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
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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-0908886];
TABASGO Foundation; U.S. Department of Energy SciDAC
[DE-FC02-06ER41453]; NSF [AST-0907903]; W. M. Keck Foundation; U.S.
Department of Energy [DE-FG02-08ER41563]; NASA
FX The research of A.V.F.'s supernova group at UC Berkeley has been
generously supported by the U.S. National Science Foundation (NSF; most
recently through grants AST-0607485 and AST-0908886), the TABASGO
Foundation, U.S. Department of Energy SciDAC grant DE-FC02-06ER41453,
and U.S. Department of Energy grant DE-FG02-08ER41563. KAIT and its
ongoing operation were made possible by donations from Sun Microsystems,
Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick
Observatory, the NSF, the University of California, the Sylvia & Jim
Katzman Foundation, the Richard and Rhoda Goldman Fund, and the TABASGO
Foundation. Supernova research at Harvard is supported in part by NSF
grant AST-0907903. Some of the data presented in this paper were
obtained at the W. M. Keck Observatory, which is operated as a
scientific partnership among the California Institute of Technology, the
University of California, and the National Aeronautics and Space
Administration (NASA); the observatory was made possible by the generous
financial support of the W. M. Keck Foundation. The authors wish to
recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community; we are most fortunate to have the
opportunity to conduct observations from this mountain. We made use of
the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 124
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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 1
PY 2012
VL 751
IS 2
AR 142
DI 10.1088/0004-637X/751/2/142
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600063
ER
PT J
AU Harris, RJ
Andrews, SM
Wilner, DJ
Kraus, AL
AF Harris, Robert J.
Andrews, Sean M.
Wilner, David J.
Kraus, Adam L.
TI A RESOLVED CENSUS OF MILLIMETER EMISSION FROM TAURUS MULTIPLE STAR
SYSTEMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; protoplanetary disks; stars: formation
ID SOLAR-TYPE STARS; SUBMILLIMETER CONTINUUM FLUX; CIRCUMSTELLAR DUST
DISKS; MAIN-SEQUENCE STARS; CLOSE BINARY STARS; T-TAURI; YOUNG BINARIES;
FORMING REGIONS; PROTOPLANETARY DISK; VLBA DETERMINATION
AB We present a high angular resolution millimeter-wave dust continuum imaging survey of circumstellar material associated with the individual components of 23 multiple star systems in the Taurus-Auriga young cluster. Combined with previous measurements in the literature, these new data permit a comprehensive look at how the millimeter luminosity (a rough tracer of disk mass) relates to the separation and mass of a stellar companion. Approximately one-third (28%-37%) of the individual stars in multiple systems have detectable millimeter emission, an incidence rate half that for single stars (similar to 62%) which does not depend on the number of companions. There is a strong, positive correlation between the luminosity and projected separation (a(p)) of a stellar pair. Wide pairs (a(p) > 300 AU) have a similar luminosity distribution as single stars, medium pairs (a(p) approximate to 30-300 AU) are a factor of five fainter, and close pairs (a(p) < 30 AU) are similar to 5x fainter yet (aside from a small, but notable population of bright circumbinary disks). In most cases, the emission is dominated by a disk around the primary (or a wide tertiary in hierarchical triples), but there is no clear relationship between luminosity and stellar mass ratio. A direct comparison of resolved disk sizes with predictions from tidal truncation models yields mixed results; some disks are much larger than expected given the projected distances of their companions. We suggest that the presence of a stellar companion impacts disk properties at a level comparable to the internal evolution mechanisms that operate in an isolated system, with both the multiple star formation process itself and star-disk tidal interactions likely playing important roles in the evolution of circumstellar material. From the perspective of the mass content of the disk reservoir, we expect that (giant) planet formation is inhibited around the components of close pairs or secondaries, but should be as likely as for single stars around the primaries (or wide tertiaries in hierarchical triples) in more widely separated multiple star systems.
C1 [Harris, Robert J.; Andrews, Sean M.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kraus, Adam L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Harris, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Smithsonian Institution; Academia Sinica
FX We are grateful to Trent Dupuy for his assistance with the probabilistic
treatment of projected orbits, to Joanna Brown for kindly providing some
supplementary observing time on the FQ Tau binary, and to an anonymous
referee for helpful suggestions on clarifying the draft manuscript. The
Submillimeter Array (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.
NR 99
TC 58
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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 1
PY 2012
VL 751
IS 2
AR 115
DI 10.1088/0004-637X/751/2/115
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600036
ER
PT J
AU Johnson, RE
Zuhone, J
Jones, C
Forman, WR
Markevitch, M
AF Johnson, Ryan E.
Zuhone, John
Jones, Christine
Forman, William R.
Markevitch, Maxim
TI SLOSHING GAS IN THE CORE OF THE MOST LUMINOUS GALAXY CLUSTER
RXJ1347.5-1145
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: interactions; X-rays: galaxies:
clusters
ID SUNYAEV-ZELDOVICH MAP; X-RAY-CLUSTER; RX J1347.5-1145; COLD FRONTS;
CHANDRA OBSERVATION; DARK-MATTER; XMM-NEWTON; J1347-1145; MASS;
CONSTRAINTS
AB We present new constraints on the merger history of the most X-ray luminous cluster of galaxies, RXJ1347.5-1145, based on its unique multiwavelength morphology. Our X-ray analysis confirms that the core gas is undergoing "sloshing" resulting from a prior, large-scale, gravitational perturbation. In combination with multiwavelength observations, the sloshing gas points to the primary and secondary clusters having had at least two prior strong gravitational interactions. The evidence supports a model in which the secondary subcluster with mass M = 4.8 +/- 2.4 x 10(14) M-circle dot has previously (greater than or similar to 0.6 Gyr ago) passed by the primary cluster, and has now returned for a subsequent crossing where the subcluster's gas has been completely stripped from its dark matter halo. RXJ1347 is a prime example of how core gas sloshing may be used to constrain the merger histories of galaxy clusters through multiwavelength analyses.
C1 [Johnson, Ryan E.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA.
[Johnson, Ryan E.; Zuhone, John; Jones, Christine; Forman, William R.; Markevitch, Maxim] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Zuhone, John; Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
RP Johnson, RE (reprint author), Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA.
EM johnsonr@denison.edu; jzuhone@cfa.harvard.edu; cjf@cfa.harvard.edu;
wrf@cfa.harvard.edu; maxim@head.cfa.harvard.edu
OI Forman, William/0000-0002-9478-1682
FU NASA; ASC/Alliance Center for Astrophysical Thermonuclear Flashes at the
University of Chicago; SAO; CFD; Chandra grant [GO8-9128X]
FX This research has made extensive use of SAOImager DS9, in addition to
software provided by the CXC in the application packages CIAO, ChIPS,
and Sherpa. This research has made use of the NASA/IPAC Extragalactic
Database (NED) which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA. The
simulation software used in this work was in part developed by the
DOE-supported ASC/Alliance Center for Astrophysical Thermonuclear
Flashes at the University of Chicago. R.E.J. was supported by an SAO
predoctoral fellowship and a CFD fellowship during this work. J.A.Z. was
supported by Chandra grant GO8-9128X, as well as by an appointment to
the NASA Postdoctoral Program at the Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA.
NR 47
TC 10
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U1 0
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 1
PY 2012
VL 751
IS 2
AR 95
DI 10.1088/0004-637X/751/2/95
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600016
ER
PT J
AU Kilic, M
Brown, WR
Prieto, CA
Kenyon, SJ
Heinke, CO
Agueros, MA
Kleinman, SJ
AF Kilic, Mukremin
Brown, Warren R.
Allende Prieto, Carlos
Kenyon, S. J.
Heinke, Craig O.
Agueeros, M. A.
Kleinman, S. J.
TI THE ELM SURVEY. IV. 24 WHITE DWARF MERGER SYSTEMS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; Galaxy: stellar content; gravitational waves;
supernovae: general; white dwarfs
ID EXTREMELY LOW-MASS; DIGITAL SKY SURVEY; DOUBLE DEGENERATE SYSTEM; BINARY
NLTT 11748; AM CVN STARS; SURFACE DETONATIONS; COMPACT OBJECTS; SDSS
1257+5428; NEUTRON-STAR; SPY PROJECT
AB We present new radial velocity and X-ray observations of extremely low mass (ELM, similar to 0.2M(circle dot)) white dwarf (WD) candidates in the Sloan Digital Sky Survey Data Release 7 area. We identify seven new binary systems with 1-18 hr orbital periods. Five of the systems will merge due to gravitational wave radiation within 10 Gyr, bringing the total number of merger systems found in the ELM Survey to 24. The ELM Survey has now quintupled the known merger WD population. It has also discovered the eight shortest period detached binary WD systems currently known. We discuss the characteristics of the merger and non-merger systems observed in the ELM Survey, including their future evolution. About half of the systems have extreme mass ratios. These are the progenitors of the AM Canum Venaticorum systems and Type Ia supernovae. The remaining targets will lead to the formation of extreme helium stars, subdwarfs, or massive WDs. We identify three targets that are excellent gravitational wave sources. These should be detected by the Laser Interferometer Space Antenna like missions within the first year of operation. The remaining targets are important indicators of what the Galactic foreground may look like for gravitational wave observatories.
C1 [Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Brown, Warren R.; Kenyon, S. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Heinke, Craig O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Agueeros, M. A.] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Kleinman, S. J.] Gemini Observ, Hilo, HI 96720 USA.
RP Kilic, M (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA.
EM kilic@ou.edu
RI Agueros, Marcel/K-7998-2014;
OI Agueros, Marcel/0000-0001-7077-3664; Kenyon, Scott/0000-0003-0214-609X;
Heinke, Craig/0000-0003-3944-6109
FU NSERC; Ingenuity New Faculty Award; Chandra [GO1-12019X]
FX We thank M. Alegria, J. McAfee, A. Milone, and J. DiMiceli for their
assistance with observations at the MMT Observatory. C.O.H. is supported
by NSERC and an Ingenuity New Faculty Award. M.A.A. gratefully
acknowledges Chandra grant GO1-12019X for support of portions of this
program.
NR 65
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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 1
PY 2012
VL 751
IS 2
AR 141
DI 10.1088/0004-637X/751/2/141
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600062
ER
PT J
AU Margutti, R
Soderberg, AM
Chomiuk, L
Chevalier, R
Hurley, K
Milisavljevic, D
Foley, RJ
Hughes, JP
Slane, P
Fransson, C
Moe, M
Barthelmy, S
Boynton, W
Briggs, M
Connaughton, V
Costa, E
Cummings, J
Del Monte, E
Enos, H
Fellows, C
Feroci, M
Fukazawa, Y
Gehrels, N
Goldsten, J
Golovin, D
Hanabata, Y
Harshman, K
Krimm, H
Litvak, ML
Makishima, K
Marisaldi, M
Mitrofanov, IG
Murakami, T
Ohno, M
Palmer, DM
Sanin, AB
Starr, R
Svinkin, D
Takahashi, T
Tashiro, M
Terada, Y
Yamaoka, K
AF Margutti, R.
Soderberg, A. M.
Chomiuk, L.
Chevalier, R.
Hurley, K.
Milisavljevic, D.
Foley, R. J.
Hughes, J. P.
Slane, P.
Fransson, C.
Moe, M.
Barthelmy, S.
Boynton, W.
Briggs, M.
Connaughton, V.
Costa, E.
Cummings, J.
Del Monte, E.
Enos, H.
Fellows, C.
Feroci, M.
Fukazawa, Y.
Gehrels, N.
Goldsten, J.
Golovin, D.
Hanabata, Y.
Harshman, K.
Krimm, H.
Litvak, M. L.
Makishima, K.
Marisaldi, M.
Mitrofanov, I. G.
Murakami, T.
Ohno, M.
Palmer, D. M.
Sanin, A. B.
Starr, R.
Svinkin, D.
Takahashi, T.
Tashiro, M.
Terada, Y.
Yamaoka, K.
TI INVERSE COMPTON X-RAY EMISSION FROM SUPERNOVAE WITH COMPACT PROGENITORS:
APPLICATION TO SN2011fe
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radiation mechanisms: non-thermal; supernovae: individual (SN2011fe)
ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; SYMBIOTIC-STAR PROGENITOR;
WHITE-DWARF MODELS; IA SUPERNOVAE; RADIO-EMISSION; LIGHT CURVES; SN
2011FE; CIRCUMSTELLAR MATERIAL; SODIUM-ABSORPTION; BURST AFTERGLOWS
AB We present a generalized analytic formalism for the inverse Compton X-ray emission from hydrogen-poor supernovae and apply this framework to SN 2011fe using Swift X-Ray Telescope (XRT), UVOT, and Chandra observations. We characterize the optical properties of SN 2011fe in the Swift bands and find them to be broadly consistent with a "normal" SN Ia, however, no X-ray source is detected by either XRT or Chandra. We constrain the progenitor system mass-loss rate (M) over dot < 2 x 10(-9) M-circle dot yr(-1) (3 sigma c.l.) for wind velocity v(w) = 100 km s(-1). Our result rules out symbiotic binary progenitors for SN 2011fe and argues against Roche lobe overflowing subgiants and main-sequence secondary stars if greater than or similar to 1% of the transferred mass is lost at the Lagrangian points. Regardless of the density profile, the X-ray non-detections are suggestive of a clean environment (n(CSM) < 150 cm(-3)) for 2 x 10(15) less than or similar to R less than or similar to 5 x 10(16) cm around the progenitor site. This is either consistent with the bulk of material being confined within the binary system or with a significant delay between mass loss and supernova explosion. We furthermore combine X-ray and radio limits from Chomiuk et al. to constrain the post-shock energy density in magnetic fields. Finally, we searched for the shock breakout pulse using gamma-ray observations from the Interplanetary Network and find no compelling evidence for a supernova-associated burst. Based on the compact radius of the progenitor star we estimate that the shock breakout pulse was likely not detectable by current satellites.
C1 [Margutti, R.; Soderberg, A. M.; Chomiuk, L.; Milisavljevic, D.; Foley, R. J.; Slane, P.; Moe, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chomiuk, L.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Chevalier, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Fransson, C.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Barthelmy, S.; Cummings, J.; Gehrels, N.; Krimm, H.; Starr, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Boynton, W.; Enos, H.; Fellows, C.; Harshman, K.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Briggs, M.; Connaughton, V.] Univ Alabama, Dept Phys, Huntsville, AL 35809 USA.
[Costa, E.; Del Monte, E.; Feroci, M.] INAF IASF Roma, I-00133 Rome, Italy.
[Fukazawa, Y.; Hanabata, Y.; Ohno, M.; Takahashi, T.] Hiroshima Univ, Dept Phys, Hiroshima 7398526, Japan.
[Goldsten, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Golovin, D.; Litvak, M. L.; Mitrofanov, I. G.; Murakami, T.; Sanin, A. B.] Moscow Space Res Inst, Moscow 117997, Russia.
[Makishima, K.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Marisaldi, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Palmer, D. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Svinkin, D.] Russian Acad Sci, AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
[Tashiro, M.; Terada, Y.] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan.
[Yamaoka, K.] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2298558, Japan.
RP Margutti, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Tashiro, Makoto/J-4562-2012; Terada, Yukikatsu/A-5879-2013; Svinkin,
Dmitry/C-1934-2014;
OI Terada, Yukikatsu/0000-0002-2359-1857; Feroci,
Marco/0000-0002-7617-3421; Costa, Enrico/0000-0003-4925-8523; Marisaldi,
Martino/0000-0002-4000-3789
FU Clay Fellowship; NASA [NNX10AR12G, NNX12AD68G, NNX07AR71G, NNX10AU34G,
NAS8-03060]; Russian Space Agency; RFBR [11-02-12082-ofi_m]
FX We thank Harvey Tananbaum and Neil Gehrels for making Chandra and Swift
observations possible. We thank Re'em Sari, Bob Kirshner, Sayan
Chakraborti, Stephan Immler, Brosk Russell, and Rodolfo Barniol Duran
for helpful discussions. L. C. is a Jansky Fellow of the National Radio
Astronomy Observatory. R.J.F. is supported by a Clay Fellowship. K.H. is
grateful for IPN support under the following NASA grants: NNX10AR12G
(Suzaku), NNX12AD68G (Swift), NNX07AR71G (MESSENGER), and NNX10AU34G
(Fermi). The Konus-Wind experiment is supported by a Russian Space
Agency contract and RFBR Grant 11-02-12082-ofi_m. P.O.S. acknowledges
partial support from NASA Contract NAS8-03060.
NR 79
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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 1
PY 2012
VL 751
IS 2
AR 134
DI 10.1088/0004-637X/751/2/134
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600055
ER
PT J
AU Perets, HB
Subr, L
AF Perets, Hagai B.
Subr, Ladislav
TI THE PROPERTIES OF DYNAMICALLY EJECTED RUNAWAY AND HYPER-RUNAWAY STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; stars: kinematics and dynamics; stars: peculiar;
stars: statistics
ID HYPERVELOCITY STARS; GALACTIC-CENTER; BLACK-HOLE; INITIAL BINARIES;
MASSIVE STARS; B-STARS; O STARS; ORIGIN; CLUSTERS; VELOCITY
AB Runaway stars are stars observed to have large peculiar velocities. Two mechanisms are thought to contribute to the ejection of runaway stars, both of which involve binarity (or higher multiplicity). In the binary supernova scenario, a runaway star receives its velocity when its binary massive companion explodes as a supernova (SN). In the alternative dynamical ejection scenario, runaway stars are formed through gravitational interactions between stars and binaries in dense, compact clusters or cluster cores. Here we study the ejection scenario. We make use of extensive N-body simulations of massive clusters, as well as analytic arguments, in order to characterize the expected ejection velocity distribution of runaway stars. We find that the ejection velocity distribution of the fastest runaways (upsilon greater than or similar to 80 km s(-1)) depends on the binary distribution in the cluster, consistent with our analytic toy model, whereas the distribution of lower velocity runaways appears independent of the binaries' properties. For a realistic log constant distribution of binary separations, we find the velocity distribution to follow a simple power law: Gamma(upsilon) alpha v(-8/3) for the high-velocity runaways and upsilon(-3/2) for the low-velocity ones. We calculate the total expected ejection rates of runaway stars from our simulated massive clusters and explore their mass function and their binarity. The mass function of runaway stars is biased toward high masses and strongly depends on their velocity. The binarity of runaways is a decreasing function of their ejection velocity, with no binaries expected to be ejected with upsilon > 150 km s(-1). We also find that hyper-runaways with velocities of hundreds of km s(-1) can be dynamically ejected from stellar clusters, but only at very low rates, which cannot account for a significant fraction of the observed population of hyper-velocity stars in the Galactic halo.
C1 [Perets, Hagai B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Subr, Ladislav] Charles Univ Prague, Fac Math & Phys, Astron Inst, CR-18000 Prague, Czech Republic.
RP Perets, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Perets, Hagai/K-9605-2015
OI Perets, Hagai/0000-0002-5004-199X
FU Czech Science Foundation [GACR-202/09/0772]; Czech Ministry of Education
[MSM0021620860]
FX H.B.P. is a CfA and BIKURA (FIRST) prize fellow. L.S. acknowledges the
support of the Czech Science Foundation via grant GACR-202/09/0772 and
from the Research Program MSM0021620860 of the Czech Ministry of
Education.
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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 1
PY 2012
VL 751
IS 2
AR 133
DI 10.1088/0004-637X/751/2/133
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600054
ER
PT J
AU Starikova, S
Berta, S
Franceschini, A
Marchetti, L
Rodighiero, G
Vaccari, M
Vikhlinin, A
AF Starikova, S.
Berta, S.
Franceschini, A.
Marchetti, L.
Rodighiero, G.
Vaccari, M.
Vikhlinin, A.
TI CLUSTERING OF STAR-FORMING GALAXIES DETECTED IN MID-INFRARED WITH THE
SPITZER WIDE-AREA SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; infrared: galaxies; large-scale structure of
universe
ID ACTIVE GALACTIC NUCLEI; SIMILAR-TO 2; ULTRALUMINOUS INFRARED GALAXIES;
DUST-OBSCURED GALAXIES; LYMAN-BREAK GALAXIES; OBSERVATIONS COSMOLOGICAL
INTERPRETATION; 2-POINT CORRELATION-FUNCTION; ANGULAR-CORRELATION
FUNCTION; HIGH-REDSHIFT GALAXIES; DARK-MATTER HALOES
AB We discuss the clustering properties of galaxies with signs of ongoing star formation detected by the Spitzer Space Telescope at the 24 mu m band in the SWIRE Lockman Hole field. The sample of mid-IR-selected galaxies includes similar to 20,000 objects detected above a flux threshold of S-24 mu m = 310 mu Jy. We adopt optical/near-IR color selection criteria to split the sample into the lower-redshift and higher-redshift galaxy populations. We measure the angular correlation function on scales of theta = 0 degrees.01-3 degrees.5, from which, using the Limber inversion along with the redshift distribution established for similarly selected source populations in the GOODS fields (Rodighiero et al.), we obtain comoving correlation lengths of r(0) = 4.98 +/- 0.28 h(-1) Mpc and r(0) = 8.04 +/- 0.69 h(-1) Mpc for the low-z (z(mean) = 0.7) and high-z (z(mean) = 1.7) subsamples, respectively. Comparing these measurements with the correlation functions of dark matter (DM) halos identified in the Bolshoi cosmological simulation, we find that the high-redshift objects reside in progressively more massive halos reaching M-tot greater than or similar to 3 x 10(12) h(-1) M-circle dot, compared to M-tot greater than or similar to 7 x 10(11) h(-1) M-circle dot for the low-redshift population. Approximate estimates of the IR luminosities based on the catalogs of 24 mu m sources in the GOODS fields show that our high-z subsample represents a population of "distant ULIRGs" with L-IR > 10(12) L-circle dot, while the low-z subsample mainly consists of "LIRGs," L-IR similar to 10(11) L-circle dot. The comparison of number density of the 24 mu m selected galaxies and of DM halos with derived minimum mass M-tot shows that only 20% of such halos may host star-forming galaxies.
C1 [Starikova, S.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Starikova, S.; Franceschini, A.; Marchetti, L.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Berta, S.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany.
[Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa.
[Vikhlinin, A.] Space Res Inst IKI, Moscow, Russia.
RP Starikova, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Vaccari, Mattia/R-3431-2016;
OI Vaccari, Mattia/0000-0002-6748-0577; Marchetti,
Lucia/0000-0003-3948-7621; Rodighiero, Giulia/0000-0002-9415-2296
FU Smithsonian Grand Challenges Consortia
FX We are grateful to A. Klypin for letting us use the outputs of the
Bolshoi cosmological simulations. We thank C. Jones for careful reading
of the manuscript and useful comments. S. S. was supported by the
Smithsonian Grand Challenges Consortia.
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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 JUN 1
PY 2012
VL 751
IS 2
AR 126
DI 10.1088/0004-637X/751/2/126
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600047
ER
PT J
AU Tang, SM
Grindlay, JE
Moe, M
Orosz, JA
Kurucz, RL
Quinn, SN
Servillat, M
AF Tang, Sumin
Grindlay, Jonathan E.
Moe, Maxwell
Orosz, Jerome A.
Kurucz, Robert L.
Quinn, Samuel N.
Servillat, Mathieu
TI DASCH DISCOVERY OF A POSSIBLE NOVA-LIKE OUTBURST IN A PECULIAR SYMBIOTIC
BINARY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: symbiotic; novae, cataclysmic variables
ID ACCRETING WHITE-DWARFS; LIGHT-CURVE; X-RAY; STARS; EVOLUTION; CATALOG;
SPECTROGRAPH; PROGENITORS; COMPONENTS; TELESCOPE
AB We present photometric and spectroscopic observations of a peculiar variable (designated DASCH J075731.1+201735 or J0757) discovered from our DASCH project using the digitized Harvard College Observatory archival photographic plates. It brightened by about 1.5 mag in B within a year starting in 1942, and then slowly faded back to its pre-outburst brightness from 1943 to 1950s. The mean brightness level was stable before and after the outburst, and ellipsoidal variations with a period of P = 119.18 +/- 0.07 days are seen, suggesting that the star is tidally distorted. Radial-velocity measurements indicate that the orbit is nearly circular (e = 0.02 +/- 0.01) with a spectroscopic period that is the same as the photometric period. The binary consists of a 1.1 +/- 0.3 M-circle dot M0III star, and a 0.6 +/- 0.2 M-circle dot companion, very likely a white dwarf (WD). Unlike other symbiotic binaries, there is no sign of emission lines or a stellar wind in the spectra. With an outburst timescale of similar to 10 years and estimated B-band peak luminosity M-B similar to 0.7, J0757 is different from any other known classic or symbiotic novae. The most probable explanation of the outburst is hydrogen shell burning on the WD, although an accretion-powered flare cannot be ruled out.
C1 [Tang, Sumin; Grindlay, Jonathan E.; Moe, Maxwell; Kurucz, Robert L.; Quinn, Samuel N.; Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP Tang, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM stang@cfa.harvard.edu
FU Smithsonian Astrophysical Observatory; NSF [AST0407380, AST0909073];
Cornel and Cynthia K. Sarosdy Fund for DASCH
FX We thank the anonymous referee for helpful comments. We are grateful to
Alison Doane, Jaime Pepper, Edward Los, Robert J. Simcoe and David
Sliski at CfA for their work on DASCH, and many volunteers who have
helped digitize logbooks, clean, and scan plates
(http://hea-www.harvard.edu/DASCH/team.php); and David Latham for his
generous help on getting TRES spectra and data reduction. We thank
Sumner Starrfield, Joanna Mikolajewska, Scott Kenyon, Mariko Kato, Lars
Bildsten, Tony Piro, Sterl Phinney, Ken Shen, Maureen van den Berg,
Rosanne Di Stefano, Jing Luan, and Perry Berlind for helpful
discussions. S. T. thanks the FLWO staff and many visiting astronomers
who acquired the TRES and FAST spectra; Andrea Dupree and Anna Frebel
for the help on obtaining and reducing the MIKE spectra; Jessica Mink
and Bill Wyatt for the initial reduction of the TRES and FAST spectra.
This paper uses data products produced by the OIR Telescope Data Center,
supported by the Smithsonian Astrophysical Observatory. This research
has made use of the GSC 2.3.2, 2MASS, SDSS, and GALEX catalogs, HEASARC,
NASA/IPAC Infrared Science Archive, and the ASAS database. This work was
supported in part by the NSF grants AST0407380 and AST0909073 and now
also the Cornel and Cynthia K. Sarosdy Fund for DASCH.
NR 55
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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 JUN 1
PY 2012
VL 751
IS 2
AR 99
DI 10.1088/0004-637X/751/2/99
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600020
ER
PT J
AU van Kempen, TA
Longmore, SN
Johnstone, D
Pillai, T
Fuente, A
AF van Kempen, T. A.
Longmore, S. N.
Johnstone, D.
Pillai, T.
Fuente, A.
TI THE SMALL-SCALE PHYSICAL STRUCTURE AND FRAGMENTATION DIFFERENCE OF TWO
EMBEDDED INTERMEDIATE-MASS PROTOSTARS IN ORION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: kinematics and dynamics; stars: formation; submillimeter: ISM;
techniques: interferometric
ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; SUBMILLIMETER CONTINUUM
OBSERVATIONS; SPECTRAL ENERGY-DISTRIBUTIONS; HERSCHEL-PACS SPECTROSCOPY;
MOLECULAR CLOUD CORES; INFRARED-DARK CLOUDS; HOT CORE; PROTOSTELLAR
CORES; RADIATION FEEDBACK
AB Intermediate-mass (IM) protostars, the bridge between the very common solar-like protostars and the more massive, but rarer, O and B stars, can only be studied at high physical spatial resolutions in a handful of clouds. In this paper, we present and analyze the continuum results from an observing campaign at the Submillimeter Array (SMA) targeting two well-studied IM protostars in Orion, NGC 2071 and L1641 S3 MMS 1. The extended SMA (eSMA) probes structure at angular resolutions up to 0.'' 2, revealing protostellar disks on scales of similar to 200 AU. Continuum flux measurements on these scales indicate that a significant amount of mass, a few tens of M-circle dot, is present. Envelope, stellar, and disk masses are derived using compact, extended, and eSMA configurations and compared against spectral energy distribution fitting models. We hypothesize that fragmentation into three components occurred within NGC 2071 at an early time, when the envelopes were less than 10% of their current masses, e.g., <0.5 M-circle dot. No fragmentation occurred for L1641 S3 MMS 1. For NGC 2071, evidence is given that the bulk of the envelope material currently around each source was accreted after the initial fragmentation. In addition, about 30% of the total core mass is not yet associated to one of the three sources. A global accretion model is favored and a potential accretion history of NGC 2071 is presented. It is shown that the relatively low level of fragmentation in NGC 2071 was stifled compared to the expected fragmentation from a Jeans argument. Similarly, the lack of fragmentation in L1641 S3 MMS 1 is likely due to similar arguments.
C1 [van Kempen, T. A.] Joint ALMA Off, Santiago, Chile.
[van Kempen, T. A.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[van Kempen, T. A.; Longmore, S. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Longmore, S. N.] European So Observ, D-85748 Garching, Germany.
[Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astron, Victoria, BC, Canada.
[Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada.
[Pillai, T.] CALTECH, Pasadena, CA 91125 USA.
[Fuente, A.] OAN, E-28803 Madrid, Spain.
RP van Kempen, TA (reprint author), Joint ALMA Off, Alonso de Cordova 3107, Santiago, Chile.
EM tkempen@alma.cl
RI Fuente, Asuncion/G-1468-2016
OI Fuente, Asuncion/0000-0001-6317-6343
FU Smithsonian Institution; Academia Sinica; SMA; Submillimeter Array; NOVA
(Nederlandse Onderzoeksschool Voor Astronomie); NSERC; Combined Array
for Research in Millimeter-wave Astronomy (CARMA); National Science
Foundation [AST 05-40399]
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.; T.v.K. and S.L. were supported as SMA postdoctoral
fellows at the Harvard-Smithsonian Center for Astrophysics (CfA) and are
grateful to the Submillimeter Array for funding their research. T.v.K.'s
current research is supported by NOVA (Nederlandse Onderzoeksschool Voor
Astronomie). T.v.K. is also grateful for the facilities at the Joint
ALMA Observatories during his association. D.J. acknowledges the support
from an NSERC Discovery Grant. T.P. acknowledges support from the
Combined Array for Research in Millimeter-wave Astronomy (CARMA), which
is supported by the National Science Foundation through grant AST
05-40399. The anonymous referee is thanked for the critical useful
positive read-through of the paper. Mark Gurwell, Ken Young (Taco), and
David Wilner of the CfA are thanked for track-sharing eSMA observations
on short notice. Taco and Remo Tilanus are thanked for their efforts on
the eSMA and assistance with data reduction. We are grateful to the
other members in the WISH intermediate mass team (Lars Kristensen, Mike
Fich, and Carolyn McCoey in particular) for supplying necessary
information on the sources and general discussions. Last but not least,
we express our appreciation for the help of Tom Megeath by sharing the
reduced Spitzer photometry and images on Orion before publication.
NR 92
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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 137
DI 10.1088/0004-637X/751/2/137
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600058
ER
PT J
AU Watson, LC
Martini, P
Lisenfeld, U
Wong, MH
Boker, T
Schinnerer, E
AF Watson, Linda C.
Martini, Paul
Lisenfeld, Ute
Wong, Man-Hong
Boker, Torsten
Schinnerer, Eva
TI PROPERTIES OF BULGELESS DISK GALAXIES. II. STAR FORMATION AS A FUNCTION
OF CIRCULAR VELOCITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: ISM; galaxies: spiral; galaxies: star formation; radio lines:
galaxies
ID MASS-METALLICITY RELATION; STELLAR POPULATION SYNTHESIS;
SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; ON SPIRAL GALAXIES;
FORMATION LAW; FORMING GALAXIES; NEARBY GALAXIES; H-ALPHA; MOLECULAR GAS
AB We study the relation between the surface density of gas and star formation rate in 20 moderately inclined, bulgeless disk galaxies (Sd-Sdm Hubble types) using CO(1-0) data from the IRAM 30 m telescope, Hi emission line data from the VLA/EVLA, H alpha data from the MDM Observatory, and polycyclic aromatic hydrocarbon emission data derived from Spitzer IRAC observations. We specifically investigate the efficiency of star formation as a function of circular velocity (v(circ)). Previous work found that the vertical dust structure and disk stability of edge-on, bulgeless disk galaxies transition from diffuse dust lanes with large scale heights and gravitationally stable disks at v(circ) < 120 km s(-1) (M-* less than or similar to 10(10) M-circle dot) to narrow dust lanes with small scale heights and gravitationally unstable disks at v(circ) > 120 km s(-1). We find no transition in star formation efficiency (Sigma(SFR)/Sigma(H) (I+H2)) at v(circ) = 120 km s(-1) or at any other circular velocity probed by our sample (v(circ) = 46-190 km s(-1)). Contrary to previous work, we find no transition in disk stability at any circular velocity in our sample. Assuming our sample has the same dust structure transition as the edge-on sample, our results demonstrate that scale height differences in the cold interstellar medium of bulgeless disk galaxies do not significantly affect the molecular fraction or star formation efficiency. This may indicate that star formation is primarily affected by physical processes that act on smaller scales than the dust scale height, which lends support to local star formation models.
C1 [Watson, Linda C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Watson, Linda C.; Martini, Paul; Wong, Man-Hong] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Martini, Paul] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Lisenfeld, Ute] Univ Granada, Dept Fis Teor & Cosmos, E-18071 Granada, Spain.
[Wong, Man-Hong] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Boker, Torsten] European Space Agcy, NL-2200 AG Noordwijk, Netherlands.
[Schinnerer, Eva] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Watson, LC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM lwatson@cfa.harvard.edu
RI Lisenfeld, Ute/A-1637-2015;
OI Lisenfeld, Ute/0000-0002-9471-5423; Schinnerer, Eva/0000-0002-3933-7677
FU NSF [AST-0705170]; Ohio State University; Spanish Ministerio de Ciencia
y Educacion [AYA2007-67625-C02-02, AYA2011-24728]; Junta de Andalucia;
NASA through JPL/Caltech; National Aeronautics and Space Administration
FX We thank Frank Bigiel for providing us with his data. We are also
grateful to Todd A. Thompson for helpful comments and discussion,
Richard W. Pogge for supplying the narrowband filters used in the Ha
observations, Roberto J. Assef, David W. Atlee, and Katharine J.
Schlesinger for obtaining some of the H alpha observations, and the
referee for comments that improved this work. L. C. W. gratefully
acknowledges support from an NSF Graduate Research Fellowship and an
Ohio State University Distinguished University Fellowship. P. M. is
grateful for support from the NSF via award AST-0705170. U. L.
acknowledges financial support from the research projects
AYA2007-67625-C02-02 and AYA2011-24728 from the Spanish Ministerio de
Ciencia y Educacion and from the Junta de Andalucia. 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
publication makes use of data products from the Two Micron All Sky
Survey, which is a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center/California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation.
NR 91
TC 5
Z9 5
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 1
PY 2012
VL 751
IS 2
AR 123
DI 10.1088/0004-637X/751/2/123
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944LU
UT WOS:000304204600044
ER
PT J
AU Miller, JS
Porter-Morgan, HA
Stevens, H
Boom, B
Krupnick, GA
Acevedo-Rodriguez, P
Fleming, J
Gensler, M
AF Miller, James S.
Porter-Morgan, Holly A.
Stevens, Hannah
Boom, Brian
Krupnick, Gary A.
Acevedo-Rodriguez, Pedro
Fleming, James
Gensler, Micah
TI Addressing target two of the Global Strategy for Plant Conservation by
rapidly identifying plants at risk
SO BIODIVERSITY AND CONSERVATION
LA English
DT Article
DE Global Strategy for Plant Conservation; Endangered species; Extinction
ID IUCN RED LIST; HERBARIUM SPECIMENS; SEED PLANTS; ASSESSMENTS; DIVERSITY;
CRITERIA; THREAT; FLORA
AB Target two of the 2002 Global Strategy for Plant Conservation (GSPC), "A preliminary assessment of the conservation status of all known plant species, at national, regional, and international levels" was not accomplished by its original 2010 target date and has therefore been included as a revised 2020 target, "An assessment of the conservation status of all known plant species, as far as possible, to guide conservation action." The most widely used system to estimate risk of extinction, the International Union for the Conservation of Nature Red List, provides conservation assessments for fewer than 15,000 plant species. Progress achieving Target two has been hampered by the large number of plant species and the difficulty assembling the data needed for Red List assessments. Two streamlined methods for identifying those plant species considered At Risk under the GSPC Target two are compared and contrasted. Both methods use readily available locality data from herbarium specimens to efficiently identify At Risk species and approximate the list of species that would be identified as threatened by Red List analyses. A comprehensive analysis of the native plant species of Puerto Rico using both streamlined methods identifies 570 of the 2,025 species at some risk of extinction. More efficient systems for assessing threat allow a more timely response to Target two, allow conservation efforts to be directed to the species that need attention, and the list of threatened plants can be used to identify priority areas for plant conservation.
C1 [Miller, James S.; Porter-Morgan, Holly A.; Stevens, Hannah; Boom, Brian; Fleming, James; Gensler, Micah] New York Bot Garden, Bronx, NY 10458 USA.
[Porter-Morgan, Holly A.] LaGuardia Community Coll, Long Isl City, NY 11101 USA.
[Krupnick, Gary A.; Acevedo-Rodriguez, Pedro] Smithsonian Inst, NMNH, Washington, DC 20013 USA.
RP Miller, JS (reprint author), New York Bot Garden, 200th St & Kazimiroff Blvd, Bronx, NY 10458 USA.
EM jmiller@nybg.org
OI Krupnick, Gary/0000-0002-1357-4826
NR 45
TC 6
Z9 6
U1 0
U2 25
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0960-3115
EI 1572-9710
J9 BIODIVERS CONSERV
JI Biodivers. Conserv.
PD JUN
PY 2012
VL 21
IS 7
BP 1877
EP 1887
DI 10.1007/s10531-012-0285-3
PG 11
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 944AY
UT WOS:000304171900013
ER
PT J
AU Ruger, N
Condit, R
AF Rueger, Nadja
Condit, Richard
TI Testing metabolic theory with models of tree growth that include light
competition
SO FUNCTIONAL ECOLOGY
LA English
DT Article
DE allometric scaling; Barro Colorado Island; hierarchical Bayesian model;
light competition; metabolic scaling theory; Panama; tropical rainforest
ID GENERAL QUANTITATIVE THEORY; SCALING THEORY; TROPICAL FORESTS; ADULT
STATURE; ALLOMETRY; ECOLOGY; SIZE; MORTALITY; DYNAMICS; PANAMA
AB 1. Metabolic scaling theory predicts that diameter growth rates of tree species are related to tree diameter by a universal scaling law. This model has been criticised because it ignores the influence of competition for resources such as light on the scaling of demographic rates with size. 2. We here test whether scaling exponents of abundant tropical tree species comply with the prediction of metabolic scaling theory and evaluate whether the scaling of growth with size depends on light availability. Light reaching each individual tree was estimated from yearly vertical censuses of canopy density, and a hierarchical Bayesian approach allowed quantifying confidence intervals for scaling exponents and accounting for different sources of error. 3. We found no universal scaling relationship, and 5070% of the species had scaling exponents that significantly differed from the predicted value of 1/3. As would be expected if competition for light were important, scaling exponents were >1/3 for the majority of species when all trees were combined. However, the community average of scaling exponents was not significantly different from the predicted value of 1/3 when only considering individuals that grew under high-light conditions. 4. These results support the hypothesis that the prediction of metabolic ecology for the scaling of tree growth with size is only valid when competition for light is unimportant.
C1 [Rueger, Nadja] Univ Leipzig, AG Spezielle Bot & Funkt Biodiversitat, D-04103 Leipzig, Germany.
[Condit, Richard] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa Ancon, Panama.
RP Ruger, N (reprint author), Univ Leipzig, AG Spezielle Bot & Funkt Biodiversitat, Johannisallee 21-23, D-04103 Leipzig, Germany.
EM nadja.rueger@uni-leipzig.de
RI Ruger, Nadja/J-6393-2015
OI Ruger, Nadja/0000-0003-2371-4172
FU John Wesley Powell Center for Analysis and Synthesis; U.S. Geological
Survey; Deutsche Forschungsgemeinschaft DFG [RU 1536/2-1]; Center for
Tropical Forest Science (CTFS); U.S. National Science Foundation
[0948585]; John D. and Catherine D. McArthur Foundation; Smithsonian
Tropical Research Institute
FX This work was conducted as part of the Tree Mass Growth Working Group
supported by the John Wesley Powell Center for Analysis and Synthesis,
funded by the U.S. Geological Survey, and we thank working group members
for discussions that spawned this paper. We thank Jens Doleschal and the
Center for Information Services and High Performance Computing,
Technische Universitat Dresden, for the parallelisation of the R code
and provision of computing resources. N.R. was funded by research grants
from Deutsche Forschungsgemeinschaft DFG (RU 1536/2-1) and the Center
for Tropical Forest Science (CTFS). We would like to thank Stephanie
Bohlman, Helene Muller-Landau, Scott Stark and two anonymous reviewers
for constructive criticism on the manuscript. The BCI plot has been made
possible through the support of the U.S. National Science Foundation
(most recently, grant no. 0948585 to S. P. Hubbell), the John D. and
Catherine D. McArthur Foundation, and the Smithsonian Tropical Research
Institute. We thank the dozens of field assistants and botanists who
have collected data on trees and carried out the canopy censuses in the
BCI plot over the past 30 years.
NR 51
TC 17
Z9 19
U1 3
U2 40
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0269-8463
J9 FUNCT ECOL
JI Funct. Ecol.
PD JUN
PY 2012
VL 26
IS 3
BP 759
EP 765
DI 10.1111/j.1365-2435.2012.01981.x
PG 7
WC Ecology
SC Environmental Sciences & Ecology
GA 945EV
UT WOS:000304256500023
ER
PT J
AU Husnoo, N
Pont, F
Mazeh, T
Fabrycky, D
Hebrard, G
Bouchy, F
Shporer, A
AF Husnoo, Nawal
Pont, Frederic
Mazeh, Tsevi
Fabrycky, Daniel
Hebrard, Guillaume
Bouchy, Francois
Shporer, Avi
TI Observational constraints on tidal effects using orbital eccentricities
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE planetary systems
ID TRANSITING HOT JUPITER; HIGH-PRECISION PHOTOMETRY; CLOSE BINARY-SYSTEMS;
NEPTUNE-MASS PLANET; SOLAR-TYPE STAR; M-DWARF GJ-436; LIGHT-CURVE; GIANT
PLANET; SPIN-ORBIT; SOUTHERN-HEMISPHERE
AB We have analysed radial velocity measurements for known transiting exoplanets to study the empirical signature of tidal orbital evolution for close-in planets. Compared to standard eccentricity determination, our approach is modified to focus on the rejection of the null hypothesis of a circular orbit. We are using a Markov Chain Monte Carlo analysis of radial velocity measurements and photometric constraints, including a component of correlated noise, as well as Bayesian model selection to check if the data justify the additional complexity of an eccentric orbit. We find that among planets with non-zero eccentricity values quoted in the literature, there is no evidence for an eccentricity detection for the seven planets CoRoT-5b, WASP-5b, WASP-6b, WASP-10b, WASP-12b, WASP-17b and WASP-18b. In contrast, we confirm the eccentricity of HAT-P-16b, e= 0.034 +/- 0.003, the smallest eccentricity that is reliably measured so far for an exoplanet as well as that of WASP-14b, which is the planet at the shortest period (P= 2.24 d), with a confirmed eccentricity, e= 0.088 +/- 0.003. As part of the study, we present new radial velocity data using the HARPS spectrograph for CoRoT-1, CoRoT-3, WASP-2, WASP-4, WASP-5 and WASP-7 as well as the SOPHIE spectrograph for HAT-P-4, HAT-P-7, TrES-2 and XO-2. We show that the dissipative effect of tides raised in the planet by the star and vice versa explain all the eccentricity and spinorbit alignment measurements available for transiting planets. We revisit the massperiod relation and consider its relation to the stopping mechanism of orbital migration for hot Jupiters. In addition to CoRoT-2 and HD 189733, we find evidence for excess rotation of the star in the systems CoRoT-18, HAT-P-20, WASP-19 and WASP-43.
C1 [Husnoo, Nawal; Pont, Frederic] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Mazeh, Tsevi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Fabrycky, Daniel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hebrard, Guillaume; Bouchy, Francois] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France.
[Hebrard, Guillaume; Bouchy, Francois] Observ Haute Provence, CNRS OAMP, F-04870 St Michel lObservatoire, France.
[Shporer, Avi] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA.
RP Husnoo, N (reprint author), Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
EM nawal@astro.ex.ac.uk
OI Fabrycky, Daniel/0000-0003-3750-0183
FU STFC; Halliday fellowship [ST/F011083/1]
FX We are grateful to the anonymous referee for the encouraging remarks and
the enormous amount of detailed feedback and sound advice, which helped
us to make this paper better. We thank the editor for his encouraging
comments. FP is grateful for the STFC grant and Halliday fellowship
ST/F011083/1. We also thank the SOPHIE Exoplanet Consortium for
arranging a flexible observation schedule for our programme, and the
whole OHP/SOPHIE team for support. NH thanks Gilles Chabrier for his
clear explanations of the equilibrium tides model.
NR 84
TC 32
Z9 32
U1 0
U2 5
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 422
IS 4
BP 3151
EP 3177
DI 10.1111/j.1365-2966.2012.20839.x
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 945AV
UT WOS:000304246100030
ER
PT J
AU Sanchez-Gallego, JR
Knapen, JH
Wilson, CD
Barmby, P
Azimlu, M
Courteau, S
AF Sanchez-Gallego, J. R.
Knapen, J. H.
Wilson, C. D.
Barmby, P.
Azimlu, M.
Courteau, S.
TI The JCMT Nearby Galaxies Legacy Survey - VII. H imaging and massive star
formation properties
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE surveys; stars: massive; H ii regions; galaxies: star formation;
galaxies: ISM
ID ALPHA SURFACE PHOTOMETRY; HUBBLE-SPACE-TELESCOPE; FORMATION RATE
INDICATORS; NEUTRAL GAS GALAXIES; SPIRAL GALAXIES; VIRGO CLUSTER; LOCAL
VOLUME; FORMATION RATES; STANDARD STARS; DISK GALAXIES
AB We present Ha fluxes, star formation rates (SFRs) and equivalent widths (EWs) for a sample of 156 nearby galaxies observed in the 12CO J= 32 line as part of the James Clerk Maxwell Telescope Nearby Galaxies Legacy Survey. These are derived from images and values in the literature and from new Ha images for 72 galaxies which we publish here. We describe the sample, observations and procedures to extract the Ha fluxes and related quantities. We discuss the SFR properties of our sample and confirm the well-known correlation with galaxy luminosity, albeit with high dispersion. Our SFRs range from 0.1 to 11 M? yr-1 with a median SFR value for the complete sample of 0.2 M? yr-1. This median value is somewhat lower than similar published measurements, which we attribute, in part, to our sample being H i selected and, thus, not biased towards high SFRs as has frequently been the case in previous studies. Additionally, we calculate internal absorptions for the Ha line, A(Ha), which are lower than many of those used in previous studies. Our derived EWs, which range from 1 to 880 angstrom with a median value of 27 angstrom, show little dependence on luminosity but rise by a factor of 5 from early- to late-type galaxies. This paper is the first in a series aimed at comparing SFRs obtained from Ha imaging of galaxies with information derived from other tracers of star formation and atomic and molecular gas.
C1 [Sanchez-Gallego, J. R.; Knapen, J. H.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Sanchez-Gallego, J. R.; Knapen, J. H.] Univ La Laguna, Dept Astrofis, E-38200 Tenerife, Spain.
[Wilson, C. D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
[Barmby, P.; Azimlu, M.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Azimlu, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Courteau, S.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada.
RP Sanchez-Gallego, JR (reprint author), Inst Astrofis Canarias, E-38205 Tenerife, Spain.
EM jrsg@iac.es
RI Barmby, Pauline/I-7194-2016
OI Barmby, Pauline/0000-0003-2767-0090
NR 82
TC 18
Z9 18
U1 1
U2 2
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 422
IS 4
BP 3208
EP 3248
DI 10.1111/j.1365-2966.2012.20845.x
PG 41
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 945AV
UT WOS:000304246100033
ER
PT J
AU Nesvorny, D
Kipping, DM
Buchhave, LA
Bakos, GA
Hartman, J
Schmitt, AR
AF Nesvorny, David
Kipping, David M.
Buchhave, Lars A.
Bakos, Gaspar A.
Hartman, Joel
Schmitt, Allan R.
TI The Detection and Characterization of a Nontransiting Planet by Transit
Timing Variations
SO SCIENCE
LA English
DT Article
ID EXTRASOLAR PLANETS; MASS; SYSTEM; EFFICIENT; EXOMOON
AB The Kepler mission is monitoring the brightness of similar to 150,000 stars, searching for evidence of planetary transits. As part of the Hunt for Exomoons with Kepler (HEK) project, we report a planetary system with two confirmed planets and one candidate planet discovered with the publicly available data for KOI-872. Planet b transits the host star with a period P-b = 33.6 days and exhibits large transit timing variations indicative of a perturber. Dynamical modeling uniquely detects an outer nontransiting planet c near the 5: 3 resonance (P-c = 57.0 days) with a mass 0.37 times that of Jupiter. Transits of a third planetary candidate are also found: a 1.7-Earth radius super-Earth with a 6.8-day period. Our analysis indicates a system with nearly coplanar and circular orbits, reminiscent of the orderly arrangement within the solar system.
C1 [Nesvorny, David] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
[Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Bakos, Gaspar A.; Hartman, Joel] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Nesvorny, D (reprint author), SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
EM davidn@boulder.swri.edu
OI Buchhave, Lars A./0000-0003-1605-5666
FU NSF [AST-1008890, AST-1108686]; NASA [NNX09AB29G]
FX This work is part of the Hunt for Exomoons with Kepler (HEK) project. We
thank the Kepler Science Team, especially the Data Analysis Working
Group, for making the data used here available. D.N. acknowledges
support from NSF AST-1008890. D. M. K. is supported by the NASA Sagan
fellowship. G. A. B. acknowledges support from NASA grant NNX09AB29G.
J.H. acknowledges support from NSF AST-1108686.
NR 23
TC 66
Z9 66
U1 1
U2 5
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 1
PY 2012
VL 336
IS 6085
BP 1133
EP 1136
DI 10.1126/science.1221141
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 950KK
UT WOS:000304647900042
PM 22582018
ER
PT J
AU Carleton, MD
Stanley, WT
AF Carleton, Michael D.
Stanley, William T.
TI Species limits within the Praomys delectorum group (Rodentia: Muridae:
Murinae) of East Africa: a morphometric reassessment and biogeographical
implications
SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Review
DE Eastern Arc Mountains; Makambako Gap; Praomys melanotus; Praomys taitae;
taxonomy
ID SMALL MAMMAL INVENTORIES; WEST USAMBARA MOUNTAINS; COMPLEX RODENTIA; ARC
MOUNTAINS; MORPHOLOGICAL EVOLUTION; UDZUNGWA MOUNTAINS; MUROID RODENTS;
MONTANE AREAS; NATIONAL-PARK; TANZANIA
AB We examined approximately 600 specimens that represent the Praomys delectorum species group (Muridae: Murinae: Praomyini), a rodent complex restricted to Afromontane landscapes in East Africa and currently viewed as a single species. Morphometric analyses of 21 population samples consistently disclosed cohesive patterns of craniodental differentiation that support the recognition of three species: Praomys delectorum Thomas, confined to extreme southern Malawi; P. melanotus Allen & Loveridge, found in highlands of south-western Tanzania and contiguous northern Malawi; and P. taitae Heller (including octomastis Hatt), distributed in mountains and foothills of southern Kenya and northern and central Tanzania. Populations of the P. delectorum group are patchily distributed in moist montane forest, most collecting localities falling within 10002400 m, and their range collectively coincides with the TanganyikaNyasa Montane Forest Group sensu Moreau. Patterns of faunal similarity derived from distributions of 65 species of terrestrial small mammals recorded from Tanzania's highlands, including the Eastern Arc Mountains, demonstrated pronounced geographical discontinuities in montane associations but failed to uncover a prominent vicariant role for the Makambako Gap. (c) 2012 The Linnean Society of London, Zoological Journal of the Linnean Society, 2012, 165, 420469.
C1 [Carleton, Michael D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Stanley, William T.] Field Museum Nat Hist, Dept Zool, Div Mammals, Chicago, IL 60605 USA.
RP Carleton, MD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
EM carletonm@si.edu
FU National Geographic Society [5053-93, 5244-94, 5711-96]; Critical
Ecosystem Partnership Fund; Field Museum of Natural History (Field
Museum/IDP Foundation, Inc.); Barbara Brown; Council on Africa; Ellen
Thorne Smith; Marshall Field Funds
FX For specimen loans and/or access to collections, we thank Robert S. Voss
and Eileen Westwig (AMNH); Paula D. Jenkins and Richard Sabin (BMNH);
Suzanne McLaren (CM); John D. Phelps III (FMNH); and Judy Chupasko and
Mark Omura (MCZ). Rebecca Banasiak (FMNH) rendered the map and
photographs of study skins (Figs 1, 8), and Dave Schmidt (USNM)
photographed specimens (Figs 6, 7); we appreciate their careful
attention to detail in helping to communicate our scientific results.
Two anonymous reviewers devoted careful scrutiny to the manuscript and
improved the clarity of our communication. Permits issued to W.T.S. to
conduct research in Tanzania were granted by the Tanzania Commission for
Science and Technology, the Tanzania Wildlife Research Institute, and
the Ministry of Natural Resources and Tourism. Support for fieldwork by
W.T.S. was provided by the National Geographic Society (Grants 5053-93,
5244-94, 5711-96), the Critical Ecosystem Partnership Fund, and the
Field Museum of Natural History (Field Museum/IDP Foundation, Inc.
African Training Fund, as well as the Barbara Brown, Council on Africa,
Ellen Thorne Smith, and Marshall Field Funds). At various times, Steven
M. Goodman, Kim M. Howell, Philip M. Kihaule, Sophy J. Machaga, and
Maiko M. Munissi helped W.T.S. to collect specimens, and Tim Davenport
supplied logistical support within Tanzania.
NR 124
TC 12
Z9 12
U1 0
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-4082
EI 1096-3642
J9 ZOOL J LINN SOC-LOND
JI Zool. J. Linn. Soc.
PD JUN
PY 2012
VL 165
IS 2
BP 420
EP 469
DI 10.1111/j.1096-3642.2012.00817.x
PG 50
WC Zoology
SC Zoology
GA 946XZ
UT WOS:000304392200008
ER
PT J
AU Nweeia, MT
Eichmiller, FC
Hauschka, PV
Tyler, E
Mead, JG
Potter, CW
Angnatsiak, DP
Richard, PR
Orr, JR
Black, SR
AF Nweeia, Martin T.
Eichmiller, Frederick C.
Hauschka, Peter V.
Tyler, Ethan
Mead, James G.
Potter, Charles W.
Angnatsiak, David P.
Richard, Pierre R.
Orr, Jack R.
Black, Sandie R.
TI Vestigial Tooth Anatomy and Tusk Nomenclature for Monodon Monoceros
SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY
BIOLOGY
LA English
DT Article
DE Monodon monoceros; narwhal; vestigial teeth; osteoanatomy; nomenclature
ID ELEPHANT LOXODONTA-AFRICANA; MAMMALIA; PROBOSCIDEA; NARWHAL; EVOLUTION;
PATTERN; EOCENE; DENTIN; IVORY; INDIA
AB Narwhal tusks, although well described and characterized within publications, are clouded by contradictory references, which refer to them as both incisors and canines. Vestigial teeth are briefly mentioned in the scientific literature with limited descriptions and no image renderings. This study first examines narwhal maxillary osteoanatomy to determine whether the erupted tusks are best described as incisiform or caniniform teeth. The study also offers evidence to support the evolutionary obsolescence of the vestigial teeth through anatomic, morphologic, and histologic descriptions. Examination of 131 skull samples, including 110 museum skull specimens and 21 harvested skulls, revealed the erupted tusks surrounded by maxillary bone over the entire length of their bone socket insertion, and are thus more accurately termed caniniform or canine teeth. The anatomy, morphology, and development of vestigial teeth in five skull samples are more fully described and documented. Vestigial tooth samples included 14 embedded pairs or individual teeth that were partially exposed or removed from the maxillary bone. Their location was posterior, ventral, and lateral to the tusks, although male vestigial teeth often exfoliate in the mouth lodging between the palatal tissue and underlying maxillary bone. Their myriad morphologies, sizes, and eruption patterns suggest that these teeth are no longer guided by function but rather by random germ cell differentiation and may eventually cease expression entirely. The conclusions reached are that the narwhal tusks are the expression of canine teeth and that vestigial teeth have no apparent functional characteristics and are following a pattern consistent with evolutionary obsolescence. Anat Rec, 2012. (c) 2012 Wiley Periodicals, Inc.
C1 [Nweeia, Martin T.] Harvard Univ, Sch Dent Med, Dept Restorat Dent & Biomat Sci, Boston, MA 02115 USA.
[Nweeia, Martin T.] Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Nweeia, Martin T.; Potter, Charles W.] Harvard Museum Comparat Zool, Dept Mammals, Boston, MA USA.
[Eichmiller, Frederick C.] Delta Dent Wisconsin, Stevens Point, WI USA.
[Hauschka, Peter V.] Childrens Hosp Boston, Dept Orthopaed Surg, Boston, MA USA.
[Tyler, Ethan] NIH, Med Arts Design Sect, Washington, DC USA.
[Angnatsiak, David P.] Inuit Hunter, Pond Inlet, NU, Canada.
[Richard, Pierre R.; Orr, Jack R.] Fisheries & Oceans Canada, Arctic Res Div, Winnipeg, MB, Canada.
[Black, Sandie R.] Calgary Zoo Anim Hlth Ctr, Vet Serv, Calgary, AB, Canada.
RP Nweeia, MT (reprint author), Harvard Univ, Sch Dent Med, Dept Restorat Dent & Biomat Sci, 188 Longwood Ave, Boston, MA 02115 USA.
EM martin_nweeia@hsdm.harvard.edu
FU National Science Foundation; Harvard School of Medicine; Harvard School
of Dental Medicine; Explorers Club; World Center for Exploration;
National Geographic Society; Smithsonian Institution; Harvard Museum of
Comparative Zoology
FX Grant sponsors: National Science Foundation, Harvard Schools of Medicine
and Dental Medicine, The Explorers Club, World Center for Exploration,
The National Geographic Society, the Smithsonian Institution, the
Harvard Museum of Comparative Zoology.
NR 79
TC 10
Z9 10
U1 13
U2 98
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1932-8486
J9 ANAT REC
JI Anat. Rec.
PD JUN
PY 2012
VL 295
IS 6
BP 1006
EP 1016
DI 10.1002/ar.22449
PG 11
WC Anatomy & Morphology
SC Anatomy & Morphology
GA 940SY
UT WOS:000303914600014
PM 22467529
ER
PT J
AU Lacy, CHS
Torres, G
Fekel, FC
Sabby, JA
Claret, A
AF Lacy, Claud H. Sandberg
Torres, Guillermo
Fekel, Francis C.
Sabby, Jeffrey A.
Claret, Antonio
TI ABSOLUTE PROPERTIES OF THE ECLIPSING BINARY STAR BF DRACONIS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; binaries: spectroscopic; stars: fundamental
parameters; stars: individual (BF Dra)
ID SPECTROSCOPIC BINARIES; MODEL ATMOSPHERES; RADIAL-VELOCITIES; PRECISION
ORBITS; BETA PHOTOMETRY; TIDAL-EVOLUTION; APSIDAL MOTION; Y-2
ISOCHRONES; MAIN-SEQUENCE; LIGHT CURVES
AB BF Dra is now known to be an eccentric double-lined F6+F6 binary star with relatively deep (0.7 mag) partial eclipses. Previous studies of the system are improved with 7494 differential photometric observations from the URSA WebScope and 9700 from the NFO WebScope, 106 high-resolution spectroscopic observations from the Tennessee State University 2 m automatic spectroscopic telescope and the 1 m coude-feed spectrometer at Kitt Peak National Observatory, and 31 accurate radial velocities from the CfA. Very accurate (better than 0.6%) masses and radii are determined from analysis of the two new light curves and four radial velocity curves. Theoretical models match the absolute properties of the stars at an age of about 2.72 Gyr and [Fe/H]= -0.17, and tidal theory correctly confirms that the orbit should still be eccentric. Our observations of BF Dra constrain the convective core overshooting parameter to be larger than about 0.13 H-p. We find, however, that standard tidal theory is unable to match the observed slow rotation rates of the components' surface layers.
C1 [Lacy, Claud H. Sandberg] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA.
[Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fekel, Francis C.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
[Sabby, Jeffrey A.] So Illinois Univ, Dept Phys, Edwardsville, IL 62026 USA.
[Claret, Antonio] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
RP Lacy, CHS (reprint author), Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA.
EM clacy@uark.edu; gtorres@cfa.harvard.edu; fekel@evans.tsuniv.edu;
jsabby@siue.edu; claret@iaa.es
FU NASA; Tennessee State University; state of Tennessee; NSF [AST-10-07992]
FX The research at Tennessee State University was supported in part by
NASA, NSF, Tennessee State University, and the state of Tennessee
through its Centers of Excellence program.; The authors thank Bill Neely
who operates and maintains the NFO WebScope for the Consortium, and who
handles preliminary processing of the images and their distribution. The
authors also thank the staff at KPNO, especially Daryl Willmarth, for
maintenance and preparation of the coude-feed telescope and
spectrometer. G.T. acknowledges partial support from the NSF grant
AST-10-07992. Thanks also to University of Arkansas graduate student
Mythra Varun Nemallapudi for initial analysis of the URSA photometry and
preliminary radial velocities.
NR 67
TC 4
Z9 4
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUN
PY 2012
VL 143
IS 6
AR 129
DI 10.1088/0004-6256/143/6/129
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944GH
UT WOS:000304186800002
ER
PT J
AU Littlefield, C
Garnavich, P
Marion, GH
Vinko, J
McClelland, C
Rettig, T
Wheeler, JC
AF Littlefield, Colin
Garnavich, Peter
Marion, G. H. Howie
Jozsef Vinko
McClelland, Colin
Rettig, Terrence
Wheeler, J. Craig
TI DISCOVERY OF A WOLF-RAYET STAR THROUGH DETECTION OF ITS PHOTOMETRIC
VARIABILITY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE stars: individual (HBHa4203-27, WR142b); stars: Wolf-Rayet
ID MASSIVE STARS; WN STARS; EXTINCTION; SPECTRA; CATALOG
AB We report the serendipitous discovery of a heavily reddened Wolf-Rayet star that we name WR 142b. While photometrically monitoring a cataclysmic variable, we detected weak variability in a nearby field star. Low-resolution spectroscopy revealed a strong emission line at 7100 angstrom, suggesting an unusual object and prompting further study. A spectrum taken with the Hobby-Eberly Telescope confirms strong He II emission and an N IV 7112 angstrom line consistent with a nitrogen-rich Wolf-Rayet star of spectral class WN6. Analysis of the He II line strengths reveals no detectable hydrogen in WR 142b. A blue-sensitive spectrum obtained with the Large Binocular Telescope shows no evidence for a hot companion star. The continuum shape and emission line ratios imply a reddening of E(B - V) = 2.2-2.6 mag. We estimate that the distance to WR 142b is 1.4 +/- 0.3 kpc.
C1 [Littlefield, Colin] Univ Notre Dame, Sch Law, Notre Dame, IN 46556 USA.
[Garnavich, Peter; McClelland, Colin; Rettig, Terrence] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Marion, G. H. Howie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jozsef Vinko] Univ Szeged, Dept Opt, Szeged, Hungary.
[Jozsef Vinko; Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Littlefield, C (reprint author), Univ Notre Dame, Sch Law, Notre Dame, IN 46556 USA.
FU NSF [AST-1109801, AST-9987045]; Ohio Board of Regents; Ohio State
University Office of Research
FX We thank Perry Berlind of the Fred Whipple Observatory, Sergey
Rostopchin of McDonald Observatory, and Rick Pogge of The Ohio State
University. Additionally, Elena Pavlenko, Maksim Andreev, and Aleksej
Sosnovskij at the Crimean Astrophysical Observatory and Brian Skiff of
the Lowell Observatory kindly contributed photometry of WR 142b. We
thank Sebastian Otero for pointing out that the star was a catalogued
emission-line object. We also thank the anonymous referee for several
useful suggestions that improved the paper. J.C.W. is supported in part
by NSF grant AST-1109801.; The MODS spectrographs were built with
funding from the NSF grant AST-9987045 and the NSF Telescope System
Instrumentation Program (TSIP), with additional funds from the Ohio
Board of Regents and the Ohio State University Office of Research.
NR 30
TC 1
Z9 1
U1 0
U2 5
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 JUN
PY 2012
VL 143
IS 6
AR 136
DI 10.1088/0004-6256/143/6/136
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944GH
UT WOS:000304186800009
ER
PT J
AU Polyakov, YS
Neilsen, J
Timashev, SF
AF Polyakov, Yuriy S.
Neilsen, Joseph
Timashev, Serge F.
TI STOCHASTIC VARIABILITY IN X-RAY EMISSION FROM THE BLACK HOLE BINARY GRS
1915+105
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries: close; black hole physics;
methods: data analysis; methods: statistical; X-rays: individual (GRS
1915+105)
ID FLICKER-NOISE SPECTROSCOPY; QUASI-PERIODIC OSCILLATIONS; FAST
FOURIER-TRANSFORM; POWER SPECTRA; SYSTEM GRS-1915+105; RADIO-EMISSION;
TIME-SERIES; HARD STATE; PHASE-LAG; SIGNALS
AB We examine stochastic variability in the dynamics of X-ray emission from the black hole system GRS 1915+105, a strongly variable microquasar commonly used for studying relativistic jets and the physics of black hole accretion. The analysis of sample observations for 13 different states in both soft (low) and hard (high) energy bands is performed by flicker-noise spectroscopy (FNS), a phenomenological time series analysis method operating on structure functions and power spectrum estimates. We find the values of FNS parameters, including the Hurst exponent, flicker-noise parameter, and characteristic timescales, for each observation based on multiple 2500 s continuous data segments. We identify four modes of stochastic variability driven by dissipative processes that may be related to viscosity fluctuations in the accretion disk around the black hole: random (RN), power-law (1F), one-scale (1S), and two-scale (2S). The variability modes are generally the same in soft and hard energy bands of the same observation. We discuss the potential for future FNS studies of accreting black holes.
C1 [Polyakov, Yuriy S.] USPolyResearch, Ashland, PA 17921 USA.
[Neilsen, Joseph] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Timashev, Serge F.] Karpov Inst Phys Chem, Moscow 103064, Russia.
[Neilsen, Joseph] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Timashev, Serge F.] Russian Acad Sci, Inst Laser & Informat Technol, Troitsk 142190, Moscow Region, Russia.
RP Polyakov, YS (reprint author), USPolyResearch, Ashland, PA 17921 USA.
EM ypolyakov@uspolyresearch.com
OI Neilsen, Joseph/0000-0002-8247-786X
FU Harvard University Graduate School of Arts and Sciences [AR0-11004X];
National Aeronautics and Space Administration through the Smithsonian
Astrophysical Observatory [SV3-73016]; National Aeronautics Space
Administration [NAS8-03060]
FX J.N. was supported in part by the Harvard University Graduate School of
Arts and Sciences, Chandra grant AR0-11004X, and the National
Aeronautics and Space Administration through the Smithsonian
Astrophysical Observatory contract SV3-73016 to MIT for support of the
Chandra X-ray Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of the National Aeronautics Space
Administration under the contract NAS8-03060.
NR 55
TC 6
Z9 6
U1 1
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUN
PY 2012
VL 143
IS 6
AR 148
DI 10.1088/0004-6256/143/6/148
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 944GH
UT WOS:000304186800021
ER
PT J
AU Ogada, DL
Torchin, ME
Kinnaird, MF
Ezenwa, VO
AF Ogada, D. L.
Torchin, M. E.
Kinnaird, M. F.
Ezenwa, V. O.
TI Effects of Vulture Declines on Facultative Scavengers and Potential
Implications for Mammalian Disease Transmission
SO CONSERVATION BIOLOGY
LA English
DT Article
DE carcass decomposition; carnivore; hyena; jackal; Kenya
ID DOGS CANIS-FAMILIARIS; MARA NATIONAL RESERVE; DOMESTIC DOGS; VERTEBRATE
SCAVENGERS; CROCUTA-CROCUTA; RURAL ZIMBABWE; SPOTTED HYENAS;
LYCAON-PICTUS; WILDLIFE; RABIES
AB Vultures (Accipitridae and Cathartidae) are the only known obligate scavengers. They feed on rotting carcasses and are the most threatened avian functional group in the world. Possible effects of vulture declines include longer persistence of carcasses and increasing abundance of and contact between facultative scavengers at these carcasses. These changes could increase rates of transmission of infectious diseases, with carcasses serving as hubs of infection. To evaluate these possibilities, we conducted a series of observations and experimental tests of the effects of vulture extirpation on decomposition rates of livestock carcasses and mammalian scavengers in Kenya. We examined whether the absence of vultures changed carcass decomposition time, number of mammalian scavengers visiting carcasses, time spent by mammals at carcasses, and potential for disease transmission at carcasses (measured by changes in intraspecific contact rates). In the absence of vultures, mean carcass decomposition rates nearly tripled. Furthermore, the mean number of mammals at carcasses increased 3-fold (from 1.5 to 4.4 individuals/carcass), and the average time spent by mammals at carcasses increased almost 3-fold (from 55 min to 143 min). There was a nearly 3-fold increase in the mean number of contacts between mammalian scavengers at carcasses without vultures. These results highlight the role of vultures in carcass decomposition and level of contact among mammalian scavengers. In combination, our findings lead us to hypothesize that changes in vulture abundance may affect patterns of disease transmission among mammalian carnivores.
C1 [Ogada, D. L.; Kinnaird, M. F.; Ezenwa, V. O.] Mpala Res Ctr, Nanyuki, Kenya.
[Ogada, D. L.] Natl Museums Kenya, Ornithol Sect, Nairobi 00100, Kenya.
Peregrine Fund, Boise, ID 83709 USA.
[Torchin, M. E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Kinnaird, M. F.] Wildlife Conservat Soc Global Programs, Bronx, NY 10460 USA.
[Ezenwa, V. O.] Univ Georgia, Dept Infect Dis, Coll Vet Med, Athens, GA 30602 USA.
[Ezenwa, V. O.] Univ Georgia, Coll Vet Med, Odum Sch Ecol, Athens, GA 30602 USA.
RP Ogada, DL (reprint author), Mpala Res Ctr, Box 555, Nanyuki, Kenya.
EM darcyogada@yahoo.com
FU Smithsonian Institution; Raptor Research Foundation; Smithsonian
Tropical Research Institute
FX This research was funded by grants from the Smithsonian Institution, The
Peregrine Fund, Raptor Research Foundation-Leslie Brown Award, Chester
Zoo, and the Smithsonian Tropical Research Institute. The Smithsonian
Mpala Fellowship provided logistical support to D.O. We thank R. Eraguay
for field assistance. Mpala Research Centre provided logistical support,
and in particular we acknowledge M. Littlewood and J. Nakalonyo for
their assistance. We gratefully acknowledge support and advice provided
by S. Thomsett, L. Frank, R. Woodroffe, and M. Virani. C. Kreuder
Johnson, E. Fleishman, K. Bildstein, and P. Daszak provided valuable
comments that significantly improved the manuscript.
NR 42
TC 33
Z9 34
U1 6
U2 67
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0888-8892
J9 CONSERV BIOL
JI Conserv. Biol.
PD JUN
PY 2012
VL 26
IS 3
BP 453
EP 460
DI 10.1111/j.1523-1739.2012.01827.x
PG 8
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 943PA
UT WOS:000304135300009
PM 22443166
ER
PT J
AU Triantis, KA
Hortal, J
Amorim, I
Cardoso, P
Santos, AMC
Gabriel, R
Borges, PAV
AF Triantis, Kostas A.
Hortal, Joaquin
Amorim, Isabel
Cardoso, Pedro
Santos, Ana M. C.
Gabriel, Rosalina
Borges, Paulo A. V.
TI Resolving the Azorean knot: a response to Carine & Schaefer (2010)
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Letter
DE Azores; Canary Islands; climate oscillations; diversification; endemism;
isolation; Macaronesia; sea-level oscillations; seamounts; stepping
stones
ID OCEANIC ISLAND BIOGEOGRAPHY; LAST GLACIAL MAXIMUM; NORTH-ATLANTIC;
PHYLOGEOGRAPHY; CLIMATE; CIRCULATION; DIVERSITY; RECORD; AREA
AB Carine & Schaefer (Journal of Biogeography, 2010, 37, 7789) suggest that the lack of past climate oscillations in the Azores may have contributed to the low plant endemism in this archipelago compared to that of the Canary Islands, a pattern they term the Azorean diversity enigma. Here we challenge their hypothesis, and discuss how the particular characteristics of the Azores may have driven current diversification patterns in this archipelago. We argue that the restricted number of Azorean endemic species and their wide distribution is explicable by the geological, geographical and ecological attributes of the archipelago. That is, the Azores are too young, too small, and too environmentally homogeneous to have hosted many in situ diversification events, so they do not host as many endemic species as other Macaronesian archipelagos, such as Madeira and especially the Canary Islands.
C1 [Triantis, Kostas A.; Hortal, Joaquin; Amorim, Isabel; Cardoso, Pedro; Santos, Ana M. C.; Gabriel, Rosalina; Borges, Paulo A. V.] Univ Acores, Azorean Biodivers Grp CITA A, P-9700042 Terceira, Acores, Portugal.
[Triantis, Kostas A.] Univ Oxford, Ctr Environm, Biodivers Res Grp, Oxford OX1 3QY, England.
[Hortal, Joaquin] CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolut, E-28006 Madrid, Spain.
[Hortal, Joaquin; Santos, Ana M. C.] Univ Fed Goias, Inst Ciencias Biol, Dept Ecol, BR-74001970 Goiania, Go, Brazil.
[Amorim, Isabel] Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England.
[Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
RP Triantis, KA (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, P-9700042 Terceira, Acores, Portugal.
EM konstantinos.triantis@ouce.ox.ac.uk
RI Triantis, Kostas/A-1018-2009; Borges, Paulo/B-2780-2008; Gabriel,
Rosalina/F-1598-2013; Santos, Ana/E-7598-2010; Hortal,
Joaquin/A-1531-2008; Cardoso, Pedro/A-8820-2008; Amorim do Rosario,
Isabel/P-5140-2015
OI Borges, Paulo/0000-0002-8448-7623; Gabriel,
Rosalina/0000-0002-3550-8010; Santos, Ana/0000-0002-9197-792X; Hortal,
Joaquin/0000-0002-8370-8877; Cardoso, Pedro/0000-0001-8119-9960; Amorim
do Rosario, Isabel/0000-0001-6847-3320
NR 37
TC 14
Z9 14
U1 0
U2 13
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0305-0270
EI 1365-2699
J9 J BIOGEOGR
JI J. Biogeogr.
PD JUN
PY 2012
VL 39
IS 6
BP 1179
EP 1184
DI 10.1111/j.1365-2699.2011.02623.x
PG 6
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 943QG
UT WOS:000304139100015
ER
PT J
AU Rotman, D
Procita, K
Hansen, D
Parr, CS
Preece, J
AF Rotman, Dana
Procita, Kezia
Hansen, Derek
Parr, Cynthia Sims
Preece, Jennifer
TI Supporting content curation communities: The case of the Encyclopedia of
Life
SO JOURNAL OF THE AMERICAN SOCIETY FOR INFORMATION SCIENCE AND TECHNOLOGY
LA English
DT Article
DE collaboration; computer mediated communications; human computer
interaction
ID CITIZEN-SCIENCE; RESOURCE; PROJECT; NETWORK
AB This article explores the opportunities and challenges of creating and sustaining large-scale content curation communities through an in-depth case study of the Encyclopedia of Life (EOL). Content curation communities are large-scale crowdsourcing endeavors that aim to curate existing content into a single repository, making these communities different from content creation communities such as Wikipedia. In this article, we define content curation communities and provide examples of this increasingly important genre. We then follow by presenting EOL, a compelling example of a content curation community, and describe a case study of EOL based on analysis of interviews, online discussions, and survey data. Our findings are characterized into two broad categories: information integration and social integration. Information integration challenges at EOL include the need to (a) accommodate and validate multiple sources and (b) integrate traditional peer reviewed sources with user-generated, nonpeer-reviewed content. Social integration challenges at EOL include the need to (a) establish the credibility of open-access resources within the scientific community and (b) facilitate collaboration between experts and novices. After identifying the challenges, we discuss the potential strategies EOL and other content curation communities can use to address them, and provide technical, content, and social design recommendations for overcoming them.
C1 [Rotman, Dana; Procita, Kezia; Hansen, Derek; Preece, Jennifer] Univ Maryland, Coll Informat Studies, College Pk, MD 20742 USA.
[Parr, Cynthia Sims] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Rotman, D (reprint author), Univ Maryland, Coll Informat Studies, College Pk, MD 20742 USA.
EM drotman@umd.edu; kprocita@umd.edu; dlhansen@umd.edu; parrc@si.edu;
preece@umd.edu
RI Parr, Cynthia/E-8013-2010
OI Parr, Cynthia/0000-0002-8870-7099
NR 58
TC 11
Z9 11
U1 3
U2 44
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1532-2882
EI 1532-2890
J9 J AM SOC INF SCI TEC
JI J. Am. Soc. Inf. Sci. Technol.
PD JUN
PY 2012
VL 63
IS 6
BP 1092
EP 1107
DI 10.1002/asi.22633
PG 16
WC Computer Science, Information Systems; Information Science & Library
Science
SC Computer Science; Information Science & Library Science
GA 943OO
UT WOS:000304133900003
ER
PT J
AU Wright, RP
Lentz, DL
Beaubien, HF
Kimbrough, CK
AF Wright, Rita P.
Lentz, David L.
Beaubien, Harriet F.
Kimbrough, Christine K.
TI New evidence for jute (Corchorus capsularis L.) in the Indus
civilization
SO ARCHAEOLOGICAL AND ANTHROPOLOGICAL SCIENCES
LA English
DT Article
DE Jute cloth; Corchorus capsularis L.; Indus civilization
AB In this paper, we report the results of an analysis of a preserved structure of jute on a ceramic artifact from the site of Harappa that is dated to 2200-1900 (cal.) BC (Fig. 1). Jute cloth has not previously been identified at this early date in the Indus civilization. Since fiber remains are rare in prehistoric South Asia, we briefly review the evidence for seed and fiber remains used in textile production in this region.
C1 [Wright, Rita P.] NYU, Dept Anthropol, New York, NY 10003 USA.
[Lentz, David L.] Univ Cincinnati, Dept Biol, Cincinnati, OH USA.
[Beaubien, Harriet F.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA.
[Kimbrough, Christine K.] EBI Consulting, Burlington, MA USA.
RP Wright, RP (reprint author), NYU, Dept Anthropol, New York, NY 10003 USA.
EM rita.wright@nyu.edu
NR 29
TC 2
Z9 2
U1 0
U2 4
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1866-9557
J9 ARCHAEOL ANTHROP SCI
JI Archaeol. Anthropol. Sci.
PD JUN
PY 2012
VL 4
IS 2
BP 137
EP 143
DI 10.1007/s12520-012-0088-1
PG 7
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 223TW
UT WOS:000324834800004
ER
PT J
AU Cline, AR
Shockley, FW
AF Cline, Andrew R.
Shockley, Floyd W.
TI A NEW SPECIES OF FALLIA SHARP (CUCUJOIDEA: DISCOLOMATIDAE) FROM THE WEST
INDIES, WITH A WORLD CHECKLIST FOR FALLIA
SO COLEOPTERISTS BULLETIN
LA English
DT Article
DE taxonomy; catalog; Hispaniola; Dominican Republic; Caribbean
ID COLEOPTERA
AB A new discolomatid species, Fallia iviei Cline and Shockley, new species, is described from the Dominican Republic. A distribution map, habitus and character images, and discussion of its biology are provided. The new species represents the first known member of the genus from the West Indies. A species checklist for all nine described species of Fallia Sharp is presented.
C1 [Cline, Andrew R.] CDFA PPDC, Sacramento, CA 95758 USA.
[Shockley, Floyd W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
RP Cline, AR (reprint author), CDFA PPDC, 3294 Meadowview Rd, Sacramento, CA 95758 USA.
EM Andrew.Cline@cdfa.ca.gov; ShockleyF@si.edu
NR 20
TC 0
Z9 0
U1 0
U2 0
PU COLEOPTERISTS SOC
PI ATHENS
PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603
USA
SN 0010-065X
J9 COLEOPTS BULL
JI Coleopt. Bull.
PD JUN
PY 2012
VL 66
IS 2
BP 93
EP 99
PG 7
WC Entomology
SC Entomology
GA 142UF
UT WOS:000318822400003
ER
PT J
AU Tenner, E
AF Tenner, Edward
TI The Idea Factory: Bell Labs and the Great Age of American Innovation
SO ISSUES IN SCIENCE AND TECHNOLOGY
LA English
DT Book Review
C1 [Tenner, Edward] Smithsonian Inst, Lemelson Ctr, Washington, DC 20560 USA.
RP Tenner, E (reprint author), Rutgers Ctr Mobile Commun Studies, Newark, NJ 07102 USA.
EM edward.h.tenner@gmail.com
NR 1
TC 0
Z9 0
U1 1
U2 1
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0748-5492
EI 1938-1557
J9 ISSUES SCI TECHNOL
JI Issues Sci. Technol.
PD SUM
PY 2012
VL 28
IS 4
BP 93
EP 95
PG 3
WC Engineering, Multidisciplinary; Engineering, Industrial;
Multidisciplinary Sciences; Social Issues
SC Engineering; Science & Technology - Other Topics; Social Issues
GA V30TV
UT WOS:000208839200029
ER
PT J
AU Zeder, MA
AF Zeder, Melinda A.
TI THE DOMESTICATION OF ANIMALS
SO JOURNAL OF ANTHROPOLOGICAL RESEARCH
LA English
DT Article
DE Domestication; Animals; Behavior; Genetics; Animal sciences; Archaeology
AB Over the past 11,000 years humans have brought a wide variety of animals under domestication. Domestic animals belong to all Linnaean animal classes mammals, birds, reptiles, amphibians, fish, insects, and even, arguably, bacteria. Raised for food, secondary products, labor, and companionship, domestic animals have become intricately woven into human economy, society, and religion. Animal domestication is an on-going process, as humans, with increasingly sophisticated technology for breeding and rearing animals in captivity, continue to bring more and more species under their control. Understanding the process of animal domestication and its reciprocal impacts on humans and animal domesticates requires a multidisciplinary approach. This paper brings together recent research in archaeology, genetics, and animal sciences in a discussion of the process of domestication, its impact on animal domesticates, and the various pathways humans and their animal partners have followed into domestication.
C1 Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA.
RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA.
EM zederm@si.edu
NR 153
TC 23
Z9 23
U1 19
U2 71
PU UNIV NEW MEXICO, DEPT ANTHROPOL
PI ALBUQUERQUE
PA MSC01 1040, ANTHROPOLOGY 1, UNIV NEW MEXICO, ALBUQUERQUE, NM 87131 USA
SN 0091-7710
EI 2153-3806
J9 J ANTHROPOL RES
JI J. Anthropol. Res.
PD SUM
PY 2012
VL 68
IS 2
BP 161
EP 190
PG 30
WC Anthropology
SC Anthropology
GA V34GZ
UT WOS:000209076200001
ER
PT J
AU De Gracia, C
O'Dea, A
Rodriguez, F
D'Croz, L
AF De Gracia, Carlos
O'Dea, Aaron
Rodriguez, Felix
D'Croz, Luis
TI Environmental response in the Pacific to aseismic Cocos Ridge subduction
(Panama and Costa Rica).
SO REVISTA DE BIOLOGIA TROPICAL
LA Spanish
DT Article
DE Talamanca Range; closure of Panama isthmus; upwelling; benthic
communities; Pacific Ocean; marine fossils
ID EASTERN PACIFIC; ARC RESPONSE; CORAL-REEFS; EXTINCTION; ISTHMUS;
CHLOROPHYLL; EMERGENCE; NUTRIENTS; DYNAMICS; AMERICA
AB The evolution of the marine communities along the Pacific coast of Central America, may have changed in response to the formation of the Isthmus of Panama. To evaluate the effect of the Aseismic Cocos Ridge (DAC) subduction on the marine benthic communities, we reconstructed benthic assemblages from Neogene fossiliferous formations in Burica and Nicoya peninsulas of Panama and Costa Rica. Paleoecological and paleoenvironmental conditions were reconstructed by comparing community structure from bulk fossil samples with dredge collections from modern Tropical American seas, using principal component analysis. Our results indicate that during the early Pliocene, before the closing of the Isthmus, some oceanic islands existed with moderate upwelling in the Burica region. After the closure, during the late Pliocene and early Pleistocene the collision of the DAC caused an uplift of the seafloor, where water depth of 2 300m became shallow waters of less than 40m depth. Meanwhile, upwelling intensified in the open ocean the uplift that had formed small islands in coastal areas of Burica, creating protected areas and limiting the upwelling effect that was given in open ocean. The subduction of the DAC continued until the islands were joined to the mainland and gradually disappeared, allowing the return of the upwelling. During the middle Pleistocene a second process of accelerated uplift with speeds of 8m/1 000 years provoked again the elevation of the seafloor and later the elevation of the Talamanca Range. The new range formed a barrier that blocked the passage of the Trade winds, created new ecological conditions and optimized and allowed the growth of the best coral reefs in the coasts of the tropical Eastern Pacific (POT) between Panama and Costa Rica.
C1 [De Gracia, Carlos; O'Dea, Aaron; Rodriguez, Felix] Smithsonian Trop Res Inst, Panama City 03092, Panama.
[D'Croz, Luis] Univ Panama, Fac Ciencias Nat & Exactas, Dept Biol Marina & Limnol, Panama City, Panama.
RP De Gracia, C (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843, Panama City 03092, Panama.
EM degraciac@gmail.com; aaronodea@gmail.com; rodriguezf@si.edu;
dcrozlc@gmail.com
NR 62
TC 0
Z9 0
U1 1
U2 6
PU REVISTA DE BIOLOGIA TROPICAL
PI SAN JOSE
PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, 00000, COSTA
RICA
SN 0034-7744
J9 REV BIOL TROP
JI Rev. Biol. Trop.
PD JUN
PY 2012
VL 60
IS 2
BP 893
EP 908
PG 16
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 168WN
UT WOS:000320738700030
PM 23894954
ER
PT J
AU Anthony, NM
Mickala, P
Abernethy, KA
Atteke, C
Bissiengou, P
Bruford, MW
Dallmeier, F
Decaens, T
Dudu, A
Freedman, A
Gonder, MK
Hardy, O
Hart, J
Jeffery, K
Johnson, M
Pambo, FK
Ley, A
Korte, L
Lahm, SA
Lee, M
Lowenstein, J
Mboumba, JF
Bourobou, DN
Ngomanda, A
Ntie, S
Sebag, D
Sullivan, J
Vanthomme, H
Vergnes, V
Verheyen, E
Zimkus, B
AF Anthony, Nicola M.
Mickala, Patrick
Abernethy, Katharine A.
Atteke, Christiane
Bissiengou, Pulcherie
Bruford, Michael W.
Dallmeier, Francisco
Decaens, Thibaud
Dudu, Akaibe
Freedman, Adam
Gonder, Mary Katherine
Hardy, Olivier
Hart, John
Jeffery, Kathryn
Johnson, Mireille
Pambo, Flore Koumba
Ley, Alexandra
Korte, Lisa
Lahm, Sally A.
Lee, Michelle
Lowenstein, Jake
Mboumba, Jean-Francois
Bourobou, Dyana Ndiade
Ngomanda, Alfred
Ntie, Stephan
Sebag, David
Sullivan, John
Vanthomme, Hadrien
Vergnes, Virginie
Verheyen, Erik
Zimkus, Breda
TI Biodiversity and conservation genetics research in Central Africa: new
approaches and avenues for international collaboration
SO CONSERVATION GENETICS RESOURCES
LA English
DT Article
DE Africa; Conservation genetics; Biodiversity
AB A five-day international workshop was recently convened at the Universit, des Sciences et Techniques de Masuku in Gabon to enhance international collaboration among Central African, US and European scientists, conservation professionals and policy makers. The overall aims of the workshop were to: (1) discuss emerging priorities in biodiversity and conservation genetics research across Central Africa, and (2) create new networking opportunities among workshop participants. Here we provide a brief overview of the meeting, outline the major recommendations that emerged from it, and provide information on new networking opportunities through the meeting web site.
C1 [Anthony, Nicola M.; Ntie, Stephan] Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA.
[Mickala, Patrick; Atteke, Christiane; Mboumba, Jean-Francois] Univ Sci & Tech Masuku, Dept Biol, Franceville, Gabon.
[Abernethy, Katharine A.] Univ Stirling, Sch Nat Sci, Stirling FK9 4LA, Scotland.
[Bissiengou, Pulcherie] Ctr Natl Rech Sci & Technol, Inst Pharmacopee & Med Tradit, Libreville, Gabon.
[Bruford, Michael W.; Johnson, Mireille] Cardiff Univ, Sch Biosci, Organisms & Environm Div, Cardiff CF10 3AX, S Glam, Wales.
[Dallmeier, Francisco; Lee, Michelle; Vanthomme, Hadrien] Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA.
[Decaens, Thibaud] Univ Rouen, Lab ECODIV, EA 1293, SFR SCALE, F-76130 Mont St Aignan, France.
[Dudu, Akaibe] Univ Kisangani, Dept Ecol & Gest Ressources Anim, Kisangani, Zaire.
[Freedman, Adam] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90092 USA.
[Gonder, Mary Katherine] SUNY Albany, Dept Biol Sci, Albany, NY 12222 USA.
[Hardy, Olivier; Ley, Alexandra] Univ Libre Brussels, B-1050 Brussels, Belgium.
[Hart, John] Lukuru Fdn, Projet Tshuapa Lomami Lualaba, Kinshasa, Zaire.
[Jeffery, Kathryn] Agence Natl Parcs Nationaux, Libreville, Gabon.
[Korte, Lisa] Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Gabon Biodivers Program, Gamba, Gabon.
[Lahm, Sally A.] Ecol & Environm Inc, Arlington, VA 22209 USA.
[Lee, Michelle] Univ Oxford, Dept Zool, Oxford OX1 3PS, England.
[Lee, Michelle; Ngomanda, Alfred] Ctr Natl Rech Sci & Technol, Inst Rech Ecol Trop, Libreville, Gabon.
[Lowenstein, Jake] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
[Lowenstein, Jake] Amer Museum Nat Hist, New York, NY 10024 USA.
[Mboumba, Jean-Francois] Univ Rennes 1, Museum Natl Hist Nat, Equipe Biodivers & Gest Terr, UMR 7204, Rennes, France.
[Bourobou, Dyana Ndiade] Ctr Natl Rech Sci & Technol, Inst Rech Agron & Forestieres, Libreville, Gabon.
[Sebag, David] Univ Rouen, Lab M2C, UMR CNRS 6143, SFR SCALE, F-76130 Mont St Aignan, France.
[Sullivan, John] Cornell Univ, Museum Vertebrates, Ithaca, NY 14850 USA.
[Vergnes, Virginie] Max Planck Inst Evolutionary Anthropol, Wild Chimpanzee Fdn, D-04103 Leipzig, Germany.
[Verheyen, Erik] Royal Belgian Inst Nat Sci, Vertebrate Dept, B-1000 Brussels, Belgium.
[Zimkus, Breda] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA.
RP Anthony, NM (reprint author), Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA.
EM nanthony@uno.edu
RI SEBAG, David/A-4139-2008; Jeffery, Kathryn/G-2530-2013; Bruford,
Michael/D-3750-2009;
OI Abernethy, Katharine/0000-0002-0393-9342; SEBAG,
David/0000-0002-6446-6921; Jeffery, Kathryn/0000-0002-2632-0008;
Bruford, Michael/0000-0001-6357-6080; Freedman, Adam
/0000-0003-4714-3925
FU NSF OISE [0968587]
FX This workshop was funded by NSF OISE 0968587. Meeting participants would
like to thank the Universite of Sciences and Techniques de Masuku for
hosting the workshop and its Chancellor (Dr. Isaac Mouaragadja) for his
support.
NR 3
TC 3
Z9 3
U1 1
U2 17
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1877-7252
J9 CONSERV GENET RESOUR
JI Conserv. Genet. Resour.
PD JUN
PY 2012
VL 4
IS 2
BP 523
EP 525
DI 10.1007/s12686-011-9554-9
PG 3
WC Biodiversity Conservation; Genetics & Heredity
SC Biodiversity & Conservation; Genetics & Heredity
GA 935QZ
UT WOS:000303536400076
ER
PT J
AU Cramer, KL
Jackson, JBC
Angioletti, CV
Leonard-Pingel, J
Guilderson, TP
AF Cramer, Katie L.
Jackson, Jeremy B. C.
Angioletti, Christopher V.
Leonard-Pingel, Jill
Guilderson, Thomas P.
TI Anthropogenic mortality on coral reefs in Caribbean Panama predates
coral disease and bleaching
SO ECOLOGY LETTERS
LA English
DT Article
DE Acropora cervicornis; Bocas del Toro; climate change; corals; Dendostrea
frons; historical ecology; land use; molluscs; shifting baselines
ID PHASE-SHIFTS; ENVIRONMENTAL-STRESS; CLIMATE-CHANGE; WEST-INDIES;
ECOSYSTEMS; RADIOCARBON; ECOLOGY; SCALE; CONVERGENCE; DEGRADATION
AB Ecology Letters (2012) Abstract Caribbean reef corals have declined precipitously since the 1980s due to regional episodes of bleaching, disease and algal overgrowth, but the extent of earlier degradation due to localised historical disturbances such as land clearing and overfishing remains unresolved. We analysed coral and molluscan fossil assemblages from reefs near Bocas del Toro, Panama to construct a timeline of ecological change from the 19th centurypresent. We report large changes before 1960 in coastal lagoons coincident with extensive deforestation, and after 1960 on offshore reefs. Striking changes include the demise of previously dominant staghorn coral Acropora cervicornis and oyster Dendrostrea frons that lives attached to gorgonians and staghorn corals. Reductions in bivalve size and simplification of gastropod trophic structure further implicate increasing environmental stress on reefs. Our paleoecological data strongly support the hypothesis, from extensive qualitative data, that Caribbean reef degradation predates coral bleaching and disease outbreaks linked to anthropogenic climate change.
C1 [Cramer, Katie L.; Jackson, Jeremy B. C.; Angioletti, Christopher V.; Leonard-Pingel, Jill] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA.
[Cramer, Katie L.; Jackson, Jeremy B. C.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama.
[Guilderson, Thomas P.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Guilderson, Thomas P.] Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA.
RP Cramer, KL (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA.
EM katie.cramer@gmail.com
NR 43
TC 33
Z9 33
U1 3
U2 82
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1461-023X
J9 ECOL LETT
JI Ecol. Lett.
PD JUN
PY 2012
VL 15
IS 6
BP 561
EP 567
DI 10.1111/j.1461-0248.2012.01768.x
PG 7
WC Ecology
SC Environmental Sciences & Ecology
GA 937NW
UT WOS:000303666200007
PM 22462739
ER
PT J
AU Staniszewski, Z
Aikin, RW
Amiri, M
Benton, SJ
Bischoff, C
Bock, JJ
Bonetti, JA
Brevik, JA
Burger, B
Dowell, CD
Duband, L
Filippini, JP
Golwala, SR
Halpern, M
Hasselfield, M
Hilton, G
Hristov, VV
Irwin, K
Kovac, JM
Kuo, CL
Lueker, M
Montroy, T
Nguyen, HT
Ogburn, RW
O'Brient, R
Orlando, A
Pryke, C
Reintsema, C
Ruhl, JE
Schwarz, R
Sheehy, C
Stokes, S
Thompson, KL
Teply, G
Tolan, JE
Turner, AD
Vieregg, AG
Wilson, P
Wiebe, D
Wong, CL
AF Staniszewski, Z.
Aikin, R. W.
Amiri, M.
Benton, S. J.
Bischoff, C.
Bock, J. J.
Bonetti, J. A.
Brevik, J. A.
Burger, B.
Dowell, C. D.
Duband, L.
Filippini, J. P.
Golwala, S. R.
Halpern, M.
Hasselfield, M.
Hilton, G.
Hristov, V. V.
Irwin, K.
Kovac, J. M.
Kuo, C. L.
Lueker, M.
Montroy, T.
Nguyen, H. T.
Ogburn, R. W.
O'Brient, R.
Orlando, A.
Pryke, C.
Reintsema, C.
Ruhl, J. E.
Schwarz, R.
Sheehy, C.
Stokes, S.
Thompson, K. L.
Teply, G.
Tolan, J. E.
Turner, A. D.
Vieregg, A. G.
Wilson, P.
Wiebe, D.
Wong, C. L.
TI The Keck Array: A Multi Camera CMB Polarimeter at the South Pole
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Transition edge sensor (TES) arrays; Cosmology; Cosmic microwave
background; Inflation
AB The Keck array is a new multi-camera Cosmic Microwave Background (CMB) polarimeter. Each camera contains 256 polarization pairs of antenna-coupled transition edge sensor (TES) bolometers. We recently deployed three of five cameras at the geographic South Pole, and plan to deploy the final two cameras in early 2012. This new telescope is an ideal instrument to search for the primordial B-mode polarization signal imprinted in the CMB by inflationary gravitational waves. We will discuss the design of the detectors and receivers, the status of current observations, and report on progress toward upgrading the instrument with the full compliment of polarized receivers.
C1 [Staniszewski, Z.; Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Dowell, C. D.; Filippini, J. P.; Golwala, S. R.; Hristov, V. V.; Lueker, M.; Nguyen, H. T.; O'Brient, R.; Orlando, A.; Teply, G.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Staniszewski, Z.; Bock, J. J.; Bonetti, J. A.; Dowell, C. D.; Nguyen, H. T.; Turner, A. D.; Wilson, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kuo, C. L.; Ogburn, R. W.; Stokes, S.; Thompson, K. L.; Tolan, J. E.] KIPAC, Menlo Pk, CA 94025 USA.
