE-AST/098528/2008 and
PTDC/CTE-AST/09860/2008.
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PY 2012
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SC Astronomy & Astrophysics
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UT WOS:000306597200045
ER
PT J
AU van Weeren, RJ
Rottgering, HJA
Rafferty, DA
Pizzo, R
Bonafede, A
Bruggen, M
Brunetti, G
Ferrari, C
Orru, E
Heald, G
McKean, JP
Tasse, C
de Gasperin, F
Birzan, L
van Zwieten, JE
van der Tol, S
Shulevski, A
Jackson, N
Offringa, AR
Conway, J
Intema, HT
Clarke, TE
van Bemmel, I
Miley, GK
White, GJ
Hoeft, M
Cassano, R
Macario, G
Morganti, R
Wise, MW
Horellou, C
Valentijn, EA
Wucknitz, O
Kuijken, K
Ensslin, TA
Anderson, J
Asgekar, A
Avruch, IM
Beck, R
Bell, ME
Bell, MR
Bentum, MJ
Bernardi, G
Best, P
Boonstra, AJ
Brentjens, M
van de Brink, RH
Broderick, J
Brouw, WN
Butcher, HR
van Cappellen, W
Ciardi, B
Eisloffel, J
Falcke, H
Fender, R
Garrett, MA
Gerbers, M
Gunst, A
van Haarlem, MP
Hamaker, JP
Hassall, T
Hessels, JWT
Koopmans, LVE
Kuper, G
van Leeuwen, J
Maat, P
Millenaar, R
Munk, H
Nijboer, R
Noordam, JE
Pandey, VN
Pandey-Pommier, M
Polatidis, A
Reich, W
Scaife, AMM
Schoenmakers, A
Sluman, J
Stappers, BW
Steinmetz, M
Swinbank, J
Tagger, M
Tang, Y
Vermeulen, R
de Vos, M
van Haarlem, MP
AF van Weeren, R. J.
Rottgering, H. J. A.
Rafferty, D. A.
Pizzo, R.
Bonafede, A.
Brueggen, M.
Brunetti, G.
Ferrari, C.
Orru, E.
Heald, G.
McKean, J. P.
Tasse, C.
de Gasperin, F.
Birzan, L.
van Zwieten, J. E.
van der Tol, S.
Shulevski, A.
Jackson, N.
Offringa, A. R.
Conway, J.
Intema, H. T.
Clarke, T. E.
van Bemmel, I.
Miley, G. K.
White, G. J.
Hoeft, M.
Cassano, R.
Macario, G.
Morganti, R.
Wise, M. W.
Horellou, C.
Valentijn, E. A.
Wucknitz, O.
Kuijken, K.
Ensslin, T. A.
Anderson, J.
Asgekar, A.
Avruch, I. M.
Beck, R.
Bell, M. E.
Bell, M. R.
Bentum, M. J.
Bernardi, G.
Best, P.
Boonstra, A-J
Brentjens, M.
van de Brink, R. H.
Broderick, J.
Brouw, W. N.
Butcher, H. R.
van Cappellen, W.
Ciardi, B.
Eisloeffel, J.
Falcke, H.
Fender, R.
Garrett, M. A.
Gerbers, M.
Gunst, A.
van Haarlem, M. P.
Hamaker, J. P.
Hassall, T.
Hessels, J. W. T.
Koopmans, L. V. E.
Kuper, G.
van Leeuwen, J.
Maat, P.
Millenaar, R.
Munk, H.
Nijboer, R.
Noordam, J. E.
Pandey, V. N.
Pandey-Pommier, M.
Polatidis, A.
Reich, W.
Scaife, A. M. M.
Schoenmakers, A.
Sluman, J.
Stappers, B. W.
Steinmetz, M.
Swinbank, J.
Tagger, M.
Tang, Y.
Vermeulen, R.
de Vos, M.
van Haarlem, M. P.
TI First LOFAR observations at very low frequencies of cluster-scale
non-thermal emission: the case of Abell 2256
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE telescopes; radio continuum: general; galaxies: clusters: individual:
Abell 2256; large-scale structure of Universe
ID MERGING GALAXY CLUSTER; EXTENDED RADIO-EMISSION; X-RAY-EMISSION; DEEP
1.4 GHZ; SHOCK ACCELERATION; PARTICLE-ACCELERATION; MAGNETIC-FIELDS;
COMA CLUSTER; SKY SURVEY; ASTROPHYSICAL SHOCKS
AB Abell 2256 is one of the best known examples of a galaxy cluster hosting large-scale diffuse radio emission that is unrelated to individual galaxies. It contains both a giant radio halo and a relic, as well as a number of head-tail sources and smaller diffuse steep-spectrum radio sources. The origin of radio halos and relics is still being debated, but over the last years it has become clear that the presence of these radio sources is closely related to galaxy cluster merger events. Here we present the results from the first LOFAR low band antenna (LBA) observations of Abell 2256 between 18 and 67 MHz. To our knowledge, the image presented in this paper at 63 MHz is the deepest ever obtained at frequencies below 100 MHz in general. Both the radio halo and the giant relic are detected in the image at 63 MHz, and the diffuse radio emission remains visible at frequencies as low as 20 MHz. The observations confirm the presence of a previously claimed ultra-steep spectrum source to the west of the cluster center with a spectral index of -2.3 +/- 0.4 between 63 and 153 MHz. The steep spectrum suggests that this source is an old part of a head-tail radio source in the cluster. For the radio relic we find an integrated spectral index of -0.81 +/- 0.03, after removing the flux contribution from the other sources. This is relatively flat which could indicate that the efficiency of particle acceleration at the shock substantially changed in the last similar to 0.1 Gyr due to an increase of the shock Mach number. In an alternative scenario, particles are re-accelerated by some mechanism in the downstream region of the shock, resulting in the relatively flat integrated radio spectrum. In the radio halo region we find indications of low-frequency spectral steepening which may suggest that relativistic particles are accelerated in a rather inhomogeneous turbulent region.
C1 [van Weeren, R. J.; Rottgering, H. J. A.; Rafferty, D. A.; Birzan, L.; van der Tol, S.; Miley, G. K.; Kuijken, K.; Garrett, M. A.; Pandey-Pommier, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Weeren, R. J.; Pizzo, R.; Heald, G.; McKean, J. P.; van Zwieten, J. E.; van Bemmel, I.; Morganti, R.; Wise, M. W.; Asgekar, A.; Avruch, I. M.; Bentum, M. J.; Boonstra, A-J; Brentjens, M.; van de Brink, R. H.; Brouw, W. N.; Butcher, H. R.; van Cappellen, W.; Falcke, H.; Garrett, M. A.; Gerbers, M.; Gunst, A.; van Haarlem, M. P.; Hamaker, J. P.; Hessels, J. W. T.; Kuper, G.; van Leeuwen, J.; Maat, P.; Millenaar, R.; Munk, H.; Nijboer, R.; Noordam, J. E.; Polatidis, A.; Schoenmakers, A.; Sluman, J.; Tang, Y.; Vermeulen, R.; de Vos, M.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Bonafede, A.; Brueggen, M.] Jacobs Univ Bremen, D-28759 Bremen, Germany.
[Brunetti, G.; Cassano, R.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06300 Nice, France.
[Orru, E.; Falcke, H.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Tasse, C.] Observ Paris, GEPI, F-92190 Meudon, France.
[de Gasperin, F.; Valentijn, E. A.; Ensslin, T. A.; Bell, M. R.; Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Shulevski, A.; Offringa, A. R.; Morganti, R.; Avruch, I. M.; Brouw, W. N.; Koopmans, L. V. E.; Pandey, V. N.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Jackson, N.; Hassall, T.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Conway, J.; Horellou, C.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden.
[Intema, H. T.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Clarke, T. E.] USN, Res Lab, Washington, DC 20375 USA.
[White, G. J.] Open Univ, Dept Phys & Astron, Heerlen, Netherlands.
[White, G. J.] Rutherford Appleton Lab, Dept Space Sci, Chilton, England.
[Hoeft, M.; Eisloeffel, J.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany.
[Wise, M. W.; Hessels, J. W. T.; van Leeuwen, J.; Swinbank, J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Anderson, J.; Beck, R.; Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Bell, M. E.; Broderick, J.; Fender, R.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Butcher, H. R.] Australian Natl Univ, Mt Stromlo Obs, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France.
[Steinmetz, M.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Tagger, M.] Lab Phys & Chim Environm & Espace, F-45071 Orleans 2, France.
RP van Weeren, RJ (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM rvweeren@strw.leidenuniv.nl
RI Falcke, Heino/H-5262-2012; Tagger, Michel/O-6615-2014; Shulevski,
Aleksandar/E-5591-2015; Ciardi, Benedetta/N-7625-2015; Intema,
Huib/D-1438-2012;
OI Falcke, Heino/0000-0002-2526-6724; Tagger, Michel/0000-0003-2962-3220;
Shulevski, Aleksandar/0000-0002-1827-0469; Cassano,
Rossella/0000-0003-4046-0637; de Gasperin,
Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660;
Intema, Huib/0000-0002-5880-2730; Swinbank, John/0000-0001-9445-1846;
Brunetti, Gianfranco/0000-0003-4195-8613
FU Royal Netherlands Academy of Arts and Sciences; Deutsche
Forschungsgemeinschaft [FOR1254, WU 588/1-1]; PRIN-INAF; ASI-INAF
[I/009/10/0]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01];
6.1 Base funding; European Commission [PERG02-GA-2007-224897]
FX We thank the anonymous referee for useful comments. LOFAR, the Low
Frequency Array designed and constructed by ASTRON, has facilities in
several countries, that are owned by various parties (each with their
own funding sources), and that are collectively operated by the
International LOFAR Telescope (ILT) foundation under a joint scientific
policy. We thank Ming Sun for providing Chandra X-ray image. We have
used the "cubehelix" color scheme from Green (2011). R.J.v.W.
acknowledges funding from the Royal Netherlands Academy of Arts and
Sciences. M. B., A. B. and M. H. acknowledge support by the Deutsche
Forschungsgemeinschaft under grant FOR1254. G. B. and R. C. acknowledge
partial support through PRIN-INAF 2009 and ASI-INAF I/009/10/0. C. F.
and G. M. acknowledge financial support by the "Agence Nationale de la
Recherche" through grant ANR-09-JCJC-0001-01. Basic research in radio
astronomy at the Naval Research Laboratory is supported by 6.1 Base
funding. The Open University is incorporated by Royal Charter (RC
000391), an exempt charity in England & Wales and a charity registered
in Scotland (SC 038302). HTI is Jansky Fellow of the National Radio
Astronomy Observatory. O.W. is supported by the "Deutsche
Forschungsgemeinschaft" (Emmy-Noether Grant WU 588/1-1) and by the
European Commission (European Reintegration Grant PERG02-GA-2007-224897
"WIDEMAP").
NR 92
TC 33
Z9 33
U1 1
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2012
VL 543
AR A43
DI 10.1051/0004-6361/201219154
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 976PQ
UT WOS:000306597200043
ER
PT J
AU Stevens, ML
Linker, JA
Riley, P
Hughes, WJ
AF Stevens, Michael L.
Linker, Jon A.
Riley, Pete
Hughes, W. Jeffrey
TI Underestimates of magnetic flux in coupled MHD model solar wind
solutions
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Corona; Solar wind; Corotating interaction regions;
Magnetohydrodynamics; Space weather
ID CORONAL HOLES; PLASMA; SPACECRAFT; PARAMETERS; DRIVEN; STREAM
AB When validated with spacecraft observations, one enduring characteristic of global MHD solar wind models is the tendency to underestimate the interplanetary magnetic flux. This study quantifies the "missing flux" problem for models used in the coordinated Center for Integrated Space Weather Modeling study of corotating interaction regions, and identifies the model parameters most strongly related to the effect. We show that two important contributions are (1) insufficient thermal pressure in the coronal model to extract the required magnetic flux and (2) numerical diffusion in the model current sheets. Using Ulysses observations, we derive a calibration for the effective temperature in the polytropic coronal Magnetohydrodynamics Around a Sphere model that produces the expected interplanetary field at high latitudes. After recalibrating, we find that a 40% discrepancy still remains in the ecliptic plane. Moreover, the problem is 5% more severe for models of the solar cycle 23 minimum than it is for models of the cycle 22 minimum. We argue that the resolution of the heliospheric current sheet strongly affects both the general underestimate and the discrepancy between the two cycles. We also argue that improved resolution of current sheets in the low corona will further reduce the effect. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Stevens, Michael L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Linker, Jon A.; Riley, Pete] Predict Sci Inc, San Diego, CA USA.
[Hughes, W. Jeffrey] Boston Univ, Boston, MA 02215 USA.
RP Stevens, ML (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mstevens@cfa.harvard.edu
OI Riley, Pete/0000-0002-1859-456X
FU NSF; NASA-NSF-AFOSR Strategic Capabilities program; NASA/Stanford's HMI
project
FX We acknowledge use of NASA/GSFC's Space Physics Data Facility's OMNIWeb
ftp service, and OMNI data. We also acknowledge the use of Royal
Greenwich Observatory-USAF/NOAA Sunspot Database. NSO/Kitt Peak data
used here are produced cooperatively by NSF/NOAO, NASA/GSFC, and
NOAA/SEL. SOLIS data used here are produced cooperatively by NSF/NSO and
NASA/LWS. EUVI images were provided by the STEREO Science Data Center.
SOHO is a project of international cooperation between ESA and NASA.
This work was supported by the NSF supported Center for Integrated Space
Weather Modeling (CISM), the joint NASA-NSF-AFOSR Strategic Capabilities
program, and by NASA/Stanford's HMI project. Computations were performed
on the NSF supported TACC Ranger supercomputer.
NR 40
TC 10
Z9 10
U1 0
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD JUL
PY 2012
VL 83
SI SI
BP 22
EP 31
DI 10.1016/j.jastp.2012.02.005
PG 10
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 978TA
UT WOS:000306767500004
ER
PT J
AU Hawn, DR
Collette, BB
AF Hawn, Donald R.
Collette, Bruce B.
TI What are the maximum size and live body coloration of opah (Teleostei:
Lampridae: Lampris species)?
SO ICHTHYOLOGICAL RESEARCH
LA English
DT Article
DE Opah; Lampris; Maximum size; Life color
ID REGIUS BONNATERRE; GUTTATUS; MOONFISH; LUNA
AB Validity of the largest size accounts is not well documented and most published accounts of body coloration describe dead specimens lacking scales instead of the color of freshly caught opah. Maximum length is at least 163 cm fork length and maximum weight about 89 kg. The body color of fresh specimens is vermilion with white spots.
C1 [Hawn, Donald R.] Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
[Collette, Bruce B.] Smithsonian Inst, Natl Marine Fisheries Serv Systemat Lab, Washington, DC 20560 USA.
RP Hawn, DR (reprint author), Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, 1000 Pope Rd, Honolulu, HI 96822 USA.
EM Donald.Hawn@noaa.gov; collettb@si.edu
NR 40
TC 2
Z9 3
U1 3
U2 10
PU SPRINGER JAPAN KK
PI TOKYO
PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065,
JAPAN
SN 1341-8998
J9 ICHTHYOL RES
JI Ichthyol. Res.
PD JUL
PY 2012
VL 59
IS 3
BP 272
EP 275
DI 10.1007/s10228-012-0277-z
PG 4
WC Zoology
SC Zoology
GA 980ZB
UT WOS:000306931600012
ER
PT J
AU Conforti, VA
Morato, RG
Augusto, AM
Sousa, LDE
de Avila, DM
Brown, JL
Reeves, JJ
AF Conforti, Valeria A.
Morato, Ronaldo G.
Augusto, Anderson M.
de Oliveira e Sousa, Lucio
de Avila, David M.
Brown, Janine L.
Reeves, Jerry J.
TI Noninvasive monitoring of adrenocortical function in captive jaguars
(Panthera onca)
SO ZOO BIOLOGY
LA English
DT Article
DE endangered cats; ACTH challenge; fecal metabolites; corticoid
metabolites; androgen metabolites
ID ENVIRONMENTAL ENRICHMENT; STEREOTYPIC BEHAVIOR; GIANT PANDAS; CORTISOL;
STRESS; METABOLISM; RESPONSES; PITUITARY; LEOPARD; CATS
AB Jaguars are threatened with extinction throughout their range. A sustainable captive population can serve as a hedge against extinction, but only if they are healthy and reproduce. Understanding how jaguars respond to stressors may help improve the captive environment and enhance their wellbeing. Thus, our objectives were to: (1) conduct an adrenocorticotrophic hormone (ACTH) challenge to validate a cortisol radioimmunoassay (RIA) for noninvasive monitoring of adrenocortical function in jaguars; (2) investigate the relationship between fecal corticoid (FCM) and androgen metabolite (FAM) concentrations in males during the ACTH challenge; and (3) establish a range of physiological concentrations of FCMs for the proposed protocol. Seven jaguars (3 M, 4 F) received 500?IU/animal of ACTH. Pre- and post-ACTH fecal samples were assayed for corticoid (M and F) and androgen metabolites (M) by RIA. Concentrations of FCMs increased (P80.01) after ACTH injection (pre-ACTH: 0.90 +/- 0.12?mu g/g dry feces; post-ACTH: 2.55 +/- 0.25?mu g/g). Considering pre- and post-ACTH samples, FCM concentrations were higher (P80.01) in males (2.15 +/- 0.20?mu g/g) than in females (1.30 +/- 0.20?mu g/g), but the magnitude of the response to ACTH was comparable (P>0.05) between genders. After ACTH injection, FAMs increased in two (of 3) males; in one male, FCMs and FAMs were positively correlated (0.60; P80.01). Excretion of FCMs was assessed in 16 jaguars (7 M, 9 F) and found to be highly variable (range, 80.111.56?mu g/g). In conclusion, this study presents a cortisol RIA for monitoring adrenocortical function in jaguars noninvasively. Zoo Biol 31:426441, 2012. (c) 2011 Wiley Periodicals, Inc.
C1 [Conforti, Valeria A.; de Avila, David M.; Reeves, Jerry J.] Washington State Univ, Dept Anim Sci, Pullman, WA 99164 USA.
[Conforti, Valeria A.; Morato, Ronaldo G.] Inst Procarnivoros, Sao Paulo, Brazil.
[Morato, Ronaldo G.] Inst Chico Mendes Conservacao Biodiversidade, Ctr Nacl Pesquisa & Conservacao Mamiferos Carnivo, Sao Paulo, Brazil.
[Augusto, Anderson M.] Fundacao Jardim Zool Cidade Rio de Janeiro, Rio De Janeiro, Brazil.
[Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA.
RP Conforti, VA (reprint author), Rua Humaita 234-801,Bloco 2, BR-22261001 Rio De Janeiro, RJ, Brazil.
EM valeria@procarnivoros.org.br
FU Eucatex, Brazil; Doctoral Enhancement Award from Washington State
University
FX The authors thank Lea, Sergio Luis, and Mario Amorim Conforti, Sergio
Luiz Conforti, and Fabiana Pizzolato de Lucena for help with sample
collection and storage. We are especially thankful to Juliana Demori
Fernandes and Bianca Campos from Instituto Pro-Carnivoros for
coordinating sample collection, storage, processing, and shipping of
samples from Brazil to the United States as well as for obtaining the
permits necessary for the exportation of samples. We are grateful to Dr.
Rebecca Spindler (Toronto Zoo) for coordinating sample collection and
shipping from some of the North American Zoos participating in this
study. Special thanks to Nada Cummings (Animal Care Coordinator, WSU)
for help with RIAs and to Virginia Stout, Tawnya Tifft, and Lindsey
Wallace (Animal Sciences students, WSU) for sample processing. We thank
the veterinarians at Fundacao RioZoo, especially Drs. Luiz Paulo Fedullo
and Daniela Prado Rodrigues, and all veterinary technicians from RioZoo
and Ilha Solteira, in special Carlos Alberto de Oliveira (Fumaca), from
Fundacao RioZoo, for technical assistance during the ACTH challenge. We
are grateful to all curators from all the participating institutions and
to all keepers for collecting, storing, and shipping the samples,
especially to Marco Antonio Bernardino, Wagner da Silva Francisco,
Jeferson Tavares, and Gilcemar Marques de Carvalho (RioZoo), and Antonio
de Oliveira, Marco Antonio dos Santos, Marcio Antonio dos Santos, and
Ezequiel Silva de Oliveira (Ilha Solteira), for providing us with
behavioral data from the jaguars participating in the ACTH challenge. We
greatly appreciate the valuable comments and suggestions from the two
anonymous reviewers. This study was funded by Eucatex, Brazil, and by
the Doctoral Enhancement Award from Washington State University.
NR 37
TC 6
Z9 6
U1 2
U2 41
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0733-3188
J9 ZOO BIOL
JI Zoo Biol.
PD JUL-AUG
PY 2012
VL 31
IS 4
BP 426
EP 441
DI 10.1002/zoo.20409
PG 16
WC Veterinary Sciences; Zoology
SC Veterinary Sciences; Zoology
GA 981YN
UT WOS:000307008900003
PM 21953790
ER
PT J
AU Onofrio, R
AF Onofrio, Roberto
TI On the role of the uncertainty principle in superconductivity and
superfluidity
SO CHINESE PHYSICS B
LA English
DT Article
DE superconductivity; superfluidity; uncertainty principle; squeezed states
ID BOSE-EINSTEIN CONDENSATION; CRITICAL-FIELD; QUANTUM-SYSTEMS; UPPER
LIMIT; GAS; ALUMINUM; STATE; PRESSURE; THORIUM
AB We discuss the general interplay between the uncertainty principle and the onset of dissipationless transport phenomena such as superconductivity and superfluidity. We argue that these phenomena are possible because of the robustness of many-body quantum states with respect to the external environment, which is directly related to the uncertainty principle as applied to coordinates and momenta of the carriers. In the case of superconductors, this implies relationships between macroscopic quantities such as critical temperature and critical magnetic field, and microscopic quantities such as the amount of spatial squeezing of a Cooper pair and its correlation time. In the case of ultracold atomic Fermi gases, this should be paralleled by a connection between the critical temperature for the onset of superfluidity and the corresponding critical velocity. Tests of this conjecture are finally sketched with particular regard to the understanding of the behaviour of superconductors under external pressures or mesoscopic superconductors, and the possibility to mimic these effects in ultracold atomic Fermi gases using Feshbach resonances and atomic squeezed states.
C1 [Onofrio, Roberto] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy.
[Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Onofrio, R (reprint author), Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Via Marzolo 8, I-35131 Padua, Italy.
EM onofrior@gmail.com
NR 48
TC 0
Z9 0
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1674-1056
J9 CHINESE PHYS B
JI Chin. Phys. B
PD JUL
PY 2012
VL 21
IS 7
AR 070306
DI 10.1088/1674-1056/21/7/070306
PG 7
WC Physics, Multidisciplinary
SC Physics
GA 976CO
UT WOS:000306558300018
ER
PT J
AU Dimichele, WA
Lucas, SG
Krainer, K
AF Dimichele, William A.
Lucas, Spencer G.
Krainer, Karl
TI VERTEBRATE TRACKWAYS AMONG A STAND OF SUPAIA WHITE PLANTS ON AN EARLY
PERMIAN FLOODPLAIN, NEW MEXICO
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID GROWTH POSITION; RED BEDS; FORESTS; CHINA; VEGETATION; MOUNTAINS;
FLORAS; BASIN; USA
AB Little is known about the habit and spatial distribution of Early Permian tropical vegetation, a sharp contrast with the Pennsylvanian from which many in-situ "T-0" assemblages are known. Even less is known about the potential interaction of plants and vertebrates. Here we report the discovery of a small stand of 34 probable Supaia White plants from the Abo Formation of New Mexico. The plants were growing on a mudflat, subject to periodic flooding and exposure. The same mudflat hosts trackways of vertebrates that appear to have walked around or between the Supaia plants. The sterns are preserved as molds, and vary from 20 mm to 70 mm in diameter, averaging 42.4 mm, indicating heights of approximately 2.5-4 m. The plants, which may be described as small trees given their estimated height, are as close as 110 mm to their nearest neighbor and average nearly 300 mm apart. A series of lines or filled fissures, which we interpret as roots, radiates from the base of each stem. Leaves of Supaia thinfeldioides White are the only foliage found in association with these sterns, on bedding planes above and at the base of the lowest expression of the stem molds. Associated vertebrate trackways either congregate around some of the stems or wend their way between the stems and include those of a single large temnospondyl amphibian (Limnopus Marsh) and many of small predatory parareptiles (Dromopus Marsh). This study demonstrates that S. thinfeldiodes were small-statured, weedy, opportunistic plants. It also shows that contemporaneous vertebrates prowled such environments, presumably either for food, shelter, or both given detectable pace and path.
C1 [Dimichele, William A.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
[Lucas, Spencer G.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA.
[Krainer, Karl] Univ Innsbruck, Inst Geol & Palaeontol, A-6020 Innsbruck, Austria.
RP Dimichele, WA (reprint author), NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
EM dimichel@si.edu; spencer.lucas@state.nm.us; karl.krainer@uibk.ac.at
RI DiMichele, William/K-4301-2012
NR 51
TC 3
Z9 3
U1 1
U2 5
PU PALEONTOLOGICAL SOC INC
PI LAWRENCE
PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA
SN 0022-3360
J9 J PALEONTOL
JI J. Paleontol.
PD JUL
PY 2012
VL 86
IS 4
BP 584
EP 594
PG 11
WC Paleontology
SC Paleontology
GA 973WY
UT WOS:000306392200002
ER
PT J
AU Cadena, EA
Bloch, JI
Jaramillo, CA
AF Cadena, Edwin A.
Bloch, Jonathan I.
Jaramillo, Carlos A.
TI NEW BOTHREMYDID TURTLE (TESTUDINES, PLEURODIRA) FROM THE PALEOCENE OF
NORTHEASTERN COLOMBIA
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID SIDE-NECKED TURTLES; DYROSAURID CROCODYLOMORPHA; CERREJON FORMATION;
EVOLUTION; MESOEUCROCODYLIA; PHYLOGENY
AB A new turtle, Puentemys mushaisaensis, from the middle to late Paleocene Cerrejon Formation of Colombia, is described on the basis of a partial skull and many partial to nearly complete carapaces and plastrons representing multiple ontogenetic stages. Whereas P. mushaisaensis is unique in aspects of its shell morphology, it shares many diagnostic characteristics of bothremydid pleurodirans, including a long exoccipital-quadrate contact, a very low and rounded almost circular carapace, and a thinner internal bone cortex than that of the external cortex in both the carapace and plastron. With a maximum carapacial length of 151 cm, P. mushaisaensis is the largest known bothremydid turtle and represents the First occurrence of bothremydids in the Paleogene of South American tropics. Results from a cladistic analysis of bothremydids indicate that P. mushaisaensis shares a close relationship with Foxemys mechinorum from the Late Cretaceous of Europe, indicating a wide-spread geographical distribution for bothremydines during the Late Cretaceous Paleocene.
C1 [Cadena, Edwin A.; Bloch, Jonathan I.] Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Cadena, Edwin A.] N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA.
[Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa 084303092, Ancon Aa, Panama.
RP Cadena, EA (reprint author), Florida Museum Nat Hist, Dickison Hall, Gainesville, FL 32611 USA.
EM eacadena@ncsu.edu
OI Bloch, Jonathan/0000-0003-1484-6931
FU Smithsonian Paleobiology Endowment Fund; Florida Museum of Natural
History; National Science Foundation [DEB-0733725]; Florida Museum of
Natural History Miss Lucy Dickinson Fellowship; Fondo para la
Investigacion de Ciencia y Tecnologia del Banco de la Republica de
Colombia; Unrestricted Endowments Smithsonian Institution Grants;
Carbones del Cerrejon LLC
FX Funding for this project came from the Smithsonian Paleobiology
Endowment Fund, the Florida Museum of Natural History, National Science
Foundation grant DEB-0733725, Florida Museum of Natural History Miss
Lucy Dickinson Fellowship, the Fondo para la Investigacion de Ciencia y
Tecnologia del Banco de la Republica de Colombia, the Unrestricted
Endowments Smithsonian Institution Grants, and Carbones del Cerrejon
LLC. We thank L Teicher, F. Chavez, C. Montes, G. Hernandez and the
geology team at Cerrejon SA for logistical support during fieldwork.
Thanks for access to collections go to V. Schneider (North Carolina
Museum of Natural History), J. Jacobs (Smithsonian National Museum of
Natural History). Special thanks go to J. Arenas, F. Herrera, A.
Hastings, A. Rincon, S. Moron, L, Meza, I. Gutierrez, G. Bayona, S.
Wing, the Colombian Petroleum Institute-Ecopetrol SA, Smithsonian
Tropical Research Institute, and the Florida Museum of Natural History.
NR 38
TC 3
Z9 3
U1 0
U2 4
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-3360
EI 1937-2337
J9 J PALEONTOL
JI J. Paleontol.
PD JUL
PY 2012
VL 86
IS 4
BP 688
EP 698
PG 11
WC Paleontology
SC Paleontology
GA 973WY
UT WOS:000306392200012
ER
PT J
AU Marvin, U
AF Marvin, Ursula
TI Response to Presentation of the Service Award of the Meteoritical
Society
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Letter
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Marvin, U (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2012
VL 47
IS 7
BP 1241
EP 1242
DI 10.1111/j.1945-5100.2012.01388.x
PG 2
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 980MS
UT WOS:000306898000015
ER
PT J
AU Graves, GR
Newsome, SD
Willard, DE
Grosshuesch, DA
Wurzel, WW
Fogel, ML
AF Graves, Gary R.
Newsome, Seth D.
Willard, David E.
Grosshuesch, David A.
Wurzel, William W.
Fogel, Marilyn L.
TI Nutritional stress and body condition in the Great Gray Owl (Strix
nebulosa) during winter irruptive migrations
SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE
LA English
DT Article
DE body mass index; Great Gray Owl (Strix nebulosa); carbon; nitrogen; C/N;
fasting; Minnesota; reversed sexual size dimorphism; stable isotopes;
starvation
ID SEXUAL SIZE DIMORPHISM; STABLE-ISOTOPE SIGNATURES; CARBON ISOTOPES;
BARN-OWLS; ANIMAL-TISSUES; TENGMALM OWL; STARVATION; NITROGEN;
DELTA-N-15; DELTA-C-13
AB The largest irruptive migration of the Great Gray Owl (Strix nebulosa Forster, 1772) recorded since 1831 occurred in Minnesota, USA, during the winter of 2004-2005. We tested the hypothesis that morphometric indicators of nutritional stress covary with stable isotope signatures in a sample of 265 owls killed by vehicle collisions. The ratio of carbon to nitrogen in muscle (C/N-muscle) was shown to be a reliable proxy of nutritional stress. delta C-13 values for liver and muscle were significantly higher in owls in poor condition, reflecting the depletion of lipid reserves in fasting individuals. On the other hand, delta N-15 values for liver and muscle were marginally lower or unchanged in owls in poor condition. Stomachs of emaciated owls were less likely to contain prey, implying that many nutritionally stressed individuals were too weak to hunt and were near the tipping point of irreversible fasts. In a broader context, sexual differences in the correlative relationships between stable isotope signatures, C/N, and body condition suggest that the consequences of reversed sexual size dimorphism extend to physiological processes during the nonbreeding season.
C1 [Graves, Gary R.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Graves, Gary R.] Univ Copenhagen, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark.
[Newsome, Seth D.; Wurzel, William W.; Fogel, Marilyn L.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA.
[Newsome, Seth D.] Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA.
[Willard, David E.] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA.
[Grosshuesch, David A.] Super Natl Forest, Grand Marais, MN 55604 USA.
[Wurzel, William W.] SUNY ESF, SUNY Coll Environm Sci & Forestry, Syracuse, NY 13210 USA.
RP Graves, GR (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC-116,POB 37012, Washington, DC 20013 USA.
EM gravesg@si.edu
RI Fogel, Marilyn/M-2395-2015; publist, CMEC/C-3010-2012; publicationpage,
cmec/B-4405-2017
OI Fogel, Marilyn/0000-0002-1176-3818;
FU National Museum of Natural History, Smithsonian Institution; National
Science Foundation [ATM-0502491]; Carnegie Institution of Washington;
W.M. Keck Foundation [072000]
FX For salvaging speciments, we thank C. Henderson, J. Hines, M. Hamady, K.
Haws, P. Perry, K. Woizeschke, J. Welsh, M. Minchak, S. Wilson, and R.
Staffon (all from the Minnesota Department of Natural Resources), J.
Lind (from Natural Resources Research Institute), and J. Goggin (from
Raptor Research Center). T. Gnoske and M. Hennen of the Field Museum
helped with specimen preparation. E. Snyder, C. Mancuso, and B. O'Connor
provided laboratory assistance. The manuscript was significantly
improved by comments on earlier drafts by John Whiteman and two
anonymous reviewers. G.R.G was supported by the Wetmore Fund (National
Museum of Natural History, Smithsonian Institution) and G.R.G. and S.D.N
were supported by the Walcott Fund (National Museum of Natural History,
Smithsonian Institution). S.D.N was also supported by the National
Science Foundation (ATM-0502491), Carnegie Institution of Washington,
and the W.M. Keck Foundation (072000).
NR 78
TC 5
Z9 6
U1 1
U2 36
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA
SN 0008-4301
J9 CAN J ZOOL
JI Can. J. Zool.-Rev. Can. Zool.
PD JUL
PY 2012
VL 90
IS 7
BP 787
EP 797
DI 10.1139/Z2012-047
PG 11
WC Zoology
SC Zoology
GA 977CM
UT WOS:000306634000001
ER
PT J
AU Lidgard, DC
Bowen, WD
Boness, DJ
AF Lidgard, D. C.
Bowen, W. D.
Boness, D. J.
TI Longitudinal changes and consistency in male physical and behavioural
traits have implications for mating success in the grey seal
(Halichoerus grypus)
SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE
LA English
DT Article
DE grey seal; Halichoerus grypus; breeding behaviour; behavioural
consistency; intraindividual
ID NORTHERN ELEPHANT SEALS; RED DEER; REPRODUCTIVE SUCCESS; SEXUAL
SELECTION; SABLE ISLAND; MESOCRICETUS-AURATUS; NATURAL-POPULATIONS;
ANIMAL PERSONALITY; BREEDING-SEASON; DIVING BEHAVIOR
AB We examined age-related changes and consistency in physical and behavioural traits of 20 male grey seals (Halichoerus grypus (Fabricius, 1791)) and implications for a proxy of mating success (number of oestrous females attended) over four successive breeding seasons on Sable Island, Canada. Across the study, young males (10-15 years) gained body mass, while old males (23-31 years) lost body mass. Body length was an important determinant of tenure (time spent at a site among females) and males of all ages exhibited a high level of consistency in duration of tenure (r = 0.40-0.50). In young males, our proxy of success showed a strong relationship with arrival body mass and also exhibited a high level of consistency (r = 0.50). None of the physical traits measured explained variation in success by exhibiting mating tactics that did not involve tenure, which is likely due to the opportunistic nature of those tactics. Whereas young male grey seals exhibited age-dependent improvements in success owing to changes in their physical state, later in life physical traits were less influential and suggest that nonphysical traits may compensate for a deteriorating physical state and its impact on male success.
C1 [Lidgard, D. C.] Dalhousie Univ, Dept Biol, Halifax, NS B3H 4R2, Canada.
[Bowen, W. D.] Fisheries & Oceans Canada, Bedford Inst Oceanog, Populat Ecol Div, Dartmouth, NS B2Y 4A2, Canada.
[Boness, D. J.] Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA.
RP Lidgard, DC (reprint author), Dalhousie Univ, Dept Biol, Halifax, NS B3H 4R2, Canada.
EM damian.lidgard@dal.ca
RI Bowen, William/D-2758-2012
FU Smithsonian Institution; Friends of the National Zoo; Christensen Fund;
Fisheries and Oceans Canada; Natural Sciences and Engineering Research
Council of Canada
FX We are very grateful to S. Ambs, D. Austin, C. Beck, G. Breed, S. Budge,
D. Coltman, M. Cooper, T. Hubbard, S. Insley, S. Iverson, S. Lang, J.
McMillan, T. Schulz, S. Tucker, and J. van Dommelen for assistance in
the field. We are also grateful for infrastructure support provided on
Sable Island by G. Forbes. The study was supported by a Smithsonian
Institution Graduate and Pre-doctorate Fellowship awarded to D.C.L., and
funds from the Friends of the National Zoo, the Smithsonian Institution,
the Christensen Fund, the Fisheries and Oceans Canada, and the Natural
Sciences and Engineering Research Council of Canada. This manuscript was
improved through comments from two anonymous reviewers and we are
grateful to them.
NR 86
TC 3
Z9 3
U1 2
U2 30
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA
SN 0008-4301
J9 CAN J ZOOL
JI Can. J. Zool.-Rev. Can. Zool.
PD JUL
PY 2012
VL 90
IS 7
BP 849
EP 860
DI 10.1139/Z2012-053
PG 12
WC Zoology
SC Zoology
GA 977CM
UT WOS:000306634000007
ER
PT J
AU Tojeiro, R
Percival, WJ
Wake, DA
Maraston, C
Skibba, RA
Zehavi, I
Ross, AJ
Brinkmann, J
Conroy, C
Guo, H
Manera, M
Masters, KL
Pforr, J
Samushia, L
Schneider, DP
Thomas, D
Weaver, BA
Bizyaev, D
Brewington, H
Malanushenko, E
Malanushenko, V
Oravetz, D
Pan, K
Shelden, A
Simmons, A
Snedden, S
AF Tojeiro, Rita
Percival, Will J.
Wake, David A.
Maraston, Claudia
Skibba, Ramin A.
Zehavi, Idit
Ross, Ashley J.
Brinkmann, Jon
Conroy, Charlie
Guo, Hong
Manera, Marc
Masters, Karen L.
Pforr, Janine
Samushia, Lado
Schneider, Donald P.
Thomas, Daniel
Weaver, Benjamin A.
Bizyaev, Dmitry
Brewington, Howard
Malanushenko, Elena
Malanushenko, Viktor
Oravetz, Daniel
Pan, Kaike
Shelden, Alaina
Simmons, Audrey
Snedden, Stephanie
TI The progenitors of present-day massive red galaxies up to z similar to
0.7-finding passive galaxies using SDSS-I/II and SDSS-III
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; galaxies: evolution; cosmology: observations
ID DIGITAL SKY SURVEY; HALO OCCUPATION DISTRIBUTION; SPECTROSCOPIC TARGET
SELECTION; COLOR-MAGNITUDE RELATION; STAR-FORMATION HISTORIES; GIANT
BRANCH STARS; 7TH DATA RELEASE; TP-AGB MODELS; LUMINOSITY FUNCTION;
STELLAR POPULATIONS
AB We present a comprehensive study of 250 000 galaxies targeted by the Baryon Oscillation Spectroscopic Survey (BOSS) up to z approximate to 0.7 with the specific goal of identifying and characterizing a population of galaxies that has evolved without significant merging. We compute a likelihood that each BOSS galaxy is a progenitor of the luminous red galaxies (LRGs) sample, targeted by SDSS-I/II up z approximate to 0.5, by using the fossil record of LRGs and their inferred star formation histories, metallicity histories and dust content. We determine merger rates, luminosity growth rates and the evolution of the large-scale clustering between the two surveys, and we investigate the effect of using different stellar population synthesis models in our conclusions. We demonstrate that our sample is slowly evolving (of the order of 2 +/- 1.5 per cent Gyr-1 by merging) by computing the change in weighted luminosity-per-galaxy between the two samples, and that this result is robust to our choice of stellar population models. Our conclusions refer to the bright and massive end of the galaxy population, with Mi0.55?-22 and M*? 1011.2 M?, corresponding roughly to 95 and 40 per cent of the LRGs and BOSS galaxy populations, respectively. Our analysis further shows that any possible excess of flux in BOSS galaxies, when compared to LRGs, from potentially unresolved targets at z approximate to 0.55 must be less than 1 per cent in the r0.55 band (approximately equivalent to the g band in the rest frame of galaxies at z= 0.55). When weighting the BOSS galaxies based on the predicted properties of the LRGs, and restricting the analysis to the reddest BOSS galaxies, we find an evolution of the large-scale clustering that is consistent with dynamical passive evolution, assuming a standard cosmology. We conclude that our likelihoods give a weighted sample that is as clean and as close to passive evolution (in dynamical terms, i.e. no or negligible merging) as possible, and that is optimal for cosmological studies.
C1 [Tojeiro, Rita; Percival, Will J.; Maraston, Claudia; Ross, Ashley J.; Manera, Marc; Masters, Karen L.; Samushia, Lado; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Wake, David A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Skibba, Ramin A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Zehavi, Idit; Guo, Hong] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA.
[Zehavi, Idit; Guo, Hong] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA.
[Brinkmann, Jon; Brewington, Howard; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Shelden, Alaina; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA.
[Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pforr, Janine] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Schneider, Donald P.; Bizyaev, Dmitry] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
RP Tojeiro, R (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England.
EM rita.tojeiro@port.ac.uk
RI Pforr, Janine/J-3967-2015; Guo, Hong/J-5797-2015
OI Pforr, Janine/0000-0002-3414-8391; Guo, Hong/0000-0003-4936-8247
FU European Research Council; Alfred P. Sloan Foundation; National Science
Foundation; U.S. Department of Energy; SDSS-III Collaboration;
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
FX RT and WJP thank the European Research Council for support. WJP also
thanks the Science and Technology Facilities Council.; 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. 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 99
TC 23
Z9 23
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 424
IS 1
BP 136
EP 156
DI 10.1111/j.1365-2966.2012.21177.x
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 970OE
UT WOS:000306140600013
ER
PT J
AU Wetzel, AR
Tinker, JL
Conroy, C
AF Wetzel, Andrew R.
Tinker, Jeremy L.
Conroy, Charlie
TI Galaxy evolution in groups and clusters: star formation rates, red
sequence fractions and the persistent bimodality
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: statistical; galaxies: clusters: general; galaxies: evolution;
galaxies: groups: general; galaxies: haloes; galaxies: star formation
ID DIGITAL SKY SURVEY; COLOR-DENSITY RELATION; REDSHIFT SURVEY; STELLAR
MASS; SATELLITE GALAXIES; ORBITAL PARAMETERS; DISTANT CLUSTERS; SPIRAL
GALAXIES; DISK GALAXIES; DATA RELEASE
AB Using galaxy group/cluster catalogues created from the Sloan Digital Sky Survey Data Release 7, we examine in detail the specific star formation rate (SSFR) distribution of satellite galaxies and its dependence on stellar mass, host halo mass and halo-centric radius. All galaxies, regardless of central satellite designation, exhibit a similar bimodal SSFR distribution, with a strong break at SSFR approximate to 10-11 yr-1 and the same high SSFR peak; in no regime is there ever an excess of galaxies in the green valley. Satellite galaxies are simply more likely to lie on the quenched (red sequence) side of the SSFR distribution. Furthermore, the satellite quenched fraction excess above the field galaxy value is nearly independent of galaxy stellar mass. An enhanced quenched fraction for satellites persists in groups with halo masses down to 3 x 1011 M? and increases strongly with halo mass and towards halo centre. We find no detectable quenching enhancement for galaxies beyond similar to 2 Rvir around massive clusters once these galaxies have been decomposed into centrals and satellites. These trends imply that (1) galaxies experience no significant environmental effects until they cross within similar to Rvir of a more massive host halo; (2) after this, star formation in active satellites continues to evolve in the same manner as active central galaxies for several Gyr; and (3) once begun, satellite star formation quenching occurs rapidly. These results place strong constraints on satellite-specific quenching mechanisms, as we will discuss further in companion papers.
C1 [Wetzel, Andrew R.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Tinker, Jeremy L.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10013 USA.
[Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Wetzel, AR (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA.
EM andrew.wetzel@yale.edu
OI Wetzel, Andrew/0000-0003-0603-8942
FU NSF; 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 ARW acknowledges partial support through an NSF Graduate Research
Fellowship and thanks the organizers, participants and staff of the
Monsters Inc. workshop at the Kavli Institute for Theoretical Physics,
supported in part by the NSF, where some of this work was completed. We
thank Michael Blanton, David Hogg and collaborators for publicly
releasing the NYU VAGC, as well as Jarle Brinchmann and the MPA-JHU
collaboration for publicly releasing their spectral reductions. We thank
Frank van den Bosch and Jarle Brinchmann for insightful conversations,
as well as Frank van den Bosch and Martin White for comments on an early
draft.; Funding for the SDSS and SDSS-II has been provided by the Alfred
P. Sloan Foundation, the Participating Institutions, the National
Science Foundation, the U.S. Department of Energy, the National
Aeronautics and Space Administration, the Japanese Monbukagakusho, the
Max Planck Society and the Higher Education Funding Council for England.
The SDSS website is http://www.sdss.org/. The SDSS is managed by the
Astrophysical Research Consortium for the Participating Institutions.
The Participating Institutions are the American Museum of Natural
History, Astrophysical Institute Potsdam, University of Basel,
University of Cambridge, Case Western Reserve University, University of
Chicago, Drexel University, Fermilab, the Institute for Advanced Study,
the Japan Participation Group, Johns Hopkins University, the Joint
Institute for Nuclear Astrophysics, the Kavli Institute for Particle
Astrophysics and Cosmology, the Korean Scientist Group, the Chinese
Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max
Planck Institute for Astronomy (MPIA), the Max Planck Institute for
Astrophysics (MPA), New Mexico State University, Ohio State University,
University of Pittsburgh, University of Portsmouth, Princeton
University, the United States Naval Observatory and the University of
Washington.
NR 97
TC 128
Z9 128
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 424
IS 1
BP 232
EP 243
DI 10.1111/j.1365-2966.2012.21188.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 970OE
UT WOS:000306140600020
ER
PT J
AU Ross, AJ
Percival, WJ
Sanchez, AG
Samushia, L
Ho, S
Kazin, E
Manera, M
Reid, B
White, M
Tojeiro, R
McBride, CK
Xu, XY
Wake, DA
Strauss, MA
Montesano, F
Swanson, MEC
Bailey, S
Bolton, AS
Dorta, AM
Eisenstein, DJ
Guo, H
Hamilton, JC
Nichol, RC
Padmanabhan, N
Prada, F
Schlegel, DJ
Magana, MV
Zehavi, I
Blanton, M
Bizyaev, D
Brewington, H
Cuesta, AJ
Malanushenko, E
Malanushenko, V
Oravetz, D
Parejko, J
Pan, KK
Schneider, DP
Shelden, A
Simmons, A
Snedden, S
Zhao, GB
AF Ross, Ashley J.
Percival, Will J.
Sanchez, Ariel G.
Samushia, Lado
Ho, Shirley
Kazin, Eyal
Manera, Marc
Reid, Beth
White, Martin
Tojeiro, Rita
McBride, Cameron K.
Xu, Xiaoying
Wake, David A.
Strauss, Michael A.
Montesano, Francesco
Swanson, Molly E. C.
Bailey, Stephen
Bolton, Adam S.
Montero Dorta, Antonio
Eisenstein, Daniel J.
Guo, Hong
Hamilton, Jean-Christophe
Nichol, Robert C.
Padmanabhan, Nikhil
Prada, Francisco
Schlegel, David J.
Magana, Mariana Vargas
Zehavi, Idit
Blanton, Michael
Bizyaev, Dmitry
Brewington, Howard
Cuesta, Antonio J.
Malanushenko, Elena
Malanushenko, Viktor
Oravetz, Daniel
Parejko, John
Pan, Kaike
Schneider, Donald P.
Shelden, Alaina
Simmons, Audrey
Snedden, Stephanie
Zhao, Gong-bo
TI The clustering of galaxies in the SDSS-III Baryon Oscillation
Spectroscopic Survey: analysis of potential systematics
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE cosmology: observations; distance scale; large-scale structure of
Universe
ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; POWER-SPECTRUM ANALYSIS;
SURVEY IMAGING DATA; EARLY DATA RELEASE; LARGE-SCALE BIAS; REDSHIFT
SURVEY; COSMOLOGICAL IMPLICATIONS; ACOUSTIC-OSCILLATIONS; ANGULAR MASKS
AB We analyse the density field of galaxies observed by the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS) included in the SDSS Data Release Nine (DR9). DR9 includes spectroscopic redshifts for over 400 000 galaxies spread over a footprint of 3275 deg2. We identify, characterize and mitigate the impact of sources of systematic uncertainty on large-scale clustering measurements, both for angular moments of the redshift-space correlation function, ?l(s), and the spherically averaged power spectrum, P(k), in order to ensure that robust cosmological constraints will be obtained from these data. A correlation between the projected density of stars and the higher redshift (0.43 < z < 0.7) galaxy sample (the approximately constant stellar mass threshold CMASS sample) due to imaging systematics imparts a systematic error that is larger than the statistical error of the clustering measurements at scales s > 120 h-1 Mpc or k < 0.01 h Mpc-1. We find that these errors can be ameliorated by weighting galaxies based on their surface brightness and the local stellar density. The clustering of CMASS galaxies found in the Northern and Southern Galactic footprints of the survey generally agrees to within 2s. We use mock galaxy catalogues that simulate the CMASS selection function to determine that randomly selecting galaxy redshifts in order to simulate the radial selection function of a random sample imparts the least systematic error on ?l(s) measurements and that this systematic error is negligible for the spherically averaged correlation function, ?0. We find a peak in ?0 at s similar to 200 h-1 Mpc, with a corresponding feature with period similar to 0.03 h Mpc-1 in P(k), and find features at least as strong in 4.8 per cent of the mock galaxy catalogues, concluding this feature is likely to be a consequence of cosmic variance. The methods we recommend for the calculation of clustering measurements using the CMASS sample are adopted in companion papers that locate the position of the baryon acoustic oscillation feature, constrain cosmological models using the full shape of ?0 and measure the rate of structure growth.
C1 [Ross, Ashley J.; Percival, Will J.; Samushia, Lado; Manera, Marc; Tojeiro, Rita; Nichol, Robert C.; Zhao, Gong-bo] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Sanchez, Ariel G.; Montesano, Francesco] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia.
[Ho, Shirley; Reid, Beth; White, Martin; Bailey, Stephen; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Ho, Shirley] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Kazin, Eyal] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[McBride, Cameron K.; Swanson, Molly E. C.; Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Xu, Xiaoying] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Wake, David A.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA.
[Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Bolton, Adam S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Montero Dorta, Antonio; Prada, Francisco] Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain.
[Guo, Hong; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA.
[Hamilton, Jean-Christophe; Magana, Mariana Vargas] Univ Paris 07, APC, CEA,Observ Paris, CNRS,IN2P3, Paris, France.
[Padmanabhan, Nikhil; Cuesta, Antonio J.; Parejko, John] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain.
[Prada, Francisco; Malanushenko, Viktor] Univ Autonoma Madrid, Inst Fis Teor, CSIC, E-28049 Madrid, Spain.
[Blanton, Michael] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Bizyaev, Dmitry; Brewington, Howard; Malanushenko, Elena; Oravetz, Daniel; Pan, Kaike; Shelden, Alaina; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
RP Ross, AJ (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England.
EM Ashley.Ross@port.ac.uk
RI Ho, Shirley/P-3682-2014; Guo, Hong/J-5797-2015; White,
Martin/I-3880-2015;
OI Ho, Shirley/0000-0002-1068-160X; Guo, Hong/0000-0003-4936-8247; White,
Martin/0000-0001-9912-5070; Cuesta Vazquez, Antonio
Jose/0000-0002-4153-9470
FU UK Science and Technology Facilities Council [ST/I001204/1]; Leverhulme
Trust; European Research Council; NSF [AST-0707266, AST-0901965]; Alfred
P. Sloan Foundation
FX AJR is grateful to the UK Science and Technology Facilities Council for
financial support through the grant ST/I001204/1. WJP is grateful for
support from the UK Science and Technology Facilities Research Council,
the Leverhulme Trust and the European Research Council. MAS acknowledges
the support of NSF grant AST-0707266. MECS was supported by the NSF
under Award No. AST-0901965.; Funding for SDSS-III has been provided by
the Alfred P. Sloan Foundation, the Participating Institutions, the
National Science Foundation and the U.S. Department of Energy Office of
Science. The SDSS-III website is http://www.sdss3.org/.
NR 63
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 424
IS 1
BP 564
EP 590
DI 10.1111/j.1365-2966.2012.21235.x
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 970OE
UT WOS:000306140600048
ER
PT J
AU Novak, GS
Jonsson, P
Primack, JR
Cox, TJ
Dekel, A
AF Novak, Gregory S.
Jonsson, Patrik
Primack, Joel R.
Cox, Thomas J.
Dekel, Avishai
TI On galaxies and homology
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; galaxies: fundamental parameters; galaxies:
kinematics and dynamics; galaxies: structure
ID INITIAL MASS FUNCTION; LENS ACS SURVEY; DIGITAL SKY SURVEY; ELLIPTIC
GALAXIES; FUNDAMENTAL PLANE; DARK-MATTER; SCALING RELATIONS;
2-DIMENSIONAL KINEMATICS; DENSITY PROFILE; SPIRAL GALAXIES
AB The definition of homology for single-component galaxies is clear, but for multicomponent (luminous and dark matter) galaxies there is some ambiguity. We attempt to clarify the situation by carefully separating the different concepts of homology that have been used to date. We argue that the most useful definition is that a set of galaxies is homologous if they are the same in all respects up to a set of three dimensional scaling constants which may differ from one galaxy to the next. Noting that we are free to choose the dimensional constants, we find that a set of hydrodynamic simulated galaxy merger remnants is significantly closer to homologous when the dimensional length constant is taken to be the radius containing equal amounts of dark and baryonic matter rather than the usual observationally motivated choice of the baryonic half-mass radius. Once the correct dimensional scaling constants are used, the stellar velocity dispersion anisotropy is essentially the sole source of the variation in the kinematic structure of these simulated merger remnants. In order to facilitate the use of these scaling constants to analyse observed galaxies, we calculated the relationship between our preferred dimensional scaling constants and the typical observationally accessible quantities.
C1 [Novak, Gregory S.] CNRS, Observ Paris, LERMA, F-75014 Paris, France.
[Novak, Gregory S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Novak, Gregory S.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Jonsson, Patrik] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jonsson, Patrik; Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Cox, Thomas J.] Carnegie Observ, Pasadena, CA 91101 USA.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
RP Novak, GS (reprint author), CNRS, Observ Paris, LERMA, 61 Av Observ, F-75014 Paris, France.
EM greg.novak@obspm.fr; pjonsson@cfa.harvard.edu; joel@scipp.ucsc.edu;
tcox@obs.carnegiescience.edu; dekel@phys.huji.ac.il
FU Princeton University Council on Science and Technology; W.M. Keck
Foundation; NASA through Space Telescopes Research Institute
[HST-AR-11758, NAS5-26555]
FX We thank Michele Cappellari for useful discussions. GSN acknowledges the
support of the Princeton University Council on Science and Technology.
PJ acknowledges support by a grant from the W.M. Keck Foundation and by
programme HST-AR-11758, provided by NASA through a grant from the Space
Telescopes Research Institute, which is operated by the Association of
Universities for Research in Astronomy, Incorporated, under NASA
contract NAS5-26555.
NR 57
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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 JUL
PY 2012
VL 424
IS 1
BP 635
EP 648
DI 10.1111/j.1365-2966.2012.21242.x
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 970OE
UT WOS:000306140600053
ER
PT J
AU Guggenberger, E
Kolenberg, K
Nemec, JM
Smolec, R
Benko, JM
Ngeow, CC
Cohen, JG
Sesar, B
Szabo, R
Catelan, M
Moskalik, P
Kinemuchi, K
Seader, SE
Smith, JC
Tenenbaum, P
Kjeldsen, H
AF Guggenberger, E.
Kolenberg, K.
Nemec, J. M.
Smolec, R.
Benko, J. M.
Ngeow, C. -C.
Cohen, J. G.
Sesar, B.
Szabo, R.
Catelan, M.
Moskalik, P.
Kinemuchi, K.
Seader, S. E.
Smith, J. C.
Tenenbaum, P.
Kjeldsen, H.
TI The complex case of V445 Lyr observed with Kepler: two Blazhko
modulations, a non-radial mode, possible triple mode RR Lyrae pulsation,
and more
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE asteroseismology; methods: data analysis; techniques: photometric;
stars: individual: KIC 6186029 (V445 Lyr); stars: individual: CoRoT
105288363; stars: variables: RR Lyrae
ID GRAVITATIONAL LENSING EXPERIMENT.; LARGE-MAGELLANIC-CLOUD; OGLE-III
CATALOG; LIGHT CURVES; STARS; SCIENCE; SPACE
AB Rapid and strong changes in the Blazhko modulation of RR Lyrae stars, as have recently been detected in high-precision satellite data, have become a crucial topic in finding an explanation of the long-standing mystery of the Blazhko effect. We present here an analysis of the most extreme case detected so far, the RRab star V445 Lyr (KIC 6186029) which was observed with the Kepler space mission. V445 Lyr shows very strong cycle-to-cycle changes in its Blazhko modulation, which are caused by both a secondary long-term modulation period and irregular variations. In addition to the complex Blazhko modulation, V445 Lyr also shows a rich spectrum of additional peaks in the frequency range between the fundamental pulsation and the first harmonic. Among those peaks, the second radial overtone could be identified, which, combined with a metallicity estimate of [Fe/H] =-2.0 dex from spectroscopy, allowed us to constrain the mass (0.550.65 M?) and luminosity (4050 L?) of V445 Lyr through theoretical Petersen diagrams. A non-radial mode and possibly the first overtone are also excited. Furthermore, V445 Lyr shows signs of the period-doubling phenomenon and a long-term period change. A detailed Fourier analysis along with a study of the O - C variation of V445 Lyr is presented, and the origin of the additional peaks and possible causes of the changes in the Blazhko modulation are discussed. The results are then put into context with those of the only other star with a variable Blazhko effect for which a long enough set of high-precision continuous satellite data has been published so far, the CoRoT star 105288363.
C1 [Guggenberger, E.; Smolec, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kolenberg, K.] Inst Sterrenkunde, B-3001 Heverlee, Belgium.
[Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada.
[Smolec, R.; Moskalik, P.] Polish Acad Sci, Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Benko, J. M.; Szabo, R.] Konkoly Observ Budapest, Res Ctr Astron & Earth Sci, H-1525 Budapest, Hungary.
[Ngeow, C. -C.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taoyuan County, Taiwan.
[Cohen, J. G.; Sesar, B.] CALTECH, Pasadena, CA 91125 USA.
[Catelan, M.] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrophys, Santiago 7820436, Chile.
[Seader, S. E.; Smith, J. C.; Tenenbaum, P.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Kinemuchi, K.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Guggenberger, E (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM elisabeth.guggenberger@univie.ac.at
RI Smolec, Radoslaw/F-1435-2013;
OI Smolec, Radoslaw/0000-0001-7217-4884; Benko, Jozsef/0000-0003-3851-6603;
Szabo, Robert/0000-0002-3258-1909
FU NASA's Science Mission Directorate; Austrian Science Fund (FWF)
[P19962-N16]; European Commission [269194]; Lendulet programme of the
Hungarian Academy of Sciences; Hungarian OTKA [K83790, MB08C 81013];
Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences;
National Science Council (of Taiwan) [NSC 98-2112-M-008-013-MY3]; NSF
[AST-0908139]; Ministry for the Economy, Development, and Tourism's
Programa Inicativa Cientifica Milenio [P07-021-F]; Proyecto Basal
[PFB-06/2007]; FONDAP Centro de Astrofisica [15010003]; Proyecto
FONDECYT Regular [1110326]; Proyecto Anillo [ACT-86]
FX Funding for this discovery mission is provided by NASA's Science Mission
Directorate. EG acknowledges support from the Austrian Science Fund
(FWF), project number P19962-N16. KK is presently a Marie Curie Fellow
(IOF-255267). The research leading to these results has received funding
from the European Commission's Seventh Framework Programme
(FP7/2007-2013) under grant agreement no. 269194 (IRSES/ASK). RSz and
JMB are supported by the Lendulet programme of the Hungarian Academy of
Sciences and the Hungarian OTKA grants K83790 and MB08C 81013. RSz was
supported by the Janos Bolyai Research Scholarship of the Hungarian
Academy of Sciences. C-CN thanks the funding from the National Science
Council (of Taiwan) under the contract NSC 98-2112-M-008-013-MY3. We
acknowledge the assistance of the queue observers, Chi-Sheng Lin and
Hsiang-Yao Hsiao from the Lulin Observatory, and we thank Jhen-kuei Guo
and Neelam Panwar for coordinating observations at the Tenagra II
Observatory. JGC and BS are grateful to NSF grant AST-0908139 for
partial support. Support for MC is provided by the Ministry for the
Economy, Development, and Tourism's Programa Inicativa Cientifica
Milenio through grant P07-021-F, awarded to The Milky Way Millennium
Nucleus; by Proyecto Basal PFB-06/2007; by FONDAP Centro de Astrofisica
15010003; by Proyecto FONDECYT Regular #1110326; and by Proyecto Anillo
ACT-86. The authors gratefully acknowledge the entire Kepler team, whose
outstanding efforts have made these results possible.
NR 51
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PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 424
IS 1
BP 649
EP 665
DI 10.1111/j.1365-2966.2012.21244.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 970OE
UT WOS:000306140600054
ER
PT J
AU Wilcock, LA
Ward-Thompson, D
Kirk, JM
Stamatellos, D
Whitworth, A
Battersby, C
Elia, D
Fuller, GA
DiGiorgio, A
Griffin, MJ
Molinari, S
Martin, P
Mottram, JC
Peretto, N
Pestalozzi, M
Schisano, E
Smith, HA
Thompson, MA
AF Wilcock, L. A.
Ward-Thompson, D.
Kirk, J. M.
Stamatellos, D.
Whitworth, A.
Battersby, C.
Elia, D.
Fuller, G. A.
DiGiorgio, A.
Griffin, M. J.
Molinari, S.
Martin, P.
Mottram, J. C.
Peretto, N.
Pestalozzi, M.
Schisano, E.
Smith, H. A.
Thompson, M. A.
TI Isolated starless cores in infrared dark clouds in the Hi-GAL survey
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation
ID RADIATIVE-TRANSFER; PROTOSTELLAR CORES; PRESTELLAR CORES; GALACTIC
PLANE; MILKY-WAY; HERSCHEL; PROTOSTARS; INSTRUMENT; CLUSTERS; DENSITY
AB In a previous paper, we identified cores within infrared dark clouds. We regarded those without embedded sources as the least evolved and labelled them starless. Here we identify the most isolated starless cores and model them using a three-dimensional multiwavelength Monte Carlo radiative transfer code. We derive the cores physical parameters and discuss the relation between the mass, temperature, density, size and the surrounding interstellar radiation field (ISRF) for the cores. The masses of the cores were found not to correlate with their radial size or central density. The temperature at the surface of a core was seen to depend almost entirely on the level of the ISRF surrounding the core. No correlation was found between the temperature at the centre of a core and its local ISRF. This was seen to depend, instead, on the density and mass of the core.
C1 [Wilcock, L. A.; Ward-Thompson, D.; Kirk, J. M.; Stamatellos, D.; Whitworth, A.; Griffin, M. J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Battersby, C.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Elia, D.; DiGiorgio, A.; Molinari, S.; Pestalozzi, M.; Schisano, E.] CNR, Inst Fis Spazio Interplanetario, I-00133 Rome, Italy.
[Fuller, G. A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Martin, P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Mottram, J. C.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Mottram, J. C.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Peretto, N.] Univ Paris Diderot, Lab AIM, CEA DSM, CNRS,IFRU Serv Astrophys,CE Saclay, F-91191 Gif Sur Yvette, France.
[Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Thompson, M. A.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
RP Wilcock, LA (reprint author), Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales.
EM lucy.wilcock@astro.cf.ac.uk
RI Molinari, Sergio/O-4095-2016;
OI Molinari, Sergio/0000-0002-9826-7525; Elia, Davide/0000-0002-9120-5890;
Stamatellos, Dimitris/0000-0002-4502-8344
FU STFC; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA
(USA); BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR
(Germany); ASI/INAF (Italy); CICYT/MCYT (Spain)
FX LAW gratefully acknowledges STFC studentship funding. SPIRE was
developed by a consortium of institutes led by Cardiff University (UK)
and including University Lethbridge (Canada); NAOC (China); CEA, LAM
(France); IFSI, University Padua (Italy); IAC (Spain); Stockholm
Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,
University Sussex (UK) and Caltech, JPL, NHSC, University Colorado
(USA). This development has been supported by national funding agencies:
CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN
(Spain); SNSB (Sweden); STFC (UK) and NASA (USA). PACS was developed by
a consortium of institutes led by MPE (Germany) and including UVIE
(Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA
(Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy) and IAC (Spain).
This development has been supported by the funding agencies BMVIT
(Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany),
ASI/INAF (Italy) and CICYT/MCYT (Spain). HIPE is a joint development by
the Herschel Science Ground Segment Consortium, consisting of ESA, the
NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia.
NR 45
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PU WILEY-BLACKWELL
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PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 424
IS 1
BP 716
EP 727
DI 10.1111/j.1365-2966.2012.21264.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 970OE
UT WOS:000306140600058
ER
PT J
AU Beckman, NG
Neuhauser, C
Muller-Landau, HC
AF Beckman, Noelle G.
Neuhauser, Claudia
Muller-Landau, Helene C.
TI The interacting effects of clumped seed dispersal and distance- and
density-dependent mortality on seedling recruitment patterns
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE aggregated distributions; Bruchidae; dispersal; diversity maintenance;
early plant recruitment; Janzen-Connell; oomycetes; plant-herbivore
interactions; spatial patterns; vertebrate-dispersed seeds
ID PROCESSES MAINTAIN DIVERSITY; TROPICAL FORESTS; SPECIES-DIVERSITY;
CALLOSOBRUCHUS-CHINENSIS; SPATIAL-PATTERNS; PLANT-DISEASE; TREE; MODELS;
PHYTOPHTHORA; PREDATION
AB 1. Seed dispersal and natural enemies both influence spatial patterns of seedlings, which in turn influence future abiotic and biotic interactions, with consequences for plant populations, distributions and diversity. Clumped seed deposition is common, especially for vertebrate-dispersed seeds, and has the potential to significantly affect interactions with density-responsive enemies, yet has received relatively little attention. 2. We used spatially explicit simulation models to examine how different patterns of seed dispersal and natural enemy attack structure seedling spatial patterns. We simulated clumped seed dispersal by combining a two-dimensional Students T dispersal kernel for expected seed rain with a negative binomial distribution for seed deposition. We based our models for seed mortality on published data reflecting differing life histories of insect seed predators and soil-borne pathogens. We varied dispersal distance, degree of clumping, type of enemy, enemy dispersal distance and fecundity among simulations. 3. Under insect seed predation, seeds escaped predation by dispersing longer distances than insects, resulting in JanzenConnell patterns in which seedling recruitment peaks at intermediate distances. When insects dispersed longer distances than seeds, higher seed densities near the tree satiated insects, resulting in McCanny patterns in which seed deposition, survivorship and seedling establishment all decrease with distance from the parent tree. Total seedling establishment was lowest when insects and seeds dispersed similar distances. 4. Under pathogen attack, JanzenConnell patterns predominated except when seedling survival was virtually zero or one everywhere, or in the case where pathogen dispersal distances exceeded seed dispersal distances, producing Hubbell patterns in which seed deposition and seedling establishment decrease with distance, though survivorship increases. 5. Clumped seed deposition increased the probability of seedling establishment under both insect seed predation and pathogen attack as it led to local satiation of insect seed predators and made it harder for pathogen distributions to track seeds. 6. Synthesis. Our modelling study suggests that the relative dispersal distances of seeds and natural enemies are crucial to determining establishment rates and spatial patterns of seedlings. Better characterization of the movement and natural histories of natural enemies is critical to improving our understanding of seedling distributions and plantenemy interactions.
C1 [Beckman, Noelle G.; Muller-Landau, Helene C.] Univ Minnesota Twin Cities, St Paul, MN 55108 USA.
[Neuhauser, Claudia] Univ Minnesota, Rochester, MN 55904 USA.
[Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA.
RP Beckman, NG (reprint author), Univ Nebraska, Sch Biol Sci, 348 Manter Hall, Lincoln, NE 68588 USA.
EM nbeckman2@unl.edu
RI Beckman, Noelle/E-5554-2011
OI Beckman, Noelle/0000-0001-5822-0610
FU National Science Foundation Graduate Research Fellowship; UMN Graduate
School Doctoral Dissertation Fellowship; UMN EEB Block Grant; Packard
Fellowship in Science and Engineering; HSBC Climate Partnership
FX We thank Jim Dalling, Linda Kinkel, George Heimpel and David Tilman for
insightful discussions and two anonymous reviewers for helpful
suggestions in revising the manuscript. We gratefully acknowledge the
support of a National Science Foundation Graduate Research Fellowship
(N.G.B.), UMN Graduate School Doctoral Dissertation Fellowship (N.G.B.),
UMN EEB Block Grant (N.G.B.), Packard Fellowship in Science and
Engineering (H. C. M.) and the HSBC Climate Partnership (H.C.M.).
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J9 J ECOL
JI J. Ecol.
PD JUL
PY 2012
VL 100
IS 4
BP 862
EP 873
DI 10.1111/j.1365-2745.2012.01978.x
PG 12
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 959TE
UT WOS:000305335400003
ER
PT J
AU Lin, LX
Comita, LS
Zheng, Z
Cao, M
AF Lin, Luxiang
Comita, Liza S.
Zheng, Zheng
Cao, Min
TI Seasonal differentiation in density-dependent seedling survival in a
tropical rain forest
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE compensatory trend; density dependence; Janzen-Connell hypothesis; mixed
models; plant-plant interactions; tropical rain forest; water
availability
ID SPECIES SHADE TOLERANCE; PLANT-SOIL FEEDBACK; TREE SEEDLINGS;
NEOTROPICAL FOREST; LOCAL NEIGHBORHOOD; SOUTHWEST CHINA; CANOPY TREE;
FOG-DRIP; GROWTH; XISHUANGBANNA
AB 1. Density-dependent survival is prevalent in tropical forests and is recognized as a potentially important mechanism for maintaining tree species diversity. However, there is little knowledge of how density dependence changes in fluctuating environments. 2. Across the 20-ha Xishuangbanna tropical seasonal rain forest dynamics plot in southwest China, which has distinct dry and wet seasons, we monitored seedling survival in 453 1-m2 quadrats over 2 years. Density dependence was assessed using generalized linear mixed models with crossed random effects. 3. When pooling all species at the community level, there were strong negative effects of conspecific tree neighbours on seedling survival over the dry-season, wet-season and 2-year intervals. The proportion of conspecific seedling neighbours had a significant negative effect in the dry season, but not in the wet season. 4. At the species level, the effects of conspecific tree and seedling neighbours varied widely among species in the community and were significantly positively related to population basal area in the community over the dry-season interval. In contrast, over the wet-season interval, the effects of conspecific tree and seedling neighbours did not significantly vary among species in the community. Overall community- and species-level results suggest that local-scale negative density dependence (NDD) tends to be stronger in the dry than wet season in the Xishuangbanna tropical forest. 5. At the scale of the 20-ha plot, we found a community compensatory trend (CCT), in which rare species had relatively higher seedling survival than common species in both the wet and dry seasons. A positive association between potential NDD and population basal area suggests that the CCT results from local-scale NDD, specifically because of negative effects of conspecific tree neighbours. 6. Synthesis. Our results demonstrate that the strength of density-dependent seedling survival can vary between seasons and among species in tropical forests. Future research is needed to assess the underlying mechanisms of this temporal and interspecific variation in NDD and its consequences for species coexistence and community composition.
C1 [Lin, Luxiang; Zheng, Zheng; Cao, Min] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Kunming 650223, Peoples R China.
[Comita, Liza S.] Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA.
[Comita, Liza S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Lin, LX (reprint author), Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Kunming 650223, Peoples R China.
EM linluxa@xtbg.ac.cn
FU National Natural Science Foundation of China [31000201]; National
Science & Technology Pillar Program from the Ministry of Environmental
Protection of China [2008BAC39B02]; National Center for Ecological
Analysis and Synthesis; NSF [EF-0553768]; University of California,
Santa Barbara; State of California
FX This study was funded by the National Natural Science Foundation of
China (31000201) and the National Science & Technology Pillar Program
from the Ministry of Environmental Protection of China (2008BAC39B02).
LSC acknowledges the support of the National Center for Ecological
Analysis and Synthesis, a centre funded by NSF (Grant #EF-0553768), the
University of California, Santa Barbara, and the State of California. We
thank Xiaoliang Li, Jiu Ma, Wenfu Zhang Xiaobao Deng, Shishun Zhou and
Hong Wang for their assistance with seedling censuses and species
identification. We thank all the people who have contributed to the
establishment of the 20-ha Xishuangbanna tropical seasonal rain forest
dynamics plot. Logistical support was provided by Xishuangbanna Station
of Tropical Rainforest Ecosystem Studies (National Forest Ecosystem
Research Station at Xishuangbanna), Chinese Academy of Sciences. We
thank David Burslem, Calum Brown, Rich Kobe, Robin Chazdon and Danae
Rozendaal for critical comments on the manuscript.
NR 60
TC 27
Z9 37
U1 5
U2 82
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-0477
J9 J ECOL
JI J. Ecol.
PD JUL
PY 2012
VL 100
IS 4
BP 905
EP 914
DI 10.1111/j.1365-2745.2012.01964.x
PG 10
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 959TE
UT WOS:000305335400007
ER
PT J
AU Parr, CS
Guralnick, R
Cellinese, N
Page, RDM
AF Parr, Cynthia S.
Guralnick, Robert
Cellinese, Nico
Page, Roderic D. M.
TI Evolutionary informatics: unifying knowledge about the diversity of life
(vol 27, pg 94, 2012)
SO TRENDS IN ECOLOGY & EVOLUTION
LA English
DT Correction
C1 [Parr, Cynthia S.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Guralnick, Robert] Univ Colorado, Museum Nat Hist, Boulder, CO 80309 USA.
[Guralnick, Robert] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
[Cellinese, Nico] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Page, Roderic D. M.] Univ Glasgow, Inst Biodivers Anim Hlth & Comparat Med, Coll Med Vet & Life Sci, Glasgow G12 8QQ, Lanark, Scotland.
RP Parr, CS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012,MRC 106, Washington, DC 20013 USA.
RI Parr, Cynthia/E-8013-2010
OI Parr, Cynthia/0000-0002-8870-7099
NR 1
TC 0
Z9 0
U1 0
U2 16
PU ELSEVIER SCIENCE LONDON
PI LONDON
PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND
SN 0169-5347
J9 TRENDS ECOL EVOL
JI Trends Ecol. Evol.
PD JUL
PY 2012
VL 27
IS 7
BP 414
EP 414
DI 10.1016/j.tree.2012.05.005
PG 1
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 973WF
UT WOS:000306389900009
ER
PT J
AU Schroll-Guz, S
AF Schroll-Guz, Savannah
TI Political Handbook of the World, 2012
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Schroll-Guz, Savannah] Smithsonian Inst Libs, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUL
PY 2012
VL 137
IS 12
BP 110
EP 110
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 972TG
UT WOS:000306302500217
ER
PT J
AU Nardini, E
Fabian, AC
Walton, DJ
AF Nardini, E.
Fabian, A. C.
Walton, D. J.
TI Investigating the reflection contribution to the X-ray emission of Ton
S180
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: individual: Ton S180; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; SEYFERT 1 GALAXIES; XMM-NEWTON;
SPECTRAL PROPERTIES; FAIRALL 9; LINE; SOFT; EXCESS; ACCRETION
AB There is now growing evidence that the soft X-ray excess is almost ubiquitous among unobscured active galaxies. In spite of the various interpretations that have been considered in the past few years, the nature of this foremost spectral feature is not firmly established yet. In this context, we review from a reflection perspective the three highest quality X-ray observations of the narrow-line type 1 Seyfert galaxy Tonantzintla (Ton) S180, obtained by XMMNewton and Suzaku. The X-ray spectrum of Ton S180 shows only moderate variations over a time span of several years, suggesting that the same physical process accounts for the bulk of the broad-band X-ray emission at the different epochs, and that the properties of the X-ray source are fairly stable. We have successfully applied in our spectral analysis a dual-reflector model, consisting of two separate components: one arises from the surface of the accretion disc, is highly ionized and blurred by relativistic effects; the other is cold, quite faint and can be associated with a distant reprocessor. Due to the strength and the nearly power-law shape of its soft excess emission, Ton S180 is one of the most challenging sources to test the X-ray reflection scenario. In this work we provide a clear illustration of the great potential and spectral flexibility of blurred reflection models, while discussing some of their current limitations and possible shortcomings.
C1 [Nardini, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabian, A. C.; Walton, D. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP Nardini, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM enardini@cfa.harvard.edu
RI XRAY, SUZAKU/A-1808-2009
FU NASA [NNX10AF50G, GO0-11017X]
FX The authors would like to thank the anonymous referee for providing
helpful comments. EN acknowledges the financial support from NASA grants
NNX10AF50G and GO0-11017X. ACF thanks the Royal Society. DJW
acknowledges the financial support provided by the STFC.
NR 64
TC 6
Z9 8
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 423
IS 4
BP 3299
EP 3307
DI 10.1111/j.1365-2966.2012.21123.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 968SB
UT WOS:000306003600022
ER
PT J
AU Jonker, PG
Miller-Jones, JCA
Homan, J
Tomsick, J
Fender, RP
Kaaret, P
Markoff, S
Gallo, E
AF Jonker, P. G.
Miller-Jones, J. C. A.
Homan, J.
Tomsick, J.
Fender, R. P.
Kaaret, P.
Markoff, S.
Gallo, E.
TI The black hole candidate MAXI J1659-152 in and towards quiescence in
X-ray and radio
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion; accretion discs; binaries: general; stars: individual: MAXI
J1659-152; X-rays: binaries
ID LOW/HARD STATE; MULTIWAVELENGTH OBSERVATIONS; OUTBURST DECAY; GRO
J1655-40; HARD STATE; GX 339-4; BINARIES; MASS; A0620-00; SPECTROSCOPY
AB In this paper we report on Expanded Very Large Array radio and Chandra and Swift X-ray observations of the outburst decay of the transient black hole candidate MAXI J1659152 in 2011. We discuss the distance to the source taking the high inclination into account and conclude that the source distance is probably 6 +/- 2 kpc. The lowest observed flux corresponds to a luminosity of erg s-1. This, together with the orbital period of 2.4 h reported in the literature, suggests that the quiescent X-ray luminosity is higher than predicted on the basis of the orbital periodquiescent X-ray luminosity relationship. It is more in line with that expected for a neutron star, although the outburst spectral and timing properties reported in the literature strongly suggest that MAXI J1659152 harbours a black hole. This conclusion is subject to confirmation of the lowest observed flux as the quiescent flux. The relation between the accretion and ejection mechanisms can be studied using the observed correlation between the radio and X-ray luminosities as these evolve over an outburst. We determine the behaviour of MAXI J1659152 in the radioX-ray diagram at low X-ray luminosities using the observations reported in this paper and at high X-ray luminosities using values reported in the literature. At high X-ray luminosities, the source lies closer to the sources that follow a correlation index steeper than 0.60.7. However, when compared to other sources that follow a steeper correlation index, the X-ray luminosity in MAXI J1659152 is also lower. The latter can potentially be explained by the high inclination of MAXI J1659152 if the X-ray emission comes from close to the source and the radio emission is originating in a more extended region. However, it is probable that the source was not in the canonical low-hard state during these radio observations and this may affect the behaviour of the source as well. At intermediate X-ray luminosities, the source makes the transition from the radio underluminous sources in the direction of the relation traced by the standard correlation similar to what has been reported for H 1743-322 in the literature. However, MAXI J1659152 remains underluminous with respect to this standard correlation.
C1 [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Homan, J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Tomsick, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Fender, R. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Markoff, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Gallo, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
RP Jonker, PG (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
EM p.jonker@sron.nl
RI Miller-Jones, James/B-2411-2013
OI Miller-Jones, James/0000-0003-3124-2814
FU National Aeronautics and Space Administration through Chandra
[GO0-11058A]; National Aeronautics Space Administration [NAS8-03060]
FX PGJ acknowledges support from a VIDI grant from the Netherlands
Organisation for Scientific Research. Support for this work was provided
by the National Aeronautics and Space Administration through Chandra
Award Number GO0-11058A issued by the Chandra X-ray Observatory Center,
which is operated by the Smithsonian Astrophysical Observatory for and
on behalf of the National Aeronautics Space Administration under
contract NAS8-03060. This research has made use of the SIMBAD data base,
operated at CDS, Strasbourg, France, of NASA's Astrophysics Data System
Bibliographic Services, of SAOImage DS9, developed by Smithsonian
Astrophysical Observatory, of software provided by the Chandra X-ray
Center (CXC) in the application packages CIAO, and of the XRT Data
Analysis Software (XRTDAS) developed under the responsibility of the ASI
Science Data Center (ASDC), Italy.
NR 60
TC 28
Z9 28
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 423
IS 4
BP 3308
EP 3315
DI 10.1111/j.1365-2966.2012.21116.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 968SB
UT WOS:000306003600023
ER
PT J
AU Vogelsberger, M
Zavala, J
Loeb, A
AF Vogelsberger, Mark
Zavala, Jesus
Loeb, Abraham
TI Subhaloes in self-interacting galactic dark matter haloes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; dark matter
ID DWARF SPHEROIDAL GALAXIES; LAMBDA-CDM; SATELLITE GALAXIES; DENSITY
PROFILES; SIMULATIONS; CONSTRAINTS; POPULATION; COSMOLOGY; CLUSTER;
MILKY
AB We present N-body simulations of a new class of self-interacting dark matter models, which do not violate any astrophysical constraints due to a non-power-law velocity dependence of the transfer cross-section which is motivated by a Yukawa-like new gauge boson interaction. Specifically, we focus on the formation of a Milky-Way-like dark matter halo taken from the Aquarius project and resimulate it for a couple of representative cases in the allowed parameter space of this new model. We find that for these cases, the main halo only develops a small core (similar to 1 kpc) followed by a density profile identical to that of the standard cold dark matter scenario outside of that radius. Neither the subhalo mass function nor the radial number density of subhaloes is altered in these models but there is a significant change in the inner density structure of subhaloes resulting in the formation of a large density core. As a consequence, the inner circular velocity profiles of the most massive subhaloes differ significantly from the cold dark matter predictions and we demonstrate that they are compatible with the observational data of the brightest Milky Way dwarf spheroidals (dSphs) in such a velocity-dependent self-interacting dark matter scenario. Specifically, and contrary to the cold dark matter case, there are no subhaloes that are more concentrated than what is inferred from the kinematics of the Milky Way dSphs. We conclude that these models offer an interesting alternative to the cold dark matter model that can reduce the recently reported tension between the brightest Milky Way satellites and the dense subhaloes found in cold dark matter simulations.
C1 [Vogelsberger, Mark; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zavala, Jesus] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Zavala, Jesus] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
RP Vogelsberger, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mvogelsberger@cfa.harvard.edu
RI Zavala Franco, Jesus/M-5152-2014
OI Zavala Franco, Jesus/0000-0003-4442-908X
FU University of Waterloo; Perimeter Institute for Theoretical Physics;
Government of Canada through Industry Canada; Province of Ontario
through the Ministry of Research Innovation; CITA National Fellowship;
NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A]
FX The simulations in this paper were run on the Odyssey cluster supported
by the FAS Science Division Research Computing Group at Harvard
University. We thank Volker Springel for giving us access to GADGET-3
and Tracy Slatyer and Douglas Finkbeiner for useful discussions. We also
thank Matthew Walker, Simon D. M. White and the referee Naoki Yoshida
for useful comments that improved the paper. JZ is supported by the
University of Waterloo and the Perimeter Institute for Theoretical
Physics. Research at Perimeter Institute is supported by the Government
of Canada through Industry Canada and by the Province of Ontario through
the Ministry of Research & Innovation. JZ acknowledges financial support
by a CITA National Fellowship. This work was supported in part by NSF
grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A (for AL).
NR 62
TC 160
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U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 423
IS 4
BP 3740
EP 3752
DI 10.1111/j.1365-2966.2012.21182.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 968SB
UT WOS:000306003600057
ER
PT J
AU Cheesman, AW
Turner, BL
Reddy, KR
AF Cheesman, Alexander W.
Turner, Benjamin L.
Reddy, K. Ramesh
TI Soil Phosphorus Forms along a Strong Nutrient Gradient in a Tropical
Ombrotrophic Wetland
SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL
LA English
DT Article
ID P-31 NMR-SPECTROSCOPY; MAGNETIC-RESONANCE-SPECTROSCOPY; MICROBIAL
BIOMASS PHOSPHORUS; CHANGUINOLA PEAT DEPOSIT; ORGANIC PHOSPHORUS;
LAKE-SEDIMENTS; INORGANIC POLYPHOSPHATE; SWAMP FOREST; ION-SINK;
DECOMPOSITION
AB Phosphorus cycling influences productivity and diversity in tropical wetlands, yet little is known about the forms of P found in the accreting organic matter of these ecosystems. We used alkaline (NaOH-ethylenediamine tetraacetic acid [EDTA]) extraction and solution P-31 nuclear magnetic resonance (NMR) spectroscopy to characterize P in surface soils across a strong nutrient gradient within a tropical ombrotrophic peat dome. From the interior bog plain to the marginal Raphia taedigera swamp, total soil P increased from 14.6 to 70.9 g m(-3) and resin-extractable P from 0.1 to 30 mg kg(-1). Phosphatase activity declined across the same transect (364-46 mu mol methylumbelliferone kg(-1) min(-1)), indicating an increase in P availability toward the periphery of the wetland. Organic P identified by solution 31P NMR spectroscopy included phosphomonoesters (12-17%), phosphodiesters (10-14%), and phosphonates (up to 3.3% of total P). Inositol phosphates were not detected in these acidic peats. Inorganic P forms included orthophosphate (9-25% of total P), pyrophosphate (up to 3%), and long-chain polyphosphates; the latter occurred in concentrations (up to 24% of total soil P) considerably higher than previously found in wetland soils. The concentration of residual (unextractable) P was similar among sites (mean 280 mg kg(-1)), resulting in an increase in its proportion of the total soil P from 29% at the P-rich margins to 55% at the P-poor interior. This is the first information on the P composition of tropical wetland soils and provides a basis for further study of the cycling and contribution of P forms to the nutrition of plants and microorganisms.
C1 [Cheesman, Alexander W.; Reddy, K. Ramesh] Univ Florida, Soil & Water Sci Dep, Wetland Biogeochem Lab, Gainesville, FL 32611 USA.
[Cheesman, Alexander W.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Cheesman, AW (reprint author), Univ Florida, Soil & Water Sci Dep, Wetland Biogeochem Lab, 106 Newell Hall, Gainesville, FL 32611 USA.
EM cheesmanA@si.edu
RI Turner, Benjamin/E-5940-2011; Cheesman, Alexander/H-5918-2013
OI Turner, Benjamin/0000-0002-6585-0722; Cheesman,
Alexander/0000-0003-3931-5766
FU USDA-CREES National Research Initiative [2004-35107-14918]; National
High Magnetic Field Laboratory
FX We thank G. Jacome and P. Gondola of the Smithsonian Tropical Research
Institute, Bocas del Toro Research Station, for logistical support and
Dr. Jim Rocca, Dr. Alex Blumenfeld, and Tania Romero for analytical
support. The project was supported by a grant from the USDA-CREES
National Research Initiative (no. 2004-35107-14918) and the External
User Program of the National High Magnetic Field Laboratory administered
through the Advanced Magnetic Resonance Imaging and Spectroscopy (AMRIS)
facility of the McKnight Brain Institute, University of Florida.
NR 85
TC 22
Z9 22
U1 3
U2 74
PU SOIL SCI SOC AMER
PI MADISON
PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA
SN 0361-5995
J9 SOIL SCI SOC AM J
JI Soil Sci. Soc. Am. J.
PD JUL
PY 2012
VL 76
IS 4
BP 1496
EP 1506
DI 10.2136/sssaj2011.0365
PG 11
WC Soil Science
SC Agriculture
GA 973JH
UT WOS:000306355900037
ER
PT J
AU Collin, R
AF Collin, Rachel
TI Nontraditional Life-History Choices: What Can "Intermediates" Tell Us
about Evolutionary Transitions between Modes of Invertebrate
Development?
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Article
ID BOCCARDIA-PROBOSCIDEA POLYCHAETA; MARINE BENTHIC INVERTEBRATES; VARIABLE
LARVAL DEVELOPMENT; EGG SIZE; POECILOGONOUS POLYCHAETE; REPRODUCTIVE
STRATEGIES; PHENOTYPIC POLYMORPHISM; CALYPTRAEID GASTROPODS;
HYDROIDS-ELEGANS; ALDERIA-MODESTA
AB Mode of development in marine invertebrates has been largely viewed as a dichotomy between small eggs that develop into free-living planktotrophic larvae and large eggs that bypass the larval stage and develop directly into juveniles. Modes of development that could be categorized as "intermediate" between these two extremes include facultative feeding larvae, short-lived planktotrophic larvae, dispersal dimorphisms, and poecilogony (in which nutritional mode varies within a species). These intermediates are rare. The few species-level phylogenies available that include them do not generally support the interpretation of intermediates as necessary, ephemeral transitional forms. Instead, they support the idea that intermediates are well adapted to their environments but that either these environments are short-lived relative to the frequency of speciation, or speciation events are associated with shifts in the mode of development. Each of the different intermediate forms could have evolved in response to variable environments. The phenotypically plastic intermediates could be a response to predictable environmental variation. Facultative feeding larvae and short-lived planktotrophic larvae could reflect conservative bet-hedging in response to unpredictable environmental variation, whereas poecilogony with mixed clutches could represent the alternative: diversifying bet-hedging. Since environmental variability is common, it remains an enigma why these intermediates are so rare. Discovery of more intermediates, and their careful description in terms of the level of variation expressed within, and among, clutches, and among females and populations, as well as determination of the genetic and environmental influences on this variation, will provide valuable test-cases for theories of the evolution of alternative phenotypes.
C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama.
EM collinr@si.edu
FU US National Science Foundation [IOS-1157279, IOS-1019727]; Company of
Biologists, Ltd.; American Microscopical Society; Society for
Integrative and Comparative Biology; SICB division DEDB; SICB division
DEE; SICB division DIZ
FX I thank Pat Krug and Bruno Pernet for a helpful discussion, and K.
McDonald for comments on an earlier version of the manuscript. I thank
Emily Knott and Damhnait McHugh for organizing the symposium
"Poecilogony as a window on larval evolution: Polymorphism of
developmental mode within marine invertebrate species,'' which was
sponsored by the US National Science Foundation (IOS-1157279), The
Company of Biologists, Ltd., the American Microscopical Society, and the
Society for Integrative and Comparative Biology, including SICB
divisions DEDB, DEE, and DIZ.; I am grateful to the US National Science
Foundation (IOS-1019727 to R. C.) for support of my research.
NR 56
TC 18
Z9 19
U1 2
U2 23
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD JUL
PY 2012
VL 52
IS 1
BP 128
EP 137
DI 10.1093/icb/ics065
PG 10
WC Zoology
SC Zoology
GA 966FP
UT WOS:000305823400012
PM 22596057
ER
PT J
AU Arnold, DE
Bohor, BF
Neff, H
Feinman, GM
Williams, PR
Dussubieux, L
Bishop, R
AF Arnold, Dean E.
Bohor, Bruce F.
Neff, Hector
Feinman, Gary M.
Williams, Patrick Ryan
Dussubieux, Laure
Bishop, Ronald
TI The first direct evidence of pre-columbian sources of palygorskite for
Maya Blue
SO JOURNAL OF ARCHAEOLOGICAL SCIENCE
LA English
DT Article
DE Maya Blue; Palygorskite; Yucatan, Mexico; Chemical analysis; Volcanic
ash
ID ICP-MS; PIGMENT; YUCATAN; MEXICO; ATTAPULGITE; PAINT; CLAY
AB Maya Blue, a nano-structured clay organic complex of palygorskite and indigo, was used predominantly before the Spanish Conquest. It has fascinated chemists, material scientists, archaeologists and art historians for decades because it is resistant to the effect of acids, alkalis, and other reagents, and its rich color has persisted for centuries in the harsh tropical climate of southern Mesoamerica. One of its components, palygorskite, is part of modern Maya indigenous knowledge, and ethnohistoric and archaeological data suggest that its modern sources were probably utilized in Prehispanic times. Yet no direct evidence verifies that palygorskite was actually mined from these sources to make Maya Blue. Here we characterize these sources compositionally, and compare our analyses to those of Maya Blue from Chichen Itza and Palenque. We demonstrate that the palygorskite in most of these samples came from modern mines, providing the first direct evidence for the use of these sources for making Maya Blue. These findings reveal that modern Maya indigenous knowledge about palygorskite, its mining, and its source locations, is at least seven centuries old. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Arnold, Dean E.] Wheaton Coll, Dept Sociol & Anthropol, Wheaton, IL 60187 USA.
