FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Ballard, S
Fabrycky, D
Fressin, F
Charbonneau, D
Desert, JM
Torres, G
Marcy, G
Burke, CJ
Isaacson, H
Henze, C
Steffen, JH
Ciardi, DR
Howell, SB
Cochran, WD
Endl, M
Bryson, ST
Rowe, JF
Holman, MJ
Lissauer, JJ
Jenkins, JM
Still, M
Ford, EB
Christiansen, JL
Middour, CK
Haas, MR
Li, J
Hall, JR
McCauliff, S
Batalha, NM
Koch, DG
Borucki, WJ
AF Ballard, Sarah
Fabrycky, Daniel
Fressin, Francois
Charbonneau, David
Desert, Jean-Michel
Torres, Guillermo
Marcy, Geoffrey
Burke, Christopher J.
Isaacson, Howard
Henze, Christopher
Steffen, Jason H.
Ciardi, David R.
Howell, Steven B.
Cochran, William D.
Endl, Michael
Bryson, Stephen T.
Rowe, Jason F.
Holman, Matthew J.
Lissauer, Jack J.
Jenkins, Jon M.
Still, Martin
Ford, Eric B.
Christiansen, Jessie L.
Middour, Christopher K.
Haas, Michael R.
Li, Jie
Hall, Jennifer R.
McCauliff, Sean
Batalha, Natalie M.
Koch, David G.
Borucki, William J.
TI THE KEPLER-19 SYSTEM: A TRANSITING 2.2 R-circle plus PLANET AND A SECOND
PLANET DETECTED VIA TRANSIT TIMING VARIATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; stars: individual (Kepler-19, KOI-84, KIC
2571238)
ID EARTH GJ 1214B; 1ST 4 MONTHS; LIGHT CURVES; TERRESTRIAL PLANETS;
EXTRASOLAR PLANETS; BINARY STARS; INITIAL CHARACTERISTICS; TRANSMISSION
SPECTRUM; PERIOD VARIATIONS; FALSE POSITIVES
AB We present the discovery of the Kepler-19 planetary system, which we first identified from a 9.3 day periodic transit signal in the Kepler photometry. From high-resolution spectroscopy of the star, we find a stellar effective temperature T-eff = 5541 +/- 60 K, a metallicity [Fe/H] = -0.13 +/- 0.06, and a surface gravity log(g) = 4.59 +/- 0.10. We combine the estimate of T-eff and [Fe/H] with an estimate of the stellar density derived from the photometric light curve to deduce a stellar mass of M-star = 0.936 +/- 0.040 M-circle dot and a stellar radius of R-star = 0.850 +/- 0.018 R-circle dot (these errors do not include uncertainties in the stellar models). We rule out the possibility that the transits result from an astrophysical false positive by first identifying the subset of stellar blends that reproduce the precise shape of the light curve. Using the additional constraints from the measured color of the system, the absence of a secondary source in the high-resolution spectrum, and the absence of a secondary source in the adaptive optics imaging, we conclude that the planetary scenario is more than three orders of magnitude more likely than a blend. The blend scenario is independently disfavored by the achromaticity of the transit: we measure a transit depth with Spitzer at 4.5 mu m of 547(-110)(+113) ppm, consistent with the depth measured in the Kepler optical bandpass of 567 +/- 6 ppm (corrected for stellar limb darkening). We determine a physical radius of the planet Kepler-19b of R-p = 2.209 +/- 0.048 R-circle plus; the uncertainty is dominated by uncertainty in the stellar parameters. From radial velocity observations of the star, we find an upper limit on the planet mass of 20.3 M-circle plus, corresponding to a maximum density of 10.4 g cm(-3). We report a significant sinusoidal deviation of the transit times from a predicted linear ephemeris, which we conclude is due to an additional perturbing body in the system. We cannot uniquely determine the orbital parameters of the perturber, as various dynamical mechanisms match the amplitude, period, and shape of the transit timing signal and satisfy the host star's radial velocity limits. However, the perturber in these mechanisms has a period less than or similar to 160 days and mass less than or similar to 6 M-Jup, confirming its planetary nature as Kepler-19c. We place limits on the presence of transits of Kepler-19c in the available Kepler data.
C1 [Ballard, Sarah; Fressin, Francois; Charbonneau, David; Desert, Jean-Michel; Torres, Guillermo; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabrycky, Daniel] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marcy, Geoffrey; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Jenkins, Jon M.; Li, Jie] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Howell, Steven B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA.
[Hall, Jennifer R.; McCauliff, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
RP Ballard, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM sballard@cfa.harvard.edu
FU NASA; W. M. Keck Foundation
FX We thank the Spitzer team at IPAC and in particular Nancy Silbermann for
scheduling the Spitzer observations of this program. This work is based
on observations made with the Spitzer Space Telescope, which is operated
by the Jet Propulsion Laboratory, California Institute of Technology
under a contract with NASA. Support for this work was provided by NASA
through an award issued by JPL/Caltech. This work is also based on
observations made with Kepler, which was competitively selected as the
tenth Discovery mission. Funding for this mission is provided by NASA's
Science Mission Directorate. The authors thank the many people who
generously gave so much of their time to make this mission a success.
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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2011
VL 743
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AR 200
DI 10.1088/0004-637X/743/2/200
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400102
ER
PT J
AU Barnard, R
Garcia, MR
Murray, SS
AF Barnard, R.
Garcia, M. R.
Murray, S. S.
TI REINSTATING THE M31 X-RAY SYSTEM RX J0042.3+4115 AS A BLACK HOLE X-RAY
BINARY AND COMPELLING EVIDENCE FOR AN EXTENDED CORONA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; X-rays: binaries; X-rays: general
ID SMALL-MAGELLANIC-CLOUD; XMM-NEWTON; GLOBULAR-CLUSTERS; SPECTRAL
TRANSITIONS; ACCRETION; STARS; X-1; CONSEQUENCES; VARIABILITY; CANDIDATE
C1 [Barnard, R.; Garcia, M. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2011
VL 743
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AR 185
DI 10.1088/0004-637X/743/2/185
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400087
ER
PT J
AU Berger, E
Chornock, R
Holmes, TR
Foley, RJ
Cucchiara, A
Wolf, C
Podsiadlowski, P
Fox, DB
Roth, KC
AF Berger, E.
Chornock, R.
Holmes, T. R.
Foley, R. J.
Cucchiara, A.
Wolf, C.
Podsiadlowski, Ph
Fox, D. B.
Roth, K. C.
TI THE SPECTROSCOPIC CLASSIFICATION AND EXPLOSION PROPERTIES OF SN 2009nz
ASSOCIATED WITH GRB 091127 AT z=0.490
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; gamma-ray burst: individual (GRB 091127)
ID GAMMA-RAY BURST; 25 APRIL 1998; OPTICAL AFTERGLOW; SUPERNOVA 2003DH;
HOST GALAXIES; GRB-031203; DISCOVERY; CONNECTION; GRB-030329; GRB-011121
AB We present spectroscopic observations of GRB 091127 (z = 0.490) at the peak of the putative associated supernova SN2009nz. Subtracting a late-time spectrum of the host galaxy, we isolate the contribution of SN2009nz and uncover broad features typical of nearby gamma-ray-burst-supernovae (GRB-SNe). This establishes unambiguously that GRB 091127 was accompanied by a broad-lined Type Ic SN, and links a cosmological long burst with a standard energy release (E(gamma,iso) approximate to 1.1 x 10(52) erg) to a massive star progenitor. The spectrum of SN 2009nz closely resembles that of SN 2006aj, with SN 2003dh also providing an acceptable match, but has significantly narrower features than SNe 1998bw and 2010bh, indicative of a lower expansion velocity. The photospheric velocity inferred from the Si II lambda 6355 absorption feature, v(ph) approximate to 17,000 km s(-1), is indeed closer to that of SNe 2006aj and 2003dh than to the other GRB-SNe. Combining the measured velocity with the light curve peak brightness and width, we estimate the following nominal (maximal) explosion parameters: M(Ni) approximate to 0.35 (0.6) M(circle dot), E(K) approximate to 2.3 x 10(51) (8.4 x 10(51)) erg, and M(ej) approximate to 1.4 (3.5) M(circle dot), similar to those of SN 2006aj. These properties indicate that SN 2009nz follows a trend of lower M(Ni) for GRB-SNe with lower E(K) and M(ej). Equally important, since GRB 091127 is a typical cosmological burst, the similarity of SN 2009nz to SN 2006aj either casts doubt on the claim that XRF 060218/SN 2006aj was powered by a neutron star or indicates that the nature of the central engine is encoded in the SN properties but not in the prompt emission. Future spectra of GRB-SNe at z greater than or similar to 0.3 will shed light on the full dispersion of SN properties for standard long GRBs, on the relation between SNe associated with sub-energetic and standard GRBs, and on a potential dispersion in the associated SN types.
C1 [Berger, E.; Chornock, R.; Holmes, T. R.; Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cucchiara, A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Cucchiara, A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Wolf, C.; Podsiadlowski, Ph] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Roth, K. C.] Gemini Observ, Hilo, HI 96720 USA.
RP Berger, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Swift AO6 [NNX10AI24G]
FX E.B. acknowledges partial support from Swift AO6 grant NNX10AI24G. This
work is based in part 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 e
Tecnologia (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion
Productiva (Argentina). This paper includes data gathered with the 6.5 m
Magellan Telescopes located at Las Campanas Observatory, Chile.
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SN 0004-637X
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JI Astrophys. J.
PD DEC 20
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SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400106
ER
PT J
AU Carson, JC
Marengo, M
Patten, BM
Luhman, KL
Sonnett, SM
Hora, JL
Schuster, MT
Allen, PR
Fazio, GG
Stauffer, JR
Schnupp, C
AF Carson, J. C.
Marengo, M.
Patten, B. M.
Luhman, K. L.
Sonnett, S. M.
Hora, J. L.
Schuster, M. T.
Allen, P. R.
Fazio, G. G.
Stauffer, J. R.
Schnupp, C.
TI A SPITZER IRAC IMAGING SURVEY FOR T DWARF COMPANIONS AROUND M, L, AND T
DWARFS: OBSERVATIONS, RESULTS, AND MONTE CARLO POPULATION ANALYSES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; brown dwarfs; infrared: stars; methods: numerical;
methods: statistical; stars: late-type; stars: low-mass
ID BINARY BROWN DWARF; EXTRASOLAR GIANT PLANETS; LOW MASS STARS;
SPACE-TELESCOPE; ULTRACOOL DWARFS; ADAPTIVE OPTICS; NEARBY STARS;
MULTIPLICITY; DISCOVERY; SEARCH
AB We report observational techniques, results, and Monte Carlo population analyses from a Spitzer Infrared Array Camera imaging survey for substellar companions to 117 nearby M, L, and T dwarf systems (median distance of 10 pc, mass range of 0.6 to similar to 0.05 M(circle dot)). The two-epoch survey achieves typical detection sensitivities to substellar companions of [4.5 mu m] <= 17.2 mag for angular separations between about 7 '' and 165 ''. Based on common proper motion analysis, we find no evidence for new substellar companions. Using Monte Carlo orbital simulations (assuming random inclination, random eccentricity, and random longitude of pericenter), we conclude that the observational sensitivities translate to an ability to detect 600-1100 K brown dwarf companions at semimajor axes greater than or similar to 35 AU and to detect 500-600 K companions at semimajor axes greater than or similar to 60 AU. The simulations also estimate a 600-1100 K T dwarf companion fraction of <3.4% for 35-1200 AU separations and <12.4% for the 500-600 K companions for 60-1000 AU separations.
C1 [Carson, J. C.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Patten, B. M.; Hora, J. L.; Schuster, M. T.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Luhman, K. L.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Sonnett, S. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Allen, P. R.] Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA.
[Stauffer, J. R.] Spitzer Sci Ctr, Pasadena, CA 91106 USA.
[Schnupp, C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Carson, JC (reprint author), Coll Charleston, Dept Phys & Astron, 58 Coming St, Charleston, SC 29424 USA.
OI Hora, Joseph/0000-0002-5599-4650
FU NASA [1256790]; National Science Foundation [AST-1009203, AST-0544588];
Pennsylvania State University; Eberly College of Science; Pennsylvania
Space Grant Consortium
FX We thank our referee, Angelle Tanner, for helpful comments which
improved the manuscript. This work is based on observations made with
the Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under a contract
with NASA. Support for part of this work was provided by NASA through an
award issued by JPL. Support for the IRAC instrument was provided by
NASA under contract number 1256790 issued by JPL. J.C.C. was supported
by grant AST-1009203 from the National Science Foundation. K. L. was
supported by grant AST-0544588 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. This research has made use of the
following databases: (1) the M, L, and T dwarf compendium housed at
DwarfArchives.org and maintained by Chris Gelino, Davy Kirkpatrick, and
Adam Burgasser; (2) the SIMBAD database, operated at CDS, Strasbourg,
France; (3) the NASA/IPAC/NExScI Star and Exoplanet Database, which is
operated by JPL; and (4) the Washington Double Star Catalog maintained
at the U. S. Naval Observatory.
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JI Astrophys. J.
PD DEC 20
PY 2011
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DI 10.1088/0004-637X/743/2/141
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SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400043
ER
PT J
AU Chomiuk, L
Chornock, R
Soderberg, AM
Berger, E
Chevalier, RA
Foley, RJ
Huber, ME
Narayan, G
Rest, A
Gezari, S
Kirshner, RP
Riess, A
Rodney, SA
Smartt, SJ
Stubbs, CW
Tonry, JL
Wood-Vasey, WM
Burgett, WS
Chambers, KC
Czekala, I
Flewelling, H
Forster, K
Kaiser, N
Kudritzki, RP
Magnier, EA
Martin, DC
Morgan, JS
Neill, JD
Price, PA
Roth, KC
Sanders, NE
Wainscoat, RJ
AF Chomiuk, L.
Chornock, R.
Soderberg, A. M.
Berger, E.
Chevalier, R. A.
Foley, R. J.
Huber, M. E.
Narayan, G.
Rest, A.
Gezari, S.
Kirshner, R. P.
Riess, A.
Rodney, S. A.
Smartt, S. J.
Stubbs, C. W.
Tonry, J. L.
Wood-Vasey, W. M.
Burgett, W. S.
Chambers, K. C.
Czekala, I.
Flewelling, H.
Forster, K.
Kaiser, N.
Kudritzki, R. -P.
Magnier, E. A.
Martin, D. C.
Morgan, J. S.
Neill, J. D.
Price, P. A.
Roth, K. C.
Sanders, N. E.
Wainscoat, R. J.
TI Pan-STARRS1 DISCOVERY OF TWO ULTRALUMINOUS SUPERNOVAE AT(z) approximate
to 0.9
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; stars: magnetars; supernovae: general; supernovae:
individual (PS1-10ky, PS1-10awh)
ID DIGITAL SKY SURVEY; GAMMA-RAY BURSTS; MASS-METALLICITY RELATION;
CORE-COLLAPSE SUPERNOVAE; SHOCK BREAKOUT; LIGHT CURVES; CIRCUMSTELLAR
INTERACTION; LUMINOUS SUPERNOVAE; RADIO SUPERNOVAE; PAIR-INSTABILITY
AB We present the discovery of two ultraluminous supernovae (SNe) at z approximate to 0.9 with the Pan-STARRS1 Medium Deep Survey. These SNe, PS1-10ky and PS1-10awh, are among the most luminous SNe ever discovered, comparable to the unusual transients SN 2005ap and SCP 06F6. Like SN 2005ap and SCP 06F6, they show characteristic high luminosities (M-bol approximate to -22.5 mag), blue spectra with a few broad absorption lines, and no evidence for H or He. We have constructed a full multi-color light curve sensitive to the peak of the spectral energy distribution in the rest-frame ultraviolet, and we have obtained time series spectroscopy for these SNe. Given the similarities between the SNe, we combine their light curves to estimate a total radiated energy over the course of explosion of (0.9-1.4) x 10(51) erg. We find photospheric velocities of 12,000-19,000 km s(-1) with no evidence for deceleration measured across similar to 3 rest-frame weeks around light curve peak, consistent with the expansion of an optically thick massive shell of material. We show that, consistent with findings for other ultraluminous SNe in this class, radioactive decay is not sufficient to power PS1-10ky, and we discuss two plausible origins for these events: the initial spin-down of a newborn magnetar in a core-collapse SN, or SN shock breakout from the dense circumstellar wind surrounding a Wolf-Rayet star.