[Amiri, M.; Halpern, M.; Hasselfield, M.; Wiebe, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Benton, S. J.; Burger, B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Kuo, C. L.; Ogburn, R. W.; Stokes, S.; Thompson, K. L.; Tolan, J. E.] Stanford Univ, Stanford, CA 94305 USA.
[Duband, L.] CEA Grenoble, Serv Basses Temp, F-38054 Grenoble, France.
[Hilton, G.; Irwin, K.; Reintsema, C.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Bischoff, C.; Kovac, J. M.; Schwarz, R.; Vieregg, A. G.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sheehy, C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Pryke, C.; Sheehy, C.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Montroy, T.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
RP Staniszewski, Z (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
EM zks@caltech.edu
RI Vieregg, Abigail/D-2287-2012;
OI Orlando, Angiola/0000-0001-8004-5054; Bischoff,
Colin/0000-0001-9185-6514
FU NASA
FX The following individuals acknowledge additional support: Z.
Staniszewski from the NASA Postdoctoral Program.
NR 7
TC 17
Z9 17
U1 1
U2 4
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0022-2291
J9 J LOW TEMP PHYS
JI J. Low Temp. Phys.
PD JUN
PY 2012
VL 167
IS 5-6
BP 827
EP 833
DI 10.1007/s10909-012-0510-1
PN 2
PG 7
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 934QY
UT WOS:000303461600041
ER
PT J
AU Guzman, HM
Breedy, O
AF Guzman, Hector M.
Breedy, Odalisca
TI Pacifigorgia marviva (Anthozoa: Octocorallia) a new species from Coiba
National Park, Pacific Panama
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE Octocorallia; Gorgoniidae; Pacifigorgia; Coiba National Park; eastern
Pacific; Panama
ID BIODIVERSITY
AB Pacifigorgia marviva, a new shallow-water species of the family Gorgoniidae, was found in Coiba National Park, Pacific Panama at 35-40 m depth. It is characterized by having white to cream, small, erect colonies composed of 1-4 fronds, stems short or absent network irregular and open without fan midribs, and polyp mounds slightly raised and sparsely distributed. All sclerites are colourless. Coenenchymal sclerites mostly composed of long spindles reaching up to 0.25 mm in length, and long and thin anthocodial rods, up to 0.16 mm in length. Morphological characters are analysed and illustrated. Scanning electron microscopy was used for sclerite study. The new species is herein described and compared with other similar species reported from the eastern Pacific. Pacifigoria marviva increases the number of Pacifigorgia species to 35; 20 in Panama representing 57% of the genus in the eastern Pacific, followed by Costa Rica and Ecuador with 14 and 10 species, respectively.
C1 [Guzman, Hector M.; Breedy, Odalisca] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscop, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica.
RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama.
EM odalisca@racsa.co.cr
FU Secretaria Nacional de Ciencia y Tecnologia of Panama [PNCOIBA08-024];
Smithsonian Tropical Research Institute
FX We are grateful to Phil Alderslade (CSIRO Marine and Atmospheric
Research, Tasmania), Stephen Cairns (Museum of Natural History,
Washington, DC), Leen van Ofwegen (Netherlands Centre for Biodiversity
Naturalis, Leiden), and Sergio Vargas (Molecular Geo- and Palaeobiology,
Geobiology and Palaeontology, LMU Munchen) for critical review of the
manuscript. We thank Percy Denyer (University of Costa Rica) for making
the figures. This work was supported by the Secretaria Nacional de
Ciencia y Tecnologia of Panama (grant number PNCOIBA08-024) and the
Smithsonian Tropical Research Institute.
NR 19
TC 3
Z9 3
U1 0
U2 6
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
EI 1469-7769
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD JUN
PY 2012
VL 92
IS 4
SI SI
BP 693
EP 698
DI 10.1017/S0025315411000373
PG 6
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 939TJ
UT WOS:000303837600006
ER
PT J
AU Erftemeijer, PLA
Hagedorn, M
Laterveer, M
Craggs, J
Guest, JR
AF Erftemeijer, Paul L. A.
Hagedorn, Mary
Laterveer, Michael
Craggs, Jamie
Guest, James R.
TI Effect of suspended sediment on fertilization success in the
scleractinian coral Pectinia lactuca
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE Pectinia lactuca; coral spawning; fertilization success; turbidity;
suspended sediment; dredging
ID ACROPORA-MILLEPORA EHRENBERG; GREAT-BARRIER-REEF; LARVAL METAMORPHOSIS;
REPRODUCTION; INHIBITION; MANAGEMENT; SETTLEMENT; ORGANISMS; FECUNDITY
AB The effect of increased levels of suspended sediment on fertilization success in the scleractinian coral Pectinia lactuca was investigated in a laboratory experiment following a mass coral spawning event on reefs off Singapore. Egg-sperm bundles were collected from tank-spawned coral colonies collected from the field several days prior to the anticipated mass spawning. Eggs and sperm from each colony were separated and distributed systematically across replicated treatments (N = 9) with three concentrations of fine suspended sediment. Spawning and embryo development in Pectinia lactuca followed a pattern similar to other scleractinian coral species. There was a significant effect of increased suspended sediment concentration on fertilization success (P < 0.05). Both high-(169 mg l(-1)) and medium-(43 mg l(-1)) suspended sediment treatments decreased fertilization success compared to controls. These results imply that increased turbidity levels (whether chronic, such as in the waters around Singapore, or short-term, caused by a dredging operation)-when coinciding with the coral spawning season-may affect the reproductive success of corals and compromise coral recruitment and recovery of degraded reefs.
C1 [Guest, James R.] Natl Univ Singapore, Dept Biol Sci, Marine Biol Lab, Singapore 117543, Singapore.
[Erftemeijer, Paul L. A.] Deltares, NL-2600 MH Delft, Netherlands.
[Hagedorn, Mary] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA.
[Laterveer, Michael] Rotterdam Zoo, NL-3000 AM Rotterdam, Netherlands.
[Craggs, Jamie] Horniman Museum & Gardens, London SE23 3PQ, England.
[Hagedorn, Mary] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Washington, DC 20008 USA.
RP Guest, JR (reprint author), Natl Univ Singapore, Dept Biol Sci, Marine Biol Lab, Singapore 117543, Singapore.
EM James.Guest@nus.edu.sg
RI Guest, James/D-5179-2011
OI Guest, James/0000-0002-9714-9009
FU Ecoshape-Building with Nature; Singapore-Delft Water Alliance (SDWA);
Singapore Ministry of Education [R-154-000-432-112]
FX We acknowledge Ecoshape-Building with Nature for their financial support
for the SECORE coral breeding workshop (30 March-8 April 2010) in
Singapore. The Tropical Marine Science Institute of the National
University of Singapore and Underwater World Singapore are thanked for
help with preparations, facilities and logistics during the workshop.
Astrid Kramer (Hydronamic) participated in the laboratory experiments
and data analysis. We appreciate the help of all other participants of
the 5th SECORE workshop with the field and laboratory work. The authors
acknowledge the support & contributions of the Singapore-Delft Water
Alliance (SDWA) and Singapore Ministry of Education Academic Research
Fund Tier 1 FRC Grant (Grant number: R-154-000-432-112). The research
presented here was carried out as part of the SDWA Marine & Coastal
Research Programme (Theme 2): 'Dredging and infrastructure development
near critical marine ecosystems' (R-264-001-001-272) and presented at
the Euro ISRS Symposium 2010: 'Reefs in a Changing Environment', 13-17
December 2010, Wageningen, The Netherlands. We thank Bert Hoeksema and
Pippa Mansell for allowing us to submit our paper for publication in
this special issue of JMBA.
NR 32
TC 12
Z9 12
U1 3
U2 24
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD JUN
PY 2012
VL 92
IS 4
SI SI
BP 741
EP 745
DI 10.1017/S0025315411000944
PG 5
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 939TJ
UT WOS:000303837600012
ER
PT J
AU Whigham, DF
Walker, CM
King, RS
Baird, SJ
AF Whigham, Dennis F.
Walker, Coowe M.
King, Ryan S.
Baird, Steven J.
TI Multiple Scales of Influence on Wetland Vegetation Associated with
Headwater Streams in Alaska, USA
SO WETLANDS
LA English
DT Article
DE Alaska; Wetland; Streamside; Calamagrostis canadensis; Kenai Peninsula;
Headwater streams
ID SPRUCE BEETLE OUTBREAK; CALAMAGROSTIS-CANADENSIS; KENAI PENINSULA; WHITE
SPRUCE; RIPARIAN RESERVES; BLUEJOINT GRASS; LITTER INPUTS; NITROGEN;
WATER; REGENERATION
AB Vegetation of wetlands adjacent to headwater streams on the Kenai Lowlands was dominated by , indicating that it is a keystone species that influences stream-wetland interactions across a wide range of geomorphic settings from which headwater streams have their origin. We sampled 30 sites as part of a project to determine the relationships between landscape features and the biological and chemical characteristics of headwater streams and their associated wetlands. In this paper we consider vegetation in wetlands adjacent to headwater streams. was the only species that occurred at all sites and only a few species were widespread and abundant across the range of sites sampled. Nonmetric multidimensional scaling of species importance values indicated that the distribution of sites and species was primarily related to stream-reach scale environmental and biological factors. Sixteen stream-reach factors were significantly correlated with the distribution of sites and species on one axis of the ordination. Headwater streams that were located in relatively flat areas with extensive wetlands had species characteristic of nutrient poor wetlands and sites located in steep valleys with narrow wetlands had species characteristic of uplands and wetlands on mineral soils. The distribution of sites and species on the second ordination axis was interpreted to be a response to biological interactions; primarily the negative relationship between and the diversity of other species. We concluded that large-scale watershed features of the landscape are less important than local scale factors in determining the characteristics of vegetation in headwater stream-wetland complexes in the Kenai Lowlands. There was no evidence, however, that differences in the stream-reach scale conditions across the study sites resulted in distinct plant communities associated with the headwater wetlands even though the headwater streams had their origin in different landscape settings.
C1 [Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Walker, Coowe M.; Baird, Steven J.] Kachemak Bay Res Reserve, Homer, AK 99603 USA.
[King, Ryan S.] Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst Res, Waco, TX 76798 USA.
RP Whigham, DF (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM whighamd@si.edu
OI Whigham, Dennis/0000-0003-1488-820X
FU US EPA
FX The project was funded through US EPA's Wetland Program Development
Grant program. Staff of the Kachemak Bay Research Reserve (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. Jeff Back deserves special recognition because of
his good spirits and efforts to keep the field teams on course and on
schedule under a wide range of climate conditions. We also thank the
Ninilchik Tribal Association and private landowners for providing access
to sampling sites. We especially thank Phil North for his encouragement,
support and efforts to make the project a reality. We thank Jay O'Neill,
Kathy Boomer, Mike Gracz and three anonymous reviewers for their
editorial suggestions.
NR 50
TC 4
Z9 4
U1 0
U2 15
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0277-5212
J9 WETLANDS
JI Wetlands
PD JUN
PY 2012
VL 32
IS 3
BP 411
EP 422
DI 10.1007/s13157-012-0274-z
PG 12
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 940IV
UT WOS:000303884100002
ER
PT J
AU Langley, JA
Megonigal, JP
AF Langley, J. Adam
Megonigal, J. Patrick
TI Field-Based Radiometry to Estimate Tidal Marsh Plant Growth in Response
to Elevated CO2 and Nitrogen Addition
SO WETLANDS
LA English
DT Article
DE Coastal wetland; Distichlis spicata; MSAVI2; ndvi; Productivity;
Schoenoplectus americanus; Spartina patens
ID ADJUSTED VEGETATION INDEX; SPECTRAL REFLECTANCE; AQUATIC VEGETATION;
ATMOSPHERIC CO2; MONITOR CHANGES; SALT MARSHES; DIVERSITY; PHENOLOGY;
SALINITY; WETLANDS
AB Plant growth is one of the most important variables to measure in long-term research plots, but the negative effects of labor-intensive and destructive sampling can restrict frequent assessment of plant biomass. Here, we used field-based, active radiometry to assess plant biomass in an ongoing, experimental manipulation of atmospheric CO2 and soil nitrogen availability in a tidal wetland. We compared the ability of several radiometric vegetation indices (VIs) to predict total plant biomass and that of two plant functional groups, sedges and grasses. All VIs estimated total biomass better in July than in October, when senescence had begun. All VIs correlated strongly and positively to grass biomass (average = 0.83) and weakly or negatively to sedge biomass ( = -0.30). Modified soil-adjusted vegetation index (MSAVI2) performed well through space (average July total biomass = 0.83) and time (across four sampling times = 0.83) and predicted CO2 and nitrogen treatment effect sizes. In conjunction with conventional biomass measurements field-based, active radiometry provides (1) a frequent estimate of biomass that can reveal plant responses to environmental stimuli that would otherwise escape detection, and (2) a viable alternative to frequent destructive sampling for assessing growth of fine-stemmed species such as and .Spartina patens and Distichlis spicata.
C1 [Langley, J. Adam; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Langley, J. Adam] Villanova Univ, Dept Biol, Villanova, PA 19085 USA.
RP Langley, JA (reprint author), Smithsonian Environm Res Ctr, POB 28, 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; 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 (grant
DE-FG02-97ER62458), the 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
Research Experience for Undergraduates (REU) Program, and the
Smithsonian Institution.
NR 33
TC 2
Z9 2
U1 2
U2 29
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0277-5212
J9 WETLANDS
JI Wetlands
PD JUN
PY 2012
VL 32
IS 3
BP 571
EP 578
DI 10.1007/s13157-012-0292-x
PG 8
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 940IV
UT WOS:000303884100015
ER
PT J
AU Leray, M
Boehm, JT
Mills, SC
Meyer, CP
AF Leray, M.
Boehm, J. T.
Mills, S. C.
Meyer, C. P.
TI Moorea BIOCODE barcode library as a tool for understanding predator-prey
interactions: insights into the diet of common predatory coral reef
fishes
SO CORAL REEFS
LA English
DT Article
DE Trophic interactions; Diet analysis; Food web; DNA identification;
Hawkfish; Squirrelfish
ID INVERTEBRATE PREDATORS; GUT CONTENTS; DNA; DIVERSITY; PRIMERS
AB Identifying species involved in consumer-resource interactions is one of the main limitations in the construction of food webs. DNA barcoding of prey items in predator guts provides a valuable tool for characterizing trophic interactions, but the method relies on the availability of reference sequences to which prey sequences can be matched. In this study, we demonstrate that the COI sequence library of the Moorea BIOCODE project, an ecosystem-level barcode initiative, enables the identification of a large proportion of semi-digested fish, crustacean and mollusks found in the guts of three Hawkfish and two Squirrelfish species. While most prey remains lacked diagnostic morphological characters, 94% of the prey found in 67 fishes had > 98% sequence similarity with BIOCODE reference sequences. Using this species-level prey identification, we demonstrate how DNA barcoding can provide insights into resource partitioning, predator feeding behaviors and the consequences of predation on ecosystem function.
C1 [Leray, M.; Mills, S. C.] Univ Perpignan, Lab Excellence Corail USR CNRS EPHE 3278, CRIOBE CBETM, F-66860 Perpignan, France.
[Leray, M.; Meyer, C. P.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Boehm, J. T.] CUNY Queens Coll, Dept Biol, Flushing, NY 11367 USA.
[Boehm, J. T.] CUNY, Grad Ctr, New York, NY 10016 USA.
RP Leray, M (reprint author), Univ Perpignan, Lab Excellence Corail USR CNRS EPHE 3278, CRIOBE CBETM, 56 Ave Paul Alduy, F-66860 Perpignan, France.
EM leray.upmc@gmail.com
RI Mills, Suzanne/K-5538-2012
FU Gordon and Betty Moore Foundation; Smithsonian Institution; France
American Cultural Exchange program (FACE-Partner University Fund)
FX We thank the BIOCODE teams who collected marine invertebrates and fish
specimen in 2006, the "Centre de Recherche Insulaire et Observatoire de
l'Environnement (CRIOBE) de Moorea'', the Richard B. Gump field station
in Moorea for logistical support and three anonymous reviewers for
helpful comments on the manuscript. We also greatly acknowledge the
Gordon and Betty Moore Foundation, Smithsonian Institution Fellowship
Program and France American Cultural Exchange program (FACE-Partner
University Fund) for financial support.
NR 25
TC 12
Z9 14
U1 3
U2 50
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0722-4028
J9 CORAL REEFS
JI Coral Reefs
PD JUN
PY 2012
VL 31
IS 2
BP 383
EP 388
DI 10.1007/s00338-011-0845-0
PG 6
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 934ND
UT WOS:000303450100008
ER
PT J
AU Rick, TC
Fitzpatrick, SM
AF Rick, Torben C.
Fitzpatrick, Scott M.
TI Archaeology and coastal conservation
SO JOURNAL OF COASTAL CONSERVATION
LA English
DT Editorial Material
ID ECOSYSTEMS
C1 [Rick, Torben C.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA.
[Fitzpatrick, Scott M.] N Carolina State Univ, Dept Sociol & Anthropol, Raleigh, NC 27695 USA.
RP Rick, TC (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA.
EM rickt@si.edu
NR 13
TC 1
Z9 1
U1 0
U2 3
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1400-0350
EI 1874-7841
J9 J COAST CONSERV
JI J. Coast. Conserv.
PD JUN
PY 2012
VL 16
IS 2
BP 135
EP 136
DI 10.1007/s11852-010-0121-4
PG 2
WC Biodiversity Conservation; Environmental Sciences; Marine & Freshwater
Biology; Water Resources
SC Biodiversity & Conservation; Environmental Sciences & Ecology; Marine &
Freshwater Biology; Water Resources
GA 935SS
UT WOS:000303541400001
ER
PT J
AU Reeder, LA
Rick, TC
Erlandson, JM
AF Reeder, Leslie A.
Rick, Torben C.
Erlandson, Jon M.
TI Our disappearing past: a GIS analysis of the vulnerability of coastal
archaeological resources in California's Santa Barbara Channel region
SO JOURNAL OF COASTAL CONSERVATION
LA English
DT Article
DE Sea level rise; Coastal erosion; Urban development; Cultural resource
vulnerability; GIS
ID SEA-LEVEL RISE; MARITIME CULTURES; BRUUN RULE; EROSION; ECOSYSTEMS;
COLLAPSE; HISTORY; FUTURE; INDEX
AB Coastal archaeological resources around the world often coincide with dense contemporary human populations and a rapidly changing physical environment. Projected sea level rise and urban expansion during the 21(st) century threaten to destroy much of our global coastal archaeological heritage. In this study, we adapt an environmental vulnerability analysis to quantify the threats of modern development and sea level rise on archaeological sites in California's Santa Barbara Channel region. Using spatial and statistical techniques, we create a Cultural Resource Vulnerability Index that combines environmental factors, current and projected urban footprints, and archaeological site positioning. We illustrate the importance of this method for targeting threatened archaeological sites for mitigation and salvage research. In the process, we highlight the significance of coastal archaeological sites for helping better understand contemporary environmental and cultural issues, underscoring the need to preserve or salvage these sites for their significant research value.
C1 [Reeder, Leslie A.] So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA.
[Rick, Torben C.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20013 USA.
[Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA.
[Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA.
RP Reeder, LA (reprint author), So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA.
EM lreeder@smu.edu; rickt@si.edu; jerland@uoregon.edu
OI Erlandson, Jon/0000-0002-4705-4319
NR 50
TC 6
Z9 6
U1 3
U2 27
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1400-0350
EI 1874-7841
J9 J COAST CONSERV
JI J. Coast. Conserv.
PD JUN
PY 2012
VL 16
IS 2
BP 187
EP 197
DI 10.1007/s11852-010-0131-2
PG 11
WC Biodiversity Conservation; Environmental Sciences; Marine & Freshwater
Biology; Water Resources
SC Biodiversity & Conservation; Environmental Sciences & Ecology; Marine &
Freshwater Biology; Water Resources
GA 935SS
UT WOS:000303541400006
ER
PT J
AU Fishelson, L
Baldwin, CC
Hastings, PA
AF Fishelson, Lev
Baldwin, Carole C.
Hastings, Philip A.
TI Comparison of the oropharyngeal cavity in the Starksiini (Teleostei:
Blenniiformes: Labrisomidae): Taste buds and teeth, including a
comparison with closely-related genera
SO JOURNAL OF MORPHOLOGY
LA English
DT Article
DE Starksiini fishes; oropharyngeal cavity; taste buds; dentition
ID FISH; SPECIALIZATIONS; PISCES; MOUTH; LIPS
AB The present study describes the distribution of taste buds and teeth in the oropharyngeal cavity of 13 species of adult (18-60 mm SL) Starksiini fishes inhabiting subtidal waters of the Neotropical region. Four types of taste buds described previously in other fish groups were observed within the oropharyngeal cavity, of which type I, situated on prominent protruding papillae, is the most common. The number of taste buds in this cavity varies considerably, ranging from ca. 202 in Starksia lepicoelia to ca. 770 in S. sluiteri. In all the studied species, taste buds are more numerous on the posterior (160-396) than on the anterior (42-294) part of the oropharyngeal cavity. The presence of different numbers of taste buds in different Starksiini species of the same standard length suggests that numbers of taste buds are not directly correlated with size and may be species-specific. Teeth are found on the premaxilla, dentary, vomer, palatine (in some species) and the upper and lower pharyngeal jaws (third pharyngobranchials and fifth ceratobranchials, respectively); the form and number of teeth and taste buds on each of these sites differs among the various species of Starksiini and between them and closely related species of the labrisomid tribes Labrisomini, Mnierpini, and Paraclinini. The results thus suggest potential systematic value in certain features of the oropharyngeal cavity for blenniiform fishes. It is also shown that benthic-feeding omnivorous fishes have higher densities of taste buds than piscivorous fishes. A possible correlation among numbers of taste buds, their positions in the oropharyngeal cavity, and other parameters is discussed. J. Morphol., 2012. (C) 2012 Wiley Periodicals, Inc.
C1 [Fishelson, Lev] Tel Aviv Univ, Dept Zool, IL-69978 Tel Aviv, Israel.
[Baldwin, Carole C.] Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Washington, DC 20560 USA.
[Hastings, Philip A.] Univ Calif San Diego, Div Marine Biol Res, Scripps Inst Oceanog, San Diego, CA 92103 USA.
RP Fishelson, L (reprint author), Tel Aviv Univ, Dept Zool, IL-69978 Tel Aviv, Israel.
EM fishelv@post.tau.ac.il
NR 34
TC 2
Z9 2
U1 0
U2 2
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0362-2525
J9 J MORPHOL
JI J. Morphol.
PD JUN
PY 2012
VL 273
IS 6
BP 618
EP 628
DI 10.1002/jmor.20008
PG 11
WC Anatomy & Morphology
SC Anatomy & Morphology
GA 930SI
UT WOS:000303159400006
PM 22234958
ER
PT J
AU Ivanenko, VN
Corgosinho, PHC
Ferrari, F
Sarradin, PM
Sarrazin, J
AF Ivanenko, Viatcheslav N.
Corgosinho, Paulo H. C.
Ferrari, Frank
Sarradin, Pierre-Marie
Sarrazin, Jozee
TI Microhabitat distribution of Smacigastes micheli (Copepoda:
Harpacticoida: Tegastidae) from deep-sea hydrothermal vents at the
Mid-Atlantic Ridge, 37 degrees N (Lucky Strike), with a morphological
description of its nauplius
SO MARINE ECOLOGY-AN EVOLUTIONARY PERSPECTIVE
LA English
DT Article
DE Confocal microscopy; Copepoda; deep-sea hydrothermal vent; ecology;
Harpacticoida; microhabitats; Mid-Atlantic Ridge; morphology; nauplius;
physico-chemical conditions; Tegastidae
ID EAST PACIFIC RISE; MUSSEL AGGREGATIONS; NORTHEAST PACIFIC; FALCATUS
NORMAN; FUCA RIDGE; CRUSTACEA; SIPHONOSTOMATOIDA; EDIFICE; OCEAN; GENUS
AB Abundant nauplii and copepodid stages attributed to Smacigastes micheli Ivanenko & Defaye (Crustacea: Copepoda: Harpacticoida: Tegastidae) were collected during the MoMARETO cruise (2006) on the Eiffel Tower edifice, the species type locality at the Lucky Strike vent field (37 degrees N) of the Mid-Atlantic Ridge at a depth of 1698 m. Specimens were sampled within different faunal assemblages dominated by either Bathymodiolus azoricus mussels or Mirocaris fortunata shrimps and the physico-chemical conditions of their related microhabitats were characterized. A new preparation method for examination of copepod nauplii with confocal microscopy was developed and applied to the specimens. The description of the sixth naupliar stage of S. micheli revealed a number of distinctions from the only known last naupliar stage of the tegastid copepod Tegastes falcatus living associated with a shallow water bryozoan. Morphological features and ecological observations suggest that S. micheli copepods could be feeding on the thick microbial mats that cover different surfaces on the Eiffel Tower edifice. The nauplii, copepodids and adults of S. micheli were found in >80% of the microhabitats sampled. These microhabitats were characterized by temperatures varying from 4.8 to 7.5 degrees C representing low hydrothermal inputs. Canonical analysis shows that the relative abundances of nauplii and adults of S. micheli were higher at the lower end of the chemical conditions, whereas the abundance of the subadult stages appears to be linked with slightly higher hydrothermal inputs. Whether this distribution is influenced by distinct physiological tolerances or nutritional needs of the different developmental stages is unknown. Total dissolved sulfur was the variable best explaining the distribution of S. micheli on the Eiffel Tower edifice.
C1 [Ivanenko, Viatcheslav N.] Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119992, Russia.
[Corgosinho, Paulo H. C.] Univ Estadual Montes Claros, Dept Biol, Zool Lab, Montes Claros, MG, Brazil.
[Ferrari, Frank] Smithsonian Inst, Natl Museum Nat Hist, IZ MSC, MRC 534, Suitland, MD USA.
[Sarradin, Pierre-Marie; Sarrazin, Jozee] IFREMER, Ctr Brest, Dept Etud Ecosyst Profonds, Lab Environm Profond, Plouzane, France.
RP Ivanenko, VN (reprint author), Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Leninskie Gory 1-12, Moscow 119992, Russia.
EM ivanenko@mail.bio.msu.ru
RI Ivanenko, Viatcheslav/B-8198-2008; Corgosinho, Paulo
Henrique/C-1047-2015
OI Ivanenko, Viatcheslav/0000-0003-1255-0491; Corgosinho, Paulo
Henrique/0000-0002-2851-6557
FU EXOCET/D European; Ifremer (France); Russian Foundation for Basic
Research [09-04-01523-a]; Ministry of Education and Science of the
Russian Federation [Pi1291, 02.740.11.0875, 14.740.11.1049]; ANR
DEEP-OASES [ANR06BDV005]; GDR ECCHIS
FX The MoMARETO cruise (2006) was led by Jozee Sarrazin and Pierre-Marie
Sarradin (chief scientists) and part of it was supported by the EXOCET/D
European program. The study of copepods was supported by grants from
Ifremer (France), the Russian Foundation for Basic Research
(09-04-01523-a) and the Ministry of Education and Science of the Russian
Federation (Pi 1291, 02.740.11.0875, 14.740.11.1049). This research
project also benefited from funds from the ANR DEEP-OASES (ANR06BDV005)
and support from the GDR ECCHIS. H.-U. Dahms kindly commented on early
drafts of the manuscript. Confocal microscopies were conducted in the
German Center for Marine Biodiversity Research of the Senckenberg
Research Institute.
NR 37
TC 4
Z9 4
U1 0
U2 16
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0173-9565
EI 1439-0485
J9 MAR ECOL-EVOL PERSP
JI Mar. Ecol.-Evol. Persp.
PD JUN
PY 2012
VL 33
IS 2
BP 246
EP 256
DI 10.1111/j.1439-0485.2011.00484.x
PG 11
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 929EF
UT WOS:000303043300009
ER
PT J
AU Elvis, M
AF Elvis, Martin
TI Let's mine asteroids - for science and profit
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 martinselvis2@gmail.com
NR 0
TC 15
Z9 15
U1 7
U2 57
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD MAY 31
PY 2012
VL 485
IS 7400
BP 549
EP 549
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 949WP
UT WOS:000304608000013
PM 22660280
ER
PT J
AU Webb, JM
Jacobus, LM
Funk, DH
Zhou, X
Kondratieff, B
Geraci, CJ
DeWalt, RE
Baird, DJ
Richard, B
Phillips, I
Hebert, PDN
AF Webb, Jeffrey M.
Jacobus, Luke M.
Funk, David H.
Zhou, Xin
Kondratieff, Boris
Geraci, Christy J.
DeWalt, R. Edward
Baird, Donald J.
Richard, Barton
Phillips, Iain
Hebert, Paul D. N.
TI A DNA Barcode Library for North American Ephemeroptera: Progress and
Prospects
SO PLOS ONE
LA English
DT Article
ID WATER-QUALITY; BIOLOGICAL IDENTIFICATIONS; TRICHOPTERA; EPHEMERELLIDAE;
BIODIVERSITY; PLECOPTERA; PHYLOGENY; SPECIMEN; LEVEL
AB DNA barcoding of aquatic macroinvertebrates holds much promise as a tool for taxonomic research and for providing the reliable identifications needed for water quality assessment programs. A prerequisite for identification using barcodes is a reliable reference library. We gathered 4165 sequences from the barcode region of the mitochondrial cytochrome c oxidase subunit I gene representing 264 nominal and 90 provisional species of mayflies (Insecta: Ephemeroptera) from Canada, Mexico, and the United States. No species shared barcode sequences and all can be identified with barcodes with the possible exception of some Caenis. Minimum interspecific distances ranged from 0.3-24.7% (mean: 12.5%), while the average intraspecific divergence was 1.97%. The latter value was inflated by the presence of very high divergences in some taxa. In fact, nearly 20% of the species included two or three haplotype clusters showing greater than 5.0% sequence divergence and some values are as high as 26.7%. Many of the species with high divergences are polyphyletic and likely represent species complexes. Indeed, many of these polyphyletic species have numerous synonyms and individuals in some barcode clusters show morphological attributes characteristic of the synonymized species. In light of our findings, it is imperative that type or topotype specimens be sequenced to correctly associate barcode clusters with morphological species concepts and to determine the status of currently synonymized species.
C1 [Webb, Jeffrey M.; Hebert, Paul D. N.] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada.
[Jacobus, Luke M.] Indiana Univ Purdue Univ Columbus, Div Sci, Columbus, IN USA.
[Funk, David H.] Stroud Water Res Ctr, Avondale, PA USA.
[Zhou, Xin] BGI, Shenzhen, Guangdong, Peoples R China.
[Kondratieff, Boris] Colorado State Univ, Dept Bioagr Sci & Pest Management, Ft Collins, CO 80523 USA.
[Geraci, Christy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA.
[DeWalt, R. Edward] Univ Illinois, Prairie Res Inst, Champaign, IL 61820 USA.
[Baird, Donald J.] Univ New Brunswick, Dept Biol, Canadian Rivers Inst, Environm Canada, Fredericton, NB E3B 6E1, Canada.
[Richard, Barton] Florida A&M Univ, Lab Aquat Entomol, Tallahassee, FL 32307 USA.
[Phillips, Iain] Saskatchewan Watershed Author, Saskatoon, SK, Canada.
RP Webb, JM (reprint author), Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada.
EM jmw975@yahoo.com
RI Zhou, Xin/D-4025-2009; Baird, Donald/A-5267-2009; Hebert,
Paul/C-4161-2013
OI Zhou, Xin/0000-0002-1407-7952; Hebert, Paul/0000-0002-3081-6700
FU Government of Canada through Genome Canada; Ontario Genomics Institute
[2008-OGI-ICI-03]; Environment Canada's Competitiveness and
Environmental Sustainability Indicators (CESI) Program
FX This project was funded by the Government of Canada through Genome
Canada and the Ontario Genomics Institute (2008-OGI-ICI-03), and
Environment Canada's Competitiveness and Environmental Sustainability
Indicators (CESI) Program. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 38
TC 29
Z9 32
U1 0
U2 38
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAY 30
PY 2012
VL 7
IS 5
AR e38063
DI 10.1371/journal.pone.0038063
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959YF
UT WOS:000305353400074
PM 22666447
ER
PT J
AU Penalver, E
Labandeira, CC
Barron, E
Delclos, X
Nel, P
Nel, A
Tafforeau, P
Soriano, C
AF Penalver, Enrique
Labandeira, Conrad C.
Barron, Eduardo
Delclos, Xavier
Nel, Patricia
Nel, Andre
Tafforeau, Paul
Soriano, Carmen
TI Thrips pollination of Mesozoic gymnosperms
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE paleoecology; paleoethology; coevolution; plant-insect interactions
ID ORDER THYSANOPTERA INSECTA; PHYLOGENETIC ANALYSIS; AUSTRALIAN CYCAD;
SOCIAL-BEHAVIOR; POLLEN; EVOLUTION; ANGIOSPERMS; ZAMIACEAE; INFERENCE;
ORIGIN
AB Within modern gymnosperms, conifers and Ginkgo are exclusively wind pollinated whereas many gnetaleans and cycads are insect pollinated. For cycads, thrips are specialized pollinators. We report such a specialized pollination mode from Early Cretaceous amber of Spain, wherein four female thrips representing a genus and two species in the family Melanthripidae were covered by abundant Cycadopites pollen grains. These females bear unique ring setae interpreted as specialized structures for pollen grain collection, functionally equivalent to the hook-tipped sensilla and plumose setae on the bodies of bees. The most parsimonious explanation for this structure is parental food provisioning for larvae, indicating subsociality. This association provides direct evidence of specialized collection and transportation of pollen grains and likely gymnosperm pollination by 110-105 million years ago, possibly considerably earlier.
C1 [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Penalver, Enrique; Barron, Eduardo] Inst Geol & Minero Espana, Museo Geominero, E-28003 Madrid, Spain.
[Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Labandeira, Conrad C.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA.
[Delclos, Xavier] Univ Barcelona, Fac Geol, Dept Estratig Paleontol & Geociencies, E-08071 Barcelona, Spain.
[Nel, Patricia; Nel, Andre] Museum Natl Hist Nat, CNRS, UMR 7205, F-75005 Paris, France.
[Nel, Patricia; Nel, Andre] AgroParisTech, Dept Sci Vie & Sante, F-75231 Paris, France.
[Tafforeau, Paul; Soriano, Carmen] European Synchrotron Radiat Facil, F-38000 Grenoble, France.
RP Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
EM labandec@si.edu
RI DELCLOS, Xavier/D-4363-2014
OI DELCLOS, Xavier/0000-0002-2233-5480
FU European Union [FR-TAF-5126]; Spanish Ministry of Economy and
Competitiveness [CGL2011-23948/BTE]
FX We thank the staff of the Museo de Ciencias Naturales de Alava in Spain
for preparation, curation, and access to specimens. We thank Bernard
Gomez from the University of Lyon-1 and Jose Baruchel and Tamzin Lafford
from the European Synchrotron Radiation Facility for their help.
Finnegan Marsh did the illustrations. We thank Peter Cloetens,
Jean-Claude Labiche, Alejandro Homs, Antonia Beteva, Alessandro Mirone,
and Max Langer from the European Synchrotron Radiation Facility for
assistance with the imaging and 3D reconstruction of specimens. E. P.
acknowledges European Union Synthesys Grant FR-TAF-5126 to study
Cretaceous thrips. This study was supported by the Spanish Ministry of
Economy and Competitiveness project CGL2011-23948/BTE. This is
contribution 174 of the Evolution of Terrestrial Ecosystems consortium
at the National Museum of Natural History, in Washington, DC.
NR 43
TC 27
Z9 27
U1 6
U2 49
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD MAY 29
PY 2012
VL 109
IS 22
BP 8623
EP 8628
DI 10.1073/pnas.1120499109
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 953PD
UT WOS:000304881700056
PM 22615414
ER
PT J
AU Mayle, M
Rittenhouse, ST
Schmelcher, P
Sadeghpour, HR
AF Mayle, M.
Rittenhouse, S. T.
Schmelcher, P.
Sadeghpour, H. R.
TI Electric field control in ultralong-range triatomic polar Rydberg
molecules
SO PHYSICAL REVIEW A
LA English
DT Article
ID DIPOLE-MOMENT; BLOCKADE; ATOMS; GAS
AB We theoretically explore the external electric field control of a species of ultralong-range molecules that emerge from the interaction of a ground-state polar molecule with a Rydberg atom. The external field mixes the Rydberg electronic states and, therefore, strongly alters the electric field seen by the polar diatomic molecule due to the Rydberg electron. As a consequence, the adiabatic potential energy curves responsible for the molecular binding can be tuned in such a way that an intersection with neighboring curves occurs. The latter leads to admixture of s-wave character in the Rydberg wave function and will substantially facilitate the experimental preparation and realization of this particular class of Rydberg molecule species.
C1 [Mayle, M.] Univ Colorado, JILA, Boulder, CO 80309 USA.
[Mayle, M.] Natl Inst Stand & Technol, Boulder, CO 80309 USA.
[Rittenhouse, S. T.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Schmelcher, P.] Univ Hamburg, Zentrum Opt Quantentechnol, D-22761 Hamburg, Germany.
RP Mayle, M (reprint author), Univ Colorado, JILA, Boulder, CO 80309 USA.
RI Mayle, Michael/A-2423-2009; Schmelcher, Peter/D-9592-2014
OI Schmelcher, Peter/0000-0002-2637-0937
FU German Academic Exchange Service (DAAD); NSF through ITAMP at Harvard
University; Smithsonian Astrophysical Observatory
FX M.M. acknowledges financial support by a fellowship within the
postdoc-programme of the German Academic Exchange Service (DAAD). S.T.R.
and H.R.S. acknowledge financial support from the NSF through ITAMP at
Harvard University and the Smithsonian Astrophysical Observatory.
NR 24
TC 13
Z9 13
U1 0
U2 7
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD MAY 24
PY 2012
VL 85
IS 5
AR 052511
DI 10.1103/PhysRevA.85.052511
PG 7
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 946XR
UT WOS:000304391300005
ER
PT J
AU Pyenson, ND
Goldbogen, JA
Vogl, AW
Szathmary, G
Drake, RL
Shadwick, RE
AF Pyenson, Nicholas D.
Goldbogen, Jeremy A.
Vogl, A. Wayne
Szathmary, Gabor
Drake, Richard L.
Shadwick, Robert E.
TI Discovery of a sensory organ that coordinates lunge feeding in rorqual
whales
SO NATURE
LA English
DT Article
ID FIN WHALES; MYSTICETE; MECHANICS; CETACEA; BALEEN
AB Top ocean predators have evolved multiple solutions to the challenges of feeding in the water(1-3). At the largest scale, rorqual whales (Balaenopteridae) engulf and filter prey-laden water by lunge feeding(4), a strategy that is unique among vertebrates(1). Lunge feeding is facilitated by several morphological specializations, including bilaterally separate jaws that loosely articulate with the skull(5,6), hyper-expandable throat pleats, or ventral groove blubber(7), and a rigid y-shaped fibrocartilage structure branching from the chin into the ventral groove blubber(8). The linkages and functional coordination among these features, however, remain poorly understood. Here we report the discovery of a sensory organ embedded within the fibrous symphysis between the unfused jaws that is present in several rorqual species, at both fetal and adult stages. Vascular and nervous tissue derived from the ancestral, anterior-most tooth socket insert into this organ, which contains connective tissue and papillae suspended in a gel-like matrix. These papillae show the hallmarks of a mechanoreceptor, containing nerves and encapsulated nerve termini. Histological, anatomical and kinematic evidence indicate that this sensory organ responds to both the dynamic rotation of the jaws during mouth opening and closure, and ventral groove blubber(7) expansion through direct mechanical linkage with the y-shaped fibrocartilage structure. Along with vibrissae on the chin(9), providing tactile prey sensation, this organ provides the necessary input to the brain for coordinating the initiation, modulation and end stages of engulfment, a paradigm that is consistent with unsteady hydrodynamic models and tag data from lunge-feeding rorquals(10-13). Despite the antiquity of unfused jaws in baleen whales since the late Oligocene(14) (similar to 23-28 million years ago), this organ represents an evolutionary novelty for rorquals, based on its absence in all other lineages of extant baleen whales. This innovation has a fundamental role in one of the most extreme feeding methods in aquatic vertebrates, which facilitated the evolution of the largest vertebrates ever.
C1 [Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Mammal, Seattle, WA 98195 USA.
[Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA.
[Goldbogen, Jeremy A.] Cascadia Res Collect, Olympia, WA 98501 USA.
[Vogl, A. Wayne] Univ British Columbia, Dept Cellular & Physiol Sci, Vancouver, BC V6T 1Z3, Canada.
[Szathmary, Gabor] FPInnovations, Vancouver, BC V6T 1W5, Canada.
[Drake, Richard L.] Case Western Reserve Univ, Cleveland Clin, Lerner Coll Med, Cleveland, OH 44195 USA.
[Shadwick, Robert E.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada.
RP Pyenson, ND (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA.
EM pyensonn@si.edu
OI Goldbogen, Jeremy/0000-0002-4170-7294
FU Natural Sciences and Engineering Research Council of Canada; Smithsonian
Institution; Remington Kellogg Fund; University of British Columbia;
Scripps Postdoctoral Research Fellowship; NSERC
FX For logistical support, we thank K. Loftsson and the staff at Hvalur hf;
D. Olafsdottir, S. D. Halldorsson and G. A. Vikingsson at the Marine
Research Institute, Reykjavik; G. Bergmann and the staff at
Hrefnuveioimenn ehf; S. Raverty; P. F. Brodie; and A. Trites. For
additional samples and data, we also thank P.-Y. Daoust, G. Williams,
the Amarok Hunters and Trappers Organization of Iqaluit, Captain S. Awa
and the Inuit whaling crew from Iqaluit, J. Higgins and the Cascadia
Research Collective, M. R. Buono, A. van Helden and the Museum of New
Zealand Te Papa Tongarewa, and R. E. Fordyce. We also thank T. S. Hunter
for assistance with laboratory samples. Comments from D. J. Bohaska, M.
T. Carrano, R. B. Irmis, J. G. Mead, J. F. Parham, C. W. Potter and J.
Velez-Juarbe improved this manuscript. N.D.P. was supported by a
postdoctoral research fellowship from the Natural Sciences and
Engineering Research Council of Canada and by funding from the
Smithsonian Institution and its Remington Kellogg Fund. J. A. G. was
supported by a University Graduate Fellowship for Research from the
University of British Columbia, a Scripps Postdoctoral Research
Fellowship and NSERC funding to R.E.S.
NR 30
TC 34
Z9 34
U1 10
U2 64
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD MAY 24
PY 2012
VL 485
IS 7399
BP 498
EP 501
DI 10.1038/nature11135
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 946IH
UT WOS:000304344500042
PM 22622577
ER
PT J
AU McNamara, BR
Nulsen, PEJ
AF McNamara, B. R.
Nulsen, P. E. J.
TI Mechanical feedback from active galactic nuclei in galaxies, groups and
clusters
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
ID COOLING-FLOW CLUSTERS; X-RAY CAVITIES; MASSIVE BLACK-HOLE; ANISOTROPIC
THERMAL CONDUCTION; EXTRAGALACTIC RADIO-SOURCES; CENTRAL DOMINANT
GALAXIES; DEEP CHANDRA OBSERVATION; DRIVEN ACCRETION FLOWS; STAR-FORMING
GALAXIES; H-ALPHA FILAMENTS
AB The radiative cooling timescales at the centers of hot atmospheres surrounding elliptical galaxies, groups and clusters are much shorter than their ages. Therefore, hot atmospheres are expected to cool and to form stars. Cold gas and star formation are observed in central cluster galaxies but at levels below those expected from an unimpeded cooling flow. X-ray observations have shown that wholesale cooling is being offset by mechanical heating from radio active galactic nuclei. Feedback is widely considered to be an important and perhaps unavoidable consequence of the evolution of galaxies and supermassive black holes. We show that cooling x-ray atmospheres and the ensuing star formation and nuclear activity are probably coupled to a self-regulated feedback loop. While the energetics are now reasonably well understood, other aspects of feedback are not. We highlight the problems of atmospheric heating and transport processes, accretion, and nuclear activity, and we discuss the potential role of black hole spin. We discuss x-ray imagery showing that the chemical elements produced by central galaxies are being dispersed on large scales by outflows launched from the vicinity of supermassive black holes. Finally, we comment on the growing evidence for mechanical heating of distant cluster atmospheres by radio jets and its potential consequences for the excess entropy in hot halos and a possible decline in the number of distant cooling flows.
C1 [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.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP McNamara, BR (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
EM mcnamara@uwaterloo.ca; pnulsen@cfa.harvard.edu
OI Nulsen, Paul/0000-0003-0297-4493
FU NASA [NAS8-03060]; Chandra Large Project [G09-0140X]; Natural Sciences
and Engineering Research Council of Canada; SSEP from Canadian Space
Agency
FX We thank Helen Russell, Massimo Gaspari, Christoph Pfrommer, Prateek
Sharma, Bill Mathews and especially Mark Voit and Peter Mendygral for
their help and advice. This work was supported in part by NASA contract
NAS8-03060, Chandra Large Project grant G09-0140X, and generous funding
from the Natural Sciences and Engineering Research Council of Canada,
and an SSEP grant from the Canadian Space Agency.
NR 318
TC 138
Z9 140
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1367-2630
J9 NEW J PHYS
JI New J. Phys.
PD MAY 23
PY 2012
VL 14
AR 055023
DI 10.1088/1367-2630/14/5/055023
PG 40
WC Physics, Multidisciplinary
SC Physics
GA 953NP
UT WOS:000304875700001
ER
PT J
AU Zaslavsky, A
Meyer-Vernet, N
Mann, I
Czechowski, A
Issautier, K
Le Chat, G
Pantellini, F
Goetz, K
Maksimovic, M
Bale, SD
Kasper, JC
AF Zaslavsky, A.
Meyer-Vernet, N.
Mann, I.
Czechowski, A.
Issautier, K.
Le Chat, G.
Pantellini, F.
Goetz, K.
Maksimovic, M.
Bale, S. D.
Kasper, J. C.
TI Interplanetary dust detection by radio antennas: Mass calibration and
fluxes measured by STEREO/WAVES
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID PLASMA-WAVE INSTRUMENT; INTERSTELLAR DUST; SOLAR-SYSTEM; ASTRONOMY
INSTRUMENT; RING PLANE; VOYAGER 1; IMPACTS; SPACECRAFT; CONSTRAINTS;
CASSINI
AB We analyze dust impacts recorded by the S/WAVES radio instrument onboard the two STEREO spacecraft near 1 A.U. during the period 2007-2010. The impact of a dust particle on a spacecraft produces a plasma cloud whose associated electric field can be detected by on-board electric antennas. For this study we use the electric potential time series recorded by the waveform sampler of the instrument. The high time resolution and long sampling times of this measurement enable us to deduce considerably more information than in previous studies based on the dynamic power spectra provided by the same instrument or by radio instruments onboard other spacecraft. The large detection area compared to conventional dust detectors provides flux data with a better statistics. We show that the dust-generated signals are of two kinds, corresponding to impacts of dust from distinctly different mass ranges. We propose calibration formulas for these signals and show that we are able to use S/WAVES as a dust detector with convincing results both in the nanometer and micrometer size ranges. In the latter, the orbital motion of the spacecraft enables us to distinguish between interstellar and interplanetary dust components. Our measurements cover the mass intervals similar to 10(-22)-10(-20) kg and similar to 10(-17)- 5 x 10(-16) kg. The flux of the larger dust agrees with measurements of other instruments on different spacecraft.
C1 [Zaslavsky, A.; Meyer-Vernet, N.; Issautier, K.; Le Chat, G.; Pantellini, F.; Maksimovic, M.] Univ Paris 07, LESIA, Univ Paris 06, Observ Paris,CNRS, F-92195 Meudon, France.
[Zaslavsky, A.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zaslavsky, A.; Kasper, J. C.] NASA Lunar Sci Inst, Moffett Field, CA USA.
[Mann, I.] Belgian Inst Space Aeron, Brussels, Belgium.
[Czechowski, A.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland.
[Goetz, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Zaslavsky, A (reprint author), Univ Paris 07, LESIA, Univ Paris 06, Observ Paris,CNRS, 5 Pl Jules Janssen, F-92195 Meudon, France.
EM arnaud.zaslavsky@obspm.fr
RI Bale, Stuart/E-7533-2011; Kasper, Justin/D-1152-2010
OI Bale, Stuart/0000-0002-1989-3596; Kasper, Justin/0000-0002-7077-930X
FU CNES; CNRS; Polish Ministry of Science [NN 203 513 038]; NASA
[NNA09DB30A]
FX We thank the team who designed and built the instrument and are very
grateful to P.L. Astier for many discussions that helped us to
understand the response of the instrument and to evaluate the spacecraft
capacitance. The French part was supported by CNES and CNRS. A.C. was
supported by Polish Ministry of Science grant NN 203 513 038. Several of
the authors were supported by NASA grant NNA09DB30A.
NR 41
TC 34
Z9 34
U1 2
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD MAY 23
PY 2012
VL 117
AR A05102
DI 10.1029/2011JA017480
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 949OV
UT WOS:000304586400002
ER
PT J
AU Tscherbul, TV
AF Tscherbul, T. V.
TI Total-angular-momentum representation for atom-molecule collisions in
electric fields
SO PHYSICAL REVIEW A
LA English
DT Article
ID REACTIVE SCATTERING; DIPOLAR COLLISIONS; POLAR-MOLECULES; COLD
MOLECULES; MAGNETIC-FIELD; ULTRACOLD; ENERGY; TEMPERATURES; CHEMISTRY;
SPIN
AB It is shown that the atom-molecule collision problem in the presence of an external electric field can be solved using the total angular momentum representation in the body-fixed coordinate frame, leading to a computationally efficient method for ab initio modeling of low-temperature scattering phenomena. Our calculations demonstrate rapid convergence of the cross sections for vibrational and Stark relaxation in He-CaD collisions with the number of total angular momentum states in the basis set, leading to a 5- to 100-fold increase in computational efficiency over the previously used methods based on the fully uncoupled space-fixed representation. These results open up the possibility of carrying out numerically converged quantum scattering calculations on a wide array of atom-molecule collisions and chemical reactions in the presence of electric fields.
C1 [Tscherbul, T. V.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
[Tscherbul, T. V.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
RP Tscherbul, TV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
EM tshcherb@cfa.harvard.edu
RI Tscherbul, Timur/K-3286-2014
OI Tscherbul, Timur/0000-0001-5689-040X
FU NSF; Institute for Theoretical Atomic, Molecular, and Optical Physics at
Harvard University; Smithsonian Astrophysical Observatory
FX The author is grateful to Rosario Gonzalez-Ferez and Roman Krems for
their interest in this work and stimulating discussions. This work was
supported by NSF grants to the Harvard-MIT Center for Ultracold Atoms
and the Institute for Theoretical Atomic, Molecular, and Optical Physics
at Harvard University and the Smithsonian Astrophysical Observatory.
NR 66
TC 5
Z9 5
U1 0
U2 14
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD MAY 22
PY 2012
VL 85
IS 5
AR 052710
DI 10.1103/PhysRevA.85.052710
PG 8
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 946XG
UT WOS:000304390200014
ER
PT J
AU Steffen, JH
Ragozzine, D
Fabrycky, DC
Carter, JA
Ford, EB
Holman, MJ
Rowe, JF
Welsh, WF
Borucki, WJ
Boss, AP
Ciardi, DR
Quinn, SN
AF Steffen, Jason H.
Ragozzine, Darin
Fabrycky, Daniel C.
Carter, Joshua A.
Ford, Eric B.
Holman, Matthew J.
Rowe, Jason F.
Welsh, William F.
Borucki, William J.
Boss, Alan P.
Ciardi, David R.
Quinn, Samuel N.
TI Kepler constraints on planets near hot Jupiters
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE extrasolar planets; planet formation; planetary dynamics
ID EARTH-LIKE PLANETS; 1ST 4 MONTHS; EXTRASOLAR PLANETS; STATISTICAL
PROPERTIES; TIMING VARIATIONS; GIANT PLANETS; LIGHT CURVES; MIGRATION;
SYSTEMS; CANDIDATES
AB We present the results of a search for planetary companions orbiting near hot Jupiter planet candidates (Jupiter-size candidates with orbital periods near 3 d) identified in the Kepler data through its sixth quarter of science operations. Special emphasis is given to companions between the 2: 1 interior and exterior mean-motion resonances. A photometric transit search excludes companions with sizes ranging from roughly two-thirds to five times the size of the Earth, depending upon the noise properties of the target star. A search for dynamically induced deviations from a constant period (transit timing variations) also shows no significant signals. In contrast, comparison studies of warm Jupiters (with slightly larger orbits) and hot Neptune-size candidates do exhibit signatures of additional companions with these same tests. These differences between hot Jupiters and other planetary systems denote a distinctly different formation or dynamical history.
C1 [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Ragozzine, Darin; Carter, Joshua A.; Holman, Matthew J.; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
[Rowe, Jason F.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Boss, Alan P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Steffen, JH (reprint author), Fermilab Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA.
EM jsteffen@fnal.gov
RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine,
Darin/C-4926-2013;
OI Ciardi, David/0000-0002-5741-3047; Fabrycky, Daniel/0000-0003-3750-0183
FU National Aeronautics and Space Administration's (NASA) Science Mission
Directorate; NASA [NNX08AR04G, HF-51272.01-A, HF-51267.01-A]; Space
Telescope Science Institute; Association of Universities for Research in
Astronomy, Inc. [NAS 5-26555]
FX Funding for the Kepler mission is provided by the National Aeronautics
and Space Administration's (NASA) Science Mission Directorate. We thank
the Kepler team for their many years of hard work. J.H.S acknowledges
support from NASA under Grant NNX08AR04G under the Kepler Participating
Scientist Program. D.C.F. and J.A.C. acknowledge support from NASA
through Hubble Fellowship Grants HF-51272.01-A and HF-51267.01-A awarded
by the Space Telescope Science Institute, operated by the Association of
Universities for Research in Astronomy, Inc., under Contract NAS
5-26555.
NR 44
TC 71
Z9 71
U1 0
U2 4
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD MAY 22
PY 2012
VL 109
IS 21
BP 7982
EP 7987
DI 10.1073/pnas.1120970109
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 947QY
UT WOS:000304445800020
PM 22566651
ER
PT J
AU Reddy, S
Driskell, A
Rabosky, DL
Hackett, SJ
Schulenberg, TS
AF Reddy, S.
Driskell, A.
Rabosky, D. L.
Hackett, S. J.
Schulenberg, T. S.
TI Diversification and the adaptive radiation of the vangas of Madagascar
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE passerines; phylogeny; diversification; foraging strategies; adaptive
radiation
ID GEOGRAPHIC RANGE EVOLUTION; PHYLOGENETIC-RELATIONSHIPS;
MAXIMUM-LIKELIHOOD; ENDEMIC RADIATION; SINGLE ORIGIN; SEQUENCE DATA;
MIXED MODELS; INDIAN-OCEAN; PASSERIFORMES; DISPERSAL
AB The vangas of Madagascar exhibit extreme diversity in morphology and ecology. Recent studies have shown that several other Malagasy species also are part of this endemic radiation, even as the monophyly of the clade remains in question. Using DNA sequences from 13 genes and representatives of all 15 vanga genera, we find strong support for the monophyly of the Malagasy vangids and their inclusion in a family along with six aberrant genera of shrike-like corvoids distributed in Asia and Africa. Biogeographic reconstructions of these lineages include both Asia and Africa as possible dispersal routes to Madagascar. To study patterns of speciation through time, we introduce a method that can accommodate phylogenetically non-random patterns of incomplete taxon sampling in diversification studies. We demonstrate that speciation rates in vangas decreased dramatically through time following the colonization of Madagascar. Foraging strategies of these birds show remarkable congruence with phylogenetic relationships, indicating that adaptations to feeding specializations played a role in the diversification of these birds. Vangas fit the model of an 'adaptive radiation' in that they show an explosive burst of speciation soon after colonization, increased diversification into novel niches and extraordinary ecomorphological diversity.
C1 [Reddy, S.] Loyola Univ, Dept Biol, Chicago, IL 60626 USA.
[Driskell, A.] Smithsonian Inst, Lab Analyt Biol, Suitland, MD 20746 USA.
[Rabosky, D. L.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Rabosky, D. L.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA.
[Hackett, S. J.] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA.
[Schulenberg, T. S.] Cornell Lab Ornithol, Ithaca, NY 14850 USA.
RP Reddy, S (reprint author), Loyola Univ, Dept Biol, Chicago, IL 60626 USA.
EM sreddy6@luc.edu
RI Rabosky, Daniel/G-4530-2015
FU Sigma Xi; University of Chicago; American Museum of Natural History;
Field Museum of Natural History; National Science Foundation
[DEB-0962078]
FX We thank Velizar Simeonovski for his extraordinary illustrations of
birds. Fieldwork in Madagascar was authorized by the Direction des Eaux
et Forests and the Commission Tripartite. For samples and logistics, we
acknowledge the Field Museum of Natural History and, in particular,
Steve Goodman. For helpful comments, we are grateful to John Bates,
Cathy Bechtoldt, Nick Block, Josh Engel, Irby Lovette, Peter Makovicky,
Rick Ree, V. V. Robin, Jason Weckstein, Dave Willard and Ben Winger. We
also thank Associate Editor Trevor Price, Per Alstrom, and an anonymous
reviewer for suggesting significant improvements to the paper.
Laboratory work was conducted at the Pritzker Laboratory of Molecular
Systematics at the Field Museum of Natural History and at the Laboratory
of Analytical Biology at the Smithsonian Institution. This research was
supported by grants from Sigma Xi, the University of Chicago (Neirman
Fund), the American Museum of Natural History (Frank M. Chapman Fund),
the Field Museum of Natural History (Reichelderfer Fund) and the
National Science Foundation (DEB-0962078). Data generated in this study
were deposited into GenBank (JQ239173-JQ239370).
NR 67
TC 25
Z9 26
U1 3
U2 59
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
EI 1471-2954
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD MAY 22
PY 2012
VL 279
IS 1735
BP 2062
EP 2071
DI 10.1098/rspb.2011.2380
PG 10
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 925RT
UT WOS:000302779600024
PM 22217720
ER
PT J
AU Reilly, NJ
Kokkin, DL
Zhuang, X
Gupta, V
Nagarajan, R
Fortenberry, RC
Maier, JP
Steimle, TC
Stanton, JF
McCarthy, MC
AF Reilly, N. J.
Kokkin, D. L.
Zhuang, X.
Gupta, V.
Nagarajan, R.
Fortenberry, R. C.
Maier, J. P.
Steimle, T. C.
Stanton, J. F.
McCarthy, M. C.
TI The electronic spectrum of Si-3 I: Triplet D-3h system
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID SMALL SILICON CLUSTERS; 1ST ROW ATOMS; PHOTOELECTRON-SPECTRA; ENERGY
GRADIENTS; CARBON CHAINS; GROUND-STATE; BASIS-SETS; SPECTROSCOPY;
TRANSITION; SIH2
AB We report the measurement of a jet-cooled electronic spectrum of the silicon trimer. Si-3 was produced in a pulsed discharge of silane in argon, and the excitation spectrum examined in the 18 000-20 800 cm(-1) region. A combination of resonant two-color two-photon ionization (R2C2PI) time-of-flight mass spectroscopy, laser-induced fluorescence/dispersed fluorescence, and equation-of-motion coupled-cluster calculations have been used to establish that the observed spectrum is dominated by the 1(3)A ''(1) - (a) over tilde (3)A'(2) transition of the D-3h isomer. The spectrum has an origin transition at 18 600 +/- 4 cm(-1) and a short progression in the symmetric stretch with a frequency of similar to 445 cm(-1), in good agreement with a predicted vertical transition energy of 2.34 eV for excitation to the 1(3)A ''(1) state, which has a calculated symmetric stretching frequency of 480 cm(-1). In addition, a similar to 505 cm(-1) ground state vibrational frequency determined from sequence bands and dispersed fluorescence is in agreement with an earlier zero-electron kinetic energy study of the lowest D-3h state and with theory. A weaker, overlapping band system with a similar to 360 cm(-1) progression, observed in the same mass channel (m/z = 84) by R2C2PI but under different discharge conditions, is thought to be due to transitions from the (more complicated) singlet C-2 upsilon ground state ((1)A(1)) state of Si-3. Evidence of emission to this latter state in the triplet dispersed fluorescence spectra suggests extensive mixing in the excited triplet and singlet manifolds. Prospects for further spectroscopic characterization of the singlet system and direct measurement of the energy separation between the lowest singlet and triplet states are discussed. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4704672]
C1 [Reilly, N. J.; Kokkin, D. L.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Reilly, N. J.; Kokkin, D. L.; McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Zhuang, X.; Steimle, T. C.] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA.
[Gupta, V.; Nagarajan, R.; Maier, J. P.] Univ Basel, Dept Chem, CH-4056 Basel, Switzerland.
[Fortenberry, R. C.] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA.
[Stanton, J. F.] Univ Texas Austin, Dept Chem & Biochem, Austin, TX 78712 USA.
RP Reilly, NJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nreilly@cfa.harvard.edu
OI McCarthy, Michael/0000-0001-9142-0008
FU National Science Foundation (NSF) [CHE-1058063, CHE-1011996]; Swiss
National Science Foundation [200020-124349/1]; Virginia Space Grant
Consortium; Robert A. Welch Foundation of Houston, Texas [F-1283]
FX The work in Cambridge is supported by National Science Foundation (NSF)
Grant No. CHE-1058063. The work in Basel is supported by the Swiss
National Science Foundation (Project No. 200020-124349/1). T.C.S.
acknowledges the NSF (Grant No. CHE-1011996) for funding support. R.C.F.
wishes to thank the Virginia Space Grant Consortium for a graduate
research fellowship, and acknowledges T. Daniel Crawford for advice on
this project. J.F.S. has been supported by the NSF and the Robert A.
Welch Foundation (Grant No. F-1283) of Houston, Texas.
NR 44
TC 7
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U1 1
U2 13
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD MAY 21
PY 2012
VL 136
IS 19
AR 194307
DI 10.1063/1.4704672
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 945VC
UT WOS:000304303500023
PM 22612095
ER
PT J
AU Anderson, GE
Gaensler, BM
Slane, PO
Rea, N
Kaplan, DL
Posselt, B
Levin, L
Johnston, S
Murray, SS
Brogan, CL
Bailes, M
Bates, S
Benjamin, RA
Bhat, NDR
Burgay, M
Burke-Spolaor, S
Chakrabarty, D
D'Amico, N
Drake, JJ
Esposito, P
Grindlay, JE
Hong, J
Israel, GL
Keith, MJ
Kramer, M
Lazio, TJW
Lee, JC
Mauerhan, JC
Milia, S
Possenti, A
Stappers, B
Steeghs, DTH
AF Anderson, Gemma E.
Gaensler, B. M.
Slane, Patrick O.
Rea, Nanda
Kaplan, David L.
Posselt, Bettina
Levin, Lina
Johnston, Simon
Murray, Stephen S.
Brogan, Crystal L.
Bailes, Matthew
Bates, Samuel
Benjamin, Robert A.
Bhat, N. D. Ramesh
Burgay, Marta
Burke-Spolaor, Sarah
Chakrabarty, Deepto
D'Amico, Nichi
Drake, Jeremy J.
Esposito, Paolo
Grindlay, Jonathan E.
Hong, Jaesub
Israel, G. L.
Keith, Michael J.
Kramer, Michael
Lazio, T. Joseph W.
Lee, Julia C.
Mauerhan, Jon C.
Milia, Sabrina
Possenti, Andrea
Stappers, Ben
Steeghs, Danny T. H.
TI MULTI-WAVELENGTH OBSERVATIONS OF THE RADIO MAGNETAR PSR J1622-4950 AND
DISCOVERY OF ITS POSSIBLY ASSOCIATED SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (G333.9+0.0); ISM: supernova remnants; pulsars:
individual (PSR J1622-4950); radio continuum: stars; stars: neutron;
X-rays: stars
ID X-RAY PULSAR; GALACTIC PLANE SURVEY; LARGE-AREA TELESCOPE; PHOTON
IMAGING CAMERA; AXP XTE J1810-197; 1E 1547.0-5408; SOURCE CATALOG;
CROSS-SECTIONS; PROPER MOTIONS; 2009 OUTBURST
AB We present multi-wavelength observations of the radio magnetar PSR J1622-4950 and its environment. Observations of PSR J1622-4950 with Chandra (in 2007 and 2009) and XMM (in 2011) show that the X-ray flux of PSR J1622-4950 has decreased by a factor of similar to 50 over 3.7 years, decaying exponentially with a characteristic time of tau = 360 +/- 11 days. This behavior identifies PSR J1622-4950 as a possible addition to the small class of transient magnetars. The X-ray decay likely indicates that PSR J1622-4950 is recovering from an X-ray outburst that occurred earlier in 2007, before the 2007 Chandra observations. Observations with the Australia Telescope Compact Array show strong radio variability, including a possible radio flaring event at least one and a half years after the 2007 X-ray outburst that may be a direct result of this X-ray event. Radio observations with the Molonglo Observatory Synthesis Telescope reveal that PSR J1622-4950 is 8' southeast of a diffuse radio arc, G333.9+0.0, which appears non-thermal in nature and which could possibly be a previously undiscovered supernova remnant (SNR). If G333.9+0.0 is an SNR then the estimates of its size and age, combined with the close proximity and reasonable implied velocity of PSR J1622-4950, suggest that these two objects could be physically associated.
C1 [Slane, Patrick O.; Drake, Jeremy J.; Grindlay, Jonathan E.; Hong, Jaesub; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rea, Nanda] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Barcelona 08193, Spain.
[Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA.
[Posselt, Bettina] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Levin, Lina; Bailes, Matthew; Bhat, N. D. Ramesh] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Levin, Lina; Johnston, Simon; Burke-Spolaor, Sarah; Keith, Michael J.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Bates, Samuel; Kramer, Michael; Stappers, Ben] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Bates, Samuel] W Virginia Univ, Dept Phys, Morgantown, WV USA.
[Benjamin, Robert A.] Univ Wisconsin, Dept Phys, Whitewater, WI 53190 USA.
[Burgay, Marta; D'Amico, Nichi; Esposito, Paolo; Milia, Sabrina; Possenti, Andrea] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy.
[Burke-Spolaor, Sarah; Lazio, T. Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chakrabarty, Deepto] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Israel, G. L.] INAF Osservatorio Astron Roma, Monteporsio Catone, Italy.
[Kramer, Michael] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Mauerhan, Jon C.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Milia, Sabrina] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy.
[Steeghs, Danny T. H.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Anderson, Gemma E.; Gaensler, B. M.] Univ Sydney, Sch Phys A29, Sydney Inst Astron, Sydney, NSW 2006, Australia.
RP Anderson, GE (reprint author), Univ Sydney, Sch Phys A29, Sydney Inst Astron, Sydney, NSW 2006, Australia.
EM g.anderson@physics.usyd.edu.au
RI Bhat, Ramesh/B-7396-2013; Steeghs, Danny/C-5468-2009; Gaensler,
Bryan/F-8655-2010; Rea, Nanda/I-2853-2015; Lee, Julia/G-2381-2015;
OI Steeghs, Danny/0000-0003-0771-4746; Rea, Nanda/0000-0003-2177-6388; Lee,
Julia/0000-0002-7336-3588; Israel, GianLuca/0000-0001-5480-6438; Burgay,
Marta/0000-0002-8265-4344; Anderson, Gemma/0000-0001-6544-8007; Posselt,
Bettina/0000-0003-2317-9747; Esposito, Paolo/0000-0003-4849-5092;
Gaensler, Bryan/0000-0002-3382-9558
FU Australian Postgraduate Award; Australian Laureate Fellowship; NASA
[NAS8-03060, NAS8-39073, GO9-0155X]; Ramon y Cajal Research Fellowship;
Formosa Program [TW2010005]; Autonomous Region of Sardinia through
program PO Sardegna FSE; STFC; ESA; Australian Research Council; Science
Foundation for Physics within the University of Sydney; Commonwealth of
Australia; NFS; Spitzer Legacy Program; [AYA2009-07391]; [SGR2009-811]
FX We thank the referee for their careful reading of the manuscript and
constructive suggestions. G. E. A acknowledges the support of an
Australian Postgraduate Award. B. M. G. acknowledges the support of an
Australian Laureate Fellowship. P.O.S. acknowledges partial support from
NASA Contract NAS8-03060. N.R. is supported by a Ramon y Cajal Research
Fellowship to CSIC, and grants AYA2009-07391 and SGR2009-811, as well as
the Formosa Program TW2010005. J.J.D was supported by NASA contract
NAS8-39073 to the Chandra X-ray Center (CXC). P. E. acknowledges
financial support from the Autonomous Region of Sardinia through a
research grant under the program PO Sardegna FSE 2007-2013, L. R.
7/2007. D. T. H. S. acknowledges an STFC Advanced Fellowship. Support
for this work was also provided by NASA through Chandra Award Number
GO9-0155X issued by the CXC, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of NASA. This research makes
use of data obtained with the Chandra X-ray Observatory, and software
provided by the CXC in the application packages CIAO. This work is based
on observations obtained with XMM-Newton, an ESA science mission with
instruments and contributions directly funded by ESA Member States and
NASA. MOST is operated with the support of the Australian Research
Council and the Science Foundation for Physics within the University of
Sydney. ATCA and Parkes, part of the Australia Telescope, are funded by
the Commonwealth of Australia for operation as a National Facility
managed by CSIRO. Observing time on the 6.5 m Baade Magellan Telescope,
located at Las Campanas Observatory, was allocated through the
Harvard-Smithsonian Center for Astrophysics. 2MASS is a joint project of
the University of Massachusetts and the IPAC/Caltech, funded by the NASA
and NFS. GLIMPSE survey data are part of the Spitzer Legacy Program. The
Spitzer Space Telescope is operated by the JPL/Caltech under a contract
with NASA. This research has made use of NASA's Astrophysics Data
System.
NR 99
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U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2012
VL 751
IS 1
AR 53
DI 10.1088/0004-637X/751/1/53
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MF
UT WOS:000303814600053
ER
PT J
AU Brown, WR
Geller, MJ
Kenyon, SJ
AF Brown, Warren R.
Geller, Margaret J.
Kenyon, Scott J.
TI MMT HYPERVELOCITY STAR SURVEY. II. FIVE NEW UNBOUND STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M31, Sextans B); Galaxy: center; Galaxy: halo;
Galaxy: kinematics and dynamics; stars: early-type
ID MASSIVE BLACK-HOLE; DIGITAL SKY SURVEY; LARGE-MAGELLANIC-CLOUD; SGR
A-ASTERISK; DARK-MATTER HALO; MILKY-WAY HALO; GALACTIC-CENTER;
WHITE-DWARF; STELLAR ORBITS; BINARY STARS
AB We present the discovery of five new unbound hypervelocity stars (HVSs) in the outer Milky Way halo. Using a conservative estimate of Galactic escape velocity, our targeted spectroscopic survey has now identified 16 unbound HVSs as well as a comparable number of HVSs ejected on bound trajectories. A Galactic center origin for the HVSs is supported by their unbound velocities, the observed number of unbound stars, their stellar nature, their ejection time distribution, and their Galactic latitude and longitude distribution. Other proposed origins for the unbound HVSs, such as runaway ejections from the disk or dwarf galaxy tidal debris, cannot be reconciled with the observations. An intriguing result is the spatial anisotropy of HVSs on the sky, which possibly reflects an anisotropic potential in the central 10-100 pc region of the Galaxy. Further progress requires measurement of the spatial distribution of HVSs over the southern sky. Our survey also identifies seven B supergiants associated with known star-forming galaxies; the absence of B supergiants elsewhere in the survey implies there are no new star-forming galaxies in our survey footprint to a depth of 1-2 Mpc.
C1 [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu
OI Kenyon, Scott/0000-0003-0214-609X
FU Smithsonian Institution
FX We thank M. Alegria, A. Milone, and J. McAfee for their assistance with
observations obtained at the MMT Observatory, a joint facility of the
Smithsonian Institution and the University of Arizona. This project
makes use of data products from the Sloan Digital Sky Survey, which is
managed by the Astrophysical Research Consortium for the Participating
Institutions. This research makes use of NASA's Astrophysics Data System
Bibliographic Services. This work was supported by the Smithsonian
Institution.
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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 MAY 20
PY 2012
VL 751
IS 1
AR 55
DI 10.1088/0004-637X/751/1/55
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MF
UT WOS:000303814600055
ER
PT J
AU Kim, DW
Fabbiano, G
Pipino, A
AF Kim, Dong-Woo
Fabbiano, Giuseppina
Pipino, Antonio
TI X-RAY PROPERTIES OF YOUNG EARLY-TYPE GALAXIES. II. ABUNDANCE RATIO IN
THE HOT INTERSTELLAR MATTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; galaxies: elliptical and lenticular, cD; galaxies:
individual (NGC 720, NGC 3923); galaxies: ISM; X-rays: galaxies
ID INTRACLUSTER MEDIUM ENRICHMENT; GALACTIC CHEMICAL EVOLUTION;
LINE-STRENGTH INDEXES; ELLIPTIC GALAXIES; XMM-NEWTON; CHANDRA
OBSERVATIONS; METAL ABUNDANCES; STELLAR POPULATIONS; GAS;
NUCLEOSYNTHESIS
AB Using Chandra X-ray observations of young, post-merger elliptical galaxies, we present X-ray characteristics of age-related observational results by comparing them with typical old elliptical galaxies in terms of metal abundances in the hot interstellar matter (ISM). While the absolute element abundances may be uncertain because of unknown systematic errors and partly because of the smaller amount of hot gas in young ellipticals, the relative abundance ratios (e. g., the a-element to Fe ratio, and most importantly the Si/Fe ratio) can be relatively well constrained. In two young elliptical galaxies (NGC 720 and NGC3923) we find that the Si to Fe abundance ratio is super-solar (at a 99% significance level), in contrast to typical old elliptical galaxies where the Si to Fe abundance ratio is close to solar. Also, the O/Mg ratio is close to solar in the two young elliptical galaxies, as opposed to the sub-solar O/Mg ratio reported in old elliptical galaxies. Both features appear to be less significant outside the effective radius (roughly 30 '' for the galaxies under study), consistent with the observations that confine to the centermost regions the signatures of recent star formation in elliptical galaxies. Observed differences between young and old elliptical galaxies can be explained by the additional contribution from SNe II ejecta in the former. In young elliptical galaxies, the later star formation associated with recent mergers would have a dual effect, resulting both in galaxy scale winds-and therefore smaller observed amounts of hot ISM-because of the additional SN II heating, and in different metal abundances, because of the additional SN II yields.
C1 [Kim, Dong-Woo; Fabbiano, Giuseppina] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Pipino, Antonio] ETH, CH-8093 Zurich, Switzerland.
RP Kim, DW (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
FU CXC CIAO software; CALDB; Chandra GO [G08-9133X]; XMM-Newton GO
[NNX09AT20G]; NASA [NAS8-39073]
FX The data analysis was supported by the CXC CIAO software and CALDB. We
have used the NASA NED and ADS facilities, and have extracted archival
data from the Chandra archives. This work was supported by the Chandra
GO grant G08-9133X (PI: Kim), XMM-Newton GO grant NNX09AT20G (PI: Kim),
and NASA contract NAS8-39073 (CXC).
NR 52
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2012
VL 751
IS 1
AR 38
DI 10.1088/0004-637X/751/1/38
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MF
UT WOS:000303814600038
ER
PT J
AU Landi, E
Raymond, JC
Miralles, MP
Hara, H
AF Landi, E.
Raymond, J. C.
Miralles, M. P.
Hara, H.
TI POST-CORONAL MASS EJECTION PLASMA OBSERVED BY HINODE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: UV
radiation; Sun: X-rays, gamma rays
ID CME CURRENT SHEETS; MAGNETIC RECONNECTION; DIMMING REGIONS; ATOMIC
DATABASE; EMISSION-LINES; SOLAR; FLARE; OUTFLOWS; TEMPERATURE; SPECTRA
AB In the present work we study the evolution of an active region after the eruption of a coronal mass ejection (CME) using observations from the EIS and XRT instruments on board Hinode. The field of view includes a post-eruption arcade, a current sheet, and a coronal dimming. The goal of this paper is to provide a comprehensive set of measurements for all these aspects of the CME phenomenon made on the same CME event. The main physical properties of the plasma along the line of sight-electron density, thermal structure, plasma composition, size, and, when possible, mass-are measured and monitored with time for the first three hours following the CME event of 2008 April 9. We find that the loop arcade observed by EIS and XRT may not be related to the post-eruption arcade. Post-CME plasma is hotter than the surrounding corona, but its temperature never exceeds 3 MK. Both the electron density and thermal structure do not show significant evolution with time, while we found that the size of the loop arcade in the Hinode plane of the sky decreased with time. The plasma composition is the same in the current sheet, in the loop arcade, and in the ambient plasma, so all these plasmas are likely of coronal origin. No significant plasma flows were detected.
C1 [Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Raymond, J. C.; Miralles, M. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hara, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
RP Landi, E (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RI Landi, Enrico/H-4493-2011
FU NASA [NNX11AB61G]; [NNX10AM17G]; [NNX11AC20G]
FX The work of E. Landi is supported by NNX10AM17G, NNX11AC20G, and other
NASA grants. The work of M.P.M. is supported by several NASA grants. The
work of J.C.R. is supported by NASA grant NNX11AB61G to the Smithsonian
Astrophysical Observatory. Hinode is a Japanese mission built and
launched by JAXA/ISAS, collaborating with NAOJ as a domestic partner,
and NASA (USA), and PPARC (UK) as international partners. We warmly
thank the anonymous referee who helped us improve our original
manuscript considerably.
NR 54
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U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2012
VL 751
IS 1
AR 21
DI 10.1088/0004-637X/751/1/21
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MF
UT WOS:000303814600021
ER
PT J
AU Milisavljevic, D
Fesen, RA
Chevalier, RA
Kirshner, RP
Challis, P
Turatto, M
AF Milisavljevic, Dan
Fesen, Robert A.
Chevalier, Roger A.
Kirshner, Robert P.
Challis, Peter
Turatto, Massimo
TI LATE-TIME OPTICAL EMISSION FROM CORE-COLLAPSE SUPERNOVAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (Cassiopeia A); ISM: supernova remnants;
supernovae: individual (SN 1957D, SN 1970G, SN 1980K, SN 1993J);
supernovae: general
ID HUBBLE-SPACE-TELESCOPE; X-RAY-EMISSION; LATE SPECTRAL EVOLUTION;
CASSIOPEIA-A SUPERNOVA; SMALL-MAGELLANIC-CLOUD; NEAR-INFRARED SPECTRA;
MAJOR DUST FACTORIES; RADIO-EMISSION; SN 1993J; II SUPERNOVAE
AB Ground-based optical spectra and Hubble Space Telescope images of 10 core-collapse supernovae (CCSNe) obtained several years to decades after outburst are analyzed with the aim of understanding the general properties of their late-time emissions. New observations of SN 1957D, 1970G, 1980K, and 1993J are included as part of the study. Blueshifted line emissions in oxygen and/or hydrogen with conspicuous line substructure are a common and long-lasting phenomenon in the late-time spectra. Followed through multiple epochs, changes in the relative strengths and velocity widths of the emission lines are consistent with expectations for emissions produced by interaction between SN ejecta and the progenitor star's circumstellar material. The most distinct trend is an increase in the strength of [OIII]/([O I]+[O II]) with age, and a decline in H alpha/([O I]+[O II]) which is broadly consistent with the view that the reverse shock has passed through the H envelope of the ejecta in many of these objects. We also present a spatially integrated spectrum of the young Galactic supernova remnant Cassiopeia A (Cas A). Similarities observed between the emission line profiles of the approximate to 330 yr old Cas A remnant and decades old CCSNe suggest that observed emission line asymmetry in evolved CCSN spectra may be associated with dust in the ejecta, and that minor peak substructure typically interpreted as "clumps" or "blobs" of ejecta may instead be linked with large-scale rings of SN debris.
C1 [Milisavljevic, Dan; Kirshner, Robert P.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Milisavljevic, Dan; Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA.
[Chevalier, Roger A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Turatto, Massimo] Osserv Astron Padova, I-35122 Padua, Italy.
RP Milisavljevic, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dmilisav@cfa.harvard.edu
OI Turatto, Massimo/0000-0002-9719-3157
FU National Science Foundation (NSF) [AST-0908237, AST-0807727,
AST-0606772, AST-0907903]; PRIN-INAF; ASI-INAF [I/009/10/0]; Canadian
Space Agency
FX We thank the referee for comments and suggestions that improved the
manuscript. We also thank John Thorstensen and MDM staff for help with
telescope operations, particularly with configuring the new acquisition
camera which made some of these observations possible, T. Matheson and
M. Modjaz for making the 2001 spectrum of SN 1993J available, and F.
Bauer for providing a spectrum of SN 1996cr. D.M. and R.A.F. acknowledge
support by NSF through grant AST-0908237. R.A.C. acknowledges support
from NSF grant AST-0807727. M.T. is supported by the PRIN-INAF 2009
"Supernovae Variety and Nucleosynthesis Yields" and by the grant
ASI-INAF I/009/10/0. This work is based in part on observations made
with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble
Legacy Archive, which is a collaboration between the Space Telescope
Science Institute (STScI/NASA), the Space Telescope European
Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data
Centre (CADC/NRC/CSA). Some data presented here were obtained at the MMT
Observatory, a joint facility of the Smithsonian Institution and the
University of Arizona. Supernova research at the Harvard College
Observatory is supported by the National Science Foundation through
grants AST-0606772 and AST-0907903. This research has made use of
SAOImage DS9, developed by Smithsonian Astrophysical Observatory, and
used the facilities of the Canadian Astronomy Data Centre operated by
the National Research Council of Canada with the support of the Canadian
Space Agency.
NR 146
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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 MAY 20
PY 2012
VL 751
IS 1
AR 25
DI 10.1088/0004-637X/751/1/25
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MF
UT WOS:000303814600025
ER
PT J
AU Murphy, NA
Miralles, MP
Pope, CL
Raymond, JC
Winter, HD
Reeves, KK
Seaton, DB
van Ballegooijen, AA
Lin, J
AF Murphy, N. A.
Miralles, M. P.
Pope, C. L.
Raymond, J. C.
Winter, H. D.
Reeves, K. K.
Seaton, D. B.
van Ballegooijen, A. A.
Lin, J.
TI ASYMMETRIC MAGNETIC RECONNECTION IN SOLAR FLARE AND CORONAL MASS
EJECTION CURRENT SHEETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; methods: numerical; Sun: coronal mass ejections
(CMEs); Sun: flares
ID HARD X-RAY; ORDER FINITE-ELEMENTS; FIELD LINE SHRINKAGE; INITIAL
PITCH-ANGLE; CME CURRENT SHEETS; FOOTPOINT EMISSIONS; SUPRA-ARCADE;
MOTIONS; LOOPS; PROMINENCES
AB We present two-dimensional resistive magnetohydrodynamic simulations of line-tied asymmetric magnetic reconnection in the context of solar flare and coronal mass ejection current sheets. The reconnection process is made asymmetric along the inflow direction by allowing the initial upstream magnetic field strengths and densities to differ, and along the outflow direction by placing the initial perturbation near a conducting wall boundary that represents the photosphere. When the upstream magnetic fields are asymmetric, the post-flare loop structure is distorted into a characteristic skewed candle flame shape. The simulations can thus be used to provide constraints on the reconnection asymmetry in post-flare loops. More hard X-ray emission is expected to occur at the footpoint on the weak magnetic field side because energetic particles are more likely to escape the magnetic mirror there than at the strong magnetic field footpoint. The footpoint on the weak magnetic field side is predicted to move more quickly because of the requirement in two dimensions that equal amounts of flux must be reconnected from each upstream region. The X-line drifts away from the conducting wall in all simulations with asymmetric outflow and into the strong magnetic field region during most of the simulations with asymmetric inflow. There is net plasma flow across the X-line for both the inflow and outflow directions. The reconnection exhaust directed away from the obstructing wall is significantly faster than the exhaust directed toward it. The asymmetric inflow condition allows net vorticity in the rising outflow plasmoid which would appear as rolling motions about the flux rope axis.
C1 [Murphy, N. A.; Miralles, M. P.; Pope, C. L.; Raymond, J. C.; Winter, H. D.; Reeves, K. K.; van Ballegooijen, A. A.; Lin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pope, C. L.] Elmhurst Coll, Elmhurst, IL USA.
[Seaton, D. B.] SIDC Royal Observ Belgium, B-1180 Brussels, Belgium.
[Lin, J.] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China.
RP Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Reeves, Katharine/P-9163-2014; LIN, JUN/B-9890-2017;
OI Murphy, Nicholas/0000-0001-6628-8033; SEATON, DANIEL/0000-0002-0494-2025
FU NASA [NNX09AB17G, NNX11AB61G, NNM07AB07C, NNX09AH22G]; NSF-REU at the
Center for Astrophysics [ATM-0851866]; NSF-SHINE [ATM0752257]; Program
973 [2011CB811403]; NSFC [10873030]; CAS [KJCX2-EW-T07, 2010Y2JB16];
Belgian Federal Science Policy Office through ESA-PRODEX [4000103240];
NASA through the NASA Advanced Supercomputing (NAS) Division at Ames
Research Center
FX The authors thank P. A. Cassak, S. E. Guidoni, Y.-K. Ko, D. E. McKenzie,
L. Ni, M. Oka, S. L. Savage, C. Shen, C. R. Sovinec, H. P. Warren, D.
Webb, Y.-H. Yang, and S. Zenitani for useful discussions. This research
is supported by NASA grants NNX09AB17G and NNX11AB61G and NASA contract
NNM07AB07C to the Smithsonian Astrophysical Observatory. M. P. M.
acknowledges support from NASA grant NNX09AH22G. C. L. P. acknowledges
support from the NSF-REU solar physics program at the Center for
Astrophysics, grant number ATM-0851866. K. K. R. is supported under the
NSF-SHINE program, grant number ATM0752257. The work of J.L. was also
supported by the Program 973 grant 2011CB811403, the NSFC grant
10873030, and the CAS grant KJCX2-EW-T07 to the Yunnan Astronomical
Observatory. D. B. S. acknowledges support from the Belgian Federal
Science Policy Office through ESA-PRODEX grant number 4000103240. N.A.M.
acknowledges the hospitality of the Yunnan Astronomical Observatory
during a visit supported by CAS grant 2010Y2JB16. The authors thank
members of the NIMROD team for code development efforts that helped make
this work possible. Resources supporting this work were provided by the
NASA High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center. This article has
benefited greatly from the use of NASA's Astrophysics Data System.
NR 131
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U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2012
VL 751
IS 1
AR 56
DI 10.1088/0004-637X/751/1/56
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MF
UT WOS:000303814600056
ER
PT J
AU Tappe, A
Forbrich, J
Martin, S
Yuan, Y
Lada, CJ
AF Tappe, A.
Forbrich, J.
Martin, S.
Yuan, Y.
Lada, C. J.
TI THE ANATOMY OF THE YOUNG PROTOSTELLAR OUTFLOW HH 211
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Herbig-Haro objects; ISM: individual objects (HH 211); ISM: jets and
outflows; ISM: molecules; shock waves
ID SPITZER-SPACE-TELESCOPE; STAR-FORMING REGIONS; EXTENDED GREEN OBJECTS;
ARRAY CAMERA IRAC; MOLECULAR-HYDROGEN; TW HYA; INFRARED SPECTROGRAPH;
SUBMILLIMETER ARRAY; PROTOPLANETARY DISK; ORGANIC-MOLECULES
AB We present Spitzer Space Telescope 5-36 mu m mapping observations toward the southeastern lobe of the young protostellar outflow HH211. The southeastern terminal shock of the outflow shows a rich mid-infrared spectrum including molecular emission lines from OH, H2O, HCO+, CO2, H-2, and HD. The spectrum also shows a rising infrared continuum toward 5 mu m, which we interpret as unresolved emission lines from highly excited rotational levels of the CO v = 1-0 fundamental band. This interpretation is supported by a strong excess flux observed in the Spitzer/IRAC 4-5 mu m channel 2 image compared to the other IRAC channels. The extremely high critical densities of the CO v = 1-0 ro-vibrational lines and a comparison to H-2 and CO excitation models suggest jet densities larger than 10(6) cm(-3) in the terminal shock. We also observed the southeastern terminal outflow shock with the Submillimeter Array and detected pure rotational emission from CO 2-1, HCO+ 3-2, and HCN 3-2. The rotationally excited CO traces the collimated outflow backbone as well as the terminal shock. HCN traces individual dense knots along the outflow and in the terminal shock, whereas HCO+ solely appears in the terminal shock. The unique combination of our mid-infrared and submillimeter observations with previously published near-infrared observations allow us to study the interaction of one of the youngest known protostellar outflows with its surrounding molecular cloud. Our results help us to understand the nature of some of the so-called green fuzzies (Extended Green Objects), and elucidate the physical conditions that cause high OH excitation and affect the chemical OH/H2O balance in protostellar outflows and young stellar objects. In an appendix to this paper, we summarize our Spitzer follow-up survey of protostellar outflow shocks to find further examples of highly excited OH occurring together with H2O and H-2.
C1 [Tappe, A.; Forbrich, J.; Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Martin, S.] European So Observ, Santiago 19, Chile.
[Yuan, Y.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Tappe, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 72, Cambridge, MA 02138 USA.
EM atappe@cfa.harvard.edu
FU NASA; NASA through JPL [1367911, 1375004]; Smithsonian Institution;
Academia Sinica
FX This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. This
research was supported by NASA through JPL-issued contracts 1367911 and
1375004. The Submillimeter Array is a joint project between the
Smithsonian Astrophysical Observatory and the Academia Sinica Institute
of Astronomy and Astrophysics and is funded by the Smithsonian
Institution and the Academia Sinica. This work is based in part on data
collected at the Subaru Telescope, which is operated by the National
Astronomical Observatory of Japan. We thank Naomi Hirano and Minho Choi
for providing the near-IR H2 images of HH211 and IRAS 4B,
Josh Walawender for the H alpha image, Jochen Eisloffel for the
near-infrared continuum image, and Dirk Froebrich and Alessio Caratti o
Garatti for providing the near-infrared spectra of HH 211. We also thank
Gregory Herczeg for very helpful discussions and sharing an early
preprint of his paper on IRAS 4B.
NR 65
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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 MAY 20
PY 2012
VL 751
IS 1
AR 9
DI 10.1088/0004-637X/751/1/9
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MF
UT WOS:000303814600009
ER
PT J
AU Chen, HR
Rao, R
Wilner, DJ
Liu, SY
AF Chen, Huei-Ru
Rao, Ramprasad
Wilner, David J.
Liu, Sheng-Yuan
TI THE MAGNETIZED ENVIRONMENT OF THE W3(H2O) PROTOSTARS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual objects (W3(H2O)); ISM: magnetic fields; stars:
formation; techniques: polarimetric
ID FORMING MOLECULAR CLOUDS; H2O MASER SOURCE; STAR-FORMATION; PROTOBINARY
SYSTEM; FIELD STRUCTURE; MASSIVE STARS; DARK CLOUDS; W3(OH); DUST;
POLARIZATION
AB We present the first interferometric polarization map of the W3(OH) massive star-forming region observed with the Submillimeter Array (SMA) at 878 mu m with an angular resolution of 1.'' 5 (about 3 x 10(3) AU). Polarization is detected in the W3(H2O) hot core, an extended emission structure in the northwest of W3(H2O), and part of the W3(OH) ultracompact H II region. TheW3(H2O) hot core is known to be associated with a synchrotron jet along the east-west direction. In this core, the inferred magnetic field orientation is well aligned with the synchrotron jet and close to the plane of sky. Using the Chandrasekhar-Fermi method with the observed dispersion in polarization angle, we estimate a plane-of-sky magnetic field strength of 17.0 mG. Combined with watermaser Zeeman measurements, the total magnetic field strength is estimated to be 17.1 mG, comparable to the field strength estimated from the synchrotron model. The magnetic field energy dominates over turbulence in this core. In addition, the depolarization effect is discerned in both SMA and James Clerk Maxwell Telescope measurements. Despite the great difference in angular resolutions and map extents, the polarization percentage shows a similar power-law dependence with the beam averaged column density. We suggest that the column density may be an important factor to consider when interpreting the depolarization effect.
C1 [Chen, Huei-Ru] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan.
[Chen, Huei-Ru] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan.
[Chen, Huei-Ru; Rao, Ramprasad; Liu, Sheng-Yuan] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Chen, HR (reprint author), Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan.
EM hchen@phys.nthu.edu.tw
FU National Science Council of Taiwan [NSC 100-2112-M-007-004-MY2]
FX This research is supported by National Science Council of Taiwan through
grant NSC 100-2112-M-007-004-MY2. Vivien Chen thank Dr. B. Matthews for
the general guideline to convert JCMT SCUPOL flux density.
NR 50
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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 MAY 20
PY 2012
VL 751
IS 1
AR L13
DI 10.1088/2041-8205/751/1/L13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MR
UT WOS:000303815800013
ER
PT J
AU Girart, JM
Patel, N
Vlemmings, WHT
Rao, R
AF Girart, J. M.
Patel, N.
Vlemmings, W. H. T.
Rao, Ramprasad
TI MAPPING THE LINEARLY POLARIZED SPECTRAL LINE EMISSION AROUND THE EVOLVED
STAR IRC+10216
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; polarization; stars: AGB and post-AGB; stars:
individual (IRC+10216, CW Leo); submillimeter: stars
ID MAGNETIC-FIELD DIRECTION; CIRCUMSTELLAR ENVELOPE; MOLECULAR LINES; SIO
MASERS; IMAGING POLARIMETRY; RADIO FREQUENCIES; FORMING REGIONS; GHZ;
MILLIARCSECOND; 21(OH)
AB We present spectro-polarimetric observations of several molecular lines obtained with the Submillimeter Array toward the carbon-rich asymptotic giant branch star IRC+10216. We have detected and mapped the linear polarization of the CO 3-2, SiS 19-18, and CS 7-6 lines. The polarization arises at a distance of similar or equal to 450 AU from the star and is blueshifted with respect to the Stokes I. The SiS 19-18 polarization pattern appears to be consistent with a locally radial magnetic field configuration. However, the CO 3-2 and CS 7-6 line polarization suggests an overall complex magnetic field morphology within the envelope. This work demonstrates the feasibility of using spectro-polarimetric observations to carry out tomographic imaging of the magnetic field in circumstellar envelopes.
C1 [Girart, J. M.] Fac Ciencies, Inst Ciencies Espai, CSIC IEEC, Bellaterra 08193, Catalunya, Spain.
[Patel, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Vlemmings, W. H. T.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden.
[Rao, Ramprasad] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA.
RP Girart, JM (reprint author), Fac Ciencies, Inst Ciencies Espai, CSIC IEEC, Campus UAB,C5p 2, Bellaterra 08193, Catalunya, Spain.
EM girart@ice.cat
RI Girart, Josep/O-1638-2014;
OI Girart, Josep/0000-0002-3829-5591; /0000-0002-2700-9916
FU Spanish MICINN [AYA2008-06189-C03]; Catalan AGAUR [2009SGR1172];
Deutsche Forschungsgemeinschaft (DFG) [VL 61/3-1]
FX We thank all members of the SMA staff who made these observations
possible. J.M.G. is supported by the Spanish MICINN AYA2008-06189-C03
and the Catalan AGAUR 2009SGR1172 grants. W. V. acknowledges support by
the Deutsche Forschungsgemeinschaft (DFG) through the Emmy Noether
Research grant VL 61/3-1.
NR 39
TC 8
Z9 8
U1 0
U2 1
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 MAY 20
PY 2012
VL 751
IS 1
AR L20
DI 10.1088/2041-8205/751/1/L20
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MR
UT WOS:000303815800020
ER
PT J
AU Platais, I
Melo, C
Quinn, SN
Clem, JL
de Mink, SE
Dotter, A
Kozhurina-Platais, V
Latham, DW
Bellini, A
AF Platais, I.
Melo, C.
Quinn, S. N.
Clem, J. L.
de Mink, S. E.
Dotter, A.
Kozhurina-Platais, V.
Latham, D. W.
Bellini, A.
TI THE EFFECTS OF DIFFERENTIAL REDDENING AND STELLAR ROTATION ON THE
APPEARANCE OF MULTIPLE POPULATIONS IN STAR CLUSTERS: THE CASE OF
TRUMPLER 20
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE open clusters and associations: general; open clusters and associations:
individual (Trumpler 20); stars: rotation; techniques: spectroscopic
ID LARGE-MAGELLANIC-CLOUD; RADIAL-VELOCITY MEASUREMENTS; MAIN-SEQUENCE
TURNOFFS; BRANCH STARS; INTERMEDIATE; EVOLUTION; I.; SPECTROGRAPH;
PARAMETERS
AB We present a detailed analysis of the upper main sequence of the similar to 1.3 Gyr old open cluster Trumpler 20. High-accuracy BVI photometry combined with the Very Large Telescope/FLAMES medium-resolution spectroscopy of 954 stars is essential to understanding the unusual appearance of the color-magnitude diagram (CMD), initially suggesting multiple populations in Trumpler 20. We show that differential reddening is a dominant contributor to the apparent splitting/widening of the main-sequence turnoff region. At its extreme, the excess differential reddening reaches Delta(B - V) similar to 0.1 while the adopted minimum reddening for the cluster is E(B - V) = 0.36. A unique sample of measured projected rotational velocities indicates that stellar rotation is high near the main-sequence turnoff, reaching v sin i similar to 180 km s(-1). By dividing the upper main-sequence stars into two equal groups of slow and fast rotators, we find that fast rotators have a marginal blueshift of delta(V - I) similar to -0.01, corresponding to a difference in the median v sin i of similar to 60 km s(-1) between these subsamples. We conclude that stellar rotation has an insignificant effect on the morphology of the upper main sequence of this intermediate-age open cluster. Trumpler 20 appears to contain a single coeval population of stars but there is evidence that the red clump is extended.
C1 [Platais, I.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Melo, C.] European So Observ, D-85748 Garching, Germany.