[Bohor, Bruce F.] US Geol Survey Emeritus, Fed Ctr, Denver, CO USA.
[Neff, Hector] Calif State Univ Long Beach, Dept Anthropol, Long Beach, CA 90840 USA.
[Arnold, Dean E.; Feinman, Gary M.; Williams, Patrick Ryan; Dussubieux, Laure] Field Museum Nat Hist, Dept Anthropol, Chicago, IL 60605 USA.
[Bishop, Ronald] Smithsonian Inst, Dept Anthropol, Washington, DC 20013 USA.
RP Arnold, DE (reprint author), Wheaton Coll, Dept Sociol & Anthropol, 501 E Coll, Wheaton, IL 60187 USA.
EM Dean.E.Arnold@wheaton.edu; Bbohor@usgs.gov; hneff@csulb.edu;
gfeinman@fieldmuseum.org; rwilliams@fieldmuseum.org;
ldussubieu@fieldmuseum.org; bishopr@si.edu
FU National Geographic Society [8433-08]; Wheaton College G.W. Aldeen
Memorial Fund; NSF [BCS-0917702, BCS-0604712]
FX This research was supported by grants to the senior author from the
National Geographic Society (Grant No. 8433-08) and the Wheaton College
G.W. Aldeen Memorial Fund. The IIRMES Archaeometry lab, where some of
the LA-ICP-MS analyses were undertaken, is supported by NSF grants
BCS-0917702 and BCS-0604712. We thank William Betterton of the USGS for
the X-ray diffraction patterns, and are grateful for the assistance of
Hilary Mulhern, Wendy Jennings, and Hayley Schumacher in the preparation
of this manuscript.
NR 57
TC 9
Z9 10
U1 0
U2 22
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0305-4403
J9 J ARCHAEOL SCI
JI J. Archaeol. Sci.
PD JUL
PY 2012
VL 39
IS 7
BP 2252
EP 2260
DI 10.1016/j.jas.2012.02.036
PG 9
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 966PH
UT WOS:000305849400033
ER
PT J
AU Ubelaker, DH
De La Paz, JS
AF Ubelaker, Douglas H.
De La Paz, Jade S.
TI Skeletal Indicators of Pregnancy and Parturition: A Historical Review
SO JOURNAL OF FORENSIC SCIENCES
LA English
DT Article
DE forensic science; forensic anthropology; parturition; parity status;
pelvis; skeletal alterations; childbirth indicators
ID SYMPHYSIS PUBIS; PREAURICULAR GROOVE; AGE-DETERMINATION; PELVIC JOINTS;
OS-PUBIS; BONE; PARITY; DELIVERY; FEMALES; SULCUS
AB Over a century of scientific literature has documented the research and analysis relating to the possible skeletal evidence of pregnancy, parturition, and childcare, yet today, there still exists variation in methodology and interpretation. Historical perspective facilitates understanding of the growth and development of the theories and research currently available to the forensic science community. Review of the relevant literature clearly indicates that specific skeletal alterations are not exclusively connected to obstetrical events. Although parturition and related events have been shown to leave various alterations on bone, the research record also demonstrates that other factors can contribute to the same or similar changes. Additionally, such alterations can often be found in nulliparous women and men and are frequently absent in parous and multiparous women. This literature review calls for the continued exploration of skeletal alterations for determining parity status in human skeletal remains.
C1 [Ubelaker, Douglas H.; De La Paz, Jade S.] NMNH, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA.
RP Ubelaker, DH (reprint author), NMNH, Dept Anthropol, Smithsonian Inst, MRC 112, Washington, DC 20560 USA.
EM ubelaked@si.edu
NR 79
TC 10
Z9 10
U1 2
U2 17
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-1198
J9 J FORENSIC SCI
JI J. Forensic Sci.
PD JUL
PY 2012
VL 57
IS 4
BP 866
EP 872
DI 10.1111/j.1556-4029.2012.02102.x
PG 7
WC Medicine, Legal
SC Legal Medicine
GA 967HE
UT WOS:000305896700002
PM 22372612
ER
PT J
AU Cron, GV
Pirone, C
Bartlett, M
Kress, WJ
Specht, C
AF Cron, Glynis V.
Pirone, Cary
Bartlett, Madelaine
Kress, W. John
Specht, Chelsea
TI Phylogenetic Relationships and Evolution in the Strelitziaceae
(Zingiberales)
SO SYSTEMATIC BOTANY
LA English
DT Article
DE Biogeography; molecular phylogenetics; morphology; pollination;
Strelitzia
ID ARCHAIC COEVOLUTIONARY SYSTEM; NONCODING CHLOROPLAST DNA;
RAVENALA-MADAGASCARIENSIS; ORCHIDANTHA LOWIACEAE; FLORAL DEVELOPMENT;
CLIVIA-MIRABILIS; SEQUENCE DATA; SOUTH-AFRICA; POLLINATION; REGINAE
AB Evolutionary trends and phylogenetic relationships in the Strelitziaceae (Zingiberales) were investigated using sequence data from ten plastid and two nuclear regions and a morphological dataset. The status of species of Strelitzia were evaluated in terms of the phylogenetic species concept. Relationships among the genera remain equivocal with two hypotheses emerging: (i) Strelitzia sister to a clade comprising Ravenala and Phenakospermum when indels are included, or (ii) Ravenala sister to the remainder of the Strelitziaceae when indels are excluded in/from the combined molecular and 'total evidence' analyses. Within Strelitzia, S. nicolai is sister to the rest of the genus, with S. alba sister to S. caudata. Strelitzia reginae is shown to be paraphyletic as S. juncea is nested within it, but more sampling at the population level is needed to confirm the taxonomic status of S. juncea. The highly localized and endangered Strelitzia alba is confirmed as a distinct species, as are S. caudata and S. nicolai, despite few morphological differences. Evolutionary trends are linked to changes in habitat and coevolution with pollinators. Climate change in southern Africa is thought to have restricted Strelitzia nicolai (or its ancestor) to the eastern coastal region, with subsequent allopatric speciation of S. alba and S. caudata, and relatively recent parapatric divergence of S. juncea from S. reginae.
C1 [Cron, Glynis V.] Univ Witwatersrand, Sch Anim Plant & Environm Sci, ZA-2050 Johannesburg, South Africa.
[Pirone, Cary] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA.
[Bartlett, Madelaine; Specht, Chelsea] Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA.
[Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, NHB 166, Washington, DC 20560 USA.
RP Cron, GV (reprint author), Univ Witwatersrand, Sch Anim Plant & Environm Sci, ZA-2050 Johannesburg, South Africa.
EM Glynis.Cron@wits.ac.za
FU United States Environmental Protection Agency (EPA) under the Greater
Research Opportunities (GRO) Graduate Program; National Research
Foundation (NRF) of South Africa
FX We thank the following persons: Dave Erickson (Smithsonian Institute),
Justin Ramsey and Adam Green (University of Rochester) for laboratory
use and the training of one of the authors (C. P.) in DNA sequencing
technique, Kishlayin Chetty and Alex Haw for field collections and
vegetative measurements of Strelitzia, Ewa Wojtasik for assistance with
ARCGIS, Fairchild Tropical Botanic Garden and the University of
California Botanical Garden and Heather Driscoll for assistance with
vouchers, and Tim Collins for reviewing the molecular data and analyses.
Laboratory work was funded in part by the United States Environmental
Protection Agency (EPA) under the Greater Research Opportunities (GRO)
Graduate Program; the field work and some sequencing were funded by the
National Research Foundation (NRF) of South Africa. We thank the
provincial authorities of KwaZulu-Natal, Eastern Cape and Western Cape
for permits to collect Strelitzia specimens, and BOL, J, MO, NBG, NH,
NU, PRE, RSA, and SAM herbaria for the loan of specimens for
morphological examination, and David Lee and David Lorence for use of
their photographs.
NR 115
TC 3
Z9 4
U1 3
U2 34
PU AMER SOC PLANT TAXONOMISTS
PI LARAMIE
PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071
USA
SN 0363-6445
EI 1548-2324
J9 SYST BOT
JI Syst. Bot.
PD JUL-SEP
PY 2012
VL 37
IS 3
BP 606
EP 619
DI 10.1600/036364412X648562
PG 14
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 965PA
UT WOS:000305778500004
ER
PT J
AU Stull, GW
Herrera, F
Manchester, SR
Jaramillo, C
Tiffney, BH
AF Stull, Gregory W.
Herrera, Fabiany
Manchester, Steven R.
Jaramillo, Carlos
Tiffney, Bruce H.
TI Fruits of an "Old World" tribe (Phytocreneae; Icacinaceae) from the
Paleogene of North and South America
SO SYSTEMATIC BOTANY
LA English
DT Article
DE Biogeography; fossil endocarps; Icacinaceae; Neotropics; Paleogene
ID NEOTROPICAL RAIN-FOREST; LATE PALEOCENE; CERREJON FORMATION; COLOMBIA;
EOCENE; PHYTOGEOGRAPHY; MENISPERMACEAE; TERTIARY; MIDDLE; ANDES
AB The Phytocreneae (Icacinaceae) are a tribe of scrambling shrubs and lianas presently distributed in tropical Africa, Madagascar, and Indo-Malesia. We describe the oldest known fossils of this tribe and provide the first recognition of this group in the Neotropical fossil record based on distinctive fruit remains. Palaeophytocrene piggae sp. nov., from the late Paleocene of western North America, and Palaeophytocrene hammenii sp. nov. and cf. Phytocrene sp., from the middle-late Paleocene of Colombia, constitute the oldest confirmed records of this tribe. Pyrenacantha austroamericana sp. nov., from the Oligocene of Peru, represents an extant Old World genus known also from the Eocene fossil record of North America and Europe. Collectively, these fossils indicate that the Phytocreneae were previously established in the Neotropics, despite their current absence from the region, and may provide evidence for Paleogene floristic exchange between North and South America.
C1 [Stull, Gregory W.; Herrera, Fabiany; Manchester, Steven R.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Stull, Gregory W.; Herrera, Fabiany; Manchester, Steven R.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Herrera, Fabiany; Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Tiffney, Bruce H.] Univ Calif Santa Barbara, Dept Earth Sci, Santa Barbara, CA 93106 USA.
RP Stull, GW (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
EM gwstull@ufl.edu
FU graduate student research awards from the American Society of Plant
Taxonomists; Society of Systematic Biologists; Evolving Earth
Foundation; Geological Society of America Foundation; Asociacion
Colombiana de Geologos y Geofisicos del Petroleo-ARES; Gary S. Morgan
Student Research Award; Lewis & Clark Foundation-American Philosophical
Society; Smithsonian Paleobiology Endowment Fund; Fundacion para la
Promocion de la Investigacion y la Tecnologia, Banco de la Republica;
Colombian Petroleum Institute; Fundacion Ares; National Science
Foundation [BSR 0743474]
FX We thank Jan Wieringa (WAG) for making modem icacinaceous fruits
available for study, Terry A. Lott (UF) for assistance with photography
and proofreading, and Mark P. Simmons and two anonymous reviewers for
providing helpful suggestions for improving the manuscript. This study
was supported by graduate student research awards from the American
Society of Plant Taxonomists and the Society of Systematic Biologists to
G. W. Stull; the Evolving Earth Foundation, the Geological Society of
America Foundation, the Asociacion Colombiana de Geologos y Geofisicos
del Petroleo-ARES, the Gary S. Morgan Student Research Award, and the
Lewis & Clark Foundation-American Philosophical Society to F. Herrera;
the Smithsonian Paleobiology Endowment Fund, the Fundacion para la
Promocion de la Investigacion y la Tecnologia, Banco de la Republica,
the Colombian Petroleum Institute, and Fundacion Ares to C. Jaramillo;
and National Science Foundation grant BSR 0743474 to S. R. Manchester.
NR 52
TC 9
Z9 11
U1 0
U2 3
PU AMER SOC PLANT TAXONOMISTS
PI LARAMIE
PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071
USA
SN 0363-6445
EI 1548-2324
J9 SYST BOT
JI Syst. Bot.
PD JUL-SEP
PY 2012
VL 37
IS 3
BP 784
EP 794
DI 10.1600/036364412X648724
PG 11
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 965PA
UT WOS:000305778500019
ER
PT J
AU Bulbul, E
Smith, RK
Loewenstein, M
AF Bulbul, Esra
Smith, Randall K.
Loewenstein, Michael
TI A NEW METHOD TO CONSTRAIN SUPERNOVA FRACTIONS USING X-RAY OBSERVATIONS
OF CLUSTERS OF GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: intracluster medium; galaxies: individual (A3112);
nuclear reactions, nucleosynthesis, abundances; supernovae: general;
X-rays: galaxies: clusters
ID GALACTIC CHEMICAL EVOLUTION; CORE-COLLAPSE SUPERNOVAE; XMM-NEWTON
SPECTROSCOPY; DELAY-TIME DISTRIBUTION; STAR-FORMATION RATE; METAL
ENRICHMENT; HIGH-REDSHIFT; INTRACLUSTER MEDIUM; ABUNDANCE PATTERN; IA
SUPERNOVAE
AB Supernova (SN) explosions enrich the intracluster medium (ICM) both by creating and dispersing metals. We introduce a method to measure the number of SNe and relative contribution of Type Ia supernovae (SNe Ia) and core-collapse supernovae (SNe cc) by directly fitting X-ray spectral observations. The method has been implemented as an XSPEC model called snapec. snapec utilizes a single-temperature thermal plasma code (apec) to model the spectral emission based on metal abundances calculated using the latest SN yields from SN Ia and SN cc explosion models. This approach provides a self-consistent single set of uncertainties on the total number of SN explosions and relative fraction of SN types in the ICM over the cluster lifetime by directly allowing these parameters to be determined by SN yields provided by simulations. We apply our approach to XMM-Newton European Photon Imaging Camera (EPIC), Reflection Grating Spectrometer (RGS), and 200 ks simulated Astro-H observations of a cooling flow cluster, A3112. We find that various sets of SN yields present in the literature produce an acceptable fit to the EPIC and RGS spectra of A3112. We infer that 30.3% +/- 5.4% to 37.1% +/- 7.1% of the total SN explosions are SNe Ia, and the total number of SN explosions required to create the observed metals is in the range of (1.06 +/- 0.34) x 10(9) to (1.28 +/- 0.43) x 10(9), from snapec fits to RGS spectra. These values may be compared to the enrichment expected based on well-established empirically measured SN rates per star formed. The proportions of SNe Ia and SNe cc inferred to have enriched the ICM in the inner 52 kpc of A3112 is consistent with these specific rates, if one applies a correction for the metals locked up in stars. At the same time, the inferred level of SN enrichment corresponds to a star-to-gas mass ratio that is several times greater than the 10% estimated globally for clusters in the A3112 mass range.
C1 [Bulbul, Esra; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bulbul, Esra; Loewenstein, Michael] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Loewenstein, Michael] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bulbul, Esra; Loewenstein, Michael] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Bulbul, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ebulbul@cfa.harvard.edu
FU NASA XMM-Newton grant [NNX09AP92G]; NASA ROSES-ADP grant [NNX09AC71G]
FX The authors thank Hiroya Yamaguchi for kindly providing help on the simx
software. We also thank the referee for their careful reading of the
paper and insightful suggestions. We gratefully acknowledge support for
this research from NASA XMM-Newton grant NNX09AP92G and NASA ROSES-ADP
grant NNX09AC71G.
NR 57
TC 14
Z9 15
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 54
DI 10.1088/0004-637X/753/1/54
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500054
ER
PT J
AU Dai, YS
Bergeron, J
Elvis, M
Omont, A
Huang, JS
Bock, J
Cooray, A
Fazio, G
Hatziminaoglou, E
Ibar, E
Magdis, GE
Oliver, SJ
Page, MJ
Perez-Fournon, I
Rigopoulou, D
Roseboom, IG
Scott, D
Symeonidis, M
Trichas, M
Vieira, JD
Willmer, CNA
Zemcov, M
AF Dai, Y. Sophia
Bergeron, Jacqueline
Elvis, Martin
Omont, Alain
Huang, Jia-Sheng
Bock, Jamie
Cooray, Asantha
Fazio, Giovanni
Hatziminaoglou, Evanthia
Ibar, Edo
Magdis, Georgios E.
Oliver, Seb J.
Page, Mathew J.
Perez-Fournon, Ismael
Rigopoulou, Dimitra
Roseboom, Isaac G.
Scott, Douglas
Symeonidis, Myrto
Trichas, Markos
Vieira, Joaquin D.
Willmer, Christopher N. A.
Zemcov, Michael
TI A POPULATION OF DUST-RICH QUASARS AT z similar to 1.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: nuclei; galaxies: starburst; infrared:
galaxies; quasars: general
ID SPECTRAL ENERGY-DISTRIBUTIONS; ULTRALUMINOUS INFRARED GALAXIES; ACTIVE
GALACTIC NUCLEI; PALOMAR-GREEN QUASARS; DIGITAL SKY SURVEY;
HIGH-REDSHIFT QUASARS; MM MAMBO/IRAM-30 M; STAR-FORMATION; HOST
GALAXIES; MU-M
AB We report Herschel SPIRE (250, 350, and 500 mu m) detections of 32 quasars with redshifts 0.5 <= z <= 3.6 from the Herschel Multi-tiered Extragalactic Survey (HerMES). These sources are from a MIPS 24 mu m flux-limited sample of 326 quasars in the Lockman Hole Field. The extensive multi-wavelength data available in the field permit construction of the rest-frame spectral energy distributions (SEDs) from ultraviolet to the mid-infrared for all sources, and to the far-infrared (FIR) for the 32 objects. Most quasars with Herschel FIR detections show dust temperatures in the range of 25-60 K, with a mean of 34 K. The FIR luminosities range from 10(11.3) to 10(13.5) L-circle dot, qualifying most of their hosts as ultra-or hyper-luminous infrared galaxies. These FIR-detected quasars may represent a dust-rich population, but with lower redshifts and fainter luminosities than quasars observed at similar to 1 mm. However, their FIR properties cannot be predicted from shorter wavelengths (0.3-20 mu m, rest frame), and the bolometric luminosities derived using the 5100 angstrom index may be underestimated for these FIR-detected quasars. Regardless of redshift, we observed a decline in the relative strength of FIR luminosities for quasars with higher near-infrared luminosities.
C1 [Dai, Y. Sophia; Elvis, Martin; Huang, Jia-Sheng; Fazio, Giovanni; Trichas, Markos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dai, Y. Sophia] Boston Coll, Chestnut Hill, MA 02468 USA.
[Bergeron, Jacqueline; Omont, Alain] Inst Astrophys, UMR7095, F-75014 Paris, France.
[Bock, Jamie; Vieira, Joaquin D.; Zemcov, Michael] CALTECH, Pasadena, CA 91125 USA.
[Bock, Jamie; Zemcov, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Hatziminaoglou, Evanthia] ESO, D-85748 Garching, Germany.
[Ibar, Edo] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ibar, Edo; Roseboom, Isaac G.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Magdis, Georgios E.; Rigopoulou, Dimitra] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Magdis, Georgios E.] CEA Saclay, CNRS, Serv Astrophys Orme Merisiers, F-91191 Gif Sur Yvette, France.
[Oliver, Seb J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Page, Mathew J.; Symeonidis, Myrto] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Perez-Fournon, Ismael] IAC, E-38205 Tenerife, Spain.
[Perez-Fournon, Ismael] ULL, Dept Astrofis, E-38205 Tenerife, Spain.
[Rigopoulou, Dimitra] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
[Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Willmer, Christopher N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Dai, YS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ydai@cfa.harvard.edu
RI Oliver, Seb/A-2479-2013; Magdis, Georgios/C-7295-2014;
OI Oliver, Seb/0000-0001-7862-1032; Magdis, Georgios/0000-0002-4872-2294;
Scott, Douglas/0000-0002-6878-9840
FU CSA (Canada); NAOC (China); CEA; CNES; CNRS (France); ASI (Italy); MCINN
(Spain); SNSB (Sweden); STFC; UKSA (UK); NASA (USA); Science and
Technology Facilities Council [ST/F002858/1, ST/I000976/1]; NASA;
Smithsonian Astrophysical Observatory; University of Arizona; SAO
Predoctoral Fellowship
FX This research has made use of data from the HerMES project-a Herschel
Key Program utilizing Guaranteed Time from the SPIRE instrument team,
ESAC scientists and a mission scientist. SPIRE has been developed by a
consortium of institutes led by Cardiff University (UK) and including
the University of Lethbridge (Canada); NAOC (China); CEA, LAM (France);
IFSI, the University of Padua (Italy); IAC (Spain); Stockholm
Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, the
University of Sussex (UK); Caltech, JPL, NHSC, the University of
Colorado (USA). This development has been supported by national funding
agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI
(Italy); MCINN (Spain); SNSB (Sweden); STFC and UKSA (UK); and NASA
(USA). The HerMES data were accessed through the HeDaM database
(http://hedam.oamp.fr) operated by CeSAM and hosted by the Laboratoire
d'Astrophysique de Marseille. We acknowledge support from the Science
and Technology Facilities Council (grant numbers ST/F002858/1 and
ST/I000976/1). This work is based partly on observations made with the
Spitzer Space Telescope and the MMT Observatory, operated by the Jet
Propulsion Laboratory, Caltech under a contract with NASA, the
Smithsonian Astrophysical Observatory and the University of Arizona,
respectively. Research by Y. S. D. is supported by the SAO Predoctoral
Fellowship.
NR 52
TC 19
Z9 19
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 33
DI 10.1088/0004-637X/753/1/33
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500033
ER
PT J
AU Doria, A
Gitti, M
Ettori, S
Brighenti, F
Nulsen, PEJ
McNamara, BR
AF Doria, Alberto
Gitti, Myriam
Ettori, Stefano
Brighenti, Fabrizio
Nulsen, Paul E. J.
McNamara, Brian R.
TI A CHANDRA-VLA INVESTIGATION OF THE X-RAY CAVITY SYSTEM AND RADIO
MINI-HALO IN THE GALAXY CLUSTER RBS 797
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: clusters: individual (RBS 797); galaxies:
clusters: intracluster medium; galaxies: jets; radio continuum:
galaxies; X-rays: galaxies: clusters
ID ACTIVE GALACTIC NUCLEI; COOLING FLOW CLUSTERS; LARGE-SCALE SHOCK;
XMM-NEWTON OBSERVATION; ROSAT BRIGHT SURVEY; PERSEUS CLUSTER; RX
J1347.5-1145; HOT ATMOSPHERES; AGN OUTBURST; EMITTING GAS
AB We present a study of the cavity system in the galaxy cluster RBS 797 based on Chandra and Very Large Array (VLA) data. RBS 797 (z = 0.35) is one of the most distant galaxy clusters in which two pronounced X-ray cavities have been discovered. The Chandra data confirm the presence of a cool core and indicate a higher metallicity along the cavity directions. This is likely due to the active galactic nucleus outburst, which lifts cool metal-rich gas from the center along the cavities, as seen in other systems. We find indications that the cavities are hotter than the surrounding gas. Moreover, the new Chandra images show bright rims contrasting with the deep, X-ray deficient cavities. The likely cause is that the expanding 1.4 GHz radio lobes have displaced the gas, compressing it into a shell that appears as bright cool arms. Finally, we show that the large-scale radio emission detected with our VLA observations may be classified as a radio mini-halo, powered by the cooling flow, as it nicely follows the trend P-radio versus P-CF predicted by the reacceleration model.
C1 [Doria, Alberto] Argelander Inst Astron, D-53121 Bonn, Germany.
[Gitti, Myriam; Brighenti, Fabrizio] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Gitti, Myriam; Ettori, Stefano] Astron Observ Bologna INAF, I-40127 Bologna, Italy.
[Gitti, Myriam] Inst Radioastron INAF, I-40129 Bologna, Italy.
[Nulsen, Paul E. J.; McNamara, Brian R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[McNamara, Brian R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada.
[McNamara, Brian R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada.
RP Doria, A (reprint author), Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany.
RI Ettori, Stefano/N-5004-2015;
OI Ettori, Stefano/0000-0003-4117-8617; Gitti, Myriam/0000-0002-0843-3009;
Nulsen, Paul/0000-0003-0297-4493
FU Chandra grant [GO0-11136X, GO0-11003X]; Natural Sciences and Engineering
Research Council of Canada; [ASI-INAF I/023/05/0]; [I/088/06/0]
FX A.D. is a member of the International Max Planck Research School (IMPRS)
for Astronomy and Astrophysics at the Universities of Bonn and Cologne.
A significant part of this work was done by A.D. as a Master student at
the University of Bologna. A.D. thanks the Harvard-Smithsonian Center
for Astrophysics for the hospitality during the finalization of this
work and acknowledges support by the Chandra grant GO0-11136X. M.G.
acknowledges support by grants ASI-INAF I/023/05/0 and I/088/06/0 and by
Chandra grants GO0-11003X and GO0-11136X. B.R.M. acknowledges support
from the Natural Sciences and Engineering Research Council of Canada.
NR 61
TC 10
Z9 10
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 47
DI 10.1088/0004-637X/753/1/47
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500047
ER
PT J
AU Graham, ML
Sand, DJ
Bildfell, CJ
Pritchet, CJ
Zaritsky, D
Hoekstra, H
Just, DW
Herbert-Fort, S
Sivanandam, S
Foley, RJ
AF Graham, M. L.
Sand, D. J.
Bildfell, C. J.
Pritchet, C. J.
Zaritsky, D.
Hoekstra, H.
Just, D. W.
Herbert-Fort, S.
Sivanandam, S.
Foley, R. J.
TI THE TYPE II SUPERNOVA RATE IN z similar to 0.1 GALAXY CLUSTERS FROM THE
MULTI-EPOCH NEARBY CLUSTER SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; supernovae: general
ID CORE-COLLAPSE SUPERNOVAE; DELAY-TIME DISTRIBUTION; STAR-FORMATION; P
SUPERNOVAE; HOST GALAXIES; IA SUPERNOVAE; LEGACY SURVEY; K-CORRECTIONS;
OBSERVATIONAL CONSTRAINTS; EVOLUTION
AB We present seven spectroscopically confirmed Type II cluster supernovae (SNe II) discovered in the Multi-Epoch Nearby Cluster Survey, a supernova survey targeting 57 low-redshift 0.05 < z < 0.15 galaxy clusters with the Canada-France-Hawaii Telescope. We find the rate of Type II supernovae within R-200 of z similar to 0.1 galaxy clusters to be 0.026(-0.018)(+0.085) (stat)(-0.001)(+0.003) (sys) SNuM. Surprisingly, one SN II is in a red-sequence host galaxy that shows no clear evidence of recent star formation (SF). This is unambiguous evidence in support of ongoing, low-level SF in at least some cluster elliptical galaxies, and illustrates that galaxies that appear to be quiescent cannot be assumed to host only Type Ia SNe. Based on this single SN II we make the first measurement of the SN II rate in red-sequence galaxies, and find it to be 0.007(-0.007)(+0.014)(stat)(-0.001)(+0.009)(sys) SNuM. We also make the first derivation of cluster specific star formation rates (sSFR) from cluster SN II rates. We find that for all galaxy types the sSFR is 5.1(-3.1)(+15.8) (stat) +/- 0.9(sys) M-circle dot yr(-1) (10(12) M-circle dot)(-1), and for red-sequence galaxies only it is 2.0(-0.9)(+4.2)(stat) +/- 0.4(sys) M-circle dot yr(-1) (10(12) M-circle dot)(-1). These values agree with SFRs measured from infrared and ultraviolet photometry, and H alpha emission from optical spectroscopy. Additionally, we use the SFR derived from our SNII rate to show that although a small fraction of cluster Type Ia SNe may originate in the young stellar population and experience a short delay time, these results do not preclude the use of cluster SN Ia rates to derive the late-time delay time distribution for SNe Ia.
C1 [Graham, M. L.; Sand, D. J.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Graham, M. L.; Sand, D. J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Bildfell, C. J.; Pritchet, C. J.] Univ Victoria, Dept Phys & Astron, STN CSC, Victoria, BC V8W 3P6, Canada.
[Zaritsky, D.; Herbert-Fort, S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Hoekstra, H.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Sivanandam, S.] Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Graham, ML (reprint author), Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Santa Barbara, CA 93117 USA.
OI Hoekstra, Henk/0000-0002-0641-3231
FU National Engineering and Science Research Council of Canada; Marie Curie
International Reintegration Grant; NWO Vidi grant; National Aeronautics
and Space Administration
FX We gratefully acknowledge the CFHT Queued Service Observations team,
without whom MENeaCS would not have been possible. We thank Nelson
Caldwell for managing the MMT/Hectospec queue, and also thank Stephenson
Yang for his dedication to essential computer and network maintenance.
C.J.P. acknowledges support from the National Engineering and Science
Research Council of Canada. H.H. acknowledges support from a Marie Curie
International Reintegration Grant and the NWO Vidi grant. This work is
based in part on data products produced at the Canadian Astronomy Data
Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a
collaborative project of NRC and CNRS. This work is based on
observations obtained with MegaPrime/MegaCam, a joint project of CFHT
and CEA/DAPINA, at the Canada-France-Hawaii Telescope (CFHT) which is
operated by the National Research Council (NRC) of Canada, the Institut
National des Sciences l'Universe of the Centre National de la Recherche
Scientifique (CNRS) of France, and the University of Hawaii.
Observations reported here were obtained at the MMT Observatory, a joint
facility of the Smithsonian Institution and the University of Arizona.
This research has made use of the VizieR catalog access tool, CDS,
Strasbourg, France. This research has made use of the NASA/IPAC
Extragalactic Database (NED) which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. This research has made
use of 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
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 67
TC 5
Z9 5
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 68
DI 10.1088/0004-637X/753/1/68
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500068
ER
PT J
AU Jimenez-Serra, I
Zhang, Q
Viti, S
Martin-Pintado, J
de Wit, WJ
AF Jimenez-Serra, I.
Zhang, Q.
Viti, S.
Martin-Pintado, J.
de Wit, W. -J.
TI CHEMICAL SEGREGATION TOWARD MASSIVE HOT CORES: THE AFGL2591 STAR-FORMING
REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (AFGL2591); ISM: molecules; stars: formation
ID MOLECULAR LINE EMISSION; YOUNG STELLAR OBJECTS; PROTOSTELLAR ENVELOPES;
CONTINUUM EMISSION; SULFUR CHEMISTRY; AFGL-2591; EVOLUTION; GL-2591;
DUST; RADIATION
AB We present high angular resolution observations (0 ''.5 x 0 ''.3) carried out with the Submillimeter Array (SMA) toward the AFGL2591 high-mass star-forming region. Our SMA images reveal a clear chemical segregation within the AFGL2591 VLA 3 hot core, where different molecular species (Types I, II, and III) appear distributed in three concentric shells. This is the first time that such a chemical segregation is ever reported at linear scales <= 3000 AU within a hot core. While Type I species (H2S and (CS)-C-13) peak at the AFGL2591 VLA 3 protostar, Type II molecules (HC3N, OCS, SO, and SO2) show a double-peaked structure circumventing the continuum peak. Type III species, represented by CH3OH, form a ring-like structure surrounding the continuum emission. The excitation temperatures of SO2, HC3N, and CH3OH (185 +/- 11 K, 150 +/- 20 K, and 124 +/- 12 K, respectively) show a temperature gradient within the AFGL2591 VLA 3 envelope, consistent with previous observations and modeling of the source. By combining the H2S, SO2, and CH3OH images, representative of the three concentric shells, we find that the global kinematics of the molecular gas follow Keplerian-like rotation around a 40 M-circle dot star. The chemical segregation observed toward AFGL2591 VLA 3 is explained by the combination of molecular UV photodissociation and a high-temperature (similar to 1000 K) gas-phase chemistry within the low extinction innermost region in the AFGL2591 VLA 3 hot core.
C1 [Jimenez-Serra, I.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Viti, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Martin-Pintado, J.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain.
[de Wit, W. -J.] European So Observ, Santiago 19, Chile.
RP Jimenez-Serra, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ijimenez-serra@cfa.harvard.edu; qzhang@cfa.harvard.edu;
sv@star.ucl.ac.uk; jmartin@cab.inta-csic.es; wdewit@eso.org
RI Martin-Pintado, Jesus/H-6107-2015;
OI Martin-Pintado, Jesus/0000-0003-4561-3508; Zhang,
Qizhou/0000-0003-2384-6589
FU Smithsonian Astrophysical Observatory through a SMA fellowship; MICINN
[ESP2007-65812-C02-C01, AYA2010-21697-C05-01]; AstroMadrid [CAM
S2009/ESP-1496]
FX We acknowledge the constructive comments from a second referee which
helped to improve the paper. I.J.-S. acknowledges the Smithsonian
Astrophysical Observatory for the support provided through a SMA
fellowship. J.M.-P. and I.J.-S. have been partially funded by MICINN
grants ESP2007-65812-C02-C01, AYA2010-21697-C05-01 and AstroMadrid (CAM
S2009/ESP-1496).
NR 47
TC 20
Z9 20
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 34
DI 10.1088/0004-637X/753/1/34
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500034
ER
PT J
AU Kratter, KM
Perets, HB
AF Kratter, Kaitlin M.
Perets, Hagai B.
TI STAR HOPPERS: PLANET INSTABILITY AND CAPTURE IN EVOLVING BINARY SYSTEMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; planets and satellites: general; stars: AGB and
post-AGB; white dwarfs
ID SOLAR-TYPE STARS; WHITE-DWARFS; STELLAR EVOLUTION; GIANT PLANETS;
RESONANCE OVERLAP; 3-BODY PROBLEM; GREAT ESCAPE; MASS; ORBITS;
MULTIPLICITY
AB Many planets are observed in stellar binary systems, and their frequency may be comparable to that of planetary systems around single stars. Binary stellar evolution in such systems influences the dynamical evolution of the resident planets. Here, we study the evolution of a single planet orbiting one star in an evolving binary system. We find that stellar evolution can trigger dynamical instabilities that drive planets into chaotic orbits. This instability leads to planet-star collisions, exchange of the planet between the binary stars ("star hoppers"), and ejection of the planet from the system. The means by which planets can be recaptured is similar to the pull-down capture mechanism for irregular solar system satellites. Because planets often suffer close encounters with the primary on the asymptotic giant branch, captures during a collision with the stellar envelope are also possible for more massive planets. Such capture could populate the habitable zone around white dwarfs.
C1 [Kratter, Kaitlin M.; Perets, Hagai B.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
RP Kratter, KM (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
RI Perets, Hagai/K-9605-2015
OI Perets, Hagai/0000-0002-5004-199X
FU Institute for Theory and Computation through Harvard College Observatory
FX The authors thank Dimitri Veras, Andrew Youdin, and Smadar Naoz for
comments on an earlier draft of this manuscript, and Nick Moeckel, Matt
Holman, Fred Rasio, Dave Spiegel, and Jason Nordhaus for helpful
discussions. The authors thank the referee for helpful comments. K.M.K.
is supported by an Institute for Theory and Computation fellowship
through the Harvard College Observatory. H.B.P. is a BIKURA (FIRST) and
CfA prize fellow.
NR 49
TC 35
Z9 35
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 91
DI 10.1088/0004-637X/753/1/91
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500091
ER
PT J
AU Rich, JA
Torrey, P
Kewley, LJ
Dopita, MA
Rupke, DSN
AF Rich, J. A.
Torrey, P.
Kewley, L. J.
Dopita, M. A.
Rupke, D. S. N.
TI AN INTEGRAL FIELD STUDY OF ABUNDANCE GRADIENTS IN NEARBY LUMINOUS
INFRARED GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; galaxies: interactions; infrared: galaxies
ID MASS-METALLICITY RELATION; ACTIVE GALACTIC NUCLEI; STAR-FORMING
GALAXIES; DIGITAL SKY SURVEY; HIGH-REDSHIFT GALAXIES; H-II REGIONS;
INTERACTING GALAXIES; SPIRAL GALAXIES; DISK GALAXIES; OPTICAL
CLASSIFICATION
AB We present for the first time metallicity maps generated using data from the Wide Field Spectrograph on the ANU 2.3 m of 10 luminous infrared galaxies (LIRGs) and discuss the abundance gradients and distribution of metals in these systems. We have carried out optical integral field spectroscopy (IFS) of several LIRGs in various merger phases to investigate the merger process. In a major merger of two spiral galaxies with preexisting disk abundance gradients, the changing distribution of metals can be used as a tracer of gas flows in the merging system as low-metallicity gas is transported from the outskirts of each galaxy to their nuclei. We employ this fact to probe merger properties by using the emission lines in our IFS data to calculate the gas-phase metallicity in each system. We create abundance maps and subsequently derive a metallicity gradient from each map. We compare our measured gradients to merger stage as well as several possible tracers of merger progress and observed nuclear abundances. We discuss our work in the context of previous abundance gradient observations and compare our results to new galaxy merger models that trace metallicity gradient. Our results agree with the observed flattening of metallicity gradients as a merger progresses. We compare our results with new theoretical predictions that include chemical enrichment. Our data show remarkable agreement with these simulations.
C1 [Rich, J. A.; Kewley, L. J.; Dopita, M. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Torrey, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dopita, M. A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Dopita, M. A.] King Abdulaziz Univ, Fac Sci, Dept Astron, Jeddah, Saudi Arabia.
[Rupke, D. S. N.] Rhodes Coll, Dept Phys, Memphis, TN 38112 USA.
RP Rich, JA (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM jrich@ifa.hawaii.edu
RI Dopita, Michael/P-5413-2014; Faculty of, Sciences, KAU/E-7305-2017;
OI Dopita, Michael/0000-0003-0922-4986; Rich, Jeffrey/0000-0002-5807-5078;
Torrey, Paul/0000-0002-5653-0786
NR 99
TC 46
Z9 46
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 5
DI 10.1088/0004-637X/753/1/5
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500005
ER
PT J
AU Sliwa, K
Wilson, CD
Petitpas, GR
Armus, L
Juvela, M
Matsushita, S
Peck, AB
Yun, MS
AF Sliwa, Kazimierz
Wilson, Christine D.
Petitpas, Glen R.
Armus, Lee
Juvela, Mika
Matsushita, Satoki
Peck, Alison B.
Yun, Min S.
TI LUMINOUS INFRARED GALAXIES WITH THE SUBMILLIMETER ARRAY. III. THE DENSE
KILOPARSEC MOLECULAR CONCENTRATIONS OF Arp 299
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (Arp 299); galaxies: interactions; galaxies:
starburst; submillimeter: galaxies
ID STAR-FORMATION EFFICIENCY; STARBURST GALAXIES; HCO+ OBSERVATIONS; IRAS
GALAXIES; GAS; CLOUDS; MERGER; HCN; SPECTROSCOPY; ARP-299
AB We have used high-resolution (similar to 2 ''.3) observations of the local (D-L = 46 Mpc) luminous infrared galaxy Arp 299 to map out the physical properties of the molecular gas that provides the fuel for its extreme star formation activity. The (CO)-C-12 J = 3-2, (CO)-C-12 J = 2-1, and (CO)-C-13 J = 2-1 lines were observed with the Submillimeter Array, and the short spacings of the (CO)-C-12 J = 2-1 and J = 3-2 observations have been recovered using the James Clerk Maxwell Telescope single dish observations. We use the radiative transfer code RADEX to estimate the physical properties (density, column density, and temperature) of the different regions in this system. The RADEX solutions of the two galaxy nuclei, IC 694 and NGC 3690, are consistent with a wide range of gas components, from warm moderately dense gas with T-kin > 30 K and n(H-2) similar to 0.3-3 x 10(3) cm(-3) to cold dense gas with T-kin similar to 10-30 K and n(H-2) > 3 x 10(3) cm(-3). The overlap region is shown to have a better constrained solution with T-kin similar to 10-50 K and n(H-2) similar to 1-30 x 10(3) cm(-3). We estimate the gas masses and star formation rates of each region in order to derive molecular gas depletion times. The depletion times of all regions (20-50 Myr) are found to be about two orders of magnitude lower than those of normal spiral galaxies. This rapid depletion time can probably be explained by a high fraction of dense gas on kiloparsec scales in Arp 299. We estimate the CO-to-H-2 factor, alpha(co) to be 0.4 +/- 0.3(3 x 10(-4)/x(CO)) M-circle dot (K km s(-1) pc(2))(-1) for the overlap region. This value agrees well with values determined previously for more advanced merger systems.
C1 [Sliwa, Kazimierz; Wilson, Christine D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
[Petitpas, Glen R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Armus, Lee] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Juvela, Mika] Univ Helsinki Observ, Helsinki, Finland.
[Matsushita, Satoki] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Peck, Alison B.] Joint ALMA Off, Santiago 7550108, Chile.
[Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
RP Sliwa, K (reprint author), McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
EM sliwak@mcmaster.ca; wilson@physics.mcmaster.ca;
gpetitpa@cfa.harvard.edu; lee@ipac.caltech.edu; mika.juvela@helsinki.fi;
satoki@asiaa.sinica.edu.tw; apeck@alma.cl; myun@astro.umass.edu
OI Juvela, Mika/0000-0002-5809-4834
FU Smithsonian Institution; Academia Sinica; Natural Science and
Engineering Research Council of Canada (NSERC)
FX The Submillimeter Array is a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics and is funded by the Smithsonian Institution and the
Academia Sinica. The James Clerk Maxwell Telescope is operated by The
Joint Astronomy Centre on behalf of the Particle Physics and Astronomy
Research Council of the United Kingdom, the Netherlands Organisation for
Scientific Research, and the National Research Council of Canada. We
thank the anonymous referee for a very useful referee report and S.
Aalto for giving us the OVRO CO J = 1-0 map. C.D.W. acknowledges support
by the Natural Science and Engineering Research Council of Canada
(NSERC).
NR 42
TC 15
Z9 15
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 46
DI 10.1088/0004-637X/753/1/46
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500046
ER
PT J
AU Su, M
Finkbeiner, DP
AF Su, Meng
Finkbeiner, Douglas P.
TI EVIDENCE FOR GAMMA-RAY JETS IN THE MILKY WAY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: starburst; gamma rays: galaxies; ISM: jets
and outflows
ID EXTRAGALACTIC RADIO-SOURCES; X-RAY; EMISSION; ENERGY; MISSION; MODELS;
GALAXY; WIND; MAPS; STAR
AB Although accretion onto supermassive black holes in other galaxies is seen to produce powerful jets in X-ray and radio, no convincing detection has ever been made of a kpc-scale jet in the Milky Way. The recently discovered pair of 10 kpc tall gamma-ray bubbles in our Galaxy may be signs of earlier jet activity from the central black hole. In this paper, we identify a gamma-ray cocoon feature in the southern bubble, a jet-like feature along the cocoon's axis of symmetry, and another directly opposite the Galactic center in the north. Both the cocoon and jet-like feature have a hard spectrum with spectral index similar to-2 from 1 to 100 GeV, with a cocoon total luminosity of (5.5 +/- 0.45) x 10(35) and luminosity of the jet-like feature of (1.8 +/- 0.35) x 10(35) erg s(-1) at 1-100 GeV. If confirmed, these jets are the first resolved gamma-ray jets ever seen.
C1 [Su, Meng; Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
RP Su, M (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
EM mengsu@cfa.harvard.edu
RI Su, Meng/J-4211-2013
FU NASA Fermi Guest Investigator Program
FX It is a pleasure to acknowledge helpful conversations with Aneta
Siemiginowska, Martin Elvis, Feng Yuan, and Roman Shcherbakov. We
acknowledge the use of public data from the Fermi data archive at
http://fermi.gsfc.nasa.gov/ssc/. M.S. and D.P.F. are partially supported
by the NASA Fermi Guest Investigator Program. This research made use of
the NASA Astrophysics Data System (ADS) and the IDL Astronomy User's
Library at Goddard (available at http://idlastro.gsfc.nasa.gov).
NR 33
TC 38
Z9 39
U1 4
U2 15
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 61
DI 10.1088/0004-637X/753/1/61
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500061
ER
PT J
AU Temim, T
Sonneborn, G
Dwek, E
Arendt, RG
Gehrz, RD
Slane, P
Roellig, TL
AF Temim, Tea
Sonneborn, George
Dwek, Eli
Arendt, Richard G.
Gehrz, Robert D.
Slane, Patrick
Roellig, Thomas L.
TI PROPERTIES AND SPATIAL DISTRIBUTION OF DUST EMISSION IN THE CRAB NEBULA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; ISM: individual objects (Crab Nebula);
ISM: supernova remnants; pulsars: individual (PSR B0531+21)
ID SPITZER-SPACE-TELESCOPE; SUPERNOVA REMNANT; INTERSTELLAR DUST;
PHOTOELECTRIC-EMISSION; INFRARED SPECTROGRAPH; EARLY UNIVERSE;
HIGH-REDSHIFT; CASSIOPEIA; SPECTROSCOPY; EXTINCTION
AB Recent infrared (IR) observations of freshly formed dust in supernova remnants have yielded significantly lower dust masses than predicted by theoretical models and measured from high-redshift observations. The Crab Nebula's pulsar wind is thought to be sweeping up freshly formed supernova (SN) dust along with the ejected gas. The evidence for this dust was found in the form of an IR excess in the integrated spectrum of the Crab and in extinction against the synchrotron nebula that revealed the presence of dust in the filament cores. We present the first spatially resolved emission spectra of dust in the Crab Nebula acquired with the Infrared Spectrograph on board the Spitzer Space Telescope. The IR spectra are dominated by synchrotron emission and show forbidden line emission from S, Si, Ne, Ar, O, Fe, and Ni. We derived a synchrotron spectral map from the 3.6 and 4.5 mu m images, and subtracted this contribution from our data to produce a map of the residual continuum emission from dust. The dust emission appears to be concentrated along the ejecta filaments and is well described by an amorphous carbon or silicate grain compositions. We find a dust temperature of 55 +/- 4 K for silicates and 60 +/- 7 K for carbon grains. The total estimated dust mass is (1.2-12) x 10(-3) M-circle dot, well below the theoretical dust yield predicted for a core-collapse supernova. Our grain heating model implies that the dust grain radii are relatively small, unlike what is expected for dust grains formed in a Type IIP SN.
C1 [Temim, Tea; Sonneborn, George; Dwek, Eli; Arendt, Richard G.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Temim, Tea] Oak Ridge Associated Univ ORAU, Oak Ridge, TN 37831 USA.
[Arendt, Richard G.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
[Gehrz, Robert D.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Roellig, Thomas L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM tea.temim@nasa.gov
OI Arendt, Richard/0000-0001-8403-8548; Temim, Tea/0000-0001-7380-3144
FU NASA; U.S. Air Force
FX This work is partly based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. R.D.G.
was supported by NASA and the U.S. Air Force.
NR 54
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 72
DI 10.1088/0004-637X/753/1/72
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500072
ER
PT J
AU Wood, BE
Laming, JM
Karovska, M
AF Wood, Brian E.
Laming, J. Martin
Karovska, Margarita
TI THE CORONAL ABUNDANCE ANOMALIES OF M DWARFS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: coronae; stars: individual (GJ 338); stars: late-type; X-rays:
stars
ID X-RAY SPECTROSCOPY; INTERMEDIATE-ACTIVITY LEVELS; XMM-NEWTON VIEW;
NON-WKB MODELS; ALPHA-CENTAURI; STELLAR CORONAE; BINARY-SYSTEM;
SOLAR-WIND; STARS; CHANDRA
AB We analyze Chandra X-ray spectra of the M0 V+M0 V binary GJ 338. As quantified by X-ray surface flux, these are the most inactive M dwarfs ever observed with X-ray grating spectroscopy. We focus on measuring coronal abundances, in particular searching for evidence of abundance anomalies related to first ionization potential (FIP). In the solar corona and wind, low-FIP elements are overabundant, which is the so-called FIP effect. For other stars, particularly very active ones, an "inverse FIP effect" is often observed, with low-FIP elements being underabundant. For both members of the GJ 338 binary, we find evidence for a modest inverse FIP effect, consistent with expectations from a previously reported correlation between spectral type and FIP bias. This amounts to strong evidence that all M dwarfs should exhibit the inverse FIP effect phenomenon, not just the active ones. We take the first step toward modeling the inverse FIP phenomenon in M dwarfs, building on past work that has demonstrated that MHD waves coursing through coronal loops can lead to a ponderomotive force that fractionates elements in a manner consistent with the FIP effect. We demonstrate that in certain circumstances this model can also lead to an inverse FIP effect, pointing the way to more detailed modeling of M dwarf coronal abundances in the future.
C1 [Wood, Brian E.; Laming, J. Martin] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Karovska, Margarita] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Wood, BE (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM brian.wood@nrl.navy.mil
FU NASA through ATP [NNH11AQ23I, GO1-12012Z]; NASA [NAS8-03060]
FX We thank Brad Wargelin and Vinay Kashyap for their assistance in
identifying the source of the asymmetry in the GJ 338A image. Support
for this work was provided by NASA through ATP award NNH11AQ23I and
Chandra Award Number GO1-12012Z issued by the Chandra X-ray Center
(CXC). M.K. is a member of CXC, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of NASA under contract
NAS8-03060.
NR 47
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2012
VL 753
IS 1
AR 76
DI 10.1088/0004-637X/753/1/76
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963OV
UT WOS:000305632500076
ER
PT J
AU Bleem, LE
van Engelen, A
Holder, GP
Aird, KA
Armstrong, R
Ashby, MLN
Becker, MR
Benson, BA
Biesiadzinski, T
Brodwin, M
Busha, MT
Carlstrom, JE
Chang, CL
Cho, HM
Crawford, TM
Crites, AT
de Haan, T
Desai, S
Dobbs, MA
Dore, O
Dudley, J
Geach, JE
George, EM
Gladders, MD
Gonzalez, AH
Halverson, NW
Harrington, N
High, FW
Holden, BP
Holzapfel, WL
Hoover, S
Hrubes, JD
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Marrone, DP
Martinez-Manso, J
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Natoli, T
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruhl, JE
Saliwanchik, BR
Sayre, JT
Schaffer, KK
Shaw, L
Shirokoff, E
Spieler, HG
Stalder, B
Stanford, SA
Staniszewski, Z
Stark, AA
Stern, D
Story, K
Vallinotto, A
Vanderlinde, K
Vieira, JD
Wechsler, RH
Williamson, R
Zahn, O
AF Bleem, L. E.
van Engelen, A.
Holder, G. P.
Aird, K. A.
Armstrong, R.
Ashby, M. L. N.
Becker, M. R.
Benson, B. A.
Biesiadzinski, T.
Brodwin, M.
Busha, M. T.
Carlstrom, J. E.
Chang, C. L.
Cho, H. M.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Desai, S.
Dobbs, M. A.
Dore, O.
Dudley, J.
Geach, J. E.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Halverson, N. W.
Harrington, N.
High, F. W.
Holden, B. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Marrone, D. P.
Martinez-Manso, J.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Natoli, T.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruhl, J. E.
Saliwanchik, B. R.
Sayre, J. T.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Spieler, H. G.
Stalder, B.
Stanford, S. A.
Staniszewski, Z.
Stark, A. A.
Stern, D.
Story, K.
Vallinotto, A.
Vanderlinde, K.
Vieira, J. D.
Wechsler, R. H.
Williamson, R.
Zahn, O.
TI A MEASUREMENT OF THE CORRELATION OF GALAXY SURVEYS WITH CMB LENSING
CONVERGENCE MAPS FROM THE SOUTH POLE TELESCOPE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmic background radiation; galaxies: structure
ID BACKGROUND POWER SPECTRUM; PHOTOMETRIC REDSHIFTS; SKY SURVEY; FIELD;
ANISOTROPIES; SAMPLE
AB We compare cosmic microwave background lensing convergence maps derived from South Pole Telescope (SPT) data with galaxy survey data from the Blanco Cosmology Survey, WISE, and a new large Spitzer/IRAC field designed to overlap with the SPT survey. Using optical and infrared catalogs covering between 17 and 68 deg(2) of sky, we detect a correlation between the SPT convergence maps and each of the galaxy density maps at >4 sigma, with zero correlation robustly ruled out in all cases. The amplitude and shape of the cross-power spectra are in good agreement with theoretical expectations and the measured galaxy bias is consistent with previous work. The detections reported here utilize a small fraction of the full 2500 deg(2) SPT survey data and serve as both a proof of principle of the technique and an illustration of the potential of this emerging cosmological probe.
C1 [Bleem, L. E.; Becker, M. R.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Bleem, L. E.; Becker, M. R.; Carlstrom, J. E.; Hoover, S.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[van Engelen, A.; Holder, G. P.; de Haan, T.; Dobbs, M. A.; Dudley, J.; Geach, J. E.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Armstrong, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Ashby, M. L. N.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Biesiadzinski, T.; McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Busha, M. T.] Univ Zurich, Inst Theoret Phys, CH-8001 Zurich, Switzerland.
[Busha, M. T.; Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Desai, S.; Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Desai, S.; Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Dore, O.; Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Dore, O.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.; Martinez-Manso, J.] 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.
[Holden, B. P.] Univ Calif Santa Cruz, SantaCruz UCO Lick Observ, Santa Cruz, CA 95065 USA.
[Joy, M.] NASA Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
[Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Vallinotto, A.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Wechsler, R. H.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
RP Bleem, LE (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Marrone,
Daniel/0000-0002-2367-1080; Becker, Matthew/0000-0001-7774-2246; Aird,
Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169;
Stark, Antony/0000-0002-2718-9996
FU Kavli Foundation; Moore Foundation; NSERC; CRC program; CIfAR; NASA
Hubble Fellowship [HF-51275.01]; KICP Fellowship; Alfred P. Sloan
Research Fellowship; DOE [DE-AC02-76SF00515, DE-AC52-06NA25396
(LA-UR-12-20137)]; BCCP fellowship; NASA; [ANT-0638937];
[ANT-0130612]; [PHY-0114422]; [AST-1009012]; [AST-1009811]
FX The SPT is supported by grants ANT-0638937 and ANT-0130612, with partial
support provided by PHY-0114422, the Kavli Foundation, and the Moore
Foundation. Work at McGill is supported by NSERC, the CRC program, and
CIfAR, and at Harvard by grant AST-1009012. R. Keisler acknowledges NASA
Hubble Fellowship grant HF-51275.01, B. A. Benson a KICP Fellowship, M.
Dobbs an Alfred P. Sloan Research Fellowship, L. Shaw grant AST-1009811,
R. Wechsler DOE contract DE-AC02-76SF00515, A. Vallinotto DOE contract
DE-AC52-06NA25396 (LA-UR-12-20137), and O. Zahn a BCCP fellowship. This
publication uses data from the Wide-field Infrared Survey Explorer, a
joint project of UCLA, and JPL/Caltech, funded by NASA, and uses data
provided by NOAO PI: 2005B-0043, distributed by the NOAO Science
Archive. NOAO is operated by AURA under cooperative agreement with the
NSF. This work is based in part on observations made with the Spitzer
Space Telescope, operated by JPL, Caltech, under a contract with NASA.
NR 42
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 1
PY 2012
VL 753
IS 1
AR L9
DI 10.1088/2041-8205/753/1/L9
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963QK
UT WOS:000305637900009
ER
PT J
AU Cohen, O
Glocer, A
AF Cohen, O.
Glocer, A.
TI AMBIPOLAR ELECTRIC FIELD, PHOTOELECTRONS, AND THEIR ROLE IN ATMOSPHERIC
ESCAPE FROM HOT JUPITERS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres
ID STELLAR X-RAY; POLAR WIND; GIANT PLANETS; MASS-LOSS; EXOPLANET
HD-209458B; EVAPORATION; HYDROGEN; AERONOMY
AB Atmospheric mass loss from Hot Jupiters can be large due to the close proximity of these planets to their host star and the strong radiation the planetary atmosphere receives. On Earth, a major contribution to the acceleration of atmospheric ions comes from the vertical separation of ions and electrons, and the generation of the ambipolar electric field. This process, known as the "polar wind," is responsible for the transport of ionospheric constituents to Earth's magnetosphere, where they are well observed. The polar wind can also be enhanced by a relatively small fraction of super-thermal electrons (photoelectrons) generated by photoionization. We formulate a simplified calculation of the effect of the ambipolar electric field and the photoelectrons on the ion scale height in a generalized manner. We find that the ion scale height can be increased by a factor of 2-15 due to the polar wind effects. We also estimate a lower limit of an order of magnitude increase of the ion density and the atmospheric mass-loss rate when polar wind effects are included.
C1 [Cohen, O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Glocer, A.] NASA, GSFC, Greenbelt, MD 20771 USA.
RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Glocer, Alex/C-9512-2012; feggans, john/F-5370-2012;
OI Glocer, Alex/0000-0001-9843-9094; Cohen, Ofer/0000-0003-3721-0215
FU SI Grand Challenges grant [40510254HH0022]
FX We thank an unknown referee for her/his review report and Jeremy Drake
for his help in preparing this manuscript. O.C. is supported by SI Grand
Challenges grant No. 40510254HH0022.
NR 35
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 1
PY 2012
VL 753
IS 1
AR L4
DI 10.1088/2041-8205/753/1/L4
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963QK
UT WOS:000305637900004
ER
PT J
AU Foley, RJ
Kromer, M
Marion, GH
Pignata, G
Stritzinger, MD
Taubenberger, S
Challis, P
Filippenko, AV
Folatelli, G
Hillebrandt, W
Hsiao, EY
Kirshner, RP
Li, W
Morrell, NI
Roepke, FK
Ciaraldi-Schoolmann, F
Seitenzahl, IR
Silverman, JM
Simcoe, RA
Berta, ZK
Ivarsen, KM
Newton, ER
Nysewander, MC
Reichart, DE
AF Foley, Ryan J.
Kromer, Markus
Marion, G. Howie
Pignata, Giuliano
Stritzinger, Maximilian D.
Taubenberger, Stefan
Challis, Peter
Filippenko, Alexei V.
Folatelli, Gaston
Hillebrandt, Wolfgang
Hsiao, Eric Y.
Kirshner, Robert P.
Li, Weidong
Morrell, Nidia I.
Roepke, Friedrich K.
Ciaraldi-Schoolmann, Franco
Seitenzahl, Ivo R.
Silverman, Jeffrey M.
Simcoe, Robert A.
Berta, Zachory K.
Ivarsen, Kevin M.
Newton, Elisabeth R.
Nysewander, Melissa C.
Reichart, Daniel E.
TI THE FIRST MAXIMUM-LIGHT ULTRAVIOLET THROUGH NEAR-INFRARED SPECTRUM OF A
TYPE Ia SUPERNOVA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE supernovae: general; supernovae: individual (SN 2011iv)
ID HUBBLE-SPACE-TELESCOPE; EJECTA VELOCITY; HOST GALAXIES; REDSHIFT;
CURVES; LUMINOSITY; MODELS; SPECTROSCOPY; BRIGHTNESS; DISTANCES
AB We present the first maximum-light ultraviolet (UV) through near-infrared (NIR) Type Ia supernova (SN Ia) spectrum. This spectrum of SN 2011iv was obtained nearly simultaneously by the Hubble Space Telescope at UV/optical wavelengths and the Magellan Baade telescope at NIR wavelengths. These data provide the opportunity to examine the entire maximum-light SN Ia spectral energy distribution. Since the UV region of an SN Ia spectrum is extremely sensitive to the composition of the outer layers of the explosion, which are transparent at longer wavelengths, this unprecedented spectrum can provide strong constraints on the composition of the SN ejecta, and similarly the SN explosion and progenitor system. SN 2011iv is spectroscopically normal, but has a relatively fast decline (Delta m(15)(B) = 1.69 +/- 0.05 mag). We compare SN 2011iv to other SNe Ia with UV spectra near maximum light and examine trends between UV spectral properties, light-curve shape, and ejecta velocity. We tentatively find that SNe with similar light-curve shapes but different ejecta velocities have similar UV spectra, while those with similar ejecta velocities but different light-curve shapes have very different UV spectra. Through a comparison with explosion models, we find that both a solar-metallicity W7 and a zero-metallicity delayed-detonation model provide a reasonable fit to the spectrum of SN 2011iv from the UV to the NIR.
C1 [Foley, Ryan J.; Marion, G. Howie; Challis, Peter; Berta, Zachory K.; Newton, Elisabeth R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kromer, Markus; Taubenberger, Stefan; Hillebrandt, Wolfgang; Roepke, Friedrich K.; Ciaraldi-Schoolmann, Franco; Seitenzahl, Ivo R.] Max Planck Inst Astrophys, D-85748 Munich, Germany.
[Pignata, Giuliano] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile.
[Stritzinger, Maximilian D.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Stritzinger, Maximilian D.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, S-10691 Stockholm, Sweden.
[Filippenko, Alexei V.; Li, Weidong; Silverman, Jeffrey M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Folatelli, Gaston] Univ Tokyo, Todai Inst Adv Study, Kavli IPMU, WPI, Kashiwa, Chiba 2778583, Japan.
[Hsiao, Eric Y.; Morrell, Nidia I.] Las Campanas Observ, Carnegie Observ, La Serena, Chile.
[Roepke, Friedrich K.; Seitenzahl, Ivo R.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Simcoe, Robert A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Ivarsen, Kevin M.; Nysewander, Melissa C.; Reichart, Daniel E.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rfoley@cfa.harvard.edu
OI Ropke, Friedrich/0000-0002-4460-0097; Berta-Thompson,
Zachory/0000-0002-3321-4924; Seitenzahl, Ivo/0000-0002-5044-2988;
Newton, Elisabeth/0000-0003-4150-841X; stritzinger,
maximilian/0000-0002-5571-1833
FU Clay Fellowship; NSF; TABASGO Foundation; NASA/HST [GO-12592]; Proyecto
FONDECYT [11090421]; proyecto regular UNAB [DI-28-11/R]; Millennium
Center for Supernova Science [ICM P10-064-F]; DFG (Transregional
Collaborative Research Center) [TRR 33]; JSC, Julich, Germany [PRACE042,
HMU14/20]
FX This research was supported by a Clay Fellowship (R.J.F.), an NSF
Graduate Research Fellowship (E.R.N.), the TABASGO Foundation (A. V.
F.), and NASA/HST grant GO-12592. G. P. acknowledges support by the
Proyecto FONDECYT 11090421, proyecto regular UNAB DI-28-11/R, and by the
grant ICM P10-064-F (Millennium Center for Supernova Science), with
input from the "Fondo de Innovacipn para la Competitividad, del
Ministerio de Economia, Fomento y Turismo de Chile." S. T. is supported
by the DFG (Transregional Collaborative Research Center TRR 33). The
simulations were performed at JSC, Julich, Germany (grants PRACE042,
HMU14/20).
NR 50
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 1
PY 2012
VL 753
IS 1
AR L5
DI 10.1088/2041-8205/753/1/L5
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 963QK
UT WOS:000305637900005
ER
PT J
AU Bernhardt, CE
Horton, BP
Stanley, JD
AF Bernhardt, Christopher E.
Horton, Benjamin P.
Stanley, Jean-Daniel
TI Nile Delta vegetation response to Holocene climate variability
SO GEOLOGY
LA English
DT Article
ID CULTURAL RESPONSES; EGYPT; ENVIRONMENT; INSOLATION; EVOLUTION; AFRICA;
SEA
AB A 7000 yr palynologic record from Burullus Lagoon, Nile Delta, Egypt, is assessed to investigate changes in terrestrial vegetation in response to Nile flow. Previous studies in this region have shown that sea-level rise in the early to mid-Holocene, and markedly increased human land use during the past several centuries, altered vegetation in and around the lagoon. The pollen record from this study documents changes in delta vegetation that likely reflect variations in Nile flow. We suggest that Cyperaceae pollen is a sensitive marker of precipitation over the Nile headwaters and the resultant Nile flow. Decreases in Cyperaceae pollen, interpreted as a marker for diminished Nile flow, as well as the increase in relative abundance of microscopic charcoal, occurred at ca. 6000-5500, ca. 5000, ca. 4200, and ca. 3000 cal. yr B.P. (calibrated years before present). These correspond to extreme regional and global aridity events associated with a more southerly mean position of the Intertropical Convergence Zone. These changes, also recorded by other proxy studies, indicate that several marked regional drought events affected the Nile Delta region and impacted ancient Egyptian and Middle Eastern civilizations.
C1 [Bernhardt, Christopher E.] US Geol Survey, Natl Ctr 926A, Reston, VA 20192 USA.
[Bernhardt, Christopher E.; Horton, Benjamin P.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA.
[Stanley, Jean-Daniel] Smithsonian Inst, Dept Paleobiol, Geoarchaeol Program, Washington, DC 20013 USA.
RP Bernhardt, CE (reprint author), US Geol Survey, Natl Ctr 926A, Reston, VA 20192 USA.
EM cbernhardt@usgs.gov
FU University of Pennsylvania
FX The first author thanks the University of Pennsylvania for financial
support and the U.S. Geological Survey, Reston, Virginia, for laboratory
support for palynological analysis. The Smithsonian's Delta-Global
Change Program in Egypt collected and provided access to core samples at
the National Museum of Natural History, Washington, D.C. Thomas Sheehan
and Bryan Landacre assisted in processing samples for pollen. D.A.
Willard, T. Cronin, and three anonymous reviewers provided insightful
reviews that significantly improved the manuscript.
NR 38
TC 32
Z9 32
U1 3
U2 23
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD JUL
PY 2012
VL 40
IS 7
BP 615
EP 618
DI 10.1130/G33012.1
PG 4
WC Geology
SC Geology
GA 966DX
UT WOS:000305818900010
ER
PT J
AU Manchester, SR
Herrera, F
Fourtanier, E
Barron, J
Martinez, JN
AF Manchester, Steven R.
Herrera, Fabiany
Fourtanier, Elisabeth
Barron, John
Martinez, Jean-Noel
TI Oligocene Age of the Classic Belen Fruit and Seed Assemblage of North
Coastal Peru based on Diatom Biostratigraphy
SO JOURNAL OF GEOLOGY
LA English
DT Article
ID SOUTH-AMERICA; PHYTOGEOGRAPHY; ORIGINS; HISTORY; BASIN
AB The Belen flora, in north coastal Peru, is the most diverse fruit and seed assemblage yet known from the Paleogene of South America. Little original paleobotanical work has been performed on this assemblage since the pioneering treatments published by E. W. Berry in the 1920s, and the precise age has not been determined. Nevertheless, the flora has been regarded as a focal point in understanding the vegetational, orogenic, and climatic history of northern South America, and in recent literature it has been assumed to be early Eocene. In order to tighten this age assignment, which has varied from early Eocene to early Oligocene in the opinions of different authors, we revisited the Belen site, measured the stratigraphic section, and processed the fruit-and seed-containing sediment for age-diagnostic microfossils. Although pollen and foraminifera were not recovered, the sediment is rich in diatoms. The diatom assemblage includes Lisitzinia ornata and Rocella vigilans, among others, indicating a latest early Oligocene age (similar to 30-28.5 Ma) for these deeper marine sediments, which we infer to have been subsequently reworked into the Belen environment. We also reevaluate the botanical identifications, which are based on the original museum specimens supplemented by more recently collected specimens. The Belen flora provides a window into extinct forests in South America that were present before the rising of the Andes in western Peru.
C1 [Manchester, Steven R.; Herrera, Fabiany] Univ Florida, Florida Museum Nat Hist, Dept Biol, Gainesville, FL 32611 USA.
[Herrera, Fabiany] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Fourtanier, Elisabeth] Calif Acad Sci, San Francisco, CA 94118 USA.
[Barron, John] US Geol Survey, Menlo Pk, CA 94025 USA.
[Martinez, Jean-Noel] Univ Nacl Piura, Inst Paleontol, Piura, Peru.
RP Manchester, SR (reprint author), Univ Florida, Florida Museum Nat Hist, Dept Biol, Gainesville, FL 32611 USA.
EM steven@flmnh.ufl.edu
FU National Science Foundation [BSR-0743474]
FX Fieldwork and analyses were supported by National Science Foundation
grant BSR-0743474 (to S. R. Manchester). We thank F. Navarro for
assistance in field reconnaissance and collection. Helpful review
comments were provided by C. Jaramillo, T. Lott, and an anonymous
reviewer.
NR 30
TC 3
Z9 3
U1 0
U2 5
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0022-1376
J9 J GEOL
JI J. Geol.
PD JUL
PY 2012
VL 120
IS 4
BP 467
EP 476
DI 10.1086/665797
PG 10
WC Geology
SC Geology
GA 965FL
UT WOS:000305752500007
ER
PT J
AU Spitler, LR
Romanowsky, AJ
Diemand, J
Strader, J
Forbes, DA
Moore, B
Brodie, JP
AF Spitler, Lee R.
Romanowsky, Aaron J.
Diemand, Juerg
Strader, Jay
Forbes, Duncan A.
Moore, Ben
Brodie, Jean P.
TI Evidence for inhomogeneous reionization in the local Universe from
metal-poor globular cluster systems
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE galaxies: haloes; galaxies: kinematics and dynamics; galaxies: star
clusters: general; dark ages; reionization; first stars
ID DARK-MATTER HALO; STAR-FORMING GALAXIES; HIGH-REDSHIFT GALAXIES;
LY-ALPHA EMITTERS; DWARF COOLING SEQUENCE; HUBBLE-SPACE-TELESCOPE;
ULTRA-DEEP-FIELD; ELLIPTIC GALAXIES; STELLAR POPULATIONS; COLOR
DISTRIBUTIONS
AB Exploiting a fundamental characteristic of galaxy assembly in the ? cold dark matter paradigm, the observed spatial biasing and kinematics of metal-poor globular star clusters are used to constrain the local reionization epoch around individual galaxies. Selecting three galaxies located in different environments, the first attempt at constraining the environmental propagation of reionization in the local Universe is carried out. The joint constraint from the three galaxies () agrees remarkably well with the latest Wilkinson Microwave Anisotropy Probe constraint on zreion for a simple instantaneous reionization model. More importantly, the range of zreion values found here is consistent with the global range of zreion estimates from other observations. We furthermore find a 1.7s indication that reionization completed in low-density environments before the intergalactic medium in high-density environments was reionized. This is consistent with certain theoretical models that predict that reionization was globally prolonged in duration, with neutral hydrogen pockets surviving in high-density environments, even after the surrounding regions were reionized. More generally, this work provides a useful constraint on the formation history of galaxy stellar haloes.
C1 [Spitler, Lee R.; Forbes, Duncan A.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Romanowsky, Aaron J.; Brodie, Jean P.] Univ Calif Observ, Santa Cruz, CA 95064 USA.
[Diemand, Juerg; Moore, Ben] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland.
[Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Spitler, LR (reprint author), Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
EM lspitler@astro.swin.edu.au
RI Spitler, Lee/A-9867-2013; Diemand, Juerg/G-9448-2011
OI Spitler, Lee/0000-0001-5185-9876;
FU ARC [DP0770233, DP1094370]; National Science Foundation [AST-0808099,
AST-0909237, AST-1109878]; Gemini programme [GN-2006B-C-18]; W.M. Keck
Foundation
FX We want to acknowledge the useful comments provided by the anonymous
reviewer. We also thank Chris Blake for assistance with the cosmological
derivations and Anna Sippel for help with the initial Subaru reductions.
LRS was supported by the ARC Discovery Programme grants DP0770233 and
DP1094370. This work was supported by the National Science Foundation
through grants AST-0808099, AST-0909237 and AST-1109878. DAF thanks the
ARC Discovery Programme for support. This paper was based in part on
data collected at Subaru Telescope, which is operated by the National
Astronomical Observatory of Japan. Some of the Subaru data were acquired
with the time-swap Gemini programme GN-2006B-C-18. Some of the data
presented herein were obtained at the W. M. Keck Observatory, which is
operated as a scientific partnership among the California Institute of
Technology, the University of California and the National Aeronautics
and Space Administration. The observatory was made possible by the
generous financial support of the W.M. Keck Foundation. Observations
reported here were obtained at the MMT Observatory, a joint facility of
the Smithsonian Institution and the University of Arizona.
NR 133
TC 13
Z9 13
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 423
IS 3
BP 2177
EP 2189
DI 10.1111/j.1365-2966.2012.21029.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961NA
UT WOS:000305470100015
ER
PT J
AU Pan, T
Loeb, A
Kasen, D
AF Pan, Tony
Loeb, Abraham
Kasen, Daniel
TI Pair-instability supernovae via collision runaway in young dense star
clusters
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: general; galaxies: star clusters: general
ID WOLF-RAYET STARS; MASS-LOSS RATES; M-CIRCLE-DOT; POPULATION-III;
LUMINOSITY FUNCTION; BLACK-HOLES; SPIRAL GALAXIES; LOW-METALLICITY;
CORE-COLLAPSE; LIGHT CURVES
AB Stars with helium cores between similar to 64 and 133 M? are theoretically predicted to die as pair-instability supernovae. This requires very massive progenitors, which are theoretically prohibited for Pop II/I stars within the Galactic stellar mass limit due to mass-loss via line-driven winds. However, the runaway collision of stars in a dense, young star cluster could create a merged star with sufficient mass to end its life as a pair-instability supernova, even with enhanced mass-loss at non-zero metallicity. We show that the predicted rate from this mechanism is consistent with the inferred volumetric rate of roughly similar to 2 x 10(-9) Mpc-3 yr-1 of the two observed pair-instability supernovae, SN 2007bi and PTF 10nmn, neither of which has metal-free host galaxies. Contrary to prior literature, only pair-instability supernovae at low redshifts z < 2 will be observable with the Large Synoptic Survey Telescope. We estimate that the telescope will observe similar to 102 such events per year that originate from the collisional runaway mergers in clusters.
C1 [Pan, Tony; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Kasen, Daniel] Lawrence Berkeley Natl Lab, Div Nucl Sci, Berkeley, CA 94708 USA.
[Kasen, Daniel] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Pan, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM span@physics.harvard.edu
FU Hertz Foundation; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A];
Office of Energy Research, Office of High Energy and Nuclear Physics,
Divisions of Nuclear Physics, of the U.S. Department of Energy
[DE-AC02-05CH11231]; NSF Astronomy and Astrophysics grant
[NSF-AST-1109896]; DOE SciDAC Program [DE-FC02-06ER41438]
FX We thank Charlie Conroy for helpful comments. TP was supported by the
Hertz Foundation. This work was supported in part by NSF grant
AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. DK was supported
in part by the Director, Office of Energy Research, Office of High
Energy and Nuclear Physics, Divisions of Nuclear Physics, of the U.S.
Department of Energy under Contract No. DE-AC02-05CH11231, and by an NSF
Astronomy and Astrophysics grant NSF-AST-1109896. This research has been
supported by the DOE SciDAC Program (DE-FC02-06ER41438). We are grateful
for computer time provided by ORNL through an INCITE award and by NERSC.
NR 60
TC 21
Z9 21
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 423
IS 3
BP 2203
EP 2208
DI 10.1111/j.1365-2966.2012.21030.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961NA
UT WOS:000305470100017
ER
PT J
AU Daly, RA
Sprinkle, TB
O'Dea, CP
Kharb, P
Baum, SA
AF Daly, Ruth. A.
Sprinkle, Trevor B.
O'Dea, Christopher P.
Kharb, Preeti
Baum, Stefi A.
TI The relationship between beam power and radio power for classical double
radio sources
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE black hole physics; galaxies: active
ID X-RAY; BLACK-HOLES; JET POWER; GALAXIES; CLUSTERS; REDSHIFT; SAMPLE;
MODEL; QUASARS; LOBES
AB Beam power is a fundamental parameter that describes, in part, the state of a supermassive black hole system. Determining the beam powers of powerful classical double radio sources requires substantial observing time, so it would be useful to determine the relationship between beam power and radio power so that radio power could be used as a proxy for beam power. A sample of 31 powerful classical double radio sources with previously determined beam and radio powers is studied; the sources have redshifts between about 0.056 and 1.8. It is found that the relationship between beam power, Lj, and radio power, P, is well described by log Lj similar to 0.84(+/- 0.14)log P+ 2.15(+/- 0.07), where both Lj and P are in units of 10(44) erg s-1. This indicates that beam power is converted to radio power with an efficiency of about 0.7 per cent. The ratio of beam power to radio power is studied as a function of redshift; there is no significant evidence for redshift evolution of this ratio over the redshift range studied. The relationship is consistent with empirical results obtained by Cavagnolo et al. for radio sources in gas-rich environments, which are primarily FanaroffRiley type I sources, and with the theoretical predictions of Willott et al.
C1 [Daly, Ruth. A.; Sprinkle, Trevor B.] Penn State Univ, Reading, PA 19608 USA.
[O'Dea, Christopher P.; Kharb, Preeti] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA.
[O'Dea, Christopher P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Baum, Stefi A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
[Baum, Stefi A.] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA.
RP Daly, RA (reprint author), Penn State Univ, Berks Campus, Reading, PA 19608 USA.
EM rdaly@psu.edu
FU Penn State University; Radcliffe Institute for Advanced Study at Harvard
University
FX We would like to thank the referee for very helpful comments and
suggestions. This work is supported in part by Penn State University
(RAD and TBS) and the Radcliffe Institute for Advanced Study at Harvard
University (SAB).
NR 40
TC 12
Z9 12
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 423
IS 3
BP 2498
EP 2502
DI 10.1111/j.1365-2966.2012.21060.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961NA
UT WOS:000305470100039
ER
PT J
AU Beaumont, CN
Goodman, AA
Alves, JF
Lombardi, M
Roman-Zuniga, CG
Kauffmann, J
Lada, CJ
AF Beaumont, Christopher N.
Goodman, Alyssa A.
Alves, Joao F.
Lombardi, Marco
Roman-Zuniga, Carlos G.
Kauffmann, Jens
Lada, Charles J.
TI A simple perspective on the mass-area relationship in molecular clouds
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; ISM: clouds; ISM: structure
ID DENSITY PROBABILITY-DISTRIBUTION; COLUMN-DENSITY; PHYSICAL-PROPERTIES;
STAR-FORMATION; SIZE RELATION; TURBULENCE; II.; UNIVERSALITY; VELOCITY;
MODELS
AB Despite over 30 yr of study, the massarea relationship within and among clouds is still poorly understood both observationally and theoretically. Modern extinction data sets should have sufficient resolution and dynamic range to characterize this relationship for nearby molecular clouds, although recent papers using extinction data seem to yield different interpretations regarding the nature and universality of this aspect of cloud structure. In this paper we try to unify these various results and interpretations by accounting for the different ways cloud properties are measured and analysed. We interpret the massarea relationship in terms of the column density distribution function and its possible variation within and among clouds. We quantitatively characterize regional variations in the column density probability distribution function (PDF). We show that structures both within and among clouds possess the same degree of universality, in that their PDF means do not systematically scale with structure size. Because of this, mass scales linearly with area.
C1 [Beaumont, Christopher N.] Univ Hawaii Manoa, Inst Astron, Honoulu, HI 96822 USA.
[Beaumont, Christopher N.; Goodman, Alyssa A.; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Alves, Joao F.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Lombardi, Marco] Univ Milan, Dipartmento Fis, I-20133 Milan, Italy.
[Roman-Zuniga, Carlos G.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, BC, Mexico.
[Kauffmann, Jens] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Beaumont, CN (reprint author), Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honoulu, HI 96822 USA.
EM beaumont@ifa.hawaii.edu
RI Goodman, Alyssa/A-6007-2010; Roman-Zuniga, Carlos/F-6602-2016;
OI Goodman, Alyssa/0000-0003-1312-0477; Roman-Zuniga,
Carlos/0000-0001-8600-4798; LOMBARDI, MARCO/0000-0002-3336-4965; Alves,
Joao/0000-0002-4355-0921
NR 36
TC 17
Z9 17
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 JUL
PY 2012
VL 423
IS 3
BP 2579
EP 2586
DI 10.1111/j.1365-2966.2012.21061.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961NA
UT WOS:000305470100044
ER
PT J
AU Ratti, EM
Jonker, PG
Miller-Jones, JCA
Torres, MAP
Homan, J
Markoff, S
Tomsick, JA
Kaaret, P
Wijnands, R
Gallo, E
Ozel, F
Steeghs, DTH
Fender, RP
AF Ratti, E. M.
Jonker, P. G.
Miller-Jones, J. C. A.
Torres, M. A. P.
Homan, J.
Markoff, S.
Tomsick, J. A.
Kaaret, P.
Wijnands, R.
Gallo, E.
Oezel, F.
Steeghs, D. T. H.
Fender, R. P.
TI The black hole candidate XTE J1752-223 towards and in quiescence:
optical and simultaneous X-ray-radio observations
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; binaries: general; stars: individual: XTE
J1752-223; X-rays: binaries
ID SPECTRAL STATE TRANSITION; VLBA CALIBRATOR SURVEY; HARD STATE; SWIFT
OBSERVATIONS; LOW/HARD STATE; OUTBURST DECAY; BINARIES; J1550-564;
CHANDRA; JETS
AB We present optical, X-ray and radio observations of the black hole transient (BHT) XTE J1752-223 towards and in quiescence. Optical photometry shows that the quiescent magnitude of XTE J1752-223 is fainter than 24.4 mag in the i' band. A comparison with measurements of the source during its 20092010 outburst shows that the outburst amplitude is more than 8 mag in the i' band. Known X-ray properties of the source combined with the faintness of the quiescence optical counterpart and the large outburst optical amplitude point towards a short orbital-period system (Porb? 6.8 h) with an M type (or later) mass donor, at a distance of 3.5 ?d? 8 kpc. Simultaneous X-ray and radio data were collected with Chandra and the Expanded Very Large Array (EVLA), allowing constraints to be placed on the quiescent X-ray and radio flux of XTE J1752-223. Furthermore, using data covering the final stage of the outburst decay, we investigated the low-luminosity end of the X-rayradio correlation for this source and compared it with other BHTs. We found that XTE J1752-223 adds to the number of outliers with respect to the standard X-rayradio luminosity relation. Furthermore, XTE J1752-223 is the second source, after the BHT H1743-322, that shows a transition from the region of the outliers towards the standard correlation at low luminosity. Finally, we report on a faint, variable X-ray source we discovered with Chandra at an angular distance of similar to 2.9 arcsec to XTE J1752-223 and at a position angle consistent with that of the radio jets previously observed from the BHT. We discuss the possibility that we detected X-ray emission associated with a jet from XTE J1752-223.
C1 [Ratti, E. M.; Jonker, P. G.; Torres, M. A. P.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.; Torres, M. A. P.; Steeghs, D. T. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 AJ Nijmegen, Netherlands.
[Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Homan, J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Markoff, S.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Gallo, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Oezel, F.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Steeghs, D. T. H.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Fender, R. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
RP Ratti, EM (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
EM e.m.ratti@sron.nl
RI Miller-Jones, James/B-2411-2013; Steeghs, Danny/C-5468-2009
OI Miller-Jones, James/0000-0003-3124-2814; Steeghs,
Danny/0000-0003-0771-4746
FU VIDI grant from the Netherlands Organization for Scientific Research;
European Research council Starting Grants; STFC Advanced Fellowship
FX Mathieu Servillat is acknowledged for providing the CTIO observation of
2010 August 31. EMR acknowledges Sara Motta for the information about
the RXTE data. PGJ acknowledges support from a VIDI grant from the
Netherlands Organization for Scientific Research. RW acknowledges
support from the European Research council Starting Grants. DTHS
acknowledges an STFC Advanced Fellowship.
NR 63
TC 37
Z9 37
U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 423
IS 3
BP 2656
EP 2667
DI 10.1111/j.1365-2966.2012.21071.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961NA
UT WOS:000305470100052
ER
PT J
AU Jelic, V
Smolcic, V
Finoguenov, A
Tanaka, M
Civano, F
Schinnerer, E
Cappelluti, N
Koekemoer, A
AF Jelic, Vibor
Smolcic, Vernesa
Finoguenov, Alexis
Tanaka, Masayuki
Civano, Francesca
Schinnerer, Eva
Cappelluti, Nico
Koekemoer, Anton
TI Extended X-ray emission from non-thermal sources in the COSMOS field: a
detailed study of a large radio galaxy at z=1.168
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; radiation mechanisms: thermal;
surveys; galaxies: active; radio continuum: galaxies; X-rays: galaxies:
clusters
ID ACTIVE GALACTIC NUCLEI; NEWTON-DEEP-FIELD; PHOTOMETRIC REDSHIFT; SOURCE
CATALOG; HOT-SPOTS; CLUSTERS; LOBES; ENVIRONMENTS; POPULATION; EVOLUTION
AB X-ray selected galaxy group samples are usually generated by searching for extended X-ray sources that reflect the thermal radiation of the intragroup medium. On the other hand, large radio galaxies that regularly occupy galaxy groups also emit in the X-ray window, and their contribution to X-ray selected group samples is still not well understood. In order to investigate their relative importance, we have carried out a systematic search for non-thermal extended X-ray sources in the Cosmic Evolution Survey (COSMOS) field. Based on the morphological coincidence of X-ray and radio extensions, out of 60 radio galaxies, and similar to 300 extended X-ray sources, we find only one candidate where the observed extended X-ray emission arises from non-thermal processes related to radio galaxies. We present a detailed analysis of this source, and its environment. Our results yield that external inverse Compton emission of the lobes is the dominant process that generates the observed X-ray emission of our extended X-ray candidate, with a minor contribution from the gas of the galaxy group hosting the radio galaxy. Finally, we show that finding only one potential candidate in the COSMOS field (in a redshift range 0 < z < 6 and with radio luminosity between 1025 and 1030 W Hz-1) is consistent with expected X-ray counts arising from synchrotron lobes. This implies that these sources are not a prominent source of contamination in samples of X-ray selected clusters/groups, but they could potentially dominate the z > 1 cluster counts at the bright end (SX > 7 x 10(-15) erg s-1 cm2).
C1 [Jelic, Vibor] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Smolcic, Vernesa] Argelander Inst Astron, D-53121 Bonn, Germany.
[Smolcic, Vernesa] European So Observ, D-85748 Garching, Germany.
[Smolcic, Vernesa] Univ Zagreb, Dept Phys, Zagreb 10002, Croatia.
[Finoguenov, Alexis] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Finoguenov, Alexis] Univ Maryland Baltimore Cty, Ctr Space Sci Technol, Baltimore, MD 21250 USA.
[Tanaka, Masayuki] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Civano, Francesca] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Schinnerer, Eva] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Cappelluti, Nico] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Koekemoer, Anton] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Jelic, V (reprint author), Netherlands Inst Radio Astron, ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands.
EM jelic@astron.nl
RI Jelic, Vibor/B-2938-2014;
OI Jelic, Vibor/0000-0002-6034-8610; Cappelluti, Nico/0000-0002-1697-186X;
Schinnerer, Eva/0000-0002-3933-7677; Koekemoer,
Anton/0000-0002-6610-2048
FU European Union [229517]; World Premier International Research Center
Initiative (WPI Initiative), MEXT, Japan; KAKENHI [23740144]
FX We acknowledge the anonymous referees for their constructive comments.
This research is in part funded by the European Union's Seventh
Framework programme under grant agreement 229517 and contract PRIN-INAF
2007, by World Premier International Research Center Initiative (WPI
Initiative), MEXT, Japan and by KAKENHI No. 23740144. FC acknowledges
the Blancheflor Boncompagni Ludovisi foundation and the Smithsonian
Scholarly Studies.
NR 59
TC 6
Z9 6
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2012
VL 423
IS 3
BP 2753
EP 2763
DI 10.1111/j.1365-2966.2012.21085.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961NA
UT WOS:000305470100061
ER
PT J
AU Calabrese, JM
AF Calabrese, Justin M.
TI How emergence and death assumptions affect count-based estimates of
butterfly abundance and lifespan
SO POPULATION ECOLOGY
LA English
DT Article
DE Butterflies; Insect count analyzer; Monitoring; Phenology; Transect
count data; Zonneveld model
ID REPRODUCTIVE ASYNCHRONY; CLIMATE-CHANGE; BRITISH BUTTERFLIES; TRANSECT
COUNTS; POPULATION; MODELS; PROTANDRY; SURVIVAL; TIME; UNCERTAINTY
AB Transect count data form the basis of many butterfly and other insect monitoring programs worldwide. A clear understanding of the limitations of such datasets, including the potential for biases in the statistical methods used to analyze them, is therefore crucial. The classical Zonneveld model (CZ) can extract estimates of a suite of demographic parameters from transect count datasets, and has also been used in theoretical analyses of protandry and reproductive asynchrony. The CZ relies on strong assumptions about the emergence and death processes underlying observed transect count datasets. Though reasonable as a starting place, a growing body of empirical evidence suggests these assumptions will, in many cases, not hold. Here, I explore how violations of these assumptions bias CZ-based estimates of two key population parameters: total population size and mean individual lifespan. To do this, I generalize the Zonneveld model by relaxing the symmetrical emergence distribution and constant death rate assumptions such that the generalized models contain the CZ as a special case. Using the generalized models as data generating processes, I then show that the CZ is able to closely mimic the shape of the abundance time course produced by either variant of the generalized model under a wide range of conditions, but produces highly biased estimates of population size and mean lifespan in doing so. My analysis therefore demonstrates both that the CZ is not robust to violations of its emergence and death assumptions, and that a good observed fit to transect count data does not mean these assumptions are satisfied.
C1 [Calabrese, Justin M.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA.
[Calabrese, Justin M.] UFZ Helmholtz Ctr Environm Res, D-04318 Leipzig, Germany.
RP Calabrese, JM (reprint author), Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA.
EM CalabreseJ@si.edu
RI Calabrese, Justin/B-9131-2012
NR 42
TC 6
Z9 6
U1 0
U2 19
PU SPRINGER TOKYO
PI TOKYO
PA 1-11-11 KUDAN-KITA, CHIYODA-KU, TOKYO, 102-0073, JAPAN
SN 1438-3896
J9 POPUL ECOL
JI Popul. Ecol.
PD JUL
PY 2012
VL 54
IS 3
BP 431
EP 442
DI 10.1007/s10144-012-0316-7
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA 964IW
UT WOS:000305688400008
ER
PT J
AU Hobbs, RJ
Howard, J
Wildt, DE
Comizzoli, P
AF Hobbs, Rebecca J.
Howard, JoGayle
Wildt, David E.
Comizzoli, Pierre
TI Absence of seasonal changes in FSHR gene expression in the cat
cumulus-oocyte complex in vivo and in vitro
SO REPRODUCTION
LA English
DT Article
ID FOLLICLE-STIMULATING-HORMONE; RIBONUCLEIC-ACID EXPRESSION; GROWTH-FACTOR
RECEPTOR; RAT GRANULOSA-CELLS; DOMESTIC CAT; LUTEINIZING-HORMONE; EMBRYO
DEVELOPMENT; GONADOTROPIN STIMULATION; MOLECULAR-CLONING; MESSENGER-RNA
AB Domestic cat oocytes are seasonally sensitive to FSH. Compared with those collected during the breeding season, oocytes from the nonbreeding (NB) season require more FSH during in vitro maturation to achieve comparable developmental competence. This study tested the hypothesis that this seasonal variation was due to altered expression of FSH receptors (FSHR) and/or FSH-induced genes. Relative expression levels of FSHR mRNA and FSH-enhanced gene estrogen receptor beta (ESR2) were measured by qPCR in whole ovaries and immature cumulus-oocyte complexes (COCs) isolated from cat ovaries during the natural breeding vs NB seasons. Expression levels of FSH-induced genes prostaglandin-endoperoxide synthase 2 (PTGS2), early growth response protein-1 (EGR1), and epidermal growth factor receptor (EGFR) were examined in mature COCs from both seasons that were a) recovered in vivo or b) matured in vitro with conventional (1 mu g/ml) or high (10 mu g/ml) FSH concentrations. Overall, FSHR mRNA levels were lower in whole ovaries during the NB compared with breeding season but were similar in immature COCs, whereas ESR2 levels did not differ in either group between intervals. We observed changes in PTGS2, EGR1, and EGFR mRNA expression patterns across maturation in COCs within but not between the two seasons. The lack of seasonal differentiation in FSH-related genes was not consistent with the decreased developmental capacity of oocytes fertilized during the NB season. These findings reveal that the seasonal decrease in cat oocyte sensitivity to FSH occurs both in vivo and in vitro. Furthermore, this decline is unrelated to changes in expression of FSHR mRNA or mRNA of FSH-induced genes in COCs from antral follicles. Reproduction (2012) 144 111-122
C1 [Hobbs, Rebecca J.; Howard, JoGayle; Comizzoli, Pierre] Ctr Species Survival, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA.