C1 [Chomiuk, L.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Chomiuk, L.; Chornock, R.; Soderberg, A. M.; Berger, E.; Foley, R. J.; Kirshner, R. P.; Czekala, I.; Sanders, N. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Huber, M. E.; Gezari, S.; Riess, A.; Rodney, S. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Narayan, G.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Smartt, S. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Flewelling, H.; Kaiser, N.; Kudritzki, R. -P.; Magnier, E. A.; Morgan, J. S.; Wainscoat, R. J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Forster, K.; Martin, D. C.; Neill, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Roth, K. C.] Gemini Observ, Hilo, HI 96720 USA.
RP Chomiuk, L (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
EM lchomiuk@cfa.harvard.edu
RI Stubbs, Christopher/C-2829-2012
OI Stubbs, Christopher/0000-0003-0347-1724
FU Smithsonian Astrophysical Observatory; FAS Science Division Research
Computing Group at Harvard University; Gemini [GN-2010A-Q-30,
GS-2010B-Q-4, GN-2010B-Q-34]; MMT; EVLA; PS1; National Science
Foundation [AST-1009749, AST-0807727]
FX We thank S. Balberg, D. Kasen, B. Metzger, R. Quimby, and R. Stoll for
helpful insights. Laura Chomiuk is a Jansky Fellow of the National Radio
Astronomy Observatory. Ryan J. Foley is supported by a Clay Fellowship.
This discovery was enabled using the PS1 System operated by the PS1
Science Consortium (PS1SC) and its member institutions. The PS1 Surveys
have been made possible through the combinations of the Institute for
Astronomy at 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
Extraterrestial Physics, Garching, The Johns Hopkins University, the
University of Durham, the University of Edinburgh, the Queen's
University of Belfast, the Harvard-Smithsonian Center for Astrophysics,
the Las Cumbres Observatory Global Network, and the National Central
University of Taiwan. Observations reported here were obtained at the
MMT Observatory, a joint facility of the Smithsonian Institution and the
University of Arizona. This paper uses data products produced by the OIR
Telescope Data Center, supported by the Smithsonian Astrophysical
Observatory. The EVLA is run by the National Radio Astronomy
Observatory, a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc.. 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 e Tecnologia
(Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva
(Argentina). Some of the image processing in this paper was run on the
Odyssey cluster supported by the FAS Science Division Research Computing
Group at Harvard University. We appreciate the excellent support by the
staffs at Gemini, MMT, EVLA, and PS1. We are grateful for access to
Gemini under programs GN-2010A-Q-30 and GS-2010B-Q-4 (PI: E. Berger) and
GN-2010B-Q-34 (PI: J. Tonry). Partial support for this work was provided
by National Science Foundation grants AST-1009749 and AST-0807727.
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JI Astrophys. J.
PD DEC 20
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SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400016
ER
PT J
AU Cucchiara, A
Cenko, SB
Bloom, JS
Melandri, A
Morgan, A
Kobayashi, S
Smith, RJ
Perley, DA
Li, W
Hora, JL
da Silva, RL
Prochaska, JX
Milne, PA
Butler, NR
Cobb, B
Worseck, G
Mundell, CG
Steele, IA
Filippenko, AV
Fumagalli, M
Klein, CR
Stephens, A
Bluck, A
Mason, R
AF Cucchiara, A.
Cenko, S. B.
Bloom, J. S.
Melandri, A.
Morgan, A.
Kobayashi, S.
Smith, R. J.
Perley, D. A.
Li, W.
Hora, J. L.
da Silva, R. L.
Prochaska, J. X.
Milne, P. A.
Butler, N. R.
Cobb, B.
Worseck, G.
Mundell, C. G.
Steele, I. A.
Filippenko, A. V.
Fumagalli, M.
Klein, C. R.
Stephens, A.
Bluck, A.
Mason, R.
TI CONSTRAINING GAMMA-RAY BURST EMISSION PHYSICS WITH EXTENSIVE EARLY-TIME,
MULTIBAND FOLLOW-UP
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: individual (GRB 110205A, GRB 110213A); techniques:
photometric; techniques: polarimetric; techniques: spectroscopic
ID EARLY OPTICAL AFTERGLOWS; REVERSE-SHOCK; LIGHT CURVES; LORENTZ FACTOR;
DATA RELEASE; SKY SURVEY; SWIFT; TELESCOPE; POLARIZATION; FLARES
AB Understanding the origin and diversity of emission processes responsible for gamma-ray bursts (GRBs) remains a pressing challenge. While prompt and contemporaneous panchromatic observations have the potential to test predictions of the internal-external shock model, extensive multiband imaging has been conducted for only a few GRBs. We present rich, early-time, multiband data sets for two Swift events, GRB 110205A and GRB 110213A. The former shows optical emission since the early stages of the prompt phase, followed by the steep rising in flux up to similar to 1000 s after the burst (t(-alpha) with alpha = -6.13 +/- 0.75). We discuss this feature in the context of the reverse-shock scenario and interpret the following single power-law decay as being forward-shock dominated. Polarization measurements, obtained with the RINGO2 instrument mounted on the Liverpool Telescope, also provide hints on the nature of the emitting ejecta. The latter event, instead, displays a very peculiar optical to near-infrared light curve, with two achromatic peaks. In this case, while the first peak is probably due to the onset of the afterglow, we interpret the second peak to be produced by newly injected material, signifying a late-time activity of the central engine.
C1 [Cucchiara, A.; Cenko, S. B.; Bloom, J. S.; Morgan, A.; Perley, D. A.; Li, W.; Butler, N. R.; Filippenko, A. V.; Klein, C. R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Cucchiara, A.; da Silva, R. L.; Prochaska, J. X.; Worseck, G.; Fumagalli, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Melandri, A.] Osservatorio Astronomicodi Brera, INAF, I-23807 Merate, LC, Italy.
[Melandri, A.; Kobayashi, S.; Smith, R. J.; Mundell, C. G.; Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Milne, P. A.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA.
[Cobb, B.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
[Stephens, A.; Bluck, A.; Mason, R.] Gemini Observ, Hilo, HI 96720 USA.
RP Cucchiara, A (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM acucchia@ucolick.org
RI Fumagalli, Michele/K-9510-2015;
OI Fumagalli, Michele/0000-0001-6676-3842; Worseck,
Gabor/0000-0003-0960-3580; Hora, Joseph/0000-0002-5599-4650
FU GN-20011A-Q-4; NSF; National Science Foundation (United States); Science
and Technology Facilities Council (United Kingdom); National Research
Council (Canada); CONICYT (Chile); Australian Research Council
(Australia); Ministerio da Ciencia e Tecnologia (Brazil); Ministerio de
Ciencia, Tecnologia e Innovacion Productiva (Argentina); Gary & Cynthia
Bengier; Richard & Rhoda Goldman Fund; NASA/Swift [NNX10AI21G,
GO-7100028]; TABASGO Foundation; NSF [AST-0908886]
FX A. C. acknowledges the anonymous referee for the valuable comments in
order to improve the quality of this work. The Gemini data, acquired
under the program ID GN-20011A-Q-4, are 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 e Tecnologia (Brazil), and Ministerio de Ciencia,
Tecnologia e Innovacion Productiva (Argentina). A. V. F., S. B. C., and
W. L. acknowledge generous financial assistance from Gary & Cynthia
Bengier, the Richard & Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G
and GO-7100028, the TABASGO Foundation, and NSF grant AST-0908886. 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, and the TABASGO Foundation. A. C. thanks C.
Guidorzi and D. A. Kann for the useful discussion and comments.
NR 102
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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 DEC 20
PY 2011
VL 743
IS 2
AR 154
DI 10.1088/0004-637X/743/2/154
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400056
ER
PT J
AU Douglass, EM
Blanton, EL
Clarke, TE
Randall, SW
Wing, JD
AF Douglass, E. M.
Blanton, Elizabeth L.
Clarke, T. E.
Randall, Scott W.
Wing, Joshua D.
TI THE MERGER ENVIRONMENT OF THE WIDE ANGLE TAIL HOSTING CLUSTER A562
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (A562);
intergalactic medium; radio continuum: galaxies; X-rays: galaxies:
clusters
ID RELAXED GALAXY CLUSTERS; X-RAY OBSERVATIONS; RADIO-SOURCES; MERGING
CLUSTERS; ABELL CLUSTERS; CHANDRA OBSERVATION; DARK ENERGY; JETS;
CONSTRAINTS; EVOLUTION
AB We present a Chandra X-ray observation and Very Large Array radio observations of the nearby (z = 0.11) galaxy cluster A562 and the wide angle tail (WAT) radio source 0647+693. The cluster displays signatures of an ongoing merger leading to the bending of the WAT source including an elongation of the X-ray surface brightness distribution along the line that bisects the WAT, an excess of displaced gas found between the radio lobes, and anisotropies within the intracluster medium projected temperature and abundance distributions. The most likely geometry of the ongoing interaction is a head-on merger occurring along the WAT bending axis. By combining observable properties of A562 and 0647+693 with common values for the conditions within merging clusters at the time of core crossing, we constrain the internal density (rho(j) = 0.001 rho(ICM)) of the jets and plasma flow velocity within the lobes (v(r) = 0.02c-0.03c) of the WAT source.
C1 [Douglass, E. M.; Blanton, Elizabeth L.; Wing, Joshua D.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Douglass, E. M.] Amer Univ Cairo, Cairo, Egypt.
[Clarke, T. E.] USN, Res Lab, Washington, DC 20375 USA.
[Randall, Scott W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Douglass, EM (reprint author), Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
RI Blanton, Elizabeth/H-4501-2014;
OI Randall, Scott/0000-0002-3984-4337
FU National Aeronautics and Space Administration [GO6-7117X]; 6.1 Base
funding; Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian
Institution; NSF; Boston University; Lowell Observatory
FX Support for this work was provided by the National Aeronautics and Space
Administration, through Chandra Award Number GO6-7117X. Basic research
in radio astronomy at the Naval Research Laboratory is funded by 6.1
Base funding. S. W. R. was supported by the Chandra X-ray Center through
NASA contract NAS8-03060 and the Smithsonian Institution. PRISM was
designed and constructed at Boston University (PI: Kenneth Janes), with
support from the NSF, Boston University and Lowell Observatory.
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 DEC 20
PY 2011
VL 743
IS 2
AR 199
DI 10.1088/0004-637X/743/2/199
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400101
ER
PT J
AU France, K
McCray, R
Penton, SV
Kirshner, RP
Challis, P
Laming, JM
Bouchet, P
Chevalier, R
Garnavich, PM
Fransson, C
Heng, K
Larsson, J
Lawrence, S
Lundqvist, P
Panagia, N
Pun, CSJ
Smith, N
Sollerman, J
Sonneborn, G
Sugerman, B
Wheeler, JC
AF France, Kevin
McCray, Richard
Penton, Steven V.
Kirshner, Robert P.
Challis, Peter
Laming, J. Martin
Bouchet, Patrice
Chevalier, Roger
Garnavich, Peter M.
Fransson, Claes
Heng, Kevin
Larsson, Josefin
Lawrence, Stephen
Lundqvist, Peter
Panagia, Nino
Pun, Chun S. J.
Smith, Nathan
Sollerman, Jesper
Sonneborn, George
Sugerman, Ben
Wheeler, J. Craig
TI HST-COS OBSERVATIONS OF HYDROGEN, HELIUM, CARBON, AND NITROGEN EMISSION
FROM THE SN 1987A REVERSE SHOCK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; shock waves; supernovae: individual (SN 1987A)
ID HUBBLE-SPACE-TELESCOPE; BALMER-DOMINATED SHOCKS; SUPERNOVA REMNANT
1987A; INNER CIRCUMSTELLAR RING; VELOCITY LY-ALPHA; X-RAY; LINE
EMISSION; TEMPERATURE EQUILIBRATION; SPECTROGRAPH OBSERVATIONS; MACH
NUMBER
AB We present the most sensitive ultraviolet observations of Supernova 1987A to date. Imaging spectroscopy from the Hubble Space Telescope-Cosmic Origins Spectrograph shows many narrow (Delta upsilon similar to 300 km s(-1)) emission lines from the circumstellar ring, broad (Delta upsilon similar to 10-20 x 103 km s(-1)) emission lines from the reverse shock, and ultraviolet continuum emission. The high signal-to-noise ratio (>40 per resolution element) broad Ly alpha emission is excited by soft X-ray and EUV heating of mostly neutral gas in the circumstellar ring and outer supernova debris. The ultraviolet continuum at lambda > 1350 angstrom can be explained by H I two-photon (2s (2)S(1/2)-1s (2)S(1/2)) emission from the same region. We confirm our earlier, tentative detection of N V lambda 1240 emission from the reverse shock and present the first detections of broad He II lambda 1640, C IV lambda 1550, and N IV] lambda 1486 emission lines from the reverse shock. The helium abundance in the high-velocity material is He/H = 0.14 +/- 0.06. The N V/H alpha line ratio requires partial ion-electron equilibration (T(e)/T(p) approximate to 0.14-0.35). We find that the N/C abundance ratio in the gas crossing the reverse shock is significantly higher than that in the circumstellar ring, a result that may be attributed to chemical stratification in the outer envelope of the supernova progenitor. The N/C abundance may have been stratified prior to the ring expulsion, or this result may indicate continued CNO processing in the progenitor subsequent to the expulsion of the circumstellar ring.
C1 [France, Kevin; Penton, Steven V.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[McCray, Richard] Univ Colorado, JILA, Boulder, CO 80309 USA.
[McCray, Richard] NIST, Boulder, CO 80309 USA.
[Kirshner, Robert P.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Laming, J. Martin] USN, Res Lab, Washington, DC 20375 USA.
[Bouchet, Patrice] DSM IRFU SAp CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Chevalier, Roger] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Garnavich, Peter M.] Univ Notre Dame, Notre Dame, IN 46556 USA.
[Fransson, Claes; Larsson, Josefin; Lundqvist, Peter; Sollerman, Jesper] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Heng, Kevin] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Lawrence, Stephen] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA.
[Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Panagia, Nino] INAF CT, Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Pun, Chun S. J.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
[Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Sonneborn, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sugerman, Ben] Goucher Coll, Dept Phys & Astron, Baltimore, MD 21204 USA.
[Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP France, K (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA.
EM kevin.france@colorado.edu
OI Sollerman, Jesper/0000-0003-1546-6615; /0000-0003-0065-2933; Heng,
Kevin/0000-0003-1907-5910
FU NASA [NNX08AC146, NAS5-98043, NAS5-26555]; HST program [GO 12241]; NASA
through a grant from the Space Telescope Science Institute [GO-12241]
FX We thank Svetozar Zhekov formaking his X-ray shock model available, and
K.F. and S.V.P. thank James Green for enjoyable discussions about the
spectroscopic imaging capabilities of COS. We thank Dave Arnett for
helpful advice regarding progenitor envelope structure. This work was
supported by NASA grants NNX08AC146 and NAS5-98043 to the University of
Colorado at Boulder. Data were obtained as part of HST program GO 12241.
Support for program GO-12241 was provided by NASA through a grant from
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555.
NR 59
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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 DEC 20
PY 2011
VL 743
IS 2
AR 186
DI 10.1088/0004-637X/743/2/186
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400088
ER
PT J
AU Hayward, CC
Keres, D
Jonsson, P
Narayanan, D
Cox, TJ
Hernquist, L
AF Hayward, Christopher C.
Keres, Dusan
Jonsson, Patrik
Narayanan, Desika
Cox, T. J.
Hernquist, Lars
TI WHAT DOES A SUBMILLIMETER GALAXY SELECTION ACTUALLY SELECT? THE
DEPENDENCE OF SUBMILLIMETER FLUX DENSITY ON STAR FORMATION RATE AND DUST
MASS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; galaxies: high-redshift; galaxies: interactions;
galaxies: starburst; infrared: galaxies; radiative transfer;
submillimeter: galaxies
ID SIMILAR-TO 2; ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI;
SMOOTHED PARTICLE HYDRODYNAMICS; SPECTRAL ENERGY-DISTRIBUTIONS; DEGREE
EXTRAGALACTIC SURVEY; SUPERMASSIVE BLACK-HOLES; HUBBLE-DEEP-FIELD;
QUASAR LUMINOSITY FUNCTION; HIGH-REDSHIFT GALAXIES
AB We perform three-dimensional dust radiative transfer (RT) calculations on hydrodynamic simulations of isolated and merging disk galaxies in order to quantitatively study the dependence of observed-frame submillimeter (submm) flux density on galaxy properties. We find that submm flux density and star formation rate (SFR) are related in dramatically different ways for quiescently star-forming galaxies and starbursts. Because the stars formed in the merger-induced starburst do not dominate the bolometric luminosity and the rapid drop in dust mass and more compact geometry cause a sharp increase in dust temperature during the burst, starbursts are very inefficient at boosting submm flux density (e. g., a greater than or similar to 16x boost in SFR yields a less than or similar to 2x boost in submm flux density). Moreover, the ratio of submm flux density to SFR differs significantly between the two modes; thus one cannot assume that the galaxies with highest submm flux density are necessarily those with the highest bolometric luminosity or SFR. These results have important consequences for the bright submillimeter-selected galaxy (SMG) population. Among them are: (1) The SMG population is heterogeneous. In addition to merger-driven starbursts, there is a subpopulation of galaxy pairs, where two disks undergoing a major merger but not yet strongly interacting are blended into one submm source because of the large (greater than or similar to 15 '' or similar to 130 kpc at z = 2) beam of single-dish submm telescopes. (2) SMGs must be very massive (M-star greater than or similar to 6 x 10(10) M-circle dot). (3) The infall phase makes the SMG duty cycle a factor of a few greater than what is expected for a merger-driven starburst. Finally, we provide fitting functions for SCUBA and AzTEC submm flux densities as a function of SFR and dust mass and bolometric luminosity and dust mass; these should be useful for calculating submm flux density in semi-analytic models and cosmological simulations when performing full RT is computationally not feasible.