[Quinn, S. N.; Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Clem, J. L.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[de Mink, S. E.; Dotter, A.; Kozhurina-Platais, V.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Bellini, A.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
RP Platais, I (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM imants@pha.jhu.edu
RI Melo, Claudio/O-2797-2013;
OI de Mink, Selma/0000-0001-9336-2825; Melo, Claudio/0000-0002-6090-8446
FU NSF [AST 09-08114]
FX We thank Nate Bastian and the anonymous referee for meritorious
suggestions. This work has been supported in part by the NSF Grant AST
09-08114 to JHU (I.P.).
NR 26
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U1 0
U2 1
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 MAY 20
PY 2012
VL 751
IS 1
AR L8
DI 10.1088/2041-8205/751/1/L8
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939MR
UT WOS:000303815800008
ER
PT J
AU Gacesa, M
Zhang, P
Kharchenko, V
AF Gacesa, M.
Zhang, P.
Kharchenko, V.
TI Non-thermal escape of molecular hydrogen from Mars
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID HOT OXYGEN CORONA; ATMOSPHERIC ESCAPE; STOCHASTIC-MODELS; SATELLITE
CORONAS; CROSS-SECTIONS; QUANTUM; SCATTERING; O(P-3)+H-2; EVOLUTION;
COLLISIONS
AB We present a detailed theoretical analysis of non-thermal escape of molecular hydrogen from Mars induced by collisions with hot atomic oxygen from the Martian corona. To accurately describe the energy transfer in O + H-2(v, j) collisions, we performed extensive quantum-mechanical calculations of state-to-state elastic, inelastic, and reactive cross sections. The escape flux of H-2 molecules was evaluated using a simplified 1D column model of the Martian atmosphere with realistic densities of atmospheric gases and hot oxygen production rates for low solar activity conditions. An average intensity of the non-thermal escape flux of H-2 of 1.9 x 10(5) cm(-2)s(-1) was obtained considering energetic O atoms produced in dissociative recombinations of O-2(+) ions. Predicted ro-vibrational distribution of the escaping H-2 was found to contain a significant fraction of higher rotational states. While the non-thermal escape rate was found to be lower than Jeans rate for H-2 molecules, the non-thermal escape rates of HD and D-2 are significantly higher than their respective Jeans rates. The accurate evaluation of the collisional escape flux of H-2 and its isotopes is important for understanding non-thermal escape of molecules from Mars, as well as for the formation of hot H-2 Martian corona. The described molecular ejection mechanism is general and expected to contribute to atmospheric escape of H-2 and other light molecules from planets, satellites, and exoplanetary bodies. Citation: Gacesa, M., P. Zhang, and V. Kharchenko (2012), Non-thermal escape of molecular hydrogen from Mars, Geophys. Res. Lett., 39, L10203, doi: 10.1029/2012GL050904.
C1 [Gacesa, M.; Zhang, P.; Kharchenko, V.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02134 USA.
[Gacesa, M.; Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT USA.
RP Kharchenko, V (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, 60 Garden St,MS 14, Cambridge, MA 02134 USA.
EM vkharchenko@cfa.harvard.edu
RI Gacesa, Marko/F-8027-2011
OI Gacesa, Marko/0000-0001-5145-051X
FU NASA [NNX09AF13G, NNX10AB88G]
FX We are grateful to D. Wang, A. Kuppermann, and J. Brandao for providing
Fortran subroutines for constructing potential energy surfaces, and to
N. Lewkow for reading and suggestions. M. G. and V. K. were supported by
NASA grants NNX09AF13G and NNX10AB88G.
NR 32
TC 5
Z9 5
U1 1
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 19
PY 2012
VL 39
AR L10203
DI 10.1029/2012GL050904
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 945GZ
UT WOS:000304262400001
ER
PT J
AU Hirsch, BT
Stanton, MA
Maldonado, JE
AF Hirsch, Ben T.
Stanton, Margaret A.
Maldonado, Jesus E.
TI Kinship Shapes Affiliative Social Networks but Not Aggression in
Ring-Tailed Coatis
SO PLOS ONE
LA English
DT Article
ID BROWN CAPUCHIN MONKEYS; GROUP SPATIAL POSITION; WHITE-FACED CAPUCHINS;
NASUA-NASUA; KIN SELECTION; CEBUS-APELLA; REPRODUCTIVE SUCCESS;
BEHAVIORAL SYNCHRONY; MICROSATELLITE LOCI; FEEDING COMPETITION
AB Animal groups typically contain individuals with varying degrees of genetic relatedness, and this variation in kinship has a major influence on patterns of aggression and affiliative behaviors. This link between kinship and social behavior underlies socioecological models which have been developed to explain how and why different types of animal societies evolve. We tested if kinship and age-sex class homophily in two groups of ring-tailed coatis (Nasua nasua) predicted the network structure of three different social behaviors: 1) association, 2) grooming, and 3) aggression. Each group was studied during two consecutive years, resulting in four group-years available for analysis (total of 65 individuals). Association patterns were heavily influenced by agonistic interactions which typically occurred during feeding competition. Grooming networks were shaped by mother-offspring bonds, female-female social relationships, and a strong social attraction to adult males. Mother-offspring pairs were more likely to associate and groom each other, but relatedness had no effect on patterns of aggressive behavior. Additionally, kinship had little to no effect on coalitionary support during agonistic interactions. Adult females commonly came to the aid of juveniles during fights with other group members, but females often supported juveniles who were not their offspring (57% of coalitionary interactions). These patterns did not conform to predictions from socioecological models.
C1 [Hirsch, Ben T.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA.
[Hirsch, Ben T.] Smithsonian Trop Res Inst, Panama City, Panama.
[Hirsch, Ben T.; Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC USA.
[Stanton, Margaret A.] Georgetown Univ, Dept Biol, Washington, DC 20057 USA.
[Maldonado, Jesus E.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Hirsch, BT (reprint author), Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA.
EM hirschb@si.edu
FU NSF doctoral dissertation improvement grant [BCS-0314525]; Smithsonian
Institution postdoctoral fellowship program; Smithsonian Undersecretary
for Science restricted endowment funds; Center for Conservation and
Evolutionary Genetics at Smithsonian Conservation Biology Institute
FX This study was funded by a NSF doctoral dissertation improvement grant
(BCS-0314525), the Smithsonian Institution postdoctoral fellowship
program, the Smithsonian Undersecretary for Science restricted endowment
funds, and the Center for Conservation and Evolutionary Genetics at
Smithsonian Conservation Biology Institute. The funders had no role in
study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 80
TC 13
Z9 13
U1 3
U2 57
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAY 18
PY 2012
VL 7
IS 5
AR e37301
DI 10.1371/journal.pone.0037301
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959VG
UT WOS:000305343500093
PM 22624010
ER
PT J
AU Rasia, E
Meneghetti, M
Martino, R
Borgani, S
Bonafede, A
Dolag, K
Ettori, S
Fabjan, D
Giocoli, C
Mazzotta, P
Merten, J
Radovich, M
Tornatore, L
AF Rasia, E.
Meneghetti, M.
Martino, R.
Borgani, S.
Bonafede, A.
Dolag, K.
Ettori, S.
Fabjan, D.
Giocoli, C.
Mazzotta, P.
Merten, J.
Radovich, M.
Tornatore, L.
TI Lensing and x-ray mass estimates of clusters (simulations)
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
ID DARK-MATTER HALOES; LARGE-SCALE STRUCTURE; LAMBDA-CDM CLUSTERS; ULTRA
DEEP FIELD; GALAXY CLUSTERS; XMM-NEWTON; COMA CLUSTER; COSMOLOGICAL
SIMULATIONS; DYNAMICAL EVOLUTION; SUNYAEV-ZELDOVICH
AB We present a comparison between weak-lensing and x-ray mass estimates of a sample of numerically simulated clusters. The sample consists of the 20 most massive objects at redshift z = 0.25 and M-vir > 5x10(14)M(circle dot) h(-1). They were found in a cosmological simulation of volume 1 h(-3) Gpc(3), evolved in the framework of a WMAP-7 normalized cosmology. Each cluster has been resimulated at higher resolution and with more complex gas physics. We processed it through Skylens and X-MAS to generate optical and x-ray mock observations along three orthogonal projections. The final sample consists of 60 cluster realizations. The optical simulations include lensing effects on background sources. Standard observational tools and methods of analysis are used to recover the mass profiles of each cluster projection from the mock catalogue. The resulting mass profiles from lensing and x-ray are individually compared to the input mass distributions. Given the size of our sample, we could also investigate the dependence of the results on cluster morphology, environment, temperature inhomogeneity and mass. We confirm previous results showing that lensing masses obtained from the fit of the cluster tangential shear profiles with Navarro-Frenk-White functionals are biased low by similar to 5-10% with a large scatter (similar to 10-25%). We show that scatter could be reduced by optimally selecting clusters either having regular morphology or living in substructure-poor environment. The x-ray masses are biased low by a large amount (similar to 25-35%), evidencing the presence of both non-thermal sources of pressure in the intra-cluster medium (ICM) and temperature inhomogeneity, but they show a significantly lower scatter than weak-lensing-derived masses. The x-ray mass bias grows from the inner to the outer regions of the clusters. We find that both biases are weakly correlated with the third-order power ratio, while a stronger correlation exists with the centroid shift. Finally, the x-ray bias is strongly connected with temperature inhomogeneities. Comparison with a previous analysis of simulations leads to the conclusion that the values of x-ray mass bias from simulations are still uncertain, showing dependences on the ICM physical treatment and, possibly, on the hydrodynamical scheme adopted.
C1 [Meneghetti, M.; Ettori, S.; Giocoli, C.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Meneghetti, M.; Ettori, S.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy.
[Martino, R.; Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Borgani, S.; Tornatore, L.] Univ Trieste, Dipartmento Fis, Sez Astron, I-34131 Trieste, Italy.
[Borgani, S.; Tornatore, L.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Borgani, S.; Fabjan, D.; Tornatore, L.] Ist Nazl Fis Nucl, Trieste, Italy.
[Bonafede, A.] Jacobs Univ Bremen, D-28759 Bremen, Germany.
[Dolag, K.] Univ Observ Munchen, D-81679 Munich, Germany.
[Fabjan, D.] Ctr Excellence SPACE SI, Ljubljana 1000, Slovenia.
[Fabjan, D.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia.
[Mazzotta, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Merten, J.] Heidelberg Univ, Zentrum Astron, ITA, D-6900 Heidelberg, Germany.
[Merten, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Merten, J.] CALTECH, Pasadena, CA 91125 USA.
[Radovich, M.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Rasia, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
EM rasia@umich.edu; meneghetti.massimo@oabo.inaf.it
RI Ettori, Stefano/N-5004-2015; Meneghetti, Massimo/O-8139-2015; Mazzotta,
Pasquale/B-1225-2016;
OI Ettori, Stefano/0000-0003-4117-8617; Meneghetti,
Massimo/0000-0003-1225-7084; Mazzotta, Pasquale/0000-0002-5411-1748;
rasia, elena/0000-0003-4175-002X; Radovich, Mario/0000-0002-3585-866X
FU HPC-EUROPA2 [228398]; European Commission; National Science Foundation
[PHY05-51164]; European Union; Ministry of Higher Education, Science and
Technology of Slovenia; Michigan Center for Theoretical Physics;
Michigan Society of Fellows; [ASI-INAF I/023/05/0]; [ASI-INAF
I/088/06/0]; [PRIN-INAF-2009]
FX We acknowledge financial support from contracts ASI-INAF I/023/05/0,
ASI-INAF I/088/06/0, PRIN-INAF-2009 grant 'Towards an Italian Network
for Computational Cosmology' and INFN PD51. This work has been performed
under the HPC-EUROPA2 project (project number 228398) with the support
of the European Commission-Capacities Area-Research Infrastructures. ER
acknowledges the support of the Michigan Society of Fellows. MM, ER, PM,
SB and SE thank the organizers of the workshop 'Galaxy cluster at the
crossroads between astrophysics and cosmology', the KITP for hospitality
and the National Science Foundation for financial support under grant
no. PHY05-51164. SB acknowledges partial support from the European
Commissions FP7 Marie Curie Initial Training Network CosmoComp (PITN-GA-
2009-238356). DF acknowledges support by the European Union and the
Ministry of Higher Education, Science and Technology of Slovenia. This
research was supported in part by the Michigan Center for Theoretical
Physics. Simulations have been carried out at CINECA (Bologna, Italy),
with CPU time allocated through an Italian SuperComputing Resource
Allocation (ISCRA) project.
NR 129
TC 98
Z9 98
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1367-2630
J9 NEW J PHYS
JI New J. Phys.
PD MAY 17
PY 2012
VL 14
AR 055018
DI 10.1088/1367-2630/14/5/055018
PG 36
WC Physics, Multidisciplinary
SC Physics
GA 953NC
UT WOS:000304874200003
ER
PT J
AU Gingerich, O
AF Gingerich, Owen
TI The Day the World Discovered the Sun: An Extraordinary Story of
Scientific Adventure and the Race to Track the Transit of Venus
SO NATURE
LA English
DT Book Review
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ginger@cfa.harvard.edu
NR 1
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 MAY 17
PY 2012
VL 485
IS 7398
BP 305
EP 306
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 943CW
UT WOS:000304099100017
ER
PT J
AU Gingerich, O
AF Gingerich, Owen
TI Chasing Venus: The Race to Measure the Heavens
SO NATURE
LA English
DT Book Review
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ginger@cfa.harvard.edu
NR 1
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 MAY 17
PY 2012
VL 485
IS 7398
BP 305
EP 306
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 943CW
UT WOS:000304099100016
ER
PT J
AU Becker, PA
Miller, PS
Gunther, MS
Somers, MJ
Wildt, DE
Maldonado, JE
AF Becker, Penny A.
Miller, Philip S.
Gunther, Micaela Szykman
Somers, Michael J.
Wildt, David E.
Maldonado, Jesus E.
TI Inbreeding Avoidance Influences the Viability of Reintroduced
Populations of African Wild Dogs (Lycaon pictus)
SO PLOS ONE
LA English
DT Article
ID GENETIC DIVERSITY; NATURAL-POPULATIONS; SOCIAL-ORGANIZATION; KIN
DISCRIMINATION; REPRODUCTIVE SKEW; EXTINCTION; SELECTION; FITNESS;
CONSEQUENCES; RECOGNITION
AB The conservation of many fragmented and small populations of endangered African wild dogs (Lycaon pictus) relies on understanding the natural processes affecting genetic diversity, demographics, and future viability. We used extensive behavioural, life-history, and genetic data from reintroduced African wild dogs in South Africa to (1) test for inbreeding avoidance via mate selection and (2) model the potential consequences of avoidance on population persistence. Results suggested that wild dogs avoided mating with kin. Inbreeding was rare in natal packs, after reproductive vacancies, and between sibling cohorts (observed on 0.8%, 12.5%, and 3.8% of occasions, respectively). Only one of the six (16.7%) breeding pairs confirmed as third-order (or closer) kin consisted of animals that were familiar with each other, while no other paired individuals had any prior association. Computer-simulated populations allowed to experience inbreeding had only a 1.6% probability of extinction within 100 years, whereas all populations avoiding incestuous matings became extinct due to the absence of unrelated mates. Populations that avoided mating with first-order relatives became extinct after 63 years compared with persistence of 37 and 19 years for those also prevented from second-order and third-order matings, respectively. Although stronger inbreeding avoidance maintains significantly more genetic variation, our results demonstrate the potentially severe demographic impacts of reduced numbers of suitable mates on the future viability of small, isolated wild dog populations. The rapid rate of population decline suggests that extinction may occur before inbreeding depression is observed.
C1 [Becker, Penny A.; Maldonado, Jesus E.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
[Becker, Penny A.; Gunther, Micaela Szykman; Wildt, David E.] Smithsonian Inst, Natl Zool Pk, Ctr Species Survival, Smithsonian Conservat Biol Inst, Front Royal, VA USA.
[Becker, Penny A.; Somers, Michael J.] Univ Pretoria, Ctr Wildlife Management, ZA-0002 Pretoria, South Africa.
[Miller, Philip S.] Int Union Conservat Nat, Species Survival Commiss, Conservat Breeding Specialist Grp, Apple Valley, MN USA.
[Gunther, Micaela Szykman] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA.
[Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Somers, Michael J.] Univ Pretoria, Ctr Invas Biol, ZA-0002 Pretoria, South Africa.
RP Becker, PA (reprint author), Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
EM SpieringP@si.edu
RI Somers, Michael/A-1523-2008;
OI Szykman Gunther, Micaela/0000-0002-7822-8094; /0000-0002-5836-8823
FU Smithsonian Institution Undersecretary for Science Endowment Fund;
University of Pretoria; Rotterdam Zoo Thandiza Fund; Humboldt State
University; Conservation Endowment Fund of the Association of Zoos and
Aquariums; Disney Wildlife Conservation Fund; Knowsley Safari Park;
DST-NRF Centre of Excellence for Invasion Biology; Khaki Fever Work
Wear; Pittsburgh Zoo Conservation Fund; Morris Animal Foundation
FX This research was supported by the Smithsonian Institution
Undersecretary for Science Endowment Fund, University of Pretoria,
Rotterdam Zoo Thandiza Fund, Humboldt State University, Conservation
Endowment Fund of the Association of Zoos and Aquariums, Disney Wildlife
Conservation Fund, Knowsley Safari Park, DST-NRF Centre of Excellence
for Invasion Biology, Khaki Fever Work Wear, Pittsburgh Zoo Conservation
Fund, and the Morris Animal Foundation. International travel was
generously provided by British Airways. The funders had no role in study
design, data collection and analysis, decision to publish, or
preparation of the manuscript.; The authors have read the journal's
policy and have the following conflicts: Funding for this study was
provided by the following commercial sources: Disney Wildlife
Conservation Fund, Knowsley Safari Park, Khaki Fever Work Wear, and
Rotterdam Zoo Thandiza Fund. This does not alter the authors' adherence
to all the PLoS ONE policies on sharing data and materials.
NR 64
TC 3
Z9 3
U1 2
U2 57
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD MAY 16
PY 2012
VL 7
IS 5
SI 1
AR e37181
DI 10.1371/journal.pone.0037181
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959UR
UT WOS:000305341300085
PM 22615933
ER
PT J
AU Turner, DD
Mlawer, EJ
Bianchini, G
Cadeddu, MP
Crewell, S
Delamere, JS
Knuteson, RO
Maschwitz, G
Mlynzcak, M
Paine, S
Palchetti, L
Tobin, DC
AF Turner, D. D.
Mlawer, E. J.
Bianchini, G.
Cadeddu, M. P.
Crewell, S.
Delamere, J. S.
Knuteson, R. O.
Maschwitz, G.
Mlynzcak, M.
Paine, S.
Palchetti, L.
Tobin, D. C.
TI Ground-based high spectral resolution observations of the entire
terrestrial spectrum under extremely dry conditions
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID FOURIER-TRANSFORM SPECTROMETER; WATER-VAPOR; RADIANCE; INSTRUMENT
AB A field experiment was conducted in northern Chile at an altitude of 5.3 km to evaluate the accuracy of line-by-line radiative transfer models in regions of the spectrum that are typically opaque at sea level due to strong water vapor absorption. A suite of spectrally resolved radiance instruments collected simultaneous observations that, for the first time ever, spanned the entire terrestrial thermal spectrum (i.e., from 10 to 3000 cm(-1), or 1000 to 3.3 mu m). These radiance observations, together with collocated water vapor and temperature profiles, are used to provide an initial evaluation of the accuracy of water vapor absorption in the far-infrared of two line-by-line radiative transfer models. These initial results suggest that the more recent of the two models is more accurate in the strongly absorbing water vapor pure rotation band. This result supports the validity of the Turner et al. (2012) study that demonstrated that the use of the more recent water vapor absorption model in climate simulations resulted in significant radiative and dynamical changes in the simulation relative to the older water vapor model. Citation: Turner, D. D., et al. (2012), Ground-based high spectral resolution observations of the entire terrestrial spectrum under extremely dry conditions, Geophys. Res. Lett., 39, L10801, doi:10.1029/2012GL051542.
C1 [Turner, D. D.] NOAA, Natl Severe Storms Lab, Norman, OK 73072 USA.
[Mlawer, E. J.; Delamere, J. S.] Atmospher & Environm Res Inc, Lexington, MA USA.
[Bianchini, G.; Palchetti, L.] CNR, Ist Fis Applicata Nello Carrara, Sesto Fiorentino, Italy.
[Cadeddu, M. P.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Crewell, S.; Maschwitz, G.] Univ Cologne, Inst Geophys & Meteorol, Cologne, Germany.
[Knuteson, R. O.; Tobin, D. C.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[Mlynzcak, M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Paine, S.] Smithsonian Astrophys Observ, Cambridge, MA USA.
RP Turner, DD (reprint author), NOAA, Natl Severe Storms Lab, 120 David L Boren Blvd, Norman, OK 73072 USA.
EM dave.turner@noaa.gov
RI Crewell, Susanne/O-1640-2013; PALCHETTI, LUCA/O-1270-2015;
OI Crewell, Susanne/0000-0003-1251-5805; PALCHETTI,
LUCA/0000-0003-4022-8125; Paine, Scott/0000-0003-4622-5857
FU Office of Science, Office of Biological and Environmental Research,
Climate and Environmental Sciences Division; NASA; Italian National
Research Council; Smithsonian Institution; German Science Foundation
(DFG)
FX The RHUBC-II campaign was organized as part of the U. S. Department of
Energy's Atmospheric Radiation Measurement (ARM) program, which is
sponsored by the Office of Science, Office of Biological and
Environmental Research, Climate and Environmental Sciences Division.
RHUBC-II was also supported in part by NASA, the Italian National
Research Council, the Smithsonian Institution, and the German Science
Foundation (DFG). We would like to thank the many scientists and
engineers who helped make the collection of this dataset possible,
including Alex Carrizo and operations staff at AstroNorte, Kim Nitschke,
Jim Mather, Charles Brinkmann, Troy Culgan, Mike Ryzcek, Rich Cageao,
Glenn Farnsworth, Mike Wojcik, Jason Swasey, Joe Lee, Erik Syrstad, Dave
Johnson, Julio Marin, Arlette Chacon, Toufic Hawat, Huabai Li, Marcos
Diaz, Francesco Castagnoli, Denny Hackel, Ray Garcia, Hank Revercomb,
Rich Coulter, and Tim Wagner. Additional information on the RHUBC-II
experiment can be found at http://acrf-campaign.arm.gov/rhubc/. RHUBC-II
data are available from the ARM data archive as an IOP dataset at
http://www.archive.arm.gov.
NR 20
TC 15
Z9 15
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAY 16
PY 2012
VL 39
AR L10801
DI 10.1029/2012GL051542
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 945GQ
UT WOS:000304261500003
ER
PT J
AU MacPherson, GJ
Kita, NT
Ushikubo, T
Bullock, ES
Davis, AM
AF MacPherson, G. J.
Kita, N. T.
Ushikubo, T.
Bullock, E. S.
Davis, A. M.
TI Well-resolved variations in the formation ages for Ca-Al-rich inclusions
in the early Solar System
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Al-26; calcium-aluminum-rich inclusions; chronology; early Solar System
ID PROTOPLANETARY DISK; REFRACTORY INCLUSIONS; AL-26; AL-26/AL-27; MG;
CONSTRAINTS; CHONDRULES; DIFFUSION; MAGNESIUM; NEBULA
AB Recent whole-rock magnesium-isotopic data for calcium-aluminum-rich inclusions (CAIs) in chondrite meteorites indicate that the primary nebular fractionation of aluminum from magnesium, probably by condensation, occurred within <20,000 years at 4.567 Ga. However, high-precision multicollector ion microprobe data for diverse CAIs from Vigarano (CV3) yield internal isochrons with a clearly resolved spread in initial Al-26/Al-27, meaning that CAIs formed and were reprocessed over a much longer time span. Primitive (unmelted) CAIs have a consistent value of 52 +/- 0.1 x 10(-5), melted CAIs range from 5.17 x 10(-5) to 4.24 x 10(-5), and one single object with a complex multistage history has an internal range of Al-26/Al-27 = (4.77 - 2.77) x 10(-5). The entire range corresponds to an age span of similar to 0.7 Ma. Thus not all CAIs formed at "time zero", and only the most primitive CAIs should be used as benchmarks for earliest Solar System chronology. Published by Elsevier B.V.
C1 [MacPherson, G. J.; Bullock, E. S.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Kita, N. T.; Ushikubo, T.] Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA.
[Davis, A. M.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Davis, A. M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
RP MacPherson, GJ (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM macphers@si.edu
RI Kita, Noriko/H-8035-2016;
OI Kita, Noriko/0000-0002-0204-0765; Davis, Andrew/0000-0001-7955-6236
FU NASA [NNX07AJ05G, NNX09AG39G, NNX09AB88G]; NSF [EAR03-19230,
EAR07-44079]
FX We are grateful to F. Richter for numerous discussions, and to two
anonymous reviewers whose detailed and constructive reviews greatly
improved the manuscript. This research was supported by NASA grants
NNX07AJ05G (G.J.M., PI), NNX09AG39G (A.M.D., PI), and NNX09AB88G (NK,
PI). WiscSIMS is partly supported by NSF (EAR03-19230, EAR07-44079).
NR 25
TC 51
Z9 52
U1 0
U2 9
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD MAY 15
PY 2012
VL 331
BP 43
EP 54
DI 10.1016/j.epsl.2012.03.010
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 969BK
UT WOS:000306030500005
ER
PT J
AU Bayona, G
Cardona, A
Jaramillo, C
Mora, A
Montes, C
Valencia, V
Ayala, C
Montenegro, O
Ibanez-Mejia, M
AF Bayona, German
Cardona, Agustin
Jaramillo, Carlos
Mora, Andres
Montes, Camilo
Valencia, Victor
Ayala, Carolina
Montenegro, Omar
Ibanez-Mejia, Mauricio
TI Early Paleogene magmatism in the northern Andes: Insights on the effects
of Oceanic Plateau-continent convergence
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Paleogene; magmatism; northern Andes; subduction; intraplate magmatism
ID MIDDLE MAGDALENA VALLEY; U-PB AGES; LLANOS FORELAND BASIN; AMERICAN
LAND-BRIDGE; EASTERN CORDILLERA; TECTONIC EVOLUTION; CARIBBEAN PLATE;
SOUTH-AMERICA; ZIRCON GEOCHRONOLOGY; TERRANE ACCRETION
AB Recognition of magmatic events in polyphase arc-continent collision margin is critical for proper tectonic reconstructions that trace the short and changing nature of the configuration of the continental margin. Additionally, the recognition of the origin of detrital volcanic zircons within continental basins becomes a challenge if only distant oceanic and continental magmatic arcs are considered as the only possible source. In this study we report U/Pb zircon ages in isolated plutons that support an early Paleogene magmatic arc that extended ca 700 km along the northern Andean continental margin. Additional detrital zircon Paleogene ages (45-65 Ma), from Paleocene-lower Eocene continental sandstones and volcaniclastic rocks in 19 localities from Colombian and Venezuela Andean basins, indicate that volcanic detritus were supplied from a magmatic arc striking parallel to the subduction zone and also show the existence of intraplate magmatism extending more than 400 km inland.
The wide distribution of this Early Paleogene magmatism along the northern South America margin is related to subduction of the buoyant Caribbean plate; the relative short period of magmatism (<10 myr) and sudden stop in early middle Eocene time may be related to the difficulty of the thick plateau to subduct and the relative strike-slip movement of the South America and Caribbean plates since middle Eocene due to northward migration of those plates. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Bayona, German; Cardona, Agustin; Jaramillo, Carlos; Montes, Camilo; Ayala, Carolina; Montenegro, Omar] Corp Geol ARES, Bogota, Colombia.
[Cardona, Agustin] Univ Nacl Colombia, Medellin, Colombia.
[Jaramillo, Carlos] Smithsonian Trop Res Inst, Ciudad De Panama, Panama.
[Mora, Andres] Inst Colombiano Petr, Bucaramanga, Colombia.
[Montes, Camilo] Univ Los Andes, Bogota, Colombia.
[Valencia, Victor] Washington State Univ, Sch Earth & Enviromental Sci, Pullman, WA 99164 USA.
[Ibanez-Mejia, Mauricio] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
RP Bayona, G (reprint author), Corp Geol ARES, Calle 44A N 53-96, Bogota, Colombia.
EM gbayona@cgares.org
OI Ibanez-Mejia, Mauricio/0000-0002-7839-2425; Montes,
Camilo/0000-0002-3553-0787
FU Corporacion Geologica ARES; Colciencias; Ecopetrol S.A-ICP (project
"Cronologia de la deformacion de cuencas subandinas"); Hocol S.A.
FX This research was funded by Corporacion Geologica ARES, Colciencias,
Ecopetrol S.A-ICP (project "Cronologia de la deformacion de cuencas
subandinas"), Hocol S.A. and Maurel & Prom. Andres Mesa (Hocol S.A.)
provided the location of Paleocene sandstones in localities 7 and 9.
Comments of Mauricio Parra and two anonymous reviewers improved the
content of this manuscript.
NR 95
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U1 0
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD MAY 15
PY 2012
VL 331
BP 97
EP 111
DI 10.1016/j.epsl.2012.03.015
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 969BK
UT WOS:000306030500009
ER
PT J
AU Burgess, EA
Lanyon, JM
Brown, JL
Blyde, D
Keeley, T
AF Burgess, Elizabeth A.
Lanyon, Janet M.
Brown, Janine L.
Blyde, David
Keeley, Tamara
TI Diagnosing pregnancy in free-ranging dugongs using fecal progesterone
metabolite concentrations and body morphometrics: A population
application
SO GENERAL AND COMPARATIVE ENDOCRINOLOGY
LA English
DT Article
DE Dugong dugon; Fecal hormones; Progesterone; Pregnancy; Body
morphometrics; Free-ranging; Ultrasonography
ID MONITORING OVARIAN-FUNCTION; MANATEE TRICHECHUS-MANATUS; STEROID
METABOLITES; REPRODUCTIVE STATUS; ENZYME-IMMUNOASSAY; LIFE-HISTORY;
QUEENSLAND; HORMONES; CYCLE; VALIDATION
AB Assessing reproductive status and monitoring reproductive rates is important in the effective management of vulnerable marine mammal species such as the dugong (Dugong dugon). Knowledge of the reproductive physiology of this species is limited, and determining reproductive parameters (e.g., sexual maturation, pregnancy, and reproductive senescence) has been restricted by a lack of non-lethal methods for assessing reproductive status in free-ranging individuals. The aim of this study was to develop a method to identify pregnant individuals in a wild dugong population. Using an enzymeimmunoassay, we quantified concentrations of fecal progesterone metabolites (fP) in 322 dugongs, including confirmed pregnant females (n = 10), presumed non-pregnant adult females (n = 25), juvenile females (n = 24), sub-adult females (n = 41), adult females of unknown pregnancy state (n = 63), and males of all sizes (n = 159). External body morphometrics of each dugong were measured, and confirmation of pregnancy in adult female dugongs was determined by ultrasonography or observation of subsequent neonates. Concentrations of fP were different between sexes and reproductive size classes (P < 0.001), and similar to 30-fold higher in confirmed pregnant dugongs (2017-7760 ng/g) compared to presumed non-pregnant females (30-221 ng/g), juvenile females (29-195 ng/g), and males (24-261 ng/g) (P < 0.001). Body measures of maximum and anal girths, and teat length were all greater in confirmed pregnant females than presumed non-pregnant females (all P < 0.05). We evaluated a Discriminant Function Analysis (DFA) to provide a model for predicting pregnant and non-pregnant dugongs. Cross-validated results showed that the DFA correctly classified 100% of pregnant and non-pregnant females using fP concentrations, body length, fineness ratio (an index of body shape), and teat length (a female reproductive trait). Using the DFA model, we classified the pregnancy status of all female dugongs and identified a total of 30 females as pregnant and 133 females as non-pregnant from the sampled population over the sample period. Pregnant dugongs in the Moreton Bay population are characterized by fecal progesterone metabolite concentrations > 1000 ng/g, body length >= 260 cm, maximum girth >= 215 cm, anal girth >= 126 cm, and teat length 5 >= cm long. In summary, analysis of fP concentrations in combination with body morphometrics may be used to diagnose pregnancy in free-ranging dugongs, and provides a new tool to monitor breeding rates of wild sirenian populations. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Burgess, Elizabeth A.; Lanyon, Janet M.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia.
[Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA.
[Blyde, David] Sea World Australia, Surfers Paradise, Qld 4217, Australia.
[Keeley, Tamara] Taronga Western Plains Zoo, Dubbo, NSW 2830, Australia.
RP Burgess, EA (reprint author), Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia.
EM e.burgess1@uq.edu.au; j.lanyon@uq.edu.au; brownjan@si.edu;
David.Blyde@wvtp.com.au; Tkeeley@zoo.nsw.gov.au
FU Winifred Violet Scott Foundation; Unimin Ltd (formerly Consolidated
Rutile Ltd); Sydney Aquarium Conservation Fund; M.A. Ingram Fund Trust;
AWARE Foundation; Australian Geographic Society; Australian Marine
Mammal Centre; Australian Postgraduate Award; Queensland-Smithsonian
FX Many thanks to the dedication of everyone in The University of
Queensland (UQ) Dugong Research Team, in particular Helen Sneath, Erin
Neal, Rob Slade, Paul Sprecher, Ben Schemel, Merrick Ekins, Giovanni
Damiani, Nick Holmes, John and Tyler Gilbert, Dave Fields, and Jan
Chambers. Trevor Long and the Sea World Research and Rescue Foundation
provided generous in-kind support for the dugong health assessment
program. We are very grateful to Wendy Blanshard for her support with
ultrasonography, and other Sea World staff including Nick Anson and
Johnno Wordsworth, as well as Andrew Barnes from Sydney Aquarium. Bob
Bonde and Cathy Beck (USGS) assisted with blood collection in 2008.
Thanks also to Jennifer Seddon (UQ Veterinary Science) for assisting
with genetic identification of dugongs, and also to Nicole Presley for
her help with HPLC analysis. This research was supported financially by
the Winifred Violet Scott Foundation, Unimin Ltd. (formerly Consolidated
Rutile Ltd), Sydney Aquarium Conservation Fund, M.A. Ingram Fund Trust,
Project AWARE Foundation, Australian Geographic Society, and Australian
Marine Mammal Centre. E. A. Burgess was the recipient of an Australian
Postgraduate Award and awarded a Queensland-Smithsonian Fellowship to
further this study. Two anonymous reviewers provided helpful comments on
the manuscript. Dugongs were sampled under The University of Queensland
Animal Ethics #ZOO/ENT/344/04/NSF/CRL, #SIB/215/ 08/ACAMMS,
#ZOO/ENT/737/08/ARC/CRL/SW/AMMC, Moreton Bay Marine Parks permit
#Q52004/CVL228 to #QS2008/CVL228 and Scientific Purposes permits
#WISP01660304 to WISPO49 37308.
NR 60
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U1 3
U2 30
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0016-6480
J9 GEN COMP ENDOCR
JI Gen. Comp. Endocrinol.
PD MAY 15
PY 2012
VL 177
IS 1
BP 82
EP 92
DI 10.1016/j.ygcen.2012.02.008
PG 11
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA 948OC
UT WOS:000304511500011
PM 22387986
ER
PT J
AU Riley, S
AF Riley, Sheila
TI Don't Mess with Travis
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Riley, Sheila] Smithsonian Inst Libs, Washington, DC 20560 USA.
RP Riley, S (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 MAY 15
PY 2012
VL 137
IS 9
BP 75
EP 75
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 944CW
UT WOS:000304177000061
ER
PT J
AU Gardner-Vandy, KG
Lauretta, DS
Greenwood, RC
McCoy, TJ
Killgore, M
Franchi, IA
AF Gardner-Vandy, Kathryn G.
Lauretta, Dante S.
Greenwood, Richard C.
McCoy, Timothy J.
Killgore, Marvin
Franchi, Ian A.
TI The Tafassasset primitive achondrite: Insights into initial stages of
planetary differentiation
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID CARBONACEOUS CHONDRITE GROUP; OXYGEN ISOTOPES; SYSTEM; METAL;
THERMODYNAMICS; CLASSIFICATION; ACAPULCOITES; BRACHINITES; INDICATORS;
LODRANITES
AB Tafassasset is an exceptional meteorite that has been linked to both the CR chondrites and the primitive achondrites. Because previous evidence suggests it might be a primitive achondrite from a known chondrite type, we have undertaken a study of the petrology, geochemistry, and formation history of the meteorite. Tafassasset is predominantly FeO-rich olivine (similar to 58%) yet contains abundant Fe, Ni-metal (similar to 10 vol.%) and sulfide (similar to 3 vol.%). Other phases include high-and low-Ca pyroxene, plagioclase, chromite, and phosphate. It has a recrystallized texture, containing equigranular grains that often meet at 120 degrees triple junctions. There are no relict chondrules in the thin sections examined, although they have been reported previously. Electron microprobe analyses reveal homogeneous olivine (Fa(28.6)), both low-and high-Ca pyroxene (Fs(23.6)Wo(3.7) and Fs(12.2)Wo(39.3+/-1)), a range of plagioclase composition (An(23-47)), Fe, Ni-metal (with 5.3-36.6 wt.% Ni and 0.1-0.8 wt.% Co), troilite, chromite, and Ca-phosphate. Bulk composition analyses reveal two chips depleted in refractory lithophile and some siderophile elements compared to CI chondrites. Exceptions are enrichments in Fe, Ni and Co. A third chip is essentially chondritic in bulk composition. Different stones of the meteorite have slightly different oxygen isotope composition, yet all lie in the CR chondrite trend with one in the acapulcoite-lodranite field. Thermodynamic calculations show that Tafassasset equilibrated at a temperature above the Fe, Ni-FeS eutectic and at an oxygen fugacity of similar to IW-1. The texture, heterogeneous distribution of mineral phases, plagioclase composition, two-mineral closure temperatures, and bulk composition all provide evidence that Tafassasset partially melted on its parent body. A comparison with the CR chondrites, the brachinites, and two anomalous achondrites indicates that Tafassasset is most similar to ungrouped primitive achondrites Lewis Cliff (LEW) 88763 and Divnoe, and to the brachinites in overall petrography, modal mineralogy, mineral compositions, oxidation state, and bulk composition. The comparison also excludes the possibility that Tafassasset formed by partial melting of a CR chondrite. Tafassasset is a primitive achondrite and likely evolved on a parent body that experienced incomplete melting, never reached isotopic homogeneity, and was from the same oxygen isotopic reservoir as the CR chondrite parent body. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Gardner-Vandy, Kathryn G.; Lauretta, Dante S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Greenwood, Richard C.; Franchi, Ian A.] Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England.
[McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Killgore, Marvin] SW Meteorite Lab, Payson, AZ 85547 USA.
RP Gardner-Vandy, KG (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA.
EM kgardner@lpl.arizona.edu
FU NASA [NNX09AQ88H, NNX10AH50G]; University of Arizona/Alfred P. Sloan
Foundation
FX We thank Ken Domanik for help with EMPA and use of the IQmaterials (TM)
program, Yulia Goreva for help with ICP-MS technique, Mark Ghiorso for
supplying the supplemental MELTS calculator, and both Harold C.
Connolly, Jr. and Devin Schrader for many useful discussions about CR
chondrites. We also think the Southwest Meteorite Laboratory and the
Museum National d'Histoire Naturelle in Paris, France for donating large
chips of Tafassasset and loaning us many thin sections for analysis.
This work was funded by NASA Grants NNX09AQ88H and NNX10AH50G to D. S.
L. and the University of Arizona/Alfred P. Sloan Foundation Indigenous
Graduate Partnership Fellowship to K.G.G.V.
NR 50
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U1 1
U2 16
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD MAY 15
PY 2012
VL 85
BP 142
EP 159
DI 10.1016/j.gca.2012.01.014
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 930AH
UT WOS:000303107200008
ER
PT J
AU Diefendorf, AF
Freeman, KH
Wing, SL
AF Diefendorf, Aaron F.
Freeman, Katherine H.
Wing, Scott L.
TI Distribution and carbon isotope patterns of diterpenoids and
triterpenoids in modern temperate C-3 trees and their geochemical
significance
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID POLYCYCLIC AROMATIC-HYDROCARBONS; EARLY DIAGENESIS; ORGANIC
GEOCHEMISTRY; LIPID BIOSYNTHESIS; THERMAL MAXIMUM; FRACTIONATION;
PLANTS; EOCENE; TERPENOIDS; BIOMARKER
AB Tricyclic diterpenoids and pentacyclic triterpenoids are nearly exclusively produced by gymnosperms and angiosperms, respectively. Even though both classes of terpenoids have long been recognized as plant biomarkers, their potential use as phylogenetically specific delta C-13 proxies remains largely unexplored. Little is known of how terpenoid abundance and carbon isotope composition vary either with plant phylogenetic position, functional group, or during synthesis. Here, we report terpenoid abundances and isotopic data for 44 tree species in 21 families, representing both angiosperms and gymnosperms, and both deciduous and evergreen leaf habits. Di- and triterpenoid abundances are significantly higher in evergreens compared to deciduous species, reflecting differences in growth strategies and increased chemical investment in longer-lived leaves. Carbon isotope abundances of terpenoid lipids are similar to leaf tissues, indicating biosynthetic isotope effects are small for both the MVA (-0.4 parts per thousand) and MEP (-0.6 parts per thousand) pathways. Leaf and molecular isotopic patterns for modern plants are consistent with observations of amber, resins and plant biomarkers in ancient sediments. The delta C-13 values of ancient diterpenoids are higher than triterpenoids by 2-5 parts per thousand, consistent with observed isotopic differences between gymnosperms and angiosperms leaves, and support the relatively small lipid biosynthetic effects reported here. All other factors being equal, evergreen plants will dominate the abundance of terpenoids contributed to soils, sediments and ancient archives, with similar inputs estimated for angiosperm and gymnosperm trees when scaled by litter flux. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Diefendorf, Aaron F.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA.
[Freeman, Katherine H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Wing, Scott L.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA.
RP Diefendorf, AF (reprint author), Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA.
EM aaron.diefendorf@uc.edu
OI Wing, Scott/0000-0002-2954-8905
FU National Science Foundation [EAR-0844212]; Penn State Biogeochemical
Research Initiative for Education (BRIE); National Science Foundation
IGERT [DGE-9972759]
FX We thank Laurie Eccles for laboratory preparation, Kevin Mueller and
Heather Graham for sample collection and laboratory assistance, Emily
Diefendorf for sample collection assistance, and Denny Walizer for
instrumentation support. We thank Roger Summons, Katherine French, Ken
Sawada and an anonymous reviewer for helpful and insightful revisions to
the manuscript. This research was supported by the National Science
Foundation Grant EAR-0844212 (to K. H. F.) and fellowship awards from
the Penn State Biogeochemical Research Initiative for Education (BRIE)
funded by the National Science Foundation IGERT Grant DGE-9972759.
NR 71
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U2 39
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD MAY 15
PY 2012
VL 85
BP 342
EP 356
DI 10.1016/j.gca.2012.02.016
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 930AH
UT WOS:000303107200021
ER
PT J
AU McLaughlin, BM
Ballance, CP
AF McLaughlin, B. M.
Ballance, C. P.
TI Photoionization cross sections for the trans-iron element Se+ from 18 to
31 eV
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
ID GIANT BRANCH STARS; ELECTRON-IMPACT EXCITATION; S-PROCESS ABUNDANCES;
R-MATRIX CALCULATION; PLANETARY-NEBULAE; ATOMIC DATA; RESONANCES;
SCATTERING; EVOLUTION; PROGRAM
AB Absolute photoionization cross-section calculations are presented for Se+ using large-scale close-coupling calculations within the Breit-Pauli and Dirac-Coulomb R-matrix approximations. The results from our theoretical work are compared with recent measurements (Esteves 2010 PhD Thesis publication number AAI3404727, University of Reno, NV, USA; Sterling et al 2011 J. Phys. B: At. Mol. Opt. Phys. 44 025701; Esteves et al 2011 Phys. Rev. A 84 013406) made at the advanced light source (ALS) radiation facility in Berkeley, CA, USA. We report on results for the photon energy range 18.0-31.0 eV, which spans the ionization thresholds of the S-4(3/2)o ground state and the low-lying D-2(5/2,3/2)o and P-2(3/2,1/2)o metastable states. Metastable fractions are inferred from our present work. Resonance energies and quantum defects of the prominent Rydberg resonances series identified in the spectra are compared for the 4p -> nd transitions with the recent ALS experimental measurements made on this complex trans-iron element.
C1 [McLaughlin, B. M.] Queens Univ Belfast, Ctr Theoret Atom Mol & Opt Phys, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
[Ballance, C. P.] Auburn Univ, Dept Phys, Allison Lab 206, Auburn, AL 36849 USA.
RP McLaughlin, BM (reprint author), Queens Univ Belfast, Ctr Theoret Atom Mol & Opt Phys, Sch Math & Phys, David Bates Bldg,7 Coll Pk, Belfast BT7 1NN, Antrim, North Ireland.
EM b.mclaughlin@qub.ac.uk; ballance@physics.auburn.edu
FU US Department of Energy (DoE) through Auburn University; US National
Science Foundation
FX CPB was supported by US Department of Energy (DoE) grants through Auburn
University. BMM acknowledges support by the US National Science
Foundation through a grant to ITAMP at the Harvard-Smithsonian Center
for Astrophysics. We thank David A Esteves for providing us with the ALS
experimental data and a copy of his thesis. The computational work was
carried out at the National Energy Research Scientific Computing Center
in Oakland, CA, USA, and on the Tera-grid at the National Institute for
Computational Sciences (NICS) in Knoxville, TN, USA.
NR 44
TC 21
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U1 0
U2 4
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 MAY 14
PY 2012
VL 45
IS 9
AR 095202
DI 10.1088/0953-4075/45/9/095202
PG 13
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 934CB
UT WOS:000303417000006
ER
PT J
AU Russell, CT
Raymond, CA
Coradini, A
McSween, HY
Zuber, MT
Nathues, A
De Sanctis, MC
Jaumann, R
Konopliv, AS
Preusker, F
Asmar, SW
Park, RS
Gaskell, R
Keller, HU
Mottola, S
Roatsch, T
Scully, JEC
Smith, DE
Tricarico, P
Toplis, MJ
Christensen, UR
Feldman, WC
Lawrence, DJ
McCoy, TJ
Prettyman, TH
Reedy, RC
Sykes, ME
Titus, TN
AF Russell, C. T.
Raymond, C. A.
Coradini, A.
McSween, H. Y.
Zuber, M. T.
Nathues, A.
De Sanctis, M. C.
Jaumann, R.
Konopliv, A. S.
Preusker, F.
Asmar, S. W.
Park, R. S.
Gaskell, R.
Keller, H. U.
Mottola, S.
Roatsch, T.
Scully, J. E. C.
Smith, D. E.
Tricarico, P.
Toplis, M. J.
Christensen, U. R.
Feldman, W. C.
Lawrence, D. J.
McCoy, T. J.
Prettyman, T. H.
Reedy, R. C.
Sykes, M. E.
Titus, T. N.
TI Dawn at Vesta: Testing the Protoplanetary Paradigm
SO SCIENCE
LA English
DT Article
ID PARENT BODY; EVOLUTION; DIFFERENTIATION; DIOGENITES; EUCRITE; ORIGIN;
CORE; SIZE
AB The Dawn spacecraft targeted 4 Vesta, believed to be a remnant intact protoplanet from the earliest epoch of solar system formation, based on analyses of howardite-eucrite-diogenite (HED) meteorites that indicate a differentiated parent body. Dawn observations reveal a giant basin at Vesta's south pole, whose excavation was sufficient to produce Vesta-family asteroids (Vestoids) and HED meteorites. The spatially resolved mineralogy of the surface reflects the composition of the HED meteorites, confirming the formation of Vesta's crust by melting of a chondritic parent body. Vesta's mass, volume, and gravitational field are consistent with a core having an average radius of 107 to 113 kilometers, indicating sufficient internal melting to segregate iron. Dawn's results confirm predictions that Vesta differentiated and support its identification as the parent body of the HEDs.
C1 [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Raymond, C. A.; Konopliv, A. S.; Asmar, S. W.; Park, R. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Coradini, A.; De Sanctis, M. C.] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, Rome, Italy.
[McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Zuber, M. T.; Smith, D. E.] MIT, Cambridge, MA 02139 USA.
[Nathues, A.; Keller, H. U.; Christensen, U. R.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Jaumann, R.; Preusker, F.; Mottola, S.; Roatsch, T.] DLR, Inst Planetary Res, Berlin, Germany.
[Scully, J. E. C.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Gaskell, R.; Tricarico, P.; Feldman, W. C.; Prettyman, T. H.; Reedy, R. C.; Sykes, M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Toplis, M. J.] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France.
[Lawrence, D. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[McCoy, T. J.] Smithsonian Inst, Washington, DC 20560 USA.
[Titus, T. N.] US Geol Survey, Flagstaff, AZ 86001 USA.
RP Russell, CT (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
EM ctrussell@igpp.ucla.edu
RI Russell, Christopher/E-7745-2012; De Sanctis, Maria
Cristina/G-5232-2013; Lawrence, David/E-7463-2015;
OI Russell, Christopher/0000-0003-1639-8298; De Sanctis, Maria
Cristina/0000-0002-3463-4437; Lawrence, David/0000-0002-7696-6667;
Reedy, Robert/0000-0002-2189-1303; Prettyman, Thomas/0000-0003-0072-2831
FU NASA; [NNM05AA86C]
FX We thank the Dawn team for the development, cruise, orbital insertion,
and operations of the Dawn spacecraft at Vesta. C. T. R. is supported by
the Discovery Program through contract NNM05AA86C to the University of
California, Los Angeles. A portion of this work was performed at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA. Dawn data are archived with the NASA Planetary Data
System.
NR 27
TC 205
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U1 2
U2 42
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 MAY 11
PY 2012
VL 336
IS 6082
BP 684
EP 686
DI 10.1126/science.1219381
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 940EH
UT WOS:000303872300039
PM 22582253
ER
PT J
AU Reddy, V
Nathues, A
Le Corre, L
Sierks, H
Li, JY
Gaskell, R
McCoy, T
Beck, AW
Schroder, SE
Pieters, CM
Becker, KJ
Buratti, BJ
Denevi, B
Blewett, DT
Christensen, U
Gaffey, MJ
Gutierrez-Marques, P
Hicks, M
Keller, HU
Maue, T
Mottola, S
McFadden, LA
McSween, HY
Mittlefehldt, D
O'Brien, DP
Raymond, C
Russell, C
AF Reddy, Vishnu
Nathues, Andreas
Le Corre, Lucille
Sierks, Holger
Li, Jian-Yang
Gaskell, Robert
McCoy, Timothy
Beck, Andrew W.
Schroeder, Stefan E.
Pieters, Carle M.
Becker, Kris J.
Buratti, Bonnie J.
Denevi, Brett
Blewett, David T.
Christensen, Ulrich
Gaffey, Michael J.
Gutierrez-Marques, Pablo
Hicks, Michael
Keller, Horst Uwe
Maue, Thorsten
Mottola, Stefano
McFadden, Lucy A.
McSween, Harry Y.
Mittlefehldt, David
O'Brien, David P.
Raymond, Carol
Russell, Christopher
TI Color and Albedo Heterogeneity of Vesta from Dawn
SO SCIENCE
LA English
DT Article
ID PARENT BODY; METEORITES; EUCRITE; EARTH; SIZE
AB Multispectral images (0.44 to 0.98 mm) of asteroid (4) Vesta obtained by the Dawn Framing Cameras reveal global color variations that uncover and help understand the north-south hemispherical dichotomy. The signature of deep lithologies excavated during the formation of the Rheasilvia basin on the south pole has been preserved on the surface. Color variations (band depth, spectral slope, and eucrite-diogenite abundance) clearly correlate with distinct compositional units. Vesta displays the greatest variation of geometric albedo (0.10 to 0.67) of any asteroid yet observed. Four distinct color units are recognized that chronicle processes-including impact excavation, mass wasting, and space weathering-that shaped the asteroid's surface. Vesta's color and photometric diversity are indicative of its status as a preserved, differentiated protoplanet.
C1 [Reddy, Vishnu; Nathues, Andreas; Le Corre, Lucille; Sierks, Holger; Schroeder, Stefan E.; Christensen, Ulrich; Gutierrez-Marques, Pablo; Maue, Thorsten] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Reddy, Vishnu; Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
[Li, Jian-Yang] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Gaskell, Robert; O'Brien, David P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[McCoy, Timothy; Beck, Andrew W.] Smithsonian Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Becker, Kris J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Buratti, Bonnie J.; Hicks, Michael; Raymond, Carol] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Denevi, Brett; Blewett, David T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Keller, Horst Uwe] TU Braunschweig, Inst Geophys & Extraterr Phys, DE-38106 Braunschweig, Germany.
[Mottola, Stefano] Deutsch Zentrum Luft & Raumfahrt DLR, German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany.
[McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Mittlefehldt, David] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA.
[Russell, Christopher] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
RP Reddy, V (reprint author), Max Planck Inst Solar Syst Res, Max Planck Str 2, D-37191 Katlenburg Lindau, Germany.
EM reddy@mps.mpg.de
RI Blewett, David/I-4904-2012; Denevi, Brett/I-6502-2012; Russell,
Christopher/E-7745-2012; Schroder, Stefan/D-9709-2013; McFadden,
Lucy-Ann/I-4902-2013; Beck, Andrew/J-7215-2015;
OI Blewett, David/0000-0002-9241-6358; Denevi, Brett/0000-0001-7837-6663;
Russell, Christopher/0000-0003-1639-8298; Schroder,
Stefan/0000-0003-0323-8324; McFadden, Lucy-Ann/0000-0002-0537-9975;
Beck, Andrew/0000-0003-4455-2299; Reddy, Vishnu/0000-0002-7743-3491; Le
Corre, Lucille/0000-0003-0349-7932
FU Max Planck Society; German Space Agency, DLR; Dawn at Vesta; NASA
FX We thank the Dawn team for the development, cruise, orbital insertion,
and operations of the Dawn spacecraft at Vesta. The Framing Camera
project is financially supported by the Max Planck Society and the
German Space Agency, DLR. We also thank the Dawn at Vesta Participating
Scientist Program for funding the research. A portion of this work was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. Dawn data are archived with the
NASA Planetary Data System.
NR 14
TC 115
Z9 115
U1 1
U2 13
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 MAY 11
PY 2012
VL 336
IS 6082
BP 700
EP 704
DI 10.1126/science.1219088
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 940EH
UT WOS:000303872300044
PM 22582258
ER
PT J
AU Page, MJ
Symeonidis, M
Vieira, JD
Altieri, B
Amblard, A
Arumugam, V
Aussel, H
Babbedge, T
Blain, A
Bock, J
Boselli, A
Buat, V
Castro-Rodriguez, N
Cava, A
Chanial, P
Clements, DL
Conley, A
Conversi, L
Cooray, A
Dowell, CD
Dubois, EN
Dunlop, JS
Dwek, E
Dye, S
Eales, S
Elbaz, D
Farrah, D
Fox, M
Franceschini, A
Gear, W
Glenn, J
Griffin, M
Halpern, M
Hatziminaoglou, E
Ibar, E
Isaak, K
Ivison, RJ
Lagache, G
Levenson, L
Lu, N
Madden, S
Maffei, B
Mainetti, G
Marchetti, L
Nguyen, HT
O'Halloran, B
Oliver, SJ
Omont, A
Panuzzo, P
Papageorgiou, A
Pearson, CP
Perez-Fournon, I
Pohlen, M
Rawlings, JI
Rigopoulou, D
Riguccini, L
Rizzo, D
Rodighiero, G
Roseboom, IG
Rowan-Robinson, M
Portal, MS
Schulz, B
Scott, D
Seymour, N
Shupe, DL
Smith, AJ
Stevens, JA
Trichas, M
Tugwell, KE
Vaccari, M
Valtchanov, I
Viero, M
Vigroux, L
Wang, L
Ward, R
Wright, G
Xu, CK
Zemcov, M
AF Page, M. J.
Symeonidis, M.
Vieira, J. D.
Altieri, B.
Amblard, A.
Arumugam, V.
Aussel, H.
Babbedge, T.
Blain, A.
Bock, J.
Boselli, A.
Buat, V.
Castro-Rodriguez, N.
Cava, A.
Chanial, P.
Clements, D. L.
Conley, A.
Conversi, L.
Cooray, A.
Dowell, C. D.
Dubois, E. N.
Dunlop, J. S.
Dwek, E.
Dye, S.
Eales, S.
Elbaz, D.
Farrah, D.
Fox, M.
Franceschini, A.
Gear, W.
Glenn, J.
Griffin, M.
Halpern, M.
Hatziminaoglou, E.
Ibar, E.
Isaak, K.
Ivison, R. J.
Lagache, G.
Levenson, L.
Lu, N.
Madden, S.
Maffei, B.
Mainetti, G.
Marchetti, L.
Nguyen, H. T.
O'Halloran, B.
Oliver, S. J.
Omont, A.
Panuzzo, P.
Papageorgiou, A.
Pearson, C. P.
Perez-Fournon, I.
Pohlen, M.
Rawlings, J. I.
Rigopoulou, D.
Riguccini, L.
Rizzo, D.
Rodighiero, G.
Roseboom, I. G.
Rowan-Robinson, M.
Sanchez Portal, M.
Schulz, B.
Scott, D.
Seymour, N.
Shupe, D. L.
Smith, A. J.
Stevens, J. A.
Trichas, M.
Tugwell, K. E.
Vaccari, M.
Valtchanov, I.
Viero, M.
Vigroux, L.
Wang, L.
Ward, R.
Wright, G.
Xu, C. K.
Zemcov, M.
TI The suppression of star formation by powerful active galactic nuclei
SO NATURE
LA English
DT Article
ID BLACK-HOLES; GALAXY FORMATION; AGN; OUTFLOWS; FEEDBACK; CATALOGS;
QUASARS; FIELDS; GROWTH; MODEL
AB The old, red stars that constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly as a result of accretion onto black holes. It is widely suspected, but unproved, that the tight correlation between the mass of the black hole and the mass of the stellar bulge(1) results from the AGN quenching the surrounding star formation as it approaches its peak luminosity(2-4). X-rays trace emission from AGN unambiguously(5), whereas powerful star-forming galaxies are usually dust-obscured and are brightest at infrared and submillimetre wavelengths(6). Here we report submillimetre and X-ray observations that show that rapid star formation was common in the host galaxies of AGN when the Universe was 2-6 billion years old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 10(44) ergs per second. This suppression of star formation in the host galaxy of a powerful AGN is a key prediction of models in which the AGN drives an outflow(7-9), expelling the interstellar medium of its host and transforming the galaxy's properties in a brief period of cosmic time.
C1 [Page, M. J.; Symeonidis, M.; Rawlings, J. I.; Seymour, N.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Altieri, B.; Conversi, L.; Sanchez Portal, M.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain.
[Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Arumugam, V.; Dunlop, J. S.; Ivison, R. J.; Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Aussel, H.; Chanial, P.; Elbaz, D.; Madden, S.; Panuzzo, P.; Riguccini, L.] Univ Paris Diderot, CE Saclay, CEA DSM IRFU, CNRS,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Babbedge, T.; Clements, D. L.; Fox, M.; O'Halloran, B.; Rizzo, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Blain, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Boselli, A.; Buat, V.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Castro-Rodriguez, N.; Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain.
[Castro-Rodriguez, N.; Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Dubois, E. N.; Farrah, D.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.; Ward, R.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Eales, S.; Gear, W.; Griffin, M.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Franceschini, A.; Mainetti, G.; Marchetti, L.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA.
[Halpern, M.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Ibar, E.; Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Isaak, K.] European Space Res & Technol Ctr ESTEC, NL-2201 AZ Noordwijk, Netherlands.
[Lagache, G.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France.
[Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, JPL, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Omont, A.; Vigroux, L.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[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.
[Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Page, MJ (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England.
EM mjp@mssl.ucl.ac.uk
RI amblard, alexandre/L-7694-2014; Ivison, R./G-4450-2011; Vaccari,
Mattia/R-3431-2016; Cava, Antonio/C-5274-2017;
OI amblard, alexandre/0000-0002-2212-5395; Ivison, R./0000-0001-5118-1313;
Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275;
Scott, Douglas/0000-0002-6878-9840; Marchetti,
Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536; Dye,
Simon/0000-0002-1318-8343; Rodighiero, Giulia/0000-0002-9415-2296;
Altieri, Bruno/0000-0003-3936-0284
FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France);
ASI (Italy); MCINN(Spain); SNSB(Sweden); STFC (UK); UKSA (UK); NASA
(USA)
FX Herschel is an ESA space observatory with science instruments provided
by European-led Principal Investigator consortia and with important
participation from NASA. SPIRE has been developed by a consortium of
institutes led by Cardiff University (UK) and which includes: University
of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI,
University of Padua (Italy); IAC (Spain); Stockholm Observatory
(Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of
Sussex (UK); and Caltech, JPL, NHSC, 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, UKSA (UK); and NASA (USA).
NR 29
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U1 0
U2 7
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD MAY 10
PY 2012
VL 485
IS 7397
BP 213
EP 216
DI 10.1038/nature11096
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 939HJ
UT WOS:000303799800035
PM 22575961
ER
PT J
AU Gezari, S
Chornock, R
Rest, A
Huber, ME
Forster, K
Berger, E
Challis, PJ
Neill, JD
Martin, DC
Heckman, T
Lawrence, A
Norman, C
Narayan, G
Foley, RJ
Marion, GH
Scolnic, D
Chomiuk, L
Soderberg, A
Smith, K
Kirshner, RP
Riess, AG
Smartt, SJ
Stubbs, CW
Tonry, JL
Wood-Vasey, WM
Burgett, WS
Chambers, KC
Grav, T
Heasley, JN
Kaiser, N
Kudritzki, RP
Magnier, EA
Morgan, JS
Price, PA
AF Gezari, S.
Chornock, R.
Rest, A.
Huber, M. E.
Forster, K.
Berger, E.
Challis, P. J.
Neill, J. D.
Martin, D. C.
Heckman, T.
Lawrence, A.
Norman, C.
Narayan, G.
Foley, R. J.
Marion, G. H.
Scolnic, D.
Chomiuk, L.
Soderberg, A.
Smith, K.
Kirshner, R. P.
Riess, A. G.
Smartt, S. J.
Stubbs, C. W.
Tonry, J. L.
Wood-Vasey, W. M.
Burgett, W. S.
Chambers, K. C.
Grav, T.
Heasley, J. N.
Kaiser, N.
Kudritzki, R. -P.
Magnier, E. A.
Morgan, J. S.
Price, P. A.
TI An ultraviolet-optical flare from the tidal disruption of a helium-rich
stellar core
SO NATURE
LA English
DT Article
ID MASSIVE BLACK-HOLE; STAR; LUMINOSITY; EVOLUTION; OUTBURST; GALAXIES
AB The flare of radiation from the tidal disruption and accretion of a star can be used as a marker for supermassive black holes that otherwise lie dormant and undetected in the centres of distant galaxies(1). Previous candidate flares(2-6) have had declining light curves in good agreement with expectations, but with poor constraints on the time of disruption and the type of star disrupted, because the rising emission was not observed. Recently, two 'relativistic' candidate tidal disruption events were discovered, each of whose extreme X-ray luminosity and synchrotron radio emission were interpreted as the onset of emission from a relativistic jet(7-10). Here we report a luminous ultraviolet-optical flare from the nuclear region of an inactive galaxy at a redshift of 0.1696. The observed continuum is cooler than expected for a simple accreting debris disk, but the well-sampled rise and decay of the light curve follow the predicted mass accretion rate and can be modelled to determine the time of disruption to an accuracy of two days. The black hole has a mass of about two million solar masses, modulo a factor dependent on the mass and radius of the star disrupted. On the basis of the spectroscopic signature of ionized helium from the unbound debris, we determine that the disrupted star was a helium-rich stellar core.
C1 [Gezari, S.; Heckman, T.; Norman, C.; Scolnic, D.; Riess, A. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Chornock, R.; Berger, E.; Challis, P. J.; Narayan, G.; Foley, R. J.; Marion, G. H.; Chomiuk, L.; Soderberg, A.; Kirshner, R. P.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Huber, M. E.; Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Heasley, J. N.; Kaiser, N.; Kudritzki, R. -P.; Magnier, E. A.; Morgan, J. S.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Forster, K.; Neill, J. D.; Martin, D. C.] CALTECH, Pasadena, CA 91125 USA.
[Lawrence, A.] Univ Edinburgh, Royal Observ, Scottish Univ Phys Alliance, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Smith, K.; Smartt, S. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh Particle Phys Astrophys & Cosmol Ctr, Pittsburgh, PA 15260 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Gezari, S (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
EM suvi@pha.jhu.edu
RI Stubbs, Christopher/C-2829-2012;
OI Stubbs, Christopher/0000-0003-0347-1724; Narayan,
Gautham/0000-0001-6022-0484; Chambers, Kenneth /0000-0001-6965-7789
FU NASA; National Science Foundation; UK Science and Technology Facilities
Council; Space Telescope Science Institute; Planetary Science Division
of the NASA Science Mission Directorate
FX We thank H. Tananbaum for approving our Chandra Director's Discretionary
Time request. We are grateful to G. Lodato for providing the tidal
disruption event models in tabular form, and to S. Moran for running
software to calculate the host-galaxy K-corrections. We thank R. E.
Williams for discussions on the line emission in the spectra. S. G. was
supported by NASA through a Hubble Fellowship grant awarded by the Space
Telescope Science Institute, which is operated by AURA Inc. for NASA.
Partial support for this work was provided by the National Science
Foundation. The PS1 survey has been made possible through contributions
of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS
Project Office, the Max-Planck Society and its participating institutes,
The Johns Hopkins University, Durham University, the University of
Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center
for Astrophysics, the Las Cumbres Observatory Global Telescope Network
Inc. and the National Central University of Taiwan, and by NASA under a
grant issued through the Planetary Science Division of the NASA Science
Mission Directorate. We acknowledge NASA's support for construction,
operation, and science analysis of the GALEX mission, which was
developed in cooperation with Centre National d'Etudes Spatiales of
France and the Korean Ministry of Science and Technology. Some of the
observations reported here were obtained at the MMT Observatory, which
is a joint facility of the Smithsonian Institution and the University of
Arizona, and at the Liverpool Telescope, which is operated with
financial support from the UK Science and Technology Facilities Council.
The computations in this paper were run on the Odyssey cluster supported
by the FAS Science Division Research Computing Group at Harvard
University. R.J.F. is a Clay Fellow.
NR 29
TC 130
Z9 130
U1 0
U2 7
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD MAY 10
PY 2012
VL 485
IS 7397
BP 217
EP 220
DI 10.1038/nature10990
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 939HJ
UT WOS:000303799800036
PM 22575962
ER
PT J
AU Aliu, E
Archambault, S
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bottcher, M
Bouvier, A
Bradbury, SM
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Ciupik, L
Collins-Hughes, E
Connolly, MP
Coppi, P
Cui, W
Decerprit, G
Dickherber, R
Dumm, J
Errando, M
Falcone, A
Feng, Q
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Godambe, S
Griffin, S
Grube, J
Gyuk, G
Hanna, D
Hawkins, K
Holder, J
Huan, H
Hughes, G
Humensky, TB
Kaaret, P
Karlsson, N
Kertzman, M
Khassen, Y
Kieda, D
Krawczynski, H
Krennrich, F
Lang, MJ
Lee, K
Madhavan, AS
Maier, G
Majumdar, P
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Ong, RA
Orr, M
Otte, AN
Palma, N
Park, N
Perkins, JS
Pichel, A
Pohl, M
Prokoph, H
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Ruppel, J
Saxon, DB
Schroedter, M
Sembroski, GH
Senturk, GD
Smith, AW
Staszak, D
Telezhinsky, I
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Varlotta, A
Vivier, M
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Williams, DA
Zitzer, B
Fortin, P
Horan, D
AF Aliu, E.
Archambault, S.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Boettcher, M.
Bouvier, A.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cannon, A.
Cesarini, A.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Coppi, P.
Cui, W.
Decerprit, G.
Dickherber, R.
Dumm, J.
Errando, M.
Falcone, A.
Feng, Q.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Godambe, S.
Griffin, S.
Grube, J.
Gyuk, G.
Hanna, D.
Hawkins, K.
Holder, J.
Huan, H.
Hughes, G.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
Lee, K.
Madhavan, A. S.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Ong, R. A.
Orr, M.
Otte, A. N.
Palma, N.
Park, N.
Perkins, J. S.
Pichel, A.
Pohl, M.
Prokoph, H.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Ruppel, J.
Saxon, D. B.
Schroedter, M.
Sembroski, G. H.
Sentuerk, G. D.
Smith, A. W.
Staszak, D.
Telezhinsky, I.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Varlotta, A.
Vivier, M.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Weisgarber, T.
Williams, D. A.
Zitzer, B.
Fortin, P.
Horan, D.
TI DISCOVERY OF HIGH-ENERGY AND VERY HIGH ENERGY gamma-RAY EMISSION FROM
THE BLAZAR RBS 0413
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (RBS 0413-VER J0319+187); gamma rays:
galaxies
ID BL-LACERTAE OBJECTS; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; ACTIVE
GALACTIC NUCLEI; LARGE-AREA TELESCOPE; LAC OBJECTS; BRIGHT BLAZARS;
RADIATION; MODEL; CATALOG; MISSION
AB We report on the discovery of high-energy (HE; E > 0.1 GeV) and very high energy (VHE; E > 100 GeV) gamma-ray emission from the high-frequency-peaked BL Lac object RBS 0413. VERITAS, a ground-based gamma-ray observatory, detected VHE. rays from RBS 0413 with a statistical significance of 5.5 standard deviations (sigma) and a gamma-ray flux of (1.5 +/- 0.6(stat) +/- 0.7(syst)) x 10(-8) photons m(-2) s(-1) (similar to 1% of the Crab Nebula flux) above 250 GeV. The observed spectrum can be described by a power law with a photon index of 3.18 +/- 0.68(stat) +/- 0.30(syst). Contemporaneous observations with the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope detected HE gamma rays from RBS 0413 with a (stat)istical significance of more than 9 sigma, a power-law photon index of 1.57 +/- 0.12(stat-0.12sys')(+0.11) and a gamma-ray flux between 300 MeV and 300 GeV of (1.64 +/- 0.43(stat-0.22sys)(+ 0.31)) x 10(-5) photons m(-2) s(-1). We present the results from Fermi-LAT and VERITAS, including a spectral energy distribution modeling of the gamma-ray, quasi-simultaneous X-ray (Swift-XRT), ultraviolet (Swift-UVOT), and R-band optical (MDM) data. We find that, if conditions close to equipartition are required, both the combined synchrotron self-Compton/external-Compton and the lepto-hadronic models are preferred over a pure synchrotron self-Compton model.
C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA.
[Archambault, S.; Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Arlen, T.; Majumdar, P.; Ong, R. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Boettcher, M.; Hawkins, K.; Palma, N.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Byrum, K.; Decerprit, G.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Collins-Hughes, E.; Khassen, Y.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Connolly, M. P.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Coppi, P.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Dumm, J.; Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Finnegan, G.; Godambe, S.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Huan, H.; Park, N.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Telezhinsky, I.] DESY, D-15738 Zeuthen, Germany.
[Humensky, T. B.; Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Perkins, J. S.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
[Perkins, J. S.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Fortin, P.; Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France.
RP Aliu, E (reprint author), Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA.
EM gunessenturk@gmail.com; fortin@llr.in2p3.fr; deirdre@llr.in2p3.fr
RI Khassen, Yerbol/I-3806-2015;
OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772;
Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794
FU US Department of Energy Office of Science; US National Science
Foundation; Smithsonian Institution; NASA; NSERC in Canada; Science
Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK
FX The VERITAS research is supported by grants from the US Department of
Energy Office of Science, the US National Science Foundation, the
Smithsonian Institution, and the NASA Swift Guest Investigator Program,
by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748),
and by STFC in the UK. We acknowledge the excellent work of the
technical support staff at the FLWO and at the collaborating
institutions in the construction and operation of the instrument.
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JI Astrophys. J.
PD MAY 10
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SC Astronomy & Astrophysics
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UT WOS:000303446500008
ER
PT J
AU Allen, TS
Gutermuth, RA
Kryukova, E
Megeath, ST
Pipher, JL
Naylor, T
Jeffries, RD
Wolk, SJ
Spitzbart, B
Muzerolle, J
AF Allen, Thomas S.
Gutermuth, Robert A.
Kryukova, Erin
Megeath, S. Thomas
Pipher, Judith L.
Naylor, Tim
Jeffries, R. D.
Wolk, Scott J.
Spitzbart, Brad
Muzerolle, James
TI SPITZER IMAGING OF THE NEARBY RICH YOUNG CLUSTER, Cep OB3b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; stars: formation; stars: pre-main sequence
ID ORION-NEBULA-CLUSTER; INFRARED ARRAY CAMERA; STAR-FORMING REGIONS;
SPACE-TELESCOPE; PROTOPLANETARY DISKS; CEPHEUS-B; ABSOLUTE CALIBRATION;
STELLAR CLUSTERS; MOLECULAR CLOUDS; MASS STARS
AB We map the full extent of a rich massive young cluster in the Cep OB3b association with the Infrared Array Camera and Multi-band Imaging Photometer System instruments aboard the Spitzer Space Telescope and the ACIS instrument aboard the Chandra X-Ray Observatory. At 700 pc, it is revealed to be the second nearest large (>1000 member), young (<5Myr) cluster known. In contrast to the nearest large cluster, the Orion Nebula Cluster, Cep OB3b is only lightly obscured and is mostly located in a large cavity carved out of the surrounding molecular cloud. Our infrared and X-ray data sets, as well as visible photometry from the literature, are used to take a census of the young stars in Cep OB3b. We find that the young stars within the cluster are concentrated in two sub-clusters; an eastern sub-cluster, near the Cep B molecular clump, and a western sub-cluster, near the Cep F molecular clump. Using our census of young stars, we examine the fraction of young stars with infrared excesses indicative of circumstellar disks. We create a map of the disk fraction throughout the cluster and find that it is spatially variable. Due to these spatial variations, the two sub-clusters exhibit substantially different average disk fractions from each other: 32%+/- 4% and 50%+/- 6%. We discuss whether the discrepant disk fractions are due to the photodestruction of disks by the high mass members of the cluster or whether they result from differences in the ages of the sub-clusters. We conclude that the discrepant disk fractions are most likely due to differences in the ages.
C1 [Allen, Thomas S.; Kryukova, Erin; Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Gutermuth, Robert A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Pipher, Judith L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Naylor, Tim] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Jeffries, R. D.] Univ Keele, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Wolk, Scott J.; Spitzbart, Brad] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Muzerolle, James] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Allen, TS (reprint author), Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
RI Naylor, Tim /A-9465-2015;
OI Wolk, Scott/0000-0002-0826-9261
FU National Aeronautics and Space Administration (NASA) [1407, GO9-0017A,
NAS8-03060, 1276271]; NASA through JPL/Caltech; National Science
Foundation [AST-1009564]; University of Massachusetts; JPL [SAO/JPL
SV4-74011]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under NASA contract 1407. Support
for this work was provided by NASA through an award issued by
JPL/Caltech. Support for this work was provided by the National
Aeronautics and Space Administration through the Chandra Award Number
GO9-0017A 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. S.T.M. and E.K. acknowledge support by NASA award 1281302.
J.L.P. acknowledges support from the NASA award 1276271. S.J.W. and
B.D.S. were supported by NASA contract NAS8-03060 to the Chandra Science
Center. Additional support for this work was provided by the National
Science Foundation award AST-1009564. 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 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 and JPL support from SAO/JPL
SV4-74011.
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JI Astrophys. J.
PD MAY 10
PY 2012
VL 750
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AR 125
DI 10.1088/0004-637X/750/2/125
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500039
ER
PT J
AU Chomiuk, L
Soderberg, AM
Moe, M
Chevalier, RA
Rupen, MP
Badenes, C
Margutti, R
Fransson, C
Fong, WF
Dittmann, JA
AF Chomiuk, Laura
Soderberg, Alicia M.
Moe, Maxwell
Chevalier, Roger A.
Rupen, Michael P.
Badenes, Carles
Margutti, Raffaella
Fransson, Claes
Fong, Wen-fai
Dittmann, Jason A.
TI EVLA OBSERVATIONS CONSTRAIN THE ENVIRONMENT AND PROGENITOR SYSTEM OF
Type Ia SUPERNOVA 2011fe
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; circumstellar matter; novae, cataclysmic variables;
supernovae: general; supernovae: individual (SN 2011fe)
ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURSTS; SN 2011FE; CIRCUMSTELLAR
MATERIAL; RADIO-EMISSION; WHITE-DWARFS; U-SCORPII; SODIUM-ABSORPTION;
SYMBIOTIC CHANNEL; REMNANT G1.9+0.3
AB We report unique Expanded Very Large Array observations of SN 2011fe representing the most sensitive radio study of a Type Ia supernova to date. Our data place direct constraints on the density of the surrounding medium at radii similar to 10(15)-10(16) cm, implying an upper limit on the mass loss rate from the progenitor system of (M) over dot less than or similar to 6x10(-10) M-circle dot yr(-1) (assuming a wind speed of 100 km s(-1)) or expansion into a uniform medium with density n(CSM) less than or similar to 6 cm(-3). Drawing from the observed properties of non-conservative mass transfer among accreting white dwarfs, we use these limits on the density of the immediate environs to exclude a phase space of possible progenitor systems for SN 2011fe. We rule out a symbiotic progenitor system and also a system characterized by high accretion rate onto the white dwarf that is expected to give rise to optically thick accretion winds. Assuming that a small fraction, 1%, of the mass accreted is lost from the progenitor system, we also eliminate much of the potential progenitor parameter space for white dwarfs hosting recurrent novae or undergoing stable nuclear burning. Therefore, we rule out much of the parameter space associated with popular single degenerate progenitor models for SN 2011fe, leaving a limited phase space largely inhabited by some double degenerate systems, as well as exotic single degenerates with a sufficient time delay between mass accretion and SN explosion.
C1 [Chomiuk, Laura; Soderberg, Alicia M.; Moe, Maxwell; Margutti, Raffaella; Fong, Wen-fai; Dittmann, Jason A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chomiuk, Laura; Rupen, Michael P.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Chevalier, Roger A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Badenes, Carles] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Badenes, Carles] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA.
[Fransson, Claes] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
RP Chomiuk, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM lchomiuk@cfa.harvard.edu
OI Badenes, Carles/0000-0003-3494-343X
FU National Aeronautics and Space Administration; NSF [AST-0807727]
FX We are grateful to Sumner Starrfield and an anonymous referee for their
insights. The National Radio Astronomy Observatory is a facility of the
National Science Foundation operated under cooperative agreement by the
Associated Universities, Inc. L.C. is a Jansky Fellow of the National
Radio Astronomy Observatory. This work made use of THINGS, "The HI
Nearby Galaxy Survey" (Walter et al. 2008). This research has also made
use of the NASA/IPAC Extragalactic Database (NED) which is operated by
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. R.A.C.
acknowledges support from the NSF under the grant AST-0807727.
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ER
PT J
AU Fabrycky, DC
Ford, EB
Steffen, JH
Rowe, JF
Carter, JA
Moorhead, AV
Batalha, NM
Borucki, WJ
Bryson, S
Buchhave, LA
Christiansen, JL
Ciardi, DR
Cochran, WD
Endl, M
Fanelli, MN
Fischer, D
Fressin, F
Geary, J
Haas, MR
Hall, JR
Holman, MJ
Jenkins, JM
Koch, DG
Latham, DW
Li, J
Lissauer, JJ
Lucas, P
Marcy, GW
Mazeh, T
McCauliff, S
Quinn, S
Ragozzine, D
Sasselov, D
Shporer, A
AF Fabrycky, Daniel C.
Ford, Eric B.
Steffen, Jason H.
Rowe, Jason F.
Carter, Joshua A.
Moorhead, Althea V.
Batalha, Natalie M.
Borucki, William J.
Bryson, Steve
Buchhave, Lars A.
Christiansen, Jessie L.
Ciardi, David R.
Cochran, William D.
Endl, Michael
Fanelli, Michael N.
Fischer, Debra
Fressin, Francois
Geary, John
Haas, Michael R.
Hall, Jennifer R.
Holman, Matthew J.
Jenkins, Jon M.
Koch, David G.
Latham, David W.
Li, Jie
Lissauer, Jack J.
Lucas, Philip
Marcy, Geoffrey W.
Mazeh, Tsevi
McCauliff, Sean
Quinn, Samuel
Ragozzine, Darin
Sasselov, Dimitar
Shporer, Avi
TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. IV. CONFIRMATION OF FOUR
MULTIPLE-PLANET SYSTEMS BY SIMPLE PHYSICAL MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: statistical; planetary systems; planets and satellites:
detection; planets and satellites: dynamical evolution and stability;
stars: individual (KID 10358759/KOI-738/Kepler-29, KID
3832474/KOI-806/Kepler-30, KID 9347899/KOI-935/Kepler-31, KID
9787239/KOI-952/Kepler-32)
ID SOLAR-TYPE STARS; MEAN-MOTION RESONANCES; SPIN-ORBIT ALIGNMENT;
SUPER-EARTHS; SOPHIE VELOCIMETRY; MASS PLANETS; HOT-JUPITER; EXTRASOLAR
PLANETS; 3-BODY PROBLEM; HARPS SEARCH
AB Eighty planetary systems of two or more planets are known to orbit stars other than the Sun. For most, the data can be sufficiently explained by non-interacting Keplerian orbits, so the dynamical interactions of these systems have not been observed. Here we present four sets of light curves from the Kepler spacecraft, each which of shows multiple planets transiting the same star. Departure of the timing of these transits from strict periodicity indicates that the planets are perturbing each other: the observed timing variations match the forcing frequency of the other planet. This confirms that these objects are in the same system. Next we limit their masses to the planetary regime by requiring the system remain stable for astronomical timescales. Finally, we report dynamical fits to the transit times, yielding possible values for the planets' masses and eccentricities. As the timespan of timing data increases, dynamical fits may allow detailed constraints on the systems' architectures, even in cases for which high-precision Doppler follow-up is impractical.
C1 [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ford, Eric B.; Moorhead, Althea V.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Rowe, Jason F.; Christiansen, Jessie L.; Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA.
[Fanelli, Michael N.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Carter, Joshua A.; Fressin, Francois; Geary, John; Holman, Matthew J.; Latham, David W.; Quinn, Samuel; Ragozzine, Darin; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, Dept Astrophys & Planetary Sci, DK-1350 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Ciardi, David R.] Caltech, NASA Exoplanet Sci Inst, Pasadena, CA 91126 USA.
[Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78730 USA.
[Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Fischer, Debra] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
[Hall, Jennifer R.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Mazeh, Tsevi] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
RP Fabrycky, DC (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM daniel.fabrycky@gmail.com
RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013;
OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
David/0000-0002-5741-3047; /0000-0001-6545-639X; Fischer,
Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; National Aeronautics and Space
Administration (NASA) [HF-51272.01-A, HF-51267.01-A, NAS 5-26555,
NNX08AR04G]; Space Telescope Science Institute; National Science
Foundation [0707203]
FX Funding for this mission is provided by NASA's Science Mission
Directorate. We thank the entire Kepler team for the many years of work
that is proving so successful. We thank E. Agol for comments and G.
Sokol for assistance analyzing starspot variations. D.C.F. and J.A.C.
acknowledge support for this work was provided by NASA through Hubble
Fellowship grants HF-51272.01-A and HF-51267.01-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555. E.B.F acknowledges support by the National Aeronautics and
Space Administration under grant NNX08AR04G issued through the Kepler
Participating Scientist Program. This material is based upon work
supported by the National Science Foundation under grant No. 0707203.
This paper uses observations obtained with facilities of the LasCumbres
Observatory Global Telescope.
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ER
PT J
AU Ford, EB
Fabrycky, DC
Steffen, JH
Carter, JA
Fressin, F
Holman, MJ
Lissauer, JJ
Moorhead, AV
Morehead, RC
Ragozzine, D
Rowe, JF
Welsh, WF
Allen, C
Batalha, NM
Borucki, WJ
Bryson, ST
Buchhave, LA
Burke, CJ
Caldwell, DA
Charbonneau, D
Clarke, BD
Cochran, WD
Desert, JM
Endl, M
Everett, ME
Fischer, DA
Gautier, TN
Gilliland, RL
Jenkins, JM
Haas, MR
Horch, E
Howell, SB
Ibrahim, KA
Isaacson, H
Koch, DG
Latham, DW
Li, J
Lucas, P
MacQueen, PJ
Marcy, GW
McCauliff, S
Mullally, FR
Quinn, SN
Quintana, E
Shporer, A
Still, M
Tenenbaum, P
Thompson, SE
Torres, G
Twicken, JD
Wohler, B
AF Ford, Eric B.
Fabrycky, Daniel C.
Steffen, Jason H.
Carter, Joshua A.
Fressin, Francois
Holman, Matthew J.
Lissauer, Jack J.
Moorhead, Althea V.
Morehead, Robert C.
Ragozzine, Darin
Rowe, Jason F.
Welsh, William F.
Allen, Christopher
Batalha, Natalie M.
Borucki, William J.
Bryson, Stephen T.
Buchhave, Lars A.
Burke, Christopher J.
Caldwell, Douglas A.
Charbonneau, David
Clarke, Bruce D.
Cochran, William D.
Desert, Jean-Michel
Endl, Michael
Everett, Mark E.
Fischer, Debra A.
Gautier, Thomas N., III
Gilliland, Ron L.
Jenkins, Jon M.
Haas, Michael R.
Horch, Elliott
Howell, Steve B.
Ibrahim, Khadeejah A.
Isaacson, Howard
Koch, David G.
Latham, David W.
Li, Jie
Lucas, Philip
MacQueen, Phillip J.
Marcy, Geoffrey W.
McCauliff, Sean
Mullally, Fergal R.
Quinn, Samuel N.
Quintana, Elisa
Shporer, Avi
Still, Martin
Tenenbaum, Peter
Thompson, Susan E.
Torres, Guillermo
Twicken, Joseph D.
Wohler, Bill
CA Kepler Sci Team
TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. II. CONFIRMATION OF TWO
MULTIPLANET SYSTEMS VIA A NON-PARAMETRIC CORRELATION ANALYSIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: detection; planets and
satellites: dynamical evolution and stability; stars: individual (KIC
3231341, 11512246, KOI 168, 1102, Kepler-23, Kepler-24); techniques:
miscellaneous
ID SOLAR-TYPE STARS; 1ST 4 MONTHS; PLANET CANDIDATES; EXTRASOLAR PLANETS;
PROTOSTELLAR DISC; Y-2 ISOCHRONES; FOLLOW-UP; STELLAR; MULTIPLICITY;
VALIDATION
AB We present a new method for confirming transiting planets based on the combination of transit timing variations (TTVs) and dynamical stability. Correlated TTVs provide evidence that the pair of bodies is in the same physical system. Orbital stability provides upper limits for the masses of the transiting companions that are in the planetary regime. This paper describes a non-parametric technique for quantifying the statistical significance of TTVs based on the correlation of two TTV data sets. We apply this method to an analysis of the TTVs of two stars with multiple transiting planet candidates identified by Kepler. We confirm four transiting planets in two multiple-planet systems based on their TTVs and the constraints imposed by dynamical stability. An additional three candidates in these same systems are not confirmed as planets, but are likely to be validated as real planets once further observations and analyses are possible. If all were confirmed, these systems would be near 4:6:9 and 2:4:6:9 period commensurabilities. Our results demonstrate that TTVs provide a powerful tool for confirming transiting planets, including low-mass planets and planets around faint stars for which Doppler follow-up is not practical with existing facilities. Continued Kepler observations will dramatically improve the constraints on the planet masses and orbits and provide sensitivity for detecting additional non-transiting planets. If Kepler observations were extended to eight years, then a similar analysis could likely confirm systems with multiple closely spaced, small transiting planets in or near the habitable zone of solar-type stars.
C1 [Ford, Eric B.; Moorhead, Althea V.; Morehead, Robert C.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Carter, Joshua A.; Fressin, Francois; Holman, Matthew J.; Ragozzine, Darin; Charbonneau, David; Desert, Jean-Michel; Quinn, Samuel N.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Allen, Christopher; Ibrahim, Khadeejah A.; McCauliff, Sean; Wohler, Bill] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Rowe, Jason F.; Burke, Christopher J.; Caldwell, Douglas A.; Clarke, Bruce D.; Jenkins, Jon M.; Li, Jie; Mullally, Fergal R.; Quintana, Elisa; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.] SETI Inst, Mountain View, CA 94043 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78730 USA.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilliland, Ron L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Shporer, Avi] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Ford, EB (reprint author), Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
EM eford@astro.ufl.edu
RI Kepler, S. O. /H-5901-2012; Carter, Joshua/A-8280-2013; Ragozzine,
Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014;
OI Kepler, S. O. /0000-0002-7470-5703; Fischer, Debra/0000-0003-2221-0861;
Fabrycky, Daniel/0000-0003-3750-0183; Caldwell,
Douglas/0000-0003-1963-9616; Buchhave, Lars A./0000-0003-1605-5666;
/0000-0001-6545-639X
FU NASA's Science Mission Directorate; National Aeronautics and Space
Administration (NASA) [NNX08AR04G, HF-51272.01-A, HF-51267.01-A, NAS
5-26555]; National Science Foundation [0707203]; Space Telescope Science
Institute
FX Funding for this mission is provided by NASA's Science Mission
Directorate. We thank the entire Kepler team for the many years of work
that is proving so successful. E.B.F. acknowledges support by the
National Aeronautics and Space Administration under grant NNX08AR04G
issued through the Kepler Participating Scientist Program. This material
is based upon work supported by the National Science Foundation under
grant 0707203. D.C.F. and J.A.C. acknowledge support for this work
provided by NASA through Hubble Fellowship grants HF-51272.01-A and
HF-51267.01-A awarded by the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., for NASA, under contract NAS 5-26555. Results are based in part on
observations obtained at the W.M. Keck Observatory, which is operated by
the University of California and the California Institute of Technology,
and at 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2012
VL 750
IS 2
AR 113
DI 10.1088/0004-637X/750/2/113
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500027
ER
PT J
AU Kipping, DM
Bakos, GA
Buchhave, L
Nesvorny, D
Schmitt, A
AF Kipping, D. M.
Bakos, G. A.
Buchhave, L.
Nesvorny, D.
Schmitt, A.
TI THE HUNT FOR EXOMOONS WITH KEPLER (HEK). I. DESCRIPTION OF A NEW
OBSERVATIONAL PROJECT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: data analysis; occultations; planetary systems; planets and
satellites: general; techniques: photometric
ID EXTRASOLAR GIANT PLANETS; TRANSIT LIGHT-CURVE; TERRESTRIAL PLANETS;
MODEL SELECTION; BLEND SCENARIOS; PHOTOMETRY; SYSTEM; SATELLITES;
CANDIDATES; MOON
AB Two decades ago, empirical evidence concerning the existence and frequency of planets around stars, other than our own, was absent. Since that time, the detection of extrasolar planets from Jupiter-sized to, most recently, Earth-sized worlds has blossomed and we are finally able to shed light on the plurality of Earth-like, habitable planets in the cosmos. Extrasolar moons may also be frequently habitable worlds, but their detection or even systematic pursuit remains lacking in the current literature. Here, we present a description of the first systematic search for extrasolar moons as part of a new observational project called "The Hunt for Exomoons with Kepler" (HEK). The HEK project distills the entire list of known transiting planet candidates found by Kepler (2326 at the time of writing) down to the most promising candidates for hosting a moon. Selected targets are fitted using a multimodal nested sampling algorithm coupled with a planet-with-moon light curve modeling routine. By comparing the Bayesian evidence of a planet-only model to that of a planet-with-moon, the detection process is handled in a Bayesian framework. In the case of null detections, upper limits derived from posteriors marginalized over the entire prior volume will be provided to inform the frequency of large moons around viable planetary hosts, eta((sic)). After discussing our methodologies for target selection, modeling, fitting, and vetting, we provide two example analyses.
C1 [Kipping, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Buchhave, L.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark.
[Nesvorny, D.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA.
RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
EM dkipping@cfa.harvard.edu
OI Buchhave, Lars A./0000-0003-1605-5666
NR 83
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2012
VL 750
IS 2
AR 115
DI 10.1088/0004-637X/750/2/115
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500029
ER
PT J
AU Kurtz, MJ
Geller, MJ
Utsumi, Y
Miyazaki, S
Dell'Antonio, IP
Fabricant, DG
AF Kurtz, Michael J.
Geller, Margaret J.
Utsumi, Yousuke
Miyazaki, Satoshi
Dell'Antonio, Ian P.
Fabricant, Daniel G.
TI TESTING WEAK-LENSING MAPS WITH REDSHIFT SURVEYS: A SUBARU FIELD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: clusters: general; galaxies:
distances and redshifts; gravitational lensing: weak; large-scale
structure of Universe
ID DIGITAL SKY SURVEY; FIBER-FED SPECTROGRAPH; LARGE-SCALE STRUCTURE;
DARK-MATTER HALOS; GALAXY CLUSTERS; MASS PROFILES; DEEP; HECTOSPEC;
CATALOG; COSMOS
AB We use a dense redshift survey in the foreground of the Subaru GTO2deg(2) weak-lensing field (centered at alpha(2000) = 16(h)04(m)44(s); delta(2000) = 43 degrees 11'24 '') to assess the completeness and comment on the purity of massive halo identification in the weak-lensing map. The redshift survey (published here) includes 4541 galaxies; 4405 are new redshifts measured with the Hectospec on the MMT. Among the weak-lensing peaks with a signal-to-noise greater than 4.25, 2/3 correspond to individual massive systems; this result is essentially identical to the Geller et al. test of the Deep Lens Survey (DLS) field F2. The Subaru map, based on images in substantially better seeing than the DLS, enables detection of less massive halos at fixed redshift as expected. We demonstrate that the procedure adopted by Miyazaki et al. for removing some contaminated peaks from the weak-lensing map improves agreement between the lensing map and the redshift survey in the identification of candidate massive systems.
C1 [Kurtz, Michael J.; Geller, Margaret J.; Fabricant, Daniel G.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Utsumi, Yousuke] Grad Univ Adv Studies, Mitaka, Tokyo, Japan.
[Utsumi, Yousuke; Miyazaki, Satoshi] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
RP Kurtz, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM mkurtz@cfa.harvard.edu; mgeller@cfa.harvard.edu;
yousuke.utsumi@nao.ac.jp; satoshi@subaru.naoj.org; ian@het.brown.edu;
dfabricant@cfa.harvard.edu
OI Utsumi, Yousuke/0000-0001-6161-8988; Kurtz, Michael/0000-0002-6949-0090
FU NSF [AST-0708433]; Smithsonian Institution
FX We thank P. Berlind and M. Calkins for their expert operation of the
Hectospec. D. Mink, J. Roll, S. Tokarz, and W. Wyatt constructed and ran
the Hectospec pipeline. Nelson Caldwell deftly manages Hectospec queue
scheduling for optimal scientific results. Eduard Westra assisted with
some of the observations. We thank Scott Kenyon for insightful comments
and discussions. We thank the anonymous referee for astute comments that
improved this paper. The Smithsonian Institution generously supported
Hectospec and this project. NSF grant AST-0708433 supports Ian Dell
Antonio's research.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2012
VL 750
IS 2
AR 168
DI 10.1088/0004-637X/750/2/168
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500082
ER
PT J
AU Lee, GH
Woo, JH
Lee, MG
Hwang, HS
Lee, JC
Sohn, J
Lee, JH
AF Lee, Gwang-Ho
Woo, Jong-Hak
Lee, Myung Gyoon
Hwang, Ho Seong
Lee, Jong Chul
Sohn, Jubee
Lee, Jong Hwan
TI DO BARS TRIGGER ACTIVITY IN GALACTIC NUCLEI?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: nuclei; galaxies: Seyfert; galaxies: spiral;
galaxies: statistics
ID DIGITAL SKY SURVEY; CENTRAL MASS CONCENTRATIONS; BARRED SPIRAL GALAXIES;
SUPERMASSIVE BLACK-HOLES; ENHANCED STAR-FORMATION; BH-SIGMA DIAGRAM;
SEYFERT-GALAXIES; HOST GALAXIES; MOLECULAR GAS; STARBURST GALAXIES
AB We investigate the connection between the presence of bars and active galactic nucleus (AGN) activity, using a volume-limited sample of similar to 9000 late-type galaxies with axis ratio b/a > 0.6 and M-r < -19.5 + 5 log h at low redshift (0.02 <= z less than or similar to 0.055), selected from Sloan Digital Sky Survey Data Release 7. We find that the bar fraction in AGN-host galaxies (42.6%) is similar to 2.5 times higher than in non-AGN galaxies (15.6%), and that the AGN fraction is a factor of two higher in strong-barred galaxies (34.5%) than in non-barred galaxies (15.0%). However, these trends are simply caused by the fact that AGN-host galaxies are on average more massive and redder than non-AGN galaxies because the fraction of strong-barred galaxies (f(SB)) increases with u - r color and stellar velocity dispersion. When u - r color and velocity dispersion (or stellar mass) are fixed, both the excess of f(SB) in AGN-host galaxies and the enhanced AGN fraction in strong-barred galaxies disappears. Among AGN-host galaxies we find no strong difference of the Eddington ratio distributions between barred and non-barred systems. These results indicate that AGN activity is not dominated by the presence of bars, and that AGN power is not enhanced by bars. In conclusion, we do not find clear evidence that bars trigger AGN activity.
C1 [Lee, Gwang-Ho; Woo, Jong-Hak; Lee, Myung Gyoon; Lee, Jong Chul; Sohn, Jubee; Lee, Jong Hwan] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea.
[Hwang, Ho Seong] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Lee, Jong Chul] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
RP Lee, GH (reprint author), Seoul Natl Univ, Dept Phys & Astron, 1 Gwanak Ro, Seoul 151742, South Korea.
EM ghlee@astro.snu.ac.kr; woo@astro.snu.ac.kr; mglee@astro.snu.ac.kr;
hhwang@cfa.harvard.edu; jclee@kasi.re.kr; jbsohn@astro.snu.ac.kr;
leejh@astro.snu.ac.kr
RI Woo, Jong-Hak/A-2790-2014
FU NRF; MEST [2010-0013875, 2010-0021558]; Centre National d'Etudes
Spatiales (CNES); Smithsonian Institution
FX We thank the anonymous referee for his/her useful comments which
significantly improved the original manuscript. G. H. L. thanks Changbom
Park and Yun-Young Choi for providing help in producing the KIAS VAGC
and performing the morphology classification. M. G. L. was supported in
part by Mid-career Research Program through the NRF grant funded by the
MEST (No. 2010-0013875). J.H.W. acknowledges support by the Basic
Science Research Program through the NRF funded by the MEST (No.