[Wildt, David E.] Ctr Species Survival, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
RP Hobbs, RJ (reprint author), Ctr Species Survival, Smithsonian Conservat Biol Inst, Natl Zool Pk,Box 37012,MRC 5502, Washington, DC 20013 USA.
EM hobbsr@si.edu
FU Lalor foundation Postdoctoral Fellowship
FX This work was funded in part by the Lalor foundation Postdoctoral
Fellowship and a gift from Dr Clinton and Missy Kelly.
NR 78
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U1 0
U2 5
PU BIOSCIENTIFICA LTD
PI BRISTOL
PA EURO HOUSE, 22 APEX COURT WOODLANDS, BRADLEY STOKE, BRISTOL BS32 4JT,
ENGLAND
SN 1470-1626
J9 REPRODUCTION
JI Reproduction
PD JUL
PY 2012
VL 144
IS 1
BP 111
EP 122
DI 10.1530/REP-12-0098
PG 12
WC Developmental Biology; Reproductive Biology
SC Developmental Biology; Reproductive Biology
GA 966FC
UT WOS:000305822000011
PM 22596062
ER
PT J
AU Vari, RP
De Santana, CD
Wosiacki, WB
AF Vari, Richard P.
De Santana, Carlos David
Wosiacki, Wolmar B.
TI South American electric knifefishes of the genus Archolaemus
(Ostariophysi, Gymnotiformes): undetected diversity in a clade of
rheophiles
SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE Guiana and Brazilian shields; monophyly; new species; revision; sexual
dimorphism; Sternopygidae
ID TOCANTINS RIVER-BASIN; CENTRAL BRAZIL; RHABDOLICHOPS GYMNOTIFORMES;
FISHES GYMNOTIFORMES; STERNOPYGIDAE; TELEOSTEI; AMAZON; DIAGNOSIS;
EVOLUTION; XINGU
AB Neotropical electric knifefishes of the family Sternopygidae previously considered to represent a single relatively geographically widespread and morphologically variable species, Archolaemus blax, were analysed and found to represent a complex of five species, four of which are new to science. A fifth undescribed species from the Rio Sao Francisco basin outside the previous known range of the genus was identified. Recognized species of Archolaemus are: A. blax, previously thought to occur in the Rio Araguari, Rio Branco, Rio Tapajos, Rio Tocantins, and Rio Xingu, but which instead proved to be endemic to the Rio Tocantins; Archolaemus ferreirai sp. nov. from the Rio Mucajai and Rio Uraricoera in the north-eastern portions of the Amazon basin; Archolaemus janeae sp. nov. of the Rio Xingu and the upper Rio Tapajos, both southern tributaries of the mainstream Amazon; Archolaemus luciae sp. nov. of the Rio Trombetas, Rio Jari, and Rio Tapajos basins of the eastern Amazon, and the independent Rio Araguari draining into the Atlantic Ocean north of the mouth of the Amazon; Archolaemus orientalis sp. nov. of the Sao Francisco basin in eastern Brazil; and Archolaemus santosi sp. nov. of the Rio Jamari in the south-western portion of the Amazon basin. The phylogenetic placements of Archolaemus and the recently described genus Japigny relative to the other members of the Eigenmanninae are discussed. A series of synapomorphies for Archolaemus are proposed and a hypothesis of the relationships within that genus is advanced. Rheophily of all members of Archolaemus is discussed, with the genus found to be the most specious clade within the Gymnotiformes living primarily in high-energy settings. The reported anterior projection of the dentary teeth in A. blax was found to be a consequence of postmortem displacement.
C1 [Vari, Richard P.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
[De Santana, Carlos David; Wosiacki, Wolmar B.] Museu Paraense Emilio Goeldi, Setor Ictiol, BR-66040170 Belem, Para, Brazil.
RP Vari, RP (reprint author), Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC 159,POB 37012, Washington, DC 20013 USA.
EM varir@si.edu
RI Wosiacki, Wolmar/I-1724-2012
OI Wosiacki, Wolmar/0000-0002-4013-8501
FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, National
Museum of Natural History, Smithsonian Institution; CNPq; Fundacao de
Amparo a Pesquisa de Estado do Para [FAPESPA: 154/2010]
FX Support for this project was provided by the Herbert R. and Evelyn
Axelrod Chair in Systematic Ichthyology, National Museum of Natural
History, Smithsonian Institution to R. P. V., and by a fellowship from
CNPq and the Fundacao de Amparo a Pesquisa de Estado do Para (FAPESPA:
154/2010) to C. D. S. We are indebted to the following individuals and
institutions for access to specimens and assistance during visits: Lucia
Rapp Py-Daniel (INPA), Paulo Buckup (MNRJ), and Osvaldo Oyakawa and
Mario de Pinna (MZUSP). We thank Bruno Prudente and Sandra Raredon
(USNM) for the maps, Renildo de Oliveira and Luiz Peixoto for assistance
with some of the photographs, Guilherme Dutra and Luiz Peixoto for
fruitful discussions on the Sternopygidae, and Jose Birindelli and Tiago
Pessali for information on the habitat of some species of Archolaemus.
The article benefitted from detailed comments received from Carl J.
Ferraris, Gloria Arratia, and an anonymous reviewer.
NR 54
TC 8
Z9 12
U1 4
U2 14
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-4082
J9 ZOOL J LINN SOC-LOND
JI Zool. J. Linn. Soc.
PD JUL
PY 2012
VL 165
IS 3
BP 670
EP 699
DI 10.1111/j.1096-3642.2012.00827.x
PG 30
WC Zoology
SC Zoology
GA 964HP
UT WOS:000305685000005
ER
PT J
AU Bakos, GA
Hartman, JD
Torres, G
Beky, B
Latham, DW
Buchhave, LA
Csubry, Z
Kovacs, G
Bieryla, A
Quinn, S
Szklenar, T
Esquerdo, GA
Shporer, A
Noyes, RW
Fischer, DA
Johnson, JA
Howard, AW
Marcy, GW
Sato, B
Penev, K
Everett, M
Sasselov, DD
Furesz, G
Stefanik, RP
Lazar, J
Papp, I
Sari, P
AF Bakos, G. A.
Hartman, J. D.
Torres, G.
Beky, B.
Latham, D. W.
Buchhave, L. A.
Csubry, Z.
Kovacs, G.
Bieryla, A.
Quinn, S.
Szklenar, T.
Esquerdo, G. A.
Shporer, A.
Noyes, R. W.
Fischer, D. A.
Johnson, J. A.
Howard, A. W.
Marcy, G. W.
Sato, B.
Penev, K.
Everett, M.
Sasselov, D. D.
Furesz, G.
Stefanik, R. P.
Lazar, J.
Papp, I.
Sari, P.
TI HAT-P-34b-HAT-P-37b: FOUR TRANSITING PLANETS MORE MASSIVE THAN JUPITER
ORBITING MODERATELY BRIGHT STARS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HAT-P-34, GSC 1622-01261,
HAT-P-35, GSC 0203-01079, HAT-P-36, ... ...); techniques: photometric;
techniques: spectroscopic
ID RADIAL-VELOCITY MEASUREMENTS; CLOSE BINARY STARS; SOLAR-TYPE STAR;
HOT-JUPITER; TIDAL EVOLUTION; ECCENTRIC ORBIT; GIANT PLANET; K-DWARF;
CHROMOSPHERIC ACTIVITY; ECLIPSING BINARIES
AB We report the discovery of four transiting extrasolar planets (HAT-P-34b-HAT-P-37b) with masses ranging from 1.05 to 3.33 M-J and periods from 1.33 to 5.45 days. These planets orbit relatively bright F and G dwarf stars (from V = 10.16 to V = 13.2). Of particular interest is HAT-P-34b which is moderately massive (3.33 M-J), has a high eccentricity of e = 0.441 +/- 0.032 at a period of P = 5.452654 +/- 0.000016 days, and shows hints of an outer component. The other three planets have properties that are typical of hot Jupiters.
C1 [Bakos, G. A.; Hartman, J. D.; Csubry, Z.; Penev, K.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Bakos, G. A.; Hartman, J. D.; Torres, G.; Beky, B.; Latham, D. W.; Csubry, Z.; Bieryla, A.; Quinn, S.; Szklenar, T.; Esquerdo, G. A.; Noyes, R. W.; Penev, K.; Everett, M.; Sasselov, D. D.; Furesz, G.; Stefanik, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary.
[Shporer, A.] LCOGT, Santa Barbara, CA USA.
[Shporer, A.] UC Santa Barbara, Dept Phys, Santa Barbara, CA USA.
[Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Howard, A. W.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Sato, B.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary.
RP Bakos, GA (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
EM gbakos@astro.princeton.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Penev, Kaloyan/0000-0003-4464-1371;
Buchhave, Lars A./0000-0003-1605-5666; Hartman,
Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861
FU NASA [NNG04GN74G, NNX08AF23G]; NSF [AST-1108686]; Kepler Mission under
NASA [NCC2-1390]; Hungarian Scientific Research Foundation (OTKA)
[K-81373]
FX HATNet operations have been funded by NASA grants NNG04GN74G and
NNX08AF23G. We acknowledge partial funding of the HATNet follow-up
effort from NSF AST-1108686. We acknowledge partial support also from
the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (D.W.L.
and PI). G.K. thanks the Hungarian Scientific Research Foundation (OTKA)
for support through grant K-81373. This research has made use of Keck
telescope time granted through NOAO (program A289Hr) and NASA (N167Hr
and N029Hr). This paper uses observations obtained with facilities of
the Las Cumbres Observatory Global Telescope. Data presented in this
paper are based on observations obtained at the HAT station at the
Submillimeter Array of SAO, and HAT station at the Fred Lawrence Whipple
Observatory of SAO. The authors recognize and acknowledge the very
significant cultural role and reverence that the summit of Mauna Kea has
always had within the indigenous Hawaiian community. We are most
fortunate to have the opportunity to conduct observations from this
mountain.
NR 88
TC 28
Z9 29
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUL
PY 2012
VL 144
IS 1
AR 19
DI 10.1088/0004-6256/144/1/19
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 960VB
UT WOS:000305418600019
ER
PT J
AU Gladman, B
Lawler, SM
Petit, JM
Kavelaars, J
Jones, RL
Parker, JW
Van Laerhoven, C
Nicholson, P
Rousselot, P
Bieryla, A
Ashby, MLN
AF Gladman, B.
Lawler, S. M.
Petit, J. -M.
Kavelaars, J.
Jones, R. L.
Parker, J. Wm.
Van Laerhoven, C.
Nicholson, P.
Rousselot, P.
Bieryla, A.
Ashby, M. L. N.
TI THE RESONANT TRANS-NEPTUNIAN POPULATIONS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE celestial mechanics; Kuiper Belt: general
ID MEAN-MOTION RESONANCES; JUPITER-FAMILY COMETS; KUIPER-BELT OBJECTS;
OUTER SOLAR-SYSTEM; DYNAMICAL CLASSIFICATION; ORBITAL STRUCTURE; KOZAI
RESONANCE; SCATTERED DISK; PERIOD COMETS; DATA RELEASE
AB The trans-Neptunian objects (TNOs) trapped in mean-motion resonances with Neptune were likely emplaced there during planet migration late in the giant-planet formation process. We perform detailed modeling of the resonant objects detected in the Canada-France Ecliptic Plane Survey (CFEPS) in order to provide population estimates and, for some resonances, constrain the complex internal orbital element distribution. Detection biases play a critical role because phase relationships with Neptune make object discovery more likely at certain longitudes. This paper discusses the 3:2, 5:2, 2:1, 3:1, 5:1, 4:3, 5:3, 7:3, 5:4, and 7:4 mean-motion resonances, all of which had CFEPS detections, along with our upper limit on 1:1 Neptune Trojans (which is consistent with their small population estimated elsewhere). For the plutinos (TNOs in the 3:2 resonance) we refine the orbital element distribution given by Kavelaars et al. in 2009 and show that steep H-magnitude distributions (N(H) proportional to 10(alpha H), with alpha = 0.8-0.9) are favored in the range H-g = 8-9, and confirm that this resonance does not share the inclination distribution of the classical Kuiper Belt. We give the first population estimate for the 5:2 resonance and find that, to within the uncertainties, the population is equal to that of the 3:2 (similar or equal to 13,000 TNOs with H-g < 9.16), whereas the 2: 1 population is smaller by a factor of 3-4 compared to the other two resonances. We also measure significant populations inhabiting the 4:3, 5:3, 7:3, 5:4, 7:4, 3:1, and 5:1 resonances, with H-g < 9.16 (D > 100 km) populations in the thousands. We compare our intrinsic population and orbital element distributions with several published models of resonant-TNO production; the most striking discrepancy is that resonances beyond the 2:1 are in reality more heavily populated than in published models.
C1 [Gladman, B.; Lawler, S. M.; Van Laerhoven, C.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Petit, J. -M.; Rousselot, P.] Observ Besancon, CNRS UMR 6213, Inst UTINAM, F-25010 Besancon, France.
[Kavelaars, J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Jones, R. L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Parker, J. Wm.; Bieryla, A.] SW Res Inst, Boulder, CO 80302 USA.
[Nicholson, P.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Bieryla, A.; Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gladman, B (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
FU National Sciences and Engineering Research Council; Canadian Foundation
for Innovation
FX We acknowledge the research support of the National Sciences and
Engineering Research Council and the Canadian Foundation for Innovation.
We thank the queued service observing operations team at CFHT for their
excellence in obtaining the CFEPS observations. J. Hahn and H. Levison
provided output from their cosmogonic models, thus allowing the
quantitative comparisons between models and observation that are the
future of Kuiper Belt studies. Lastly, we acknowledge the historical
debt this subject owes to Brian Marsden, and honor his dedication to
orbital computation.
NR 54
TC 30
Z9 30
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUL
PY 2012
VL 144
IS 1
AR 23
DI 10.1088/0004-6256/144/1/23
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 960VB
UT WOS:000305418600023
ER
PT J
AU Greiss, S
Steeghs, D
Gansicke, BT
Martin, EL
Groot, PJ
Irwin, MJ
Gonzalez-Solares, E
Greimel, R
Knigge, C
Ostensen, RH
Verbeek, K
Drew, JE
Drake, J
Jonker, PG
Ripepi, V
Scaringi, S
Southworth, J
Still, M
Wright, NJ
Farnhill, H
van Haaften, LM
Shah, S
AF Greiss, S.
Steeghs, D.
Gaensicke, B. T.
Martin, E. L.
Groot, P. J.
Irwin, M. J.
Gonzalez-Solares, E.
Greimel, R.
Knigge, C.
Ostensen, R. H.
Verbeek, K.
Drew, J. E.
Drake, J.
Jonker, P. G.
Ripepi, V.
Scaringi, S.
Southworth, J.
Still, M.
Wright, N. J.
Farnhill, H.
van Haaften, L. M.
Shah, S.
TI INITIAL DATA RELEASE OF THE KEPLER-INT SURVEY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE catalogs; stars: emission-line, Be; stars: general; surveys; techniques:
photometric
ID NORTHERN GALACTIC PLANE; H-ALPHA SURVEY; DIGITAL SKY SURVEY; CATACLYSMIC
VARIABLES; ECLIPSING BINARIES; COMPACT PULSATORS; MISSION FIELD; V344
LYRAE; 1ST; IPHAS
AB This paper describes the first data release of the Kepler-INT Survey (KIS) that covers a 116 deg(2) region of the Cygnus and Lyra constellations. The Kepler field is the target of the most intensive search for transiting planets to date. Despite the fact that the Kepler mission provides superior time-series photometry, with an enormous impact on all areas of stellar variability, its field lacks optical photometry complete to the confusion limit of the Kepler instrument necessary for selecting various classes of targets. For this reason, we follow the observing strategy and data reduction method used in the IPHAS and UVEX galactic plane surveys in order to produce a deep optical survey of the Kepler field. This initial release concerns data taken between 2011 May and August, using the Isaac Newton Telescope on the island of La Palma. Four broadband filters were used, U, g, r, i, as well as one narrowband one, H alpha, reaching down to a 10 sigma limit of similar to 20th mag in the Vega system. Observations covering similar to 50 deg(2), thus about half of the field, passed our quality control thresholds and constitute this first data release. We derive a global photometric calibration by placing the KIS magnitudes as close as possible to the Kepler Input Catalog (KIC) photometry. The initial data release catalog containing around 6 million sources from all the good photometric fields is available for download from the KIS Web site (www.astro.warwick.ac.uk/research/kis/) as well as via MAST (KIS magnitudes can be retrieved using the MAST enhanced target search page http://archive.stsci.edu/kepler/kepler_fov/search.php and also via Casjobs at MAST Web site http://mastweb.stsci.edu/kplrcasjobs/).
C1 [Greiss, S.; Steeghs, D.; Gaensicke, B. T.] Univ Warwick, Dept Phys, Astron & Astrophys Grp, Coventry CV4 7AL, W Midlands, England.
[Martin, E. L.] INTA CSIC Ctr Astrobiol, Torrejon De Ardoz, Spain.
[Groot, P. J.; Verbeek, K.; Jonker, P. G.; Scaringi, S.; van Haaften, L. M.; Shah, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Irwin, M. J.; Gonzalez-Solares, E.] Univ Cambridge, Inst Astron, Cambridge Astron Survey Unit, Cambridge CB3 0HA, England.
[Greimel, R.] Karl Franzens Univ Graz, Inst Phys, A-8010 Graz, Austria.
[Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Ostensen, R. H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Drew, J. E.; Farnhill, H.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Drake, J.; Jonker, P. G.; Wright, N. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands.
[Ripepi, V.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy.
[Southworth, J.] Keele Univ, Astrophys Grp, Newcastle Under Lyme ST5 5BG, England.
[Still, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Still, M.] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
RP Greiss, S (reprint author), Univ Warwick, Dept Phys, Astron & Astrophys Grp, Coventry CV4 7AL, W Midlands, England.
EM s.greiss@warwick.ac.uk
RI Gaensicke, Boris/A-9421-2012; Steeghs, Danny/C-5468-2009; Groot,
Paul/K-4391-2016;
OI Gaensicke, Boris/0000-0002-2761-3005; Steeghs,
Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X; Scaringi,
Simone/0000-0001-5387-7189; Drew, Janet/0000-0003-1192-7082
FU STFC; European Research Council under the European Community [227224];
Research Council of K. U. Leuven [GOA/2008/04]
FX D. Steeghs acknowledges an STFC Advanced Fellowship.; R. H. Ostensen
acknowledges funding from the European Research Council under the
European Community's Seventh Framework Programme (FP7/2007-2013)/ERC
grant agreement No. 227224 (prosperity), as well as from the Research
Council of K. U. Leuven grant agreement GOA/2008/04.
NR 43
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U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUL
PY 2012
VL 144
IS 1
AR 24
DI 10.1088/0004-6256/144/1/24
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 960VB
UT WOS:000305418600024
ER
PT J
AU Kenyon, SJ
Bromley, BC
AF Kenyon, Scott J.
Bromley, Benjamin C.
TI COAGULATION CALCULATIONS OF ICY PLANET FORMATION AT 15-150 AU: A
CORRELATION BETWEEN THE MAXIMUM RADIUS AND THE SLOPE OF THE SIZE
DISTRIBUTION FOR TRANS-NEPTUNIAN OBJECTS (vol 143, pg 63, 2012)
SO ASTRONOMICAL JOURNAL
LA English
DT Correction
DE errata, addenda
ID KUIPER-BELT; LUMINOSITY FUNCTION
AB We correct errors in our comparisons of model results with observations and fix typographical errors in mathematical expressions for the accretion time. Reanalyzing the observations leads to new values for the target slope of the cumulative size distribution for large objects as a function of the slope of the power-law relation between albedo and radius. Despite these changes, the analysis still strongly prefers models where trans-Neptunian objects grow from an initial population of small (1-10 km) planetesimals.
C1 [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Bromley, Benjamin C.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA.
RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu
OI Kenyon, Scott/0000-0003-0214-609X
NR 10
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUL
PY 2012
VL 144
IS 1
AR 29
DI 10.1088/0004-6256/144/1/29
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 960VB
UT WOS:000305418600029
ER
PT J
AU Welch, AJ
Fleischer, RC
James, HF
Wiley, AE
Ostrom, PH
Adams, J
Duvall, F
Holmes, N
Hu, D
Penniman, J
Swindle, KA
AF Welch, A. J.
Fleischer, R. C.
James, H. F.
Wiley, A. E.
Ostrom, P. H.
Adams, J.
Duvall, F.
Holmes, N.
Hu, D.
Penniman, J.
Swindle, K. A.
TI Population divergence and gene flow in an endangered and highly mobile
seabird
SO HEREDITY
LA English
DT Article
DE Cytochrome b; intron; microsatellite; population; Hawaiian petrel;
Pterodroma sandwichensis
ID MULTILOCUS GENOTYPE DATA; DARK-RUMPED PETRELS; DIFFERENTIATION MEASURE;
INTRODUCED PREDATORS; NEWELLS SHEARWATERS; WANDERING ALBATROSS;
DISPERSAL PATTERNS; SOFTWARE PACKAGE; COMPUTER-PROGRAM; HAWAIIAN PETREL
AB Seabirds are highly vagile and can disperse up to thousands of kilometers, making it difficult to identify the factors that promote isolation between populations. The endemic Hawaiian petrel (Pterodroma sandwichensis) is one such species. Today it is endangered, and known to breed only on the islands of Hawaii, Maui, Lanai and Kauai. Historical records indicate that a large population formerly bred on Molokai as well, but this population has recently been extirpated. Given the great dispersal potential of these petrels, it remains unclear if populations are genetically distinct and which factors may contribute to isolation between them. We sampled petrels from across their range, including individuals from the presumably extirpated Molokai population. We sequenced 524 bp of mitochondrial DNA, 741 bp from three nuclear introns, and genotyped 18 microsatellite loci in order to examine the patterns of divergence in this species and to investigate the potential underlying mechanisms. Both mitochondrial and nuclear data sets indicated significant genetic differentiation among all modern populations, but no differentiation was found between historic samples from Molokai and modern birds from Lanai. Population-specific nonbreeding distribution and strong natal philopatry may reduce gene flow between populations. However, the lack of population structure between extirpated Molokai birds and modern birds on Lanai indicates that there was substantial gene flow between these populations and that petrels may be able to overcome barriers to dispersal prior to complete extirpation. Hawaiian petrel populations could be considered distinct management units, however, the dwindling population on Hawaii may require translocation to prevent extirpation in the near future. Heredity (2012) 109, 19-28; doi:10.1038/hdy.2012.7; published online 21 March 2012
C1 [Welch, A. J.; Fleischer, R. C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC USA.
[Welch, A. J.; Fleischer, R. C.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA.
[James, H. F.; Wiley, A. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Wiley, A. E.; Ostrom, P. H.] Michigan State Univ, Dept Zool, E Lansing, MI USA.
[Adams, J.] US Geol Survey, Western Ecol Res Ctr, Pacific Coastal & Marine Sci Ctr, Santa Cruz, CA USA.
[Duvall, F.] Dept Land & Nat Resources, Wailuku, HI USA.
[Holmes, N.] Kauai Endangered Seabird Recovery Project, Waimea, HI USA.
[Hu, D.] Natl Pk Serv, Pacific W Reg Off, Honolulu, HI USA.
[Penniman, J.] Univ Hawaii, Pacific Cooperat Studies Unit, Honolulu, HI 96822 USA.
[Swindle, K. A.] US Fish & Wildlife Serv, Off Law Enforcement, Honolulu, HI USA.
RP Welch, AJ (reprint author), SUNY Buffalo, Dept Biol Sci, 109 Cooke Hall, Buffalo, NY 14260 USA.
EM andreann@buffalo.edu
FU Behavior, Ecology and Evolution Program at the University of Maryland;
Smithsonian Office of Fellowships; Smithsonian's Walcott Fund; Center
for Conservation and Evolutionary Genetics; National Science Foundation
[DEB-0745604]
FX We thank David Anderson, David Duffy, David Ainley and Seth Judge for
access to samples and/or valuable discussion on petrel biology. We thank
Hawaii Volcanoes National Park for providing permission to sample
salvaged petrel carcasses. For the permission and assistance in sampling
museum specimens, we thank James Dean, Megan Spitzer and Christina
Gebhard of the Bird Division at the Smithsonian Institution's National
Museum of Natural History; Carla Kishinami and Lydia Garetano at the
Bernice P Bishop Museum; and Kimball Garrett at the Los Angeles County
Museum of Natural History. We thank Amy Wilson, Frank Hailer and Brandt
Ryder for discussion on data analysis; Peter Pyle, Hannah Nevins and
three anonymous reviewers for comments on earlier drafts, as well as
Heather Lerner, Nancy Rotzel, Emily Latch and other members of the
Center for Conservation and Evolutionary Genetics at the Smithsonian
Institution's National Zoological Park. Funding for this study was
provided by the Behavior, Ecology and Evolution Program at the
University of Maryland, the Smithsonian Office of Fellowships, the
Smithsonian's Walcott Fund, the Center for Conservation and Evolutionary
Genetics and the National Science Foundation (grant # DEB-0745604 to P
Ostrom, R Fleischer and H James). Procedures for handling live birds
were approved by the Western Ecological Research Center Animal Care and
Use Committee (protocol 9370BQ9TSK1102) and the Smithsonian National
Museum of Natural History Animal Care and Use Committee (protocol
200903). Samples were collected under the Endangered Species Act permit
TE-145562 and the cooperative agreement between the Hawaii Department of
Land and Natural Resources and the US Fish and Wildlife Service. The use
of trade names in this study is for descriptive purposes only and does
not imply endorsement by the US Government.
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PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0018-067X
J9 HEREDITY
JI Heredity
PD JUL
PY 2012
VL 109
IS 1
BP 19
EP 28
DI 10.1038/hdy.2012.7
PG 10
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 960CX
UT WOS:000305366700004
PM 22434012
ER
PT J
AU Pekar, S
Smerda, J
Hruskova, M
Sedo, O
Muster, C
Cardoso, P
Zdrahal, Z
Korenko, S
Bures, P
Liznarova, E
Sentenska, L
AF Pekar, S.
Smerda, J.
Hruskova, M.
Sedo, O.
Muster, C.
Cardoso, P.
Zdrahal, Z.
Korenko, S.
Bures, P.
Liznarova, E.
Sentenska, L.
TI Prey-race drives differentiation of biotypes in ant-eating spiders
SO JOURNAL OF ANIMAL ECOLOGY
LA English
DT Article
DE ecological speciation; phylogeography; prey capture trade-offs;
specialized predator; venom composition
ID SYMPATRIC SPECIATION; ARANEAE ZODARIIDAE; ADAPTIVE RADIATION;
MITOCHONDRIAL-DNA; VENOM EVOLUTION; GENE FLOW; DIVERSITY; INSECTS;
CAPTURE; DIET
AB 1. Disruptive natural selection resulting from specialization on different hosts is recognized as one of the most important driving forces in the diversification of herbivores and parasites. It has been proposed that a similar mechanism could apply to carnivorous predators too, although the evidence is still lacking. 2. Here, we show that the differentiation of biotypes of specialized ant-eating spiders of the genus Zodarion has probably been induced by prey-shifting. We focused on two forms of one species Z. styliferum from the Iberian Peninsula that presumably represent ecological races. We conducted geographic, ecological, venom-oriented, reproductive and genetic divergence analysis among multiple populations collected at a number of sites across Portugal and Madeira. 3. Geographic analysis revealed that the two forms occur in mosaic sympatry. Each form was found to associate in nature with a different ant species in a different habitat. Specifically, the styliferum form hunted predominantly Messor ants, and the extraneum form hunted mainly Camponotus ants. Laboratory experiments revealed that the two forms exhibit a significant preference for attacking focal ants, demonstrating higher paralysis efficiency, and also show different venom composition. Cross-mating of the two forms was significantly less likely than between pairs of the same form, suggesting moderate assortative mating. Phylogenetic analyses indicate low genetic differentiation of the two forms and parallel-repeated evolution of biotypes. 4. Adaptive prey-shifting correlated with habitat preference are at present the most valid explanations for biotype formation in Zodarion. The speciation of ant-eating Zodarion spiders thus appears to follow a scenario similar to that of host-shifting in parasites and herbivores.
C1 [Pekar, S.; Smerda, J.; Hruskova, M.; Korenko, S.; Bures, P.; Liznarova, E.; Sentenska, L.] Masaryk Univ, Fac Sci, Dept Bot & Zool, CS-61137 Brno, Czech Republic.
[Sedo, O.; Zdrahal, Z.] Masaryk Univ, Prote Core Facil, Mendel Ctr Plant Genom & Prote, Cent European Technol Inst, Brno 62500, Czech Republic.
[Muster, C.] Ernst Moritz Arndt Univ Greifswald, Zool Inst & Museum, Greifswald, Germany.
[Cardoso, P.] Univ Azores, Azorean Biodivers Grp CITA A, P-9700042 Angra Do Heroismo, Portugal.
[Cardoso, P.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
RP Pekar, S (reprint author), Masaryk Univ, Fac Sci, Dept Bot & Zool, Kotlarska 2, CS-61137 Brno, Czech Republic.
EM pekar@sci.muni.cz
RI Sedo, Ondrej/D-9868-2012; Zdrahal, Zbynek/D-9491-2012; Cardoso,
Pedro/A-8820-2008;
OI Cardoso, Pedro/0000-0001-8119-9960; Pekar, Stano/0000-0002-0197-5040
FU Ministry of Education, Youth and Sports of the Czech Republic
[0021622416, 0021622415, LC06034]; Portuguese Foundation for Science and
Technology [SFRH/BPD/40688/2007]
FX We would like to thank P. Werner for helping with the identification of
ants and staff at the Parque Natural do Vale do Guadiana in Mertola, C.
Meierrose for logistical support and two anonymous reviewers for useful
comments. The study was supported by grants no. 0021622416, 0021622415
and LC06034 from the Ministry of Education, Youth and Sports of the
Czech Republic. PC is supported by the Portuguese Foundation for Science
and Technology (SFRH/BPD/40688/2007).
NR 74
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0021-8790
EI 1365-2656
J9 J ANIM ECOL
JI J. Anim. Ecol.
PD JUL
PY 2012
VL 81
IS 4
BP 838
EP 848
DI 10.1111/j.1365-2656.2012.01957.x
PG 11
WC Ecology; Zoology
SC Environmental Sciences & Ecology; Zoology
GA 959SS
UT WOS:000305333900012
PM 22313500
ER
PT J
AU Knope, ML
Morden, CW
Funk, VA
Fukami, T
AF Knope, Matthew L.
Morden, Clifford W.
Funk, Vicki A.
Fukami, Tadashi
TI Area and the rapid radiation of Hawaiian Bidens (Asteraceae)
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Article
DE Adaptive radiation; Asteraceae; carrying capacity; Compositae;
diversification rate; endemism; extinction; island evolution; islands;
speciation
ID SILVERSWORD ALLIANCE COMPOSITAE; ADAPTIVE RADIATION; DIVERGENCE TIMES;
DIVERSIFICATION; BIOGEOGRAPHY; PHYLOGENY; EVOLUTION; SEQUENCES; CLADES;
TREES
AB Aim To estimate the rate of adaptive radiation of endemic Hawaiian Bidens and to compare their diversification rates with those of other plants in Hawaii and elsewhere with rapid rates of radiation. Location Hawaii. Methods Fifty-nine samples representing all 19 Hawaiian species, six Hawaiian subspecies, two Hawaiian hybrids and an additional two Central American and two African Bidens species had their DNA extracted, amplified by polymerase chain reaction and sequenced for four chloroplast and two nuclear loci, resulting in a total of approximately 5400 base pairs per individual. Internal transcribed spacer sequences for additional outgroup taxa, including 13 non-Hawaiian Bidens, were obtained from GenBank. Phylogenetic relationships were assessed by maximum likelihood and Bayesian inference. The age of the most recent common ancestor and diversification rates of Hawaiian Bidens were estimated using the methods of previously published studies to allow for direct comparison with other studies. Calculations were made on a per-unit-area basis. Results We estimate the age of the Hawaiian clade to be 1.33.1 million years old, with an estimated diversification rate of 0.32.3 species/million years and 4.8 x 10(-5) to 1.3 x 10(-4) species Myr-1 km-2. Bidens species are found in Europe, Africa, Asia and North and South America, but the Hawaiian species have greater diversity of growth form, floral morphology, dispersal mode and habitat type than observed in the rest of the genus world-wide. Despite this diversity, we found little genetic differentiation among the Hawaiian species. This is similar to the results from other molecular studies on Hawaiian plant taxa, including others with great morphological variability (e.g. silverswords, lobeliads and mints). Main conclusions On a per-unit-area basis, Hawaiian Bidens have among the highest rates of speciation for plant radiations documented to date. The rapid diversification within such a small area was probably facilitated by the habitat diversity of the Hawaiian Islands and the adaptive loss of dispersal potential. Our findings point to the need to consider the spatial context of diversification specifically, the relative scale of habitable area, environmental heterogeneity and dispersal ability to understand the rate and extent of adaptive radiation.
C1 [Knope, Matthew L.; Fukami, Tadashi] Stanford Univ, Dept Biol, Stanford, CA 94305 USA.
[Morden, Clifford W.] Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA.
[Morden, Clifford W.] Univ Hawaii Manoa, PCSU, Honolulu, HI 96822 USA.
[Funk, Vicki A.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA.
RP Knope, ML (reprint author), Stanford Univ, Dept Biol, 371 Serra Mall, Stanford, CA 94305 USA.
EM knope@stanford.edu
RI Fukami, Tadashi/A-2934-2010
OI Fukami, Tadashi/0000-0001-5654-4785
FU University of Hawaii Ecology, Evolution, and Conservation Biology
Research Grant Award [DGEO2-32016]; Department of Zoology, University of
Hawaii, Manoa; Department of Biology, Stanford University
FX We thank Dan Crawford (University of Kansas), Fred Ganders (UBC),
Gabriel Johnson (Smithsonian), Karen Shigematsu and Alvin Yoshinaga
(Lyon Arboretum), Ken Wood and Mike DeMotta (Allerton NTBG) and Kawika
Winters (Limahuli NTBG) for DNA or tissue donation; Dave Carlon, Ken
Hayes, Shaobin Hou and Gabriel Johnson for assistance with DNA
sequencing; Yi 'Apollo' Qi for assistance with ARCGIS; Gerry Carr and
Pasha Feinberg for image preparation; Pat Aldrich, Stephanie Dunbar-Co,
Shama Hinard, Jeffrey Knope, Tatiana Kutynina, Kathy McMillen, Kurtis
McMillen, Colin Olito, Hank Oppenheimer and Maggie Sporck for assistance
in the field; and Melinda Belisle, Rodolfo Dirzo, Elizabeth Hadly, Shama
Hinard, Olivia Isaac, Sterling Keeley, Jeffrey Knope, Jonathan Payne,
Cindy Sayre, Peter Vitousek, Ward Watt, Belinda Wheeler and Robert J.
Whittaker for comments. Funding was provided in part by a University of
Hawaii Ecology, Evolution, and Conservation Biology Research Grant Award
to M. L. K. (National Science Foundation GK12 Fellowship grant no.
DGEO2-32016 to K. Y. Kaneshiro) and support from the Department of
Zoology, University of Hawaii, Manoa and the Department of Biology,
Stanford University.
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PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0305-0270
J9 J BIOGEOGR
JI J. Biogeogr.
PD JUL
PY 2012
VL 39
IS 7
BP 1206
EP 1216
DI 10.1111/j.1365-2699.2012.02687.x
PG 11
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 961GP
UT WOS:000305452500002
ER
PT J
AU Tyuterev, VG
Perrin, AM
Rothman, LS
AF Tyuterev, Vladimir G.
Perrin, Agnes M.
Rothman, Laurence S.
TI Special issue honoring three great contributors and mentors in
high-resolution molecular spectroscopy: Jean-Marie Flaud, Claude
Camy-Peyret, and Alain Barbe Preface
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
C1 [Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Tyuterev, Vladimir G.] Univ Reims, Fac Sci Exactes & Nat, Grp Spectrometrie Mol & Atmospher, F-51687 Reims, France.
[Perrin, Agnes M.] Univ Paris Est Creteil, F-94010 Creteil, France.
[Perrin, Agnes M.] Univ Paris Diderot, CNRS, Lab Interuniv Syst Atmospher, F-94010 Creteil, France.
RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA.
EM LRothman@CfA.Harvard.edu
NR 0
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUL
PY 2012
VL 113
IS 11
SI SI
BP 821
EP 824
DI 10.1016/j.jqsrt.2012.03.004
PG 4
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 959YX
UT WOS:000305355200001
ER
PT J
AU Richard, C
Gordon, IE
Rothman, LS
Abel, M
Frommhold, L
Gustafsson, M
Hartmann, JM
Hermans, C
Lafferty, WJ
Orton, GS
Smith, KM
Tran, H
AF Richard, C.
Gordon, I. E.
Rothman, L. S.
Abel, M.
Frommhold, L.
Gustafsson, M.
Hartmann, J. -M.
Hermans, C.
Lafferty, W. J.
Orton, G. S.
Smith, K. M.
Tran, H.
TI New section of the HITRAN database: Collision-induced absorption (CIA)
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Collision-induced absorption; HITRAN; Atmospheric absorption;
Interacting molecular pairs
ID COOL WHITE-DWARFS; MOLECULAR SPECTROSCOPIC DATABASE;
INFRARED-ABSORPTION; MODEL ATMOSPHERES; TITANS ATMOSPHERE; EARTHS
ATMOSPHERE; LOW-TEMPERATURES; BROWN DWARFS; 1ST STARS; A-BAND
AB This paper describes the addition of Collision-Induced Absorption (CIA) into the HITRAN compilation. The data from different experimental and theoretical sources have been cast into a consistent format and formalism. The implementation of these new spectral data into the HITRAN database is invaluable for modeling and interpreting spectra of telluric and other planetary atmospheres as well as stellar atmospheres. In this implementation for HITRAN, CIAs of N-2, H-2, O-2, CO2, and CH4 due to various collisionally interacting atoms or molecules are presented. Some CIA spectra are given over an extended range of frequencies, including several H-2 overtone bands that are dipole-forbidden in the non-interacting molecules. Temperatures from tens to thousands of Kelvin are considered, as required, for example, in astrophysical analyses of objects, including cool white dwarfs, brown dwarfs. M dwarfs, cool main sequence stars, solar and extra-solar planets, and the formation of so-called first stars. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Richard, C.; Gordon, I. E.; Rothman, L. S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Abel, M.; Frommhold, L.] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA.
[Gustafsson, M.] Univ Gothenburg, Dept Chem, SE-41296 Gothenburg, Sweden.
[Hartmann, J. -M.; Tran, H.] Univ Paris Diderot, Inst Pierre Simon Laplace, Univ Paris Est Creteil, CNRS,UMR 7583, F-94010 Creteil, France.
[Hermans, C.] Belgian Inst Space Aeron, B-1180 Brussels, Belgium.
[Lafferty, W. J.] NIST, Opt Technol Div, Gaithersburg, MD 20899 USA.
[Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Smith, K. M.] RAL Space, Rutherford Appleton Lab, Didcot, Oxon, England.
RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA.
EM lrothman@cfa.harvard.edu
RI Gustafsson, Magnus/A-1661-2010; Tran, Ha/I-5076-2013;
OI Gustafsson, Magnus/0000-0002-7629-0169; Gordon,
Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847
FU NASA through the Planetary Atmospheres grant [NNX10AB94G]; Earth
Observing System (EOS) [NAG5-13534]
FX This effort has been supported by NASA through the Planetary Atmospheres
grant NNX10AB94G and the Earth Observing System (EOS) under grant
NAG5-13534.
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JUL
PY 2012
VL 113
IS 11
SI SI
BP 1276
EP 1285
DI 10.1016/j.jqsrt.2011.11.004
PG 10
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 959YX
UT WOS:000305355200041
ER
PT J
AU Pruss, SB
Clemente, H
Laflamme, M
AF Pruss, Sara B.
Clemente, Hannah
Laflamme, Marc
TI Early (Series 2) Cambrian archaeocyathan reefs of southern Labrador as a
locus for skeletal carbonate production
SO LETHAIA
LA English
DT Article
DE Archaeocyatha; bioherms; carbonates; calcification; point count analysis
ID UNITED-STATES CALIFORNIA; PROTEROZOIC NAMA GROUP; RANGE PROVINCE;
METAZOAN REEFS; EXTINCTION; NAMIBIA; CANADA; LAURENTIA; HISTORY; FOSSILS
AB Pruss, S.B., Clemente, H. & Laflamme, M. 2012: Early (Series 2) Cambrian archaeocyathan reefs of southern Labrador as a locus for skeletal carbonate production. Lethaia, Vol. 45, pp. 401410. Archaeocyathan reefs, the first reefs produced by animals, are prominent, global features of early Cambrian successions. However, microbialites the dominant reef components of the Proterozoic were still abundant in most archaeocyathan reefs. Although such reefs were a locus for carbonate production, it is unclear how much carbonate was produced skeletally. This analysis of well-known early Cambrian archaeocyathan patch reefs of the Forteau Formation, southern Labrador, demonstrates that skeletal carbonate was abundantly produced in these archaeocyathan reefs, although only about half was produced by archaeocyathans. Trilobites, echinoderms and brachiopods contributed substantially to the total carbonate budget, particularly in grainstone facies flanking the reefs. Through point count analysis of samples collected from the reef core and flanking grainstones, it can be demonstrated that skeletal material was most abundant in grainstone facies, where animals such as trilobites and echinoderms contributed significantly to carbonate production. In contrast, microbial fabrics were more abundant than skeletal fabrics in the reef core, although archaeocyathan material was more abundant than other skeletal debris. Similar to modern reefs, these reefs created a variety of habitats that allowed for the proliferation of skeletal organisms living on and around the reef, thereby promoting skeletal carbonate production through ecosystem engineering. ?Archaeocyatha, bioherms, carbonates, calcification, point count analysis
C1 [Pruss, Sara B.; Clemente, Hannah] Smith Coll, Dept Geosci, Northampton, MA 01063 USA.
[Laflamme, Marc] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
RP Pruss, SB (reprint author), Smith Coll, Dept Geosci, Northampton, MA 01063 USA.
EM spruss@smith.edu; hannah.cle@gmail.com; laflammem@si.edu
FU National Science and Engineering Council of Canada; Bateman; Smithsonian
Postdoctoral Fellowships
FX We acknowledge the Smith College Department of Geosciences Marshall
Schalk Fund, Smith College International Studies Experience Grants,
Smith College Student Aid Society (to HC), Alexandra Breus for thin
section preparation, Tony Caldanaro for machinery training, Mike
Vollinger for printing, and Katie Castagno for field assistance. We also
thank S. Finnegan, A. Knoll and A. Bush for helpful discussion. ML
acknowledges the generous funding provided by the National Science and
Engineering Council of Canada, Bateman, and Smithsonian Postdoctoral
Fellowships.
NR 42
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-1164
J9 LETHAIA
JI Lethaia
PD JUL
PY 2012
VL 45
IS 3
BP 401
EP 410
DI 10.1111/j.1502-3931.2011.00299.x
PG 10
WC Paleontology
SC Paleontology
GA 960MH
UT WOS:000305392100008
ER
PT J
AU Mei, ZX
Udo, Z
Lin, J
AF Mei ZhiXing
Udo, Ziegler
Lin Jun
TI Numerical experiments of disturbance to the solar atmosphere caused by
eruptions
SO SCIENCE CHINA-PHYSICS MECHANICS & ASTRONOMY
LA English
DT Article
DE sun: coronal mass ejections; sun: flares; sun: magnetic fields; plasmas:
MHD waves; plasma: shock waves
ID CORONAL MASS EJECTIONS; ULTRAVIOLET IMAGING TELESCOPE; X-RAY
OBSERVATIONS; II RADIO-BURSTS; EIT WAVES; MORETON WAVE; MAGNETIC
RECONNECTION; CATASTROPHE MODEL; TRANSPORT SCHEME; FLARE WAVES
AB Despite extensive research on various global waves in solar eruptions, debate continues on the intrinsic nature of them. In this work, we performed numerical experiments of the coronal mass ejection with emphases on the associated large-scale MHD waves. A fast-mode shock forms in front of the flux rope during the eruption with a dimming region following it, and the development of a three-component structure of the ejecta is observed. At the flank of the flux rope, the slow-mode shock and the velocity vortices are also invoked. The dependence of the eruption energetics on the strength of the background field and the coronal plasma density distribution is apparent: the stronger the background field is, and/or the lower the coronal plasma density is, the more energetic the eruption is. In the lower Alfv,n speed environment, the slow mode shock and the large scale velocity vortices may be the source of the EIT wave. In the high Alfv,n speed environment, on the other hand, the echo due to the reflection of the fast shock on the bottom boundary could be so strong that its interaction with the slow mode shock and the velocity vortices produces the second echo propagating downward and causing the secondary disturbance to the boundary surface. We suggest that this second echo, together with the slow shock and the velocity vortices, could constitute a possible candidate of the source for the EIT wave.
C1 [Mei ZhiXing; Lin Jun] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Peoples R China.
[Mei ZhiXing] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China.
[Udo, Ziegler] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany.
[Lin Jun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Mei, ZX (reprint author), Chinese Acad Sci, Yunnan Astron Observ, POB 110, Kunming 650011, Peoples R China.
EM meizhixing@ynao.ac.cn
FU National Basic Research Program of China [2011CB811403]; National
Natural Science Foundation of China [10873030]; Chinese Academy of
Sciences [2009J2-34]; CMA [GYHY201106011]; NASA [NNX11AB61G];
Smithsonian Institution Sprague Endowment Fund
FX We are grateful to FORBES T G, RAYMOND J C, SHEN C and DAI S for
valuable discussions. This work was supported by the National Basic
Research Program of China (Grant No. 2011CB811403), the National Natural
Science Foundation of China (Grant No. 10873030), the Chinese Academy of
Sciences (Grant No. 2009J2-34), the CMA (Grant No. GYHY201106011), NASA
(Grant No. NNX11AB61G) and the Smithsonian Institution Sprague Endowment
Fund during FY10. The NIRVANA v3.4 code used in this work was developed
by UDO Ziegler at the Leibniz-Institut fur Astrophysik Potsdam.
Calculations in this work were completed with the help of the HPC
Center, Kunming Institute of Botany, Chinese Academy of Sciences.
NR 66
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PU SCIENCE PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 1674-7348
EI 1869-1927
J9 SCI CHINA PHYS MECH
JI Sci. China-Phys. Mech. Astron.
PD JUL
PY 2012
VL 55
IS 7
SI SI
BP 1316
EP 1329
DI 10.1007/s11433-012-4752-3
PG 14
WC Physics, Multidisciplinary
SC Physics
GA 960VI
UT WOS:000305419500028
ER
PT J
AU Konstantinidis, P
Johnson, GD
AF Konstantinidis, Peter
Johnson, G. David
TI Ontogeny of the jaw apparatus and suspensorium of the Tetraodontiformes
SO ACTA ZOOLOGICA
LA English
DT Article
DE development; comparative anatomy; ethmopalatine articulation;
Tetraodontiformes
ID FEEDING MECHANISM; PUFFERFISH INFLATION; OCEAN SUNFISHES;
ACTINOPTERYGIAN FISHES; FUNCTIONAL-MORPHOLOGY; QUEEN TRIGGERFISH;
CHECKERED PUFFER; BALISTES-VETULA; AXIAL SKELETON; LEIS CONUNDRUM
AB Konstantinidis, P. and Johnson, G. David 2012. Ontogeny of the jaw apparatus and suspensorium of the Tetraodontiformes. Acta Zoologica (Stockholm) 93: 351366. The jaw apparatus and suspensorium of adult Tetraodontiformes are well adapted to a durophagous feeding habit. Anatomical indicators are the short, stout jaws and a suspensorium in which the quadrate lies in the same vertical plane as the autopalatine. In contrast, the palatoquadrate of larval Tetraodontiformes generally resembles that of larval percomorphs a more posteriorly positioned quadrate and a slender and long Meckelian cartilage. Among Tetraodontiformes, the Triacanthodidae retain a protrusible upper jaw and a versatile suspensorium. The jaws of the Balistoidei have greater mobility achieved by a reduced autopalatine that has lost its bony contact with the suspensorium. In contrast to the Balistoidei, the beak-like jaws of the Tetraodontoidei lack individual teeth in the biting part of the jaws. The autopalatine is enlarged, which results in immobilization of the ethmopalatine articulation. The Ostraciidae are exceptional in having the distal part of the autopalatine reduced, while the proximal part remains attached to the suspensorium.
C1 [Konstantinidis, Peter] Nat Hist Museum, Dept Zool, London SW7 5BD, England.
[Johnson, G. David] Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Dept Zool, Washington, DC 20013 USA.
RP Konstantinidis, P (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England.
EM peter.konstantinidis@uni-jena.de
FU Department of Zoology of the Natural History Museum, London
FX For their constructive comments, we are grateful to Timo Moritz and Eric
Hilton. We thank Sebastien Lavoue, Matt Harris, James Maclaine, Oliver
Crimmen, Lukas Ruber, and Kai Winkelmann. We also thank James Tyler for
sharing his knowledge with us. For the supply of larval and adult
material, the authors are indebted to Karsten Hartel from the MCZ,
Keiichi Matsuura from the NSMT, Mark McGrouther and Jeff Leis from the
AMS, and Mark Sabaj from the ANSP. We are thankful to Ralf Britz, NHM,
who initiated the project and helped to obtain necessary stages of
Monotrete suvattii. PK also thank Prof Wolfgang Maier from the
University of Tuebingen and Prof Phil Rainbow from the Natural History
Museum in London. The project is part of a Ph.D. thesis, which is funded
by the Department of Zoology of the Natural History Museum, London.
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PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0001-7272
J9 ACTA ZOOL-STOCKHOLM
JI Acta Zool.
PD JUL
PY 2012
VL 93
IS 3
BP 351
EP 366
DI 10.1111/j.1463-6395.2011.00509.x
PG 16
WC Anatomy & Morphology; Zoology
SC Anatomy & Morphology; Zoology
GA 958ZP
UT WOS:000305279800008
ER
PT J
AU Mi, XC
Swenson, NG
Valencia, R
Kress, WJ
Erickson, DL
Perez, AJ
Ren, HB
Su, SH
Gunatilleke, N
Gunatilleke, S
Hao, ZQ
Ye, WH
Cao, M
Suresh, HS
Dattaraja, HS
Sukumar, R
Ma, KP
AF Mi, Xiangcheng
Swenson, Nathan G.
Valencia, Renato
Kress, W. John
Erickson, David L.
Perez, Alvaro J.
Ren, Haibao
Su, Sheng-Hsin
Gunatilleke, Nimal
Gunatilleke, Savi
Hao, Zhanqing
Ye, Wanhui
Cao, Min
Suresh, H. S.
Dattaraja, H. S.
Sukumar, R.
Ma, Keping
TI The Contribution of Rare Species to Community Phylogenetic Diversity
across a Global Network of Forest Plots
SO AMERICAN NATURALIST
LA English
DT Article
DE rare species; community phylogenetic diversity; species abundance
distribution; phylogenetic relatedness; niche differentiation; community
assembly
ID ECOLOGICAL COMMUNITIES; TAXONOMIC DISTINCTNESS; EVOLUTIONARY HISTORY;
RELATIVE ABUNDANCE; NICHE CONSERVATISM; BIODIVERSITY; PATTERNS; TREE;
PRODUCTIVITY; RELATEDNESS
AB Niche differentiation has been proposed as an explanation for rarity in species assemblages. To test this hypothesis requires quantifying the ecological similarity of species. This similarity can potentially be estimated by using phylogenetic relatedness. In this study, we predicted that if niche differentiation does explain the co-occurrence of rare and common species, then rare species should contribute greatly to the overall community phylogenetic diversity (PD), abundance will have phylogenetic signal, and common and rare species will be phylogenetically dissimilar. We tested these predictions by developing a novel method that integrates species rank abundance distributions with phylogenetic trees and trend analyses, to examine the relative contribution of individual species to the overall community PD. We then supplement this approach with analyses of phylogenetic signal in abundances and measures of phylogenetic similarity within and between rare and common species groups. We applied this analytical approach to 15 long-term temperate and tropical forest dynamics plots from around the world. We show that the niche differentiation hypothesis is supported in six of the nine gap-dominated forests but is rejected in the six disturbance-dominated and three gap-dominated forests. We also show that the three metrics utilized in this study each provide unique but corroborating information regarding the phylogenetic distribution of rarity in communities.
C1 [Mi, Xiangcheng; Ren, Haibao; Ma, Keping] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China.
[Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA.
[Valencia, Renato; Perez, Alvaro J.] Pontificia Univ Catolica Ecuador, Escuela Ciencias Biol, Lab Ecol Plantas, Quito, Ecuador.
[Kress, W. John; Erickson, David L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
[Su, Sheng-Hsin] Taiwan Forestry Res Inst, Taipei 10066, Taiwan.
[Gunatilleke, Nimal; Gunatilleke, Savi] Univ Peradeniya, Fac Sci, Dept Bot, Peradeniya 20400, Sri Lanka.
[Hao, Zhanqing] Chinese Acad Sci, Inst Appl Ecol, Shenyang 110016, Peoples R China.
[Ye, Wanhui] Chinese Acad Sci, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China.
[Cao, Min] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Kunming 650223, Peoples R China.
[Suresh, H. S.; Dattaraja, H. S.; Sukumar, R.] Indian Inst Sci, Ctr Ecol Sci, Bangalore 560012, Karnataka, India.
RP Ma, KP (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, 20 Nanxincun, Beijing 100093, Peoples R China.
EM kpma@ibcas.ac.cn
RI Raman, Sukumar/C-9809-2013; Swenson, Nathan/A-3514-2012
OI Swenson, Nathan/0000-0003-3819-9767
FU C.A.S. [KSCX2-EW-Z-5]; Natural Science Foundation of China [31061160188,
31011120470]; National Science Foundation; Andrew W. Mellon Foundation;
Peninsula Community Foundation; Smithsonian Institution; Smithsonian
Tropical Research Institute; Arnold Arboretum (Harvard University);
Indian Institute of Science; Forest Research Institute of Malaysia;
Royal Thai Forest Department, the National Institute of Environmental
Studies (Japan); Taiwan Forestry Research Institute and Forestry Bureau;
SENESCYT (Secretaria Nacional de Educacion Superior, Ciencia, Tecnologia
e Innovacion); PUCE (Pontificia Universidad Catolica de Ecuador);
Donaciones del Impuesto a la Renta (Ecuador); John D. and Catherine T.
MacArthur Foundation
FX The data analyses reported in this study were supported by the Key
Innovation Project of C.A.S. (KSCX2-EW-Z-5) and the Natural Science
Foundation of China projects (31061160188 and 31011120470). We are
grateful to C. Cannon, L. Comita, R. Condit, M. Helmus, F. Slik, H. Su,
and two reviewers for their insightful comments and suggestions on the
earlier form of the manuscript. Data collection was funded by many
organizations, principally, the National Science Foundation; the Andrew
W. Mellon Foundation; the Peninsula Community Foundation; the
Smithsonian Institution; the Smithsonian Tropical Research Institute;
the Arnold Arboretum (Harvard University); the Indian Institute of
Science; the Forest Research Institute of Malaysia; the Royal Thai
Forest Department, the National Institute of Environmental Studies
(Japan); the Taiwan Forestry Research Institute and Forestry Bureau;
SENESCYT (Secretaria Nacional de Educacion Superior, Ciencia, Tecnologia
e Innovacion), PUCE (Pontificia Universidad Catolica de Ecuador), and
Donaciones del Impuesto a la Renta (Ecuador); and the John D. and
Catherine T. MacArthur Foundation. We thank the hundreds of
field-workers who measured and mapped the trees analyzed in this study.
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PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0003-0147
J9 AM NAT
JI Am. Nat.
PD JUL
PY 2012
VL 180
IS 1
BP E17
EP E30
DI 10.1086/665999
PG 14
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA 956JU
UT WOS:000305086700002
PM 22673660
ER
PT J
AU Bartel, N
Bietenholz, MF
Lebach, DE
Lederman, JI
Petrov, L
Ransom, RR
Ratner, MI
Shapiro, II
AF Bartel, N.
Bietenholz, M. F.
Lebach, D. E.
Lederman, J. I.
Petrov, L.
Ransom, R. R.
Ratner, M. I.
Shapiro, I. I.
TI VLBI FOR GRAVITY PROBE B. III. A LIMIT ON THE PROPER MOTION OF THE
"CORE" OF THE QUASAR 3C 454.3
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: close; radio continuum: stars; stars: activity; stars:
imaging; stars: individual (IM Pegasi); techniques: interferometric
ID CELESTIAL REFERENCE FRAME; HIGH-PRECISION ASTROMETRY; BASE-LINE ARRAY;
RADIO INTERFEROMETRY; KINEMATICS; OUTBURST; POSITION; DISTANCE; OPACITY;
GEODESY
AB We made very long baseline interferometry observations at 8.4 GHz between 1997 and 2005 to estimate the coordinates of the "core" component of the superluminal quasar, 3C 454.3, the ultimate reference point in the distant universe for the NASA/Stanford Gyroscope Relativity Mission, Gravity Probe B (GP-B). These coordinates are determined relative to those of the brightness peaks of two other compact extragalactic sources, B2250+194 and B2252+172, nearby on the sky, and within a celestial reference frame (CRF), defined by a large suite of compact extragalactic radio sources, and nearly identical to the International Celestial Reference Frame 2 (ICRF2). We find that B2250+194 and B2252+172 are stationary relative to each other, and also in the CRF, to within 1s upper limits of 15 and 30 mu as yr(-1) in a and d, respectively. The core of 3C 454.3 appears to jitter in its position along the jet direction over similar to 0.2 mas, likely due to activity close to the putative supermassive black hole nearby, but on average is stationary in the CRF within 1s upper limits on its proper motion of 39 mu as yr(-1) (1.0c) and 30 mu as yr(-1) (0.8c) in a and d, respectively, for the period 2002-2005. Our corresponding limit over the longer interval, 1998-2005, of more importance to GP-B, is 46 and 56 mu as yr(-1) in a and d, respectively. Some of 3C 454.3's jet components show significantly superluminal motion with speeds of up to similar to 200 mu as yr-1 or 5c in the CRF. The core of 3C 454.3 thus provides for GP-B a sufficiently stable reference in the distant universe.
C1 [Bartel, N.; Bietenholz, M. F.; Ransom, R. R.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Lebach, D. E.; Ratner, M. I.; Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lederman, J. I.] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 1P3, Canada.
[Petrov, L.] Astrogeo Ctr, Falls Church, VA 22043 USA.
[Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
[Ransom, R. R.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada.
RP Bartel, N (reprint author), York Univ, Dept Phys & Astron, 4700 Keele St, Toronto, ON M3J 1P3, Canada.
FU NASA; Stanford University; SAO
FX This research was primarily supported by NASA, through a contract with
Stanford University to SAO, and a subcontract from SAO to York
University. The National Radio Astronomy Observatory is a facility of
the National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. The DSN is operated by JPL/Caltech, under
contract with NASA. This research has made use of the United States
Naval Observatory (USNO) Radio Reference Frame Image Database (RRFID).
We have made use of NASA's Astrophysics Data System Abstract Service,
developed and maintained at SAO. Jeff Cadieux and Julie Tome helped with
the data reduction during their tenure as students at York University.
We thank the International VLBI Service for Geodesy and Astrometry (IVS;
Schluter & Behrend 2007) for their support.
NR 44
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUL
PY 2012
VL 201
IS 1
AR 3
DI 10.1088/0067-0049/201/1/3
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956JZ
UT WOS:000305087200003
ER
PT J
AU Bietenholz, MF
Bartel, N
Lebach, DE
Ransom, RR
Ratner, MI
Shapiro, II
AF Bietenholz, M. F.
Bartel, N.
Lebach, D. E.
Ransom, R. R.
Ratner, M. I.
Shapiro, I. I.
TI VLBI FOR GRAVITY PROBE B. VII. THE EVOLUTION OF THE RADIO STRUCTURE OF
IM PEGASI
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: close; radio continuum: stars; stars: activity; stars:
imaging; stars: individual (IM Pegasi); techniques: interferometric
ID RS-CANUM-VENATICORUM; UX ARIETIS; GUIDE STAR; BINARY-SYSTEMS;
FLUX-DENSITY; II PEGASI; EMISSION; ALGOL; MISSION; CVN
AB We present measurements of the total radio flux density as well as very long baseline interferometry images of the star, IM Pegasi, which was used as the guide star for the NASA/ Stanford relativity mission Gravity Probe B. We obtained flux densities and images from 35 sessions of observations at 8.4 GHz (lambda=3.6 cm) between 1997 January and 2005 July. The observations were accurately phase-referenced to several extragalactic reference sources, and we present the images in a star-centered frame, aligned by the position of the star as derived from our fits to its orbital motion, parallax, and proper motion. Both the flux density and the morphology of IM Peg are variable. For most sessions, the emission region has a single-peaked structure, but 25% of the time, we observed a two-peaked (and on one occasion perhaps a three-peaked) structure. On average, the emission region is elongated by 1.4 +/- 0.4 mas (FWHM), with the average direction of elongation being close to that of the sky projection of the orbit normal. The average length of the emission region is approximately equal to the diameter of the primary star. No significant correlation with the orbital phase is found for either the flux density or the direction of elongation, and no preference for any particular longitude on the star is shown by the emission region.
C1 [Bietenholz, M. F.; Bartel, N.; Ransom, R. R.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Lebach, D. E.; Ratner, M. I.; Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
[Ransom, R. R.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada.
RP Bietenholz, MF (reprint author), York Univ, Dept Phys & Astron, 4700 Keele St, Toronto, ON M3J 1P3, Canada.
FU NASA; Stanford University; SAO
FX This research was primarily supported by NASA, through a contract with
Stanford University to SAO and a subcontract from SAO to York
University. The National Radio Astronomy Observatory is a facility of
the National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. The DSN is operated by JPL/Caltech, under
contract with NASA. This research has made use of the United States
Naval Observatory (USNO) Radio Reference Frame Image Database (RRFID).
We have also made use of NASA's Astrophysics Data System Abstract
Service, developed and maintained at SAO. Jeff Cadieux and Julie Tome
helped with the data reduction during their tenure as students at York
University. Finally, we thank the anonymous referee for useful comments.
NR 51
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUL
PY 2012
VL 201
IS 1
AR 7
DI 10.1088/0067-0049/201/1/7
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956JZ
UT WOS:000305087200007
ER
PT J
AU Lebach, DE
Bartel, N
Bietenholz, MF
Campbell, RM
Gordon, D
Lederman, JI
Lestrade, JF
Ransom, RR
Ratner, MI
Shapiro, II
AF Lebach, D. E.
Bartel, N.
Bietenholz, M. F.
Campbell, R. M.
Gordon, D.
Lederman, J. I.
Lestrade, J. -F.
Ransom, R. R.
Ratner, M. I.
Shapiro, I. I.
TI VLBI FOR GRAVITY PROBE B. IV. A NEW ASTROMETRIC ANALYSIS TECHNIQUE AND A
COMPARISON WITH RESULTS FROM OTHER TECHNIQUES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE astrometry; binaries: close; radio continuum: stars; stars: activity;
stars: imaging; stars: individual (IM Pegasi); techniques:
interferometric
ID BASE-LINE INTERFEROMETRY; RADIO-SOURCES; MAPPING FUNCTIONS; POSITION;
GEODESY; EPHEMERIDES
AB When very long baseline interferometry (VLBI) observations are used to determine the position or motion of a radio source relative to reference sources nearby on the sky, the astrometric information is usually obtained via (1) phase-referenced maps or (2) parametric model fits to measured fringe phases or multiband delays. In this paper, we describe a "merged" analysis technique which combines some of the most important advantages of these other two approaches. In particular, our merged technique combines the superior model-correction capabilities of parametric model fits with the ability of phase-referenced maps to yield astrometric measurements of sources that are too weak to be used in parametric model fits. We compare the results from this merged technique with the results from phase-referenced maps and from parametric model fits in the analysis of astrometric VLBI observations of the radio-bright star IM Pegasi (HR 8703) and the radio source B2252+ 172 nearby on the sky. In these studies we use central-core components of radio sources 3C 454.3 and B2250+ 194 as our positional references. We obtain astrometric results for IMPeg with our merged technique even when the source is too weak to be used in parametric model fits, and we find that our merged technique yields astrometric results superior to the phase-referenced mapping technique. We used our merged technique to estimate the proper motion and other astrometric parameters of IM Peg in support of the NASA/Stanford Gravity Probe B mission.
C1 [Lebach, D. E.; Ratner, M. I.; Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bartel, N.; Bietenholz, M. F.; Lederman, J. I.; Ransom, R. R.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Campbell, R. M.] Joint Inst VLBI Europe, NL-7991 PD Dwingeloo, Netherlands.
[Gordon, D.] NASA, NVI Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lestrade, J. -F.] CNRS, Observ Paris, F-75014 Paris, France.
[Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
[Ransom, R. R.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada.
RP Lebach, DE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NASA [NAS8-39225]; Stanford University [PR 6750]; Smithsonian
Institution; York University
FX We thank N. Nunes for developing the graphical software package we used
to phase-connect our VLBI data. We thank the VLBI group of NASA's
Goddard Space Flight Center, and L. Petrov in particular, for providing
technical support and information. We are also grateful to the many
people involved in our campaign of VLBI observations who went above and
beyond the call of duty, including S. Dains, C. Garcia Miro, E. Moll,
and L. Cameron. We thank C. Jacobs and O. Sovers for information about
the coordinates of the three 70 m NASA DSN antennas used in our
observations, and R. C. Walker for information about the VLA
coordinates. We thank J. L. Davis and S. S. Shapiro for their
information and insight on the use of our Kalman-filter estimator
(SOLVK). Finally, we thank R. C. Walker, K. Desai, and E. Greisen for
their support in our use of AIPS. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. This
research made use ofNASA'sAstrophysicsData System, whichwas conceived,
developed, and continues to be operated by the Smithsonian Astrophysical
Observatory at the Harvard-Smithsonian Center for Astrophysics. Our work
was supported by NASA prime award NAS8-39225, Stanford University
subaward PR 6750, the Smithsonian Institution, and York University.
NR 46
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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 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUL
PY 2012
VL 201
IS 1
AR 4
DI 10.1088/0067-0049/201/1/4
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956JZ
UT WOS:000305087200004
ER
PT J
AU Ransom, RR
Bartel, N
Bietenholz, MF
Lebach, DE
Lestrade, JF
Ratner, MI
Shapiro, II
AF Ransom, R. R.
Bartel, N.
Bietenholz, M. F.
Lebach, D. E.
Lestrade, J. -F.
Ratner, M. I.
Shapiro, I. I.
TI VLBI FOR GRAVITY PROBE B. VI. THE ORBIT OF IM PEGASI AND THE LOCATION OF
THE SOURCE OF RADIO EMISSION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: close; radio continuum: stars; stars: activity; stars:
imaging; stars: individual (IM Pegasi); techniques: interferometric
ID RS-CANUM-VENATICORUM; CLOSE BINARY STARS; GUIDE STAR; SYSTEMS; MISSION;
ALGOL; POSITION; ASTROMETRY
AB We present a physical interpretation for the locations of the sources of radio emission in IM Pegasi (IM Peg, HR 8703), the guide star for the NASA/ Stanford relativity mission Gravity Probe B. This emission is seen in each of our 35 epochs of 8.4 GHz very long baseline interferometry observations taken from 1997 to 2005. We found that the mean position of the radio emission is at or near the projected center of the primary to within about 27% of its radius, identifying this active star as the radio emitter. The positions of the radio brightness peaks are scattered across the disk of the primary and slightly beyond, preferentially along an axis with position angle, P. A.=-38 degrees +/- 8 degrees, which is closely aligned with the sky projections of the orbit normal (P. A. = -49 degrees.5 +/- 8 degrees.6) and the expected spin axis of the primary. Comparison with simulations suggests that brightness peaks are 3.6+ 0.4-0.7 times more likely to occur (per unit surface area) near the pole regions of the primary (latitude, |lambda| >= 70 degrees) than near the equator (|lambda| <= 20 degrees.), and to also occur close to the surface with similar to 2/3 of them at altitudes not higher than 25% of the radius of the primary.
C1 [Ransom, R. R.; Bartel, N.; Bietenholz, M. F.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Lebach, D. E.; Ratner, M. I.; Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lestrade, J. -F.] Observ Paris, LERMA, F-75014 Paris, France.
[Ransom, R. R.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada.
[Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
RP Ransom, RR (reprint author), Okanagan Coll, 583 Duncan Ave W, Penticton, BC V2A 2K8, Canada.
FU NASA; Stanford University; SAO
FX We thank the anonymous referee for a constructive review of the paper
and for comments helpful in the preparation of the final manuscript.
This research was primarily supported by NASA, through a contract with
Stanford University to SAO, and a subcontract from SAO to York
University. The VLBA is an instrument of the National Radio Astronomy
Observatory (NRAO), a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
The DSN is operated by JPL/Caltech, under contract with NASA. We have
made use of NASA's Astrophysics Data System Abstract Service, developed
and maintained at SAO. Jeff Cadieux and Julie Tome assisted with the
reduction of the VLBI data during their tenures as students at York
University.
NR 39
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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 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUL
PY 2012
VL 201
IS 1
AR 6
DI 10.1088/0067-0049/201/1/6
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956JZ
UT WOS:000305087200006
ER
PT J
AU Ransom, RR
Bartel, N
Bietenholz, MF
Lebach, DE
Lederman, JI
Luca, P
Ratner, MI
Shapiro, II
AF Ransom, R. R.
Bartel, N.
Bietenholz, M. F.
Lebach, D. E.
Lederman, J. I.
Luca, P.
Ratner, M. I.
Shapiro, I. I.
TI VLBI FOR GRAVITY PROBE B. II. MONITORING OF THE STRUCTURE OF THE
REFERENCE SOURCES 3C 454.3, B2250+194, AND B2252+172
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: active; galaxies: individual (B2252+172); galaxies: jets;
quasars: individual (3C 454.3, B2250+194); radio continuum: galaxies;
techniques: interferometric
ID ACTIVE GALACTIC NUCLEI; CELESTIAL REFERENCE FRAME; BASE-LINE
INTERFEROMETRY; RADIO-SOURCES; OPTICAL-IDENTIFICATION; QUASARS;
SPECTRUM; ASTROMETRY; EMISSION; POSITION
AB We used 8.4 GHz very long baseline interferometry images obtained at up to 35 epochs between 1997 and 2005 to examine the radio structures of the main reference source, 3C 454.3, and two secondary reference sources, B2250+ 194 and B2252+ 172, for the guide star for the NASA/Stanford relativity mission Gravity Probe B ( GP-B). For one epoch in 2004 May, we also obtained images at 5.0 and 15.4 GHz. The 35 8.4 GHz images for quasar 3C 454.3 confirm a complex, evolving, core-jet structure. We identified at each epoch a component, C1, near the easternmost edge of the core region. Simulations of the core region showed that C1 is located, on average, 0.18 +/- 0.06 mas west of the unresolved "core" identified in 43 GHz images. We also identified in 3C 454.3 at 8.4 GHz several additional components that moved away from C1 with proper motions ranging in magnitude between 0.9 c and 5 c. The detailed motions of the components exhibit two distinct bends in the jet axis located similar to 3 and similar to 5.5 mas west of C1. The spectra between 5.0 and 15.4 GHz for the "moving" components are steeper than those for C1. The 8.4 GHz images of B2250+ 194 and B2252+ 172, in contrast to those of 3C 454.3, reveal compact structures. The spectrum between 5.0 and 15.4 GHz for B2250+ 194 is inverted while that for B2252+ 172 is flat. Based on its position near the easternmost edge of the 8.4 GHz radio structure, close spatial association with the 43 GHz core, and relatively flat spectrum, we believe 3C 454.3 component C1 to be the best choice for the ultimate reference point for the GP-B guide star. The compact structures and inverted-to-flat spectra of B2250+ 194 and B2252+ 172 make these objects valuable secondary reference sources.
C1 [Ransom, R. R.; Bartel, N.; Bietenholz, M. F.; Luca, P.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Lebach, D. E.; Ratner, M. I.; Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lederman, J. I.] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 1P3, Canada.
[Ransom, R. R.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada.
[Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
RP Ransom, RR (reprint author), Okanagan Coll, 583 Duncan Ave W, Penticton, BC V2A 2K8, Canada.
NR 44
TC 7
Z9 7
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUL
PY 2012
VL 201
IS 1
AR 2
DI 10.1088/0067-0049/201/1/2
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956JZ
UT WOS:000305087200002
ER
PT J
AU Ratner, MI
Bartel, N
Bietenholz, MF
Lebach, DE
Lestrade, JF
Ransom, RR
Shapiro, II
AF Ratner, M. I.
Bartel, N.
Bietenholz, M. F.
Lebach, D. E.
Lestrade, J. -F.
Ransom, R. R.
Shapiro, I. I.
TI VLBI FOR GRAVITY PROBE B. V. PROPER MOTION AND PARALLAX OF THE GUIDE
STAR, IM PEGASI
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE astrometry; binaries: close; gravitation; radio continuum: stars; stars:
activity; stars: individual (IM Pegasi)
ID BINARY; RADIO; HIPPARCOS
AB We present the principal astrometric results of the very long baseline interferometry (VLBI) program undertaken in support of the Gravity Probe B (GP-B) relativity mission. VLBI observations of the GP-B guide star, the RS CVn binary IM Pegasi (HR 8703), yielded positions at 35 epochs between 1997 and 2005. We discuss the statistical assumptions behind these results and our methods for estimating the systematic errors. We find the proper motion of IM Peg in an extragalactic reference frame closely related to the International Celestial Reference Frame 2 (ICRF2) to be -20.83 +/- 0.03 +/- 0.09 mas yr(-1) in right ascension and -27.27 +/- 0.03 +/- 0.09 mas yr-1 in declination. For each component, the first uncertainty is the statistical standard error and the second is the total standard error (SE) including plausible systematic errors. We also obtain a parallax of 10.37 +/- 0.07 mas (distance: 96.4 +/- 0.7 pc), for which there is no evidence of any significant contribution of systematic error. Our parameter estimates for the similar to 25 day period orbital motion of the stellar radio emission have SEs corresponding to similar to 0.10 mas on the sky in each coordinate. The total SE of our estimate of IM Peg's proper motion is similar to 30% smaller than the accuracy goal set by the GP-B project before launch: 0.14 mas yr(-1) for each coordinate of IM Peg's proper motion. Our results ensure that the uncertainty in IM Peg's proper motion makes only a very small contribution to the uncertainty of the GP-B relativity tests.
C1 [Ratner, M. I.; Lebach, D. E.; Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bartel, N.; Bietenholz, M. F.; Ransom, R. R.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Lestrade, J. -F.] CNRS, Observ Paris, F-75014 Paris, France.
[Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada.
RP Ratner, MI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NASA; Stanford University to the Smithsonian Astrophysical Observatory
(SAO); Swiss Federal Institute of Technology Zurich (ETH-Z); Tennessee
State University; University of Pittsburgh; U.S. Naval Observatory
FX This research was primarily supported by NASA, through a contract from
Stanford University to the Smithsonian Astrophysical Observatory (SAO),
as well as a major subcontract from SAO to York University, and lesser
subcontracts from SAO to the Swiss Federal Institute of Technology
Zurich (ETH-Z), Tennessee State University, the University of
Pittsburgh, and the U.S. Naval Observatory. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. The DSN is
operated by JPL/Caltech, under contract with NASA. We have made use of
NASA's Astrophysics Data System Abstract Service, initiated, developed,
and maintained at SAO.
NR 26
TC 9
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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
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUL
PY 2012
VL 201
IS 1
AR 5
DI 10.1088/0067-0049/201/1/5
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956JZ
UT WOS:000305087200005
ER
PT J
AU Shapiro, II
Bartel, N
Bietenholz, MF
Lebach, DE
Lestrade, JF
Ransom, RR
Ratner, MI
AF Shapiro, I. I.
Bartel, N.
Bietenholz, M. F.
Lebach, D. E.
Lestrade, J. -F.
Ransom, R. R.
Ratner, M. I.
TI VLBI FOR GRAVITY PROBE B. I. OVERVIEW
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE astrometry; binaries: close; gravitation; radio continuum: galaxies;
radio continuum: stars; stars: activity; stars: individual (IM Pegasi);
techniques: interferometric
ID BINARY IM-PEGASI; RADIO INTERFEROMETRY; ASTROMETRY; POSITION; STARS;
MISSION; CATALOG
AB We describe the NASA/Stanford gyroscope relativity mission, Gravity Probe B (GP-B), and provide an overview of the following series of six astrometric and astrophysical papers that report on our radio observations and analyses made in support of this mission. The main goal of this 8.5 year program of differential very long baseline interferometry astrometry was to determine the proper motion of the guide star of the GP-B mission, the RS CVn binary IM Pegasi (IM Peg; HR 8703). This proper motion is determined with respect to compact, extragalactic reference sources. The results are -20.833 +/- 0.090 mas yr(-1) and -27.267 +/- 0.095 mas yr(-1) for, respectively, the right ascension and declination, in local Cartesian coordinates, of IM Peg's proper motion, and 10.370 +/- 0.074 mas (i. e., 96.43 +/- 0.69 pc) for its parallax (and distance). Each quoted uncertainty is meant to represent an similar to 70% confidence interval that includes the estimated contribution from systematic error. These results are accurate enough not to discernibly degrade the GP-B estimates of its gyroscopes' relativistic precessions: the frame-dragging and geodetic effects.
C1 [Shapiro, I. I.; Lebach, D. E.; Ratner, M. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bartel, N.; Bietenholz, M. F.; Ransom, R. R.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Lestrade, J. -F.] CNRS, Observ Paris, F-75014 Paris, France.
[Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
[Ransom, R. R.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Radio Astrophys Observ, Penticton, BC V2A 6K3, Canada.
RP Shapiro, II (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 28
TC 10
Z9 10
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUL
PY 2012
VL 201
IS 1
AR 1
DI 10.1088/0067-0049/201/1/1
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956JZ
UT WOS:000305087200001
ER
PT J
AU Eberhard, WG
Hesselberg, T
AF Eberhard, William G.
Hesselberg, Thomas
TI Cues that Spiders (Araneae: Araneidae, Tetragnathidae) Use to Build
Orbs: Lapses in Attention to One Set of Cues because of Dissonance with
Others?
SO ETHOLOGY
LA English
DT Article
ID WEB-CONSTRUCTION; WEAVING SPIDERS; REGENERATED LEGS; CONSEQUENCES;
ORIENTATION; PATTERNS; BEHAVIOR; GEOMETRY; GRAVITY; DESIGN
AB Even for small animals such as spiders, behavioral decisions are sometimes influenced by multiple cues. Orb webs constitute exquisitely precise records of the stimuli the spider experienced and the decisions that it made while building its web. In addition, because spiders appear to sense their webs largely by touch, direct behavioral observations can determine which stimuli they probably sense. Previous studies have shown that when an orb-weaving spider decides how far apart to space successive sticky lines during orb construction, it responds to at least five different kinds of stimuli, all of which apparently use a cue from the web, the location of the previous, inner loop of sticky spiral (IL location), as a point of reference. Here we show that two additional cues from the web, which are related to the position of the temporary spiral (TS), also influence sticky spiral spacing. A combination of direct observations of spider movements, analyses of complete and partially complete webs, and responses to experimental modifications of the web of two species in different families, Micrathena duodecimspinosa (Araneidae) and Leucauge mariana (Tetragnathidae), indicate that both the TS-IL distance itself and the short-term memory of the change in TS-IL distance compared with that on other recently encountered radii correlate with sticky spiral spacing. When the TS-IL distance was large, the spiders apparently ceased to attend to other cues. Thus, even the relatively stereotyped behavior of orb construction includes variation that stems from attention-like mental processes.
C1 [Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica.
[Hesselberg, Thomas] Univ Oxford, Dept Zool, Oxford OX1 3PS, England.
RP Eberhard, WG (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
EM william.eberhard@gmail.com
FU Smithsonian Tropical Research Institute; Universidad de Costa Rica
FX We thank David Zed for help with statistics and two anonymous reviewers
for their useful comments on an earlier version of this manuscript. We
also thank the Smithsonian Tropical Research Institute and the
Universidad de Costa Rica for financial support.
NR 37
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U1 1
U2 26
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0179-1613
J9 ETHOLOGY
JI Ethology
PD JUL
PY 2012
VL 118
IS 7
BP 610
EP 620
DI 10.1111/j.1439-0310.2012.02048.x
PG 11
WC Psychology, Biological; Behavioral Sciences; Zoology
SC Psychology; Behavioral Sciences; Zoology
GA 956XR
UT WOS:000305123400002
ER
PT J
AU Li, Y
Lin, J
AF Li, Y.
Lin, J.
TI Acceleration of Electrons and Protons in Reconnecting Current Sheets
Including Single or Multiple X-points
SO SOLAR PHYSICS
LA English
DT Article
DE Solar flares; Magnetic reconnection; Current sheet; Energetic particles
ID CORONAL MASS EJECTIONS; PARTICLE-ACCELERATION; MAGNETIC RECONNECTION;
SOLAR-FLARES; ENERGY-SPECTRUM; 2-RIBBON FLARES; FIELD; MODEL;
SEPARATION; TURBULENCE
AB Kinematic characteristics of electrons and protons in the magnetic reconnecting current sheet in the presence of a guide field are investigated. Particle trajectories are calculated for different values of the guide field by a test-particle calculation. The relationship between the final energy and the initial position has also been studied. We found that the addition of a guide field not only allows particles to get more energy and not only results in the separation of electrons and protons, but also causes the reconnecting electric field to selectively accelerate electrons and protons for different initial positions. The energy spectrum eventually obtained is the common power-law spectrum, and as the guide field increases, the index for the spectrum of electrons decreases rapidly. However, for a weak background magnetic field, proton spectra are not very sensitive to the guide field; but for a strong background field, the dependence of the spectrum index is similar to the electron spectrum. Meanwhile, kinematic characteristics of the accelerated particles in the current sheet including multiple X-points and O-points were also investigated. The result indicates that the existence of the multiple X- and O-points helps particles trapped in the accelerating region to gain more energy, and yields the double or multiple power-law feature.
C1 [Li, Y.; Lin, J.] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Peoples R China.
[Li, Y.] Chinese Acad Sci, Grad Univ, Beijing 10049, Peoples R China.
[Lin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Li, Y (reprint author), Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Peoples R China.
EM liyan821@ynao.ac.cn
RI LIN, JUN/B-9890-2017
FU Program 973 grant [2011CB811403]; NSFC [10873030, 10903027]; Yunnan
Science Foundation of China [2009CD120]; NASA [NNX11AB61G]; Smithsonian
Institution
FX We thank the anonymous referee for constructive comments and suggestions
that much improved the original version of the manuscript. This work was
supported by Program 973 grant 2011CB811403, NSFC grant 10873030,
10903027, and Yunnan Science Foundation of China grant 2009CD120. J.L.
acknowledge support from NASA grant NNX11AB61G to SAO, and from a grant
from the Smithsonian Institution Sprague Endowment Fund during FY10.
NR 59
TC 14
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U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD JUL
PY 2012
VL 279
IS 1
BP 91
EP 113
DI 10.1007/s11207-012-9956-1
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 957AK
UT WOS:000305130700006
ER
PT J
AU Le Chat, G
Issautier, K
Meyer-Vernet, N
AF Le Chat, G.
Issautier, K.
Meyer-Vernet, N.
TI The Solar Wind Energy Flux
SO SOLAR PHYSICS
LA English
DT Article
DE Plasma physics; Solar wind; Energy flux
ID CORONAL MASS EJECTIONS; PROTON TEMPERATURE; PLASMA-EXPERIMENT; CYCLE;
INVARIANCE; SPACECRAFT; VELOCITY
AB The solar-wind energy flux measured near the Ecliptic is known to be independent of the solar-wind speed. Using plasma data from Helios, Ulysses, and Wind covering a large range of latitudes and time, we show that the solar-wind energy flux is independent of the solar-wind speed and latitude within 10 %, and that this quantity varies weakly over the solar cycle. In other words the energy flux appears as a global solar constant. We also show that the very high-speed solar wind (V (SW)> 700 km s(-1)) has the same mean energy flux as the slower wind (V (SW)< 700 km s(-1)), but with a different histogram. We use this result to deduce a relation between the solar-wind speed and density, which formalizes the anti-correlation between these quantities.
C1 [Le Chat, G.; Issautier, K.; Meyer-Vernet, N.] Univ Paris Diderot, LESIA, Observ Paris, CNRS,UPMC, F-92195 Meudon, France.
[Le Chat, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
RP Le Chat, G (reprint author), Univ Paris Diderot, LESIA, Observ Paris, CNRS,UPMC, 5 Pl Jules Janssen, F-92195 Meudon, France.
EM gaetan.lechat@obspm.fr
NR 29
TC 10
Z9 10
U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD JUL
PY 2012
VL 279
IS 1
BP 197
EP 205
DI 10.1007/s11207-012-9967-y
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 957AK
UT WOS:000305130700011
ER
PT J
AU Hao, G
Boyle, M
Zhou, L
Duan, Y
AF Hao, G.
Boyle, M.
Zhou, L.
Duan, Y.
TI Novel autotransporters encoded by the citrus huanglongbing bacterium,
'Candidatus Liberibacter asiaticus'
SO PHYTOPATHOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the American-Phytopathological-Society (APS)
CY AUG 04-08, 2012
CL Providence, RI
SP Amer Phytopathol Soc (APS)
C1 [Hao, G.; Zhou, L.; Duan, Y.] US Hort Res Lab, Ft Pierce, FL USA.
[Boyle, M.] Smithsonian Marine Stn, Ft Pierce, FL USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER PHYTOPATHOLOGICAL SOC
PI ST PAUL
PA 3340 PILOT KNOB ROAD, ST PAUL, MN 55121 USA
SN 0031-949X
J9 PHYTOPATHOLOGY
JI Phytopathology
PD JUL
PY 2012
VL 102
IS 7
SU 4
BP 50
EP 50
PG 1
WC Plant Sciences
SC Plant Sciences
GA 196SX
UT WOS:000322797800265
ER
PT J
AU Quinn, EA
Largado, F
Power, M
Kuzawa, CW
AF Quinn, Elizabeth A.
Largado, Fe
Power, Michael
Kuzawa, Christopher W.
TI Predictors of breast milk macronutrient composition in filipino mothers
SO AMERICAN JOURNAL OF HUMAN BIOLOGY
LA English
DT Article
ID FATTY-ACID-COMPOSITION; RURAL AFRICAN WOMEN; LATER OBESITY RISK;
BODY-MASS INDEX; LACTATION PERFORMANCE; CALORIC RESTRICTION; HOLSTEIN
HEIFERS; SWEDISH MOTHERS; NOURISHED WOMEN; ENERGY CONTENTS
AB Objectives: There is increasing evidence that breastfeeding has long-term effects on offspring biology and health, which has heightened interest in understanding the extent of variation in breast milk composition and its underlying determinants. Here, we report variation in milk macronutrient composition in a well-characterized cohort of young Filipino mothers and test underlying maternal predictors of this variation. Methods: Morning breast milk samples, anthropometrics, dietary recalls, and other interview data were collected in 102 Filipino young breastfeeding mothers (age range 24.625.4 years) living in Cebu City, Philippines. Milk samples were analyzed for protein, fat, sugar, and milk energy density. Regression models were used to test associations between milk macronutrient composition and maternal diet, body composition, breastfeeding duration, and feeding frequency. Results: Consistent with past studies, milk fat and energy increased with duration of breastfeeding; there were no associations between maternal diet or percent body fat and milk composition with the exception of a modest, inverse association between maternal adiposity and milk sugar content. Conclusions: The relative lack of associations between maternal diet or body composition and milk composition at Cebu is consistent with past studies and suggests that milk composition may be buffered against fluctuations in maternal dietary intake or nutritional status. We speculate that the tendency for milk composition to vary between populations faced with different nutritional ecologies, but to show minimal responsiveness to intake during lactation, may enhance the reliability of milk composition as a stable intergenerational cue of typical local environmental quality. Am. J. Hum. Biol. 2012. (C) 2012 Wiley Periodicals, Inc.
C1 [Quinn, Elizabeth A.] Washington Univ, Dept Anthropol, St Louis, MO 63130 USA.
[Largado, Fe] Univ San Carlos, Off Populat Studies, Cebu, Philippines.
[Power, Michael] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA.
[Kuzawa, Christopher W.] Northwestern Univ, Dept Anthropol, Evanston, IL 60208 USA.
[Kuzawa, Christopher W.] Northwestern Univ, Cells Soc 2, Inst Policy Res, Evanston, IL USA.
RP Quinn, EA (reprint author), Washington Univ, Dept Anthropol, St Louis, MO 63130 USA.
EM equinn@artsci.wustl.edu
OI Power, Michael/0000-0002-6120-3528
FU National Science Foundation [0726231, BCS-0746320]
FX Contract grant sponsor: National Science Foundation (Doctoral
Dissertation Improvement); Contract grant number: 0726231; Contract
grant sponsor: National Science Foundation; Contract grant number:
BCS-0746320.
NR 84
TC 20
Z9 21
U1 2
U2 15
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1042-0533
J9 AM J HUM BIOL
JI Am. J. Hum. Biol.
PD JUL-AUG
PY 2012
VL 24
IS 4
BP 533
EP 540
DI 10.1002/ajhb.22266
PG 8
WC Anthropology; Biology
SC Anthropology; Life Sciences & Biomedicine - Other Topics
GA 954ZI
UT WOS:000304986300021
PM 22434662
ER
PT J
AU Hultgren, KM
Duffy, JE
AF Hultgren, Kristin M.
Duffy, J. Emmett
TI Phylogenetic community ecology and the role of social dominance in
sponge-dwelling shrimp
SO ECOLOGY LETTERS
LA English
DT Article
DE Competition; coral reefs; eusociality; habitat filtering; phylogenetic
community ecology; snapping shrimp; spatial scale; Synalpheus
ID SNAPPING SHRIMPS; ALPHEIDAE SYNALPHEUS; SPATIAL SCALES; TRAIT;
ASSEMBLAGES; EUSOCIALITY; EVOLUTION; PATTERNS; FOREST; SIGNAL
AB When functional traits are evolutionarily conserved, phylogenetic relatedness can serve as a proxy for ecological similarity to examine whether functional differences among species mediate community assembly. Using phylogenetic- and trait-based analyses, we demonstrate that sponge-dwelling shrimp (Synalpheus) assemblages are structured by size-based habitat filtering, interacting with competitive exclusion mediated by social system. Most shrimp communities were more closely related and/or more similar in size than randomized communities, consistent with habitat filtering facilitated by phylogenetically conserved body size. Those sponges with greater space heterogeneity hosted shrimp communities with greater size diversity, corroborating the importance of size in niche use. However, communities containing eusocial shrimp which cooperatively defend territories were less phylogenetically related and less similar in size, suggesting that eusociality enhances competitive ability and drives competitive exclusion. Our analyses demonstrate that community assembly in this diverse system occurs via traits mediating niche use and differential competitive ability.
C1 [Hultgren, Kristin M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Duffy, J. Emmett] Virginia Inst Marine Sci, Gloucester Pt, VA 23062 USA.
RP Hultgren, KM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 163,POB 37012, Washington, DC 20013 USA.
EM hultgrenk@si.edu
NR 46
TC 9
Z9 9
U1 3
U2 40
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1461-023X
EI 1461-0248
J9 ECOL LETT
JI Ecol. Lett.
PD JUL
PY 2012
VL 15
IS 7
BP 704
EP 713
DI 10.1111/j.1461-0248.2012.01788.x
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 955EN
UT WOS:000305000000009
PM 22548770
ER
PT J
AU White, KP
Langley, JA
Cahoon, DR
Megonigal, JP
AF White, K. P.
Langley, J. A.
Cahoon, D. R.
Megonigal, J. P.