C1 [Hayward, Christopher C.; Keres, Dusan; Jonsson, Patrik; Narayanan, Desika; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Keres, Dusan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Keres, Dusan] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
[Narayanan, Desika] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA.
[Cox, T. J.] Carnegie Observ, Pasadena, CA 91101 USA.
RP Hayward, CC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM chayward@cfa.harvard.edu
RI Hayward, Christopher/I-4756-2012
OI Hayward, Christopher/0000-0003-4073-3236
FU NASA [HST-HF-51276.01-A]; W. M. Keck Foundation; National Science
Foundation [AST-1009452]; FAS Research Computing Group at Harvard
University
FX C.C.H. thanks Scott Chapman, Emanuele Daddi, Helmut Dannerbauer, Phil
Hopkins, Brandon Kelly, Chris McKee, Michal Michalowski, Diego Munoz,
Alex Pope, Barry Rothberg, Greg Snyder, and Josh Younger for useful
discussion and Jeff Pettibone for hospitality which facilitated the
writing of this paper. We thank Volker Springel for providing the
non-public version of Gadget-2 used for this work and Brant Robertson
for use of his code to generate initial disk galaxies scaled to high
redshift. D. K. is supported by NASA through Hubble Fellowship grant
HST-HF-51276.01-A. P.J. acknowledges support by a grant from the W. M.
Keck Foundation. D.N. acknowledges support from a National Science
Foundation Grant (AST-1009452). The simulations in this paper were
performed on the Odyssey cluster supported by the FAS Research Computing
Group at Harvard University.
NR 191
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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 DEC 20
PY 2011
VL 743
IS 2
AR 159
DI 10.1088/0004-637X/743/2/159
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400061
ER
PT J
AU Ingleby, L
Calvet, N
Bergin, E
Herczeg, G
Brown, A
Alexander, R
Edwards, S
Espaillat, C
France, K
Gregory, SG
Hillenbrand, L
Roueff, E
Valenti, J
Walter, F
Johns-Krull, C
Brown, J
Linsky, J
McClure, M
Ardila, D
Abgrall, H
Bethell, T
Hussain, G
Yang, H
AF Ingleby, Laura
Calvet, Nuria
Bergin, Edwin
Herczeg, Gregory
Brown, Alexander
Alexander, Richard
Edwards, Suzan
Espaillat, Catherine
France, Kevin
Gregory, Scott G.
Hillenbrand, Lynne
Roueff, Evelyne
Valenti, Jeff
Walter, Frederick
Johns-Krull, Christopher
Brown, Joanna
Linsky, Jeffrey
McClure, Melissa
Ardila, David
Abgrall, Herve
Bethell, Thomas
Hussain, Gaitee
Yang, Hao
TI NEAR-ULTRAVIOLET EXCESS IN SLOWLY ACCRETING T TAURI STARS: LIMITS
IMPOSED BY CHROMOSPHERIC EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; circumstellar matter; stars: pre-main
sequence
ID PRE-MAIN-SEQUENCE; ETA-CHAMAELEONTIS CLUSTER; LOW-MASS STARS;
PLANET-FORMING REGION; X-RAY-RADIATION; FAR-ULTRAVIOLET; CIRCUMSTELLAR
DISKS; PROTOPLANETARY DISKS; BROWN DWARFS; MAGNETOSPHERIC ACCRETION
AB Young stars surrounded by disks with very low mass accretion rates are likely in the final stages of inner disk evolution and therefore particularly interesting to study. We present ultraviolet (UV) observations of the similar to 5-9 Myr old stars RECX-1 and RECX-11, obtained with the Cosmic Origins Spectrograph and Space Telescope Imaging Spectrograph on the Hubble Space Telescope, as well as optical and near-infrared spectroscopic observations. The two stars have similar levels of near-UV emission, although spectroscopic evidence indicates that RECX-11 is accreting and RECX-1 is not. The line profiles of Ha and He I lambda 10830 in RECX-11 show both broad and narrow redshifted absorption components that vary with time, revealing the complexity of the accretion flows. We show that accretion indicators commonly used to measure mass accretion rates, e. g., U-band excess luminosity or the Ca ii triplet line luminosity, are unreliable for low accretors, at least in the middle K spectral range. Using RECX-1 as a template for the intrinsic level of photospheric and chromospheric emission, we determine an upper limit of 3 x 10(-10) M(circle dot) yr(-1) for RECX-11. At this low accretion rate, recent photoevaporation models predict that an inner hole should have developed in the disk. However, the spectral energy distribution of RECX-11 shows fluxes comparable to the median of Taurus in the near-infrared, indicating that substantial dust remains. Fluorescent H2 emission lines formed in the innermost disk are observed in RECX-11, showing that gas is present in the inner disk, along with the dust.
C1 [Ingleby, Laura; Calvet, Nuria; Bergin, Edwin; McClure, Melissa; Bethell, Thomas] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Herczeg, Gregory] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Brown, Alexander; France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Alexander, Richard] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Edwards, Suzan] Smith Coll, Dept Astron, Northampton, MA 01063 USA.
[Espaillat, Catherine; Brown, Joanna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gregory, Scott G.; Hillenbrand, Lynne] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Roueff, Evelyne; Abgrall, Herve] Observ Paris, CNRS, UMR 8102, Sect Meudon, F-92195 Meudon, France.
[Roueff, Evelyne; Abgrall, Herve] LUTH, F-92195 Meudon, France.
[Valenti, Jeff] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Walter, Frederick] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Johns-Krull, Christopher] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA.
[Linsky, Jeffrey; Yang, Hao] Univ Colorado, JILA, Boulder, CO 80309 USA.
[Linsky, Jeffrey; Yang, Hao] NIST, Boulder, CO 80309 USA.
[Ardila, David] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Hussain, Gaitee] ESO, D-85748 Garching, Germany.
RP Ingleby, L (reprint author), Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA.
EM lingleby@umich.edu; ncalvet@umich.edu; gregoryh@mpe.mpg.de
RI Yang, Hao/F-8396-2014;
OI Yang, Hao/0000-0002-9423-2333; McClure, Melissa/0000-0003-1878-327X;
Gregory, Scott/0000-0003-3674-5568; Herczeg, Gregory/0000-0002-7154-6065
FU NASA [11616]; University of Colorado; Association of Universities for
Research in Astronomy, Inc. under NASA [NAS 5-26555]; National Science
Foundation [0901947]; Science & Technology Facilities Council (STFC)
FX We thank Will Fischer for help reducing the Phoenix data to obtain the
He I line profile. We thank the SMARTS service for obtaining the SMARTS
spectra. Stony Brook University is a member of the SMARTS partnership.
This work was supported by NASA grants for Guest Observer program 11616
to the University of Michigan, Caltech, Stony Brook University, and the
University of Colorado. Based on observations made with the NASA/ESA
Hubble Space Telescope, obtained from the Space Telescope Science
Institute data archive. STScI is operated by the Association of
Universities for Research in Astronomy, Inc. under NASA contract NAS
5-26555. C. E. was supported by the National Science Foundation under
award no. 0901947. R. A. acknowledges support from the Science &
Technology Facilities Council (STFC) through an Advanced Fellowship
(ST/G00711X/1).
NR 95
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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 DEC 20
PY 2011
VL 743
IS 2
AR 105
DI 10.1088/0004-637X/743/2/105
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400007
ER
PT J
AU Kriek, M
van Dokkum, PG
Whitaker, KE
Labbe, I
Franx, M
Brammer, GB
AF Kriek, Mariska
van Dokkum, Pieter G.
Whitaker, Katherine E.
Labbe, Ivo
Franx, Marijn
Brammer, Gabriel B.
TI H alpha AND 4000 angstrom BREAK MEASUREMENTS FOR similar to 3500
K-SELECTED GALAXIES AT 0.5 < z < 2.0
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: stellar content
ID STAR-FORMING GALAXIES; MEDIUM-BAND SURVEY; STELLAR POPULATION SYNTHESIS;
HIGH-REDSHIFT GALAXIES; INITIAL MASS FUNCTION; DIGITAL SKY SURVEY;
SIMILAR-TO 2; INFRARED SPECTROSCOPIC SURVEY; EVOLUTION SURVEY COSMOS;
ACTIVE GALACTIC NUCLEI
AB We measure spectral features of similar to 3500 K-selected galaxies at 0.5 < z < 2.0 from high-quality medium-band photometry using a new technique. First, we divide the galaxy sample in 32 subsamples based on the similarities between the full spectral energy distributions (SEDs) of the galaxies. For each of these 32 galaxy types we construct a composite SED by de-redshifting and scaling the observed photometry. This approach increases the signal-to-noise ratio and sampling of galaxy SEDs and allows for model-independent stellar population studies. The composite SEDs are of spectroscopic quality and facilitate-for the first time-H alpha measurements for a large magnitude-limited sample of distant galaxies. The line widths indicate a photometric redshift uncertainty of Delta z < 0.02 x (1 + z). The composite SEDs also show the Balmer and 4000 angstrom breaks, Mg II absorption at similar to 2800 angstrom, the dust absorption feature at 2175 angstrom, and blended [O III]+H beta emission. We compare the total equivalent width of H alpha, [N II], and [S II] (WH alpha+) with the strength of the 4000 angstrom break (D(4000)) and the best-fit specific star formation rate, and find that all these properties are strongly correlated. This is a reassuring result, as currently most distant stellar population studies are based on just continuum emission. Furthermore, the relation between WH alpha+ and D(4000) provides interesting clues to the star formation histories of galaxies, as these features are sensitive to different stellar ages. We find that the correlation between WH alpha+ and D(4000) at 0.5 < z < 2.0 is similar to z similar to 0 and that the suppression of star formation in galaxies at z < 2 is generally not abrupt, but a gradual process.
C1 [Kriek, Mariska] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[van Dokkum, Pieter G.; Whitaker, Katherine E.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Labbe, Ivo] Carnegie Observ, Pasadena, CA 91101 USA.
[Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Brammer, Gabriel B.] European So Observ, Santiago 19, Chile.
RP Kriek, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Clay Fellowship
FX We thank the members of the NMBS team for their help with the
observations and construction of the catalogs, Charlie Conroy, Ryan
Foley, and Jeremiah Ostriker for useful discussions, and the COSMOS and
AEGIS teams for the release of high-quality multi-wavelength data sets
to the community. M.K. acknowledges support of a Clay Fellowship
administered by the Smithsonian Astrophysical Observatory.
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 DEC 20
PY 2011
VL 743
IS 2
AR 168
DI 10.1088/0004-637X/743/2/168
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400070
ER
PT J
AU Ladd, EF
Wong, T
Bourke, TL
Thompson, KL
AF Ladd, E. F.
Wong, T.
Bourke, T. L.
Thompson, K. L.
TI INTERACTIONS BETWEEN FORMING STARS AND DENSE GAS IN THE SMALL LOW-MASS
CLUSTER CEDERBLAD 110
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects: Ced 110; ISM: individual objects: Chamaeleon I;
ISM: jets and outflows; ISM: kinematics and dynamics
ID INTERSTELLAR MOLECULAR CLOUDS; YOUNG STELLAR CLUSTERS; HERBIG-HARO
OBJECTS; I DARK CLOUD; CHAMELEON-I; CORE CHAMELEON-MMS1; N2H+; REGION;
EVOLUTION; DEPLETION
AB We present observations of dense gas and outflow activity in the Cederblad 110 region of the Chamaeleon I dark cloud complex. The region contains nine forming low-mass stars in evolutionary stages ranging from Class 0 to Class II/III crowded into a 0.2 pc region with high surface density (Sigma(YSO) similar to 150 pc(-2)). The analysis of our N2H+ (J = 1 -> 0) maps indicates the presence of 13 +/- 3 solar masses of dense (n similar to 10(5) cm(-3)) gas in this region, much of which is unstable against gravitational collapse. The most unstable material is located near the Class 0 source MMS-1, which is almost certainly actively accreting material from its dense core. Smaller column densities of more stable dense gas are found toward the region's Class I sources, IRS 4, 11, and 6. Little or no dense gas is colocated with the Class II and III sources in the region. The outflow from IRS 4 is interacting with the dense core associated with MMS-1. The molecular component of the outflow, measured in the (J = 1 -> 0) line of (CO)-C-12, appears to be deflected by the densest part of the core, after which it appears to plow through some of the lower column density portions of the core. The working surface between the head of the outflow lobe and the dense core material can be seen in the enhanced velocity dispersion of the dense gas. IRS 2, the Class III source that produces the optical reflection nebula that gives the Cederblad 110 region its name, may also be influencing the dense gas in the region. A dust temperature gradient across the MMS-1 dense core is consistent with warming from IRS 2, and a sharp gradient in dense gas column density may be caused by winds from this source. Taken together, our data indicate that this region has been producing several young stars in the recent past, and that sources which began forming first are interacting with the remaining dense gas in the region, thereby influencing current and future star formation activity.
C1 [Ladd, E. F.] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA.
[Wong, T.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Thompson, K. L.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA.
RP Ladd, EF (reprint author), Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA.
EM ladd@bucknell.edu
FU US National Science Foundation (NSF) [AST 03-0750]; Australia Telescope
National Facility (ATNF) Distiguished Visitor Program;
Harvard-Smithsonian Center for Astrophysics; Bucknell University Office
of the Dean of Arts Sciences; NSF [PHYS 05-52790, AST 07-08158];
Bucknell University Research Experiences for Undergraduates (REU)
FX We are grateful to M. Hiramatsu for providing the 12CO (J = 3
-> 2) data from Hiramatsu et al. (2007). E. F. L. acknowledges support
from US National Science Foundation (NSF) Grant AST 03-0750, the
Australia Telescope National Facility (ATNF) Distiguished Visitor
Program, the Visiting Scientist Program at the Harvard-Smithsonian
Center for Astrophysics, and the Bucknell University Office of the Dean
of Arts & Sciences. K. L. T. acknowledges support from NSF Grant PHYS
05-52790, which supports the Bucknell University Research Experiences
for Undergraduates (REU) program. T. L. B. acknowledges support from NSF
Grant AST 07-08158. We thank the anonymous referee for comments that
materially improved this work.
NR 63
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U1 0
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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 DEC 20
PY 2011
VL 743
IS 2
AR 108
DI 10.1088/0004-637X/743/2/108
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400010
ER
PT J
AU Mainzer, A
Grav, T
Bauer, J
Masiero, J
McMillan, RS
Cutri, RM
Walker, R
Wright, E
Eisenhardt, P
Tholen, DJ
Spahr, T
Jedicke, R
Denneau, L
DeBaun, E
Elsbury, D
Gautier, T
Gomillion, S
Hand, E
Mo, W
Watkins, J
Wilkins, A
Bryngelson, GL
Molina, AD
Desai, S
Camus, MG
Hidalgo, SL
Konstantopoulos, I
Larsen, JA
Maleszewski, C
Malkan, MA
Mauduit, JC
Mullan, BL
Olszewski, EW
Pforr, J
Saro, A
Scotti, JV
Wasserman, LH
AF Mainzer, A.
Grav, T.
Bauer, J.
Masiero, J.
McMillan, R. S.
Cutri, R. M.
Walker, R.
Wright, E.
Eisenhardt, P.
Tholen, D. J.
Spahr, T.
Jedicke, R.
Denneau, L.
DeBaun, E.
Elsbury, D.
Gautier, T.
Gomillion, S.
Hand, E.
Mo, W.
Watkins, J.
Wilkins, A.
Bryngelson, G. L.
Del Pino Molina, A.
Desai, S.
Gomez Camus, M.
Hidalgo, S. L.
Konstantopoulos, I.