2010-0021558). H. S. H. acknowledges the Centre National d'Etudes
Spatiales (CNES) and the Smithsonian Institution for the support of his
post-doctoral fellowship.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2012
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AR 141
DI 10.1088/0004-637X/750/2/141
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500055
ER
PT J
AU Lissauer, JJ
Marcy, GW
Rowe, JF
Bryson, ST
Adams, E
Buchhave, LA
Ciardi, DR
Cochran, WD
Fabrycky, DC
Ford, EB
Fressin, F
Geary, J
Gilliland, RL
Holman, MJ
Howell, SB
Jenkins, JM
Kinemuchi, K
Koch, DG
Morehead, RC
Ragozzine, D
Seader, SE
Tanenbaum, PG
Torres, G
Twicken, JD
AF Lissauer, Jack J.
Marcy, Geoffrey W.
Rowe, Jason F.
Bryson, Stephen T.
Adams, Elisabeth
Buchhave, Lars A.
Ciardi, David R.
Cochran, William D.
Fabrycky, Daniel C.
Ford, Eric B.
Fressin, Francois
Geary, John
Gilliland, Ronald L.
Holman, Matthew J.
Howell, Steve B.
Jenkins, Jon M.
Kinemuchi, Karen
Koch, David G.
Morehead, Robert C.
Ragozzine, Darin
Seader, Shawn E.
Tanenbaum, Peter G.
Torres, Guillermo
Twicken, Joseph D.
TI ALMOST ALL OF KEPLER'S MULTIPLE-PLANET CANDIDATES ARE PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; planets and satellites: detection; techniques:
photometric
ID TRANSITING PLANET; TIMING VARIATIONS; LIGHT CURVES; SYSTEM; STAR;
VALIDATION; CATALOG; CAMERA
AB We present a statistical analysis that demonstrates that the overwhelming majority of Kepler candidate multiple transiting systems (multis) indeed represent true, physically associated transiting planets. Binary stars provide the primary source of false positives among Kepler planet candidates, implying that false positives should be nearly randomly distributed among Kepler targets. In contrast, true transiting planets would appear clustered around a smaller number of Kepler targets if detectable planets tend to come in systems and/or if the orbital planes of planets encircling the same star are correlated. There are more than one hundred times as many Kepler planet candidates in multi-candidate systems as would be predicted from a random distribution of candidates, implying that the vast majority are true planets. Most of these multis are multiple-planet systems orbiting the Kepler target star, but there are likely cases where (1) the planetary system orbits a fainter star, and the planets are thus significantly larger than has been estimated, or (2) the planets orbit different stars within a binary/multiple star system. We use the low overall false-positive rate among Kepler multis, together with analysis of Kepler spacecraft and ground-based data, to validate the closely packed Kepler-33 planetary system, which orbits a star that has evolved somewhat off of the main sequence. Kepler-33 hosts five transiting planets, with periods ranging from 5.67 to 41 days.
C1 [Lissauer, Jack J.; Rowe, Jason F.; Jenkins, Jon M.; Seader, Shawn E.; Tanenbaum, Peter G.; Twicken, Joseph D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Adams, Elisabeth; Fressin, Francois; Geary, John; Holman, Matthew J.; Ragozzine, Darin; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Ciardi, David R.] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ford, Eric B.; Morehead, Robert C.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
EM Jack.Lissauer@nasa.gov
RI Ragozzine, Darin/C-4926-2013;
OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
David/0000-0002-5741-3047; /0000-0001-6545-639X; Fabrycky,
Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [HF-51272.01-A]; STScI; [NAS
5-26555]
FX Kepler was competitively selected as the 10th Discovery mission. Funding
for this mission is provided by NASA's Science Mission Directorate. The
authors thank the many people who gave so generously of their time to
make the Kepler mission a success, chief among them Bill Borucki, who
has devoted decades to developing and implementing Kepler. Useful
comments were provided by Natalie Batalha, Ruth Murray-Clay, Dimitar
Sasselov, Jason Steffen, and especially by Tim Brown. Kevin Zahnle and
Mark Marley provided constructive comments on the manuscript. D.C.F.
acknowledges NASA support through Hubble Fellowship grant No.
HF-51272.01-A, awarded by STScI, operated by AURA under contract NAS
5-26555.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
PD MAY 10
PY 2012
VL 750
IS 2
AR 112
DI 10.1088/0004-637X/750/2/112
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500026
ER
PT J
AU Siemiginowska, A
Stawarz, L
Cheung, CC
Aldcroft, TL
Bechtold, J
Burke, DJ
Evans, D
Holt, J
Jamrozy, M
Migliori, G
AF Siemiginowska, Aneta
Stawarz, Lukasz
Cheung, Chi C.
Aldcroft, Thomas L.
Bechtold, Jill
Burke, D. J.
Evans, Daniel
Holt, Joanna
Jamrozy, Marek
Migliori, Giulia
TI DEEP CHANDRA X-RAY IMAGING OF A NEARBY RADIO GALAXY 4C+29.30:
X-RAY/RADIO CONNECTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (4C+29.30); galaxies: jets;
radiation mechanisms: non-thermal; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; PARTICLE-ACCELERATION; CENTAURUS-A; QUIET
QUASARS; INTERSTELLAR-MEDIUM; RELATIVISTIC JET; ACCRETION MODELS;
PARAMETER SPACE; PERSEUS CLUSTER; BLACK-HOLES
AB We report results from our deep Chandra X-ray observations of a nearby radio galaxy, 4C+29.30 (z = 0.0647). The Chandra image resolves structures on sub-arcsec to arcsec scales, revealing complex X-ray morphology and detecting the main radio features: the nucleus, a jet, hotspots, and lobes. The nucleus is absorbed (N-H similar or equal to 3.95(-0.33)(+0.27) x 10(23) cm(-2)) with an unabsorbed luminosity of L2-10 keV similar or equal to (5.08 +/- 0.52) x 10(43) erg s(-1) characteristic of Type 2 active galactic nuclei. Regions of soft (< 2 keV) X-ray emission that trace the hot interstellar medium (ISM) are correlated with radio structures along the main radio axis, indicating a strong relation between the two. The X-ray emission extends beyond the radio source and correlates with the morphology of optical-line-emitting regions. We measured the ISM temperature in several regions across the galaxy to be kT similar or equal to 0.5 keV, with slightly higher temperatures (of a few keV) in the center and in the vicinity of the radio hotspots. Assuming that these regions were heated by weak shocks driven by the expanding radio source, we estimated the corresponding Mach number of 1.6 in the southern regions. The thermal pressure of the X-ray-emitting gas in the outermost regions suggests that the hot ISM is slightly underpressured with respect to the cold optical-line-emitting gas and radio-emitting plasma, which both seem to be in a rough pressure equilibrium. We conclude that 4C+29.30 displays a complex view of interactions between the jet-driven radio outflow and host galaxy environment, signaling feedback processes closely associated with the central active nucleus.
C1 [Siemiginowska, Aneta; Aldcroft, Thomas L.; Burke, D. J.; Evans, Daniel; Migliori, Giulia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stawarz, Lukasz] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Stawarz, Lukasz; Jamrozy, Marek] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Cheung, Chi C.] Natl Acad Sci, Washington, DC 20001 USA.
[Bechtold, Jill] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Evans, Daniel] Elon Univ, Dept Phys, Elon, NC 27244 USA.
[Holt, Joanna] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Siemiginowska, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM asiemiginowska@cfa.harvard.edu
RI Jamrozy, Marek/F-4507-2015;
OI Burke, Douglas/0000-0003-4428-7835
FU Polish MNiSW [N-N203-380336]; MNiSW [3812/B/H03/2009/36]; NASA [DPR
S-15633-Y, NAS8-39073]; [GO0-11133X]; [NNX08AX35G]
FX The authors thank the anonymous referee for insightful comments and
Malgorzata Sobolewska, Ralph Kraft, and Dharam Vir Lal for fruitful
discussion. L.S. is grateful for the support from Polish MNiSW through
the grant N-N203-380336. M.J. was supported by MNiSW funds for
scientific research in years 2009-2012 under the contract no.
3812/B/H03/2009/36. Work at NRL is sponsored by NASA DPR S-15633-Y. This
research has made use of data obtained by the Chandra X-ray Observatory,
and Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS,
and Sherpa. This research is funded in part by NASA contract NAS8-39073.
Partial support for this work was provided by the Chandra grant
GO0-11133X and XMM-Newton grant NNX08AX35G.
NR 78
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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 MAY 10
PY 2012
VL 750
IS 2
AR 124
DI 10.1088/0004-637X/750/2/124
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500038
ER
PT J
AU Soria, R
Kuntz, KD
Winkler, PF
Blair, WP
Long, KS
Plucinsky, PP
Whitmore, BC
AF Soria, Roberto
Kuntz, K. D.
Winkler, P. Frank
Blair, William P.
Long, Knox S.
Plucinsky, Paul P.
Whitmore, Bradley C.
TI THE BIRTH OF AN ULTRALUMINOUS X-RAY SOURCE IN M83
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies: individual
(M83); X-rays: binaries
ID MASS BLACK-HOLE; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; NEARBY
GALAXY SURVEY; CHANDRA DEEP SURVEY; ACCRETION DISKS; OPTICAL
COUNTERPARTS; STARBURST GALAXY; BINARY-SYSTEMS; HOST GALAXIES
AB A previously undetected (L-X < 10(36) erg s(-1)) source in the strongly star-forming galaxy M83 entered an ultraluminous state between 2009 August and 2010 December. It was first seen with Chandra on 2010 December 23 at L-X approximate to 4 x 10(39) erg s(-1) and has remained ultraluminous through our most recent observations in 2011 December, with typical flux variation of a factor of two. The spectrum is well fitted by a combination of absorbed power-law and disk blackbody models. While the relative contributions of the models vary with time, we have seen no evidence for a canonical state transition. The luminosity and spectral properties are consistent with accretion powered by a black hole with M-BH approximate to 40-100 M-circle dot. In 2011 July we found a luminous, blue optical counterpart that had not been seen in deep Hubble Space Telescope observations obtained in 2009 August. These optical observations suggest that the donor star is a low-mass star undergoing Roche lobe overflow, and that the blue optical emission seen during the outburst is coming from an irradiated accretion disk. This source shows that ultraluminous X-ray sources (ULXs) with low-mass companions are an important component of the ULX population in star-forming galaxies and provides further evidence that the blue optical counterparts of some ULXs need not indicate a young, high-mass companion, but rather that they may indicate X-ray reprocessing.
C1 [Soria, Roberto] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Kuntz, K. D.; Blair, William P.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
[Long, Knox S.; Whitmore, Bradley C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Soria, R (reprint author), Curtin Univ Technol, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia.
EM roberto.soria@icrar.org; kuntz@pha.jhu.edu; winkler@middlebury.edu;
wpb@pha.jhu.edu; long@stsci.edu; plucinsky@cfa.harvard.edu;
whitmore@stsci.edu
FU NASA [NAS 5-26555, NAS8-03060]; NOAO; Swift team; National Aeronautics
and Space Administration through Chandra [G01-12115]; Chandra X-ray
Observatory Center; National Science Foundation [AST-0908566];
[NAS83060]; [GO1-12115]; [GO-12513]; [GO-12683]; [GO-11360];
[GS-2011A-C-1]
FX Based on observations made with NASA's Chandra X-Ray Observatory, the
NASA/ESA Hubble Space Telescope (HST), Swift, the 6.5 m Magellan
Telescopes located at Las Campanas Observatory, and the Gemini
Observatory. NASA's Chandra Observatory is operated by Smithsonian
Astrophysical Observatory under contract NAS83060, and the data were
obtained through program GO1-12115. The HST observations were obtained
at the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy (AURA), Inc.,
under NASA contract NAS 5-26555. The new HST observations were obtained
through programs GO-12513 and GO-12683. Data in the HST archive from
program GO-11360 were also used. The ground-based observations were
obtained from the Magellan I Telescope at the Las Campanas Observatory
and from the Gemini South Telescope of the Gemini Observatory, both
awarded through NOAO, which is operated by Association of Universities
for Research in Astronomy, Inc., for the National Science Foundation.;
Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Grant No. G01-12115, 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. P. F. W. and W. P. B. are grateful for both observing and
travel support for the Gemini observations from the Gemini office at
NOAO. P. F. W. also acknowledges financial support from the National
Science Foundation through grant AST-0908566 and the hospitality of the
Research School of Astronomy and Astrophysics, Australian National
University, during a portion of the work presented here.; We acknowledge
the use of public data from the Swift data archive. This research has
made use of data obtained from the High Energy Astrophysics Science
Archive Research Center (HEASARC), provided by NASA's Goddard Space
Flight Center.; The Gemini data were obtained under program
GS-2011A-C-1. The Gemini Observatory is operated by AURA under a
cooperative agreement with the NSF on behalf of the Gemini partnership:
the National Science Foundation (United States), the Science and
Technology Facilities Council (United Kingdom), the National Research
Council (Canada), CONICYT (Chile), the Australian Research Council
(Australia), Ministerio da Ciencia, Tecnologia e Innovacion (Brazil),
and Ministerio de Ciencia, Tecnologia e Innovacion Productiva
(Argentina).
NR 116
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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 MAY 10
PY 2012
VL 750
IS 2
AR 152
DI 10.1088/0004-637X/750/2/152
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500066
ER
PT J
AU Tonry, JL
Stubbs, CW
Lykke, KR
Doherty, P
Shivvers, IS
Burgett, WS
Chambers, KC
Hodapp, KW
Kaiser, N
Kudritzki, RP
Magnier, EA
Morgan, JS
Price, PA
Wainscoat, RJ
AF Tonry, J. L.
Stubbs, C. W.
Lykke, K. R.
Doherty, P.
Shivvers, I. S.
Burgett, W. S.
Chambers, K. C.
Hodapp, K. W.
Kaiser, N.
Kudritzki, R. -P.
Magnier, E. A.
Morgan, J. S.
Price, P. A.
Wainscoat, R. J.
TI THE Pan-STARRS1 PHOTOMETRIC SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atmospheric effects; instrumentation: photometers; surveys; techniques:
photometric
ID DIGITAL SKY SURVEY; ATMOSPHERIC EXTINCTION; STELLAR LOCUS; CALIBRATION;
TELESCOPES; HIPPARCOS; PASSBANDS; STANDARDS; PANSTARRS; IMAGER
AB The Pan-STARRS1 survey is collecting multi-epoch, multi-color observations of the sky north of declination -30 degrees to unprecedented depths. These data are being photometrically and astrometrically calibrated and will serve as a reference for many other purposes. In this paper, we present our determination of the Pan-STARRS1 photometric system: g(P1), r(P1), i(P1), z(P1), y(P1), and w(P1). The Pan-STARRS1 photometric system is fundamentally based on the Hubble Space Telescope Calspec spectrophotometric observations, which in turn are fundamentally based on models of white dwarf atmospheres. We define the Pan-STARRS1 magnitude system and describe in detail our measurement of the system passbands, including both the instrumental sensitivity and atmospheric transmission functions. By-products, including transformations to other photometric systems, Galactic extinction, and stellar locus, are also provided. We close with a discussion of remaining systematic errors.
C1 [Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kaiser, N.; Kudritzki, R. -P.; Magnier, E. A.; Morgan, J. S.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Stubbs, C. W.; Shivvers, I. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stubbs, C. W.; Doherty, P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Lykke, K. R.] NIST, Gaithersburg, MD 20899 USA.
[Shivvers, I. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Tonry, JL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
RI Stubbs, Christopher/C-2829-2012;
OI Stubbs, Christopher/0000-0003-0347-1724; Shivvers,
Isaac/0000-0003-3373-8047; Chambers, Kenneth /0000-0001-6965-7789
FU National Science Foundation [AST-1009749]; National Aeronautics and
Space Administration [NNX08AR22G]
FX Support for this work was provided by National Science Foundation grant
AST-1009749. The PS1 Surveys have been made possible through
contributions of the Institute for Astronomy, the University of Hawaii,
the Pan-STARRS Project Office, the Max-Planck Society and its
participating institutes, the Max-Planck Institute for Astronomy,
Heidelberg and the Max-Planck Institute for Extraterrestrial Physics,
Garching, The Johns Hopkins University, Durham University, the
University of Edinburgh, Queen'sUniversity Belfast, the
Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory
Global Telescope Network, Incorporated, the National Central University
of Taiwan, and the National Aeronautics and Space Administration under
grant no. NNX08AR22G issued through the Planetary Science Division of
the NASA Science Mission Directorate.
NR 41
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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 MAY 10
PY 2012
VL 750
IS 2
AR 99
DI 10.1088/0004-637X/750/2/99
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500013
ER
PT J
AU Wei, LH
Keto, E
Ho, LC
AF Wei, Lisa H.
Keto, Eric
Ho, Luis C.
TI TWO POPULATIONS OF MOLECULAR CLOUDS IN THE ANTENNAE GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 4038, NGC 4039); galaxies: ISM; galaxies:
starburst; galaxies: star clusters: general
ID YOUNG STAR-CLUSTERS; SPACE-TELESCOPE OBSERVATIONS; X-RAY SOURCES;
GLOBULAR-CLUSTERS; CHANDRA OBSERVATIONS; GALACTIC-CENTER; NGC 4038/4039;
LUMINOSITY FUNCTION; INTERSTELLAR-MEDIUM; FORMING RINGS
AB Super star clusters-extremely massive clusters found predominately in starburst environments-are essential building blocks in the formation of galaxies and thought to dominate star formation in the high-redshift universe. However, the transformation from molecular gas into these ultracompact star clusters is not well understood. To study this process, we used the Submillimeter Array and the Plateau de Bure Interferometer to obtain high angular resolution (similar to 1 ''.5 or 160 pc) images of the Antennae overlap region in CO(2-1) to search for the molecular progenitors of the super star clusters. We resolve the molecular gas distribution into a large number of clouds, extending the differential cloud mass function down to a 5 sigma completeness limit of 3.8 x 10(5) M-circle dot. We identify a distinct break in the mass function around log M-mol/M-circle dot approximate to 6.5, which separates the molecular clouds into two distinct populations. The smaller, less massive clouds reside in more quiescent areas in the region, while the larger, more massive clouds cluster around regions of intense star formation. A broken power-law fit to the mass function yields slopes of alpha = -1.39 +/- 0.10 and alpha = -1.44 +/- 0.14 for the low- and high-mass cloud population, well matched to the mass function found for super star clusters in the Antennae galaxies. We find large velocity gradients and velocity dispersions at the locations of intense star formation, suggestive of compressive shocks. It is likely that these environmental factors contribute to the formation of the observed massive molecular clouds and super star clusters in the Antennae galaxies.
C1 [Wei, Lisa H.; Keto, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ho, Luis C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
RP Wei, LH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Carnegie Institution for Science; Smithsonian Institution; Academia
Sinica; NASA
FX We thank the anonymous referee for helpful comments which improved this
manuscript. We thank Zhao-Yu Li for help in generating the three-color
image in Figure 1. We are grateful to Alberto Bolatto, Izaskun
Jimenez-Serra, and Peter Teuben for helpful discussions. The research of
L.C.H. is supported by the Carnegie Institution for Science. The
Submillimeter Array is a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics and is funded by the Smithsonian Institution and the
Academia Sinica. This work is based in part on archival data obtained
with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2012
VL 750
IS 2
AR 136
DI 10.1088/0004-637X/750/2/136
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934LT
UT WOS:000303446500050
ER
PT J
AU Hermes, JJ
Montgomery, MH
Winget, DE
Brown, WR
Kilic, M
Kenyon, SJ
AF Hermes, J. J.
Montgomery, M. H.
Winget, D. E.
Brown, Warren R.
Kilic, Mukremin
Kenyon, Scott J.
TI SDSS J184037.78+642312.3: THE FIRST PULSATING EXTREMELY LOW MASS WHITE
DWARF
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: close; Galaxy: stellar content; stars: individual (SDSS
J184037.78+642312.3); stars: variables: general; white dwarfs
ID ZZ-CETI STARS; BINARY; HELIUM; EVOLUTION; I.
AB We report the discovery of the first pulsating extremely low mass (ELM) white dwarf (WD), SDSS J184037.78+642312.3 (hereafter J1840). This DA (hydrogen-atmosphere) WD is by far the coolest and the lowest-mass pulsating WD, with T-eff = 9100 +/- 170 K and log g = 6.22 +/- 0.06, which corresponds to a mass of similar to 0.17 M-circle dot. This low-mass pulsating WD greatly extends the DAV (or ZZ Ceti) instability strip, effectively bridging the log g gap between WDs and main-sequence stars. We detect high-amplitude variability in J1840 on timescales exceeding 4000 s, with a non-sinusoidal pulse shape. Our observations also suggest that the variability is multi-periodic. The star is in a 4.6 hr binary with another compact object, most likely another WD. Future, more extensive time-series photometry of this ELM WD offers the first opportunity to probe the interior of a low-mass, presumably He-core WD using the tools of asteroseismology.
C1 [Hermes, J. J.; Montgomery, M. H.; Winget, D. E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Hermes, J. J.; Montgomery, M. H.; Winget, D. E.] McDonald Observ, Ft Davis, TX 79734 USA.
[Brown, Warren R.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA.
RP Hermes, JJ (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM jjhermes@astro.as.utexas.edu
OI Kenyon, Scott/0000-0003-0214-609X
FU NSF [AST-0909107]; Norman Hackerman Advanced Research Program
[003658-0252-2009]
FX J.J.H., M.H.M., and D.E.W. gratefully acknowledge the support of the NSF
under grant AST-0909107 and the Norman Hackerman Advanced Research
Program under grant 003658-0252-2009. The authors are grateful to the
McDonald Observatory support staff, F. Mullally for developing much of
the data analysis pipeline used here, and to J. Pelletier of the UT
Freshman Research Initiative for some of the analysis used in Table 2.
NR 38
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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 MAY 10
PY 2012
VL 750
IS 2
AR L28
DI 10.1088/2041-8205/750/2/L28
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934MP
UT WOS:000303448700002
ER
PT J
AU Krauss, MI
Soderberg, AM
Chomiuk, L
Zauderer, BA
Brunthaler, A
Bietenholz, MF
Chevalier, RA
Fransson, C
Rupen, M
AF Krauss, M. I.
Soderberg, A. M.
Chomiuk, L.
Zauderer, B. A.
Brunthaler, A.
Bietenholz, M. F.
Chevalier, R. A.
Fransson, C.
Rupen, M.
TI EXPANDED VERY LARGE ARRAY OBSERVATIONS OF THE RADIO EVOLUTION OF SN
2011dh
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE supernovae: individual (SN 2011dh)
ID IIB SUPERNOVA; YELLOW SUPERGIANTS; BINARY PROGENITOR; 1993J; 2003BG;
EXPANSION; EMISSION; COMPACT; MASS; M51
AB We report on Expanded Very Large Array observations of the Type IIb supernova 2011dh, performed over the first 100 days of its evolution and spanning 1-40 GHz in frequency. The radio emission is well described by the self-similar propagation of a spherical shockwave, generated as the supernova ejecta interact with the local circumstellar environment. Modeling this emission with a standard synchrotron self-absorption (SSA) model gives an average expansion velocity of v approximate to 0.1c, supporting the classification of the progenitor as a compact star (R-star approximate to 10(11) cm). We find that the circumstellar density is consistent with a rho proportional to r(-2) profile. We determine that the progenitor shed mass at a constant rate of approximate to 3 x 10(-5) M-circle dot yr(-1), assuming a wind velocity of 1000 km s(-1) (values appropriate for a Wolf-Rayet star), or approximate to 7 x 10(-7) M-circle dot yr(-1) assuming 20 km s(-1) (appropriate for a yellow supergiant [YSG] star). Both values of the mass-loss rate assume a converted fraction of kinetic to magnetic energy density of epsilon(B) = 0.1. Although optical imaging shows the presence of a YSG, the rapid optical evolution and fast expansion argue that the progenitor is a more compact star-perhaps a companion to the YSG. Furthermore, the excellent agreement of the radio properties of SN 2011dh with the SSA model implies that any YSG companion is likely in a wide, non-interacting orbit.
C1 [Krauss, M. I.; Chomiuk, L.; Brunthaler, A.; Rupen, M.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Soderberg, A. M.; Chomiuk, L.; Zauderer, B. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brunthaler, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bietenholz, M. F.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Bietenholz, M. F.] Hartebeesthoek Radio Observ, ZA-1740 Krugersdorp, South Africa.
[Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Fransson, C.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden.
RP Krauss, MI (reprint author), Natl Radio Astron Observ, Socorro, NM 87801 USA.
FU European Union [275596]
FX The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. A. B. was supported by a Marie Curie Outgoing
International Fellowship (FP7) of the European Union (project number
275596). We thank the anonymous referee for helpful comments and
suggestions. We acknowledge with thanks the variable star observations
from the AAVSO International database contributed by observers worldwide
and used in this research. This research has made use of NASA's
Astrophysics Data System Bibliographic Services. L. C. is a Jansky
Fellow of the National Radio Astronomy Observatory.
NR 43
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U1 0
U2 1
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 MAY 10
PY 2012
VL 750
IS 2
AR L40
DI 10.1088/2041-8205/750/2/L40
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934MP
UT WOS:000303448700014
ER
PT J
AU Strader, J
Chomiuk, L
Maccarone, TJ
Miller-Jones, JCA
Seth, AC
Heinke, CO
Sivakoff, GR
AF Strader, Jay
Chomiuk, Laura
Maccarone, Thomas J.
Miller-Jones, James C. A.
Seth, Anil C.
Heinke, Craig O.
Sivakoff, Gregory R.
TI NO EVIDENCE FOR INTERMEDIATE-MASS BLACK HOLES IN GLOBULAR CLUSTERS:
STRONG CONSTRAINTS FROM THE JVLA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE black hole physics; globular clusters: general; radio continuum: general
ID X-RAY BINARY; SPACE-TELESCOPE EVIDENCE; SAGITTARIUS A-ASTERISK;
OMEGA-CENTAURI; STAR-CLUSTERS; ACCRETION MODEL; RADIO-EMISSION; DWARF
GALAXY; IONIZED-GAS; LARGE ARRAY
AB With a goal of searching for accreting intermediate-mass black holes (IMBHs), we report the results of ultra-deep Jansky Very Large Array radio continuum observations of the cores of three Galactic globular clusters: M15, M19, and M22. We reach rms noise levels of 1.5-2.1 mu Jy beam (1) at an average frequency of 6 GHz. No sources are observed at the center of any of the clusters. For a conservative set of assumptions about the properties of the accretion, we set 3 sigma upper limits on IMBHs from 360 to 980 M-circle dot. These limits are among the most stringent obtained for any globular cluster. They add to a growing body of work that suggests either (1) IMBHs greater than or similar to 1000 M-circle dot are rare in globular clusters or (2) when present. IMBHs accrete in an extraordinarily inefficient manner.
C1 [Strader, Jay; Chomiuk, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chomiuk, Laura] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Maccarone, Thomas J.] Univ Southampton, Sch Phys & Astron, Highfield SO17 IBJ, England.
[Miller-Jones, James C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Seth, Anil C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Heinke, Craig O.; Sivakoff, Gregory R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
RP Strader, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jstrader@cfa.harvard.edu
RI Miller-Jones, James/B-2411-2013; Sivakoff, Gregory/G-9602-2011;
OI Miller-Jones, James/0000-0003-3124-2814; Sivakoff,
Gregory/0000-0001-6682-916X; Heinke, Craig/0000-0003-3944-6109
FU NSERC; Ingenuity New Faculty Award
FX NRAO is a facility of the NSF operated under cooperative agreement by
AUI. L. C. is a Jansky Fellow of NRAO. G. R. S. and C.O.H. are supported
by NSERC, and C.O.H. also by an Ingenuity New Faculty Award.
NR 50
TC 43
Z9 43
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD MAY 10
PY 2012
VL 750
IS 2
AR L27
DI 10.1088/2041-8205/750/2/L27
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934MP
UT WOS:000303448700001
ER
PT J
AU Tomsick, JA
Bodaghee, A
Rodriguez, J
Chaty, S
Camilo, F
Fornasini, F
Rahoui, F
AF Tomsick, John A.
Bodaghee, Arash
Rodriguez, Jerome
Chaty, Sylvain
Camilo, Fernando
Fornasini, Francesca
Rahoui, Farid
TI IS IGR J11014-6103 A PULSAR WITH THE HIGHEST KNOWN KICK VELOCITY?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: supernova remnants; pulsars: general; stars: individual (IGR
J11014-6103, SNR G290.1-00.8); stars: neutron; X-rays: stars
ID CENTRAL COMPACT OBJECT; X-RAY; INTERSTELLAR-MEDIUM; PSR B2224+65;
PUPPIS-A; DISCOVERY; YOUNG; ABSORPTION; TAILS
AB We report on Chandra X-ray and Parkes radio observations of IGR J11014-6103, which is a possible pulsar wind nebula with a complex X-ray morphology and a likely radio counterpart. With the superb angular resolution of Chandra, we find evidence that a portion of the extended emission may be related to a bow shock due to the putative pulsar moving through the interstellar medium. The inferred direction of motion is consistent with IGR J11014-6103 having been born in the event that produced the supernova remnant (SNR) MSH 11-61A. If this association is correct, then previous constraints on the expansion of MSH 11-61A imply a transverse velocity for IGR J11014-6103 of 2400-2900 km s(-1), depending on the SNR model used. This would surpass the kick velocities of any known pulsars and rival or surpass the velocities of any compact objects that are associated with SNRs. While it is important to confirm the nature of the source, our radio pulsation search did not yield a detection.
C1 [Tomsick, John A.; Bodaghee, Arash; Fornasini, Francesca] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Rodriguez, Jerome; Chaty, Sylvain] Univ Paris 07, CEA Saclay, Serv Astrophys, CNRS,CEA,UMR 7158,DSM,IRFU, FR-91191 Gif Sur Yvette, France.
[Camilo, Fernando] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Rahoui, Farid] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Tomsick, JA (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM jtomsick@ssl.berkeley.edu
OI Rodriguez, Jerome/0000-0002-4151-4468; Chaty,
Sylvain/0000-0002-5769-8601
FU NASA [GO1-12046X, NAS8-03060]; Chandra X-Ray Observatory Center;
Commonwealth of Australia
FX We acknowledge useful discussions with J. Halpern, V. Kaspi, S. Boggs,
and H. Tananbaum. Support for this work was provided by NASA through
Chandra Award Number GO1-12046X issued by the Chandra X-Ray Observatory
Center, which is operated by the Smithsonian Astrophysical Observatory
under NASA contract NAS8-03060. The Parkes Observatory is part of the
Australia Telescope, which is funded by the Commonwealth of Australia
for operation as a National Facility managed by CSIRO.
NR 29
TC 9
Z9 9
U1 0
U2 1
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 MAY 10
PY 2012
VL 750
IS 2
AR L39
DI 10.1088/2041-8205/750/2/L39
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 934MP
UT WOS:000303448700013
ER
PT J
AU Boyer, D
Crofoot, MC
Walsh, PD
AF Boyer, Denis
Crofoot, Margaret C.
Walsh, Peter D.
TI Non-random walks in monkeys and humans
SO JOURNAL OF THE ROYAL SOCIETY INTERFACE
LA English
DT Article
DE movement ecology; home range; memory; human mobility; capuchin monkeys;
scaling laws
ID HUMAN MOBILITY; ANOMALOUS DIFFUSION; PATTERNS; MODELS; MECHANISMS;
EMERGENCE; MOVEMENT; DYNAMICS; HOME; LAWS
AB Principles of self-organization play an increasingly central role in models of human activity. Notably, individual human displacements exhibit strongly recurrent patterns that are characterized by scaling laws and can be mechanistically modelled as self-attracting walks. Recurrence is not, however, unique to human displacements. Here we report that the mobility patterns of wild capuchin monkeys are not random walks, and they exhibit recurrence properties similar to those of cell phone users, suggesting spatial cognition mechanisms shared with humans. We also show that the highly uneven visitation patterns within monkey home ranges are not entirely self-generated but are forced by spatio-temporal habitat heterogeneities. If models of human mobility are to become useful tools for predictive purposes, they will need to consider the interaction between memory and environmental heterogeneities.
C1 [Boyer, Denis] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 04510, DF, Mexico.
[Boyer, Denis] Univ Nacl Autonoma Mexico, Ctr Ciencias Complejidad, Mexico City 04510, DF, Mexico.
[Crofoot, Margaret C.] Smithsonian Trop Res Inst, Panama City, Panama.
[Crofoot, Margaret C.] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany.
[Crofoot, Margaret C.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA.
[Walsh, Peter D.] VaccinApe, Bethesda, MD 20816 USA.
RP Boyer, D (reprint author), Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 04510, DF, Mexico.
EM boyer@fisica.unam.mx
FU National Center for Ecological Analysis and Synthesis; NSF
[DEB-0553768]; University of California, Santa Barbara; State of
California; Harvard University
FX This work was conducted as a part of the 'Efficient Wildlife Disease
Control: from Social Network Self-organization to Optimal Vaccination'
Working Group supported by the National Center for Ecological Analysis
and Synthesis, a centre funded by the NSF (grant no. DEB-0553768), the
University of California, Santa Barbara, and the State of California.
Funding for the data collection was provided to M.C.C. by the
Smithsonian Tropical Research Institute and the Frederik Sheldon
Travelling Fellowship from the Harvard University. Required permits were
obtained from the Autoridad Nacional del Ambiente, Panama and the
Smithsonian Tropical Research Institute Institutional Animal Care and
Use Committee. All research complied with the laws of the Republic of
Panama and the United States.
NR 34
TC 15
Z9 15
U1 1
U2 28
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1742-5689
EI 1742-5662
J9 J R SOC INTERFACE
JI J. R. Soc. Interface
PD MAY 7
PY 2012
VL 9
IS 70
BP 842
EP 847
DI 10.1098/rsif.2011.0582
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 916WQ
UT WOS:000302134300004
PM 22031731
ER
PT J
AU Ortega-Jimenez, VM
Dudley, R
AF Ortega-Jimenez, Victor Manuel
Dudley, Robert
TI Aerial shaking performance of wet Anna's hummingbirds
SO JOURNAL OF THE ROYAL SOCIETY INTERFACE
LA English
DT Article
DE feather; flexibility; flight; hovering; manoeuvrability; oscillation
ID WING-SPREADING BEHAVIOR; MANEUVERING FLIGHT; FEATHERS; WATER;
HYDROPHOBICITY; BIRD; COST
AB External wetting poses problems of immediate heat loss and long-term pathogen growth for vertebrates. Beyond these risks, the locomotor ability of smaller animals, and particularly of fliers, may be impaired by water adhering to the body. Here, we report on the remarkable ability of hummingbirds to perform rapid shakes in order to expel water from their plumage even while in flight. Kinematic performance of aerial versus non-aerial shakes (i.e. those performed while perching) was compared. Oscillation frequencies of the head, body and tail were lower in aerial shakes. Tangential speeds and accelerations of the trunk and tail were roughly similar in aerial and non-aerial shakes, but values for head motions in air were twice as high when compared with shakes while perching. Azimuthal angular amplitudes for both aerial and non-aerial shakes reached values greater than 180 degrees for the head, greater than 45 degrees for the body trunk and slightly greater than 90 degrees for the tail and wings. Using a feather on an oscillating disc to mimic shaking motions, we found that bending increased average speeds by up to 36 per cent and accelerations of the feather tip up to fourfold relative to a hypothetical rigid feather. Feather flexibility may help to enhance shedding of water and reduce body oscillations during shaking.
C1 [Ortega-Jimenez, Victor Manuel; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama.
RP Ortega-Jimenez, VM (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
EM vortega@berkeley.edu
OI Ortega-Jimenez, Victor Manuel/0000-0003-0024-5086
FU UC University of California MEXUS-CONACYT
FX We thank members of the Dudley laboratory, especially Nir Sapir, Marta
Wolf and Dennis Evangelista, for comments and suggestions on the
manuscript, and David Hu for insightful critique. We also thank Sarahi
Arriaga-Ramirez for sharing her MATLAB skills with us. We also thank the
two anonymous reviewers for their comments. V.M.O.-J. was supported by
UC University of California MEXUS-CONACYT, and dedicates this paper to
his parents (a mis padres). Hummingbird care and experimental procedures
were approved by the IACUC of the University of California, Berkeley.
NR 30
TC 10
Z9 10
U1 0
U2 13
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1742-5689
J9 J R SOC INTERFACE
JI J. R. Soc. Interface
PD MAY 7
PY 2012
VL 9
IS 70
BP 1093
EP 1099
DI 10.1098/rsif.2011.0608
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 916WQ
UT WOS:000302134300027
PM 22072447
ER
PT J
AU Squyres, SW
Arvidson, RE
Bell, JF
Calef, F
Clark, BC
Cohen, BA
Crumpler, LA
de Souza, PA
Farrand, WH
Gellert, R
Grant, J
Herkenhoff, KE
Hurowitz, JA
Johnson, JR
Jolliff, BL
Knoll, AH
Li, R
McLennan, SM
Ming, DW
Mittlefehldt, DW
Parker, TJ
Paulsen, G
Rice, MS
Ruff, SW
Schroder, C
Yen, AS
Zacny, K
AF Squyres, S. W.
Arvidson, R. E.
Bell, J. F., III
Calef, F., III
Clark, B. C.
Cohen, B. A.
Crumpler, L. A.
de Souza, P. A., Jr.
Farrand, W. H.
Gellert, R.
Grant, J.
Herkenhoff, K. E.
Hurowitz, J. A.
Johnson, J. R.
Jolliff, B. L.
Knoll, A. H.
Li, R.
McLennan, S. M.
Ming, D. W.
Mittlefehldt, D. W.
Parker, T. J.
Paulsen, G.
Rice, M. S.
Ruff, S. W.
Schroeder, C.
Yen, A. S.
Zacny, K.
TI Ancient Impact and Aqueous Processes at Endeavour Crater, Mars
SO SCIENCE
LA English
DT Article
ID MERIDIANI-PLANUM; SUEVITE BRECCIA; RIES CRATER; GERMANY; ORIGIN; VEINS;
HISTORY; GYPSUM; WATER; ROCK
AB The rover Opportunity has investigated the rim of Endeavour Crater, a large ancient impact crater on Mars. Basaltic breccias produced by the impact form the rim deposits, with stratigraphy similar to that observed at similar-sized craters on Earth. Highly localized zinc enrichments in some breccia materials suggest hydrothermal alteration of rim deposits. Gypsum-rich veins cut sedimentary rocks adjacent to the crater rim. The gypsum was precipitated from low-temperature aqueous fluids flowing upward from the ancient materials of the rim, leading temporarily to potentially habitable conditions and providing some of the waters involved in formation of the ubiquitous sulfate-rich sandstones of the Meridiani region.
C1 [Squyres, S. W.; Rice, M. S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Arvidson, R. E.; Jolliff, B. L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63031 USA.
[Bell, J. F., III; Ruff, S. W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Calef, F., III; Hurowitz, J. A.; Parker, T. J.; Yen, A. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Clark, B. C.; Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA.
[Cohen, B. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Crumpler, L. A.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA.
[de Souza, P. A., Jr.] Univ Tasmania, Human Interface Technol Lab, Launceston, Tas 7250, Australia.
[Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada.
[Grant, J.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Herkenhoff, K. E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Johnson, J. R.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Knoll, A. H.] Harvard Univ, Bot Museum, Cambridge, MA 02138 USA.
[Li, R.] Ohio State Univ, Dept Civil Environm & Geodet Engn, Columbus, OH 43210 USA.
[McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
[Ming, D. W.; Mittlefehldt, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Paulsen, G.; Zacny, K.] Honeybee Robot & Spacecraft Mech Corp, Pasadena, CA 91103 USA.
[Schroeder, C.] Univ Bayreuth, D-72076 Tubingen, Germany.
[Schroeder, C.] Univ Tubingen, D-72076 Tubingen, Germany.
RP Squyres, SW (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
EM squyres@astro.cornell.edu
RI Schroder, Christian/B-3870-2009; de Souza, Paulo/B-8961-2008; Johnson,
Jeffrey/F-3972-2015
OI Schroder, Christian/0000-0002-7935-6039; de Souza,
Paulo/0000-0002-0091-8925;
FU NASA
FX This research was carried out for the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA.
NR 36
TC 76
Z9 77
U1 1
U2 60
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD MAY 4
PY 2012
VL 336
IS 6081
BP 570
EP 576
DI 10.1126/science.1220476
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 935DJ
UT WOS:000303498800041
PM 22556248
ER
PT J
AU Munroe, TA
AF Munroe, Thomas A.
TI The spotted flounder, Azygopus flemingi Nielsen 1961 (Pisces:
Pleuronectiformes: Rhombosoleidae), from deep waters off New Zealand: a
second valid species of Azygopus Norman 1926, with notes on
distribution, size, maturity, and ecology
SO ZOOTAXA
LA English
DT Article
DE rhombosoleid flatfish; taxonomy; New Zealand endemic fishes; deep-sea
flatfish; species re-description; squamation; scale morphology; Azygopus
pinnifasciatus; sexual dimorphism
ID DEMERSAL FISH ASSEMBLAGES
AB Since its description, Azyygopus Norman, 1926 was considered by subsequent authors to be a monotypic genus in the Order Pleuronectiformes comprised only of A. pinnifasciatus Norman, 1926, known from deep waters (90-900 m, usually 200-600 m) off the southern and southeastern coasts of Australia. In 1961, a subspecies, A. pinnifasciatus flemingi Nielsen, was described based on three specimens collected at 610 m in the Tasman Sea off the South Island, New Zealand. From its description to contemporary literature evaluating its status, recognition of A. p. flemingi as a distinct taxon has been rejected by all but two studies reporting on Azygopus from New Zealand waters. Until the late 20th century, specimens of Azygopus had been rarely collected off New Zealand and little was known about these fishes. Over the past 25 years, collecting by scientific expeditions and expanding deep-sea fisheries have captured over 195 specimens of Azygopus from a variety of deep-sea locations around New Zealand. Recently-captured specimens of Azygopus collected around New Zealand and deposited in fish collections have been identified as either A. pinnifasciatus Norman or A. flemingi Nielsen, suggesting the possibility that two species of Azygopus occur in New Zealand waters. This study examined the holotype, a paratype, and 25 non-type specimens of A. pinnifasciatus collected off Australia, and the most comprehensive series of specimens of Azygopus collected from New Zealand waters. These specimens included the holotype and two paratypes of A. p. flemingi and 191 other specimens collected from throughout the entire depth range (153-942 m) and representing wide coverage of geographic areas around New Zealand where Azygopus have been collected. Comparisons of these specimens indicate that a second species, A. flemingi Nielsen, should be recognized in the genus Azygopus, and that this species is the only member of this genus occurring in New Zealand waters. Azygopus flemingi is readily distinguished from A. pinnifasciatus by conspicuous differences in ocular-and blind-side color patterns, in numbers of ocular-side pelvic-fin rays, total vertebrae, lateral-line scales, and gillrakers on the first gill arch, morphology of blind-side scales and squamation patterns, length of blind-side pectoral fins, presence/absence of scales between upper jaw and ventral margin of lower eye, and pigment patterns on dorsal and anal fins of adults. Adult A. flemingi and A. pinnifasciatus are sexually dimorphic in several features. Data on maximum size and size at maturity, and depth of occurrence are summarized for A. flemingi.
C1 NMFS NOAA, Smithsonian Inst, Natl Systemat Lab, NHB, Washington, DC 20013 USA.
RP Munroe, TA (reprint author), NMFS NOAA, Smithsonian Inst, Natl Systemat Lab, NHB, POB 37012,WC 57,MRC 153, Washington, DC 20013 USA.
EM munroet@si.edu
FU NMNZ Te Papa; NZ Foundation for Research Science and Technology through
the Te Papa Biosystematics of NZ EEZ Fishes within NIWA's Marine
Biodiversity and Biosecurity OBI [C01X0502]
FX I thank members of the fish group at the Museum of New Zealand Te Papa
for their kind hospitality and assistance during my visits to the fish
collection. C. Struthers and A. Stewart located data and references and
retrieved catalogue information for specimens of A. flemingi curated at
NMNZ; R. Crec'hriou (formerly NMNZ) and J. Barker (NMNZ) provided
radiographs. The author also extends his gratitude to the following
individuals for their assistance with obtaining data and other
information that greatly improved the scope of this study: M. McGrouther
and A. Hay (AMS) assisted with information on type specimens, provided
the photograph and radiograph of the holotype of A. pinnifasciatus, and
also arranged for loan of specimens from the fish collection at AMS; D.
Bray (NMV) arranged for loan of specimens of A. pinnifasciatus; M.
Lockett (AMS) examined color details and provided counts and
measurements of the holotype of A. pinnifasciatus; P. Moller (ZMUC)
provided counts, measurements, radiograph, and photograph of the
holotype of A. flemingi; G. Shinohara (NSMT) provided catalogue
information and radiographs of specimens curated at NSMT; J. Nielsen
(ZMUC) provided comments regarding taxonomic decisions made in the
original description of A. pinnifasciatus flemingi; T. Trinski provided
catalogue information for specimens curated at the Auckland Museum fish
collection. Color photographs of fishes used in this study were kindly
provided by C. Struthers (NMNZ Te Papa), M. Allen and M. McGrouther
(AMS). M. Freeborn (NMNZ) provided illustrations used in the manuscript.
C. Struthers and M. Nizinski (NMFS/National Systematics Laboratory)
assisted with preparation of figures. C. Struthers prepared the
distribution map. M. Francis, NIWA, provided information on abundance
from the Ministry of Fisheries research trawl database. K. Graham,
Research Associate, AMS, provided information on A. pinnifasciatus
distribution and abundance off southeastern Australia. A. Stewart
provided helpful comments in his review of a preliminary draft of the
manuscript. The author extends his appreciation to C. Roberts, NMNZ Te
Papa, for his continued support and for kindly arranging funding to help
support this study which was conducted at the Museum of New Zealand Te
Papa. Partial financial support for this work was provided by the NZ
Foundation for Research Science and Technology through the Te Papa
Biosystematics of NZ EEZ Fishes subcontract within NIWA's Marine
Biodiversity and Biosecurity OBI program (contract C01X0502). Thanks to
all investigators who retained specimens during their survey work.
NR 27
TC 1
Z9 1
U1 1
U2 1
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD MAY 2
PY 2012
IS 3297
BP 1
EP 33
PG 33
WC Zoology
SC Zoology
GA 940JE
UT WOS:000303885000001
ER
PT J
AU Urashima, T
Asakuma, S
Leo, F
Fukuda, K
Messer, M
Oftedal, OT
AF Urashima, Tadasu
Asakuma, Sadaki
Leo, Fiame
Fukuda, Kenji
Messer, Michael
Oftedal, Olav T.
TI The Predominance of Type I Oligosaccharides Is a Feature Specific to
Human Breast Milk
SO ADVANCES IN NUTRITION
LA English
DT Article; Proceedings Paper
CT 1st International Conference on Glycobiology of Human Milk
Oligosaccharides
CY MAY 16-17, 2011
CL Copenhagen, DENMARK
ID BIFIDOBACTERIUM-LONGUM; HUMAN COLOSTRUM; FED BABIES; LACTATION;
SIALYLOLIGOSACCHARIDES; QUANTIFICATION; DERIVATIZATION; CHROMATOGRAPHY;
DEGRADATION; SIALYL
AB Human milk and colostrum contain similar to 12-13 g/L and similar to 22-24 g/L of oligosaccharides, respectively. The chemical structures of >100 human milk oligosaccharides (HMO) have been characterized to date. We determined the concentrations of 10 neutral and 9 acidic colostrum HMO collected during the first 3 d of lactation by using reverse phase HPLC after derivatization with 2-aminopyridine or 1-methyl-3-phenyl-5-pyrazolon. The predominant oligosaccharides were Fuc(alpha 1-2)Gal(beta 1-4Glc (2'-FL), Fuc(alpha 1-2)Gal(beta 1-3)GlcNAc(beta 1-3)Gal(beta 1-4)Glc (LNFP I), Fuc(alpha 1-2)Gal(beta 1-3)Fuc(alpha 1-4)]GlcNAc(beta 1-3)Gal(beta 1-4)Glc (LNDFH I), and Gal(beta 1-3)GlcNAc(beta 1-3)Gal(beta 1-4)Glc (LNT), the concentration of each of which was similar to 1-3 g/L. Because these HMO, other than 2'-FL, all contain the Lacto-N-biose type I structure [Gal(beta 1-3)GlcNAc], we conclude that HMO containing the type I structure predominate over those containing the N-acetyllactosamine type II structure [Gal(beta 1-4)GlcNAc]. This appears to be a feature that is specific to humans, because the milk and colostrum of other species, including apes and monkeys, either contain only type II oligosaccharides or type II predominate over type I. It is possible that type I HMO may have importance as substrates for beneficial bifidobacteria in breast-fed infants. The biological importance of type I HMO predominance warrants further study, both in relation to human health and to human evolution. Adv. Nutr. 3: 473S-482S, 2012.
C1 [Urashima, Tadasu; Fukuda, Kenji] Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 080, Japan.
[Asakuma, Sadaki] Natl Agr Res Ctr Hokkaido Reg, Sapporo, Hokkaido, Japan.
[Messer, Michael] Univ Sydney, Sch Mol & Microbial Biosci, Sydney, NSW 2006, Australia.
[Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Urashima, T (reprint author), Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 080, Japan.
EM urashima@obihiro.ac.jp
NR 42
TC 41
Z9 41
U1 2
U2 20
PU AMER SOC NUTRITION-ASN
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 2161-8313
J9 ADV NUTR
JI Adv. Nutr.
PD MAY
PY 2012
VL 3
IS 3
BP 473S
EP 482S
DI 10.3945/an.111.001412
PG 10
WC Nutrition & Dietetics
SC Nutrition & Dietetics
GA 066KP
UT WOS:000313220000028
PM 22585927
ER
PT J
AU Ryder, TB
Fleischer, RC
Shriver, WG
Marra, PP
AF Ryder, Thomas B.
Fleischer, Robert C.
Shriver, W. Greg
Marra, Peter P.
TI The ecological-evolutionary interplay: density-dependent sexual
selection in a migratory songbird
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Density; extra-pair paternity; sexual selection; urbanization
ID EXTRA-PAIR PATERNITY; MATING SYSTEMS; GREAT TITS; BODY SIZE;
REPRODUCTIVE SUCCESS; AGELAIUS-PHOENICEUS; NATURAL-SELECTION; FEMALE
CHOICE; PARUS-MAJOR; DNA MARKERS
AB Little is understood about how environmental heterogeneity influences the spatial dynamics of sexual selection. Within human-dominated systems, habitat modification creates environmental heterogeneity that could influence the adaptive value of individual phenotypes. Here, we used the gray catbird to examine if the ecological conditions experienced in the suburban matrix (SM) and embedded suburban parks (SP) influence reproductive strategies and the strength of sexual selection. Our results show that these habitats varied in a key ecological factor, breeding density. Moreover, this ecological factor was closely tied to reproductive strategies such that local breeding density predicted the probability that a nest would contain extra-pair offspring. Partitioning reproductive variance showed that while within-pair success was more important in both habitats, extra-pair success increased the opportunity for sexual selection by 39% at higher breeding densities. Body size was a strong predictor of relative reproductive success and was under directional selection in both habitats. Importantly, our results show that the strength of sexual selection did not differ among habitats at the landscape scale but rather that fine-scale variation in an ecological factor, breeding density, influenced sexual selection on male phenotypes. Here, we document density-dependent sexual selection in a migratory bird and hypothesize that coarse-scale environmental heterogeneity, in this case generated by anthropogenic habitat modification, changed the fine-scale ecological conditions that drove the spatial dynamics of sexual selection.
C1 [Ryder, Thomas B.; Marra, Peter P.] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA.
[Fleischer, Robert C.] Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA.
[Shriver, W. Greg] Univ Delaware, Dept Entomol & Wildlife Ecol, Newark, DE 19716 USA.
RP Ryder, TB (reprint author), Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA.
EM rydert@si.edu
FU Pedigree; Maryland Ornithological Society
FX Funded by the Pedigree and Maryland Ornithological Society.
NR 89
TC 13
Z9 14
U1 4
U2 57
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD MAY
PY 2012
VL 2
IS 5
BP 976
EP 987
DI 10.1002/ece3.254
PG 12
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA 055WE
UT WOS:000312447700010
PM 22837842
ER
PT J
AU De Leon, LF
Rolshausen, G
Bermingham, E
Podos, J
Hendry, AP
AF De Leon, Luis Fernando
Rolshausen, Gregor
Bermingham, Eldredge
Podos, Jeffrey
Hendry, Andrew P.
TI Individual specialization and the seeds of adaptive radiation in
Darwin's finches
SO EVOLUTIONARY ECOLOGY RESEARCH
LA English
DT Article
DE adaptive radiation; Darwin's finches; ecological speciation; Galapagos;
individual specialization; intraspecific competition; niche variation
ID GALAPAGOS GROUND FINCHES; ECOLOGICAL SPECIATION; DISRUPTIVE SELECTION;
NICHE EXPANSION; DIET VARIATION; RESOURCE SPECIALIZATION; SYMPATRIC
SPECIATION; NATURAL-POPULATIONS; EXTERNAL MORPHOLOGY; GEOSPIZA-FORTIS
AB Background: Empirical and theoretical studies suggest that individual specialization can he an important force in evolutionary diversification. However, few studies of natural populations have explicitly considered the impact of individual specialization on adaptive divergence.
Questions: To what extent do individuals within a bimodal Darwin's finch population specialize on different resources? Is this individual specialization likely to enhance adaptive divergence?
Field site: El Garrapatero, Santa Cruz Island. Galapagos. Ecuador.
Organism: A population of the medium ground finch, Geospiza fortis. showing large - and bimodal - morphological and genetic variation resulting from ecologically based adaptive divergence.
Methods: We described the diets of individual G. fortis through feeding observations in the wild. We calculated several indices of individual specialization. We then examined the relationship between individual specialization, adaptive morphological traits (beak and head dimensions), and neutral genetic variation (microsatellites). We also performed a cluster analysis on the basis of individual foraging observations and asked whether the clusters were morphologically and genetically divergent.
Results: We found significant levels of individual specialization and expected, but weak, associations between individual diet differences, morphological traits, and neutral genetic variation. The cluster analysis yielded two distinct diet-clusters of individuals that differed in morphological traits but not in neutral genetic markers. In the early stages of adaptive radiation, individual specialization appears to be associated with morphological divergence but not neutral genetic divergence.
C1 [Rolshausen, Gregor] INDICASAT AIP, Inst Invest Cient & Serv Alta Tecnol AIP, Panama City 5, Panama.
[De Leon, Luis Fernando; Rolshausen, Gregor; Hendry, Andrew P.] McGill Univ, Redpath Museum, Montreal, PQ H3A 2K6, Canada.
[De Leon, Luis Fernando; Rolshausen, Gregor; Hendry, Andrew P.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
[De Leon, Luis Fernando; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama.
[Podos, Jeffrey] Univ Massachusetts, Dept Biol, Amherst, MA 01003 USA.
RP De Leon, LF (reprint author), INDICASAT AIP, Inst Invest Cient & Serv Alta Tecnol AIP, POB 0843-01103, Panama City 5, Panama.
EM luis.deleonreyna@gmail.com
FU Secretaria Nacional de Ciencia, Tecnologia e Innovacion; Institut par la
Formacion y Aprovechamiento de los Recursos Humanos, Panama; US National
Science Foundation; Natural Sciences and Engineering Research Council of
Canada; Smithsonian Tropical Research Institute
FX The Galapagos National Park Service and the Charles Darwin Research
Station provided logistical support and permits. E. Hilton, M.
Rossi-Santos, D. Ruiz. A. Gabela, P. Kelley, M. Hendry, S. Huber. K.
Huyghe, B. Vanhooydonck, and D. Delaney provided field assistance. J.
Racymaekers provided useful suggestions for data analysis. D. Sharpe
provided useful comments on an earlier version of the manuscript.
Funding was provided by the Secretaria Nacional de Ciencia, Tecnologia e
Innovacion and the Institut par la Formacion y Aprovechamiento de los
Recursos Humanos, Panama (L.F. De Leon); the US National Science
Foundation (J. Podos); the Natural Sciences and Engineering Research
Council of Canada (A.P. Hendry); and the Smithsonian Tropical Research
Institute (E. Bermingham). We thank the associated editor and anonymous
reviewers for providing valuable comments on an earlier version of the
manuscript.
NR 76
TC 4
Z9 4
U1 22
U2 119
PU EVOLUTIONARY ECOLOGY LTD
PI TUCSON
PA UNIV ARIZONA, 321 BIOSCIENCES WEST, TUCSON, AZ 85721 USA
SN 1522-0613
EI 1937-3791
J9 EVOL ECOL RES
JI Evol. Ecol. Res.
PD MAY
PY 2012
VL 14
IS 4
BP 365
EP 380
PG 16
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 055JX
UT WOS:000312413300002
ER
PT J
AU Launius, RD
Conway, EM
Johnston, AK
Wang, ZC
Hersch, MH
Paikowsky, D
Whalen, DJ
Toldi, E
Dougherty, K
Hays, PL
Levasseur, J
McNutt, RL
Sherwood, B
AF Launius, Roger D.
Conway, Erik M.
Johnston, Andrew K.
Wang, Zse Chien
Hersch, Matthew H.
Paikowsky, Deganit
Whalen, David J.
Toldi, Eric
Dougherty, Kerrie
Hays, Peter L.
Levasseur, Jennifer
McNutt, Ralph L., Jr.
Sherwood, Brent
TI Spaceflight: The Development of Science, Surveillance, and Commerce in
Space
SO PROCEEDINGS OF THE IEEE
LA English
DT Article
DE Cold War; communications satellites; earth science; human presence in
space; lunar science; national security; navigation and positioning;
remote sensing; solar science; solar system; spaceflight
ID OUTER SOLAR-SYSTEM
AB To commemorate the centennial of the PROCEEDINGS OF THE IEEE, several authors from diverse areas of expertise examine space exploration from its beginnings in the middle of the last century and look onward to half a century in the future. Beginning by examining the reasons why the two 20th century superpowers believed that space exploration was an important investment, the chronological review of early developments includes discussions on science, commerce, and national security; the evolution of space-related technologies; progress and advancements in launch vehicles, spacecraft, and spacecraft payloads; and improvements in space communications and tracking. With the subjects of robotic solar system exploration and crewed missions to space discussed in some detail, the great advances of the last 60 years establish a foundation for addressing the challenges of future human flight beyond Earth's vicinity-challenges that are technical, political, social, and economic in nature. The authors take a pragmatic view in making forecasts for the future of spaceflight: they limit their conjecture, for the most part, to the next 50 years. While it is very difficult to make realistic predictions for longer periods, the authors are confident that space exploration continues to grasp the public's imagination and desire to know more about the universe, and that it continues to build on many of the same questions that inspired the space program in the mid-20th century.
C1 [Launius, Roger D.; Johnston, Andrew K.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
[Sherwood, Brent] CALTECH, Jet Prop Lab, Innovat Foundry, Pasadena, CA 91109 USA.
[Hersch, Matthew H.] Univ Penn, Philadelphia, PA 19104 USA.
[Paikowsky, Deganit] Tel Aviv Univ, IL-69978 Tel Aviv, Israel.
[Whalen, David J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
[Dougherty, Kerrie] Powerhouse Museum, Sydney, NSW 1238, Australia.
[Hays, Peter L.] SAIC Inc, Washington, DC 20005 USA.
[McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
EM LauniusR@si.edu
RI McNutt, Ralph/E-8006-2010
OI McNutt, Ralph/0000-0002-4722-9166
FU National Aeronautics and Space Administration
FX This paper was prepared in part with the support of the National
Aeronautics and Space Administration.
NR 69
TC 3
Z9 3
U1 1
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9219
J9 P IEEE
JI Proc. IEEE
PD MAY
PY 2012
VL 100
SI SI
BP 1785
EP 1818
DI 10.1109/JPROC.2012.2187143
PG 34
WC Engineering, Electrical & Electronic
SC Engineering
GA 020TR
UT WOS:000309838000061
ER
PT J
AU Catlos, E
Jacob, L
Oyman, T
Sorensen, S
AF Catlos, Elizabeth
Jacob, Lauren
Oyman, Tolga
Sorensen, Sorena
TI LONG-TERM EXHUMATION OF AN AEGEAN METAMORPHIC CORE COMPLEX GRANITOIDS IN
THE NORTHERN MENDERES MASSIF, WESTERN TURKEY
SO AMERICAN JOURNAL OF SCIENCE
LA English
DT Article
DE Zircon geochronology; cathodoluminescence; Menderes Massif; granitoid;
western Turkey; subduction
ID U-TH-PB; EASTERN MEDITERRANEAN REGION; HELLENIC SUBDUCTION ZONE;
EXTENSIONAL TECTONICS; ANATOLIDE BELT; TRACE-ELEMENT; GEOCHEMICAL
CLASSIFICATION; CONTINENTAL EXTENSION; NORTHWESTERN ANATOLIA; TERTIARY
EXTENSION
AB The Egrigoz, Koyunoba, and Alacam plutons are located in the northern portion of the Menderes Massif, a region characterized today by large-scale extension. To gain a better understanding of their exhumation history, we acquired zircon ages, geochemical analyses, and cathodoluminescence (CL) images to search for evidence of micro- to macro-scales of deformation. The combination is a powerful means to decipher their tectonomagmatic history. In situ ion microprobe U-238/Pb-206 zircon ages of the granitoids range from 30.0 +/- 3.9 Ma to 14.7 +/- 2.6 Ma (+/-1 sigma) and indicate the plutons crystallized over similar to 15 m.y. The dated zircons show CL zoning consistent with igneous crystallization and are only located adjacent to or as inclusions in biotite grains The youngest ages are dominated by a blue color in CL, whereas a majority of older zircons are yellow. Higher Th/U contents are typically shown by zircons with black or dark green colors in CL. Most of the samples of these granitoids indicate they are magnesian, calc-alkalic and peraluminous granite to granodiorites, but variations exist, likely reflecting heterogeneity caused by magma mixing, partial melting, crustal contamination, and post-emplacement fluid interactions as evidenced by the CL images. CL images show that all samples experienced magma mixing, multiple episodes of brittle deformation, and fluid-mediated alteration. Sources for the generation of Northern Menderes Massif granitoids include simple slab induced upwelling from the subduction of the African plate along the Hellenic arc, adiabatic decompression as the northern edge of Turkey's Anatolide-Tauride block delaminates, and upwelling asthenosphere as the continental lithosphere thins during extension. We present a model in which western Turkey is an amalgamation of stacked subduction zones that transition from north to south over time. Northern Menderes Massif granitoids document their complex geologic history in their ages, chemistry, and textures.
C1 [Catlos, Elizabeth] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA.
[Jacob, Lauren] Apache Corp, Houston, TX 77056 USA.
[Oyman, Tolga] Dokuz Eylul Univ, Fac Engn, Dept Geol Engn, TR-35160 Izmir, Turkey.
[Sorensen, Sorena] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA.
RP Catlos, E (reprint author), Univ Texas Austin, Dept Geol Sci, 1 Univ Stn C1100, Austin, TX 78712 USA.
EM ejcatlos@gmail.com
RI Catlos, Elizabeth/B-7943-2011;
OI Oyman, Tolga/0000-0003-2132-2511
FU National Science Foundation [0937254]; Jackson School of Geosciences;
Smithsonian Institution's National Museum of Natural History Fellowship
program
FX This material is based upon work supported by the National Science
Foundation under Grant No. 0937254. Additional funding was provided by
the Jackson School of Geosciences. Samples were obtained with the help
of Drs. Yasar Kibici, Ibrahim Cemen, and Mehmet Demirbilek and students
Okan Yildiz, Ozge Karaman, and Esra Yalcin. Comments from Drs. Mark
Cloos, Dan Barker, Stuart Thomson, and Seth Kruckenberg, greatly
improved the original manuscript. The authors thank the UCLA National
Ion Microprobe Facility (particularly Drs. Rita Economos and Axel
Schmitt), which is partially supported by funding from the National
Science Foundation's Instrumentation and Facilities Program. Ages were
obtained with the help of Jackson School students Kathryn Huber and Tim
Shin. Thin section scale CL imagery was generated with the support of
the Smithsonian Institution's National Museum of Natural History
Fellowship program. Some figures were drafted with the assistance of
Karen Black.
NR 129
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Z9 5
U1 2
U2 11
PU AMER JOURNAL SCIENCE
PI NEW HAVEN
PA YALE UNIV, PO BOX 208109, NEW HAVEN, CT 06520-8109 USA
SN 0002-9599
EI 1945-452X
J9 AM J SCI
JI Am. J. Sci.
PD MAY
PY 2012
VL 312
IS 5
BP 534
EP 571
DI 10.2475/05.2012.03
PG 38
WC Geosciences, Multidisciplinary
SC Geology
GA 990II
UT WOS:000307623800003
ER
PT J
AU Rondeau, B
Cenki-Tok, B
Fritsch, E
Mazzero, F
Gauthier, JP
Bodeur, Y
Bekele, E
Gaillou, E
Ayalew, D
AF Rondeau, Benjamin
Cenki-Tok, Benedicte
Fritsch, Emmanuel
Mazzero, Francesco
Gauthier, Jean-Pierre
Bodeur, Yves
Bekele, Eyassu
Gaillou, Eloise
Ayalew, Dereje
TI Geochemical and petrological characterization of gem opals from Wegel
Tena, Wollo, Ethiopia: opal formation in an Oligocene soil
SO GEOCHEMISTRY-EXPLORATION ENVIRONMENT ANALYSIS
LA English
DT Article
DE opal formation; Ethiopia; pedogenesis; plant fossils; chemical
impurities
ID NEUTRON-ACTIVATION ANALYSIS; OF-COLOR OPAL; TRACE-ELEMENTS; ICP-MS;
FELDSPAR; URANIUM; EARTH
AB Gem opals from Wegel Tena, Wollo Province, Ethiopia, occur in Oligocene rhyolitic ignimbrites. They display a unique geochemistry, with some samples yielding the highest Ba concentrations ever recorded. They are generally much richer in chemical impurities than opals from other localities. For example, the sum Al+Fe or the sum Na+Mg+Ca+K+Ba are often higher. These geochemical features make them easy to distinguish from other opals worldwide. We observed strong geochemical variations and some good positive correlations in our samples, such as Al+Fe vs. Na+Mg+Ca+K+Ba, Al vs Ca, or Ba vs Ca. This shows that the crystallography of opal has controlled, at least in part, the incorporation of chemical impurities, although opal is not well-crystallized. In addition, the multimodal distributions of several chemical impurities (e.g. U vs Sr, Al vs Ca, Ba vs Ca, etc.) suggest at least two origins of silica: weathering of feldspars and weathering of volcanic glass. In addition, opals from Wegel Tena contain numerous well-preserved microscopic plant fossils. Moreover, their host rock exhibits features typical of pedogenesis (abundant clays, desiccation cracks, and grain size sorting). We propose that the opals at Wegel Tena formed during the Oligocene period when volcanic emissions stopped for a time long enough to allow weathering of ingimbrites and therefore liberation of silica. This accompanied the formation of soil and development of plant life, and some plants were trapped in opal.
C1 [Rondeau, Benjamin; Bodeur, Yves] Univ Nantes, Lab Planetol & Geodynam, UMR CNRS 6112, F-44322 Nantes 3, France.
[Cenki-Tok, Benedicte] Univ Bern, Inst Geol, CH-3012 Bern, Switzerland.
[Fritsch, Emmanuel] Univ Nantes, Inst Mat Jean Rouxel, UMR CNRS 6205, F-44322 Nantes 3, France.
[Mazzero, Francesco] Opalinda, F-75002 Paris, France.
[Gauthier, Jean-Pierre] Ctr Rech Gemmol, F-44322 Nantes 3, France.
[Bekele, Eyassu] Eyaopal, Addis Ababa, Ethiopia.
[Gaillou, Eloise] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
[Ayalew, Dereje] Univ Addis Ababa, Dept Earth Sci, Addis Ababa, Ethiopia.
RP Rondeau, B (reprint author), Univ Nantes, Lab Planetol & Geodynam, UMR CNRS 6112, 2 Rue Houssiniere,BP 92208, F-44322 Nantes 3, France.
EM benjamin.rondeau@univ-nantes.fr
RI Gaillou, Eloise/D-1753-2009
OI Gaillou, Eloise/0000-0002-7949-268X
FU Swiss National Fond [200021-103479/1]
FX BCT thanks T. Pettke for assistance during LA-ICP-MS analyses. The
electron microprobe at the University of Bern is partly funded by the
Swiss National Fond (Grant 200021-103479/1). SEM maps were acquired
thanks to the help of Nicolas Stephant and Stephane Grolleau, IMN. We
thank Thomas Cenki for collecting the samples studied here. We thank
Antoine Bezos for constructive discussions on the interpretation of
chemical analyses. This article has been considerably strengthened and
clarified, thanks to Alan Pring, Lee Groat and John Carranza who
reviewed it.
NR 31
TC 2
Z9 2
U1 5
U2 13
PU GEOLOGICAL SOC PUBL HOUSE
PI BATH
PA UNIT 7, BRASSMILL ENTERPRISE CENTRE, BRASSMILL LANE, BATH BA1 3JN, AVON,
ENGLAND
SN 1467-7873
J9 GEOCHEM-EXPLOR ENV A
JI Geochem.-Explor. Environ. Anal.
PD MAY
PY 2012
VL 12
IS 2
BP 93
EP 104
DI 10.1144/1467-7873/10-MINDEP-058
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 983KU
UT WOS:000307119000002
ER
PT J
AU Hinson, DP
Wang, HQ
Smith, MD
AF Hinson, David P.
Wang, Huiqun
Smith, Michael D.
TI A multi-year survey of dynamics near the surface in the northern
hemisphere of Mars: Short-period baroclinic waves and dust storms
SO ICARUS
LA English
DT Article
DE Mars, Atmosphere; Mars, Climate; Atmospheres, Dynamics; Meteorology
ID ASYNOPTIC SATELLITE-OBSERVATIONS; WESTERN BOUNDARY CURRENTS; TES NADIR
DATA; MARTIAN ATMOSPHERE; GLOBAL SURVEYOR; SPECTRAL-ANALYSIS; ORBITER
CAMERA; THERMAL TIDES; MGS TES; INTERANNUAL VARIABILITY
AB Baroclinic waves figure prominently in the dynamics of the northern hemisphere of Mars, and extensive observations by the Viking Landers and two atmospheric sounders on Mars Global Surveyor have revealed many of their basic properties. However, previous investigations considered these data sets individually, so that their cumulative value is not fully appreciated. We have re-examined these data to extract new information about the dynamics near the surface at mid-to-high northern latitudes. By applying the same method of spectral analysis to each type of observation, we derive a uniform, multi-year characterization of basic elements of martian weather. This survey documents the time evolution of baroclinic waves among modes with different periods and zonal wave numbers. We devote particular attention to a recurring "wave-3 mode", which is distinguished by its capacity to initiate regional dust storms in the topographic basins of the northern hemisphere. Our results include a detailed case study that shows how the intermittence of this mode and the strong zonal modulation of its amplitude influence the timing and location of these distinctive "flushing" dust storms. More generally, we find that the properties of the wave-3 mode are largely the same whenever it appears and that its intermittence plays an important role in the annual dust cycle. (c) 2012 Elsevier Inc. All rights reserved.
C1 [Hinson, David P.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Hinson, David P.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
[Wang, Huiqun] Smithsonian Astrophys Observ, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Smith, Michael D.] NASA, Planetary Syst Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hinson, DP (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM dhinson@seti.org
FU NASA of the Mars Data Analysis Program [NNX08AL24G]
FX Funding for this research was provided by NASA under Grant NNX08AL24G
(Hinson) of the Mars Data Analysis Program.
NR 54
TC 11
Z9 11
U1 1
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAY
PY 2012
VL 219
IS 1
BP 307
EP 320
DI 10.1016/j.icarus.2012.03.001
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 975WA
UT WOS:000306541000029
ER
PT J
AU McGuire, KL
Fierer, N
Bateman, C
Treseder, KK
Turner, BL
AF McGuire, Krista L.
Fierer, Noah
Bateman, Carling
Treseder, Kathleen K.
Turner, Benjamin L.
TI Fungal Community Composition in Neotropical Rain Forests: the Influence
of Tree Diversity and Precipitation
SO MICROBIAL ECOLOGY
LA English
DT Article
ID SOIL MICROBIAL COMMUNITIES; LITTER DECOMPOSITION; ECOSYSTEM FUNCTION;
MYCORRHIZAL FUNGI; TROPICAL FORESTS; DISTRIBUTIONAL PATTERNS;
ENVIRONMENTAL-SAMPLES; SPECIES-DIVERSITY; PLANT DIVERSITY; BOREAL FOREST
AB Plant diversity is considered one factor structuring soil fungal communities because the diversity of compounds in leaf litter might determine the extent of resource heterogeneity for decomposer communities. Lowland tropical rain forests have the highest plant diversity per area of any biome. Since fungi are responsible for much of the decomposition occurring in forest soils, understanding the factors that structure fungi in tropical forests may provide valuable insight for predicting changes in global carbon and nitrogen fluxes. To test the role of plant diversity in shaping fungal community structure and function, soil (0-20 cm) and leaf litter (O horizons) were collected from six established 1-ha forest census plots across a natural plant diversity gradient on the Isthmus of Panama. We used 454 pyrosequencing and phospholipid fatty acid analysis to evaluate correlations between microbial community composition, precipitation, soil nutrients, and plant richness. In soil, the number of fungal taxa increased significantly with increasing mean annual precipitation, but not with plant richness. There were no correlations between fungal communities in leaf litter and plant diversity or precipitation, and fungal communities were found to be compositionally distinct between soil and leaf litter. To directly test for effects of plant species richness on fungal diversity and function, we experimentally re-created litter diversity gradients in litter bags with 1, 25, and 50 species of litter. After 6 months, we found a significant effect of litter diversity on decomposition rate between one and 25 species of leaf litter. However, fungal richness did not track plant species richness. Although studies in a broader range of sites is required, these results suggest that precipitation may be a more important factor than plant diversity or soil nutrient status in structuring tropical forest soil fungal communities.
C1 [McGuire, Krista L.; Bateman, Carling] Columbia Univ, Barnard Coll, New York, NY 10027 USA.
[Fierer, Noah] Univ Colorado, Boulder, CO 80309 USA.
[Treseder, Kathleen K.] Univ Calif Irvine, Irvine, CA USA.
[Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP McGuire, KL (reprint author), Columbia Univ, Barnard Coll, 3009 Broadway, New York, NY 10027 USA.
EM kmcguire@barnard.columbia.edu; noah.fierer@colorado.edu;
carling.bateman@gmail.com; treseder@uci.edu; turnerbl@si.edu
RI Turner, Benjamin/E-5940-2011; Treseder, Kathleen/E-5148-2011
OI Turner, Benjamin/0000-0002-6585-0722;
FU NSF Ecosystems [DEB-0640666]; Kearney Foundation
FX We thank Joe Wright and Osvaldo Calderon for collection and
identification of all litter species in the decomposition experiment.
Collecting and export permits were granted from the Autoridad Nacional
del Ambiente of Panama. Jenny Talbot and Angela Nguyen assisted with C
and N measurements, and Steve Allison and Donovan German helped with
extracellular enzyme assays and data interpretation. We also thank two
anonymous reviewers for helping to improve the quality and clarity of
the manuscript. This work was funded by NSF Ecosystems (DEB-0640666) and
the Kearney Foundation.
NR 61
TC 42
Z9 43
U1 9
U2 120
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0095-3628
J9 MICROB ECOL
JI Microb. Ecol.
PD MAY
PY 2012
VL 63
IS 4
BP 804
EP 812
DI 10.1007/s00248-011-9973-x
PG 9
WC Ecology; Marine & Freshwater Biology; Microbiology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology;
Microbiology
GA 970KM
UT WOS:000306127300010
PM 22080256
ER
PT J
AU Schiffbauer, JD
Laflamme, M
AF Schiffbauer, James D.
Laflamme, Marc
TI LAGERSTATTEN THROUGH TIME: A COLLECTION OF EXCEPTIONAL PRESERVATIONAL
PATHWAYS FROM THE TERMINAL NEOPROTEROZOIC THROUGH TODAY
SO PALAIOS
LA English
DT Editorial Material
ID BURGESS SHALE-TYPE; EDIACARAN ANIMAL EMBRYOS; SOFT-TISSUE PRESERVATION;
ENCYSTING PROTISTS; FOSSILIZED NUCLEI; CLAY-MINERALS; SOUTH CHINA; 1ST
FINDS; ORIGIN; ORDOVICIAN
C1 [Schiffbauer, James D.] Virginia Tech, Inst Crit Technol & Appl Sci, Nanoscale Characterizat & Fabricat Lab, Blacksburg, VA 24061 USA.
[Schiffbauer, James D.] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA.
[Laflamme, Marc] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20013 USA.
RP Schiffbauer, JD (reprint author), Virginia Tech, Inst Crit Technol & Appl Sci, Nanoscale Characterizat & Fabricat Lab, 1991 Kraft Dr, Blacksburg, VA 24061 USA.
EM jdschiff@vt.edu; LaflammeM@si.edu
NR 45
TC 8
Z9 8
U1 2
U2 24
PU SEPM-SOC SEDIMENTARY GEOLOGY
PI TULSA
PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA
SN 0883-1351
EI 1938-5323
J9 PALAIOS
JI Palaios
PD MAY-JUN
PY 2012
VL 27
IS 5-6
BP 275
EP 278
DI 10.2110/palo.2012.SO3
PG 4
WC Geology; Paleontology
SC Geology; Paleontology
GA 972UB
UT WOS:000306304900001
ER
PT J
AU Cardoso, P
Borges, PAV
Triantis, KA
Ferrandez, MA
Martin, JL
AF Cardoso, Pedro
Borges, Paulo A. V.
Triantis, Kostas A.
Ferrandez, Miguel A.
Martin, Jose L.
TI The underrepresentation and misrepresentation of invertebrates in the
IUCN Red List
SO BIOLOGICAL CONSERVATION
LA English
DT Letter
C1 [Cardoso, Pedro; Borges, Paulo A. V.; Triantis, Kostas A.] Univ Acores, Azorean Biodivers Grp CITA A, P-9700042 Angra Do Heroismo, Portugal.
[Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
[Triantis, Kostas A.] Univ Athens, Dept Ecol & Taxon, Fac Biol, Athens 11528, Greece.
[Ferrandez, Miguel A.] Soc Study & Conservat Spiders, Madrid, Spain.
[Martin, Jose L.] Canary Agcy Sustainable Dev & Climate Change, Santa Cruz De Tenerife, Canary Islands, Spain.
RP Cardoso, P (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, Rua Capitao Joao dAvila, P-9700042 Angra Do Heroismo, Portugal.
EM pcardoso@ennor.org
RI Borges, Paulo/B-2780-2008; Cardoso, Pedro/A-8820-2008
OI Borges, Paulo/0000-0002-8448-7623; Cardoso, Pedro/0000-0001-8119-9960
NR 3
TC 10
Z9 12
U1 1
U2 27
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0006-3207
J9 BIOL CONSERV
JI Biol. Conserv.
PD MAY
PY 2012
VL 149
IS 1
BP 147
EP 148
DI 10.1016/j.biocon.2012.02.011
PG 2
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 964UY
UT WOS:000305723400019
ER
PT J
AU Shlaer, B
Vilenkin, A
Loeb, A
AF Shlaer, Benjamin
Vilenkin, Alexander
Loeb, Abraham
TI Early structure formation from cosmic string loops
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE reionization; Cosmic strings; domain walls; monopoles; first stars; high
redshift galaxies
ID MICROWAVE-ANISOTROPY; REIONIZATION EPOCH; VACUUM STRINGS; EVOLUTION;
RADIATION; UNIVERSE; DENSITY
AB We examine the effects of cosmic strings on structure formation and on the ionization history of the universe. While Gaussian perturbations from inflation are known to provide the dominant contribution to the large scale structure of the universe, density perturbations due to strings are highly non-Gaussian and can produce nonlinear structures at very early times. This could lead to early star formation and reionization of the universe. We improve on earlier studies of these effects by accounting for high loop velocities and for the filamentary shape of the resulting halos. We find that for string energy scales G mu greater than or similar to 10(-7), the effect of strings on the CMB temperature and polarization power spectra can be significant and is likely to be detectable by the Planck satellite. We mention shortcomings of the standard cosmological model of galaxy formation which may be remedied with the addition of cosmic strings, and comment on other possible observational implications of early structure formation by strings.
C1 [Shlaer, Benjamin; Vilenkin, Alexander] Tufts Univ, Dept Phys & Astron, Inst Cosmol, Medford, MA 02155 USA.
[Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theoret & Comp, Cambridge, MA 02138 USA.
RP Shlaer, B (reprint author), Tufts Univ, Dept Phys & Astron, Inst Cosmol, 212 Coll Ave, Medford, MA 02155 USA.
EM shlaer@cosmos.phy.tufts.edu; vilenkin@cosmos.phy.tufts.edu;
aoeb@cfa.harvard.edu
FU NSF [AST-0907890, PHY-0855447]; NASA [NNX08AL43G, NNA09DB30A]
FX We thank Ken Olum and Xavier Siemens for helpful discussions. AL was
supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G
and NNA09DB30A. BS and AV were supported by NSF grant PHY-0855447. We
made use of the CAMB software package to generate the matter power
spectrum and CMB angular power spectra.
NR 81
TC 12
Z9 12
U1 0
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD MAY
PY 2012
IS 5
AR 026
DI 10.1088/1475-7516/2012/05/026
PG 29
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 960UA
UT WOS:000305415200027
ER
PT J
AU Alemseged, Z
Kiura, PW
Mbua, E
Njau, J
Pobiner, B
AF Alemseged, Zeresenay
Kiura, Purity W.
Mbua, Emma
Njau, Jackson
Pobiner, Briana
TI A platform for East African paleoanthropology: Third biannual conference
of the EAAPP
SO EVOLUTIONARY ANTHROPOLOGY
LA English
DT News Item
C1 [Alemseged, Zeresenay] Calif Acad Sci, Dept Anthropol, San Francisco, CA 94118 USA.
[Kiura, Purity W.] Natl Museums Kenya, Archaeol Sect, Nairobi, Kenya.
[Mbua, Emma] Natl Museums Kenya, Dept Earth Sci, Nairobi, Kenya.
[Njau, Jackson] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Pobiner, Briana] Smithsonian Inst, MRC 112, Washington, DC 20013 USA.
RP Alemseged, Z (reprint author), Calif Acad Sci, Dept Anthropol, 55 Mus Concourse Dr, San Francisco, CA 94118 USA.
EM zeray@calacademy.org
NR 2
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1060-1538
J9 EVOL ANTHROPOL
JI Evol. Anthropol.
PD MAY-JUN
PY 2012
VL 21
IS 3
BP 89
EP 91
DI 10.1002/evan.21309
PG 3
WC Anthropology
SC Anthropology
GA 962AN
UT WOS:000305511500002
PM 22900270
ER
PT J
AU Onofrio, R
AF Onofrio, Roberto
TI Gravitational vacuum polarization phenomena due to the Higgs field
SO EUROPEAN PHYSICAL JOURNAL C
LA English
DT Article
ID EQUIVALENCE PRINCIPLE; BEAM-BALANCE; CASIMIR FORCE; DIMENSIONS;
MILLIMETER; RESEARCHES
AB In the standard model the mass of elementary particles is considered as a dynamical property emerging from their interaction with the Higgs field. We show that this assumption implies peculiar deviations from the law of universal gravitation in its distance and mass dependence, as well as from the superposition principle. The experimental observation of the predicted deviations from the law of universal gravitation seems out of reach. However, we argue that a new class of experiments aimed at studying the influence of surrounding masses on the gravitational force-similar to the ones performed by Quirino Majorana almost a century ago-could be performed to test the superposition principle and to give direct limits on the presence of nonminimal couplings between the Higgs field and the spacetime curvature. From the conceptual viewpoint, the violation of the superposition principle for gravitational forces due to the Higgs field creates a conflict with the notion that gravitational potentials, as assumed in Newtonian gravitation or in post-Newtonian parameterizations of metric theories, are well-defined concepts to describe gravity in their non-relativistic limit.
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 45
TC 6
Z9 6
U1 0
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1434-6044
J9 EUR PHYS J C
JI Eur. Phys. J. C
PD MAY
PY 2012
VL 72
IS 5
AR 2006
DI 10.1140/epjc/s10052-012-2006-1
PG 8
WC Physics, Particles & Fields
SC Physics
GA 952GG
UT WOS:000304778800019
ER
PT J
AU Jenks, KE
Kitamura, S
Lynam, AJ
Ngoprasert, D
Chutipong, W
Steinmetz, R
Sukmasuang, R
Grassman, LI
Cutter, P
Tantipisanuh, N
Bhumpakphan, N
Gale, GA
Reed, DH
Leimgruber, P
Songsasen, N
AF Jenks, Kate E.
Kitamura, Shumpei
Lynam, Antony J.
Ngoprasert, Dusit
Chutipong, Wanlop
Steinmetz, Robert
Sukmasuang, Ronglarp
Grassman, Lon I., Jr.
Cutter, Passanan
Tantipisanuh, Naruemon
Bhumpakphan, Naris
Gale, George A.
Reed, David H.
Leimgruber, Peter
Songsasen, Nucharin
TI Mapping the distribution of dholes, Cuon alpinus (Canidae, Carnivora),
in Thailand
SO MAMMALIA
LA English
DT Article
DE Cuon alpinus; MaxEnt; maximum entropy modeling; Southeast Asia; species
distribution modeling
ID SPECIES DISTRIBUTIONS; SPATIAL ECOLOGY; CONSERVATION; PREDICTION;
PREDATION; WILDLIFE; INDIA; CATS
AB No recent attempt has been made to survey dhole distribution, or to estimate remaining population numbers. We surveyed 15 protected areas in Thailand with camera traps from 1996 to 2010. We used the photo locations of dholes (n = 96) in the maximum entropy (MaxEnt) model along with six environmental variables to model current dhole distribution, as well as species predictive occurrence layers for sambar, red muntjac, wild boar, tiger, and leopard. The MaxEnt model identified the predicted probability of the presence of leopards and sambar as positive and the most important variables in modeling dhole presence, indicating that maintaining a sufficient prey base may be the most important factor determining continued survival of dholes. Roughly 7% of the total land area in Thailand is potentially suitable for dholes. However, surveys to date have focused on protected areas, which make up just a third of the potential suitable areas for dholes. Only in four protected areas do they occur across the entire landscape, suggesting that in the majority of places where they occur, habitats are not uniformly suitable. Using the model, we identified several potential areas where dholes have not been reported, and therefore status surveys are needed, and where future research of the species might be focused.
C1 [Jenks, Kate E.] Univ Massachusetts, Grad Program Organism & Evolutionary Biol, Amherst, MA 01003 USA.
[Jenks, Kate E.] Univ Massachusetts, Grad Program Wildlife & Fisheries Conservat, Amherst, MA 01003 USA.
[Jenks, Kate E.; Leimgruber, Peter; Songsasen, Nucharin] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
[Kitamura, Shumpei] Museum Nat & Human Activ, Sanda, Hyogo 6691546, Japan.
[Lynam, Antony J.] Global Conservat Program, Wildlife Conservat Soc, Bronx, NY 10540 USA.
[Ngoprasert, Dusit; Chutipong, Wanlop; Tantipisanuh, Naruemon; Gale, George A.] King Mongkuts Univ Technol Thonburi, Sch Bioresources & Technol, Conservat Ecol Program, Bangkok 10140, Thailand.
[Steinmetz, Robert] World Wildlife Fund Nat Thailand, Bangkok 10900, Thailand.
[Sukmasuang, Ronglarp; Bhumpakphan, Naris] Kasetsart Univ, Fac Forestry, Dept Forest Biol, Bangkok 10900, Thailand.
[Grassman, Lon I., Jr.] Texas A&M Univ, Caesar Kleberg Wildlife Res Inst, Feline Res Ctr, Kingsville, TX 78363 USA.
[Cutter, Passanan] Univ Minnesota, Conservat Biol Program, St Paul, MN 55108 USA.
[Reed, David H.] Univ Louisville, Dept Biol, Louisville, KY 40292 USA.
RP Jenks, KE (reprint author), Univ Massachusetts, Grad Program Organism & Evolutionary Biol, 611 N Pleasant St, Amherst, MA 01003 USA.
EM kate@katejenks.info
RI Leimgruber, Peter/O-1304-2015;
OI Leimgruber, Peter/0000-0002-3682-0153; Lynam, Antony/0000-0002-8395-7902
FU Clouded Leopard Project; TRF/BIOTEC; Kasetsart University; Smithsonian
Conservation Biology Institute; Wildlife Conservation Society Thailand;
World Wide Fund for Nature - Thailand; Smithsonian Institution; National
Science Foundation; Association of Zoos and Aquariums Conservation
Endowment; Smithsonian Endowment Fund; Mahidol University; National
Center for Genetic Engineering and Biotechnology; Hornbill Research
Foundation; JSPS
FX This paper is dedicated to the memory of David H. Reed. We wish to thank
the Clouded Leopard Project, TRF/BIOTEC Special Program for Biodiversity
Research and Training Thailand, Kasetsart University, and the
Smithsonian Conservation Biology Institute for providing funding for the
initial conference that brought all the authors together to discuss
collaboration. We are grateful to the following institutions for
allowing us to use data collected under their auspices: the Wildlife
Conservation Society Thailand, World Wide Fund for Nature - Thailand,
and Smithsonian Institution. K. Jenks was supported by a National
Science Foundation Graduate Research Fellowship, Association of Zoos and
Aquariums Conservation Endowment Fund, and a Smithsonian Endowment Fund.
S. Kitamura was funded by the Mahidol University Government Research
Grant, the National Center for Genetic Engineering and Biotechnology,
the Hornbill Research Foundation, and a JSPS Research Fellowship. We
thank J.W. Duckworth and A. Wilting for their kind assistance in
identifying the carnivores in our data set. T. K. Fuller and two
anonymous reviewers provided helpful comments on earlier drafts of the
manuscript.
NR 47
TC 8
Z9 10
U1 4
U2 57
PU WALTER DE GRUYTER & CO
PI BERLIN
PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY
SN 0025-1461
J9 MAMMALIA
JI Mammalia
PD MAY
PY 2012
VL 76
IS 2
BP 175
EP 184
DI 10.1515/mammalia-2011-0063
PG 10
WC Zoology
SC Zoology
GA 957BV
UT WOS:000305134500007
ER
PT J
AU Kallal, RJ
Godfrey, SJ
Ortner, DJ
AF Kallal, R. J.
Godfrey, S. J.
Ortner, D. J.
TI Bone Reactions on a Pliocene Cetacean Rib Indicate Short-Term Survival
of Predation Event
SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY
LA English
DT Article
DE whale; neogene; lesions; periosteal reaction; trophic interaction
ID WHITE SHARK CARCHARODON; MARINE MAMMALS; SPERM-WHALES; ATTACK; LAMNIDAE;
BEHAVIOR; DOLPHIN; MARKS; PERU
AB There is little osteological evidence of non-lethal predation events in the archaeological or vertebrate paleontological record. A small section of Pliocene cetacean rib collected from the Yorktown Formation within the PCS Phosphate Mine (formerly Lee Creek Mine), Aurora, North Carolina, U.S.A., shows evidence of this kind of trophic interaction. In this case study, we offer a diagnosis of bone traumatic pathology in which three bone-forming lesions on the partial rib are interpreted as the reaction to a bite inflicted by a macro-predator, the first such report from a marine environment. In addition to the three well-defined lesions, a thin layer of woven bone covers much of the remaining cortical bone. The combination of the three bone-forming lesions and the thin layer of woven bone suggest the presence of an inflammatory process almost certainly caused by infection secondary to the trauma. Survival following the traumatic event was probably less than 6 weeks. The Neogene chondrichthyan fauna from this locality preserves several large predators, including Carcharocles megalodon, Carcharodon carcharias, Isurus xiphidon and Parotodus benedeni, which were all capable, at least in terms of their size, of having bitten the cetacean. Although most of the odontocetes known from the Yorktown Formation were too small to have inflicted this wound, some of the physeterids may have been large enough to have caused the lesions on the partial rib. This evidence of predation in Pliocene whale bone raises the possibility of similar lesions being found in whale bone recovered from archaeological sites. Copyright (c) 2010 John Wiley & Sons, Ltd.
C1 [Kallal, R. J.; Godfrey, S. J.] Calvert Marine Museum, Dept Paleontol, Solomons, MD 20688 USA.
[Ortner, D. J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA.
RP Godfrey, SJ (reprint author), Calvert Marine Museum, Dept Paleontol, POB 97, Solomons, MD 20688 USA.
EM Godfresj@co.cal.md.us
NR 51
TC 3
Z9 3
U1 1
U2 15
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1047-482X
EI 1099-1212
J9 INT J OSTEOARCHAEOL
JI Int. J. Osteoarchaeol.
PD MAY-JUN
PY 2012
VL 22
IS 3
BP 253
EP 260
DI 10.1002/oa.1199
PG 8
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA 951IO
UT WOS:000304714400001
ER
PT J
AU Onaga, H
Fiedler, GC
Baeza, JA
AF Onaga, Hitoshi
Fiedler, G. Curt
Baeza, J. Antonio
TI PROTANDRIC SIMULTANEOUS HERMAPHRODITISM IN PARHIPPOLYTE MISTICIA (CLARK,
1989) (CARIDEA: HIPPOLYTIDAE): IMPLICATIONS FOR THE EVOLUTION OF MIXED
SEXUAL SYSTEMS IN SHRIMP
SO JOURNAL OF CRUSTACEAN BIOLOGY
LA English
DT Article
DE Barbouridae; Lysmatidae; mating system; Parhippolyte; sex allocation;
sex ratio
ID LYSMATA-WURDEMANNI DECAPODA; MARINE SHRIMP; SOCIAL MONOGAMY;
EXHIPPOLYSMATA-OPLOPHOROIDES; ADAPTIVE SIGNIFICANCE;
REPRODUCTIVE-BIOLOGY; CARIBBEAN SEA; ALLOCATION; RECRUITMENT; CRUSTACEA
AB The sexual system of the shrimp Parhippolyte misticia (Clark, 1989), inhabiting the rocky subtidal at Okinawa, Japan and Kimbe Bay, Papua New Guinea, was examined. Dissections suggested that the population consisted of male phase (MP) and functional simultaneous euhermaphrodite (EH) individuals. MPs have cincinulli and appendices masculinae on the first and second pair of pleopods, respectively, gonopores located at the coxae of the third pair of walking legs, and ovotestes with a well-developed male portion containing sperm, but an undeveloped female portion. EHs lacked appendices masculinae and cincinulli. However, they have male gonopores and ovotestes with well-developed ovaries containing mature oocytes and testes with sperm. When EHs were maintained in pairs, both shrimp molted and spawned eggs which attached below the pleon and developed as embryos, demonstrating that EHs can reproduce as males and inseminate other Elis acting as females. These results demonstrate that P misticia is a protandric simultaneous hermaphrodite, as reported before for other shrimp of the genera Lysmata and Exhippolysmata. Also, these results suggest that protandric simultaneous hermaphroditism might have evolved more than once independently in shrimp from the diverse and species-rich Infraorder Caridea. Future research aimed at disentangling the phylogenetic relationship of Parhippolyte, Lysmata, Exhippolysmata and other closely related genera (Calliasmata, Lysmatella, Barbouria) and describing the sociobiology of additional representatives from the genera above is needed to understand the evolutionary history of sexual systems in caridean shrimp.
C1 [Baeza, J. Antonio] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA.
[Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
[Baeza, J. Antonio] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile.
[Onaga, Hitoshi; Fiedler, G. Curt] Univ Maryland, Univ Coll, Asia Div, USAG J Unit 45013, Zama Shi, Kanagawa 2280827, Japan.
RP Baeza, JA (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA.
EM baezaa@si.edu
OI Baeza, Juan Antonio/0000-0002-2573-6773
FU National Geographic Society; Smithsonian Marine Station (SMSFP, Fort
Pierce, Florida, USA); Smithsonian Tropical Research Institute (STRI,
Bocas del Toro, Panama)
FX Logistical support from James D. Reimer, Yoshikatsu Nakano, Yoshihisa
Fujita, Obushi Masami and Takuma Fujii at Okinawa and from Raphael
Ritson-Williams and Jimmy O'Donnell at Papua New Guinea, is deeply
appreciated by JAB. Logistic support from Mahonia na Dari and Walindi
Plantation Resort (and their staff members) at Papua New Guinea is
kindly acknowledged by JAB. This research was partially funded by a
Committee for Research and Exploration Grant of the National Geographic
Society (to JAB). JAB deeply thanks support from the Smithsonian Marine
Station (SMSFP, Fort Pierce, Florida, USA) Fellowship and Smithsonian
Tropical Research Institute (STRI, Bocas del Toro, Panama) Marine
Fellowship. This article is SMSFP contribution number 874.
NR 73
TC 6
Z9 8
U1 0
U2 7
PU CRUSTACEAN SOC
PI SAN ANTONIO
PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA
SN 0278-0372
EI 1937-240X
J9 J CRUSTACEAN BIOL
JI J. Crustac. Biol.
PD MAY
PY 2012
VL 32
IS 3
BP 383
EP 394
DI 10.1163/193724012X626520
PG 12
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 953AR
UT WOS:000304839800004
ER
PT J
AU Luque, J
Feldmann, RM
Schweitzer, CE
Jaramillo, C
Cameron, CB
AF Luque, Javier
Feldmann, Rodney M.
Schweitzer, Carrie E.
Jaramillo, Carlos
Cameron, Christopher B.