TI C-3 and C-4 Biomass Allocation Responses to Elevated CO2 and Nitrogen:
Contrasting Resource Capture Strategies
SO ESTUARIES AND COASTS
LA English
DT Article
DE Biomass; Chesapeake Bay; Productivity; Sea level rise; Tidal marsh;
Turnover
ID ATMOSPHERIC CO2; CHESAPEAKE BAY; SEA-LEVEL; INCREASES CARBON; GROUND
BIOMASS; FINE ROOTS; MARSH; ENRICHMENT; COMPETITION; DYNAMICS
AB Plants alter biomass allocation to optimize resource capture. Plant strategy for resource capture may have important implications in intertidal marshes, where soil nitrogen (N) levels and atmospheric carbon dioxide (CO2) are changing. We conducted a factorial manipulation of atmospheric CO2 (ambient and ambient + 340 ppm) and soil N (ambient and ambient + 25 g m(-2) year(-1)) in an intertidal marsh composed of common North Atlantic C-3 and C-4 species. Estimation of C-3 stem turnover was used to adjust aboveground C-3 productivity, and fine root productivity was partitioned into C-3-C-4 functional groups by isotopic analysis. The results suggest that the plants follow resource capture theory. The C-3 species increased aboveground productivity under the added N and elevated CO2 treatment (P < 0.0001), but did not under either added N or elevated CO2 alone. C-3 fine root production decreased with added N (P < 0.0001), but fine roots increased under elevated CO2 (P = 0.0481). The C-4 species increased growth under high N availability both above- and belowground, but that stimulation was diminished under elevated CO2. The results suggest that the marsh vegetation allocates biomass according to resource capture at the individual plant level rather than for optimal ecosystem viability in regards to biomass influence over the processes that maintain soil surface elevation in equilibrium with sea level.
C1 [Langley, J. A.; Megonigal, J. P.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[White, K. P.] Univ Idaho, Dept Forest Ecol & Biogeosci, Moscow, ID 83844 USA.
[White, K. P.] Univ Idaho, Dept Stat Sci, Moscow, ID 83844 USA.
[Langley, J. A.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA.
[Cahoon, D. R.] US Geol Survey, Patuxent Wildlife Res Ctr, Beltsville, MD 20705 USA.
RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM adam.langley@villanova.edu; megonigalp@si.edu
FU USGS [06ERAG0011]; US Department of Energy [DE-FG02-97ER62458]; US
Department of Energy's Office of Science (BER) through the Coastal
Center of the National Institute of Climate Change Research at Tulane
University; National Science Foundation [DEB-0950080]; Research
Experience for Undergraduates (REU) program; Smithsonian Institution
FX We thank J. Duls, J. Keller, M. Sigrist, G. Peresta, B. Drake, E. Sage,
A. Martin, D. McKinley, and N. Mudd for the construction and maintenance
of the field site at the Smithsonian Climate Change Facility. The field
study was supported by the USGS Global Change Research Program
(cooperative agreement 06ERAG0011), the US Department of Energy
(DE-FG02-97ER62458), US Department of Energy's Office of Science (BER)
through the Coastal Center of the National Institute of Climate Change
Research at Tulane University, the National Science Foundation's
Long-term Research Environmental Biology program (DEB-0950080) and
Research Experience for Undergraduates (REU) program, and the
Smithsonian Institution. Use of trade, product, or firm names does not
imply endorsement by the US Government. We also thank the anonymous
reviewers for the comments that greatly improved this paper.
NR 42
TC 5
Z9 5
U1 0
U2 35
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1559-2723
J9 ESTUAR COAST
JI Estuaries Coasts
PD JUL
PY 2012
VL 35
IS 4
BP 1028
EP 1035
DI 10.1007/s12237-012-9500-4
PG 8
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 951CF
UT WOS:000304697600009
ER
PT J
AU Janiak, DS
Osman, RW
AF Janiak, Dean S.
Osman, Richard W.
TI Experimental Effects of the Grass Shrimp, Palaemonetes pugio, on
Hard-Substrate Communities in Chesapeake Bay and an Adjacent Coastal
Bay, USA
SO ESTUARIES AND COASTS
LA English
DT Article
DE Palaemonetes pugio; Chesapeake Bay; Benthos; Hard-substrate; Predation
ID SPARTINA-ALTERNIFLORA; ESTUARINE HABITATS; RUPPIA-MARITIMA;
ZOSTERA-MARINA; PREDATION RISK; SALT-MARSH; ABUNDANCE; HOLTHUIS; PREY;
MEIOFAUNA
AB With increased shoreline hardening and development, it is important to understand the ecological processes occurring in these and adjacent coastal habitats. A common species found associated with these hard-substrate habitats in Chesapeake Bay is the grass shrimp, Palaemonetes pugio. Caging experiments were conducted from June to August 2010 to examine the effects of shrimp on the recruitment and development of hard-substrate communities. Experiments were conducted at two low-salinity sites within Chesapeake Bay and one high-salinity site in an adjacent coastal bay in Virginia. The addition of grass shrimp reduced recruitment of polychaetes and scyphistomae of the sea nettle, Chrysaora quinquecirrha, and increased recruitment of encrusting bryozoans and the oyster, Crassostrea virginica. After 12 weeks, sea nettles at one low-salinity site, dominated predator-exclusion treatments. At the high-salinity site, oysters dominated when shrimp were present. Although it is unclear whether the results of short-term caging studies can be applied across larger temporal and spatial scales, the significant effects of grass shrimp on two important Chesapeake Bay species suggests that increases in hard-substrate habitat could have broader impacts within this and other systems.
C1 [Janiak, Dean S.; Osman, Richard W.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Janiak, DS (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM janiakd@si.edu
FU Smithsonian Marine Science Network
FX This work was supported by funds from the Smithsonian Marine Science
Network. We would like to thank the VIMS Eastern Shore lab and the
Morgan State University Estuarine Research Center for their assistance
and allowing us to conduct experiments at their sites. We would also
like to thank CR Janiak for field assistance, useful comments on an
earlier draft, and the design of Fig. 1. The manuscript benefited
greatly from the comments of four anonymous reviewers.
NR 38
TC 1
Z9 1
U1 1
U2 11
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1559-2723
J9 ESTUAR COAST
JI Estuaries Coasts
PD JUL
PY 2012
VL 35
IS 4
BP 1128
EP 1136
DI 10.1007/s12237-012-9486-y
PG 9
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 951CF
UT WOS:000304697600018
ER
PT J
AU Sepulveda, AJ
Lowe, WH
Marra, PP
AF Sepulveda, Adam J.
Lowe, Winsor H.
Marra, Peter P.
TI Using stable isotopes to test for trophic niche partitioning: a case
study with stream salamanders and fish
SO FRESHWATER BIOLOGY
LA English
DT Article
DE coexistence; Dicamptodon aterrimus; diet; headwater stream; stable
isotope
ID SIZE-STRUCTURED POPULATIONS; INTRAGUILD PREDATION; BREEDING SALAMANDER;
GENE FLOW; DYNAMICS; ECOLOGY; CANNIBALISM; EVOLUTION; TROUT; WIDTH
AB 1. Stream salamanders and fish often co-occur even though fish prey on and outcompete salamanders. However, the mechanisms that allow palatable salamanders to coexist with fish are unknown. 2. We tested mechanisms in the field that promote coexistence between Idaho giant salamanders (Dicamptodon aterrimus) and stream salmonid fishes in headwater streams. Previous research in this system indicated that salamander dispersal did not promote coexistence with fish. We tested the hypothesis that D center dot aterrimus shift their diet when they occur with fish, facilitating coexistence through local niche partitioning. 3. We used nitrogen and carbon stable isotopes to describe the trophic niche of D center dot aterrimus and fish in three co-occurring populations of salamanders and fish and three populations of salamanders without fish. We used two approaches to quantify trophic niche partitioning with stable isotopes: 95% kernel density estimators and isotopic mixing models. 4. We found that salamanders and fish were generalists that consumed aquatic invertebrates primarily, but both species were also cannibalistic and predatory on one another. We also found no support for trophic niche partitioning as a coexistence mechanism because there were no differences in the trophic niche metrics among salamander populations with and without fish. 5. Although we did not identify mechanisms that facilitate salamander and fish coexistence, our empirical data and use of novel approaches to describe the trophic niche did yield important insights on the role of predatorprey interactions and cannibalism as alternative coexistence mechanisms. In addition, we found that 95% kernel estimators are a simple and robust method to describe population-level measure of trophic structure.
C1 [Sepulveda, Adam J.] US Geol Survey, No Rocky Mt Sci Ctr, Bozeman, MT 59715 USA.
[Lowe, Winsor H.] Univ Montana, Div Biol Sci, Missoula, MT 59812 USA.
[Marra, Peter P.] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC USA.
RP Sepulveda, AJ (reprint author), US Geol Survey, No Rocky Mt Sci Ctr, 2327 Univ Way,Suite 2, Bozeman, MT 59715 USA.
EM asepulveda@usgs.gov
FU Society for Northwestern Vertebrate Biology; Charlotte Martin
Foundation; Pacific Rivers Council; USGS Montana River Center;
University of Montana
FX This research was funded by grants from the Society for Northwestern
Vertebrate Biology, Charlotte Martin Foundation, the Pacific Rivers
Council, USGS Montana River Center and the University of Montana. We
thank Christine France (Smithsonian OUSS/MCI Stable Isotope Mass
Spectrometry Facility) for assistance with sample analysis. We thank
Jeff Bates and Joe Hanlon for assisting with fieldwork. This manuscript
benefited from the comments of Steve Corn, Megan Layhee, John Maron,
Scott Mills, Mike Schwartz, Art Woods and Mike Young. Any use of trade,
product or firm names is for descriptive purposes only and does not
imply endorsement by the U.S. Government.
NR 48
TC 3
Z9 3
U1 6
U2 62
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0046-5070
J9 FRESHWATER BIOL
JI Freshw. Biol.
PD JUL
PY 2012
VL 57
IS 7
BP 1399
EP 1409
DI 10.1111/j.1365-2427.2012.02800.x
PG 11
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 955EU
UT WOS:000305000700006
ER
PT J
AU Carvalho, JC
Cardoso, P
Gomes, P
AF Carvalho, Jose C.
Cardoso, Pedro
Gomes, Pedro
TI Determining the relative roles of species replacement and species
richness differences in generating beta-diversity patterns
SO GLOBAL ECOLOGY AND BIOGEOGRAPHY
LA English
DT Article
DE Diversity partitioning; nestedness; richness gradient; similarity
indices; species loss; species replacement
ID DISTANCE DECAY; COMMUNITIES; SIMILARITY; GRADIENTS; TURNOVER
AB Aim To determine the relative contribution of species replacement and species richness differences to the emergence of beta-diversity patterns. Innovation A novel method that disentangles all compositional differences (beta cc, overall beta diversity) in its two components, species replacement (beta-3) and species richness differences (beta rich) is proposed. The performance of the method was studied with ternary plots, which allow visualization of the influence of the relative proportions of shared and unique species of two sites over each metric. The method was also tested in different hypothetical gradients and with real datasets. The novel method was compared with a previous proposal based on the partitioning of overall compositional differences (beta sor) in replacement (beta sim) and nestedness (beta nes). The linear response of beta cc contrasts with the curvilinear response of beta sor to linear gradients of dissimilarity. When two sites did not share any species, beta sim was always 1 and beta-3 only reached 1 when the number of exclusive species of both sites was equal. beta-3 remained constant along gradients of richness differences with constant replacement, while beta sim decreased. beta rich had a linear response to a linear gradient of richness differences with constant species replacement, whereas beta nes exhibited a hump-shaped response. Moreover, beta sim > beta nes when clearly almost all species of one site were lost, whereas beta-3 < beta rich in the same circumstances. Main conclusions The behaviour of the partition of beta cc into beta-3 and beta rich is consistent with the variation of replacement and richness differences. The partitioning of beta sor into beta sim and beta nes overestimates the replacement component and underestimates richness differences. The novel methodology allows the discrimination of different causes of beta-diversity patterns along latitudinal, biogeographic or ecological gradients, by estimating correctly the relative contributions of replacement and richness differences.
C1 [Carvalho, Jose C.; Gomes, Pedro] Univ Minho, Dept Biol, CBMA Mol & Environm Ctr, P-4710057 Braga, Portugal.
[Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
[Cardoso, Pedro] Univ Azores, Azorean Biodivers Grp CITA A, Angra do Heroismo, Portugal.
RP Carvalho, JC (reprint author), Univ Minho, Dept Biol, CBMA Mol & Environm Ctr, Gualtar Campus, P-4710057 Braga, Portugal.
EM josecarvalho@bio.uminho.pt
RI Cardoso, Pedro/A-8820-2008; Gomes, Pedro/I-8348-2015; CBMA,
CBMA/J-1937-2016
OI Cardoso, Pedro/0000-0001-8119-9960; Gomes, Pedro/0000-0002-5595-6988;
CBMA, CBMA/0000-0002-2841-2678
FU Luso-American Foundation; Portuguese Foundation for Science and
Technology [SFRH/BPD/40688/2007]
FX We thank David Currie, Jose A. Diniz-Filho, Joseph A. Veech, Adriano S.
Melo and an anonymous referee for providing helpful suggestions on an
earlier version of the manuscript. J.C.C. express his gratitude to the
Luso-American Foundation for its support (FLAD C&T Links 2010 grant).
P.C. was supported by the Portuguese Foundation for Science and
Technology (SFRH/BPD/40688/2007).
NR 34
TC 60
Z9 61
U1 4
U2 63
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 JUL
PY 2012
VL 21
IS 7
BP 760
EP 771
DI 10.1111/j.1466-8238.2011.00694.x
PG 12
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 957SU
UT WOS:000305183900008
ER
PT J
AU Holland, ND
Kuhnz, LA
Osborn, KJ
AF Holland, Nicholas D.
Kuhnz, Linda A.
Osborn, Karen J.
TI Morphology of a new deep-sea acorn worm (class Enteropneusta, phylum
Hemichordata): A part-time demersal drifter with externalized ovaries
SO JOURNAL OF MORPHOLOGY
LA English
DT Article
DE Hemichordata; Enteropneusta; Torquaratoridae; Allapasus aurantiacus
ID SACCOGLOSSUS-KOWALEVSKII; PACIFIC; GENUS; FLOW
AB Ten individuals of an enteropneust in the family Torquaratoridae were videotaped between 2,900 and 3,500 m in the Eastern Pacificone drifting a few centimeters above the bottom, two exposed on the substrate, and seven partly burrowed, reflecting a bentho-pelagic life style. Here, we describe a captured specimen (26 cm living length) as the holotype of Allapasus aurantiacus n. gen., n. sp. The small proboscis is dome-shaped, and the collar is only slightly wider than deep; both of these body regions are more muscular than in other torquaratorids, which presumably facilitates burrowing. The proboscis complex, in contrast to that of shallow-living enteropneusts, lacks a pericardial sac and is located relatively posteriorly in the proboscis stalk. The stomochord is separated from the main course of the gut by the intervention of a small, plate-like proboscis skeleton lacking posterior horns. The most anterior region of the trunk houses the pharynx, in which the pharyngeal skeletal bars are not connected by synapticles. The postpharyngeal trunk comprises three intestinal regions: prehepatic, hepatic (with conspicuous sacculations), and posthepatic. On either side of the worm, a flap of body wall (lateral wing) runs the entire length of the trunk. The two lateral wings can wrap the body so their edges meet in the dorsal midline, although they often gape open along the pharyngeal region. The holotype is a female (presumably the species is gonochoric) with numerous ovaries located in the lateral wings along the pharyngeal region. Each larger ovary contains a single primary oocyte (up to 1,500 mu m in diameter) and bulges outwards in an epidermal pouch attached to the rest of the body by a slender stalk. Such externalized ovaries are unprecedented in any animal, and nothing is yet known of their role in the reproductive biology of A. aurantiacus. J. Morphol. 2012. (c) 2012 Wiley Periodicals, Inc.
C1 [Holland, Nicholas D.] Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA.
[Kuhnz, Linda A.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA.
[Osborn, Karen J.] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA.
RP Holland, ND (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA.
EM nholland@ucsd.edu
OI Osborn, Karen/0000-0002-4226-9257
FU David and Lucile Packard Foundation
FX Contract grant sponsor: David and Lucile Packard Foundation.
NR 35
TC 11
Z9 11
U1 1
U2 12
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 JUL
PY 2012
VL 273
IS 7
BP 661
EP 671
DI 10.1002/jmor.20013
PG 11
WC Anatomy & Morphology
SC Anatomy & Morphology
GA 953LI
UT WOS:000304868400001
PM 22419131
ER
PT J
AU Saltonstall, K
Lambertini, C
AF Saltonstall, Kristin
Lambertini, Carla
TI The value of repetitive sequences in chloroplast DNA for phylogeographic
inference: A comment on Vachon & Freeland 2011
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Letter
DE chloroplast DNA; microsatellites; minisatellites; mutations; parsimony
networks; phylogeography
ID PHRAGMITES-AUSTRALIS; MICROSATELLITE VARIATION; INTERGENIC REGIONS; GENE
GENEALOGIES; EVOLUTION; POACEAE; POPULATIONS; INDELS; GENOME
AB In a recent Technical Advance article, Vachon and Freeland (2011, Molecular Ecology Resources, 11, 279-285.) evaluate the utility of repetitive and non-repetitive variation in the chloroplast genome for phylogeographic inference, using variation in Phragmites australis as an example. While we agree that repetitive and nonrepetitive regions evolve at different rates and homoplasy can impact results, we disagree with the conclusion that repetitive regions are inappropriate for large-scale phylogeographic studies. Here we describe limitations to the study dataset and analysis, and provide an alternative viewpoint on the utility of repetitive regions for phylogeographic studies.
C1 [Saltonstall, Kristin] Smithsonian Trop Res Inst, Panama City, Panama.
[Lambertini, Carla] Aarhus Univ, Dept Biosci, DK-8000 Aarhus C, Denmark.
RP Saltonstall, K (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama.
EM kristin.saltonstall@aya.yale.edu
RI Lambertini, Carla/H-3655-2014
OI Lambertini, Carla/0000-0002-2450-5455
NR 22
TC 8
Z9 8
U1 0
U2 22
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1755-098X
J9 MOL ECOL RESOUR
JI Mol. Ecol. Resour.
PD JUL
PY 2012
VL 12
IS 4
BP 581
EP 585
DI 10.1111/j.1755-0998.2012.03146.x
PG 5
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 956DO
UT WOS:000305070300002
PM 22533707
ER
PT J
AU Quicke, DLJ
Smith, MA
Janzen, DH
Hallwachs, W
Fernandez-Triana, J
Laurenne, NM
Zaldivar-Riveron, A
Shaw, MR
Broad, GR
Klopfstein, S
Shaw, SR
Hrcek, J
Hebert, PDN
Miller, SE
Rodriguez, JJ
Whitfield, JB
Sharkey, MJ
Sharanowski, BJ
Jussila, R
Gauld, ID
Chesters, D
Vogler, AP
AF Quicke, Donald L. J.
Smith, M. Alex
Janzen, Daniel H.
Hallwachs, Winnie
Fernandez-Triana, Jose
Laurenne, Nina M.
Zaldivar-Riveron, Alejandro
Shaw, Mark R.
Broad, Gavin R.
Klopfstein, Seraina
Shaw, Scott R.
Hrcek, Jan
Hebert, Paul D. N.
Miller, Scott E.
Rodriguez, Josephine J.
Whitfield, James B.
Sharkey, Michael J.
Sharanowski, Barbara J.
Jussila, Reijo
Gauld, Ian D.
Chesters, Douglas
Vogler, Alfried P.
TI Utility of the DNA barcoding gene fragment for parasitic wasp phylogeny
(Hymenoptera: Ichneumonoidea): data release and new measure of taxonomic
congruence
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Article
DE Braconidae; cytochrome oxidase 1; Ichneumonidae; sampling density;
Simpson dominance index; taxonomic retention index
ID PARTIAL 16S RDNA; BRACONIDAE HYMENOPTERA; MOLECULAR PHYLOGENY;
RIBOSOMAL-RNA; 28S GENES; INSECTA; SUBFAMILIES; SEQUENCES; ALIGNMENT;
ORIGIN
AB The enormous cytochrome oxidase subunit I (COI) sequence database being assembled from the various DNA barcoding projects as well as from independent phylogenetic studies constitutes an almost unprecedented amount of data for molecular systematics, in addition to its role in species identification and discovery. As part of a study of the potential of this gene fragment to improve the accuracy of phylogenetic reconstructions, and in particular, exploring the effects of dense taxon sampling, we have assembled a data set for the hyperdiverse, cosmopolitan parasitic wasp superfamily Ichneumonoidea, including the release of 1793 unpublished sequences. Of approximately 84 currently recognized Ichneumonoidea subfamilies, 2500 genera and 41 000 described species, barcoding 5'-COI data were assembled for 4168 putative species-level terminals (many undescribed), representing 671 genera and all but ten of the currently recognized subfamilies. After the removal of identical and near-identical sequences, the 4174 initial sequences were reduced to 3278. We show that when subjected to phylogenetic analysis using both maximum likelihood and parsimony, there is a broad correlation between taxonomic congruence and number of included sequences. We additionally present a new measure of taxonomic congruence based upon the Simpson diversity index, the Simpson dominance index, which gives greater weight to morphologically recognized taxonomic groups (subfamilies) recovered with most representatives in one or a few contiguous groups or subclusters.
C1 [Quicke, Donald L. J.; Chesters, Douglas; Vogler, Alfried P.] Univ London Imperial Coll Sci Technol & Med, Div Biol, London SW7 2AZ, England.
[Quicke, Donald L. J.; Broad, Gavin R.; Gauld, Ian D.; Chesters, Douglas; Vogler, Alfried P.] Nat Hist Museum, Dept Entomol, London SW7 5DB, England.
[Smith, M. Alex; Fernandez-Triana, Jose; Hebert, Paul D. N.] Univ Guelph, Biodivers Inst Ontario, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada.
[Janzen, Daniel H.; Hallwachs, Winnie] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA.
[Fernandez-Triana, Jose] Canadian Natl Collect Insects, Ottawa, ON K1A 0C6, Canada.
[Laurenne, Nina M.] Aalto Univ, Dept Media Technol, Sch Sci, FI-00076 Aalto, Finland.
[Laurenne, Nina M.] Univ Helsinki, Dept Comp Sci, FIN-00014 Helsinki, Finland.
[Zaldivar-Riveron, Alejandro] Univ Nacl Autonoma Mexico, Inst Biol, Colecc Nacl Insectos, Mexico City 04510, DF, Mexico.
[Shaw, Mark R.] Natl Museums Scotland, Edinburgh EH1 1JF, Midlothian, Scotland.
[Klopfstein, Seraina] Nat Hist Museum, Dept Invertebrates, CH-3005 Bern, Switzerland.
[Klopfstein, Seraina] Univ Bern, Inst Zool, Div Community Ecol, CH-3012 Bern, Switzerland.
[Shaw, Scott R.] Univ Wyoming, Dept Renewable Resources 3354, Insect Museum, Laramie, WY 82071 USA.
[Hrcek, Jan] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice 37005, Czech Republic.
[Hrcek, Jan] Univ S Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic.
[Miller, Scott E.] Smithsonian Inst, Washington, DC 20013 USA.
[Rodriguez, Josephine J.] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth NCEAS, Santa Barbara, CA 93101 USA.
[Whitfield, James B.] Univ Illinois, Dept Entomol, Urbana, IL 61801 USA.
[Sharkey, Michael J.] Univ Kentucky, Dept Entomol, Lexington, KY 40546 USA.
[Sharanowski, Barbara J.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA.
RP Quicke, DLJ (reprint author), Univ London Imperial Coll Sci Technol & Med, Div Biol, London SW7 2AZ, England.
EM d.quicke@imperial.ac.uk
RI Smith, M Alex/B-4468-2013; Hebert, Paul/C-4161-2013; Hrcek,
Jan/D-7335-2015; Sharanowski, Barbara/I-2176-2016;
OI Smith, M Alex/0000-0002-8650-2575; Hebert, Paul/0000-0002-3081-6700;
Hrcek, Jan/0000-0003-0711-6447; Sharanowski,
Barbara/0000-0002-8085-5900; Quicke, Donald/0000-0003-4471-6775; Miller,
Scott/0000-0002-4138-1378
FU NSF [BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730, 0515699,
DEB-0841885, DEB-0542864]; Grant Agency of the Czech Republic
[206/09/0115]; NERC [NDC519583, NER/S/A/2006/14013]; CONABIO [HB033];
CONACyT [511]; Canadian Barcode of Life Research Network from Genome
Canada through the Ontario Genomics Institute; NSERC
FX We would like to thank the following people who kindly provided
additional specimens for sequencing: Andy Deans (North Carolina State
University, Raleigh), Brian Fisher and Robert Zuparko (California
Academy of Sciences, San Francisco), Kees van Achterberg (Leiden). This
research was supported by specimens and barcodes obtained under the
following grants: NSF grants BSR 9024770 and DEB 9306296, 9400829,
9705072, 0072730, and 0515699 to D. H. Janzen (as described in Janzen et
al. 2009); NSF grant (DEB-0841885) to G. Weiblen; NSF grant DEB-0542864
(TIGER Project) to M. J. Sharkey; Grant Agency of the Czech Republic
grant 206/09/0115 to V. Novotny; NERC grant NDC519583 to D. L. J. Quicke
(and A. Purvis); CONABIO (HB033), CONACyT grants (Red Tematica de
Codigos de Barra de la Vida, Proyecto Ciencia Basica CONACyT no. 511) to
AZR; MAS was supported by Canadian Barcode of Life Research Network from
Genome Canada through the Ontario Genomics Institute and an NSERC
Discovery Grant. D. Chesters was funded by NERC Case studentship
NER/S/A/2006/14013.
NR 52
TC 16
Z9 18
U1 1
U2 34
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1755-098X
J9 MOL ECOL RESOUR
JI Mol. Ecol. Resour.
PD JUL
PY 2012
VL 12
IS 4
BP 676
EP 685
DI 10.1111/j.1755-0998.2012.03143.x
PG 10
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 956DO
UT WOS:000305070300013
PM 22487608
ER
PT J
AU Kara, EL
Hanson, P
Hamilton, D
Hipsey, MR
McMahon, KD
Read, JS
Winslow, L
Dedrick, J
Rose, K
Carey, CC
Bertilsson, S
Marques, DD
Beversdorf, L
Miller, T
Wu, C
Hsieh, YF
Gaiser, E
Kratz, T
AF Kara, Emily L.
Hanson, Paul
Hamilton, David
Hipsey, Matthew R.
McMahon, Katherine D.
Read, Jordan S.
Winslow, Luke
Dedrick, John
Rose, Kevin
Carey, Cayelan C.
Bertilsson, Stefan
Marques, David da Motta
Beversdorf, Lucas
Miller, Todd
Wu, Chin
Hsieh, Yi-Fang
Gaiser, Evelyn
Kratz, Tim
TI Time-scale dependence in numerical simulations: Assessment of physical,
chemical, and biological predictions in a stratified lake at temporal
scales of hours to months
SO ENVIRONMENTAL MODELLING & SOFTWARE
LA English
DT Article
DE Ecosystem modeling; Phytoplankton; Spectral analysis; Wavelet analysis;
Automated observatory; Sensor network
ID FOOD SELECTION; CHLOROPHYLL-A; ELEMENTAL STOICHIOMETRY;
TEMPERATURE-DEPENDENCE; SPATIAL HETEROGENEITY; EUTROPHICATION MODEL;
SENSITIVITY-ANALYSIS; PLANKTON PATCHINESS; SUBTROPICAL LAKE;
DISSOLVED-OXYGEN
AB We evaluated the predictive ability of a one-dimensional coupled hydrodynamic-biogeochemical model across multiple temporal scales using wavelet analysis and traditional goodness-of-fit metrics. High-frequency in situ automated sensor data and long-term manual observational data from Lake Mendota, Wisconsin, USA, were used to parameterize, calibrate, and evaluate model predictions. We focused specifically on short-term predictions of temperature, dissolved oxygen, and phytoplankton biomass over one season. Traditional goodness-of-fit metrics indicated more accurate prediction of physics than chemical or biological variables in the time domain. This was confirmed by wavelet analysis in both the time and frequency domains. For temperature, predicted and observed global wavelet spectra were closely related, while observed dissolved oxygen and chlorophyll fluorescence spectral characteristics were not reproduced by the model for key time scales, indicating that processes not modeled may be important drivers of the observed signal. Although the magnitude and timing of physical and biological changes were simulated adequately at the seasonal time scale through calibration, time scale-specific dynamics, for example short-term cycles, were difficult to reproduce, and were relatively insensitive to the effects of varying parameters. The use of wavelet analysis is novel to aquatic ecosystem modeling, is complementary to traditional goodness-of-fit metrics, and allows for assessment of variability at specific temporal scales. In this way, the effect of processes operating at distinct temporal scales can be isolated and better understood, both in situ and in silico. Wavelet transforms are particularly well suited for assessment of temporal and spatial heterogeneity when coupled to high-frequency data from automated in situ or remote sensing platforms. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Kara, Emily L.; McMahon, Katherine D.; Read, Jordan S.; Beversdorf, Lucas; Miller, Todd; Wu, Chin; Hsieh, Yi-Fang] Univ Wisconsin, Dept Civil & Environm Engn, Madison, WI 53706 USA.
[Hanson, Paul; Winslow, Luke; Dedrick, John; Kratz, Tim] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA.
[Hamilton, David] Univ Waikato, Dept Biol Sci, Hamilton 3240, New Zealand.
[Hipsey, Matthew R.] Univ Western Australia, Sch Earth & Environm, Crawley, WA 6009, Australia.
[McMahon, Katherine D.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA.
[Rose, Kevin] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Carey, Cayelan C.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA.
[Bertilsson, Stefan] Uppsala Univ, Dept Ecol Genet & Limnol, S-75236 Uppsala, Sweden.
[Marques, David da Motta] Univ Fed Rio Grande do Sul, Inst Pesquisa Hidraul, BR-91501970 Porto Alegre, RS, Brazil.
[Gaiser, Evelyn] SE Environm Res Ctr, Dept Biol Sci, Miami, FL 33199 USA.
RP Kara, EL (reprint author), Univ Wisconsin, Dept Civil & Environm Engn, 1415 Engn Dr, Madison, WI 53706 USA.
EM kara@wisc.edu
RI McMahon, Katherine/I-3651-2012; Wu, Chin/C-2042-2009; Hipsey,
Matthew/C-3551-2009; Carey, Cayelan/D-4874-2016;
OI Wu, Chin/0000-0001-8393-1940; Hipsey, Matthew/0000-0001-8386-4354;
Carey, Cayelan/0000-0001-8835-4476; Winslow, Luke/0000-0002-8602-5510;
Read, Emily/0000-0002-9617-9433; McMahon, Katherine
D./0000-0002-7038-026X
FU US National Science Foundation; National Science Foundation (NSF) [CBET
0738039, 0903560, 0822700]; National Institute of Food and Agriculture,
United States Department of Agriculture [WIS01516]; EARS IGERT program
FX This work was funded in part by grants from the US National Science
Foundation to the Global Lake Ecological Observatory Network (GLEON).
ELK and KDM were supported by an NSF CAREER award (CBET 0738039) and the
National Institute of Food and Agriculture, United States Department of
Agriculture (ID number WIS01516). KCR was supported by a the EARS IGERT
program, NSF DGE IGERT #0903560. This material is based upon NTL LTER
work supported by the National Science Foundation under Cooperative
Agreement #0822700. Wavelet software was provided by C. Torrence and G.
Compo, and is available at URL:
http://atoc.colorado.edu/research/wavelets/. We are grateful for the
thoughtful comments of four anonymous reviewers.
NR 116
TC 18
Z9 18
U1 2
U2 47
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1364-8152
J9 ENVIRON MODELL SOFTW
JI Environ. Modell. Softw.
PD JUL
PY 2012
VL 35
BP 104
EP 121
DI 10.1016/j.envsoft.2012.02.014
PG 18
WC Computer Science, Interdisciplinary Applications; Engineering,
Environmental; Environmental Sciences
SC Computer Science; Engineering; Environmental Sciences & Ecology
GA 944PY
UT WOS:000304217500010
ER
PT J
AU Sessa, EB
Zimmer, EA
Givnish, TJ
AF Sessa, Emily B.
Zimmer, Elizabeth A.
Givnish, Thomas J.
TI Unraveling reticulate evolution in North American Dryopteris
(Dryopteridaceae)
SO BMC EVOLUTIONARY BIOLOGY
LA English
DT Article
DE Ferns; Divergence time estimates; Genetic distances; Hybridization;
Introgression; Phylogeny; Polyploidy
ID LENGTH DIFFERENCE TEST; FERN GENUS ASTROLEPIS; CHLOROPLAST DNA;
MOLECULAR PHYLOGENY; DIVERGENCE TIMES; FILIX-MAS; PHLOROGLUCINOL
DERIVATIVES; HISTORICAL BIOGEOGRAPHY; POLYPLOID SPECIATION; RECURRENT
FORMATION
AB Background: The thirteen species of Dryopteris in North America have long been suspected of having undergone a complicated history of reticulate evolution via allopolyploid hybridization. Various explanations for the origins of the allopolyploid taxa have been suggested, and though most lines of evidence have supported the so-called "semicristata" hypothesis, contention over the group's history has continued in several recent, conflicting studies.
Results: Sequence data from nine plastid and two nuclear markers were collected from 73 accessions representing 35 species of Dryopteris. Sequences from each of the allopolyploids are most closely related to their progenitor species as predicted by the "semicristata" hypothesis. Allotetraploid D. campyloptera appears to be derived from a hybrid between diploid D. expansa and D. intermedia; D. celsa, from diploid D. ludoviciana x D. goldiana; and D. carthusiana and D. cristata, from diploid "D. semicristata" x D. intermedia and D. ludoviciana, respectively. Allohexaploid D. clintoniana appears to be derived from D. cristata x D. goldiana. The earliest estimated dates of formation of the allopolyploids, based on divergence time analyses, were within the last 6 Ma. We found no evidence for recurrent formation of any of the allopolyploids. The sexual allopolyploid taxa are derived from crosses between parents that show intermediate levels of genetic divergence relative to all pairs of potential progenitors. In addition, the four allotetraploids are transgressive with respect to geographic range relative to one or both of their parents (their ranges extend beyond those of the parents), suggesting that ecological advantages in novel habitats or regions may promote long-term regional coexistence of the hybrid taxa with their progenitors.
Conclusions: This study provides the first thorough evaluation of the North American complex of woodferns using extensive sampling of taxa and genetic markers. Phylogenies produced from each of three datasets (one plastid and two nuclear) support the "semicristata" hypothesis, including the existence of a missing diploid progenitor, and allow us to reject all competing hypotheses. This study demonstrates the value of using multiple, biparentally inherited markers to evaluate reticulate complexes, assess the frequency of recurrent polyploidization, and determine the relative importance of introgression vs. hybridization in shaping the histories of such groups.
C1 [Sessa, Emily B.; Givnish, Thomas J.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA.
[Zimmer, Elizabeth A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
RP Sessa, EB (reprint author), Univ Wisconsin, Dept Bot, 430 Lincoln Dr, Madison, WI 53706 USA.
EM esessa@wisc.edu
FU National Science Foundation (DDIG) [DEB-1110335]; Huron Mountain
Wildlife Foundation; Botanical Society of America; American Society of
Plant Taxonomists; Torrey Botanical Society; Smithsonian Graduate
Research Fellowship
FX The authors thank E. Alverson, S. Bornell, B. Gilman, T. Grabs, A.
Jandl, C. Line, S. Lorbeer, B. & A. Manierre, T. Meyer, A. Reznicek, C.
Taylor, B. Vesterby, S. Wechsler, D. Werier, F. R. Wesley, K. Woods, and
especially T. Goforth for help in the field; J. Geiger, S. Hennequin, C.
Rothfels, and J. E. Watkins for providing material; D. Giblin, M.
McNamara, R. Moran, R. Olmstead, A. Smith, M. Sundue, and S. Vance for
help with arranging herbarium visits; herbaria BH, NY, MO, UC, US, WTU
for letting us view specimens; and the Finger Lakes Land Trust, Huron
Mountain Club, Fernwood Botanical Gardens, and University of
Wisconsin-Madison Arboretum for allowing us to visit and collect
Dryopteris in the field. Profound thanks to M. Ames, C. Ane, B. Berger,
A. Gardner, P. Gonsiska, B. Grady, J. Hunt, R. Jabaily, D. Stein, and K.
Sytsma for advice and discussion. We gratefully acknowledge financial
support for this research from: the National Science Foundation (DDIG
award to EBS, TJG; grant DEB-1110335); the Huron Mountain Wildlife
Foundation (EBS, TJG); graduate research awards from the Botanical
Society of America, American Society of Plant Taxonomists, and Torrey
Botanical Society (EBS), and a Smithsonian Graduate Research Fellowship
(EBS). Funding sources had no involvement in study design, data
collection, analysis, interpretation, or article preparation or
submission.
NR 130
TC 18
Z9 19
U1 2
U2 36
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 JUN 30
PY 2012
VL 12
AR 104
DI 10.1186/1471-2148-12-104
PG 24
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA 051NE
UT WOS:000312133200001
PM 22748145
ER
PT J
AU Campbell, BA
AF Campbell, Bruce A.
TI High circular polarization ratios in radar scattering from geologic
targets
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID POLARIMETRIC SAR DATA; GALILEAN SATELLITES; SURFACE-ROUGHNESS; 70-CM
WAVELENGTH; LAVA FLOW; MODEL; ARECIBO; VENUS; MARS; MOON
AB We examine and model the occurrence of circular polarization ratio (CPR or mu(c)) values greater than unity in terrestrial and planetary radar observations as a guide to the range of associated surface morphology. Lunar crater deposits exhibit maximum mu(c) values at 12.6 and 70-cm wavelength of 2 to 3. CPR values for Maxwell Montes on Venus range up to about 1.5 at 12.6-cm wavelength. Echoes from SP Flow in Arizona exhibit mu(c) up to 2 at 24-cm wavelength. Scattering from rock edges and cracks (dipole-like) produces mu(c) of unity for single scattering and up to about 2 for multiple reflections. Scattering from natural corner reflectors (dihedrals) formed by pairs of rock facets can yield an average mu(c) of 3-4, but likely requires non-random or scale-limited surface roughness properties in order to dominate the observed echo. The dihedral mechanism is required to satisfy the highest lunar mu(c) observations, while echoes from SP Flow and Maxwell Montes could be explained by just the dipole mechanism. The dihedral scenario requires rocky facets on scales many times the radar wavelength, which the blocks at SP Flow (and the unknown surface texture of Maxwell) may not provide. The random dipole model is less demanding in terms of structures and scales, and likely increases the CPR of lunar or asteroid regoliths through scattering from and between rocks.
C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA.
EM campbellb@si.edu
FU NASA
FX The author thanks C. Neish and W. Fa for helpful reviews of the paper
and M. Shepard for comments on earlier drafts. This work was supported
in part by grants from the NASA Planetary Astronomy and Planetary
Geology and Geophysics Programs.
NR 47
TC 17
Z9 18
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JUN 30
PY 2012
VL 117
AR E06008
DI 10.1029/2012JE004061
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 968PE
UT WOS:000305994900003
ER
PT J
AU Hines, HM
Papa, R
Ruiz, M
Papanicolaou, A
Wang, C
Nijhout, HF
McMillan, WO
Reed, RD
AF Hines, Heather M.
Papa, Riccardo
Ruiz, Mayte
Papanicolaou, Alexie
Wang, Charles
Nijhout, H. Frederik
McMillan, W. Owen
Reed, Robert D.
TI Transcriptome analysis reveals novel patterning and pigmentation genes
underlying Heliconius butterfly wing pattern variation
SO BMC GENOMICS
LA English
DT Article
DE Heliconius; Adaptation; Pigmentation; Ommochrome; Melanin; Genomics;
Evo-devo
ID GENOME-WIDE IDENTIFICATION; BOMBYX-MORI; EVO-DEVO;
DROSOPHILA-MELANOGASTER; LINKAGE MAP; EVOLUTION; COLOR; EXPRESSION;
GENETICS; YELLOW
AB Background: Heliconius butterfly wing pattern diversity offers a unique opportunity to investigate how natural genetic variation can drive the evolution of complex adaptive phenotypes. Positional cloning and candidate gene studies have identified a handful of regulatory and pigmentation genes implicated in Heliconius wing pattern variation, but little is known about the greater developmental networks within which these genes interact to pattern a wing. Here we took a large-scale transcriptomic approach to identify the network of genes involved in Heliconius wing pattern development and variation. This included applying over 140 transcriptome microarrays to assay gene expression in dissected wing pattern elements across a range of developmental stages and wing pattern morphs of Heliconius erato.
Results: We identified a number of putative early prepattern genes with color-pattern related expression domains. We also identified 51 genes differentially expressed in association with natural color pattern variation. Of these, the previously identified color pattern "switch gene" optix was recovered as the first transcript to show color-specific differential expression. Most differentially expressed genes were transcribed late in pupal development and have roles in cuticle formation or pigment synthesis. These include previously undescribed transporter genes associated with ommochrome pigmentation. Furthermore, we observed upregulation of melanin-repressing genes such as ebony and Dat1 in non-melanic patterns.
Conclusions: This study identifies many new genes implicated in butterfly wing pattern development and provides a glimpse into the number and types of genes affected by variation in genes that drive color pattern evolution.
C1 [Hines, Heather M.; McMillan, W. Owen] N Carolina State Univ, Dept Genet, Raleigh, NC 27695 USA.
[Hines, Heather M.] Penn State Univ, Dept Biol, University Pk, PA 16802 USA.
[Papa, Riccardo; Reed, Robert D.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA.
[Papa, Riccardo; Ruiz, Mayte] Univ Puerto Rico, Dept Biol, San Juan, PR 00921 USA.
[Papa, Riccardo; Ruiz, Mayte] Univ Puerto Rico, Ctr Appl Trop Ecol & Conservat, San Juan, PR 00921 USA.
[Papanicolaou, Alexie] CSIRO Ecosyst Sci, Canberra, ACT 2601, Australia.
[Wang, Charles] City Hope Natl Med Ctr, Beckman Res Inst, Funct Genom Core, Duarte, CA 91010 USA.
[Nijhout, H. Frederik] Duke Univ, Dept Biol, Durham, NC 27708 USA.
[McMillan, W. Owen; Reed, Robert D.] Smithsonian Trop Res Inst, Panama City, Panama.
[Reed, Robert D.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA.
RP Hines, HM (reprint author), N Carolina State Univ, Dept Genet, Box 7614, Raleigh, NC 27695 USA.
EM hmh19@psu.edu
RI Reed, Robert/A-2419-2008; Papanicolaou, Alexie/A-1618-2011
OI Papanicolaou, Alexie/0000-0002-3635-6848
FU Ruth L. Kirschstein National Research Service Award [F32 GM889942]; NASA
[NNX10AM80H, NNX07AO30A]; NSF [IBN-0344705, DEB-0844244, DEB-0715096,
IOS-1052541]
FX We wish to thank the Ministerio del Ambiente in Ecuador and the
Intendencia Forestal y de Fauna Silvestre Instituto Nacional de Recurso
Naturales in Peru for permission to collect butterflies. A special
thanks goes to Ana Maria Quiles and to at the Smithsonian Tropical
Research Institute for help rearing larvae and maintaining the
Heliconius insectaries in Puerto Rico and Panama respectively. We would
like to thank Eric Stone for advice on the manuscript and Arnaud Martin
for advice on candidate genes and providing images. This project is
funded by a Ruth L. Kirschstein National Research Service Award F32
GM889942 (HMH), a NASA grant (NNX10AM80H and NNX07AO30A) to RP, and NSF
grants IBN-0344705 (WOM, HFN), DEB-0844244 (WOM, RDR), DEB-0715096 (WOM,
RDR), and IOS-1052541 (RDR, WOM, RP).
NR 84
TC 23
Z9 23
U1 1
U2 62
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2164
J9 BMC GENOMICS
JI BMC Genomics
PD JUN 29
PY 2012
VL 13
AR 288
DI 10.1186/1471-2164-13-288
PG 16
WC Biotechnology & Applied Microbiology; Genetics & Heredity
SC Biotechnology & Applied Microbiology; Genetics & Heredity
GA 008DA
UT WOS:000308936300001
PM 22747837
ER
PT J
AU Marriner, N
Flaux, C
Kaniewski, D
Morhange, C
Leduc, G
Moron, V
Chen, Z
Gasse, F
Empereur, JY
Stanley, JD
AF Marriner, Nick
Flaux, Clement
Kaniewski, David
Morhange, Christophe
Leduc, Guillaume
Moron, Vincent
Chen, Zhongyuan
Gasse, Francoise
Empereur, Jean-Yves
Stanley, Jean-Daniel
TI ITCZ and ENSO-like pacing of Nile delta hydro-geomorphology during the
Holocene
SO QUATERNARY SCIENCE REVIEWS
LA English
DT Article
DE Nile; Delta; Holocene climate change; ITCZ; ENSO; Civilizations
ID NORTH-ATLANTIC CLIMATE; LAST GLACIAL MAXIMUM; AFRICAN RAINFALL; DIATOM
RECORD; EAST-AFRICA; SUDAN; MONSOON; EVOLUTION; SAHARA; VARIABILITY
AB The Nile valley accommodates the world's longest river and shaped the development of numerous complex societies, providing a reliable source of water for farming and linking populations to sub-Saharan Africa and the Mediterranean Sea. Its fertile delta lay at the heart of ancient Egyptian civilization, however little is known of its morpho-sedimentary response to basin-wide changes in Holocene hydrology. Here, we present two well-resolved records from the Nile delta (based on similar to 320 radiocarbon dates) to reconstruct the timing and rhythm of catchment-scale modifications during the past 8000 years. On the orbital timescale, we demonstrate that Nilotic hydrology and sedimentation have responded to low-latitude insolation forcing while, on sub-millennial timescales, many of the major phases of deltaic modification were mediated by climate events linked to El Nino Southern Oscillation-type (ENSO) variability. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Marriner, Nick; Gasse, Francoise] CEREGE UMR 7330, CNRS, F-13545 Aix En Provence 04, France.
[Flaux, Clement; Morhange, Christophe; Moron, Vincent] Univ Aix Marseille, CEREGE UMR 7330, F-13545 Aix En Provence 04, France.
[Kaniewski, David] Univ Toulouse 3, EcoLab Lab Ecol Fonct, F-31062 Toulouse 9, France.
[Leduc, Guillaume] Univ Kiel, Inst Earth Sci, D-24118 Kiel, Germany.
[Moron, Vincent] Columbia Univ, Int Res Inst Climate & Soc, New York, NY USA.
[Chen, Zhongyuan] E China Normal Univ, Shanghai 200062, Peoples R China.
[Empereur, Jean-Yves] CNRS, UMS 1812, Ctr Etudes Alexandrines, Alexandria 21131, Egypt.
[Stanley, Jean-Daniel] Smithsonian Inst, Geoarchaeol Program, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Marriner, N (reprint author), CEREGE UMR 7330, CNRS, BP 80, F-13545 Aix En Provence 04, France.
EM marriner@cerege.fr
RI Leduc, Guillaume/A-8930-2008;
OI Marriner, Nick/0000-0002-7916-6059
FU ANR Paleomed [09-BLAN-0323-01]; Artemis INSU; PEPS INSHS; PEPS INEE
FX We thank two anonymous referees, R. Bonnefille, M. Taieb and E. Van
Campo for critical review and comments on earlier versions of the
manuscript. Research was funded by ANR Paleomed (09-BLAN-0323-01),
Artemis INSU, PEPS INSHS and PEPS INEE.
NR 79
TC 28
Z9 30
U1 2
U2 36
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0277-3791
J9 QUATERNARY SCI REV
JI Quat. Sci. Rev.
PD JUN 29
PY 2012
VL 45
BP 73
EP 84
DI 10.1016/j.quascirev.2012.04.022
PG 12
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 981QB
UT WOS:000306983200007
ER
PT J
AU Zimbelman, JR
Scheidt, SP
AF Zimbelman, James R.
Scheidt, Stephen P.
TI Hesperian Age for Western Medusae Fossae Formation, Mars
SO SCIENCE
LA English
DT Article
ID CRATER
C1 [Zimbelman, James R.; Scheidt, Stephen P.] Smithsonian Inst, Natl Air & Space Museum, MRC 315, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
RP Zimbelman, JR (reprint author), Smithsonian Inst, Natl Air & Space Museum, MRC 315, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
EM zimbelmanj@si.edu
FU NASA from the Planetary Geology and Geophysics program [NNX07AP42G]
FX This work was supported by NASA grant NNX07AP42G from the Planetary
Geology and Geophysics program.
NR 11
TC 20
Z9 20
U1 3
U2 10
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JUN 29
PY 2012
VL 336
IS 6089
BP 1683
EP 1683
DI 10.1126/science.1221094
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 965VD
UT WOS:000305794500043
PM 22628559
ER
PT J
AU Munoz, F
Couteron, P
Hubbell, SP
AF Munoz, Francois
Couteron, Pierre
Hubbell, Stephen P.
TI Comment on "Global Correlations in Tropical Tree Species Richness and
Abundance Reject Neutrality"
SO SCIENCE
LA English
DT Editorial Material
ID MODELS; DIVERSITY
C1 [Munoz, Francois; Couteron, Pierre] Univ Montpellier 2, F-34398 Montpellier 5, France.
[Munoz, Francois; Couteron, Pierre] Inst Rech Dev, UMR AMAP, F-34398 Montpellier 5, France.
[Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Miami, FL 34002 USA.
RP Munoz, F (reprint author), Univ Montpellier 2, TA A-51-PS2, F-34398 Montpellier 5, France.
EM francois.munoz@cirad.fr
RI Munoz, Francois/C-4239-2015
OI Munoz, Francois/0000-0001-8776-4705
NR 6
TC 4
Z9 4
U1 0
U2 19
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JUN 29
PY 2012
VL 336
IS 6089
DI 10.1126/science.1222718
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 965VD
UT WOS:000305794500021
PM 22745404
ER
PT J
AU Thompson, FC
AF Thompson, F. Christian
TI Costarica Mengual & Thompson, 2009 (Insecta: Diptera: Syrphidae) junior
homonym of Costarica Kocak & Kemal, 2008 (Insecta: Orthoptera): proposed
replacement by Tiquicia nom. nov.
SO ZOOTAXA
LA English
DT Letter
C1 Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA.
RP Thompson, FC (reprint author), Smithsonian Inst, Dept Entomol, NHB-0169, Washington, DC 20560 USA.
EM thompsonf@si.edu
NR 3
TC 4
Z9 5
U1 0
U2 1
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JUN 29
PY 2012
IS 3360
BP 68
EP 68
PG 1
WC Zoology
SC Zoology
GA 974MS
UT WOS:000306440200003
ER
PT J
AU Turner, AJ
Henze, DK
Martin, RV
Hakami, A
AF Turner, A. J.
Henze, D. K.
Martin, R. V.
Hakami, A.
TI The spatial extent of source influences on modeled column concentrations
of short-lived species
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID NOX EMISSIONS; ISOPRENE EMISSIONS; INTEX-B; SPACE; CHEMISTRY; NITROGEN
AB Providing top-down constraints on emissions is an important application of model-based analysis of remote-sensing observations of chemically reactive species, yet the degree to which column concentrations are governed by local vs distant sources within models themselves has yet to be fully characterized. We use a chemical transport model and its adjoint to quantify source contributions to weekly column concentrations of ammonia, nitrogen dioxide, sulfur dioxide, and formaldehyde. This efficient approach for quantifying the spatial extent of source influences is validated and then applied to an array of sites and seasons. Overall, we find instances for each species where emissions from at least 500 km away must be taken into account to retrieve 90% of the total column influence. This demonstrates that the common practice of assuming a local relationship between satellite observations and emissions in top-down constraints could lead to considerable biases, an issue that will be exacerbated as the resolution of models and observations are refined in coming years. Citation: Turner, A. J., D. K. Henze, R. V. Martin, and A. Hakami (2012), The spatial extent of source influences on modeled column concentrations of short-lived species, Geophys. Res. Lett., 39, L12806, doi:10.1029/2012GL051832.
C1 [Turner, A. J.; Henze, D. K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
[Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hakami, A.] Carleton Univ, Dept Civil & Environm Engn, Ottawa, ON K1S 5B6, Canada.
RP Turner, AJ (reprint author), Univ Colorado, Dept Mech Engn, 427 UCB, Boulder, CO 80309 USA.
EM alexander.turner@colorado.edu
RI Martin, Randall/C-1205-2014
OI Martin, Randall/0000-0003-2632-8402
FU NASA Applied Sciences Program grant [NNX09AN77G]; University of
Colorado's Discovery Learning Center Apprenticeship program; Environment
Canada
FX This work was supported through NASA Applied Sciences Program grant
NNX09AN77G, the University of Colorado's Discovery Learning Center
Apprenticeship program, and access to the NASA Advanced Supercomputing
Facility. Activities at Dalhousie University were supported by
Environment Canada.
NR 33
TC 13
Z9 13
U1 0
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 JUN 28
PY 2012
VL 39
AR L12806
DI 10.1029/2012GL051832
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 968NP
UT WOS:000305989600003
ER
PT J
AU Malabarba, LR
Jerep, FC
AF Malabarba, Luiz R.
Jerep, Fernando C.
TI A New Genus and Species of Cheirodontine Fish from South America
(Teleostei: Characidae)
SO COPEIA
LA English
DT Article
ID CAUDAL-FIN
AB Ctenocheirodon pristis, a new genus and species of cheirodontine fish from South America is described. The new genus possesses derived ventral procurrent caudal-fin rays and anal-fin rays that support its placement among characids of the tribe Cheirodontinl. The new genus and species is diagnosed from the other members of the tribe by the shape of ventral procurrent caudal-fin rays and anal-fin rays.
C1 [Malabarba, Luiz R.] Univ Fed Rio Grande do Sul, Dept Zool, BR-91501970 Porto Alegre, RS, Brazil.
[Jerep, Fernando C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
RP Malabarba, LR (reprint author), Univ Fed Rio Grande do Sul, Dept Zool, Av Paulo Gama S-No, BR-91501970 Porto Alegre, RS, Brazil.
EM malabarb@ufrgs.br; fjerep@gmail.com
RI Malabarba, Luiz/I-3225-2012; Jerep, Fernando/F-5274-2015
FU CNPq [479412/2008-1, 300705/2010-7]; Smithsonian Institution
FX We are grateful to C. Lucena (MCP), J. Figueiredo and O. Oyakawa
(MZUSP), P. Lucinda (UNT), and R. Vari and S. Weitzman (USNM) for the
loan of specimens. This paper was improved with comments from R. Vari
and J. Mirande. Financial support was provided by the CNPq
(479412/2008-1; 300705/2010-7) to LRM and Smithsonian Institution to
FCJ.
NR 8
TC 2
Z9 2
U1 0
U2 1
PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS
PI MIAMI
PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200
SW 8TH STREET, MIAMI, FL 33199 USA
SN 0045-8511
J9 COPEIA
JI Copeia
PD JUN 27
PY 2012
IS 2
BP 243
EP 250
DI 10.1643/CI-11-143
PG 8
WC Zoology
SC Zoology
GA 967SS
UT WOS:000305928700009
ER
PT J
AU Uchida, H
Tsunemi, H
Katsuda, S
Mori, K
Petre, R
Yamaguchi, H
AF Uchida, Hiroyuki
Tsunemi, Hiroshi
Katsuda, Satoru
Mori, Koji
Petre, Robert
Yamaguchi, Hiroya
TI A Suzaku Study of Ejecta Structure and Origin of Hard X-Ray Emission in
the Supernova Remnant G 156.2+5.7
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE ISM: abundances; ISM: individual (G 156.2+5.7); ISM: supernova remnants;
X-rays: ISM
ID SNR G156.2+5.7; CYGNUS LOOP; ABUNDANCES; DISCOVERY; GALAXIES; ELEMENTS;
BRIGHT
AB We report on an X-ray study of the evolved Galactic supernova remnant (SNR) G 156.2+5.7 based on six pointing observations with Suzaku. The remnant's large extent (100' in diameter) allows us to investigate its radial structure in the northwestern and eastern directions from the apparent center. The X-ray spectra were well fit with a two-component non-equilibrium ionization model representing the swept-up interstellar medium (ISM) and the metal-rich ejecta. We found prominent central concentrations of Si, S, and Fe from the ejecta component; the lighter elements of 0, Ne, and Mg were distributed more uniformly. The temperature of the ISM component suggests a slow shock (similar to 610-960 km s(-1)); hence, the remnant's age is estimated to be similar to 7000-15000 yr, assuming its distance to be similar to 1.1 kpc. G 156.2+5.7 has also been thought to emit hard, non-thermal X-rays, despite being considerably older than any other such remnant. In response to a recent discovery of a background cluster of galaxies (2XMM J045637.2+522411), we carefully excluded its contribution, and reexamined the origin of the hard X-ray emission. We found that the residual hard X-ray emission is consistent with the expected level of the cosmic X-ray background. Thus, no robust evidence for non-thermal emission was obtained from G 156.2+5.7. These results are consistent with the picture of an evolved SNR.
C1 [Uchida, Hiroyuki] Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Tsunemi, Hiroshi] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Katsuda, Satoru] RIKEN, Wako, Saitama 3510198, Japan.
[Mori, Koji] Miyazaki Univ, Fac Engn, Dept Appl Phys, Miyazaki 8892192, Japan.
[Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yamaguchi, Hiroya] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Uchida, H (reprint author), Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
EM uchida@cr.scphys.kyoto-u.ac.jp
RI XRAY, SUZAKU/A-1808-2009
FU Japan Society for the Promotion of Science (JSPS); Ministry of
Education, Culture, Sports, Science and Technology [23000004]
FX HU is supported by Japan Society for the Promotion of Science (JSPS)
Research Fellowship for Young Scientists. HY is supported by JSPS
Research Fellowship for Research Abroad. The work is partially supported
by a Grant-in-Aid from the Ministry of Education, Culture, Sports,
Science and Technology (No.23000004).
NR 31
TC 4
Z9 4
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD JUN 25
PY 2012
VL 64
IS 3
AR 61
DI 10.1093/pasj/64.3.61
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 966WN
UT WOS:000305868200019
ER
PT J
AU Wilson, AS
Marra, PP
Fleischer, RC
AF Wilson, Amy S.
Marra, Peter P.
Fleischer, Robert C.
TI Temporal patterns of genetic diversity in Kirtland's warblers (Dendroica
kirtlandii), the rarest songbird in North America
SO BMC ECOLOGY
LA English
DT Article
ID EFFECTIVE POPULATION-SIZE; MICROSATELLITE DNA MARKERS; GREATER
PRAIRIE-CHICKENS; ALLELE FREQUENCY DATA; LINKAGE DISEQUILIBRIUM;
OVERLAPPING GENERATIONS; COMPUTER-PROGRAM; BOTTLENECK; SOFTWARE; LOCI
AB Background: Kirtland's warblers are the rarest songbird species in North America, rarity due in part to a reliance on early successional Jack Pine forests. Habitat loss due to fire suppression led to population declines to fewer than 200 males during the 1970s. Subsequent conservation management has allowed the species to recover to over 1700 males by 2010. In this study, we directly examine the impact that low population sizes have had on genetic variation in Kirtland's warblers. We compare the molecular variation of samples collected in Oscoda County, Michigan across three time periods: 1903-1912, 1929-1955 and 2008-2009.
Results: In a hierarchical rarified sample of 20 genes and one time period, allelic richness was highest in 1903-1912 sample (A(R) = 5.96), followed by the 1929-1955 sample (A(R) = 5.74), and was lowest in the 2008-2009 sample (A(R) = 5.54). Heterozygosity measures were not different between the 1929-1955 and 2008-2009 samples, but were lower in the 1903-1912 sample. Under some models, a genetic bottleneck signature was present in the 1929-1955 and 2008-2009 samples but not in the 1903-1912 sample.
Conclusions: We suggest that these temporal genetic patterns are the result of the declining Kirtland's warbler population compressing into available habitat and a consequence of existing at low numbers for several decades.
C1 [Wilson, Amy S.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA.
[Wilson, Amy S.; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA.
RP Wilson, AS (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA.
EM asg.wilson@gmail.com
FU Smithsonian Institution Postdoctoral Fellowship; George Didden
Postdoctoral Fellowship from the Smithsonian Conservation Biology
Institute, National Zoological Park; Center for Conservation and
Evolutionary Genetics
FX We thank the Museum of Zoology at the University of Michigan for the
generous provisioning of historic samples and J. Hinshaw for providing
access. We also thank Sarah Rockwell, Carol Bcetti and the Kirtland's
warbler Recovery Team. F. Hailer and N. McInerny provided useful
laboratory advice. Financial support was provided to A. Wilson by a
Smithsonian Institution Postdoctoral Fellowship, and a George Didden
Postdoctoral Fellowship from the Smithsonian Conservation Biology
Institute, National Zoological Park. Funding for laboratory supplies was
provided by the Center for Conservation and Evolutionary Genetics.
NR 70
TC 5
Z9 6
U1 2
U2 40
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1472-6785
J9 BMC ECOL
JI BMC Ecol.
PD JUN 22
PY 2012
VL 12
AR 8
DI 10.1186/1472-6785-12-8
PG 11
WC Ecology
SC Environmental Sciences & Ecology
GA 996HW
UT WOS:000308076500001
PM 22726952
ER
PT J
AU Buchhave, LA
Latham, DW
Johansen, A
Bizzarro, M
Torres, G
Rowe, JF
Batalha, NM
Borucki, WJ
Brugamyer, E
Caldwell, C
Bryson, ST
Ciardi, DR
Cochran, WD
Endl, M
Esquerdo, GA
Ford, EB
Geary, JC
Gilliland, RL
Hansen, T
Isaacson, H
Laird, JB
Lucas, PW
Marcy, GW
Morse, JA
Robertson, P
Shporer, A
Stefanik, RP
Still, M
Quinn, SN
AF Buchhave, Lars A.
Latham, David W.
Johansen, Anders
Bizzarro, Martin
Torres, Guillermo
Rowe, Jason F.
Batalha, Natalie M.
Borucki, William J.
Brugamyer, Erik
Caldwell, Caroline
Bryson, Stephen T.
Ciardi, David R.
Cochran, William D.
Endl, Michael
Esquerdo, Gilbert A.
Ford, Eric B.
Geary, John C.
Gilliland, Ronald L.
Hansen, Terese
Isaacson, Howard
Laird, John B.
Lucas, Philip W.
Marcy, Geoffrey W.
Morse, Jon A.
Robertson, Paul
Shporer, Avi
Stefanik, Robert P.
Still, Martin
Quinn, Samuel N.
TI An abundance of small exoplanets around stars with a wide range of
metallicities
SO NATURE
LA English
DT Article
ID PLANETESIMAL FORMATION; GIANT PLANETS; HOST STARS; MASS;
PHOTOEVAPORATION; CANDIDATES; PARAMETERS; LIFETIMES; SEARCH; SYSTEM
AB The abundance of heavy elements (metallicity) in the photospheres of stars similar to the Sun provides a 'fossil' record of the chemical composition of the initial protoplanetary disk. Metal-rich stars are much more likely to harbour gas giant planets(1-4), supporting the model that planets form by accumulation of dust and ice particles(5). Recent ground-based surveys suggest that this correlation is weakened for Neptunian-sized planets(4,6-9). However, how the relationship between size and metallicity extends into the regime of terrestrial-sized exoplanets is unknown. Here we report spectroscopic metallicities of the host stars of 226 small exoplanet candidates discovered by NASA's Kepler mission(10), including objects that are comparable in size to the terrestrial planets in the Solar System. We find that planets with radii less than four Earth radii form around host stars with a wide range of metallicities (but on average a metallicity close to that of the Sun), whereas large planets preferentially form around stars with higher metallicities. This observation suggests that terrestrial planets may be widespread in the disk of the Galaxy, with no special requirement of enhanced metallicity for their formation.
C1 [Buchhave, Lars A.; Hansen, Terese] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.; Bizzarro, Martin] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
[Latham, David W.; Torres, Guillermo; Esquerdo, Gilbert A.; Geary, John C.; Stefanik, Robert P.; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Johansen, Anders] Lund Univ, Lund Observ, S-22100 Lund, Sweden.
[Rowe, Jason F.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA.
[Brugamyer, Erik; Caldwell, Caroline; Cochran, William D.; Endl, Michael; Robertson, Paul] Univ Texas Austin, Austin, TX 78712 USA.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91109 USA.
[Ford, Eric B.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Laird, John B.] Bowling Green State Univ, Bowling Green, OH 43403 USA.
[Lucas, Philip W.] Univ Hertfordshire, Ctr Astrophys, Hatfield AL10 9AB, Herts, England.
[Morse, Jon A.] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA.
[Shporer, Avi] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Buchhave, LA (reprint author), Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark.
EM buchhave@astro.ku.dk
RI Bizzarro, Martin/I-8701-2012;
OI Bizzarro, Martin/0000-0001-9966-2124; Buchhave, Lars
A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047
FU NASA's Science Mission Directorate; Danish National Research Foundation;
Carlsberg Foundation; European Research Council under ERC Starting Grant
agreement [278675-PEBBLE2PLANET]
FX The Kepler mission was competitively selected as the tenth NASA
Discovery mission. Funding for this mission is provided by NASA's
Science Mission Directorate. The Centre for Star and Planet Formation is
funded by the Danish National Research Foundation. L. A. B. was funded
by the Carlsberg Foundation. A.J. was partially funded by the European
Research Council under ERC Starting Grant agreement
278675-PEBBLE2PLANET.
NR 27
TC 207
Z9 208
U1 2
U2 25
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUN 21
PY 2012
VL 486
IS 7403
BP 375
EP 377
DI 10.1038/nature11121
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 961LV
UT WOS:000305466800037
PM 22722196
ER
PT J
AU Rest, A
Prieto, JL
Walborn, NR
Smith, N
Bianco, FB
Chornock, R
Welch, DL
Howell, DA
Huber, ME
Foley, RJ
Fong, W
Sinnott, B
Bond, HE
Smith, RC
Toledo, I
Minniti, D
Mandel, K
AF Rest, A.
Prieto, J. L.
Walborn, N. R.
Smith, N.
Bianco, F. B.
Chornock, R.
Welch, D. L.
Howell, D. A.
Huber, M. E.
Foley, R. J.
Fong, W.
Sinnott, B.
Bond, H. E.
Smith, R. C.
Toledo, I.
Minniti, D.
Mandel, K.
TI The Great Eruption of eta Carinae reply
SO NATURE
LA English
DT Letter
ID ECHOES
C1 [Rest, A.; Walborn, N. R.; Bond, H. E.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Prieto, J. L.] Carnegie Observ, Pasadena, CA 91101 USA.
[Prieto, J. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Smith, N.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bianco, F. B.; Howell, D. A.] Global Telescope Network, Las Cumbres Observ, Goleta, CA 93117 USA.
[Bianco, F. B.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Chornock, R.; Foley, R. J.; Fong, W.; Mandel, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Welch, D. L.; Sinnott, B.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
[Huber, M. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Smith, R. C.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile.
[Toledo, I.] ALMA, San Pedro De Atacama, Chile.
[Minniti, D.] Pontificia Univ Catolica, Dept Astron & Astrophys, Santiago 22, Chile.
[Mandel, K.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
RP Rest, A (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM arest@stsci.edu
NR 5
TC 0
Z9 0
U1 0
U2 1
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUN 21
PY 2012
VL 486
IS 7403
BP E1
EP E2
DI 10.1038/nature11167
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 961LV
UT WOS:000305466800002
ER
PT J
AU Pedersen, TM
Gallegos, CL
Nielsen, SL
AF Pedersen, Troels Moller
Gallegos, Charles L.
Nielsen, Soren Laurentius
TI Influence of near-bottom re-suspended sediment on benthic light
availability
SO ESTUARINE COASTAL AND SHELF SCIENCE
LA English
DT Article
DE light attenuation; radiative transfer modeling; seagrass distribution;
sediment organic content; turbidity
ID EELGRASS ZOSTERA-MARINA; SUBMERSED AQUATIC VEGETATION; SEAGRASS DEPTH
LIMITS; WATER-QUALITY; CHESAPEAKE BAY; HABITAT REQUIREMENTS;
OPTICAL-PROPERTIES; EUTROPHICATION; ATTENUATION; LAGOON
AB Increased light attenuation in the water column is a common consequence of the increased organic loading that accompanies anthropogenic eutrophication in coastal systems. Frequently, the best water quality correlate of the light attenuation coefficient is the total suspended solids, even in systems in which nutrient loading occurs primarily by groundwater input, that is, without strong river inputs of sediment. Alteration of bottom sediment texture, organic content, and bulk density by organic loading has been well documented. Here we report the effect of sediment re-suspension on near-bottom light attenuation using an array of in situ light sensors with very close spacing near the sediment-water interface and a radiative transfer (RT) modeling with the software "Hydrolight". We found that the light attenuation coefficient over 4.5 cm just above the bottom exceeded the attenuation found higher in the water column by a factor ranging from 1.6 to >30. RT modeling indicated that light received at the bottom could be overestimated by a factor 4 or more by extrapolating measurements not taking the near-bottom light attenuation into account. The results may help explain the wide range of seagrass light requirements observed in different systems. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Pedersen, Troels Moller; Nielsen, Soren Laurentius] Roskilde Univ, Dept Environm Social & Spatial Change, DK-4000 Roskilde, Denmark.
[Gallegos, Charles L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Nielsen, SL (reprint author), Roskilde Univ, Dept Environm Social & Spatial Change, POB 260, DK-4000 Roskilde, Denmark.
EM nielsen@ruc.dk
OI Gallegos, Charles/0000-0001-5112-0166; Nielsen, Soren
Laurentius/0000-0003-4309-5153
FU Danish Strategic Research Council [2104-07-0011]
FX IMP and SLN were supported by grant 2104-07-0011 (REEL-GRASS) from The
Danish Strategic Research Council. This sponsor had no role in
determining study design, collection or treatment of data, writing, or
in the decision to submit to this journal.
NR 46
TC 8
Z9 8
U1 2
U2 31
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0272-7714
J9 ESTUAR COAST SHELF S
JI Estuar. Coast. Shelf Sci.
PD JUN 20
PY 2012
VL 106
BP 93
EP 101
DI 10.1016/j.ecss.2012.04.027
PG 9
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 966UL
UT WOS:000305862800010
ER
PT J
AU Robbins, RK
Anderson, RA
Sullivan, JB
AF Robbins, Robert K.
Anderson, Richard A.
Sullivan, J. Bolling
TI THE NICARAGUAN HAIRSTREAK BUTTERFLY FAUNA (THECLINAE: EUMAEINI), ITS
BIOGEOGRAPHY, AND THE HISTORY OF NICARAGUAN COLLECTORS
SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY
LA English
DT Article
DE Belt; Biogeography; Biologia Centrali Americana; Godman; Salvin
ID PHYLOGENETIC ANALYSIS; LYCAENIDAE THECLINAE; LEPIDOPTERA; TAXONOMY
AB The hairstreak butterfly fauna of Nicaragua has not been comprehensively updated since Godman and Salvin listed 71. species in the Biologia Centrali-Americana over a century ago. Based primarily on Eumaeini in the Anderson and Sullivan Collections (Smithsonian Institution), we treat 149 thecline species recorded from Nicaragua with their localities and months of capture. None are endemic to Nicaragua, but 15 species have the northern or southern limit of their known distribution in Nicaragua. We relate the distributions of these 15 species, many of which are figured, to the life zones and physical features of Nicaragua and adjoining countries. Those eumaeine names for which Nicaragua is a type locality are noted, and a few unresolved taxonomic problems among the Nicaraguan fauna are pointed out. We list another 73 hairstreak species that are recorded both to the northwest and southeast of Nicaragua, but not in Nicaragua. Finally, we present brief historical comments on the collectors of Nicaraguan hairstreaks.
C1 [Robbins, Robert K.] Smithsonian Inst, Washington, DC 20013 USA.
RP Robbins, RK (reprint author), Smithsonian Inst, POB 37012,NHB MRC 105, Washington, DC 20013 USA.
EM RobbinsR@SI.edu; ragabry@tampabay.rr.com; sullivan14@earthlink.net
NR 41
TC 3
Z9 3
U1 0
U2 6
PU LEPIDOPTERISTS SOC
PI LOS ANGELES
PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA
SN 0024-0966
J9 J LEPID SOC
JI J. Lepid. Soc.
PD JUN 20
PY 2012
VL 66
IS 2
BP 61
EP 75
PG 15
WC Entomology
SC Entomology
GA 968ZL
UT WOS:000306025400001
ER
PT J
AU Di Stefano, R
AF Di Stefano, R.
TI DISCOVERING HABITABLE EARTHS, HOT JUPITERS, AND OTHER CLOSE PLANETS WITH
MICROLENSING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: general; gravitational lensing: micro; planets and satellites:
detection; surveys
ID PROPER MOTION STARS; MAGELLANIC CLOUDS; GALACTIC BULGE; SYSTEMS; EVENTS;
CHANNEL; LENSES; FIELDS; LIGHT
AB Searches for planets via gravitational lensing have focused on cases in which the projected separation, a, between planet and star is comparable to the Einstein radius, RE. This paper considers smaller orbital separations and demonstrates that evidence of close-orbit planets can be found in the low-magnification portion of the light curves generated by the central star. We develop a protocol for discovering hot Jupiters as well as Neptune-mass and Earth-mass planets in the stellar habitable zone. When planets are not discovered, our method can be used to quantify the probability that the lens star does not have planets within specified ranges of the orbital separation and mass ratio. Nearby close-orbit planets discovered by lensing can be subject to follow-up observations to study the newly discovered planets or to discover other planets orbiting the same star. Careful study of the low-magnification portions of lensing light curves should produce, in addition to the discoveries of close-orbit planets, definite detections of wide-orbit planets through the discovery of "repeating" lensing events. We show that events exhibiting extremely high magnification can effectively be probed for planets in close, intermediate, and wide distance regimes simply by adding several-time-per-night monitoring in the low-magnification wings, possibly leading to gravitational lensing discoveries of multiple planets occupying a broad range of orbits, from close to wide, in a single planetary system.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NSF [AST-0908878]
FX I thank Ann Esin and James Matthews for conversations and for help with
the figures. This work was supported in part by NSF under grant
AST-0908878.
NR 28
TC 7
Z9 7
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 105
DI 10.1088/0004-637X/752/2/105
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000028
ER
PT J
AU Foley, RJ
Simon, JD
Burns, CR
Gal-Yam, A
Hamuy, M
Kirshner, RP
Morrell, NI
Phillips, MM
Shields, GA
Sternberg, A
AF Foley, Ryan J.
Simon, Joshua D.
Burns, Christopher R.
Gal-Yam, Avishay
Hamuy, Mario
Kirshner, Robert P.
Morrell, Nidia I.
Phillips, Mark M.
Shields, Gregory A.
Sternberg, Assaf
TI LINKING TYPE Ia SUPERNOVA PROGENITORS AND THEIR RESULTING EXPLOSIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE distance scale; dust, extinction; supernovae: general
ID DELAYED-DETONATION MODEL; DARK-ENERGY CONSTRAINTS; LIGHT CURVES;
CIRCUMSTELLAR MATERIAL; INTERSTELLAR-MEDIUM; WHITE-DWARFS; SN 2011FE;
SODIUM-ABSORPTION; HUBBLE DIAGRAM; TELESCOPE
AB Comparing the ejecta velocities at maximum brightness and narrow circumstellar/interstellar Na D absorption line profiles of a sample of 23 Type Ia supernovae (SNe Ia), we determine that the properties of SN Ia progenitor systems and explosions are intimately connected. As demonstrated by Sternberg et al., half of all SNe Ia with detectable Na D absorption at the host-galaxy redshift in high-resolution spectroscopy have Na D line profiles with significant blueshifted absorption relative to the strongest absorption component, which indicates that a large fraction of SN Ia progenitor systems have strong outflows. In this study, we find that SNe Ia with blueshifted circumstellar/interstellar absorption systematically have higher ejecta velocities and redder colors at maximum brightness relative to the rest of the SN Ia population. This result is robust at a 98.9%-99.8% confidence level, providing the first link between the progenitor systems and properties of the explosion. This finding is further evidence that the outflow scenario is the correct interpretation of the blueshifted Na D absorption, adding additional confirmation that some SNe Ia are produced from a single-degenerate progenitor channel. An additional implication is that either SN Ia progenitor systems have highly asymmetric outflows that are also aligned with the SN explosion or SNe Ia come from a variety of progenitor systems where SNe Ia from systems with strong outflows tend to have more kinetic energy per unit mass than those from systems with weak or no outflows.
C1 [Foley, Ryan J.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Simon, Joshua D.; Burns, Christopher R.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Gal-Yam, Avishay] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile.
[Morrell, Nidia I.; Phillips, Mark M.] Carnegie Observ, Las Campanas Observ, La Serena, Chile.
[Shields, Gregory A.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Sternberg, Assaf] Max Planck Inst Astrophys, D-85741 Garching, Germany.
RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rfoley@cfa.harvard.edu
RI Hamuy, Mario/G-7541-2016; Horesh, Assaf/O-9873-2016
OI Horesh, Assaf/0000-0002-5936-1156
FU Clay Fellowship; ISF foundation; Minerva foundation; ARCHES award; Lord
Sieff of Brimpton Fund; Minerva Fellowship; CONICYT [FONDECYT Regular
1060808, Centro de Astrofisica FONDAP 15010003, Centro BASAL CATA
(PFB-06), Millenium Center for Supernova Science (P10-064-F)]; NSF
[AST-0907903]
FX R.J.F. is supported by a Clay Fellowship. A.G.Y is supported by grants
from the ISF and Minerva foundations, an ARCHES award, and the Lord
Sieff of Brimpton Fund. A.S. is supported by a Minerva Fellowship. M.H.
acknowledges support by CONICYT through grants FONDECYT Regular 1060808,
Centro de Astrofisica FONDAP 15010003, Centro BASAL CATA (PFB-06), and
the Millenium Center for Supernova Science (P10-064-F). Supernova
research at Harvard College Observatory is supported by NSF grant
AST-0907903.
NR 78
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 101
DI 10.1088/0004-637X/752/2/101
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000024
ER
PT J
AU Johnson, LC
Seth, AC
Dalcanton, JJ
Caldwell, N
Fouesneau, M
Gouliermis, DA
Hodge, PW
Larsen, SS
Olsen, KAG
San Roman, I
Sarajedini, A
Weisz, DR
Williams, BF
Beerman, LC
Bianchi, L
Dolphin, AE
Girardi, L
Guhathakurta, P
Kalirai, J
Lang, D
Monachesi, A
Nanda, S
Rix, HW
Skillman, ED
AF Johnson, L. Clifton
Seth, Anil C.
Dalcanton, Julianne J.
Caldwell, Nelson
Fouesneau, Morgan
Gouliermis, Dimitrios A.
Hodge, Paul W.
Larsen, Soren S.
Olsen, Knut A. G.
San Roman, Izaskun
Sarajedini, Ata
Weisz, Daniel R.
Williams, Benjamin F.
Beerman, Lori C.
Bianchi, Luciana
Dolphin, Andrew E.
Girardi, Leo
Guhathakurta, Puragra
Kalirai, Jason
Lang, Dustin
Monachesi, Antonela
Nanda, Sanjay
Rix, Hans-Walter
Skillman, Evan D.
TI PHAT STELLAR CLUSTER SURVEY. I. YEAR 1 CATALOG AND INTEGRATED PHOTOMETRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; galaxies: individual (M31); galaxies: star clusters: general
ID LARGE-MAGELLANIC-CLOUD; YOUNG STAR-CLUSTERS; ASYMPTOTIC GIANT BRANCH;
GALACTIC OPEN CLUSTERS; SPACE-TELESCOPE SURVEY; M31 GLOBULAR-CLUSTERS;
INITIAL MASS FUNCTION; LOCAL GROUP GALAXIES; LUMINOSITY FUNCTION; SPIRAL
GALAXIES
AB The Panchromatic Hubble Andromeda Treasury (PHAT) survey is an ongoing Hubble Space Telescope (HST) multi-cycle program to obtain high spatial resolution imaging of one-third of the M31 disk at ultraviolet through near-infrared wavelengths. In this paper, we present the first installment of the PHAT stellar cluster catalog. When completed, the PHAT cluster catalog will be among the largest and most comprehensive surveys of resolved star clusters in any galaxy. The exquisite spatial resolution achieved with HST has allowed us to identify hundreds of new clusters that were previously inaccessible with existing ground-based surveys. We identify 601 clusters in the Year 1 sample, representing more than a factor of four increase over previous catalogs within the current survey area (390 arcmin(2)). This work presents results derived from the first similar to 25% of the survey data; we estimate that the final sample will include similar to 2500 clusters. For the Year 1 objects, we present a catalog with positions, radii, and six-band integrated photometry. Along with a general characterization of the cluster luminosities and colors, we discuss the cluster luminosity function, the cluster size distributions, and highlight a number of individually interesting clusters found in the Year 1 search.
C1 [Johnson, L. Clifton; Dalcanton, Julianne J.; Fouesneau, Morgan; Hodge, Paul W.; Weisz, Daniel R.; Williams, Benjamin F.; Beerman, Lori C.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Seth, Anil C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gouliermis, Dimitrios A.] Univ Heidelberg, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Gouliermis, Dimitrios A.; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Larsen, Soren S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Olsen, Knut A. G.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[San Roman, Izaskun; Sarajedini, Ata] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Bianchi, Luciana] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85756 USA.
[Girardi, Leo] Osservatorio Astron Padova INAF, I-35122 Padua, Italy.
[Guhathakurta, Puragra] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Kalirai, Jason] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Lang, Dustin] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Monachesi, Antonela] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Nanda, Sanjay] Indian Inst Technol, Kanpur 208016, Uttar Pradesh, India.
[Skillman, Evan D.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
RP Johnson, LC (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM lcjohnso@astro.washington.edu
OI Gouliermis, Dimitrios/0000-0002-2763-0075; Johnson,
Lent/0000-0001-6421-0953
FU NASA from the Space Telescope Science Institute [HST-GO-12055]; NASA
[NAS5-26555]; German Aerospace Center (DLR); German Research Foundation
(DFG) [50 OR 0908, GO 1659/3-1]
FX The authors acknowledge the collective efforts of the entire PHAT team
in this project. Also, the authors thank the anonymous referee for a
prompt and useful report. This research made extensive use of NASA's
Astrophysics Data System Bibliographic Services. Support for this work
was provided by NASA through grant number HST-GO-12055 from the Space
Telescope Science Institute, which is operated by AURA, Inc., under NASA
contract NAS5-26555. D.A.G. acknowledges financial support from the
German Aerospace Center (DLR) and the German Research Foundation (DFG)
through grants 50 OR 0908 and GO 1659/3-1, respectively.
NR 84
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 95
DI 10.1088/0004-637X/752/2/95
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000018
ER
PT J
AU Ma, CJ
Owers, M
Nulsen, PEJ
McNamara, BR
Murray, SS
Couch, WJ
AF Ma, Cheng-Jiun
Owers, Matt
Nulsen, Paul E. J.
McNamara, Brian R.
Murray, Stephen S.
Couch, Warrick J.
TI ABELL 1201: A MINOR MERGER AT SECOND CORE PASSAGE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (A1201)
ID X-RAY DATA; COLD-FRONT; GALAXY CLUSTERS; HYDRA-A; GAS; CHANDRA;
COMPILATION; TEMPERATURE; SAMPLE
AB We present an analysis of the structures and dynamics of the merging cluster Abell 1201, which has two sloshing cold fronts around a cooling core, and an offset gas core approximately 500 kpc northwest of the center. New Chandra and XMM-Newton data reveal a region of enhanced brightness east of the offset core, with breaks in surface brightness along its boundary to the north and east. This is interpreted as a tail of gas stripped from the offset core. Gas in the offset core and the tail is distinguished from other gas at the same distance from the cluster center chiefly by having higher density, hence lower entropy. In addition, the offset core shows marginally lower temperature and metallicity than the surrounding area. The metallicity in the cool core is high and there is an abrupt drop in metallicity across the southern cold front. We interpret the observed properties of the system, including the placement of the cold fronts, the offset core, and its tail in terms of a simple merger scenario. The offset core is the remnant of a merging subcluster, which first passed pericenter southeast of the center of the primary cluster and is now close to its second pericenter passage, moving at similar or equal to 1000 km s(-1). Sloshing excited by the merger gave rise to the two cold fronts and the disposition of the cold fronts reveals that we view the merger from close to the plane of the orbit of the offset core.
C1 [Ma, Cheng-Jiun; Nulsen, Paul E. J.; McNamara, Brian R.; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ma, Cheng-Jiun; McNamara, Brian R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Owers, Matt] Australian Astron Observ, Epping, NSW 1710, Australia.
[Owers, Matt; Couch, Warrick J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[McNamara, Brian R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21205 USA.
RP Ma, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Owers, Matt/0000-0002-2879-1663; Nulsen, Paul/0000-0003-0297-4493
FU NASA [NAS8-03060, NNX08AD68G]; Chandra Large Project Grant [G09-0140X];
Australian Research Council
FX This work was partly supported by NASA grants NAS8-03060 and NNX08AD68G.
C.J.M. and B.R.M. are supported by Chandra Large Project Grant:
G09-0140X. B. R. M. acknowledges generous support from the Natural
Sciences and Engineering Research Council of Canada. M.S.O. and W.J.C.
acknowledge the financial support of the Australian Research Council. We
have made use of data obtained under the Chandra HRC GTO program and
software provided by the Chandra X-ray Center (CXC) in the application
packages CIAO, ChIPS, and Sherpa. STSDAS is a product of the Space
Telescope Science Institute, which is operated by AURA for NASA.
NR 38
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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 JUN 20
PY 2012
VL 752
IS 2
AR 139
DI 10.1088/0004-637X/752/2/139
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000062
ER
PT J
AU Mainzer, A
Grav, T
Masiero, J
Bauer, J
McMillan, RS
Giorgini, J
Spahr, T
Cutri, RM
Tholen, DJ
Jedicke, R
Walker, R
Wright, E
Nugent, CR
AF Mainzer, A.
Grav, T.
Masiero, J.
Bauer, J.
McMillan, R. S.
Giorgini, J.
Spahr, T.
Cutri, R. M.
Tholen, D. J.
Jedicke, R.
Walker, R.
Wright, E.
Nugent, C. R.
TI CHARACTERIZING SUBPOPULATIONS WITHIN THE NEAR-EARTH OBJECTS WITH
NEOWISE: PRELIMINARY RESULTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atlases; catalogs; minor planets, asteroids: general; surveys
ID MAIN-BELT ASTEROIDS; INFRARED-SURVEY-EXPLORER; APOLLO-AMOR OBJECTS;
WISE/NEOWISE OBSERVATIONS; APPROACHING ASTEROIDS; DYNAMICAL EVOLUTION;
SIZE DISTRIBUTIONS; SUFFICIENT SOURCE; POPULATION; MAGNITUDE
AB We present the preliminary results of an analysis of the sub-populations within the near-Earth asteroids, including the Atens, Apollos, Amors, and those that are considered potentially hazardous using data from the Wide-field Infrared Survey Explorer (WISE). In order to extrapolate the sample of objects detected by WISE to the greater population, we determined the survey biases for asteroids detected by the project's automated moving object processing system (known as NEOWISE) as a function of diameter, visible albedo, and orbital elements. Using this technique, we are able to place constraints on the number of potentially hazardous asteroids larger than 100 m and find that there are similar to 4700 +/- 1450 such objects. As expected, the Atens, Apollos, and Amors are revealed by WISE to have somewhat different albedo distributions, with the Atens being brighter than the Amors. The cumulative size distributions of the various near-Earth object (NEO) subgroups vary slightly between 100 m and 1 km. A comparison of the observed orbital elements of the various sub-populations of the NEOs with the current best model is shown.
C1 [Mainzer, A.; Masiero, J.; Bauer, J.; Giorgini, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Bauer, J.; Cutri, R. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[McMillan, R. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[Tholen, D. J.; Jedicke, R.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Walker, R.] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Wright, E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Nugent, C. R.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM amainzer@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; Planetary Science
Division of the 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, funded by the National Aeronautics and Space
Administration. 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. We thank our referee, Dr.
Alan Harris of the Space Science Institute, for his helpful comments,
which led to a number of new insights, in particular the suggestion to
split the Amors by perihelion. We gratefully acknowledge the
extraordinary services specific to NEOWISE contributed by the
International Astronomical Union's Minor Planet Center, operated by the
Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for
Astronomical Telegrams, operated by Harvard University. We also thank
the worldwide community of dedicated amateur and professional
astronomers devoted to minor planet follow-up observations. 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.
NR 55
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 110
DI 10.1088/0004-637X/752/2/110
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000033
ER
PT J
AU Masiunas, LC
Gutermuth, RA
Pipher, JL
Megeath, ST
Myers, PC
Allen, LE
Kirk, HM
Fazio, GG
AF Masiunas, L. C.
Gutermuth, R. A.
Pipher, J. L.
Megeath, S. T.
Myers, P. C.
Allen, L. E.
Kirk, H. M.
Fazio, G. G.
TI A STRUCTURAL ANALYSIS OF STAR-FORMING REGION AFGL 490
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; stars: formation; stars: pre-main sequence
ID SPITZER-SPACE-TELESCOPE; YOUNG STELLAR CLUSTERS; MOLECULAR CLOUDS;
SURFACE-DENSITY; C2D SURVEY; NEARBY; PHOTOMETRY; KILOPARSEC; EVOLUTION;
MODELS
AB We present Spitzer IRAC and MIPS observations of the star-forming region containing intermediate-mass young stellar object (YSO) AFGL 490. We supplement these data with near-IR Two Micron All Sky Survey photometry and with deep Simultaneous Quad Infrared Imaging Device observations off the central high-extinction region. We have more than doubled the known membership of this region to 57 Class I and 303 Class II YSOs via the combined 1-24 mu m photometric catalog derived from these data. We construct and analyze the minimum spanning tree of their projected positions, isolating one locally overdense cluster core containing 219 YSOs (60.8% of the region's members). We find this cluster core to be larger yet less dense than similarly analyzed clusters. Although the structure of this cluster core appears irregular, we demonstrate that the parsec-scale surface densities of both YSOs and gas are correlated with a power-law slope of 2.8, as found for other similarly analyzed nearby molecular clouds. We also explore the mass segregation implications of AFGL 490's offset from the center of its core, finding that it has no apparent preferential central position relative to the low-mass members.
C1 [Masiunas, L. C.] Smith Coll, Coll Astron Dept 5, Northampton, MA 01063 USA.
[Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Pipher, J. L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Myers, P. C.; Kirk, H. M.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
RP Masiunas, LC (reprint author), Smith Coll, Coll Astron Dept 5, Northampton, MA 01063 USA.
FU National Aeronautics and Space Administration; National Science
Foundation; NASA [1407, NNX11AD14G]; NASA through JPL [960541]; Smith
College Summer Research Fellows (SURF) Program; Massachusetts Space
Grant Consortium; Five College Astronomy Department
FX 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
SIMBAD database, operated at CDS, Strasbourg, France. This research has
made use of the VizieR catalog access tool, CDS, Strasbourg, France.
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 1407 with NASA.
Support for the IRAC instrument was provided by NASA through contract
960541 issued by JPL. R. A. G. gratefully acknowledges support from NASA
grant NNX11AD14G. L. C. M. wishes to acknowledge funding support from
the Smith College Summer Research Fellows (SURF) Program, the
Massachusetts Space Grant Consortium, and the Five College Astronomy
Department.
NR 33
TC 10
Z9 10
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 127
DI 10.1088/0004-637X/752/2/127
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000050
ER
PT J
AU Newman, SF
Griffin, KS
Genzel, R
Davies, R
Forster-Schreiber, NM
Tacconi, LJ
Kurk, J
Wuyts, S
Genel, S
Lilly, SJ
Renzini, A
Bouche, N
Burkert, A
Cresci, G
Buschkamp, P
Carollo, CM
Eisenhauer, F
Hicks, E
Lutz, D
Mancini, C
Naab, T
Peng, YJ
Vergani, D
AF Newman, Sarah F.
Griffin, Kristen Shapiro
Genzel, Reinhard
Davies, Ric
Foerster-Schreiber, Natascha M.
Tacconi, Linda J.
Kurk, Jaron
Wuyts, Stijn
Genel, Shy
Lilly, Simon J.