Larsen, J. A.
Maleszewski, C.
Malkan, M. A.
Mauduit, J. -C.
Mullan, B. L.
Olszewski, E. W.
Pforr, J.
Saro, A.
Scotti, J. V.
Wasserman, L. H.
TI NEOWISE OBSERVATIONS OF NEAR-EARTH OBJECTS: PRELIMINARY RESULTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; minor planets, asteroids: general; planets
and satellites: general; surveys
ID THERMAL-MODEL CALIBRATION; INFRARED-SURVEY-EXPLORER; JUPITER-FAMILY
COMETS; MAIN-BELT ASTEROIDS; APPROACHING ASTEROIDS; SUFFICIENT SOURCE;
DISTRIBUTIONS; HAZARD; METEORITES; PHOTOMETRY
AB With the NEOWISE portion of the Wide-field Infrared Survey Explorer (WISE) project, we have carried out a highly uniform survey of the near-Earth object (NEO) population at thermal infrared wavelengths ranging from 3 to 22 mu m, allowing us to refine estimates of their numbers, sizes, and albedos. The NEOWISE survey detected NEOs the same way whether they were previously known or not, subject to the availability of ground-based follow-up observations, resulting in the discovery of more than 130 new NEOs. The survey's uniform sensitivity, observing cadence, and image quality have permitted extrapolation of the 428 near-Earth asteroids (NEAs) detected by NEOWISE during the fully cryogenic portion of the WISE mission to the larger population. We find that there are 981 +/- 19 NEAs larger than 1 km and 20,500 +/- 3000 NEAs larger than 100 m. We show that the Spaceguard goal of detecting 90% of all 1 km NEAs has been met, and that the cumulative size distribution is best represented by a broken power law with a slope of 1.32 +/- 0.14 below 1.5 km. This power-law slope produces similar to 13,200 +/- 1900 NEAs with D > 140 m. Although previous studies predict another break in the cumulative size distribution below D similar to 50-100 m, resulting in an increase in the number of NEOs in this size range and smaller, we did not detect enough objects to comment on this increase. The overall number for the NEA population between 100 and 1000 m is lower than previous estimates. The numbers of near-Earth comets and potentially hazardous NEOs will be the subject of future work.
C1 [Mainzer, A.; Bauer, J.; Masiero, J.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.; Mo, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bauer, J.; Cutri, R. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Maleszewski, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Walker, R.] Monterey Inst Res Astron, Monterey, CA USA.
[Wright, E.; Malkan, M. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Tholen, D. J.; Jedicke, R.; Denneau, L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[DeBaun, E.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Elsbury, D.] Univ Calif Santa Barbara, Santa Barbara, CA 93103 USA.
[Gautier, T.] Cornell Univ, Ithaca, NY 14853 USA.
[Gomillion, S.] Embry Riddle Aeronaut Univ, Dept Engn Phys, Daytona Beach, FL 32114 USA.
[Hand, E.] Univ Missouri, Dept Mech Engn, Kansas City, MO 64110 USA.
[Watkins, J.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bryngelson, G. L.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Del Pino Molina, A.; Hidalgo, S. L.] Inst Astrofis Canarias, E-38200 Tenerife, Canary Islands, Spain.
[Desai, S.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Gomez Camus, M.] Univ Andres Bello, Fac Ingn, Dept Ciencias Fis, Santiago, Chile.
[Konstantopoulos, I.; Mullan, B. L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Larsen, J. A.] USN Acad, Dept Phys, Annapolis, MD 21402 USA.
[Mauduit, J. -C.] CALTECH, Infrared Proc & Anal Ctr, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Olszewski, E. W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Pforr, J.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Saro, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Wasserman, L. H.] Lowell Observ, Flagstaff, AZ 86001 USA.
RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM amainzer@jpl.nasa.gov
RI Pforr, Janine/J-3967-2015; del Pino Molina, Andres/I-7976-2016;
OI Pforr, Janine/0000-0002-3414-8391; del Pino Molina,
Andres/0000-0003-4922-5131; Konstantopoulos,
Iraklis/0000-0003-2177-0146; Masiero, Joseph/0000-0003-2638-720X;
Hidalgo, Sebastian/0000-0002-0002-9298
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 DLR, for his thoughtful comments which materially
improved this work. We also thank Dr. Alan Harris of the Space Sciences
Institute for useful conversations. 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 67
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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 DEC 20
PY 2011
VL 743
IS 2
AR 156
DI 10.1088/0004-637X/743/2/156
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400058
ER
PT J
AU Oberg, KI
Qi, CH
Wilner, DJ
Andrews, SM
AF Oeberg, Karin I.
Qi, Chunhua
Wilner, David J.
Andrews, Sean M.
TI THE IONIZATION FRACTION IN THE DM Tau PROTOPLANETARY DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: molecules; protoplanetary disks; radio lines: ISM;
stars: formation; techniques: high angular resolution
ID PRESTELLAR CORES; T-TAURI; DEUTERATED MOLECULES; CIRCUMSTELLAR DISK;
INTERSTELLAR ICES; LINE EMISSION; GRAIN-GROWTH; CHEMISTRY; DESORPTION;
DUST
AB We present millimeter-wave observations of several molecular ions in the disk around the pre-main-sequence star DM Tau and use these to investigate the ionization fraction in different regions of the disk. New Submillimeter Array (SMA) observations of H(2)D(+) J = 1(1,0)-1(1,1), N(2)H(+) J = 4-3, and CO J = 3-2 are presented. H(2)D(+) and N(2)H(+) are not detected and using the CO 3-2 disk size the observations result in an upper limit of < 0.47 K km s(-1) for both lines, a factor of 2.5 below previous single-dish H(2)D(+) observations. Assuming LTE, a disk midplane temperature of 10-20 K and estimates of the H(2)D(+) o/p ratio, the observed limit corresponds to N(H2D+) < 4-21 x 10(12) cm(-2). We adopt a parametric model for the disk structure from the literature and use new IRAM 30 m telescope observations of the H(13)CO(+) J = 3-2 line and previously published SMA observations of the N(2)H(+) J = 3-2, HCO(+) J = 3-2, and DCO(+) J = 3-2 lines to constrain the ionization fraction, x(i), in three temperature regions in the disk where theoretical considerations suggest different ions should dominate: (1) a warm, upper layer with T > 20 K where CO is in the gas phase and HCO+ is most abundant, where we estimate x(i) similar or equal to 4 x 10(-10); (2) a cooler molecular layer with T = 16-20 K where N(2)H(+) and DCO(+) abundances are predicted to peak, with x(i) similar or equal to 3 x 10(-11); and (3) the cold, dense midplane with T < 16 K where H(3)(+) and its deuterated isotopologues are the main carriers of positive charge, with x(i) < 3 x 10(-10). While there are considerable uncertainties, these estimates are consistent with a decreasing ionization fraction into the deeper, colder, and denser disk layers. Stronger constraints on the ionization fraction in the disk midplane will require not only substantially more sensitive observations of the H(2)D(+) 1(1,0)-1(1,1) line, but also robust determinations of the o/p ratio, observations of D(2)H(+), and stronger constraints on where N(2) is present in the gas phase.
C1 [Oeberg, Karin I.; Qi, Chunhua; Wilner, David J.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG
(Germany); IGN (Spain); NASA [NAS 5-26555]; NASA Origins of Solar
Systems [NNX11AK63]; Space Telescope Science Institute
FX This manuscript has benefited from comments by an anonymous referee and
from discussions with Eric Herbst and Ted Bergin. 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 IRAM 30 m
telescope is operated by IRAM, which is supported by INSU/CNRS (France),
MPG (Germany), and IGN (Spain). Support for K.I.O. is provided by NASA
through a Hubble Fellowship grant 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. We
also acknowledge NASA Origins of Solar Systems grant No. NNX11AK63.
NR 34
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U2 4
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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 DEC 20
PY 2011
VL 743
IS 2
AR 152
DI 10.1088/0004-637X/743/2/152
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400054
ER
PT J
AU Perlman, ES
Adams, SC
Cara, M
Bourque, M
Harris, DE
Madrid, JP
Simons, RC
Clausen-Brown, E
Cheung, CC
Stawarz, L
Georganopoulos, M
Sparks, WB
Biretta, JA
AF Perlman, Eric S.
Adams, Steven C.
Cara, Mihai
Bourque, Matthew
Harris, D. E.
Madrid, Juan P.
Simons, Raymond C.
Clausen-Brown, Eric
Cheung, C. C.
Stawarz, Lukasz
Georganopoulos, Markos
Sparks, William B.
Biretta, John A.
TI OPTICAL POLARIZATION AND SPECTRAL VARIABILITY IN THE M87 JET
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (M87); galaxies: jets; galaxies:
nuclei
ID SPACE-TELESCOPE OBSERVATIONS; ACTIVE GALACTIC NUCLEI; HELICAL
MAGNETIC-FIELD; RADIO GALAXY M87; LINEAR-POLARIZATION; RELATIVISTIC
JETS; RAY-EMISSION; HST-1; INSTABILITY; MODEL
AB During the last decade, M87's jet has been the site of an extraordinary variability event, with one knot (HST-1) increasing by over a factor 100 in brightness. Variability has also been seen on timescales of months in the nuclear flux. Here we discuss the optical-UV polarization and spectral variability of these components, which show vastly different behavior. HST-1 shows a highly significant correlation between flux and polarization, with P increasing from similar to 20% at minimum to >40% at maximum, while the orientation of its electric vector stayed constant. HST-1's optical-UV spectrum is very hard (alpha(UV-O) similar to 0.5, F(v) alpha v(-alpha)), and displays "hard lags" during epochs 2004.9-2005.5, including the peak of the flare, with soft lags at later epochs. We interpret the behavior of HST-1 as enhanced particle acceleration in a shock, with cooling from both particle aging and the relaxation of the compression. We set 2 sigma upper limits of 0.5 delta pc and 1.02c on the size and advance speed of the flaring region. The slight deviation of the electric vector orientation from the jet position angle (P. A.) makes it likely that on smaller scales the flaring region has either a double or twisted structure. By contrast, the nucleus displays much more rapid variability, with a highly variable electric vector orientation and "looping" in the (I, P) plane. The nucleus has a much steeper spectrum (alpha(UV-O) similar to 1.5) but does not show UV-optical spectral variability. Its behavior can be interpreted as either a helical distortion to a steady jet or a shock propagating through a helical jet.
C1 [Perlman, Eric S.; Cara, Mihai; Bourque, Matthew; Simons, Raymond C.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Adams, Steven C.] Univ Georgia, Dept Phys & Astron, Athens, GA 30605 USA.
[Bourque, Matthew; Harris, D. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Madrid, Juan P.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Clausen-Brown, Eric] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA.
[Stawarz, Lukasz] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Georganopoulos, Markos] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Sparks, William B.; Biretta, John A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Perlman, ES (reprint author), Florida Inst Technol, Dept Phys & Space Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA.
EM eperlman@fit.edu
RI Cara, Mihai/G-1023-2013;
OI Perlman, Eric/0000-0002-3099-1664
FU NASA under LTSA [NNX07AM17G]; HST [GO-11138.01]; NASA Fermi
[NNX10AO46G]; National Science Foundation Research Experiences for
Undergraduates (REU) [NSFAST-1004872]
FX We thank an anonymous referee for thoughtful comments that significantly
improved the quality of this paper. E. S. P., M. G., M. C., and R. C. S.
acknowledge support from NASA under LTSA program Grant NNX07AM17G and
HST Grant GO-11138.01. E. C. acknowledges support from the NASA Fermi
Grant NNX10AO46G. S. C. A. and M. B. acknowledge SARA REU fellowships,
funded by the National Science Foundation Research Experiences for
Undergraduates (REU) program through grant NSFAST-1004872. E. S. P.
acknowledges interesting discussions with L. Sironi and M. Birkinshaw
which helped with understanding the variability behavior we see.
NR 65
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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 DEC 20
PY 2011
VL 743
IS 2
AR 119
DI 10.1088/0004-637X/743/2/119
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400021
ER
PT J
AU Pineda, JE
Arce, HG
Schnee, S
Goodman, AA
Bourke, T
Foster, JB
Robitaille, T
Tanner, J
Kauffmann, J
Tafalla, M
Caselli, P
Anglada, G
AF Pineda, Jaime E.
Arce, Hector G.
Schnee, Scott
Goodman, Alyssa A.
Bourke, Tyler
Foster, Jonathan B.
Robitaille, Thomas
Tanner, Joel
Kauffmann, Jens
Tafalla, Mario
Caselli, Paola
Anglada, Guillem
TI THE ENIGMATIC CORE L1451-mm: A FIRST HYDROSTATIC CORE? OR A HIDDEN
VeLLO?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: individual objects (L1451, Perseus); ISM: molecules;
stars: formation; stars: low-mass
ID 2-DIMENSIONAL RADIATIVE-TRANSFER; SPITZER C2D SURVEY; PERSEUS MOLECULAR
CLOUD; YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; DENSE CORES;
STAR-FORMATION; PROTOSTELLAR ENVELOPES; DARK CLOUDS; SUBMILLIMETER ARRAY
AB We present the detection of a dust continuum source at 3 mm (CARMA) and 1.3 mm (Submillimeter Array, SMA), and (12)CO (2-1) emission (SMA) toward the L1451-mm dense core. These detections suggest a compact object and an outflow where no point source at mid-infrared wavelengths is detected using Spitzer. An upper limit for the dense core bolometric luminosity of 0.05 L(circle dot) is obtained. By modeling the broadband spectral energy distribution and the continuum interferometric visibilities simultaneously, we confirm that a central source of heating is needed to explain the observations. This modeling also shows that the data can be well fitted by a dense core with a young stellar object (YSO) and a disk, or by a dense core with a central first hydrostatic core (FHSC). Unfortunately, we are not able to decide between these two models, which produce similar fits. We also detect (12)CO (2-1) emission with redshifted and blueshifted emission suggesting the presence of a slow and poorly collimated outflow, in opposition to what is usually found toward YSOs but in agreement with prediction from simulations of an FHSC. This presents the best candidate, so far, for an FHSC, an object that has been identified in simulations of collapsing dense cores. Whatever the true nature of the central object in L1451-mm, this core presents an excellent laboratory to study the earliest phases of low-mass star formation.
C1 [Pineda, Jaime E.; Goodman, Alyssa A.; Bourke, Tyler; Foster, Jonathan B.; Robitaille, Thomas; Kauffmann, Jens] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Arce, Hector G.; Tanner, Joel] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Schnee, Scott] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Tafalla, Mario] Observ Astron Nacl IGN, E-28014 Madrid, Spain.
[Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Anglada, Guillem] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
RP Pineda, JE (reprint author), ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM jaime.pineda@manchester.ac.uk
RI Pineda, Jaime/J-7405-2013; Goodman, Alyssa/A-6007-2010;
OI Pineda, Jaime/0000-0002-3972-1978; Goodman, Alyssa/0000-0003-1312-0477;
Robitaille, Thomas/0000-0002-8642-1329
FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Smithsonian Institution;
Academia Sinica; state of California; state of Illinois; state of
Maryland; James S. McDonnell Foundation; Gordon and Betty Moore
Foundation; Kenneth T. and Eileen L. Norris Foundation; University of
Chicago; Associates of the California Institute of Technology; National
Science Foundation; NSF [AST-9613615]; Association of Universities for
Research in Astronomy, Inc. [AF002]; Fundacion Andes [C-13442]; NRAO
[GSSP06-0015, GSSP08-0031]; National Science Foundation [AST-0407172,
AST-0908159, AST-0845619]; NASA Origins [NXX09AB89G]; MICINN
[AYA2008-06189-C03-01]; Junta de Andalucia; Associated Universities,
Inc.
FX Based on observations carried out with the IRAM 30 m Telescope, the
Submillimeter Array, and CARMA. IRAM is supported by INSU/CNRS (France),
MPG (Germany), and IGN (Spain). The Submillimeter Array is a joint
project between the Smithsonian Astrophysical Observatory and the
Academia Sinica Institute of Astronomy and Astrophysics and is funded by
the Smithsonian Institution and the Academia Sinica. 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.; J.E.P. acknowledges support by the NSF through grant
AF002 from the Association of Universities for Research in Astronomy,
Inc., under NSF cooperative agreement AST-9613615 and by Fundacion Andes
under project no. C-13442. Support for this work was provided by the NSF
through awards GSSP06-0015 and GSSP08-0031 from the NRAO. This material
is based upon work supported by the National Science Foundation under
grant nos. AST-0407172 and AST-0908159 to AAG and AST-0845619 to HGA. T.