TI THE OLDEST FROG CRABS (DECAPODA: BRACHYURA: RANINOIDA) FROM THE APTIAN
OF NORTHERN SOUTH AMERICA
SO JOURNAL OF CRUSTACEAN BIOLOGY
LA English
DT Article
DE Albian; Aptian; body plan; Brachyura; Cretaceous; Neotropics; raninoid
crabs
ID MIDCRETACEOUS OCEAN CIRCULATION; CRETACEOUS ARCTIC-OCEAN; COON CREEK
FORMATION; ONTONG-JAVA PLATEAU; MODEL SIMULATION; UNION COUNTY;
CRUSTACEA; SURFACE; GREENHOUSE; MEXICO
AB Raninoida, also known as "frog crabs," is a clade of extant true crabs (Brachyura) characterized by a fusiform carapace (raninid-type), narrow thoracic sternum, pleon partially exposed dorsally, and paddle-like limbs, all of which are well suited to their cryptic burrowing lifestyle. However, the most basal raninoids from the Cretaceous were morphologically different, with ornamented carapaces that were wider than long (necrocarcinid-type), a broader thoracic sternum, and the pleon fitting between the legs assisted by pleonal locking mechanisms. During Albian times (similar to 112 to 99.6 Ma.) both body plans flourished worldwide. In contrast, pre-Albian (older than similar to 112 Ma.) fusiform families have not yet been reported. The discovery of Notopocorystes kerri n. sp., a fusiform crab from the upper Aptian (similar to 115 Ma.) of Colombia, South America, and the re-examination of Planocarcinus olssoni (Rathbun, 1937) n. comb., a necrocarcinidlike crab from the same age and locality, extend the record of the two body plans back into the Aptian of the equatorial Neotropics. Notopocorystes kerri is the oldest fusiform raninoid known to date, revealing that the morphological innovation of a fusiform carapace was already evolved in Raninoida before the rapid radiation experienced during Albian times. Our findings are suggestive of a still unresolved Palaeocorystidae, containing the rootstock for the post-Aptian Raninidae/Symethidae clade, with the most basal palaeocorystids lying in proximity to, and possibly derived from, a necrocarcinid-like ancestor.
C1 [Luque, Javier; Cameron, Christopher B.] Univ Montreal, Dept Sci Biol, Montreal, PQ H3C 3J7, Canada.
[Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa 084303092, Panama.
[Feldmann, Rodney M.] Kent State Univ, Dept Geol, Kent, OH 44242 USA.
[Schweitzer, Carrie E.] Kent State Univ Stark, Dept Geol, N Canton, OH 44720 USA.
RP Luque, J (reprint author), Univ Montreal, Dept Sci Biol, CP 6128, Montreal, PQ H3C 3J7, Canada.
EM javierluquec@gmail.com
OI Luque, Javier/0000-0002-4391-5951
FU American Museum of Natural History (AMNH); NSERC; Smithsonian Tropical
Research Institute (STRI)
FX We thank the Smithsonian Tropical Research Institute (STRI), and the
Lerner Gray Memorial Fund of the American Museum of Natural History
(AMNH) for providing (to JL) facilities and funds to allow the
development of the present research. Kecia Kerr (McGill University) for
the valuable field assistance and improvements to the manuscript, and
Fernando Etayo-Serna (INGEOMINAS) for intellectual support. Daniele
Guinot (MHNH), Matatsune Takeda (Teikyo Heisei University), Francisco
Vega (UNAM), Angel Aguirre and the staff of the STRI Library provided
literature items. Jose Arenas (INGEOMINAS, Colombia) supplied export
permits. Tomoki Kase (National Museum of Nature and Science, Tokyo)
provided a photo of one specimen from Japan. Julia Figueroa and family
provided kind hospitality and permission to collect on their property.
Two anonymous reviewers are gratefully acknowledged for their
constructive comments. Partial funding for this project was provided by
an NSERC grant to CBC.
NR 121
TC 10
Z9 12
U1 0
U2 7
PU CRUSTACEAN SOC
PI SAN ANTONIO
PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA
SN 0278-0372
EI 1937-240X
J9 J CRUSTACEAN BIOL
JI J. Crustac. Biol.
PD MAY
PY 2012
VL 32
IS 3
BP 405
EP 420
DI 10.1163/193724012X626539
PG 16
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 953AR
UT WOS:000304839800006
ER
PT J
AU Chullasorn, S
Dahms, HU
Iwasaki, N
Kangtia, P
Ferrari, FD
Jeon, HJ
Yang, WX
AF Chullasorn, Supawadee
Dahms, Hans-U.
Iwasaki, Nozomu
Kangtia, Pawana
Ferrari, Frank D.
Jeon, Hyoung Joo
Yang, Wan-Xi
TI Naupliar Development of an Ancorabolid, Paralaophontodes sp (Copepoda:
Harpacticoida) Sheds Light on Harpacticoid Evolution
SO ZOOLOGICAL STUDIES
LA English
DT Article
DE Naupliar characters; Evolution; Systematics; Phylogeny; Development;
Ancorabolidae
ID CYCLOPIDAE; CRUSTACEA; RECORD
AB Supawadee Chullasorn, Hans-U. Dahms, Nozomu Iwasaki, Pawana Kangtia, Frank D. Ferrari, Hyoung Joo Jeon, and Wan-Xi Yang (2012) Naupliar development of an ancorabolid, Paralaophontodes sp. (Copepoda: Harpacticoida) sheds light on harpacticoid evolution. Zoological Studies 51(3): 372-382. Loss of the naupliar arthrite during the molt to naupliar stage (N) VI provides a developmental apomorphy for all Harpacticoida and sheds light on the evolution within this diverse copepod taxon. Naupliar development of Paralaophontodes sp. is unusual because the bud of swimming legs 1 and 2 does not bear setae at N VI and because the naupliar arthrite, present on the coxa of antenna 2 during the 1st 5 stages, fails to form during the molt to N VI; in addition, setal elements are lost from the basis and endopod of the mandible during this molt. This is only known from some harpacticoid copepods belonging to Tisbe; loss of setal elements on the mandible was also otherwise reported for species of the Tachidiidae and Harpacticidae. Five naupliar stages of the ancorabolid, Paralaophontodes sp., are described. A key to the identification of the stages is provided. Stages can be distinguished by the number of segments of the exopod of antenna 2, setation of the limbs including the bud of the caudal ramus, and the presence and setation of the bud of maxilla 1. This is the 1st description of nauplii of a species belonging to the oligoarthran family Ancorabolidae. http://zoolstud.sinica.edu.tw/Journals/51.3/372.pdf
C1 [Yang, Wan-Xi] Zhejiang Univ, Coll Life Sci, Sperm Lab, Hangzhou 310058, Zhejiang, Peoples R China.
[Chullasorn, Supawadee] Ramkhamhang Univ, Fac Sci, Dept Biol, Bangkok 10240, Thailand.
[Dahms, Hans-U.; Kangtia, Pawana] Sangmyung Univ 7, Coll Nat Sci, Green Life Sci Dept, Seoul 110743, South Korea.
[Iwasaki, Nozomu] Kochi Univ, Usa Marine Biol Inst, Tosa, Kochi 7811164, Japan.
[Ferrari, Frank D.] Smithsonian Inst, Natl Museum Nat Hist, Suitland, MD 20746 USA.
[Jeon, Hyoung Joo] Inland Fisheries Res Inst, Natl Fisheries Res & Dev Inst, Gyeonggi Do 1143, South Korea.
RP Yang, WX (reprint author), Zhejiang Univ, Coll Life Sci, Sperm Lab, Zi Jin Gang Campus,866 Yu Hang Tang Rd, Hangzhou 310058, Zhejiang, Peoples R China.
EM wxyang@spermlab.org
FU Ramkhamhaeng University (Bangkok); National Research Foundation of Korea
(NRF); Ministry of Education, Science and Technology [2010-A001-0057];
National Nature Science Foundation of China [31072198, 30671606]
FX The work of S. Chullasorn is supported by Ramkhamhaeng University
(Bangkok). The work of H.-U. Dahms is supported by Basic Science
Research Program through the National Research Foundation of Korea (NRF)
funded by the Ministry of Education, Science and Technology
(2010-A001-0057). The work of W.X. Yang is supported by the National
Nature Science Foundation of China (Grant No. 31072198 and 30671606).
NR 31
TC 3
Z9 3
U1 0
U2 3
PU ACAD SINICA INST ZOOLOGY
PI TAIPEI
PA EDITORIAL OFFICE, TAIPEI 115, TAIWAN
SN 1021-5506
J9 ZOOL STUD
JI Zool. Stud.
PD MAY
PY 2012
VL 51
IS 3
BP 372
EP 382
PG 11
WC Zoology
SC Zoology
GA 953RN
UT WOS:000304891000009
ER
PT J
AU Fontani, F
Caselli, P
Zhang, Q
Brand, J
Busquet, G
Palau, A
AF Fontani, F.
Caselli, P.
Zhang, Q.
Brand, J.
Busquet, G.
Palau, Aina
TI Temperature and kinematics of protoclusters with intermediate and
high-mass stars: the case of IRAS 05345+3157
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; radio lines: ISM; ISM: individual objects: IRAS
05345+3157; ISM: kinematics and dynamics; ISM: molecules
ID DENSE INTERSTELLAR CLOUDS; LARGE ARRAY OBSERVATIONS; PRE-STELLAR CORES;
INITIAL CONDITIONS; STARLESS CORES; PROTOSTELLAR CANDIDATES; PRESTELLAR
CORES; NH3 OBSERVATIONS; PIPE NEBULA; DEPLETION
AB Context. Improving our understanding of the complex star formation process in clusters requires studies of star-forming clouds to search for dependencies of the physical properties on environmental variables, such as overall density, stellar crowding and feedback from massive (proto-) stars.
Aims. We aim to map at small spatial scales the temperature and the velocity field in the protocluster associated with IRAS 05345+3157, which contains both intermediate-/high-mass protostellar candidates and starless condensations, and is thus an excellent location to investigate the role of massive protostars on protocluster evolution.
Methods. We observed the ammonia (1, 1) and (2, 2) inversion transitions with the VLA. Ammonia is the best thermometer for dense and cold gas, and the observed transitions have critical densities able to trace the kinematics of the intracluster gaseous medium.
Results. The ammonia emission is extended and distributed in two filamentary structures. The starless condensations are colder than the star-forming cores, but the gas temperature across the whole protocluster is higher (by a factor of 1.3-1.5) than that measured typically in both infrared dark clouds and low-mass protoclusters. The non-thermal contribution to the observed line broadening is at least a factor of 2 larger than the expected thermal broadening even in starless condensations, contrary to the close-to-thermal line widths measured in low-mass quiescent dense cores. The NH3/N2H+ abundance ratio is greatly enhanced (a factor of 10) in the pre-stellar core candidates, probably due to freeze-out of most molecular species heavier than He.
Conclusions. The more massive and evolved objects likely play a dominant role in the physical properties and kinematics of the protocluster. The high level of turbulence and the fact that the measured core masses are larger than the expected thermal Jeans masses indicate that turbulence likely was an important factor in the initial fragmentation of the parental clump and can provide support against further fragmentation of the cores.
C1 [Fontani, F.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Caselli, P.] Univ Leeds, Sch Phys & Astrophys, Leeds LS2 9JT, W Yorkshire, England.
[Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brand, J.] Ist Radioastron, INAF, I-40129 Bologna, Italy.
[Busquet, G.] Ist Astrofis & Planetol Spaziali, INAF, I-00133 Rome, Italy.
[Palau, Aina] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Bellaterra 08193, Spain.
RP Fontani, F (reprint author), Osserv Astrofis Arcetri, INAF, Lgo E Fermi 5, I-50125 Florence, Italy.
EM fontani@arcetri.astro.it
OI Brand, Jan/0000-0003-1615-9043; Fontani, Francesco/0000-0003-0348-3418;
Zhang, Qizhou/0000-0003-2384-6589
FU Spanish MICINN [AYA2008-06189-C03]; FEDER; JAE-Doc CSIC fellowship;
European Social Fund; Italian Space Agency (ASI) [I/005/07/01]
FX F.F. is grateful to R. Cesaroni for a careful reading of the manuscript
and for providing useful comments and suggestions. A.P. 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. G.B. is funded by an Italian Space Agency (ASI) fellowship under
contract number I/005/07/01. Many thanks to the anonymous referee for
his/her useful comments and suggestions.
NR 55
TC 10
Z9 10
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2012
VL 541
AR A32
DI 10.1051/0004-6361/201118153
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 946XN
UT WOS:000304390900032
ER
PT J
AU Liseau, R
Goldsmith, PF
Larsson, B
Pagani, L
Bergman, P
Le Bourlot, J
Bell, TA
Benz, AO
Bergin, EA
Bjerkeli, P
Black, JH
Bruderer, S
Caselli, P
Caux, E
Chen, JH
de Luca, M
Encrenaz, P
Falgarone, E
Gerin, M
Goicoechea, JR
Hjalmarson, A
Hollenbach, DJ
Justtanont, K
Kaufman, MJ
Le Petit, F
Li, D
Lis, DC
Melnick, GJ
Nagy, Z
Olofsson, AOH
Olofsson, G
Roueff, E
Sandqvist, A
Snell, RL
van der Tak, FFS
van Dishoeck, EF
Vastel, C
Viti, S
Yildiz, UA
AF Liseau, R.
Goldsmith, P. F.
Larsson, B.
Pagani, L.
Bergman, P.
Le Bourlot, J.
Bell, T. A.
Benz, A. O.
Bergin, E. A.
Bjerkeli, P.
Black, J. H.
Bruderer, S.
Caselli, P.
Caux, E.
Chen, J. -H.
de Luca, M.
Encrenaz, P.
Falgarone, E.
Gerin, M.
Goicoechea, J. R.
Hjalmarson, A.
Hollenbach, D. J.
Justtanont, K.
Kaufman, M. J.
Le Petit, F.
Li, D.
Lis, D. C.
Melnick, G. J.
Nagy, Z.
Olofsson, A. O. H.
Olofsson, G.
Roueff, E.
Sandqvist, Aa.
Snell, R. L.
van der Tak, F. F. S.
van Dishoeck, E. F.
Vastel, C.
Viti, S.
Yildiz, U. A.
TI Multi-line detection of O-2 toward rho Ophiuchi A
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: abundances; ISM: molecules; ISM: lines and bands; ISM: clouds; ISM:
individual objects: rho Oph A SM1; stars: formation
ID INTERSTELLAR HYDROGEN-PEROXIDE; C-I EMISSION; DARK-CLOUD; MOLECULAR
CLOUDS; SUBMILLIMETER OBSERVATIONS; PHOTODISSOCIATION REGIONS; ODIN
SATELLITE; DUST GRAINS; MAIN CLOUD; OPH CLOUD
AB Context. Models of pure gas-phase chemistry in well-shielded regions of molecular clouds predict relatively high levels of molecular oxygen, O-2, and water, H2O. These high abundances imply high cooling rates, leading to relatively short timescales for the evolution of gravitationally unstable dense cores, forming stars and planets. Contrary to expectations, the dedicated space missions SWAS and Odin typically found only very small amounts of water vapour and essentially no O-2 in the dense star-forming interstellar medium.
Aims. Only toward rho OphA did Odin detect a very weak line of O-2 at 119 GHz in a beam of size 10 arcmin. The line emission of related molecules changes on angular scales of the order of some tens of arcseconds, requiring a larger telescope aperture such as that of the Herschel Space Observatory to resolve the O-2 emission and pinpoint its origin.
Methods. We use the Heterodyne Instrument for the Far Infrared (HIFI) aboard Herschel to obtain high resolution O-2 spectra toward selected positions in the rho Oph A core. These data are analysed using standard techniques for O2 excitation and compared to recent PDR-like chemical cloud models.
Results. The N-J = 3(3)-1(2) line at 487.2 GHz is clearly detected toward all three observed positions in the rho Oph A core. In addition, an oversampled map of the 5(4)-3(4) transition at 773.8 GHz reveals the detection of the line in only half of the observed area. On the basis of their ratios, the temperature of the O-2 emitting gas appears to vary quite substantially, with warm gas (greater than or similar to 50 K) being adjacent to a much colder region, of temperatures lower than 30 K.
Conclusions. The exploited models predict that the O-2 column densities are sensitive to the prevailing dust temperatures, but rather insensitive to the temperatures of the gas. In agreement with these models, the observationally determined O-2 column densities do not seem to depend strongly on the derived gas temperatures, but fall into the range N(O-2) = 3 to greater than or similar to 6 x 10(15) cm(-2). Beam-averaged O-2 abundances are about 5 x 10(-8) relative to H-2. Combining the HIFI data with earlier Odin observations yields a source size at 119 GHz in the range of 4 to 5 arcmin, encompassing the entire rho Oph A core. We speculate that one of the reasons for the generally very low detection rate of O-2 is the short period of time during which O-2 molecules are reasonably abundant in molecular clouds.
C1 [Liseau, R.; Bjerkeli, P.; Black, J. H.; Hjalmarson, A.; Justtanont, K.] Onsala Space Observ, Chalmers Univ Technol, Dept Earth & Space Sci, S-43992 Onsala, Sweden.
[Goldsmith, P. F.; Chen, J. -H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Larsson, B.; Olofsson, G.; Sandqvist, Aa.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden.
[Pagani, L.; Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France.
[Pagani, L.; Encrenaz, P.] Observ Paris, UMR 8112, CNRS, F-75014 Paris, France.
[Bergman, P.; Olofsson, A. O. H.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden.
[Le Bourlot, J.; de Luca, M.; Le Petit, F.; Roueff, E.] Observ Paris, LUTH, F-75014 Paris, France.
[Bell, T. A.; Goicoechea, J. R.] Ctr Astrobiol, CSICINTA, Madrid 28850, Spain.
[Benz, A. O.; Bruderer, S.] ETH, Inst Astron, CH-8092 Zurich, Switzerland.
[Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England.
[Caux, E.; Vastel, C.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Caux, E.; Vastel, C.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Falgarone, E.; Gerin, M.] Observ Paris, UMR8112, CNRS, LRA LERMA, F-75231 Paris 05, France.
[Falgarone, E.; Gerin, M.] Ecole Normale Super, F-75231 Paris 05, France.
[Hollenbach, D. J.] SETI Inst, Mountain View, CA 94043 USA.
[Kaufman, M. J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Li, D.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Li, D.; Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Nagy, Z.; van der Tak, F. F. S.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
[Nagy, Z.; van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Snell, R. L.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[van Dishoeck, E. F.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Bruderer, S.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Viti, S.] UCL, Dept Phys & Astron, London, England.
RP Liseau, R (reprint author), Onsala Space Observ, Chalmers Univ Technol, Dept Earth & Space Sci, S-43992 Onsala, Sweden.
EM rene.liseau@chalmers.se
RI Yildiz, Umut/C-5257-2011; Goldsmith, Paul/H-3159-2016
OI Yildiz, Umut/0000-0001-6197-2864;
NR 63
TC 46
Z9 46
U1 1
U2 9
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 MAY
PY 2012
VL 541
AR A73
DI 10.1051/0004-6361/201118575
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 946XN
UT WOS:000304390900073
ER
PT J
AU Michalowski, MJ
Dunlop, JS
Cirasuolo, M
Hjorth, J
Hayward, CC
Watson, D
AF Michalowski, M. J.
Dunlop, J. S.
Cirasuolo, M.
Hjorth, J.
Hayward, C. C.
Watson, D.
TI The stellar masses and specific star-formation rates of submillimetre
galaxies
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: high-redshift;
galaxies: ISM; galaxies: starburst; submillimeter: galaxies
ID HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; SPECTRAL
ENERGY-DISTRIBUTION; EXTRAGALACTIC LEGACY SURVEY; MILLIMETER-SELECTED
GALAXY; ACTIVE GALACTIC NUCLEI; DUST-OBSCURED GALAXIES; ULTRA DEEP
SURVEY; TP-AGB STARS; SIMILAR-TO 3
AB Establishing the stellar masses, and hence specific star-formation rates of submillimetre galaxies is crucial for determining the role of such objects in the cosmic history of galaxy/star formation. However, there is as yet no consensus over the typical stellar masses of submillimetre galaxies, as illustrated by the widely differing results reported from recent optical-infrared studies of submillimetre galaxies with spectroscopic redshifts z similar or equal to 2-3. Specifically, even for the same set of submillimetre galaxies, the reported average stellar masses have ranged over an order of magnitude, from similar or equal to 5 x 10(10) M-circle dot to less than or similar to 5 x 10(11) M-circle dot. Here we study how different methods of analysis can lead to such widely varying results. We find that, contrary to recent claims in the literature, potential contamination of IRAC 3-8 mu m photometry from hot dust associated with an active nucleus is not the origin of the published discrepancies in derived stellar masses. Instead, we expose in detail how inferred stellar mass depends on assumptions made in the photometric fitting, and quantify the individual and cumulative effects of different choices of initial mass function, different "brands" of evolutionary synthesis models, and different forms of assumed star-formation history. We review current observational evidence for and against these alternatives as well as clues from the hydrodynamical simulations, and conclude that, for the most justifiable choices of these model inputs, the average stellar mass of luminous (S-850 greater than or similar to 5 mJy) submillimetre galaxies is similar or equal to 2 x 10(11) M-circle dot to within a factor similar or equal to 2. We also check and confirm that this number is perfectly reasonable in the light of the latest measurements of the dynamical masses of these objects (similar or equal to 2-6x10(11) M-circle dot from CO (1-0) observations), and the evolving stellar mass function of the overall galaxy population. Galaxy stellar masses of this order imply that the average specific star-formation rate of submillimetre galaxies is comparable to that of other star-forming galaxies at z > 2, at 2-3 Gyr(-1). This supports the view that, while rare outliers may be found at any stellar mass, most submillimetre galaxies simply form the top end of the "main-sequence" of star-forming galaxies at these redshifts. Conversely, this argues strongly against the viewpoint, frequently simply asserted in the literature, that submillimetre galaxies are extreme pathological objects, of little relevance in the cosmic history of star-formation.
C1 [Michalowski, M. J.; Dunlop, J. S.; Cirasuolo, M.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Hjorth, J.; Watson, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Hayward, C. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Michalowski, MJ (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
EM mm@roe.ac.uk
RI Hayward, Christopher/I-4756-2012; Hjorth, Jens/M-5787-2014; Watson,
Darach/E-4521-2015
OI Hayward, Christopher/0000-0003-4073-3236; Hjorth,
Jens/0000-0002-4571-2306; Watson, Darach/0000-0002-4465-8264
FU UK Science & Technology Facilities Council; Royal Society; European
Research Council; Danish National Research Foundation
FX We thank Joanna Baradziej and our anonymous referee for help with
improving this paper and Georgios Magdis for comments. M.J.M. and J.S.D.
acknowledge the support of the UK Science & Technology Facilities
Council. J.S.D. acknowledges the support of the Royal Society via a
Wolfson Research Merit award, and the support of the European Research
Council through an Advanced Grant. The Dark Cosmology Centre is funded
by the Danish National Research Foundation. This research has made use
of Tool for OPerations on Catalogues And Tables (TOPCAT; Taylor 2005):
www.starlink.ac.uk/topcat/ and NASA's Astrophysics Data System
Bibliographic Services.
NR 116
TC 74
Z9 74
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 MAY
PY 2012
VL 541
AR A85
DI 10.1051/0004-6361/201016308
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 946XN
UT WOS:000304390900085
ER
PT J
AU Poppenhaeger, K
Czesla, S
Schroter, S
Lalitha, S
Kashyap, V
Schmitt, JHMM
AF Poppenhaeger, K.
Czesla, S.
Schroeter, S.
Lalitha, S.
Kashyap, V.
Schmitt, J. H. M. M.
TI The high-energy environment in the super-Earth system CoRoT-7
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: activity; planetary systems; planets and satellites: atmospheres;
X-rays: stars; stars: coronae; X-rays: individuals: CoRoT-7
ID X-RAY; PLANETARY-ATMOSPHERES; INTERSTELLAR-MEDIUM; HOT JUPITERS; GJ
1214B; H-I; EVOLUTION; MASS; SPECTROSCOPY; EVAPORATION
AB High-energy irradiation of exoplanets has been identified to be a key influence on the stability of these planets' atmospheres. So far, irradiation-driven mass-loss has been observed only in two Hot Jupiters, and the observational data remain even more sparse in the super-Earth regime. We present an investigation of the high-energy emission in the CoRoT-7 system, which hosts the first known transiting super-Earth. To characterize the high-energy XUV radiation field into which the rocky planets CoRoT-7b and CoRoT-7c are immersed, we analyzed a 25 ks XMM-Newton observation of the host star. Our analysis yields the first clear (3.5 sigma) X-ray detection of CoRoT-7. We determine a coronal temperature of approximate to 3 MK and an X-ray luminosity of 3 x 10(28) erg s(-1). The level of XUV irradiation on CoRoT-7b amounts to approximate to 37 000 erg cm(-2) s(-1). Current theories for planetary evaporation can only provide an order-of-magnitude estimate for the planetary mass loss; assuming that CoRoT-7b has formed as a rocky planet, we estimate that CoRoT-7b evaporates at a rate of about 1.3 x 10(11) gs(-1) and has lost approximate to 4-10 earth masses in total.
C1 [Poppenhaeger, K.; Czesla, S.; Schroeter, S.; Lalitha, S.; Schmitt, J. H. M. M.] Hamburger Sternwarte, D-21029 Hamburg, Germany.
[Kashyap, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Poppenhaeger, K (reprint author), Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
EM katja.poppenhaeger@hs.uni-hamburg.de
OI Poppenhaeger, Katja/0000-0003-1231-2194
FU German Research Foundation (DFG) [Graduiertenkolleg 1351]; DLR
[50OR0703]
FX K.P. and S.L. acknowledge funding from the German Research Foundation
(DFG) via Graduiertenkolleg 1351. S.C. and S.S. acknowledge financial
support from DLR grant 50OR0703.
NR 34
TC 9
Z9 9
U1 1
U2 2
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2012
VL 541
AR A26
DI 10.1051/0004-6361/201118507
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 946XN
UT WOS:000304390900026
ER
PT J
AU van Haaften, LM
Nelemans, G
Voss, R
Jonker, PG
AF van Haaften, L. M.
Nelemans, G.
Voss, R.
Jonker, P. G.
TI Formation of the planet around the millisecond pulsar J1719-1438
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE pulsars: individual: J1719-1438; binaries: close; planets and
satellites: formation
ID X-RAY BINARIES; WHITE-DWARF DONORS; SAX J1808.4-3658; ORBITAL-PERIOD;
BLACK-WIDOW; EVOLUTION; ACCRETION; STARS; SECONDARIES; HELIUM
AB Context. Recently the discovery of PSR J1719-1438, a 5.8 ms pulsar with a companion in a 2.2 h orbit, was reported. The combination of this orbital period and the very low mass function is unique. The discoverers, Bailes et al. (2011, Science, 333, 1717), proposed an ultracompact X-ray binary (UCXB) as the progenitor system. However, the standard UCXB scenario would not produce this system as the time required to reach this orbital period exceeds the current estimate of the age of the Universe. The detached state of the system aggravates the problem. The inclination of the system is an important unknown, and Bailes et al. noted that for very low (a priori very unlikely) inclinations the system is better explained as having a brown dwarf companion rather than an UCXB origin.
Aims. We want to understand the evolutionary history of PSR J1719-1438, and determine under which circumstances it could have evolved from an UCXB.
Methods. We model UCXB evolution varying the donor size and investigate the effect of a wind mass loss from the donor, and compare the results with the observed characteristics of PSR J1719-1438.
Results. An UCXB can reach a 2.2 h orbit within the age of the Universe, provided that 1) the millisecond pulsar can significantly heat and expand the donor by pulsar irradiation, or 2) the system loses extra orbital angular momentum, e. g. via a fast wind from the donor.
Conclusions. The most likely scenario for the formation of PSR J1719-1438 is UCXB evolution driven by angular momentum loss via the usual gravitational wave emission, which is enhanced by angular momentum loss via a donor wind of greater than or similar to 3 x 10(-13) M-circle dot yr(-1). Depending on the size of the donor during the evolution, the companion presently probably has a mass of similar to 1-3 Jupiter masses, making it a very low mass white dwarf as proposed by Bailes et al. Its composition can be either helium or carbon-oxygen. A helium white dwarf companion makes the long (for an UCXB) orbital period easier to explain, but the required inclination makes it a priori less likely than a carbon-oxygen white dwarf.
C1 [van Haaften, L. M.; Nelemans, G.; Voss, R.; Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Nelemans, G.] Katholieke Univ Leuven, Inst Astron, B-3001 Louvain, Belgium.
[Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP van Haaften, LM (reprint author), Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
EM L.vanHaaften@astro.ru.nl
RI Nelemans, Gijs/D-3177-2012
OI Nelemans, Gijs/0000-0002-0752-2974
FU Netherlands Organisation for Scientific Research (NWO)
FX L.M.v.H. is supported by the Netherlands Organisation for Scientific
Research (NWO). G.N., R.V. and P.G.J. are supported by NWO VIDI grants.
NR 24
TC 17
Z9 17
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2012
VL 541
AR A22
DI 10.1051/0004-6361/201218798
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 946XN
UT WOS:000304390900022
ER
PT J
AU DeVience, SJ
Walsworth, RL
Rosen, MS
AF DeVience, Stephen J.
Walsworth, Ronald L.
Rosen, Matthew S.
TI Dependence of nuclear spin singlet lifetimes on RF spin-locking power
SO JOURNAL OF MAGNETIC RESONANCE
LA English
DT Article
DE Nuclear singlet state; Long-lived coherence; Spin-lattice relaxation;
Spin-locking
ID LONG-LIVED STATES; SOLUTION NMR; HYPERPOLARIZED C-13;
MAGNETIC-RESONANCE; SLOW DIFFUSION; RELAXATION; SPECTROSCOPY; SYSTEMS;
FIELD
AB We measure the lifetime of long-lived nuclear spin singlet states as a function of the strength of the RF spin-locking field and present a simple theoretical model that agrees well with our measurements, including the low-RF-power regime. We also measure the lifetime of a long-lived coherence between singlet and triplet states that does not require a spin-locking field for preservation. Our results indicate that for many molecules, singlet states can be created using weak RF spin-locking fields: more than two orders of magnitude lower RF power than in previous studies. Our findings suggest that for many endogenous biomolecules, singlets and related states with enhanced lifetimes might be achievable in vivo with safe levels of RF power. (C) 2012 Elsevier Inc. All rights reserved.
C1 [DeVience, Stephen J.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[DeVience, Stephen J.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA.
[Walsworth, Ronald L.; Rosen, Matthew S.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Rosen, Matthew S.] Harvard Univ, Sch Med, Boston, MA 02115 USA.
[Rosen, Matthew S.] Martinos Ctr Biomed Imaging, Charlestown, MA 02129 USA.
RP DeVience, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, MS 59,60 Garden St, Cambridge, MA 02138 USA.
EM devience@fas.harvard.edu; rwalsworth@cfa.harvard.edu;
mrosen@cfa.harvard.edu
RI DeVience, Stephen/D-7274-2012
OI DeVience, Stephen/0000-0003-3142-7296
NR 28
TC 11
Z9 11
U1 0
U2 20
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1090-7807
J9 J MAGN RESON
JI J. Magn. Reson.
PD MAY
PY 2012
VL 218
BP 5
EP 10
DI 10.1016/j.jmr.2012.03.016
PG 6
WC Biochemical Research Methods; Physics, Atomic, Molecular & Chemical;
Spectroscopy
SC Biochemistry & Molecular Biology; Physics; Spectroscopy
GA 948GK
UT WOS:000304491400002
PM 22578548
ER
PT J
AU Bar-Gill, N
Pham, LM
Belthangady, C
Le Sage, D
Cappellaro, P
Maze, JR
Lukin, MD
Yacoby, A
Walsworth, R
AF Bar-Gill, N.
Pham, L. M.
Belthangady, C.
Le Sage, D.
Cappellaro, P.
Maze, J. R.
Lukin, M. D.
Yacoby, A.
Walsworth, R.
TI Suppression of spin-bath dynamics for improved coherence of
multi-spin-qubit systems
SO NATURE COMMUNICATIONS
LA English
DT Article
ID NUCLEAR-SPIN; ELECTRONIC SPIN; NANOSCALE RESOLUTION; MAGNETIC-RESONANCE;
SPECTRAL DIFFUSION; RELAXATION-TIMES; DIAMOND; DECOHERENCE; READOUT;
NOISE
AB Multi-qubit systems are crucial for the advancement and application of quantum science. Such systems require maintaining long coherence times while increasing the number of qubits available for coherent manipulation. For solid-state spin systems, qubit coherence is closely related to fundamental questions of many-body spin dynamics. Here we apply a coherent spectroscopic technique to characterize the dynamics of the composite solid-state spin environment of nitrogen-vacancy colour centres in room temperature diamond. We identify a possible new mechanism in diamond for suppression of electronic spin-bath dynamics in the presence of a nuclear spin bath of sufficient concentration. This suppression enhances the efficacy of dynamical decoupling techniques, resulting in increased coherence times for multi-spin-qubit systems, thus paving the way for applications in quantum information, sensing and metrology.
C1 [Bar-Gill, N.; Belthangady, C.; Le Sage, D.; Walsworth, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bar-Gill, N.; Lukin, M. D.; Yacoby, A.; Walsworth, R.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Pham, L. M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Cappellaro, P.] MIT, Dept Nucl Sci & Engn, Cambridge, MA 02139 USA.
[Maze, J. R.] Pontificia Univ Catolica Chile, Dept Phys, Santiago 7820436, Chile.
RP Bar-Gill, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nbar-gill@cfa.harvard.edu; rwalsworth@cfa.harvard.edu
RI Cappellaro, Paola/B-1413-2010;
OI Cappellaro, Paola/0000-0003-3207-594X; Le Sage,
David/0000-0003-1678-9491
FU NIST; NSF [DMG-1005926]; US Army Research Office; DARPA
FX We gratefully acknowledge fruitful discussions with Patrick Maletinsky
and Shimon Kolkowitz; and assistance with samples by Daniel Twitchen and
Matthew Markham (Element 6) and Patrick Doering and Robert Linares
(Apollo). This work was supported by NIST, NSF, US Army Research Office
and DARPA (QuEST and QuASAR programs). PC was partially funded by NSF
under grant no. DMG-1005926.
NR 43
TC 60
Z9 60
U1 2
U2 42
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD MAY
PY 2012
VL 3
AR 858
DI 10.1038/ncomms1856
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 949XP
UT WOS:000304611400053
PM 22617298
ER
PT J
AU Mehdiabadi, NJ
Mueller, UG
Brady, SG
Himler, AG
Schultz, TR
AF Mehdiabadi, Natasha J.
Mueller, Ulrich G.
Brady, Sean G.
Himler, Anna G.
Schultz, Ted R.
TI Symbiont fidelity and the origin of species in fungus-growing ants
SO NATURE COMMUNICATIONS
LA English
DT Article
ID LEAF-CUTTING ANTS; MULTIPLE SEQUENCE ALIGNMENT; ATTINE ANT; PHYLOGENETIC
ANALYSIS; COEVOLUTION; FORMICIDAE; EVOLUTION; MUTUALISM; COOPERATION;
AGRICULTURE
AB A major problem in evolutionary biology is explaining the success of mutualism. Solving this problem requires understanding the level of fidelity between interacting partners. Recent studies have proposed that fungus-growing ants and their fungal cultivars are the products of 'diffuse' coevolution, in which single ant and fungal species are not exclusive to one another. Here we show for ants and associated fungi in the Cyphomyrmex wheeleri species group that each ant species has been exclusively associated with a single fungal cultivar 'species' for millions of years, even though alternative cultivars are readily available, and that rare shifts to new cultivars are associated with ant speciation. Such long-term partner fidelity may have facilitated 'tight' ant-fungus coevolution, and shifts to new fungal cultivars may have had a role in the origin of new ant species.
C1 [Mehdiabadi, Natasha J.; Brady, Sean G.; Schultz, Ted R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
[Mehdiabadi, Natasha J.; Brady, Sean G.; Schultz, Ted R.] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Washington, DC 20013 USA.
[Mehdiabadi, Natasha J.; Schultz, Ted R.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Mueller, Ulrich G.; Himler, Anna G.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Mueller, Ulrich G.] Smithsonian Trop Res Inst, Balboa, Panama.
[Himler, Anna G.] Univ Arizona, Dept Entomol, Tucson, AZ 85721 USA.
RP Mehdiabadi, NJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012, Washington, DC 20013 USA.
EM Mehdiabadi@si.edu; schultzt@si.edu
FU Smithsonian; NMNH Laboratories of Analytical Biology; NSF [DEB-0949689,
DEB-0110073, DEB-0206372, IOS-0920138, EF-0431330]
FX We thank Lee Weigt and other members of the Laboratories of Analytical
Biology (NMNH) for their help and support throughout this project. We
also thank Rachelle Adams, Donat Agosti, Stefan Cover, Cameron Currie,
Nicole Gerardo, Lacey Loudermilk, Alexander Mikheyev, Shauna Price, Kaci
Richardson, Andre Rodrigues, Jarrod Scott, Adam Smith, Heraldo
Vasconcelos, Santiago Villamarin and Tanya Vo for collecting colonies.
We thank Patrick Abbot, Jerry Coyne and Phil Ward for improving earlier
versions of the manuscript and Paul Armstrong, Faridah Nor Dahlan,
Jeffrey Hunt, Heather Ishak, Matthew Kweskin, Eugenia Okonski, Steve
Rehner, Jeffrey Sosa-Calvo, Phil Ward, Hong Zhao and members of the
Mueller Lab and the Schultz Lab for help and discussion. Funding was
provided by a Smithsonian Postdoctoral Fellowship (NJM), a Smithsonian
Scholarly Studies grant (TRS, SGB), NMNH Laboratories of Analytical
Biology (NJM, Lee Weigt), and NSF grants DEB-0949689 (TRS, NJM, UGM),
DEB-0110073 (UGM, TRS), DEB-0206372 (AGH, UGM), IOS-0920138 (UGM) and
EF-0431330 (SGB, TRS).
NR 53
TC 20
Z9 20
U1 3
U2 49
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD MAY
PY 2012
VL 3
AR 840
DI 10.1038/ncomms1844
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 949XP
UT WOS:000304611400035
PM 22588302
ER
PT J
AU Herrera, F
Manchester, SR
Jaramillo, C
AF Herrera, Fabiany
Manchester, Steven R.
Jaramillo, Carlos
TI Permineralized fruits from the late Eocene of Panama give clues of the
composition of forests established early in the uplift of Central
America
SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY
LA English
DT Article
DE Dracontomelon; Eocene; Humiriaceae; Neotropical rainforests; Panama;
Vitaceae
ID NEOTROPICAL RAIN-FOREST; SOUTH-AMERICA; CERREJON FORMATION; SEED
MORPHOLOGY; LATE PALEOCENE; VITACEAE; COLOMBIA; PALEOGEOGRAPHY;
BIOGEOGRAPHY; PHYLOGENY
AB Central American rainforests are among the most diverse biomes in the world today. However, we know little about their history because of a poor fossil record. Here, we augment previous studies based on fossil pollen of Panama with an investigation of eight species of endocarps and seeds from an upper Eocene locality near Tonosi on the Pacific coast of central Panama. Affinities at the family/order level include: Arecaceae, Vitaceae, Humiriaceae, Anacardiaceae, and Lamiales. Biogeographically, two of the Tonosi fossil taxa, Dracontomelon and cf. Leen, are interesting because they occur today only in lowland rainforests of the Old World. The new fossil genus Saxuva, together with cf. Leea, are the earliest evidence of Vitaceae (the grape family) in the Neotropics. The new genus Lacunofructus is the oldest record for Humiriaceae and supports the previously suggested Neotropical origin for the family. We interpret the Tonosi macroflora as a record of the vegetation which colonized land that emerged as part of the Eocene volcanic arc in southern Central America. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Herrera, Fabiany; Manchester, Steven R.] Univ Florida, Dept Biol, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Herrera, Fabiany; Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama.
RP Herrera, F (reprint author), Univ Florida, Dept Biol, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
EM fherrera@flmnh.ufl.edu
FU PCP PIRE (Partnerships for International Research and Education); U.S.
NSF (National Science Foundation) [0966884]; Evolving Earth Foundation;
Geological Society of America Foundation; Asociacion Colombiana de
Geologos y Geofisicos del Petroleo-ARES; Smithsonian Institution; Gary
S. Morgan Student Research Award; Lewis & Clark Foundation-American
Philosophical Society; NSF [EF-0431266, BSR-0743474, DEB-0733725]; Mark
Tupper and Ricardo Perez SA
FX This research was made possible through funding from PCP PIRE
(Partnerships for International Research and Education) supported by the
U.S. NSF (National Science Foundation) grant 0966884 (OISE, EAR, DRL).
From the Evolving Earth Foundation, the Geological Society of America
Foundation, the Asociacion Colombiana de Geologos y Geofisicos del
Petroleo-ARES, the Smithsonian Institution, the Gary S. Morgan Student
Research Award, and the Lewis & Clark Foundation-American Philosophical
Society to F. Herrera; NSF grants EF-0431266 and BSR-0743474 to S.R.
Manchester; NSF grant DEB-0733725 and funding provided by Mark Tupper
and Ricardo Perez SA to C. Jaramillo. We thank Bruce Tiffney and one
anonymous reviewer for their constructive comments and Giovanni Bedoya
for nomenclatural suggestions. We thank Bruce MacFadden, Austin Hendy,
Alexis Rojas, Roger Portell, Catalina Pimiento, Monica Carvalho, Camila
Martinez, Camilo Montes, Gary Morgan, Aaron Wood, Luz Oviedo, Claudia
Grant, and Maria Ines Barreto for their assistance in the field trips.
Terry Lott provided helpful reviews of the manuscript. Iju Chen provided
photos of extant seeds and helpful comments about the systematic of the
Vitaceae fossils. F. Herrera thanks Benjamin Himschoot for his support.
NR 54
TC 11
Z9 11
U1 0
U2 16
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0034-6667
EI 1879-0615
J9 REV PALAEOBOT PALYNO
JI Rev. Palaeobot. Palynology
PD MAY 1
PY 2012
VL 175
BP 10
EP 24
DI 10.1016/j.revpalbo.2012.02.007
PG 15
WC Plant Sciences; Paleontology
SC Plant Sciences; Paleontology
GA 950ZH
UT WOS:000304689900002
ER
PT J
AU Peters, VE
Carroll, CR
AF Peters, Valerie E.
Carroll, C. Ronald
TI Temporal variation in coffee flowering may influence the effects of bee
species richness and abundance on coffee production
SO AGROFORESTRY SYSTEMS
LA English
DT Article
DE Agroforestry; Bees; Climate; Shade-coffee; Phenology
ID PLANT-POLLINATOR INTERACTIONS; TROPICAL FORESTS; CROP POLLINATION;
CLIMATE-CHANGE; LIFE-HISTORY; PHENOLOGY; DENSITY; POLLEN; MANAGEMENT;
DIVERSITY
AB Accurately estimating the contribution of pollinators to production in crop species is important but could be challenging for species that are widely cultivated. One factor that may influence the pollinator-production relationship across regions is phenology, or the timing of recurring biological events, because crop phenology can be proximately controlled by climatic variables and phenology can affect plant reproductive success. For the economically important crop, coffee (), at least three aspects of flowering phenology (onset, density and frequency) are influenced by precipitation, which varies across coffee's cultivated range. Of these aspects of flowering phenology, flower density may particularly impact production in coffee because high-density flowering can severely limit outcrossing which is a major contributor to high yields and larger, high quality beans. We studied the coffee plant-pollinator interaction over 3 years and across two distinct types of coffee blooms: (1) low-density, synchronous flowering and (2) high-density, synchronous (mass) flowering. Bee species richness was similar for four out of five flowering periods (9.8 +/- A 2.7 95% CI), but nearly tripled during one high-density flowering period (26 +/- A 8.6 95% CI). During low-density flowering coffee fruit set rates were varied, but when coffee flowered at high-density, initial fruit set rates remained close to 60% (the rate obtained from manual self-pollination of coffee flowers in pollination experiments). We discuss how changing precipitation patterns may alter coffee flowering phenology and the coffee plant-pollinator relationship, providing insight into how climate change may influence this interaction as well as the resultant coffee production.
C1 [Peters, Valerie E.; Carroll, C. Ronald] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA.
RP Peters, VE (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA.
EM cazamosca@gmail.com
FU EarthWatch Institute
FX This research was supported by grants from the EarthWatch Institute. We
thank all the EarthWatch volunteers and two field assistants, M. Garro
Cruz and R. Rojas Herrera. We are especially grateful for the support of
the individual farmers and for their hospitality, without their support
and willingness to open their farms to research this study would not
have been possible, O. Salazar, A. Vega, G. Lobo, R. Leiton, O. Ramirez
and O. Garro.
NR 41
TC 3
Z9 4
U1 10
U2 79
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-4366
J9 AGROFOREST SYST
JI Agrofor. Syst.
PD MAY
PY 2012
VL 85
IS 1
SI SI
BP 95
EP 103
DI 10.1007/s10457-011-9476-2
PG 9
WC Agronomy; Forestry
SC Agriculture; Forestry
GA 943VH
UT WOS:000304153100008
ER
PT J
AU Mascaro, J
Hughes, RF
Schnitzer, SA
AF Mascaro, Joseph
Hughes, R. Flint
Schnitzer, Stefan A.
TI Novel forests maintain ecosystem processes after the decline of native
tree species
SO ECOLOGICAL MONOGRAPHS
LA English
DT Article
DE biodiversity-ecosystem function paradigm; diversity-productivity
relationship; new forests; no-analog communities; novel ecosystems
ID NUTRIENT-USE EFFICIENCY; TROPICAL DRY FOREST; LEAF LIFE-SPAN; PLANT
DIVERSITY; PUERTO-RICO; PRIMARY SUCCESSION; PRODUCTIVITY RELATIONSHIPS;
EUROPEAN GRASSLANDS; BIOLOGICAL INVASION; GLOBAL CHANGE
AB The positive relationship between species diversity (richness and evenness) and critical ecosystem functions, such as productivity, carbon storage, and nutrient cycling, is often used to predict the consequences of extinction. At regional scales, however, plant species richness is mostly increasing rather than decreasing because successful plant species introductions far outnumber extinctions. If these regional increases in richness lead to local increases in diversity, a reasonable prediction is that productivity, carbon storage, and nutrient cycling will increase following invasion, yet this prediction has rarely been tested empirically. We tested this prediction in novel forest communities dominated by introduced species (similar to 90% basal area) in lowland Hawaiian rain forests by comparing their functionality to that of native forests. We conducted our comparison along a natural gradient of increasing nitrogen availability, allowing for a more detailed examination of the role of plant functional trait differences (specifically, N-2 fixation) in driving possible changes to ecosystem function. Hawaii is emblematic of regional patterns of species change; it has much higher regional plant richness than it did historically, due to >1000 plant species introductions and only; 71 known plant extinctions, resulting in an similar to 100% increase in richness. At local scales, we found that novel forests had significantly higher tree species richness and higher diversity of dominant tree species. We further found that aboveground biomass, productivity, nutrient turnover (as measured by soil-available and litter-cycled nitrogen and phosphorus), and belowground carbon storage either did not differ significantly or were significantly greater in novel relative to native forests. We found that the addition of introduced N-2-fixing tree species on N-limited substrates had the strongest effect on ecosystem function, a pattern found by previous empirical tests. Our results support empirical predictions of the functional effects of diversity, but they also suggest basic ecosystem processes will continue even after dramatic losses of native species diversity if simple functional roles are provided by introduced species. Because large portions of the Earth's surface are undergoing similar transitions from native to novel ecosystems, our results are likely to be broadly applicable.
C1 [Mascaro, Joseph; Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53211 USA.
[Hughes, R. Flint] US Forest Serv, Inst Pacific Isl Forestry, USDA, Hilo, HI 96720 USA.
[Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Mascaro, J (reprint author), Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA.
EM jmascaro@stanford.edu
OI Schnitzer, Stefan/0000-0002-2715-9455
FU National Science Foundation; Doctoral Dissertation Improvement Grant
[DEB-0808498]; University of Wisconsin-Milwaukee (UWM); USDA Forest
Service Institute for Pacific Islands Forestry
FX We thank A. Uowolo, G. Sanchez, K. Nelson-Kaula, N. Crabbe, M. Kaeske,
J. Brown, R. McDowell, and C. McFadden for laboratory and field
assistance; P. Hart, K. Carlson, N. Zimmerman, S. Cordell, and other
USFS-IPIF and USGS-BRD personnel for contributing vegetation data; and
J. Baldwin for assisting in analyses. The collection of below-ground
data was made possible by the University of Hawai'i Pacific Internship
Program for Exploring Science. G. Asner, R. Laungani, K. McElligott, and
two anonymous reviewers commented on a previous draft of the manuscript,
which also benefited from insightful discussion with A. Lugo, J.
Kellner, C. Farrior, E. Marris, R. MacKenzie, C. Giardina, T. Varga, N.
Lasca, J. Karron, and E. Young, as well as participants of a workshop on
novel ecosystems at the Ecological Society of America meeting in
Milwaukee, Wisconsin, in 2008. This research was supported by a National
Science Foundation Graduate Research Fellowship to J. Mascaro, a
Doctoral Dissertation Improvement Grant to S. A. Schnitzer, R. F.
Hughes, and J. Mascaro (DEB-0808498), a University of
Wisconsin-Milwaukee (UWM) Golda Meir Library Scholar Award to J.
Mascaro, and a UWM Graduate Fellowship to J. Mascaro. Additional funding
and logistical support was provided by the USDA Forest Service Institute
for Pacific Islands Forestry.
NR 112
TC 46
Z9 46
U1 15
U2 153
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 0012-9615
EI 1557-7015
J9 ECOL MONOGR
JI Ecol. Monogr.
PD MAY
PY 2012
VL 82
IS 2
BP 221
EP 238
DI 10.1890/11-1014.1
PG 18
WC Ecology
SC Environmental Sciences & Ecology
GA 946RG
UT WOS:000304370800005
ER
PT J
AU Estrada-Villegas, S
Mcgill, BJ
Kalko, EKV
AF Estrada-Villegas, Sergio
Mcgill, Brian J.
Kalko, Elisabeth K. V.
TI Climate, habitat, and species interactions at different scales determine
the structure of a Neotropical bat community
SO ECOLOGY
LA English
DT Article
DE acoustic monitoring; community composition and structure;
Emballonuridae; emergent properties; insectivorous bats; Mormoopidae;
Neotropics; Panama; rainfall gradient; spatial scale; variance
partitioning; Vespertilionidae
ID AERIAL INSECTIVOROUS BATS; TROPICAL FOREST; EATING BATS; RICHNESS;
DIVERSITY; ECOLOGY; LANDSCAPE; PATTERNS; URBANIZATION; ECHOLOCATION
AB Climate, habitat, and species interactions are factors that control community properties (e.g., species richness, abundance) across various spatial scales. Usually, researchers study how a few properties are affected by one factor in isolation and at one scale. Hence, there are few multi-scale studies testing how multiple controlling factors simultaneously affect community properties at different scales. We ask whether climate, habitat structure, or insect resources at each of three spatial scales explains most of the variation in six community properties and which theory best explains the distribution of selected community properties across a rainfall gradient. We studied a Neotropical insectivorous bat ensemble in the Isthmus of Panama with acoustic monitoring techniques. Using climatological data, habitat surveys, and insect captures in a hierarchical sampling design we determined how much variation of the community properties was explained by the three factors employing two approaches for variance partitioning. Our results revealed that most of the variation in species richness, total abundance, and feeding activity occurred at the smallest spatial scale and was explained by habitat structure. In contrast, climate at large scales explained most of the variation in individual species' abundances. Although each species had an idiosyncratic response to the gradient, species richness peaked at intermediate levels of precipitation, whereas total abundance was very similar across sites, suggesting density compensation. All community properties responded in a different manner to the factor and scale under consideration.
C1 [Estrada-Villegas, Sergio] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
[Estrada-Villegas, Sergio; Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, 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.
[Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany.
RP Estrada-Villegas, S (reprint author), McGill Univ, Dept Biol, 1205 Docteur 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 Institute;
NSERC
FX S. Estrada-Villegas thanks Laura Jara Reyes for her invaluable support
throughout the project. Julie Messier, Richard Feldman, Peter White,
Christoph Meyer, Maria del Carmen Ruiz-Jaen, Andrew Gonzales, and Brock
Fenton provided great help and valuable comments to the manuscript. We
thank the Neotropical Environment Option and the Smithsonian Tropical
Research Institute for excellent logistics and funding. NSERC provided
funding to B. J. McGill. S. Estrada-Villegas dedicates this work to his
mentor and friend, Elisabeth Kalko: From the first moment "Eli" and I
met, she overwhelmed me with joy, candor, and generosity. As her pupil,
we shared the delight for fieldwork and the marvels of the tropics: We
stood in awe at the Tabebuia blooming or any torrential thunderstorm. As
her colleague, I tried to be as graceful, as curious, as bright, and as
reliable as she was with every endeavor. Eli's sense of duty is yet to
be matched. As a friend, her enthusiasm, her right-timed and sincere
counsel, her generosity and humbleness will be utterly missed. This work
represents only a fraction of her passions: tropical bats, echolocation,
and community ecology.
NR 67
TC 8
Z9 8
U1 3
U2 82
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 0012-9658
EI 1939-9170
J9 ECOLOGY
JI Ecology
PD MAY
PY 2012
VL 93
IS 5
BP 1183
EP 1193
PG 11
WC Ecology
SC Environmental Sciences & Ecology
GA 946QK
UT WOS:000304368100023
PM 22764504
ER
PT J
AU Ponzio, MF
Monfort, SL
Busso, JM
Carlini, VP
Ruiz, RD
De Cuneo, MF
AF Ponzio, Marina F.
Monfort, Steven L.
Busso, Juan Manuel
Carlini, Valeria P.
Ruiz, Ruben D.
De Cuneo, Marta Fiol
TI Adrenal activity and anxiety-like behavior in fur-chewing chinchillas
(Chinchilla lanigera)
SO HORMONES AND BEHAVIOR
LA English
DT Article
DE Abnormal repetitive behavior; Fur-chewing; Stress; Urinary cortisol
metabolite; Plus-maze
ID OBSESSIVE-COMPULSIVE DISORDER; PLUS-MAZE; TRICHOTILLOMANIA; PREGNANCY;
MICE
AB Due to its complexity, in combination with a lack of scientific reports, fur-chewing became one of the most challenging behavioral problems common to captive chinchillas. In the last years, the hypothesis that fur-chewing is an abnormal repetitive behavior and that stress plays a role in its development and performance has arisen.
Here, we investigated whether a relationship existed between the expression and intensity of fur-chewing behavior, elevated urinary cortisol excretion and anxiety-related behaviors. Specifically, we evaluated the following parameters in behaviorally normal and fur-chewing animals of both sexes: 1) mean concentrations of urinary cortisol metabolites and 2) anxiety-like behavior in an elevated plus-maze test. Urinary cortisol metabolites were higher only in females that expressed the most severe form of the fur-chewing behavior (P <= 0.05). Likewise, only fur-chewing females exhibited increased (P <= 0.05) anxiety-like behaviors associated with the elevated plus-maze test. Overall, these data provided additional evidence to support the concept that fur-chewing is a manifestation of physiological stress in chinchilla, and that a female sex bias exists in the development of this abnormal behavior. (C) 2012 Elsevier Inc. All rights reserved.
C1 [Ponzio, Marina F.; Busso, Juan Manuel; Carlini, Valeria P.; Ruiz, Ruben D.; De Cuneo, Marta Fiol] Univ Nacl Cordoba, Fac Ciencias Med, Inst Fis, RA-5000 Cordoba, Argentina.
[Monfort, Steven L.] Smithsonian Conservat Biol Inst, Front Royal, VA USA.
RP Ponzio, MF (reprint author), X5000ESU, RA-1085 Cordoba, Argentina.
EM mponzio@mater.fcm.unc.edu.ar
FU Ministerio de Ciencia y Tecnologia de la Provincia de Cordoba; FONCyT;
SECyT-UNC; Smithsonian Conservation Biology Institute
FX Financial support was provided by Ministerio de Ciencia y Tecnologia de
la Provincia de Cordoba, FONCyT, SECyT-UNC, and the Smithsonian
Conservation Biology Institute. All Argentinean authors are established
investigators from the Consejo Nacional de Investigaciones Cientificas y
Tecnologicas (CONICET), Argentina.
NR 30
TC 7
Z9 7
U1 1
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0018-506X
J9 HORM BEHAV
JI Horm. Behav.
PD MAY
PY 2012
VL 61
IS 5
BP 758
EP 762
DI 10.1016/j.yhbeh.2012.03.017
PG 5
WC Behavioral Sciences; Endocrinology & Metabolism
SC Behavioral Sciences; Endocrinology & Metabolism
GA 946GP
UT WOS:000304339800013
PM 22504323
ER
PT J
AU Jones, CE
Lounibos, LP
Marra, PP
Kilpatrick, AM
AF Jones, Christy E.
Lounibos, L. Philip
Marra, Peter P.
Kilpatrick, A. Marm
TI Rainfall Influences Survival of Culex pipiens (Diptera: Culicidae) in a
Residential Neighborhood in the Mid-Atlantic United States
SO JOURNAL OF MEDICAL ENTOMOLOGY
LA English
DT Article
DE Culex pipiens; dispersal; mosquito; survival; West Nile virus
ID WEST-NILE-VIRUS; MARK-RELEASE-RECAPTURE; TARSALIS DIPTERA; SOUTHERN
CALIFORNIA; MOSQUITOS DIPTERA; HOST SELECTION; BRIDGE VECTOR;
AEDES-AEGYPTI; TRANSMISSION; ECOLOGY
AB Measurement of the survival and dispersal rates of mosquito vectors is an important step in designing and implementing control strategies. Vector survival plays a key role in determining the intensity of pathogen transmission, and vector movement determines the spatial scale on which control efforts must operate to be effective. We provide the first estimates of field survival and dispersal rates for Culex pipiens L. in North America, an important enzootic and bridge vector for West Nile virus (WNV). We conducted mark-release-recapture studies in a residential area near Washington, DC, in two consecutive years and fit nonlinear regression models to the recapture data that incorporate weather information into survival and recapture probabilities. We found that daily survival rates were not significantly different between the 2 yr but were negatively affected by rainfall. The daily survival rate was 0.904 +/- 0.037 (SE), which implies an average longevity of 10.4 d. As with other vector-borne pathogens, the measured survival rate suggests that at our site the majority of WNV-infected Cx. pipiens mosquitoes may perish before becoming infectious (being able to transmit WNV to hosts). We found relatively little evidence of dispersal after the initial night after release. Our results suggest that transmission of WNV and other pathogens transmitted by Cx. pipiens may be highly local and they highlight the importance of factors that influence survival of mosquito vectors.
C1 [Jones, Christy E.; Lounibos, L. Philip] Univ Florida, Florida Med Entomol Lab, Vero Beach, FL 32962 USA.
[Marra, Peter P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA.
RP Jones, CE (reprint author), Univ Florida, Florida Med Entomol Lab, 200 9th St SE, Vero Beach, FL 32962 USA.
EM chrjson@yahoo.com; akilpatr@ucsc.edu
FU NSF as part of NSF-NIH [EF-0914866]; NIH [1R01AI090159-01]
FX We thank Mary Ashley Laine, Alex Martin, Alex Arp, Katie Jensen, and
Juraj Cech for assistance in the field; George O'Meara for helpful
advice and discussion; and the many residents of Takoma Park who allowed
us to trap mosquitoes in their yards. We thank K. Feldman and R. Gibbs
for support, guidance, and/or permission to perform this study. This
work was funded by NSF grant EF-0914866 as part of the joint NSF-NIH
Ecology of Infectious Disease program, and NIH grant 1R01AI090159-01.
NR 35
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U1 1
U2 34
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-2585
EI 1938-2928
J9 J MED ENTOMOL
JI J. Med. Entomol.
PD MAY
PY 2012
VL 49
IS 3
BP 467
EP 473
DI 10.1603/ME11191
PG 7
WC Entomology; Veterinary Sciences
SC Entomology; Veterinary Sciences
GA 941TU
UT WOS:000303989900005
PM 22679852
ER
PT J
AU Cadena, E
Bourque, JR
Rincon, AF
Bloch, JI
Jaramillo, CA
MacFadden, BJ
AF Cadena, Edwin
Bourque, Jason R.
Rincon, Aldo F.
Bloch, Jonathan I.
Jaramillo, Carlos A.
MacFadden, Bruce J.
TI NEW TURTLES (CHELONIA) FROM THE LATE EOCENE THROUGH LATE MIOCENE OF THE
PANAMA CANAL BASIN
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID SIDE-NECKED TURTLES; SOUTH-AMERICA; TESTUDINES; HISTORY; GENUS;
EVOLUTION
AB Four distinct fossil turtle assemblages (Chelonia) are recognized from the Panama Canal Basin. The oldest, from the late Eocene-early Oligocene Gatuncillo Formation, is dominated by podocnemidid pleurodires. The early Miocene Culebra Formation includes both podocnemidids and trionychids. The early to middle Miocene Cucaracha Formation includes taxa classified in Geoemydidae (including Rhinoclemmys panamaensis n. sp.), Kinosternidae (represented by Staurotypus moschus n. sp.), large testudinids, trionychids, and podocnemidids, and finally, the late Miocene Gatun Formation records cheloniid sea turtles. These fossils include the oldest known representatives of Rhinoclemmys, the oldest record of kinosternids in Central America with a more extensive southern paleodistribution for Staurotypus and staurotypines in general, early occurrences of giant tortoises in the Neotropics, the oldest occurrence of soft-shell turtles in the tropics, the oldest late Eocene-early Oligocene Neotropical occurrences of podocnemidids. The Panamanian fossil turtles represent clades that are primarily endemic to North America, showing their very early arrival into the Neotropics prior to the complete emergence of the Isthmus of Panama, as well as their first contact with Caribbean-South American pleurodires by the early Miocene.
C1 [Cadena, Edwin; Bourque, Jason R.; Rincon, Aldo F.; Bloch, Jonathan I.; MacFadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Cadena, Edwin; Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Panama City 340020948, AA, Panama.
RP Cadena, E (reprint author), Univ Florida, Florida Museum Nat Hist, Dickinson Hall, Gainesville, FL 32611 USA.
EM eacadena@ncsu.edu; jbourque@flmnh.ufl.edu; jbloch@flmnh.ufl.edu;
jaramilloc@si.edu
OI Bloch, Jonathan/0000-0003-1484-6931
FU National Science Foundation [OISE 0638810, EAR 0642528, EAR 0824299,
PIRE 0966884]; Smithsonian Institution; Panama Canal Authority; SENACYT;
Florida Museum of Natural History; M. Tupper; R. Perez SA
FX Funding for this project came from National Science Foundation grants
OISE 0638810, EAR 0642528, and EAR 0824299, PIRE 0966884 (OISE, EAR,
DRL), the Smithsonian Institution, the Panama Canal Authority, M.
Tupper, SENACYT, R. Perez SA, the Florida Museum of Natural History Miss
Lucy Dickinson Fellowship. Thanks go to the Authority of the Panama
Canal for access to the Panama Canal areas. Thanks for access to
collections to K. de Querioz, J. Jacobs (Smithsonian National Museum of
Natural History, Washington, USA); E. Gaffney and C. Mehling, (Fossil
Amphibians, Reptiles, and Birds Collections, Division of Paleontology,
American Museum of Natural History, New York, U.S.A.); P. Pritchard
(Chelonian Research Institute, Oviedo, Florida U.S.A.); R. Rowe (Utah
Museum of Natural History, Salt Lake City, Utah U.S.A.), K. Krysko
(Florida Museum of Natural History, Herpetology collection, Gainesville,
Florida U.S.A.), R. Hulbert, Jr. (Florida Museum of Natural History,
Vertebrate Paleontology collection, Gainesville, Florida U.S.A.).
Special thanks to N. Cannarozzi (who found Rhinoclemmys panamaensis
holotype), S. Moron, A. Gomez, L. Grawe, and all other paleontologists
and geologists working at the Panama Canal Basin.
NR 64
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U1 1
U2 11
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 MAY
PY 2012
VL 86
IS 3
BP 539
EP 557
PG 19
WC Paleontology
SC Paleontology
GA 944DS
UT WOS:000304179200013
ER
PT J
AU Plotkin, H
Clarke, RS
McCoy, TJ
Corrigan, CM
AF Plotkin, Howard
Clarke, Roy S., Jr.
McCoy, Timothy J.
Corrigan, Catherine M.
TI The Old Woman, California, IIAB iron meteorite
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Review
AB The Old Woman meteorite, discovered in March 1976 by two prospectors searching for a fabled lost Spanish gold mine in mountains similar to 270 km east of Los Angeles, has achieved the status of a legend among meteorite hunters and collectors. The question of the ownership of the 2753 kg group IIAB meteorite, the second largest ever found in the United States (34 degrees 28'N, 115 degrees 14'W), gave rise to disputes involving the finders, the Bureau of Land Management, the Secretary of the Department of the Interior, the State of California, the California members of the U.S. Congress, various museums in California, the Smithsonian Institution, and the Department of Justice. Ultimately, ownership of the meteorite was transferred to the Smithsonian under the powers of the 1906 Antiquities Act, a ruling upheld in a U.S. District Court and a U.S. Court of Appeals. After additional debate, the Smithsonian removed a large cut for study and curation, and for disbursement of specimens to qualified researchers. The main mass was then returned to California on long-term loan to the Bureau of Land Managements Desert Discovery Center in Barstow. The Old Woman meteorite litigation served as an important test case for the ownership and control of meteorites found on federal lands. The Old Woman meteorite appears to be structurally unique in containing both hexahedral and coarsest octahedral structures in the same mass, unique oriented schreibersites within hexahedral areas, and polycrystalline parent austenite crystals. These structures suggest that different portions of the meteorite may have transformed via different mechanisms upon subsolidus cooling, making the large slices of Old Woman promising targets for future research.
C1 [Plotkin, Howard] Univ Western Ontario, Dept Philosophy, London, ON N6A 3K7, Canada.
[Clarke, Roy S., Jr.; McCoy, Timothy J.; Corrigan, Catherine M.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Plotkin, H (reprint author), Univ Western Ontario, Dept Philosophy, London, ON N6A 3K7, Canada.
EM hplotkin@rogers.com
FU Smithsonian Institution's Edward P. and Rebecca Rogers Henderson
Endowment
FX First and foremost, the authors thank Tim Rose, Department of Mineral
Sciences, Smithsonian Institution, National Museum of Natural History,
for the hours spent on careful preparation and cutting of the Old Woman
meteorite. The authors also thank the staff of the Office of the
Smithsonian Institution Archives, particularly Pam Henson and Brian
Daniels, for their assistance in locating relevant documents. We thank
former Smithsonian Assistant General Counsel George S. Robinson, who
provided helpful comments on an earlier draft of the manuscript. We
thank Nicole Lunning, Department of Mineral Sciences, Smithsonian
Institution, National Museum of Natural History, for the preparation of
the maps and figures. We thank Katrina Jackson, former Smithsonian
summer intern, for her work on Scanning Electron Microscope imagery of
the meteorite. We are particularly grateful to Ed Scott and Ursula
Marvin, who provided insightful reviews. The section on the
metallography of Old Woman was dramatically modified as a result.
Finally, we gratefully acknowledge the Smithsonian Institution's Edward
P. and Rebecca Rogers Henderson Endowment for travel and research
funding.
NR 60
TC 1
Z9 1
U1 1
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 MAY
PY 2012
VL 47
IS 5
BP 929
EP 946
DI 10.1111/j.1945-5100.2012.01348.x
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 945UD
UT WOS:000304300900011
ER
PT J
AU Horton, DE
Poulsen, CJ
Montanez, IP
DiMichele, WA
AF Horton, Daniel E.
Poulsen, Christopher J.
Montanez, Isabel P.
DiMichele, William A.
TI Eccentricity-paced late Paleozoic climate change
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE Pangaea; Cyclothems; Milankovitch; Ice sheet response to climate;
Cyclostratigraphy; Carbon dioxide; Orbital forcing; Late Paleozoic ice
age; Tropical climate
ID TROPICAL RAIN-FORESTS; TRANSFER SCHEME LSX; NORTH-AMERICA; SEA-LEVEL;
PENNSYLVANIAN CYCLOTHEMS; ICE-AGE; MODEL; HISTORY; CYCLES; PLANT
AB Cyclic sedimentary deposits characterize low-latitude late Paleozoic successions and preserve evidence of dynamic climate change on the Pangaean supercontinent. Although their orbitally paced glacioeustatic origins are widely accepted, their climatic signatures are open to interpretation. In this study, we utilize the GENESIS general circulation model (GCM) coupled to dynamic ice sheet and ecosystem components, to explore the response of low-latitude continental climate and high-latitude ice sheets to orbital and atmospheric pCO(2) forcing. Our results suggest that atmospheric pCO(2) concentration exerts the primary control over low-latitude continental climate and high-latitude glaciation. Our experiments constrain the atmospheric pCO(2) window within which late Paleozoic climate was amenable to orbitally-driven glacial-interglacial fluctuations. The results suggest that both high-latitude ice-sheet accumulation and ablation and low-latitude climate change were paced by the eccentricity of Earth's orbit. Periods of high eccentricity amplified precession-driven changes in insolation and promoted high-latitude ice sheet volume fluctuations as well as increased low-latitude precipitation variability. When eccentricity was low, the amplification of precessionally-driven insolation fluctuations was reduced, which promoted high-latitude continental ice sheet stability and less variable low-latitude precipitation. Based on these modeling results we discuss the implications of eccentricity paced precessional-scale climatic changes on low-latitude Pangaean depositional environments. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Horton, Daniel E.; Poulsen, Christopher J.] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA.
[Montanez, Isabel P.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA.
[DiMichele, William A.] Smithsonian Inst, Natl Museum Nat Hist MRC 121, Washington, DC 20560 USA.
RP Horton, DE (reprint author), Stanford Univ, Dept Environm Earth Syst Sci, 473 Via Ortega, Stanford, CA 94305 USA.
EM danethan@stanford.edu; poulsen@umich.edu; ipmontanez@ucdavis.edu;
dimichel@si.edu
RI DiMichele, William/K-4301-2012; Poulsen, Christopher/C-6213-2009;
OI Poulsen, Christopher/0000-0001-5104-4271; Horton,
Daniel/0000-0002-2065-4517
FU NSF [EAR-0544760, EAR-0545701, EAR-1024737]; Rocky Mountain Association
of Geologists
FX D.E.H. and C.J.P. were supported by NSF grant EAR-0544760. D.E.H.
received additional support from the Rocky Mountain Association of
Geologists Veterans Memorial Scholarship. I.P.M. was supported by NSF
grant EAR-0545701 and EAR-1024737. We offer our thanks to the members of
the Climate Change Research Laboratory at the University of Michigan for
inspiring discussions and we thank T. Olszewski and an anonymous
reviewer for constructive manuscript reviews.
NR 55
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U1 4
U2 66
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-0182
J9 PALAEOGEOGR PALAEOCL
JI Paleogeogr. Paleoclimatol. Paleoecol.
PD MAY 1
PY 2012
VL 331
BP 150
EP 161
DI 10.1016/j.palaeo.2012.03.014
PG 12
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA 941PY
UT WOS:000303976300012
ER
PT J
AU Stull, GW
DiMichele, WA
Falcon-Lang, HJ
Nelson, WJ
Elrick, S
AF Stull, Gregory W.
DiMichele, William A.
Falcon-Lang, Howard J.
Nelson, W. John
Elrick, Scott
TI Palaeoecology of Macroneuropteris scheuchzeri, and its implications for
resolving the paradox of 'xeromorphic' plants in Pennsylvanian wetlands
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE Pennsylvanian; Tropical; Seed fern; Pteridosperm; Xeromorphy; Coal
swamp; Paleoecology
ID TROPICAL RAIN-FORESTS; MIDCONTINENT NORTH-AMERICA; CENTRAL APPALACHIAN
BASIN; PALEOZOIC ICE-AGE; SEED-FERN; ATMOSPHERIC OXYGEN; CLIMATE-CHANGE;
GROWTH HABIT; NOVA-SCOTIA; MEDULLOSAN PTERIDOSPERMS
AB The medullosan pteridosperm Macroneuropteris scheuchzeri (Hoffmann) Cleal, Shute & Zodrow was widespread and abundant in the Middle to Late Pennsylvanian forests of tropical Pangaea. On the basis of its thick cuticles, few adaxial stomata, sunken stomata, and dense trichomes, it has been inferred to be a xeromorphic plant. Here we test that hypothesis by analyzing its facies distribution, especially in relation to coals, at 273 site collections from similar to 45 stratigraphic horizons accessioned in the Smithsonian National Museum of Natural History, Washington, D.C., U.S.A. The collections represent mostly (par)autochthonous assemblages and cover the taxon's complete known temporal range west of the Appalachians in west-central Pangaea. Chi-square analysis of facies-occurrence data indicates that M. scheuchzeri had a strong preference for mineral-enriched wetlands that immediately preceded and followed the development of peat swamps and mires (coals), particularly during the late Middle Pennsylvanian (late Moscovian) times, coincident with a period of reduced polar ice volume. In the late Pennsylvanian, following an interval of global warming and tropical wetland reorganization, palaeoequatorial climate shifted to an overall drier mode. This was accompanied by the disappearance of M. scheuchzeri from Europe and its limitation, west of the Appalachians, to the wettest available habitats on the landscape. Thus, our data falsify the hypothesis that M. scheuchzeri was a conventional xerophyte, but highlight the paradox of a plant with apparent xeromorphic features confined to a wetland habitat. We consider several possible explanations for this association: (1) response to nutrient deficiency, (2) response to substrate salinity (due to growth in coastal mangrove habitats), (3) response to the composition of the Palaeozoic atmosphere, (4) return on investment (long leaf lifespan), and (5) phylogenetic constraint reflecting ancestral conditions. Our findings have broader implications for interpreting a wide variety of other Pennsylvanian wetland plants, which similarly show 'xermorphic' features. Published by Elsevier B.V.
C1 [DiMichele, William A.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
[Stull, Gregory W.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Stull, Gregory W.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England.
[Falcon-Lang, Howard J.] Univ Munster, Forsch Stelle Palaobot, Geol Palaontol Inst, D-48143 Munster, Germany.
[Nelson, W. John; Elrick, Scott] Illinois State Geol Survey, Coal Sect, Champaign, IL 61820 USA.
RP DiMichele, WA (reprint author), NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
EM dimichel@si.edu
RI DiMichele, William/K-4301-2012
FU National Museum of Natural History; SI Endowment Funds; NERC
[NE/F014120/2]; Humboldt Fellowship for Advanced Researchers
FX GS acknowledges support from the Natural History Research Experiences
(NHRE) internship program offered by the National Museum of Natural
History. WD acknowledges support from the NMNH Small Grants program and
the SI Endowment Funds. HFL acknowledges a NERC Advanced Fellowship
(NE/F014120/2) held at Royal Holloway and a Humboldt Fellowship for
Advanced Researchers held at the Universitat Munster. We thank Robyn
Burnham for comments on the manuscript, Martin Buzas for discussion
about the statistical analysis, Robert Hook for providing detailed
information on Texas stratigraphy, Josephine Sanchez and Dan S. Chaney
for assistance with photography and other tasks related to this work,
and Hans Kerp for sharing his wide knowledge of Palaeozoic
pteridosperms. Hermann Pfefferkorn and an anonymous reviewer made
critical suggestions on an earlier version of this paper, which resulted
in substantial improvements. We sincerely thank Philip Heckel for his
advice on the stratigraphy that underlies Fig. 1, and Robert Wagner for
sharing his thoughts on plant biostratigraphy and the distribution on
Macroneuropteris scheuchzeri in Europe. We are also indebted to many
coal-mine operators and private property owners for permission to
collect fossils on their land.
NR 154
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U1 4
U2 19
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-0182
EI 1872-616X
J9 PALAEOGEOGR PALAEOCL
JI Paleogeogr. Paleoclimatol. Paleoecol.
PD MAY 1
PY 2012
VL 331
BP 162
EP 176
DI 10.1016/j.palaeo.2012.03.019
PG 15
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA 941PY
UT WOS:000303976300013
ER
PT J
AU Chen, HD
Zhang, J
Ma, SL
AF Chen, Hua-Dong
Zhang, Jun
Ma, Su-Li
TI The kinematics of an untwisting solar jet in a polar coronal hole
observed by SDO/AIA
SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS
LA English
DT Article
DE Sun: activity; Sun: chromosphere; Sun: magnetic fields; Sun: flares;
Sun: rotation
ID H-ALPHA-SURGES; X-RAY JETS; MAGNETIC-FIELD STRENGTH; EXTREME-ULTRAVIOLET
JETS; ACTIVE-REGION; FINE-STRUCTURE; EMERGING FLUX; HINODE XRT; QUIET
SUN; MARCH 19
AB Using the multi-wavelength data from the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) spacecraft, we study a jet occurring in a coronal hole near the northern pole of the Sun. The jet presented distinct upward helical motion during ejection. By tracking six identified moving features (MFs) in the jet, we found that the plasma moved at an approximately constant speed along the jet's axis. Meanwhile, the MFs made a circular motion in the plane transverse to the axis. Inferred from linear and trigonometric fittings to the axial and transverse heights of the six tracks, the mean values of the axial velocities, transverse velocities, angular speeds, rotation periods, and rotation radii of the jet are 114 km s(-1), 136 km s(-1), 0.81 degrees s(-1), 452 s and 9.8 x 10(3) km respectively. As the MFs rose, the jet width at the corresponding height increased. For the first time, we derived the height variation of the longitudinal magnetic field strength in the jet from the assumption of magnetic flux conservation. Our results indicate that at heights of 1 x 10(4) similar to 7 x 10(4) km from the base of the jet, the flux density in the jet decreases from about 15 to 3 G as a function of B = 0.5(R/R-circle dot - 1)(-0.84) (G) A comparison was made with other results in previous studies.
C1 [Chen, Hua-Dong; Ma, Su-Li] China Univ Petr, Coll Sci, Qingdao 266555, Peoples R China.
[Chen, Hua-Dong; Zhang, Jun] Chinese Acad Sci, Natl Astron Observ, Key Lab Solar Act, Beijing 100012, Peoples R China.
[Ma, Su-Li] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Chen, HD (reprint author), China Univ Petr, Coll Sci, Qingdao 266555, Peoples R China.
EM hdchen@upc.edu.cn
RI Ma, Suli/J-9141-2012; Ma, Suli/F-2232-2014
OI Ma, Suli/0000-0002-5431-6065
FU National Natural Science Foundation of China [11103090, 11025315,
40890161, 10921303, 40825014, 40890162]; CAS [KJCX2-YW-T04]; National
Basic Research Program of China (973 Program) [2011CB811403]; Shandong
Provincial Natural Science Foundation, China [ZR 2011AQ009]
FX The authors sincerely thank the anonymous referee for very helpful and
constructive comments that improved this paper. We are grateful to all
the members of the Solar Magnetism and Activity group of National
Astronomical Observatories of CAS for their invaluable help. We
acknowledge the AIA team for easy access to the calibrated data. The AIA
data are courtesy of SDO (NASA) and the AIA consortium. This work was
supported by the National Natural Science Foundation of China (Grant
Nos. 11103090, 11025315, 40890161, 10921303, 40825014, and 40890162),
the CAS project KJCX2-YW-T04, the National Basic Research Program of
China (973 Program, No. 2011CB811403), and the Shandong Provincial
Natural Science Foundation, China (ZR 2011AQ009).
NR 77
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PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES
PI BEIJING
PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA
SN 1674-4527
J9 RES ASTRON ASTROPHYS
JI Res. Astron. Astrophys.
PD MAY
PY 2012
VL 12
IS 5
BP 573
EP 583
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 946WA
UT WOS:000304387000009
ER
PT J
AU Montes, C
Cardona, A
McFadden, R
Moron, SE
Silva, CA
Restrepo-Moreno, S
Ramirez, DA
Hoyos, N
Wilson, J
Farris, D
Bayona, GA
Jaramillo, CA
Valencia, V
Bryan, J
Flores, JA
AF Montes, Camilo
Cardona, A.
McFadden, R.
Moron, S. E.
Silva, C. A.
Restrepo-Moreno, S.
Ramirez, D. A.
Hoyos, N.
Wilson, J.
Farris, D.
Bayona, G. A.
Jaramillo, C. A.
Valencia, V.
Bryan, J.
Flores, J. A.
TI Evidence for middle Eocene and younger land emergence in central Panama:
Implications for Isthmus closure
SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN
LA English
DT Article
ID TRACK ANNEALING KINETICS; CENTRAL-AMERICAN ISTHMUS; SINGLE-GRAIN AGES;
SOUTH-AMERICA; STATISTICAL-MODELS; TECTONIC EVOLUTION; WESTERN COLOMBIA;
HELIUM DIFFUSION; APATITE; FISSION
AB The rise of the Isthmus of Panama, linked to a number of climatic, paleoceanographic, and biological events, has been studied mostly from indirect, often distal, geochemical and biotic evidence. We have upgraded existing geologic mapping in central Panama with more than 2000 field stations, over 40 petrographic analyses, and more than 30 new geochronological and thermochronological analyses. This data set suggests that the isthmus was an uninterrupted chain above sea level from late Eocene until at least late Miocene times. The basement complex of central Panama is a folded-faulted, similar to 3-km-thick arc sequence, intruded by granitoid bodies and onlapped by mildly deformed upper Eocene and Oligocene strata. Six U/Pb zircon ages in the granitoids-along with published geochronological data-reveal intense late Paleocene to middle Eocene magmatism (58-39 Ma), a temporary cessation of magmatic activity between 38 and 27 Ma, and renewed magmatism between 25 and 15 Ma in a position similar to 75 km south of the former magmatic axis. Thermochronological analyses in zircon (eight U-Th/He ages), and in apatite crystals (four U-Th/He ages and nine fission-track ages) obtained from a subset of 58-54 Ma granitoid bodies record a concordant Lutetian-age (47-42 Ma) cooling from similar to 200 degrees C to similar to 70 degrees C in similar to 5 m.y., and cooling below similar to 40 degrees C between 12 and 9 Ma. Cooling is linked to exhumation by an angular unconformity that separates the deformed basement complex below from mildly deformed, upper Eocene to Oligocene terrestrial to shallow-marine strata above. Exhumation and erosion of the basement complex are independently confirmed by lower Miocene strata that have a detrital zircon signature that closely follows the central Panama basement complex age distribution. These results greatly restrict the width and depth of the strait separating southern Central America from South America, and challenge the widely accepted notion that the Central American Seaway closed in late Pliocene time, when the ice age began.
C1 [Montes, Camilo; Cardona, A.; McFadden, R.; Moron, S. E.; Silva, C. A.; Restrepo-Moreno, S.; Ramirez, D. A.; Hoyos, N.; Wilson, J.; Jaramillo, C. A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Montes, Camilo] Univ de los Andes, Bogota, DC, Colombia.
[Cardona, A.] Univ Nacl Colombia, Medellin, Colombia.
[Restrepo-Moreno, S.] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA.
[Farris, D.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Bayona, G. A.] Corp Geolog Ares, Bogota, Colombia.
[Valencia, V.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[Bryan, J.] NW Florida State Coll, Niceville, FL 32578 USA.
[Flores, J. A.] Univ Salamanca, Dept Geol, Fac Ciencias, E-37008 Salamanca, Spain.
RP Montes, C (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama.
EM cmontes@uniandes.edu.co
RI Flores, Jose-Abel/D-4218-2009;
OI Flores, Jose-Abel/0000-0003-1909-293X; Ramirez,
Diego/0000-0001-6018-3273; Montes, Camilo/0000-0002-3553-0787
FU ACP (Panama Canal Authority) [SAA-199520-KRP]; Senacyt [SUM-07-001,
EST010-080 A]; Colciencias, U.S. National Science Foundation (NSF)
[0966884]; Mark Tupper, NSF [EAR-0824299]; National Geographic;
Smithsonian Institution; Ricardo Perez S.A.
FX This project was supported by ACP (Panama Canal Authority) contract
SAA-199520-KRP; Senacyt grants SUM-07-001 and EST010-080 A; Colciencias,
U.S. National Science Foundation (NSF) grant 0966884 (OISE, EAR, DRL),
Mark Tupper, NSF EAR-0824299, National Geographic, Smithsonian
Institution, and Ricardo Perez S.A. Thanks go to H. Broce, F. Guardia,
P. Francesci, V. Luque, A. Baresh, F. Moreno, and L. Oviedo for their
help. G. Worner kindly provided early copies of his manuscripts and
data. Access to field areas and collection permits were granted by ACP,
Ministerio de Industria y Comercio, and Odebretch. We are grateful to P.
Molnar, S. Johnston, J. Pindell, P. Mann, D. Foster, and P. O'Sullivan,
as well as to all participants of the February 2010 IGCP (International
Union of Geological Sciences) 546 "Subduction Zones of the Caribbean"
and IGCP 574 "Bending and Bent Orogens, and Continental Ribbons" for
their critical reviews.
NR 95
TC 130
Z9 134
U1 7
U2 88
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0016-7606
J9 GEOL SOC AM BULL
JI Geol. Soc. Am. Bull.
PD MAY-JUN
PY 2012
VL 124
IS 5-6
BP 780
EP 799
DI 10.1130/B30528.1
PG 20
WC Geosciences, Multidisciplinary
SC Geology
GA 937XG
UT WOS:000303696600010
ER
PT J
AU Jackson, FE
Roberts, TP
Alexander, DM
Gelbord, JM
Goulding, AD
Ward, MJ
Wardlow, JL
Watson, MG
AF Jackson, F. E.
Roberts, T. P.
Alexander, D. M.
Gelbord, J. M.
Goulding, A. D.
Ward, M. J.
Wardlow, J. L.
Watson, M. G.
TI On the nature of high X-ray luminosities in Sloan Digital Sky Survey
galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: starburst
ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; ULTRALUMINOUS INFRARED
GALAXIES; POINT-SOURCE CATALOGS; STAR-FORMATION RATE; XMM-NEWTON;
STARBURST GALAXIES; OPTICAL SPECTROSCOPY; SEYFERT-GALAXIES; NEARBY
GALAXIES
AB Surveys have revealed a class of object displaying both high X-ray luminosities (L-X > 10(42) erg s(-1)) and a lack of a discernible active galactic nucleus (AGN) in the optical band. If these sources are powered by star formation activity alone, they would be the most extreme X-ray luminosity star-forming galaxies known. We have investigated the mechanism driving the X-ray luminosities of such galaxies by studying the X-ray emission of three moderate redshift (z similar to 0.1) examples of this class, selected from a cross-correlation of the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5) and XMM-Newton serendipitous survey (2XMMp-DR0) catalogues. X-ray spatial and long-term variability diagnostics of these sources suggest that they are compact X-ray emitters. This result is supported by the detection of rapid short-term variability in an observation of one of the sources. The X-ray spectra of all three sources are best fitted with a simple absorbed power-law model, thus betraying no significant signs of star formation. These results indicate that the X-ray emission is powered by AGN activity. But why do these sources not display optical AGN signatures? We show that the most likely explanation is that the optical AGN emission lines are being diluted by star formation signatures from within their host galaxies.
C1 [Jackson, F. E.; Roberts, T. P.; Alexander, D. M.; Gelbord, J. M.; Goulding, A. D.; Ward, M. J.; Wardlow, J. L.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Gelbord, J. M.] Penn State Univ, Dept Astron & Astrophys, Eberly Coll Sci, Davey Lab 525, University Pk, PA 16802 USA.
[Goulding, A. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wardlow, J. L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Watson, M. G.] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England.
RP Jackson, FE (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England.
EM fjackson@head.cfa.harvard.edu
RI Wardlow, Julie/C-9903-2015;
OI Wardlow, Julie/0000-0003-2376-8971; Alexander, David/0000-0002-5896-6313
FU Alfred P. Sloan Foundation; National Science Foundation; US Department
of Energy; National Aeronautics and Space Administration; Japanese
Monbukagakusho; Max Planck Society; Higher Education Funding Council for
England
FX This work is based on observations obtained with XMM-Newton, an ESA
science mission with instruments and contributions directly funded by
ESA Member States and the USA (NASA). This research has made use of
software provided by the Chandra X-ray Center (CXC) in the application
package CIAO. Funding for the SDSS and SDSS-II has been provided by the
Alfred P. Sloan Foundation, the Participating Institutions, the National
Science Foundation, the US Department of Energy, the National
Aeronautics and Space Administration, the Japanese Monbukagakusho, the
Max Planck Society and the Higher Education Funding Council for England.
The SDSS website is http://www.sdss.org/. The SDSS is managed by the
Astrophysical Research Consortium for the Participating Institutions.
This research has made use of the NASA/IPAC Extragalactic Database
(NED), which is operated by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration. This research has also made use of the SIMBAD
data base, operated at CDS, Strasbourg, France.
NR 86
TC 3
Z9 3
U1 0
U2 3
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 MAY
PY 2012
VL 422
IS 1
BP 2
EP 13
DI 10.1111/j.1365-2966.2011.20164.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940SE
UT WOS:000303912600022
ER
PT J
AU Danielson, ALR
Lehmer, BD
Alexander, DM
Brandt, WN
Luo, B
Miller, N
Xue, YQ
Stott, JP
AF Danielson, A. L. R.
Lehmer, B. D.
Alexander, D. M.
Brandt, W. N.
Luo, B.
Miller, N.
Xue, Y. Q.
Stott, J. P.
TI The cosmic history of hot gas cooling and radio active galactic nucleus
activity in massive early-type galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: evolution; X-rays:
galaxies
ID DEEP-FIELD-SOUTH; YALE-CHILE MUSYC; SUPERMASSIVE BLACK-HOLE;
NEAR-INFRARED CATALOG; POINT-SOURCE CATALOGS; 1.4 GHZ OBSERVATIONS;
X-RAY LUMINOSITY; ELLIPTIC GALAXIES; PHOTOMETRIC REDSHIFTS; JET POWER
AB We study the X-ray properties of 393 optically selected early-type galaxies (ETGs) over the redshift range of z approximate to 0.0-1.2 in the Chandra Deep Fields (CDFs). To measure the average X-ray properties of the ETG population, we use X-ray stacking analyses with a subset of 158 passive ETGs (148 of which were individually undetected in X-ray). This ETG subset was constructed to span the redshift ranges of z = 0.1-1.2 in the approximate to 4 Ms CDF-South and approximate to 2 Ms CDF-North and z = 0.1-0.6 in the approximate to 250 ks Extended-CDF-South where the contribution from individually undetected active galactic nuclei (AGN) is expected to be negligible in our stacking. We find that 55 of the ETGs are detected individually in X-ray, and 12 of these galaxies have properties consistent with being passive hot-gas-dominated systems (i.e. systems not dominated by an X-ray bright AGN). On the basis of our analyses, we find little evolution in the mean 0.5-2 keV to B-band luminosity ratio (L-X/L-B proportional to [1 + z](1.2)) since z approximate to 1.2, implying that some heating mechanism prevents the gas from cooling in these systems. We consider that feedback from radio-mode AGN activity could be responsible for heating the gas. We select radio AGN in the ETG population using their far-infrared/radio flux ratio. Our radio observations allow us to constrain the duty cycle history of radio AGN activity in our ETG sample. We estimate that if scaling relations between radio and mechanical power hold out to z approximate to 1.2 for the ETG population being studied here, the average mechanical power from AGN activity is a factor of approximate to 1.4-2.6 times larger than the average radiative cooling power from hot gas over the redshift range z approximate to 0-1.2. The excess of inferred AGN mechanical power from these ETGs is consistent with that found in the local Universe for similar types of galaxies.
C1 [Danielson, A. L. R.; Lehmer, B. D.; Alexander, D. M.; Stott, J. P.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Brandt, W. N.; Xue, Y. Q.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Brandt, W. N.; Xue, Y. Q.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Luo, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Miller, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Danielson, ALR (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England.
EM a.l.r.danielson@durham.ac.uk
RI Brandt, William/N-2844-2015;
OI Brandt, William/0000-0002-0167-2453; Stott, John/0000-0002-1679-9983;
Alexander, David/0000-0002-5896-6313
FU STFC; Einstein Fellowship program; CXC [SP1-12007A]
FX We thank the anonymous referee for their helpful comments. ALRD
acknowledges an STFC studentship. We would like to thank Ian Smail for
useful comments and feedback on this work. We also thank Philip Best for
providing us with his sample for comparing to our work and Laura Birzan
for useful advice. BDL acknowledges financial support from the Einstein
Fellowship program. WNB and YQX thank CXC grant SP1-12007A. DMA
acknowledges financial support from STFC.
NR 87
TC 9
Z9 9
U1 0
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 1
BP 494
EP 509
DI 10.1111/j.1365-2966.2012.20626.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940SE
UT WOS:000303912600055
ER
PT J
AU Chakravorty, S
Misra, R
Elvis, M
Kembhavi, AK
Ferland, G
AF Chakravorty, Susmita
Misra, Ranjeev
Elvis, Martin
Kembhavi, Ajit K.
Ferland, Gary
TI The influence of soft spectral components on the structure and stability
of warm absorbers in active galactic nuclei
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; quasars: absorption lines; galaxies: Seyfert; X-rays:
galaxies; X-rays: ISM
ID X-RAY-SPECTRA; XMM-NEWTON OBSERVATIONS; QUASI-STELLAR OBJECTS;
SUPERSOLAR METAL ABUNDANCES; HIGH-REDSHIFT QUASARS; RADIO-QUIET QUASARS;
BROAD-LINE REGION; BIG BLUE BUMP; ACCRETION DISKS; ENERGY-DISTRIBUTIONS
AB The radiation from the central regions of active galactic nuclei, including that from the accretion disc surrounding the black hole, is likely to peak in the extreme-ultraviolet similar to 13-100 eV. However, due to Galactic absorption, we are limited to constrain the physical properties, i.e. the black hole mass and the accretion rate, from what observations we have below similar to 10 eV or above similar to 100 eV. In this paper, we predict the thermal and ionization states of warm absorbers as a function of the shape of the unobservable continuum. In particular we model an accretion disc at kT(in) similar to 10 eV and a soft excess at kT(se) similar to 150 eV. The warm absorber, which is the highly ionized gas along the line of sight to the continuum, shows signatures in the similar to 0.3-2 keV energy range consisting of numerous absorption lines and edges of various ions, some of the prominent ones being H- and He-like oxygen, neon, magnesium and silicon. We find that the properties of the warm absorber are significantly influenced by the changes in the temperature of the accretion disc, as well as by the strength of the soft excess, as they affect the optical depth particularly for iron and oxygen. These trends may help develop a method of characterizing the shape of the unobservable continuum and the occurrence of warm absorbers.
C1 [Chakravorty, Susmita; Misra, Ranjeev; Kembhavi, Ajit K.] IUCAA, Pune 411007, Maharashtra, India.
[Chakravorty, Susmita] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Chakravorty, Susmita; Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ferland, Gary] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA.
RP Chakravorty, S (reprint author), IUCAA, Post Bag 4, Pune 411007, Maharashtra, India.
EM schakravorty@head.cfa.harvard.edu; rmisra@iucaa.ernet.in;
elvis@head.cfa.harvard.edu; akk@iucaa.ernet.in; gary@pa.uky.edu
OI Ferland, Gary/0000-0003-4503-6333
NR 97
TC 11
Z9 11
U1 1
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 1
BP 637
EP 651
DI 10.1111/j.1365-2966.2012.20641.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940SE
UT WOS:000303912600067
ER
PT J
AU Schmidtobreick, L
Rodriguez-Gil, P
Long, KS
Gansicke, BT
Tappert, C
Torres, MAP
AF Schmidtobreick, L.
Rodriguez-Gil, P.
Long, K. S.
Gaensicke, B. T.
Tappert, C.
Torres, M. A. P.
TI Discovery of H alpha satellite emission in a low state of the SW
Sextantis star BB Doradus
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; magnetic fields; stars: activity; stars:
individual: BB Dor; novae, cataclysmic variables; stars: winds, outflows
ID ROTATING MAGNETOSPHERE MODEL; DW URSAE MAJORIS; CATACLYSMIC VARIABLES;
AM-HERCULIS; WHITE-DWARF; SECONDARY-STAR; TT-ARIETIS; SPECTROSCOPY;
BINARIES; DISTRIBUTIONS
AB BB Dor was observed during its low state in 2009. Signatures of both binary components are revealed in the average optical spectrum; no signature of accretion is observed. Narrow emission lines of H alpha, He I and Na D, as well as TiO absorption troughs, trace the motion of the irradiated secondary star. We detect two additional components in the H alpha emission line that share many characteristics of similar 'satellite' lines observed in the low state of magnetic cataclysmic variables of AM Her type. It is the first time such emission components are detected for an SW Sex star.
C1 [Schmidtobreick, L.] European So Observ, Santiago 19, Chile.
[Rodriguez-Gil, P.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Santa Cruz De T, Spain.
[Rodriguez-Gil, P.] Univ La Laguna, Dept Astrofis, E-38203 San Cristobal la Laguna, Santa Cruz De T, Spain.
[Rodriguez-Gil, P.] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De La Palma, Spain.
[Long, K. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gaensicke, B. T.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Tappert, C.] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile.
[Torres, M. A. P.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Schmidtobreick, L (reprint author), European So Observ, Casilla 19001, Santiago 19, Chile.
EM lschmidt@eso.org
RI Gaensicke, Boris/A-9421-2012; Rodriguez-Gil, Pablo/H-7709-2015
OI Gaensicke, Boris/0000-0002-2761-3005; Rodriguez-Gil,
Pablo/0000-0002-4717-5102
FU European Southern Observatory, Paranal [082.D-0154]; Spanish MICINN
[CSD2006-00070]; First Science; GTC; ASTROMOL [CSD2009-00038]
FX Based on observations collected at the European Southern Observatory,
Paranal (programme 082.D-0154).; Partially funded by the Spanish MICINN
under the Consolider-Ingenio 2010 Programme grants CSD2006-00070, First
Science with the GTC, and CSD2009-00038, ASTROMOL. PR-G thanks ESO for a
stay within the Visitor Scientist programme. The use of MOLLY developed
by Tom Marsh is gratefully acknowledged. We thank the team on Paranal
for taking the spectra in ToO mode, i.e. Emanuela Pompei and Thomas
Rivinius.
NR 38
TC 4
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U1 0
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 1
BP 731
EP 737
DI 10.1111/j.1365-2966.2012.20653.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940SE
UT WOS:000303912600075
ER
PT J
AU Gibson, NP
Aigrain, S
Pont, F
Sing, DK
Desert, JM
Evans, TM
Henry, G
Husnoo, N
Knutson, H
AF Gibson, N. P.
Aigrain, S.
Pont, F.