Renzini, Alvio
Bouche, Nicolas
Burkert, Andreas
Cresci, Giovanni
Buschkamp, Peter
Carollo, C. Marcella
Eisenhauer, Frank
Hicks, Erin
Lutz, Dieter
Mancini, Chiara
Naab, Thorsten
Peng, Yingjie
Vergani, Daniela
TI SHOCKED SUPERWINDS FROM THE z similar to 2 CLUMPY STAR-FORMING GALAXY,
ZC406690
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: star formation;
ISM: jets and outflows
ID INTEGRAL FIELD SPECTROSCOPY; LYMAN-BREAK GALAXIES; GIANT MOLECULAR
CLOUDS; ULTRA DEEP FIELD; INFRARED LUMINOSITY FUNCTIONS; LOW-METALLICITY
GALAXIES; DATA REDUCTION SOFTWARE; TULLY-FISHER RELATION; H-ALPHA
EMISSION; HIGH-REDSHIFT
AB We have obtained high-resolution data of the z similar to 2 ring-like, clumpy star-forming galaxy (SFG) ZC406690 using the VLT/SINFONI with adaptive optics (in K band) and in seeing-limited mode (in H and J bands). Our data include all of the main strong optical emission lines: [O II], [O III], H alpha, H beta, [N II], and [S II]. We find broad, blueshifted H alpha and [O III] emission line wings in the spectra of the galaxy's massive, star-forming clumps (sigma similar to 85 km s(-1)) and even broader wings (up to 70% of the total Ha flux, with s similar to 290 km s(-1)) in regions spatially offset from the clumps by similar to 2 kpc. The broad emission likely originates from large-scale outflows with mass outflow rates from individual clumps that are 1-8x the star formation rate (SFR) of the clumps. Based on emission line ratio diagnostics ([N II]/H alpha and [S II]/H alpha) and photoionization and shock models, we find that the emission from the clumps is due to a combination of photoionization from the star-forming regions and shocks generated in the outflowing component, with 5%-30% of the emission deriving from shocks. In terms of the ionization parameter (6x10(7) to 10(8) cm s(-1), based on both the SFR and the O-32 ratio), density (local electron densities of 300-1800 cm(-3) in and around the clumps, and ionized gas column densities of 1200-8000 M(circle dot)pc(-2)), and SFR (10-40 M-circle dot yr(-1)), these clumps more closely resemble nuclear starburst regions of local ultraluminous infrared galaxies and dwarf irregulars than H II regions in local galaxies. However, the star-forming clumps are not located in the nucleus as in local starburst galaxies but instead are situated in a ring several kpc from the center of their high-redshift host galaxy, and have an overall disk-like morphology. The two brightest clumps are quite different in terms of their internal properties, energetics, and relative ages, and thus we are given a glimpse at two different stages in the formation and evolution of rapidly star-forming giant clumps at high-z.
C1 [Newman, Sarah F.; Genzel, Reinhard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Griffin, Kristen Shapiro] Northrop Grumman Aerosp Syst, Aerosp Res Labs, Redondo Beach, CA 90278 USA.
[Genzel, Reinhard; Davies, Ric; Foerster-Schreiber, Natascha M.; Tacconi, Linda J.; Kurk, Jaron; Wuyts, Stijn; Genel, Shy; Buschkamp, Peter; Eisenhauer, Frank; Lutz, Dieter] Max Planck Inst Extraterr Physik MPE, D-85748 Garching, Germany.
[Genzel, Reinhard] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Genel, Shy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lilly, Simon J.; Carollo, C. Marcella; Peng, Yingjie] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
[Renzini, Alvio; Mancini, Chiara] Osserv Astron Padova, I-35122 Padua, Italy.
[Bouche, Nicolas] Univ Calif Santa Barbara, Dept Phys & Astron, Santa Barbara, CA 93106 USA.
[Burkert, Andreas] Univ Sternwarte Ludwig Maximilians Univ USM, Dept Phys, D-81679 Munich, Germany.
[Cresci, Giovanni] Osserv Astrofis Arcetri, Ist Nazl Astrofis, I-50125 Florence, Italy.
[Hicks, Erin] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Naab, Thorsten] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Vergani, Daniela] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
RP Newman, SF (reprint author), Univ Calif Berkeley, Dept Astron, Campbell Hall, Berkeley, CA 94720 USA.
EM sfnewman@berkeley.edu
OI Vergani, Daniela/0000-0003-0898-2216; Genel, Shy/0000-0002-3185-1540;
Cresci, Giovanni/0000-0002-5281-1417
FU NSF; ASI; INAF
FX We thank the ESO staff, especially those at Paranal Observatory, for
their ongoing support during the many past and continuing observing runs
over which the SINS project is being carried out. We also acknowledge
the SINFONI and PARSEC teams, whose devoted work on the instrument and
laser paved the way for the success of the SINS observations. We also
thank Mike Dopita and Emily Levesque for sharing the data from their
photoionization and shock models and for useful discussions regarding
those models. We also thank Sylvain Veilleux, Amiel Sternberg, and Eliot
Quataert for helpful conversations concerning this work. S.F.N. is
supported by an NSF grfp grant. C. M., A. R., and D. V. acknowledge
partial support by the ASI grant "COFIS-Analisi Dati" and by the INAF
grant "PRIN-2008."
NR 120
TC 41
Z9 41
U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 111
DI 10.1088/0004-637X/752/2/111
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000034
ER
PT J
AU Prescott, MKM
Dey, A
Brodwin, M
Chaffee, FH
Desai, V
Eisenhardt, P
Floc'h, E
Jannuzi, BT
Kashikawa, N
Matsuda, Y
Soifer, BT
AF Prescott, Moire K. M.
Dey, Arjun
Brodwin, Mark
Chaffee, Frederic H.
Desai, Vandana
Eisenhardt, Peter
Le Floc'h, Emeric
Jannuzi, Buell T.
Kashikawa, Nobunari
Matsuda, Yuichi
Soifer, B. T.
TI RESOLVING THE GALAXIES WITHIN A GIANT Ly alpha NEBULA: WITNESSING THE
FORMATION OF A GALAXY GROUP?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift
ID STAR-FORMING GALAXIES; SPITZER-SPACE-TELESCOPE; ULTRA DEEP FIELD;
EQUAL-TO 2.3; HIGH-REDSHIFT; COLD ACCRETION; COLLAPSING PROTOGALAXIES;
STELLAR POPULATIONS; COOLING RADIATION; SPIDERWEB GALAXY
AB Detailed analysis of the substructure of Ly alpha nebulae can put important constraints on the physical mechanisms at work and the properties of galaxies forming within them. Using high-resolution Hubble Space Telescope (HST) imaging of a Ly alpha nebula at z approximate to 2.656, we have taken a census of the compact galaxies in the vicinity, used optical/near-infrared colors to select system members, and put constraints on the morphology of the spatially extended emission. The system is characterized by (1) a population of compact, low-luminosity (similar to 0.1 L*) sources-17 primarily young, small (R-e approximate to 1-2 kpc), disky galaxies including an obscured active galactic nucleus-that are all substantially offset (greater than or similar to 20 kpc) from the line-emitting nebula; (2) the lack of a central galaxy at or near the peak of the Ly alpha emission; and (3) several nearly coincident, spatially extended emission components-Ly alpha, He II, and UV continuum-that are extremely smooth. These morphological findings are difficult to reconcile with theoretical models that invoke outflows, cold flows, or resonant scattering, suggesting that while all of these physical phenomena may be occurring, they are not sufficient to explain the powering and large extent of Ly alpha nebulae. In addition, although the compact galaxies within the system are irrelevant as power sources, the region is significantly overdense relative to the field galaxy population (by at least a factor of four). These observations provide the first estimate of the luminosity function of galaxies within an individual Ly alpha nebula system and suggest that large Ly alpha nebulae may be the seeds of galaxy groups or low-mass clusters.
C1 [Prescott, Moire K. M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Prescott, Moire K. M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brodwin, Mark] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA.
[Chaffee, Frederic H.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
[Desai, Vandana; Soifer, B. T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Eisenhardt, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Le Floc'h, Emeric] Univ Paris, CNRS, DSM, Lab AIM,CEA, F-91191 Gif Sur Yvette, France.
[Kashikawa, Nobunari] Natl Inst Nat Sci, Natl Astron Observ Japan, Div Opt & Infrared Astron, Mitaka, Tokyo 1818588, Japan.
[Matsuda, Yuichi] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Soifer, B. T.] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA.
EM mkpresco@physics.ucsb.edu
FU NSF Graduate Research Fellowship; P.E.O. Fellowship; TABASGO Prize
Postdoctoral Fellowship; NASA [NAS 5-26555]; NOAO; Spitzer Space
Telescope project
FX The authors thank Kate Brand, Galina Soutchkova, and Sangeeta Malhotra
for their assistance with the HST observation planning and execution. We
are grateful to Crystal Martin, Kristian Finlator, Avi Loeb, Dan
Weedman, Tommaso Treu, Matt Auger, and the anonymous referee for useful
discussions and suggestions. M.K. M.P. acknowledges support from an NSF
Graduate Research Fellowship, a P.E.O. Fellowship, and a TABASGO Prize
Postdoctoral Fellowship. This work was based on observations made with
the NASA/ESA Hubble Space Telescope (HST Cycle 14; GO# 10591), 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. This work is also based in part on data collected
at the Subaru Telescope, which is operated by the National Astronomical
Observatory of Japan, and on data from the NOAO Deep Wide-Field Survey
(B. Jannuzi, A. Dey) as distributed by the NOAO Science Archive. A.D.
and B.T.J.'s research activities are supported by NOAO. NOAO is operated
by the Association of Universities for Research in Astronomy (AURA),
Inc. under a cooperative agreement with the National Science Foundation.
V.D. and B.T.S. are supported by the Spitzer Space Telescope project,
which is managed by JPL on behalf of NASA.
NR 81
TC 26
Z9 26
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 86
DI 10.1088/0004-637X/752/2/86
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000009
ER
PT J
AU Soderberg, AM
Margutti, R
Zauderer, BA
Krauss, M
Katz, B
Chomiuk, L
Dittmann, JA
Nakar, E
Sakamoto, T
Kawai, N
Hurley, K
Barthelmy, S
Toizumi, T
Morii, M
Chevalier, RA
Gurwell, M
Petitpas, G
Rupen, M
Alexander, KD
Levesque, EM
Fransson, C
Brunthaler, A
Bietenholz, MF
Chugai, N
Grindlay, J
Copete, A
Connaughton, V
Briggs, M
Meegan, C
von Kienlin, A
Zhang, X
Rau, A
Golenetskii, S
Mazets, E
Cline, T
AF Soderberg, A. M.
Margutti, R.
Zauderer, B. A.
Krauss, M.
Katz, B.
Chomiuk, L.
Dittmann, J. A.
Nakar, E.
Sakamoto, T.
Kawai, N.
Hurley, K.
Barthelmy, S.
Toizumi, T.
Morii, M.
Chevalier, R. A.
Gurwell, M.
Petitpas, G.
Rupen, M.
Alexander, K. D.
Levesque, E. M.
Fransson, C.
Brunthaler, A.
Bietenholz, M. F.
Chugai, N.
Grindlay, J.
Copete, A.
Connaughton, V.
Briggs, M.
Meegan, C.
von Kienlin, A.
Zhang, X.
Rau, A.
Golenetskii, S.
Mazets, E.
Cline, T.
TI PANCHROMATIC OBSERVATIONS OF SN 2011dh POINT TO A COMPACT PROGENITOR
STAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: individual (SN 2011dh)
ID CORE-COLLAPSE SUPERNOVAE; WOLF-RAYET STARS; SHOCK BREAKOUT; YELLOW
SUPERGIANTS; RADIO SUPERNOVAE; SPIRAL GALAXIES; IIB SUPERNOVA; LIGHT
CURVES; MASS-LOSS; 1993J
AB We report the discovery and detailed monitoring of X-ray emission associated with the Type IIb SN 2011dh using data from the Swift and Chandra satellites, placing it among the best-studied X-ray supernovae (SNe) to date. We further present millimeter and radio data obtained with the Submillimeter Array, the Combined Array for Research in Millimeter-wave Astronomy, and the Expanded Very Large Array during the first three weeks after explosion. Combining these observations with early optical photometry, we show that the panchromatic data set is well described by non-thermal synchrotron emission (radio/mm) with inverse Compton scattering (X-ray) of a thermal population of optical photons. In this scenario, the shock partition fractions deviate from equipartition by a factor, (epsilon(e)/epsilon(B)) similar to 30. We derive the properties of the shock wave and the circumstellar environment and find a time-averaged shock velocity of (v) over bar approximate to 0.1c and a progenitor mass-loss rate of (M) over dot approximate to 6x10(-5) M-circle dot yr(-1) (for an assumed wind velocity, v(w) = 1000 km s(-1)). We show that these properties are consistent with the sub-class of Type IIb SNe characterized by compact progenitors (Type cIIb) and dissimilar from those with extended progenitors (Type eIIb). Furthermore, we consider the early optical emission in the context of a cooling envelope model to estimate a progenitor radius of R-* approximate to 10(11) cm, in line with the expectations for a Type cIIb SN. Together, these diagnostics are difficult to reconcile with the extended radius of the putative yellow supergiant progenitor star identified in archival Hubble Space Telescope observations, unless the stellar density profile is unusual. Finally, we searched for the high-energy shock breakout pulse using X-ray and gamma-ray observations obtained during the purported explosion date range. Based on the compact radius of the progenitor, we estimate that the shock breakout pulse was detectable with current instruments but likely missed due to their limited temporal/spatial coverage. Future all-sky missions will regularly detect shock breakout emission from compact SN progenitors enabling prompt follow-up observations with sensitive multi-wavelength facilities.
C1 [Soderberg, A. M.; Margutti, R.; Zauderer, B. A.; Chomiuk, L.; Dittmann, J. A.; Gurwell, M.; Petitpas, G.; Alexander, K. D.; Grindlay, J.; Copete, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Krauss, M.; Chomiuk, L.; Rupen, M.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Katz, B.] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA.
[Nakar, E.] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Sakamoto, T.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Sakamoto, T.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Kawai, N.; Toizumi, T.; Morii, M.] Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan.
[Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Levesque, E. M.] Univ Colorado 389 UCB, Dept Astrophys & Planetary Sci, CASA, Boulder, CO 80309 USA.
[Fransson, C.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden.
[Brunthaler, A.; von Kienlin, A.; Zhang, X.; Rau, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bietenholz, M. F.] York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada.
[Bietenholz, M. F.] Hartebeesthoek Radio Observ, ZA-1740 Krugersdorp, South Africa.
[Chugai, N.] RAS, Inst Astron, Moscow 11917, Russia.
[Connaughton, V.; Briggs, M.] Univ Alabama, Dept Phys, Huntsville, AL 35809 USA.
[Meegan, C.] NSSTC, Univ Space Res Assoc, Huntsville, AL 35805 USA.
[Golenetskii, S.; Mazets, E.] Russian Acad Sci, Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
RP Soderberg, AM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Golenetskii, Sergey/B-3818-2015;
OI Alexander, Kate/0000-0002-8297-2473
FU NASA [NNX10AI23G, NNX09AU03G, NNX07AR71G, NNX10AR12G, NAS8-03060]; NASA
through Chandra X-ray Center; 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 Maryland; National Science
Foundation; CARMA partner universities; Smithsonian Institution;
Academia Sinica; state of Illinois
FX We thank Philip Massey, Edo Berger, Ryan Foley, Maria Drout, and Robert
Kirshner for useful conversations. K.H. is grateful for IPN support from
NASA grants NNX10AI23G, NNX09AU03G, NNX07AR71G, and NNX10AR12G. B.K. and
E. M. L. are supported by NASA through Einstein Postdoctoral Fellowship
awarded by the Chandra X-ray Center, which is operated by the
Smithsonian Astrophysical Observatory for NASA under contract
NAS8-03060. 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 SMA is a joint project between the
Smithsonian Astrophysical Observatory and the Academia Sinica Institute
of Astronomy and Astrophysics, and is funded by the Smithsonian
Institution and the Academia Sinica. The EVLA is operated by the
National Radio Astronomy Observatory, a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc.
NR 72
TC 44
Z9 44
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 78
DI 10.1088/0004-637X/752/2/78
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000001
ER
PT J
AU Wagg, J
Pope, A
Alberts, S
Armus, L
Brodwin, M
Bussmann, RS
Desai, V
Dey, A
Jannuzi, B
Le Floc'h, E
Melbourne, J
Stern, D
AF Wagg, Jeff
Pope, Alexandra
Alberts, Stacey
Armus, Lee
Brodwin, Mark
Bussmann, Robert S.
Desai, Vandana
Dey, Arjun
Jannuzi, Buell
Le Floc'h, Emeric
Melbourne, Jason
Stern, Daniel
TI CO J=2-1 LINE EMISSION IN CLUSTER GALAXIES AT z similar to 1: FUELING
STAR FORMATION IN DENSE ENVIRONMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: evolution; galaxies: formation;
ISM: molecules
ID ACTIVE GALACTIC NUCLEI; DUST-OBSCURED GALAXIES; MASSIVE DISK GALAXIES;
QUASAR HOST GALAXIES; IRAC SHALLOW SURVEY; WIDE-FIELD SURVEY; MOLECULAR
GAS; SUBMILLIMETER GALAXIES; FORMING GALAXIES; REDSHIFT SURVEY
AB We present observations of CO J = 2-1 line emission in infrared-luminous cluster galaxies at z similar to 1 using the IRAM Plateau de Bure Interferometer. Our two primary targets are optically faint, dust-obscured galaxies (DOGs) found to lie within 2 Mpc of the centers of two massive (> 10(14) M-circle dot) galaxy clusters. CO line emission is not detected in either DOG. We calculate 3 sigma upper limits to the CO J = 2-1 line luminosities, L'(CO) < 6.08 x 10(9) and <6.63 x 10(9) K km s(-1) pc(2). Assuming a CO-to-H-2 conversion factor derived for ultraluminous infrared galaxies in the local universe, this translates to limits on the cold molecular gasmass of M-H2 < 4.86 x 10(9) M-circle dot and M-H2 < 5.30 x 10(9) M-circle dot. Both DOGs exhibit mid-infrared continuum emission that follows a power law, suggesting that an active galactic nucleus (AGN) contributes to the dust heating. As such, estimates of the star formation efficiencies in these DOGs are uncertain. A third cluster member with an infrared luminosity, L-IR < 7.4 x 10(11) L-circle dot, is serendipitously detected in CO J = 2-1 line emission in the field of one of the DOGs located roughly two virial radii away from the cluster center. The optical spectrum of this object suggests that it is likely an obscured AGN, and the measured CO line luminosity is L'(CO) = (1.94 +/- 0.35) x 10(10) K km s(-1) pc(2), which leads to an estimated cold molecular gas mass M-H2 = (1.55 +/- 0.28) x 10(10) M-circle dot. A significant reservoir of molecular gas in a z similar to 1 galaxy located away from the cluster center demonstrates that the fuel can exist to drive an increase in star formation and AGN activity at the outskirts of high-redshift clusters.
C1 [Wagg, Jeff] European So Observ, Santiago 19, Chile.
[Pope, Alexandra; Alberts, Stacey] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Armus, Lee; Desai, Vandana] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Brodwin, Mark] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA.
[Bussmann, Robert S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dey, Arjun; Jannuzi, Buell] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Le Floc'h, Emeric] Univ Paris Diderot, CNRS, AIM, CEA Saclay, F-91191 Gif Sur Yvette, France.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wagg, J (reprint author), European So Observ, Casilla 19001, Santiago 19, Chile.
EM jwagg@eso.org
FU Marie Curie Actions of the European Commission (FP7-COFUND); W. M. Keck
Foundation; NASA
FX We thank Jan-Martin Winters, Melanie Krips, and Roberto Neri for their
helpful advice and guidance with the data analysis. For their
contributions to this survey, we thank Anthony Gonzalez and Thomas
Soifer, as well as Adam Stanford for the LRIS spectrum. This work was
co-funded under the Marie Curie Actions of the European Commission
(FP7-COFUND). Some of the data presented herein were obtained at the W.
M. Keck Observatory, which is operated as a scientific partnership among
the California Institute of Technology, the University of California,
and the National Aeronautics and Space Administration. The Observatory
was made possible by the generous financial support of the W. M. Keck
Foundation. Part of this work is based on observations made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was provided by NASA. Herschel is an ESA
space observatory with science instruments provided by European-led
Principal Investigator consortia and with important participation from
NASA.
NR 54
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 91
DI 10.1088/0004-637X/752/2/91
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000014
ER
PT J
AU Wang, T
Huang, JS
Faber, SM
Fang, GW
Wuyts, S
Fazio, GG
Yan, HJ
Dekel, A
Guo, YC
Ferguson, HC
Grogin, N
Lotz, JM
Weiner, B
McGrath, EJ
Kocevski, D
Hathi, NP
Lucas, RA
Koekemoer, AM
Kong, X
Gu, QS
AF Wang, Tao
Huang, Jia-Sheng
Faber, S. M.
Fang, Guanwen
Wuyts, Stijn
Fazio, G. G.
Yan, Haojing
Dekel, Avishai
Guo, Yicheng
Ferguson, Henry C.
Grogin, Norman
Lotz, Jennifer M.
Weiner, Benjamin
McGrath, Elizabeth J.
Kocevski, Dale
Hathi, Nimish P.
Lucas, Ray A.
Koekemoer, A. M.
Kong, Xu
Gu, Qiu-Sheng
TI CANDELS: CORRELATIONS OF SPECTRAL ENERGY DISTRIBUTIONS AND MORPHOLOGIES
WITH STAR FORMATION STATUS FOR MASSIVE GALAXIES AT z similar to 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift;
galaxies: structure
ID HUBBLE-SPACE-TELESCOPE; EXTREMELY RED OBJECTS; DEEP FIELD-SOUTH;
HIGH-REDSHIFT GALAXIES; INFRARED SPECTROSCOPIC SURVEY; STELLAR
POPULATION SYNTHESIS; PASSIVELY EVOLVING GALAXIES; EXTRAGALACTIC LEGACY
SURVEY; COMPACT QUIESCENT GALAXIES; K-SELECTED GALAXIES
AB We present a study on spectral energy distributions, morphologies, and star formation for an IRAC-selected extremely red object sample in the GOODS Chandra Deep Field-South. This work was enabled by new HST/WFC3 near-IR imaging from the CANDELS survey as well as the deepest available X-ray data from Chandra 4 Ms observations. This sample consists of 133 objects with the 3.6 mu m limiting magnitude of [3.6] = 21.5 and is approximately complete for galaxies with M-* > 10(11) M-circle dot at 1.5 <= z <= 2.5. We classify this sample into two types, quiescent and star-forming galaxies (SFGs), in the observed infrared color-color ([3.6]-[24] versus K - [3.6]) diagram. The further morphological study of this sample shows a consistent result with the observed color classification. The classified quiescent galaxies are bulge dominated and SFGs in the sample have disk or irregular morphologies. Our observed infrared color classification is also consistent with the rest-frame color (U - V versus V - J) classification. We also found that quiescent and SFGs are well separated in the nonparametric morphology parameter (Gini versus M-20) diagram measuring their concentration and clumpiness: quiescent galaxies have a Gini coefficient higher than 0.58 and SFGs have a Gini coefficient lower than 0.58. We argue that the star formation quenching process must lead to or be accompanied by the increasing galaxy concentration. One prominent morphological feature of this sample is that disks are commonly seen in this massive galaxy sample at 1.5 <= z <= 2.5: 30% of quiescent galaxies and 70% of SFGs withM(*) > 10(11) M-circle dot have disks in their rest-frame optical morphologies. The prevalence of these extended, relatively undisturbed disks challenges the merging scenario as the main mode of massive galaxy formation.
C1 [Wang, Tao; Gu, Qiu-Sheng] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China.
[Wang, Tao; Huang, Jia-Sheng; Fang, Guanwen; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Faber, S. M.; McGrath, Elizabeth J.; Kocevski, Dale] Univ Calif Santa Cruz, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95064 USA.
[Fang, Guanwen; Kong, Xu] Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Peoples R China.
[Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Yan, Haojing] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Guo, Yicheng] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Ferguson, Henry C.; Grogin, Norman; Lotz, Jennifer M.; Lucas, Ray A.; Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Weiner, Benjamin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Hathi, Nimish P.] Carnegie Observ, Pasadena, CA 91101 USA.
RP Wang, T (reprint author), Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China.
EM taowang@nju.edu.cn
RI Hathi, Nimish/J-7092-2014;
OI Hathi, Nimish/0000-0001-6145-5090; Koekemoer, Anton/0000-0002-6610-2048
FU NASA [NAS5-26555]; National Natural Science Foundation of China
[11133001, 10878010, 10873012]; National Basic Research Program (973
program) [2007CB815404, 2007CB815405]
FX 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. We gratefully acknowledge R. Abraham for access to
his morphology analysis code. This work is also supported under the
National Natural Science Foundation of China under grants (11133001,
10878010, and 10873012) and the National Basic Research Program (973
program No. 2007CB815404 and 2007CB815405). We are greatful to the
anonymous referee for helpful comments.
NR 115
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2012
VL 752
IS 2
AR 134
DI 10.1088/0004-637X/752/2/134
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965AK
UT WOS:000305738000057
ER
PT J
AU Braje, TJ
Rick, TC
Erlandson, JM
AF Braje, Todd J.
Rick, Torben C.
Erlandson, Jon M.
TI A trans-Holocene historical ecological record of shellfish harvesting on
California's Northern Channel Islands
SO QUATERNARY INTERNATIONAL
LA English
DT Article
ID SAN-MIGUEL ISLAND; HUMAN IMPACTS; SOUTHERN CALIFORNIA; MARITIME
CULTURES; CLIMATE-CHANGE; PACIFIC COAST; ROSA ISLAND; DAISY CAVE;
AMERICA; ABALONE
AB For over 10,000 years, shellfish were an important food and raw material resource for ancient peoples on California's Northern Channel Islands. Early Channel Island peoples often focused on large, easy-togather intertidal species such as California mussels (Mytilus californianus) and black abalone (Haliotis cracherodii), with later peoples expanding their shellfish economy to include a wider range of species. By the time of European contact (AD 1542-1820) the Island Chumash lived in large, sedentary villages and collected a diverse range of shellfish species by the millions. Although predation by the Chumash and their ancestors affected the size of several key shellfish species, 19th and 20th century commercial harvests targeted specific, high-value species for global markets, bringing several shellfish species (e.g., white [Haliotis sorenseni], pink [Haliotis corrugata], and black abalone) to the brink of extinction. This analysis of shellfish remains from Northern Channel Island archaeological sites tracks the changing role of shellfish in human subsistence economies from Terminal Pleistocene to Historic times. An archaeological record featuring several millennia of relative resiliency under intensive Native American predation suggests that regulated, sustainable, and productive shellfish fisheries can be maintained if balanced and healthy near-shore ecosystems are rebuilt. (C) 2011 Elsevier Ltd and INQUA. All rights reserved.
C1 [Braje, Todd J.] San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA.
[Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA.
[Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA.
RP Braje, TJ (reprint author), San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA.
EM tbraje@mail.sdsu.edu; rickt@si.edu; jerland@uoregon.edu
OI Erlandson, Jon/0000-0002-4705-4319
FU National Science Foundation; National Park Service; Western National
Parks Association; University of Oregon; Smithsonian Institution
FX Our research on the Channel Islands has been supported by multiple
grants from the National Science Foundation, the National Park Service,
and the Western National Parks Association, as well as support from the
University of Oregon and the Smithsonian Institution. We are grateful to
Ann Huston, Don Morris, Kelly Minas, and Ian Williams of Channel Islands
National Park for helping facilitate our research. Thanks to Tiina Manne
and Britt Starkovich for inviting us to participate in the Society for
American Archaeology session that resulted in this manuscript. Finally,
we thank the editors, two anonymous reviewers, and production staff of
Quaternary International for helping bring this paper to fruition.
NR 74
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1040-6182
EI 1873-4553
J9 QUATERN INT
JI Quat. Int.
PD JUN 20
PY 2012
VL 264
BP 109
EP 120
DI 10.1016/j.quaint.2011.09.011
PG 12
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 963WU
UT WOS:000305656500010
ER
PT J
AU Parrent, JT
Howell, DA
Friesen, B
Thomas, RC
Fesen, RA
Milisavljevic, D
Bianco, FB
Dilday, B
Nugent, P
Baron, E
Arcavi, I
Ben-Ami, S
Bersier, D
Bildsten, L
Bloom, J
Cao, Y
Cenko, SB
Filippenko, AV
Gal-Yam, A
Kasliwal, MM
Konidaris, N
Kulkarni, SR
Law, NM
Levitan, D
Maguire, K
Mazzali, PA
Ofek, EO
Pan, Y
Polishook, D
Poznanski, D
Quimby, RM
Silverman, JM
Sternberg, A
Sullivan, M
Walker, ES
Xu, D
Buton, C
Pereira, R
AF Parrent, J. T.
Howell, D. A.
Friesen, B.
Thomas, R. C.
Fesen, R. A.
Milisavljevic, D.
Bianco, F. B.
Dilday, B.
Nugent, P.
Baron, E.
Arcavi, I.
Ben-Ami, S.
Bersier, D.
Bildsten, L.
Bloom, J.
Cao, Y.
Cenko, S. B.
Filippenko, A. V.
Gal-Yam, A.
Kasliwal, M. M.
Konidaris, N.
Kulkarni, S. R.
Law, N. M.
Levitan, D.
Maguire, K.
Mazzali, P. A.
Ofek, E. O.
Pan, Y.
Polishook, D.
Poznanski, D.
Quimby, R. M.
Silverman, J. M.
Sternberg, A.
Sullivan, M.
Walker, E. S.
Xu, Dong
Buton, C.
Pereira, R.
TI ANALYSIS OF THE EARLY-TIME OPTICAL SPECTRA OF SN 2011fe IN M101
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE supernovae: general; supernovae: individual (SN 2011fe)
ID IA SUPERNOVA SPECTRA; WHITE-DWARF STAR; FACTORY OBSERVATIONS; COMPANION
STAR; PROGENITOR; DIVERSITY; FEATURES; SIGNATURES; MERGERS; EJECTA
AB The nearby Type Ia supernova (SN Ia) SN 2011fe in M101 (cz = 241 km s(-1)) provides a unique opportunity to study the early evolution of a "normal" SN Ia, its compositional structure, and its elusive progenitor system. We present 18 high signal-to-noise spectra of SN 2011fe during its first month beginning 1.2 days post-explosion and with an average cadence of 1.8 days. This gives a clear picture of how various line-forming species are distributed within the outer layers of the ejecta, including that of unburned material (C+O). We follow the evolution of C II absorption features until they diminish near maximum light, showing overlapping regions of burned and unburned material between ejection velocities of 10,000 and 16,000 km s(-1). This supports the notion that incomplete burning, in addition to progenitor scenarios, is a relevant source of spectroscopic diversity among SNe Ia. The observed evolution of the highlyDoppler-shifted OI lambda 7774 absorption features detected within 5 days post-explosion indicates the presence of OI with expansion velocities from 11,500 to 21,000 km s(-1). The fact that some OI is present above C II suggests that SN 2011fe may have had an appreciable amount of unburned oxygen within the outer layers of the ejecta.
C1 [Parrent, J. T.; Fesen, R. A.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.
[Parrent, J. T.; Howell, D. A.; Bianco, F. B.; Dilday, B.] Global Telescope Network, Las Cumbres Observ, Goleta, CA 93117 USA.
[Howell, D. A.; Bianco, F. B.; Dilday, B.; Bildsten, L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93117 USA.
[Friesen, B.; Baron, E.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Thomas, R. C.; Nugent, P.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Milisavljevic, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Nugent, P.; Bloom, J.; Cenko, S. B.; Filippenko, A. V.; Silverman, J. M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Baron, E.] Hamburger Sternwarte, D-21029 Hamburg, Germany.
[Baron, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Arcavi, I.; Ben-Ami, S.; Gal-Yam, A.; Ofek, E. O.; Xu, Dong] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Cao, Y.; Konidaris, N.; Kulkarni, S. R.; Levitan, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Kasliwal, M. M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Law, N. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Maguire, K.; Pan, Y.; Sullivan, M.] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England.
[Mazzali, P. A.; Sternberg, A.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Mazzali, P. A.] INAF Osservatorio Astron, I-35122 Padua, Italy.
[Polishook, D.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Poznanski, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Quimby, R. M.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Walker, E. S.] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Buton, C.] Univ Bonn, Phys Inst, D-53115 Bonn, Germany.
[Pereira, R.] Univ Lyon, F-69622 Villeurbanne, France.
[Pereira, R.] Univ Lyon 1, F-69622 Villeurbanne, France.
[Pereira, R.] Inst Phys Nucl, CNRS, IN2P3, Lyon, France.
RP Parrent, JT (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.
OI Baron, Edward/0000-0001-5393-1608; Sullivan, Mark/0000-0001-9053-4820
FU Las Cumbres Observatory Global Telescope Network; Office of Science of
the U.S. Department of Energy [DE-AC02-05CH11231]
FX This work was supported by the Las Cumbres Observatory Global Telescope
Network. This research used resources of the National Energy Research
Scientific Computing Center, which is supported by the Office of Science
of the U.S. Department of Energy under contract no. DE-AC02-05CH11231.
NR 42
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U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUN 20
PY 2012
VL 752
IS 2
AR L26
DI 10.1088/2041-8205/752/2/L26
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961JV
UT WOS:000305461600009
ER
PT J
AU Hagedorn, M
McCarthy, M
Carter, VL
Meyers, SA
AF Hagedorn, Mary
McCarthy, Megan
Carter, Virginia L.
Meyers, Stuart A.
TI Oxidative Stress in Zebrafish (Danio rerio) Sperm
SO PLOS ONE
LA English
DT Article
ID SPONTANEOUS LIPID-PEROXIDATION; OXYGEN SPECIES GENERATION;
HUMAN-SPERMATOZOA; SUPEROXIDE-DISMUTASE; HYDROGEN-PEROXIDE; DNA-DAMAGE;
GLUTATHIONE-PEROXIDASE; EQUINE SPERMATOZOA; MOUSE SPERMATOZOA;
HIGH-THROUGHPUT
AB Laboratories around the world have produced tens of thousands of mutant and transgenic zebrafish lines. As with mice, maintaining all of these valuable zebrafish genotypes is expensive, risky, and beyond the capacity of even the largest stock centers. Because reducing oxidative stress has become an important aspect of reducing the variability in mouse sperm cryopreservation, we examined whether antioxidants might improve cryopreservation of zebrafish sperm. Four experiments were conducted in this study. First, we used the xanthine-xanthine oxidase (X-XO) system to generate reactive oxygen species (ROS). The X-XO system was capable of producing a stress reaction in zebrafish sperm reducing its sperm motility in a concentration dependent manner (P<0.05). Second, we examined X-XO and the impact of antioxidants on sperm viability, ROS and motility. Catalase (CAT) mitigated stress and maintained viability and sperm motility (P>0.05), whereas superoxide dismutase (SOD) and vitamin E did not (P<0.05). Third, we evaluated ROS in zebrafish spermatozoa during cryopreservation and its effect on viability and motility. Methanol (8%) reduced viability and sperm motility (P<0.05), but the addition of CAT mitigated these effects (P>0.05), producing a mean 2.0 to 2.9-fold increase in post-thaw motility. Fourth, we examined the effect of additional cryoprotectants and CAT on fresh sperm motility. Cryoprotectants, 8% methanol and 10% dimethylacetamide (DMA), reduced the motility over the control value (P<0.5), whereas 10% dimethylformamide (DMF) with or without CAT did not (P>0.05). Zebrafish sperm protocols should be modified to improve the reliability of the cryopreservation process, perhaps using a different cryoprotectant. Regardless, the simple addition of CAT to present-day procedures will significantly improve this process, assuring increased and less variable fertilization success and allowing resource managers to dependably plan how many straws are needed to safely cryopreserve a genetic line.
C1 [Hagedorn, Mary; Carter, Virginia L.] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Washington, DE USA.
[Hagedorn, Mary; Carter, Virginia L.] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI USA.
[McCarthy, Megan; Meyers, Stuart A.] Univ Calif Davis, Dept Anat, Sch Vet Med, Davis, CA 95616 USA.
RP Hagedorn, M (reprint author), Smithsonian Conservat Biol Inst, Dept Reprod Sci, Washington, DE USA.
EM hagedornm@si.edu
FU National Institutes of Health (NIH) [R24 RR016581, RO1 2RR016581];
Zebrafish International Research Center
FX This work was supported by a grant to MM from National Institutes of
Health (NIH) # R24 RR016581 and SM from NIH # RO1 2RR016581. The funders
had no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.; We would like to thank Dr.
Bruce Draper for his kind assistance during the preliminary studies for
this work and the Zebrafish International Research Center for their
support and comments on this manuscript. In addition, we would like to
thank the three anonymous reviewers whose comments greatly improved this
paper. This manuscript has been approved for publication by the Hawaii
Institute of Marine Biology as contribution #1490.
NR 59
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U1 1
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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 JUN 19
PY 2012
VL 7
IS 6
AR e39397
DI 10.1371/journal.pone.0039397
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 963VI
UT WOS:000305652700078
PM 22724013
ER
PT J
AU Yeung, TK
Le Sage, D
Pham, LM
Stanwix, PL
Walsworth, RL
AF Yeung, T. K.
Le Sage, D.
Pham, L. M.
Stanwix, P. L.
Walsworth, R. L.
TI Anti-reflection coating for nitrogen-vacancy optical measurements in
diamond
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID NANOSCALE RESOLUTION; SPIN-QUBIT; COHERENCE
AB We realize anti-reflection (AR) coatings for optical excitation and fluorescence measurements of nitrogen-vacancy (NV) color centers in bulk diamond by depositing quarter-wavelength thick silica layers on the diamond surface. These AR coatings improve NV-diamond optical measurements by reducing optical reflection at the diamond-air interface from approximate to 17% to approximate to 2%, which allows more effective NV optical excitation and more efficient detection of NV fluorescence. We also show that diamond AR coatings eliminate standing-wave interference patterns of excitation laser intensity within bulk diamond, and thereby greatly reduce spatial variations in NV fluorescence, which can degrade spatially resolved magnetic field sensing using NV centers. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4730401]
C1 [Yeung, T. K.; Pham, L. M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Yeung, T. K.; Le Sage, D.; Stanwix, P. L.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Le Sage, D.; Stanwix, P. L.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Yeung, TK (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
RI Stanwix, Paul/A-5280-2009;
OI Stanwix, Paul/0000-0002-7069-8569; Le Sage, David/0000-0003-1678-9491
FU NIST; NSF; DARPA (QuEST program); DARPA (QuASAR program)
FX We gratefully acknowledge the provision of diamond samples by Apollo
Diamond and Element Six. This work was supported by NIST, NSF, and DARPA
(QuEST and QuASAR programs).
NR 21
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U1 0
U2 16
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD JUN 18
PY 2012
VL 100
IS 25
AR 251111
DI 10.1063/1.4730401
PG 4
WC Physics, Applied
SC Physics
GA 964EL
UT WOS:000305676400011
ER
PT J
AU Phillips, DF
Glenday, AG
Li, CH
Cramer, C
Furesz, G
Chang, GQ
Benedick, AJ
Chen, LJ
Kartner, FX
Korzennik, S
Sasselov, D
Szentgyorgyi, A
Walsworth, RL
AF Phillips, David F.
Glenday, Alexander G.
Li, Chih-Hao
Cramer, Claire
Furesz, Gabor
Chang, Guoqing
Benedick, Andrew J.
Chen, Li-Jin
Kaertner, Franz X.
Korzennik, Sylvain
Sasselov, Dimitar
Szentgyorgyi, Andrew
Walsworth, Ronald L.
TI Calibration of an astrophysical spectrograph below 1 m/s using a laser
frequency comb
SO OPTICS EXPRESS
LA English
DT Article
ID ASTRO-COMB; OPTICAL-FIBERS; MASS PLANETS; HARPS SEARCH; CM S(-1);
PRECISION; SPECTRA; DECELERATION; SYSTEM; PHASE
AB We deployed two wavelength calibrators based on laser frequency combs ("astro-combs") at an astronomical telescope. One astro-comb operated over a 100 nm band in the deep red (similar to 800 nm) and a second operated over a 20 nm band in the blue (similar to 400 nm). We used these red and blue astro-combs to calibrate a high-resolution astrophysical spectrograph integrated with a 1.5 m telescope, and demonstrated calibration precision and stability sufficient to enable detection of changes in stellar radial velocity <1 m/s. (C) 2012 Optical Society of America
C1 [Phillips, David F.; Glenday, Alexander G.; Li, Chih-Hao; Cramer, Claire; Furesz, Gabor; Korzennik, Sylvain; Sasselov, Dimitar; Szentgyorgyi, Andrew; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Furesz, Gabor] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary.
[Chang, Guoqing; Benedick, Andrew J.; Chen, Li-Jin; Kaertner, Franz X.] MIT, Dept Elect Engn & Comp Sci, Cambridge, MA 02139 USA.
[Chang, Guoqing; Benedick, Andrew J.; Chen, Li-Jin; Kaertner, Franz X.] MIT, Elect Res Lab, Cambridge, MA 02139 USA.
[Kaertner, Franz X.] Univ Hamburg, Dept Phys, Hamburg, Germany.
[Kaertner, Franz X.] DESY, D-2000 Hamburg, Germany.
[Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
RP Phillips, DF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dphil@cfa.harvard.edu
FU NSF [AST-0804441, ATI-0905214, ATI-1006503]; NASA [NNX09AC92G];
Hungarian OTKA-NFU Mobility grant [MB08C 81013]
FX This work was performed with support from NSF grants AST-0804441,
ATI-0905214 and ATI-1006503; NASA grant NNX09AC92G; and internal support
from the Smithsonian Astrophysical Observatory. GF acknowledges
financial support from the Hungarian OTKA-NFU Mobility grant MB08C
81013. We would like to thank Keith Lykke for the use of a wavemeter
during this project.
NR 30
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U1 2
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PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JUN 18
PY 2012
VL 20
IS 13
BP 13711
EP 13726
DI 10.1364/OE.20.013711
PG 16
WC Optics
SC Optics
GA 961NV
UT WOS:000305473000013
PM 22714437
ER
PT J
AU Opresko, DM
Wagner, D
Montgomery, AD
Brugler, MR
AF Opresko, D. M.
Wagner, D.
Montgomery, A. D.
Brugler, M. R.
TI Discovery of Aphanipathes verticillata (Cnidaria: Anthozoa:
Antipatharia) in the Hawaiian Islands
SO ZOOTAXA
LA English
DT Article
DE Aphanipathidae; Aphanipathes verticillata mauiensis; new subspecies;
black coral; range extension
ID MITOCHONDRIAL-DNA; SCLERACTINIA; POCILLOPORIDAE; EVOLUTION; SPACERS;
CORALS; GENE
AB Mesophotic coral reef surveys conducted off Maui in 2008-2009 revealed several specimens superficially resembling the commercial black coral species Antipathes griggi Opresko 2009. After subsequent microscopic examination of the skeletal features, these colonies proved to be morphologically very similar to Aphanipathes verticillata Brook 1889, a species never before reported from the Hawaiian Islands. A comparison with samples of the type material of A. verticillata indicated that the specimens collected in Hawaiian waters differed from the type in having simplier and less dense tubercles on the skeletal spines, a character which merits the recognition of the Hawaiian population as a new subspecies, A. verticillata mauiensis. Colonies of the new subspecies exhibit considerable morphological variation; DNA analysis of fifteen specimens ruled out the possibility of the presence of a cryptic species. Further DNA investigations on specimens from various localities in the western Pacific and Indian Ocean are needed to better understand the genetic relationship between the two forms. The morphological similarity of A. verticillata mauiensis with Antipathes griggi raises questions concerning the validity of past field surveys evaluating the population size and structure of A. griggi since it is possible that the two species could easily be misidentified based on gross morphology alone. Additional studies are also needed to document the geographic and bathymetric distribution of the subspecies along the Hawaiian Island chain.
C1 [Opresko, D. M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Wagner, D.] Papahanaumokuakea Marine Natl Monument, Honolulu, HI 96825 USA.
[Montgomery, A. D.] US Fish & Wildlife Serv, Pacific Isl Fish & Wildlife Off, Honolulu, HI 96850 USA.
[Brugler, M. R.] Amer Museum Nat Hist, Div Invertebrate Zool, Sackler Inst Comparat Genom, New York, NY 10024 USA.
RP Opresko, DM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM dmopresko@hotmail.com; Daniel.Wagner@noaa.gov; Tony_Montgomery@fws.gov;
mbrugler@amnh.org
FU Smithsonian Institution, Washington, DC; Oak Ridge National Laboratory,
Oak Ridge, TN; National Oceanic and Atmospheric Administration (NOAA)
Coastal Ocean Program [NA07NOS4780189]; NOAA Coral Reef Conservation
Program [NA05OAR4301108]; NOAA Fisheries Disaster Relief Program
[NA03NMF4520452]; Western Pacific Fisheries Management Council
[NA07NMF4410114]; National Science Foundation [OCE-0623678]; National
Marine Sanctuary Program [NWHICRER MOA 2005-008/6882]; National Science
Foundation grant, Assembling the Cnidarian Tree of Life [EF-0531570]
FX This work was supported in part by the Smithsonian Institution,
Washington, DC, Oak Ridge National Laboratory, Oak Ridge, TN, the
National Oceanic and Atmospheric Administration (NOAA) Coastal Ocean
Program (NA07NOS4780189 to the State of Hawai'i Department of Land and
Natural Resources [DLNR]), the NOAA Coral Reef Conservation Program
(NA05OAR4301108 to the Hawai'i Undersea Research Laboratory [HURL]), the
NOAA Fisheries Disaster Relief Program (NA03NMF4520452 to the State of
Hawai'i/DLNR), the Western Pacific Fisheries Management Council
(NA07NMF4410114 to the University of Hawai'i through NOAA's Coral Reef
Conservation Grant Program), the National Science Foundation
(OCE-0623678), and the National Marine Sanctuary Program (NWHICRER MOA
2005-008/6882). Partial support for the molecular analysis was provided
by a subcontract to Scott C. France from a National Science Foundation
grant, Assembling the Cnidarian Tree of Life (#EF-0531570). M. R.
Brugler thanks Dr. France for his guidance and support while performing
the molecular analysis at the University of Louisiana at Lafayette. D.
M. Opresko is a Research Associate at the NMNH, Smithsonian Institution,
and gratefully acknowledges that affiliation. The findings and
conclusions in this article are those of the authors and do not
necessarily represent the views of the U.S. Fish and Wildlife Service.
NR 28
TC 3
Z9 4
U1 1
U2 4
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JUN 15
PY 2012
IS 3348
BP 24
EP 39
PG 16
WC Zoology
SC Zoology
GA 958VI
UT WOS:000305268400002
ER
PT J
AU Hong, T
AF Hong, Terry
TI The Red Chamber
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Hong, Terry] Smithsonian Book Dragon, Washington, DC 20013 USA.
RP Hong, T (reprint author), Smithsonian Book Dragon, Washington, DC 20013 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUN 15
PY 2012
VL 137
IS 11
BP 68
EP 68
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 961WZ
UT WOS:000305501500090
ER
PT J
AU Hong, T
AF Hong, Terry
TI Atlas: The Archaeology of an Imaginary City
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA.
RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUN 15
PY 2012
VL 137
IS 11
BP 69
EP 69
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 961WZ
UT WOS:000305501500092
ER
PT J
AU Riley, SM
AF Riley, Sheila M.
TI House Blood: A Joe DeMarco Thriller
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Riley, Sheila M.] Smithsonian Inst Libs, Washington, DC 20560 USA.
RP Riley, SM (reprint author), Smithsonian Inst Libs, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUN 15
PY 2012
VL 137
IS 11
BP 72
EP 72
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 961WZ
UT WOS:000305501500102
ER
PT J
AU Durant, SM
Pettorelli, N
Bashir, S
Woodroffe, R
Wacher, T
De Ornellas, P
Ransom, C
Abaigar, T
Abdelgadir, M
El Alqamy, H
Beddiaf, M
Belbachir, F
Belbachir-Bazi, A
Berbash, AA
Beudels-Jamar, R
Boitani, L
Breitenmoser, C
Cano, M
Chardonnet, P
Collen, B
Cornforth, WA
Cuzin, F
Gerngross, P
Haddane, B
Hadjeloum, M
Jacobson, A
Jebali, A
Lamarque, F
Mallon, D
Minkowski, K
Monfort, S
Ndoassal, B
Newby, J
Ngakoutou, BE
Niagate, B
Purchase, G
Samaila, S
Samna, AK
Sillero-Zubiri, C
Soultan, AE
Price, MRS
Baillie, JEM
AF Durant, S. M.
Pettorelli, N.
Bashir, S.
Woodroffe, R.
Wacher, T.
De Ornellas, P.
Ransom, C.
Abaigar, T.
Abdelgadir, M.
El Alqamy, H.
Beddiaf, M.
Belbachir, F.
Belbachir-Bazi, A.
Berbash, A. A.
Beudels-Jamar, R.
Boitani, L.
Breitenmoser, C.
Cano, M.
Chardonnet, P.
Collen, B.
Cornforth, W. A.
Cuzin, F.
Gerngross, P.
Haddane, B.
Hadjeloum, M.
Jacobson, A.
Jebali, A.
Lamarque, F.
Mallon, D.
Minkowski, K.
Monfort, S.
Ndoassal, B.
Newby, J.
Ngakoutou, B. E.
Niagate, B.
Purchase, G.
Samaila, S.
Samna, A. K.
Sillero-Zubiri, C.
Soultan, A. E.
Price, M. R. Stanley
Baillie, J. E. M.
TI Forgotten Biodiversity in Desert Ecosystems
SO SCIENCE
LA English
DT Letter
C1 [Durant, S. M.; Pettorelli, N.; Woodroffe, R.; Belbachir, F.; Collen, B.; Cornforth, W. A.] Zool Soc London, Inst Zool, London NW1 4RY, England.
[Durant, S. M.; Purchase, G.] Wildlife Conservat Soc, Bronx, NY 10460 USA.
[Wacher, T.; De Ornellas, P.; Ransom, C.; Purchase, G.; Baillie, J. E. M.] Zool Soc London, Conservat Programmes, London NW1 4RY, England.
[Abaigar, T.; Cano, M.] CSIC, EEZA, La Canada De San Urbano 04120, Almeria, Spain.
[Abdelgadir, M.] Univ Hail, Dept Biol, Hail, Saudi Arabia.
[El Alqamy, H.; Soultan, A. E.] EEAA, Nat Conservat Sect, Cairo, Egypt.
[Beddiaf, M.] Off Natl Parc Culturel Tassili Ajjer, Djanet 33100, Algeria.
[Belbachir-Bazi, A.] Univ Bejaia, Fac Sci Nat & Vie, Lab Ecol & Environm, Bejaia 06000, Algeria.
[Berbash, A. A.] EGA, Nat Conservat Dept, Tripoli, Libya.
[Beudels-Jamar, R.] Royal Belgian Inst Nat Sci, B-1000 Brussels, Belgium.
[Boitani, L.] Univ Roma La Sapienza, Dept Biol & Biotechnol, I-00185 Rome, Italy.
[Breitenmoser, C.] KORA, IUCN SSC Cat Specialist Grp, CH-3074 Muri, Switzerland.
[Chardonnet, P.] IGF Fdn, F-75003 Paris, France.
[Gerngross, P.] BIOGEOMAPS, Umwelt PR Gerngross e U, A-1070 Vienna, Austria.
[Haddane, B.] Fdn Mohamed VI Protect Environm, Temara 12000, Morocco.
[Hadjeloum, M.] Chef Bur Gest & Prservat Faune, Direct Protect Faune & Flore, Ben Aknoun Alger, Algeria.
[Jacobson, A.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Jacobson, A.] Natl Geog Soc, Big Cats Initiat, Washington, DC 20036 USA.
[Jebali, A.] TWCS, Dept Biol, Fac Sci Tunis, Tunis 2092, Tunisia.
[Lamarque, F.] Minist Ecol Dev Durable & Energ, F-92055 La Defense Cedex, France.
[Mallon, D.] Manchester Metropolitan Univ, Div Biol & Conservat Ecol, Manchester M1 5GD, Lancs, England.
[Monfort, S.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
[Ndoassal, B.; Ngakoutou, B. E.] Direct Parcs Natl Reserv Faune & Chasse, Ndjamena, Tchad, Chad.
[Newby, J.] Sahara Conservat Fund, CH-1148 Lisle, Switzerland.
[Samaila, S.; Samna, A. K.] Direct Faune Chasse & Aires Protegee, Niamey, Niger.
[Sillero-Zubiri, C.; Price, M. R. Stanley] Univ Oxford, Recanati Kaplan Ctr, Dept Zool, Wildlife Conservat Res Unit, Tubney OX13 5QL, Oxon, England.
RP Durant, SM (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England.
EM sdurant@wcs.org
RI Collen, Ben/D-5055-2011; Collen, Ben/F-2543-2016
OI Collen, Ben/0000-0003-2564-4243
NR 10
TC 15
Z9 15
U1 2
U2 41
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JUN 15
PY 2012
VL 336
IS 6087
BP 1379
EP 1380
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 958BT
UT WOS:000305211700016
PM 22700901
ER
PT J
AU Jansen, PA
Forget, PM
AF Jansen, Patrick A.
Forget, Pierre-Michel
TI Predatory Publishers and Plagiarism Prevention
SO SCIENCE
LA English
DT Letter
C1 [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, Wageningen, Netherlands.
[Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Forget, Pierre-Michel] Museum Natl Hist Nat, Brunoy, France.
RP Jansen, PA (reprint author), Wageningen Univ, Dept Environm Sci, Wageningen, Netherlands.
EM patrick.jansen@wur.nl
RI Forget, Pierre-Michel/B-4355-2009; Jansen, Patrick/G-2545-2015
OI Forget, Pierre-Michel/0000-0002-9252-974X; Jansen,
Patrick/0000-0002-4660-0314
NR 5
TC 3
Z9 3
U1 5
U2 21
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JUN 15
PY 2012
VL 336
IS 6087
BP 1380
EP 1380
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 958BT
UT WOS:000305211700018
PM 22700902
ER
PT J
AU McMichael, CH
Piperno, DR
Bush, MB
Silman, MR
Zimmerman, AR
Raczka, MF
Lobato, LC
AF McMichael, C. H.
Piperno, D. R.
Bush, M. B.
Silman, M. R.
Zimmerman, A. R.
Raczka, M. F.
Lobato, L. C.
TI Sparse Pre-Columbian Human Habitation in Western Amazonia
SO SCIENCE
LA English
DT Article
ID BRAZILIAN AMAZON; FOREST; TREES
AB Locally extensive pre-Columbian human occupation and modification occurred in the forests of the central and eastern Amazon Basin, but whether comparable impacts extend westward and into the vast terra firme (interfluvial) zones, remains unclear. We analyzed soils from 55 sites across central and western Amazonia to assess the history of human occupation. Sparse occurrences of charcoal and the lack of phytoliths from agricultural and disturbance species in the soils during pre-Columbian times indicated that human impacts on interfluvial forests were small, infrequent, and highly localized. No human artifacts or modified soils were found at any site surveyed. Riverine bluff areas also appeared less heavily occupied and disturbed than similar settings elsewhere. Our data indicate that human impacts on Amazonian forests were heterogeneous across this vast landscape.
C1 [McMichael, C. H.; Bush, M. B.; Raczka, M. F.] Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA.
[Piperno, D. R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA.
[Piperno, D. R.] Smithsonian Trop Res Inst, Balboa, Panama.
[Silman, M. R.] Wake Forest Univ, Dept Biol, Winston Salem, NC 27106 USA.
[Silman, M. R.] Ctr Energy Environm & Sustainabil, Winston Salem, NC 27106 USA.
[Zimmerman, A. R.] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA.
[Lobato, L. C.] Univ Fed Rondonia, Lab Geog Humana & Planejamento Ambiental, Porto Velho, Rondonia, Brazil.
RP McMichael, CH (reprint author), Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA.
EM cmcmicha@my.fit.edu
OI Bush, Mark/0000-0001-6894-8613; Zimmerman, Andrew/0000-0001-5137-4916
FU NSF [DEB 0742301, DEB 0743666]; Florida Institute of Technology;
Smithsonian National Museum of Natural History; Smithsonian Tropical
Research Institute
FX Field work and 14C dating of charcoal fragments were funded
by the NSF Ecology Program (awards DEB 0742301 and DEB 0743666). Other
funding was provided by the Florida Institute of Technology; the
Smithsonian National Museum of Natural History, including a Restricted
Endowment and Small Grant Award; and the Smithsonian Tropical Research
Institute. All data will be deposited in the Neotoma Database
(www.neotomadb.org/). We thank B. McMichael, A. Correa-Metrio, J.
Hernandez, T. Harrison, and B. Rado for field assistance.
NR 31
TC 51
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U1 8
U2 50
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JUN 15
PY 2012
VL 336
IS 6087
BP 1429
EP 1431
DI 10.1126/science.1219982
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 958BT
UT WOS:000305211700042
PM 22700926
ER
PT J
AU Low, R
Weimer, H
Nipper, J
Balewski, JB
Butscher, B
Buchler, HP
Pfau, T
AF Loew, Robert
Weimer, Hendrik
Nipper, Johannes
Balewski, Jonathan B.
Butscher, Bjoern
Buechler, Hans Peter
Pfau, Tilman
TI An experimental and theoretical guide to strongly interacting Rydberg
gases
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
ID BOSE-EINSTEIN CONDENSATION; DIGITAL QUANTUM SIMULATION;
PHASE-TRANSITION; ENERGY-TRANSFER; MOTT INSULATOR; NOBEL LECTURE;
NEUTRAL ATOMS; SINGLE ATOMS; LASER; BLOCKADE
AB We review experimental and theoretical tools to excite, study and understand strongly interacting Rydberg gases. The focus lies on the excitation of dense ultracold atomic samples close to, or within quantum degeneracy, high-lying Rydberg states. The major part is dedicated to highly excited S-states of rubidium, which feature an isotropic van der Waals potential. Nevertheless, the setup and the methods presented are also applicable to other atomic species used in the field of laser cooling and atom trapping.
C1 [Loew, Robert; Nipper, Johannes; Balewski, Jonathan B.; Butscher, Bjoern; Pfau, Tilman] Univ Stuttgart, Inst Phys, D-70569 Stuttgart, Germany.
[Weimer, Hendrik] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Weimer, Hendrik] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Buechler, Hans Peter] Univ ,Stuttgart, Inst Theoret Phys 3, D-70569 Stuttgart, Germany.
RP Low, R (reprint author), Univ Stuttgart, Inst Phys, D-70569 Stuttgart, Germany.
EM r.loew@physik.uni-stuttgart.de
RI Pfau, Tilman/G-1774-2011; Loew, Robert/I-8206-2014
FU Deutsche Forschungsgemeinschaft (DFG); European Commission; National
Science Foundation; Postdoctoral Program of the German Academic Exchange
Service (DAAD)
FX The authors thank Helmar Bender, Vera Bendkowsky, Axel Grabowski, Rolf
Heidemann, Peter Kollmann, Eva Kuhnle, Ludmila Kukota, Ulrich Krohn,
Johannes Nold and Alban Urvoy for their experimental and theoretical
contributions. Funding for the ultracold rubidium Rydberg setup has been
provided by the Deutsche Forschungsgemeinschaft (DFG) and the European
Commission. HW acknowledges support by the National Science Foundation
through a grant for the Institute for Theoretical Atomic, Molecular and
Optical Physics at Harvard University and Smithsonian Astrophysical
Observatory and by a fellowship within the Postdoctoral Program of the
German Academic Exchange Service (DAAD).
NR 126
TC 110
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U1 4
U2 43
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD JUN 14
PY 2012
VL 45
IS 11
AR 113001
DI 10.1088/0953-4075/45/11/113001
PG 21
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 958ZZ
UT WOS:000305280800001
ER
PT J
AU Kocsis, B
Levin, J
AF Kocsis, Bence
Levin, Janna
TI Repeated bursts from relativistic scattering of compact objects in
galactic nuclei
SO PHYSICAL REVIEW D
LA English
DT Article
ID NEUTRON-STAR MERGERS; GAMMA-RAY BURSTS; MASS BLACK-HOLES;
GRAVITATIONAL-RADIATION; GLOBULAR-CLUSTERS; STANDARD SIRENS;
BINARY-SYSTEMS; POINT-MASSES; 3C 66B; WAVES
AB Galactic nuclei are densely populated by stellar mass compact objects such as black holes and neutron stars. Bound, highly eccentric binaries form as a result of gravitational wave (GW) losses during close flybys between these objects. We study the evolution of these systems using 2.5 and 3.5 order post-Newtonian (PN) equations of motion. The GW signal consists of many thousand repeated bursts (RB) for minutes to days (depending on the impact parameter and masses), followed by a powerful GW chirp and an eccentric merger. We show that a significant signal-to-noise ratio accumulates already in the RB phase, corresponding to a detection limit around 200-300 Mpc and 300-600 Mpc for advanced LIGO for an average orientation black hole/neutron star or black hole/black hole binary, respectively. The theoretical errors introduced by the inaccuracy of the PN templates are typically much less severe for the RB phase than in the following eccentric merger. The GW signal in the RB phase is broadband; we show that encounters involving intermediate mass black holes are detectable in multiple frequency bands coincidentally using LIGO and LISA.
C1 [Kocsis, Bence] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Levin, Janna] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Levin, Janna] Columbia Univ, Inst Strings Cosmol & Astroparticle Phys, New York, NY 10027 USA.
RP Kocsis, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Kocsis, Bence/C-3061-2013
OI Kocsis, Bence/0000-0002-4865-7517
FU NSF [AST-0908365]; KITP [NSF PHY05- 51164]; NASA through Einstein
Postdoctoral Fellowship by Chandra X-ray Observatory Center [PF9-00063];
National Aeronautics Space Administration [NAS8-03060]; Hungarian
Research Fund OTKA [68228]
FX We gratefully acknowledge valuable discussions with Szabolcs Marka who
suggested this collaboration, Sean McWilliams, Scott Hughes, Alessandra
Buonanno, and Ryan O'Leary. This work was supported by NSF Grant No.
AST-0908365. J. L. gratefully acknowledges support of KITP under Grant
No. NSF PHY05- 51164. B. K. acknowledges support from NASA through
Einstein Postdoctoral Fellowship No. PF9-00063) by the Chandra X-ray
Observatory Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of the National Aeronautics Space
Administration under Contract No. NAS8-03060, and the Hungarian Research
Fund OTKA (Grant No. 68228).
NR 61
TC 36
Z9 36
U1 0
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD JUN 14
PY 2012
VL 85
IS 12
AR 123005
DI 10.1103/PhysRevD.85.123005
PG 16
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 958QS
UT WOS:000305256100004
ER
PT J
AU Elvis, M
AF Elvis, Martin
TI A midlife crisis for X-ray astronomy
SO NATURE
LA English
DT Editorial Material
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM elvis@cfa.harvard.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUN 14
PY 2012
VL 486
IS 7402
BP 181
EP 182
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 957UH
UT WOS:000305189000011
PM 22699593
ER
PT J
AU Medeiros, MJ
Adamski, D
AF Medeiros, Matthew J.
Adamski, David
TI Three new species of Hawaiian moths from Kahoolawe island (Lepidoptera:
Crambidae & Coleophoridae)
SO ZOOTAXA
LA English
DT Article
DE Blastobasini; endemic species; Hawai'i; Kaho'olawe; morphology; taxonomy
AB Three new species of Hawaiian Lepidoptera are described herein: Pigritia uuku sp. nov. (Coleophoridae: Blastobasinae), Orthomecyna keoniae sp. nov. (Crambidae), and Tamsica kawikae sp. nov. (Crambidae) from Kahoolawe Island.
C1 [Medeiros, Matthew J.] Urban Sch San Francisco, San Francisco, CA 94117 USA.
[Medeiros, Matthew J.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Adamski, David] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
RP Medeiros, MJ (reprint author), Urban Sch San Francisco, 1563 Page St, San Francisco, CA 94117 USA.
EM matt.j.medeiros@gmail.com; adamskid@si.edu
NR 10
TC 1
Z9 1
U1 0
U2 0
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD JUN 11
PY 2012
IS 3341
BP 59
EP 63
PG 5
WC Zoology
SC Zoology
GA 957VK
UT WOS:000305193700005
ER
PT J
AU Chitta, LP
van Ballegooijen, AA
van der Voort, LR
DeLuca, EE
Kariyappa, R
AF Chitta, L. P.
van Ballegooijen, A. A.
van der Voort, L. Rouppe
DeLuca, E. E.
Kariyappa, R.
TI DYNAMICS OF THE SOLAR MAGNETIC BRIGHT POINTS DERIVED FROM THEIR
HORIZONTAL MOTIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: photosphere; Sun: surface magnetism
ID ALFVENIC WAVES; QUIET SUN; PHOTOSPHERE; ELEMENTS; TELESCOPE; CORONA;
FLUX; CHROMOSPHERE; DIFFUSION; MISSION
AB The subarcsecond bright points (BPs) associated with the small-scale magnetic fields in the lower solar atmosphere are advected by the evolution of the photospheric granules. We measure various quantities related to the horizontal motions of the BPs observed in two wavelengths, including the velocity autocorrelation function. A 1 hr time sequence of wideband Ha observations conducted at the Swedish 1 m Solar Telescope (SST) and a 4 hr Hinode G-band time sequence observed with the Solar Optical Telescope are used in this work. We follow 97 SST and 212 Hinode BPs with 3800 and 1950 individual velocity measurements, respectively. For its high cadence of 5 s as compared to 30 s for Hinode data, we emphasize more the results from SST data. The BP positional uncertainty achieved by SST is as low as 3 km. The position errors contribute 0.75 km(2) s(-2) to the variance of the observed velocities. The raw and corrected velocity measurements in both directions, i.e., (v(x), v(y)), have Gaussian distributions with standard deviations of (1.32, 1.22) and (1.00, 0.86) km s(-1), respectively. The BP motions have correlation times of about 22-30 s. We construct the power spectrum of the horizontal motions as a function of frequency, a quantity that is useful and relevant to the studies of generation of Alfven waves. Photospheric turbulent diffusion at timescales less than 200 s is found to satisfy a power law with an index of 1.59.
C1 [Chitta, L. P.; van Ballegooijen, A. A.; DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chitta, L. P.; Kariyappa, R.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[van der Voort, L. Rouppe] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway.
RP Chitta, LP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-15, Cambridge, MA 02138 USA.
RI DeLuca, Edward/L-7534-2013;
OI DeLuca, Edward/0000-0001-7416-2895; Chitta, Lakshmi
Pradeep/0000-0002-9270-6785
FU NASA [NNM07AB07C]
FX The authors thank the referee for many comments and suggestions that
helped improve the presentation of the manuscript. L.P.C. is a 2011-2012
SAO Pre-Doctoral Fellow at the Harvard-Smithsonian Center for
Astrophysics. The Swedish 1 m Solar Telescope is operated on the island
of La Palma 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. Funding for L. P.
C. and E. E. D. is provided by NASA contract NNM07AB07C. Hinode is a
Japanese mission developed and launched by ISAS/JAXA, collaborating with
NAOJ as a domestic partner, NASA and STFC (UK) as international
partners. Scientific operation of the Hinode mission is conducted by the
Hinode science team organized at ISAS/JAXA. This team mainly consists of
scientists from institutes in the partner countries. Support for the
post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK),
NASA (USA), ESA, and NSC (Norway). This research has made use of NASA's
Astrophysics Data System.
NR 30
TC 26
Z9 26
U1 2
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 48
DI 10.1088/0004-637X/752/1/48
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400048
ER
PT J
AU Civano, F
Elvis, M
Lanzuisi, G
Aldcroft, T
Trichas, M
Bongiorno, A
Brusa, M
Blecha, L
Comastri, A
Loeb, A
Salvato, M
Fruscione, A
Koekemoer, A
Komossa, S
Gilli, R
Mainieri, V
Piconcelli, E
Vignali, C
AF Civano, F.
Elvis, M.
Lanzuisi, G.
Aldcroft, T.
Trichas, M.
Bongiorno, A.
Brusa, M.
Blecha, L.
Comastri, A.
Loeb, A.
Salvato, M.
Fruscione, A.
Koekemoer, A.
Komossa, S.
Gilli, R.
Mainieri, V.
Piconcelli, E.
Vignali, C.
TI CHANDRA HIGH-RESOLUTION OBSERVATIONS OF CID-42, A CANDIDATE RECOILING
SUPERMASSIVE BLACK HOLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: interactions; galaxies: nuclei
ID ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION; QUASAR SDSS J092712.65+294344.0;
GRAVITATIONAL-WAVE RECOIL; RADIATION RECOIL; GALAXIES; CATALOG;
SLINGSHOT; ACCRETION; BINARIES
AB We present Chandra High Resolution Camera observations of CID-42, a candidate recoiling supermassive black hole (SMBH) at z = 0.359 in the COSMOS survey. CID-42 shows two optical compact sources resolved in the HST/ACS image embedded in the same galaxy structure and a velocity offset of similar to 1300 km s(-1) between the H beta broad and narrow emission line, as presented by Civano et al. Two scenarios have been proposed to explain the properties of CID-42: a gravitational wave (GW) recoiling SMBH and a double Type 1/Type 2 active galactic nucleus (AGN) system, where one of the two is recoiling because of slingshot effect. In both scenarios, one of the optical nuclei hosts an unobscured AGN, while the other one, either an obscured AGN or a star-forming compact region. The X-ray Chandra data allow us to unambiguously resolve the X-ray emission and unveil the nature of the two optical sources in CID-42. We find that only one of the optical nuclei is responsible for the whole X-ray unobscured emission observed and a 3 sigma upper limit on the flux of the second optical nucleus is measured. The upper limit on the X-ray luminosity plus the analysis of the multiwavelength spectral energy distribution indicate the presence of a star-forming region in the second source rather than an obscured SMBH, thus favoring the GW recoil scenario. However, the presence of a very obscured SMBH cannot be fully ruled out. A new X-ray feature, in a SW direction with respect to the main source, is discovered and discussed.
C1 [Civano, F.; Elvis, M.; Lanzuisi, G.; Aldcroft, T.; Trichas, M.; Fruscione, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Lanzuisi, G.; Piconcelli, E.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Lanzuisi, G.; Bongiorno, A.; Brusa, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Blecha, L.; Loeb, A.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Comastri, A.; Gilli, R.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Salvato, M.; Komossa, S.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Komossa, S.] Tech Univ Munich, Fak Fuer Phys, D-85748 Garching, Germany.
[Komossa, S.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mainieri, V.] ESO, D-85748 Garching, Germany.
[Piconcelli, E.] ESA, XMM Newton Sci Operat Ctr, Villanueva De La Canada 28691, Spain.
[Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Komossa, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
RP Civano, F (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
RI Vignali, Cristian/J-4974-2012; Lanzuisi, Giorgio/K-4378-2013; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015;
OI Brusa, Marcella/0000-0002-5059-6848; Vignali,
Cristian/0000-0002-8853-9611; Koekemoer, Anton/0000-0002-6610-2048;
Lanzuisi, Giorgio/0000-0001-9094-0984; Comastri,
Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177;
Bongiorno, Angela/0000-0002-0101-6624; piconcelli,
enrico/0000-0001-9095-2782
FU NASA [GO7-8136A]; Blancheflor Boncompagni Ludovisi foundation;
Smithsonian Scholarly Studies
FX F.C. thanks A. Marinucci, A. Goulding, V. Kashyap, and E. Schinnerer for
useful discussions on the X-ray data. The authors thank the referee for
the useful suggestions which improved the quality of the manuscript.
This work was supported by the NASA Chandra grant GO7-8136A, the
Blancheflor Boncompagni Ludovisi foundation, and the Smithsonian
Scholarly Studies.
NR 53
TC 28
Z9 28
U1 2
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 49
DI 10.1088/0004-637X/752/1/49
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400049
ER
PT J
AU Godet, O
Plazolles, B
Kawaguchi, T
Lasota, JP
Barret, D
Farrell, SA
Braito, V
Servillat, M
Webb, N
Gehrels, N
AF Godet, O.
Plazolles, B.
Kawaguchi, T.
Lasota, J. -P.
Barret, D.
Farrell, S. A.
Braito, V.
Servillat, M.
Webb, N.
Gehrels, N.
TI INVESTIGATING SLIM DISK SOLUTIONS FOR HLX-1 IN ESO 243-49
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: individual
(ESO 243-49); methods: data analysis; X-rays: individuals (HLX-1)
ID X-RAY SOURCES; MASS BLACK-HOLE; SPECTRAL STATE TRANSITIONS; NOVA MUSCAE
1991; ACCRETION DISKS; VARIABILITY; BINARIES; MODEL; IRRADIATION;
EVOLUTION
AB The hyperluminous X-ray source HLX-1 in the galaxy ESO 243-49, currently the best intermediate-mass black hole (BH) candidate, displays spectral transitions similar to those observed in Galactic BH binaries, but with a luminosity 100-1000 times higher. We investigated the X-ray properties of this unique source by fitting multiepoch data collected by Swift, XMM-Newton, and Chandra with a disk model computing spectra for a wide range of sub- and super-Eddington accretion rates assuming a non-spinning BH and a face-on disk (i = 0 degrees). Under these assumptions we find that the BH in HLX-1 is in the intermediate-mass range (similar to 2 x 10(4) M-circle dot) and the accretion flow is in the sub-Eddington regime. The disk radiation efficiency is eta = 0.11 +/- 0.03. We also show that the source does follow the L-X alpha T-4 relation for our mass estimate. At the outburst peaks, the source radiates near the Eddington limit. The accretion rate then stays constant around 4 x 10(-4) M-circle dot yr(-1) for several days and then decreases exponentially. Such "plateaus" in the accretion rate could be evidence that enhanced mass-transfer rate is the driving outburst mechanism in HLX-1. We also report on the new outburst observed in 2011 August by the Swift X-Ray Telescope. The time of this new outburst further strengthens the similar to 1 year recurrence timescale.
C1 [Godet, O.; Plazolles, B.; Barret, D.; Webb, N.] Univ Toulouse, UPS, IRAP, F-31028 Toulouse 4, France.
[Godet, O.; Plazolles, B.; Barret, D.; Webb, N.] CNRS, UMR5277, F-31028 Toulouse, France.
[Kawaguchi, T.] Univ Tsukuba, Ctr Computat Sci, Tsukuba, Ibaraki 3058577, Japan.
[Lasota, J. -P.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France.
[Lasota, J. -P.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Farrell, S. A.; Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Farrell, S. A.] Univ Sydney, Sch Phys A29, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Godet, O (reprint author), Univ Toulouse, UPS, IRAP, 9 Ave Colonel Roche, F-31028 Toulouse 4, France.
OI Braito, Valentina/0000-0002-2629-4989
FU NASA [GO0-11063X, DD0-11050X]; NSF [AST-0909073]; UK Science and
Technology Funding Council; Australian Research Council [DP110102889];
UK STFC research council; French Space Agency CNES
FX We thank the anonymous referee for his useful comments that helped to
improve the paper. We are grateful to Ken Ebisawa and Takashi Okajima
for creating a new fits model for XSPEC incorporating the extended black
hole mass ranges. We thank Shane Davis for his useful suggestions during
the writing of this paper. M.S. acknowledges supports from NASA/Chandra
Grants GO0-11063X, DD0-11050X and NSF Grant AST-0909073. S.A.F.
acknowledges funding from the UK Science and Technology Funding Council.
S.A.F. is the recipient of an Australian Research Council Postdoctoral
Fellowship, funded by grant DP110102889. V.B. acknowledge support from
the UK STFC research council. J.P.L. acknowledges support from the
French Space Agency CNES.
NR 60
TC 28
Z9 28
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 34
DI 10.1088/0004-637X/752/1/34
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400034
ER
PT J
AU Hsu, WH
Hartmann, L
Allen, L
Hernandez, J
Megeath, ST
Mosby, G
Tobin, JJ
Espaillat, C
AF Hsu, Wen-Hsin
Hartmann, Lee
Allen, Lori
Hernandez, Jesus
Megeath, S. T.
Mosby, Gregory
Tobin, John J.
Espaillat, Catherine
TI THE LOW-MASS STELLAR POPULATION IN L1641: EVIDENCE FOR ENVIRONMENTAL
DEPENDENCE OF THE STELLAR INITIAL MASS FUNCTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: formation; stars: low-mass; stars: luminosity function, mass
function; stars: pre-main sequence; surveys
ID ORION NEBULA CLUSTER; MULTICOLOR OPTICAL SURVEY; TAURUS-AURIGA;
MULTIOBJECT SPECTROGRAPH; MOLECULAR CLOUD; STARS; REGION;
CLASSIFICATION; HECTOSPEC; COLORS
AB We present results from an optical photometric and spectroscopic survey of the young stellar population in L1641, the low-density star-forming region of the Orion A cloud south of the Orion Nebula Cluster (ONC). Our goal is to determine whether L1641 has a large enough low-mass population to make the known lack of high-mass stars a statistically significant demonstration of environmental dependence of the upper mass stellar initial mass function (IMF). Our spectroscopic sample consists of IR-excess objects selected from the Spitzer/IRAC survey and non-excess objects selected from optical photometry. We have spectral confirmation of 864 members, with another 98 probable members; of the confirmed members, 406 have infrared excesses and 458 do not. Assuming the same ratio of stars with and without IR excesses in the highly extincted regions, L1641 may contain as many as similar to 1600 stars down to similar to 0.1 M-circle dot, comparable within a factor of two to the ONC. Compared to the standard models of the IMF, L1641 is deficient in O and early B stars to a 3 sigma-4 sigma significance level, assuming that we know of all the massive stars in L1641. With a forthcoming survey of the intermediate-mass stars, we will be in a better position to make a direct comparison with the neighboring, dense ONC, which should yield a stronger test of the dependence of the high-mass end of the stellar IMF on environment.
C1 [Hsu, Wen-Hsin; Hartmann, Lee] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Allen, Lori] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Hernandez, Jesus] Ctr Invest Astron, Merida 5101 A, Venezuela.
[Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Mosby, Gregory] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Tobin, John J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Espaillat, Catherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hsu, WH (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
FU NSF [AST-0807305]; Origins [NNX08AI39G]; Smithsonian Astrophysical
Observatory
FX We thank the referee for helpful suggestions to improve the manuscript.
W. H. and L. H. acknowledge the support of NSF Grant AST-0807305 and the
Origins Grant NNX08AI39G. This paper uses data obtained at the MMT
Observatory, a joint facility of the Smithsonian Institution and the
University of Arizona, and the 6.5 m Magellan Telescopes located at Las
Campanas Observatory, Chile. This paper uses data products produced by
the OIR Telescope Data Center, supported by the Smithsonian
Astrophysical Observatory.
NR 51
TC 26
Z9 26
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 59
DI 10.1088/0004-637X/752/1/59
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400059
ER
PT J
AU Hwang, HS
Geller, MJ
Diaferio, A
Rines, KJ
AF Hwang, Ho Seong
Geller, Margaret J.
Diaferio, Antonaldo
Rines, Kenneth J.
TI A WISE VIEW OF A NEARBY SUPERCLUSTER A2199
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (Abell 2199); galaxies: evolution;
galaxies: formation; galaxies: luminosity function, mass function;
infrared: galaxies
ID DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; INFRARED LUMINOSITY FUNCTION;
ACTIVE GALACTIC NUCLEI; COLOR-MAGNITUDE RELATION; H-ALPHA; COMA CLUSTER;
MU-M; ENVIRONMENTAL DEPENDENCE; STELLAR POPULATIONS
AB We use Wide-field Infrared Survey Explorer (WISE) data covering the entire region (similar to 130 deg(2)) of the A2199 supercluster at z = 0.03 to study the mid-infrared (MIR) properties of supercluster galaxies. We identify an "MIR star-forming sequence" in the WISE [3.4]-[12] color-12 mu m luminosity diagram, consisting of late-type, star-forming galaxies. At a fixed star formation rate, the MIR-detected galaxies at 22 mu m or 12 mu m tend to be more metal-rich and to have higher surface brightness than those without MIR detection. Using these MIR-detected galaxies, we construct the IR luminosity function (LF) and investigate its environmental dependence. Both total IR (TIR) and 12 mu m LFs are dominated by late-type, star-forming galaxies. The contribution of active galactic nucleus host galaxies increases with both TIR and 12 mu m luminosities. The contribution of early-type galaxies to the 12 mu m LFs increases with decreasing luminosity. The faint-end slope of the TIR LFs does not change with environment, but the change of faint-end slope in the 12 mu m LFs with the environment is significant: there is a steeper faint-end slope in the cluster core than in the cluster outskirts. This steepening results primarily from the increasing contribution of early-type galaxies toward the cluster. These galaxies are passively evolving, and contain old stellar populations with weak MIR emission from the circumstellar dust around asymptotic giant branch stars.
C1 [Hwang, Ho Seong; Geller, Margaret J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Diaferio, Antonaldo] Univ Torino, Dipartimento Fis, I-10125 Turin, Italy.
[Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Rines, Kenneth J.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA.
RP Hwang, HS (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM hhwang@cfa.harvard.edu; mgeller@cfa.harvard.edu; diaferio@ph.unito.it;
kenneth.rines@wwu.edu
FU Smithsonian Institution; INFN [PD51]; MIUR [2008NR3EBK_003]; Cottrell
College Science Award from the Research Corporation; National
Aeronautics and Space Administration
FX We thank the anonymous referee for constructive comments that helped us
to improve the manuscript. We thank Scott Kenyon for carefully reading
the manuscript. We also thank Gwang-Ho Lee, David Elbaz, Jongwan Ko,
Minjin Kim, Jong Chul Lee, Jubee Sohn, and Hyunjin Shim for useful
discussion. H. S. H. acknowledges the Smithsonian Institution for the
support of his post-doctoral fellowship. The Smithsonian Institution
also supports M.J.G.'s research. A. D. acknowledges partial support from
the INFN grant PD51 and the PRIN-MIUR-2008 grant 2008NR3EBK_003
"Matter-antimatter asymmetry, dark matter and dark energy in the LHC
era." K. R. was funded in part by a Cottrell College Science Award from
the Research Corporation. 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 112
TC 15
Z9 15
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 64
DI 10.1088/0004-637X/752/1/64
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400064
ER
PT J
AU Kelly, BC
Shetty, R
Stutz, AM
Kauffmann, J
Goodman, AA
Launhardt, R
AF Kelly, Brandon C.
Shetty, Rahul
Stutz, Amelia M.
Kauffmann, Jens
Goodman, Alyssa A.
Launhardt, Ralf
TI DUST SPECTRAL ENERGY DISTRIBUTIONS IN THE ERA OF HERSCHEL AND PLANCK: A
HIERARCHICAL BAYESIAN-FITTING TECHNIQUE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: ISM; ISM: structure; methods: data analysis; methods:
statistical; stars: formation
ID STAR-FORMING CORES; T-TAURI STARS; TEMPERATURE-DEPENDENCE;
PROTOPLANETARY DISKS; INFRARED GALAXIES; SILICATE GRAINS; SUBMILLIMETER;
INDEX; MASS; EMISSIVITY
AB We present a hierarchical Bayesian method for fitting infrared spectral energy distributions (SEDs) of dust emission to observed fluxes. Under the standard assumption of optically thin single temperature (T) sources, the dust SED as represented by a power-law-modified blackbody is subject to a strong degeneracy between T and the spectral index beta. The traditional non-hierarchical approaches, typically based on chi(2) minimization, are severely limited by this degeneracy, as it produces an artificial anti-correlation between T and beta even with modest levels of observational noise. The hierarchical Bayesian method rigorously and self-consistently treats measurement uncertainties, including calibration and noise, resulting in more precise SED fits. As a result, the Bayesian fits do not produce any spurious anti-correlations between the SED parameters due to measurement uncertainty. We demonstrate that the Bayesian method is substantially more accurate than the chi(2) fit in recovering the SED parameters, as well as the correlations between them. As an illustration, we apply our method to Herschel and submillimeter ground-based observations of the star-forming Bok globule CB244. This source is a small, nearby molecular cloud containing a single low-mass protostar and a starless core. We find that T and beta are weakly positively correlated-in contradiction with the chi(2) fits, which indicate a T-beta anti-correlation from the same data set. Additionally, in comparison to the chi(2) fits the Bayesian SED parameter estimates exhibit a reduced range in values.
C1 [Kelly, Brandon C.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kelly, Brandon C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Shetty, Rahul] Univ Heidelberg, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany.
[Stutz, Amelia M.; Launhardt, Ralf] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Kauffmann, Jens] NASA JPL, Pasadena, CA 91109 USA.
RP Kelly, BC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Goodman, Alyssa/A-6007-2010;
OI Goodman, Alyssa/0000-0003-1312-0477; Stutz, Amelia/0000-0003-2300-8200
FU National Science Foundation [AST-0908159]; NASA through Space Telescope
Science Institute [HF-01220.01, HF-51243.01]; Southern California Center
for Galaxy Evolution; University of California Office of Research;
German Bundesministerium fur Bildung und Forschung via the ASTRONET
project STAR FORMAT [05A09VHA]; NASA [NAS 5-26555]; The Milky Way System
[SFB 881]
FX We are grateful to Scott Schnee, David Hogg, Karin Sandstrom, Cornelis
Dullemond, Chris Beaumont, Paul Clark, Ralf Klessen, Bruce Draine,
Jonathan Foster, Xiao-Li Meng, Alexander Blocker, and Chris Hayward for
useful discussions regarding dust emission and Bayesian inference. We
are also grateful to an anonymous referee whose suggestions for
additional tests helped improve the paper. This material is based upon
work supported by the National Science Foundation under grant No.
AST-0908159. B. K. acknowledges support by NASA through Hubble
Fellowship grants HF-01220.01 and HF-51243.01 awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555, and from the Southern California Center for Galaxy
Evolution, a multi-campus research program funded by the University of
California Office of Research. R.S. is supported by the German
Bundesministerium fur Bildung und Forschung via the ASTRONET project
STAR FORMAT (grant 05A09VHA), and the SFB 881 "The Milky Way System."
NR 53
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 55
DI 10.1088/0004-637X/752/1/55
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400055
ER
PT J
AU Kocsis, B
Ray, A
Portegies Zwart, S
AF Kocsis, Bence
Ray, Alak
Portegies Zwart, Simon
TI MAPPING THE GALACTIC CENTER WITH GRAVITATIONAL WAVE MEASUREMENTS USING
PULSAR TIMING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: nuclei; gravitational waves; pulsars: general
ID MASSIVE BLACK-HOLE; SAGITTARIUS-A-ASTERISK; DENSE STAR-CLUSTERS;
BINARY-SYSTEMS; HYPERVELOCITY STARS; MILLISECOND PULSAR;
GLOBULAR-CLUSTERS; STELLAR REMNANTS; RADIATION; SEGREGATION
AB We examine the nHz gravitational wave (GW) foreground of stars and black holes (BHs) orbiting SgrA* in the Galactic center. A cusp of stars and BHs generates a continuous GW spectrum below 40 nHz; individual BHs within 1 mpc to SgrA* stick out in the spectrum at higher GW frequencies. The GWs and gravitational near-field effects can be resolved by timing pulsars within a few pc of this region. Observations with the Square Kilometer Array may be especially sensitive to intermediate-mass BHs in this region, if present. A 100 ns-10 mu s timing accuracy is sufficient to detect BHs of mass 1000 M-circle dot with pulsars at distance 0.1-1 pc in a 3 yr observation baseline. Unlike electromagnetic imaging techniques, the prospects for resolving individual objects through GW measurements improve closer to SgrA*, even if the number density of objects steeply increases inward. Scattering by the interstellar medium will pose the biggest challenge for such observations.
C1 [Kocsis, Bence; Ray, Alak] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ray, Alak] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Portegies Zwart, Simon] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Kocsis, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM bkocsis@cfa.harvard.edu; akr@tifr.res.in; spz@strw.leidenuniv.nl
RI Kocsis, Bence/C-3061-2013
OI Kocsis, Bence/0000-0002-4865-7517
FU NASA issued by the Chandra X-ray Observatory Center [PF9-00063];
National Aeronautics Space Administration [NAS8-03060]; Hungarian
Research Fund OTKA [68228]; Netherlands Research Council NWO
[639.073.803]; Netherlands Research School for Astronomy (NOVA); Tata
Institute of Fundamental Research (TIFR) [11P-409]; ITC
FX B.K. acknowledges support from NASA through Einstein Postdoctoral
Fellowship Award Number PF9-00063 issued by the Chandra X-ray
Observatory Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of the National Aeronautics Space
Administration under contract NAS8-03060. A. R. thanks the Director and
members of the Institute for Theory and Computation (ITC), Harvard
University for hospitality. He also thanks Woldek Kluzniak, Duncan
Lorimer, and Maura McLaughlin for discussions. This work was supported
by the Hungarian Research Fund OTKA (grant 68228), Netherlands Research
Council NWO (grant no. 639.073.803), the Netherlands Research School for
Astronomy (NOVA), the Eleventh Five Year Plan Project No. 11P-409 at
Tata Institute of Fundamental Research (TIFR), and by funding from the
ITC for a sabbatical visit of A.R.
NR 78
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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 JUN 10
PY 2012
VL 752
IS 1
AR 67
DI 10.1088/0004-637X/752/1/67
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400067
ER
PT J
AU Lehmer, BD
Xue, YQ
Brandt, WN
Alexander, DM
Bauer, FE
Brusa, M
Comastri, A
Gilli, R
Hornschemeier, AE
Luo, B
Paolillo, M
Ptak, A
Shemmer, O
Schneider, DP
Tozzi, P
Vignali, C
AF Lehmer, B. D.
Xue, Y. Q.
Brandt, W. N.
Alexander, D. M.
Bauer, F. E.
Brusa, M.
Comastri, A.
Gilli, R.
Hornschemeier, A. E.
Luo, B.
Paolillo, M.
Ptak, A.
Shemmer, O.
Schneider, D. P.
Tozzi, P.
Vignali, C.
TI THE 4 Ms CHANDRA DEEP FIELD-SOUTH NUMBER COUNTS APPORTIONED BY SOURCE
CLASS: PERVASIVE ACTIVE GALACTIC NUCLEI AND THE ASCENT OF NORMAL
GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: active; galaxies: starburst; X-rays:
galaxies
ID X-RAY-EMISSION; STAR-FORMATION HISTORY; LUMINOUS INFRARED GALAXIES;
LYMAN BREAK GALAXIES; SIMILAR-TO 1; XMM-NEWTON; SOURCE CATALOG;
STELLAR-MASS; MULTIWAVELENGTH PROJECT; HIGH-REDSHIFT
AB We present 0.5-2 keV, 2-8 keV, 4-8 keV, and 0.5-8 keV (hereafter soft, hard, ultra-hard, and full bands, respectively) cumulative and differential number-count (log N-log S) measurements for the recently completed approximate to 4 Ms Chandra Deep Field-South (CDF-S) survey, the deepest X-ray survey to date. We implement a new Bayesian approach, which allows reliable calculation of number counts down to flux limits that are factors of approximate to 1.9-4.3 times fainter than the previously deepest number-count investigations. In the soft band (SB), the most sensitive bandpass in our analysis, the approximate to 4 Ms CDF-S reaches a maximum source density of approximate to 27,800 deg(-2). By virtue of the exquisite X-ray and multiwavelength data available in the CDF-S, we are able to measure the number counts from a variety of source populations (active galactic nuclei (AGNs), normal galaxies, and Galactic stars) and subpopulations (as a function of redshift, AGN absorption, luminosity, and galaxy morphology) and test models that describe their evolution. We find that AGNs still dominate the X-ray number counts down to the faintest flux levels for all bands and reach a limiting SB source density of approximate to 14,900 deg(-2), the highest reliable AGN source density measured at any wavelength. We find that the normal-galaxy counts rise rapidly near the flux limits and, at the limiting SB flux, reach source densities of approximate to 12,700 deg(-2) and make up 46% +/- 5% of the total number counts. The rapid rise of the galaxy counts toward faint fluxes, as well as significant normal-galaxy contributions to the overall number counts, indicates that normal galaxies will overtake AGNs just below the approximate to 4 Ms SB flux limit and will provide a numerically significant new X-ray source population in future surveys that reach below the approximate to 4 Ms sensitivity limit. We show that a future approximate to 10 Ms CDF-S would allow for a significant increase in X-ray-detected sources, with many of the new sources being cosmologically distant (z greater than or similar to 0.6) normal galaxies.
C1 [Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, B. D.; Hornschemeier, A. E.; Ptak, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Xue, Y. Q.; Brandt, W. N.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Xue, Y. Q.; Brandt, W. N.; Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Brusa, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Comastri, A.; Gilli, R.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Luo, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Paolillo, M.] Univ Naples Federico II, Dipartimento Sci Fis, I-80126 Naples, Italy.
[Shemmer, O.] Univ N Texas, Dept Phys, Denton, TX 76203 USA.
[Tozzi, P.] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy.
[Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
RP Lehmer, BD (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA.