L. B. acknowledges support from NASA Origins grant NXX09AB89G. G. A.
acknowledges support from MICINN AYA2008-06189-C03-01 grant (cofunded
with FEDER funds), and from Junta de Andalucia. We wish to thank the
anonymous referee for suggestions that helped improve this paper. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.
NR 76
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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 DEC 20
PY 2011
VL 743
IS 2
AR 201
DI 10.1088/0004-637X/743/2/201
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400103
ER
PT J
AU Salyk, C
Blake, GA
Boogert, ACA
Brown, JM
AF Salyk, C.
Blake, G. A.
Boogert, A. C. A.
Brown, J. M.
TI CO ROVIBRATIONAL EMISSION AS A PROBE OF INNER DISK STRUCTURE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE protoplanetary disks; stars: pre-main sequence
ID T-TAURI STARS; HERBIG AE/BE STARS; YOUNG STELLAR OBJECTS; NEAR-INFRARED
EMISSION; PLANET-FORMING ZONES; MAIN-SEQUENCE STARS; PROTOPLANETARY
DISKS; CIRCUMSTELLAR DISK; AB-AURIGAE; TRANSITIONAL DISKS
AB We present an analysis of CO emission lines from a sample of T Tauri, Herbig Ae/Be, and transitional disks with known inclinations in order to study the structure of inner disk molecular gas. We calculate CO inner radii by fitting line profiles with a simple parameterized model. We find that, for optically thick disks, CO inner radii are strongly correlated with the total system luminosity (stellar plus accretion) and consistent with the dust sublimation radius. Transitional disk inner radii show the same trend with luminosity, but are systematically larger. Using rotation diagram fits, we derive, for classical T Tauri disks, emitting areas consistent with a ring of width similar to 0.15 AU located at the CO inner radius; emitting areas for transitional disks are systematically smaller. We also measure lower rotational temperatures for transitional disks, and disks around Herbig Ae/Be stars, than for those around T Tauri stars. Finally, we find that rotational temperatures are similar to, or slightly lower than, the expected temperature of blackbody grains located at the CO inner radius, in contrast to expectations of thermal decoupling between gas and dust.
C1 [Salyk, C.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Boogert, A. C. A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Brown, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Salyk, C (reprint author), Univ Texas Austin, McDonald Observ, 1 Univ Stn,C1402, Austin, TX 78712 USA.
FU W. M. Keck Foundation
FX 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 77
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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 DEC 20
PY 2011
VL 743
IS 2
AR 112
DI 10.1088/0004-637X/743/2/112
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400014
ER
PT J
AU Winston, E
Wolk, SJ
Bourke, TL
Megeath, ST
Gutermuth, R
Spitzbart, B
AF Winston, E.
Wolk, S. J.
Bourke, T. L.
Megeath, S. T.
Gutermuth, R.
Spitzbart, B.
TI THE STRUCTURE OF THE STAR-FORMING CLUSTER RCW 38
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: stars; stars: formation; stars: massive; stars: pre-main
sequence; X-rays: stars
ID YOUNG STELLAR OBJECTS; INFRARED ARRAY CAMERA; SPITZER-SPACE-TELESCOPE;
MULTIBAND IMAGING PHOTOMETER; POINT-SOURCE IDENTIFICATION;
COLOR-MAGNITUDE DIAGRAMS; SERPENS CLOUD CORE; X-RAY-EMISSION; T-TAURI
STARS; MOLECULAR CLOUD
AB We present a study of the structure of the high-mass star-forming region RCW 38 and the spatial distribution of its young stellar population. Spitzer Infrared Array Camera (IRAC) photometry (3-8 mu m) is combined with Two Micron All Sky Survey near-IR data to identify young stellar objects (YSOs) by IR-excess emission from their circumstellar material. Chandra X-ray data are used to identify class III pre-main-sequence stars lacking circumstellar material. We identify 624 YSOs: 23 class 0/I and 90 flat spectrum protostars, 437 class II stars, and 74 class III stars. We also identify 29 (27 new) O star candidates over the IRAC field. Seventy-two stars exhibit IR-variability, including 7 class 0/I and 12 flat spectrum YSOs. A further 177 tentative candidates are identified by their location in the IRAC [3.6] versus [3.6]-[5.8] color-magnitude diagram. We find strong evidence of subclustering in the region. Three subclusters were identified surrounding the central cluster, with massive and variable stars in each subcluster. The central region shows evidence of distinct spatial distributions of the protostars and pre-main-sequence stars. A previously detected IR cluster, DB2001_Obj36, has been established as a subcluster of RCW 38. This suggests that star formation in RCW 38 occurs over a more extended area than previously thought. The gas-to-dust ratio is examined using the X-ray derived hydrogen column density, N(H) and the K-band extinction, and found to be consistent with the diffuse interstellar medium, in contrast with Serpens and NGC 1333. We posit that the high photoionizing flux of massive stars in RCW 38 affects the agglomeration of the dust grains.
C1 [Winston, E.] ESA ESTEC SRE SA, NL-2201 AZ Noordwijk, Netherlands.
[Wolk, S. J.; Bourke, T. L.; Spitzbart, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA.
[Gutermuth, R.] Smith Coll, Coll Astron Dept 5, Northampton, MA 01027 USA.
[Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
RP Winston, E (reprint author), ESA ESTEC SRE SA, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
EM ewinston@rssd.esa.int
OI Wolk, Scott/0000-0002-0826-9261
FU NASA [1407, 1256790, 960541, NAS5-26555]; National Aeronautics and Space
Administration; National Science Foundation; National Aeronautics and
Space Administration's Earth Science Technology Office [NCC5-626]; Space
Telescope Science Institute [11123]
FX The authors thank the referee for many helpful comments. This work is
based on observations made with the Spitzer Space Telescope (PID 20127),
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 contract 1256790 issued by JPL/Caltech. Support
for the IRAC instrument was provided by NASA through contract 960541
issued by JPL. 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 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
research made use of Montage, funded by the National Aeronautics and
Space Administration's Earth Science Technology Office, Computation
Technologies Project, under Cooperative Agreement Number NCC5-626
between NASA and the California Institute of Technology. Montage is
maintained by the NASA/IPAC Infrared Science Archive. T. L. B.
acknowledges support from NASA through a grant for HST program 11123
from the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Incorporated,
under NASA contract NAS5-26555.
NR 75
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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 DEC 20
PY 2011
VL 743
IS 2
AR 166
DI 10.1088/0004-637X/743/2/166
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863PO
UT WOS:000298178400068
ER
PT J
AU Palau, A
Fuente, A
Girart, JM
Fontani, F
Boissier, J
Pietu, V
Sanchez-Monge, A
Busquet, G
Estalella, R
Zapata, LA
Zhang, QZ
Neri, R
Ho, PTP
Alonso-Albi, T
Audard, M
AF Palau, Aina
Fuente, Asuncion
Girart, Josep M.
Fontani, Francesco
Boissier, Jeremie
Pietu, Vincent
Sanchez-Monge, Alvaro
Busquet, Gemma
Estalella, Robert
Zapata, Luis A.
Zhang, Qizhou
Neri, Roberto
Ho, Paul T. P.
Alonso-Albi, Tomas
Audard, Marc
TI INTERMEDIATE-MASS HOT CORES AT similar to 500 AU: DISKS OR OUTFLOWS?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual objects (IRAS 22198+6336, AFGL 5142); ISM: lines and
bands; radio continuum: ISM; stars: formation
ID STAR-FORMING REGIONS; ORION-KL; HIGH-RESOLUTION; PROTOSTELLAR CORES;
COMPLEX-MOLECULES; IRAS 22198+6336; MILLIMETER; CHEMISTRY; AFGL-5142;
IRAS-16293-2422
AB Observations with the Plateau de Bure Interferometer in the most extended configuration toward two intermediate-mass star-forming regions, IRAS 22198+6336 and AFGL 5142, reveal the presence of several complex organic molecules at similar to 500 AU scales, confirming the presence of hot cores in both regions. The hot cores are not rich in CN-bearing molecules, as often seen in massive hot cores, and are mainly traced by CH(3)CH(2)OH, (CH(2)OH)(2), CH(3)COCH(3), and CH(3)OH, with, additionally, CH(3)CHO, CH(3)OD, and HCOOD for IRAS 22198+6336, and C(6)H and O(13)CS for AFGL 5142. The emission of complex molecules is resolved down to sizes of similar to 300 and similar to 600 AU, for IRAS 22198+6336 and AFGL 5142, respectively, and most likely is tracing protostellar disks rather than flattened envelopes or toroids as is usually found. This is especially clear for the case of IRAS 22198+6336, where we detect a velocity gradient for all the mapped molecules perpendicular to the most chemically rich outflow of the region, yielding a dynamic mass less than or similar to 4 M(circle dot). As for AFGL 5142, the hot core emission is resolved into two elongated cores separated similar to 1800 AU. A detailed comparison of the complex molecule peaks to the new CO (2-1) data and H(2)O maser data from the literature suggests also that for AFGL 5142 the complex molecules are mainly associated with disks, except for a faint and extended molecular emission found to the west, which is possibly produced in the interface between one of the outflows and the dense surrounding gas.
C1 [Palau, Aina; Girart, Josep M.] CSIC IEEC, Inst Ciencias Espai, Bellaterra 08193, Catalunya, Spain.
[Fuente, Asuncion; Alonso-Albi, Tomas] Observ Astron Nacl, Madrid 28803, Spain.
[Fontani, Francesco; Sanchez-Monge, Alvaro] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Boissier, Jeremie] INAF, Ist Radioastron, Bologna, Italy.
[Boissier, Jeremie] ESO, D-85748 Garching, Muenchen, Germany.
[Pietu, Vincent; Neri, Roberto] IRAM, F-38406 St Martin Dheres, France.
[Busquet, Gemma] INAF, Ist Fis Spazio Interplanetario, Area Recerca Tor Vergata, I-00133 Rome, Italy.
[Estalella, Robert] Univ Barcelona, Inst Ciencias Cosmos, Dept Astron & Meteorol, IEEC UB, E-08028 Barcelona, Spain.
[Zapata, Luis A.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico.
[Zhang, Qizhou; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Audard, Marc] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland.
RP Palau, A (reprint author), CSIC IEEC, Inst Ciencias Espai, Campus UAB Fac Ciencias,Torre C5,Parell 2, Bellaterra 08193, Catalunya, Spain.
EM palau@ieec.uab.es
RI Girart, Josep/O-1638-2014; Fuente, Asuncion/G-1468-2016;
OI Girart, Josep/0000-0002-3829-5591; Fuente, Asuncion/0000-0001-6317-6343;
Fontani, Francesco/0000-0003-0348-3418; Zhang,
Qizhou/0000-0003-2384-6589
FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Spanish MICINN
[AYA2008-06189-C03, CSD2009-00038]; FEDER; JAE-Doc CSIC; European Social
Fund; European Community [FP7/2007-2013, 229517]
FX Based on observations carried out with the IRAM Plateau de Bure
Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany),
and IGN (Spain).; A.P. is grateful to Catherine Walsh and Belen Tercero
for useful discussions on modeling of protostellar disks and line
identification, and to the referee, Simon Bruderer, whose comments
largely improved the quality of this Letter. 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.
This Letter was partially supported by the Spanish MICINN program
"CONSOLIDER INGENIO 2010: Molecular Astrophysics, Herschel-ALMA Era,
ASTROMOL" (CSD2009-00038), and by the European Community's Seventh
Framework Program (FP7/2007-2013) under agreement 229517.
NR 43
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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 DEC 20
PY 2011
VL 743
IS 2
AR L32
DI 10.1088/2041-8205/743/2/L32
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 863HD
UT WOS:000298152500007
ER
PT J
AU Herre, EA
Shuker, DM
West, SA
AF Herre, Edward Allen
Shuker, David M.
West, Stuart A.
TI Social Evolution: Evolving Sex Ratios
SO CURRENT BIOLOGY
LA English
DT Editorial Material
ID ADJUSTMENT; WASPS
C1 [Herre, Edward Allen] Smithsonian Trop Res Inst, Dpo, AA 34002 USA.
[Shuker, David M.] Univ St Andrews, Sch Biol, St Andrews KY16 9TH, Fife, Scotland.
[West, Stuart A.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England.
RP Herre, EA (reprint author), Smithsonian Trop Res Inst, Unit 9100,Box 0948, Dpo, AA 34002 USA.
EM herrea@si.edu
RI Shuker, David/E-8827-2013; West, Stuart/M-3608-2014
OI West, Stuart/0000-0003-2152-3153
NR 14
TC 0
Z9 0
U1 1
U2 25
PU CELL PRESS
PI CAMBRIDGE
PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA
SN 0960-9822
EI 1879-0445
J9 CURR BIOL
JI Curr. Biol.
PD DEC 20
PY 2011
VL 21
IS 24
BP R992
EP R994
DI 10.1016/j.cub.2011.10.047
PG 3
WC Biochemistry & Molecular Biology; Cell Biology
SC Biochemistry & Molecular Biology; Cell Biology
GA 867FK
UT WOS:000298440100011
PM 22192832
ER
PT J
AU Tryon, CA
Kuhn, SL
Slimak, L
Logan, MAV
Balkan-Atli, N
AF Tryon, Christian A.
Kuhn, Steven L.
Slimak, Ludovic
Logan, M. Amelia V.
Balkan-Atli, Nur
TI Scale in tephrostratigraphic correlation: An example from Turkish
Pleistocene archaeological sites
SO QUATERNARY INTERNATIONAL
LA English
DT Article
ID MIDDLE STONE-AGE; CENTRAL ANATOLIA; KALETEPE-DERESI-3 TURKEY; NUMERICAL
CONSIDERATIONS; GEOCHEMICAL ANALYSIS; KAPTHURIN FORMATION; DISTAL
MICROTEPHRA; QUATERNARY TEPHRAS; CENTRAL ALASKA; GLASS SHARDS
AB Issues of scale are persistent but rarely made explicit in tephrostratigraphy. Eruption magnitude, the nature of available outcrop, and the resolution and type of data available define the scale of any proposed correlation. Different scales require different approaches to demonstrate, or more accurately, to estimate the likelihood of correlation among two or more deposits. This is emphasized through a probabilistic approach to the correlation of proximal and distal tephra deposits associated with Lower and Middle Paleolithic archaeological sites from central Turkey through the use of discriminant analyses and multiple analyses of variance. (C) 2011 Elsevier Ltd and INQUA. All rights reserved.
C1 [Tryon, Christian A.] NYU, Dept Anthropol, Ctr Study Human Origins, New York, NY 10003 USA.
[Kuhn, Steven L.] Univ Arizona, Dept Anthropol, Tucson, AZ 85721 USA.
[Slimak, Ludovic] Univ Toulouse 2, TRACES, CNRS, UMR 5608, F-31058 Toulouse, France.
[Logan, M. Amelia V.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
[Balkan-Atli, Nur] Istanbul Univ, Fac Letters, Prehist Sect, TR-34134 Istanbul, Turkey.
RP Tryon, CA (reprint author), NYU, Dept Anthropol, Ctr Study Human Origins, 25 Waverly Pl, New York, NY 10003 USA.
EM christian.tryon@nyu.edu; skuhn@email.arizona.edu; slimakl@yahoo.fr;
logana@si.edu; nbalkan@istanbul.edu.tr
OI Tryon, Christian/0000-0002-2354-3273
FU Leakey Foundation; Wenner-Gren Foundation; New York University; National
Science Foundation
FX The work reported in this paper was funded by grants from the Leakey
Foundation, the Wenner-Gren Foundation, and New York University, and is
the outcome of numerous discussions with and encouragement from David
Lowe, Christopher Campisano, Kieran McNulty, Anthony Philpotts, Jeremy
Delaney, Matthew Tocheri, Rhonda Kauffman, and everyone at INQUA's
Active Tephra in Kyushu conference. Many of the ideas here, more fully
developed in Kyushu, owe their original genesis to Tryon's invitation by
David Killick to speak at the National Science Foundation IGERT-funded
program in Archaeological Science at the University of Arizona and the
discussion that ensued. Nicholas Pearce, Lindsay McHenry, and an
anonymous reviewer provided excellent comments that substantially
improved the quality of the manuscript. This is a contribution towards
meeting objective three of the INTREPID project of INQUA's International
focus group on tephrochronology and volcanism.
NR 66
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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 DEC 20
PY 2011
VL 246
BP 124
EP 133
DI 10.1016/j.quaint.2011.05.039
PG 10
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 864WG
UT WOS:000298270600012
ER
PT J
AU Harasewych, MG
Sikaroodi, M
Gillevet, PM
AF Harasewych, M. G.
Sikaroodi, Masoumeh
Gillevet, Patrick M.