Sing, D. K.
Desert, J. -M.
Evans, T. M.
Henry, G.
Husnoo, N.
Knutson, H.
TI Probing the haze in the atmosphere of HD 189733b with Hubble Space
Telescope/WFC3 transmission spectroscopy
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; techniques: spectroscopic; stars: individual: HD
189733; planetary systems
ID HUBBLE-SPACE-TELESCOPE; TIME-SERIES PHOTOMETRY; EXTRASOLAR PLANET;
RAYLEIGH-SCATTERING; MU-M; SPECTRUM; TRANSIT; HD-189733; SPITZER
AB We present Hubble Space Telescope near-infrared transmission spectroscopy of the transiting exoplanet HD 189733b, using the Wide Field Camera 3 (WFC3). This consists of time series spectra of two transits, used to measure the wavelength dependence of the planetary radius. These observations aim to test whether the Rayleigh scattering haze detected at optical wavelengths extends into the near-infrared, or if it becomes transparent leaving molecular features to dominate the transmission spectrum. Due to saturation and non-linearity affecting the brightest (central) pixels of the spectrum, light curves were extracted from the blue and red ends of the spectra only, corresponding to wavelength ranges of 1.099-1.168 and 1.521-1.693 mu m, respectively, for the first visit, and 1.082-1.128 and 1.514-1.671 mu m for the second. The light curves were fitted using a Gaussian process model to account for instrumental systematics whilst simultaneously fitting for the transit parameters. This gives values of the planet-to-star radius ratio for the blue and red light curves of 0.156 50 +/- 0.000 48 and 0.156 34 +/- 0.000 32, respectively, for visit 1 and 0.157 16 +/- 0.000 78 and 0.156 30 +/- 0.000 37 for visit 2 (using a quadratic limb-darkening law). The planet-to-star radius ratios measured in both visits are consistent, and we see no evidence for the drop in absorption expected if the haze that is observed in the optical becomes transparent in the infrared. This tentatively suggests that the haze dominates the transmission spectrum of HD 189733b into near-infrared wavelengths, although more robust observations are required to provide conclusive evidence.
C1 [Gibson, N. P.; Aigrain, S.; Evans, T. M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Pont, F.; Sing, D. K.; Husnoo, N.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Henry, G.] Tennessee State Univ, Nashville, TN 37209 USA.
[Knutson, H.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Gibson, NP (reprint author), Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
EM neale.gibson@astro.ox.ac.uk
OI Gibson, Neale/0000-0002-9308-2353; Sing, David /0000-0001-6050-7645
FU NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; STFC
[ST/G002266/2]; WFC3 instrument team
FX All of the data presented in this paper were obtained from the
Multi-mission Archive at the Space Telescope Science Institute (MAST).
STScI is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for
non-HST data is provided by the NASA Office of Space Science via grant
NNX09AF08G and by other grants and contracts. NPG and SA acknowledge
support from STFC grant ST/G002266/2. We are extremely grateful for the
support provided the WFC3 instrument team, in particular H. Bushouse,
and discussions with P. McCullough. Finally, we thank the referee, R.
Gilliland, for his careful reading of the manuscript and helpful
suggestions.
NR 33
TC 54
Z9 55
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 MAY
PY 2012
VL 422
IS 1
BP 753
EP 760
DI 10.1111/j.1365-2966.2012.20655.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940SE
UT WOS:000303912600077
ER
PT J
AU Wilcock, LA
Ward-Thompson, D
Kirk, JM
Stamatellos, D
Whitworth, A
Elia, D
Fuller, GA
DiGiorgio, A
Griffin, MJ
Molinari, S
Martin, P
Mottram, JC
Peretto, N
Pestalozzi, M
Schisano, E
Plume, R
Smith, HA
Thompson, MA
AF Wilcock, L. A.
Ward-Thompson, D.
Kirk, J. M.
Stamatellos, D.
Whitworth, A.
Elia, D.
Fuller, G. A.
DiGiorgio, A.
Griffin, M. J.
Molinari, S.
Martin, P.
Mottram, J. C.
Peretto, N.
Pestalozzi, M.
Schisano, E.
Plume, R.
Smith, H. A.
Thompson, M. A.
TI Cores in infrared dark clouds (IRDCs) seen in the Hi-GAL survey between
l=300 degrees and 330 degrees
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation
ID MASSIVE STAR-FORMATION; GALACTIC PLANE; INSTRUMENT; CANDIDATES;
PROTOSTARS; EMISSION; CLUSTERS; CATALOG; RADIO
AB We have used data taken as part of the Herschel infrared Galactic Plane survey (Hi-GAL) to study 3171 infrared dark cloud (IRDC) candidates that were identified in the mid-IR (8 mu m) by Spitzer (we refer to these as 'Spitzer-dark' regions). They all lie in the range l = 300-330 degrees and vertical bar b vertical bar <= 1 degrees. Of these, only 1205 were seen in emission in the far-IR (250-500 mu m) by Herschel (we call these 'Herschel-bright' clouds). It is predicted that a dense cloud will not only be seen in absorption in the mid-IR, but will also be seen in emission in the far-IR at the longest Herschel wavebands (250-500 mu m). If a region is dark at all wavelengths throughout the mid-IR and far-IR, then it is most likely to be simply a region of lower background IR emission (a 'hole in the sky'). Hence, it appears that previous surveys, based on Spitzer and other mid-IR data alone, may have overestimated the total IRDC population by a factor of similar to 2. This has implications for estimates of the star formation rate in IRDCs in the Galaxy. We studied the 1205 Herschel-bright IRDCs at 250 mu m and found that 972 of them had at least one clearly defined 250-mu m peak, indicating that they contained one or more dense cores. Of these, 653 (67 per cent) contained an 8-mu m point source somewhere within the cloud, 149 (15 per cent) contained a 24-mu m point source but no 8-mu m source and 170 (18 per cent) contained no 24- or 8-mu m point sources. We use these statistics to make inferences about the lifetimes of the various evolutionary stages of IRDCs.
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.
[DiGiorgio, A.; Molinari, S.; Pestalozzi, M.; Schisano, E.] CNR, Inst Fis Spazio Interplanetario, I-00133 Rome, Italy.
[Elia, D.; 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.
[Peretto, N.] CEA DSM CNRS Univ Paris Diderot, Lab AIM, IFRU Serv Astrophys, CE Saclay, F-91191 Gif Sur Yvette, France.
[Plume, R.] Univ Calgary, Dept Phys Astron, Calgary, AB T2N 1N4, Canada.
[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
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 acknowledges STFC studentship funding. SPIRE was developed by a
consortium of institutes led by Cardiff University (UK) and including
Univ. Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, Univ.
Padua (Italy); IAC (Spain); Stockholm-Observatory (Sweden); Imperial
College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech,
JPL, NHSC, Univ. Colorado (USA). This development was 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); IAC (Spain). This development was 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. This work is also based, in part, on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA.
NR 46
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PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 2
BP 1071
EP 1082
DI 10.1111/j.1365-2966.2012.20680.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940SG
UT WOS:000303912800013
ER
PT J
AU Guidorzi, C
Margutti, R
Amati, L
Campana, S
Orlandini, M
Romano, P
Stamatikos, M
Tagliaferri, G
AF Guidorzi, C.
Margutti, R.
Amati, L.
Campana, S.
Orlandini, M.
Romano, P.
Stamatikos, M.
Tagliaferri, G.
TI Average power density spectrum of Swift long gamma-ray bursts in the
observer and in the source-rest frames
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; gamma-ray burst: general
ID INTERNAL SHOCK MODEL; LIGHT CURVES; COSMOLOGICAL PARAMETERS; CENTRAL
ENGINE; VARIABILITY; ACCRETION; DURATION; ORIGIN; GRB; EMISSION
AB We calculate the average power density spectra (PDSs) of 244 long gamma-ray bursts detected with the Swift Burst Alert Telescope (BAT) in the 15-150 keV band from 2005 January to 2011 August. For the first time we derived the average PDS in the source-rest frame of 97 gamma-ray bursts (GRBs) with known redshift. For 49 of them an average PDS was also obtained in a common source-frame energy band to account for the dependence of time profiles on energy. Previous results obtained on Burst and Transient Source Experiment (BATSE) GRBs with unknown redshift showed that the average spectrum in the 25-2000 keV band could be modelled with a power law with a 5/3 index over nearly two decades of frequency with a break at similar to 1 Hz. Depending on the normalization and on the subset of GRBs considered, our results show analogous to steeper slopes (between 1.7 and 2.0) of the power law. However, no clear evidence for the break at similar to 1 Hz was found, although the softer energy band of BAT compared with BATSE might account for that. We instead find a break at lower frequency corresponding to a typical source-rest-frame characteristic time of a few seconds. We furthermore find no significant differences between observer-and source-rest frames. Notably, no distinctive PDS features are found for GRBs with different intrinsic properties of the prompt emission either. Finally, the average PDS of GRBs at higher redshifts shows possibly shallower power-law indices than that of low-z GRBs. It is not clear whether this is due to an evolution with z of the average PDS.
C1 [Guidorzi, C.] Univ Ferrara, Dept Phys, I-44122 Ferrara, Italy.
[Margutti, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Amati, L.; Orlandini, M.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-40129 Bologna, Italy.
[Campana, S.; Tagliaferri, G.] INAF, Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Romano, P.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-90146 Palermo, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
RP Guidorzi, C (reprint author), Univ Ferrara, Dept Phys, Via Saragat 1, I-44122 Ferrara, Italy.
EM guidorzi@fe.infn.it
RI Amati, Lorenzo/N-5586-2015; Orlandini, Mauro/H-3114-2014;
OI Amati, Lorenzo/0000-0001-5355-7388; Orlandini,
Mauro/0000-0003-0946-3151; Campana, Sergio/0000-0001-6278-1576;
Tagliaferri, Gianpiero/0000-0003-0121-0723
FU ASI [I/088/06/0]
FX CG acknowledges ASI for financial support (ASI-INAF contract
I/088/06/0).
NR 50
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U1 0
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 2
BP 1785
EP 1803
DI 10.1111/j.1365-2966.2012.20758.x
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940SG
UT WOS:000303912800075
ER
PT J
AU Stone, N
Loeb, A
AF Stone, Nicholas
Loeb, Abraham
TI Tidal disruption flares of stars from moderately recoiled black holes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE black hole physics; gravitational waves; galaxies: nuclei
ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; GRAVITATIONAL-WAVE RECOIL;
ACTIVE GALACTIC NUCLEI; SDSS J092712.65+294344.0; DYNAMICAL FRICTION;
ACCRETION DISCS; SPIN EVOLUTION; CENTERS; BINARIES
AB We analyse stellar tidal disruption events as a possible observational signature of gravitational wave induced recoil of supermassive black holes. As a black hole wanders through its galaxy, it will tidally disrupt bound and unbound stars at rates potentially observable by upcoming optical transient surveys. To quantify these rates, we explore a broad range of host galaxy and black hole kick parameters. We find that emission from a transient accretion disc can produce similar to 1 event per year which the Large Synoptic Survey Telescope would identify as spatially offset, while super-Eddington outflows, if they exist, are likely to produce similar to 10 spatially offset events per year. A majority of tidal disruption flares, and a large majority of flares with an observable spatial offset, are due to bound rather than unbound stars. The total number of disruption events due to recoiled black holes could be almost 1 per cent of the total stellar tidal disruption rate.
C1 [Stone, Nicholas; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Stone, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nstone@cfa.harvard.edu; aloeb@cfa.harvard.edu
FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A]
FX We thank Laura Blecha, Alister Graham, Bence Kocsis and Ryan O'Leary for
helpful suggestions. This work was supported in part by NSF grant
AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A.
NR 91
TC 15
Z9 15
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 3
BP 1933
EP 1947
DI 10.1111/j.1365-2966.2012.20577.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939YZ
UT WOS:000303858400008
ER
PT J
AU Natarajan, P
Volonteri, M
AF Natarajan, Priyamvada
Volonteri, Marta
TI The mass function of black holes 1 < z < 4.5: comparison of models with
observations
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: nuclei; quasars: general; cosmology: observations; cosmology:
theory
ID DARK-MATTER HALOES; HIGH-REDSHIFT; VELOCITY DISPERSION; LUMINOSITY
FUNCTION; ANGULAR-MOMENTUM; 1ST STARS; GROWTH; EVOLUTION; QUASARS;
ACCRETION
AB In this paper, we compare the observationally derived black hole mass function (BHMF) of luminous (>10451046 erg s-1) broad-line quasars (BLQSOs) at 1 < z < 4.5 drawn from the Sloan Digital Sky Survey (SDSS) presented by Kelly et al., with models of merger-driven black hole (BH) growth in the context of standard hierarchical structure formation models. In these models, we explore two distinct black hole seeding prescriptions at the highest redshifts: light seeds remnants of Population III stars and massive seeds that form from the direct collapse of pre-galactic discs. The subsequent merger triggered mass build-up of the black hole population is tracked over cosmic time under the assumption of a fixed accretion rate as well as rates drawn from the distribution derived by Merloni & Heinz. Four model snapshots at z= 1.25, 2, 3.25 and 4.25 are compared with the SDSS-derived BHMFs of BLQSOs. We find that the light seed models fall short of reproducing the observationally derived mass function of BLQSOs at MBH > 109 M? throughout the redshift range; the massive seed models with a fixed accretion rate of 0.3 Edd, or with accretion rates drawn from the Merloni & Heinz distribution provide the best fit to the current observational data at z > 2, although they overestimate the high-mass end of the mass function at lower redshifts. At low redshifts, a drastic drop in the accretion rate is observed and this is explained as arising due to the diminished gas supply available due to consumption by star formation or changes in the geometry of the inner feeding regions. Therefore, the overestimate at the high-mass end of the black hole mass function for the massive seed models can be easily modified, as the accretion rate is likely significantly lower at these epochs than what we assume. For the Merloni & Heinz model, examining the Eddington ratio distributions fEdd, we find that they are almost uniformly sampled from fEdd= 10-2 to 1 at z? 1, while at high redshift, current observations suggest accretion rates close to Eddington, if not mildly super-Eddington, at least for these extremely luminous quasars. Our key findings are that the duty cycle of super-massive black holes powering BLQSOs increases with increasing redshift for all models and models with Population III remnants as black hole seeds are unable to fit the observationally derived BHMFs for BLQSOs, lending strong support for the massive seeding model.
C1 [Natarajan, Priyamvada] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Natarajan, Priyamvada] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Volonteri, Marta] Univ Michigan, Dept Phys & Astron, Ann Arbor, MI 48109 USA.
RP Natarajan, P (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
EM priyamvada.natarajan@yale.edu
FU John Simon Guggenheim Foundation
FX PN acknowledges support from the John Simon Guggenheim Foundation and a
residency at the Rockefeller Bellagio Center where a portion of this
work was completed. She also thanks the Institute for Theory and
Computation at Harvard for hosting her during her Guggenheim Fellowship
year.
NR 50
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U1 0
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PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 3
BP 2051
EP 2057
DI 10.1111/j.1365-2966.2012.20708.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939YZ
UT WOS:000303858400016
ER
PT J
AU Rodriguez-Gil, P
Schmidtobreick, L
Long, KS
Gansicke, BT
Torres, MAP
Rubio-Diez, MM
Santander-Garcia, M
AF Rodriguez-Gil, P.
Schmidtobreick, L.
Long, K. S.
Gaensicke, B. T.
Torres, M. A. P.
Rubio-Diez, M. M.
Santander-Garcia, M.
TI The fight for accretion: discovery of intermittent mass transfer in BB
Doradus in the low state
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion; accretion discs; binaries: close; stars: individual: BB Dor;
novae; cataclysmic variables
ID MAGNETIC CATACLYSMIC VARIABLES; VY SCULPTORIS STARS; SW SEXTANTIS STARS;
X-RAY OBSERVATIONS; AM-HERCULIS; EFFECTIVE TEMPERATURES; WHITE-DWARFS;
PERIOD GAP; XMM-NEWTON; OLD NOVAE
AB Our long-term photometric monitoring of southern nova-like cataclysmic variables with the 1.3-m Small and Moderate Aperture Research Telescope System (SMARTS) telescope found BB Doradus fading from V similar to 14.3 towards a deep low state at V similar to 19.3 in 2008 April. Here we present time-resolved optical spectroscopy of BB Dor in this faint state in 2009. The optical spectrum in quiescence is a composite of a hot white dwarf with Teff= 30 000 +/- 5000 K and a M3M4 secondary star with narrow emission lines (mainly of the Balmer series and He i) superposed. We associate these narrow profiles with an origin on the donor star. An analysis of the radial velocity curve of the Ha emission from the donor star allowed the measurement of an orbital period of 0.154 095 +/- 0.000 003 d (3.698 28 +/- 0.000 07 h), different from all previous estimates. We detected episodic accretion events which veiled the spectra of both stars and radically changed the line profiles within a time-scale of tens of minutes. This shows that accretion is not completely quenched in the low state. During these accretion episodes the line wings are stronger and their radial velocity curve is delayed by similar to 0.2 cycle, similar to that observed in SW Sex and AM Her stars in the high state, with respect to the motion of the white dwarf. Two scenarios are proposed to explain the extra emission: impact of the material on the outer edge of a cold, remnant accretion disc, or the combined action of a moderately magnetic white dwarf (B1? 5 MG) and the magnetic activity of the donor star.
C1 [Rodriguez-Gil, P.] Univ La Laguna, Dept Astrofis, E-38204 Tenerife, Spain.
[Rodriguez-Gil, P.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Rodriguez-Gil, P.] Isaac Newton Grp Telescopes, E-38700 Santa Cruz de La Palma, Spain.
[Schmidtobreick, L.] European So Observ, Santiago 19001, Chile.
[Long, K. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gaensicke, B. T.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Torres, M. A. P.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rubio-Diez, M. M.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain.
[Santander-Garcia, M.] Observ Astron Nacl, E-28803 Madrid, Spain.
RP Rodriguez-Gil, P (reprint author), Univ La Laguna, Dept Astrofis, E-38204 Tenerife, Spain.
EM prguez@iac.es
RI Gaensicke, Boris/A-9421-2012; Rodriguez-Gil, Pablo/H-7709-2015
OI Gaensicke, Boris/0000-0002-2761-3005; Rodriguez-Gil,
Pablo/0000-0002-4717-5102
FU National Science Foundation; Spanish MICINN [CSD2006-00070,
CSD2009-00038]
FX Visiting astronomer, Cerro Tololo Inter-American Observatory and
National Optical Astronomy Observatory, which are operated by the
Association of Universities for Research in Astronomy, under contract
with the National Science Foundation.; We thank the anonymous referee
for comments that improved this manuscript. The use of Tom Marsh's MOLLY
package is gratefully acknowledged. PRG thanks the ESO/Santiago Visiting
Scientist Program for the approval of a scientific visit during which
part of this work was completed. Partially funded by the Spanish MICINN
under the Consolider-Ingenio 2010 Program grants CSD2006-00070: First
Science with the GTC and CSD2009-00038: ASTROMOL. We are indebted to the
SMARTS service observers Juan Espinoza, David Gonzalez, Manuel
Hernandez, Rodrigo Hernandez, Alberto Miranda, Alberto Pasten, Mauricio
Rojas, Jacqueline Seron, Joselino Vasquez and Jose Velasquez.
NR 47
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U1 0
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 3
BP 2332
EP 2340
DI 10.1111/j.1365-2966.2012.20783.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939YZ
UT WOS:000303858400038
ER
PT J
AU Huitson, CM
Sing, DK
Vidal-Madjar, A
Ballester, GE
Etangs, ALD
Desert, JM
Pont, F
AF Huitson, C. M.
Sing, D. K.
Vidal-Madjar, A.
Ballester, G. E.
Etangs, A. Lecavelier des
Desert, J. -M.
Pont, F.
TI Temperature-pressure profile of the hot Jupiter HD 189733b from HST
sodium observations: detection of upper atmospheric heating
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: spectroscopic; planets and satellites: individual: HD
189733b; stars: individual: HD 189733
ID HUBBLE-SPACE-TELESCOPE; GIANT PLANET ATMOSPHERES; TIME-SERIES
PHOTOMETRY; EXTRASOLAR PLANET; TRANSMISSION SPECTRA; INFRARED-EMISSION;
209458B; ABSORPTION; CARBON; SPECTROSCOPY
AB We present transmission spectra of the hot Jupiter HD 189733b taken with the Space Telescope Imaging Spectrograph (STIS) aboard Hubble Space Telescope (HST). The spectra cover the wavelength range 58086380 angstrom with a resolving power of R= 5000. We detect absorption from the Na i doublet within the exoplanets atmosphere at the 9s confidence level within a 5 angstrom band (absorption depth 0.09 +/- 0.01 per cent) and use the data to measure the doublets spectral absorption profile. We detect only the narrow cores of the doublet. The narrowness of the feature could be due to an obscuring high-altitude haze of an unknown composition or a significantly sub-solar Na i abundance hiding the line wings beneath an H2 Rayleigh signature. These observations are consistent with previous broad-band spectroscopy from Advanced Camera for Surveys (ACS) and STIS, where a featureless spectrum was seen. We also investigate the effects of starspots on the Na i line profile, finding that their impact is minimal and within errors in the sodium feature. We compare the spectral absorption profile over 5.5 scale heights with model spectral absorption profiles and constrain the temperature at different atmospheric regions, allowing us to construct a vertical temperature profile. We identify two temperature regimes: a 1280 +/- 240 K region derived from the Na i doublet line wings corresponding to altitudes below similar to 500 km, and a 2800 +/- 400 K region derived from the Na i doublet line cores corresponding to altitudes from similar to 500 to 4000 km. The zero altitude is defined by the white-light radius of RP/R?= 0.15628 +/- 0.00009. The temperature rises with altitude, which is likely evidence of a thermosphere. The absolute pressure scale depends on the species responsible for the Rayleigh signature and its abundance. We discuss a plausible scenario for this species, a high-altitude silicate haze and the atmospheric temperaturepressure profile that results. In this case, the high-altitude temperature rise for HD 189733b occurs at pressures of 10-5 to 10-8 bar.
C1 [Huitson, C. M.; Sing, D. K.; Pont, F.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England.
[Vidal-Madjar, A.; Etangs, A. Lecavelier des] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France.
[Ballester, G. E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Huitson, CM (reprint author), Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England.
EM chuitson@astro.ex.ac.uk
OI HUITSON, CATHERINE/0000-0002-4734-691X; Sing, David /0000-0001-6050-7645
FU STFC; NASA [HST-GO-11576-01-A]
FX We thank David Charbonneau and Ron Gilliland for their last minute idea
of the real time HST pointing correction which saved the data quality of
visit 3. We also thank Jonathan Fortney for providing his model
atmospheres and Adam Showman for providing his model T-P profiles. We
thank our reviewer, Ignas Snellen, for pointing out problems with using
the integrated AD profile to determine atmospheric temperature. This led
us to the idea of using the spectral AD profile, which has greatly
improved the paper. This work is based on observations with the NASA/ESA
HST. This research has made use of NASA's Astrophysics Data System, and
components of the IDL astronomy library. CMH acknowledges support from
STFC. GEB acknowledges support by NASA through grant HST-GO-11576-01-A
to University of Arizona from STScI.
NR 45
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 3
BP 2477
EP 2488
DI 10.1111/j.1365-2966.2012.20805.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939YZ
UT WOS:000303858400051
ER
PT J
AU Pan, T
Kasen, D
Loeb, A
AF Pan, Tony
Kasen, Daniel
Loeb, Abraham
TI Pair-instability supernovae at the epoch of reionization
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: Population II; stars: Population III; supernovae: general; dark
ages; reionization; first stars
ID METAL-POOR STARS; DELAY-TIME DISTRIBUTION; INITIAL MASS FUNCTION; EARLY
RELEASE SCIENCE; POPULATION III STARS; SIMILAR-TO 7; IA SUPERNOVAE;
LIGHT CURVES; 1ST STARS; LOW-METALLICITY
AB Pristine stars with masses between similar to 140 and 260 M? are theoretically predicted to die as pair-instability supernovae. These very massive progenitors could come from Population III (Pop III) stars in the early universe. We model the light curves and spectra of pair-instability supernovae over a range of masses and envelope structures. At redshifts of reionization z= 6, we calculate the rates and detectability of pair-instability and core-collapse supernovae, and show that with the James Webb Space Telescope it is possible to determine the contribution of Pop III and Pop II stars towards reionization by constraining the stellar initial mass function at that epoch using these supernovae. We also find the rates of Type Ia supernovae, and show that they are not rare during reionization, and can be used to probe the mass function at 48 M?. If the budget of ionizing photons was dominated by contributions from top-heavy Pop III stars, we predict that the bright end of the galaxy luminosity function will be contaminated by pair-instability supernovae.
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] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kasen, Daniel] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Nucl Sci, 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 US Department of Energy
[DE-AC02-05CH11231]; DOE SciDAC [DE-FC02-06ER41438]; ORNL through INCITE
FX We thank Bob Kirshner, Kaisey Mandel and Jonathan Pritchard for helpful
discussions. TP was supported by the Hertz Foundation. This work was
supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G
and NNA09DB30A. This work is supported by the Director, Office of Energy
Research, Office of High Energy and Nuclear Physics, Divisions of
Nuclear Physics, of the US Department of Energy under Contract No.
DE-AC02-05CH11231. This research has been supported by the DOE SciDAC
Programme (DE-FC02-06ER41438). We are grateful for computer time
provided by ORNL through an INCITE award and by NERSC.
NR 81
TC 42
Z9 42
U1 0
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY
PY 2012
VL 422
IS 3
BP 2701
EP 2711
DI 10.1111/j.1365-2966.2012.20837.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 939YZ
UT WOS:000303858400072
ER
PT J
AU Maletinsky, P
Hong, S
Grinolds, MS
Hausmann, B
Lukin, MD
Walsworth, RL
Loncar, M
Yacoby, A
AF Maletinsky, P.
Hong, S.
Grinolds, M. S.
Hausmann, B.
Lukin, M. D.
Walsworth, R. L.
Loncar, M.
Yacoby, A.
TI A robust scanning diamond sensor for nanoscale imaging with single
nitrogen-vacancy centres
SO NATURE NANOTECHNOLOGY
LA English
DT Article
ID FIELD OPTICAL MICROSCOPY; MAGNETIC-RESONANCE; COUPLED ELECTRON;
LIGHT-SOURCE; SPIN; RESOLUTION; PHOTON; FABRICATION
AB The nitrogen-vacancy defect centre in diamond(1-4) has potential applications in nanoscale electric and magnetic-field sensing(2-6), single-photon microscopy(7,8), quantum information processing(9) and bioimaging(10). These applications rely on the ability to position a single nitrogen-vacancy centre within a few nanometres of a sample, and then scan it across the sample surface, while preserving the centre's spin coherence and readout fidelity. However, existing scanning techniques, which use a single diamond nanocrystal grafted onto the tip of a scanning probe microscope(2,8,11,12), suffer from short spin coherence times due to poor crystal quality, and from inefficient far-field collection of the fluorescence from the nitrogen-vacancy centre. Here, we demonstrate a robust method for scanning a single nitrogen-vacancy centre within tens of nanometres from a sample surface that addresses both of these concerns. This is achieved by positioning a single nitrogen-vacancy centre at the end of a high-purity diamond nanopillar, which we use as the tip of an atomic force microscope. Our approach ensures long nitrogen-vacancy spin coherence times (similar to 75 mu s), enhanced nitrogen-vacancy collection efficiencies due to waveguiding, and mechanical robustness of the device (several weeks of scanning time). We are able to image magnetic domains with widths of 25 nm, and demonstrate a magnetic field sensitivity of 56 nT Hz(-1/2) at a frequency of 33 kHz, which is unprecedented for scanning nitrogen-vacancy centres.
C1 [Maletinsky, P.; Grinolds, M. S.; Lukin, M. D.; Walsworth, R. L.; Yacoby, A.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Hong, S.; Hausmann, B.; Loncar, M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Yacoby, A (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
EM yacoby@physics.harvard.edu
RI Hong, Sungkun/D-3282-2014; Maletinsky, Patrick/L-1851-2015
OI Hong, Sungkun/0000-0003-0985-6641; Maletinsky,
Patrick/0000-0003-1699-388X
FU Swiss National Science Foundation; Kwanjeong Scholarship Foundation;
Department of Defense (NDSEG); National Science Foundation (NSF) [ECS
0335765]; NIST; DARPA
FX The authors thank B.D. Terris and N. Supper from Hitachi GST for
providing the magnetic recording samples. P.M. acknowledges support from
the Swiss National Science Foundation and S.H. thanks the Kwanjeong
Scholarship Foundation for funding. M.S.G. is supported by fellowships
from the Department of Defense (NDSEG programme) and the National
Science Foundation (NSF). This work was supported by NIST and DARPA
QuEST and QuASAR programmes and in part was performed at the Center for
Nanoscale Systems (CNS), a member of the National Nanotechnology
Infrastructure Network (NNIN), which is supported by the NSF (under
award no. ECS 0335765). CNS is part of Harvard University.
NR 36
TC 190
Z9 191
U1 8
U2 169
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1748-3387
J9 NAT NANOTECHNOL
JI Nat. Nanotechnol.
PD MAY
PY 2012
VL 7
IS 5
BP 320
EP 324
DI 10.1038/NNANO.2012.50
PG 5
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA 940JC
UT WOS:000303884800011
PM 22504708
ER
PT J
AU Fitzgerald, EMG
Carrano, MT
Holland, T
Wagstaff, BE
Pickering, D
Rich, TH
Vickers-Rich, P
AF Fitzgerald, Erich M. G.
Carrano, Matthew T.
Holland, Timothy
Wagstaff, Barbara E.
Pickering, David
Rich, Thomas H.
Vickers-Rich, Patricia
TI First ceratosaurian dinosaur from Australia
SO NATURWISSENSCHAFTEN
LA English
DT Article
DE Dinosauria; Theropoda; Ceratosauria; Abelisauroidea; Gondwana;
Cretaceous
ID SOUTHERN TYRANT REPTILE; ABELISAUROID DINOSAURIA; THEROPOD DINOSAUR;
POLAR DINOSAURS; OSTEOLOGY; EVOLUTION; CHINA; GONDWANA; FAUNAS; ASIA
AB The basal theropod dinosaur clade Ceratosauria, and its subclade Abelisauroidea, is characteristic of late Mesozoic terrestrial vertebrate faunas in western Gondwana (South America, Africa, Madagascar, and India) and Europe. Yet unambiguous records of ceratosaurs have hitherto been absent from Australia, where the theropod assemblage appears to include several typically Laurasian clades. Here, we report the first evidence of ceratosaurs (and potentially abelisauroids) from eastern Gondwana--a diagnostic astragalocalcaneum from the Aptian (121-125 Ma) of Victoria, Australia. Ceratosauria thus occurred in both western and eastern Gondwana during the Early Cretaceous. This fossil adds to the poorly known dinosaur fauna of Australia, a major clade of basal theropods, emphasising that its mid-Cretaceous theropod diversity was surprisingly cosmopolitan despite relative geographic isolation, including clades that have been thought to be typical of both Gondwana and Laurasia--Ceratosauria, Spinosauridae, Carcharodontosauria, Tyrannosauroidea, and Deinonychosauria. Such a contemporaneous association of theropod clades is unknown from other Gondwanan continents and questions the views that the late Mesozoic dinosaur fauna of Australia was dominated by Gondwanan or Laurasian elements, extreme isolation, relictualism, and/or novelty as a 'centre of origin'. The cosmopolitan theropod fauna of Australia probably reflects the global distribution of these clades early in their history, prior to significant continental breakup.
C1 [Fitzgerald, Erich M. G.; Holland, Timothy; Pickering, David; Rich, Thomas H.; Vickers-Rich, Patricia] Museum Victoria, Melbourne, Vic 3001, Australia.
[Fitzgerald, Erich M. G.; Carrano, Matthew T.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Holland, Timothy; Rich, Thomas H.; Vickers-Rich, Patricia] Monash Univ, Sch Geosci, Melbourne, Vic 3800, Australia.
[Wagstaff, Barbara E.] Univ Melbourne, Sch Earth Sci, Melbourne, Vic 3010, Australia.
RP Fitzgerald, EMG (reprint author), Museum Victoria, GPO Box 666, Melbourne, Vic 3001, Australia.
EM efitzgerald@museum.vic.gov.au
RI Carrano, Matthew/C-7601-2011
OI Carrano, Matthew/0000-0003-2129-1612
FU Australian Research Council [LP0989203, LP100100330]; Museum Victoria;
Harold Mitchell Foundation; Smithsonian Institution; Monash University
FX BEW is supported by Australian Research Council Linkage Grant LP0989203.
EMGF thanks Museum Victoria, the Harold Mitchell Foundation, and the
Smithsonian Institution for their support. PVR and THR are supported by
Australian Research Council Linkage Grant LP100100330, Museum Victoria
and Monash University. L. Kool is thanked for performing the initial
preparation of NMV P221202. We thank M. Cleeland for his discovery of
NMV P221202.
NR 58
TC 7
Z9 7
U1 1
U2 15
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0028-1042
EI 1432-1904
J9 NATURWISSENSCHAFTEN
JI Naturwissenschaften
PD MAY
PY 2012
VL 99
IS 5
BP 397
EP 405
DI 10.1007/s00114-012-0915-3
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 944BW
UT WOS:000304174400006
PM 22552426
ER
PT J
AU Griffith, RL
Cooper, MC
Newman, JA
Moustakas, LA
Stern, D
Comerford, JM
Davis, M
Lotz, JM
Barden, M
Conselice, CJ
Capak, PL
Faber, SM
Kirkpatrick, JD
Koekemoer, AM
Koo, DC
Noeske, KG
Scoville, N
Sheth, K
Shopbell, P
Willmer, CNA
Weiner, B
AF Griffith, Roger L.
Cooper, Michael C.
Newman, Jeffrey A.
Moustakas, Leonidas A.
Stern, Daniel
Comerford, Julia M.
Davis, Marc
Lotz, Jennifer M.
Barden, Marco
Conselice, Christopher J.
Capak, Peter L.
Faber, S. M.
Kirkpatrick, J. Davy
Koekemoer, Anton M.
Koo, David C.
Noeske, Kai G.
Scoville, Nick
Sheth, Kartik
Shopbell, Patrick
Willmer, Christopher N. A.
Weiner, Benjamin
TI THE ADVANCED CAMERA FOR SURVEYS GENERAL CATALOG: STRUCTURAL PARAMETERS
FOR APPROXIMATELY HALF A MILLION GALAXIES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; galaxies: evolution; galaxies: photometry; galaxies:
structure; surveys
ID DEEP FIELD-SOUTH; EMISSION-LINE GALAXIES; ACTIVE GALACTIC NUCLEI; LYMAN
BREAK GALAXIES; GOODS-N FIELD; SIMILAR-TO 1; REDSHIFT SURVEY;
PHOTOMETRIC REDSHIFTS; SPECTROSCOPIC SURVEY; OPTICAL SPECTROSCOPY
AB We present the Advanced Camera for Surveys General Catalog (ACS-GC), a photometric and morphological database using publicly available data obtained with the Advanced Camera for Surveys (ACS) instrument on the Hubble Space Telescope. The goal of the ACS-GC database is to provide a large statistical sample of galaxies with reliable structural and distance measurements to probe the evolution of galaxies over a wide range of look-back times. The ACS-GC includes approximately 470,000 astronomical sources (stars + galaxies) derived from the AEGIS, COSMOS, GEMS, and GOODS surveys. Galapagos was used to construct photometric (SEXTRACTOR) and morphological (GALFIT) catalogs. The analysis assumes a single Sersic model for each object to derive quantitative structural parameters. We include publicly available redshifts from the DEEP2, COMBO-17, TKRS, PEARS, ACES, CFHTLS, and zCOSMOS surveys to supply redshifts (spectroscopic and photometric) for a considerable fraction (similar to 74%) of the imaging sample. The ACS-GC includes color postage stamps, GALFIT residual images, and photometry, structural parameters, and redshifts combined into a single catalog.
C1 [Griffith, Roger L.; Kirkpatrick, J. Davy] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Cooper, Michael C.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA.
[Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh Particle Phys Astrophys & Cosmol Ctr, Pittsburgh, PA 15260 USA.
[Moustakas, Leonidas A.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Comerford, Julia M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Davis, Marc] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Lotz, Jennifer M.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Barden, Marco] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
[Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Capak, Peter L.; Scoville, Nick; Sheth, Kartik; Shopbell, Patrick] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Noeske, Kai G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Willmer, Christopher N. A.; Weiner, Benjamin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Griffith, RL (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
RI Conselice, Christopher/B-4348-2013; Moustakas, Leonidas/F-3052-2014;
OI Moustakas, Leonidas/0000-0003-3030-2360; Conselice,
Christopher/0000-0003-1949-7638; Weiner, Benjamin/0000-0001-6065-7483;
Koekemoer, Anton/0000-0002-6610-2048
FU NASA/ESA [GO-10134, GO-09822, GO-09425.01, GO-09583.01, GO-9500]; NASA
[NAS 5-26555]; NSF [AST00-71048]; NASA LTSA [NNG04GC89G]; ESO Paranal
Observatory [LP175.A-0839]
FX This work is based on (GO-10134, GO-09822, GO-09425.01, GO-09583.01,
GO-9500) program observations with the NASA/ESA Hubble Space Telescope,
obtained at the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-26555. Work on this paper is based on observations
obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA,
at the Canada-France-Hawaii Telescope ( CFHT), which is operated by the
National Research Council (NRC) of Canada, the Institut National des
Science de l'Univers of the Centre National de la Recherche Scientifique
(CNRS) of France, and the University of Hawaii. This work is based in
part on data products produced at TERAPIX and the Canadian Astronomy
Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey,
a collaborative project of NRC and CNRS. Funding for the DEEP2 Galaxy
Redshift Survey has been provided in part by NSF grant AST00-71048 and
NASA LTSA grant NNG04GC89G. This work is also based on zCOSMOS
observations carried out using the Very Large Telescope at the ESO
Paranal Observatory under Program ID: LP175.A-0839. 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.
NR 63
TC 15
Z9 15
U1 1
U2 8
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 MAY
PY 2012
VL 200
IS 1
AR 9
DI 10.1088/0067-0049/200/1/9
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940YF
UT WOS:000303928300009
ER
PT J
AU Kochanek, CS
Eisenstein, DJ
Cool, RJ
Caldwell, N
Assef, RJ
Jannuzi, BT
Jones, C
Murray, SS
Forman, WR
Dey, A
Brown, MJI
Eisenhardt, P
Gonzalez, AH
Green, P
Stern, D
AF Kochanek, C. S.
Eisenstein, D. J.
Cool, R. J.
Caldwell, N.
Assef, R. J.
Jannuzi, B. T.
Jones, C.
Murray, S. S.
Forman, W. R.
Dey, A.
Brown, M. J. I.
Eisenhardt, P.
Gonzalez, A. H.
Green, P.
Stern, D.
TI AGES: THE AGN AND GALAXY EVOLUTION SURVEY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmology: observations; galaxies: evolution; galaxies: general;
quasars: general
ID WIDE-FIELD SURVEY; IRAC SHALLOW SURVEY; DIGITAL-SKY-SURVEY; RESOLUTION
SPECTRAL TEMPLATES; QUASAR LUMINOSITY FUNCTION; ACTIVE GALACTIC NUCLEI;
FIBER-FED SPECTROGRAPH; VLT DEEP SURVEY; X-RAY SURVEY; STELLAR MASS
AB The AGN and Galaxy Evolution Survey (AGES) is a redshift survey covering, in its standard fields, 7.7 deg(2) of the Bootes field of the NOAO Deep Wide-Field Survey. The final sample consists of 23,745 redshifts. There are well-defined galaxy samples in 10 bands (the B-W, R, I, J, K, IRAC3.6, 4.5, 5.8, and 8.0 mu m, and MIPS 24 mu m bands) to a limiting magnitude of I < 20 mag for spectroscopy. For these galaxies, we obtained 18,163 redshifts from a sample of 35,200 galaxies, where random sparse sampling was used to define statistically complete sub-samples in all 10 photometric bands. The median galaxy redshift is 0.31, and 90% of the redshifts are in the range 0.085 < z < 0.66. Active galactic nuclei (AGNs) were selected as radio, X-ray, IRAC mid-IR, and MIPS 24 mu m sources to fainter limiting magnitudes (I < 22.5 mag for point sources). Redshifts were obtained for 4764 quasars and galaxies with AGN signatures, with 2926, 1718, 605, 119, and 13 above redshifts of 0.5, 1, 2, 3, and 4, respectively. We detail all the AGES selection procedures and present the complete spectroscopic redshift catalogs and spectral energy distribution decompositions. Photometric redshift estimates are provided for all sources in the AGES samples.
C1 [Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Eisenstein, D. J.; Caldwell, N.; Jones, C.; Murray, S. S.; Forman, W. R.; Green, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cool, R. J.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Cool, R. J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Assef, R. J.; Eisenhardt, P.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jannuzi, B. T.; Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA.
RP Kochanek, CS (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
RI Brown, Michael/B-1181-2015
OI Brown, Michael/0000-0002-1207-9137
FU NASA at Jet Propulsion Laboratory; NSF; NOAO; Smithsonian Institution;
NASA [NAS8-38248, NAS8-01130, NAS8- 39073, NAS8-03060, GO3-4176A]
FX We thank the Hectospec instrument team and all the MMT Hectospec queue
observers for making this project possible. We also thank T. Soifer, D.
Weedman, J. Houck, M. Rieke, and collaborators for permission to use the
results of their GTO Spitzer/MIPS survey of the Bootes field. R.J.A. is
supported by an appointment to the NASA Postdoctoral Program at the Jet
Propulsion Laboratory, administered by Oak Ridge Associated Universities
through a contract with NASA. B.T.J. and A.D. are supported by the NSF
through its funding of NOAO, which is operated for the NSF by AURA under
a cooperative agreement. C.J., S.S.M., and W.R.F. acknowledge support
from the Smithsonian Institution and by NASA contracts NAS8-38248,
NAS8-01130, NAS8- 39073, and NAS8-03060, and NASA grant GO3-4176A.
Observations reported here were obtained at the MMT Observatory, a joint
facility of the Smithsonian Institution and the University of Arizona.
This work made use of images and/or data products provided by the NOAO
Deep Wide-Field Survey, which is supported by the National Optical
Astronomy Observatory (NOAO). NOAO is operated by AURA, Inc., under a
cooperative agreement with the National Science Foundation. 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.
NR 74
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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 MAY
PY 2012
VL 200
IS 1
AR 8
DI 10.1088/0067-0049/200/1/8
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940YF
UT WOS:000303928300008
ER
PT J
AU Spezzano, S
Tamassia, F
Thorwirth, S
Thaddeus, P
Gottlieb, CA
McCarthy, MC
AF Spezzano, S.
Tamassia, F.
Thorwirth, S.
Thaddeus, P.
Gottlieb, C. A.
McCarthy, M. C.
TI A HIGH-RESOLUTION ISOTOPIC STUDY OF THE ROTATIONAL SPECTRUM OF c-C3H2
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE ISM: molecules; line: identification; molecular data; molecular
processes; radio lines: ISM
ID RING MOLECULE C3H2; ASTRONOMICAL SPECTROSCOPY; DEUTERIUM FRACTIONATION;
HYPERFINE-STRUCTURE; COLOGNE DATABASE; 2ND DERIVATIVES; DIFFUSE CLOUDS;
DARK CLOUDS; BASIS-SETS; MANY-BODY
AB The rotational spectra of the normal and seven isotopic species of cyclopropenylidene c-C3H2 have been measured at high spectral resolution by Fourier transform microwave spectroscopy of a supersonic molecular beam between 10 and 43 GHz. Deuterium quadrupole coupling and carbon-13 spin-rotation hyperfine constants were determined in addition to the rotational constants. Quartic and sextic centrifugal distortion constants derived from 28 lines between 150 and 316 GHz of the doubly deuterated species c-C3D2 allow the rotational spectrum to be calculated to 0.5 km s(-1) or better in equivalent radial velocity up to 500 GHz. Spectroscopic constants determined from four centimeter-wave and 19 millimeter-wave lines of the normal species c-C3H2, including 15 with sharp Lambdips, allow prediction of the most important astronomical transitions (i.e., those with Delta J = 1 and K-a <= 3) to 0.05 km s(-1) or better at 500 GHz. The doubly deuterated species is a good candidate for detection in cold dark clouds, because deuterium fractionation is high in c-C3H2 and lines of C3HD are fairly intense in these sources. An accurate empirical equilibrium structure of c-C3H2, derived from the experimental rotational constants of normal and isotopic c-C3H2, corrected for zero-point vibrational effects, is compared with previously reported structures.
C1 [Spezzano, S.; Thaddeus, P.; Gottlieb, C. A.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Spezzano, S.; Thaddeus, P.; Gottlieb, C. A.; McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Spezzano, S.; Tamassia, F.] Univ Bologna, Dipartimento Chim Fis & Inorgan, I-40136 Bologna, Italy.
[Spezzano, S.; Thorwirth, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
RP Spezzano, S (reprint author), Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
EM pthaddeus@cfa.harvard.edu; cgottlieb@cfa.harvard.edu;
mccarthy@cfa.harvard.edu
RI Thorwirth, Sven/C-6217-2011;
OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy,
Michael/0000-0001-9142-0008
FU NASA [NNX08AE05G, NNX08AI41G]; Alma Mater Studiorum-University of
Bologna; Deutsche Forschungsgemeinschaft (DFG) [TH 1301/3-1]
FX We wish to thank Y. Shirley for suggesting we undertake the laboratory
measurements of c-C3D2. The work in Cambridge is
supported by NASA grants NNX08AE05G and NNX08AI41G. S. Spezzano thanks
Alma Mater Studiorum-University of Bologna for the 'Fondazione
Toso-Montanari' fellowship. S.T. is grateful to the Deutsche
Forschungsgemeinschaft (DFG) for research Grant No. TH 1301/3-1.
NR 53
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U1 3
U2 14
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 MAY
PY 2012
VL 200
IS 1
AR 1
DI 10.1088/0067-0049/200/1/1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 940YF
UT WOS:000303928300001
ER
PT J
AU Neale, PJ
Sobrino, C
Gargett, AE
AF Neale, Patrick J.
Sobrino, Cristina
Gargett, Ann E.
TI Vertical mixing and the effects of solar radiation on photosystem II
electron transport by phytoplankton in the Ross Sea Polynya
SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS
LA English
DT Article
DE Photosynthesis; Phytoplankton; Turbulence; Mixing processes; Southern
Ocean; Acoustic backscatter; Fast repetition rate fluorometry
ID FRAGILARIOPSIS-CYLINDRUS BACILLARIOPHYCEAE; REPETITION RATE FLUOROMETRY;
SOUTHERN-OCEAN; PHAEOCYSTIS-ANTARCTICA; LANGMUIR CIRCULATION; PRIMARY
PRODUCTIVITY; PHOTOSYNTHESIS; RATES; WATER; FLUORESCENCE
AB Detailed studies were made in the springtime Ross Sea Polynya of the interaction between near-surface mixing processes, inferred from Thorpe scales and acoustic backscatter, and the quantum efficiency and rate of PSII electron transport of phytoplankton photosynthesis measured at fine depth and time scales by active fluorometry. The phytoplankton assemblage was dominated by Phaeocystis antarctica. Surface conditions alternated between windy episodes producing Langmuir circulation (LC) or calm periods favoring internal waves, in both cases there was significant vertical transport of phytoplankton. During LC episodes, strong near-surface ( < 10 m) vertical gradients in quantum efficiency and inhibition of electron transport were observed despite evidence of vigorous vertical exchange. Under sunny mid-day conditions, profiles of PSII electron transport had sub-surface peaks and electron transport at PAR irradiances > 40 mu mol photons m(-2) s(-1) was generally lower compared to early morning profiles on the same day. In time-series deployments, intrinsic quantum efficiency (F-v'/F-m') was relatively constant under calm conditions at 12 m, but highly variable at 6 m under LC conditions. Simultaneously measured time-series of acoustic backscatter and F-v'/F-m' during LC conditions were negatively correlated, i.e. high backscatter arising from the downward advection of surface originating micro-bubbles coincided with low intrinsic efficiency. Transport also occurred in connection with finer-scale features, possibly arising from breaking surface waves. These results show that LC in the Ross Sea Polynya, in combination with changes in quenching driven by near surface UVR and PAR exposure, reduce photosynthetic electron transport over much of the upper mixed layer. Further observations and modeling will be needed to establish the extent to which this decreases water column productivity. Published by Elsevier Ltd.
C1 [Neale, Patrick J.; Sobrino, Cristina] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Gargett, Ann E.] Old Dominion Univ, Ctr Coastal Phys Oceanog, Norfolk, VA 23508 USA.
RP Neale, PJ (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM nealep@si.edu
RI Sobrino, Cristina/J-3534-2012;
OI Sobrino, Cristina/0000-0003-0431-1220
FU National Science Foundation [OPP-0127037, OPP-0127022, OPP-0125818];
Scientific Committee for Antarctic Research; Spanish Ministry of
Education and Science; RVIB Nathaniel B. Palmer
FX The National Science Foundation is acknowledged for support to the
MIXURS project (OPP-0127037 to P.J. Neale, OPP-0127022 to W. Jeffrey and
OPP-0125818 to A.E. Gargett). C. Sobrino was supported by an Asturias
Fellowship from the Scientific Committee for Antarctic Research and by
the Spanish Ministry of Education and Science. The authors gratefully
acknowledge the support of the officers and crew of the RVIB Nathaniel
B. Palmer, the technical support staff from Raytheon Polar Services, and
scientists aboard the October-December, 2005, Ross Sea cruise (NBP0508).
Teresa Garner is thanked for programming support. John Marra and the
Lamont-Doherty Earth Observatory are gratefully acknowledged for the
loan of a FASTracka I instrument.
NR 50
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U1 1
U2 27
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0637
J9 DEEP-SEA RES PT I
JI Deep-Sea Res. Part I-Oceanogr. Res. Pap.
PD MAY
PY 2012
VL 63
BP 118
EP 132
DI 10.1016/j.dsr.2012.01.011
PG 15
WC Oceanography
SC Oceanography
GA 936VV
UT WOS:000303619000009
ER
PT J
AU Gammill, WM
Fites, JS
Rollins-Smith, LA
AF Gammill, Whitney M.
Fites, J. Scott
Rollins-Smith, Louise A.
TI Norepinephrine depletion of antimicrobial peptides from the skin glands
of Xenopus laevis
SO DEVELOPMENTAL AND COMPARATIVE IMMUNOLOGY
LA English
DT Article
DE Antimicrobial peptide; Batrachochytrium dendrobatidis; Chytridiomycosis;
Granular gland; Mucus gland; Norepinephrine
ID EMERGING INFECTIOUS-DISEASE; GLOBAL AMPHIBIAN DECLINES;
BATRACHOCHYTRIUM-DENDROBATIDIS; POPULATION DECLINES; AMERICAN BULLFROG;
RANA-PIPIENS; IMMUNE DEFENSES; CHYTRID FUNGUS; TREE FROGS;
CHYTRIDIOMYCOSIS
AB The dermal granular glands of the South African clawed frog, Xenopus laevis, contain antimicrobial peptides (AMPs) that are secreted following local nerve stimulation. These natural antibiotics are active against bacteria and fungi including Batrachochytrium dendrobatidis, a fungal pathogen that causes the skin disease chytridiomycosis. Granular gland secretion can be stimulated in the laboratory by norepinephrine injection. We found that two injections of 80 nmol/g norepinephrine were necessary to fully deplete the AMP stores. One injection resulted in the secretion of most of the stored peptides. A second injection, 2 days later, released a small amount of additional AMPs that are not compositionally different from those released by the first injection. A third injection, 4 days after the first, did not result in further AMP release. Mass spectrometry and histology confirmed that glands are depleted after two injections. Periodic acid-Schiff staining indicated that mucus gland secretion was also induced by norepinephrine. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Gammill, Whitney M.; Rollins-Smith, Louise A.] Vanderbilt Univ, Med Ctr, Dept Pathol Microbiol & Immunol, Nashville, TN 37232 USA.
[Fites, J. Scott; Rollins-Smith, Louise A.] Vanderbilt Univ, Dept Biol Sci, Nashville, TN 37235 USA.
[Rollins-Smith, Louise A.] Vanderbilt Univ, Med Ctr, Dept Pediat, Nashville, TN 37232 USA.
[Rollins-Smith, Louise A.] Smithsonian Inst, Natl Zool Pk, Ctr Species Survival Conservat & Sci, Washington, DC 20013 USA.
RP Rollins-Smith, LA (reprint author), Vanderbilt Univ, Med Ctr, Dept Pathol Microbiol & Immunol, A-5301 Med Ctr N, Nashville, TN 37232 USA.
EM louise.rollins-smith@vanderbilt.edu
FU National Science Foundation [IOS-0619536, IOS-0843207]
FX This work was supported by the National Science Foundation Grants
IOS-0619536 and IOS-0843207 (to L.R.-S.) and a National Science
Foundation Graduate Research Fellowship (to W.M.G.). The authors thank
James D. Pask (Department of Pathology, Microbiology and Immunology,
Vanderbilt University, Nashville, TN) and the Vanderbilt Mass
Spectrometry Core for assistance with MALDI-TOF Mass Spectrometry. The
authors also thank Dr. Laetitia Tatiersky (Department of Pathobiology,
University of Guelph, Ontario, Canada) for her advice in histology
staining methods, the Vanderbilt Immunohistochemistry Core for
assistance with skin tissue histology, and the laboratory of Dr. Eric
Skaar at Vanderbilt University for the use of their Olympus microscope,
camera, and software for histology photography.
NR 83
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U1 2
U2 21
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0145-305X
J9 DEV COMP IMMUNOL
JI Dev. Comp. Immunol.
PD MAY
PY 2012
VL 37
IS 1
BP 19
EP 27
DI 10.1016/j.dci.2011.12.012
PG 9
WC Immunology; Zoology
SC Immunology; Zoology
GA 942EG
UT WOS:000304024700003
PM 22227319
ER
PT J
AU Kelley, KA
Cottrell, E
AF Kelley, Katherine A.
Cottrell, Elizabeth
TI The influence of magmatic differentiation on the oxidation state of Fe
in a basaltic arc magma
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE oxygen fugacity; XANES; melt Inclusions; subduction; volatiles;
degassing
ID OVERLYING SUBDUCTION ZONES; MELT INCLUSIONS; OXYGEN FUGACITY; REDOX
STATES; MARIANA ARC; UPPER-MANTLE; ISLAND ARCS; WAVELENGTH SHIFTS; GLASS
INCLUSIONS; WESTERN PACIFIC
AB Subduction zone basalts are more oxidized than basalts from other tectonic settings (e.g., higher Fe3+/Sigma Fe), and this contrast may play a central role in the unique geochemical processes that generate arc and continental crust. The processes generating oxidized arc magmas, however, are poorly constrained, although they appear inherently linked to subduction. Near-surface differentiation processes unique to arc settings might drive oxidation of magmas that originate in equilibrium with a relatively reduced mantle source. Alternatively, arc magmas could record the oxidation conditions of a relatively oxidized mantle source. Here, we present new measurements of olivine-hosted melt inclusions from a single eruption of Agrigan volcano, Marianas, in order to test the influence of differentiation processes vs. source conditions on the Fe3+/Sigma Fe ratio, a proxy for system oxygen fugacity (fO(2)). We determined Fe3+/Sigma Fe rations in glass inclusions using mu-XANES and couple these data with major elements, dissolved volatiles, and trace elements. After correcting for post-entrapment crystallization, Fe3+/Sigma Fe ratios in the Agrigan melt inclusions (0.219 to 0.282), and their modeled fO(2)s (Delta QFM +1.0 to +1.8), are uniformly more oxidized than MORB, and preserve a portion of the evolution of this magma from 5.7 to 3.2 wt.% MgO. Fractionation of olivine +/- clinopyroxene +/- plagioclase should increase Fe3+/Sigma Fe MgO. decreases in the melt, but the data show Fe3+/Sigma Fe ratios decreasing as MgO decreases below 5 wt.% MgO. The major element trajectories, taken in combination with this strong reduction trend, are inconsistent with crystallization of common ferromagnesian phases found in the bulk Agrigan sample, including magnetite. Rather, decreasing Fe3+/Sigma Fe rations correlate with decreading S concentrations, suggesting that electronic exchange associated with SO2 degassing may dominbate Fe3+/Sigma Fe variations in the melt during differentiation. In the case of this magma, the dominant effect of differentiation on magmatic fO(2) reduction rather than oxidation. Tracing back Agrigan melts with MgO > 5 wt.% (i.e., minimally degassed for S) along a modeled olivine factionation trend to primary melt in equilibrium with Fo(90) olivine reveals melts in equilibrium with the mantle beneath Agrigan at fO(2)s Delta QFM +1 to +1.6, significantly more oxidized than current constraints for the mantle beneath mid-ocean ridges. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Kelley, Katherine A.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA.
[Cottrell, Elizabeth] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
RP Kelley, KA (reprint author), Univ Rhode Isl, Grad Sch Oceanog, Narragansett Bay Campus, Narragansett, RI 02882 USA.
EM kelley@gso.uri.edu; cottrelle@si.edu
RI Kelley, Katherine/J-3728-2013
OI Kelley, Katherine/0000-0002-7516-2683
FU NSF [OCE-0644625, EAR-0838328, MARGINS-EAR-0841108,
MARGINS-EAR-0841006]; U.S. Department of Energy, Office of Science,
Office of Basic Energy Sciences [DE-AC02-98CH10886]; EC; URI
FX We are grateful for thorough reviews from Cin-Ty Lee, Chris Ballhaus,
and Leonid Danyushevsky. We acknowledge constructive discussions with
and inspiration from Cin-Ty Lee, Marc Hirschmann, Mac Rutherford, and
Becky Lange. Terry Plank generously shared the source sample material
and unpublished data to assist with this study, in addition to valuable
thoughts and data on V partitioning. This work was made possible by the
contributions of Benjamin Parks, who generated a pilot data set for this
study through the GSO SURFO program, and Maryjo Brounce and Christa
Jackson, who assisted in all aspects of data collection. Tony Lanzirotti
contributed invaluable expertise in mu-XANES analysis and beamline
operations at X26A. NSF Award OCE-0644625 provided curatorial support
for marine geological samples at the University of Rhode Island. Use of
the National Synchrotron Light Source, Brookhaven National Laboratory,
was supported by the U.S. Department of Energy, Office of Science,
Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886.
We acknowledge support from Smithsonian's Scholarly Studies Program
(EC), a URI ADVANCE fellowship (KK) and NSF awards EAR-0838328 (KK),
MARGINS-EAR-0841108 (KK) and MARGINS-EAR-0841006 (EC).
NR 81
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Z9 63
U1 3
U2 66
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD MAY 1
PY 2012
VL 329
BP 109
EP 121
DI 10.1016/j.epsl.2012.02.010
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 936ZW
UT WOS:000303629800011
ER
PT J
AU Crouse, DL
Peters, PA
van Donkelaar, A
Goldberg, MS
Villeneuve, PJ
Brion, O
Khan, S
Atari, DO
Jerrett, M
Pope, CA
Brauer, M
Brook, JR
Martin, RV
Stieb, D
Burnett, RT
AF Crouse, Dan L.
Peters, Paul A.
van Donkelaar, Aaron
Goldberg, Mark S.
Villeneuve, Paul J.
Brion, Orly
Khan, Saeeda
Atari, Dominic Odwa
Jerrett, Michael
Pope, C. Arden, III
Brauer, Michael
Brook, Jeffrey R.
Martin, Randall V.
Stieb, David
Burnett, Richard T.
TI Risk of Non accidental and Cardiovascular Mortality in Relation to
Long-term Exposure to Low Concentrations of Fine Particulate Matter: A
Canadian National-Level Cohort Study
SO ENVIRONMENTAL HEALTH PERSPECTIVES
LA English
DT Article
DE Canada; cardiovascular mortality; cohort study; fine particulate matter
ID AIR-POLLUTION; DISEASE; HEALTH; ASSOCIATION; CITIES
AB BACKGROUND: Few cohort studies have evaluated the risk of mortality associated with long-term exposure to fine particulate matter [<= 2.5 mu m in aerodynamic diameter (PM2.5)]. This is the first national-level cohort study to investigate these risks in Canada.
OBJECTIVE: We investigated the association between long-term exposure to ambient PM2.5 and cardio vascular mortality in non immigrant Canadian adults.
METHODS: We assigned estimates of exposure to ambient PM2.5 derived from satellite observations to a cohort of 2.1 million Canadian adults who in 1991 were among the 20% of the population mandated to provide detailed census data. We identified deaths occurring between 1991 and 2001 through record linkage. We calculated hazard ratios (HRs) and 95% confidence intervals (CIs) adjusted for available individual-level and contextual covariates using both standard Cox proportional survival models and nested, spatial random-effects survival models.
RESULTS: Using standard Cox models, we calculated HRs of 1.15 (95% CI: 1.13, 1.16) from non-accidental causes and 1.31 (95% CI: 1.27, 1.35) from ischemic heart disease for each 10-mu g/m(3) increase in concentrations of PM2.5. Using spatial random-effects models controlling for the same variables, we calculated HRs of 1.10 (95% CI: 1.05, 1.15) and 1.30 (95% CI: 1.18, 1.43), respectively. We found similar associations between non accidental mortality and PM2.5 based on satellite-derived estimates and ground-based measurements in a subanalysis of subjects in 11 cities.
CONCLUSIONS: In this large national cohort of non immigrant Canadians, mortality was associated with long-term exposure to PM2.5. Associations were observed with exposures to PM2.5 at concentrations that were predominantly lower (mean, 8.7 mu g/m(3); interquartile range, 6.2 mu g/m(3)) than those reported previously.
C1 [Crouse, Dan L.] Hlth Canada, Ctr Environm Hlth, Environm Hlth Sci & Res Bur, Ottawa, ON K1A 0K9, Canada.
[Peters, Paul A.; Khan, Saeeda; Atari, Dominic Odwa] STAT Canada, Hlth Anal Div, Ottawa, ON, Canada.
[van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Goldberg, Mark S.] McGill Univ, Dept Med, Montreal, PQ, Canada.
[Villeneuve, Paul J.; Brook, Jeffrey R.] Univ Toronto, Dalla Lana Sch Publ Hlth, Toronto, ON, Canada.
[Jerrett, Michael] Univ Calif Berkeley, Sch Publ Hlth, Berkeley, CA 94720 USA.
[Pope, C. Arden, III] Brigham Young Univ, Dept Econ, Provo, UT 84602 USA.
[Brauer, Michael] Univ British Columbia, Sch Populat & Publ Hlth, Vancouver, BC V5Z 1M9, Canada.
[Brook, Jeffrey R.] Environm Canada, Air Qual Res Div, Downsview, ON, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Crouse, DL (reprint author), Hlth Canada, Ctr Environm Hlth, Environm Hlth Sci & Res Bur, Room 155,50 Columbine Dr, Ottawa, ON K1A 0K9, Canada.
EM daniel.crouse@hc-sc.gc.ca
RI Martin, Randall/C-1205-2014;
OI Martin, Randall/0000-0003-2632-8402; Peters, Paul/0000-0001-5225-2005;
Brauer, Michael/0000-0002-9103-9343
FU Canadian government laboratory from the Natural Sciences and Engineering
Research Council of Canada
FX We thank S. Judek of Health Canada for compiling the ground-based data
for fine particulate matter. D. L. C. gratefully acknowledges receipt of
a visiting fellowship in a Canadian government laboratory from the
Natural Sciences and Engineering Research Council of Canada.
NR 31
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U1 7
U2 63
PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE
PI RES TRIANGLE PK
PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233,
RES TRIANGLE PK, NC 27709-2233 USA
SN 0091-6765
J9 ENVIRON HEALTH PERSP
JI Environ. Health Perspect.
PD MAY
PY 2012
VL 120
IS 5
BP 708
EP 714
DI 10.1289/ehp.1104049
PG 7
WC Environmental Sciences; Public, Environmental & Occupational Health;
Toxicology
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Toxicology
GA 935UF
UT WOS:000303546000035
PM 22313724
ER
PT J
AU Andrews, BJ
Manga, M
AF Andrews, Benjamin J.
Manga, Michael
TI Experimental study of turbulence, sedimentation, and coignimbrite mass
partitioning in dilute pyroclastic density currents
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE Pyroclastic density current; Experiments; Turbulence; Pyroclastic
deposits
ID MOUNT ST-HELENS; DEPOSITIONAL PROCESSES; LASCAR VOLCANO; CANARY-ISLANDS;
SURGE DEPOSITS; IGNIMBRITE; FLOWS; DYNAMICS; TRANSPORT; ERUPTION
AB Laboratory density currents comprising warm talc powder turbulently suspended in air simulate many aspects of dilute pyroclastic density currents (PDCs) and demonstrate links between bulk current behavior, sedimentation, and turbulent structures. The densimetric and thermal Richardson, Froude, Stokes, and settling numbers match those of natural PDCs as does the ratio of thermal to kinetic energy density. The experimental currents have lower bulk Reynolds numbers than natural PDCs, but the experiments are fully turbulent. Consequently, the experiments are dynamically similar to the dilute portions of some natural currents. In general, currents traverse the floor of the experimental tank, sedimenting particles and turbulently entraining, heating, and thermally expanding air until all particle sediments or the currents become buoyant and lift off to form coignimbrite plumes. When plumes form, currents often undergo local flow reversals. Current runout distance and liftoff position decrease with increasing densimetric Richardson number and thermal energy density. As those parameters increase, total sedimentation decreases such that >50% of initial current mass commonly fractionates into the plumes, in agreement with some observations of recent volcanic eruptions. Sedimentation profiles are best described by an entraining sedimentation model rather than the exponential fit resulting from non-entraining box models. Time series analysis shows that sedimentation is not a constant rate process in the experiments, but rather occurs as series of sedimentation-erosion couplets that propagate across the tank floor tracking current motion and behavior. During buoyant liftoff, sedimentation beneath the rising plumes often becomes less organized. Auto-correlation analysis of time series of particle concentration is used to characterize the turbulent structures of the currents and indicates that currents quickly partition into a slow-moving upper portion and faster, more concentrated, lower portion. Air entrainment occurs within the upper region. Turbulent structures within the lower region track sedimentation-erosion waves and indicate that eddies control deposition. Importantly, both eddies and sedimentation waves track reversals in flow direction that occur following buoyant liftoff. Further, these results suggest that individual laminations within PDC deposits may record passage of single eddies, thus the duration of individual PDCs may be estimated as the product of the number of laminations and the current's turbulent timescale. Published by Elsevier B.V.
C1 [Andrews, Benjamin J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Manga, Michael] UC Berkeley, Dept Earth & Planetary Sci, Berkeley, CA USA.
RP Andrews, BJ (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM andrewsb@si.edu
RI Manga, Michael/D-3847-2013;
OI Manga, Michael/0000-0003-3286-4682
FU NSF [EAR-0847366, EAR-080954]
FX BJA was supported by the NSF Earth Sciences Postdoctoral Fellowship
program under grant EAR-0847366. MM was supported by NSF grant
EAR-080954. The experimental facility was constructed at UC Richmond
Field Station with the assistance of Stuart Foster in a space provided
by Leonard Sklar and Bill Dietrich. William Gange assisted with running
many experiments. James E. Gardner graciously provided grain size
analyses of the talc powder. Thoughtful reviews by G. Lube and P.
Dellino improved this paper.
NR 46
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U1 2
U2 21
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD MAY 1
PY 2012
VL 225
BP 30
EP 44
DI 10.1016/j.jvolgeores.2012.02.011
PG 15
WC Geosciences, Multidisciplinary
SC Geology
GA 941DK
UT WOS:000303943700003
ER
PT J
AU Coyne, P
Pisha, B
Dalton, B
Zeph, LA
Smith, NC
AF Coyne, Peggy
Pisha, Bart
Dalton, Bridget
Zeph, Lucille A.
Smith, Nancy Cook
TI Literacy by Design: A Universal Design for Learning Approach for
Students With Significant Intellectual Disabilities
SO REMEDIAL AND SPECIAL EDUCATION
LA English
DT Article
DE literacy; mental retardation; universal design for learning; technology
ID INSTRUCTION; PROGRAM
AB Literacy instruction for students with significant intellectual disabilities traditionally emphasizes isolated skills instruction focusing on sight words and basic vocabulary. Recent research suggests these students benefit from high-quality instruction that includes comprehension and storybook reading. This study examined the effect of a technology-based universal design for learning (UDL) approach to literacy instruction, Literacy by Design (LBD), on the reading achievement of 16 students with significant intellectual disabilities in Grades K-2. The LBD approach emphasizes reading for meaning, combining UDL-scaffolded e-books and letter and word recognition software. Nine teachers received training in research-based literacy practices. Of these, five received LBD training and implemented it four to five times weekly. Controlling for initial reading achievement, the LBD group made significantly greater gains on the Woodcock-Johnson Test of Achievement III Passage Comprehension subtest. Implications for research and practice in beginning reading instruction for children with significant intellectual disabilities are discussed.
C1 [Coyne, Peggy; Pisha, Bart] CAST, Wakefield, MA 01881 USA.
[Dalton, Bridget] Vanderbilt Univ, Peabody Coll Educ, Nashville, TN USA.
[Zeph, Lucille A.] Univ Maine, Orono, ME USA.
[Smith, Nancy Cook] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA.
RP Coyne, P (reprint author), CAST, 40 Harvard Mills Sq,Suite 3, Wakefield, MA 01881 USA.
EM pcoyne@cast.org
NR 47
TC 15
Z9 15
U1 5
U2 31
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 0741-9325
J9 REM SPEC EDUC
JI Remedial Spec. Educ.
PD MAY-JUN
PY 2012
VL 33
IS 3
BP 162
EP 172
DI 10.1177/0741932510381651
PG 11
WC Education, Special
SC Education & Educational Research
GA 939MA
UT WOS:000303814000003
ER
PT J
AU Gould, RR
Sunbury, S
Krumhansl, R
AF Gould, Roy R.
Sunbury, Susan
Krumhansl, Ruth
TI Using online telescopes to explore exoplanets from the physics classroom
SO AMERICAN JOURNAL OF PHYSICS
LA English
DT Article
ID PLANETS
AB The search for habitable planets offers excellent opportunities to advance students' understanding of core ideas in physics, including gravity and the laws of motion, the interaction of light and matter, and especially the nature of scientific inquiry. Thanks to the development of online telescopes, students can detect more than a dozen of the known exoplanets from the classroom, using data they gather, assess, and interpret for themselves. We present a suite of activities in which students apply basic physics concepts to their investigations of exoplanets. The activities were developed and successfully tested with physics and earth science teachers in secondary schools in 14 states. Included are additional challenges and assessments suitable for introductory college physics courses. (C) 2012 American Association of Physics Teachers. [DOI:10.1119/1.3671072]
C1 [Gould, Roy R.; Sunbury, Susan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Krumhansl, Ruth] Educ Dev Ctr Inc, Newton, MA 02458 USA.
RP Gould, RR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rgould@cfa.harvard.edu
FU National Science Foundation [0733252]
FX The authors thank the reviewers for their helpful suggestions. The
authors are grateful to David Charbonneau, Lisa Kaltenegger, Matt
Holman, and Phil Sadler for their advice during this project, and to our
project collaborators Mary Dussault, Frank Sienkiewicz, Freeman Deutsch
and Aladdin Ibrahim; and to the teachers who helped to develop and test
these materials. This paper is based on work supported by the National
Science Foundation under grant No. 0733252. Any opinions, findings, and
conclusions or recommendations expressed in this material are those of
the authors and do not necessarily reflect the views of the National
Science Foundation.
NR 14
TC 2
Z9 2
U1 0
U2 2
PU AMER ASSOC PHYSICS TEACHERS AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0002-9505
J9 AM J PHYS
JI Am. J. Phys.
PD MAY
PY 2012
VL 80
IS 5
BP 445
EP 451
DI 10.1119/1.3671072
PG 7
WC Education, Scientific Disciplines; Physics, Multidisciplinary
SC Education & Educational Research; Physics
GA 927YY
UT WOS:000302947800014
ER
PT J
AU Hamdan, R
El-Rifai, HM
Cheesman, AW
Turner, BL
Reddy, KR
Cooper, WT
AF Hamdan, Rasha
El-Rifai, Hasan M.
Cheesman, Alexander W.
Turner, Benjamin L.
Reddy, K. Ramesh
Cooper, William T.
TI Linking Phosphorus Sequestration to Carbon Humification in Wetland Soils
by P-31 and C-13 NMR Spectroscopy
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID MAGNETIC-RESONANCE-SPECTROSCOPY; NATURAL ORGANIC MATERIALS;
HYDROFLUORIC-ACID; FOREST SOILS; CPMAS NMR; MATTER; DECOMPOSITION;
SPECTRA; EXTRACTION; FRACTIONS
AB Phosphorus sequestration in wetland soils is a prerequisite for long-term maintenance of water quality in downstream aquatic systems, but can be compromised if phosphorus is released following changes in nutrient status or hydrological regimen. The association of phosphorus with relatively refractory natural organic matter (e.g., humic substances) might protect soil phosphorus from such changes. Here we used hydrofluoric acid (HF) pretreatment to remove phosphorus associated with metals or anionic sorption sites, allowing us to isolate a pool of phosphorus associated with the soil organic fraction. Solution P-31 and solid state C-13 NMR spectra for wetland soils were acquired before and after hydrofluoric acid pretreatment to assess quantitatively and qualitatively the changes in phosphorus and carbon functional groups. Organic phosphorus was largely unaffected by HF treatment in soils dominated by refractory alkyl and aromatic carbon groups, indicating association of organic phosphorus with stable, humified soil organic matter. Conversely, a considerable decrease in organic phosphorus following HF pretreatment was detected in soils where O-alkyl groups represented the major fraction of the soil carbon. These correlations suggest that HF treatment can be used as a method to distinguish phosphorus fractions that are bound to the inorganic soil components from those fractions that are stabilized by incorporation into soil organic matter.
C1 [Hamdan, Rasha; El-Rifai, Hasan M.; Cooper, William T.] Florida State Univ, Dept Chem & Biochem, Tallahassee, FL 32306 USA.
[Cheesman, Alexander W.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Reddy, K. Ramesh] Univ Florida, Dept Soil & Water Sci, Gainesville, FL 32611 USA.
RP Cooper, WT (reprint author), Florida State Univ, Dept Chem & Biochem, Tallahassee, FL 32306 USA.
EM cooper@chem.fsu.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 U.S. Department of Agriculture [CSREES 2004-35107-14918]
FX This work was supported by a grant from the U.S. Department of
Agriculture (CSREES 2004-35107-14918). 31P and 13C
NMR spectra were acquired in the Florida State University Department of
Chemistry and Biochemistry NMR facility. The assistance of Dr. Tom
Gedris, Staff Supervisor, is greatly appreciated.
NR 48
TC 20
Z9 21
U1 1
U2 86
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD MAY 1
PY 2012
VL 46
IS 9
BP 4775
EP 4782
DI 10.1021/es204072k
PG 8
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 933GO
UT WOS:000303348800018
PM 22423890
ER
PT J
AU Turner, BL
Cheesman, AW
Godage, HY
Riley, AM
Potter, BVL
AF Turner, Benjamin L.
Cheesman, Alexander W.
Godage, H. Yasmin
Riley, Andrew M.
Potter, Barry V. L.
TI Determination of neo- and D-chiro-Inositol Hexakisphosphate in Soils by
Solution P-31 NMR Spectroscopy
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID NUCLEAR-MAGNETIC-RESONANCE; ORGANIC PHOSPHORUS; SCYLLO-INOSITOL;
ALKALINE EXTRACTS; HEXAPHOSPHATE; PHOSPHATES; IDENTIFICATION; SEDIMENTS;
FORMS; EDTA
AB The inositol phosphates are an abundant but poorly understood group of organic phosphorus compounds found widely in the environment. Four stereoisomers of inositol hexakisphosphate (IP6) occur, although for three of these (scyllo, flea, and D-chiro) the origins, dynamics, and biological function remain unknown, due in large part to analytical limitations in their measurement in environmental samples. We synthesized authentic neo- and n-chiro-IP6 and used them to identify signals from these compounds in three soils from the Falkland Islands. Both compounds resisted hypobromite oxidation and gave quantifiable P-31 NMR signals at delta = 6.67 ppm (equatorial phosphate groups of the 4-equatorial/2-axial conformer of neo-IP6) and delta = 6.48 ppm (equatorial phosphate groups of the 2-equatorial/4-axial conformer of D-chiro-IP6) in soil extracts. Inositol hexakisphosphate accounted for 46-54% of the soil organic phosphorus, of which the four stereoisomers constituted, on average, 55.9% (myo), 32.8% (scyllo), 6.1% (neo), and 5.2% (n-chiro). Reappraisal of the literature based on the new signal assignments revealed that neo- and D-chiro-IP6 occur widely in both terrestrial and aquatic ecosystems. These results confirm that the inositol phosphates can constitute a considerable fraction of the organic phosphorus in soils and reveal the prevalence of neo- and D-chiro-IP6 in the environment. The hypobromite oxidation and solution P-31 NMR spectroscopy procedure allows the simultaneous quantification of all four IP6 stereoisomers in environmental samples and provides a platform for research into the origins and ecological significance of these enigmatic compounds.
C1 [Turner, Benjamin L.; Cheesman, Alexander W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Godage, H. Yasmin; Riley, Andrew M.; Potter, Barry V. L.] Univ Bath, Dept Pharm & Pharmacol, Wolfson Lab Med Chem, Bath BA2 7AY, Avon, England.
RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama.
EM TurnerBL@si.edu
RI Turner, Benjamin/E-5940-2011; Riley, Andrew/F-3526-2013; Cheesman,
Alexander/H-5918-2013
OI Turner, Benjamin/0000-0002-6585-0722; Cheesman,
Alexander/0000-0003-3931-5766
FU Wellcome Trust [082837]; National High Magnetic Field Laboratory
FX We thank Jim Rocca for technical support, Andrew Bell for providing soil
samples, and Alan Richardson for providing an authentic sample of
scyllo-IP6 from Dr. Dennis Cosgrove's original collection.
The NMR spectroscopy was funded by 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. We thank the
Wellcome Trust for a Programme Grant (082837) to B.V.L.P. and A.M.R.
NR 54
TC 49
Z9 50
U1 3
U2 52
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD MAY 1
PY 2012
VL 46
IS 9
BP 4994
EP 5002
DI 10.1021/es204446z
PG 9
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 933GO
UT WOS:000303348800044
PM 22489788
ER
PT J
AU Stanley, JD
Bernasconi, MP
AF Stanley, Jean-Daniel
Bernasconi, Maria Pia
TI Buried and Submerged Greek Archaeological Coastal Structures and
Artifacts as Gauges to Measure Late Holocene Seafloor Subsidence off
Calabria, Italy
SO GEOARCHAEOLOGY-AN INTERNATIONAL JOURNAL
LA English
DT Article
ID ANCIENT HARBOR STRUCTURES; REGIONAL UPLIFT; CROTONE BASIN; TECTONIC
IMPLICATIONS; SOUTHERN CALABRIA; NORTHERN CALABRIA; IONIAN CALABRIA;
MARINE TERRACES; LATE QUATERNARY; SILA MASSIF
AB This synthesis integrates recently acquired archaeological and geological data with earlier documented observations to shed light on the subsidence of ancient Greek coastal facilities in southern Italy. These are now positioned between former shorelines and inner shelf sectors at five Calabrian margin localities. Submergence of coastal to inner shelf facilities has resulted in part from sea-level rise by about 2 m associated with glacio-hydro-isostatic factors since archaic to classic Greek time. This phenomenon alone, however, does not explain the wide variation of measured subsidence rates from site-to-site. The marked lowering of coastal site substrates by seismo-tectonic activity (including extensional fault motion), stratal readjustments at depth, and compaction of underlying sediment sequences is significant. Four of the subsided facilities are positioned near emerged Calabrian areas where prevailing Holocene average annual land uplift rates range to 1.0 mm/yr; at the fifth, near Hipponion, terrains have risen by nearly 2 mm/yr. In marked contrast, submerged and/or buried structures record the following late Holocene long-term average rates of coastal margin subsidence: Sybaris-Thuri on the Taranto Gulf margin (0.51.0 mm/yr); Hipponion-Vibo Valentia along the Tyrrhenian coast (0.8 to 3.2 mm/yr); and Locri-Epizefiri, Kaulonia, and Capo Colonna on Calabria's Ionian margin (1.6, 1.62.4, and 4.0 mm/yr, respectively). (c) 2012 Wiley Periodicals, Inc.
C1 [Stanley, Jean-Daniel] Smithsonian Inst, Dept Paleobiol, Geoarchaeol Program, Washington, DC 20560 USA.
[Bernasconi, Maria Pia] Univ Calabria, Dipartimento Sci Terra, Arcavacata Di Rende, CS, Italy.
RP Stanley, JD (reprint author), Smithsonian Inst, Dept Paleobiol, Geoarchaeol Program, Washington, DC 20560 USA.
EM stanleyd@si.edu
FU Department of Paleobiology; ADRC Office, U.S. National Museum of Natural
History, Smithsonian Institution, Washington, D.C.; Universita della
Calabria, Rende
FX We express our special appreciation to Dr. Maria Teresa Iannelli,
Soprintendenza Archaeologica della Calabria, Reggio Calabria, for her
continued generous support of our research efforts on the coastal
margins of Calabria. We thank Dr. J.G. Royal, RPM-Nautical Foundation,
Key West, Florida and G.A.J. Nickerson, Highland Geo Solutions,
Taymouth, New Brunswick, Canada, for generously providing reprocessed
multibeam sonar data sets from the Capo Colonna area and their
assistance in interpreting them. Engineer P. Cappa of the Protected
Marine Area "Capo Rizzuto," Crotone, made available valuable background
data in the form of reports needed for our work on the margin seaward of
the Crotone peninsula. Drs. C. Sabbione and M. Milanesio facilitated our
study on the marine basin site at and seaward of the Locri-Epizefiri
coastal margin, and Dr S. Luppino, Director of the Sybaris Museum and
Archaeological Park, assisted us at the excavated site of Casa Bianca.
Dr. S. Mariottini, Kodros Association, Mentana, Italy, generously shared
photographic, video and other information on the submerged sites off
Kaulonia and Hipponion-Vibo Valentia. Helpful reviews of earlier drafts
of this article were made by Profs. E. Le Pera and F. Scarciglia,
University of Calabria, Rende, Ms. K. Corwin, Smithsonian Institution,
and two anonymous reviewers. Partial funding for this project was
provided (to J.-D.S.) by research awards from the Department of
Paleobiology and the ADRC Office, U.S. National Museum of Natural
History, Smithsonian Institution, Washington, D.C., and (to M. P. B.) by
Universita della Calabria, Rende.
NR 90
TC 11
Z9 11
U1 0
U2 8
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0883-6353
J9 GEOARCHAEOLOGY
JI Geoarchaeology
PD MAY-JUN
PY 2012
VL 27
IS 3
BP 189
EP 205
DI 10.1002/gea.21405
PG 17
WC Archaeology; Geosciences, Multidisciplinary
SC Archaeology; Geology
GA 929CQ
UT WOS:000303039200001
ER
PT J
AU Novikova, I
Walsworth, RL
Xiao, YH
AF Novikova, Irina
Walsworth, Ronald L.
Xiao, Yanhong
TI Electromagnetically induced transparency-based slow and stored light in
warm atoms
SO LASER & PHOTONICS REVIEWS
LA English
DT Review
DE Spin coherence; electromagnetically induced transparency; slow light;
stored light; vapor cells; warm atoms
ID POLARIZATION SELF-ROTATION; SCALABLE QUANTUM NETWORKS; VAPOR CELLS;
RUBIDIUM VAPOR; SQUEEZED-LIGHT; COHERENT MEDIA; SINGLE-PHOTONS;
GROUP-VELOCITY; LINEAR OPTICS; BUFFER-GAS
AB This paper reviews recent efforts to realize a high-efficiency memory for optical pulses using slow and stored light based on electromagnetically induced transparency (EIT) in ensembles of warm atoms in vapor cells. After a brief summary of basic continuous-wave and dynamic EIT properties, studies using weak classical signal pulses in optically dense coherent media are discussed, including optimization strategies for stored light efficiency and pulse-shape control, and modification of EIT and slow/stored light spectral properties due to atomic motion. Quantum memory demonstrations using both single photons and pulses of squeezed light are then reviewed. Finally a brief comparison with other approaches is presented.
C1 [Novikova, Irina] Coll William & Mary, Fac Phys, Williamsburg, VA 23187 USA.
[Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Walsworth, Ronald L.] Harvard Univ, Cambridge, MA 02138 USA.
[Xiao, Yanhong] Fudan Univ, Fac Phys, Shanghai 200433, Peoples R China.
RP Novikova, I (reprint author), Coll William & Mary, Fac Phys, Williamsburg, VA 23187 USA.
EM inovikova@physics.wm.edu
RI Novikova, Irina/B-9041-2008
NR 178
TC 65
Z9 66
U1 9
U2 71
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 1863-8880
EI 1863-8899
J9 LASER PHOTONICS REV
JI Laser Photon. Rev.
PD MAY
PY 2012
VL 6
IS 3
BP 333
EP 353
DI 10.1002/lpor.201100021
PG 21
WC Optics; Physics, Applied; Physics, Condensed Matter
SC Optics; Physics
GA 936NO
UT WOS:000303597400005
ER
PT J
AU Nunez, ET
Sobrino, C
Neale, PJ
Ceinos, RM
Du, SJ
Rotllant, J
AF Torres Nunez, Eva
Sobrino, Cristina
Neale, Patrick J.
Maria Ceinos, Rosa
Du, ShaJun
Rotllant, Josep
TI Molecular Response to Ultraviolet Radiation Exposure in Fish Embryos:
Implications for Survival and Morphological Development
SO PHOTOCHEMISTRY AND PHOTOBIOLOGY
LA English
DT Article
ID SOLAR UV-RADIATION; NUCLEOTIDE EXCISION-REPAIR; AQUATIC ECOSYSTEMS; B
RADIATION; TERRESTRIAL ECOSYSTEMS; ZEBRAFISH EMBRYOS; SKIN FIBROBLASTS;
DNA-DAMAGE; SPARC; EXPRESSION
AB UVR exposure is known to cause developmental defects in a variety of organisms including aquatic species but little is known about the underlying molecular mechanisms. In this work we used zebrafish (Danio rerio) embryos as a model system to characterize the UVR effects on fish species. Larval viability was measured for embryos exposed to several UVR spectral treatments by using a solar simulator lamp and an array of UV cutoff filters under controlled conditions in the laboratory. Survival rate and occurrence of development abnormalities, mainly caudal (posterior) notochord bending/torsion, were seriously affected in UV-exposed larvae reaching values of 53% and 72%, respectively, compared with nonUV-exposed larvae after 6 days postfertilization (dpf). In order to elucidate the molecular mechanisms involved, a matricellular glycoprotein named osteonectin and the expression of a DNA-repair related gene, p53, were studied in relation to UVR exposure. The results indicate that osteonectin and p53 expression were increased under UVR exposure due to wavelengths shorter than 335 nm (i.e. mainly UVB) and 350 nm (i.e. short UVA and UVB), respectively. Furthermore, parallel experiments with microinjections of osteonectin-capped RNA showed that malformations induced by osteonectin overexpression were similar to those observed after a UVR exposure. Consequently this study shows a potential role of osteonectin in morphological deformities induced by solar UV radiation in zebrafish embryos.
C1 [Torres Nunez, Eva; Maria Ceinos, Rosa; Rotllant, Josep] IIM CSIC, Inst Invest Marinas, Vigo, Spain.
[Sobrino, Cristina] Univ Vigo, Dept Ecoloxia & Bioloxia Anim, Vigo 36310, Spain.
[Neale, Patrick J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Du, ShaJun] COMB UMBI, Ctr Marine Biotechnol, Baltimore, MD USA.
RP Rotllant, J (reprint author), IIM CSIC, Inst Invest Marinas, Vigo, Spain.
EM rotllant@iim.csic.es
RI Sobrino, Cristina/J-3534-2012; Rotllant, Josep/K-1146-2014; Ceinos,
Rosa/F-1683-2016;
OI Rotllant, Josep/0000-0001-5331-807X; Ceinos, Rosa/0000-0002-3321-2961;
du, Jim/0000-0001-9227-4153; Sobrino, Cristina/0000-0003-0431-1220
FU FPI [BES-2009-016797]; JAEDoc; Smithsonian Institution; MICIN
[AGL2008-00392/ACU]
FX This work was partly funded by a PhD grant (FPI BES-2009-016797) and a
postdoctoral grant (JAEDoc) to ETN and RMC, respectively, by a
Smithsonian Institution postdoctoral grant to CS and by the MICIN
AGL2008-00392/ACU.
NR 44
TC 4
Z9 4
U1 0
U2 16
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0031-8655
J9 PHOTOCHEM PHOTOBIOL
JI Photochem. Photobiol.
PD MAY-JUN
PY 2012
VL 88
IS 3
BP 701
EP 707
DI 10.1111/j.1751-1097.2012.01088.x
PG 7
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA 935EH
UT WOS:000303501300027
ER
PT J
AU Meyer, KA
Mackay, DH
van Ballegooijen, AA
AF Meyer, K. A.
Mackay, D. H.
van Ballegooijen, A. A.
TI Solar Magnetic Carpet II: Coronal Interactions of Small-Scale Magnetic
Fields
SO SOLAR PHYSICS
LA English
DT Article
DE Sun: magnetic fields
ID ELEMENTARY HEATING EVENTS; RAY BRIGHT POINTS; 2 FLUX SOURCES; QUIET-SUN;
CHROMOSPHERIC NETWORK; ACTIVE REGIONS; MODEL; RECONNECTION;
CANCELLATION; EMERGENCE
AB This paper is the second in a series of studies working towards constructing a realistic, evolving, non-potential coronal model for the solar magnetic carpet. In the present study, the interaction of two magnetic elements is considered. Our objectives are to study magnetic energy build-up, storage and dissipation as a result of emergence, cancellation, and flyby of these magnetic elements. In the future these interactions will be the basic building blocks of more complicated simulations involving hundreds of elements. Each interaction is simulated in the presence of an overlying uniform magnetic field, which lies at various orientations with respect to the evolving magnetic elements. For these three small-scale interactions, the free energy stored in the field at the end of the simulation ranges from 0.2 -aEuro parts per thousand 2.1x10(26) ergs, whilst the total energy dissipated ranges from 1.3 -aEuro parts per thousand 6.3x10(26) ergs. For all cases, a stronger overlying field results in higher energy storage and dissipation. For the cancellation and emergence simulations, motion perpendicular to the overlying field results in the highest values. For the flyby simulations, motion parallel to the overlying field gives the highest values. In all cases, the free energy built up is sufficient to explain small-scale phenomena such as X-ray bright points or nanoflares. In addition, if scaled for the correct number of magnetic elements for the volume considered, the energy continually dissipated provides a significant fraction of the quiet Sun coronal heating budget.
C1 [Meyer, K. A.; Mackay, D. H.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
[van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Meyer, KA (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
EM karen@mcs.st-and.ac.uk
OI van Ballegooijen, Adriaan/0000-0002-5622-3540
FU ISSI (Bern); STFC; Royal Society; EU; ISSI
FX We thank the anonymous referee, whose comments and suggestions have
greatly improved the paper. In particular, we thank the referee for
informing us of the calculation of the theoretical maximum free magnetic
energy for an anti-parallel emergence in Section 3.3. K. A. M. would
like to thank ISSI (Bern) for their support of the team 'Solar
small-scale transient phenomena and their role in coronal heating', and
the Harvard-Smithsonian Center for Astrophysics for their warm
hospitality during the summers of 2010 and 2011. K. A. M. and D. H. M.
acknowledge the financial support of the STFC. DHM would like to thank
the Royal Society for their support through the research grant scheme,
the EU-FP7 collaborative project SWIFF and ISSI.
NR 59
TC 6
Z9 6
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 MAY
PY 2012
VL 278
IS 1
BP 149
EP 175
DI 10.1007/s11207-011-9924-1
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 933WJ
UT WOS:000303395600009
ER
PT J
AU Hope, KL
Tell, LA
Byrne, BA
Murray, S
Wetzlich, SE
Ware, LH
Lynch, W
Padilla, LR
Boedeker, NC
AF Hope, Katharine L.
Tell, Lisa A.
Byrne, Barbara A.
Murray, Suzan
Wetzlich, Scott E.
Ware, Lisa H.
Lynch, Warren
Padilla, Luis R.
Boedeker, Nancy C.
TI Pharmacokinetics of a single intramuscular injection of ceftiofur
crystalline-free acid in American black ducks (Anas rubripes)
SO AMERICAN JOURNAL OF VETERINARY RESEARCH
LA English
DT Article
ID ARA-ARARAUNA; PLASMA; BLUE; DESFUROYLCEFTIOFUR; METABOLITE; PARROTS;
SODIUM; CATTLE; BIRDS; MODEL
AB Objective-To determine the pharmacokinetic properties of 1 IM injection of ceftiofur crystalline-free acid (CCFA) in American black ducks (Anas rubripes).
Animals-20 adult American black ducks (6 in a preliminary experiment and 14 in a primary experiment).
Procedures-Dose and route of administration of CCFA for the primary experiment were determined in a preliminary experiment. In the primary experiment, CCFA (10 mg/kg, IM) was administered to ducks. Ducks were allocated into 2 groups, and blood samples were obtained 0.25, 0.5, 1, 2, 4, 8, 12, 48, 96, 144, 192, and 240 hours or 0.25, 0.5, 1, 2, 4, 8, 24, 72, 120, 168, and 216 hours after administration of CCFA. Plasma concentrations of ceftiofur free acid equivalents (CFAEs) were determined by use of high-performance liquid chromatography. Data were evaluated by use of a naive pooled-data approach.
Results-The area under the plasma concentration versus time curve from 0 hours to infinity was 783 h.mu g/mL, maximum plasma concentration observed was 13.1 mu g/mL, time to maximum plasma concentration observed was 24 hours, terminal phase half-life was 32.0 hours, time that concentrations of CFAEs were higher than the minimum inhibitory concentration (1.0 mu g/mL) for many pathogens of birds was 123 hours, and time that concentrations of CFAEs were higher than the target plasma concentration (4.0 mu g/mL) was 73.3 hours.
Conclusions and Clinical Relevance-On the basis of the time that CFAE concentrations were higher than the target plasma concentration, a dosing interval of 3 days can be recommended for future multidose CCFA studies. (Am J Vet Res 2012;73:620-627)
C1 [Hope, Katharine L.; Murray, Suzan; Boedeker, Nancy C.] Smithsonian Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA.
[Tell, Lisa A.; Wetzlich, Scott E.] Univ Calif Davis, Sch Vet Med, Dept Med & Epidemiol, Davis, CA 95616 USA.
[Byrne, Barbara A.] Univ Calif Davis, Sch Vet Med, Dept Pathol Microbiol & Immunol, Davis, CA 95616 USA.
[Ware, Lisa H.; Lynch, Warren; Padilla, Luis R.] Smithsonian Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
RP Hope, KL (reprint author), Smithsonian Natl Zool Pk, Dept Anim Hlth, 3001 Connecticut Ave NW, Washington, DC 20008 USA.
EM hopek@si.edu
FU Smithsonian Conservation and Biology Institute; Smithsonian National
Zoological Park Department of Animal Health; Smithsonian National
Zoological Park Department of Animal Programs
FX Supported by the Smithsonian National Zoological Park Departments of
Animal Health and Animal Programs and by the Smithsonian Conservation
and Biology Institute.
NR 31
TC 10
Z9 11
U1 1
U2 15
PU AMER VETERINARY MEDICAL ASSOC
PI SCHAUMBURG
PA 1931 N MEACHAM RD SUITE 100, SCHAUMBURG, IL 60173-4360 USA
SN 0002-9645
J9 AM J VET RES
JI Am. J. Vet. Res.
PD MAY
PY 2012
VL 73
IS 5
BP 620
EP 627
PG 8
WC Veterinary Sciences
SC Veterinary Sciences
GA 933LY
UT WOS:000303364300005
PM 22533392
ER
PT J
AU Bryan, ML
Alsubai, KA
Latham, DW
Parley, NR
Cameron, AC
Quinn, SN
Carter, JA
Fulton, BJ
Berlind, P
Brown, WR
Buchhave, LA
Calkins, ML
Esquerdo, GA
Furesz, G
Jorgensen, UG
Horne, KD
Stefanik, RP
Street, RA
Torres, G
West, RG
Dominik, M
Harpsoe, KBW
Liebig, C
Novati, SC
Ricci, D
Skottfelt, JF
AF Bryan, Marta L.
Alsubai, Khalid A.
Latham, David W.
Parley, Neil R.
Cameron, Andrew Collier
Quinn, Samuel N.
Carter, Joshua A.
Fulton, Benjamin J.
Berlind, Perry
Brown, Warren R.
Buchhave, Lars A.
Calkins, Michael L.
Esquerdo, Gilbert A.
Furesz, Gabor
Jorgensen, Uffe Grae
Horne, Keith D.
Stefanik, Robert P.
Street, Rachel A.
Torres, Guillermo
West, Richard G.
Dominik, Martin
Harpsoe, Kennet B. W.
Liebig, Christine
Novati, Sebastiano Calchi
Ricci, Davide
Skottfelt, Jesper F.
TI QATAR-2: A K DWARF ORBITED BY A TRANSITING HOT JUPITER AND A MORE
MASSIVE COMPANION IN AN OUTER ORBIT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (Qatar-2); techniques: photometric;
techniques: radial velocities; techniques: spectroscopic
ID PROPER-MOTION STARS; LIGHT CURVES; PLANET; ALGORITHM; CANDIDATES;
PARAMETERS; ATMOSPHERE; SPECTRUM; SYSTEMS; SEARCH
AB We report the discovery and initial characterization of Qatar-2b, a hot Jupiter transiting a V = 13.3 mag K dwarf in a circular orbit with a short period, P-b = 1.34 days. The mass and radius of Qatar-2b are M-P = 2.49 M-J and R-P = 1.14 R-J, respectively. Radial-velocity monitoring of Qatar-2 over a span of 153 days revealed the presence of a second companion in an outer orbit. The Systemic Console yielded plausible orbits for the outer companion, with periods on the order of a year and a companion mass of at least several M-J. Thus, Qatar-2 joins the short but growing list of systems with a transiting hot Jupiter and an outer companion with a much longer period. This system architecture is in sharp contrast to that found by Kepler for multi-transiting systems, which are dominated by objects smaller than Neptune, usually with tightly spaced orbits that must be nearly coplanar.