RI Paolillo, Maurizio/J-1733-2012; Vignali, Cristian/J-4974-2012; Brandt,
William/N-2844-2015; Comastri, Andrea/O-9543-2015; Gilli,
Roberto/P-1110-2015;
OI Paolillo, Maurizio/0000-0003-4210-7693; Vignali,
Cristian/0000-0002-8853-9611; Brandt, William/0000-0002-0167-2453;
Comastri, Andrea/0000-0003-3451-9970; Gilli,
Roberto/0000-0001-8121-6177; Shemmer, Ohad/0000-0003-4327-1460;
Alexander, David/0000-0002-5896-6313; Brusa,
Marcella/0000-0002-5059-6848
FU Einstein Fellowship Program; CXC [SP1-12007A, SAO SP1-12007B]; NASA ADP
[NNX10AC99G]; Science and Technology Facilities Council; Financiamento
Basal; CONICYT-Chile FONDECYT [1101024]; FONDAP-CATA [15010003];
ASI-INAF [I/088/06, I/009/10/0]
FX We thank the anonymous referee for reviewing the manuscript and
providing useful suggestions. We thank Andy Fabian for useful
discussions and acknowledge James Aird, Hermann Brunner, Fabrizio Fiore,
Simonetta Puccetti, and Shaji Vattakunnel for sharing data; these
contributions have helped the quality of this paper. We gratefully
acknowledge financial support from the Einstein Fellowship Program
(B.D.L.), CXC grant SP1-12007A and NASA ADP grant NNX10AC99G (Y.Q.X. and
W.N.B.), the Science and Technology Facilities Council (D.M.A.),
Financiamento Basal, CONICYT-Chile FONDECYT 1101024 and FONDAP-CATA
15010003, and CXC grant SAO SP1-12007B (F.E.B.), and ASI-INAF grants
I/088/06 and I/009/10/0 (A.C., R.G., C.V.).
NR 98
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 46
DI 10.1088/0004-637X/752/1/46
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400046
ER
PT J
AU Melnick, GJ
Tolls, V
Goldsmith, PF
Kaufman, MJ
Hollenbach, DJ
Black, JH
Encrenaz, P
Falgarone, E
Gerin, M
Hjalmarson, A
Li, D
Lis, DC
Liseau, R
Neufeld, DA
Pagani, L
Snell, RL
van der Tak, F
van Dishoeck, EF
AF Melnick, Gary J.
Tolls, Volker
Goldsmith, Paul F.
Kaufman, Michael J.
Hollenbach, David J.
Black, John H.
Encrenaz, Pierre
Falgarone, Edith
Gerin, Maryvonne
Hjalmarson, Ake
Li, Di
Lis, Dariusz C.
Liseau, Rene
Neufeld, David A.
Pagani, Laurent
Snell, Ronald L.
van der Tak, Floris
van Dishoeck, Ewine F.
TI HERSCHEL SEARCH FOR O-2 TOWARD THE ORION BAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: individual objects (Orion); ISM:
molecules; submillimeter: ISM
ID SUBMILLIMETER OBSERVATIONS; MOLECULAR CLOUDS; WATER ICE; INTERSTELLAR
CHLORONIUM; THERMAL BALANCE; CHEMICAL-MODELS; PHOTODESORPTION; EMISSION;
MILLIMETER; REGION
AB We report the results of a search for molecular oxygen (O-2) toward the Orion Bar, a prominent photodissociation region at the southern edge of the HII region created by the luminous Trapezium stars. We observed the spectral region around the frequency of the O-2 N-J = 3(3)-1(2) transition at 487 GHz and the 5(4)-3(4) transition at 774 GHz using the Heterodyne Instrument for the Far-Infrared on the Herschel Space Observatory. Neither line was detected, but the 3 sigma upper limits established here translate to a total line-of-sight O-2 column density <1.5 x 10(16) cm(-2) for an emitting region whose temperature is between 30 K and 250 K, or <1 x 10(16) cm(-2) if the O-2 emitting region is primarily at a temperature of less than or similar to 100 K. Because the Orion Bar is oriented nearly edge-on relative to our line of sight, the observed column density is enhanced by a factor estimated to be between 4 and 20 relative to the face-on value. Our upper limits imply that the face-on O-2 column density is less than 4 x 10(15) cm(-2), a value that is below, and possibly well below, model predictions for gas with a density of 10(4)-10(5) cm-(3) exposed to a far-ultraviolet flux 10(4) times the local value, conditions inferred from previous observations of the Orion Bar. The discrepancy might be resolved if (1) the adsorption energy of O atoms to ice is greater than 800 K; (2) the total face-on AV of the Bar is less than required for O-2 to reach peak abundance; (3) the O-2 emission arises within dense clumps with a small beam filling factor; or (4) the face-on depth into the Bar where O-2 reaches its peak abundance, which is density dependent, corresponds to a sky position different from that sampled by our Herschel beams.
C1 [Melnick, Gary J.; Tolls, Volker] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Goldsmith, Paul F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kaufman, Michael J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Hollenbach, David J.] SETI Inst, Mountain View, CA 94043 USA.
[Black, John H.; Hjalmarson, Ake; Liseau, Rene] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden.
[Encrenaz, Pierre; Pagani, Laurent] Observ Paris, LERMA, F-75014 Paris, France.
[Encrenaz, Pierre; Pagani, Laurent] Observ Paris, CNRS, UMR8112, LRA LERMA, F-75014 Paris, France.
[Falgarone, Edith; Gerin, Maryvonne] Observ Paris, CNRS, UMR8112, LRA LERMA, F-75231 Paris 05, France.
[Falgarone, Edith; Gerin, Maryvonne] Ecole Normale Super, F-75231 Paris 05, France.
[Li, Di] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Lis, Dariusz C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Snell, Ronald L.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[van der Tak, Floris] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
[van der Tak, Floris] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands.
[van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Melnick, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 66, Cambridge, MA 02138 USA.
RI Goldsmith, Paul/H-3159-2016
FU NASA through JPL/Caltech
FX Support for this work was provided by NASA through an award issued by
JPL/Caltech.
NR 46
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 26
DI 10.1088/0004-637X/752/1/26
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400026
ER
PT J
AU Myers, PC
AF Myers, Philip C.
TI MASS AND LUMINOSITY EVOLUTION OF YOUNG STELLAR OBJECTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; stars: formation
ID STAR CLUSTER FORMATION; RADIATION-HYDRODYNAMIC SIMULATIONS; INTERSTELLAR
CLOUDS; MOLECULAR CLOUDS; FORMING REGION; SPITZER SURVEY; DENSE CORES;
INITIAL CONDITIONS; EMBEDDED CLUSTERS; DISK POPULATION
AB A model of protostar mass and luminosity evolution in clusters gives new estimates of cluster age, protostar birthrate, accretion rate, and mean accretion time. The model assumes constant protostar birthrate, core-clump accretion, and equally likely accretion stopping. Its parameters are set to reproduce the initial mass function and to match protostar luminosity distributions in nearby star-forming regions. It obtains cluster ages and birthrates from the observed numbers of protostars and pre-main sequence (PMS) stars, and from the modal value of the protostar luminosity. In 31 embedded clusters and complexes, the global cluster age is 1-3 Myr, matching available estimates based on optical spectroscopy (OS) and evolutionary tracks. This method of age estimation is simpler than OS and is more useful for young embedded clusters where optical spectroscopy is not possible. In the youngest clusters, the protostar fraction decreases outward from the densest gas, indicating that the local star-forming age increases outward from a few 0.1 Myr in small protostar-dominated zones to a few Myr in large PMS-dominated zones.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM pmyers@cfa.harvard.edu
NR 86
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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 JUN 10
PY 2012
VL 752
IS 1
AR 9
DI 10.1088/0004-637X/752/1/9
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400009
ER
PT J
AU Riess, AG
Macri, L
Casertano, S
Lampeitl, H
Ferguson, HC
Filippenko, AV
Jha, SW
Li, WD
Chornock, R
Silverman, JM
AF Riess, Adam G.
Macri, Lucas
Casertano, Stefano
Lampeitl, Hubert
Ferguson, Henry C.
Filippenko, Alexei V.
Jha, Saurabh W.
Li, Weidong
Chornock, Ryan
Silverman, Jeffrey M.
TI A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE
SPACE TELESCOPE AND WIDE FIELD CAMERA 3 (vol 730, pg 119, 2011)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Riess, Adam G.; Casertano, Stefano; Ferguson, Henry C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Macri, Lucas] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Lampeitl, Hubert] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Filippenko, Alexei V.; Li, Weidong; Silverman, Jeffrey M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Riess, AG (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
NR 2
TC 14
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 76
DI 10.1088/0004-637X/752/1/76
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400076
ER
PT J
AU Sun, MY
Liu, T
Gu, WM
Lu, JF
AF Sun, Mou-Yuan
Liu, Tong
Gu, Wei-Min
Lu, Ju-Fu
TI GRAVITATIONAL WAVES OF JET PRECESSION IN GAMMA-RAY BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; gamma-ray burst:
general; gravitational waves
ID NEUTRINO-DOMINATED ACCRETION; BLACK-HOLES; OBSERVATIONAL EVIDENCE;
GALACTIC NUCLEI; LIGHT CURVES; DISKS; DRIVEN; MODELS; LUMINOSITY;
PHYSICS
AB The physical nature of gamma-ray bursts (GRBs) is believed to involve an ultra-relativistic jet. The observed complex structure of light curves motivates the idea of jet precession. In this work, we study the gravitational waves of jet precession based on neutrino-dominated accretion disks around black holes, which may account for the central engine of GRBs. In our model, the jet and the inner part of the disk may precess along with the black hole, which is driven by the outer part of the disk. Gravitational waves are therefore expected to be significant from this black-hole-inner-disk precession system. By comparing our numerical results with the sensitivity of some detectors, we find that it is possible for DECIGO and BBO to detect such gravitational waves, particularly for GRBs in the Local Group.
C1 [Sun, Mou-Yuan; Liu, Tong; Gu, Wei-Min; Lu, Ju-Fu] Xiamen Univ, Dept Phys, Xiamen 361005, Fujian, Peoples R China.
[Sun, Mou-Yuan; Liu, Tong; Gu, Wei-Min; Lu, Ju-Fu] Xiamen Univ, Inst Theoret Phys & Astrophys, Xiamen 361005, Fujian, Peoples R China.
[Gu, Wei-Min] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Liu, T (reprint author), Xiamen Univ, Dept Phys, Xiamen 361005, Fujian, Peoples R China.
EM tongliu@xmu.edu.cn
RI Gu, WM/G-3984-2010;
OI Sun, Mouyuan/0000-0002-0771-2153
FU National Basic Research Program (973 Program) of China [2009CB824800];
National Natural Science Foundation of China [10833002, 11073015,
11103015]
FX We thank the anonymous referee for very useful suggestions and comments.
We thank Ye-Fei Yuan, Matias M. Reynoso, and Gustavo E. Romero for
beneficial discussions. This work was supported by the National Basic
Research Program (973 Program) of China under grant 2009CB824800, and
the National Natural Science Foundation of China under grants 10833002,
11073015, and 11103015.
NR 43
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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 JUN 10
PY 2012
VL 752
IS 1
AR 31
DI 10.1088/0004-637X/752/1/31
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400031
ER
PT J
AU Takahashi, S
Saigo, K
Ho, PTP
Tomida, K
AF Takahashi, Satoko
Saigo, Kazuya
Ho, Paul T. P.
Tomida, Kengo
TI SPATIALLY RESOLVING SUBSTRUCTURES WITHIN THE MASSIVE ENVELOPE AROUND AN
INTERMEDIATE-MASS PROTOSTAR: MMS 6/OMC-3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE evolution; ISM: clouds; stars: formation; stars: individual (OMC3-MMS 6)
ID MOLECULAR CLOUD CORE; STAR-FORMING REGIONS; STELLAR DENSITIES; GASEOUS
DISKS; DENSE CORES; 1ST CORES; COLLAPSE; OUTFLOWS; ORION; FRAGMENTATION
AB With the Submillimeter Array, the brightest (sub)millimeter continuum source in the Orion Molecular Cloud-2/3 region, MMS 6, has been observed in the 850 mu m continuum emission with approximately 10 times better angular resolution than previous studies (approximate to 0 ''.3, approximate to 120 AU at Orion). The deconvolved size, the mass, and the column density of MMS 6-main are estimated to be 0 ''.32 x 0 ''.29 (132 AU x 120 AU), 0.29 M-circle dot, and 2.1 x 10(25) cm(-2), respectively. The estimated extremely high mean number density, 1.5 x 10(10) cm(-3), suggests that MMS 6-main is likely optically thick at 850 mu m. We compare our observational data with three theoretical core models: prestellar core, protostellar core + disk-like structure, and first adiabatic core. These comparisons clearly show that the observational data cannot be modeled as a simple prestellar core with a gas temperature of 20 K. A self-luminous source is necessary to explain the observed flux density in the (sub) millimeter wavelengths. Our recent detection of a very compact and energetic outflow in the CO (3-2) and HCN (4-3) lines supports the presence of a protostar. We suggest that MMS 6 is one of the first cases of an intermediate-mass protostellar core at an extremely young stage. In addition to the MMS 6-main peak, we have also spatially resolved a number of spiky structures and sub-clumps, distributed over the central 1000 AU. The masses of these sub-clumps are estimated to be 0.066-0.073 M-circle dot, which are on the order of brown dwarf masses. Higher angular resolution and higher sensitivity observations with ALMA and EVLA will reveal the origin and nature of these structures such as whether they are originated from fragmentations, spiral arms, or inhomogeneity within the disk-like structures/envelope.
C1 [Takahashi, Satoko; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Saigo, Kazuya; Tomida, Kengo] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Tomida, Kengo] Grad Univ Adv Studies, Natl Astron Observ Japan, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Tomida, Kengo] Princeton Univ, Dept Astrophys, Princeton, NJ 08544 USA.
RP Takahashi, S (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.
EM satoko_t@asiaa.sinica.edu.tw
OI Tomida, Kengo/0000-0001-8105-8113
FU Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan; Japan
Society for the Promotion of Science (JSPS)
FX We thank our two anonymous referees for very helpful suggestions which
improved the clarity and logic of the paper. We acknowledge the staff at
the Submillimeter Array for their assistance with the observations. We
thank Keiichi Asada for fruitful discussions. S. T. is financially
supported by a postdoctoral fellowship at the Institute of Astronomy and
Astrophysics, Academia Sinica, Taiwan. K. T. was supported by the
Research Fellowship from the Japan Society for the Promotion of Science
(JSPS) for Young Scientists.
NR 48
TC 7
Z9 7
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 10
DI 10.1088/0004-637X/752/1/10
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400010
ER
PT J
AU Wellons, S
Soderberg, AM
Chevalier, RA
AF Wellons, Sarah
Soderberg, Alicia M.
Chevalier, Roger A.
TI RADIO OBSERVATIONS REVEAL UNUSUAL CIRCUMSTELLAR ENVIRONMENTS FOR SOME
TYPE Ibc SUPERNOVA PROGENITORS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: winds, outflows; supernovae: general
ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; LUMINOUS BLUE VARIABLES;
MASSIVE STARS; IB/C SUPERNOVAE; IC SUPERNOVAE; PRESUPERNOVA EVOLUTION;
BINARY PROGENITOR; LIGHT CURVES; SN 1993J
AB We present extensive radio observations of the nearby Type Ibc supernovae (SNe Ibc) 2004cc, 2004dk, and 2004gq spanning Delta t approximate to 8-1900 days after explosion. Using a dynamical model developed for synchrotron emission from a slightly decelerated shock wave, we estimate the velocity and energy of the fastest ejecta and the density profile of the circumstellar medium. The shock waves of all three supernovae are characterized by non-relativistic velocities of (v) over bar approximate to (0.1-25)c and associated energies of E approximate to (2-10) x 10(47) erg, in line with the expectations for a typical homologous explosion. Smooth circumstellar density profiles are indicated by the early radio data and we estimate the progenitor mass-loss rates to be (M) over dot approximate to (0.6-13) x 10(-5) M-circle dot yr(-1) (wind velocity, v(w) = 10(3) km s(-1)). These estimates approach the saturation limit ((M) over dot approximate to 10(-4) M-circle dot yr(-1)) for line-driven winds from Wolf-Rayet stars, the favored progenitors of SNe Ibc including those associated with long-duration gamma-ray bursts. Intriguingly, at later epochs all three supernovae show evidence for abrupt radio variability that we attribute to large density modulations (factor of similar to 3-6) at circumstellar radii of r approximate to (1-50) x 10(16) cm. If due to variable mass loss, these modulations are associated with progenitor activity on a timescale of similar to 10-100 years before explosion. We consider these results in the context of variable mass-loss mechanisms including wind clumping, metallicity-independent continuum-driven ejections, and binary-induced modulations. It may also be possible that the SN shock waves are dynamically interacting with wind termination shocks; however, this requires the environment to be highly pressurized and/or the progenitor to be rapidly rotating prior to explosion. The proximity of the density modulations to the explosion sites may suggest a synchronization between unusual progenitor mass loss and the SN explosion, reminiscent of Type IIn supernovae. This study underscores the utility of radio observations for tracing the final evolutionary stage(s) of SN progenitor systems.
C1 [Wellons, Sarah; Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chevalier, Roger A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
RP Wellons, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU National Science Foundation Research Experiences for Undergraduates
(REU); Department of Defense [0754568]; Smithsonian Institution
FX We thank our anonymous referees, Norbert Langer, Stan Owocki, Nathan
Smith, Vikram Dwarkadas, and Shri Kulkarni, for helpful discussions. S.
W. and A. M. S. acknowledge support by the National Science Foundation
Research Experiences for Undergraduates (REU) and Department of Defense
Awards to Stimulate and Support Undergraduate Research Experiences
(ASSURE) programs under grant no. 0754568 and by the Smithsonian
Institution.
NR 109
TC 23
Z9 23
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2012
VL 752
IS 1
AR 17
DI 10.1088/0004-637X/752/1/17
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 961KN
UT WOS:000305463400017
ER
PT J
AU Pe'er, A
AF Pe'er, Asaf
TI DYNAMICAL MODEL OF AN EXPANDING SHELL
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE hydrodynamics; ISM: jets and outflows; plasmas; shock waves
ID GAMMA-RAY BURSTS; RELATIVISTIC BLAST WAVES; EQUITEMPORAL SURFACES; GRS
1915+105; AFTERGLOWS; EMISSION; JETS; SUPERNOVAE; FIREBALLS; SHOCKS
AB Expanding blast waves are ubiquitous in many astronomical sources, such as supernova remnants, X-ray emitting binaries, and gamma-ray bursts. I consider here the dynamics of such an expanding blast wave, both in the adiabatic and the radiative regimes. As the blast wave collects material from its surroundings, it decelerates. A full description of the temporal evolution of the blast wave requires consideration of both the energy density and the pressure of the shocked material. The obtained equation is different from earlier works in which only the energy was considered. The solution converges to the familiar results in both the ultrarelativistic and the sub-relativistic (Newtonian) regimes.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Pe'er, A (reprint author), Harvard Smithsonian Ctr Astrophys, MS 51,60 Garden St, Cambridge, MA 02138 USA.
NR 35
TC 18
Z9 18
U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUN 10
PY 2012
VL 752
IS 1
AR L8
DI 10.1088/2041-8205/752/1/L8
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 948FL
UT WOS:000304488900008
ER
PT J
AU Ikegami, M
Whigham, DF
Werger, MJA
AF Ikegami, Makihiko
Whigham, Dennis F.
Werger, Marinus J. A.
TI Effects of local density of clonal plants on their sexual and vegetative
propagation strategies in a lattice structure model
SO ECOLOGICAL MODELLING
LA English
DT Article
DE Clonal plant; Lattice model; Life history strategy; Vegetative
propagation; Sexual propagation
ID REPRODUCTIVE STRATEGIES; POPULATION-DYNAMICS; SEED REPRODUCTION;
ALLOCATION; HABITAT; INTEGRATION; COMPETITION
AB Clonal plants can propagate both sexually and vegetatively and the balance between the efforts of sexual and vegetative propagation can be determined by inter- and intra-specific competition. This raises the question of whether sexual propagation becomes more suitable than vegetative propagation or vice versa. Some studies suggest seed production is positively correlated with plant density, and others, negatively. To evaluate the effects of local density of ramets on plant propagation strategy, we developed a lattice model where two strategies compete with each other. In the model, a plant changes its strategy based on local density as defined by the proportion of neighboring lattice cells containing plants. One strategy produces seeds at high local density (SEEDING at HLD) and produces ramets at low local density, and the other strategy produces ramets at high local density (RAMETING at HLD) and seeds at low local density. Seeds can spread all cells while ramets can reach only adjacent cells, and if an individual from a seed competes with an individual from a vegetative propagule, the latter always wins. Each plant has different thresholds to change its strategy from sexual to vegetative, or vice versa, along with local density. In the model, a realized density depends on both reproductive rate and mortality; thus, we evaluate the performance of each strategy under different mortalities.
When mortality is high, a realized density becomes low. Under this condition, plants reproduce mainly by seeds (either the SEEDING at HLD plants with lower threshold values, or RAMETING at HLD plants with higher threshold values) and show high performance. High mortality results in many vacant lattice cells that do not have neighboring plants. Since vegetative propagules cannot reach these isolated vacant lattice cells while seeds can, plants that propagate mostly or exclusively by seed become dominant. When mortality is low, the local density becomes high and few cells are available for new individuals. Under this condition, SEEDING at HLD becomes dominant. SEEDING at HLD plants with a high threshold value almost always reproduce ramets, but they also produce seeds when neighboring cells are completely occupied. Although SEEDING at HLD plants with a high threshold value and RAMETING at HLD plants have an equal chance to get established by vegetative propagation, SEEDING at HLD plants also produce seeds when there are no vacant neighboring cells (i.e., high density), and those seeds can, although rarely, establish new individuals. In conclusion, the production of ramets at lower densities and the production of seeds at higher densities seem to be a proper strategy in our model. (C) 2012 Published by Elsevier B.V.
C1 [Ikegami, Makihiko; Werger, Marinus J. A.] Univ Utrecht, Dept Plant Ecol & Biodiversity, NL-3508 TB Utrecht, Netherlands.
[Ikegami, Makihiko; Whigham, Dennis F.; Werger, Marinus J. A.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Whigham, Dennis F.] Univ Utrecht, Dept Landscape Ecol, NL-3508 TB Utrecht, Netherlands.
RP Ikegami, M (reprint author), Univ Calif Santa Barbara, Donald Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
EM makihiko@mbox.kyoto-inet.or.jp
RI IKEGAMI, Makihiko/E-6612-2012;
OI Whigham, Dennis/0000-0003-1488-820X
FU Andrew W. Mellon Foundation through the Smithsonian Institution; Faculty
of Biology at Utrecht University
FX We would like to thank Doug Bradley at UCSB and two anonymous reviewers
for their comments to improve the readability of this manuscript. This
study was financially supported by a grant to MJAW from the Andrew W.
Mellon Foundation through the Smithsonian Institution and by the Faculty
of Biology at Utrecht University.
NR 41
TC 6
Z9 7
U1 2
U2 22
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0304-3800
J9 ECOL MODEL
JI Ecol. Model.
PD JUN 10
PY 2012
VL 234
SI SI
BP 51
EP 59
DI 10.1016/j.ecolmodel.2012.03.026
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 950GB
UT WOS:000304636500006
ER
PT J
AU Xi, Z
Bradley, RK
Wurdack, KJ
Wong, KM
Sugumaran, M
Bomblies, K
Rest, JS
Davis, CC
AF Xi, Zhenxiang
Bradley, Robert K.
Wurdack, Kenneth J.
Wong, K. M.
Sugumaran, M.
Bomblies, Kirsten
Rest, Joshua S.
Davis, Charles C.
TI Horizontal transfer of expressed genes in a parasitic flowering plant
SO BMC GENOMICS
LA English
DT Article
DE Rafflesia; Transcriptome; Phylogenomics; Horizontal gene transfer; Codon
usage
ID GENOME SEQUENCE; DNA-SEQUENCES; CODON USAGE; EVOLUTION; ANGIOSPERMS;
ANNOTATION; ALGORITHM; DISCOVERY; RESOURCE; EXCHANGE
AB Background: Recent studies have shown that plant genomes have potentially undergone rampant horizontal gene transfer (HGT). In plant parasitic systems HGT appears to be facilitated by the intimate physical association between the parasite and its host. HGT in these systems has been invoked when a DNA sequence obtained from a parasite is placed phylogenetically very near to its host rather than with its closest relatives. Studies of HGT in parasitic plants have relied largely on the fortuitous discovery of gene phylogenies that indicate HGT, and no broad systematic search for HGT has been undertaken in parasitic systems where it is most expected to occur.
Results: We analyzed the transcriptomes of the holoparasite Rafflesia cantleyi Solms-Laubach and its obligate host Tetrastigma rafflesiae Miq. using phylogenomic approaches. Our analyses show that several dozen actively transcribed genes, most of which appear to be encoded in the nuclear genome, are likely of host origin. We also find that hundreds of vertically inherited genes (VGT) in this parasitic plant exhibit codon usage properties that are more similar to its host than to its closest relatives.
Conclusions: Our results establish for the first time a substantive number of HGTs in a plant host-parasite system. The elevated rate of unidirectional host-to- parasite gene transfer raises the possibility that HGTs may provide a fitness benefit to Rafflesia for maintaining these genes. Finally, a similar convergence in codon usage of VGTs has been shown in microbes with high HGT rates, which may help to explain the increase of HGTs in these parasitic plants.
C1 [Rest, Joshua S.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA.
[Xi, Zhenxiang; Bomblies, Kirsten; Davis, Charles C.] Harvard Univ Hebaria, Dept Organism & Evolut Biol, Cambridge, MA 02138 USA.
[Bradley, Robert K.] Fred Hutchinson Canc Res Ctr, Div Publ Hlth Sci, Computat Biol Program, Seattle, WA 98109 USA.
[Bradley, Robert K.] Fred Hutchinson Canc Res Ctr, Div Basic Sci, Seattle, WA 98109 USA.
[Wurdack, Kenneth J.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA.
[Wong, K. M.] Singapore Bot Gardens, Singapore 259569, Singapore.
[Sugumaran, M.] Univ Malaya, Inst Biol Sci, Rimba Ilmu Bot Garden, Kuala Lumpur 50603, Malaysia.
RP Rest, JS (reprint author), SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA.
EM joshua.rest@stonybrook.edu; cdavis@oeb.harvard.edu
RI MANICKAM, SUGUMARAN/B-5268-2010;
OI Rest, Joshua/0000-0002-9582-1041; Bomblies, Kirsten/0000-0002-2434-3863;
Bradley, Robert/0000-0002-8046-1063
FU National Science Foundation (NSF) Assembling the Tree of Life
[DEB-0622764]; NSF [DEB-1120243]
FX We thank Stijn van Dongen, Casey Dunn, Michael Ethier, Amir Karger,
Devin Locke, Sergey Lukyanov, Evandro Novaes, Alexis Stamatakis, and
Jiangwen Zhang for technical assistance. We also thank William Anderson,
Mark Beilstein, Andrew Knoll, Christopher Marx, Sarah Mathews, Brian
O'Meara, and members of the Davis laboratory for helpful discussions.
CCD was supported by the National Science Foundation (NSF) Assembling
the Tree of Life grant DEB-0622764 and NSF DEB-1120243.
NR 45
TC 35
Z9 39
U1 4
U2 62
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2164
J9 BMC GENOMICS
JI BMC Genomics
PD JUN 8
PY 2012
VL 13
AR 227
DI 10.1186/1471-2164-13-227
PG 8
WC Biotechnology & Applied Microbiology; Genetics & Heredity
SC Biotechnology & Applied Microbiology; Genetics & Heredity
GA 014YK
UT WOS:000309411700001
PM 22681756
ER
PT J
AU Wilson, JK
Spence, HE
Kasper, J
Golightly, M
Blake, JB
Mazur, JE
Townsend, LW
Case, AW
Looper, MD
Zeitlin, C
Schwadron, NA
AF Wilson, Jody K.
Spence, Harlan E.
Kasper, Justin
Golightly, Michael
Blake, J. Bern
Mazur, Joe E.
Townsend, Lawrence W.
Case, Anthony W.
Looper, Mark Dixon
Zeitlin, Cary
Schwadron, Nathan A.
TI The first cosmic ray albedo proton map of the Moon
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LUNAR PROSPECTOR; FAST-NEUTRONS; DEPOSITS; POLES
AB Neutrons emitted from the Moon are produced by the impact of galactic cosmic rays (GCRs) within the regolith. GCRs are high-energy particles capable of smashing atomic nuclei in the lunar regolith and producing a shower of energetic protons, neutrons and other subatomic particles. Secondary particles that are ejected out of the regolith become "albedo" particles. The neutron albedo has been used to study the hydrogen content of the lunar regolith, which motivates our study of albedo protons. In principle, the albedo protons should vary as a function of the input GCR source and possibly as a result of surface composition and properties. During the LRO mission, the total detection rate of albedo protons between 60 MeV and 150 MeV has been declining since 2009 in parallel with the decline in the galactic cosmic ray flux, which validates the concept of an albedo proton source. On the other hand, the average yield of albedo protons has been increasing as the galactic cosmic ray spectrum has been hardening, consistent with a disproportionately stronger modulation of lower energy GCRs as solar activity increases. We construct the first map of the normalized albedo proton emission rate from the lunar surface to look for any albedo variation that correlates with surface features. The map is consistent with a spatially uniform albedo proton yield to within statistical uncertainties.
C1 [Wilson, Jody K.; Golightly, Michael; Schwadron, Nathan A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Spence, Harlan E.] Univ New Hampshire, Inst Earth Oceans & Space, Durham, NH 03824 USA.
[Kasper, Justin; Case, Anthony W.] Harvard Smithsonian Ctr Astrophys, High Energy Astrophys Div, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Blake, J. Bern; Looper, Mark Dixon] Aerosp Corp, Dept Space Sci, Los Angeles, CA 90009 USA.
[Mazur, Joe E.] Aerosp Corp, Space Sci Dept Chantilly, Chantilly, VA USA.
[Townsend, Lawrence W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA.
[Zeitlin, Cary] SW Res Inst, Boulder, CO USA.
RP Wilson, JK (reprint author), Univ New Hampshire, Ctr Space Sci, Morse Hall Room 353,8 Coll Rd, Durham, NH 03824 USA.
EM jody.wilson@unh.edu
RI Spence, Harlan/A-1942-2011; Kasper, Justin/D-1152-2010;
OI Kasper, Justin/0000-0002-7077-930X; Spence, Harlan/0000-0002-2526-2205
FU NASA [NNG11PA03C]
FX This work is supported by the NASA CRaTER contract NNG11PA03C. We thank
Alexander Boyd for assistance with data reduction.
NR 35
TC 6
Z9 6
U1 1
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JUN 5
PY 2012
VL 117
AR E00H23
DI 10.1029/2011JE003921
PG 7
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 957IS
UT WOS:000305155700001
ER
PT J
AU Perego, UA
Lancioni, H
Tribaldos, M
Angerhofer, N
Ekins, JE
Olivieri, A
Woodward, SR
Pascale, JM
Cooke, R
Motta, J
Achilli, A
AF Perego, Ugo A.
Lancioni, Hovirag
Tribaldos, Maribel
Angerhofer, Norman
Ekins, Jayne E.
Olivieri, Anna
Woodward, Scott R.
Pascale, Juan Miguel
Cooke, Richard
Motta, Jorge
Achilli, Alessandro
TI Decrypting the Mitochondrial Gene Pool of Modern Panamanians
SO PLOS ONE
LA English
DT Article
ID NATIVE-AMERICAN POPULATIONS; Y-CHROMOSOME; COSTA-RICA; LATE PLEISTOCENE;
MTDNA VARIATION; NORTH-AMERICA; DNA; DIVERSITY; EVOLUTIONARY; HISTORY
AB The Isthmus of Panama-the narrow neck of land connecting the northern and southern American landmasses-was an obligatory corridor for the Paleo-Indians as they moved into South America. Archaeological evidence suggests an unbroken link between modern natives and their Paleo-Indian ancestors in some areas of Panama, even if the surviving indigenous groups account for only 12.3% of the total population. To evaluate if modern Panamanians have retained a larger fraction of the native pre-Columbian gene pool in their maternally-inherited mitochondrial genome, DNA samples and historical records were collected from more than 1500 volunteer participants living in the nine provinces and four indigenous territories of the Republic. Due to recent gene-flow, we detected similar to 14% African mitochondrial lineages, confirming the demographic impact of the Atlantic slave trade and subsequent African immigration into Panama from Caribbean islands, and a small European (similar to 2%) component, indicating only a minor influence of colonialism on the maternal side. The majority (similar to 83%) of Panamanian mtDNAs clustered into native pan-American lineages, mostly represented by haplogroup A2 (51%). These findings reveal an overwhelming native maternal legacy in today's Panama, which is in contrast with the overall concept of personal identity shared by many Panamanians. Moreover, the A2 sub-clades A2ad and A2af (with the previously named 6 bp Huetar deletion), when analyzed at the maximum level of resolution (26 entire mitochondrial genomes), confirm the major role of the Pacific coastal path in the peopling of North, Central and South America, and testify to the antiquity of native mitochondrial genomes in Panama.
C1 [Perego, Ugo A.; Angerhofer, Norman; Ekins, Jayne E.; Woodward, Scott R.] Sorenson Mol Geneal Fdn, Salt Lake City, UT USA.
[Lancioni, Hovirag; Achilli, Alessandro] Univ Perugia, Dipartimento Biol Cellulare & Ambientale, I-06100 Perugia, Italy.
[Tribaldos, Maribel; Pascale, Juan Miguel; Motta, Jorge] Inst Conmemorativo Gorgas Estudios Salud, Panama City, Panama.
[Angerhofer, Norman; Woodward, Scott R.] Ancestry, Provo, UT USA.
[Olivieri, Anna] Univ Pavia, Dipartimento Biol & Biotecnol, I-27100 Pavia, Italy.
[Cooke, Richard] Smithsonian Trop Res Inst, Apdo, Ancon, Panama.
RP Perego, UA (reprint author), Sorenson Mol Geneal Fdn, Salt Lake City, UT USA.
EM alessandro.achilli@unipg.it
RI Lancioni, Hovirag/F-9067-2014; OLIVIERI, ANNA/I-9235-2012; Achilli,
Alessandro/I-9236-2012
OI Lancioni, Hovirag/0000-0001-5514-1853; OLIVIERI,
ANNA/0000-0002-3941-8098; Achilli, Alessandro/0000-0001-6871-3451
FU Instituto Conmemorativo Gorgas de Estudios de la Salud; Gorgas Internal
Grant for Genealogy Studies; Italian Ministry of the University:
FIRB-Futuro in Ricerca; Progetti Ricerca Interesse Nazionale; Sorenson
Molecular Genealogy Foundation
FX This research received support from the Instituto Conmemorativo Gorgas
de Estudios de la Salud (to JM), Gorgas Internal Grant for Genealogy
Studies (to JMP), the Italian Ministry of the University: FIRB-Futuro in
Ricerca 2008 (to AA and AO), Progetti Ricerca Interesse Nazionale 2009
(to AA), and the Sorenson Molecular Genealogy Foundation (to UAP, NA and
SRW). The authors are grateful to all the donors for providing
biological specimens, and to everyone at the Instituto Conmemorativo
Gorgas and at the Sorenson Molecular Genealogy Foundation for their work
on the preliminary data. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 57
TC 16
Z9 16
U1 0
U2 6
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JUN 4
PY 2012
VL 7
IS 6
AR e38337
DI 10.1371/journal.pone.0038337
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959UU
UT WOS:000305341700060
PM 22675545
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI PANAMA EXPOSED
SO SMITHSONIAN
LA English
DT Editorial Material
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SMITHSONIAN ASSOC
PI WASHINGTON
PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA
SN 0037-7333
J9 SMITHSONIAN
JI Smithsonian
PD JUN
PY 2012
VL 43
IS 3
BP 8
EP 8
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 126SS
UT WOS:000317642100002
ER
PT J
AU Sonsthagen, SA
Chesser, RT
Bell, DA
Dove, CJ
AF Sonsthagen, Sarah A.
Chesser, R. Terry
Bell, Douglas A.
Dove, Carla J.
TI Hybridization among Arctic white-headed gulls (Larus spp.) obscures the
genetic legacy of the Pleistocene
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Genetic structure; hybridization; Larus; Pleistocene glacial refugia;
white-headed gulls
ID GLAUCESCENS-OCCIDENTALIS COMPLEX; MITOCHONDRIAL-DNA; NORTH-AMERICA;
DIFFERENTIATION MEASURE; POPULATION PARAMETERS; LATE QUATERNARY; HYBRID
ZONES; ICE AGES; PHYLOGEOGRAPHY; CONSEQUENCES
AB We studied the influence of glacial oscillations on the genetic structure of seven species of white-headed gull that breed at high latitudes (Larus argentatus, L. canus, L. glaucescens, L. glaucoides, L. hyperboreus, L. schistisagus, and L. thayeri). We evaluated localities hypothesized as ice-free areas or glacial refugia in other Arctic vertebrates using molecular data from 11 microsatellite loci, mitochondrial DNA (mtDNA) control region, and six nuclear introns for 32 populations across the Holarctic. Moderate levels of genetic structure were observed for microsatellites (F-ST = 0.129), introns (Phi(ST) = 0.185), and mtDNA control region (Phi(ST) = 0.461), with among-group variation maximized when populations were grouped based on subspecific classification. Two haplotype and at least two allele groups were observed across all loci. However, no haplotype/allele group was composed solely of individuals of a single species, a pattern consistent with recent divergence. Furthermore, northernmost populations were not well differentiated and among-group variation was maximized when L. argentatus and L. hyberboreus populations were grouped by locality rather than species, indicating recent hybridization. Four populations are located in putative Pleistocene glacial refugia and had larger tau estimates than the other 28 populations. However, we were unable to substantiate these putative refugia using coalescent theory, as all populations had genetic signatures of stability based on mtDNA. The extent of haplotype and allele sharing among Arctic white-headed gull species is noteworthy. Studies of other Arctic taxa have generally revealed species-specific clusters as well as genetic structure within species, usually correlated with geography. Aspects of white-headed gull behavioral biology, such as colonization ability and propensity to hybridize, as well as their recent evolutionary history, have likely played a large role in the limited genetic structure observed.
C1 [Sonsthagen, Sarah A.; Dove, Carla J.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Dept Vertebrate Zool, Washington, DC 20013 USA.
[Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20560 USA.
[Bell, Douglas A.] Calif Acad Sci, Dept Ornithol & Mammol, San Francisco, CA 94118 USA.
RP Sonsthagen, SA (reprint author), US Geol Survey, Alaska Sci Ctr, Anchorage, AK 99508 USA.
EM ssonsthagen@usgs.gov
FU Federal Aviation Administration (FAA); Laboratories of Analytical
Biology; Division of Birds, National Museum of Natural History,
Smithsonian Institution
FX Funding was provided by the Federal Aviation Administration (FAA) and
the Laboratories of Analytical Biology and Division of Birds, National
Museum of Natural History, Smithsonian Institution. We thank the
following for their significant contributions of tissues for this work:
N. Rice, Academy of Natural Sciences of Philadelphia; P. Sweet, American
Museum of Natural History; R. Zink and M. Westberg, Bell Museum of
Natural History; S. Birks, Burke Museum of Natural History and Culture;
D. Boertmann, National Environmental Research Group, Denmark; D.
Willard, Field Museum of Natural History; R. Brumfield and D. Dittmann,
Louisiana State University Museum of Natural Science; K. Garrett,
Natural History Museum of Los Angeles County; J. Dean, National Museum
of Natural History; J. Hudon, Royal Alberta Museum; A. Baker and O.
Haddrath, Royal Ontario Museum; K. Winker and D. Gibson, University of
Alaska Museum; and R. Bowie and C. Cicero, University of California
Berkeley Museum of Vertebrate Zoology. We would also like to thank the
numerous individuals that helped facilitate field work for the various
museums; J. Hunt, Smithsonian Institution, who provided technical
laboratory support; C. Milensky and F. Dahlan, Smithsonian Institution,
for assistance with sample collection and preparation; and A. Driskell,
M. Heacker, and L. Weigt, Smithsonian Institution, K. Omland, University
of Maryland Baltimore County, and R. Wilson, University of Alaska
Fairbanks, for their guidance and advice throughout this project, as
well as two anonymous reviewers comments on earlier drafts of this
manuscript. Any use of trade, product, or firm names is for descriptive
purposes only and does not imply endorsement by the U. S. Government.
NR 72
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Z9 8
U1 3
U2 21
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD JUN
PY 2012
VL 2
IS 6
BP 1278
EP 1295
DI 10.1002/ece3.240
PG 18
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA 055WF
UT WOS:000312447900015
PM 22833800
ER
PT J
AU McKenzie, LA
Johnston, EL
Brooks, R
AF McKenzie, Louise A.
Johnston, Emma L.
Brooks, Robert
TI Using clones and copper to resolve the genetic architecture of metal
tolerance in a marine invader
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Bryozoan; contamination; factor analytical modeling; genetic
correlation; genetic variance and covariance; modular organism;
trade-off
ID DIFFERENTIAL TOLERANCE; PHENOTYPIC PLASTICITY; BIOLOGICAL INVASIONS;
RAPID EVOLUTION; BUGULA-NERITINA; HEAVY-METALS; POLLUTION; RESISTANCE;
INVERTEBRATE; ENVIRONMENT
AB The global spread of invasive species may be facilitated by adaptation to the practices that humans use to manage those species. For example, marine invertebrates that adapt to metal-based antifouling biocides on ship hulls may be more likely to be introduced to and establish in metal-polluted environments. We tested this idea by studying clonal variation in tolerance to, and ability to recover from, exposure to copper in a widespread invasive marine bryozoan, Watersipora subtorquata. We cloned colonies of this organism to independently test multiple environments in a genotype by environment design, and then created a genetic variance-covariance matrix. Genotypes were exposed to a gradient of copper concentrations and growth measured during exposure and after a recovery period. There was a significant genotype x environment interaction in growth during exposure and recovery. We found clonal variation in tolerance and ability to recover from exposure to copper, with growth during exposure apparently trading off against growth after exposure. A weak genetic correlation between growth during and after exposure further indicated that they are separate traits. Overall, the genetic variation within this population indicates that there is considerable potential for adaptation to copper, but this comes at a cost to growth in unpolluted environments.
C1 [McKenzie, Louise A.; Johnston, Emma L.; Brooks, Robert] Univ New S Wales, Evolut & Ecol Res Ctr, Sydney, NSW 2052, Australia.
RP McKenzie, LA (reprint author), Smithsonian Environm Res Ctr, Marine Invas Lab, POB 28, Edgewater, MD 21037 USA.
EM mckenziel@si.edu
RI Brooks, Robert/A-1251-2008; Johnston, Emma/B-7210-2009
OI Brooks, Robert/0000-0001-6926-0781; Johnston, Emma/0000-0002-2117-366X
FU Australian Government; Australian Research Council
FX Supported by the Australian Government and Australian Research Council
through research fellowships, postgraduate awards, and grants.
NR 62
TC 2
Z9 2
U1 1
U2 32
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD JUN
PY 2012
VL 2
IS 6
BP 1319
EP 1329
DI 10.1002/ece3.241
PG 11
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA 055WF
UT WOS:000312447900019
PM 22833804
ER
PT J
AU King, RS
Walker, CM
Whigham, DF
Baird, SJ
Back, JA
AF King, Ryan S.
Walker, Coowe M.
Whigham, Dennis F.
Baird, Steven J.
Back, Jeffrey A.
TI Catchment topography and wetland geomorphology drive macroinvertebrate
community structure and juvenile salmonid distributions in south-central
Alaska headwater streams
SO FRESHWATER SCIENCE
LA English
DT Article
DE Salmonidae; topographic wetness; peatlands; land cover; wetland
classification; landscape indicators
ID COHO SALMON; ENVIRONMENTAL-CONDITIONS; LAND-COVER; FOOD WEBS; PATTERNS;
SCALE; CONSERVATION; HABITAT; BIODIVERSITY; LANDSCAPE
AB Conservation and management of headwater streams amid rapid global change require an understanding of the spatial and environmental factors that drive species distributions and associated ecosystem processes. We used a hierarchical analytical framework to model effects of catchment-scale topography and wetland geomorphic classes on stream physical habitat, chemistry, and macroinvertebrate and fish communities in 30 headwater streams across the Kenai Lowlands, southcentral Alaska, USA. We identified 135 macroinvertebrate taxa, 122 of which were aquatic insects, of which 79 were dipterans. We collected only 6 species of fish, but juvenile coho salmon and Dolly Varden were collected in 17 and 25 of the 30 streams and reached densities >500 and 1300/km, respectively. Flow-weighted slope, an indicator of water residence time and gradient, was the best catchment-scale correlate of macroinvertebrate and fish community structure, and its effect was mediated by wetland geomorphic classes and numerous water chemistry, substrate composition, and channel geomorphology variables measured at the reach scale. Many macroinvertebrate taxa showed high fidelity to different levels of the topographic gradient, resulting in high beta diversity but relatively similar levels of alpha diversity across the gradient. Juvenile salmonids were segregated among streams by both species and age classes. Coho salmon fry and parr (, 10 cm total length [TL]) had significant unimodal distributions that peaked in streams with intermediate slopes and gravel substrate, whereas presmolts (>= 10 cm) were found only in lowest-sloping streams with mostly peat substrate and deep, slow channels. Large Dolly Varden (>= 8 cm) were found across the entire gradient but were most abundant in high-sloping catchments, whereas small Dolly Varden (<8 cm) followed a similar distribution but were absent from the lowest-gradient sites with low flow velocity, dissolved O-2, and gravel substrate. Predictive modeling indicated that all of the 547 km of headwater streams in the study area might serve as potential habitat for >= 1 species and age class of salmonids. Our study should assist in development of catchment management tools for identifying and prioritizing conservation efforts in the region and may serve as a framework for other studies concerning biodiversity and focal species conservation in headwater streams.
C1 [King, Ryan S.; Back, Jeffrey A.] Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst Res, Waco, TX 76798 USA.
[Walker, Coowe M.; Baird, Steven J.] Kachemak Bay Res Reserve, Homer, AK 99603 USA.
[Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP King, RS (reprint author), Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst Res, 1 Bear Pl 97388, Waco, TX 76798 USA.
EM ryan_s_king@baylor.edu; coowe.walker@alaska.gov; whighamd@si.edu;
steve.baird@alaska.gov; jeff_back@baylor.edu
OI Whigham, Dennis/0000-0003-1488-820X
FU US Environmental Protection Agency through the Wetland Protection
Development Grant program [CD-96011801-0]
FX This project was funded by a grant from US Environmental Protection
Agency Region 10 through the Wetland Protection Development Grant
program, contract # CD-96011801-0, and significant cost-sharing from
Baylor University and the Kachemak Bay Research Reserve (KBRR). Staff of
KBRR (Amy Alderfer, Kim Donohue, Conrad Field) and several volunteers
(Jennifer Brewer, Shan Burson, Patrick Dougherty, Dwayne Evans, Rachel
Hovel, Megan Murphy, Caitlin Schott, Simeon Smith, Scott Thompson)
assisted with various parts of the project. We thank the Ninilchik
Tribal Association and private landowners for providing access to
sampling sites, Angela Doroff and Terry Thompson for providing office
space and resources at KBRR to RSK that facilitated completion of this
manuscript, and Becky Shaftel for providing helpful comments on an
earlier version on this manuscript. We especially thank Phil North for
his encouragement, support, and efforts to make the project a reality.
Although this work was funded, in part, by the US Environmental
Protection Agency, no official endorsement should be inferred.
NR 76
TC 7
Z9 7
U1 5
U2 51
PU SOC FRESWATER SCIENCE
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA
SN 2161-9565
J9 FRESHW SCI
JI Freshw. Sci.
PD JUN
PY 2012
VL 31
IS 2
BP 341
EP 364
DI 10.1899/11-109.1
PG 24
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 021SD
UT WOS:000309904800006
ER
PT J
AU Bellemain, E
Gaggiotti, OE
Fahey, A
Bermingham, E
Ricklefs, RE
AF Bellemain, Eva
Gaggiotti, Oscar E.
Fahey, Anna
Bermingham, Eldredge
Ricklefs, Robert E.
TI Demographic history and genetic diversity in West Indian Coereba
flaveola populations
SO GENETICA
LA English
DT Article
DE Coereba flaveola; Demography; Genetic diversity; Migration; Caribbean;
Nuclear sequences; Mitochondrial sequences
ID DNA POLYMORPHISM; INFERENCE; NUCLEAR; BIOGEOGRAPHY; EXPRESSION;
COALESCENT; LIKELIHOOD; BIRDS
AB The bananaquit (Coereba flaveola) has been well studied throughout the Caribbean region from a phylogenetic perspective. However, data concerning the population genetics and long-term demography of this bird species are lacking. In this study, we focused on three populations within the Lesser Antilles and one on Puerto Rico and assessed genetic and demographic processes, using five nuclear and two mitochondrial markers. We found that genetic diversity of bananaquits on Puerto Rico exceeds that on the smaller islands (Dominica, Guadeloupe and Grenada); this might reflect either successive founder events from Puerto Rico to Grenada, or more rapid drift in smaller populations subsequent to colonization. Population growth rate estimates showed no evidence of rapid expansion and migration was indicated only between populations from the closest islands of Dominica and Guadeloupe. Overall, our results suggest that a "demographic fission" model, considering only mutation and drift, but without migration, can be applied to these bananaquit populations in the West Indies.
C1 [Bellemain, Eva] Spygen, Savoie Technolac, F-73375 Le Bourget Du Lac, France.
[Bellemain, Eva; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama.
[Gaggiotti, Oscar E.] Univ Grenoble 1, CNRS, UMR 5553, Lab Ecol Alpine, F-38041 Grenoble 9, France.
[Fahey, Anna] Purdue Univ, Dept Forestry & Nat Resources, W Lafayette, IN 47907 USA.
[Ricklefs, Robert E.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA.
RP Bellemain, E (reprint author), Spygen, Savoie Technolac, 12 Allee Lac Garde,Batiment House Boat 7,BP 274, F-73375 Le Bourget Du Lac, France.
EM evabellemain@gmail.com
RI Gaggiotti, Oscar/G-2459-2010
OI Gaggiotti, Oscar/0000-0003-1827-1493
FU Smithsonian Institution James Bond Restricted Endowment; National
Geographic Society; National Science Foundation; Smithsonian Institution
FX This work was conducted at the Smithsonian Tropical Research Institute,
Panama and supported by the Smithsonian Institution James Bond
Restricted Endowment. Research by E. Bermingham and RER on West Indian
birds has been supported by the National Geographic Society, the
National Science Foundation, and the Smithsonian Institution. We are
grateful to L. Garcia, M. Gonzalez and C. Vergara for technical support
in the laboratory. We also thank two anonymous reviewers for their
valuable comments and their constructive suggestions to the manuscript.
NR 32
TC 0
Z9 0
U1 1
U2 17
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0016-6707
J9 GENETICA
JI Genetica
PD JUN
PY 2012
VL 140
IS 4-6
BP 137
EP 148
DI 10.1007/s10709-012-9665-6
PG 12
WC Genetics & Heredity
SC Genetics & Heredity
GA 008PF
UT WOS:000308968300004
PM 22855326
ER
PT J
AU Loss, SR
AF Loss, Scott R.
TI Nesting Density of Hermit Thrushes in a Remnant Invasive Earthworm-free
Portion of a Wisconsin Hardwood Forest
SO WILSON JOURNAL OF ORNITHOLOGY
LA English
DT Article
ID COMMUNITIES; PREDATION; SUCCESS
AB I observed an exceptionally high density of Hermit Thrush (Catharus guttatus) nests (3.1 nests/ha) over two breeding seasons in an isolated 1.3-ha portion of an earthworm-free study site in the Chequamegon-Nicolet National Forest, Wisconsin. This density was much greater than the 0.1 to 0.6 nests/ha observed over the rest of the study area and exceeds by an order of magnitude most previously reported estimates for this species. The mean distance among Hermit Thrush nests in earthworm-free sites (215 m; 95% CI = 180-250 m) was lower than in invaded sites (250 m; 95% CI = 236-264 m); this difference was not statistically significant. Nest density did not differ significantly between categories. An abundance of suitable nest sites in a favored nesting substrate (clubmoss; Lycopodium spp.) could have contributed to the exceptionally high density of Hermit Thrush nests observed. High Hermit Thrush nest densities may occur in association with forest floor conditions that are characteristic of earthworm-free areas. Received 3 August 2011. Accepted 16 January 2012.
C1 [Loss, Scott R.] Univ Minnesota, Conservat Biol Grad Program, St Paul, MN 55108 USA.
RP Loss, SR (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA.
EM LossS@si.edu
RI Loss, Scott/B-1504-2014
FU American Museum of Natural History; Bell Museum of Natural History;
Dayton-Wilkie Foundation; Explorer's Club; Minnesota Ornithologists'
Union; Wisconsin Society for Ornithology; University of Minnesota;
National Science Foundation IGERT [NSF DGE-0653827]
FX Field research was funded by the American Museum of Natural History,
Bell Museum of Natural History, Dayton-Wilkie Foundation, Explorer's
Club, Minnesota Ornithologists' Union, and Wisconsin Society for
Ornithology. SRL was supported by a University of Minnesota Graduate
School Fellowship and a National Science Foundation IGERT grant: Risk
Analysis for Introduced Species and Genotypes (NSF DGE-0653827). I thank
C. C. Hakseth, L. E. Lambert, J. C. Mulligan, M. W. Sharrow, Tammy
Johns, H. M. Streby, S. M. Peterson, B. M. Breen, C.-M. Hung, and S. S.
Loss for field assistance. I also thank R. B. Blair, L. E. Frelich, D.
E. Andersen, and P. V. Bolstad, for guidance. B. M. Breen, H. M. Streby,
and K. S. G. Sundar for comments that improved the manuscript, and the
Cable Natural History Museum for housing and office support. Fieldwork
was conducted with appropriate permits and approval by the University of
Minnesota Institutional Animal Care and Use Committee (protocol
0904A63062).
NR 20
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Z9 3
U1 0
U2 5
PU WILSON ORNITHOLOGICAL SOC
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA
SN 1559-4491
J9 WILSON J ORNITHOL
JI Wilson J. Ornithol.
PD JUN
PY 2012
VL 124
IS 2
BP 375
EP 379
PG 5
WC Ornithology
SC Zoology
GA 005YO
UT WOS:000308786200023
ER
PT J
AU Li, X
Brinckerhoff, WB
Managadze, GG
Pugel, DE
Corrigan, CM
Doty, JH
AF Li, X.
Brinckerhoff, W. B.
Managadze, G. G.
Pugel, D. E.
Corrigan, C. M.
Doty, J. H.
TI Laser ablation mass spectrometer (LAMS) as a standoff analyzer in space
missions for airless bodies
SO INTERNATIONAL JOURNAL OF MASS SPECTROMETRY
LA English
DT Article
DE Laser ablation mass spectrometer (LAMS); Time-of-flight; Standoff
analyzer
ID ION
AB A laser ablation mass spectrometer (LAMS) based on a time-of-flight (TOF) analyzer with adjustable drift length is proposed as a standoff elemental composition sensor for space missions to airless bodies. It is found that the use of a retarding potential analyzer in combination with a two-stage reflectron enables LAMS to be operated at variable drift length. For field-free drift lengths between 33 cm and 100 cm, at least unit mass resolution can be maintained solely by adjustment of internal voltages, and without resorting to drastic reductions in sensitivity. Therefore. LAMS should be able to be mounted on a platform or robotic arm and analyze samples at standoff distances of up to several tens of cm, permitting high operational flexibility and wide area coverage of heterogeneous regolith on airless bodies. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Li, X.] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA.
[Brinckerhoff, W. B.; Pugel, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Managadze, G. G.] Space Res Inst IKI, Moscow, Russia.
[Corrigan, C. M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
[Doty, J. H.] Rice Univ, Houston, TX USA.
RP Li, X (reprint author), Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
EM xiang.li@nasa.gov
RI Li, Xiang/F-4539-2012; Brinckerhoff, William/F-3453-2012
OI Brinckerhoff, William/0000-0001-5121-2634
FU NASA Planetary Instrument Definition and Development (PIDDP) program;
Goddard Internal Research and Development program
FX This work was supported by the NASA Planetary Instrument Definition and
Development (PIDDP) program and by the Goddard Internal Research and
Development program.
NR 17
TC 4
Z9 4
U1 0
U2 15
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1387-3806
J9 INT J MASS SPECTROM
JI Int. J. Mass Spectrom.
PD JUN 1
PY 2012
VL 323
BP 63
EP 67
DI 10.1016/j.ijms.2012.06.020
PG 5
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 005RU
UT WOS:000308768400011
ER
PT J
AU Nicholson, C
AF Nicholson, Catherine
TI FINDING the STONES
SO PROLOGUE-QUARTERLY OF THE NATIONAL ARCHIVES AND RECORDS ADMINISTRATION
LA English
DT Article
C1 [Nicholson, Catherine] NARA Conservat Labs, Nara, Japan.
[Nicholson, Catherine] Smithsonian Inst, Natl Gallery Art, Boston Publ Lib, Washington, DC 20560 USA.
RP Nicholson, C (reprint author), NARA Conservat Labs, Nara, Japan.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU NATL ARCHIVES RECORDS ADMINISTRATION
PI WASHINGTON
PA TRUST FUND BOARD, WASHINGTON, DC 20408 USA
SN 0033-1031
J9 PROLOGUE
JI Prologue
PD SUM
PY 2012
VL 44
IS 2
BP 22
EP 29
PG 8
WC History
SC History
GA 990AU
UT WOS:000307604200004
ER
PT J
AU Aitken-Palmer, C
Hou, R
Burrell, C
Zhang, ZH
Wang, CD
Spindler, R
Wildt, DE
Ottinger, MA
Howard, J
AF Aitken-Palmer, Copper
Hou, Rong
Burrell, Caitlin
Zhang, Zhihe
Wang, Chengdong
Spindler, Rebecca
Wildt, David E.
Ottinger, Mary Ann
Howard, JoGayle
TI Protracted Reproductive Seasonality in the Male Giant Panda (Ailuropoda
melanoleuca) Reflected by Patterns in Androgen Profiles, Ejaculate
Characteristics, and Selected Behaviors
SO BIOLOGY OF REPRODUCTION
LA English
DT Article
DE Ailuropoda melanoleuca; giant panda; male sexual function; seasonal
reproduction; seasonality; sperm; steroid hormones; testis
ID URSUS-THIBETANUS-JAPONICUS; JAPANESE BLACK BEAR; CHEMICAL COMMUNICATION;
STEROIDOGENIC ENZYMES; IMMUNOLOCALIZATION; SPERMATOGENESIS;
TESTOSTERONE; AMERICANUS; MARITIMUS; HABITAT
AB The female giant panda (Ailuropoda melanoleuca) experiences a brief (24-72 h) seasonal estrus, occurring once annually in spring (February-May). Our aim was to determine the existence and temporal profile of reproductive seasonality in the male of this species. The study was facilitated by 3 yr of access to eight giant panda males living in a large breeding center in China. Seasonal periods for the male were defined on the basis of female reproductive activity as prebreeding, breeding (early, peak, late), and nonbreeding seasons. Testes size, fecal androgen excretion, ejaculated sperm density, and frequency of reproductive behaviors (i.e., locomotion, scent marking, vocalizations) increased (P < 0.05) from the prebreeding period (October 1-January 31) to the early breeding season (February 1-March 21). Testes volume and sperm concentration were maximal from March 22 through April 15, a period coinciding with maximal female breeding activity. The occurrence of male reproductive behaviors and fecal androgen concentrations began declining during peak breeding and continued from April 16 through May 31 (late breeding period), returning to nadir throughout the nonbreeding interval (June 1-September 30). Reproductive quiescence throughout the latter period was associated with basal testes size/volume and aspermic ejaculates. Our results reveal that testes morphometry, fecal androgen excretion, seminal quality, and certain behaviors integrated together clearly demonstrate reproductive seasonality in the male giant panda. The coordinated increases in testes size, androgen production, sperm density, and sexual behaviors occur over a protracted interval, likely to prepare for and then accommodate a brief, unpredictable female estrus.
C1 [Aitken-Palmer, Copper] Natl Zool Pk, Dept Conservat Med, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA.
[Hou, Rong; Zhang, Zhihe; Wang, Chengdong] Chengdu Res Base Giant Panda Breeding, Chengdu, Peoples R China.
[Spindler, Rebecca] Toronto Zoo, Toronto, ON, Canada.
[Ottinger, Mary Ann] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA.
RP Aitken-Palmer, C (reprint author), Natl Zool Pk, Dept Conservat Med, Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA.
EM aitkenc@si.edu
FU Morris Animal Foundation; Friends of the National Zoo; University of
Maryland Department of Animal and Avian Sciences; Chengdu Research Base
of Giant Panda Breeding
FX Supported by the Morris Animal Foundation, Friends of the National Zoo,
University of Maryland Department of Animal and Avian Sciences, and the
Chengdu Research Base of Giant Panda Breeding. International travel was
supported by United Airlines. Research was conducted in partial
fulfillment of Ph.D. requirements for C.A.P. at the University of
Maryland.
NR 38
TC 3
Z9 3
U1 2
U2 39
PU SOC STUDY REPRODUCTION
PI MADISON
PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA
SN 0006-3363
J9 BIOL REPROD
JI Biol. Reprod.
PD JUN
PY 2012
VL 86
IS 6
AR 195
DI 10.1095/biolreprod.112.099044
PG 10
WC Reproductive Biology
SC Reproductive Biology
GA 975YP
UT WOS:000306548000026
PM 22492970
ER
PT J
AU Berube, MD
Dunbar, SG
Rutzler, K
Hayes, WK
AF Berube, Melissa D.
Dunbar, Stephen G.
Ruetzler, Klaus
Hayes, William K.
TI Home Range and Foraging Ecology of Juvenile Hawksbill Sea Turtles
(Eretmochelys imbricata) on Inshore Reefs of Honduras
SO CHELONIAN CONSERVATION AND BIOLOGY
LA English
DT Article
DE fixed kernel density; hawksbill; minimum convex polygon; radio
telemetry; sponges
ID KEMPS RIDLEY TURTLES; GULF-OF-CALIFORNIA; CHELONIA-MYDAS; GREEN TURTLES;
HABITAT USE; CARETTA-CARETTA; COASTAL WATERS; MARINE TURTLES;
COSTA-RICA; CORAL-REEF
AB Despite the recognition of the historical importance of hawksbills in the Caribbean region of Honduras, prior sea turtle research in the area has been extremely limited, and little is known about hawksbill turtle (Eretmochelys imbricata) ecology from this region. We tracked 6 juvenile hawksbills (28.7-35.6 cm, straight carapace length ISM) with radiotelemetry off the coast of Roatan in the Bay Islands of Honduras, conducted habitat assessments at 14 sites, and examined the diet of 5 juvenile hawksbills (19.8-49.7 cm, SCL) using gastric (n = 4) and fecal (n = 1) samples. Home ranges of all 6 turtles were small, with 100% minimum convex polygons from 0.15 to 0.55 km(2), and a 50% fixed kernel density for all animals pooled of 5.46 km(2). The habitat assessment showed that common prey items in hawksbill diets were abundant in areas where juvenile hawksbills were resident and in nonresident areas, with sponges (Chondrilla sp., Geodia sp.).) and octocorals (Pseudopterogorgia sp.) being most prevalent. We found sponge to be the primary component in the diet, comprising 59% of total ingesta. The most prevalent sponge species an the diet samples were Melophlus ruber and Chondrilla caribensis. Although C. caribensis is a common constituent of hawksbill diets, the current study provides the first report of M. ruber as a component of hawksbill diets. Home ranges of juvenile hawksbills in the Port Royal region of Roatan are small (< 1 km(2)), and their primary dietary component is the sponge M. ruber. Conservation efforts on Roatan should be established in the Port Royal region, and should include protection of dietary items and turtles.
C1 [Berube, Melissa D.; Dunbar, Stephen G.; Hayes, William K.] Loma Linda Univ, Dept Earth & Biol Sci, Loma Linda, CA 92350 USA.
[Dunbar, Stephen G.] Outreach & Res Inc, Protect Turtle Ecol Ctr Training, Colton, CA 92324 USA.
[Berube, Melissa D.; Dunbar, Stephen G.] Turtle Awareness & Protect Studies, Roatan, Honduras.
[Ruetzler, Klaus] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA.
RP Berube, MD (reprint author), Loma Linda Univ, Dept Earth & Biol Sci, Griggs Hall, Loma Linda, CA 92350 USA.
EM mberube@llu.edu; sdunbar@llu.edu; ruetzler@si.edu; whayes@llu.edu
RI Hayes, William/L-1284-2013
OI Hayes, William/0000-0002-0903-0519
FU Protective Turtle Ecology Center for Training, Outreach and Research,
Inc.; Reef House Resort; Department of Earth and Biological Sciences at
Loma Linda University; State of the World's Sea Turtles
FX Logistical and financial support were provided by the Protective Turtle
Ecology Center for Training, Outreach and Research, Inc; the owners of
the Reef House Resort; the Department of Earth and Biological Sciences
at Loma Linda University; and the State of the World's Sea Turtles. We
thank the Honduras Natural Resources and Environment Secretariat, and
Direccion General de Pesca y Acuicultura for providing research permits
for this work. Thanks to Dr Rob van Soest for providing information
about Melophlus ruber. We also thank Dr Art Rodgers and Dr Jeff Seminal
for their input on home range analysis, Dr Anne Meylan for her insights
into gastric lavages and hawksbill diets, and Aaron Corbit for his help
with compositional analysis. This work was carried out under permit
DGPA/5428/2007 from the Secretariat of Agriculture and Ranching, and is
in compliance with Loma Linda University IACUC protocol 86004. This is
contribution number 2 of the Protective Turtle Ecology Center for
Training, Outreach and Research, Inc.
NR 74
TC 4
Z9 4
U1 6
U2 62
PU CHELONIAN RESEARCH FOUNDATION
PI LUNENBURG
PA 168 GOODRICH ST., LUNENBURG, MA USA
SN 1071-8443
EI 1943-3956
J9 CHELONIAN CONSERV BI
JI Chelonian Conserv. Biol.
PD JUN
PY 2012
VL 11
IS 1
BP 33
EP 43
PG 11
WC Zoology
SC Zoology
GA 975HF
UT WOS:000306500600004
ER
PT J
AU Machlis, G
Frankovich, TA
Alcolado, PM
Garcia-Machado, E
Hernandez-Zanuy, AC
Hueter, RE
Knowlton, N
Perera, E
Tunnell, JW
AF Machlis, Gary
Frankovich, Thomas A.
Alcolado, Pedro M.
Garcia-Machado, Erik
Caridad Hernandez-Zanuy, Aida
Hueter, Robert E.
Knowlton, Nancy
Perera, Erick
Tunnell, John W., Jr.
TI OCEAN POLICY US-Cuba Scientific Collaboration Emerging Issues and
Opportunities in Marine and Related Environmental Sciences
SO OCEANOGRAPHY
LA English
DT Editorial Material
ID FISH
C1 [Machlis, Gary] Univ Idaho, Dept Forest Resources, Moscow, ID 83843 USA.
[Frankovich, Thomas A.] Florida Int Univ, SE Environm Res Ctr, Miami, FL 33199 USA.
[Alcolado, Pedro M.; Caridad Hernandez-Zanuy, Aida] CYTED Iberoamer Network BIODIVMAR, Inst Oceanol, Havana, Cuba.
[Garcia-Machado, Erik; Perera, Erick] Univ Havana, Ctr Marine Res, Miramar, Cuba.
[Hueter, Robert E.] Mote Marine Lab, Directorate Marine Biol & Conservat, Sarasota, FL 34236 USA.
[Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Tunnell, John W., Jr.] Harte Res Inst Gulf Mexico Studies, Corpus Christi, TX USA.
[Tunnell, John W., Jr.] Texas A&M Univ Corpus Christi, Corpus Christi, TX USA.
RP Machlis, G (reprint author), Univ Idaho, Dept Forest Resources, Moscow, ID 83843 USA.
EM gmachlis@uidaho.edu
RI Perera, Erick/F-2917-2012
OI Perera, Erick/0000-0001-6108-1340
NR 18
TC 0
Z9 0
U1 1
U2 10
PU OCEANOGRAPHY SOC
PI ROCKVILLE
PA P.O. BOX 1931, ROCKVILLE, MD USA
SN 1042-8275
J9 OCEANOGRAPHY
JI Oceanography
PD JUN
PY 2012
VL 25
IS 2
BP 227
EP 231
PG 5
WC Oceanography
SC Oceanography
GA 970WD
UT WOS:000306162100029
ER
PT J
AU King, DI
Chandler, CC
Rappole, JH
Chandler, RB
Mehlman, DW
AF King, David I.
Chandler, Carlin C.
Rappole, John H.
Chandler, Richard B.
Mehlman, David W.
TI Establishing quantitative habitat targets for a 'Critically Endangered'
Neotropical migrant (Golden-cheeked Warbler Dendroica chrysoparia)
during the non-breeding season
SO BIRD CONSERVATION INTERNATIONAL
LA English
DT Article
ID HIERARCHICAL-MODELS; CONSERVATION; ABUNDANCE; ECOLOGY
AB The Golden-checked Warbler Dendroica chrysoparia is a federally endangered Neotropical migrant that inhabits montane pine-oak forests in Mexico and northern Central America during the non-breeding season. Although it is known that Golden-checked Warblers are closely associated with 'encino' oaks (evergreen or holm oak) such as Quercus sapotifolia, Q. eliptica and Q. elongata, which have shiny, narrow, elliptical, or oblong leaves, quantitative habitat targets are useful for effectively incorporating this information into conservation planning and forest management practices. We analysed data on wintering Golden-checked Warblers collected during the non-breeding season in Honduras from 1996 to 1998 to identify quantitative targets for habitat conditions for this species. Data on warbler abundance were collected using line transect surveys located in montane pine-oak forests in a stratified-random fashion. Habitat data were collected at five 0.04 ha plots on these same transects and the averaged values used as predictors of Golden-checked Warbler abundance. We found that Golden-checked Warblers were strongly associated with the basal area of encino oaks and density of 'roble' oaks, such as Q. segoviensis, Q. purulhana and Q. rugosa, which have large, lobed leaves. Density of Golden-checked Warblers peaked at approximate to 5.6 m(-2) ha(-1) basal area of encino and approximate to 7 roble oaks ha(-1). These values can be used to identify quantitative habitat targets that can be directly incorporated into forest management practices to ensure that these activities maintain habitat conditions necessary for their use by Golden-checked Warblers.
C1 [King, David I.] Univ Massachusetts, No Res Stn, USDA, US Forest Serv, Amherst, MA 01003 USA.
[Chandler, Carlin C.; Chandler, Richard B.] Univ Massachusetts, Dept Nat Resources Conservat, Amherst, MA 01003 USA.
[Rappole, John H.] Conservat Res Ctr, Smithsonian Inst, Front Royal, VA 22630 USA.
[Mehlman, David W.] Nature Conservancy, Migratory Bird Program, Albuquerque, NM 87104 USA.
RP King, DI (reprint author), Univ Massachusetts, No Res Stn, USDA, US Forest Serv, 160 Holdsworth Way,202 Holdsworth Hall, Amherst, MA 01003 USA.
EM dking@fs.fed.us
RI Chandler, Richard/D-8831-2014; Chandler, Richard/F-9702-2016
FU USDA Forest Service International Program; The Nature Conservancy
Migratory Bird Program
FX We thank the USDA Forest Service International Program who funded this
work through a cooperative agreement with The Nature Conservancy
Migratory Bird Program. We also thank Edgard Herrera for his valuable
advice and support, Martha Moreno, Marvin Martinez, and Julio Merida for
their help with fieldwork 2006-2008, and Scott Schlossberg and Mitch
Hartley for his comments on an earlier draft of this manuscript.
NR 20
TC 0
Z9 0
U1 1
U2 29
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0959-2709
J9 BIRD CONSERV INT
JI Bird Conserv. Int.
PD JUN
PY 2012
VL 22
IS 2
BP 213
EP 221
DI 10.1017/S095927091100027X
PG 9
WC Ornithology
SC Zoology
GA 971MP
UT WOS:000306208300010
ER
PT J
AU Beck, AW
Welten, KC
McSween, HY
Viviano, CE
Caffee, MW
AF Beck, Andrew W.
Welten, Kees C.
McSween, Harry Y., Jr.
Viviano, Christina E.
Caffee, Marc W.
TI Petrologic and textural diversity among the PCA 02 howardite group, one
of the largest pieces of the Vestan surface
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID ASTEROID 4 VESTA; HED PARENT BODY; AMS STANDARDS; DIOGENITES;
CONSTRAINTS; METEORITES; ORIGIN; GEOCHEMISTRY; METAMORPHISM; EVOLUTION
AB Nine howardites and two diogenites were recovered from the Pecora Escarpment Icefield (PCA) in 2002. Cosmogenic radionuclide abundances indicate that the samples are paired and that they constituted an approximately 1 m (diameter) meteoroid prior to atmospheric entry. At about 1 m in diameter, the PCA 02 HED group represents one of the largest single pre-atmospheric pieces of the Vestan surface yet described. Mineral and textural variations were measured in six of the PCA 02 howardites to investigate meter-scale diversity of the Vestan surface. Mineral compositions span the range of known eucrite and diogenite compositions. Additional non-diogenitic groups of Mg- and Fe-rich olivine are observed, and are interpreted to have been formed by exogenic contamination and impact melting, respectively. These howardites contain olivine-rich impact melts that likely formed from dunite- and harzburgite-rich target rocks. Containing the first recognized olivine-rich HED impact melts, these samples provide meteoritic evidence that olivine-rich lithologies have been exposed on the surface of Vesta. Finally, we present a new method for mapping distributions of lithologies in howardites using 8 elemental X-ray maps. Proportions of diogenite and eucrite vary considerably among the PCA 02 howardites, suggesting they originated from a heterogeneous portion of the Vestan surface. While whole sample modes are dominated by diogenite, the finer grain size fractions are consistently more eucritic. This discrepancy has implications for near-infrared spectral observations of portions of Vestas surface that are similar to the PCA 02 howardites, as the finer grained eucritic material will disproportionately dominate the spectra.
C1 [Beck, Andrew W.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
[Welten, Kees C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Viviano, Christina E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[McSween, Harry Y., Jr.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[Caffee, Marc W.] Purdue Univ, PRIME Lab, W Lafayette, IN 47907 USA.
RP Beck, AW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, 10th & Constitut NW, Washington, DC 20560 USA.
EM becka@si.edu
RI Viviano-Beck, Christina/F-3942-2015; Beck, Andrew/J-7215-2015; Caffee,
Marc/K-7025-2015
OI Viviano-Beck, Christina/0000-0003-1601-2105; Beck,
Andrew/0000-0003-4455-2299; Caffee, Marc/0000-0002-6846-8967
FU NASA Cosmochemistry [NNG06GG36G]; UCLA Dawn Team
FX The authors thank the MWG and ANSMET for the collection and allocation
of meteorite samples. This work was partially supported by NASA
Cosmochemistry Grant NNG06GG36G and UCLA Dawn Team subcontract to HYM.
We thank D. Mittlefehldt and A. Patzer for their constructive comments.
We also thank MAPS AE A. Ruzicka and referees J.-A. Barrat and P.
Buchanan for their helpful reviews and editorial handling.
NR 59
TC 34
Z9 34
U1 1
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUN
PY 2012
VL 47
IS 6
BP 947
EP 969
DI 10.1111/j.1945-5100.2012.01360.x
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 971BR
UT WOS:000306177400001
ER
PT J
AU Olson, SL
AF Olson, Storrs L.
TI Notes on the appendicular myology of the Scarlet Finch Haematospiza
sipahi (Fringillidae: Carduelinae)
SO ORNITHOLOGICAL SCIENCE
LA English
DT Article
DE Carduelinae; Drepanidini; Fringillidae; Hematospiza sipahi; Myology;
Scarlet Finch
ID HAWAIIAN HONEYCREEPERS DREPANIDIDAE; APPENDAGE MYOLOGY
AB The appendicular myology of the Scarlet Finch Haematospiza sipahi was found to be primitive in all of the characters known to show variation within the subfamily Carduelinae (Fringillidae). It is the only species of cardueline known so far to exhibit this combination of myological characters, although taxon sampling is still inadequate. Haematospiza provides a reasonable model for the last common ancestor of the Hawaiian radiation of carduelines of the tribe Drepanidini.
C1 Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, Smithsonian Inst, Washington, DC 20013 USA.
RP Olson, SL (reprint author), Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, Smithsonian Inst, POB 30712,NHB MRC 116, Washington, DC 20013 USA.
EM olsons@si.edu
NR 8
TC 0
Z9 0
U1 1
U2 2
PU ORNITHOLOGICAL SOC JAPAN, UNIV TOKYO, SCH AGR
PI TOKYO
PA YAYOI 1-1-1, TOKYO, 113-8657, JAPAN
SN 1347-0558
J9 ORNITHOL SCI
JI Ornithol. Sci.
PD JUN
PY 2012
VL 11
IS 1
BP 57
EP 58
PG 2
WC Ornithology
SC Zoology
GA 970QH
UT WOS:000306146900007
ER
PT J
AU Bethermin, M
Le Floc'h, E
Ilbert, O
Conley, A
Lagache, G
Amblard, A
Arumugam, V
Aussel, H
Berta, S
Bock, J
Boselli, A
Buat, V
Casey, CM
Castro-Rodriguez, N
Cava, A
Clements, DL
Cooray, A
Dowell, CD
Eales, S
Farrah, D
Franceschini, A
Glenn, J
Griffin, M
Hatziminaoglou, E
Heinis, S
Ibar, E
Ivison, RJ
Kartaltepe, JS
Levenson, L
Magdis, G
Marchetti, L
Marsden, G
Nguyen, HT
O'Halloran, B
Oliver, SJ
Omont, A
Page, MJ
Panuzzo, P
Papageorgiou, A
Pearson, CP
Perez-Fournon, I
Pohlen, M
Rigopoulou, D
Roseboom, IG
Rowan-Robinson, M
Salvato, M
Schulz, B
Scott, D
Seymour, N
Shupe, DL
Smith, AJ
Symeonidis, M
Trichas, M
Tugwell, KE
Vaccari, M
Valtchanov, I
Vieira, JD
Viero, M
Wang, L
Xu, CK
Zemcov, M
AF Bethermin, M.
Le Floc'h, E.
Ilbert, O.
Conley, A.
Lagache, G.
Amblard, A.
Arumugam, V.
Aussel, H.
Berta, S.
Bock, J.
Boselli, A.
Buat, V.
Casey, C. M.
Castro-Rodriguez, N.
Cava, A.
Clements, D. L.
Cooray, A.
Dowell, C. D.
Eales, S.
Farrah, D.
Franceschini, A.
Glenn, J.
Griffin, M.
Hatziminaoglou, E.
Heinis, S.
Ibar, E.
Ivison, R. J.
Kartaltepe, J. S.
Levenson, L.
Magdis, G.
Marchetti, L.
Marsden, G.
Nguyen, H. T.
O'Halloran, B.
Oliver, S. J.
Omont, A.
Page, M. J.
Panuzzo, P.
Papageorgiou, A.
Pearson, C. P.
Perez-Fournon, I.
Pohlen, M.
Rigopoulou, D.
Roseboom, I. G.
Rowan-Robinson, M.
Salvato, M.
Schulz, B.
Scott, D.
Seymour, N.
Shupe, D. L.
Smith, A. J.
Symeonidis, M.
Trichas, M.
Tugwell, K. E.
Vaccari, M.
Valtchanov, I.
Vieira, J. D.
Viero, M.
Wang, L.
Xu, C. K.
Zemcov, M.
TI HerMES: deep number counts at 250 mu m, 350 mu m and 500 mu m in the
COSMOS and GOODS-N fields and the build-up of the cosmic infrared
background
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmology: observations; diffuse radiation; galaxies: statistics;
galaxies: photometry; submillimeter: galaxies; submillimeter: diffuse
background
ID HERSCHEL-SPIRE INSTRUMENT; LESS-THAN 2; STAR-FORMATION; LUMINOSITY
FUNCTION; DUSTY GALAXIES; SCUBA GALAXIES; SUBMILLIMETER; EVOLUTION;
SPITZER; BLAST
AB Aims. The Spectral and Photometric Imaging REceiver (SPIRE) onboard the Herschel space telescope has provided confusion limited maps of deep fields at 250 mu m, 350 mu m, and 500 mu m, as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). Unfortunately, due to confusion, only a small fraction of the cosmic infrared background (CIB) can be resolved into individually-detected sources. Our goal is to produce deep galaxy number counts and redshift distributions below the confusion limit at SPIRE wavelengths (similar to 20 mJy), which we then use to place strong constraints on the origins of the cosmic infrared background and on models of galaxy evolution.
Methods. We individually extracted the bright SPIRE sources (>20 mJy) in the COSMOS field with a method using the positions, the flux densities, and the redshifts of the 24 mu m sources as a prior, and derived the number counts and redshift distributions of the bright SPIRE sources. For fainter SPIRE sources (<20 mJy), we reconstructed the number counts and the redshift distribution below the confusion limit using the deep 24 mu m catalogs associated with photometric redshift and information provided by the stacking of these sources into the deep SPIRE maps of the GOODS-N and COSMOS fields. Finally, by integrating all these counts, we studied the contribution of the galaxies to the CIB as a function of their flux density and redshift.
Results. Through stacking, we managed to reconstruct the source counts per redshift slice down to similar to 2 mJy in the three SPIRE bands, which lies about a factor 10 below the 5s confusion limit. Our measurements place tight constraints on source population models. None of the pre-existing models are able to reproduce our results at better than 3-sigma. Finally, we extrapolate our counts to zero flux density in order to derive an estimate of the total contribution of galaxies to the CIB, finding 10.1 (+2.6)(2.3) nW m(-2) sr(-1), 6.5 (+1.7)(1.6) nW m(-2) sr(-1), and 2.8 (+0.9)(0.8) nW m(-2) sr(-1) at 250 mu m, 350 mu m, and 500 mu m, respectively. These values agree well with FIRAS absolute measurements, suggesting our number counts and their extrapolation are sufficient to explain the CIB. We find that half of the CIB is emitted at z = 1.04, 1.20, and 1.25, respectively. Finally, combining our results with other works, we estimate the energy budget contained in the CIB between 8 mu m and 1000 mu m: 26(-3)(+7) nW m(-2) sr(-1).
C1 [Bethermin, M.; Le Floc'h, E.; Aussel, H.; Magdis, G.; Panuzzo, P.] Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, CEA DSM Irfu,CNRS, F-91191 Gif Sur Yvette, France.
[Bethermin, M.; Lagache, G.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Bethermin, M.; Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France.
[Ilbert, O.; Boselli, A.; Buat, V.; Heinis, S.] Univ Aix Marseille, Lab Astrophys Marseille, OAMP, CNRS, F-13388 Marseille 13, France.
[Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Arumugam, V.; Ivison, R. J.; Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Berta, S.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
[Bock, J.; Cooray, A.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Vieira, J. D.; Viero, M.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA.
[Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Casey, C. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Castro-Rodriguez, N.; Perez-Fournon, I.] IAC, Tenerife 38200, Spain.
[Castro-Rodriguez, N.; Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.
[Cava, A.] Univ Complutense Madrid, Fac CC, Dept Astrofis, E-28040 Madrid, Spain.
[Clements, D. L.; O'Halloran, B.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Eales, S.; Griffin, M.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Farrah, D.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Franceschini, A.; Marchetti, L.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Glenn, J.] Univ Colorado, CASA UCB 389, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Kartaltepe, J. S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Marsden, G.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Omont, A.] UPMC Univ Paris 6, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Page, M. J.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada.
[Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Salvato, M.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Salvato, M.] Excellence Cluster, D-85748 Garching, Germany.
[Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Ctr Infrared Proc & Anal, JPL, Pasadena, CA 91125 USA.
[Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain.
[Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa.
RP Bethermin, M (reprint author), Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, CEA DSM Irfu,CNRS, Pt Courrier 131, F-91191 Gif Sur Yvette, France.
EM matthieu.bethermin@cea.fr
RI Magdis, Georgios/C-7295-2014; amblard, alexandre/L-7694-2014; Ivison,
R./G-4450-2011; Vaccari, Mattia/R-3431-2016;
OI Magdis, Georgios/0000-0002-4872-2294; amblard,
alexandre/0000-0002-2212-5395; Ivison, R./0000-0001-5118-1313; Vaccari,
Mattia/0000-0002-6748-0577; Scott, Douglas/0000-0002-6878-9840;
Marchetti, Lucia/0000-0003-3948-7621; Seymour,
Nicholas/0000-0003-3506-5536; Bethermin, Matthieu/0000-0002-3915-2015
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA
(USA); ERC-StG [UPGAL 240039]; Science and Technology Facilities Council
[ST/F002858/1, ST/I000976/1]; Italian Space Agency (ASI Herschel Science
Contract) [I/005/07/0]
FX We thank the COSMOS and GOODS teams for releasing publicly their data.
Thanks to Georges Helou for suggesting that the distribution of the
colors is more likely log-normal than normal. MB thank Herve Dole for
his advices about stacking, and Elizabeth Fernandez for providing a mock
catalog from the Bethermin et al. model. SPIRE has been developed by a
consortium of institutes led by Cardiff Univ. (UK) and including Univ.
Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua
(Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College
London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC,
Univ. Colorado (USA). This development has been supported by national
funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France);
ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA
(USA). MB acknowledge financial support from ERC-StG grant UPGAL 240039.
SJO acknowledge support from the Science and Technology Facilities
Council [grant number ST/F002858/1] and [grant number ST/I000976/1]. M.
V. was supported by the Italian Space Agency (ASI Herschel Science
Contract I/005/07/0). The data presented in this paper will be released
through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES).
NR 73
TC 72
Z9 72
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2012
VL 542
AR A58
DI 10.1051/0004-6361/201118698
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965YI
UT WOS:000305803300063
ER
PT J
AU Nooraee, N
Callanan, PJ
Barnard, R
Garcia, MR
Murray, SS
Moss, A
AF Nooraee, N.
Callanan, P. J.
Barnard, R.
Garcia, M. R.
Murray, S. S.
Moss, A.
TI Chandra, Swift, and HST studies of the CXOM31 J004253.1+411422 Very
bright X-ray transient in M31
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: general; X-rays: binaries; galaxies: groups: individual: M 31
ID LIGHT CURVES; BINARIES; NOVAE; DISC
AB Context. A very bright transient X-ray source, CXOM31 J004253.1+411422, was found by Chandra/HRC in the M31 bulge. We present Chandra, Swift, and Hubble Space Telescope (HST) observations of this source.
Aims. Since this source is the brightest known X-ray transient in M31, we want to study its nature with Chandra and Swift. Comparing the results of Galactic transients and M31 transients can give a better understanding of the nature of extragalactic binaries.
Methods. We fitted disk black body and power law models to X-ray data from Chandra and Swift. Follow-up HST/ACS imaging during and after the outburst revealed a transient optical counterpart.
Results. Our HST observations show an optical counterpart with optical magnitude B = 23.91 +/- 0.08. Using the empirical relations between X-ray luminosity and absolute visual magnitude, we estimate the orbital period of the system is about similar to 15 h.
Conclusions. Our optical identification of the brightest X-ray transient so far discovered in M31 suggests an orbital period of about 15 h. The decay light curve is consistent with previous models of X-ray novae outbursts.
C1 [Nooraee, N.] Dublin Inst Adv Studies, Dublin 2, Ireland.
[Nooraee, N.; Callanan, P. J.; Moss, A.] Natl Univ Ireland Univ Coll Cork, Cork, Ireland.
[Barnard, R.; Garcia, M. R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Murray, S. S.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
RP Nooraee, N (reprint author), Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland.
EM nnooraee@cp.dias.ie
NR 22
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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
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2012
VL 542
AR A120
DI 10.1051/0004-6361/201118109
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965YI
UT WOS:000305803300026
ER
PT J
AU Oppermann, N
Junklewitz, H
Robbers, G
Bell, MR
Ensslin, TA
Bonafede, A
Braun, R
Brown, JC
Clarke, TE
Feain, IJ
Gaensler, BM
Hammond, A
Harvey-Smith, L
Heald, G
Johnston-Hollitt, M
Klein, U
Kronberg, PP
Mao, SA
McClure-Griffiths, NM
O'Sullivan, SP
Pratley, L
Robishaw, T
Roy, S
Schnitzeler, DHFM
Sotomayor-Beltran, C
Stevens, J
Stil, JM
Sunstrum, C
Tanna, A
Taylor, AR
Van Eck, CL
AF Oppermann, N.
Junklewitz, H.
Robbers, G.
Bell, M. R.
Ensslin, T. A.
Bonafede, A.
Braun, R.
Brown, J. C.
Clarke, T. E.
Feain, I. J.
Gaensler, B. M.
Hammond, A.
Harvey-Smith, L.
Heald, G.
Johnston-Hollitt, M.
Klein, U.
Kronberg, P. P.
Mao, S. A.
McClure-Griffiths, N. M.
O'Sullivan, S. P.
Pratley, L.
Robishaw, T.
Roy, S.
Schnitzeler, D. H. F. M.
Sotomayor-Beltran, C.
Stevens, J.
Stil, J. M.
Sunstrum, C.
Tanna, A.
Taylor, A. R.
Van Eck, C. L.
TI An improved map of the Galactic Faraday sky
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: magnetic fields; Galaxy: structure; ISM: magnetic fields;
radio continuum: ISM; methods: data analysis; techniques: polarimetric
ID EXTRAGALACTIC RADIO-SOURCES; SCALE MAGNETIC-FIELD; WESTERBORK SINGS
SURVEY; ROTATION MEASURE SKY; MILKY-WAY; PLANE SURVEY;
INTERSTELLAR-MEDIUM; B3-VLA SAMPLE; SPIRAL ARMS; OBSERVATIONAL
CONSTRAINTS
AB We aim to summarize the current state of knowledge regarding Galactic Faraday rotation in an all-sky map of the Galactic Faraday depth. For this we have assembled the most extensive catalog of Faraday rotation data of compact extragalactic polarized radio sources to date. In the map-making procedure we used a recently developed algorithm that reconstructs the map and the power spectrum of a statistically isotropic and homogeneous field while taking into account uncertainties in the noise statistics. This procedure is able to identify some rotation angles that are offset by an integer multiple of pi. The resulting map can be seen as an improved version of earlier such maps and is made publicly available, along with a map of its uncertainty. For the angular power spectrum we find a power law behavior C-l proportional to l(-2.17) for a Faraday sky where an overall variance profile as a function of Galactic latitude has been removed, in agreement with earlier work. We show that this is in accordance with a 3D Fourier power spectrum P(k) proportional to k(-2.17) of the underlying field n(e)B(r) under simplifying geometrical and statistical assumptions.
C1 [Oppermann, N.; Junklewitz, H.; Robbers, G.; Bell, M. R.; Ensslin, T. A.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Bonafede, A.] Jacobs Univ Bremen, D-28759 Bremen, Germany.
[Braun, R.; Feain, I. J.; Harvey-Smith, L.; Mao, S. A.; McClure-Griffiths, N. M.; O'Sullivan, S. P.; Schnitzeler, D. H. F. M.; Stevens, J.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Brown, J. C.; Stil, J. M.; Sunstrum, C.; Taylor, A. R.; Van Eck, C. L.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Clarke, T. E.] USN, Res Lab, Washington, DC 20375 USA.
[Gaensler, B. M.; Hammond, A.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Heald, G.] ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Johnston-Hollitt, M.; Pratley, L.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand.
[Klein, U.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Kronberg, P. P.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Kronberg, P. P.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Mao, S. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Robishaw, T.] HIA NRC, Domin Radio Astrophys Observ, Penticton, BC V2A 6J9, Canada.
[Roy, S.] TIFR, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India.
[Schnitzeler, D. H. F. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Sotomayor-Beltran, C.] Ruhr Univ Bochum, Inst Astron, D-44780 Bochum, Germany.