TI The Delray Beach, Florida, colony of Cerion (Paracerion) tridentatum
costellata Pilsbry, 1946 (Gastropoda: Pulmonata: Cerionidae): Evidence
for indirect Cuban origins
SO NAUTILUS
LA English
DT Article
DE Native species; introduced species; cytochrome c oxidase I
ID LAND SNAIL CERION; HYBRIDIZATION; HISTORY; BAHAMAS
AB A large colony of Cerion has recently been reported from Delray Beach, Florida, far north from the ranges of both native and introduced species of Cerion. Specimens correspond morphologically to the type series of Cerion (Paracerion) tridentatum costellata Pilsbry, 1946, which no longer survives at its type locality (Fort Jefferson, Garden Key, Dry Tortugas, Florida.) Historical data indicate that this taxon is a hybrid of two or more of the five Cuban species of Cerion introduced to Fort Jefferson by Bartsch in June, 1924. Museum records document that a propagule of this hybrid taxon was transplanted to Boynton Beach in the late 1940s and proliferated to give rise to the Delray Beach colony. Partial cytochrome c oxidase I sequences reveal the Delray colony to be monophyletic, and of exclusively Cuban ancestry. Limited sampling confirms the presence of mitochondrial genes from two (C. tridentatum and C. sculptum marielinum) of the five Cerion taxa introduced to Fort Jefferson in 1924. A larger sample size, together with data from nuclear genes, will be needed to rule out the presence of rare alleles from other taxa. Transplantation of this newly formed hybrid propagule to an area distant from either parent population has allowed it to evolve in isolation and provides a unique opportunity to study the origins and persistence of genetic diversity within the genus Cerion.
C1 [Harasewych, M. G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Sikaroodi, Masoumeh; Gillevet, Patrick M.] George Mason Univ, Dept Environm Sci & Policy, Manassas, VA 20110 USA.
RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
EM Harasewych@si.edu; msikaroo@gmu.edu; pgilleve@gmu.edu
FU NSF [EAR 1016936]
FX We are very grateful to Wayne Harland, Anne Joffe, Harry G. Lee, M.D.,
Anton Oleinik; Yolanda Villacampa, Peggy Williams, and the late Stephen.
J. Gould and Glenn Goodfriend for contributing many of the samples of
Cerion from throughout the range of the genus. We thank Dr. Gary
Rosenberg and Paul Callomon for access to the collections of Cerion at
the Academy of Natural Sciences of Philadelphia. The assistance of Ms.
Jeanne Allegretti, Palm Beach County Property Appraiser, in determining
the precise location of the "McGinty lawn" is very much appreciated.
This research was supported in part by NSF Grant # EAR 1016936. This is
Smithsonian Marine Station at Fort Pierce Contribution Number 856.
NR 31
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PI SANIBEL
PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD,
SANIBEL, FL 33957 USA
SN 0028-1344
J9 NAUTILUS
JI Nautilus
PD DEC 16
PY 2011
VL 125
IS 4
BP 173
EP 181
PG 9
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 871EC
UT WOS:000298719700001
ER
PT J
AU Baldwin, CC
Brito, BJ
Smith, DG
Weigt, LA
Escobar-Briones, E
AF Baldwin, Carole C.
Brito, Balam J.
Smith, David G.
Weigt, Lee A.
Escobar-Briones, Elva
TI Identification of early life-history stages of Caribbean Apogon
(Perciformes: Apogonidae) through DNA Barcoding
SO ZOOTAXA
LA English
DT Article
DE CO1; cardinalfishes; fish larvae; pigmentation patterns; chromatophores;
Belize
ID GOBIIDAE; LARVAL; SEA
AB Early life-history stages of 12 of 17 species of western Central Atlantic Apogon were identified using molecular data. A neighbor-joining tree was constructed from mitochondrial cytochrome oxidase-c subunit I (COI) sequences, and genetic lineages of Apogon in the tree were identified to species based on adults in the lineages. Relevant portions of the tree subsequently were used to identify larvae of Apogon species from Carrie Bow Cay, Belize, and juveniles from Belize and other western Central Atlantic localities. Diagnostic morphological characters of larvae and juveniles were investigated by examining preserved vouchers from which the DNA was extracted and digital color photographs of those specimens taken before preservation. Orange and yellow chromatophore patterns are the easiest and sometimes only means of separating Apogon larvae. Patterns of melanophores and morphometric features are of limited diagnostic value. For juveniles, chromatophore patterns and the developing dark blotches characteristic of adults are the most useful diagnostic features. Larvae were identified for Apogon aurolineatus, A. binotatus, A. maculatus, A. mosavi, A. phenax, A. planifrons, and A. townsendi. Juveniles were identified for those species (except A. planifrons) and for A. pseudomaculatus, A. lachneri, A. pillionatus, A. robbyi, and A. quadrisquamatus. One larval specimen occurs in an unidentified genetic lineage, and five adults occur in another unidentified genetic lineage. Apogon species can be divided into at least four groups based on pigmentation patterns in early life stages. Further investigation is needed to determine if those groups are meaningful in the generic classification of Apogon species.
C1 [Baldwin, Carole C.; Smith, David G.; Weigt, Lee A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Brito, Balam J.; Escobar-Briones, Elva] Univ Nacl Autonoma Mexico, Inst Ciencias Mar & Limnol, Mexico City 04510, DF, Mexico.
RP Baldwin, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
EM baldwinc@si.edu; ixbalamquemx@gmail.com; smithd@si.edu; weigtl@si.edu;
escobri@cmarl.unam.mx
FU Consejo Nacional de Ciencia y Tecnologia (CONACyT); PAPIIT [IN 207410];
Direccion General de Posgrados (DGP, UNAM)
FX We thank A. Driskell and A. Ormos for laboratory and logistical
assistance; M. Carpenter, A. Driskell, C. DeCourley, Z. Foltz, J. Lang,
L. Lang, D. Miller, J. Mounts, and R. Murphy for assistance in the
field; P. Diaz, M. Lavin, L. Sanchez and A. Kobelkowsky for their
guidance of the first author; J. T. Williams, J. Van Tassell, and D. R.
Robertson for providing images; D. R. Robertson, D. Griswold, and C.
Castillo for help with image editing; the Smithsonian Marine Science
Network and the National Museum of Natural History Small-Grants Program
for financial support to the first author; the Consejo Nacional de
Ciencia y Tecnologia (CONACyT) for financial support for the second
author to conduct research at the Smithsonian's National Museum of
Natural History; PAPIIT IN 207410 for support granted to E. Escobar; and
the Direccion General de Posgrados (DGP, UNAM) for financial support
within the International Exchange Student Program. Research in Florida
was conducted pursuant to SAL # 07SR-1024B to the first author. A.
Gazit, K. Wilson, and M. Kunen facilitated collecting in Curacao through
the CARM-ABI laboratory. Fieldwork in the Bahamas was conducted under
the auspices of the Perry Institute of Marine Science, with logistical
assistance from B. Gadd, E. Lamarre, and D. O'Donnell, This is Caribbean
Coral Reef Ecosystems Program (CCRE) contribution number XXX and
Smithsonian Marine Station at Ft. Pierce, FL (SMSFP) contribution number
XXX.
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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 DEC 16
PY 2011
IS 3133
BP 1
EP 36
PG 36
WC Zoology
SC Zoology
GA 887OW
UT WOS:000299938900001
ER
PT J
AU Mascaro, J
Detto, M
Asner, GP
Muller-Landau, HC
AF Mascaro, Joseph
Detto, Matteo
Asner, Gregory P.
Muller-Landau, Helene C.
TI Evaluating uncertainty in mapping forest carbon with airborne LiDAR
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Aboveground biomass; Crown radius; Light detection and ranging; Tree
allometry; Tropical forest carbon stocks; Spatial autocorrelation
ID BARRO-COLORADO ISLAND; TROPICAL RAIN-FOREST; ABOVEGROUND BIOMASS;
PANAMA; AMAZON
AB Airborne LiDAR is increasingly used to map carbon stocks in tropical forests, but our understanding of mapping errors is constrained by the spatial resolution (i.e., plot size) used to calibrate LiDAR with field data (typically 0.1-0.36 ha). Reported LiDAR errors range from 17 to 40 Mg C ha(-1), but should be lower at coarser resolutions because relative errors are expected to scale with (plot area)(-1/2). We tested this prediction empirically using a 50-ha plot with mapped trees, allowing an assessment of LiDAR prediction errors at multiple spatial resolutions. We found that errors scaled approximately as expected, declining by 38% (compared to 40% predicted from theory) from 0.36- to 1-ha resolution. We further reduced errors at all spatial resolutions by accounting for tree crowns that are bisected by plot edges (not typically done in forestry), and collectively show that airborne LiDAR can map carbon stocks with 10% error at 1-ha resolution a level comparable to the use of field plots alone. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Mascaro, Joseph; Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Mascaro, Joseph; Detto, Matteo; Muller-Landau, Helene C.] 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
RI Asner, Gregory/G-9268-2013
OI Asner, Gregory/0000-0001-7893-6421
FU Gordon and Betty Moore Foundation; John D. and Catherine T. MacArthur
Foundation; HSBC Climate Partnership; National Science Foundation
[DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102,
DEB-9909347, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058,
DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197]; Center for Tropical
Forest Science; Smithsonian Tropical Research Institute; Mellon
Foundation; Celera Foundation
FX We thank Ty Kennedy-Bowdoin, James Jacobson, David Knapp, Aravindh
Balaji and the rest of the Carnegie Airborne Observatory team for
collecting and processing airborne LiDar data, and two anonymous
reviewers for comments on a previous version of this manuscript. This
study was supported by the Gordon and Betty Moore Foundation, the John
D. and Catherine T. MacArthur Foundation, and the HSBC Climate
Partnership. The Carnegie Airborne Observatory is made possible by the
Gordon and Betty Moore Foundation, W.M. Keck foundation, and William
Hearst III. The BCI forest dynamics research project is made possible by
National Science Foundation grants to S. P. Hubbell: DEB-0640386,
DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347,
DEB-9615226, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058,
DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197, support from the
Center for Tropical Forest Science, the Smithsonian Tropical Research
Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon
Foundation, the Celera Foundation, and numerous private individuals, and
through the hard work of over 100 people from 10 countries over the past
two decades. The plot project is part the Center for Tropical Forest
Science, a global network of large-scale demographic tree plots.
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 15
PY 2011
VL 115
IS 12
BP 3770
EP 3774
DI 10.1016/j.rse.2011.07.019
PG 5
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 865LB
UT WOS:000298311300067
ER
PT J
AU Lazio, TJW
MacDowall, RJ
Burns, JO
Jones, DL
Weiler, KW
Demaio, L
Cohen, A
Dalal, NP
Polisensky, E
Stewart, K
Bale, S
Gopalswamy, N
Kaiser, M
Kasper, J
AF Lazio, T. Joseph W.
MacDowall, R. J.
Burns, Jack O.
Jones, D. L.
Weiler, K. W.
Demaio, L.
Cohen, A.
Dalal, N. Paravastu
Polisensky, E.
Stewart, K.
Bale, S.
Gopalswamy, N.
Kaiser, M.
Kasper, J.
TI The Radio Observatory on the Lunar Surface for Solar studies
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Heliophysics; Instrumentation: interferometers; Moon; Particle
acceleration; Radio astronomy
ID CORONAL MASS EJECTIONS; CYGNUS-A; BURSTS; EMISSION; INTERPLANETARY;
ACCELERATION; DENSITY; EVENTS; ARRAY; SPACECRAFT
AB The Radio Observatory on the Lunar Surface for Solar studies (ROLSS) is a concept for a near-side low radio frequency imaging interferometric array designed to study particle acceleration at the Sun and in the inner heliosphere. The prime science mission is to image the radio emission generated by Type II and III solar radio burst processes with the aim of determining the sites at and mechanisms by which the radiating particles are accelerated. Specific questions to be addressed include the following: (1) Isolating the sites of electron acceleration responsible for Type II and III solar radio bursts during coronal mass ejections (CMEs); and (2) Determining if and the mechanism(s) by which multiple, successive CMEs produce unusually efficient particle acceleration and intense radio emission. Secondary science goals include constraining the density of the lunar ionosphere by searching for a low radio frequency cutoff to solar radio emission and constraining the low energy electron population in astrophysical sources. Key design requirements on ROLSS include the operational frequency and angular resolution. The electron densities in the solar corona and inner heliosphere are such that the relevant emission occurs at frequencies below 10 MHz. Second, resolving the potential sites of particle acceleration requires an instrument with an angular resolution of at least 2 degrees, equivalent to a linear array size of approximately 1000 m. Operations would consist of data acquisition during the lunar day, with regular data downlinks. No operations would occur during lunar night.
ROLSS is envisioned as an interferometric array, because a single aperture would be impractically large. The major components of the ROLSS array are 3 antenna arms arranged in a Y shape, with a central electronics package (CEP) located at the center. The Y configuration for the antenna arms both allows for the formation of reasonably high dynamic range images on short time scales as well as relatively easy deployment. Each antenna arm is a linear strip of polyimide film (e.g., Kapton (TM)) on which 16 science antennas are located by depositing a conductor (e.g., silver). The antenna arms can be rolled for transport, with deployment consisting of unrolling the rolls. Each science antenna is a single polarization dipole. The arms also contain transmission lines for carrying the radio signals from the science antennas to the CEP. The CEP itself houses the receivers for the science antennas, the command and data handling hardware, and, mounted externally, the downlink antenna.
We have conducted two experiments relevant to the ROLSS concept. First, we deployed a proof-of-concept science antenna. Comparison of the impedance of the antenna feed points with simulations showed a high level of agreement, lending credence to the antenna concept. Second, we exposed a sample of space-qualified polyimide film, with a silver coating on one side, to temperature cycling and UV exposure designed to replicate a year on the lunar surface. No degradation of the polyimide film's material or electric properties was found. Both of these tests support the notion of using polyimide-film based antennas.
The prime science mission favors an equatorial site, and a site on the limb could simplify certain aspects of the instrument design. A site on the lunar near side is sufficient for meeting the science goals. While the site should be of relatively low relief topography, the entire site does not have to be flat as the fraction of the area occupied by the antenna arms is relatively small (similar to 0.3%). Further, the antenna arms do not have to lay flat as deviations of +/- 1 m are still small relative to the observational wavelengths. Deployment could be accomplished either with astronauts, completely robotically, or via a combination of crewed and robotic means.
Future work for the ROLSS concept includes more exhaustive testing of the radio frequency (RF) and environmental suitability of polyimide film-based science antennas, ultra-low power electronics in order to minimize the amount of power storage needed, batteries with a larger temperature range for both survival and operation, and rovers (robotic, crewed, or both) for deployment.
The ROLSS array could also serve as the precursor to a larger array on the far side of the Moon for astrophysical and cosmological studies. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Lazio, T. Joseph W.; Weiler, K. W.; Polisensky, E.; Stewart, K.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[Lazio, T. Joseph W.; MacDowall, R. J.; Burns, Jack O.; Jones, D. L.; Weiler, K. W.] NASA, Ames Res Ctr, Lunar Sci Inst, Sunnyvale, CA 94089 USA.
[MacDowall, R. J.; Demaio, L.; Gopalswamy, N.; Kaiser, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Burns, Jack O.] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Jones, D. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cohen, A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Bale, S.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Bale, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Kasper, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lazio, TJW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Joseph.Lazio@jpl.nasa.gov
RI Bale, Stuart/E-7533-2011; MacDowall, Robert/D-2773-2012; Gopalswamy,
Nat/D-3659-2012; Kasper, Justin/D-1152-2010
OI Bale, Stuart/0000-0002-1989-3596; Kasper, Justin/0000-0002-7077-930X
FU NASA [NNA09DB30A]
FX We thank J. Schmidt for helpful discussions about the implementation of
CME models for ROLSS, the crew of the GSFC IDL for their assistance in
refining the design, and the editor for her patience and assistance in
making sure that this manuscript was published. Part of this research
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration. The ROLSS concept study was funded by the NASA Lunar
Sortie Science Opportunities (LSSO) program. The LUNAR consortium is
funded by the NASA Lunar Science Institute (via Cooperative Agreement
NNA09DB30A) to investigate concepts for astrophysical observatories on
the Moon.
NR 46
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD DEC 15
PY 2011
VL 48
IS 12
BP 1942
EP 1957
DI 10.1016/j.asr.2011.07.006
PG 16
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 847UP
UT WOS:000296998300003
ER
PT J
AU Acciari, VA
Aliu, E
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bradbury, SM
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Christiansen, JL
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Duke, C
Errando, M
Falcone, A
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Godambe, S
Griffin, S
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Hughes, G
Hui, CM
Humensky, TB
Jackson, DJ
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Krawczynski, H
Krennrich, F
Lang, MJ
Madhavan, AS
Maier, G
McArthur, S
McCann, A
Moriarty, P
Newbold, MD
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
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
Swordy, SP
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Varlotta, A
Vassiliev, VV
Vincent, S
Vivier, M
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Williams, DA
Wood, M
AF Acciari, V. A.