C1 [Bryan, Marta L.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Alsubai, Khalid A.] Qatar Fdn, Doha, Qatar.
[Latham, David W.; Quinn, Samuel N.; Carter, Joshua A.; Berlind, Perry; Brown, Warren R.; Calkins, Michael L.; Esquerdo, Gilbert A.; Furesz, Gabor; Stefanik, Robert P.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Parley, Neil R.; Cameron, Andrew Collier; Horne, Keith D.; Dominik, Martin; Liebig, Christine] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Fulton, Benjamin J.; Street, Rachel A.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Buchhave, Lars A.; Jorgensen, Uffe Grae; Harpsoe, Kennet B. W.; Skottfelt, Jesper F.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.; Jorgensen, Uffe Grae; Harpsoe, Kennet B. W.; Skottfelt, Jesper F.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[West, Richard G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Novati, Sebastiano Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, I-84081 Baronissi, SA, Italy.
[Novati, Sebastiano Calchi] Ist Nazl Fis Nucl, Grp Collegato Salerno, Sez Napoli, Salerno, Italy.
[Ricci, Davide] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Furesz, Gabor] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary.
RP Bryan, ML (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
RI Carter, Joshua/A-8280-2013;
OI Dominik, Martin/0000-0002-3202-0343; Buchhave, Lars
A./0000-0003-1605-5666; Cameron, Andrew/0000-0002-8863-7828; Ricci,
Davide/0000-0002-9790-0552
FU Hungarian OTKA-NFU [MB08C 81013]; Qatar Foundation from QNRF
[NPRP-09-476-1-078]; Communaute francaise de Belgique-Actions de
recherche concertees-Academie universitaire Wallonie-Europe
FX G.F. acknowledges financial support from the Hungarian OTKA-NFU Mobility
grant MB08C 81013. C.L. acknowledges the Qatar Foundation for support
from QNRF grant NPRP-09-476-1-078. D.R. (boursier FRIA) acknowledges
support from the Communaute francaise de Belgique-Actions de recherche
concertees-Academie universitaire Wallonie-Europe. The Byrne Observatory
at Sedgwick (BOS) is operated by the Las Cumbres Observatory Global
Telescope Network and is located at the Sedgwick Reserve, a part of the
University of California Natural Reserve System. We thank the anonymous
referee for several helpful suggestions for improving the clarity of the
manuscript and the interpretation of the results.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY
PY 2012
VL 750
IS 1
AR 84
DI 10.1088/0004-637X/750/1/84
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500084
ER
PT J
AU Dawson, RI
Murray-Clay, R
AF Dawson, Rebekah I.
Murray-Clay, Ruth
TI NEPTUNE'S WILD DAYS: CONSTRAINTS FROM THE ECCENTRICITY DISTRIBUTION OF
THE CLASSICAL KUIPER BELT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE celestial mechanics; Kuiper belt: general; planets and satellites:
dynamical evolution and stability; planets and satellites: individual
(Neptune)
ID SOLAR-SYSTEM; INCLINATION DISTRIBUTION; ORIGIN; MIGRATION; INSTABILITY;
OBJECTS; BODIES; URANUS; ORBIT; AU
AB Neptune's dynamical history shaped the current orbits of Kuiper Belt objects (KBOs), leaving clues to the planet's orbital evolution. In the "classical" region, a population of dynamically "hot" high-inclination KBOs overlies a flat "cold" population with distinct physical properties. Simulations of qualitatively different histories for Neptune, including smooth migration on a circular orbit or scattering by other planets to a high eccentricity, have not simultaneously produced both populations. We explore a general Kuiper Belt assembly model that forms hot classical KBOs interior to Neptune and delivers them to the classical region, where the cold population forms in situ. First, we present evidence that the cold population is confined to eccentricities well below the limit dictated by long-term survival. Therefore, Neptune must deliver hot KBOs into the long-term survival region without excessively exciting the eccentricities of the cold population. Imposing this constraint, we explore the parameter space of Neptune's eccentricity and eccentricity damping, migration, and apsidal precession. We rule out much of parameter space, except where Neptune is scattered to a moderately eccentric orbit (e > 0.15) and subsequently migrates a distance Delta a(N) = 1-6 AU. Neptune's moderate eccentricity must either damp quickly or be accompanied by fast apsidal precession. We find that Neptune's high eccentricity alone does not generate a chaotic sea in the classical region. Chaos can result from Neptune's interactions with Uranus, exciting the cold KBOs and placing additional constraints. Finally, we discuss how to interpret our constraints in the context of the full, complex dynamical history of the solar system.
C1 [Dawson, Rebekah I.; Murray-Clay, Ruth] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Dawson, RI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
EM rdawson@cfa.harvard.edu
FU National Science Foundation [DGE064449, DGE0946799, DGE 1144152]; FAS
Sciences Division Research Computing Group
FX R.I.D. gratefully acknowledges support by the National Science
Foundation Graduate Research Fellowship under grants DGE064449,
DGE0946799, and DGE 1144152. The numerical integrations in this paper
were run on the Odyssey cluster supported by the FAS Sciences Division
Research Computing Group. We thank Gurtina Besla, David Charbonneau,
Matija Cuk, Matthew Holman, Kaitlin Kratter, David Latham, Renu
Malhotra, Diego Munoz, Darin Raggozine, Schuyler Wolff, and Kathryn Volk
for helpful discussions. We thank Konstantin Batygin, Daniel Fabrycky,
Darin Raggozine, Kathryn Volk, and Jack Wisdom for insightful comments
on a manuscript draft. We are grateful to Hal Levison for many helpful
comments on improving this paper. We gratefully acknowledge an anonymous
referee for constructive feedback.
NR 44
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY
PY 2012
VL 750
IS 1
AR 43
DI 10.1088/0004-637X/750/1/43
PG 29
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500043
ER
PT J
AU Dupree, AK
Brickhouse, NS
Cranmer, SR
Luna, GJM
Schneider, EE
Bessell, MS
Bonanos, A
Crause, LA
Lawson, WA
Mallik, SV
Schuler, SC
AF Dupree, A. K.
Brickhouse, N. S.
Cranmer, S. R.
Luna, G. J. M.
Schneider, E. E.
Bessell, M. S.
Bonanos, A.
Crause, L. A.
Lawson, W. A.
Mallik, S. V.
Schuler, S. C.
TI TW Hya: SPECTRAL VARIABILITY, X-RAYS, AND ACCRETION DIAGNOSTICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars: individual (TW Hydrae); stars:
pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; stars:
winds, outflows
ID TAURI MAGNETOSPHERIC ACCRETION; EMISSION-LINE DIAGNOSTICS; ORION NEBULA
CLUSTER; DISK ACCRETION; BROWN DWARFS; TIME-SERIES; STARS; HYDRAE;
MODELS; SPECTROSCOPY
AB The nearest accreting T Tauri star, TW Hya was intensively and continuously observed over similar to 17 days with spectroscopic and photometric measurements from four continents simultaneous with a long segmented exposure using the Chandra satellite. Contemporaneous optical photometry from WASP-S indicates a 4.74 day period was present during this time. The absence of a similar periodicity in the H alpha flux and the total X-ray flux which are dominated by accretion processes and the stellar corona, respectively, points to a different source of photometric variations. The H alpha emission line appears intrinsically broad and symmetric, and both the profile and its variability suggest an origin in the post-shock cooling region. An accretion event, signaled by soft X-rays, is traced spectroscopically for the first time through the optical emission line profiles. After the accretion event, downflowing turbulent material observed in the H alpha and H beta lines is followed by He I (lambda 5876) broadening near the photosphere. Optical veiling resulting from the heated photosphere increases with a delay of similar to 2 hr after the X-ray accretion event. The response of the stellar coronal emission to an increase in the veiling follows similar to 2.4 hr later, giving direct evidence that the stellar corona is heated in part by accretion. Subsequently, the stellar wind becomes re-established. We suggest a model that incorporates the dynamics of this sequential series of events: an accretion shock, a cooling downflow in a supersonically turbulent region, followed by photospheric and later, coronal heating. This model naturally explains the presence of broad optical and ultraviolet lines, and affects the mass accretion rates determined from emission line profiles.
C1 [Dupree, A. K.; Brickhouse, N. S.; Cranmer, S. R.; Luna, G. J. M.; Schneider, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bessell, M. S.] Mt Stromlo & Siding Spring Observ, Australian Natl Observ, Canberra, ACT 2611, Australia.
[Bonanos, A.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece.
[Crause, L. A.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Lawson, W. A.] Univ New S Wales, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia.
[Mallik, S. V.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[Schuler, S. C.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Bonanos, Alceste/K-5392-2013;
OI Bonanos, Alceste/0000-0003-2851-1905; Brickhouse,
Nancy/0000-0002-8704-4473
FU Science and Technology Facilities Council of the UK
FX We are grateful to Jonathan Irwin for assistance with the WASP data. The
WASP consortium comprises the University of Cambridge, Keele University,
University of Leicester, The Open University, The Queens University
Belfast, St. Andrews University, and the Isaac Newton Group. Funding for
WASP comes from the consortium universities and from the Science and
Technology Facilities Council of the UK. We appreciate the efforts of
Luca DiFabrizio who reduced the TNG/SARG spectrum. This paper includes
data gathered with the 6.5 m Magellan Telescopes located at Las Campanas
Observatory, Chile. Also, based on observations obtained at the Gemini
Observatory, which is operated by the Association of Universities for
Research in Astronomy, Inc., under a cooperative agreement with the NSF
on behalf of the Gemini partnership: the National Science Foundation
(United States), the Science and Technology Facilities Council (United
Kingdom), the National Research Council (Canada), CONICYT (Chile), the
Australian Research Council (Australia), Ministerio da Ciencia,
Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e
Innovacion Productiva (Argentina).
NR 51
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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 MAY
PY 2012
VL 750
IS 1
AR 73
DI 10.1088/0004-637X/750/1/73
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500073
ER
PT J
AU Gunther, HM
Wolk, SJ
Drake, JJ
Lisse, CM
Robrade, J
Schmitt, JHMM
AF Guenther, H. M.
Wolk, S. J.
Drake, J. J.
Lisse, C. M.
Robrade, J.
Schmitt, J. H. M. M.
TI SOFT CORONAL X-RAYS FROM beta PICTORIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: chromospheres; stars: coronae; stars:
individual: beta Pictoris; X-rays: stars
ID HIGH-RESOLUTION CAMERA; IN-FLIGHT PERFORMANCE; DARKEST BRIGHT STAR;
WIND-SHOCK MODEL; SOLAR-LIKE STARS; ALL-SKY SURVEY; OB-TYPE STARS;
CIRCUMSTELLAR DISK; MOVING GROUP; HERBIG STAR
AB A-type stars are expected to be X-ray dark, yet weak emission has been detected from several objects in this class. We present new Chandra/HRC-I observations of the A5 V star beta Pictoris. It is clearly detected with a flux of (9 +/- 2) x 10(-4) counts s(-1). In comparison with previous data this constrains the emission mechanism and we find that the most likely explanation is an optically thin, collisionally dominated, thermal emission component with a temperature around 1.1 MK. We interpret this component as a very cool and dim corona, with log L-X/L-bol = -8.2 (0.2-2.0 keV). Thus, it seems that beta Pictoris shares more characteristics with cool stars than previously thought.
C1 [Guenther, H. M.; Wolk, S. J.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Robrade, J.; Schmitt, J. H. M. M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany.
RP Gunther, HM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM hguenther@cfa.harvard.edu
RI Lisse, Carey/B-7772-2016;
OI Lisse, Carey/0000-0002-9548-1526; Gunther, Hans
Moritz/0000-0003-4243-2840
FU National Aeronautics and Space Administration through Chandra X-ray
Observatory Center [GO2-13015X]; National Aeronautics Space
Administration [NAS8-03060]
FX Support for this work was provided by the National Aeronautics and Space
Administration through the Chandra Award Number GO2-13015X 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 the contract NAS8-03060.
NR 42
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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 MAY
PY 2012
VL 750
IS 1
AR 78
DI 10.1088/0004-637X/750/1/78
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500078
ER
PT J
AU Hughes, AM
Wilner, DJ
Mason, B
Carpenter, JM
Plambeck, R
Chiang, HF
Andrews, SM
Williams, JP
Hales, A
Su, K
Chiang, E
Dicker, S
Korngut, P
Devlin, M
AF Hughes, A. Meredith
Wilner, David J.
Mason, Brian
Carpenter, John M.
Plambeck, Richard
Chiang, Hsin-Fang
Andrews, Sean M.
Williams, Jonathan P.
Hales, Antonio
Su, Kate
Chiang, Eugene
Dicker, Simon
Korngut, Phil
Devlin, Mark
TI CONFIRMING THE PRIMARILY SMOOTH STRUCTURE OF THE VEGA DEBRIS DISK AT
MILLIMETER WAVELENGTHS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; planet-disk interactions;
stars: individual (Vega)
ID BETA-PICTORIS; KUIPER-BELT; HR 8799; CIRCUMSTELLAR DISK; SOLAR-SYSTEM;
NEARBY STARS; DUSTY DEBRIS; HD 107146; POLE-ON; SUBMILLIMETER
AB Clumpy structure in the debris disk around Vega has been previously reported at millimeter wavelengths and attributed to concentrations of dust grains trapped in resonances with an unseen planet. However, recent imaging at similar wavelengths with higher sensitivity has disputed the observed structure. We present three new millimeter-wavelength observations that help to resolve the puzzling and contradictory observations. We have observed the Vega system with the Submillimeter Array (SMA) at a wavelength of 880 mu m and an angular resolution of 5 ''; with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) at a wavelength of 1.3 mm and an angular resolution of 5 ''; and with the Green Bank Telescope (GBT) at a wavelength of 3.3 mm and angular resolution of 10 ''. Despite high sensitivity and short baselines, we do not detect the Vega debris disk in either of the interferometric data sets (SMA and CARMA), which should be sensitive at high significance to clumpy structure based on previously reported observations. We obtain a marginal (3 sigma) detection of disk emission in the GBT data; the spatial distribution of the emission is not well constrained. We analyze the observations in the context of several different models, demonstrating that the observations are consistent with a smooth, broad, axisymmetric disk with inner radius 20-100 AU and width greater than or similar to 50 AU. The interferometric data require that at least half of the 860 mu m emission detected by previous single-dish observations with the James Clerk Maxwell Telescope be distributed axisymmetrically, ruling out strong contributions from flux concentrations on spatial scales of less than or similar to 100 AU. These observations support recent results from the Plateau de Bure Interferometer indicating that previous detections of clumpy structure in the Vega debris disk were spurious.
C1 [Hughes, A. Meredith; Plambeck, Richard; Chiang, Eugene] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Wilner, David J.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mason, Brian] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Carpenter, John M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Chiang, Hsin-Fang] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Chiang, Hsin-Fang] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Hales, Antonio] Joint ALMA Observ, Santiago, Chile.
[Su, Kate] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Dicker, Simon; Korngut, Phil; Devlin, Mark] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
RP Hughes, AM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM mhughes@astro.berkeley.edu
OI Williams, Jonathan/0000-0001-5058-695X; Su, Kate/0000-0002-3532-5580
FU Miller Institute for Basic Research in Science; NSF [AST-1007905,
AST-0909210]; Millennium Science Initiative, Chilean Ministry of
Economy: Nucleus [P10-022-F]; [AGBT08C026]
FX We thank Mark Wyatt for providing us with his model of the planetesimal
distribution in the Vega system. The authors also thank the MUSTANG
instrument team from the University of Pennsylvania, NRAO, Cardiff
University, NASA-GSFC, and NIST for their efforts on the instrument and
software that have made this work possible. The GBT data were obtained
under the auspices of observing program AGBT08C026. A.M.H. is supported
by a fellowship from the Miller Institute for Basic Research in Science.
S. Dicker is supported by NSF AST-1007905. A.H. acknowledges support
from Millennium Science Initiative, Chilean Ministry of Economy: Nucleus
P10-022-F. E.C. acknowledges support by NSF grant AST-0909210.
NR 55
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY
PY 2012
VL 750
IS 1
AR 82
DI 10.1088/0004-637X/750/1/82
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500082
ER
PT J
AU King, C
Brown, WR
Geller, MJ
Kenyon, SJ
AF King, Charles, III
Brown, Warren R.
Geller, Margaret J.
Kenyon, Scott J.
TI IDENTIFYING STAR STREAMS IN THE MILKY WAY HALO
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE blue stragglers; galaxies: individual (Sagittarius dwarf galaxy);
Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: stellar content;
Galaxy: structure; stars: horizontal-branch
ID SAGITTARIUS DWARF GALAXY; ALL-SKY SURVEY; VELOCITY EXPERIMENT RAVE;
HYPERVELOCITY STARS; STELLAR HALO; THEORETICAL ISOCHRONES; PHOTOMETRIC
SYSTEMS; TIDAL STREAMS; GALACTIC HALO; DATA RELEASE
AB We develop statistical methods for identifying star streams in the halo of the Milky Way that exploit observed spatial and radial velocity distributions. Within a great circle, departures of the observed spatial distribution from random provide a measure of the likelihood of a potential star stream. Comparisons between the radial velocity distribution within a great circle and the radial velocity distribution of the entire sample also measure the statistical significance of potential streams. The radial velocities enable construction of a more powerful joint statistical test for identifying star streams in the Milky Way halo. Applying our method to halo stars in the Hypervelocity Star (HVS) survey, we detect the Sagittarius stream at high significance. Great circle counts and comparisons with theoretical models suggest that the Sagittarius stream comprises 10%-17% of the halo stars in the HVS sample. The population of blue stragglers and blue horizontal branch stars varies along the stream and is a potential probe of the distribution of stellar populations in the Sagittarius dwarf galaxy prior to disruption.
C1 [King, Charles, III; Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[King, Charles, III] Pleiades Consulting Grp Inc, Lincoln, MA 01773 USA.
RP King, C (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM cking@cfa.harvard.edu; wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu;
skenyon@cfa.harvard.edu
OI Kenyon, Scott/0000-0003-0214-609X
FU Smithsonian Institution; Pleiades Consulting Group Inc.
FX We thank M. Alegria, J. McAfee, A. Milone, and the rest of the MMTO
staff for their assistance with observations obtained at the MMT
Observatory. We thank David Law for providing us with N-body simulations
from his model of the Sagittarius stream. We also thank the referee for
helpful comments. This project makes use of data products from the Sloan
Digital Sky Survey, which is managed by the Astrophysical Research
Consortium for the Participating Institutions. This research makes use
of NASA's Astrophysics Data System Bibliographic Services. This work was
supported by the Smithsonian Institution. C.K. gratefully acknowledges
additional support from Pleiades Consulting Group Inc. and dedicates
this work to the memory of Dr. Natarajan Visvanathan.
NR 49
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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 MAY
PY 2012
VL 750
IS 1
AR 81
DI 10.1088/0004-637X/750/1/81
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500081
ER
PT J
AU Meyers, J
Aldering, G
Barbary, K
Barrientos, LF
Brodwin, M
Dawson, KS
Deustua, S
Doi, M
Eisenhardt, P
Faccioli, L
Fakhouri, HK
Fruchter, AS
Gilbank, DG
Gladders, MD
Goldhaber, G
Gonzalez, AH
Hattori, T
Hsiao, E
Ihara, Y
Kashikawa, N
Koester, B
Konishi, K
Lidman, C
Lubin, L
Morokuma, T
Oda, T
Perlmutter, S
Postman, M
Ripoche, P
Rosati, P
Rubin, D
Rykoff, E
Spadafora, A
Stanford, SA
Suzuki, N
Takanashi, N
Tokita, K
Yasuda, N
AF Meyers, J.
Aldering, G.
Barbary, K.
Barrientos, L. F.
Brodwin, M.
Dawson, K. S.
Deustua, S.
Doi, M.
Eisenhardt, P.
Faccioli, L.
Fakhouri, H. K.
Fruchter, A. S.
Gilbank, D. G.
Gladders, M. D.
Goldhaber, G.
Gonzalez, A. H.
Hattori, T.
Hsiao, E.
Ihara, Y.
Kashikawa, N.
Koester, B.
Konishi, K.
Lidman, C.
Lubin, L.
Morokuma, T.
Oda, T.
Perlmutter, S.
Postman, M.
Ripoche, P.
Rosati, P.
Rubin, D.
Rykoff, E.
Spadafora, A.
Stanford, S. A.
Suzuki, N.
Takanashi, N.
Tokita, K.
Yasuda, N.
CA Supernova Cosmology Project
TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. III. CORRELATED
PROPERTIES OF TYPE Ia SUPERNOVAE AND THEIR HOSTS AT 0.9 < z < 1.46
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; dark energy; distance scale; galaxies:
clusters: general; galaxies: elliptical and lenticular, cD; supernovae:
general
ID EARLY-TYPE GALAXIES; COLOR-MAGNITUDE RELATION; HIGH-REDSHIFT CLUSTERS;
DIGITAL SKY SURVEY; SIMILAR-TO 1; INITIAL MASS FUNCTION; AMES ELLIPTIC
GALAXIES; RECENT STAR-FORMATION; IRAC SHALLOW SURVEY; DISTANT CLUSTERS
AB Using the sample of Type Ia supernovae (SNe Ia) discovered by the Hubble Space Telescope (HST) Cluster Supernova Survey and augmented with HST-observed SNe Ia in the Great Observatories Origins Deep Survey (GOODS) fields, we search for correlations between the properties of SNe and their host galaxies at high redshift. We use galaxy color and quantitative morphology to determine the red sequence in 25 clusters and develop a model to distinguish passively evolving early-type galaxies from star-forming galaxies in both clusters and the field. With this approach, we identify 6 SN Ia hosts that are early-type cluster members and 11 SN Ia hosts that are early-type field galaxies. We confirm for the first time at z > 0.9 that SNe Ia hosted by early-type galaxies brighten and fade more quickly than SNe Ia hosted by late-type galaxies. We also show that the two samples of hosts produce SNe Ia with similar color distributions. The relatively simple spectral energy distributions expected for passive galaxies enable us to measure stellar masses of early-type SN hosts. In combination with stellar mass estimates of late-type GOODS SN hosts from Thomson & Chary, we investigate the correlation of host mass with Hubble residual observed at lower redshifts. Although the sample is small and the uncertainties are large, a hint of this relation is found atz > 0.9. By simultaneously fitting the average cluster galaxy formation history and dust content to the red-sequence scatters, we show that the reddening of early-type cluster SN hosts is likely E(B - V) less than or similar to 0.06. The similarity of the field and cluster early-type host samples suggests that field early-type galaxies that lie on the red sequence may also be minimally affected by dust. Hence, the early-type-hosted SNe Ia studied here occupy a more favorable environment to use as well-characterized high-redshift standard candles than other SNe Ia.
C1 [Meyers, J.; Barbary, K.; Fakhouri, H. K.; Goldhaber, G.; Perlmutter, S.; Rubin, D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Meyers, J.; Aldering, G.; Barbary, K.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Perlmutter, S.; Ripoche, P.; Rubin, D.; Rykoff, E.; Spadafora, A.; Suzuki, N.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Barrientos, L. F.] Pontificia Univ Catolica Chile, Dept Astron, Santiago, Chile.
[Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Deustua, S.; Fruchter, A. S.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan.
[Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Hattori, T.] Natl Inst Nat Sci, Natl Astron Observ Japan, Hilo, HI 96720 USA.
[Kashikawa, N.; Morokuma, T.; Takanashi, N.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Konishi, K.; Yasuda, N.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95618 USA.
[Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Rosati, P.] ESO, D-85748 Garching, Germany.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
RP Meyers, J (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
EM jmeyers314@berkeley.edu
RI Perlmutter, Saul/I-3505-2015;
OI Perlmutter, Saul/0000-0002-4436-4661; Meyers, Joshua/0000-0002-2308-4230
FU NASA from the Space Telescope Science Institute [GO-10496]; NASA [NAS
5-26555]; Office of Science, Office of High Energy and Nuclear Physics,
of the U.S. Department of Energy [AC02-05CH11231]; JSPS [20040003]
FX We thank a very helpful referee for suggestions that improved the
quality of this paper. We also thank Pasquale Temi for comments on the
infrared dust properties of nearby early-type galaxies. Financial
support for this work was provided by NASA through program GO-10496 from
the Space Telescope Science Institute, which is operated by AURA, Inc.,
under NASA contract NAS 5-26555. This work was also supported in part by
the Director, Office of Science, Office of High Energy and Nuclear
Physics, of the U.S. Department of Energy under Contract No.
AC02-05CH11231, as well as a JSPS core-to-core program "International
Research Network for Dark Energy" and by a JSPS research grant
(20040003). 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. Finally, this work would not have been possible without the
dedicated efforts of the daytime and nighttime support staff at the
Cerro Paranal Observatory.
NR 154
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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 MAY
PY 2012
VL 750
IS 1
AR 1
DI 10.1088/0004-637X/750/1/1
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500001
ER
PT J
AU Neilsen, J
Remillard, RA
Lee, JC
AF Neilsen, Joseph
Remillard, Ronald A.
Lee, Julia C.
TI RADIATION PRESSURE AND MASS EJECTION IN rho-LIKE STATES OF GRS 1915+105
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; instabilities; X-rays:
binaries; X-rays: individual (GRS 1915+105)
ID BLACK-HOLE CANDIDATE; X-RAY-BURSTS; ACCRETION DISK; COMPLEX BEHAVIOR;
IGR J17091-3624; UNIFIED MODEL; GRS-1915+105; VARIABILITY; JET;
INSTABILITY
AB We present a unifying scenario to address the physical origin of the diversity of X-ray light curves within the rho variability class of the microquasar GRS 1915+105. This "heartbeat" state is characterized by a bright flare that recurs every similar to 50-100 s, but the profile and duration of the flares vary significantly from observation to observation. Based on a comprehensive, phase-resolved study of heartbeats in the Rossi X-ray Timing Explorer archive, we demonstrate that very different X-ray light curves do not require origins in different accretion processes. Indeed, our detailed comparison of the phase-resolved spectra of a double-peaked oscillation and a single-peaked oscillation shows that different cycles can have basically similar X-ray spectral evolution. We argue that all heartbeat oscillations can be understood as the result of a combination of a thermal-viscous radiation pressure instability, a local Eddington limit in the disk, and a sudden, radiation-pressure-driven evaporation or ejection event in the inner accretion disk. This ejection appears to be a universal, fundamental part of the rho state, and is largely responsible for a hard X-ray pulse seen in the light curve of all cycles. We suggest that the detailed shape of oscillations in the mass accretion rate through the disk is responsible for the phenomenological differences between different rho-type light curves, and we discuss how future time-dependent simulations of disk instabilities may provide new insights into the role of radiation pressure in the accretion flow.
C1 [Neilsen, Joseph; Remillard, Ronald A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Neilsen, Joseph; Lee, Julia C.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Neilsen, Joseph; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Neilsen, J (reprint author), MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
EM jneilsen@space.mit.edu
OI Neilsen, Joseph/0000-0002-8247-786X
FU Chandra [G07-8044X]; Harvard University Graduate School of Arts and
Sciences; National Aeronautics and Space Administration through the
Smithsonian Astrophysical Observatory [SV3-73016]; National Aeronautics
Space Administration [NAS8-03060]
FX We thank Diego Altamirano for provocative discussions of IGR 17091-3624
and GRS 1915+105. J.N. gratefully acknowledges funding support from
Chandra grant G07-8044X and the Harvard University Graduate School of
Arts and Sciences, as well as support from the National Aeronautics and
Space Administration through the Smithsonian Astrophysical Observatory
contract SV3-73016 to MIT for support of the Chandra X-ray Center, which
is operated by the Smithsonian Astrophysical Observatory for and on
behalf of the National Aeronautics Space Administration under contract
NAS8-03060. R.A.R. acknowledges partial support from the NASA contract
to MIT for the support of RXTE instruments. This research has made use
of data obtained from the High Energy Astrophysics Science Archive
Research Center (HEASARC), provided by NASA's Goddard Space Flight
Center.
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 MAY
PY 2012
VL 750
IS 1
AR 71
DI 10.1088/0004-637X/750/1/71
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500071
ER
PT J
AU Perets, HB
Kouwenhoven, MBN
AF Perets, Hagai B.
Kouwenhoven, M. B. N.
TI ON THE ORIGIN OF PLANETS AT VERY WIDE ORBITS FROM THE RECAPTURE OF FREE
FLOATING PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; planetary systems; planets and satellites: detection;
planets and satellites: dynamical evolution and stability; planets and
satellites: formation; stars: kinematics and dynamics
ID SOLAR-TYPE STARS; UPPER SCORPIUS; BROWN DWARF; DYNAMICAL INTERACTIONS;
STELLAR CLUSTERS; AGE DISTRIBUTION; MASS COMPANIONS; GIANT PLANETS;
BINARY STARS; EVOLUTION
AB In recent years, several planets have been discovered at wide orbits (>100 AU) around their host stars. Theoretical studies encounter difficulties in explaining their formation and origin. Here we propose a novel scenario for the production of planetary systems at such orbits, through the dynamical recapture of free floating planets (FFPs) in dispersing stellar clusters and stellar associations. This process is a natural extension of the recently suggested scenario for the formation of wide stellar binaries. We use N-body simulations of dispersing clusters with 10-1000 stars and comparable numbers of FFPs to study this process. We find that planets are captured into wide orbits in the typical range similar to few x 100-10(6) AU and have a wide range of eccentricities (thermal distribution). Typically, 3-6 x (f(FFP)/1)% of all stars capture a planetary companion with such properties (where f(FFP) is the number of FFP per star in the birth clusters). The planetary capture efficiency is comparable to that of capture-formed stellar binaries, and shows a similar dependence on the cluster size and structure. It is almost independent of the specific planetary mass; planets as well as substellar companions of any mass can be captured. The capture efficiency decreases with increasing cluster size, and for a given cluster size it increases with the host/primary mass. We also find that more than one planet can be captured around the same host through independent consecutive captures; similarly, planets can be captured into binary systems, both in circumstellar and circumbinary orbits. We also expect planets to be captured into pre-existing planetary (and protoplanetary systems) as well as into orbits around black holes and massive white dwarfs, if these formed early enough before the cluster dispersal. In particular, stellar black holes have a high capture efficiency (>50% and 5-10 x (f(FFP)/1)% for capture of stars and planetary companions, respectively) due to their large mass. Finally, although rare, two FFPs or brown dwarfs can become bound and form an FFP-binary system with no stellar host.
C1 [Perets, Hagai B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kouwenhoven, M. B. N.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
RP Perets, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM hperets@physics.cfa.harvard.edu; thijskouwenhoven@gmail.com
RI Kouwenhoven, M.B.N./G-3854-2015; Perets, Hagai/K-9605-2015
OI Kouwenhoven, M.B.N./0000-0002-1805-0570; Perets,
Hagai/0000-0002-5004-199X
FU Peter and Patricia Gruber Foundation through the IAU-PPGF; Peking
University [985]; National Natural Science Foundation of China
[11010237, 11050110414, 11173004]
FX H.B.P. is a CfA and BIKURA (FIRST) fellow. M.B.N.K. was supported by the
Peter and Patricia Gruber Foundation through the IAU-PPGF fellowship, by
the Peking University One Hundred Talent Fund (985), and by the National
Natural Science Foundation of China (grants 11010237, 11050110414,
11173004). The authors thank Michael Ireland, Nathan Kaib, Sally
Dodson-Robinson, and the anonymous referee for helpful comments that
helped improve this manuscript.
NR 45
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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 MAY
PY 2012
VL 750
IS 1
AR 83
DI 10.1088/0004-637X/750/1/83
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500083
ER
PT J
AU Savcheva, A
Pariat, E
van Ballegooijen, A
Aulanier, G
DeLuca, E
AF Savcheva, A.
Pariat, E.
van Ballegooijen, A.
Aulanier, G.
DeLuca, E.
TI SIGMOIDAL ACTIVE REGION ON THE SUN: COMPARISON OF A
MAGNETOHYDRODYNAMICAL SIMULATION AND A NONLINEAR FORCE-FREE FIELD MODEL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: flares; Sun: magnetic topology
ID QUASI-SEPARATRIX LAYERS; CORONAL MASS EJECTIONS; MAGNETIC-FLUX ROPES;
CURRENT-SHEET FORMATION; GLOBAL SOLAR CORONA; PHOTOSPHERIC MOTIONS;
HEMISPHERIC PATTERN; KINK INSTABILITY; NULL POINTS; FILAMENT
AB In this paper we show that when accurate nonlinear force-free field (NLFFF) models are analyzed together with high-resolution magnetohydrodynamic (MHD) simulations, we can determine the physical causes for the coronal mass ejection (CME) eruption on 2007 February 12. We compare the geometrical and topological properties of the three-dimensional magnetic fields given by both methods in their pre-eruptive phases. We arrive at a consistent picture for the evolution and eruption of the sigmoid. Both the MHD simulation and the observed magnetic field evolution show that flux cancellation plays an important role in building the flux rope. We compute the squashing factor, Q, in different horizontal maps in the domains. The main shape of the quasi-separatrix layers (QSLs) is very similar between the NLFFF and MHD models. The main QSLs lie on the edge of the flux rope. While the QSLs in the NLFFF model are more complex due to the intrinsic large complexity in the field, the QSLs in the MHD model are smooth and possess lower maximum value of Q. In addition, we demonstrate the existence of hyperbolic flux tubes (HFTs) in both models in vertical cross sections of Q. The main HFT, located under the twisted flux rope in both models, is identified as the most probable site for reconnection. We also show that there are electric current concentrations coinciding with the main QSLs. Finally, we perform torus instability analysis and show that a combination between reconnection at the HFT and the resulting expansion of the flux rope into the torus instability domain is the cause of the CME in both models.
C1 [Savcheva, A.; van Ballegooijen, A.; DeLuca, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Savcheva, A.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Pariat, E.; Aulanier, G.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France.
RP Savcheva, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM savcheva@bu.edu
RI DeLuca, Edward/L-7534-2013;
OI DeLuca, Edward/0000-0001-7416-2895; van Ballegooijen,
Adriaan/0000-0002-5622-3540
FU NASA [NNM07AB07C]
FX Hinode is a Japanese mission developed, launched, and operated by
ISAS/JAXA in partnership with NAOJ, NASA, and STFC (UK). Additional
operational support is provided by ESA, NSC (Norway). This work was
supported by NASA contract NNM07AB07C to SAO. The QSL computations have
been performed on the multi-processors TRU64 computer of the LESIA.
NR 93
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY
PY 2012
VL 750
IS 1
AR 15
DI 10.1088/0004-637X/750/1/15
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929LB
UT WOS:000303063500015
ER
PT J
AU Warren, BH
Bermingham, E
Bourgeois, Y
Estep, LK
Prys-Jones, RP
Strasberg, D
Thebaud, C
AF Warren, Ben H.
Bermingham, Eldredge
Bourgeois, Yann
Estep, Laura K.
Prys-Jones, Robert P.
Strasberg, Dominique
Thebaud, Christophe
TI HYBRIDIZATION AND BARRIERS TO GENE FLOW IN AN ISLAND BIRD RADIATION
SO EVOLUTION
LA English
DT Article
DE Darwin's finches; Foudia; hybridization; incomplete lineage sorting;
Indian Ocean islands; introgression; Madagascar; reproductive isolation;
secondary contact; speciation
ID WESTERN INDIAN-OCEAN; DIVERGENCE POPULATION-GENETICS; DARWINS FINCHES;
POSTZYGOTIC ISOLATION; COMORES ARCHIPELAGO; HYBRID INVIABILITY; SEXUAL
ISOLATION; EVOLUTION; SPECIATION; PATTERNS
AB While reinforcement may play a role in all major modes of speciation, relatively little is known about the timescale over which species hybridize without evolving complete reproductive isolation. Birds have high potential for hybridization, and islands provide simple settings for uncovering speciation and hybridization patterns. Here we develop a phylogenetic hypothesis for a phenotypically diverse radiation of finch-like weaver-birds (Foudia) endemic to the western Indian Ocean islands. We find that unlike Darwin's finches, each island-endemic Foudia population is a monophyletic entity for which speciation can be considered complete. In explaining the only exceptionsmismatches between taxonomy, mitochondrial, and nuclear dataphylogenetic and coalescent methods support introgressive hybridization rather than incomplete lineage sorting. Human introductions of known timing of one island-endemic species, to all surrounding archipelagos provide two fortuitous experiments; (1) population sampling at known times in recent evolutionary history, (2) bringing allopatric lineages of an island radiation into secondary contact. Our results put a minimum time bound on introgression (235 years), and support hybridization between species in natural close contact (parapatry), but not between those in natural allopatry brought into contact by human introduction. Time in allopatry, rather than in sympatry, appears key in the reproductive isolation of Foudia species.
C1 [Warren, Ben H.] Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England.
[Warren, Ben H.; Strasberg, Dominique] Univ La Reunion CIRAD, UMR PVBMT, St Pierre 97410, Reunion.
[Warren, Ben H.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Unit 9100, DPO, AA 34002 USA.
[Warren, Ben H.; Prys-Jones, Robert P.] Nat Hist Museum, Dept Zool, Bird Grp, Tring HP23 6AP, Herts, England.
[Bourgeois, Yann; Thebaud, Christophe] Univ Toulouse 3, Lab Evolut & Diversite Biol, CNRS, UMR 5174, F-31062 Toulouse 9, France.
[Estep, Laura K.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA.
RP Warren, BH (reprint author), Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England.
EM ben.warren@cirad.fr
RI Thebaud, Christophe/N-3916-2016;
OI Thebaud, Christophe/0000-0002-8586-1234; Strasberg,
Dominique/0000-0003-3012-252X
FU CNDRS; CNDRS d'Anjouan; Conservation de la Biodiversite Moheli; DAF-SEF;
MEF Madagascar; MHN La Reunion; MICET; MNPCS; MWF; Nature Seychelles;
SBS; SDOE; SEOR; SIF; Biotechnology and Biological Sciences Research
Council; Biotas [ANR-2006-BDIV002]; Copenhagen Biosystematics Centre;
Entente Cordiale; The Natural History Museum; Pamela Salter Fund;
Smithsonian Molecular Systematics and Evolution Program; Laboratoire
d'Excellence" TULIP [ANR-10-LABX41]
FX We thank M. Gonzalez for help in the laboratory, O. Sanjur for advice,
and all those who loaned samples (see File S1). We further thank Lynx
Edicions for allowing us to reproduce T. Worfolk'sFoudia paintings and
T. Worfolk for painting two additional taxa especially for this
publication. This study would not have been possible without the support
of the following organizations: CNDRS, CNDRS d'Anjouan, Conservation de
la Biodiversite Moheli, DAF-SEF, MEF Madagascar, MHN La Reunion, MICET,
MNPCS, MWF, Nature Seychelles, SBS, SDOE, SEOR, and SIF. We are very
grateful to B. Abderemane, B. Andriamihaja, J. Cousin, N. Jivan Shah, C.
Jones, M. Le Corre, Y. Mungroo, J. Nevill, B. Paris, and A. Sidi for
their support, and to S. Anli, T. Ghestemme, C. Moussa Iboura, R.
Nichols, S. Rasamison, F. Ratrimomanarivo and I. Said for help in the
field. This work was funded by Biotechnology and Biological Sciences
Research Council, Biotas ANR-2006-BDIV002, Copenhagen Biosystematics
Centre, Entente Cordiale, The Natural History Museum, Pamela Salter
Fund, Smithsonian Molecular Systematics and Evolution Program, and the
Laboratoire d'Excellence" TULIP (ANR-10-LABX41). Sequences have been
deposited in Genbank (Accession numbers: JN411136-JN411259).
NR 66
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U1 2
U2 46
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0014-3820
J9 EVOLUTION
JI Evolution
PD MAY
PY 2012
VL 66
IS 5
BP 1490
EP 1505
DI 10.1111/j.1558-5646.2011.01550.x
PG 16
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 929FS
UT WOS:000303047300015
PM 22519786
ER
PT J
AU Karmacharya, B
Hostetler, JA
Conner, LM
Morris, G
Oli, MK
AF Karmacharya, Binab
Hostetler, Jeffrey A.
Conner, L. Mike
Morris, Gail
Oli, Madan K.
TI Longleaf pine management practices and their impact on small mammal
populations
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Capture-mark-recapture (CMR) methods; Longleaf pine management;
Herbicide application; Herbicide-fire combination; Prescribed fire;
Survival rate
ID HISPID COTTON RAT; PRESCRIBED FIRE; PEROMYSCUS-GOSSYPINUS; HABITAT;
FLORIDA; SOUTH; MICE; RESTORATION; ECOSYSTEM; SURVIVAL
AB Rapid decline and degradation of longleaf pine ecosystems in the southeastern United States are conservation concerns. Prescribed fire is the primary management activity in this fire-dependent ecosystem, but prescribed fire is under increasing scrutiny, primarily due to air quality issues. There are concerns that prescribed fire may be removed, or replaced by herbicide, as a forest management tool without adequate understanding of the ecological consequences associated with such a change in management. We conducted a capture-mark-recapture study from April 1999 to April 2002 to examine experimentally the effect of prescribed fire, herbicide application and herbicide-prescribed fire combination on apparent survival rates of cotton mouse (Peromyscus gossypinus) and cotton rat (Sigmodon hispidus) populations. There was no evidence that herbicide application affected survival of cotton mice. Evidence to support effects of prescribed fire and herbicide-fire combination on survival of cotton mice was weak, although apparent monthly survival generally increased after these treatments. There was strong evidence that prescribed fire and herbicide-fire treatments affected survival of cotton rats, but the evidence for the effect of herbicide alone on survival was weak; survival rates declined in response to all three treatments but most strongly in response to the prescribed fire treatment. Fire alone had a stronger effect than an herbicide-fire treatment in both species. Without clear understanding of their ecological impacts, alternatives to prescribed fire should be employed with caution. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Conner, L. Mike; Morris, Gail] Joseph W Jones Ecol Res Ctr, Newton, GA 39870 USA.
[Hostetler, Jeffrey A.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA.
[Karmacharya, Binab; Oli, Madan K.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA.
RP Conner, LM (reprint author), Joseph W Jones Ecol Res Ctr, 3988 Jones Ctr Dr Newton, Newton, GA 39870 USA.
EM binabk@ufl.edu; hostetle@ufl.edu; mconner@jonesctr.org;
gmorris@jonesctr.org; olim@ufl.edu
RI Hostetler, Jeffrey/A-3345-2011
OI Hostetler, Jeffrey/0000-0003-3669-1758
FU Jones Ecological Research Center; Department of Wildlife Ecology and
Conservation, University of Florida; United States Foreign Fulbright
Program Division
FX We thank all the field technicians who were involved in the fieldwork
during the period of this study. Our warmest thanks are extended to M.
Simmons who worked hard for the management of our database. Fieldwork
was funded by Jones Ecological Research Center, and the graduate program
for Binab Karmacharya was supported by the Department of Wildlife
Ecology and Conservation, University of Florida and United States
Foreign Fulbright Program Division.
NR 41
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Z9 2
U1 6
U2 42
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD MAY 1
PY 2012
VL 271
BP 140
EP 146
DI 10.1016/j.foreco.2012.01.031
PG 7
WC Forestry
SC Forestry
GA 928ZE
UT WOS:000303030200017
ER
PT J
AU Liu, HP
Hershler, R
Marn, J
Worsfold, TM
AF Liu, H. -P.
Hershler, R.
Marn, J.
Worsfold, T. M.
TI Microsatellite evidence for tetraploidy in invasive populations of the
New Zealand mudsnail, Potamopyrgus antipodarum (Gray, 1843)
SO JOURNAL OF MOLLUSCAN STUDIES
LA English
DT Editorial Material
ID FRESH-WATER SNAIL; PROSOBRANCHIA; DINUCLEOTIDE; HYDROBIIDAE; MECHANISMS;
PLANTS
C1 [Hershler, R.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Liu, H. -P.; Marn, J.] Metropolitan State Coll, Dept Biol, Denver, CO 80217 USA.
[Worsfold, T. M.] Unicomarine, Diamond Ctr 7, Letchworth SG6 1LW, Herts, England.
RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W 305,MRC 163, Washington, DC 20013 USA.
EM hershlerr@si.edu
NR 28
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U1 1
U2 12
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0260-1230
J9 J MOLLUS STUD
JI J. Molluscan Stud.
PD MAY
PY 2012
VL 78
BP 227
EP 230
DI 10.1093/mollus/eyr055
PN 2
PG 4
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 932ZY
UT WOS:000303330200011
ER
PT J
AU Loss, SR
Niemi, GJ
Blair, RB
AF Loss, Scott R.
Niemi, Gerald J.
Blair, Robert B.
TI Invasions of non-native earthworms related to population declines of
ground-nesting songbirds across a regional extent in northern hardwood
forests of North America
SO LANDSCAPE ECOLOGY
LA English
DT Article
DE Hermit Thrush; Invasive earthworms; Lumbricus; Minnesota, USA; Ovenbird;
Wisconsin, USA
ID HABITAT FRAGMENTATION; INFECTIOUS-DISEASE; BIRD POPULATIONS; PAIRING
SUCCESS; BOREAL FORESTS; MANAGED FOREST; UNITED-STATES; OVENBIRD;
LANDSCAPES; MINNESOTA
AB Non-native invasive earthworms (Lumbricus spp.) substantially change previously earthworm-free hardwood forests of North America by consuming the leaf litter layer, reducing cover and richness of herbaceous plants, and increasing dominance of sedges and grasses. These changes have been associated with reduced density of Ovenbirds (Seiurus aurocapilla) and Hermit Thrushes (Catharus guttatus) in 10-20 ha forest stands, and with reduced Ovenbird nesting success. Whether earthworms reduce songbird populations across a regional extent is unclear. We investigated relationships among Lumbricus, vegetation structure, landscape patterns of forest cover, and density of four ground-nesting songbird species at points scattered across the Chequamegon-Nicolet (Wisconsin) and Chippewa (Minnesota) National Forests, USA. In both national forests, Ovenbird density was significantly lower at invaded points than Lumbricus-free points, but only in sugar maple (Acer saccharum) and sugar maple/basswood (Tilia americana) (hereafter, maple-basswood) woodlands. Density of the Hermit Thrush, Black-and-white Warbler (Mniotilta varia), and Veery (Catharus fuscescens) did not differ in relation to Lumbricus. In maple-basswood forests, Lumbricus biomass was the best predictor of Ovenbird density, with greater biomass associated with reduced density. Vegetation structure and landscape pattern variables received weak support as density predictors. Across all forest types, Ovenbird density was most strongly related to forest cover within 500 and 1,000 m radii. Our results suggest that earthworm invasions may pose a regional threat to Ovenbirds within maple-basswood forests of the U.S. northern Midwest.
C1 [Loss, Scott R.] Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA.
[Loss, Scott R.] Univ Minnesota, Conservat Biol Grad Program, St Paul, MN 55108 USA.
[Niemi, Gerald J.] Univ Minnesota, Nat Resources Res Inst, Dept Biol, Duluth, MN 55812 USA.
[Blair, Robert B.] Univ Minnesota, Dept Fisheries Wildlife & Conservat Biol, St Paul, MN 55108 USA.
RP Loss, SR (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk,Box 37012,MRC 5503, Washington, DC 20013 USA.
EM LossS@si.edu
RI Loss, Scott/B-1504-2014;
OI Blair, Robert/0000-0001-5321-6452
FU American Museum of Natural History; Bell Museum of Natural History;
Dayton-Wilkie Foundation; Explorers Club; Minnesota Ornithologists'
Union; U.S. Department of Agriculture (Chequamegon-Nicolet National
Forest); Wisconsin Society for Ornithology; University of Minnesota;
National Science Foundation [NSF-DGE-0653827]
FX Research was funded by the American Museum of Natural History, Bell
Museum of Natural History, Dayton-Wilkie Foundation, The Explorers Club,
Minnesota Ornithologists' Union, U.S. Department of Agriculture
(Chequamegon-Nicolet National Forest), and Wisconsin Society for
Ornithology. S.R.L. was supported by a University of Minnesota Graduate
School Fellowship and National Science Foundation Interdisciplinary
Graduate Education and Research Traineeship: Risk Analysis for
Introduced Species/Genotypes (NSF-DGE-0653827). We thank C. Hakseth, L.
Raab, and K. Bennett for earthworm sampling assistance, J. Bednar, P.
Dolan-Linne, A. Bracey, J. Bailley, C. Lapin, D. Ostrowski, H. Seeland,
and J. Smith for conducting bird surveys, and A. Grinde for compiling
vegetation and bird data. We thank L.E. Frelich, D.E. Andersen, P.
Bolstad, A. Holdsworth, and C. Hale for guiding the study's development.
Work was conducted with appropriate permits and approval by the
University of Minnesota Institutional Animal Care and Use Committee.
NR 63
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U1 3
U2 53
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0921-2973
J9 LANDSCAPE ECOL
JI Landsc. Ecol.
PD MAY
PY 2012
VL 27
IS 5
BP 683
EP 696
DI 10.1007/s10980-012-9717-4
PG 14
WC Ecology; Geography, Physical; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA 929JC
UT WOS:000303056100006
ER
PT J
AU Gomes, ACS
Luizao, FJ
AF Gomes, Ana C. S.
Luizao, Flavio J.
TI Leaf and Soil Nutrients in a Chronosequence of Second-Growth Forest in
Central Amazonia: Implications for Restoration of Abandoned Lands
SO RESTORATION ECOLOGY
LA English
DT Article
DE Bellucia dichotoma; Cecropia sciadophylla; natural regeneration;
nutrient dynamics; nutrient resorption efficiency; Vismia cayennensis
ID LITTER DECOMPOSITION; SECONDARY FORESTS; TROPICAL FORESTS; EASTERN
AMAZONIA; USE EFFICIENCY; RAIN-FOREST; CARBON; NITROGEN; RESORPTION;
REGENERATION
AB Subsistence agriculture, cattle ranching, and periodical land abandonment are common land-use practices in Amazonia. Because changes in land use affect biogeochemical cycles, secondary forests growing after land abandonment develop at varying speeds and spatial patterns, due in part to varying nutrient dynamics. Leaf and soil nutrient concentrations can provide useful information on nutrient cycling processes and strategies of nutrient use by trees that are suitable for introduction to abandoned areas. To understand nutrient dynamics in secondary forests from different regeneration stages, as well as the importance of pioneer species in the regeneration process, we measured the concentration of macronutrients in leaves of three pioneer tree species (Vismia cayennensis, Cecropia sciadophylla, and Bellucia dichotoma) in central Amazon secondary forests. We also measured macronutrients in the topsoil under the trees. We found that type of prior land use, time since abandonment, and number of fire events were significantly correlated with the concentrations of leaf and soil macronutrients, explaining between 10 and 38% of the variation in macronutrient concentrations. The observed patterns suggest that management practices affect the processes involved in N cycling and availability. Of the three pioneer species, C. sciadophylla showed the highest nutrient resorption efficiency and the highest leaf nutritional quality. We suggest that these two features determine a higher potential of C. sciadophylla for natural regeneration and restoration of abandoned lands.
C1 [Gomes, Ana C. S.; Luizao, Flavio J.] INPA, Dept Ecol CPEC, BR-69011970 Manaus, Amazonas, Brazil.
[Gomes, Ana C. S.] INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil.
[Gomes, Ana C. S.] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil.
RP Gomes, ACS (reprint author), INPA, Dept Ecol CPEC, CP 478, BR-69011970 Manaus, Amazonas, Brazil.
EM anacarlag@gmail.com
FU CNPq/Banco Mundial; Brazilian LTER; CAPES
FX We thank Tania Pimentel and the staff of LTSP/INPA for facilitating
laboratory analysis; Rubenildo Lima (LBA Program) and the Biological
Dynamics of Forest Fragments Project (BDFFP) for assistance with field
logistics; Natan and Osmar for assistance with field work; E.A.
Davidson, A. Vicentini, and G. Ferraz for comments on early versions of
the manuscript; R. J. Burnham for reviewing the English. Research was
funded by the PPG-7 (CNPq/Banco Mundial), the Brazilian LTER Program,
and a grant from CAPES to A.C.S. Gomes. This is publication number 568
in the BDFFP technical series.
NR 38
TC 4
Z9 4
U1 3
U2 46
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1061-2971
EI 1526-100X
J9 RESTOR ECOL
JI Restor. Ecol.
PD MAY
PY 2012
VL 20
IS 3
BP 339
EP 345
DI 10.1111/j.1526-100X.2011.00773.x
PG 7
WC Ecology
SC Environmental Sciences & Ecology
GA 929JB
UT WOS:000303056000009
ER
PT J
AU Eberhard, WG
Wcislo, WT
AF Eberhard, William G.
Wcislo, William T.
TI Plenty of Room at the Bottom? Tiny animals solve problems of housing and
maintaining oversized brains, shedding new light on nervous-system
evolution
SO AMERICAN SCIENTIST
LA English
DT Article
ID MINIATURIZATION; SIZE; CONSEQUENCES; COLEOPTERA; PTILIIDAE; ALLOMETRY;
INSECTS; SPIDERS
C1 [Eberhard, William G.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Eberhard, WG (reprint author), Smithsonian Trop Res Inst, Apartado 0843, Balboa, Panama.
EM william.eberhard@gmail.com
NR 8
TC 7
Z9 7
U1 1
U2 15
PU SIGMA XI-SCI RES SOC
PI RES TRIANGLE PK
PA PO BOX 13975, RES TRIANGLE PK, NC 27709 USA
SN 0003-0996
J9 AM SCI
JI Am. Scientist
PD MAY-JUN
PY 2012
VL 100
IS 3
BP 226
EP 233
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 926MH
UT WOS:000302834600019
ER
PT J
AU Blondin, S
Matheson, T
Kirshner, RP
Mandel, KS
Berlind, P
Calkins, M
Challis, P
Garnavich, PM
Jha, SW
Modjaz, M
Riess, AG
Schmidt, P
AF Blondin, S.
Matheson, T.
Kirshner, R. P.
Mandel, K. S.
Berlind, P.
Calkins, M.
Challis, P.
Garnavich, P. M.
Jha, S. W.
Modjaz, M.
Riess, A. G.
Schmidt, P.
TI THE SPECTROSCOPIC DIVERSITY OF TYPE Ia SUPERNOVAE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE supernovae: general; surveys
ID HIGH-VELOCITY FEATURES; BVRI LIGHT CURVES; NEAR-INFRARED OBSERVATIONS;
DELAYED-DETONATION MODELS; FAILED DEFLAGRATION MODEL; PHOTOMETRY DATA
RELEASE; LOW-LUMINOSITY HOST; LATE-TIME SPECTRA; WHITE-DWARF STAR;
OPTICAL SPECTROSCOPY
AB We present 2603 spectra of 462 nearby Type Ia supernovae (SNe Ia), including 2065 previously unpublished spectra, obtained during 1993-2008 through the Center for Astrophysics Supernova Program. There are on average eight spectra for each of the 313 SNe Ia with at least two spectra. Most of the spectra were obtained with the FAST spectrograph at the Fred Lawrence Whipple Observatory 1.5 m telescope and reduced in a consistent manner, making this data set well suited for studies of SN Ia spectroscopic diversity. Using additional data from the literature, we study the spectroscopic and photometric properties of SNe Ia as a function of spectroscopic class using the classification schemes of Branch et al. and Wang et al. The width-luminosity relation appears to be steeper for SNe Ia with broader lines, although the result is not statistically significant with the present sample. Based on the evolution of the characteristic Si II lambda 6355 line, we propose improved methods for measuring velocity gradients, revealing a larger range than previously suspected, from similar to 0 to similar to 400 km s(-1) day(-1) considering the instantaneous velocity decline rate at maximum light. We find a weaker and less significant correlation between Si II velocity and intrinsic B-V color at maximum light than reported by Foley et al., owing to a more comprehensive treatment of uncertainties and host galaxy dust. We study the extent of nuclear burning and the presence of unburnt carbon in the outermost layers of the ejecta and report new detections of C II lambda 6580 in 23 early-time SN Ia spectra. The frequency of C II detections is not higher in SNe Ia with bluer colors or narrower light curves, in conflict with the recent results of Thomas et al. Based on nebular spectra of 27 SNe Ia, we find no relation between the FWHM of the iron emission feature at similar to 4700 angstrom and Delta m(15)(B) after removing the two low-luminosity SN 1986G and SN 1991bg, suggesting that the peak luminosity is not strongly dependent on the kinetic energy of the explosion for most SNe Ia. Finally, we confirm the correlation of velocity shifts in some nebular lines with the intrinsic B-V color of SNe Ia at maximum light, although several outliers suggest a possible non-monotonic behavior for the largest blueshifts.
C1 [Blondin, S.] Aix Marseille Univ, Ctr Phys Particules Marseille, CNRS, IN2P3, F-13288 Marseille 9, France.
[Matheson, T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Kirshner, R. P.; Mandel, K. S.; Challis, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mandel, K. S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England.
[Berlind, P.; Calkins, M.] FL Whipple Observ, Amado, AZ 85645 USA.
[Garnavich, P. M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Jha, S. W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Modjaz, M.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Riess, A. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Riess, A. G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Schmidt, P.] Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
RP Blondin, S (reprint author), Aix Marseille Univ, Ctr Phys Particules Marseille, CNRS, IN2P3, 163 Ave Luminy, F-13288 Marseille 9, France.
EM blondin@cppm.in2p3.fr
OI Schmidt, Brian/0000-0001-6589-1287
FU NSF [AST 09-07903, AST-0847157]
FX We thank the staffs of the F. L. Whipple, MMT, and Las Campanas
observatories for their extensive assistance and support during this
project, as well as everyone who assisted with observations (see Table
A1). We acknowledge useful discussions with David Branch, Luc Dessart,
Gaston Folatelli, Ryan Foley, Keiichi Maeda, and Xiaofeng Wang.
Additional thanks to Mohan Ganeshalingam, Weidong Li, and Jeff Silverman
from the Berkeley SN Group for sending us tmax(B) values for
six SNe Ia; and to Stephen Bailey from the SNfactory collaboration for
sending us the results of SALT2 fits to five SNe Ia; to Giuseppe
Altavilla, Stefano Benetti, Seppo Mattila, Jesper Sollerman, and Max
Stritzinger, for sending us spectroscopic data. Some of the non-CfA
spectra used in this paper were downloaded from the SUSPECT archive.
Support for supernova research at Harvard University, including the CfA
Supernova Archive, is provided in part by NSF grant AST 09-07903. S.W.J.
is supported at Rutgers University in part by NSF CAREER award
AST-0847157. This research has made use of the NASA/IPAC Extragalactic
Database (NED), which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration.
NR 178
TC 99
Z9 99
U1 2
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD MAY
PY 2012
VL 143
IS 5
AR 126
DI 10.1088/0004-6256/143/5/126
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 928BI
UT WOS:000302954200023
ER
PT J
AU Bonaca, A
Juric, M
Ivezic, Z
Bizyaev, D
Brewington, H
Malanushenko, E
Malanushenko, V
Oravetz, D
Pan, KK
Shelden, A
Simmons, A
Snedden, S
AF Bonaca, Ana
Juric, Mario
Ivezic, Zeljko
Bizyaev, Dmitry
Brewington, Howard
Malanushenko, Elena
Malanushenko, Viktor
Oravetz, Daniel
Pan, Kaike
Shelden, Alaina
Simmons, Audrey
Snedden, Stephanie
TI UPDATE ON THE NATURE OF VIRGO OVERDENSITY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE Galaxy: formation; Galaxy: halo; Galaxy: structure
ID DIGITAL SKY SURVEY; RR-LYRAE STARS; SURVEY COMMISSIONING DATA; MILKY-WAY
TOMOGRAPHY; STELLAR STREAM; SDSS-III; HALO; M31; SAGITTARIUS; ANDROMEDA
AB We use the Eighth Data Release of Sloan Digital Sky Survey catalog with its additional sky coverage of the southern Galactic hemisphere to measure the extent and to study the nature of the Virgo Overdensity (VOD). The data show that the VOD extends over no less than 2000 deg(2), with its true extent likely closer to 3000 deg(2). We test whether the VOD can be attributed to a tilt in the stellar halo ellipsoid with respect to the plane of the Galactic disk and find that the observed symmetry of the north-south Galactic hemisphere star counts excludes this possibility. We argue that the Virgo Overdensity, in spite of its wide area and cloud-like appearance, is still best explained by a minor merger. Its appearance and position are qualitatively similar to a near perigalacticon merger event and, assuming that the VOD and the Virgo Stellar Stream (VSS) share the same progenitor, consistent with the VSS orbit determined by Casetti-Dinescu et al.
C1 [Bonaca, Ana] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Bonaca, Ana] Univ Zagreb, Fac Sci, Dept Phys, Zagreb 41000, Croatia.
[Juric, Mario] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Ivezic, Zeljko] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Bizyaev, Dmitry; Brewington, Howard; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Shelden, Alaina; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA.
RP Bonaca, A (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
EM ana.bonaca@yale.edu; mjuric@cfa.harvard.edu
FU NASA [HST-HF-51255.01-A, NAS 5-26555]; Space Telescope Science
Institute; Alfred P. Sloan Foundation; National Science Foundation; US
Department of Energy; University of Arizona; SDSS-III Collaboration;
Brazilian Participation Group; Brookhaven National Laboratory;
University of Cambridge; University of Florida; French Participation
Group; German Participation Group; Instituto de Astrofisica de Canarias;
Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins
University; Lawrence Berkeley National Laboratory; Max Planck Institute
for Astrophysics; 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 The authors wish to thank Marla Geha, Dana Casetti, and Nhung Ho for
reading the early versions of the manuscript and providing thoughtful
comments, and Branimir Sesar for help with accessing the SDSS data. M.J.
gratefully acknowledges support by NASA through Hubble Fellowship grant
HST-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 contract NAS 5-26555.; Funding for
SDSS-III has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, and the US
Department of Energy. The SDSS-III Web site is http://www.sdss3.org/.;
SDSS-III is managed by the Astrophysical Research Consortium for the
Participating Institutions of the SDSS-III Collaboration including the
University of Arizona, the Brazilian Participation Group, Brookhaven
National Laboratory, University of Cambridge, University of Florida, the
French Participation Group, the German Participation Group, 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, 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 41
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Z9 15
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 MAY
PY 2012
VL 143
IS 5
AR 105
DI 10.1088/0004-6256/143/5/105
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 928BI
UT WOS:000302954200002
ER
PT J
AU Boyer, ML
Srinivasan, S
van Loon, JT
McDonald, I
Meixner, M
Zaritsky, D
Gordon, KD
Kemper, F
Babler, B
Block, M
Bracker, S
Engelbracht, CW
Hora, J
Indebetouw, R
Meade, M
Misselt, K
Robitaille, T
Sewillo, M
Shiao, B
Whitney, B
AF Boyer, Martha L.
Srinivasan, Sundar
van Loon, Jacco Th.
McDonald, Iain
Meixner, Margaret
Zaritsky, Dennis
Gordon, Karl D.
Kemper, F.
Babler, Brian
Block, Miwa
Bracker, Steve
Engelbracht, Charles W.
Hora, Joe
Indebetouw, Remy
Meade, Marilyn
Misselt, Karl
Robitaille, Thomas
Sewillo, Marta
Shiao, Bernie
Whitney, Barbara
TI SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED,
LOW-METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). II. COOL EVOLVED
STARS (vol 142, pg 103, 2011)
SO ASTRONOMICAL JOURNAL
LA English
DT Correction
C1 [Boyer, Martha L.; Meixner, Margaret; Gordon, Karl D.; Shiao, Bernie] STScI, Baltimore, MD 21218 USA.
[Srinivasan, Sundar] CNRS, Inst Astrophys Paris, UPR 341, F-75014 Paris, France.
[van Loon, Jacco Th.] Keele Univ, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[McDonald, Iain; Kemper, F.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Zaritsky, Dennis; Block, Miwa; Engelbracht, Charles W.; Misselt, Karl] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Babler, Brian; Bracker, Steve; Meade, Marilyn; Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Hora, Joe; Robitaille, Thomas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Sewillo, Marta] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Boyer, ML (reprint author), STScI, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM mboyer@stsci.edu
RI Kemper, Francisca/D-8688-2011
OI Kemper, Francisca/0000-0003-2743-8240
NR 1
TC 0
Z9 0
U1 0
U2 5
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 MAY
PY 2012
VL 143
IS 5
AR 127
DI 10.1088/0004-6256/143/5/127
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 928BI
UT WOS:000302954200024
ER
PT J
AU Foley, RJ
Filippenko, AV
Kessler, R
Bassett, B
Frieman, JA
Garnavich, PM
Jha, SW
Konishi, K
Lampeitl, H
Riess, AG
Sako, M
Schneider, DP
Sollerman, J
Smith, M
AF Foley, Ryan J.
Filippenko, Alexei V.
Kessler, Richard
Bassett, Bruce
Frieman, Joshua A.
Garnavich, Peter M.
Jha, Saurabh W.
Konishi, Kohki
Lampeitl, Hubert
Riess, Adam G.
Sako, Masao
Schneider, Donald P.
Sollerman, Jesper
Smith, Mathew
TI A MISMATCH IN THE ULTRAVIOLET SPECTRA BETWEEN LOW-REDSHIFT AND
INTERMEDIATE-REDSHIFT TYPE Ia SUPERNOVAE AS A POSSIBLE SYSTEMATIC
UNCERTAINTY FOR SUPERNOVA COSMOLOGY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE cosmology: observations; distance scale; supernovae: general
ID DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; BVRI LIGHT CURVES;
PHOTOMETRY DATA RELEASE; DARK ENERGY; OPTICAL PHOTOMETRY; STANDARD
STARS; HOST GALAXIES; LEGACY SURVEY; K-CORRECTIONS
AB We present Keck high-quality rest-frame ultraviolet (UV) through optical spectra of 21 Type Ia supernovae (SNe Ia) in the redshift range 0.11 <= z <= 0.37 and a mean redshift of 0.22 that were discovered during the Sloan Digital Sky Survey-II (SDSS-II) SN Survey. Using the broadband photometry of the SDSS survey, we are able to reconstruct the SN host-galaxy spectral energy distributions (SEDs), allowing for a correction for the host-galaxy contamination in the SN Ia spectra. Comparison of composite spectra constructed from a subsample of 17 high-quality spectra to those created from a low-redshift sample with otherwise similar properties shows that the Keck/SDSS SNe Ia have, on average, extremely similar rest-frame optical spectra but show a UV flux excess. This observation is confirmed by comparing synthesized broadband colors of the individual spectra, showing a difference in mean colors at the 2.4 sigma-4.4 sigma level for various UV colors. We further see a slight difference in the UV spectral shape between SNe with low-mass and high-mass host galaxies. Additionally, we detect a relationship between the flux ratio at 2770 and 2900 angstrom and peak luminosity that differs from that observed at low redshift. We find that changing the UV SED of an SN Ia within the observed dispersion can change the inferred distance moduli by similar to 0.1 mag. This effect only occurs when the data probe the rest-frame UV. We suggest that this discrepancy could be due to differences in the host-galaxy population of the two SN samples or to small-sample statistics.
C1 [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Foley, Ryan J.; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kessler, Richard; Frieman, Joshua A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Kessler, Richard; Frieman, Joshua A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Bassett, Bruce; Smith, Mathew] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Rondebosch, South Africa.
[Bassett, Bruce] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Bassett, Bruce] African Inst Math Sci, Cape Town, South Africa.
[Frieman, Joshua A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Konishi, Kohki] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Lampeitl, Hubert] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 2EG, Hants, England.
[Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Riess, Adam G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Sollerman, Jesper] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rfoley@cfa.harvard.edu
OI Bassett, Bruce/0000-0001-7700-1069; Sollerman,
Jesper/0000-0003-1546-6615
FU Clay Fellowship; W. M. Keck Foundation; NSF [AST-0443378, AST-0507475,
AST-0607485, AST-0908886, AST-0847157]; U.S. Department of Energy (DOE)
[DE-FG02-08ER41562]; NASA/HST from the Space Telescope Science Institute
[GO-10182]; NASA [NAS5-26555]; Alfred P. Sloan Foundation; DOE; 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 R.J.F. is supported by a Clay Fellowship.; The SDSS-II SN team supplied
targets, photometry, and light-curve fits for this project; in
particular, G. Miknaitis provided some of the necessary data and
discussions. We thank J. M. Silverman for help with some of the
observations, and R. Chornock for useful discussions and for performing
additional spectral reductions of several objects. We are grateful to M.
Blanton for discussions about the kcorrect software and J. Bloom for
insightful comments on an early draft of this work. We thank the
referee, M. Stritzinger, for helpful comments. The spectra of
intermediate-redshift SNe in this study 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 (NASA); the
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. The spectra of low-redshift SNe in this study
were obtained with the 3 m Shane telescope at Lick Observatory, which is
owned and operated by the University of California. We thank the Keck
and Lick staffs for their assistance with the observations.; A.V.F. is
grateful for the hospitality of the Aspen Center for Physics, where this
paper was finalized during the 2012 January program on "The Physics of
Astronomical Transients." This research was made possible by NSF Grants
AST-0443378, AST-0507475, AST-0607485, and AST-0908886, as well as by
NSF CAREER award AST-0847157 to S.W.J. at Rutgers University. Additional
support was provided by U.S. Department of Energy (DOE) Grant
DE-FG02-08ER41562 and by the TABASGO Foundation. We also acknowledge
funding from NASA/HST Grant GO-10182 from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA Contract NAS5-26555.; Funding
for the SDSS and SDSS-II has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, NSF, DOE, NASA, the Japanese
Monbukagakusho, the Max Planck Society, and the Higher Education Funding
Council for England. The SDSS Web Site is http://www.sdss.org/.; The
SDSS is managed by the Astrophysical Research Consortium for the
Participating Institutions. The Participating Institutions are the
American Museum of Natural History, Astrophysical Institute Potsdam,
University of Basel, University of Cambridge, Case Western Reserve
University, University of Chicago, Drexel University, Fermilab, the
Institute for Advanced Study, the Japan Participation Group, Johns
Hopkins University, the Joint Institute for Nuclear Astrophysics, the
Kavli Institute for Particle Astrophysics and Cosmology, the Korean
Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, Ohio State University, University of Pittsburgh, University
of Portsmouth, Princeton University, the United States Naval
Observatory, and the University of Washington.
NR 92
TC 23
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAY
PY 2012
VL 143
IS 5
AR 113
DI 10.1088/0004-6256/143/5/113
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 928BI
UT WOS:000302954200010
ER
PT J
AU Melbourne, J
Soifer, BT
Desai, V
Pope, A
Armus, L
Dey, A
Bussmann, RS
Jannuzi, BT
Alberts, S
AF Melbourne, J.
Soifer, B. T.
Desai, Vandana
Pope, Alexandra
Armus, Lee
Dey, Arjun
Bussmann, R. S.
Jannuzi, B. T.
Alberts, Stacey
TI THE SPECTRAL ENERGY DISTRIBUTIONS AND INFRARED LUMINOSITIES OF z
approximate to 2 DUST-OBSCURED GALAXIES FROM Herschel AND Spitzer
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: high-redshift; galaxies: starburst; infrared: galaxies;
submillimeter: galaxies
ID SUBMILLIMETER-SELECTED GALAXIES; SPACE-TELESCOPE MORPHOLOGIES; ACTIVE
GALACTIC NUCLEUS; KECK ADAPTIVE OPTICS; ARRAY CAMERA IRAC; WIDE-FIELD
SURVEY; MU-M OBSERVATIONS; STAR-FORMATION; HIGH-REDSHIFT; ULTRALUMINOUS
GALAXIES
AB Dust-obscured galaxies (DOGs) are a subset of high-redshift (z approximate to 2) optically-faint ultra-luminous infrared galaxies (ULIRGs, e. g., L-IR > 10(12) L-circle dot). We present new far-infrared photometry, at 250, 350, and 500 mu m(observed-frame), from the Herschel Space Telescope for a large sample of 113 DOGs with spectroscopically measured redshifts. Approximately 60% of the sample are detected in the far-IR. The Herschel photometry allows the first robust determinations of the total infrared luminosities of a large sample of DOGs, confirming their high IR luminosities, which range from 10(11.6) L-circle dot < L-IR(8-1000 mu m) < 10(13.6) L-circle dot. 90% of the Herschel-detected DOGs in this sample are ULIRGs and 30% have L-IR > 10(13) L-circle dot. The rest-frame near-IR (1-3 mu m) spectral energy distributions (SEDs) of the Herschel-detected DOGs are predictors of their SEDs at longer wavelengths. DOGs with "power-law" SEDs in the rest-frame near-IR show observed-frame 250/24 mu m flux density ratios similar to the QSO-like local ULIRG, Mrk 231. DOGs with a stellar "bump" in their rest-frame near-IR show observed-frame 250/24 mu m flux density ratios similar to local star-bursting ULIRGs like NGC 6240. None show 250/24 mu m flux density ratios similar to extreme local ULIRG, Arp 220; though three show 350/24 mu m flux density ratios similar to Arp 220. For the Herschel-detected DOGs, accurate estimates (within similar to 25%) of total IR luminosity can be predicted from their rest-frame mid-IR data alone (e. g., from Spitzer observed-frame 24 mu m luminosities). Herschel-detected DOGs tend to have a high ratio of infrared luminosity to rest-frame 8 mu m luminosity (the IR8 = L-IR(8-1000 mu m)/nu L-nu (8 mu m) parameter of Elbaz et al.). Instead of lying on the z = 1-2 "infrared main sequence" of star-forming galaxies (like typical LIRGs and ULIRGs at those epochs) the DOGs, especially large fractions of the bump sources, tend to lie in the starburst sequence. While, Herschel-detected DOGs are similar to scaled up versions of local ULIRGs in terms of 250/24 mu m flux density ratio, and IR8, they tend to have cooler far-IR dust temperatures (20-40K for DOGs versus 40-50K for local ULIRGs) as measured by the rest-frame 80/115 mu m flux density ratios (e. g., observed-frame 250/350 mu m ratios at z = 2). DOGs that are not detected by Herschel appear to have lower observed-frame 250/24 mu m ratios than the detected sample, either because of warmer dust temperatures, lower IR luminosities, or both.
C1 [Melbourne, J.; Soifer, B. T.] CALTECH, Div Phys Math & Astron, Caltech Opt Observ, Pasadena, CA 91125 USA.
[Soifer, B. T.; Desai, Vandana; Armus, Lee] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Pope, Alexandra; Alberts, Stacey] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Dey, Arjun; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Melbourne, J (reprint author), CALTECH, Div Phys Math & Astron, Caltech Opt Observ, Mail Stop 320-47, Pasadena, CA 91125 USA.
EM jmel@caltech.edu; bts@submm.caltech.edu; vandesai@gmail.com;
pope@astro.umass.edu; lee@ipac.caltech.edu; dey@noao.edu;
rbussmann@cfa.harvard.edu; jannuzi@noao.edu; bts@ipac.caltech.edu
FU NOAO; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA
(USA)
FX This work is based (in part) on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. We
acknowledge the MIPS GTO team for producing the Spitzer 24 mu m imaging
and source catalogs of the Bootes field. SPIRE has been developed by a
consortium of institutes led by Cardiff University (UK) and including
Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ.
Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial
College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech,
JPL, NHSC, Univ. Colorado (USA). This development has been supported by
national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA
(USA). We also acknowledge the HerMES collaboration for providing this
excellent data set across the Bootes field. The US Herschel Science
Center also provided a workshop on SPIRE image reduction and photometry
that was very valuable for our understanding of the data. The research
activities of A. D. and B.T.J. 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.
NR 75
TC 29
Z9 29
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD MAY
PY 2012
VL 143
IS 5
AR 125
DI 10.1088/0004-6256/143/5/125
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 928BI
UT WOS:000302954200022
ER
PT J
AU Caputi, KI
Dunlop, JS
McLure, RJ
Huang, JS
Fazio, GG
Ashby, MLN
Castellano, M
Fontana, A
Cirasuolo, M
Almaini, O
Bell, EF
Dickinson, M
Donley, JL
Faber, SM
Ferguson, HC
Giavalisco, M
Grogin, NA
Kocevski, DD
Koekemoer, AM
Koo, DC
Lai, K
Newman, JA
Somerville, RS
AF Caputi, K. I.
Dunlop, J. S.
McLure, R. J.
Huang, J. -S.
Fazio, G. G.
Ashby, M. L. N.
Castellano, M.
Fontana, A.
Cirasuolo, M.
Almaini, O.
Bell, E. F.
Dickinson, M.
Donley, J. L.
Faber, S. M.
Ferguson, H. C.
Giavalisco, M.
Grogin, N. A.
Kocevski, D. D.
Koekemoer, A. M.
Koo, D. C.
Lai, K.
Newman, J. A.
Somerville, R. S.
TI THE NATURE OF EXTREMELY RED H - [4.5] > 4 GALAXIES REVEALED WITH SEDS
AND CANDELS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; infrared: galaxies
ID EXTRAGALACTIC LEGACY SURVEY; SPITZER-SPACE-TELESCOPE; HIGH-REDSHIFT
QUASARS; MASSIVE GALAXIES; SIGNIFICANT POPULATION; MIDINFRARED
SELECTION; LUMINOSITY FUNCTION; STELLAR MASS; DEEP SURVEY; DUST
AB We have analyzed a sample of 25 extremely red H - [4.5] > 4 galaxies, selected using 4.5 mu m data from the Spitzer SEDS survey and deep H-band data from the Hubble Space Telescope CANDELS survey, over similar to 180 arcmin(2) of the UKIDSS Ultra-Deep Survey field. Our aim is to investigate the nature of this rare population of mid-infrared (mid-IR) sources that display such extreme near-to-mid-IR colors. Using up to 17-band photometry (U through 8.0 mu m), we have studied in detail their spectral energy distributions, including possible degeneracies in the photometric redshift/internal extinction (z(phot)-A(V)) plane. Our sample appears to include sources of very different nature. Between 45% and 75% of them are dust-obscured, massive galaxies at 3 < z(phot) < 5. All of the 24 mu m detected sources in our sample are in this category. Two of these have S(24 mu m) > 300 mu Jy, which at 3 < z(phot) < 5 suggests that they probably host a dust-obscured active galactic nucleus. Our sample also contains four highly obscured (A(V) > 5) sources at z(phot) < 1. Finally, we analyze in detail two z(phot) similar to 6 galaxy candidates, and discuss their plausibility and implications. Overall, our red galaxy sample contains the tip of the iceberg of a larger population of z > 3 galaxies to be discovered with the future James Webb Space Telescope.
C1 [Caputi, K. I.; Dunlop, J. S.; McLure, R. J.; Cirasuolo, M.] Univ Edinburgh, SUPA, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Huang, J. -S.; Fazio, G. G.; Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Castellano, M.; Fontana, A.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Cirasuolo, M.] Royal Observ, Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Almaini, O.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Bell, E. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Donley, J. L.; Ferguson, H. C.; Grogin, N. A.; Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Faber, S. M.; Kocevski, D. D.; Koo, D. C.; Lai, K.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Newman, J. A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Newman, J. A.] Univ Pittsburgh, PITT PAC, Pittsburgh, PA 15260 USA.
[Somerville, R. S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
RP Caputi, KI (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
EM karina@astro.rug.nl
OI Koekemoer, Anton/0000-0002-6610-2048; fontana,
adriano/0000-0003-3820-2823; Bell, Eric/0000-0002-5564-9873
NR 38
TC 17
Z9 17
U1 0
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 MAY 1
PY 2012
VL 750
IS 1
AR L20
DI 10.1088/2041-8205/750/1/L20
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929CV
UT WOS:000303039700020
ER
PT J
AU Chandra, P
Chevalier, RA
Irwin, CM
Chugai, N
Fransson, C
Soderberg, AM
AF Chandra, Poonam
Chevalier, Roger A.
Irwin, Christopher M.
Chugai, Nikolai
Fransson, Claes
Soderberg, Alicia M.
TI STRONG EVOLUTION OF X-RAY ABSORPTION IN THE TYPE IIn SUPERNOVA SN 2010jl
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; hydrodynamics; supernovae: general; supernovae:
individual (SN 2010jl); X-rays: general
ID EMISSION; SPECTRA; PLASMAS; LINES; DUST
AB We report two epochs of Chandra-ACIS X-ray imaging spectroscopy of the nearby bright Type IIn supernova SN 2010jl, taken around two months and then a year after the explosion. The majority of the X-ray emission in both spectra is characterized by a high temperature (greater than or similar to 10 keV) and is likely to be from the forward shocked region resulting from circumstellar interaction. The absorption column density in the first spectrum is high (similar to 10(24) cm(-2)), more than three orders of magnitude higher than the Galactic absorption column, and we attribute it to absorption by circumstellar matter. In the second epoch observation, the column density has decreased by a factor of three, as expected for shock propagation in the circumstellar medium. The unabsorbed 0.2-10 keV luminosity at both epochs is similar to 7 x 10(41) erg s(-1). The 6.4 keV Fe line clearly present in the first spectrum is not detected in the second spectrum. The strength of the fluorescent line is roughly that expected for the column density of circumstellar gas, provided the Fe is not highly ionized. There is also evidence for an absorbed power-law component in both spectra, which we attribute to a background ultraluminous X-ray source.
C1 [Chandra, Poonam] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada.
[Chevalier, Roger A.; Irwin, Christopher M.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Chugai, Nikolai] Russian Acad Sci, Inst Astron, Moscow 109017, Russia.
[Fransson, Claes] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Soderberg, Alicia M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Chandra, P (reprint author), Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada.
EM Poonam.Chandra@rmc.ca
FU NASA through Chandra X-ray Observatory Center [GO0-211080X, GO2-13082X,
NAS8-03060]
FX We are grateful to the referee for useful comments. Support for this
work was provided by NASA through Chandra Awards GO0-211080X and
GO2-13082X 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.
NR 20
TC 22
Z9 22
U1 0
U2 1
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 MAY 1
PY 2012
VL 750
IS 1
AR L2
DI 10.1088/2041-8205/750/1/L2
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929CV
UT WOS:000303039700002
ER
PT J
AU Owers, MS
Couch, WJ
Nulsen, PEJ
Randall, SW
AF Owers, Matt S.
Couch, Warrick J.
Nulsen, Paul E. J.
Randall, Scott W.
TI SHOCKING TAILS IN THE MAJOR MERGER ABELL 2744
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: clusters: individual (Abell 2744); X-rays: galaxies: clusters
ID GALAXY REDSHIFT SURVEY; ULTRA DEEP FIELD; STAR-FORMATION; RAM-PRESSURE;
STARBURST GALAXIES; COMA CLUSTER; INTRACLUSTER MEDIUM; TADPOLE GALAXIES;
MERGING CLUSTERS; SPIRAL GALAXIES
AB We identify four rare "jellyfish" galaxies in Hubble Space Telescope imagery of the major merger cluster Abell 2744. These galaxies harbor trails of star-forming knots and filaments which have formed in situ in gas tails stripped from the parent galaxies, indicating they are in the process of being transformed by the environment. Further evidence for rapid transformation in these galaxies comes from their optical spectra, which reveal starburst, poststarburst, and active galactic nucleus features. Most intriguingly, three of the jellyfish galaxies lie near intracluster medium features associated with a merging "Bullet-like" subcluster and its shock front detected in Chandra X-ray images. We suggest that the high-pressure merger environment may be responsible for the star formation in the gaseous tails. This provides observational evidence for the rapid transformation of galaxies during the violent core passage phase of a major cluster merger.
C1 [Owers, Matt S.; Couch, Warrick J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Owers, Matt S.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Nulsen, Paul E. J.; Randall, Scott W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Owers, MS (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
EM mowers@aao.gov.au
OI Randall, Scott/0000-0002-3984-4337; Owers, Matt/0000-0002-2879-1663
FU Australian Research Council; NASA [NAS8-03060]
FX We thank the referee, Curtis Struck, for his helpful comments. M.S.O.
and W.J.C. acknowledge the financial support of the Australian Research
Council. P.E.J.N. was partly supported by NASA grant NAS8-03060.
NR 49
TC 30
Z9 30
U1 0
U2 1
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 MAY 1
PY 2012
VL 750
IS 1
AR L23
DI 10.1088/2041-8205/750/1/L23
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929CV
UT WOS:000303039700023
ER
PT J
AU Testa, P
Reale, F
AF Testa, Paola
Reale, Fabio
TI HINODE/EIS SPECTROSCOPIC VALIDATION OF VERY HOT PLASMA IMAGED WITH THE
SOLAR DYNAMICS OBSERVATORY IN NON-FLARING ACTIVE REGION CORES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: UV radiation; Sun: X-rays, gamma rays;
techniques: imaging spectroscopy
ID ULTRAVIOLET IMAGING SPECTROMETER; EMISSION-LINES; RAY TELESCOPE;
FUNDAMENTAL LIMITATIONS; TEMPERATURE STRUCTURE; LOOPS OBSERVATIONS;
DENSITY STRUCTURE; ATOMIC DATABASE; CORONAL LOOPS; SPECTRA
AB We use coronal imaging observations with the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA), and Hinode/Extreme-ultraviolet Imaging Spectrometer (EIS) spectral data to explore the potential of narrowband EUV imaging data for diagnosing the presence of hot (T greater than or similar to 5 MK) coronal plasma in active regions. We analyze observations of two active regions (AR 11281, AR 11289) with simultaneous AIA imaging and EIS spectral data, including the Ca XVII line (at 192.8 angstrom), which is one of the few lines in the EIS spectral bands sensitive to hot coronal plasma even outside flares. After careful co-alignment of the imaging and spectral data, we compare the morphology in a three-color image combining the 171, 335, and 94 angstrom AIA spectral bands, with the image obtained for Ca XVII emission from the analysis of EIS spectra. We find that in the selected active regions the Ca XVII emission is strong only in very limited areas, showing striking similarities with the features bright in the 94 angstrom (and 335 angstrom) AIA channels and weak in the 171 angstrom band. We conclude that AIA imaging observations of the solar corona can be used to track hot plasma (6-8 MK), and so to study its spatial variability and temporal evolution at high spatial and temporal resolution.
C1 [Testa, Paola] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Reale, Fabio] Univ Palermo, Dipartimento Fis, I-90134 Palermo, Italy.
[Reale, Fabio] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy.
RP Testa, P (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 58, Cambridge, MA 02138 USA.
EM ptesta@cfa.harvard.edu
OI Reale, Fabio/0000-0002-1820-4824
FU Lockheed-Martin [SP02H1701R]; NASA [NNM07AB07C, NNX10AF29G, 3001762433];
Italian Ministero dell'Universita e Ricerca and Agenzia Spaziale
Italiana (ASI) [ASI/INAFI/023/09/0]
FX We thank H. Warren for providing fitting routines for the EIS analysis,
not included in the SolarSoft package. P.T. was supported by contract
SP02H1701R from Lockheed-Martin, NASA contract NNM07AB07C to the
Smithsonian Astrophysical Observatory, and NASA grants NNX10AF29G and
3001762433. F.R. acknowledges support from Italian Ministero
dell'Universita e Ricerca and Agenzia Spaziale Italiana (ASI) contract
ASI/INAFI/023/09/0 "Attivita scientifica per l'analisi dati Sole e
plasma - Fase E2/F." Hinode is a Japanese mission developed and launched
by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as
international partners. It is operated by these agencies in co-operation
with ESA and the NSC (Norway).
NR 32
TC 34
Z9 34
U1 0
U2 1
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 MAY 1
PY 2012
VL 750
IS 1
AR L10
DI 10.1088/2041-8205/750/1/L10
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 929CV
UT WOS:000303039700010
ER
PT J
AU Dunbar, J
Eichorst, SA
Gallegos-Graves, L
Silva, S
Xie, G
Hengartner, NW
Evans, RD
Hungate, BA
Jackson, RB
Megonigal, JP
Schadt, CW
Vilgalys, R
Zak, DR
Kuske, CR
AF Dunbar, John
Eichorst, Stephanie A.
Gallegos-Graves, La Verne
Silva, Shannon
Xie, Gary
Hengartner, N. W.
Evans, R. David
Hungate, Bruce A.
Jackson, Robert B.
Megonigal, J. Patrick
Schadt, Christopher W.
Vilgalys, Rytas
Zak, Donald R.
Kuske, Cheryl R.
TI Common bacterial responses in six ecosystems exposed to 10 years of
elevated atmospheric carbon dioxide
SO ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID MICROBIAL COMMUNITY STRUCTURE; NET NITROGEN MINERALIZATION;
SPECIES-SPECIFIC RESPONSES; CO2 ENRICHMENT FACE; SOIL ORGANIC-MATTER;
LITTER QUALITY; LEAF-LITTER; PHYLUM ACIDOBACTERIA; POPLAR PLANTATION;
DECIDUOUS FOREST
AB Six terrestrial ecosystems in the USA were exposed to elevated atmospheric CO2 in single or multifactorial experiments for more than a decade to assess potential impacts. We retrospectively assessed soil bacterial community responses in all six-field experiments and found ecosystem-specific and common patterns of soil bacterial community response to elevated CO2. Soil bacterial composition differed greatly across the six ecosystems. No common effect of elevated atmospheric CO2 on bacterial biomass, richness and community composition across all of the ecosystems was identified, although significant responses were detected in individual ecosystems. The most striking common trend across the sites was a decrease of up to 3.5-fold in the relative abundance of Acidobacteria Group 1 bacteria in soils exposed to elevated CO2 or other climate factors. The Acidobacteria Group 1 response observed in exploratory 16S rRNA gene clone library surveys was validated in one ecosystem by 100-fold deeper sequencing and semi-quantitative PCR assays. Collectively, the 16S rRNA gene sequencing approach revealed influences of elevated CO2 on multiple ecosystems. Although few common trends across the ecosystems were detected in the small surveys, the trends may be harbingers of more substantive changes in less abundant, more sensitive taxa that can only be detected by deeper surveys.
C1 [Dunbar, John; Eichorst, Stephanie A.; Gallegos-Graves, La Verne; Silva, Shannon; Xie, Gary; Kuske, Cheryl R.] Los Alamos Natl Lab, Biosci Div, Los Alamos, NM 87545 USA.
[Hengartner, N. W.] Los Alamos Natl Lab, Comp Computat & Stat Sci Div, Los Alamos, NM USA.
[Evans, R. David] Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA.
[Hungate, Bruce A.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA.
[Hungate, Bruce A.] No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA.
[Jackson, Robert B.] Duke Univ, Dept Biol, Durham, NC 27708 USA.
[Jackson, Robert B.; Vilgalys, Rytas] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Washington, DC 20013 USA.
[Schadt, Christopher W.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA.
[Zak, Donald R.] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA.
[Zak, Donald R.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA.
RP Kuske, CR (reprint author), Los Alamos Natl Lab, Biosci Div, Los Alamos, NM 87545 USA.
EM kuske@lanl.gov
RI Hungate, Bruce/F-8991-2011; Schadt, Christopher/B-7143-2008; Eichorst,
Stephanie A/A-1079-2017;
OI Hungate, Bruce/0000-0002-7337-1887; Schadt,
Christopher/0000-0001-8759-2448; Eichorst, Stephanie
A/0000-0002-9017-7461; xie, gary/0000-0002-9176-924X; Vilgalys,
Rytas/0000-0001-8299-3605
FU U.S. Department of Energy (DOE), Office of Science, Biological and
Environmental Research [2009LANLF260]
FX This work was supported by the U.S. Department of Energy (DOE), Office
of Science, Biological and Environmental Research Program, through a
Science Focus Area grant to C. R. K. and J. M. D. (2009LANLF260). Sanger
and 454 titanium pyrosequencing were conducted by the U. S. DOE Joint
Genome Institute. The six elevated CO2 research sites in this study were
supported by the U. S. DOE Office of Science, Biological and
Environmental Research Program. The authors thank Yvonne Rogers and
Shannon Johnson for their technical assistance, Lawrence Ticknor for
statistics consultation, and many people at the six field sites for site
access and technical support.
NR 85
TC 34
Z9 35
U1 2
U2 69
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1462-2912
J9 ENVIRON MICROBIOL
JI Environ. Microbiol.
PD MAY
PY 2012
VL 14
IS 5
BP 1145
EP 1158
DI 10.1111/j.1462-2920.2011.02695.x
PG 14
WC Microbiology
SC Microbiology
GA 927TW
UT WOS:000302934000004
PM 22264231
ER
PT J
AU Dew, RM
Rehan, SM
Tierney, SM
Chenoweth, LB
Schwarz, MP
AF Dew, R. M.
Rehan, S. M.
Tierney, S. M.
Chenoweth, L. B.
Schwarz, M. P.
TI A single origin of large colony size in allodapine bees suggests a
threshold event among 50 million years of evolutionary tinkering
SO INSECTES SOCIAUX
LA English
DT Article
DE Eusociality; Morphological castes; Social evolution; Allodapini; Bees
ID SOCIAL EVOLUTION; MOLECULAR PHYLOGENETICS; HYMENOPTERA; APIDAE;
AUSTRALIA
AB Evolutionary origins of highly eusocial organization involving morphological castes have been very rare, yet these origins have often led to enormous diversification and ecological success. This suggests that once an apparently severe selective barrier to highly eusocial behaviour is overcome, major new adaptive landscapes open up. One would therefore expect a discontinuity in patterns of evolutionary change across this barrier. However, we do not know if highly eusocial organization has evolved incrementally from less complex societies, or if it has involved some kind of evolutionary leap. Our study examines this issue using colony size data from 33 allodapine bee species, with a crown age of ca. 47 Mya. Our species cover all major allodapine clades, and include Exoneurella tridentata, the only known allodapine with morphologically discrete castes. Phylogenetic analyses indicate a strong effect of phylogeny on the evolution of maximum brood size, but the effect of phylogeny on maximum colony size (number of adults) depends on whether E. tridentata is excluded or included in analyses. We found no evidence of punctuational change in maximum colony or brood sizes over the phylogeny as a whole, but colony and brood sizes in E. tridentata fall well beyond variation among the other allodapines. Colony size in E. tridentata therefore represents an evolutionary outcome that does not fit within the kinds of incremental changes found in other allodapines. We propose that E. tridentata indicates the crossing of an important threshold, and this has entailed some very unusual ecological circumstances.
C1 [Rehan, S. M.] Brock Univ, Dept Biol Sci, St Catharines, ON L2S 3A1, Canada.
[Dew, R. M.; Rehan, S. M.; Chenoweth, L. B.; Schwarz, M. P.] Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA, Australia.
[Tierney, S. M.] Smithsonian Trop Res Inst, Balboa 084303092, Panama.
RP Rehan, SM (reprint author), Brock Univ, Dept Biol Sci, Glenridge Ave, St Catharines, ON L2S 3A1, Canada.
EM rebecca.rmd@hotmail.com; sandra.rehan@gmail.com; tierneys@si.edu;
luke.chenoweth@flinders.edu.au; michael.schwarz@flinders.edu.au
RI Tierney, Simon/H-2410-2015
OI Tierney, Simon/0000-0002-8812-6753
FU Schwarz lab; Australian Research Council; Natural Sciences and
Engineering Research Council; Smithsonian Tropical Research Institute
FX The authors would like to thank past and present members of the Schwarz
lab for their assistance and support, including their previous work
collecting gene sequences. This work was supported by Australian
Research Council grants to MPS, Natural Sciences and Engineering
Research Council Post Graduate Scholarship to SMR and an Earl S Tupper
Fellowship from the Smithsonian Tropical Research Institute to SMT.
NR 25
TC 7
Z9 7
U1 1
U2 14
PU SPRINGER BASEL AG
PI BASEL
PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND
SN 0020-1812
J9 INSECT SOC
JI Insect. Soc.
PD MAY
PY 2012
VL 59
IS 2
BP 207
EP 214
DI 10.1007/s00040-011-0206-6
PG 8
WC Entomology
SC Entomology
GA 925HG
UT WOS:000302751200009
ER
PT J
AU Lovette, IJ
Arbogast, BS
Curry, RL
Zink, RM
Botero, CA
Sullivan, JP
Talaba, AL
Harris, RB
Rubenstein, DR
Ricklefs, RE
Bermingham, E
AF Lovette, Irby J.
Arbogast, Brian S.
Curry, Robert L.
Zink, Robert M.
Botero, Carlos A.
Sullivan, John P.
Talaba, Amanda L.
Harris, Rebecca B.
Rubenstein, Dustin R.
Ricklefs, Robert E.
Bermingham, Eldredge
TI Phylogenetic relationships of the mockingbirds and thrashers (Aves:
Mimidae)
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE Mimidae; Mockingbird; Thrasher; Galapagos; Phylogeny; Classification
ID MITOCHONDRIAL SEQUENCE DATA; CURVE-BILLED THRASHER; GALAPAGOS
MOCKINGBIRDS; MOLECULAR PHYLOGENY; NORTHERN MOCKINGBIRDS;
GEOGRAPHIC-VARIATION; AVIAN RADIATION; SPECIES LIMITS; PASSERIDA AVES;
MAJOR LINEAGES
AB The mockingbirds, thrashers and allied birds in the family Mimidae are broadly distributed across the Americas. Many aspects of their phylogenetic history are well established, but there has been no previous phylogenetic study that included all species in this radiation. Our reconstructions based on mitochondrial and nuclear DNA sequence markers show that an early bifurcation separated the Mimidae into two clades, the first of which includes North and Middle American taxa (Melanotis, Melanoptila, Dumetella) plus a small radiation that likely occurred largely within the West Indies (Ramphocinclus, Allenia, Margarops, Cinclocerthia). The second and larger radiation includes the Toxostoma thrasher clade, along with the monotypic Sage Thrasher (Oreoscoptes) and the phenotypically diverse and broadly distributed Mimus mockingbirds. This mockingbird group is biogeographically notable for including several lineages that colonized and diverged on isolated islands, including the Socorro Mockingbird (Mimus graysoni, formerly Mimodes) and the diverse and historically important Galapagos mockingbirds (formerly Nesomimus). Our reconstructions support a sister relationship between the Galapagos mockingbird lineage and the Bahama Mockingbird (M. gundlachi) of the West Indies, rather than the Long-tailed Mockingbird (M. longicaudatus) or other species presently found on the South American mainland. Relationships within the genus Toxostoma conflict with traditional arrangements but support a tree based on a preivous mtDNA study. For instance, the southern Mexican endemic Ocellated Thrasher (T. ocellatum) is not an isolated sister species of the Curve-billed thrasher (T. curvirostre). (C) 2011 Published by Elsevier Inc.