[Tanna, A.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
RP Oppermann, N (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
EM niels@mpa-garching.mpg.de
RI Johnston-Hollitt, Melanie/B-1803-2013; Gaensler, Bryan/F-8655-2010;
Robishaw, Timothy/B-2654-2014;
OI Robishaw, Timothy/0000-0002-4217-5138; McClure-Griffiths,
Naomi/0000-0003-2730-957X; Gaensler, Bryan/0000-0002-3382-9558
FU 6.1 Base funding; Australian Research Council [FF0561298, FL100100114,
FS100100033]; Victoria University of Wellington Faculty of Science;
Marsden Development Fund; Commonwealth of Australia
FX The authors would like to thank Steven R. Spangler for the valuable
contributions he made to this paper as a referee. N.O. thanks Marco
Selig and Maximilian Ullherr for fruitful discussions during the genesis
of this work. Some of the results in this paper have been derived using
the HEALPix (Gorski et al. 2005) package. The calculations were
performed using the sage (Stein et al. 2010) mathematics software. This
research has made use of NASA's Astrophysics Data System. This research
was performed in the framework of the DFG Forschergruppe 1254
"Magnetisation of Interstellar and Intergalactic Media: The Prospects of
Low-Frequency Radio Observations". Basic research in radio astronomy at
the Naval Research Laboratory is funded by 6.1 Base funding. B. M. G.
and T. R. acknowledge the support of the Australian Research Council
through grants FF0561298, FL100100114 and FS100100033. M.J.-H. and L. P.
acknowledge support of the Victoria University of Wellington Faculty of
Science and Marsden Development Fund research grants awarded to M.J.-H.
The Australia Telescope Compact Array is part of the Australia Telescope
National Facility, which is funded by the Commonwealth of Australia for
operation as a National Facility managed by CSIRO. This paper includes
archived data obtained through the Australia Telescope Online
Archive9.
NR 115
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
EI 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2012
VL 542
AR A93
DI 10.1051/0004-6361/201118526
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965YI
UT WOS:000305803300050
ER
PT J
AU Ranalli, P
Comastri, A
Zamorani, G
Cappelluti, N
Civano, F
Georgantopoulos, I
Gilli, R
Schinnerer, E
Smolcic, V
Vignali, C
AF Ranalli, P.
Comastri, A.
Zamorani, G.
Cappelluti, N.
Civano, F.
Georgantopoulos, I.
Gilli, R.
Schinnerer, E.
Smolcic, V.
Vignali, C.
TI X-ray properties of radio-selected star forming galaxies in the
Chandra-COSMOS survey
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: galaxies; radio continuum: galaxies; galaxies: fundamental
parameters; galaxies: star formation; galaxies: active; galaxies:
high-redshift
ID DEEP FIELD-NORTH; ACTIVE GALACTIC NUCLEUS; FORMATION RATE INDICATOR;
XMM-NEWTON; LUMINOSITY FUNCTION; STARBURST GALAXIES; FORMATION HISTORY;
SOURCE POPULATION; SOURCE CATALOG; VLA SURVEY
AB X-ray surveys contain sizable numbers of star forming galaxies, beyond the AGN which usually make the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multiwavelength properties. We aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples.
We build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colours and observed with Chandra. A similarly selected control sample of AGN is also used for comparison. We review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. is such that similar to 30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples.
The radio/X-ray luminosity correlation for star forming galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, tough it is likely explained by a bias arising from the radio selection. Finally, we discuss the X-ray number counts of star forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra deep fields. The classification scheme proposed here may find application in future works and surveys.
C1 [Ranalli, P.; Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Ranalli, P.; Georgantopoulos, I.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece.
[Comastri, A.; Zamorani, G.; Cappelluti, N.; Georgantopoulos, I.; Gilli, R.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Smolcic, V.] Argelander Inst Astron, D-53121 Bonn, Germany.
[Smolcic, V.] European So Observ, D-85748 Garching, Germany.
[Smolcic, V.] Univ Zagreb, Dept Phys, Zagreb 10002, Croatia.
RP Ranalli, P (reprint author), Univ Bologna, Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy.
EM piero.ranalli@oabo.inaf.it
RI Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; Vignali,
Cristian/J-4974-2012; Ranalli, Piero/K-6363-2013; Georgantopoulos,
Ioannis/L-3687-2013;
OI Comastri, Andrea/0000-0003-3451-9970; Gilli,
Roberto/0000-0001-8121-6177; Vignali, Cristian/0000-0002-8853-9611;
Ranalli, Piero/0000-0003-3956-755X; Cappelluti,
Nico/0000-0002-1697-186X; Zamorani, Giovanni/0000-0002-2318-301X;
Schinnerer, Eva/0000-0002-3933-7677
FU Greek General Secretariat of Research and Technology [ASI-INAF
I/009/10/0]; European Union [229517]
FX We thank an anonymous referee whose comments have contributed to improve
the presentation of this paper. This research has made use of the Perl
Data Language (PDL) which provides a high-level numerical functionality
for the Perl programming language (Glazebrook & Economou 1997,
http://pdl.perl.org). We acknowledge financial contribution from the
agreement ASI-INAF I/009/10/0, and a grant from the Greek General
Secretariat of Research and Technology in the framework of the program
Support of Postdoctoral Researchers. The research leading to these
results has received funding from the European Union's Seventh Framework
programme under grant agreement 229517.
NR 76
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2012
VL 542
AR A16
DI 10.1051/0004-6361/201118723
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965YI
UT WOS:000305803300068
ER
PT J
AU Schneider, PC
Gunther, HM
Schmitt, JHMM
AF Schneider, P. C.
Guenther, H. M.
Schmitt, J. H. M. M.
TI The evolution of the X-ray emission of HH 2 Investigating heating and
cooling processes
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Herbig-Haro objects; ISM: jets and outflows; ISM: individual objects: HH
2; X-rays: ISM; stars: winds, outflows
ID HERBIG-HARO OBJECT-1; DG-TAURI; TELESCOPE OBSERVATIONS; PROTOSTELLAR
JET; ATOMIC DATABASE; PROPER MOTIONS; YOUNG STARS; MASS-LOSS; DISCOVERY;
ACCRETION
AB Young stellar objects often drive powerful bipolar outflows, which evolve on timescales of a few years. An increasing number of these outflows has been detected in X-rays implying the existence of million degree plasma almost co-spatial with the lower temperature gas observed in the optical and near-infrared. The details of the heating and cooling processes of the X-ray emitting part of these so-called Herbig-Haro objects are still ambiguous, e. g., whether the cooling is dominated by expansion, radiation, or thermal conduction.
We present a second epoch Chandra observation of the first X-ray detected Herbig-Haro object (HH 2) and derive the proper-motion of the X-ray emitting plasma and its cooling history. We argue that the most likely explanation for the constancy of the X-ray luminosity, the alignment with the optical emission and the proper-motion is that the cooling is dominated by radiative losses leading to cooling times exceeding a decade. We explain that a strong shock caused by fast material ramming into slower gas in front of it about ten years ago can explain the X-ray emission while being compatible with the available multi-wavelength data of HH 2.
C1 [Schneider, P. C.; Schmitt, J. H. M. M.] Hamburger Sternwarte, D-21029 Hamburg, Germany.
[Guenther, H. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Schneider, PC (reprint author), Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
EM cschneider@hs.uni-hamburg.de
OI Gunther, Hans Moritz/0000-0003-4243-2840
FU DLR [50 OR 1112]; NASA [GO1-12067X, NAS8-03060]; Chandra X-ray
Observatory Center
FX PCS was supported by the DLR under grant 50 OR 1112. HMG was supported
by NASA through Chandra Award Number GO1-12067X issued by the Chandra
X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of NASA under contract
NAS8-03060. The work used data obtained by the Chandra X-ray Observatory
and by the Hubble Space Telescope.
NR 35
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2012
VL 542
AR A123
DI 10.1051/0004-6361/201118605
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 965YI
UT WOS:000305803300054
ER
PT J
AU Prager, KC
Mazet, JAK
Munson, L
Cleaveland, S
Donnelly, CA
Dubovi, EJ
Gunther, MS
Lines, R
Mills, G
Davies-Mostert, HT
McNutt, JW
Rasmussen, G
Terio, K
Woodroffe, R
AF Prager, K. C.
Mazet, Jonna A. K.
Munson, Linda
Cleaveland, Sarah
Donnelly, Christl A.
Dubovi, Edward J.
Gunther, Micaela Szykman
Lines, Robin
Mills, Gus
Davies-Mostert, Harriet T.
McNutt, J. Weldon
Rasmussen, Gregory
Terio, Karen
Woodroffe, Rosie
TI The effect of protected areas on pathogen exposure in endangered African
wild dog (Lycaon pictus) populations
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE African wild dog; Canine distemper virus; Rabies virus; Domestic dog;
Infectious disease; Exposure risk
ID CANINE-DISTEMPER VIRUS; MADIKWE-GAME-RESERVE; DOMESTIC DOGS;
SOUTH-AFRICA; SERENGETI ECOSYSTEM; ANTIBODY-RESPONSE; TSUMKWE DISTRICT;
SEROLOGIC SURVEY; IMMUNE-RESPONSE; RABIES VACCINE
AB Infectious diseases impact African wild dogs (Lycaon pictus), but the nature and magnitude of this threat likely varies among populations according to different factors, such as the presence and prevalence of pathogens and land-use characteristics. We systematically evaluated these factors to assist development of locally appropriate strategies to mitigate disease risk. Wild dogs from 16 sites representing five unconnected populations were examined for rabies virus, canine distemper virus (CDV), canine parvovirus, canine coronavirus, and Babesia spp. exposure. Analyses revealed widespread exposure to viral pathogens, but Babesia was never detected. Exposure to CDV was associated with unprotected and protected-unfenced areas where wild dogs likely have a high probability of domestic dog contact and, in the case of protected-unfenced areas, likely reside amongst high wildlife densities. Our findings also suggest that domestic dog contact may increase rabies and coronavirus exposure risk. Therefore, domestic dogs may be a source of CDV, rabies and coronavirus, while wildlife may also play an important role in CDV transmission dynamics. Relatively high parvovirus seroprevalence across land-use types suggests that it might persist in the absence of spillover from domestic dogs. Should intervention be needed to control pathogens in wild dogs, efforts to prevent rabies and coronavirus exposure might be directed at reducing infection in the presumed domestic dog reservoir through vaccination. If prevention of CDV and parvovirus infections were deemed a management necessity, control of disease in domestic dogs may be insufficient to reduce transmission risks, and vaccination of wild dogs themselves may be the optimal strategy. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Prager, K. C.; Mazet, Jonna A. K.; Munson, Linda; Woodroffe, Rosie] Univ Calif Davis, Wildlife Hlth Ctr, Davis, CA 95616 USA.
[Cleaveland, Sarah] Univ Glasgow, Boyd Orr Ctr Populat & Ecosyst Hlth, Glasgow, Lanark, Scotland.
[Donnelly, Christl A.] Univ London Imperial Coll Sci Technol & Med, Dept Infect Dis Epidemiol, MRC Ctr Outbreak Anal & Modelling, London W2 1PG, England.
[Dubovi, Edward J.] Cornell Univ, Coll Vet Med, Anim Hlth Diagnost Ctr, Ithaca, NY 14852 USA.
[Gunther, Micaela Szykman] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA.
[Gunther, Micaela Szykman] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
[Lines, Robin] Zambian Carnivore Programme, Mfuwe, Eastern Provinc, Zambia.
[Mills, Gus] Kgalagadi Cheetah Project, ZA-8800 Upington, South Africa.
[Davies-Mostert, Harriet T.] Endangered Wildlife Trust, ZA-1645 Modderfontein, Gauteng, South Africa.
[Davies-Mostert, Harriet T.; Rasmussen, Gregory] Univ Oxford, Dept Zool, Recanati Kaplan Ctr, Wildlife Conservat Res Unit, Abingdon OX13 5QL, Oxon, England.
[McNutt, J. Weldon] Botswana Predator Conservat Project, Moun, Botswana.
[Terio, Karen] Univ Illinois, Zool Pathol Program, Maywood, IL USA.
[Woodroffe, Rosie] Regents Pk, Inst Zool, London NW1 4RY, England.
RP Prager, KC (reprint author), Univ Calif Davis, Wildlife Hlth Ctr, 1 Shields Ave, Davis, CA 95616 USA.
EM kcprager@ucla.edu
OI Szykman Gunther, Micaela/0000-0002-7822-8094; Donnelly,
Christl/0000-0002-0195-2463
FU Morris Animal Foundation; African Wildlife Foundation; Disney Wildlife
Conservation Fund; National Geographic Society; SeaWorld-Busch Gardens
Conservation Fund; Wildlife Conservation Society; Frankfurt Zoological
Society; Smithsonian Institution/Smithsonian Conservation Biology
Institute; AZA Conservation Endowment Fund; MRC
FX The Morris Animal Foundation provided funding to K.P. and R.W.;
long-term support for R.W.'s work also came from the African Wildlife
Foundation, Disney Wildlife Conservation Fund, National Geographic
Society, SeaWorld-Busch Gardens Conservation Fund and the Wildlife
Conservation Society. The Frankfurt Zoological Society provided funding
for work in the Serengeti in the 1980s and early 1990s, and the
Smithsonian Institution/Smithsonian Conservation Biology Institute and
the AZA Conservation Endowment Fund provided funding for M.S.G. C.A.D.
thanks MRC for Centre funding. These funders had no role in study
design, collection and analysis and interpretation of data, in the
writing of the report, and in the decision to submit the paper for
publication. The authors would like to thank Charles Rupprecht at the
Centers for Disease Control and Prevention for generously running our
rabies serology, Gabriella Flacke and Penny Spiering for providing
detailed data on many of the wild dogs from the South African
metapopulation, Stacy Schultz for technical assistance with the Babesia
qPCR, and the members of the South Africa wild dog advisory group. The
authors would also like to acknowledge members of the Wild Dog Advisory
Group, South Africa, in particular Steve Dell, Declan Hofmeyr and
Katherine Potgierter, for providing samples and the staff of South
African National Parks. The authors would like to thank two anonymous
reviewers for their helpful comments and suggestions.
NR 61
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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 2012
VL 150
IS 1
BP 15
EP 22
DI 10.1016/j.biocon.2012.03.005
PG 8
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 964VF
UT WOS:000305724100003
ER
PT J
AU Nolan, GA
McFarland, AL
Zajicek, JM
Waliczek, TM
AF Nolan, Geralyn A.
McFarland, Amy L.
Zajicek, Jayne M.
Waliczek, Tina M.
TI The Effects of Nutrition Education and Gardening on Attitudes,
Preferences, and Knowledge of Minority Second to Fifth Graders in the
Rio Grande Valley Toward Fruit and Vegetables
SO HORTTECHNOLOGY
LA English
DT Article
DE social issues; obesity; Type II diabetes; horticulture; health; fruit
and vegetable questionnaire
ID CARDIOVASCULAR-DISEASE; CHILDHOOD OBESITY; CHILDRENS FRUIT; PREVENT
OBESITY; UNITED-STATES; CONSUMPTION; PROGRAM; HEALTH; ADOLESCENTS;
CURRICULUM
AB Child obesity has become a national concern. Obesity in children ages 6-17 years has more than doubled in the past 30 years. Only 20% of children today consume the recommended daily servings of fruit and vegetables. This trend is even more pronounced in minority populations. Past studies have reported a horticulture-based curriculum, including gardening, can improve children's attitudes toward eating fruit and vegetables. To investigate whether children of a minority population can benefit from gardening combined with a curriculum on nutrition, research was conducted with elementary schools in a primarily Hispanic region of Texas. Elementary school teachers participating in this research agreed to have school gardens and complete all activities in a curriculum on nutrition provided to them through the Texas Agrilife Extension Service. One hundred and forty-one children in the participating schools completed a pre- and posttest evaluating their nutritional knowledge, preference for fruit and vegetables, and snack choices before and after a gardening program supplemented with nutrition education. Differences were detected between pre- and posttest scores for all three variables. After comparing pre- and posttest scores, it was concluded that gardening and nutritional instruction had a positive effect on students' nutritional knowledge, fruit and vegetable preference (FVP), and snack choices.
C1 [Waliczek, Tina M.] Texas State Univ San Marcos, Dept Agr, San Marcos, TX 78666 USA.
[Nolan, Geralyn A.; Zajicek, Jayne M.] Texas A&M Univ, Dept Hort Sci, College Stn, TX 77843 USA.
[McFarland, Amy L.] Smithsonian Inst, Smithsonian Gardens, Washington, DC 20013 USA.
RP Waliczek, TM (reprint author), Texas State Univ San Marcos, Dept Agr, San Marcos, TX 78666 USA.
EM tc10@txstate.edu
NR 42
TC 5
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U1 4
U2 50
PU AMER SOC HORTICULTURAL SCIENCE
PI ALEXANDRIA
PA 113 S WEST ST, STE 200, ALEXANDRIA, VA 22314-2851 USA
SN 1063-0198
J9 HORTTECHNOLOGY
JI HortTechnology
PD JUN
PY 2012
VL 22
IS 3
BP 299
EP 304
PG 6
WC Horticulture
SC Agriculture
GA 967AF
UT WOS:000305877800004
ER
PT J
AU Scarlata, CD
Elias, BA
Godwin, JR
Powell, RA
Shepherdson, D
Shipley, LA
Brown, JL
AF Scarlata, Candace D.
Elias, Becky A.
Godwin, John R.
Powell, Roger A.
Shepherdson, David
Shipley, Lisa A.
Brown, Janine L.
TI Relationship between fecal hormone concentrations and reproductive
success in captive pygmy rabbits (Brachylagus idahoensis)
SO JOURNAL OF MAMMALOGY
LA English
DT Article
DE captive breeding; conception; fecal glucocorticoids; hormones;
lactation; litter size; mating; progestagens; stress; reproduction
ID DOMESTIC-ANIMALS; STRESS RESPONSES; LITTER SIZE; PROGESTERONE;
PREGNANCY; SHEEP; GLUCOCORTICOIDS; CONSERVATION; WILDLIFE; BEHAVIOR
AB The Columbia Basin pygmy rabbit (Brachylagus idahoensis) is critically endangered and the focus of a captive-breeding program. However, reproductive success in captivity to date has not been sufficient to sustain reintroduction efforts. The goal of this study was to investigate patterns of fecal progestagen and glucocorticoid excretion in females during mating, gestation, and lactation and identify hormonal relationships to reproductive success. Fresh fecal samples were collected from 48 adult, female rabbits over 3 breeding seasons at a frequency of 4-7 samples per week. Results showed that a large (17-fold) increase in progestagen concentrations 1 day after mating provides a reliable means of determining if a successful mating occurred. In general, higher glucocorticoid concentrations during the breeding season, specifically during mating and gestation, were associated with lower reproductive success. Females that failed to conceive during the breeding season had higher glucocorticoid and lower progestagen baseline concentrations than females that did conceive. Glucocorticoid excretion during late gestation, but not lactation, was negatively associated with litter success, suggesting it affects offspring survival more during the prenatal than the postnatal period. Progestagen and glucocorticoid concentrations at the end of gestation were positively related to litter size, which may be an important factor in juvenile survival. In summary, higher concentrations of fecal glucocorticoids during the breeding season were associated with reduced conception rates and survival of subsequent litters. Ultimately, identifying what factors cause elevated glucocorticoids in pygmy rabbits could provide opportunities to alleviate negative stressors and increase the reproductive output of the captive population.
C1 [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA.
[Scarlata, Candace D.; Godwin, John R.; Powell, Roger A.] N Carolina State Univ, Dept Biol, Raleigh, NC 27695 USA.
[Elias, Becky A.; Shipley, Lisa A.] Washington State Univ, Dept Nat Resource Sci, Pullman, WA 99164 USA.
[Shepherdson, David] Oregon Zoo, Portland, OR 97221 USA.
RP Brown, JL (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA.
EM brownjan@si.edu
FU Morris Animal Foundation; Smithsonian Institution; Washington Department
of Fish and Wildlife; North Carolina State University; Washington State
University; Friends of the National Zoo
FX We thank all the pygmy rabbit keepers (M. Illig, B. Elias, J.
Jackson-VonDohlen, A. Williams, H. Starr, R. Lamson, K. Walker, and L.
Klinski) for their dedication to the rabbits and for all the hours spent
collecting samples and behavioral data. In addition, thanks to N.
Presley, N. Abbondanza, and S. Putnam for their patience and technical
assistance in the laboratory. We are grateful to H. Patisaul and S.
Kennedy Stoskopf for insightful thoughts on the development of this
study and for helpful comments on drafts of the manuscript. Funding for
this project was provided by a large grant from the Morris Animal
Foundation and several supporting grants from the Smithsonian
Institution, Friends of the National Zoo, Washington Department of Fish
and Wildlife, North Carolina State University, and Washington State
University.
NR 55
TC 8
Z9 8
U1 6
U2 38
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-2372
EI 1545-1542
J9 J MAMMAL
JI J. Mammal.
PD JUN
PY 2012
VL 93
IS 3
BP 759
EP 770
DI 10.1644/11-MAMM-A-223.1
PG 12
WC Zoology
SC Zoology
GA 969HA
UT WOS:000306045100015
ER
PT J
AU Woodman, N
AF Woodman, Neal
TI Taxonomic status and relationships of Sorex obscurus parvidens Jackson,
1921, from California
SO JOURNAL OF MAMMALOGY
LA English
DT Article
DE Eulipotyphla; Insectivora; morphology; shrew; Soricidae; Soricomorpha
ID ORNATUS
AB The San Bernardino shrew, Sorex obscurus parvidens Jackson, 1921, is a population inhabiting the San Bernardino and San Gabriel mountains of southern California. For the past 9 decades, this population has been considered either a subspecies of S. obscurus Merriam, 1895, S. vagrans Baird, 1857, or S. monticola Merriam, 1890; or an undifferentiated population of S. ornatus Merriam, 1895. Aside from the changing taxonomic landscape that contextualizes the genus Sorex, previous study of S. obscurus parvidens has been retarded by the perception of limited available samples (typically, fewer than 8 specimens); misinterpretation of the provenance of specimens identified as S. obscurus parvidens; misunderstanding of the type locality; and inclusion of specimens of this taxon in the type series of another species with which S. obscurus parvidens has been both contrasted and allied at different times. My investigation of S. obscurus parvidens indicates that it is a distinctive population that is morphologically closest to S. ornatus, and it corresponds to the Southern Clade of that species. However, the appropriate names for deep clades within S. ornatus remain uncertain. Until this uncertainty is resolved, S. obscurus parvidens should be considered a distinctive population within S. ornatus; for conservation purposes, it should be recognized as S. ornatus parvidens.
C1 Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20013 USA.
RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20013 USA.
EM woodmann@si.edu
OI Woodman, Neal/0000-0003-2689-7373
NR 32
TC 0
Z9 1
U1 0
U2 3
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-2372
EI 1545-1542
J9 J MAMMAL
JI J. Mammal.
PD JUN
PY 2012
VL 93
IS 3
BP 826
EP 838
DI 10.1644/11-MAMM-A-354.1
PG 13
WC Zoology
SC Zoology
GA 969HA
UT WOS:000306045100022
ER
PT J
AU Hunt, G
AF Hunt, Gene
TI Measuring rates of phenotypic evolution and the inseparability of tempo
and mode
SO PALEOBIOLOGY
LA English
DT Article
ID NATURAL-SELECTION; FOSSIL RECORD; RANDOM-WALKS; CONTEMPORARY
MICROEVOLUTION; QUANTITATIVE GENETICS; STABILIZING SELECTION; PHYLETIC
EVOLUTION; MODERN LIFE; BODY-SIZE; EXTINCTION
AB Rates of phenotypic evolution are central to many issues in paleontology, but traditional rate metrics such as darwins or haldanes are seldom used because of their strong dependence on interval length. In this paper, I argue that rates are usefully thought of as model parameters that relate magnitudes of evolutionary divergence to elapsed time. Starting with models of directional evolution, random walks, and stasis, T derive for each a reasonable rate metric. These metrics can be linked to existing approaches in evolutionary biology, and simulations show that they can be estimated accurately at any temporal resolution via maximum likelihood, but only when that metric's underlying model is true.
The estimation of generational rates of a random walk under realistic paleontological conditions is compared with simulations to that of a prominent alternative approach, Gingerich's LRI (log-rate, log-interval) method. Generational rates are estimated poorly by LRI; they often reflect sampling error more than the actual pace of change. Further simulations show that under some realistic conditions, it is simply not possible to infer generational rates from coarsely sampled populations.
These modeling results indicate a complex dependence between evolutionary mode and the measurement of evolutionary rates, and that there is unlikely to be a rate metric that works well for all traits and time scales. Compilations of paleontological and phylogenetic data indicate that all of the three rate metrics derived here show some relationship with interval length. Although there is no perfect rate metric, at present the most practical choices derive from the parameters of the stasis and random walk models. The latter, called the step variance, is particularly promising as a rate metric in paleontology and comparative biology.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
RP Hunt, G (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
EM hunte@si.edu
RI Hunt, Gene/B-3783-2010
OI Hunt, Gene/0000-0001-6430-5020
NR 68
TC 36
Z9 36
U1 3
U2 52
PU PALEONTOLOGICAL SOC INC
PI LAWRENCE
PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA
SN 0094-8373
J9 PALEOBIOLOGY
JI Paleobiology
PD SUM
PY 2012
VL 38
IS 3
BP 351
EP 373
DI 10.1666/11047.1
PG 23
WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology
SC Biodiversity & Conservation; Environmental Sciences & Ecology;
Evolutionary Biology; Paleontology
GA 966YZ
UT WOS:000305874600001
ER
PT J
AU Pardo-Diaz, C
Salazar, C
Baxter, SW
Merot, C
Figueiredo-Ready, W
Joron, M
McMillan, WO
Jiggins, CD
AF Pardo-Diaz, Carolina
Salazar, Camilo
Baxter, Simon W.
Merot, Claire
Figueiredo-Ready, Wilsea
Joron, Mathieu
McMillan, W. Owen
Jiggins, Chris D.
TI Adaptive Introgression across Species Boundaries in Heliconius
Butterflies
SO PLOS GENETICS
LA English
DT Article
ID DNA-SEQUENCE DATA; DROSOPHILA-PSEUDOOBSCURA; NATURAL HYBRIDIZATION;
CONVERGENT EVOLUTION; HYBRID SPECIATION; SEXUAL SELECTION; PATTERN
MIMICRY; GENE FLOW; HISTORY; RESISTANCE
AB It is widely documented that hybridisation occurs between many closely related species, but the importance of introgression in adaptive evolution remains unclear, especially in animals. Here, we have examined the role of introgressive hybridisation in transferring adaptations between mimetic Heliconius butterflies, taking advantage of the recent identification of a gene regulating red wing patterns in this genus. By sequencing regions both linked and unlinked to the red colour locus, we found a region that displays an almost perfect genotype by phenotype association across four species, H. melpomene, H. cydno, H. timareta, and H. heurippa. This particular segment is located 70 kb downstream of the red colour specification gene optix, and coalescent analysis indicates repeated introgression of adaptive alleles from H. melpomene into the H. cydno species clade. Our analytical methods complement recent genome scale data for the same region and suggest adaptive introgression has a crucial role in generating adaptive wing colour diversity in this group of butterflies.
C1 [Pardo-Diaz, Carolina; Salazar, Camilo; Baxter, Simon W.; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge, England.
[Salazar, Camilo; McMillan, W. Owen; Jiggins, Chris D.] Smithsonian Trop Res Inst, Panama City, Panama.
[Merot, Claire; Joron, Mathieu] Museum Natl Hist Nat, CNRS, UMR 7205, CP50, Paris, France.
[Figueiredo-Ready, Wilsea] Fed Univ Para, Inst Estudos Costeiros, Braganca, Brazil.
RP Pardo-Diaz, C (reprint author), Univ Cambridge, Dept Zool, Cambridge, England.
EM cp419@cam.ac.uk
RI Joron, Mathieu/C-9178-2009; Jiggins, Chris/B-9960-2008; Salazar,
camilo/A-1647-2010; Pardo-Diaz, Carolina/C-7936-2016
OI Joron, Mathieu/0000-0003-1043-4147; Jiggins, Chris/0000-0002-7809-062X;
Salazar, camilo/0000-0001-9217-6588; Pardo-Diaz,
Carolina/0000-0002-7259-1183
FU Leverhulme Trust; BBSRC; Smithsonian Tropical Research Institute (STRI);
NSF [DBI-0923119, IOS 1052541]
FX CP-D and CDJ were funded by a Leverhulme Trust Research Leadership Grant
and by the BBSRC; CS by the Smithsonian Tropical Research Institute
(STRI); and WOM by STRI and NSF grants, DBI-0923119, and IOS 1052541.
The funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 57
TC 87
Z9 87
U1 5
U2 82
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1553-7404
J9 PLOS GENET
JI PLoS Genet.
PD JUN
PY 2012
VL 8
IS 6
AR e1002752
DI 10.1371/journal.pgen.1002752
PG 13
WC Genetics & Heredity
SC Genetics & Heredity
GA 968EW
UT WOS:000305961000019
PM 22737081
ER
PT J
AU Reasenberg, RD
AF Reasenberg, Robert D.
TI Aligning a reflection cavity by Anderson's method
SO APPLIED OPTICS
LA English
DT Article
ID OPTICAL-RESONATOR; ALIGNMENT; STABILIZATION
AB The sounding rocket principle of equivalence measurement uses a set of four laser gauges operating in Fabry-Perot cavities to determine the relative acceleration of two test masses that are chemically different. One end of each cavity is a flat mirror on a test mass. Because the test masses are unconstrained and thus expected to rotate slightly during measurement, and because the distance measurements are made at the sub-picometer level, it is essential to have real-time alignment of the beam entering the cavity. However, the cavity must be used in reflection and space is limited. We show that Anderson's alignment method can be used in reflection, but that it requires that the Fabry-Perot cavity have mirrors with significantly unequal reflectivities.
C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Reasenberg, RD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM reasenberg@cfa.harvard.edu
FU Smithsonian Institution; NASA Astrophysics Division [NNX08AO04G]
FX This work was supported by the Smithsonian Institution. SR-POEM has been
supported by the NASA Astrophysics Division through grant NNX08AO04G. I
thank J.D. Phillips for his thoughtful comments on the manuscript.
NR 8
TC 1
Z9 1
U1 4
U2 5
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD JUN 1
PY 2012
VL 51
IS 16
BP 3132
EP 3136
DI 10.1364/AO.51.003132
PG 5
WC Optics
SC Optics
GA 955JT
UT WOS:000305015300005
PM 22695543
ER
PT J
AU Mathis, WN
Freidberg, A
AF Mathis, Wayne N.
Freidberg, Amnon
TI Periscelis stuckenbergi sp n., the first record of the genus from the
Afrotropical Region (Diptera: Periscelididae: Periscelidinae)
SO AFRICAN INVERTEBRATES
LA English
DT Article
DE Diptera; Periscelididae; Periscelidinae; Periscelis; Afrotropical;
Ethiopia; new species
ID AULACIGASTRIDAE
AB A new species of the genus Periscelis Loew (P. stuckenbergi, Diptera: Periscelididae: Periscelidinae), the first from the Afrotropical Region, is described. Brief diagnoses of the family, subfamily, genus, subgenus and species are provided to facilitate identification of members of this uncommon family. A key to the sub-families of the family and subgenera of Periscelis and habitus photographs and detailed illustrations of structures of the male terminalia are also included.
C1 [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA.
[Freidberg, Amnon] Tel Aviv Univ, George S Wise Fac Life Sci, Dept Zool, IL-69978 Tel Aviv, Israel.
RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MRC 169, Washington, DC 20013 USA.
EM mathisw@si.edu; afdipter@post.tau.ac.il
NR 25
TC 0
Z9 0
U1 0
U2 0
PU COUNCIL NATAL MUSEUM
PI PIETERMARITZBURG
PA PRIVATE BAG 9070, PIETERMARITZBURG, KWAZULU-NATAL 00000, SOUTH AFRICA
SN 1681-5556
J9 AFR INVERTEBR
JI Afr. Invertebr.
PD JUN
PY 2012
VL 53
IS 1
BP 231
EP 238
PG 8
WC Entomology; Paleontology; Zoology
SC Entomology; Paleontology; Zoology
GA 961IE
UT WOS:000305457100016
ER
PT J
AU Woodley, NE
AF Woodley, Norman E.
TI Brianmyia stuckenbergi, a new genus and species of Prosopochrysini from
South Africa (Diptera: Stratiomyidae)
SO AFRICAN INVERTEBRATES
LA English
DT Article
DE Stratiomyidae; Brianmyia; soldier flies; Afrotropical; South Africa;
Drakensberg; new genus; new species
AB A new genus and species of Stratiomyidae, Brianmyia stuckenbergi gen. et sp. n., are described from the Drakensberg, KwaZulu-Natal, South Africa. The new genus is placed in the tribe Prosopochrysini of the subfamily Stratiomyinae and is the first genus and species of this tribe known from southern Africa.
C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst NHB 168, Washington, DC 20013 USA.
RP Woodley, NE (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst NHB 168, POB 37012, Washington, DC 20013 USA.
EM norman.woodley@ars.usda.gov
RI Woodley, Norman/M-6160-2014
NR 7
TC 1
Z9 1
U1 0
U2 0
PU COUNCIL NATAL MUSEUM
PI PIETERMARITZBURG
PA PRIVATE BAG 9070, PIETERMARITZBURG, KWAZULU-NATAL 00000, SOUTH AFRICA
SN 1681-5556
J9 AFR INVERTEBR
JI Afr. Invertebr.
PD JUN
PY 2012
VL 53
IS 1
BP 369
EP 374
PG 6
WC Entomology; Paleontology; Zoology
SC Entomology; Paleontology; Zoology
GA 961IE
UT WOS:000305457100021
ER
PT J
AU White, WH
Erwin, TL
Viator, BJ
AF White, W. H.
Erwin, T. L.
Viator, B. J.
TI LEPTOTRACHELUS DORSALIS (COLEOPTERA: CARABIDAE): A CANDIDATE BIOLOGICAL
CONTROL AGENT OF THE SUGARCANE BORER IN LOUISIANA
SO FLORIDA ENTOMOLOGIST
LA English
DT Article
DE Diatraea saccharalis; fire ants; habitat manipulation; augmentative
release; predators
ID LEPIDOPTERA; PYRALIDAE; SUSCEPTIBILITY; TEBUFENOZIDE; CRAMBIDAE;
PREDATORS; FIELDS
AB Following registration and the wide-spread use of insect growth regulators (e.g. tebufenozide and novaluron) for control of sugarcane borer, Diatraea saccharalis (F.) (Lepidoptera: Crambidae), in Louisiana, larvae of the ground beetle, Leptotrachelus dorsalis (F.) (Coleoptera: Carabidae, have become more abundant in sugarcane fields. In a survey of the 18 parishes growing sugarcane in Louisiana, L. dorsalis was found in 8 (44%) of those parishes. The highest number of beetles occurred in a field where 10% of the stalks sampled were harboring larvae. Laboratory studies revealed a developmental period of 37 d from egg deposition to adult emergence. Three larval instars were identified with the first 2 lasting 5 d, and the third instar requiring 17 d. In a voracity study, larvae were found to consume on average 798 first instar sugarcane borer larvae per ground beetle larva. Seventy-five percent of those sugarcane borer larvae were consumed by third instar beetle larvae. Field surveys suggest that adults migrate into sugarcane fields when above-ground internodes form on the sugarcane stalk (June) and increase in numbers thereafter. All 3 instars of the beetle can be found in sugarcane fields during the critical period of Jun to Sep when sugarcane is subject to economic injury by sugarcane borer. If L. dorsalis are abundant in fields during establishment of second generation sugarcane borer, our data suggests they are capable of holding the average season-long damage at or below 10% bored internodes. This level of damage is the recognized economic injury level for sugarcane borer in Louisiana. Our study indicates that L. dorsalis is a good candidate for continued research on augmentative releases as a strategy to increase beetle numbers in sugarcane fields early in the growing season and thus enhance their efficacy as predators of sugarcane borer larvae.
C1 [White, W. H.] ARS, USDA, Sugarcane Res Unit, Houma, LA 70360 USA.
[Erwin, T. L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Hyper Divers Grp, Washington, DC 20013 USA.
[Viator, B. J.] Calvin Viator PhD & Associates LLC, Labadieville, LA 70372 USA.
RP White, WH (reprint author), ARS, USDA, Sugarcane Res Unit, 5883 USDA Rd, Houma, LA 70360 USA.
FU American Sugar Cane League of the U.S.A., Inc.
FX The authors express gratitude to Randy Richard and Elta Duet for
valuable assistance in the laboratory and field. Financial assistance
from the American Sugar Cane League of the U.S.A., Inc. is gratefully
acknowledged. Mention of trade names or commercial products in this
article is solely for the purpose of providing specific information and
does not imply recommendation or endorsement by the U.S. Department of
Agriculture.
NR 21
TC 2
Z9 2
U1 0
U2 2
PU FLORIDA ENTOMOLOGICAL SOC
PI LUTZ
PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA
SN 0015-4040
J9 FLA ENTOMOL
JI Fla. Entomol.
PD JUN
PY 2012
VL 95
IS 2
BP 261
EP 267
PG 7
WC Entomology
SC Entomology
GA 960EL
UT WOS:000305370700003
ER
PT J
AU Page, RA
Schnelle, T
Kalko, EKV
Bunge, T
Bernal, XE
AF Page, Rachel A.
Schnelle, Tanja
Kalko, Elisabeth K. V.
Bunge, Thomas
Bernal, Ximena E.
TI Sequential assessment of prey through the use of multiple sensory cues
by an eavesdropping bat
SO NATURWISSENSCHAFTEN
LA English
DT Article
DE Multimodal cues; Foraging strategies; Prey palatability; Prey size;
Predator flexibility; Trachops cirrhosus
ID FROG-EATING BATS; TRACHOPS-CIRRHOSUS; MOTH CLICKS; CALLS; ECHOLOCATION;
APOSEMATISM; EVOLUTION; BEHAVIOR; GLANDS
AB Predators are often confronted with a broad diversity of potential prey. They rely on cues associated with prey quality and palatability to optimize their hunting success and to avoid consuming toxic prey. Here, we investigate a predator's ability to assess prey cues during capture, handling, and consumption when confronted with conflicting information about prey quality. We used advertisement calls of a preferred prey item (the tA(0)ngara frog) to attract fringe-lipped bats, Trachops cirrhosus, then offered palatable, poisonous, and chemically manipulated anurans as prey. Advertisement calls elicited an attack response, but as bats approached, they used additional sensory cues in a sequential manner to update their information about prey size and palatability. While both palatable and poisonous small anurans were readily captured, large poisonous toads were approached but not contacted suggesting the use of echolocation for assessment of prey size at close range. Once prey was captured, bats used chemical cues to make final, post-capture decisions about whether to consume the prey. Bats dropped small, poisonous toads as well as palatable frogs coated in toad toxins either immediately or shortly after capture. Our study suggests that echolocation and chemical cues obtained at close range supplement information obtained from acoustic cues at long range. Updating information about prey quality minimizes the occurrence of costly errors and may be advantageous in tracking temporal and spatial fluctuations of prey and exploiting novel food sources. These findings emphasize the sequential, complex nature of prey assessment that may allow exploratory and flexible hunting behaviors.
C1 [Page, Rachel A.; Kalko, Elisabeth K. V.; Bernal, Ximena E.] Smithsonian Trop Res Inst, Panama City, Panama.
[Schnelle, Tanja; Kalko, Elisabeth K. V.; Bunge, Thomas] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany.
[Bernal, Ximena E.] Texas Tech Univ, Lubbock, TX 79409 USA.
RP Page, RA (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama.
EM PageR@si.edu
NR 25
TC 9
Z9 9
U1 8
U2 39
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0028-1042
J9 NATURWISSENSCHAFTEN
JI Naturwissenschaften
PD JUN
PY 2012
VL 99
IS 6
BP 505
EP 509
DI 10.1007/s00114-012-0920-6
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 961OV
UT WOS:000305476200009
PM 22592417
ER
PT J
AU Guo, CQ
Edwards, D
Wu, PC
Duckett, JG
Hueber, FM
Li, CS
AF Guo, Cai-Qing
Edwards, Dianne
Wu, Peng-Cheng
Duckett, Jeffrey G.
Hueber, Francis M.
Li, Cheng-Sen
TI Riccardiothallus devonicus gen. et sp nov., the earliest simple thalloid
liverwort from the Lower Devonian of Yunnan, China
SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY
LA English
DT Article
DE Aneuraceae; Riccardiothallus devonicus; fossil liverwort; Lower
Devonian; Yunnan; China
ID EARLY LAND PLANTS; POSONGCHONG FORMATION; SOUTHEASTERN YUNNAN; FERN
GAMETOPHYTES; HOPE BAY; PROVINCE; EVOLUTION; HEPATICAE; MARCHANTIOPHYTA;
ANTARCTICA
AB This paper describes a fossil liverwort in the Posongchong Formation, Lower Devonian (Pragian), Yunnan, China preserved as a partially permineralized compression in gray arenaceous mudstone. The plant comprises a regularly-bifurcating flat ecostate multilayered thallus with entire margins. Following comparisons of this fossil with gametophytes of extant and fossil liverworts, a new genus Riccardiothallus was established in the family Aneuraceae (Jungermanniopsida). The fossil, which appears to be closely similar to several members of the extant genus Riccardia, is the earliest unequivocal megafossil evidence of a liverwort. Considering the sedimentary environment of Riccardiothallus devonicus and the habitats of many extant Riccardia species, we conclude that Riccardiothallus devonicus probably lived in a warm and humid riverine environment. The age (Pragian, 407-411 Ma) of Riccardiothallus devonicus suggests that the differentiation of Jungermanniopsida and Metzgeriidae was in the Early Devonian, significantly earlier than the assumptions derived from analyses of chloroplast DNA sequences of modern liverworts and current total evidence phylogenies (Late Devonian, 359-385 Ma: Late Carboniferous, 299-307 Ma). (C) 2012 Elsevier B.V. All rights reserved.
C1 [Guo, Cai-Qing; Wu, Peng-Cheng; Li, Cheng-Sen] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China.
[Guo, Cai-Qing] Chinese Acad Geol Sci, Inst Geol, Beijing 100037, Peoples R China.
[Edwards, Dianne] Cardiff Univ, Sch Earth & Ocean Sci, Cardiff CF10 3AT, S Glam, Wales.
[Duckett, Jeffrey G.] Nat Hist Museum, Dept Bot, London SW7 5BD, England.
[Hueber, Francis M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Li, CS (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China.
EM lics@ibcas.ac.cn
NR 64
TC 13
Z9 16
U1 1
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0034-6667
J9 REV PALAEOBOT PALYNO
JI Rev. Palaeobot. Palynology
PD JUN
PY 2012
VL 176
BP 35
EP 40
DI 10.1016/j.revpalbo.2012.03.012
PG 6
WC Plant Sciences; Paleontology
SC Plant Sciences; Paleontology
GA 961VB
UT WOS:000305496500003
ER
PT J
AU Harris, EM
Horn, JW
Wagner, WL
AF Harris, Elizabeth M.
Horn, James W.
Wagner, Warren L.
TI Floral development of the divergent endemic Hawaiian genus Schiedea
(Caryophyllaceae), with special emphasis on the floral nectaries
SO TAXON
LA English
DT Article
DE Caryophyllaceae; floral development; floral dimorphism; floral nectary;
Hawaii; Schiedea
ID ALSINIDENDRON CARYOPHYLLACEAE; INFLORESCENCE TRAITS; GENETIC
CORRELATIONS; POLLINATION BIOLOGY; WIND POLLINATION; BREEDING SYSTEMS;
SENSU-LATO; EVOLUTION; ALSINOIDEAE; HERITABILITIES
AB The endemic Hawaiian genus Schiedea has among the most architecturally complex flowers of any genus of Caryophyllaceae. To understand the developmental basis of the unusual floral features that characterize Schiedea, we studied the floral organogenesis of 6 of the 34 species of the genus using SEM, supplementing these observations with a focused investigation of nectary histology. The early ontogeny of Schiedea flowers is like that of many other Caryophyllaceae in that: (1) the five sepals are initiated in a 2/5 spiral, with the first, antesepalous whorl of stamens initiated in an imperfectly contrarotating sequence relative to the sepals; (2) the alternisepalous stamen whorl initiates slightly external to and at a lower level on the floral apex than the antesepalous whorl; and (3) petal primordia, if initiated (rare), arise on a primordium common with an alternisepalous stamen. Hence, most floral features that distinguish the genus, such as the (often) reflexed sepals and elongate stamen filaments, arise late in floral ontogeny. The only unique trait to Schiedea flowers are the elongate, tubular nectary extensions. They are antesepalous and arise from the abaxial surface of a ring-shaped proliferation of tissue that surrounds the bases of the developing stamens. The shape of each nectary in early ontogeny is highly similar to the mature "swallow's nest" nectaries present in many genera of a major crown clade of Caryophyllaceae (Pleurcaryophyllaceae, containing Schiedea), suggesting that the development of the needle- to scale-like nectary extensions of Schiedea might represent terminal additions onto a "swallow's nest" nectary ontogenetic program.
C1 [Horn, James W.; Wagner, Warren L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
[Harris, Elizabeth M.] Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA.
RP Wagner, WL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA.
EM wagnerw@si.edu
FU National Science Foundation [BSR 88-17616, BSR 89-18366, DEB 92-07724];
Smithsonian Institution
FX This research was supported by grants from the National Science
Foundation (BSR 88-17616, BSR 89-18366, DEB 92-07724) to Stephen Weller
and Ann Sakai, and a grant from the Scholarly Studies Program of the
Smithsonian Institution (Wagner, Weller, Sakai, D. Soltis, and P.
Soltis). We thank Stephen Weller and Ann Sakai for providing cultivated
material of the species examined in this study, and for their conceptual
input on the project at its initiation. We thank Richard Crang for
facilitating the use of the SEM at the EM facility at the University of
Illinois. Alice Tangerini assisted in designing the photographic plates,
and produced the final digital versions. Denise Mix provided lab
assistance. Ann Sakai, Louis Ronse De Craene, and an anonymous reviewer
contributed helpful comments on the manuscript.
NR 45
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PU INT ASSOC PLANT TAXONOMY-IAPT
PI BRATISLAVA
PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23
BRATISLAVA, SLOVAKIA
SN 0040-0262
J9 TAXON
JI Taxon
PD JUN
PY 2012
VL 61
IS 3
BP 576
EP 591
PG 16
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 961BO
UT WOS:000305439100007
ER
PT J
AU Goodman, AA
AF Goodman, A. A.
TI Principles of high-dimensional data visualization in astronomy
SO ASTRONOMISCHE NACHRICHTEN
LA English
DT Article
DE cosmology: large-scale structure; ISM: clouds; methods: data analysis;
techniques: image processing; techniques: radial velocities
ID 3D VISUALIZATION
AB Astronomical researchers often think of analysis and visualization as separate tasks. In the case of high-dimensional data sets, though, interactive exploratory data visualization can give far more insight than an approach where data processing and statistical analysis are followed, rather than accompanied, by visualization. This paper attempts to charts a course toward linked view systems, where multiple views of high-dimensional data sets update live as a researcher selects, highlights, or otherwise manipulates, one of several open views. For example, imagine a researcher looking at a 3D volume visualization of simulated or observed data, and simultaneously viewing statistical displays of the data set's properties (such as an x -y plot of temperature vs. velocity, or a histogram of vorticities). Then, imagine that when the researcher selects an interesting group of points in any one of these displays, that the same points become a highlighted subset in all other open displays. Selections can be graphical or algorithmic, and they can be combined, and saved. For tabular (ASCII) data, this kind of analysis has long been possible, even though it has been under-used in astronomy. The bigger issue for astronomy and other high-dimensional fields, though, is that no extant system allows for full integration of images and data cubes within a linked-view environment. The paper concludes its history and analysis of the present situation with suggestions that look toward cooperatively-developed open-source modular software as a way to create an evolving, flexible, high-dimensional, linked-view visualization environment useful in astro-physical research ((c) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Goodman, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM agoodman@cfa.harvard.edu
RI Goodman, Alyssa/A-6007-2010
OI Goodman, Alyssa/0000-0003-1312-0477
FU Microsoft Research; National Science Foundation; NASA
FX The author thanks her collaborators Michelle Borkin and Christopher
Beaumont for their significant contributions to this work, and Bernice
Rogowitz and Hanspeter Pfister for excellent suggestions on improving
it. Microsoft Research, the National Science Foundation, and NASA all
fund the author's work on astronomical data visualization.
NR 18
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PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 0004-6337
J9 ASTRON NACHR
JI Astro. Nachr.
PD JUN
PY 2012
VL 333
IS 5-6
SI SI
BP 505
EP 514
DI 10.1002/asna.201211705
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 959SA
UT WOS:000305331900016
ER
PT J
AU Brammer, GB
van Dokkum, PG
Franx, M
Fumagalli, M
Patel, S
Rix, HW
Skelton, RE
Kriek, M
Nelson, E
Schmidt, KB
Bezanson, R
da Cunha, E
Erb, DK
Fan, XH
Schreiber, NF
Illingworth, GD
Labbe, I
Leja, J
Lundgren, B
Magee, D
Marchesini, D
McCarthy, P
Momcheva, I
Muzzin, A
Quadri, R
Steidel, CC
Tal, T
Wake, D
Whitaker, KE
Williams, A
AF Brammer, Gabriel B.
van Dokkum, Pieter G.
Franx, Marijn
Fumagalli, Mattia
Patel, Shannon
Rix, Hans-Walter
Skelton, Rosalind E.
Kriek, Mariska
Nelson, Erica
Schmidt, Kasper B.
Bezanson, Rachel
da Cunha, Elisabete
Erb, Dawn K.
Fan, Xiaohui
Schreiber, Natascha Foerster
Illingworth, Garth D.
Labbe, Ivo
Leja, Joel
Lundgren, Britt
Magee, Dan
Marchesini, Danilo
McCarthy, Patrick
Momcheva, Ivelina
Muzzin, Adam
Quadri, Ryan
Steidel, Charles C.
Tal, Tomer
Wake, David
Whitaker, Katherine E.
Williams, Anna
TI 3D-HST: A WIDE-FIELD GRISM SPECTROSCOPIC SURVEY WITH THE HUBBLE SPACE
TELESCOPE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: high-redshift; surveys
ID ULTRA-DEEP-FIELD; EMISSION-LINE GALAXIES; STAR-FORMATION HISTORY;
LYMAN-BREAK GALAXIES; EXTRAGALACTIC LEGACY SURVEY; ACTIVE GALACTIC
NUCLEI; MEDIUM-BAND SURVEY; GREATER-THAN 1; GOODS-N FIELD; SIMILAR-TO 2
AB We present 3D-HST, a near-infrared spectroscopic Treasury program with the Hubble Space Telescope for studying the physical processes that shape galaxies in the distant universe. 3D-HST provides rest-frame optical spectra for a sample of similar to 7000 galaxies at 1 < z < 3.5, the epoch when similar to 60% of all star formation took place, the number density of quasars peaked, the first galaxies stopped forming stars, and the structural regularity that we see in galaxies today must have emerged. 3D-HST will cover three quarters (625 arcmin(2)) of the CANDELS Treasury survey area with two orbits of primary WFC3/G141 grism coverage and two to four orbits with the ACS/G800L grism in parallel. In the IR, these exposure times yield a continuum signal-to-noise ratio of similar to 5 per resolution element at H-140 similar to 23.1 and a 5 sigma emission-line sensitivity of similar to 5 x 10(-17) erg s(-1) cm(-2) for typical objects, improving by a factor of similar to 2 for compact sources in images with low sky background levels. The WFC3/G141 spectra provide continuous wavelength coverage from 1.1 to 1.6 mu m at a spatial resolution of similar to 0.'' 13, which, combined with their depth, makes them a unique resource for studying galaxy evolution. We present an overview of the preliminary reduction and analysis of the grism observations, including emission-line and redshift measurements from combined fits to the extracted grism spectra and photometry from ancillary multi-wavelength catalogs. The present analysis yields redshift estimates with a precision of sigma(z) = 0.0034(1 + z), or sigma(nu) approximate to 1000 km s(-1). We illustrate how the generalized nature of the survey yields near-infrared spectra of remarkable quality for many different types of objects, including a quasar at z = 4.7, quiescent galaxies at z similar to 2, and the most distant T-type brown dwarf star known. The combination of the CANDELS and 3D-HST surveys will provide the definitive imaging and spectroscopic data set for studies of the 1 < z < 3.5 universe until the launch of the James Webb Space Telescope.
C1 [Brammer, Gabriel B.] European So Observ, Santiago, Chile.
[van Dokkum, Pieter G.; Skelton, Rosalind E.; Nelson, Erica; Bezanson, Rachel; Leja, Joel; Lundgren, Britt; Momcheva, Ivelina; Tal, Tomer; Wake, David; Whitaker, Katherine E.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Franx, Marijn; Fumagalli, Mattia; Patel, Shannon; Labbe, Ivo; Muzzin, Adam] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Rix, Hans-Walter; Schmidt, Kasper B.; da Cunha, Elisabete] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Kriek, Mariska] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Erb, Dawn K.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA.
[Fan, Xiaohui] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Schreiber, Natascha Foerster] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Illingworth, Garth D.; Magee, Dan] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
[Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
[McCarthy, Patrick; Momcheva, Ivelina; Quadri, Ryan] Carnegie Observ, Pasadena, CA 91101 USA.
[Steidel, Charles C.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Williams, Anna] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
RP Brammer, GB (reprint author), European So Observ, Alonso de Cordova 3107,Casilla 19001, Santiago, Chile.
EM gbrammer@eso.org
RI Skelton, Rosalind/S-1845-2016;
OI Skelton, Rosalind/0000-0001-7393-3336; Leja, Joel/0000-0001-6755-1315;
da Cunha, Elisabete/0000-0001-9759-4797
FU Space Telescope Science Institute [HST-GO-12177]; European Commission;
European Research Council under the European Community [227749]
FX Prism Spectral Libraries, maintained by Adam Burgasser at
http://pono.ucsd.edu/adam/browndwarfs/spexprism. 3D-HST is supported in
part by grant HST-GO-12177 awarded by the Space Telescope Science
Institute. Additional funding for this research was provided by the
Marie Curie Actions of the European Commission (FP7-COFUND) and the
European Research Council under the European Community's Seventh
Framework Programme (FP7/2007-2013)/ERC grant agreement 227749.
NR 96
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUN
PY 2012
VL 200
IS 2
AR 13
DI 10.1088/0067-0049/200/2/13
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956KH
UT WOS:000305088000003
ER
PT J
AU Dalcanton, JJ
Williams, BF
Lang, D
Lauer, TR
Kalirai, JS
Seth, AC
Dolphin, A
Rosenfield, P
Weisz, DR
Bell, EF
Bianchi, LC
Boyer, ML
Caldwell, N
Dong, H
Dorman, CE
Gilbert, KM
Girardi, L
Gogarten, SM
Gordon, KD
Guhathakurta, P
Hodge, PW
Holtzman, JA
Johnson, LC
Larsen, SS
Lewis, A
Melbourne, JL
Olsen, KAG
Rix, HW
Rosema, K
Saha, A
Sarajedini, A
Skillman, ED
Stanek, KZ
AF Dalcanton, Julianne J.
Williams, Benjamin F.
Lang, Dustin
Lauer, Tod R.
Kalirai, Jason S.
Seth, Anil C.
Dolphin, Andrew
Rosenfield, Philip
Weisz, Daniel R.
Bell, Eric F.
Bianchi, Luciana C.
Boyer, Martha L.
Caldwell, Nelson
Dong, Hui
Dorman, Claire E.
Gilbert, Karoline M.
Girardi, Leo
Gogarten, Stephanie M.
Gordon, Karl D.
Guhathakurta, Puragra
Hodge, Paul W.
Holtzman, Jon A.
Johnson, L. Clifton
Larsen, Soren S.
Lewis, Alexia
Melbourne, Jason L.
Olsen, Knut A. G.
Rix, Hans-Walter
Rosema, Keith
Saha, Abhijit
Sarajedini, Ata
Skillman, Evan D.
Stanek, Krzysztof Z.
TI THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: individual (M31); galaxies: stellar content; stars: general;
stars: imaging
ID STAR-FORMATION HISTORY; BRIGHT YOUNG CLUSTERS; RED GIANT STARS; H-II
REGIONS; PERIOD-LUMINOSITY RELATION; SPACE-TELESCOPE SURVEY; LOCAL GROUP
GALAXIES; SUPER-NOVA REMNANTS; STELLAR CONTENT; OUTER DISK
AB The Panchromatic Hubble Andromeda Treasury is an ongoing Hubble Space Telescope Multi-Cycle Treasury program to image similar to 1/3 of M31's star-forming disk in six filters, spanning from the ultraviolet (UV) to the near-infrared (NIR). We use the Wide Field Camera 3 (WFC3) and Advanced Camera for Surveys (ACS) to resolve the galaxy into millions of individual stars with projected radii from 0 to 20 kpc. The full survey will cover a contiguous 0.5 deg(2)area in 828 orbits. Imaging is being obtained in the F275W and F336W filters on the WFC3/UVIS camera, F475W and F814W on ACS/WFC, and F110W and F160W on WFC3/IR. The resulting wavelength coverage gives excellent constraints on stellar temperature, bolometric luminosity, and extinction for most spectral types. The data produce photometry with a signal-to-noise ratio of 4 at m(F275W) = 25.1, m(F336W) = 24.9, m(F475W) = 27.9, m(F814W) = 27.1, m(F110W) = 25.5, and m(F160W) = 24.6 for single pointings in the uncrowded outer disk; in the inner disk, however, the optical and NIR data are crowding limited, and the deepest reliable magnitudes are up to 5 mag brighter. Observations are carried out in two orbits per pointing, split between WFC3/UVIS and WFC3/IR cameras in primary mode, with ACS/WFC run in parallel. All pointings are dithered to produce Nyquist-sampled images in F475W, F814W, and F160W. We describe the observing strategy, photometry, astrometry, and data products available for the survey, along with extensive testing of photometric stability, crowding errors, spatially dependent photometric biases, and telescope pointing control. We also report on initial fits to the structure of M31's disk, derived from the density of red giant branch stars, in a way that is independent of assumed mass-to-light ratios and is robust to variations in dust extinction. These fits also show that the 10 kpc ring is not just a region of enhanced recent star formation, but is instead a dynamical structure containing a significant overdensity of stars with ages > 1Gyr.
C1 [Dalcanton, Julianne J.; Williams, Benjamin F.; Rosenfield, Philip; Weisz, Daniel R.; Gilbert, Karoline M.; Gogarten, Stephanie M.; Hodge, Paul W.; Johnson, L. Clifton; Lewis, Alexia] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Lang, Dustin] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Lauer, Tod R.; Dong, Hui; Olsen, Knut A. G.; Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Kalirai, Jason S.; Boyer, Martha L.; Gordon, Karl D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Seth, Anil C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Dolphin, Andrew] Raytheon Co, Tucson, AZ 85756 USA.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Bianchi, Luciana C.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dorman, Claire E.; Guhathakurta, Puragra] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Girardi, Leo] Osservatorio Astron Padova INAF, I-35122 Padua, Italy.
[Holtzman, Jon A.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Larsen, Soren S.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Melbourne, Jason L.] CALTECH, Caltech Opt Observ, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Rosema, Keith] Random Walk Grp, Seattle, WA 98105 USA.
[Sarajedini, Ata] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Skillman, Evan D.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Stanek, Krzysztof Z.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
RP Dalcanton, JJ (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
OI Gogarten, Stephanie/0000-0002-7231-9745; Rosenfield,
Philip/0000-0001-9306-6049; Johnson, Lent/0000-0001-6421-0953; Bell,
Eric/0000-0002-5564-9873
FU Space Telescope Science Institute [GO-12055]; [ASI-INAF I/009/10/0]
FX The authors are very happy to acknowledge discussions with Jay Anderson,
Tom Brown, Suzanne Hawley, and Alesandro Bressan. We are grateful to
Stefano Casertano for sharing the code to produce the exposure time maps
in Figure 5, Alesandro Bressan for providing the tracks plotted in
Figure 24, Jean-Charles Cuillandre for allowing us to use his CFHT
imaging to tie our data to a global astrometric frame, to Pauline Barmby
for providing us the Spitzer IRAC images, and the anonymous referee for
an extremely knowledgeable and prompt report. The project has received
superb support from personnel at the Space Telescope Science Institute,
including Alison Vick, Ken Sembach, Neill Reid, and the ACS and WFC3
instrument teams. Zolt Levay is particularly thanked for the beautiful
visualizations found in Figure 6, which far surpassed anything we were
able to generate on our own. Stan Vlcek, Sarah Garner, and Pat Taylor at
UW have been instrumental in helping with logistics for the project.
This work was supported by the Space Telescope Science Institute through
GO-12055. L.G. acknowledges support from contract ASI-INAF I/009/10/0.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUN
PY 2012
VL 200
IS 2
AR 18
DI 10.1088/0067-0049/200/2/18
PG 37
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956KH
UT WOS:000305088000008
ER
PT J
AU Hicken, M
Challis, P
Kirshner, RP
Rest, A
Cramer, CE
Wood-Vasey, WM
Bakos, G
Berlind, P
Brown, WR
Caldwell, N
Calkins, M
Currie, T
de Kleer, K
Esquerdo, G
Everett, M
Falco, E
Fernandez, J
Friedman, AS
Groner, T
Hartman, J
Holman, MJ
Hutchins, R
Keys, S
Kipping, D
Latham, D
Marion, GH
Narayan, G
Pahre, M
Pal, A
Peters, W
Perumpilly, G
Ripman, B
Sipocz, B
Szentgyorgyi, A
Tang, SM
Torres, MAP
Vaz, A
Wolk, S
Zezas, A
AF Hicken, Malcolm
Challis, Peter
Kirshner, Robert P.
Rest, Armin
Cramer, Claire E.
Wood-Vasey, W. Michael
Bakos, Gaspar
Berlind, Perry
Brown, Warren R.
Caldwell, Nelson
Calkins, Mike
Currie, Thayne
de Kleer, Kathy
Esquerdo, Gil
Everett, Mark
Falco, Emilio
Fernandez, Jose
Friedman, Andrew S.
Groner, Ted
Hartman, Joel
Holman, Matthew J.
Hutchins, Robert
Keys, Sonia
Kipping, David
Latham, Dave
Marion, George H.
Narayan, Gautham
Pahre, Michael
Pal, Andras
Peters, Wayne
Perumpilly, Gopakumar
Ripman, Ben
Sipocz, Brigitta
Szentgyorgyi, Andrew
Tang, Sumin
Torres, Manuel A. P.
Vaz, Amali
Wolk, Scott
Zezas, Andreas
TI CfA4: LIGHT CURVES FOR 94 TYPE Ia SUPERNOVAE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE supernovae: general
ID HUBBLE-SPACE-TELESCOPE; DARK-ENERGY CONSTRAINTS; PHOTOMETRY DATA
RELEASE; INFRARED PHOTOMETRY; LUMINOSITY INDICATORS; IMAGE SUBTRACTION;
HOST GALAXIES; CONSTANT; MAGNITUDES; UNIVERSE
AB We present multi-band optical photometry of 94 spectroscopically confirmed Type Ia supernovae (SNe Ia) in the redshift range 0.0055-0.073, obtained between 2006 and 2011. There are a total of 5522 light-curve points. We show that our natural-system SN photometry has a precision of less than or similar to 0.03 mag in BV r'i', less than or similar to 0.06 mag in u', and less than or similar to 0.07 mag in U for points brighter than 17.5 mag and estimate that it has a systematic uncertainty of 0.014, 0.010, 0.012, 0.014, 0.046, and 0.073 mag in BV r'i'u'U, respectively. Comparisons of our standard-system photometry with published SN Ia light curves and comparison stars reveal mean agreement across samples in the range of similar to 0.00-0.03 mag. We discuss the recent measurements of our telescope-plus-detector throughput by direct monochromatic illumination by Cramer et al. This technique measures the whole optical path through the telescope, auxiliary optics, filters, and detector under the same conditions used to make SN measurements. Extremely well characterized natural-system passbands (both in wavelength and over time) are crucial for the next generation of SN Ia photometry to reach the 0.01 mag accuracy level. The current sample of low-z SNe Ia is now sufficiently large to remove most of the statistical sampling error from the dark-energy error budget. But pursuing the dark-energy systematic errors by determining highly accurate detector passbands, combining optical and near-infrared (NIR) photometry and spectra, using the nearby sample to illuminate the population properties of SNe Ia, and measuring the local departures from the Hubble flow will benefit from larger, carefully measured nearby samples.
C1 [Hicken, Malcolm; Challis, Peter; Kirshner, Robert P.; Bakos, Gaspar; Berlind, Perry; Brown, Warren R.; Caldwell, Nelson; Calkins, Mike; Falco, Emilio; Fernandez, Jose; Friedman, Andrew S.; Groner, Ted; Hartman, Joel; Holman, Matthew J.; Hutchins, Robert; Keys, Sonia; Kipping, David; Latham, Dave; Marion, George H.; Narayan, Gautham; Pahre, Michael; Pal, Andras; Peters, Wayne; Ripman, Ben; Sipocz, Brigitta; Szentgyorgyi, Andrew; Tang, Sumin; Torres, Manuel A. P.; Wolk, Scott; Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rest, Armin] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Cramer, Claire E.] NIST, Gaithersburg, MD 20899 USA.
[Wood-Vasey, W. Michael] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Bakos, Gaspar; Hartman, Joel] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08542 USA.
[Currie, Thayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[de Kleer, Kathy] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Esquerdo, Gil; Everett, Mark] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Perumpilly, Gopakumar] Univ S Dakota, Dept Phys, Vermillion, SD 57069 USA.
[Vaz, Amali] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
RP Hicken, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mhicken@cfa.harvard.edu
RI Friedman, Andrew/I-4691-2013; Zezas, Andreas/C-7543-2011;
OI Friedman, Andrew/0000-0003-1334-039X; Zezas,
Andreas/0000-0001-8952-676X; Wolk, Scott/0000-0002-0826-9261; Narayan,
Gautham/0000-0001-6022-0484; Hartman, Joel/0000-0001-8732-6166
FU NSF [AST0606772, AST0907903]
FX We thank the staff at FLWO for their dedicated work in maintaining the
1.2 m telescope and instruments. We also thank M. Stritzinger, W. Li,
and M. Ganeshalingam for help in comparing the CfA4 sample with the CSP2
and LOSS samples. Finally, we appreciate discussions with K. Mandel.
This work has been supported, in part, by NSF grants AST0606772 and
AST0907903 to Harvard University.
NR 72
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUN
PY 2012
VL 200
IS 2
AR 12
DI 10.1088/0067-0049/200/2/12
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956KH
UT WOS:000305088000002
ER
PT J
AU Trichas, M
Green, PJ
Silverman, JD
Aldcroft, T
Barkhouse, W
Cameron, RA
Constantin, A
Ellison, SL
Foltz, C
Haggard, D
Jannuzi, BT
Kim, DW
Marshall, HL
Mossman, A
Perez, LM
Romero-Colmenero, E
Ruiz, A
Smith, MG
Smith, PS
Torres, G
Wik, DR
Wilkes, BJ
Wolfgang, A
AF Trichas, Markos
Green, Paul J.
Silverman, John D.
Aldcroft, Tom
Barkhouse, Wayne
Cameron, Robert A.
Constantin, Anca
Ellison, Sara L.
Foltz, Craig
Haggard, Daryl
Jannuzi, Buell T.
Kim, Dong-Woo
Marshall, Herman L.
Mossman, Amy
Perez, Laura M.
Romero-Colmenero, Encarni
Ruiz, Angel
Smith, Malcolm G.
Smith, Paul S.
Torres, Guillermo
Wik, Daniel R.
Wilkes, Belinda J.
Wolfgang, Angie
TI THE CHANDRA MULTI-WAVELENGTH PROJECT: OPTICAL SPECTROSCOPY AND THE
BROADBAND SPECTRAL ENERGY DISTRIBUTIONS OF X-RAY-SELECTED AGNs
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: evolution; galaxies: Seyfert; galaxies: starburst; quasars:
general; techniques: spectroscopic; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; DIGITAL-SKY-SURVEY;
ULTRALUMINOUS INFRARED GALAXIES; QUASAR LUMINOSITY FUNCTION;
STAR-FORMATION; BLACK-HOLES; HELLAS2XMM SURVEY; REDSHIFT SURVEY; SOURCE
CATALOGS
AB From optical spectroscopy of X-ray sources observed as part of the Chandra Multi-wavelength Project (ChaMP), we present redshifts and classifications for a total of 1569 Chandra sources from our targeted spectroscopic follow-up using the FLWO/1.5 m, SAAO/1.9 m, WIYN 3.5 m, CTIO/4 m, KPNO/4 m, Magellan/6.5 m, MMT/6.5 m, and Gemini/8 m telescopes, and from archival Sloan Digital Sky Survey (SDSS) spectroscopy. We classify the optical counterparts as 50% broad-line active galactic nuclei (AGNs), 16% emission line galaxies, 14% absorption line galaxies, and 20% stars. We detect QSOs out to z similar to 5.5 and galaxies out to z similar to 3. We have compiled extensive photometry, including X-ray (ChaMP), ultraviolet (GALEX), optical (SDSS and ChaMP-NOAO/MOSAIC follow-up), near-infrared (UKIDSS, Two Micron All Sky Survey, and ChaMP-CTIO/ISPI follow-up), mid-infrared (WISE), and radio (FIRST and NVSS) bands. Together with our spectroscopic information, this enables us to derive detailed spectral energy distributions (SEDs) for our extragalactic sources. We fit a variety of template SEDs to determine bolometric luminosities, and to constrain AGNs and starburst components where both are present. While similar to 58% of X-ray Seyferts (10(42) erg s(-1) < L2-10 keV < 10(44) erg s(-1)) require a starburst event (>5% starburst contribution to bolometric luminosity) to fit observed photometry only 26% of the X-ray QSO (L2-10 keV > 10(44) erg s(-1)) population appear to have some kind of star formation contribution. This is significantly lower than for the Seyferts, especially if we take into account torus contamination at z > 1 where the majority of our X-ray QSOs lie. In addition, we observe a rapid drop of the percentage of starburst contribution as X-ray luminosity increases. This is consistent with the quenching of star formation by powerful QSOs, as predicted by the merger model, or with a time lag between the peak of star formation and QSO activity. We have tested the hypothesis that there should be a strong connection between X-ray obscuration and star formation but we do not find any association between X-ray column density and star formation rate both in the general population or the star-forming X-ray Seyferts. Our large compilation also allows us to report here the identification of 81 X-ray Bright Optically inactive Galaxies, 78 z > 3 X-ray sources, and eight Type-2 QSO candidates. Also, we have identified the highest redshift (z = 5.4135) X-ray-selected QSO with optical spectroscopy.
C1 [Trichas, Markos; Green, Paul J.; Aldcroft, Tom; Kim, Dong-Woo; Mossman, Amy; Torres, Guillermo; Wilkes, Belinda J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Silverman, John D.] Univ Tokyo, Inst Phys & Math Universe IPMU, Kashiwa, Chiba 2778568, Japan.
[Barkhouse, Wayne] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA.
[Cameron, Robert A.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Cameron, Robert A.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Constantin, Anca] James Madison Univ, Dept Phys & Astron, PHCH, Harrisonburg, VA 22807 USA.
[Ellison, Sara L.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada.
[Foltz, Craig] Natl Sci Fdn, Div Astron Sci, Arlington, VA 22230 USA.
[Haggard, Daryl] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA.
[Jannuzi, Buell T.] Kitt Peak Natl Observ, NOAO, Tucson, AZ 85726 USA.
[Marshall, Herman L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Perez, Laura M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Romero-Colmenero, Encarni] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Ruiz, Angel] Osservatorio Astron Brera INAF, Milan, Italy.
[Smith, Malcolm G.] Cerro Tololo Interamer Observ, La Serena, Chile.
[Smith, Paul S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Wik, Daniel R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wolfgang, Angie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
RP Trichas, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mtrichas@cfa.harvard.edu
RI Ruiz, Angel/B-4914-2008;
OI Ruiz, Angel/0000-0002-3352-4383; Constantin, Anca/0000-0002-2441-1619;
Wilkes, Belinda/0000-0003-1809-2364
FU National Aeronautics and Space Administration [AR9-0020X, AR1-12016X,
NAS8-03060]
FX The authors thank Francesca Civano and Hagai Netzer for their useful
comments. Support for this work was provided by the National Aeronautics
and Space Administration through Chandra Award nos. AR9-0020X and
AR1-12016X, issued by the Chandra X-ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of the National Aeronautics Space Administration under contract
NAS8-03060.
NR 92
TC 26
Z9 26
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUN
PY 2012
VL 200
IS 2
AR 17
DI 10.1088/0067-0049/200/2/17
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956KH
UT WOS:000305088000007
ER
PT J
AU Bain, DJ
Green, MB
Campbell, JL
Chamblee, JF
Chaoka, S
Fraterrigo, JM
Kaushal, SS
Martin, SL
Jordan, TE
Parolari, AJ
Sobczak, WV
Weller, DE
Wollheim, WM
Boose, ER
Duncan, JM
Gettel, GM
Hall, BR
Kumar, P
Thompson, JR
Vose, JM
Elliott, EM
Leigh, DS
AF Bain, Daniel J.
Green, Mark B.
Campbell, John L.
Chamblee, John F.
Chaoka, Sayo
Fraterrigo, Jennifer M.
Kaushal, Sujay S.
Martin, Sherry L.
Jordan, Thomas E.
Parolari, Anthony J.
Sobczak, William V.
Weller, Donald E.
Wollheim, Wilfred M.
Boose, Emery R.
Duncan, Jonathan M.
Gettel, Gretchen M.
Hall, Brian R.
Kumar, Praveen
Thompson, Jonathan R.
Vose, James M.
Elliott, Emily M.
Leigh, David S.
TI Legacy Effects in Material Flux: Structural Catchment Changes Predate
Long-Term Studies
SO BIOSCIENCE
LA English
DT Article
DE legacy effect; long-term studies; structural and signal legacy effects;
sedimentation
ID RHODE RIVER WATERSHEDS; NORTHERN HARDWOOD FOREST; LAND-USE CHANGE;
AGRICULTURAL ABANDONMENT; AIR-TEMPERATURE; SOIL-NITROGEN; FRESH-WATER;
CARBON; PRECIPITATION; DISCHARGES
AB Legacy effects of past land use and disturbance are increasingly recognized, yet consistent definitions of and criteria for defining them do not exist. To address this gap in biological- and ecosystem-assessment frameworks, we propose a general metric for evaluating potential legacy effects, which are computed by normalizing altered system function persistence with duration of disturbance. We also propose two distinct legacy-effect categories: signal effects from lags in transport and structural effects from physical landscape changes. Using flux records for water, sediment, nitrogen, and carbon from long-term study sites in the eastern United States from 1500 to 2000, we identify gaps in our understanding of legacy effects and reveal that changes in basin sediment dynamics precede instrumented records. These sediment dynamics are not generally incorporated into interpretations of contemporary records, although their potential legacy effects are substantial. The identification of legacy effects may prove to be a fundamental component of landscape management and effective conservation and restoration practice.
C1 [Bain, Daniel J.; Elliott, Emily M.] Univ Pittsburgh, Dept Geol & Planetary Sci, Pittsburgh, PA 15260 USA.
[Green, Mark B.] Plymouth State Univ, Ctr Environm, Plymouth, NH USA.
[Green, Mark B.; Campbell, John L.] US Forest Serv, No Res Stn, Durham, NH USA.
[Chaoka, Sayo; Kumar, Praveen] Univ Illinois, Dept Civil & Environm Engn, Urbana, IL 61801 USA.
[Fraterrigo, Jennifer M.] Univ Illinois, Dept Nat Resources & Environm Sci, Urbana, IL 61801 USA.
[Kaushal, Sujay S.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA.
[Kaushal, Sujay S.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Martin, Sherry L.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA.
[Jordan, Thomas E.; Weller, Donald E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Parolari, Anthony J.] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA.
[Sobczak, William V.] Coll Holy Cross, Dept Biol, Worcester, MA 01610 USA.
[Wollheim, Wilfred M.] Univ New Hampshire, Dept Nat Resources & Environm, Durham, NH 03824 USA.
[Wollheim, Wilfred M.] Univ New Hampshire, Environm & Complex Syst Res Ctr, Durham, NH 03824 USA.
[Boose, Emery R.; Hall, Brian R.] Harvard Univ Harvard Forest, Petersham, MA USA.
[Duncan, Jonathan M.] Univ N Carolina, Dept Geog, Chapel Hill, NC USA.
[Gettel, Gretchen M.] United Nations Educ Sci & Cultural Org, Int Inst Infrastruct Hydraul & Environm Engn, Delft, Netherlands.
[Thompson, Jonathan R.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA USA.
[Vose, James M.] US Forest Serv, So Res Stn, Otto, NC USA.
[Leigh, David S.] Univ Georgia, Dept Geog, Athens, GA 30602 USA.
RP Bain, DJ (reprint author), Univ Pittsburgh, Dept Geol & Planetary Sci, Pittsburgh, PA 15260 USA.
EM dbain@pitt.edu
RI Kumar, Praveen/D-2036-2010; Chamblee, John/A-7168-2013; Elliott, Emily
/E-8122-2011; Bain, Daniel/G-3055-2013; Parolari, Anthony/I-5137-2013;
Gettel, Gretchen/M-8983-2013; Kaushal, Sujay/G-1062-2013;
OI Kumar, Praveen/0000-0002-4787-0308; Chamblee, John/0000-0002-7776-0302;
Elliott, Emily /0000-0002-9653-1513; Gettel,
Gretchen/0000-0002-9288-1583; Kaushal, Sujay/0000-0003-0834-9189; Green,
Mark/0000-0002-7415-7209; Campbell, John/0000-0003-4956-1696; Weller,
Donald/0000-0002-7629-5437
FU Long Term Ecological Research Network Office (National Science
Foundation [NSF]) [DEB-0236154]; NSF Division of Earth Sciences
[0854957]; NSF's Long-Term Ecological Research Network [DEB-1027188,
DEB-0823293, DEB-1114804, DEB-0620443, NSF-OCE-0423565,
NSF-OCE-1058747]; NSF [DEB-79-11563, DEB-82072-12, CEE-8219615,
BSR-8316948, BSR-8615902, BSR-8905219, BSR-891703, BSR-9085219,
DEB-92-06811, DEB-93-17968]; National Oceanic and Atmospheric
Administration [NA66RG0129]; US Environmental Protection Agency [804536]
FX This manuscript grew out of a working group sponsored by the Long Term
Ecological Research Network Office (National Science Foundation [NSF]
Cooperative Agreement no. DEB-0236154), with supplementary funding from
NSF Division of Earth Sciences grant no. 0854957 to the City University
of New York. This material is based on work at Long Term Ecological
Research sites supported by the NSF's Long-Term Ecological Research
Network under the following grant numbers: DEB-1027188 to the Baltimore
Ecosystem Study, DEB-0823293 to the Coweeta Hydrologic Laboratory,
DEB-1114804 to the Hubbard Brook Experimental Forest, DEB-0620443 to the
Harvard Forest site, and NSF-OCE-0423565 and NSF-OCE-1058747 to the Plum
Island Ecosystem. The Smithsonian Environmental Research Center
watershed discharge data were collected with support from the NSF (grant
nos. DEB-79-11563, DEB-82072-12, CEE-8219615, BSR-8316948, BSR-8615902,
BSR-8905219, BSR-891703, BSR-9085219, DEB-92-06811, and DEB-93-17968),
from the National Oceanic and Atmospheric Administration Coastal Oceans
Program (grant no. NA66RG0129), the US Environmental Protection Agency
(grant no. 804536), and the Smithsonian Institution Environmental
Sciences Program. The careful comments of three anonymous reviewers
improved the article.
NR 57
TC 26
Z9 28
U1 2
U2 59
PU AMER INST BIOLOGICAL SCI
PI WASHINGTON
PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA
SN 0006-3568
J9 BIOSCIENCE
JI Bioscience
PD JUN
PY 2012
VL 62
IS 6
BP 575
EP 584
DI 10.1525/bio.2012.62.6.8
PG 10
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 958TB
UT WOS:000305262500008
ER
PT J
AU Altieri, AH
Bertness, MD
Coverdale, TC
Herrmann, NC
Angelini, C
AF Altieri, Andrew H.
Bertness, Mark D.
Coverdale, Tyler C.
Herrmann, Nicholas C.
Angelini, Christine
TI A trophic cascade triggers collapse of a salt-marsh ecosystem with
intensive recreational fishing
SO ECOLOGY
LA English
DT Article
DE Cape Cod, Massachusetts, USA; conservation; food web; human impacts;
marine; overfishing; plant-herbivore interactions; recreational fishing;
Spartina alterniflora; top-down control; top predator; trophic cascade
ID CORAL-REEFS; CALLINECTES-SAPIDUS; CONSUMER CONTROL; CHESAPEAKE BAY;
HUMAN IMPACTS; ST-LAWRENCE; NEW-ENGLAND; BLUE CRABS; DIE-OFF; FISHERIES
AB Overexploitation of predators has been linked to the collapse of a growing number of shallow-water marine ecosystems. However, salt-marsh ecosystems are often viewed and managed as systems controlled by physical processes, despite recent evidence for herbivore-driven die-off of marsh vegetation. Here we use field observations, experiments, and historical records at 14 sites to examine whether the recently reported die-off of northwestern Atlantic salt marshes is associated with the cascading effects of predator dynamics and intensive recreational fishing activity. We found that the localized depletion of top predators at sites accessible to recreational anglers has triggered the proliferation of herbivorous crabs, which in turn results in runaway consumption of marsh vegetation. This suggests that overfishing may be a general mechanism underlying the consumer-driven die-off of salt marshes spreading throughout the western Atlantic. Our findings support the emerging realization that consumers play a dominant role in regulating marine plant communities and can lead to ecosystem collapse when their impacts are amplified by human activities, including recreational fishing.
C1 [Altieri, Andrew H.; Bertness, Mark D.; Coverdale, Tyler C.; Herrmann, Nicholas C.; Angelini, Christine] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA.
RP Altieri, AH (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
EM AltieriA@si.edu
OI Coverdale, Tyler/0000-0003-0910-9187
NR 61
TC 53
Z9 53
U1 18
U2 169
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 0012-9658
J9 ECOLOGY
JI Ecology
PD JUN
PY 2012
VL 93
IS 6
BP 1402
EP 1410
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 959EV
UT WOS:000305296600017
PM 22834380
ER
PT J
AU Souto, T
Ticktin, T
AF Souto, Tamia
Ticktin, Tamara
TI Understanding Interrelationships Among Predictors (Age, Gender, and
Origin) of Local Ecological Knowledge
SO ECONOMIC BOTANY
LA English
DT Article
DE Local ecological knowledge; mestizo; Venezuela; multiple regression
analysis
ID MEDICINAL-PLANTS; BRAZIL; FOREST; ETHNOBOTANY; DIVERSITY; COMMUNITIES;
CONSERVATION; NICARAGUA; AMAZONIA; COAST
AB Understanding Interrelationships among Predictors (Age, Gender, and Origin) of Local Ecological Knowledge. Understanding which factors predict local ecological knowledge can provide insight into how this knowledge is learned and how it may change in the future. We assess how knowledge of both useful plants and plant natural history vary according to gender, age, and origin in mestizo communities in Venezuela's Caura Basin. Two sets of structured questionnaires were carried out with a total of 83 adults in three communities. Multiple regression analyses were used to identify the predictors of knowledge of 6 plant-use categories and natural history knowledge of 12 plant species. Gender, age, and origin (a parts per thousand yen2 generations in the Caura vs. foreign-born) were all important predictors of knowledge of useful plants and natural history; however, their importance differed between the two types of knowledge. Origin was a more important predictor of knowledge of useful plants, whereas age was more important in predicting knowledge of natural history. This suggests differences in how each type of knowledge is learned and transmitted. Gender was an important predictor variable in most models, reflecting gender roles in the Caura mestizo communities. Also, for most categories of plant-use knowledge, the interactions among predictors were significant, indicating that the effect of one variable depended on the level of the other. These results illustrate how overlooking interactions among variables, as most studies to date have done, can risk misinterpretation of results by simplifying complex situations.
C1 [Souto, Tamia; Ticktin, Tamara] Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA.
[Souto, Tamia] Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA.
RP Souto, T (reprint author), Univ Hawaii Manoa, Dept Bot, 3190 Maile Way, Honolulu, HI 96822 USA.
EM soutot@si.edu
FU National Science Foundation; Wildlife Conservation Society
FX The authors are very grateful to all the wonderful families of
Trincheras, Jabillal, and Puerto Cabello for their time and for sharing
their ethnobotanical knowledge of the Caura forests with us. Special
thanks to Enrique Bastidas and his family for their support,
collaboration, and participation during the field work, and to H.
McMillen and O. Gaoue for their help during the analysis and writing of
this paper. We also thank two anonymous reviewers for their useful
suggestions for improving a previous version of this manuscript. This
research was funded by a National Science Foundation Graduate Research
Fellowship Award and a Wildlife Conservation Society Award to T. S.
NR 35
TC 10
Z9 11
U1 1
U2 22
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0013-0001
J9 ECON BOT
JI Econ. Bot.
PD JUN
PY 2012
VL 66
IS 2
BP 149
EP 164
DI 10.1007/s12231-012-9194-3
PG 16
WC Plant Sciences
SC Plant Sciences
GA 958IT
UT WOS:000305230700004
ER
PT J
AU Kim, M
Nam, SW
Shin, W
Coats, DW
Park, MG
AF Kim, Miran
Nam, Seung Won
Shin, Woongghi
Coats, D. Wayne
Park, Myung Gil
TI DINOPHYSIS CAUDATA (DINOPHYCEAE) SEQUESTERS AND RETAINS PLASTIDS FROM
THE MIXOTROPHIC CILIATE PREY MESODINIUM RUBRUM
SO JOURNAL OF PHYCOLOGY
LA English
DT Article
DE Dinophysis caudata; Mesodinium rubrum; kleptoplastid; plastid;
single-cell TEM; ultrastructure
ID MYRIONECTA-RUBRA; MOLECULAR EVIDENCE; GENETIC ANALYSES; DINOFLAGELLATE;
ACUMINATA; CHLOROPLASTS; KLEPTOPLASTIDY; ENDOSYMBIONT; STRAINS; FORTII
AB PhototrophicDinophysis Ehrenberg species are well known to have chloroplasts of a cryptophyte origin, more specifically of the cryptophyte genus complex Teleaulax/Geminigera. Nonetheless, whether chloroplasts of phototrophicDinophysis are permanent plastids or periodically derived kleptoplastids (stolen chloroplasts) has not been confirmed. Indeed, molecular sequence data and ultrastructural data lead to contradictory interpretations about the status of Dinophysis plastids. Here, we used established cultures of D. caudata strain DC-LOHABE01 and M. rubrum strain MR-MAL01 to address the status of Dinophysis plastids. Our approach was to experimentally generate D. caudata with green plastids and then follow the ingestion and fate of reddish-brown prey plastids using light microscopy, time-lapse videography, and single-cell TEM. Our results for D. caudata resolve the apparent discrepancy between morphological and molecular data by showing that plastids acquired when feeding on M. rubrum are structurally modified and retained as stellate compound chloroplasts characteristic of Dinophysis species.
C1 [Kim, Miran; Park, Myung Gil] Chonnam Natl Univ, Dept Oceanog, LOHABE, Kwangju 500757, South Korea.
[Nam, Seung Won; Shin, Woongghi] Chungnam Natl Univ, Dept Biol Sci, Taejon 306764, South Korea.
[Coats, D. Wayne] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Park, MG (reprint author), Chonnam Natl Univ, Dept Oceanog, LOHABE, Kwangju 500757, South Korea.
EM mpark@chonnam.ac.kr
RI Shin, Woongghi/D-5677-2013
FU NRF; MEST [2011-0015820]; National Research Foundation of Korea; Korean
Government (MEST) [NRF-C1ABA001-2010-0020700]
FX This work was supported by Mid-career Researcher Program through NRF
grant funded by the MEST (2011-0015820) and the National Research
Foundation of Korea Grant funded by the Korean Government (MEST)
(NRF-C1ABA001-2010-0020700) (M.G.P).
NR 33
TC 23
Z9 23
U1 0
U2 23
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD JUN
PY 2012
VL 48
IS 3
BP 569
EP 579
DI 10.1111/j.1529-8817.2012.01150.x
PG 11
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 952RP
UT WOS:000304810200008
PM 27011072
ER
PT J
AU Servillat, M
Heinke, CO
Ho, WCG
Grindlay, JE
Hong, J
van den Berg, M
Bogdanov, S
AF Servillat, M.
Heinke, C. O.
Ho, W. C. G.
Grindlay, J. E.
Hong, J.
van den Berg, M.
Bogdanov, S.
TI Neutron star atmosphere composition: the quiescent, low-mass X-ray
binary in the globular cluster M28
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE equation of state; stars: neutron; globular clusters: individual: M28;
globular clusters: individual: NGC 6626; X-rays: binaries; X-rays:
individual: CXOGlb J182432; 8-245208
ID SPACE-TELESCOPE OBSERVATIONS; EQUATION-OF-STATE; THERMAL EMISSION;
XMM-NEWTON; OPTICAL COUNTERPART; INTERSTELLAR-MEDIUM; OMEGA-CENTAURI;
MAXIMUM MASS; MILKY-WAY; NGC 6440
AB Using deep Chandra observations of the globular cluster M28, we study the quiescent X-ray emission of a neutron star in a low-mass X-ray binary in order to constrain the chemical composition of the neutron star atmosphere and the equation of state of dense matter. We fit the spectrum with different neutron star atmosphere models composed of hydrogen, helium or carbon. The parameter values obtained with the carbon model are unphysical and such a model can be ruled out. Hydrogen and helium models give realistic parameter values for a neutron star, and the derived mass and radius are clearly distinct depending on the composition of the atmosphere. The hydrogen model gives masses/radii consistent with the canonical values of 1.4 M? and 10 km, and would allow for the presence of exotic matter inside neutron stars. On the other hand, the helium model provides solutions with higher masses/radii, consistent with the stiffest equations of state. Measurements of neutron star masses/radii by spectral fitting should consider the possibility of heavier element atmospheres, which produce larger masses/radii for the same data, unless the composition of the accretor is known independently.
C1 [Servillat, M.; Grindlay, J. E.; Hong, J.; van den Berg, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Servillat, M.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM CEA DSM IRFU SAp, F-91191 Gif Sur Yvette, France.
[Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Ho, W. C. G.] Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England.
[van den Berg, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Bogdanov, S.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
RP Servillat, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mservillat@cfa.harvard.edu
OI Bogdanov, Slavko/0000-0002-9870-2742; Heinke, Craig/0000-0003-3944-6109
FU NASA [GO0-11063X]; NSF [AST-0909073]; Centre National d'Etudes Spatiales
(CNES); NSERC; Ingenuity New Faculty Award; STFC in the UK
FX We thank the referee for their careful reading and useful suggestions
that strengthened the paper. MS acknowledges supports from NASA/Chandra
grant GO0-11063X, NSF grant AST-0909073 and the Centre National d'Etudes
Spatiales (CNES). COH is supported by NSERC and an Ingenuity New Faculty
Award. WCGH appreciates the use of the computer facilities at KIPAC and
acknowledges support from STFC in the UK.
NR 59
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Z9 28
U1 0
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN
PY 2012
VL 423
IS 2
BP 1556
EP 1561
DI 10.1111/j.1365-2966.2012.20976.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956DU
UT WOS:000305070900044
ER
PT J
AU Fontani, F
Palau, A
Busquet, G
Isella, A
Estalella, R
Sanchez-Monge, A
Caselli, P
Zhang, Q
AF Fontani, F.
Palau, Aina
Busquet, G.
Isella, A.
Estalella, R.
Sanchez-Monge, A.
Caselli, P.
Zhang, Q.
TI Dense gas in IRAS 20343+4129: an ultracompact H ii region caught in the
act of creating a cavity
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; ISM: individual objects: IRAS 20343+4129; ISM:
molecules
ID MASSIVE STAR-FORMATION; YOUNG STELLAR OBJECTS; INITIAL CONDITIONS;
PROTOSTELLAR CANDIDATES; CONTINUUM OBSERVATIONS; INVERSION TRANSITION;
CORES; AMMONIA; NH3; CLOUD
AB The intermediate- to high-mass star-forming region IRAS 20343+4129 is an excellent laboratory to study the influence of high- and intermediate-mass young stellar objects on nearby starless dense cores, and investigate for possible implications in the clustered star formation process. We present 3 mm observations of continuum and rotational transitions of several molecular species (C2H, c-C3H2, N2H+, NH2D) obtained with the Combined Array for Research in Millimetre-wave Astronomy, as well as 1.3 cm continuum and NH3 observations carried out with the Very Large Array, to reveal the properties of the dense gas. We confirm undoubtedly previous claims of an expanding cavity created by an ultracompact H ii region associated with a young B2 zero-age main sequence (ZAMS) star. The dense gas surrounding the cavity is distributed in a filament that seems squeezed in between the cavity and a collimated outflow associated with an intermediate-mass protostar. We have identified 5 mm continuum condensations in the filament. All of them show column densities consistent with potentially being the birthplace of intermediate- to high-mass objects. These cores appear different from those observed in low-mass clustered environments in several observational aspects (kinematics, temperature, chemical gradients), indicating a strong influence of the most massive and evolved members of the protocluster. We suggest a possible scenario in which the B2 ZAMS star driving the cavity has compressed the surrounding gas, perturbed its properties and induced the star formation in its immediate surroundings.