Aliu, E.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cannon, A.
Cesarini, A.
Christiansen, J. L.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Duke, C.
Errando, M.
Falcone, A.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Godambe, S.
Griffin, S.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Holder, J.
Hughes, G.
Hui, C. M.
Humensky, T. B.
Jackson, D. J.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
Madhavan, A. S.
Maier, G.
McArthur, S.
McCann, A.
Moriarty, P.
Newbold, M. D.
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
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.
Swordy, S. P.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Varlotta, A.
Vassiliev, V. V.
Vincent, S.
Vivier, M.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Weisgarber, T.
Williams, D. A.
Wood, M.
TI VERITAS OBSERVATIONS OF GAMMA-RAY BURSTS DETECTED BY SWIFT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; gamma-ray burst: general
ID HIGH-ENERGY EMISSION; LARGE-AREA TELESCOPE; AFTERGLOW EMISSION; FERMI
OBSERVATIONS; LIGHT CURVES; 1ST SURVEY; GEV-TEV; GRB; FLARES; COMPONENT
AB We present the results of 16 Swift-triggered Gamma-ray burst (GRB) follow-up observations taken with the Very Energetic Radiation Imaging Telescope Array System (VERITAS) telescope array from 2007 January to 2009 June. The median energy threshold and response time of these observations were 260 GeV and 320 s, respectively. Observations had an average duration of 90 minutes. Each burst is analyzed independently in two modes: over the whole duration of the observations and again over a shorter timescale determined by the maximum VERITAS sensitivity to a burst with a t(-1.5) time profile. This temporal model is characteristic of GRB afterglows with high-energy, long-lived emission that have been detected by the Large Area Telescope on board the Fermi satellite. No significant very high energy (VHE) gamma-ray emission was detected and upper limits above the VERITAS threshold energy are calculated. The VERITAS upper limits are corrected for gamma-ray extinction by the extragalactic background light and interpreted in the context of the keV emission detected by Swift. For some bursts the VHE emission must have less power than the keV emission, placing constraints on inverse Compton models of VHE emission.
C1 [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Aliu, E.; Errando, M.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Arlen, T.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Byrum, K.; Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Collins-Hughes, E.; 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.
[Christiansen, J. L.; Jackson, D. J.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Newbold, M. D.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Griffin, S.; Guenette, R.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[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.
[Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.] DESY, D-15738 Zeuthen, Germany.
[Humensky, T. B.; Park, N.; Reyes, L. C.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Madhavan, A. S.; Orr, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Pohl, M.; Ruppel, J.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Sentuerk, G. D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
RP Aune, T (reprint author), Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610;
Ward, John E/0000-0003-1973-0794; Lang, Mark/0000-0003-4641-4201
FU US Department of Energy; US National Science Foundation; Smithsonian
Institution; NSERC in Canada; Science Foundation Ireland [SFI
10/RFP/AST2748]; STFC in the UK; NASA [NNX09AR06G]
FX This research is supported by grants from the US Department of Energy,
the US National Science Foundation, and the Smithsonian Institution, by
NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and
by STFC in the UK. We acknowledge the excellent work of the technical
support staff at the FLWO and the collaborating institutions in the
construction and operation of the instrument. We acknowledge the support
provided by NASA Swift Guest Investigator (GI) grant NNX09AR06G. T. Aune
gratefully acknowledges the support provided by a NASA Graduate Student
Researchers Program fellowship. This work made use of data supplied by
the UK Swift Science Data Centre at the University of Leicester.
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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 DEC 10
PY 2011
VL 743
IS 1
AR 62
DI 10.1088/0004-637X/743/1/62
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300062
ER
PT J
AU Bean, JL
Desert, JM
Kabath, P
Stalder, B
Seager, S
Kempton, EMR
Berta, ZK
Homeier, D
Walsh, S
Seifahrt, A
AF Bean, Jacob L.
Desert, Jean-Michel
Kabath, Petr
Stalder, Brian
Seager, Sara
Kempton, Eliza Miller-Ricci
Berta, Zachory K.
Homeier, Derek
Walsh, Shane
Seifahrt, Andreas
TI THE OPTICAL AND NEAR-INFRARED TRANSMISSION SPECTRUM OF THE SUPER-EARTH
GJ 1214b: FURTHER EVIDENCE FOR A METAL-RICH ATMOSPHERE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual
(GJ 1214b); techniques: photometric
ID GROUND-BASED DETECTION; THERMAL EMISSION; SECONDARY ECLIPSE; TRANSITS;
SPECTROSCOPY; WASP-19B; PLANETS; MODELS; KS
AB We present an investigation of the transmission spectrum of the 6.5 M(circle plus) planet GJ 1214b based on new ground-based observations of transits of the planet in the optical and near-infrared, and on previously published data. Observations with the VLT + FORS and Magellan + MMIRS using the technique of multi-object spectroscopy with wide slits yielded new measurements of the planet's transmission spectrum from 0.61 to 0.85 mu m, and in the J, H, and K atmospheric windows. We also present a new measurement based on narrow-band photometry centered at 2.09 mu m with the VLT + HAWKI. We combined these data with results from a reanalysis of previously published FORS data from 0.78 to 1.00 mu m using an improved data reduction algorithm, and previously reported values based on Spitzer data at 3.6 and 4.5 mu m. All of the data are consistent with a featureless transmission spectrum for the planet. Our K-band data are inconsistent with the detection of spectral features at these wavelengths reported by Croll and collaborators at the level of 4.1 sigma. The planet's atmosphere must either have at least 70% H(2)O by mass or optically thick high-altitude clouds or haze to be consistent with the data.
C1 [Bean, Jacob L.; Desert, Jean-Michel; Stalder, Brian; Berta, Zachory K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kabath, Petr] European So Observ, Santiago 19, Chile.
[Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Seager, Sara] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Kempton, Eliza Miller-Ricci] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Homeier, Derek] Univ Lyon, Ecole Normale Super Lyon, CNRS, Ctr Rech Astrophys Lyon,UMR 5574, F-69364 Lyon 07, France.
[Walsh, Shane] Curtin Univ, Australian Astron Observ, Perth, WA 6845, Australia.
[Walsh, Shane] Curtin Univ, Curtin Inst Radio Astron, Perth, WA 6845, Australia.
[Seifahrt, Andreas] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
RP Bean, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jbean@cfa.harvard.edu
OI Homeier, Derek/0000-0002-8546-9128; Berta-Thompson,
Zachory/0000-0002-3321-4924
FU NASA; NSF-MRI [0723073]; NSF [AST-1108860]
FX We thank Bryce Croll and Bjorn Benneke for discussions pertaining to
this work. We thank Brian McCleod and Warren Brown for sharing their
knowledge about the MMIRS instrument, and Brice-Olivier Demory for
information about the HAWKI instrument. J.L.B. and E. K. acknowledge
funding from NASA through the Sagan Fellowship Program. B. S.
acknowledges support from NSF-MRI grant 0723073. A. S. acknowledges
support from NSF grant AST-1108860. The results presented are based on
observations made with ESO Telescopes at the Paranal Observatories under
program 087.C-0505, and on observations made with the 6.5 m Magellan
telescopes located at Las Campanas Observatory.
NR 35
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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 DEC 10
PY 2011
VL 743
IS 1
AR 92
DI 10.1088/0004-637X/743/1/92
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300092
ER
PT J
AU Bogdan, A
Kraft, RP
Forman, WR
Jones, C
Randall, SW
Sun, M
O'Dea, CP
Churazov, E
Baum, SA
AF Bogdan, Akos
Kraft, Ralph P.
Forman, William R.
Jones, Christine
Randall, Scott W.
Sun, Ming
O'Dea, Christopher P.
Churazov, Eugene
Baum, Stefi A.
TI CHANDRA AND ROSAT OBSERVATIONS OF A194: DETECTION OF AN X-RAY CAVITY AND
MAPPING THE DYNAMICS OF THE CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: clusters: individual (A194); galaxies:
stellar content; intergalactic medium; X-rays: galaxies: clusters
ID EXTRAGALACTIC RADIO-SOURCES; DISTANT GALAXIES; COOLING CLUSTERS;
HIGH-RESOLUTION; STAR-FORMATION; XMM-NEWTON; MASS; BINARIES; JET;
SPECTROSCOPY
AB Based on Chandra and ROSAT observations, we investigated the nearby poor cluster A194, which hosts two luminous radio galaxies, NGC 547 (3C 40B) and NGC 541 (3C 40A). We demonstrated the presence of a large X-ray cavity (r similar to 34 kpc) formed by the giant southern radio lobe arising from 3C 40B in NGC 547. The estimated age of the cavity is t = 7.9 x 10(7) years and the total work of the active galactic nucleus is 3.3 x 10(59) erg, hence the cavity power is P(cav) = 1.3 x 10(44) erg s(-1). Furthermore, in the Chandra images of NGC 545 and NGC 541 we detected sharp surface brightness edges, identified as merger cold fronts, and extended tails. Using the pressure ratios between inside and outside the cold fronts we estimated that the velocities of NGC 545 and NGC 541 correspond to Mach numbers of M = 1.0(-0.5)(+0.3) and M = 0.9(-0.5)(+0.2), respectively. The low radial velocities of these galaxies relative to the mean radial velocity of A194 imply that their motion is oriented approximately in the plane of the sky. Based on these and earlier observations, we concluded that NGC 545 and NGC 541 are falling through the cluster, whose center is NGC 547, suggesting that A194 is undergoing a significant cluster merger event. Additionally, we detected 20 bright X-ray sources around NGC 547 and NGC 541, a surprisingly large number, since the predicted number of resolved low-mass X-ray binaries and cosmic X-ray background sources is 2.2 and 4.1, respectively. To explain the nature of additional sources, different possibilities were considered, none of which are satisfactory. We also studied the origin of X-ray emission in Minkowski's object (MO) and concluded that it is most likely dominated by the population of high-mass X-ray binaries rather than by hot diffuse interstellar medium. Moreover, in view of the galaxy dynamics in A194, we explored the possibility that the starburst in MO was triggered by its past interaction with NGC 541, and concluded that it may be a viable path.
C1 [Bogdan, Akos; Kraft, Ralph P.; Forman, William R.; Jones, Christine; Randall, Scott W.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Sun, Ming] Univ Virginia, Dept Astron, Charlottesville, VA 22901 USA.
[O'Dea, Christopher P.; Baum, Stefi A.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Churazov, Eugene] Max Planck Inst Astrophys, D-85741 Garching, Germany.
RP Bogdan, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM abogdan@head.cfa.harvard.edu
RI Churazov, Eugene/A-7783-2013;
OI Randall, Scott/0000-0002-3984-4337
FU National Aeronautics and Space Administration; National Science
Foundation; Associated Universities, Inc.; Smithsonian Institution;
Chandra X-ray Center through NASA [NAS8-03060]
FX The authors thank Martin Hardcastle for critical reading of the
manuscript and the anonymous referee for helpful and constructive
comments. This research has made use of Chandra archival data provided
by the Chandra X-ray Center (CXC). The publication makes use of software
provided by the 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. The Digitized Sky Survey (DSS) and the
NASA/IPAC Extragalactic Database (NED) have been used. The Very Large
Array (VLA) is a facility of the National Radio Astronomy Observatory
(NRAO). The NRAO is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc. W.
F. and C.J. acknowledge support from the Smithsonian Institution. The
financial support for this work was partially provided by the Chandra
X-ray Center through NASA contract NAS8-03060, and the Smithsonian
Institution.
NR 46
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2011
VL 743
IS 1
AR 59
DI 10.1088/0004-637X/743/1/59
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300059
ER
PT J
AU Chung, SM
Eisenhardt, PR
Gonzalez, AH
Stanford, SA
Brodwin, M
Stern, D
Jarrett, T
AF Chung, Sun Mi
Eisenhardt, Peter R.
Gonzalez, Anthony H.
Stanford, Spencer A.
Brodwin, Mark
Stern, Daniel
Jarrett, Thomas
TI A WISE VIEW OF STAR FORMATION IN LOCAL GALAXY CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: evolution; galaxies: star
formation; infrared: galaxies
ID INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; LOW-DENSITY ENVIRONMENTS;
FORMATION RATES; INFRARED GALAXIES; H-ALPHA; LUMINOSITY FUNCTIONS; DATA
RELEASE; EVOLUTION; DEPENDENCE
AB We present results from a systematic study of star formation in local galaxy clusters using 22 mu m data from the Wide-field Infrared Survey Explorer ( WISE). The 69 systems in our sample are drawn from the Cluster Infall Regions Survey, and all have robust mass determinations. The all-sky WISE data enable us to quantify the amount of star formation, as traced by 22 mu m, as a function of radius well beyond R-200, and investigate the dependence of total star formation rate upon cluster mass. We find that the fraction of star-forming galaxies increases with cluster radius but remains below the field value even at 3R(200). We also find that there is no strong correlation between the mass-normalized total specific star formation rate and cluster mass, indicating that the mass of the host cluster does not strongly influence the total star formation rate of cluster members.
C1 [Chung, Sun Mi; Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Eisenhardt, Peter R.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jarrett, Thomas] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
RP Chung, SM (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
EM schung@astro.ufl.edu
FU National Aeronautics and Space Administration
FX This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. The authors thank Emilio Donoso for his help and advice
on navigating the SDSS database. We also thank the anonymous referee for
a careful reading and comments which improved the paper.
NR 56
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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 DEC 10
PY 2011
VL 743
IS 1
AR 34
DI 10.1088/0004-637X/743/1/34
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300034
ER
PT J
AU Cyganowski, CJ
Brogan, CL
Hunter, TR
Churchwell, E
AF Cyganowski, C. J.
Brogan, C. L.
Hunter, T. R.
Churchwell, E.
TI DEEP VERY LARGE ARRAY RADIO CONTINUUM SURVEYS OF GLIMPSE EXTENDED GREEN
OBJECTS (EGOs)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: ISM; ISM: jets and outflows; radio continuum: ISM; stars:
formation; techniques: interferometric
ID STAR-FORMING REGIONS; H-II REGIONS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG
STELLAR OBJECTS; ULTRACOMPACT HII-REGIONS; METHANOL MASER SURVEY;
GALACTIC PLANE; MASSIVE STARS; PHYSICAL-PROPERTIES; RECOMBINATION LINE
AB We present the results of deep, high angular resolution Very Large Array surveys for radio continuum emission toward a sample of 14 GLIMPSE Extended Green Objects (EGOs). Identified as massive young stellar object (MYSO) outflow candidates based on their extended 4.5 mu m emission in Spitzer images, the EGOs in our survey sample are also associated with 6.7 GHz Class II and/or 44 GHz Class I CH(3)OH masers. No continuum is detected at 3.6 or 1.3 cm toward the majority (57%) of our targets (median rms similar to 0.03 and 0.25 mJy beam(-1)). Only two EGOs are associated with optically thin emission consistent with ultracompact/compact H II regions. Both of these sources exhibit cm-gamma multiplicity, with evidence that one of the less-evolved members may be driving the 4.5 mu m outflow. Most of the other cm-gamma EGO counterparts are weak (less than or similar to 1 mJy), unresolved, undetected at 1.3 cm, and characterized by intermediate spectral indices consistent with hypercompact (HC) H II regions or ionized winds or jets. One EGO centimeter (cm) counterpart, likely an optically thick HC H II region, is detected only at 1.3 cm and is associated with hot core line emission and H(2)O and 6.7 GHz CH(3)OH masers. The results of our exceptionally sensitive survey indicate that EGOs signify an early stage of massive star formation, before photoionizing feedback from the central MYSO significantly influences the (proto) cluster environment. Actively driving outflows (and so, presumably, actively accreting), the surveyed EGOs are associated with significant clump-scale gas reservoirs, providing sufficient material for sustained, rapid accretion.
C1 [Cyganowski, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brogan, C. L.; Hunter, T. R.] NRAO, Charlottesville, VA 22903 USA.
[Churchwell, E.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
RP Cyganowski, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ccyganowski@cfa.harvard.edu
OI Hunter, Todd/0000-0001-6492-0090
FU NSF [AST-0808119, AST-1003134]
FX This research has made use of NASA's Astrophysics Data System
Bibliographic Services and the SIMBAD database operated at CDS,
Strasbourg, France. Support for this work was provided by NSF grant
AST-0808119. C.J.C. is supported by an NSF Astronomy and Astrophysics
Postdoctoral Fellowship under award AST-1003134. C.J.C. thanks C.