C1 [Lovette, Irby J.; Sullivan, John P.; Talaba, Amanda L.; Harris, Rebecca B.] Cornell Univ, Cornell Lab Ornithol, Fuller Evolutionary Biol Program, Ithaca, NY 14950 USA.
[Arbogast, Brian S.] Univ N Carolina, Dept Biol & Marine Biol, Wilmington, NC 28403 USA.
[Curry, Robert L.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA.
[Zink, Robert M.] Univ Minnesota, Bell Museum, St Paul, MN 55108 USA.
[Botero, Carlos A.] Natl Evolutionary Synth Ctr, Durham, NC 27707 USA.
[Rubenstein, Dustin R.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
[Ricklefs, Robert E.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA.
[Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama.
RP Lovette, IJ (reprint author), Cornell Univ, Cornell Lab Ornithol, Fuller Evolutionary Biol Program, 159 Sapsucker Woods Rd, Ithaca, NY 14950 USA.
EM IJL2@cornell.edu
RI Lovette, Irby/P-3477-2014; Rubenstein, Dustin/A-3451-2015;
OI Rubenstein, Dustin/0000-0002-4999-3723; Botero, Carlos
A./0000-0003-0955-2795
FU Microsoft Corporation; National Evolutionary Synthesis Center (NESCent),
NSF [EF-0905606]; [NSF-DEB-0924741]; [NSF-DEB-0515981]
FX We thank B. McCleery and D. Rabosky for advice and assistance, and two
reviewers for the comments on the manuscript. Part of this work was
carried out using the resources of the Computational Biology Service
Unit at Cornell University which is partially funded by Microsoft
Corporation. We thank the following institutions, their field
collaborators, and their collections staff for the loan of genetic
materials: Academy of Natural Sciences, Philadelphia; Bell Museum of
Natural History, University of Minnesota; Cornell University Museum of
Vertebrates; Louisiana State University Museum of Natural Science; Museo
Nacional de Historia Natural, Santiago, Chile; San Diego State
University Museum of Biodiversity; Wake Forest University. We thank B.
Arbogast and D. Cadena for providing previously unpublished sequences
generated in their laboratories. We are grateful to P. Tubaro of the
Museo Argentino de Ciencias Naturales, Buenos Aires for his guidance in
obtaining specimens of South American mockingbird species. CAB is funded
by the National Evolutionary Synthesis Center (NESCent), NSF Grant
EF-0905606. This Project was additionally supported by awards
NSF-DEB-0924741 and NSF-DEB-0515981.
NR 67
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U1 3
U2 35
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1055-7903
EI 1095-9513
J9 MOL PHYLOGENET EVOL
JI Mol. Phylogenet. Evol.
PD MAY
PY 2012
VL 63
IS 2
BP 219
EP 229
DI 10.1016/j.ympev.2011.07.009
PG 11
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 917TR
UT WOS:000302202000001
PM 21867766
ER
PT J
AU Horn, JW
van Ee, BW
Morawetz, JJ
Riina, R
Steinmann, VW
Berry, PE
Wurdack, KJ
AF Horn, James W.
van Ee, Benjamin W.
Morawetz, Jeffery J.
Riina, Ricarda
Steinmann, Victor W.
Berry, Paul E.
Wurdack, Kenneth J.
TI Phylogenetics and the evolution of major structural characters in the
giant genus Euphorbia L. (Euphorbiaceae)
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE Character state reconstruction; Convergent evolution; Cyathium;
Euphorbia; Growth form; Multigene analyses; Xerophyte
ID CHAIN MONTE-CARLO; SUBGENUS CHAMAESYCE EUPHORBIACEAE;
FLOWER-INFLORESCENCE BOUNDARY; SOUTHEASTERN UNITED STATES;
DNA-SEQUENCES; DISCRETE CHARACTERS; MAXIMUM-LIKELIHOOD; CORRELATED
EVOLUTION; MOLECULAR PHYLOGENY; CLADE EUPHORBIA
AB Euphorbia is among the largest genera of angiosperms, with about 2000 species that are renowned for their remarkably diverse growth forms. To clarify phylogenetic relationships in the genus, we used maximum likelihood, Bayesian, and parsimony analyses of DNA sequence data from 10 markers representing all three plant genomes, averaging more than 16 kbp for each accession. Taxon sampling included 176 representatives from Euphorbioideae (including 161 of Euphorbia). Analyses of these data robustly resolve a backbone topology of four major, subgeneric clades-Esula, Rhizanthium, Euphorbia, and Chamaesyce-that are successively sister lineages. Ancestral state reconstructions of six reproductive and growth form characters indicate that the earliest Euphorbia species were likely woody, non-succulent plants with helically arranged leaves and 5-glanded cyathia in terminal inflorescences. The highly modified growth forms and reproductive features in Euphorbia have independent origins within the subgeneric clades. Examples of extreme parallelism in trait evolution include at least 14 origins of xeromorphic growth forms and at least 13 origins of seed caruncles. The evolution of growth form and inflorescence position are significantly correlated, and a pathway of evolutionary transitions is supported that has implications for the evolution of Euphorbia xerophytes of large stature. Such xerophytes total more than 400 species and are dominants of vegetation types throughout much of arid Africa and Madagascar. Published by Elsevier Inc.
C1 [Horn, James W.; Wurdack, Kenneth J.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA.
[van Ee, Benjamin W.] Black Hills State Univ Herbarium, Spearfish, SD 57799 USA.
[Morawetz, Jeffery J.] Rancho Santa Ana Bot Garden, Claremont, CA 91711 USA.
[Riina, Ricarda; Berry, Paul E.] Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48108 USA.
[Riina, Ricarda; Berry, Paul E.] Univ Michigan Herbarium, Ann Arbor, MI 48108 USA.
[Riina, Ricarda] CSIC, E-28014 Madrid, Spain.
[Steinmann, Victor W.] Ctr Reg Bajio, Inst Ecol, AC, Patzcuaro 61600, Michoacan, Mexico.
RP Wurdack, KJ (reprint author), Smithsonian Inst, Dept Bot, NMNH MRC 166,POB 37012, Washington, DC 20013 USA.
EM wurdackk@si.edu
RI Riina, Ricarda/J-1032-2014
OI Riina, Ricarda/0000-0002-7423-899X
FU National Science Foundation PBI [DEB 0616533]; Smithsonian Institution
FX The authors thank the following individuals and institutions for
providing plant or DNA samples: T. Haevermans (P), D. Hannon (RSA,
Huntington), Y. Yang and B. Dorsey (MICH), Rolf Becker (PRE), J. Molero
(BCN), UC Davis Botanical Conservatory, Huntington Botanical Gardens,
International Euphorbia Society, FTG, K, MICH, MO, NY, RSA, US, and WAG.
Support for this study came from a National Science Foundation PBI Grant
(DEB 0616533) and the Smithsonian Institution.
NR 140
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U1 5
U2 78
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 1055-7903
EI 1095-9513
J9 MOL PHYLOGENET EVOL
JI Mol. Phylogenet. Evol.
PD MAY
PY 2012
VL 63
IS 2
BP 305
EP 326
DI 10.1016/j.ympev.2011.12.022
PG 22
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 917TR
UT WOS:000302202000009
PM 22273597
ER
PT J
AU Barrantes, G
Eberhard, WG
AF Barrantes, Gilbert
Eberhard, William G.
TI Extreme Behavioral Adjustments by an Orb-Web Spider to Restricted Spaces
SO ETHOLOGY
LA English
DT Article
ID NEPHILA-CLAVIPES ARANEAE; AGGREGATIVE BEHAVIOR; WEAVING SPIDERS;
TETRAGNATHIDAE; ICHNEUMONIDAE; HYMENOPTERA; STRATEGIES; ARANEIDAE;
CONSTRUCTION; PARASITOIDS
AB Adaptive flexibility in response to environmental variation is often advantageous and occurs in many types of traits in many species. Although the basic designs of the orb webs of a given species are relatively uniform, spiders can adjust their webs to some types of environmental variation. This study of adult female Leucauge argyra tests the extremes to which they can adjust with respect to reduced area in which to build, and documents probably the most pronounced flexibility in orb design ever recorded. These adjustments revealed several behavioral rules that guide orb construction behavior. Spiders adjusted at least seven probably independent aspects of orb design when confined in tiny spaces that spanned about 7% of the maximum distance normally spanned by webs in the field and that had diameters that were only about three times the length of the spider itself. Webs in intermediate sized containers had intermediate designs, and many of the adjustments appear to result from extensions of the behavioral rules guiding orb construction in less severely restricted spaces in the field.
C1 [Barrantes, Gilbert; Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Jose 2060, Costa Rica.
[Eberhard, William G.] Smithsonian Trop Res Inst, Panama City, FL USA.
RP Barrantes, G (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ Rodrigo Facio, San Jose 2060, Costa Rica.
EM gilbert.barrantes@gmail.com
FU Smithsonian Tropical Research Institute; Vicerrectoria de Investigacion
of the Universidad de Costa Rica
FX Anita Aisenberg generously shared her key discovery that female L.
argyra will build orbs in small plastic cups; Jairo Moya made useful
suggestions regarding the designs of containers and helped construct
them. Sr. Pedro Gaspar allowed us to work in his oil palm plantation.
The Smithsonian Tropical Research Institute and the Vicerrectoria de
Investigacion of the Universidad de Costa Rica provided financial
support.
NR 48
TC 8
Z9 9
U1 3
U2 35
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0179-1613
J9 ETHOLOGY
JI Ethology
PD MAY
PY 2012
VL 118
IS 5
BP 438
EP 449
DI 10.1111/j.1439-0310.2012.02029.x
PG 12
WC Psychology, Biological; Behavioral Sciences; Zoology
SC Psychology; Behavioral Sciences; Zoology
GA 924OA
UT WOS:000302700000003
ER
PT J
AU Puerta-Pinero, C
Brotons, L
Coll, L
Gonzalez-Olabarria, JR
AF Puerta-Pinero, C.
Brotons, L.
Coll, L.
Gonzalez-Olabarria, J. R.
TI Valuing acorn dispersal and resprouting capacity ecological functions to
ensure Mediterranean forest resilience after fire
SO EUROPEAN JOURNAL OF FOREST RESEARCH
LA English
DT Article
DE Disturbance; Ecosystem services; Garrulus glandarius; Pinus spp; Quercus
spp; Resprouters
ID ECOSYSTEM SERVICES; CATALONIA NORTHEAST; SEED DISPERSAL; SPAIN;
MANAGEMENT; REGENERATION; ORGANISMS; LANDSCAPE; SURVIVAL; STAND
AB Ecological processes within forests provide vital ecosystem services to society, most of which depend on the persistence of tree cover that can be altered after the impact of a disturbance. The aim of the present study was to examine the role of seed dispersal and resprouting that mediate resilience to large fires and evaluate the economic costs that these ecological functions provide. We used field data from 412 plots of the Spanish National Forest Inventory providing information on pre- and post-fire conditions of Mediterranean Pinus spp. and Quercus spp.-dominated forests. Then, we determined the need for restoration (N (Rest)) and estimated the minimum pre-fire densities needed to ensure adequate post-fire cover. Economic valuations were assessed through three different scenarios (Sc) of possible human-management actions aimed at ensuring proper post-fire tree cover: Sc. 1) a pre-fire management scenario evaluating the costs of planting Quercus spp. seedlings in the understory, mimicking the whole dispersal function; Sc. 2) a pre-fire scenario in which enrichment plantations increased the densities of natural oaks; and Sc. 3) a post-fire scenario where the restoration is done through planting pines within the burned area. Approximately 90% of the burned area (371 out of 412 plots) was able to recover after fire supporting the view that Mediterranean forests are resilient to fire. This resilience was primarily mediated by biotic seed dispersal and posterior resprouting of tree species. These ecological functions saved between 626 and 1,326 a,not sign/ha compared to the human-management actions. Ensuring key ecological processes within forests increases forest resilience and recovery after fire leading to a generally significant saving of economic resources. In a perspective of increased future impact of disturbances and decrease availability of economic resources for forest management, the implications of the present study can be far reaching and extended to other forest planning exercises.
C1 [Puerta-Pinero, C.; Brotons, L.; Coll, L.; Gonzalez-Olabarria, J. R.] Ctr Tecnol Forestal Catalunya CTFC, Solsona 25280, Spain.
RP Puerta-Pinero, C (reprint author), Smithsonian Trop Res Inst, Unit 0948 DPO AA, Miami, FL 34002 USA.
EM puertac@si.edu
RI Gonzalez Olabarria, Jose Ramon/D-2575-2009; Puerta Pinero,
Carolina/B-3186-2012; Coll, Lluis/E-8724-2015; Brotons,
Lluis/D-1570-2009
OI Gonzalez Olabarria, Jose Ramon/0000-0002-5040-712X; Puerta Pinero,
Carolina/0000-0002-0584-7548; Coll, Lluis/0000-0002-8035-5949; Brotons,
Lluis/0000-0002-4826-4457
FU Spanish Ministry of Science and Innovation [CGL2008-05506-C02-01/BOS];
Consolider-Ingenio Montes project [CSD2008-00040]; Ramon y Cajal; Juan
de la Cierva; Fundacion Caja Madrid; Catalan Government [SGR2009-531]
FX We thank Ryan Chisholm and several anonymous referees for their review
of this manuscript. Cian Gill kindly helped us with English translation
and grammar. This research was primarily supported by the Spanish
Ministry of Science and Innovation via CGL2008-05506-C02-01/BOS project
and the Consolider-Ingenio Montes project (CSD2008-00040); a Ramon y
Cajal contract to LB and LC; and a Juan de la Cierva contract to JRG.
CPP was partially supported by a Fundacion Caja Madrid grant. Partial
funding was also provided by the Catalan Government grant SGR2009-531.
NR 36
TC 11
Z9 11
U1 1
U2 27
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1612-4669
J9 EUR J FOREST RES
JI Eur. J. For. Res.
PD MAY
PY 2012
VL 131
IS 3
BP 835
EP 844
DI 10.1007/s10342-011-0557-6
PG 10
WC Forestry
SC Forestry
GA 920PJ
UT WOS:000302418400028
ER
PT J
AU Ugan, A
Coltrain, J
AF Ugan, Andrew
Coltrain, Joan
TI Stable isotopes, diet, and taphonomy: a look at using isotope-based
dietary reconstructions to infer differential survivorship in
zooarchaeological assemblages
SO JOURNAL OF ARCHAEOLOGICAL SCIENCE
LA English
DT Article
DE Stable isotopes; Great Basin; Taphonomy; Dietary reconstruction; SISUS
ID MEDIEVAL WARM PERIOD; BONE-COLLAGEN; POPULATION-DENSITY; LATE HOLOCENE;
GREAT-BASIN; AMINO-ACIDS; PROTEIN DIGESTIBILITY; FORAGING EFFICIENCY;
RESOURCE DEPRESSION; BIOLOGICAL APATITE
AB Archaeology has always faced the problem of making informed inferences based on an incomplete record. Zooarchaeological studies of prehistoric hunting and diet offer a clear case in point, where a range of behavioral and taphonomic factors can produce a substantial disconnect between what people actually captured and ate and what archaeologists recover and interpret. We explore this disconnect by presenting stable C and N data for wild faunas, archaeological maize, and three human burials from Fremont-period sites in southeastern Utah, the United States. We use these data to estimate faunal contributions to prehistoric diets and compare the results with previous zooarchaeological analyses of faunas from the same sites. Results for the two approaches differ sharply, with isotopic estimates showing much higher contributions of small and lowland game. We discuss these results in terms of both local prehistory and wider issues of taphonomy and dietary analysis. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Ugan, Andrew] Smithsonian Trop Res Inst, Unit 9100, Dpo, AA 34002 USA.
[Ugan, Andrew; Coltrain, Joan] Univ Utah, Dept Anthropol, Salt Lake City, UT 84112 USA.
RP Ugan, A (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948, Dpo, AA 34002 USA.
EM andrew.ugan@gmail.com; joan.coltrain@anthro.utah.edu
FU NSF [0552214]
FX We would like to thank Marian Jacklin, Heritage Manager for the Dixie
National Forest, for help obtaining pine nuts from Parowan Valley, the
folks at the SIRFER lab, University of Utah, for their help with running
the animal samples, and Ben Turner and Dayana Agudo at the STRI isotope
facility for help with the modern pine nuts. The quality of the
manuscript was substantially improved by the comments of two anonymous
reviewers. Permission for destructive analysis of the faunal specimens
was granted by the Utah Museum of Natural History. Support for this
project provided by NSF grant 0552214.
NR 133
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U1 4
U2 20
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0305-4403
EI 1095-9238
J9 J ARCHAEOL SCI
JI J. Archaeol. Sci.
PD MAY
PY 2012
VL 39
IS 5
BP 1401
EP 1411
DI 10.1016/j.jas.2011.12.027
PG 11
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 910EV
UT WOS:000301620900021
ER
PT J
AU Laliberte, E
Turner, BL
Costes, T
Pearse, SJ
Wyrwoll, KH
Zemunik, G
Lambers, H
AF Laliberte, Etienne
Turner, Benjamin L.
Costes, Thomas
Pearse, Stuart J.
Wyrwoll, Karl-Heinz
Zemunik, Graham
Lambers, Hans
TI Experimental assessment of nutrient limitation along a 2-million-year
dune chronosequence in the south-western Australia biodiversity hotspot
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE co-limitation; ecosystem decline; ecosystem progression; ecosystem
retrogression; pedogenesis; plant-soil (below-ground) interactions;
productivity; soil age; stoichiometry; succession
ID LONG-TERM CHRONOSEQUENCES; SWAN COASTAL-PLAIN; PHOSPHORUS LIMITATION;
SOIL DEVELOPMENT; LUPINUS-ALBUS; RAIN-FOREST; ECOSYSTEM RETROGRESSION;
ROCK PHOSPHATE; CO-LIMITATION; PERTH BASIN
AB 1. The classical model of long-term ecosystem development suggests that primary productivity is limited by nitrogen (N) on young substrates and phosphorus (P) on older substrates. Measurements of foliar and soil nutrients along soil chronosequences support this model, but direct tests through nutrient-addition experiments are rare.
2. We conducted a nutrient-limitation bioassay using phytometer species grown in soils from five stages of a >2-million-year dune chronosequence in south-western Australia. This long-term chronosequence is located within a region of exceptionally high plant species diversity and has not been previously studied in the context of ecosystem development.
3. Growth of unfertilized phytometers, a proxy for primary productivity, peaked on young soils (hundreds to a few thousand years) and then declined steadily on older soils. This decline was linked to P limitation, and its rapid appearance (<7000 years) compared to other sequences reflects the low P concentration in the parent material. As predicted, growth of canola was N-limited on the youngest soil (stage 1), co-limited by multiple nutrients in stage 2 and increasingly P-limited thereafter.
4. Growth of wheat was P-limited from stage 2 onwards, yet on the youngest soil it was co-limited by potassium (K) and micronutrients - most likely iron (Fe). Nitrogen addition also decreased the root: shoot ratio of wheat such that shoot growth was higher than in the control. We attribute these responses to a parent material that is very low in K and N and strongly alkaline (pH [H2O] > 9), being of a marine origin (i.e. carbonate dunes). Fe is poorly soluble at high pH and K likely plays a role in the secretion of Fe-mobilizing exudates from wheat roots.
5. Synthesis. Our results provide strong support for the long-term ecosystem-development model, particularly with regard to the appearance of P limitation and associated declines in productivity. However, our study also shows that N cannot be assumed to invariably be the most important limiting nutrient in young soils, and it is unlikely to be the only limiting nutrient in calcareous soils. This south-western Australian long-term chronosequence provides an excellent opportunity to explore edaphic controls over plant species diversity.
C1 [Laliberte, Etienne; Turner, Benjamin L.; Costes, Thomas; Pearse, Stuart J.; Zemunik, Graham; Lambers, Hans] Univ Western Australia, Sch Plant Biol, Crawley 6009, Australia.
[Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Costes, Thomas] Inst Natl Hort & Paysage, Ctr Angers, F-49045 Angers 01, France.
[Wyrwoll, Karl-Heinz] Univ Western Australia, Sch Earth & Environm, Crawley 6009, Australia.
RP Laliberte, E (reprint author), Univ Western Australia, Sch Plant Biol, 35 Stirling Highway, Crawley 6009, Australia.
EM etienne.laliberte@uwa.edu.au
RI Laliberte, Etienne/B-6855-2008; Turner, Benjamin/E-5940-2011; Lambers,
Hans/A-1544-2008; Pearse, Stuart/A-6610-2008
OI Laliberte, Etienne/0000-0002-3167-2622; Turner,
Benjamin/0000-0002-6585-0722; Lambers, Hans/0000-0002-4118-2272; Pearse,
Stuart/0000-0003-3737-0788
FU University of Western Australia; Australian Research Council (ARC) DECRA
[DE120100352]; ARC
FX We thank the Western Australia Department of Environment and
Conservation (DEC), particularly Niall Sheehy, for their cooperation
with soil collection and Tania Romero, Dianne de la Cruz and Luis Ramos
for laboratory support. We also thank the Editor and two anonymous
reviewers for comments that helped to strengthen the manuscript. Wheat
seed was generously supplied by Daniel Mullan from Intergrain Pty Ltd,
lupin seed by Bevan Buirchell from the Department of Agriculture and
Food Western Australia (DAFWA) and canola seed by Matthew Nelson from
Canola Breeders Western Australia Pty Ltd (CBWA). E. L. was supported by
a Research Fellowship from the University of Western Australia and by an
Australian Research Council (ARC) DECRA (DE120100352). H. L.
acknowledges financial support from ARC.
NR 82
TC 53
Z9 53
U1 6
U2 99
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-0477
EI 1365-2745
J9 J ECOL
JI J. Ecol.
PD MAY
PY 2012
VL 100
IS 3
BP 631
EP 642
DI 10.1111/j.1365-2745.2012.01962.x
PG 12
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 923MK
UT WOS:000302623200006
ER
PT J
AU Katabuchi, M
Kurokawa, H
Davies, SJ
Tan, S
Nakashizuka, T
AF Katabuchi, Masatoshi
Kurokawa, Hiroko
Davies, Stuart J.
Tan, Sylvester
Nakashizuka, Tohru
TI Soil resource availability shapes community trait structure in a
species-rich dipterocarp forest
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE determinants of plant community diversity and structure; functional
traits; habitat filtering; Lambir; limiting similarity; null models;
soil nutrients; tropical forest dynamics plot
ID RAIN-FOREST; FUNCTIONAL TRAITS; TROPICAL FOREST; HABITAT SPECIALIZATION;
PHYLOGENETIC STRUCTURE; LIMITING SIMILARITY; PLANT-COMMUNITIES;
AMAZONIAN FOREST; TREE COMMUNITY; WOOD DENSITY
AB 1. Habitat filtering and limiting similarity have been proposed as two opposing forces structuring community memberships. Community assembly theory proposes habitat filtering as a mechanism restricting community membership according to the ecological strategies of species in a given environment. Limiting similarity posits that some species exclude others that are ecologically similar.
2. We quantified nine ecophysiological and life-history traits for 80 dipterocarp species in the 52-ha Lambir Forest Dynamics Plot (FDP; Lambir Hills National Park, Sarawak, Malaysia). We studied forests on four soil types differing in fertility and moisture, focusing on soil resource availabilities as environmental determinants of habitat filtering processes. We used a null-model approach to detect the strengths of habitat filtering and limiting similarity. We quantified the relative contributions of soil resources (nutrients and water) to habitat filtering by comparing the strength of habitat filtering processes (i.e. effect sizes) at the overall plot scale and at the individual soil-type scale. We also compared the strengths of assembly processes among soil types.
3. Compared to a null model at microscale (20 x 20 m), trait range and variance were reduced for seven of nine functional traits, suggesting the importance of habitat filtering in the dipterocarp community. We also found a broader distribution of five traits, and more even spacing for seven traits (20 x 20 m), which is consistent with the concept of limiting similarity. Randomizations that swapped species occurrences within soil types (i.e. null models removing soil effects in assembly processes) were much closer to observed values, and there were no phylogenetic constraints on habitat association. Hence, soil resource availability acted as a habitat filtering mechanismin the FDP; relative contributions to habitat filtering ranged from 35% for seed mass to 77% for relative growth rate. Furthermore, soil types apparently affected the strengths of habitat filtering and limiting similarity.
4. Synthesis. We demonstrate that soil resource availability is a crucial determinant of habitat filtering in this species-rich tropical rain forest; the strengths of assembly processes differed among soil types. Variation in soil resource availability can shape the distribution of traits through community assembly processes, promoting trait diversification and species coexistence.
C1 [Katabuchi, Masatoshi; Kurokawa, Hiroko; Nakashizuka, Tohru] Tohoku Univ, Grad Sch Life Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Davies, Stuart J.] Harvard Univ, Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Cambridge, MA 02138 USA.
[Tan, Sylvester] Sarawak Forestry Corp, Kuching 93250, Sarawak, Malaysia.
RP Katabuchi, M (reprint author), Tohoku Univ, Grad Sch Life Sci, Aoba Ku, 6-3 Aoba, Sendai, Miyagi 9808578, Japan.
EM mattocci27@gmail.com
FU NSF [DEB-9107247, DEB-9629601]; Monbusho grant [06041094, 08NP0901,
09NP0901]; JSPS; Ministry of the Environment, Japan [S-9-3]; [2337007]
FX We thank the Forest Department of Sarawak and Sarawak Forest Research
Corporation for their kind permission to conduct research in Lambir
Hills National Park. We also thank many people who contributed to the
52-ha Long-Term Ecological Research Project. The 52-ha Long-Term
Ecological Research Project is a collaborative project of the Forest
Department of Sarawak, Malaysia, Harvard University, USA (under NSF
awards DEB-9107247 and DEB-9629601 to P. S. Ashton), and Osaka City
University, Japan (under Monbusho grant 06041094 to T. Yamakura,
08NP0901 to S. Tamura and 09NP0901 to S. Sasaki). We are also grateful
to Douglas and Rose for their assistance in the field, to N. Swenson for
helpful advice on the analyses, to M. Aiba, P. Bellingham, W. Cornwell,
H. Cornelissen, K. Kitajima and one anonymous referee for constructive
comments on an early draft of the manuscript. This study was supported
by Grant-in-Aid for JSPS Fellows to M. Kand partly supported by
Grant-in-Aid for Scientific Research (B) (2337007) and the Environment
Research and Technology Development Fund (S-9-3) of the Ministry of the
Environment, Japan.
NR 56
TC 31
Z9 33
U1 10
U2 69
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-0477
J9 J ECOL
JI J. Ecol.
PD MAY
PY 2012
VL 100
IS 3
BP 643
EP 651
DI 10.1111/j.1365-2745.2011.01937.x
PG 9
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 923MK
UT WOS:000302623200007
ER
PT J
AU Allendorf, TD
Aung, M
Songer, M
AF Allendorf, Teri D.
Aung, Myint
Songer, Melissa
TI Using residents' perceptions to improve park-people relationships in
Chatthin Wildlife Sanctuary, Myanmar
SO JOURNAL OF ENVIRONMENTAL MANAGEMENT
LA English
DT Article
DE Protected areas; Residents; Attitudes; Perceptions; Park-people;
Communities
ID PROTECTED AREA MANAGEMENT; CONSERVATION ATTITUDES; NATIONAL-PARK;
COMMUNITY ATTITUDES; LOCAL PEOPLE; TANZANIA; BURMA; NEPAL; BIODIVERSITY;
ELEPHANTS
AB The complex and context-specific relationships that local residents have with neighboring protected areas present many challenges for protected area (PA) management. While long-term, interdisciplinary approaches may be necessary to fully understand park-people relationships within a particular PA, the reality is that management decisions for the majority of PAs in the world are made by protected area staff with little or no external assistance. One potential entry point for management to understand park-people relationships and improve management is through understanding people's perceptions of PAs. This paper presents a study from Chatthin Wildlife Sanctuary in central Myanmar designed to explore the impact of using residents' attitudes to directly inform management strategies. We conducted a survey to determine attitudes and determinants of attitudes toward CWS. In response to the survey, the warden made changes to the Sanctuary's management strategy to accommodate local needs and perceptions. Four years later, we repeated the survey to explore the effects of the management changes on people's perceptions and found that people were significantly more likely to like the sanctuary, less likely to mention problems, and more likely to mention benefits. People's negative perceptions of management conflicts and crop damage decreased and their positive perceptions of conservation and ecosystem service benefits and extraction benefits increased. This study demonstrates that residents' perceptions can be used by management as a starting point to improve park-people relationships through feasible and targeted interventions that are meaningful to local communities and their relationships with PAs. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Allendorf, Teri D.] Univ Wisconsin Madison, Land Tenure Ctr, Mazomanie, WI 53560 USA.
[Aung, Myint] Friends Wildlife, Yankin Township, Yangon, Myanmar.
[Songer, Melissa] Conservat Ecol Ctr, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
RP Allendorf, TD (reprint author), Univ Wisconsin Madison, Land Tenure Ctr, 110 Elm St, Mazomanie, WI 53560 USA.
EM allendorf@wisc.edu; myintaungwildlife@gmail.com; songerm@si.edu
FU National Zoo
FX We thank Khine Khine Swe, Thida Oo, and Kyaw Kyaw Moe for their
assistance collecting the interview data. We thank the staff of Chatthin
Wildlife Sanctuary for facilitating the surveys. We thank the Friends of
the National Zoo for providing financial support.
NR 46
TC 12
Z9 14
U1 3
U2 37
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0301-4797
EI 1095-8630
J9 J ENVIRON MANAGE
JI J. Environ. Manage.
PD MAY
PY 2012
VL 99
BP 36
EP 43
DI 10.1016/j.jenvman.2012.01.004
PG 8
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 920YX
UT WOS:000302446300005
PM 22318239
ER
PT J
AU Wiensz, JT
Bourassa, AE
Lloyd, ND
Wiacek, A
Martin, RV
Degenstein, DA
AF Wiensz, J. Truitt
Bourassa, Adam E.
Lloyd, Nick D.
Wiacek, Aldona
Martin, Randall V.
Degenstein, Doug A.
TI Photon conservation in scattering by large ice crystals with the
SASKTRAN radiative transfer model
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Ice; Cirrus; Aerosol; Spherical successive-orders; Forward scattering
ID ALGEBRAIC RECONSTRUCTION TECHNIQUE; TRUNCATION APPROXIMATION; PHASE
FUNCTIONS; RETRIEVAL
AB The scattering of visible light by ice crystals and dust in radiative transfer models is challenging in part due to the large amount of scattering in the forward direction. We introduce a technique that ensures numerical conservation of photons in any radiative transfer model and that quantifies the integration error associated with highly asymmetric phase functions. When applied to a successive-orders of scatter model, the technique illustrates the high accuracy obtained in numerical integration of molecular and aerosol scattering. As well, a phase function truncation and renormalization technique is applied to scattering by ice crystals with very large size parameters, between 100 and 1000, and the scaled radiative transfer equation is solved with the spherical successive-orders model, SASKTRAN. Since computations shown this work are performed in a fully spherical model atmosphere, the computed radiances are not subject to the discontinuity at the horizon that is inherent in models using a plane-parallel assumption. The methods introduced in this work are of particular interest in modeling limb radiances in the presence of thin cirrus clouds. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Wiensz, J. Truitt; Bourassa, Adam E.; Lloyd, Nick D.; Degenstein, Doug A.] Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK S7N 0W0, Canada.
[Wiacek, Aldona; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Wiensz, JT (reprint author), Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK S7N 0W0, Canada.
EM truitt.wiensz@usask.ca
RI Martin, Randall/C-1205-2014
OI Martin, Randall/0000-0003-2632-8402
FU Natural Sciences and Engineering Research Council (Canada); European
Space Agency; Sweden (SNSB); Canada (CSA); France (CNES); Finland
(Tekes)
FX This work was supported by the Canadian Space Agency, the Natural
Sciences and Engineering Research Council (Canada) and the European
Space Agency. Odin is a Swedish-led satellite project funded jointly by
Sweden (SNSB), Canada (CSA), France (CNES) and Finland (Tekes).
NR 16
TC 2
Z9 2
U1 0
U2 2
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 MAY
PY 2012
VL 113
IS 8
BP 582
EP 593
DI 10.1016/j.jqsrt.2012.02.007
PG 12
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 921UT
UT WOS:000302504100002
ER
PT J
AU Bolanos, JA
Baeza, JA
Hernandez, JE
Lira, C
Lopez, R
AF Bolanos, Juan A.
Antonio Baeza, J.
Hernandez, Jesus E.
Lira, Carlos
Lopez, Regulo
TI Population dynamics and reproductive output of the non-indigenous crab
Charybdis hellerii in the south-eastern Caribbean Sea
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE invasive species; size at first maturity; recruitment; sex-ratio;
Venezuela
ID LIFE-HISTORY; 1ST RECORD; BRACHYURA; DECAPODA; CRUSTACEA; PORTUNIDAE;
ATLANTIC; MILNEEDWARDS,A.; COAST; GULF
AB Charybdis hellerii is one of several poorly known non-indigenous crabs in the Caribbean. In this study we report on the reproductive dynamic of a shallow subtidal population that invaded Isla Margarita, Venezuela, south-eastern Caribbean Sea > 15 years ago and has persisted in the region up to date. Male and female crabs, both large and small, were found year-round at the study site. The size-frequency distribution indicated a lifespan of 2-3 years. Charybdis hellerii reproduces continuously but with very low intensity during the year. Small individuals (<25 mm carapace length) were uncommon and intermittently found during the study period. Sex-ratio varied between 0.1 and 0.65 (mean +/- SD = of 0.46 +/- 0.14) and did not differ significantly from 1:1 ratio during most of the year. The size of the smallest brooding female was 36.81 mm carapace width (CW). Behavioural size at first maturity (movable abdomen) in males and females was estimated to be 22.39 mm CW (confidence limits: 18.35-24.72) and 37.43 mm CW (35.55-39.09), respectively. Reproductive output, estimated as the ratio of embryo to female body dry mass, varied between 0.052 and 0.084 (0.07 +/- 0.008). Also, reproductive output was size-dependent with large females allocating proportionally less resources to egg production than small females. The reproductive schedule here reported for C. hellerii disagrees with the generalized idea of exotic populations 'thriving' in an environment free of natural enemies (e.g. predators, competitors and diseases).
C1 [Bolanos, Juan A.; Hernandez, Jesus E.; Lira, Carlos; Lopez, Regulo] Univ Oriente, Escuela Ciencias Aplicadas Mar, Grp Invest Carcinol, Isla Margarita, Venezuela.
[Antonio Baeza, J.] Old Dominion Univ, Norfolk, VA USA.
[Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
[Antonio Baeza, J.] Univ Catolica Norte, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile.
RP Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM baezaa@si.edu
OI Baeza, Juan Antonio/0000-0002-2573-6773
FU STRI; SMSFP
FX J.A.B. acknowledges the support from a STRI Marine Postdoctoral
Fellowship and a SMSFP Postdoctoral Fellowship. Sampling was conducted
according to Venezuelan federal laws. We appreciate the helpful comments
by Angelo Jason Spadaro and Fernando Mantelatto. This is contribution
number 850 from the Smithsonian Marine Station at Fort Pierce.
NR 32
TC 8
Z9 8
U1 0
U2 13
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD MAY
PY 2012
VL 92
IS 3
BP 469
EP 474
DI 10.1017/S002531541100052X
PG 6
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 920AS
UT WOS:000302373900006
ER
PT J
AU Sadler, PM
Sonnert, G
Hazari, Z
Tai, R
AF Sadler, Philip M.
Sonnert, Gerhard
Hazari, Zahra
Tai, Robert
TI Stability and Volatility of STEM Career Interest in High School: A
Gender Study
SO SCIENCE EDUCATION
LA English
DT Article
ID SCIENCE; WOMEN; CHOICE; EXPECTATIONS; METAANALYSIS; ENGINEERS; MODEL;
GIRLS; MATH
AB This retrospective cohort study characterizes how interest in science, technology, engineering, mathematics (STEM) careers changes during high school for more than 6,000 students in a representative national sample of 34 two- and four-year colleges taking mandatory college English courses. Overall, large gender differences in career plans were found, with males showing far more interest particularly in engineering, whereas females were more attracted to careers in health and medicine during their high school years. The key factor predicting STEM career interest at the end of high school was interest at the start of high school. There was an additional effect of gender, indicating both a lower retention of STEM career interest among females and a greater difficulty in attracting females to STEM fields during high school. During the high school years, the percentage of males interested in a STEM career remained stable (from 39.5 to 39.7), whereas for females it declined from 15.7 to 12.7. The students' initial specific (disciplinary) career interests were found to influence the stability of their interest in a STEM career, with those interested in physics careers at the start of high school having the highest retention in STEM. (c) 2012 Wiley Periodicals, Inc. Sci Ed 96:411-427, 2012
C1 [Sadler, Philip M.; Sonnert, Gerhard] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hazari, Zahra] Clemson Univ, Dept Engn & Sci Educ, Clemson, SC 29634 USA.
[Hazari, Zahra] Clemson Univ, Dept Math Sci, Clemson, SC 29634 USA.
[Tai, Robert] Univ Virginia, Curry Sch Educ, Charlottesville, VA 22903 USA.
RP Sadler, PM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM psadler@cfa.harvard.edu
NR 57
TC 56
Z9 56
U1 11
U2 59
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0036-8326
J9 SCI EDUC
JI Sci. Educ.
PD MAY
PY 2012
VL 96
IS 3
BP 411
EP 427
DI 10.1002/sce.21007
PG 17
WC Education & Educational Research
SC Education & Educational Research
GA 924UI
UT WOS:000302716400003
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI THE GREEN MUSEUM
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 MAY
PY 2012
VL 43
IS 2
BP 12
EP 12
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 126SQ
UT WOS:000317641900002
ER
PT J
AU Lenky, C
Eisert, R
Oftedal, OT
Metcalf, V
AF Lenky, Crystal
Eisert, Regina
Oftedal, Olav T.
Metcalf, Victoria
TI Proximate composition and energy density of nototheniid and myctophid
fish in McMurdo Sound and the Ross Sea, Antarctica
SO POLAR BIOLOGY
LA English
DT Article
DE Dissostichus mawsoni; Proximate composition; Nototheniid; Diet; Ross
Sea; Weddell seal
ID WEDDELL SEALS; MACQUARIE ISLAND; WAX ESTERS; FATTY-ACID; FUR SEALS;
FOOD-WEB; LEPTONYCHOTES-WEDDELLII; ECOLOGICAL IMPLICATIONS; MESOPELAGIC
FISHES; KERGUELEN ISLANDS
AB Nototheniid and myctophid fish are primary prey for marine piscivores, yet little is known about their nutritional value. In this study, we characterized the proximate composition [PC: water, fat (neutral lipids), crude protein (CP) and ash] and energy density (ED; kJ g(-1)) of fifteen fish species from McMurdo Sound and the Ross Sea, Antarctica. We assayed the entire fish for all species except for the large Antarctic toothfish, Dissostichus mawsoni (muscle tissue only). On a wet mass basis (WM), fish were variable in composition: moisture content ranged from 64.9 to 87.3% WM, fat from 0.5 to 17.4% WM, CP from 7.7 to 16.7% WM, ash from 11.2 to 21.0% FFDM (fat-free dry mass), and ED from 2.9 to 10.3 kJ g(-1). Myctophids and pelagic nototheniids such as Pleuragramma antarcticum and D. mawsoni were high in fat content (7-17% WM), while a bathylagid and benthic nototheniids including most Trematomus spp. and Lepidonotothen squamifrons were low in fat (0.5-4% WM). The epibenthic Trematomus species (T. eulepidotus and T. lepidorhinus) were intermediate. Energy density tracked fat content, with highest values in myctophids and pelagic nototheniids. The variation in nutrient and energy density confirms that prey composition must be taken into account when modelling energy and nutrient fluxes within the Antarctic ecosystem. Further analyses of prey collected over a number of different locations and seasons are needed in order to determine how the nutritional value of certain species might affect annual or decadal variation in reproductive success or population size of top predators.
C1 [Lenky, Crystal; Eisert, Regina] Univ Canterbury, Christchurch, New Zealand.
[Eisert, Regina; Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Metcalf, Victoria] Lincoln Univ, Dept Wine Food & Mol Biosci, Canterbury, New Zealand.
RP Lenky, C (reprint author), Univ Canterbury, Private Bag 4800, Christchurch, New Zealand.
EM crystal.lenky@pg.canterbury.ac.nz
RI Metcalf, Victoria/C-1933-2013;
OI Metcalf, Victoria/0000-0002-0833-7965
FU National Science Foundation, Office of Polar Programs [0538592]
FX We would like to thank Dr. Gretchen Hofmann (University of California
Santa Barbara, Santa Barbara, CA), Dr. Art DeVries (University of
Illinois, Urbana-Champaign, IL), and Dr. Matt Pinkerton (National
Institute of Water and Atmospheric Research, Wellington, New Zealand)
for providing samples. Specimens and data collected by and made
available through the New Zealand International Polar Year-Census of
Antarctic Marine Life Project are gratefully acknowledged. We would also
like to thank Michael Jakubasz (Smithsonian National Zoological Park)
for his help with all of the assays, Luis Apiolaza (University of
Canterbury) for statistical advice and David Ainley and Graham Worthy
for their comments on an earlier version of this manuscript. This
manuscript was greatly improved by comments from three anonymous
reviewers. This work was supported by the National Science Foundation,
Office of Polar Programs grant 0538592 to Oftedal, Eisert and DJ Boness.
NR 54
TC 9
Z9 9
U1 3
U2 30
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0722-4060
J9 POLAR BIOL
JI Polar Biol.
PD MAY
PY 2012
VL 35
IS 5
BP 717
EP 724
DI 10.1007/s00300-011-1116-9
PG 8
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 921MB
UT WOS:000302480600007
ER
PT J
AU Sohn, JC
Labandeira, C
Davis, D
Mitter, C
AF Sohn, Jae-Cheon
Labandeira, Conrad
Davis, Donald
Mitter, Charles
TI An annotated catalog of fossil and subfossil Lepidoptera (Insecta:
Holometabola) of the world
SO ZOOTAXA
LA English
DT Article
DE Nomenclature; paleobiodiversity; paleontology; plant-insect
interactions; taxonomy
ID BALTIC AMBER; DOMINICAN AMBER; NORTH-AMERICA; LEAF MINES; FEEDING
DAMAGE; NEW-ZEALAND; OAK LEAF; PLANT; EOCENE; MOTH
AB In this catalog, we attempt to assemble all fossil records of Lepidoptera described formally or informally in the world literature. A total of 667 records dealing with at least 4,568 specimens have been compiled. They include descriptions of 131 fossil genera and 229 fossil species, as well as 72 extant genera and 21 extant species to which some of these fossils supposedly belong or show superficial similarity. Replacement names of two fossil genera are proposed to avoid homonymy: Baltopsyche Sohn, gen. nov. for Palaeopsyche Sobczyk and Kobbert, 2009 and Netoxena Sohn, gen. nov. for Xena Martins-Neto, 1999. New generic combinations are proposed for: Tortrix? destructus Cockerell, 1916, Tortrix florissantanus Cockerell, 1907, and Tortrix sp. sensu Gravenhorst (1835), all three to Tortricites Kozlov, 1988; Pterophorus oligocenicus Bigot, Nel and Nel, 1986, to Merrifieldia Tutt, 1905; Aporia sp. sensu Branscheid (1969) to Pierites Heer, 1849; Noctua spp. sensu Hope (1836) and Lomnicki (1894), both to Noctuites Heer, 1849. Eleven names improperly proposed for lepidopteran fossils are invalidated: Baltonides roeselliformis Skalski in KosmowskaCeranowicz and Popiolek, 1981; Baltodines Kupryjanowicz, 2001; Barbarothea Scudder, 1890; Lepidopterites Piton, 1936; Palaeozygaena Reiss, 1936; Psamateia calipsa Martins-Neto, 2002; Saxibatinca meyi Skalski in Kristensen and Skalski, 1998; Spatalistiforma submerga Skalski, 1976; Thanatites juvenalis Scudder, 1875; Tortricibaltia diakonoffi Skalski, 1976; and Zygaenites Reiss, 1936. An unnecessary subsequent type designation for Pierites Heer, 1849, is discussed. A total of 129 records include lepidopteran fossils which cannot be placed in any taxonomic rank. There also exist at least 25 fossil records which lack any evidence of the supposed lepidopteran association. Misidentified specimens, including 18 fossil genera, 29 fossil species and 12 unnamed fossils, are excluded from Lepidoptera. All the known lepidopteran fossils are annotated by fossil type, specimen deposition, excavation locality, association with plants when present, and geological age. A bibliographic list of lepidopteran fossils is provided.
C1 [Sohn, Jae-Cheon; Labandeira, Conrad; Mitter, Charles] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Sohn, Jae-Cheon; Labandeira, Conrad] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
[Davis, Donald] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA.
RP Sohn, JC (reprint author), Univ Maryland, Dept Entomol, 4112 Plant Sci Bldg, College Pk, MD 20742 USA.
EM jsohn@umd.edu; LABANDEC@si.edu; DAVISD@si.edu; cmitter@umd.edu
RI Yakovlev, Roman/J-7243-2013
FU U.S. National Science Foundation [0531769]
FX We would like to express our cordial appreciation to two anonymous
reviewers for critically editing our manuscript and providing valuable
information that we had missed. We are very grateful to our colleagues
in the Lepidoptera Assembling the Tree of Life project (LepTree) for
much useful advice. We especially thank Joaquin Baixeras (University of
Valencia, Spain), John Brown (United States Department of Agriculture,
Washington DC, USA), Axel Hausmann (Zoological State Collection, Munich,
Germany), Masakazu Hayashi (Hoshizaki Green Foundation, Shimane, Japan),
Akito Kawahara (University of Florida, USA), David Lees (Natural History
Museum, London, United Kingdom), David Smith (retired, United States
Department of Agriculture, Washington DC, USA), Torsten Wappler
(Steinmann Institut fur Geologie, Universitat Bonn, Germany) and Andreas
Zwick (Stuttgart State Museum of Natural History, Germany) for
assistance in locating fossil specimens and references, and for comments
on fossil taxonomy. We are also indebted to many museum curators,
including Martin Gross (Universalmuseum Joanneum, Vienna, Austria),
Mathias Harzhauser (Natural History Museum Vienna, Austria), James Hogan
(Oxford University Museum of Natural History, United Kingdom), Paul
Jeffery (Oxford University Museum of Natural History, United Kingdom),
Michael Krings (Bayerische Staatssammlung fur Palaontologie, Munich,
Germany), Andreas Kroh (Natural History Museum Vienna, Austria),
Christian Neumann (Museum fur Naturkunde, Berlin, Germany), Martin Nose
(Bayerische Staatssammlung fur Palaontologie, Munich, Germany), Claire
Mellish (Natural History Museum, London, United Kingdom), Philip D.
Perkins (Museum of Comparative Zoology, Harvard University, USA), Naomi
Pierce (Museum of Comparative Zoology, Harvard University, USA),
Alexandr P. Rasnitsyn (Palaeontological Institute, Russian Academy of
Sciences, Moscow, Russia), and Irene Zorn (Geological Survey of Austria,
Vienna, Austria). We thank Kim Mitter (University of Maryland, College
Park, USA) for translating Russian literature, Cynthia Parr (United
States Museum of Natural History, Washington DC, USA) and Dana Campbell
(University of Maryland, College Park, USA) for managing the online
content of our fossil project, and April J. Dinwiddie (Yale University,
New Haven, USA) for assistance in assembling raw data. Financial support
was provided by the U.S. National Science Foundation's Assembling the
Tree of Life program, award number 0531769. This is contribution 244 of
the Evolution of Terrestrial Ecosystems consortium of the National
Museum of Natural History, in Washington, D.C.
NR 459
TC 8
Z9 9
U1 3
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 APR 30
PY 2012
IS 3286
BP 1
EP 116
PG 116
WC Zoology
SC Zoology
GA 940HH
UT WOS:000303880100001
ER
PT J
AU Loreau, J
Zhang, P
Dalgarno, A
AF Loreau, Jerome
Zhang, Peng
Dalgarno, Alexander
TI Scattering of nitrogen molecules by silver atoms
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID COUPLED-CLUSTER THEORY; COMPOUND STATE RESONANCES; CONSISTENT
BASIS-SETS; GAUSSIAN-BASIS SETS; POLARIZATION PROPAGATOR; HARTREE-FOCK;
ENERGIES; GROUP-11; SODIUM; BORON
AB We present a quantal study of the rotationally elastic and inelastic scattering of Ag and N-2, with the nitrogen molecule treated as a rigid rotor. The two-dimensional potential energy surface of the AgN2 complex is obtained ab initio by means of the spin unrestricted coupled-cluster method with single, double, and perturbative triple excitations. The global minimum is found to be located at an internuclear distance of 8.13 a(0) and an angle of 127.2 degrees. The long-range part of the potential is constructed from the dynamic electric dipole polarizabilities of Ag and N-2. Elastic, excitation, and relaxation cross sections and rates are calculated for energies between 0.1 and 5000 cm(-1). The momentum transfer cross sections and rates are also computed. Finally, we compare the cross sections for Ag-N-2 and Na-N-2 to explore the possibility of using silver instead of sodium in experimental tests. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.3703518]
C1 [Loreau, Jerome; Zhang, Peng; Dalgarno, Alexander] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA.
[Zhang, Peng] Duke Univ, Dept Chem, Durham, NC 27708 USA.
RP Loreau, J (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, 60 Garden St, Cambridge, MA 02138 USA.
EM jloreau@cfa.harvard.edu
OI Loreau, Jerome/0000-0002-6142-1509
FU Belgian American Educational Foundation; Chemical Science, Geoscience,
and Bioscience Division of the Office of Basic Energy Science, Office of
Science, U.S. Department of Energy
FX The authors would like to thank D. Budker for useful discussions as well
as J. Mitroy and H. Sadeghpour for providing us with the dynamical
electric dipole polarizabilities for the Ag atom. J.L. is supported by a
fellowship from the Belgian American Educational Foundation, and the
research of A.D. and P.Z. is supported by the Chemical Science,
Geoscience, and Bioscience Division of the Office of Basic Energy
Science, Office of Science, U.S. Department of Energy.
NR 33
TC 4
Z9 4
U1 1
U2 12
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD APR 28
PY 2012
VL 136
IS 16
AR 164305
DI 10.1063/1.3703518
PG 8
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 936PJ
UT WOS:000303602200019
PM 22559480
ER
PT J
AU McLaughlin, BM
Ballance, CP
AF McLaughlin, B. M.
Ballance, C. P.
TI Photoionization cross section calculations for the halogen-like ions Kr+
and Xe+
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
ID NEUTRON-CAPTURE ELEMENTS; R-MATRIX THEORY; PLANETARY-NEBULAE; 4D
PHOTOIONIZATION; ATOMIC IONS; RESONANCES; ABUNDANCES; SPECTRA; PROGRAM;
STARS
AB Photoionization cross section calculations on the halogen-like ions; Kr+ and Xe+ have been performed for a photon energy range from each ion threshold to 15 eV, using large-scale close-coupling calculations within the Dirac-Coulomb R-matrix approximation. The results from our theoretical work are compared with recent measurements made at the ASTRID merged-beam set-up at the University of Aarhus in Denmark and from the Fourier transform ion cyclotron resonance trap method at the SOLEIL synchrotron radiation facility in Saint-Aubin, France Bizau et al (2011 J. Phys. B: At. Mol. Opt. Phys. 44 055205) and the advanced light source Muller (2012 private communication), Aguliar et al (2012 J. Phys.: Conf. Ser. at press). For each of these complex ions our theoretical cross section results over the photon energy range investigated are seen to be in excellent agreement with experiment. Resonance energy positions and quantum defects of the prominent Rydberg resonances series identified in the spectra are compared with experiment for these complex halogen-like ions.
C1 [McLaughlin, B. M.] Queens Univ Belfast, Ctr Theoret Atom Mol & Opt Phys, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
[Ballance, C. P.] Auburn Univ, Dept Phys, Allison Lab 206, Auburn, AL 36849 USA.
RP McLaughlin, BM (reprint author), Queens Univ Belfast, Ctr Theoret Atom Mol & Opt Phys, Sch Math & Phys, David Bates Bldg,7 Coll Pk, Belfast BT7 1NN, Antrim, North Ireland.
EM b.mclaughlin@qub.ac.uk; ballance@physics.auburn.edu
FU US Department of Energy (DoE) through Auburn University; US National
Science Foundation at the Harvard-Smithsonian Center for Astrophysics
FX CPB was supported by US Department of Energy (DoE) grants through Auburn
University. BMM acknowledges support by the US National Science
Foundation through a grant to ITAMP at the Harvard-Smithsonian Center
for Astrophysics. We thank Dr Jean-Marc Bizau for providing us with the
recent ASTRID/SOLEIL experimental data on these ions and Professor
Alfred Mueller for the ALS experimental data. The computational work was
carried out at the National Energy Research Scientific Computing Center
in Oakland, CA, USA and on the Tera-grid at the National Institute for
Computational Sciences (NICS) in Knoxville, TN, USA.
NR 36
TC 19
Z9 19
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
EI 1361-6455
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD APR 28
PY 2012
VL 45
IS 8
AR 085701
DI 10.1088/0953-4075/45/8/085701
PG 7
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 925RL
UT WOS:000302778700025
ER
PT J
AU Schneps, MH
Brockmole, JR
Sonnert, G
Pomplun, M
AF Schneps, Matthew H.
Brockmole, James R.
Sonnert, Gerhard
Pomplun, Marc
TI History of Reading Struggles Linked to Enhanced Learning in Low Spatial
Frequency Scenes
SO PLOS ONE
LA English
DT Article
ID REPORT SCALE ASRS; DEVELOPMENTAL DYSLEXIA; WORKING-MEMORY;
VISUAL-SEARCH; PERIPHERAL-VISION; CORTICAL DYNAMICS; EYE-MOVEMENTS;
ATTENTION; CHILDREN; ADULTS
AB People with dyslexia, who face lifelong struggles with reading, exhibit numerous associated low-level sensory deficits including deficits in focal attention. Countering this, studies have shown that struggling readers outperform typical readers in some visual tasks that integrate distributed information across an expanse. Though such abilities would be expected to facilitate scene memory, prior investigations using the contextual cueing paradigm failed to find corresponding advantages in dyslexia. We suggest that these studies were confounded by task-dependent effects exaggerating known focal attention deficits in dyslexia, and that, if natural scenes were used as the context, advantages would emerge. Here, we investigate this hypothesis by comparing college students with histories of severe lifelong reading difficulties (SR) and typical readers (TR) in contexts that vary attention load. We find no differences in contextual-cueing when spatial contexts are letter-like objects, or when contexts are natural scenes. However, the SR group significantly outperforms the TR group when contexts are low-pass filtered natural scenes [F(3, 39) = 3.15, p <.05]. These findings suggest that perception or memory for low spatial frequency components in scenes is enhanced in dyslexia. These findings are important because they suggest strengths for spatial learning in a population otherwise impaired, carrying implications for the education and support of students who face challenges in school.
C1 [Schneps, Matthew H.; Sonnert, Gerhard] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA.
[Brockmole, James R.] Univ Notre Dame, Dept Psychol, Notre Dame, IN 46556 USA.
[Pomplun, Marc] Univ Massachusetts, Dept Comp Sci, Boston, MA 02125 USA.
RP Schneps, MH (reprint author), Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, 60 Garden St, Cambridge, MA 02138 USA.
EM mschneps@cfa.harvard.edu
FU National Science Foundation [HRD-0930962]; George E. Burch Foundation
FX This work was supported by National Science Foundation Grant HRD-0930962
(http://www.nsf.gov/awardsearch/showAward.do?AwardNumber = 0930962), and
by the George E. Burch Foundation (http://www.si.edu/ofg/) that provided
a fellowship to MS. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 88
TC 9
Z9 9
U1 2
U2 18
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 27
PY 2012
VL 7
IS 4
AR e35724
DI 10.1371/journal.pone.0035724
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959TJ
UT WOS:000305336000053
PM 22558210
ER
PT J
AU Studds, CE
DeLuca, WV
Baker, ME
King, RS
Marra, PP
AF Studds, Colin E.
DeLuca, William V.
Baker, Matthew E.
King, Ryan S.
Marra, Peter P.
TI Land Cover and Rainfall Interact to Shape Waterbird Community
Composition
SO PLOS ONE
LA English
DT Article
ID CHESAPEAKE BAY; COASTAL URBANIZATION; NITROGEN EXPORT; UNITED-STATES;
RIVER ESTUARY; MARINE; ABUNDANCE; NUTRIENT; USA; CLIMATE
AB Human land cover can degrade estuaries directly through habitat loss and fragmentation or indirectly through nutrient inputs that reduce water quality. Strong precipitation events are occurring more frequently, causing greater hydrological connectivity between watersheds and estuaries. Nutrient enrichment and dissolved oxygen depletion that occur following these events are known to limit populations of benthic macroinvertebrates and commercially harvested species, but the consequences for top consumers such as birds remain largely unknown. We used non-metric multidimensional scaling (MDS) and structural equation modeling (SEM) to understand how land cover and annual variation in rainfall interact to shape waterbird community composition in Chesapeake Bay, USA. The MDS ordination indicated that urban subestuaries shifted from a mixed generalist-specialist community in 2002, a year of severe drought, to generalist-dominated community in 2003, of year of high rainfall. The SEM revealed that this change was concurrent with a sixfold increase in nitrate-N concentration in subestuaries. In the drought year of 2002, waterbird community composition depended only on the direct effect of urban development in watersheds. In the wet year of 2003, community composition depended both on this direct effect and on indirect effects associated with high nitrate-N inputs to northern parts of the Bay, particularly in urban subestuaries. Our findings suggest that increased runoff during periods of high rainfall can depress water quality enough to alter the composition of estuarine waterbird communities, and that this effect is compounded in subestuaries dominated by urban development. Estuarine restoration programs often chart progress by monitoring stressors and indicators, but rarely assess multivariate relationships among them. Estuarine management planning could be improved by tracking the structure of relationships among land cover, water quality, and waterbirds. Unraveling these complex relationships may help managers identify and mitigate ecological thresholds that occur with increasing human land cover.
C1 [Studds, Colin E.; Marra, Peter P.] Smithsonian Inst, Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
[DeLuca, William V.] Univ Massachusetts, Dept Environm Conservat, Amherst, MA 01003 USA.
[Baker, Matthew E.] Univ Maryland, Dept Geog & Environm Syst, Baltimore, MD 21201 USA.
[King, Ryan S.] Baylor Univ, Dept Biol, Ctr Reservoir & Aquat Syst, Waco, TX 76798 USA.
RP Studds, CE (reprint author), Univ Queensland, Sch Biol Sci, Brisbane, Qld, Australia.
EM c.studds@uq.edu.au
RI Studds, Colin/C-3701-2012; Baker, Matthew/I-2839-2014
OI Baker, Matthew/0000-0001-5069-0204
FU United States Environmental Protection Agency's (USEPA) Science to
Achieve Results (STAR) Estuarine and Great Lakes (EaGLe) program
[R-82868401]; USEPA
FX This study was funded by a grant from the United States Environmental
Protection Agency's (USEPA) Science to Achieve Results (STAR) Estuarine
and Great Lakes (EaGLe) program to the Atlantic Slope Consortium, USEPA
Agreement #R-82868401. Although the research described in this article
was funded by the USEPA, it was not subjected to the Agency's peer and
policy review and therefore does not necessarily reflect the views of
the Agency and no official endorsement should be inferred. The funders
has no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.
NR 57
TC 7
Z9 7
U1 6
U2 55
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 27
PY 2012
VL 7
IS 4
AR e35969
DI 10.1371/journal.pone.0035969
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959TJ
UT WOS:000305336000093
PM 22558286
ER
PT J
AU Van Soest, RWM
Boury-Esnault, N
Vacelet, J
Dohrmann, M
Erpenbeck, D
De Voogd, NJ
Santodomingo, N
Vanhoorne, B
Kelly, M
Hooper, JNA
AF Van Soest, Rob W. M.
Boury-Esnault, Nicole
Vacelet, Jean
Dohrmann, Martin
Erpenbeck, Dirk
De Voogd, Nicole J.
Santodomingo, Nadiezhda
Vanhoorne, Bart
Kelly, Michelle
Hooper, John N. A.
TI Global Diversity of Sponges (Porifera)
SO PLOS ONE
LA English
DT Review
ID CANADIAN CONTINENTAL-SHELF; NORTH-EAST ATLANTIC; GREAT-BARRIER-REEF;
CARNIVOROUS SPONGES; CALCAREOUS SPONGES; MEDITERRANEAN SEA;
ASBESTOPLUMA-HYPOGEA; PHYLOGENETIC-SIGNAL; MOLECULAR PHYLOGENY; CRYPTIC
SPECIATION
AB With the completion of a single unified classification, the Systema Porifera (SP) and subsequent development of an online species database, the World Porifera Database (WPD), we are now equipped to provide a first comprehensive picture of the global biodiversity of the Porifera. An introductory overview of the four classes of the Porifera is followed by a description of the structure of our main source of data for this paper, the WPD. From this we extracted numbers of all 'known' sponges to date: the number of valid Recent sponges is established at 8,553, with the vast majority, 83%, belonging to the class Demospongiae. We also mapped for the first time the species richness of a comprehensive set of marine ecoregions of the world, data also extracted from the WPD. Perhaps not surprisingly, these distributions appear to show a strong bias towards collection and taxonomy efforts. Only when species richness is accumulated into large marine realms does a pattern emerge that is also recognized in many other marine animal groups: high numbers in tropical regions, lesser numbers in the colder parts of the world oceans. Preliminary similarity analysis of a matrix of species and marine ecoregions extracted from the WPD failed to yield a consistent hierarchical pattern of ecoregions into marine provinces. Global sponge diversity information is mostly generated in regional projects and resources: results obtained demonstrate that regional approaches to analytical biogeography are at present more likely to achieve insights into the biogeographic history of sponges than a global perspective, which appears currently too ambitious. We also review information on invasive sponges that might well have some influence on distribution patterns of the future.
C1 [Van Soest, Rob W. M.; De Voogd, Nicole J.] Netherlands Ctr Biodivers Naturalis, Leiden, Netherlands.
[Boury-Esnault, Nicole; Vacelet, Jean] Aix Marseille Univ, Ctr Oceanol Marseille, CNRS, DIMAR,UMR 6540, Marseille, France.
[Dohrmann, Martin] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Erpenbeck, Dirk] Univ Munich, Dept Earth & Environm Sci, Munich, Germany.
[Erpenbeck, Dirk] Univ Munich, GeoBioctr LMU, Munich, Germany.
[Santodomingo, Nadiezhda] Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England.
[Vanhoorne, Bart] Flanders Marine Inst VLIZ, Oostende, Belgium.
[Kelly, Michelle] Natl Inst Water & Atmospher Res Ltd, Natl Ctr Aquat Biodivers & Biosecur, Auckland, New Zealand.
[Hooper, John N. A.] Queensland Museum, Brisbane, Qld, Australia.
[Hooper, John N. A.] Griffiths Univ, Eskitis Inst Cell & Mol Therapies, Gold Coast, Qld, Australia.
RP Van Soest, RWM (reprint author), Netherlands Ctr Biodivers Naturalis, Leiden, Netherlands.
EM rob.vansoest@ncbnaturalis.nl
RI de Voogd, Nicole/I-9280-2012;
OI de Voogd, Nicole/0000-0002-7985-5604; Hooper, John/0000-0003-1722-5954
NR 171
TC 109
Z9 111
U1 6
U2 97
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 27
PY 2012
VL 7
IS 4
AR e35105
DI 10.1371/journal.pone.0035105
PG 23
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959TJ
UT WOS:000305336000024
PM 22558119
ER
PT J
AU Mah, CL
Blake, DB
AF Mah, Christopher L.
Blake, Daniel B.
TI Global Diversity and Phylogeny of the Asteroidea (Echinodermata)
SO PLOS ONE
LA English
DT Review
ID SEA STARS LEPTASTERIAS; OF-THORNS STARFISH; INTERTIDAL COMMUNITY
STRUCTURE; STICHASTER-AUSTRALIS VERRILL; SOFT-SEDIMENT ASSEMBLAGES;
HIGH-DISPERSAL STARFISH; PHOTOPERIODIC REGULATION; NEW-ZEALAND;
FEEDING-BEHAVIOR; ASTERIAS-AMURENSIS
AB Members of the Asteroidea (phylum Echinodermata), popularly known as starfish or sea stars, are ecologically important and diverse members of marine ecosystems in all of the world's oceans. We present a comprehensive overview of diversity and phylogeny as they have figured into the evolution of the Asteroidea from Paleozoic to the living fauna. Living post-Paleozoic asteroids, the Neoasteroidea, are morphologically separate from those in the Paleozoic. Early Paleozoic asteroid faunas were diverse and displayed morphology that foreshadowed later living taxa. Preservation presents significant difficulties, but fossil occurrence and current accounts suggests a diverse Paleozoic fauna, which underwent extinction around the Permian-Triassic interval was followed by re-diversification of at least one surviving lineage. Ongoing phylogenetic classification debates include the status of the Paxillosida and the Concentricycloidea. Fossil and molecular evidence has been and continues to be part of the ongoing evolution of asteroid phylogenetic research. The modern lineages of asteroids include the Valvatacea, the Forcipulatacea, the Spinlosida, and the Velatida. We present an overview of diversity in these taxa, as well as brief notes on broader significance, ecology, and functional morphology of each. Although much asteroid taxonomy is stable, many new taxa remain to be discovered with many new species currently awaiting description. The Goniasteridae is currently one of the most diverse families within the Asteroidea. New data from molecular phylogenetics and the advent of global biodiversity databases, such as the World Asteroidea Database (http://www.marinespecies.org/Asteroidea/) present important new springboards for understanding the global biodiversity and evolution of asteroids.
C1 [Mah, Christopher L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Mah, Christopher L.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Blake, Daniel B.] Univ Illinois, Dept Geol, Urbana, IL USA.
RP Mah, CL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
EM mahch@si.edu
FU National Science Foundation [1036358]
FX This publication has been supported by National Science Foundation
1036358 Assembling the Echinoderm Tree of Life grant to Louisiana State
University. The funders had no role in study design, data collection and
analysis, decision to publish, or preparation of the manuscript.
NR 275
TC 23
Z9 23
U1 5
U2 83
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 27
PY 2012
VL 7
IS 4
AR e35644
DI 10.1371/journal.pone.0035644
PG 22
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959TJ
UT WOS:000305336000043
PM 22563389
ER
PT J
AU Arnold, T
Mealey, C
Leahey, H
Miller, AW
Hall-Spencer, JM
Milazzo, M
Maers, K
AF Arnold, Thomas
Mealey, Christopher
Leahey, Hannah
Miller, A. Whitman
Hall-Spencer, Jason M.
Milazzo, Marco
Maers, Kelly
TI Ocean Acidification and the Loss of Phenolic Substances in Marine Plants
SO PLOS ONE
LA English
DT Article
ID EELGRASS ZOSTERA-MARINA; SEAGRASS POSIDONIA-OCEANICA; CARBON-DIOXIDE;
ELEVATED CO2; HERBIVORE INTERACTIONS; INORGANIC CARBON; WASTING DISEASE;
LABYRINTHULA-ZOSTERAE; THALASSIA-TESTUDINUM; PROTEIN COMPETITION
AB Rising atmospheric CO2 often triggers the production of plant phenolics, including many that serve as herbivore deterrents, digestion reducers, antimicrobials, or ultraviolet sunscreens. Such responses are predicted by popular models of plant defense, especially resource availability models which link carbon availability to phenolic biosynthesis. CO2 availability is also increasing in the oceans, where anthropogenic emissions cause ocean acidification, decreasing seawater pH and shifting the carbonate system towards further CO2 enrichment. Such conditions tend to increase seagrass productivity but may also increase rates of grazing on these marine plants. Here we show that high CO2 / low pH conditions of OA decrease, rather than increase, concentrations of phenolic protective substances in seagrasses and eurysaline marine plants. We observed a loss of simple and polymeric phenolics in the seagrass Cymodocea nodosa near a volcanic CO2 vent on the Island of Vulcano, Italy, where pH values decreased from 8.1 to 7.3 and pCO(2) concentrations increased ten-fold. We observed similar responses in two estuarine species, Ruppia maritima and Potamogeton perfoliatus, in in situ Free-Ocean-Carbon-Enrichment experiments conducted in tributaries of the Chesapeake Bay, USA. These responses are strikingly different than those exhibited by terrestrial plants. The loss of phenolic substances may explain the higher-than-usual rates of grazing observed near undersea CO2 vents and suggests that ocean acidification may alter coastal carbon fluxes by affecting rates of decomposition, grazing, and disease. Our observations temper recent predictions that seagrasses would necessarily be "winners" in a high CO2 world.
C1 [Arnold, Thomas; Mealey, Christopher; Leahey, Hannah; Maers, Kelly] Dickinson Coll, Dept Biol Sci, Carlisle, PA 17013 USA.
[Arnold, Thomas; Miller, A. Whitman] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Hall-Spencer, Jason M.] Univ Plymouth, Sch Marine Sci & Engn, Plymouth PL4 8AA, Devon, England.
[Milazzo, Marco] Univ Palermo, Dipartimento Sci Terra & Mare, Palermo, Italy.
RP Arnold, T (reprint author), Dickinson Coll, Dept Biol Sci, Carlisle, PA 17013 USA.
EM arnoldt@dickinson.edu
RI Milazzo, Marco/F-8596-2012
OI Milazzo, Marco/0000-0002-2202-0542
FU NASA [09-GCCE-0139]; Smithsonian Institution; EU [265103]; Dickinson
College
FX This work was funded by an award from NASA (09-GCCE-0139), a senior
postdoctoral fellowship award from the Smithsonian Institution to T. M.
A., the EU 'Mediterranean Sea Acidification under a changing climate'
project (MedSeA; grant agreement 265103), and Research and Development
grants to T. M. A. from Dickinson College. The funders had no role in
study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 80
TC 55
Z9 55
U1 3
U2 113
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 25
PY 2012
VL 7
IS 4
AR e35107
DI 10.1371/journal.pone.0035107
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959VP
UT WOS:000305345200025
PM 22558120
ER
PT J
AU Wilson, LB
Koval, A
Szabo, A
Breneman, A
Cattell, CA
Goetz, K
Kellogg, PJ
Kersten, K
Kasper, JC
Maruca, BA
Pulupa, M
AF Wilson, L. B., III
Koval, A.
Szabo, A.
Breneman, A.
Cattell, C. A.
Goetz, K.
Kellogg, P. J.
Kersten, K.
Kasper, J. C.
Maruca, B. A.
Pulupa, M.
TI Observations of electromagnetic whistler precursors at supercritical
interplanetary shocks
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID EARTHS BOW SHOCK; WIND SPACECRAFT; PERPENDICULAR SHOCKS; MACH NUMBER;
SOLAR-WIND; PLASMA; WAVES; SIMULATIONS; DISSIPATION
AB We present observations of electromagnetic precursor waves, identified as whistler mode waves, at supercritical interplanetary shocks using the Wind search coil magnetometer. The precursors propagate obliquely with respect to the local magnetic field, shock normal vector, solar wind velocity, and they are not phase standing structures. All are right-hand polarized with respect to the magnetic field ( spacecraft frame), and all but one are right-hand polarized with respect to the shock normal vector in the normal incidence frame. They have rest frame frequencies f(ci) < f << f(ce) and wave numbers 0.02 less than or similar to k rho(ce) less than or similar to 5.0. Particle distributions show signatures of specularly reflected gyrating ions, which may be a source of free energy for the observed modes. In one event, we simultaneously observe perpendicular ion heating and parallel electron acceleration, consistent with wave heating/acceleration due to these waves. Although the precursors can have delta B/B-o as large as 2, fluxgate magnetometer measurements show relatively laminar shock transitions in three of the four events. Citation: Wilson, L. B., III, et al. (2012), Observations of electromagnetic whistler precursors at supercritical interplanetary shocks, Geophys. Res. Lett., 39, L08109, doi:10.1029/2012GL051581.
C1 [Wilson, L. B., III; Koval, A.; Szabo, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20707 USA.
[Koval, A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Breneman, A.; Cattell, C. A.; Goetz, K.; Kellogg, P. J.; Kersten, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Kasper, J. C.; Maruca, B. A.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pulupa, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Wilson, LB (reprint author), NASA, Goddard Space Flight Ctr, Code 672, Greenbelt, MD 20707 USA.
EM lynn.b.wilsoniii@gmail.com
RI Kasper, Justin/D-1152-2010; Wilson III, Lynn/D-4425-2012;
OI Kasper, Justin/0000-0002-7077-930X; Wilson III,
Lynn/0000-0002-4313-1970; Pulupa, Marc/0000-0002-1573-7457; Cattell,
Cynthia/0000-0002-3805-320X
FU NESSF [NNX07AU72H, NNX07AI05G]; Leonard Burlaga/Arctowski Medal
Fellowship; NASA [NNX10AT09G]
FX We thank S. D. Bale, J. R. Wygant, and R. Lysak for useful discussions
of the physics involved in our study. All Wind spacecraft data were
produced under Wind MO&DA grants. This research was partially supported
by NESSF grant NNX07AU72H, grant NNX07AI05G, the Leonard
Burlaga/Arctowski Medal Fellowship, and UCB work sponsored by NASA grant
NNX10AT09G.
NR 29
TC 22
Z9 22
U1 2
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 25
PY 2012
VL 39
AR L08109
DI 10.1029/2012GL051581
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 933AF
UT WOS:000303330900005
ER
PT J
AU Osborn, KJ
Kuhnz, LA
Priede, IG
Urata, M
Gebruk, AV
Holland, ND
AF Osborn, Karen J.
Kuhnz, Linda A.
Priede, Imants G.
Urata, Makoto
Gebruk, Andrey V.
Holland, Nicholas D.
TI Diversification of acorn worms (Hemichordata, Enteropneusta) revealed in
the deep sea
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE deep sea; epibenthic; demersal; Enteropneusta; Hemichordata;
Torquaratoridae
ID EASTERN PACIFIC; FLOOR; GENUS; HARRIMANIIDAE; PHYLOGENY; EVOLUTION;
REVISION; INSIGHTS
AB Enteropneusts (phylum Hemichordata), although studied extensively because of their close relationship to chordates, have long been considered shallow-water, burrowing animals. The present paper more than doubles the number of enteropneust species recorded in the deep sea based on high-resolution imaging and sampling with remotely operated vehicles. We provide direct evidence that some enteropneusts are highly mobile-using changes in posture and currents to drift between feeding sites-and are prominent members of deep, epibenthic communities. In addition, we provide ecological information for each species. We also show that despite their great morphological diversity, most deep-living enteropneusts form a single clade (the rediagnosed family Torquaratoridae) on the basis of rDNA sequences and morphology of the proboscis skeleton and stomochord. The phylogenetic position of the torquaratorids indicates that the group, after evolving from near-shore ancestors, radiated extensively in the deep sea.
C1 [Osborn, Karen J.] Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA.
[Kuhnz, Linda A.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA.
[Priede, Imants G.] Univ Aberdeen, Oceanlab, Aberdeen AB41 6AA, Scotland.
[Urata, Makoto] Hiroshima Univ, Marine Biol Lab, Onomichi 7220073, Japan.
[Gebruk, Andrey V.] Russian Acad Sci, PP Shirshov Oceanol Inst, Moscow 117997, Russia.
[Holland, Nicholas D.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
RP Osborn, KJ (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
EM osbornk@si.edu
OI Osborn, Karen/0000-0002-4226-9257
FU David and Lucile Packard Foundation; UK Natural Environment Research
Council
FX We thank Dave Clague, Steve Haddock, Bob Vrijenhoek, Lynne Christianson,
Shannon Johnson, Lonny Lundsten, Ken Smith, Antonina Rogacheva, Bruce
Robison, Mike Vecchione, Susumu Ohtsuka and Sadaharu Iwasaki for
contributions to the project. Steve Hammond, Verena Tunnicliffe and the
NOAA Office of Ocean Exploration and Research provided access to images
from INDEX 2010: Indonesia-USA Deep-Sea Exploration of the Sangihe
Talaud Region expedition. We also thank the pilots and crews of the
abovementioned ROVs and RV Western Flyer, RRS James Cook and Okeanos
Explorer. The Pacific collections were funded by the David and Lucile
Packard Foundation and the North Atlantic collections by the UK Natural
Environment Research Council.
NR 38
TC 26
Z9 27
U1 0
U2 18
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
EI 1471-2954
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD APR 22
PY 2012
VL 279
IS 1733
BP 1646
EP 1654
DI 10.1098/rspb.2011.1916
PG 9
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 906GM
UT WOS:000301332900025
PM 22090391
ER
PT J
AU Pazourek, R
Feist, J
Nagele, S
Burgdorfer, J
AF Pazourek, Renate
Feist, Johannes
Nagele, Stefan
Burgdoerfer, Joachim
TI Attosecond Streaking of Correlated Two-Electron Transitions in Helium
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID DEPENDENT SCHRODINGER-EQUATION; PHASE-SHIFT; TIME; SPECTROSCOPY; DELAY
AB We present fully ab initio simulations of attosecond streaking for ionization of helium accompanied by shakeup of the second electron. This process represents a prototypical case for strongly correlated electron dynamics on the attosecond time scale. We show that streaking spectroscopy can provide detailed information on the Eisenbud-Wigner-Smith time delay as well as on the infrared-field dressing of both bound and continuum states. We find a novel contribution to the streaking delay that stems from the interplay of electron-electron and infrared-field interactions in the exit channel. We quantify all the contributions with attosecond precision and provide a benchmark for future experiments.
C1 [Pazourek, Renate; Nagele, Stefan; Burgdoerfer, Joachim] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria.
[Feist, Johannes] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Pazourek, R (reprint author), Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria.
EM renate.pazourek@tuwien.ac.at; stefan.nagele@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 [P21141-N16, P23359-N16]; COST Action [CM0702]; National
Science Foundation through TeraGrid/XSEDE resources [TG-PHY090031]; TU
Vienna Doctoral Program Functional Matter; NSF; [SFB 041]
FX This work was supported by the FWF-Austria, Grant No. P21141-N16,
P23359-N16, and SFB 041 (VICOM), the COST Action CM0702 (CUSPFEL), and
in part by the National Science Foundation through TeraGrid/XSEDE
resources provided by NICS and TACC under Grant TG-PHY090031. The
computational results presented have also been achieved in part using
the Vienna Scientific Cluster (VSC). R. P. acknowledges support by the
TU Vienna Doctoral Program Functional Matter and J.F. acknowledges
support by the NSF through a grant to ITAMP.
NR 36
TC 54
Z9 54
U1 1
U2 30
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 APR 20
PY 2012
VL 108
IS 16
AR 163001
DI 10.1103/PhysRevLett.108.163001
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 929MY
UT WOS:000303070600006
PM 22680715
ER
PT J
AU Bromley, BC
Kenyon, SJ
Geller, MJ
Brown, WR
AF Bromley, Benjamin C.
Kenyon, Scott J.
Geller, Margaret J.
Brown, Warren R.
TI BINARY DISRUPTION BY MASSIVE BLACK HOLES: HYPERVELOCITY STARS, S STARS,
AND TIDAL DISRUPTION EVENTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: stellar content;
Galaxy: structure; stars: early-type
ID SAGITTARIUS-A-ASTERISK; N-BODY SIMULATIONS; GALACTIC-CENTER; YOUNG
STARS; GALAXY; FLARES; VELOCITIES; EJECTION; HISTORY; CLUSTER
AB We examine whether disrupted binary stars can fuel black hole growth. In this mechanism, tidal disruption produces a single hypervelocity star (HVS) ejected at high velocity and a former companion star bound to the black hole. After a cluster of bound stars forms, orbital diffusion allows the black hole to accrete stars by tidal disruption at a rate comparable to the capture rate. In the Milky Way, HVSs and the S star cluster imply similar rates of 10(-5) to 10(-3) yr(-1) for binary disruption. These rates are consistent with estimates for the tidal disruption rate in nearby galaxies and imply significant black hole growth from disrupted binaries on 10 Gyr timescales.
C1 [Bromley, Benjamin C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Kenyon, Scott J.; Geller, Margaret J.; Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Bromley, BC (reprint author), Univ Utah, Dept Phys & Astron, 115 S 1400 E,Rm 201, Salt Lake City, UT 84112 USA.
EM bromley@physics.utah.edu; skenyon@cfa.harvard.edu;
mgeller@cfa.harvard.edu; wbrown@cfa.harvard.edu
OI Kenyon, Scott/0000-0003-0214-609X
NR 50
TC 17
Z9 17
U1 0
U2 2
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 APR 20
PY 2012
VL 749
IS 2
AR L42
DI 10.1088/2041-8205/749/2/L42
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 923SD
UT WOS:000302638300026
ER
PT J
AU Wilner, DJ
Andrews, SM
MacGregor, MA
Hughes, AM
AF Wilner, David J.
Andrews, Sean M.
MacGregor, Meredith A.
Hughes, A. Meredith
TI A RESOLVED MILLIMETER EMISSION BELT IN THE AU Mic DEBRIS DISK
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; planet-disk interactions; stars: individual (AU
Microscopii); submillimeter: planetary systems
ID MICROSCOPII CIRCUMSTELLAR DISK; NEARBY YOUNG STARS; BETA-PICTORIS; DUST
DYNAMICS; PLANETS; SEARCH; EVOLUTION; DISCOVERY; PROFILES; DENSITY
AB We present imaging observations at 1.3 mm of the debris disk surrounding the nearby M-type flare star AU Mic with beam size 3 '' (30 AU) from the Submillimeter Array. These data reveal a belt of thermal dust emission surrounding the star with the same edge-on geometry as the more extended scattered light disk detected at optical wavelengths. Simple modeling indicates a central radius of similar to 35 AU for the emission belt. This location is consistent with the reservoir of planetesimals previously invoked to explain the shape of the scattered light surface brightness profile through size-dependent dust dynamics. The identification of this belt further strengthens the kinship between the debris disks around AU Mic and its more massive sister star beta Pic, members of the same similar to 10 Myr old moving group.
C1 [Wilner, David J.; Andrews, Sean M.; MacGregor, Meredith A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hughes, A. Meredith] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Wilner, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI MacGregor, Meredith/0000-0001-7891-8143
FU Miller Institute for Basic Research in Science
FX We thank James Graham for providing the Hubble Space Telescope image in
Figure 1. A.M.H. is supported by a fellowship from the Miller Institute
for Basic Research in Science.
NR 34
TC 17
Z9 17
U1 0
U2 2
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 APR 20
PY 2012
VL 749
IS 2
AR L27
DI 10.1088/2041-8205/749/2/L27
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 923SD
UT WOS:000302638300011
ER
PT J
AU Appelquist, T
Babich, R
Brower, RC
Buchoff, MI
Cheng, M
Clark, MA
Cohen, SD
Fleming, GT
Kiskis, J
Lin, MF
Neil, ET
Osborn, JC
Rebbi, C
Schaich, D
Syritsyn, S
Voronov, G
Vranas, P
Wasem, J
AF Appelquist, T.
Babich, R.
Brower, R. C.
Buchoff, M. I.
Cheng, M.
Clark, M. A.
Cohen, S. D.
Fleming, G. T.
Kiskis, J.
Lin, M. F.
Neil, E. T.
Osborn, J. C.
Rebbi, C.
Schaich, D.
Syritsyn, S.
Voronov, G.
Vranas, P.
Wasem, J.
TI WW scattering parameters via pseudoscalar phase shifts
SO PHYSICAL REVIEW D
LA English
DT Article
ID CHIRAL PERTURBATION-THEORY; FLAVORS; LATTICE; SYSTEM
AB Using domain-wall lattice simulations, we study pseudoscalar-pseudoscalar scattering in the maximal isospin channel for an SU(3) gauge theory with two and six fermion flavors in the fundamental representation. This calculation of the S-wave scattering length is related to the next-to-leading order corrections to WW scattering in technicolor models through the low-energy coefficients of the chiral Lagrangian. While two- and six-flavor scattering lengths are similar for a fixed ratio of the pseudoscalar mass to its decay constant, six-flavor scattering shows a somewhat less repulsive next-to-leading order interaction than its two-flavor counterpart. Estimates are made for the WW scattering parameters and the plausibility of detection is discussed.
C1 [Appelquist, T.; Fleming, G. T.; Lin, M. F.; Voronov, G.] Yale Univ, Dept Phys, Sloane Lab, New Haven, CT 06520 USA.
[Babich, R.; Brower, R. C.; Rebbi, C.; Schaich, D.] Boston Univ, Dept Phys, Boston, MA 02215 USA.
[Buchoff, M. I.; Cheng, M.; Vranas, P.; Wasem, J.] Lawrence Livermore Natl Lab, Phys Sci Directorate, Livermore, CA 94550 USA.
[Clark, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cohen, S. D.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Kiskis, J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Neil, E. T.] Fermilab Natl Accelerator Lab, Dept Theoret Phys, Batavia, IL 60510 USA.
[Osborn, J. C.] Argonne Leadership Comp Facil, Argonne, IL 60439 USA.
[Schaich, D.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Syritsyn, S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Appelquist, T (reprint author), Yale Univ, Dept Phys, Sloane Lab, New Haven, CT 06520 USA.
RI Schaich, David/J-6644-2013; Fleming, George/L-6614-2013;
OI Schaich, David/0000-0002-9826-2951; Fleming, George/0000-0002-4987-7167;
Cohen, Saul/0000-0001-6804-3320
FU NNSA; Office of Science of the U. S. Department of Energy; U. S.
National Science Foundation; United States Department of Energy
[DE-AC02-07CH11359]
FX This work was performed with the aid of Chroma [36] and CPS. We thank
Tom Luu, Andre Walker-Loud, and Brian Tiburzi for helpful insight
throughout this work. We thank the LLNL Multiprogrammatic and
Institutional Computing program for time on the BlueGene/L supercomputer
and on the Hera, Atlas, and Zeus computing clusters along with funding
from LDRD 10-ERD-033. This work was supported by the NNSA and Office of
Science of the U. S. Department of Energy, and by the U. S. National
Science Foundation. Fermilab is operated by Fermi Research Alliance,
LLC, under Contract No. DE-AC02-07CH11359 with the United States
Department of Energy.
NR 36
TC 6
Z9 6
U1 0
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD APR 19
PY 2012
VL 85
IS 7
AR 074505
DI 10.1103/PhysRevD.85.074505
PG 8
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 928PB
UT WOS:000302994100005
ER
PT J
AU Machida, RJ
Kweskin, M
Knowlton, N
AF Machida, Ryuji J.
Kweskin, Matthew
Knowlton, Nancy
TI PCR Primers for Metazoan Mitochondrial 12S Ribosomal DNA Sequences
SO PLOS ONE
LA English
DT Article
ID RNA GENE; DIVERSITY; BIOSPHERE; REGIONS
AB Background: Assessment of the biodiversity of communities of small organisms is most readily done using PCR-based analysis of environmental samples consisting of mixtures of individuals. Known as metagenetics, this approach has transformed understanding of microbial communities and is beginning to be applied to metazoans as well. Unlike microbial studies, where analysis of the 16S ribosomal DNA sequence is standard, the best gene for metazoan metagenetics is less clear. In this study we designed a set of PCR primers for the mitochondrial 12S ribosomal DNA sequence based on 64 complete mitochondrial genomes and then tested their efficacy.
Methodology/Principal Findings: A total of the 64 complete mitochondrial genome sequences representing all metazoan classes available in GenBank were downloaded using the NCBI Taxonomy Browser. Alignment of sequences was performed for the excised mitochondrial 12S ribosomal DNA sequences, and conserved regions were identified for all 64 mitochondrial genomes. These regions were used to design a primer pair that flanks a more variable region in the gene. Then all of the complete metazoan mitochondrial genomes available in NCBI's Organelle Genome Resources database were used to determine the percentage of taxa that would likely be amplified using these primers. Results suggest that these primers will amplify target sequences for many metazoans.
Conclusions/Significance: Newly designed 12S ribosomal DNA primers have considerable potential for metazoan metagenetic analysis because of their ability to amplify sequences from many metazoans.
C1 [Machida, Ryuji J.; Kweskin, Matthew; Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Machida, RJ (reprint author), Acad Sinica, Biodivers Res Ctr, Taipei 115, Taiwan.
EM ryujimachida@gate.sinica.edu.tw
FU Alfred P. Sloan Foundation; Sant Chair of Marine Science
FX Financial support was provided by the Alfred P. Sloan Foundation and the
Sant Chair of Marine Science discretionary funds. The funders had no
role in study design, data collection and analysis, decision to publish,
or preparation of the manuscript.
NR 25
TC 12
Z9 12
U1 0
U2 11
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 19
PY 2012
VL 7
IS 4
AR e35887
DI 10.1371/journal.pone.0035887
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 959TL
UT WOS:000305336200070
PM 22536450
ER
PT J
AU Montes, C
Bayona, G
Cardona, A
Buchs, DM
Silva, CA
Moron, S
Hoyos, N
Ramirez, DA
Jaramillo, CA
Valencia, V
AF Montes, Camilo
Bayona, G.
Cardona, A.
Buchs, D. M.
Silva, C. A.
Moron, S.
Hoyos, N.
Ramirez, D. A.
Jaramillo, C. A.
Valencia, V.
TI Arc-continent collision and orocline formation: Closing of the Central
American seaway
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID SOUTHERN CENTRAL-AMERICA; LARGE IGNEOUS PROVINCE; PANAMA DEFORMED BELT;
EL-VALLE VOLCANO; COSTA-RICA; PALEOMAGNETIC DATA; CARIBBEAN PLATE;
TECTONIC EVOLUTION; WESTERN COLOMBIA; EASTERN PANAMA
AB Closure of the Central American seaway was a local tectonic event with potentially global biotic and environmental repercussions. We report geochronological (six U/Pb LA-ICP-MS zircon ages) and geochemical (19 XRF and ICP-MS analyses) data from the Isthmus of Panama that allow definition of a distinctive succession of plateau sequences to subduction-related protoarc to arc volcaniclastic rocks intruded by Late Cretaceous to middle Eocene intermediate plutonic rocks (67.6 +/- 1.4 Ma to 41.1 +/- 0.7 Ma). Paleomagnetic analyses (24 sites, 192 cores) in this same belt reveal large counterclockwise vertical-axis rotations (70.9 degrees +/- 6.7 degrees), and moderate clockwise rotations (between 40 degrees +/- 4.1 degrees and 56.2 degrees +/- 11.1 degrees) on either side of an east-west trending fault at the apex of the Isthmus (Rio Gatun Fault), consistent with Isthmus curvature. An Oligocene-Miocene arc crosscuts the older, deformed and segmented arc sequences, and shows no significant vertical-axis rotation or deformation. There are three main stages of deformation: 1) left-lateral, strike-slip offset of the arc (similar to 100 km), and counterclockwise vertical-axis rotation of western arc segments between 38 and 28 Ma; 2) clockwise rotation of central arc segments between 28 and 25 Ma; and 3) orocline tightening after 25 Ma. When this reconstruction is placed in a global plate tectonic framework, and published exhumation data is added, the Central American seaway disappears at 15 Ma, suggesting that by the time of northern hemisphere glaciation, deep-water circulation had long been severed in Central America.
C1 [Montes, Camilo; Cardona, A.; Hoyos, N.; Ramirez, D. A.; Jaramillo, C. A.] Smithsonian Trop Res Inst, Balboa, Panama.
[Montes, Camilo] Univ Los Andes, Bogota, Colombia.
[Bayona, G.] Corp Geol Ares, Bogota, Colombia.
[Cardona, A.] Univ Nacl Colombia, Medellin, Colombia.
[Buchs, D. M.] Helmholtz Ctr Ocean Res Kiel, GEOMAR, Res Div Dynam Ocean Floor 4, D-24148 Kiel, Germany.
[Silva, C. A.] Oklahoma State Univ, Dept Geol, Stillwater, OK 74078 USA.
[Moron, S.] Univ Minnesota, Dept Geol, Minneapolis, MN 55455 USA.
[Valencia, V.] Washington State Univ, Dept Earth & Environm Sci, Pullman, WA 99164 USA.
RP Montes, C (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama.
EM cmontes@uniandes.edu.co
OI Ramirez, Diego/0000-0001-6018-3273; Buchs, David/0000-0001-8866-8125;
Montes, Camilo/0000-0002-3553-0787
FU Panama Canal Authority [SAA-199520-KRP]; Senacyt [SUM-07-001, EST010-080
A]; U.S. National Science Foundation (NSF) [0966884]; Colciencias; Swiss
National Science Foundation [PBLA2-122660]; NSF EAR [0824299]; National
Geographic; Smithsonian Institution; Ricardo Perez S.A.
FX Project supported by Panama Canal Authority contract SAA-199520-KRP;
Mark Tupper; Senacyt grants SUM-07-001 and EST010-080 A; U.S. National
Science Foundation (NSF) grant 0966884 (OISE, EAR, DRL); Colciencias;
Swiss National Science Foundation (project PBLA2-122660); NSF EAR
0824299; National Geographic; Smithsonian Institution; and Ricardo Perez
S.A. Thanks to J.E.T. Channell, K. Huang, S. Zapata, R. Arculus, C.
Allen, A. Christy and U. Troitzsch. Access and collection permits were
granted by Panama Canal Authority and Ministerio de Industria y
Comercio. We are grateful to all participants of February's 2010 joint
workshop IGCP 546 "Subduction Zones of the Caribbean" and 574 "Bending
and Bent Orogens, and Continental Ribbons." Thanks to G. Worner, J.
Pindell, S. Johnson, P. Molnar, R. Somoza, and P. Mann for their reviews
and comments to our manuscript as it evolved.
NR 99
TC 63
Z9 65
U1 3
U2 57
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD APR 18
PY 2012
VL 117
AR B04105
DI 10.1029/2011JB008959
PG 25
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 930DG
UT WOS:000303116500001
ER
PT J
AU Chen, HX
Sun, SC
Sundberg, P
Ren, WC
Norenburg, JL
AF Chen, Hai-Xia
Sun, Shi-Chun
Sundberg, Per
Ren, Wei-Cheng
Norenburg, Jon L.
TI A comparative study of nemertean complete mitochondrial genomes,
including two new ones for Nectonemertes cf. mirabilis and Zygeupolia
rubens, may elucidate the fundamental pattern for the phylum Nemertea
SO BMC GENOMICS
LA English
DT Article
DE MtDNA; Nemertea; Nectonemertes mirabilis; Zygeupolia rubens; Phylogeny;
Gene rearrangement
ID MULTIPLE SEQUENCE ALIGNMENT; 18S RDNA SEQUENCES; TRANSFER-RNA GENES;
PHYLOGENETIC POSITION; DNA-SEQUENCE; SECONDARY STRUCTURES; TANDEM
REPEATS; MIXED MODELS; EVOLUTION; ORDER
AB Background: The mitochondrial genome is important for studying genome evolution as well as reconstructing the phylogeny of organisms. Complete mitochondrial genome sequences have been reported for more than 2200 metazoans, mainly vertebrates and arthropods. To date, from a total of about 1275 described nemertean species, only three complete and two partial mitochondrial DNA sequences from nemerteans have been published. Here, we report the entire mitochondrial genomes for two more nemertean species: Nectonemertes cf. mirabilis and Zygeupolia rubens.
Results: The sizes of the entire mitochondrial genomes are 15365 bp for N. cf. mirabilis and 15513 bp for Z. rubens. Each circular genome contains 37 genes and an AT-rich non-coding region, and overall nucleotide composition is AT-rich. In both species, there is significant strand asymmetry in the distribution of nucleotides, with the coding strand being richer in T than A and in G than C. The AT-rich non-coding regions of the two genomes have some repeat sequences and stem-loop structures, both of which may be associated with the initiation of replication or transcription. The 22 tRNAs show variable substitution patterns in nemerteans, with higher sequence conservation in genes located on the H strand. Gene arrangement of N. cf. mirabilis is identical to that of Paranemertes cf. peregrina, both of which are Hoplonemertea, while that of Z. rubens is the same as in Lineus viridis, both of which are Heteronemertea. Comparison of the gene arrangements and phylogenomic analysis based on concatenated nucleotide sequences of the 12 mitochondrial protein-coding genes revealed that species with closer relationships share more identical gene blocks.
Conclusion: The two new mitochondrial genomes share many features, including gene contents, with other known nemertean mitochondrial genomes. The tRNA families display a composite substitution pathway. Gene order comparison to the proposed ground pattern of Bilateria and some lophotrochozoans suggests that the nemertean ancestral mitochondrial gene order most closely resembles the heteronemertean type. Phylogenetic analysis proposes a sister-group relationship between Hetero- and Hoplonemertea, which supports one of two recent alternative hypotheses of nemertean phylogeny.
C1 [Norenburg, Jon L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Chen, Hai-Xia; Sundberg, Per] Univ Gothenburg, Dept Biol & Environm Sci, SE-40530 Gothenburg, Sweden.
[Chen, Hai-Xia; Sun, Shi-Chun] Ocean Univ China, Inst Evolut & Marine Biodivers, Qingdao 266003, Peoples R China.
[Ren, Wei-Cheng] Univ Gothenburg, Sahlgrenska Acad, Dept Rheumatol & Inflammat Res, SE-40530 Gothenburg, Sweden.
RP Norenburg, JL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
EM norenburgj@si.edu
RI Norenburg, Jon/K-3481-2015
OI Norenburg, Jon/0000-0001-7776-1527
FU National Natural Science Foundation of China [30970333]; Swedish
Research Council; Smithsonian Institution Scholarly Studies, Research
Opportunities, and Marine Science Network; Smithsonian Marine Station at
Fort Pierce; US National Science Foundation
FX This work was supported by the National Natural Science Foundation of
China (to SCS, grant no. 30970333,), the Swedish Research Council (to
PS), Smithsonian Institution Scholarly Studies, Research Opportunities,
and Marine Science Network awards (to JLN) and represents contribution
878 of the Smithsonian Marine Station at Fort Pierce. JLN is grateful to
James Childress (UCSB) and his support from the US National Science
Foundation for the opportunity to collect living Nectonemertes cf.
mirabilis.
NR 82
TC 11
Z9 11
U1 1
U2 19
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 APR 17
PY 2012
VL 13
AR 139
DI 10.1186/1471-2164-13-139
PG 18
WC Biotechnology & Applied Microbiology; Genetics & Heredity
SC Biotechnology & Applied Microbiology; Genetics & Heredity
GA 955GO
UT WOS:000305005300001
PM 22507536
ER
EF