C1 [Fontani, F.; Sanchez-Monge, A.] IINAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Palau, Aina] CSIC, Inst Ciencies Espai, IEEC, Fac Ciencies, E-08193 Bellaterra, Catalunya, Spain.
[Busquet, G.] INAF Ist Fis Spazio Interplanetario, I-00133 Rome, Italy.
[Isella, A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Estalella, R.] Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol IEEC UB, E-08028 Barcelona, Spain.
[Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Fontani, F (reprint author), IINAF Osservatorio Astrofis Arcetri, Lgo E Fermi 5, I-50125 Florence, Italy.
EM fontani@arcetri.astro.it
OI Fontani, Francesco/0000-0003-0348-3418; Zhang,
Qizhou/0000-0003-2384-6589
FU Owens Valley Radio Observatory; Spanish MICINN [AYA2008-06189-C03];
JAE-Doc CSIC; European Social Fund under the programme 'Junta para la
Ampliacion de Estudios'; Italian Space Agency (ASI) [I/005/07/01];
National Science Foundation [AST 05-40399]
FX 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. We acknowledge support from the Owens Valley Radio
Observatory, which is supported by the National Science Foundation
through grant AST 05-40399. AP is grateful to Inma Sepulveda for
insightful discussions. AP is supported by the Spanish MICINN grant
AYA2008-06189-C03 (co-funded with FEDER funds) and by a JAE-Doc CSIC
fellowship co-funded with the European Social Fund under the programme
'Junta para la Ampliacion de Estudios'. GB is funded by an Italian Space
Agency (ASI) fellowship under contract number I/005/07/01. We are
grateful to the anonymous referee for his/her valuable comments and
suggestions.
NR 56
TC 9
Z9 9
U1 1
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN
PY 2012
VL 423
IS 2
BP 1691
EP 1706
DI 10.1111/j.1365-2966.2012.20990.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956DU
UT WOS:000305070900055
ER
PT J
AU Hirsch, BT
Kays, R
Jansen, PA
AF Hirsch, Ben T.
Kays, Roland
Jansen, Patrick A.
TI A telemetric thread tag for tracking seed dispersal by scatter-hoarding
rodents
SO PLANT ECOLOGY
LA English
DT Article
DE Radio telemetry; Seed tag; Animal dispersed seeds; Astrocaryum; Agouti
ID LONG-DISTANCE DISPERSAL; CENTRAL-AMERICAN AGOUTI;
ASTROCARYUM-STANDLEYANUM; DASYPROCTA-PUNCTATA; RAIN-FOREST; PANAMA;
MOVEMENTS; CACHES; PLANTS; FIELD
AB The seeds of many tree species are dispersed more than once, and this secondary seed dispersal is believed to enhance seedling recruitment. However, the effectiveness of secondary seed dispersal has rarely been assessed because it is difficult to track seeds until they die or germinate. We describe a new technique that uses thread tags attached to radio transmitters (telemetric thread tags) to track long-distance multistep seed dispersal by scatter-hoarding rodents. These telemetric thread tags can be turned off with a magnet and are reactivated when the seed moves. This method allows for seed tracking with minimal cache disturbance or distance bias, over long time spans, multiple seed movements, and with few effects on animal behavior. We used telemetric thread tags to track seed dispersal of the palm tree Astrocaryum standleyanum in a Neotropical forest, and achieved near-complete recovery of dispersed seeds tracked over distances as far as 241 m. We were also able to record the recovery time and fate of cached seeds without disturbing caches. Neither the removal rate nor the dispersal distance differed between seeds with telemetric thread tags and thread-tagged seeds. We conclude that telemetric thread tags can be used to document secondary seed dispersal by scatter-hoarding animals with unprecedented efficacy and precision. Given the size of these tags relative to the size of seeds and their dispersers, this method is applicable to the majority of tree species that are secondarily dispersed by scatter-hoarding mammals.
C1 [Hirsch, Ben T.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA.
[Hirsch, Ben T.; Kays, Roland; Jansen, Patrick A.] Smithsonian Trop Res Inst, Unit 9100, DPO AA, Panama City 340029898, Panama.
[Kays, Roland] N Carolina Museum Nat Sci, Nat Res Ctr, Raleigh, NC 27601 USA.
[Jansen, Patrick A.] Univ Wageningen & Res Ctr, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands.
[Jansen, Patrick A.] Univ Groningen, Community & Conservat Ecol Grp, NL-9700 CC Groningen, Netherlands.
RP Hirsch, BT (reprint author), Ohio State Univ, Sch Environm & Nat Resources, 2021 Coffey Rd, Columbus, OH 43210 USA.
EM hirschb@si.edu
RI Jansen, Patrick/G-2545-2015
OI Jansen, Patrick/0000-0002-4660-0314
FU National Science Foundation [NSF-DEB 0717071]; Netherlands Organization
for Scientific Research [W85-239, 863-07-008]
FX We thank Tom Garin (ATS), Daniel Obando, Alejandro Ortega and Meg
Crofoot for technical support; Lieneke Bakker, Reyna Bell, Chris Carson,
Willem-Jan Emsens, Matt McElroy, Veronica Pereira, Torrey Rodgers,
Sumana Serchan, Michiel Veldhuis, Brian Watts, and Veronica Zamora
Guttierez for field assistance; the Smithsonian Tropical Research
Institute for facilities and administrative support. Joe Wright allowed
us access to unpublished data on seed weight, and brought up the
original idea for radio-tracking seeds with ARTS. We thank two anonymous
reviewers for their helpful comments and suggestions. We also thank
Patricia Kernan for the figure artwork. This study was supported by
funding from the National Science Foundation (NSF-DEB 0717071 to RWK)
and the Netherlands Organization for Scientific Research (Grants:
W85-239 and 863-07-008 to P.A.J.).
NR 56
TC 19
Z9 20
U1 2
U2 30
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1385-0237
J9 PLANT ECOL
JI Plant Ecol.
PD JUN
PY 2012
VL 213
IS 6
BP 933
EP 943
DI 10.1007/s11258-012-0054-0
PG 11
WC Plant Sciences; Ecology; Forestry
SC Plant Sciences; Environmental Sciences & Ecology; Forestry
GA 958KJ
UT WOS:000305235100005
ER
PT J
AU Frohlich, B
AF Froehlich, Bruno
TI Living with herds: human-animal coexistence in Mongolia
SO ANTIQUITY
LA English
DT Book Review
C1 [Froehlich, Bruno] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Frohlich, B (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM frohlich@si.edu
NR 1
TC 0
Z9 0
U1 0
U2 0
PU ANTIQUITY
PI YORK
PA KINGS MANOR, YORK YO1 7EP, ENGLAND
SN 0003-598X
J9 ANTIQUITY
JI Antiquity
PD JUN
PY 2012
VL 86
IS 332
BP 592
EP 594
PG 3
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA 951OE
UT WOS:000304729100043
ER
PT J
AU Burenin, RA
Vikhlinin, AA
AF Burenin, R. A.
Vikhlinin, A. A.
TI Cosmological parameters constraints from galaxy cluster mass function
measurements in combination with other cosmological data
SO ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS
LA English
DT Article
DE Cosmology; cosmological parameters; galaxy clusters
ID HUBBLE-SPACE-TELESCOPE; MICROWAVE BACKGROUND ANISOTROPIES; DARK ENERGY;
HYDROGEN RECOMBINATION; LIGHT CURVES; CALIBRATION; NEUTRINOS; CONSTANT;
OMEGA(M); SPECTRUM
AB We present the cosmological parameters constraints obtained from the combination of galaxy cluster mass function measurements (Vikhlinin et al. 2009a, 2009b) with new cosmological data obtained during last three years: updated measurements of cosmic microwave background anisotropy with Wilkinson Microwave Anisotropy Probe (WMAP) observatory, and at smaller angular scales with South Pole Telescope (SPT), new Hubble constant measurements, baryon acoustic oscillations and supernovae Type Ia observations. New constraints on total neutrino mass I m pound (nu) and effective number of neutrino species are obtained. In models with free number of massive neutrinos the constraints on these parameters are notably less strong, and all considered cosmological data are consistent with non-zero total neutrino mass I m pound (nu) a parts per thousand 0.4 eV and larger than standard effective number of neutrino species, N (eff) a parts per thousand 4. These constraints are compared to the results of neutrino oscillations searches at short baselines. The updated dark energy equation of state parameter constraints are presented. We show that taking in account systematic uncertanties, current cluster mass funstion data provide similarly powerful constraints on dark energy equation of state, as compared to the constraints from supernovae Type Ia observations.
C1 [Burenin, R. A.] Space Res Inst IKI, Moscow, Russia.
[Vikhlinin, A. A.] Harvard Smithsonian Ctr Astrophys CfA, Boston, MA USA.
RP Burenin, RA (reprint author), Space Res Inst IKI, Moscow, Russia.
EM rodion@hea.iki.rssi.ru
FU Russian Foundation for Basic Research [08-02-00974, 09-02-12384-ofi-m,
10-02-01442, 11-02-12271-ofi-m]; Russian Federation [Nsh-5069.2010.2];
Russian Academy of Sciences [P-21, OPhN-16]
FX We are grateful to D. S. Gorbunov for useful discussion of the results
of our work and for a number of important remarks and suggestions. In
this work the results of calculations on MVS-100K supercomputer of Joint
Supercomputer Center of the Russian Academy of Sciences (JSCC RAS) were
used. The work is supported by Russian Foundation for Basic Research,
grants 08-02-00974, 09-02-12384-ofi-m, 10-02-01442, 11-02-12271-ofi-m,
the Program for Support of Leading Scientific Schools of the Russian
Federation (Nsh-5069.2010.2), and the Programs of the Russian Academy of
Sciences P-21 and OPhN-16.
NR 87
TC 18
Z9 18
U1 0
U2 1
PU MAIK NAUKA/INTERPERIODICA/SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA
SN 1063-7737
EI 1562-6873
J9 ASTRON LETT+
JI Astron. Lett.-J. Astron. Space Astrophys.
PD JUN
PY 2012
VL 38
IS 6
BP 347
EP 363
DI 10.1134/S1063773712060011
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 956ZM
UT WOS:000305128100001
ER
PT J
AU Koblitz, K
AF Koblitz, Karen
TI Remembering Ken Price 1935-2012
SO CERAMICS-ART AND PERCEPTION
LA English
DT Biographical-Item
C1 [Koblitz, Karen] Univ So Calif, Ceram Roski Sch Fine Arts, Los Angeles, CA 90089 USA.
[Koblitz, Karen] Smithsonian Inst, Renwick Gallery Amer Art, Washington, DC 20560 USA.
RP Koblitz, K (reprint author), Univ So Calif, Ceram Roski Sch Fine Arts, Los Angeles, CA 90089 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU CERAMIC ART
PI SHERIDAN
PA 23 NORTH SCOTT ST, STE 19, SHERIDAN, WYOMING 82801 USA
SN 1035-1841
J9 CERAMICS-ART PERCEPT
JI Ceramics-Art Percept.
PD JUN-AUG
PY 2012
IS 88
BP 115
EP 115
PG 1
WC Art
SC Art
GA 955QA
UT WOS:000305034800031
ER
PT J
AU Zigler, KS
Byrne, M
Raff, EC
Lessios, HA
Raff, RA
AF Zigler, Kirk S.
Byrne, Maria
Raff, Elizabeth C.
Lessios, H. A.
Raff, Rudolf A.
TI NATURAL HYBRIDIZATION IN THE SEA URCHIN GENUS PSEUDOBOLETIA BETWEEN
SPECIES WITHOUT APPARENT BARRIERS TO GAMETE RECOGNITION
SO EVOLUTION
LA English
DT Article
DE Bindin; echinoid; gamete compatibility; hybridization; Pseudoboletia;
speciation
ID ACROSOMAL SPERM PROTEIN; REPRODUCTIVE ISOLATION; POSITIVE SELECTION;
MITOCHONDRIAL-DNA; STRONGYLOCENTROTUS-DROEBACHIENSIS;
POPULATION-STRUCTURE; ACROCNIDA-BRACHIATA; STARS LEPTASTERIAS; HYBRID
SPECIATION; MARINE SPECIATION
AB Marine species with high dispersal potential often have huge ranges and minimal population structure. Combined with the paucity of geographic barriers in the oceans, this pattern raises the question as to how speciation occurs in the sea. Over the past 20 years, evidence has accumulated that marine speciation is often linked to the evolution of gamete recognition proteins. Rapid evolution of gamete recognition proteins in gastropods, bivalves, and sea urchins is correlated with gamete incompatibility and contributes to the maintenance of species boundaries between sympatric congeners. Here, we present a counterexample to this general pattern. The sea urchins Pseudoboletia indiana and P. maculata have broad ranges that overlap in the Indian and Pacific oceans. Cytochrome oxidase I sequences indicated that these species are distinct, and their 7.3% divergence suggests that they diverged at least 2 mya. Despite this, we suspected hybridization between them based on the presence of morphologically intermediate individuals in sympatric populations at Sydney, Australia. We assessed the opportunity for hybridization between the two species and found that (1) individuals of the two species occur within a meter of each other in nature, (2) they have overlapping annual reproductive cycles, and (3) their gametes cross-fertilize readily in the laboratory and in the field. We genotyped individuals with intermediate morphology and confirmed that many were hybrids. Hybrids were fertile, and some female hybrids had egg sizes intermediate between the two parental species. Consistent with their high level of gamete compatibility, there is minimal divergence between P. indiana and P. maculata in the gamete recognition protein bindin, with a single fixed amino acid difference between the two species. Pseudoboletia thus provides a well-characterized exception to the idea that broadcast spawning marine species living in sympatry develop and maintain species boundaries through the divergence of gamete recognition proteins and the associated evolution of gamete incompatibility.
C1 [Zigler, Kirk S.] Univ South, Dept Biol, Sewanee, TN 37383 USA.
[Byrne, Maria] Univ Sydney, Sch Med, Sydney, NSW 2006, Australia.
[Byrne, Maria; Raff, Elizabeth C.; Raff, Rudolf A.] Univ Sydney, Sch Biol Sci, Sydney, NSW 2006, Australia.
[Raff, Elizabeth C.; Raff, Rudolf A.] Indiana Univ, Dept Biol, Bloomington, IN 47401 USA.
[Lessios, H. A.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Zigler, KS (reprint author), Univ South, Dept Biol, Sewanee, TN 37383 USA.
EM kzigler@sewanee.edu
RI Byrne, Maria/K-6355-2016
OI Byrne, Maria/0000-0002-8902-9808
FU National Science Foundation; Australian Research Council; Smithsonian
Tropical Research Institute
FX We thank A. Pile for her help in designing and carrying out the scuba
experiment for hybrid fertilization in the field, and for her help in
obtaining the transect and depth data at Green Point in 2005. We thank
H. Sowden, L. Edwards, H. Giragossyan, and A. Smoothey for their help
with sea urchin collecting, obtaining data on Pseudoboletia species
distribution in 2003 and 2004, and carrying out the field fertilization
experiment; J. Villinski for his help with the field fertilization
experiment; T. Prowse and S. Barbosa for assistance with the
reproductive study; L. Geyer, A. Calderon, L. Calderon, and A. Sidik for
assistance in the laboratory; D. R. Robertson for collecting the
Pseudoboletia from Sao Tome and Easter Island. KSZ was supported by the
National Science Foundation International Research Fellowship Program.
This work was also supported by a grant from the Australian Research
Council to MB; general research funds from the Smithsonian Tropical
Research Institute to HAL; and a National Science Foundation grant to
RAR. Contribution number 63 of the Sydney Institute of Marine Science.
NR 70
TC 5
Z9 5
U1 2
U2 35
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0014-3820
J9 EVOLUTION
JI Evolution
PD JUN
PY 2012
VL 66
IS 6
BP 1695
EP 1708
DI 10.1111/j.1558-5646.2012.01609.x
PG 14
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 951YR
UT WOS:000304757200003
PM 22671540
ER
PT J
AU Armitage, SAO
Fernandez-Marin, H
Wcislo, WT
Boomsma, JJ
AF Armitage, Sophie A. O.
Fernandez-Marin, Hermogenes
Wcislo, William T.
Boomsma, Jacobus J.
TI AN EVALUATION OF THE POSSIBLE ADAPTIVE FUNCTION OF FUNGAL BROOD COVERING
BY ATTINE ANTS
SO EVOLUTION
LA English
DT Article
DE Formicidae; fungus-growing ants; mycelium; parasites; pupae;
prophylactic behavior
ID LEAF-CUTTING ANTS; GROWING ANTS; ANTIBIOTIC METABOLITE; ORIENTAL HORNET;
HYMENOPTERA; EVOLUTION; ACROMYRMEX; FORMICIDAE; BACTERIA; GARDENS
AB Fungus-growing ants (Myrmicinae: Attini) live in an obligate symbiotic relationship with a fungus that they rear for food, but they can also use the fungal mycelium to cover their brood. We surveyed colonies from 20 species of fungus-growing ants and show that brood-covering behavior occurs in most species, but to varying degrees, and appears to have evolved shortly after the origin of fungus farming, but was partly or entirely abandoned in some genera. To understand the evolution of the trait we used quantitative phylogenetic analyses to test whether brood-covering behavior covaries among attine ant clades and with two hygienic traits that reduce risk of disease: mycelial brood cover did not correlate with mutualistic bacteria that the ants culture on their cuticles for their antibiotics, but there was a negative relationship between metapleural gland grooming and mycelial cover. A broader comparative survey showed that the pupae of many ant species have protective cocoons but that those in the subfamily Myrmicinae do not. We therefore evaluated the previously proposed hypothesis that mycelial covering of attine ant brood evolved to provide cocoon-like protection for the brood.
C1 [Armitage, Sophie A. O.; Fernandez-Marin, Hermogenes; Boomsma, Jacobus J.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark.
[Armitage, Sophie A. O.] Univ Munster, Inst Evolut & Biodivers, D-48149 Munster, Germany.
[Fernandez-Marin, Hermogenes; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Armitage, SAO (reprint author), Univ Copenhagen, Dept Biol, Ctr Social Evolut, Univ Pk 15, DK-2100 Copenhagen, Denmark.
EM sophie.armitage@uni-muenster.de; FernandezH@si.edu
RI Boomsma, Jacobus/M-2785-2014; Armitage, Sophie/A-6961-2012
OI Boomsma, Jacobus/0000-0002-3598-1609; Armitage,
Sophie/0000-0002-5561-9543
FU Intra-European Marie Curie Fellowship; Volkswagen Foundation;
Smithsonian; SENACYT; Danish National Research Foundation; Smithsonian
Tropical Research Institute (STRI)
FX We would like to thank A. Wild, A. Ivens, D. Kronauer, E. Strohm, H. de
Fine Licht, J. Longino, J. Broch, J. Ceballos, J. Heinze, K. Petersen,
R. Peu beta, S. Tragust, and S. Cremer for their help with data
collection and/or for sharing their knowledge with us. We would also
like to thank U. Mueller and an anonymous reviewer for their detailed
and helpful comments on the manuscript. SAOA was supported by an
Intra-European Marie Curie Fellowship and a Volkswagen Foundation
Postdoctoral Fellowship, HFM was supported by a Smithsonian and SENACYT
Postdoctoral Fellowships, and HFM and JJB were supported by the Danish
National Research Foundation. WTWis grateful for general research
support from Smithsonian Tropical Research Institute (STRI). All authors
thank the Autoridad Nacional del Ambiente of the Republic of Panama for
permits to collect and export ants. This work was done in compliance
with all applicable laws.
NR 70
TC 10
Z9 10
U1 0
U2 33
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0014-3820
EI 1558-5646
J9 EVOLUTION
JI Evolution
PD JUN
PY 2012
VL 66
IS 6
BP 1966
EP 1975
DI 10.1111/j.1558-5646.2011.01568.x
PG 10
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 951YR
UT WOS:000304757200023
PM 22671560
ER
PT J
AU Wood, B
Schroer, K
AF Wood, Bernard
Schroer, Kes
TI Reconstructing the Diet of an Extinct Hominin Taxon: The Role of Extant
Primate Models
SO INTERNATIONAL JOURNAL OF PRIMATOLOGY
LA English
DT Article
DE Comparative primatology; Diet reconstruction; Modeling; Paranthropus
boisei
ID MONKEYS CEBUS-APELLA; UNDERGROUND-STORAGE ORGANS; DENTAL MICROWEAR
TEXTURE; FINITE-ELEMENT-ANALYSIS; PONGO-PYGMAEUS-WURMBII; LARGE-BODIED
HOMINOIDS; FALLBACK FOODS; ENAMEL THICKNESS; PARANTHROPUS-BOISEI; GENUS
CEBUS
AB Modern humans represent the only surviving species of an otherwise extinct clade of primates, the hominins. As the closest living relatives to extinct hominins, extant primates are an important source of comparative information for the reconstruction of the diets of extinct hominins. Methods such as comparative and functional morphology, finite element analysis, dental wear, dental topographic analysis, and stable isotope biogeochemistry must be validated and tested within extant populations before they can be applied to extinct taxa. Here we review how these methods have and might be used to reconstruct the diet of a particular extinct hominin, Paranthropus boisei, which has no extant analogue for its highly derived masticatory morphology. Our review emphasizes the potential and limitations of using extant primates as models for the reconstruction of extinct hominin diets. We encourage paleoanthropologists and those who study the feeding behaviors of extant primates to work together to investigate and validate methods for interpreting the diets of all extinct primates, including hominins.
C1 [Wood, Bernard; Schroer, Kes] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA.
[Wood, Bernard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA.
RP Schroer, K (reprint author), George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA.
EM bernardawood@gmail.com; kes.schroer@gmail.com
FU GW Provost; NSF-IGERT [DGE-0801634]; NSF-GRFP
FX B. Wood and K. Schroer thank Erin Vogel and Janine Chalk for their kind
invitation to contribute to this volume and for their comments on a
draft. Linda Gordon and Darrin Lunde (NMNH) provided assistance with
collections. The manuscript was improved by the comments of Joanna
Setchell, Andrew Zipkin, Sarah Elton, and two anonymous reviewers. We
also thank Joram Berlowitz, Andrew Cunningham, Ian Gilby, John Gurche,
Alan Houle, Charlie Jansen, Carson Murray, Matt Sponheimer, and Erin
Vogel. We thank the GW Provost, NSF-IGERT DGE-0801634, and NSF-GRFP (to
K. Schroer) for research support.
NR 122
TC 19
Z9 19
U1 3
U2 60
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0164-0291
EI 1573-8604
J9 INT J PRIMATOL
JI Int. J. Primatol.
PD JUN
PY 2012
VL 33
IS 3
BP 716
EP 742
DI 10.1007/s10764-012-9602-7
PG 27
WC Zoology
SC Zoology
GA 951ES
UT WOS:000304704200012
ER
PT J
AU Whattam, SA
Montes, C
McFadden, RR
Cardona, A
Ramirez, D
Valencia, V
AF Whattam, Scott A.
Montes, Camilo
McFadden, Rory R.
Cardona, Agustin
Ramirez, Diego
Valencia, Victor
TI Age and origin of earliest adakitic-like magmatism in Panama:
Implications for the tectonic evolution of the Panamanian magmatic arc
system
SO LITHOS
LA English
DT Article
DE Panama; Panamanian magmatic arc system; Central American arc system;
Magmatic arc; Adakite; Adakitic-like intrusions
ID LOWER CONTINENTAL-CRUST; PORPHYRY COPPER MINERALIZATION; NORTHWESTERN
SOUTH-AMERICA; UNDERPLATED BASALTIC CRUST; NORTHERN VOLCANIC ZONE; SLAB
MELT METASOMATISM; RIDGE-TRENCH COLLISION; LARGE IGNEOUS PROVINCE;
COSTA-RICA; EAST CHINA
AB 40-20 Ma marks a fundamental interval in the evolution of the 70-0 Ma Panamanian magmatic arc system. During this period, there is no evidence of Panamanian magmatic arc activity to the east of the Panama Canal Basin while to the west and in localized regions to the east of the Panama Canal Basin a phase of intrusive-only activity is recorded. Fundamentally, geochemical and geochronological evidence presented herein indicate that this intrusive activity was predominantly 'adakitic-like' and becomes younger from west to east along an approximately W-E striking lineament. Granodiorites of the Petaquilla batholith, western Panama yield LAM-ICP-MS Pb-206/U-238 zircon ages of 29.0 + 0.7, -0.6 Ma, 28.5 + 0.7, -0.5 Ma, 28.3 + 0.5, -0.4 Ma and 26.2 + 0.5, -0.9 Ma. To the east of the Panama Canal Basin zircons from a hypabyssal diorite of the mainly intermediate Maje subvolcanic suite, cedes a mean Pb-206/U-238 age of 18.9 + 0.4 Ma. Relative to other 70-5 Ma Panamanian magmatic arc lavas and intrusives, Maje and Petaquilla intrusives yield adakitic-like major and trace element abundances (e.g., > 15 wt.% Al(2)O3, generally > 3.5 wt.% Na2O, > 400 ppm Sr, < 1.9 ppm Yb, < 18 ppm Y, Sr/Y that ranges to > 120) and strongly fractionated HREE patterns. These 30-26 Ma (Petaquilla) and 19 Ma (Maje) suites are also compositionally similar to a subvolcanic suite of rare, circa 25 Ma adakitic-like, andesitic intrusives which occur within the Panama Canal Basin midway between Petaquilla and Male and at the same approximate latitude as Petaquilla and Maje. Collectively, the geochemical and geochronological data for the adakitic-like intrusives arc consistent with formation via partial melting of lowermost, mafic crust above a sub-horizontal slab tear that propagated from the west (Petaquilla) to the east (Male) between 30 and 19 Ma. Our new tectonic model postulates that collision between the Panamanian magmatic arc system and an 'indentor' (e.g., a tract of thickened buoyant, oceanic crust or plateau) occurred at about 40 Ma, a time of which coincides with the initiation of left-lateral offset of the Early (i.e., 70-40 Ma) Arc system. This collision resulted in the shutdown of the Early Arc system, possible steepening of the subducting Farallon slab and ultimately slab break-off and the phase of mainly adakitic-like intrusive activity. Subsequent to slab removal by similar to 20 Ma, NE-dipping subduction jumped to the south and initiated production of the Later (i.e., post 20 Ma) Arc system soon thereafter. Crown Copyright (C) 2012 Published by Elsevier B.V. All rights reserved.
C1 [Whattam, Scott A.] Korea Univ, Dept Earth & Environm Sci, Seoul 136701, South Korea.
[Whattam, Scott A.; Montes, Camilo; Cardona, Agustin; Ramirez, Diego] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Montes, Camilo; Cardona, Agustin] Corp Geol Ares, Bogota, Colombia.
[McFadden, Rory R.] Salem State Univ, Dept Geol Sci, Salem, MA 01970 USA.
[Valencia, Victor] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
RP Whattam, SA (reprint author), Korea Univ, Dept Earth & Environm Sci, Seoul 136701, South Korea.
EM whattam@korea.ac.kr
OI Ramirez, Diego/0000-0001-6018-3273; Whattam, Scott/0000-0001-9193-9002;
Montes, Camilo/0000-0002-3553-0787
FU ACP [SAA-199520-KRP]; U.S. National Science Foundation (NSF) [0966884];
NSF [EAR 0824299]
FX This study was made possible by ACP (Panama Canal Authority) contract
SAA-199520-KRP and the U.S. National Science Foundation (NSF) grant
0966884 (OISE, EAR, DRL), and Mr. Mark Tupper, NSF EAR 0824299. Access
to field areas and collection permits were granted by Ministerio de
lndustria y Comercio. Minera Panama is thanked for providing core
samples from Petaquilla. Federerico Moreno and the Department of
Geological Sciences, University of Florida, are thanked for the CL
images. Ed. A.C. Kerr, E. Gazel and an anonymous reviewer are thanked
for their detailed and insightful comments. J.K. Kim is acknowledged for
insightful comments which improved aspects of data presentation.
NR 135
TC 11
Z9 12
U1 0
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0024-4937
J9 LITHOS
JI Lithos
PD JUN
PY 2012
VL 142
BP 226
EP 244
DI 10.1016/j.lithos.2012.02.017
PG 19
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 951MU
UT WOS:000304725500015
ER
PT J
AU Hirsch, BT
Visser, MD
Kays, R
Jansen, PA
AF Hirsch, Ben T.
Visser, Marco D.
Kays, Roland
Jansen, Patrick A.
TI Quantifying seed dispersal kernels from truncated seed-tracking data
SO METHODS IN ECOLOGY AND EVOLUTION
LA English
DT Article
DE censored tail reconstruction; censored tail reconstruction; kernel;
long-distance dispersal; seed dispersal; seed tracking; thread tag
ID TROPICAL FORESTS; PLANT-POPULATIONS; SPATIAL-PATTERNS; WIND DISPERSAL;
RAIN-FOREST; SHADOWS; CONSEQUENCES; RECRUITMENT; DEPENDENCE; BEHAVIOR
AB 1. Seed dispersal is a key biological process that remains poorly documented because dispersing seeds are notoriously hard to track. While long-distance dispersal is thought to be particularly important, seed-tracking studies typically yield incomplete data sets that are biased against long-distance movements. 2. We evaluate an analytical procedure developed by Jansen, Bongers & Hemerik (2004) to infer the tail of a seed dispersal kernel from incomplete frequency distributions of dispersal distances obtained by tracking seeds. This censored tail reconstruction (CTR) method treats dispersal distances as waiting times in a survival analysis and censors nonretrieved seeds according to how far they can reliably be tracked. We tested whether CTR can provide unbiased estimates of long-distance movements which typically cannot be tracked with traditional field methods. 3. We used a complete frequency distribution of primary seed dispersal distances of the palm Astrocaryum standleyanum, obtained with telemetric thread tags that allow tracking seeds regardless of the distance moved. We truncated and resampled the data set at various distances, fitted kernel functions on CTR estimates of dispersal distance and determined how well this function approximated the true dispersal kernel. 4. Censored tail reconstruction with truncated data approximated the true dispersal kernel remarkably well but only when the best-fitting function (lognormal) was used. We were able to select the correct function and derive an accurate estimate of the seed dispersal kernel even after censoring 5060% of the dispersal events. However, CTR results were substantially biased if 5% or more of seeds within the search radius were overlooked by field observers and erroneously censored. Similar results were obtained using additional simulated dispersal kernels. 5. Our study suggests that the CTR method can accurately estimate the dispersal kernel from truncated seed-tracking data if the kernel is a simple decay function. This method will improve our understanding of the spatial patterns of seed movement and should replace the usual practice of omitting nonretrieved seeds from analyses in seed-tracking studies.
C1 [Hirsch, Ben T.; Kays, Roland] New York State Museum & Sci Serv, Albany, NY 12230 USA.
[Hirsch, Ben T.; Visser, Marco D.; Kays, Roland; Jansen, Patrick A.] Smithsonian Trop Res Inst, Unit 9100, DPO, AA 34002 USA.
[Visser, Marco D.] Radboud Univ Nijmegen, Dept Expt Plant Ecol, NL-6525 AJ Nijmegen, Netherlands.
[Jansen, Patrick A.] Univ Wageningen & Res Ctr, Ctr Ecosyst Studies, NL-6700 AA Wageningen, Netherlands.
[Jansen, Patrick A.] Univ Groningen, Community & Conservat Ecol Grp, NL-9700 CC Groningen, Netherlands.
RP Hirsch, BT (reprint author), New York State Museum & Sci Serv, 3140 CEC, Albany, NY 12230 USA.
EM hirschb@si.edu
RI Jansen, Patrick/G-2545-2015
OI Jansen, Patrick/0000-0002-4660-0314
FU National Science Foundation [NSF-DEB 0717071]; Netherlands Organization
for Scientific Research [W85-239, 863-07-008]; Smithsonian Tropical
Research Institute
FX We thank Eelke Jongejans and two anonymous reviewers for valuable
comments to an earlier version of the manuscript. This study was
supported by funding from the National Science Foundation (NSF-DEB
0717071 to RWK) and the Netherlands Organization for Scientific Research
(grants W85-239 and 863-07-008 to P.A.J.). M. D. V. acknowledges funding
from the Smithsonian Tropical Research Institute fellowship programme.
NR 43
TC 13
Z9 14
U1 5
U2 38
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2041-210X
EI 2041-2096
J9 METHODS ECOL EVOL
JI Methods Ecol. Evol.
PD JUN
PY 2012
VL 3
IS 3
BP 595
EP 602
DI 10.1111/j.2041-210X.2011.00183.x
PG 8
WC Ecology
SC Environmental Sciences & Ecology
GA 953VX
UT WOS:000304902500018
ER
PT J
AU Luna, GJM
Diaz, MP
Brickhouse, NS
Moraes, M
AF Luna, G. J. M.
Diaz, M. P.
Brickhouse, N. S.
Moraes, M.
TI XMM-Newton EPIC and OM observation of Nova Centauri 1986 (V842 Cen)
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE novae; cataclysmic variables; X-rays: general
ID WHITE-DWARF MASSES; CATACLYSMIC VARIABLES; INTERMEDIATE POLARS; RAY
OBSERVATIONS; OUTBURSTS; EMISSION; REMNANTS; SPECTRA; MODELS
AB We report the results from the temporal and spectral analysis of an XMMNewton observation of Nova Centauri 1986 (V842 Cen). We detect a period at 3.51 +/- 0.4 h in the EPIC data and at 4.0 +/- 0.8 h in the Optical Monitor (OM) data. The X-ray spectrum is consistent with the emission from an absorbed thin thermal plasma with a temperature distribution given by an isobaric cooling flow. The maximum temperature of the cooling flow model is keV. Such a high temperature can be reached in a shocked region and, given the periodicity detected, most likely arises in a magnetically channelled accretion flow characteristic of intermediate polars. The pulsed fraction of the 3.51-h modulation decreases with energy as observed in the X-ray light curves of magnetic cataclysmic variables, possibly due either to occultation of the accretion column by the white dwarf body or phase-dependent to absorption. We do not find the 57-s white dwarf spin period, with a pulse amplitude of 4 mmag, reported by Woudt et al. in either the OM data, which are sensitive to pulse amplitudes ?0.03 mag, or the EPIC data, sensitive to pulse fractions p? 14 +/- 2 per cent.
C1 [Luna, G. J. M.] Consejo Nacl Invest Cient & Tecn, IAFE, Caba, Argentina.
[Luna, G. J. M.] Inst Ciencias Astron Tierra & Espacio, San Juan, Argentina.
[Diaz, M. P.] Univ Sao Paulo, IAG, BR-05508900 Sao Paulo, Brazil.
[Brickhouse, N. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Luna, GJM (reprint author), Consejo Nacl Invest Cient & Tecn, IAFE, CC67,Suc 28,C1428ZAA, Caba, Argentina.
EM gjmluna@iafe.uba.ar
RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; diaz,
marcos/I-7233-2013;
OI Brickhouse, Nancy/0000-0002-8704-4473
FU ESA; NASA
FX We acknowledge the anonymous referee for the comments that helped
improve the manuscript. We acknowledge Raimundo Lopes de Oliveira for
useful tips and discussion about data analysis. This study is based on
observations obtained with XMM-Newton, an ESA science mission with
instruments and contributions directly funded by ESA member states and
NASA.
NR 19
TC 1
Z9 1
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN
PY 2012
VL 423
IS 1
BP L75
EP L78
DI 10.1111/j.1745-3933.2012.01260.x
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 952SU
UT WOS:000304813500016
ER
PT J
AU Marinucci, A
Risaliti, G
Wang, JF
Nardini, E
Elvis, M
Fabbiano, G
Bianchi, S
Matt, G
AF Marinucci, A.
Risaliti, G.
Wang, Junfeng
Nardini, E.
Elvis, M.
Fabbiano, G.
Bianchi, S.
Matt, G.
TI The X-ray reflector in NGC 4945: a time- and space-resolved portrait
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion; accretion discs; galaxies: active; galaxies: Seyfert
ID XMM-NEWTON; CHANDRA ACIS; NGC-4945; GALAXY; SPECTROSCOPY; RESOLUTION
AB We present a time, spectral and imaging analysis of the X-ray reflector in NGC 4945, which reveals its geometrical and physical structure with unprecedented detail. NGC 4945 hosts one of the brightest AGN in the sky above 10 keV, but it is only visible through its reflected/scattered emission below 10 keV, due to absorption by a column density of similar to 4 x 1024 cm-2. A new Suzaku campaign of five observations spanning similar to 6 months, together with past XMMNewton and Chandra observations, shows a remarkable constancy (within <10 per cent) of the reflected component. Instead, Swift-BAT reveals strong intrinsic variability on time-scales longer than 1 yr. Modelling the circumnuclear gas as a thin cylinder with the axis on the plane of the sky, we show that the reflector is at a distance =30-50 pc, well within the imaging capabilities of Chandra at the distance of NGC 49-45 (1 arcsec similar to 18 pc). Accordingly, the Chandra imaging reveals a resolved, flattened, similar to 150 pc long clumpy structure, whose spectrum is fully due to cold reflection of the primary AGN emission. The clumpiness may explain the small covering factor derived from the spectral and variability properties.
C1 [Marinucci, A.; Bianchi, S.; Matt, G.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy.
[Marinucci, A.; Risaliti, G.; Wang, Junfeng; Nardini, E.; Elvis, M.; Fabbiano, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
RP Marinucci, A (reprint author), Univ Roma Tre, Dipartimento Fis, Via Vasca Navale 84, I-00146 Rome, Italy.
EM marinucci@fis.uniroma3.it
RI Bianchi, Stefano/B-4804-2010; XRAY, SUZAKU/A-1808-2009;
OI Bianchi, Stefano/0000-0002-4622-4240; Risaliti,
Guido/0000-0002-3556-977X
FU NASA [NNX11AC85G, NNX10AF50G, GO8-9101X, GO1-12009X]
FX The authors are grateful to the referee for her/his useful comments. AM,
GR and EM acknowledge NASA grants NNX11AC85G and NNX10AF50G. JW
acknowledges support from NASA grants GO8-9101X and GO1-12009X.
NR 19
TC 20
Z9 20
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN
PY 2012
VL 423
IS 1
BP L6
EP L10
DI 10.1111/j.1745-3933.2012.01232.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 952SU
UT WOS:000304813500002
ER
PT J
AU Bell, JA
AF Bell, Joshua A.
TI LINES THAT CONNECT: Rethinking Pattern and Mind in the Pacific
SO PACIFIC AFFAIRS
LA English
DT Book Review
C1 [Bell, Joshua A.] Smithsonian Inst, Washington, DC 20560 USA.
RP Bell, JA (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU PACIFIC AFFAIRS UNIV BRITISH COLUMBIA
PI VANCOUVER
PA #164-1855 WEST MALL, VANCOUVER, BC V6T 1Z2, CANADA
SN 0030-851X
J9 PAC AFF
JI Pac. Aff.
PD JUN
PY 2012
VL 85
IS 2
BP 460
EP 461
PG 2
WC Area Studies
SC Area Studies
GA 952LE
UT WOS:000304793200049
ER
PT J
AU Peterson, PM
Romaschenko, K
Snow, N
Johnson, G
AF Peterson, Paul M.
Romaschenko, Konstantin
Snow, Neil
Johnson, Gabriel
TI A molecular phylogeny and classification of Leptochloa (Poaceae:
Chloridoideae: Chlorideae) sensu lato and related genera
SO ANNALS OF BOTANY
LA English
DT Article
DE Classification; Dinebra; Diplachne; Disakisperma; Drake-brockmania; ITS;
Leptochloa; phylogeny; plastid DNA sequences; Poaceae; Trichloris;
Trigonochloa
ID LENGTH DIFFERENCE TEST; INCONGRUENCE; SEQUENCES; ERAGROSTIDEAE;
INFERENCE; MRBAYES; UTILITY; TREES
AB Leptochloa (including Diplachne) sensu lato (s.l.) comprises a diverse assemblage of C-4 (NAD-ME and PCK) grasses with approx. 32 annual or perennial species. Evolutionary relationships and a modern classification of Leptochloa spp. based on the study of molecular characters have only been superficially investigated in four species. The goals of this study were to reconstruct the evolutionary history of Leptochloa s.l. with molecular data and broad taxon sampling.
A phylogenetic analysis was conducted of 130 species (mostly Chloridoideae), of which 22 are placed in Leptochloa, using five plastid (rpL32-trn-L, ndhA intron, rps16 intron, rps16-trnK and ccsA) and the nuclear ITS 1 and 2 (ribosomal internal transcribed spacer regions) to infer evolutionary relationships and revise the classification.
Leptochloa s.l. is polyphyletic and strong support was found for five lineages. Embedded within the Leptochloa sensu stricto (s.s.) clade are two Trichloris spp. and embedded in Dinebra are Drake-brockmania and 19 Leptochloa spp.
The molecular results support the dissolution of Leptochloa s.l. into the following five genera: Dinebra with 23 species, Diplachne with two species, Disakisperma with three species, Leptochloa s.s. with five species and a new genus, Trigonochloa, with two species.
C1 [Peterson, Paul M.; Romaschenko, Konstantin] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot MRC 166, Washington, DC 20013 USA.
[Romaschenko, Konstantin] Bot Inst Barcelona CSIC ICUB, Lab Mol Systemat, Barcelona 08038, Spain.
[Snow, Neil] Montana Nat Heritage Program, Helena, MT 59620 USA.
[Johnson, Gabriel] Smithsonian Inst, Dept Bot, Suitland, MD 20746 USA.
[Johnson, Gabriel] Labs Analyt Biol, Suitland, MD 20746 USA.
RP Peterson, PM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot MRC 166, Washington, DC 20013 USA.
EM peterson@si.edu
RI Romaschenko, Konstantin/K-3096-2014
OI Romaschenko, Konstantin/0000-0002-7248-4193
FU National Geographic Society Committee for Research and Exploration
[8087-06]; Smithsonian Institution; Scholarly Studies Program; Research
Opportunities; Atherton Seidell Foundation; Biodiversity Surveys and
Inventories Program; Small Grants Program; Laboratory of Analytical
Biology
FX We thank the National Geographic Society Committee for Research and
Exploration (Grant No. 8087-06) for field and laboratory support, the
Smithsonian Institution's Restricted Endowments Fund, the Scholarly
Studies Program, Research Opportunities, Atherton Seidell Foundation,
Biodiversity Surveys and Inventories Program, Small Grants Program, and
the Laboratory of Analytical Biology, all for financial support. We
would also like to acknowledge Lee Weigt, Jeffery Hunt and David
Erickson for help in the laboratory; Robert J. Soreng, Jeffery M.
Saarela, Gene Rosenberg, Emmet J. Judziewicz, Carol R. Annable and Nancy
Refulio Rodriguez for accompanying the first author on numerous field
expeditions; Robert J. Soreng for many extended discussions pertinent to
the manuscript; and Jeffery M. Saarela and an anonymous reviewer for
providing helpful comments on the manuscript.
NR 48
TC 17
Z9 22
U1 0
U2 10
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0305-7364
J9 ANN BOT-LONDON
JI Ann. Bot.
PD JUN
PY 2012
VL 109
IS 7
BP 1317
EP 1329
DI 10.1093/aob/mcs077
PG 13
WC Plant Sciences
SC Plant Sciences
GA 948WA
UT WOS:000304532300011
PM 22628365
ER
PT J
AU Borda-de-Agua, L
Borges, PAV
Hubbell, SP
Pereira, HM
AF Borda-de-Agua, Luis
Borges, Paulo A. V.
Hubbell, Stephen P.
Pereira, Henrique M.
TI Spatial scaling of species abundance distributions
SO ECOGRAPHY
LA English
DT Article
ID IMAGE-ANALYSIS; NEUTRAL THEORY; GENERAL-THEORY; BIODIVERSITY; MOMENTS;
AREA; POPULATION; INVARIANCE; DIVERSITY; PATTERNS
AB Species abundance distributions are an essential tool in describing the biodiversity of ecological communities. We now know that their shape changes as a function of the size of area sampled. Here we analyze the scaling properties of species abundance distributions by using the moments of the logarithmically transformed number of individuals. We find that the moments as a function of area size are well fitted by power laws and we use this pattern to estimate the species abundance distribution for areas larger than those sampled. To reconstruct the species abundance distribution from its moments, we use discrete Tchebichef polynomials. We exemplify the method with data on tree and shrub species from a 50 ha plot of tropical rain forest on Barro Colorado Island, Panama. We test the method within the 50 ha plot, and then we extrapolate the species abundance distribution for areas up to 5 km2. Our results project that for areas above 50 ha the species abundance distributions have a bimodal shape with a local maximum occurring for the singleton classes and that this maximum increases with sampled area size.
C1 [Borda-de-Agua, Luis; Pereira, Henrique M.] Univ Lisbon, Fac Ciencias, Ctr Biol Ambiental, P-1749016 Lisbon, Portugal.
[Pereira, Henrique M.] Inst Super Tecn, Dept Engn Civil & Arquitectura, P-1049001 Lisbon, Portugal.
[Borges, Paulo A. V.] Univ Acores, Azorean Biodivers Grp CITA A, P-9700 Angra Do Heroismo, Azores, Portugal.
[Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Hubbell, Stephen P.] Smithsonian Trop Res Inst, Unit 0948, Ctr Trop Forest Sci, Apo Aa 340020948, Panama.
RP Borda-de-Agua, L (reprint author), Univ Lisbon, Fac Ciencias, Ctr Biol Ambiental, P-1749016 Lisbon, Portugal.
EM lbagua@gmail.com
RI Pereira, Henrique/B-3975-2009; Borges, Paulo/B-2780-2008; Borda-de-Agua,
Luis/D-6063-2011
OI Pereira, Henrique/0000-0003-1043-1675; Borges,
Paulo/0000-0002-8448-7623; Borda-de-Agua, Luis/0000-0002-0802-6235
FU ABAFOBIO from Fundacao para a Ciencia e Tecnologia, Portugal
[PTDC/AMB/73901/2006]; National Science Foundation; Smithsonian Tropical
Research Inst.
FX We thank B. McGill, and A. L. Sizling for suggestions that substantially
improved the manuscript. LBA thanks the Azorean Biodiversity Group for
the kind hospitality during his stay at the Univ. of Azores. This work
was supported by the ABAFOBIO (PTDC/AMB/73901/2006) grant from Fundacao
para a Ciencia e Tecnologia, Portugal. SPH thanks the National Science
Foundation, the Smithsonian Tropical Research Inst., and numerous
private foundations for support of both his theoretical and empirical
work on and off Barro Colorado Island.
NR 44
TC 8
Z9 11
U1 3
U2 44
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0906-7590
J9 ECOGRAPHY
JI Ecography
PD JUN
PY 2012
VL 35
IS 6
BP 549
EP 556
DI 10.1111/j.1600-0587.2011.07128.x
PG 8
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 952BX
UT WOS:000304765800008
ER
PT J
AU Russell, HR
McNamara, BR
Sanders, JS
Fabian, AC
Nulsen, PEJ
Canning, REA
Baum, SA
Donahue, M
Edge, AC
King, LJ
O'Dea, CP
AF Russell, H. R.
McNamara, B. R.
Sanders, J. S.
Fabian, A. C.
Nulsen, P. E. J.
Canning, R. E. A.
Baum, S. A.
Donahue, M.
Edge, A. C.
King, L. J.
O'Dea, C. P.
TI Shock fronts, electron-ion equilibration and intracluster medium
transport processes in the merging cluster Abell 2146
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: individual: Abell 2146; galaxies: clusters:
intracluster medium; X-rays: galaxies: clusters
ID NONEQUILIBRIUM IONIZATION STATE; FAST MODE SHOCKS; X-RAY;
MAGNETIC-FIELD; COLD FRONTS; DARK-MATTER; COLLISIONLESS SHOCKS;
INTERGALACTIC MEDIUM; CHANDRA OBSERVATION; THERMAL CONDUCTION
AB We present a new 400-ks Chandra X-ray observation of the merging galaxy cluster Abell 2146. This deep observation reveals detailed structure associated with the major merger event including the Mach number M= 2.3 +/- 0.2 bow shock ahead of the dense, ram pressure stripped subcluster core and the first known example of an upstream shock in the intracluster medium (ICM) (M= 1.6 +/- 0.1). By measuring the electron temperature profile behind each shock front, we determine the time-scale for the electron population to thermally equilibrate with the shock-heated ions. We find that the temperature profile behind the bow shock is consistent with the time-scale for Coulomb collisional equilibration and the post-shock temperature is lower than expected for instant shock heating of the electrons. Although like the Bullet cluster the electron temperatures behind the upstream shock front are hotter than expected, favouring the instant heating model, the uncertainty on the temperature values is greater here and there is significant substructure complicating the interpretation. We also measured the width of each shock front and the contact discontinuity on the leading edge of the subcluster core to investigate the suppression of transport processes in the ICM. The upstream shock is similar to 440 kpc in length but appears remarkably narrow over this distance with a best-fitting width of only 6+5-3 kpc compared with the mean free path of 23 +/- 5 kpc. The leading edge of the subcluster core is also narrow with an upper limit on the width of only 2 kpc separating the cool, multiphase gas at 0.52 keV from the shock-heated surrounding ICM at similar to 6 keV. The strong suppression of diffusion and conduction across this edge suggests a magnetic draping layer may have formed around the subcluster core. The deep Chandra observation has also revealed a cool, dense plume of material extending similar to 170 kpc perpendicular to the merger axis, which is likely to be the disrupted remnant of the primary cluster core. This asymmetry in the cluster morphology indicates the merger has a non-zero impact parameter. We suggest that this also explains why the south-western edge of the subcluster core is narrow and stable over similar to 150 kpc in length, but the north-eastern edge is broad and being stripped of material.
C1 [Russell, H. R.; McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada.
[McNamara, B. R.; Nulsen, P. E. J.; O'Dea, C. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sanders, J. S.; Fabian, A. C.; Canning, R. E. A.; King, L. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Baum, S. A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
[Baum, S. A.] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA.
[Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[King, L. J.] Univ Texas Dallas, Dept Phys, Richardson, TX 75080 USA.
[O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA.
RP Russell, HR (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
EM helen.russell@uwaterloo.ca
OI Edge, Alastair/0000-0002-3398-6916; Sanders, Jeremy/0000-0003-2189-4501;
Nulsen, Paul/0000-0003-0297-4493
FU Canadian Space Agency; National Aeronautics and Space Administration
[16617775, NAS8-03060]; Royal Society; STFC; Radcliffe Institute for
Advanced Study at Harvard University
FX HRR and BRM acknowledge generous financial support from the Canadian
Space Agency Space Science Enhancement Program. HRR also acknowledges
support for this work provided by the National Aeronautics and Space
Administration through Chandra Award Number 16617775 issued by the
Chandra X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of the National Aeronautics
and Space Administration under contract NAS8-03060. ACF and LJK thank
the Royal Society for support. REAC acknowledges funding from the STFC.
SAB is supported in part by the Radcliffe Institute for Advanced Study
at Harvard University. We thank the reviewer for helpful and
constructive comments. We thank Poshak Gandhi and Sakurako Okamoto for
help with the Subaru observations of Abell 2146. We thank Eugene
Churazov, Roderick Johnstone and Julie Hlavacek-Larrondo for helpful
discussions.
NR 86
TC 32
Z9 32
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN
PY 2012
VL 423
IS 1
BP 236
EP 255
DI 10.1111/j.1365-2966.2012.20808.x
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 949TP
UT WOS:000304599100020
ER
PT J
AU Hussain, GAJ
Brickhouse, NS
Dupree, AK
Reale, F
Favata, F
Jardine, MM
AF Hussain, G. A. J.
Brickhouse, N. S.
Dupree, A. K.
Reale, F.
Favata, F.
Jardine, M. M.
TI Chandra study of the eclipsing M dwarf binary, YY Gem
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: spectroscopic; binaries: eclipsing; stars: coronae; stars:
flare; stars: magnetic field; X-rays: stars
ID X-RAY SPECTROSCOPY; MAIN-SEQUENCE; CORONAL STRUCTURE; STELLAR FLARES;
EMISSION; SYSTEM; STARS; LOOPS; DECAY; MASS
AB The eclipsing M dwarf binary system, YY Gem, was observed using Chandra covering 140 ks (2Prot) in total, split into two even exposures separated by 0.76 d (0.94 Prot). The system was extremely active: three energetic flares were observed over the course of these observations. The flaring and non-flaring states of the system are analysed in this paper. The activity level increased between the first and second observations even during the quiescent (non-flaring) phases. An analysis of the dynamics of the X-ray-emitting plasma suggests that both components are significantly active. Contemporaneous Ha spectra also suggest that both components show similar levels of activity. The primary star is the likely source of at least two of the flares. From a detailed analysis of the flare emission at the maximum temperature and maximum density with single loop flare models, we find loop lengths of similar to 0.7R*, 1.5R* and 1.8R*. All of these flares are strongly associated with hot (>10 MK) X-ray emission which appears to predominantly trace the orbital motion of the primary star. The two largest flaring loops are similar to the largest sizes reported in other active M stars and span nearly half the interbinary system; this may indicate magnetospheric interaction between the binary star coronae. We discuss the time and spectral resolution requirements that are necessary to recover detailed information about coronal structure from the X-ray spectra in similar cool star systems.
C1 [Hussain, G. A. J.] ESO, D-85748 Garching, Germany.
[Brickhouse, N. S.; Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Reale, F.] Univ Palermo, Dipartimento Fis, I-90134 Palermo, Italy.
[Favata, F.] European Space Agcy, F-75015 Paris, France.
[Jardine, M. M.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
RP Hussain, GAJ (reprint author), ESO, Karl-Schwarzschild-Str 2, D-85748 Garching, Germany.
EM ghussain@eso.org
OI Brickhouse, Nancy/0000-0002-8704-4473; Reale, Fabio/0000-0002-1820-4824
FU NSF-PREST [AST-0440784]; Agenzia Spaziale Italiana (ASI), ASI-INAF
[I/009/10/0]; National Aeronautics and Space Administration through
Chandra X-ray Observatory Center [GO6-7012X]; National Aeronautics Space
Administration [NAS8-03060]
FX The authors would like to thank the referee, John Pye, for his careful
reading of the manuscript and helpful comments. This research utilized
spectra obtained in service observing mode by Nancy D. Morrison, Erica
N. Hesselbach and Gregory B. Thompson at Ritter Observatory with support
from the NSF-PREST programme under grant no. AST-0440784. FR
acknowledges support from Agenzia Spaziale Italiana (ASI), ASI-INAF
Contract I/009/10/0. Support for this work was provided by the National
Aeronautics and Space Administration through Chandra Award Number
GO6-7012X issued by the Chandra X-ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of the National Aeronautics Space Administration under contract
NAS8-03060. This research has made use of software provided by the
Chandra X-ray Center (CXC) in the application packages CIAO and SHERPA.
NR 35
TC 3
Z9 3
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN
PY 2012
VL 423
IS 1
BP 493
EP 504
DI 10.1111/j.1365-2966.2012.20894.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 949TP
UT WOS:000304599100038
ER
PT J
AU Estrada-Villegas, S
McGill, BJ
Kalko, EKV
AF Estrada-Villegas, Sergio
McGill, Brian J.
Kalko, Elisabeth K. V.
TI Determinants of species evenness in a neotropical bat ensemble
SO OIKOS
LA English
DT Article
ID MYOTIS-NIGRICANS; MODEL SELECTION; BODY-MASS; DIVERSITY; RICHNESS;
COMMUNITY; ABUNDANCE; FOREST; ECOLOGY; INDEXES
AB Evenness is an important property of communities. Species richness alone does not capture the fact that one or a few species may dominate total abundance and biomass of a community. This in turn has important consequences for ecosystem functioning and species interactions. Evenness has been observed to vary systematically along environmental and productivity gradients. However, a truly general theory about which factors control evenness in a community has yet to emerge. Prior research on evenness has suggested that high richness, biomass and abundance should lead to lower community evenness in our study system of bats in Panama. However, only few empirical studies examine the simultaneous effects of species richness, biomass or abundance on evenness. For the first time, we applied path analysis in the study of evenness to tease apart the relative importance and direction (positive or negative) of causality among these three factors. As predicted, we found that evenness decreases with increasing species richness, abundance and biomass. The negative effect of abundance was mediated by the positive joint effect of biomass and richness. The selected models varied in the strength of the correlation between the three variables with evenness but their direction was consistent. Overall, we argue that rarity, high mobility and differences in resource availability at sites with lower environmental stress can explain the negative effects of richness on evenness.
C1 [Estrada-Villegas, Sergio] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
[Estrada-Villegas, Sergio] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[McGill, Brian J.] Univ Maine, Sch Biol & Ecol, Orono, ME 04469 USA.
[McGill, Brian J.] Univ Maine, Sustainabil Solut Initiat, Orono, ME 04469 USA.
RP Estrada-Villegas, S (reprint author), McGill Univ, Dept Biol, 1205 Dr Penfield Ave, Montreal, PQ H3A 1B1, Canada.
EM sergio.estradavillegas@mail.mcgill.ca
RI McGill, Brian/A-3476-2008
OI McGill, Brian/0000-0002-0850-1913
FU Neotropical Environment Option; Smithsonian Tropical Research Inst.;
NSERC
FX SEV would like to thank Laura Jara Reyes for her invaluable support
throughout the project. Eric Pedersen and Allen Larocque provided great
help with path analysis. Julie Messier, Richard Feldman, Peter White and
Christoph Meyer provided valuable comments to the manuscript. The
discussion and the analysis therein benefitted from very constructive
conversations with Andrew Gonzalez. Richard Stevens was very helpful in
the latest revision. We thank the Neotropical Environment Option and the
Smithsonian Tropical Research Inst. for excellent logistics and funding.
We also thank the InterContinental Playa Bonita Resort and Spa for
allowing us to work in their property. NSERC provided funding to BJM.
This work is dedicated to Prof. Dr. Elisabeth K. V. Kalko. Her humble
personality, true friendship, deep love for all natures' wonders, her
sense of responsibility and profound interest in tropical community
ecology will be greatly missed. Dr. Kalko was affiliated to the
Institute of Experimental Ecology, University of Ulm, Germany, and the
Smithsonian Tropical Research Institute, Panama.
NR 57
TC 5
Z9 5
U1 3
U2 32
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0030-1299
EI 1600-0706
J9 OIKOS
JI Oikos
PD JUN
PY 2012
VL 121
IS 6
BP 927
EP 941
DI 10.1111/j.1600-0706.2011.19837.x
PG 15
WC Ecology
SC Environmental Sciences & Ecology
GA 946XD
UT WOS:000304389900014
ER
PT J
AU Arnoldi, MJ
Morphy, H
Nzewi, USC
Thompson, K
Kreamer, CM
Ross, DH
AF Arnoldi, Mary Jo
Morphy, Howard
Nzewi, Ugochukwu-Smooth C.
Thompson, Krista
Kreamer, Christine Mullen
Ross, Doran H.
TI Ivan Karp (1943-2011) in memoriam
SO AFRICAN ARTS
LA English
DT Biographical-Item
C1 [Arnoldi, Mary Jo] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA.
[Morphy, Howard] Australian Natl Univ, Res Sch Humanities & Arts, Canberra, ACT 0200, Australia.
[Nzewi, Ugochukwu-Smooth C.] Emory Univ, Art Hist Dept, Atlanta, GA 30322 USA.
[Thompson, Krista] Northwestern Univ, Art Hist Dept, Evanston, IL 60208 USA.
[Kreamer, Christine Mullen] Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA.
[Ross, Doran H.] UCLA African Studies, Los Angeles, CA USA.
RP Arnoldi, MJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA.
EM arnoldim@si.edu; howard.morphy@anu.edu.au; unzewi@emory.edu;
krista-thompson@northwestern.edu; kream-erc@si.edu;
Center.dross@arts.ucla.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU MIT PRESS
PI CAMBRIDGE
PA 55 HAYWARD STREET, CAMBRIDGE, MA 02142 USA
SN 0001-9933
J9 AFR ARTS
JI Afr. Arts
PD SUM
PY 2012
VL 45
IS 2
BP 8
EP 11
PG 4
WC Art
SC Art
GA 942DV
UT WOS:000304023500002
ER
PT J
AU Ackermann, M
Ajello, M
Ballet, J
Barbiellini, G
Bastieri, D
Bellazzini, R
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bottacini, E
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cavazzuti, E
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Cutini, S
D'Ammando, F
de Palma, F
Dermer, CD
Silva, EDE
Drell, PS
Drlica-Wagner, A
Dubois, R
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Fuhrmann, L
Fukazawa, Y
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guiriec, S
Hadasch, D
Hayashida, M
Hughes, RE
Itoh, R
Johannesson, G
Johnson, AS
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Larsson, S
Lee, SH
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nishino, S
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ozaki, M
Paneque, D
Panetta, JH
Pelassa, V
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Rastawicki, D
Razzano, M
Readhead, A
Reimer, A
Reimer, O
Reyes, LC
Richards, JL
Sbarra, C
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Szostek, A
Takahashi, H
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Winer, BL
Wood, KS
Yang, Z
Zimmer, S
Moderski, R
Nalewajko, K
Sikora, M
Villata, M
Raiteri, CM
Aller, HD
Aller, MF
Arkharov, AA
Benitez, E
Berdyugin, A
Blinov, DA
Boettcher, M
Calle, OJAB
Buemi, CS
Carosati, D
Chen, WP
Diltz, C
Di Paola, A
Dolci, M
Efimova, NV
Forne, E
Gurwell, MA
Heidt, J
Hiriart, D
Jordan, B
Kimeridze, G
Konstantinova, TS
Kopatskaya, EN
Koptelova, E
Kurtanidze, OM
Lahteenmaki, A
Larionova, EG
Larionova, LV
Larionov, VM
Leto, P
Lindfors, E
Lin, HC
Morozova, DA
Nikolashvili, MG
Nilsson, K
Oksman, M
Roustazadeh, P
Sievers, A
Sigua, LA
Sillanpaa, A
Takahashi, T
Takalo, LO
Tornikoski, M
Trigilio, C
Troitsky, IS
Umana, G
Angelakis, E
Krichbaum, TP
Nestoras, I
Riquelme, D
Krips, M
Trippe, S
Arai, A
Kawabata, KS
Sakimoto, K
Sasada, M
Sato, S
Uemura, M
Yamanaka, M
Yoshida, M
Belloni, T
Tagliaferri, G
Bonning, EW
Isler, J
Urry, CM
Hoversten, E
Falcone, A
Pagani, C
Stroh, M
AF Ackermann, M.
Ajello, M.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bellazzini, R.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bottacini, E.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Cutini, S.
D'Ammando, F.
de Palma, F.
Dermer, C. D.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Dubois, R.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Fuhrmann, L.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guiriec, S.
Hadasch, D.
Hayashida, M.
Hughes, R. E.
Itoh, R.
Johannesson, G.
Johnson, A. S.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Larsson, S.
Lee, S. -H.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Naumann-Godo, M.
Nishino, S.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Pelassa, V.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Rastawicki, D.
Razzano, M.
Readhead, A.
Reimer, A.
Reimer, O.
Reyes, L. C.
Richards, J. L.
Sbarra, C.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Szostek, A.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Zimmer, S.
Moderski, R.
Nalewajko, K.
Sikora, M.
Villata, M.
Raiteri, C. M.
Aller, H. D.
Aller, M. F.
Arkharov, A. A.
Benitez, E.
Berdyugin, A.
Blinov, D. A.
Boettcher, M.
Calle, O. J. A. Bravo
Buemi, C. S.
Carosati, D.
Chen, W. P.
Diltz, C.
Di Paola, A.
Dolci, M.
Efimova, N. V.
Forne, E.
Gurwell, M. A.
Heidt, J.
Hiriart, D.
Jordan, B.
Kimeridze, G.
Konstantinova, T. S.
Kopatskaya, E. N.
Koptelova, E.
Kurtanidze, O. M.
Lahteenmaki, A.
Larionova, E. G.
Larionova, L. V.
Larionov, V. M.
Leto, P.
Lindfors, E.
Lin, H. C.
Morozova, D. A.
Nikolashvili, M. G.
Nilsson, K.
Oksman, M.
Roustazadeh, P.
Sievers, A.
Sigua, L. A.
Sillanpaa, A.
Takahashi, T.
Takalo, L. O.
Tornikoski, M.
Trigilio, C.
Troitsky, I. S.
Umana, G.
Angelakis, E.
Krichbaum, T. P.
Nestoras, I.
Riquelme, D.
Krips, M.
Trippe, S.
Arai, A.
Kawabata, K. S.
Sakimoto, K.
Sasada, M.
Sato, S.
Uemura, M.
Yamanaka, M.
Yoshida, M.
Belloni, T.
Tagliaferri, G.
Bonning, E. W.
Isler, J.
Urry, C. M.
Hoversten, E.
Falcone, A.
Pagani, C.
Stroh, M.
CA Fermi-LAT Collaboration
GASP-WEBT Consortium
F-GAMMA
Iram-PdBI
Kanata
RXTE
SMARTS
Swift-XRT
TI MULTI-WAVELENGTH OBSERVATIONS OF BLAZAR AO 0235+164 IN THE 2008-2009
FLARING STATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (AO 0235+164); galaxies: active;
galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal
ID BL-LACERTAE OBJECT; ACTIVE GALACTIC NUCLEI; SOUTHERN SPECTROPHOTOMETRIC
STANDARDS; RELATIVISTIC RECONFINEMENT SHOCKS; SPECTRAL
ENERGY-DISTRIBUTIONS; LARGE-AREA TELESCOPE; GAMMA-RAY OUTBURST;
SOFT-X-RAY; RADIO-SOURCES; ABSORPTION-LINE
AB The blazarAO 0235+164 (z=0.94) has been one of the most active objects observed by Fermi Large Area Telescope (LAT) since its launch in Summer 2008. In addition to the continuous coverage by Fermi, contemporaneous observations were carried out from the radio to gamma-ray bands between 2008 September and 2009 February. In this paper, we summarize the rich multi-wavelength data collected during the campaign (including F-GAMMA, GASP-WEBT, Kanata, OVRO, RXTE, SMARTS, Swift, and other instruments), examine the cross-correlation between the light curves measured in the different energy bands, and interpret the resulting spectral energy distributions in the context of well-known blazar emission models. We find that the gamma-ray activity is well correlated with a series of near-IR/optical flares, accompanied by an increase in the optical polarization degree. On the other hand, the X-ray light curve shows a distinct 20 day high state of unusually soft spectrum, which does not match the extrapolation of the optical/UV synchrotron spectrum. We tentatively interpret this feature as the bulk Compton emission by cold electrons contained in the jet, which requires an accretion disk corona with an effective covering factor of 19% at a distance of 100 R-g. We model the broadband spectra with a leptonic model with external radiation dominated by the infrared emission from the dusty torus.
C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Rastawicki, D.; Reimer, A.; Reimer, O.; Szostek, A.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ajello, M.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Raino, S.; Rastawicki, D.; Reimer, A.; Reimer, O.; Szostek, A.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Ballet, J.; Casandjian, J. M.; Charles, E.; Grenier, I. A.; Naumann-Godo, M.] CEA IRFU CNRS Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Sbarra, C.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Bregeon, J.; Pesce-Rollins, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS IN2P3, Lab Univ & Particules Montpellier, Montpellier, France.
[D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy.
[D'Ammando, F.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy.
[Dermer, C. D.; Lovellette, M. N.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ferrara, E. C.; Gehrels, N.; McEnery, J. E.; Thompson, D. J.; Troja, E.; Wood, K. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fuhrmann, L.; Angelakis, E.; Krichbaum, T. P.; Nestoras, I.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Fukazawa, Y.; Itoh, R.; Mizuno, T.; Nishino, S.; Sakimoto, K.; Sasada, M.; Yamanaka, M.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.; Pelassa, V.] Univ Alabama Huntsville, CSPAR, Huntsville, AL 35899 USA.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France.
[Larsson, S.; Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, S-10691 Stockholm, Sweden.
[Larsson, S.; Yang, Z.; Zimmer, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden.
[Larsson, S.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden.
[Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Lott, B.] Univ Bordeaux 1, CEN Bordeaux Gradignan, CNRS IN2p3, F-33175 Gradignan, France.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohsugi, T.; Takahashi, H.; Kawabata, K. S.; Uemura, M.; Yoshida, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.; Takahashi, T.] Inst Space & Astronaut Sci, JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Razzano, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Razzano, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Readhead, A.; Richards, J. L.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93401 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Vianello, G.; Vitale, V.] CIFS, I-10133 Turin, Italy.
Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Moderski, R.; Nalewajko, K.; Sikora, M.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Nalewajko, K.] Univ Colorado, Boulder, CO 80309 USA.
[Villata, M.; Raiteri, C. M.] INAF, Osservatorio Astron Torino, I-10025 Pino Torinese, TO, Italy.
[Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Arkharov, A. A.; Blinov, D. A.; Efimova, N. V.; Larionov, V. M.] Pulkovo Observ, St Petersburg 196140, Russia.
[Benitez, E.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City, DF, Mexico.
[Berdyugin, A.; Lindfors, E.; Roustazadeh, P.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland.
[Diltz, C.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Boettcher, M.; Calle, O. J. A. Bravo; Efimova, N. V.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Larionov, V. M.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia.
[Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, I-95123 Catania, Italy.
[Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain.
[Carosati, D.] INAF, TNG Fdn Galileo Galilei, La Palma, Spain.
[Chen, W. P.; Kopatskaya, E. N.; Koptelova, E.; Lin, H. C.] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan.
[Di Paola, A.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy.
[Dolci, M.] Osservatorio Astron Collurania Vincenzo Cerruli, I-64100 Teramo, Italy.
[Forne, E.] Agrupacio Astron Sabadell, Sabadell 08206, Spain.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Heidt, J.] Heidelberg Univ, Konigstuhl, Landessternwarte, D-69117 Heidelberg, Germany.
[Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico.
[Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland.
[Kimeridze, G.; Kurtanidze, O. M.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia.
[Koptelova, E.] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan.
[Torres, D. F.; Lahteenmaki, A.; Oksman, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland.
[Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia.
[Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikio, Finland.
[Sievers, A.; Riquelme, D.] Inst Radio Astron Millimetr, Granada 18012, Spain.
[Krips, M.] Domaine Univ, Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Trippe, S.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea.
[Arai, A.] Kyoto Univ, Grad Sch Sci, Dept Phys, Kyoto, Japan.
[Sato, S.] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Belloni, T.; Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Bonning, E. W.; Isler, J.; Urry, C. M.] Yale Univ, Dept Astron, Dept Phys, New Haven, CT 06520 USA.
[Bonning, E. W.; Isler, J.; Urry, C. M.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Hoversten, E.; Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Pagani, C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM eduardo@slac.stanford.edu; fabio.gargano@ba.infn.it;
madejski@slac.stanford.edu; silvia.raino@ba.infn.it;
lreyes04@calpoly.edu; knalew@colorado.edu; sikora@camk.edu.pl
RI Urry, Claudia/G-7381-2011; Lahteenmaki, Anne/L-5987-2013; Kurtanidze,
Omar/J-6237-2014; Morozova, Daria/H-1298-2013; Troitskiy,
Ivan/K-7979-2013; Grishina, Tatiana/H-6873-2013; Johannesson,
Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano,
Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016;
lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss,
Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer,
Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013;
Kopatskaya, Evgenia/H-4720-2013; Larionova, Elena/H-7287-2013; Efimova,
Natalia/I-2196-2013; Blinov, Dmitry/G-9925-2013; Ozaki,
Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Orlando,
E/R-5594-2016;
OI Urry, Claudia/0000-0002-0745-9792; Morozova, Daria/0000-0002-9407-7804;
Troitskiy, Ivan/0000-0002-4218-0148; Grishina,
Tatiana/0000-0002-3953-6676; Johannesson, Gudlaugur/0000-0003-1458-7036;
Loparco, Francesco/0000-0002-1173-5673; Gargano,
Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X;
Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; lubrano, pasquale/0000-0003-0221-4806;
Morselli, Aldo/0000-0002-7704-9553; giglietto,
nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Larionov,
Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X;
Larionova, Elena/0000-0002-2471-6500; Efimova,
Natalia/0000-0002-8071-4753; Blinov, Dmitry/0000-0003-0611-5784; Dolci,
Mauro/0000-0001-8000-5642; Buemi, Carla Simona/0000-0002-7288-4613;
Villata, Massimo/0000-0003-1743-6946; Larionova,
Liudmila/0000-0002-0274-1481; giommi, paolo/0000-0002-2265-5003; Umana,
Grazia/0000-0002-6972-8388; Caraveo, Patrizia/0000-0003-2478-8018; Leto,
Paolo/0000-0003-4864-2806; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI,
Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Raiteri,
Claudia Maria/0000-0003-1784-2784; Sasada, Mahito/0000-0001-5946-9960;
Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577;
Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti,
Marcello/0000-0002-8657-8852; Angelakis, Emmanouil/0000-0001-7327-5441;
Cutini, Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495;
Tagliaferri, Gianpiero/0000-0003-0121-0723
FU National Aeronautics and Space Administration [NNX10AJ70G]; Department
of Energy in the United States; Commissariat a l'Energie Atomique;
Centre National de la Recherche Scientifique/Institut National de
Physique Nucleaire et de Physique des Particules in France; Agenzia
Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy;
Ministry of Education, Culture, Sports, Science and Technology (MEXT);
High Energy Accelerator Research Organization (KEK); Japan Aerospace
Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish
Research Council; Swedish National Space Board in Sweden; Istituto
Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in
France; Polish MNiSW [N N203 301635]; Kavli Institute for Cosmological
Physics at the University of Chicago [NSF PHY-0114422, NSF PHY-0551142];
Georgian National Science Foundation [GNSF/ST08/4-404]; Academy of
Finland [212656, 210338, 121148]; Smithsonian Institution; Academia
Sinica; Fermi GI [011283, 31155, NNX10AP16G, NNX11AO13G]; Fermi Guest
Investigator [NNX08AW56G, NNX09AU10G]; University of Michigan;
[AST-0607523]
FX The Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.;
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France.; We
acknowledge the support by the Polish MNiSW grant N N203 301635.; L. C.
Reyes acknowledges support from NASA through Swift Guest Investigator
Grant NNX10AJ70G; as well as support by the Kavli Institute for
Cosmological Physics at the University of Chicago through grants NSF
PHY-0114422 and NSF PHY-0551142 and an endowment from the Kavli
Foundation and its founder Fred Kavli.; The Abastumani team acknowledges
financial support by the Georgian National Science Foundation through
grant GNSF/ST08/4-404.; The Metsahovi team acknowledges the support from
the Academy of Finland to our observing projects (numbers 212656,
210338, 121148, and others).; The Submillimeter Array is a joint project
between the Smithsonian Astrophysical Observatory and the Academia
Sinica Institute of Astronomy and Astrophysics and is funded by the
Smithsonian Institution and the Academia Sinica.; The acquisition and
analysis of the SMARTS data are supported by Fermi GI grants 011283 and
31155 (PI:C. Bailyn).; Data from the Steward Observatory
spectropolarimetric monitoring project were used. This program is
supported by Fermi Guest Investigator grants NNX08AW56G and NNX09AU10G.;
UMRAO research is supported by a series of grants from the NSF and NASA,
most recently AST-0607523 and Fermi GI grants NNX10AP16G and NNX11AO13G,
respectively; funds for telescope operation are provided by the
University of Michigan.
NR 112
TC 25
Z9 25
U1 0
U2 17
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2012
VL 751
IS 2
AR 159
DI 10.1088/0004-637X/751/2/159
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600080
ER
PT J
AU Bietenholz, MF
Brunthaler, A
Soderberg, AM
Krauss, M
Zauderer, B
Bartel, N
Chomiuk, L
Rupen, MP
AF Bietenholz, M. F.
Brunthaler, A.
Soderberg, A. M.
Krauss, M.
Zauderer, B.
Bartel, N.
Chomiuk, L.
Rupen, M. P.
TI VLBI OBSERVATIONS OF THE NEARBY TYPE IIb SUPERNOVA 2011dh
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radio continuum: general; supernovae: individual (SN 2011dh)
ID SN 1993J VLBI; ANISOTROPIC EXPANSION; RADIO SUPERNOVAE; SPIRAL GALAXIES;
SN-1993J VLBI; PROGENITOR; COMPACT; M51; EVOLUTION; SHELL
AB We report on phase-referenced very long baseline interferometry radio observations of the Type IIb supernova 2011dh, at times t = 83 days and 179 days after the explosion and at frequencies, respectively, of 22.2 and 8.4 GHz. We detected SN 2011dh at both epochs. At the first epoch only an upper limit on SN 2011dh's angular size was obtained, but at the second epoch, we determine the angular radius of SN 2011dh's radio emission to be 0.25 +/- 0.08 mas by fitting a spherical shell model directly to the visibility measurements. At a distance of 8.4 Mpc, this angular radius corresponds to a time-averaged (since t = 0) expansion velocity of the forward shock of 21,000 +/- 7000 km s(-1). Our measured values of the radius of the emission region are in excellent agreement with those derived from fitting synchrotron self-absorbed models to the radio spectral energy distribution, providing strong confirmation for the latter method of estimating the radius. We find that SN 2011dh's radius evolves in a power-law fashion, with R proportional to t(0.92+/-0.10).
C1 [Bietenholz, M. F.] Hartebeesthoek Radio Observ, ZA-1740 Krugersdorp, South Africa.
[Bietenholz, M. F.; Bartel, N.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Brunthaler, A.; Krauss, M.; Chomiuk, L.; Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Soderberg, A. M.; Zauderer, B.; Chomiuk, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Bietenholz, MF (reprint author), Hartebeesthoek Radio Observ, POB 443, ZA-1740 Krugersdorp, South Africa.
FU NSERC; European Union [275596]
FX Research at York University was partly supported by NSERC. A. B. was
supported by a Marie Curie Outgoing International Fellowship (FP7) of
the European Union (project number 275596). L. C. is a Jansky Fellow at
the NRAO. We thank NRAO for scheduling these target-of-opportunity
observations. Our results are partly based on observations with the 100
m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at
Effelsberg. We made use of the Swinburne University of Technology
software correlator, developed as part of the Australian Major National
Research Facilities Programme and operated under license. In addition,
we also made use of NASA's Astrophysics Data System Bibliographic
Services.
NR 41
TC 17
Z9 17
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2012
VL 751
IS 2
AR 125
DI 10.1088/0004-637X/751/2/125
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600046
ER
PT J
AU Chaty, S
Rahoui, F
AF Chaty, S.
Rahoui, F.
TI BROADBAND ESO/VISIR-SPITZER INFRARED SPECTROSCOPY OF THE OBSCURED
SUPERGIANT X-RAY BINARY IGR J16318-4848
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars; stars: emission-line, Be; stars:
winds, outflows; X-rays: binaries; X-rays: individual (IGR J16318-4848)
ID MULTIWAVELENGTH OBSERVATIONS; CIRCUMSTELLAR DISKS; COMPANION STAR; DUST
GRAINS; GX 301-2; MU-M; EXTINCTION; SPECTRA; HOLE
AB A new class of X-ray binaries has recently been discovered by the high-energy observatory INTEGRAL. It is composed of intrinsically obscured supergiant high-mass X-ray binaries, unveiled by means of multi-wavelength X-ray, optical, near-and mid-infrared observations, in particular, photometric and spectroscopic observations using ESO facilities. However, the fundamental questions about these intriguing sources, namely, their formation, evolution, and the nature of their environment, are still unsolved. Among them, IGR J16318-4848, a compact object orbiting around a supergiant B[e] star, seems to be one of the most extraordinary celestial sources of our Galaxy. We present here new ESO/Very Large Telescope (VLT) VISIR mid-infrared (MIR) spectroscopic observations of this source. First, line diagnostics allow us to confirm the presence of absorbing material (dust and cold gas) enshrouding the whole binary system, and to characterize the nature of this material. Second, by fitting broadband near-to mid-infrared spectral energy distribution, including ESONTT/SofI, VLT/VISIR, and Spitzer data, with a phenomenological model for sgB[e] stars, we show that the star is surrounded by an irradiated rim heated to a temperature of similar to 3800-5500 K, along with a viscous disk component at an inner temperature of similar to 750 K. VISIR data allow us to exclude the spherical geometry for the dust component. This detailed study will allow us in the future to get better constraints on the formation and evolution of such rare and short-living high-mass X-ray binary systems in our Galaxy.
C1 [Chaty, S.; Rahoui, F.] Univ Paris Diderot, AIM, UMR E 9005, CEA,DSM,CNRS,Irfu,Serv Astrophys,Ctr Saclay, FR-91191 Gif Sur Yvette, France.
[Rahoui, F.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Rahoui, F.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Chaty, S (reprint author), Univ Paris Diderot, AIM, UMR E 9005, CEA,DSM,CNRS,Irfu,Serv Astrophys,Ctr Saclay, FR-91191 Gif Sur Yvette, France.
EM sylvain.chaty@cea.fr; frahoui@cfa.harvard.edu
OI Chaty, Sylvain/0000-0002-5769-8601
FU Centre National d'Etudes Spatiales (CNES); [079.D-0454]
FX S.C. thanks the ESO staff who were very helpful during visitor
observations, Peter A. Curran for a careful rereading of the paper and
useful comments, and finally the anonymous referee for constructive
comments on this paper. IRAF is distributed by the National Optical
Astronomy Observatory, which is operated by the Association of
Universities for Research in Astronomy (AURA) under cooperative
agreement with the National Science Foundation. This research has made
use of NASA's Astrophysics Data System Bibliographic Services. This work
was supported by the Centre National d'Etudes Spatiales (CNES). It is
based on observations obtained with MINE: the Multi-wavelength INTEGRAL
NEtwork. This work is also based on observations made with ESO
Telescopes at the La Silla or Paranal Observatories under the program ID
079.D-0454.
NR 33
TC 14
Z9 14
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2012
VL 751
IS 2
AR 150
DI 10.1088/0004-637X/751/2/150
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600071
ER
PT J
AU Chen, XP
Arce, HG
Dunham, MM
Zhang, QZ
Bourke, TL
Launhardt, R
Schmalzl, M
Henning, T
AF Chen, Xuepeng
Arce, Hector G.
Dunham, Michael M.
Zhang, Qizhou
Bourke, Tyler L.
Launhardt, Ralf
Schmalzl, Markus
Henning, Thomas
TI SUBMILLIMETER ARRAY AND SPITZER OBSERVATIONS OF BOK GLOBULE CB 17: A
CANDIDATE FIRST HYDROSTATIC CORE?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: individual objects (CB 17, L1389); ISM: jets and
outflows; stars: formation
ID TRANSLUCENT MOLECULAR CLOUDS; LOW-MASS PROTOSTARS; STAR-FORMATION; DENSE
CORES; BIPOLAR FLOWS; PROTOSTELLAR CORES; LINE FORMATION; DARK CLOUDS;
EVOLUTION; OUTFLOWS
AB We present high angular resolution Submillimeter Array (SMA) and Spitzer observations toward the Bok globule CB 17. SMA 1.3 mm dust continuum images reveal within CB 17 two sources with an angular separation of similar to 21 '' (similar to 5250 AU at a distance of similar to 250 pc). The northwestern continuum source, referred to as CB 17 IRS, dominates the infrared emission in the Spitzer images, drives a bipolar outflow extending in the northwest-southeast direction, and is classified as a low-luminosity Class 0/I transition object (L-bol similar to 0.5 L-circle dot). The southeastern continuum source, referred to as CB 17 MMS, has faint dust continuum emission in the SMA 1.3 mm observations (similar to 6 sigma detection; similar to 3.8 mJy), but is not detected in the deep Spitzer infrared images at wavelengths from 3.6 to 70 mu m. Its bolometric luminosity and temperature, estimated from its spectral energy distribution, are <= 0.04 L-circle dot and <= 16 K, respectively. The SMA CO (2-1) observations suggest that CB 17 MMS may drive a low-velocity molecular outflow (similar to 2.5 km s(-1)), extending in the east-west direction. Comparisons with prestellar cores and Class 0 protostars suggest that CB 17 MMS is more evolved than prestellar cores but less evolved than Class 0 protostars. The observed characteristics of CB 17 MMS are consistent with the theoretical predictions from radiative/magnetohydrodynamical simulations of a first hydrostatic core, but there is also the possibility that CB 17 MMS is an extremely low luminosity protostar deeply embedded in an edge-on circumstellar disk. Further observations are needed to study the properties of CB 17 MMS and to address more precisely its evolutionary stage.
C1 [Chen, Xuepeng; Arce, Hector G.; Dunham, Michael M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Zhang, Qizhou; Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Launhardt, Ralf; Schmalzl, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Schmalzl, Markus] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Chen, XP (reprint author), Yale Univ, Dept Astron, Box 208101, New Haven, CT 06520 USA.
EM xuepeng.chen@yale.edu
OI Zhang, Qizhou/0000-0003-2384-6589
FU Smithsonian Institution; Academia Sinica; National Science Foundation
[0845619, 0708158]
FX The Submillimeter Array is a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics and is funded by the Smithsonian Institution and the
Academia Sinica.; We thank the SMA staff for technical support during
the observations and the Spitzer Science Center for their maintenance of
the Spitzer data. This material is based on work supported by NSF grant
AST-0845619 to H.G.A. This research is supported in part by the National
Science Foundation under grant number 0708158 (T.L.B.).
NR 60
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Z9 29
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2012
VL 751
IS 2
AR 89
DI 10.1088/0004-637X/751/2/89
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600010
ER
PT J
AU Fang, GW
Kong, X
Chen, Y
Lin, XB
AF Fang, Guanwen
Kong, Xu
Chen, Yang
Lin, Xuanbin
TI PASSIVE AND STAR-FORMING GALAXIES AT 1.4 <= z <= 2.5 IN THE AEGIS FIELD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: evolution; galaxies: formation;
galaxies: high-redshift; galaxies: photometry
ID EXTENDED GROTH STRIP; EXTRAGALACTIC LEGACY SURVEY; NEAR-INFRARED
SPECTROSCOPY; ACTIVE GALACTIC NUCLEI; STELLAR MASS FUNCTION; EXTREMELY
RED OBJECTS; K-SELECTED GALAXIES; WIDE AREA SURVEY; HIGH-REDSHIFT;
QUIESCENT GALAXIES
AB Using a simple two-color selection based on g-, z-, and K-band photometry, we choose from 1609 star-forming galaxies (sgzKs) and 422 passively evolving galaxies (pgzKs) at z similar to 2 from a K-band-selected sample (K-AB < 22.0) in an area of similar to 0.44 deg(2) of the All-wavelength Extended Groth Strip International Survey. The number of counts of pgzKs in our sample turn over at K-AB similar to 21.0, and both the number of faint and bright objects (including sgzKs and pgzKs) exceed the predictions of a recent semi-analytic model of galaxy formation; a more successful model is need to explain this diversity. We also find that the star formation rate (SFR) and specific SFR (sSFR) of sgzKs increases with redshift at all masses, implying that star-forming galaxies were much more active on average in the past. Moreover, the sSFR of massive galaxies is lower at all redshifts, suggesting that star formation contributes more to the mass growth of low-mass galaxies than to high-mass galaxies. From the Hubble Space Telescope Wide Field Camera 3 near-infrared imaging data we find that morphologies of z similar to 2 galaxies not only have diffuse structures with lower G and higher M-20 values, but also have single-object morphologies (higher G and lower M20), implying that there are morphological variety and different formation process for these galaxies at z similar to 2. Finally, we also study the fraction of active galactic nuclei (AGNs) in the gzKs, 82 of 828 gzKs with four IRAC bands can be classified as AGNs (similar to 10%). Most of these AGN candidates have L0.5-10 keV > 10(41) erg s(-1).
C1 [Fang, Guanwen; Kong, Xu; Chen, Yang; Lin, Xuanbin] Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Peoples R China.
[Fang, Guanwen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fang, Guanwen; Kong, Xu] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China.
[Kong, Xu; Lin, Xuanbin] Chinese Acad Sci, USTC, Key Lab Res Galaxies & Cosmol, Hefei 230026, Peoples R China.
RP Fang, GW (reprint author), Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Peoples R China.
EM wen@mail.ustc.edu.cn; xkong@ustc.edu.cn
RI Chen, Yang/O-7911-2014
OI Chen, Yang/0000-0002-3759-1487
FU NSF; NASA [NAS5-26555]; STFC; National Natural Science Foundation of
China (NSFC) [10873012]; Key Laboratory for the Structure and Evolution
of Celestial Objects, CAS; Chinese Universities Scientific Fund (CUSF)
FX We thank the anonymous referee for valuable comments and suggestions
that have improved the paper. We thank J.-S. Huang and H. J. McCracken
for helpful suggestions and discussions. This study makes use of data
from AEGIS, a multi-wavelength sky survey conducted with the Chandra,
GALEX, Hubble, Keck, CFHT, MMT, Subaru, Palomar, Spitzer, VLA, and other
telescopes and supported in part by the NSF, NASA, and the STFC. This
work is also 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 the
NASA contract NAS5-26555. The work is supported by the National Natural
Science Foundation of China (NSFC, No. 10873012), the Open Research
Program of Key Laboratory for the Structure and Evolution of Celestial
Objects, CAS, and Chinese Universities Scientific Fund (CUSF).
NR 90
TC 11
Z9 14
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2012
VL 751
IS 2
AR 109
DI 10.1088/0004-637X/751/2/109
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600030
ER
PT J
AU Ganeshalingam, M
Li, WD
Filippenko, AV
Silverman, JM
Chornock, R
Foley, RJ
Matheson, T
Kirshner, RP
Milne, P
Calkins, M
Shen, KJ
AF Ganeshalingam, Mohan
Li, Weidong
Filippenko, Alexei V.
Silverman, Jeffrey M.
Chornock, Ryan
Foley, Ryan J.
Matheson, Thomas
Kirshner, Robert P.
Milne, Peter
Calkins, Mike
Shen, Ken J.
TI THE LOW-VELOCITY, RAPIDLY FADING TYPE Ia SUPERNOVA 2002es
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general; supernovae: individual (SN 2002es, SN 1999bh)
ID AUTOMATIC IMAGING TELESCOPE; PHOTOMETRIC STANDARD STARS; DARK-ENERGY
CONSTRAINTS; DIGITAL SKY SURVEY; LIGHT CURVES; HOST GALAXIES; IMPROVED
DISTANCES; CELESTIAL EQUATOR; LOW-LUMINOSITY; CORE-COLLAPSE
AB SN 2002es is a peculiar subluminous Type Ia supernova (SN Ia) with a combination of observed characteristics never before seen in an SN Ia. At maximum light, SN 2002es shares spectroscopic properties with the underluminous SN 1991bg subclass of SNe Ia, but with substantially lower expansion velocities(similar to 6000 km s(-1)) more typical of the peculiar SN 2002cx subclass. Photometrically, SN 2002es differs from both SN 1991bg-like and SN 2002cx-like supernovae. Although at maximum light it is subluminous (M-B = -17.78 mag), SN 2002es has a relatively broad light curve (Delta m(15)(B) = 1.28 +/- 0.04 mag), making it a significant outlier in the light-curve width versus luminosity relationship. We estimate a Ni-56 mass of 0.17 +/- 0.05 M-circle dot synthesized in the explosion, relatively low for an SN Ia. One month after maximum light, we find an unexpected plummet in the bolometric luminosity. The late-time decay of the light curves is inconsistent with our estimated Ni-56 mass, indicating that either the light curve was not completely powered by Ni-56 decay or the ejecta became optically thin to gamma-rays within a month after maximum light. The host galaxy is classified as an S0 galaxy with little to no star formation, indicating that the progenitor of SN 2002es is likely from an old stellar population. We also present a less extensive data set for SN 1999bh, an object which shares similar photometric and spectroscopic properties. Both objects were found as part of the Lick Observatory Supernova Search, allowing us to estimate that these objects should account for 2.5% of SNe Ia within a fixed volume. Current theoretical models are unable to explain the observed characteristics of SN 2002es.
C1 [Ganeshalingam, Mohan; Li, Weidong; Filippenko, Alexei V.; Silverman, Jeffrey M.; Shen, Ken J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Chornock, Ryan; Foley, Ryan J.; Kirshner, Robert P.; Calkins, Mike] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Milne, Peter] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Shen, Ken J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Ganeshalingam, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM mganesh@astro.berkeley.edu
FU U.S. National Science Foundation (NSF) [AST-0607485, AST-0