Purcell for providing the CORNISH aperture photometry program and for
helpful discussions, J. Mottram for providing the calibration factor for
MIPS 24 mu m flux to bolometric luminosity calculated from the RMS
sample, M. Hoare for providing the data files for his published plots,
and T. Robitaille for helpful discussions about SED fitting.
NR 95
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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 DEC 10
PY 2011
VL 743
IS 1
AR 56
DI 10.1088/0004-637X/743/1/56
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300056
ER
PT J
AU Drake, JJ
AF Drake, Jeremy J.
TI NEON INSIGHTS FROM OLD SOLAR X-RAYS: A PLASMA TEMPERATURE DEPENDENCE OF
THE CORONAL NEON CONTENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: abundances; Sun: activity; Sun: corona; X-rays: stars
ID B-TYPE STARS; ELECTRON-IMPACT EXCITATION; NE/O ABUNDANCE RATIO; LV 2
ORION; CHEMICAL ABUNDANCES; PLANETARY-NEBULAE; ATOMIC DATABASE;
EMISSION-LINES; MODEL PROBLEM; ELEMENTAL ABUNDANCES
AB An analysis using modern atomic data of fluxes culled from the literature for OVIII and NeIX lines observed in solar active regions by the P78 and Solar Maximum Mission satellites confirms that the coronal Ne/O abundance ratio varies by a factor of two or more, and finds an increase in Ne/O with increasing active region plasma temperature. The latter is reminiscent of evidence for increasing Ne/O with stellar activity in low- activity coronae that reaches a "neon saturation" in moderately active stars at approximately twice the historically accepted solar value of about 0.15 by number. We argue that neon saturation represents the underlying stellar photospheric compositions, and that low- activity coronae, including that of the Sun, are generally depleted in neon. The implication would be that the solar Ne/O abundance ratio should be revised upward by a factor of about two to n(Ne)/n(O) similar to 0.3. Diverse observations of neon in the local cosmos provide some support for such a revision. Neon would still be of some relevance for reconciling helioseismology with solar models computed using recently advocated chemical mixtures with lower metal content.
C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS-3,60 Garden St, Cambridge, MA 02138 USA.
EM jdrake@cfa.harvard.edu
FU NASA AISRP; NASA [NAS8-39073]
FX The author is grateful to the anonymous referee for helping clarify and
improve the manuscript. J.J.D. thanks the NASA AISRP for providing
financial assistance for the development of the PINTofALE package.
J.J.D. was funded by NASA contract NAS8-39073 to the Chandra X-ray
Center during the course of this research and thanks the Director, H.
Tananbaum, for continuing support and encouragement.
NR 58
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2011
VL 743
IS 1
AR 22
DI 10.1088/0004-637X/743/1/22
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300022
ER
PT J
AU Green, PJ
Myers, AD
Barkhouse, WA
Aldcroft, TL
Trichas, M
Richards, GT
Ruiz, A
Hopkins, PF
AF Green, Paul J.
Myers, Adam D.
Barkhouse, Wayne A.
Aldcroft, Thomas L.
Trichas, Markos
Richards, Gordon T.
Ruiz, Angel
Hopkins, Philip F.
TI A MULTIWAVELENGTH STUDY OF BINARY QUASARS AND THEIR ENVIRONMENTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: active; galaxies: interactions; galaxies:
nuclei; quasars: emission lines
ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES;
PHOTOMETRICALLY CLASSIFIED QUASARS; DOUBLE-PEAKED EMITTER;
ABSORPTION-LINE QUASARS; CHANDRA DEEP FIELD; X-RAY OBSERVATIONS;
SIMILAR-TO 3-4; GALAXY MERGERS
AB We present Chandra X-ray imaging and spectroscopy for 14 quasars in spatially resolved pairs targeted as part of a complete sample of binary quasars with small transverse separations drawn from Sloan Digital Sky Survey (SDSSDR6) photometry. We measure the X-ray properties of all 14 QSOs, and study the distribution of X-ray and optical-to-X-ray power-law indices in these binary quasars. We find no significant difference when compared with large control samples of isolated quasars, true even for SDSS J1254+0846, discussed in detail in a companion paper, which clearly inhabits an ongoing, pre-coalescence galaxy merger showing obvious tidal tails. We present infrared photometry from our observations with SAO Wide-field InfraRed Camera at the MMT, and from the Wide-field Infrared Survey Explorer Preliminary Data Release, and fit simple spectral energy distributions to all 14 QSOs. We find preliminary evidence that substantial contributions from star formation are required, but possibly no more so than for isolated X-ray-detected QSOs. Sensitive searches of the X-ray images for extended emission and the optical images for optical galaxy excess show that these binary QSOs-expected to occur in strong peaks of the dark matter distribution-are not preferentially found in rich cluster environments. While larger binary QSO samples with richer far-IR and submillimeter multiwavelength data might better reveal signatures of merging and triggering, optical color selection of QSO pairs may be biased against such signatures. X-ray and/or variability selection of QSO pairs, while challenging, should be attempted. We present in an Appendix a primer on X-ray flux and luminosity calculations.
C1 [Green, Paul J.; Aldcroft, Thomas L.; Trichas, Markos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Barkhouse, Wayne A.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA.
[Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 15260 USA.
[Ruiz, Angel] CSIC UC, IFCA, Santander 39005, Spain.
[Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Hopkins, Philip F.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
RP Green, PJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM pgreen@cfa.harvard.edu
RI Ruiz, Angel/B-4914-2008
OI Ruiz, Angel/0000-0002-3352-4383
FU National Aeronautics and Space Administration [GO9-0114A, GO9-0114B,
NAS8-03060]; Alfred P. Sloan Foundation; NSF; US Department of Energy;
Japanese Monbukagakusho; Max Planck Society; Higher Education Funding
Council for England
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Award Numbers GO9-0114A and GO9-0114B
issued by the Chandra Xray Observatory Center, which is operated by the
Smithsonian Astrophysical Observatory for and on behalf of the National
Aeronautics Space Administration under contract NAS8-03060. Discovery
optical images were obtained at Kitt Peak National Observatory, 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 data obtained from the Chandra Data Archive and software provided
by the Chandra X-ray Center (CXC) in the application packages CIAO and
Sherpa. This paper has used data from the SDSS archive. Funding for the
SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation,
the Participating Institutions, the NSF, the US Department of Energy,
the National Aeronautics and Space Administration (NASA), the Japanese
Monbukagakusho, the Max Planck Society, and the Higher Education Funding
Council for England. The SDSS Web site is at http://www.sdss.org/.
NR 118
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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 DEC 10
PY 2011
VL 743
IS 1
AR 81
DI 10.1088/0004-637X/743/1/81
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300081
ER
PT J
AU Keisler, R
Reichardt, CL
Aird, KA
Benson, BA
Bleem, LE
Carlstrom, JE
Chang, CL
Cho, HM
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Dudley, J
George, EM
Halverson, NW
Holder, GP
Holzapfel, WL
Hoover, S
Hou, Z
Hrubes, JD
Joy, M
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
McMahon, JJ
Mehl, J
Meyer, SS
Millea, M
Mohr, JJ
Montroy, TE
Natoli, T
Padin, S
Plagge, T
Pryke, C
Ruhl, JE
Schaffer, KK
Shaw, L
Shirokoff, E
Spieler, HG
Staniszewski, Z
Stark, AA
Story, K
van Engelen, A
Vanderlinde, K
Vieira, JD
Williamson, R
Zahn, O
AF Keisler, R.
Reichardt, C. L.
Aird, K. A.
Benson, B. A.
Bleem, L. E.
Carlstrom, J. E.
Chang, C. L.
Cho, H. M.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Dudley, J.
George, E. M.
Halverson, N. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hou, Z.
Hrubes, J. D.
Joy, M.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Millea, M.
Mohr, J. J.
Montroy, T. E.
Natoli, T.
Padin, S.
Plagge, T.
Pryke, C.
Ruhl, J. E.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Spieler, H. G.
Staniszewski, Z.
Stark, A. A.
Story, K.
van Engelen, A.
Vanderlinde, K.
Vieira, J. D.
Williamson, R.
Zahn, O.
TI A MEASUREMENT OF THE DAMPING TAIL OF THE COSMIC MICROWAVE BACKGROUND
POWER SPECTRUM WITH THE SOUTH POLE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmological parameters; cosmology:
observations
ID ATACAMA COSMOLOGY TELESCOPE; BIG-BANG NUCLEOSYNTHESIS; MASSIVE GALAXY
CLUSTERS; PRIMORDIAL NUCLEOSYNTHESIS; OBSERVED GROWTH; CONSTRAINTS;
ANISOTROPIES; POLARIZATION; TEMPERATURE; ABUNDANCE
AB We present a measurement of the angular power spectrum of the cosmic microwave background (CMB) using data from the South Pole Telescope (SPT). The data consist of 790 deg(2) of sky observed at 150 GHz during 2008 and 2009. Here we present the power spectrum over the multipole range 650 < l < 3000, where it is dominated by primary CMB anisotropy. We combine this power spectrum with the power spectra from the seven-year Wilkinson Microwave Anisotropy Probe (WMAP) data release to constrain cosmological models. We find that the SPT and WMAP data are consistent with each other and, when combined, are well fit by a spatially flat, Lambda CDM cosmological model. The SPT+WMAP constraint on the spectral index of scalar fluctuations is n(s) = 0.9663 +/- 0.0112. We detect, at similar to 5 sigma significance, the effect of gravitational lensing on the CMB power spectrum, and find its amplitude to be consistent with the Lambda CDM cosmological model. We explore a number of extensions beyond the Lambda CDM model. Each extension is tested independently, although there are degeneracies between some of the extension parameters. We constrain the tensor-to-scalar ratio to be r < 0.21 (95% CL) and constrain the running of the scalar spectral index to be dn(s)/d ln k = -0.024 +/- 0.013. We strongly detect the effects of primordial helium and neutrinos on the CMB; a model without helium is rejected at 7.7 sigma, while a model without neutrinos is rejected at 7.5 sigma. The primordial helium abundance is measured to be Y-p = 0.296 +/- 0.030, and the effective number of relativistic species is measured to be N-eff = 3.85 +/- 0.62. The constraints on these models are strengthened when the CMB data are combined with measurements of the Hubble constant and the baryon acoustic oscillation feature. Notable improvements include n(s) = 0.9668 +/- 0.0093, r < 0.17 (95% CL), and N-eff = 3.86 +/- 0.42. The SPT+WMAP data show a mild preference for low power in the CMB damping tail, and while this preference may be accommodated by models that have a negative spectral running, a high primordial helium abundance, or a high effective number of relativistic species, such models are disfavored by the abundance of low-redshift galaxy clusters.
C1 [Keisler, R.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Keisler, R.; Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Reichardt, C. L.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Aird, K. A.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Hrubes, J. D.; Leitch, E. M.; Luong-Van, D.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; 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.
[de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Joy, M.] NASA Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA.
[Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; 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.
[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.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
RP Keisler, R (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
EM rkeisler@uchicago.edu
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; Stark,
Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937, ANT-0130612, AST-1009811,
0709498]; NSF Physics Frontier Center [PHY-0114422]; National Sciences
and Engineering Research Council of Canada; Canada Research Chairs
program; Canadian Institute for Advanced Research; NASA [51275.01];
KICP; Alfred P. Sloan; Yale University; Office of Science of the U.S.
Department of Energy [DE-AC02-05CH11231]
FX The South Pole Telescope is supported by the National Science Foundation
through grants ANT-0638937 and ANT-0130612. Partial support is also
provided by the NSF Physics Frontier Center grant PHY-0114422 to the
Kavli Institute of Cosmological Physics at the University of Chicago,
the Kavli Foundation, and the Gordon and Betty Moore Foundation. The
McGill group acknowledges funding from the National Sciences and
Engineering Research Council of Canada, Canada Research Chairs program,
and the Canadian Institute for Advanced Research. We acknowledge use of
the FNAL-KICP Joint Cluster. R. Keisler acknowledges support from NASA
Hubble Fellowship grant HF-51275.01. B. A. Benson is supported by a KICP
Fellowship. M. Dobbs acknowledges support from an Alfred P. Sloan
Research Fellowship. L. Shaw acknowledges the support of Yale University
and NSF grant AST-1009811. M. Millea and L. Knox acknowledge the support
of NSF grant 0709498. 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. We acknowledge the use of the Legacy Archive for
Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is
provided by the NASA Office of Space Science.
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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 DEC 10
PY 2011
VL 743
IS 1
AR 28
DI 10.1088/0004-637X/743/1/28
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300028
ER
PT J
AU Machacek, ME
Jerius, D
Kraft, R
Forman, WR
Jones, C
Randall, S
Giacintucci, S
Sun, M
AF Machacek, Marie E.
Jerius, Diab
Kraft, Ralph
Forman, William R.
Jones, Christine
Randall, Scott
Giacintucci, Simona
Sun, Ming
TI DEEP CHANDRA OBSERVATIONS OF EDGES AND BUBBLES IN THE NGC 5846 GALAXY
GROUP
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: groups: individual (NGC 5846); intergalactic medium; X-rays:
galaxies; X-rays: galaxies: clusters
ID COMPACT ELLIPTIC GALAXIES; ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION;
COOLING FLOWS; XMM-NEWTON; HOT GAS; GASEOUS ATMOSPHERE; COLD FRONTS;
BLACK-HOLES; CLUSTER
AB We use a combined 120 ks Chandra exposure to analyze X-ray edges produced by non-hydrostatic gas motions (sloshing) from galaxy collisions, and cavities formed by active galactic nucleus (AGN) activity. Evidence for gas sloshing is seen in the spiral morphology and multiple cold front edges in NGC 5846's X-ray surface brightness distribution, while the lack of spiral structure in the temperature map suggests that the perturbing interaction was not in the plane of the sky. Density and spectral modeling across the edges indicate that the relative motion of gas in the cold fronts is at most transonic. Evidence for AGN activity is seen in two inner bubbles at 0.6 kpc, filled with 5 GHz and 1.5 GHz radio plasma and coincident with Ha emission, and in a ghost bubble at 5.2 kpc west of NGC 5846's nucleus. The outburst energy and ages for the inner (ghost) bubbles are similar to 10(55) erg and similar to 2 Myr (similar to 5 x 10(55) erg and 12 Myr), respectively, implying an AGN duty cycle of 10 Myr. The inner bubble rims are threaded with nine knots, whose total 0.5-2 keV X-ray luminosity is 0.3 x 10(40) erg s(-1), a factor similar to 2-3 less than that of the surrounding rims, and 0.7 keV mean temperature is indistinguishable from that of the rims. We suggest that the knots may be transient clouds heated by the recent passage of a shock from the last AGN outburst. We also observe gas stripping from a cE galaxy, NGC 5846A, in a 0.5 kpc long (similar to 10(5) M-circle dot) hot gas tail, as it falls toward NGC 5846.
C1 [Machacek, Marie E.; Jerius, Diab; Kraft, Ralph; Forman, William R.; Jones, Christine; Randall, Scott] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Sun, Ming] Univ Virginia, Dept Astron, Charlottesville, VA 22901 USA.
RP Machacek, ME (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mmachacek@cfa.harvard.edu
OI Randall, Scott/0000-0002-3984-4337; Forman, William/0000-0002-9478-1682
FU NASA [NNX07AH65G]; Smithsonian Institution
FX This work is supported in part by NASA grant NNX07AH65G and the
Smithsonian Institution. This work 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. We thank John ZuHone and
Ryan Johnson for helpful discussions.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2011
VL 743
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DI 10.1088/0004-637X/743/1/15
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300015
ER
PT J
AU Martinez-Sykora, J
De Pontieu, B
Testa, P
Hansteen, V
AF Martinez-Sykora, Juan
De Pontieu, Bart
Testa, Paola
Hansteen, Viggo
TI FORWARD MODELING OF EMISSION IN SOLAR DYNAMICS OBSERVATORY/ATMOSPHERIC
IMAGING ASSEMBLY PASSBANDS FROM DYNAMIC THREE-DIMENSIONAL SIMULATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; magnetohydrodynamics (MHD); methods: data analysis;
methods: numerical; methods: observational; radiative transfer; Sun:
atmosphere
ID FLUX TUBE EMERGENCE; TRANSITION REGION; CONVECTION ZONE; II SPICULES;
CORONA; LINES; CHROMOSPHERE; ATMOSPHERE; FIBRILS; PLASMA
AB It is typically assumed that emission in the passbands of the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) is dominated by single or several strong lines from ions that under equilibrium conditions are formed in a narrow range of temperatures. However, most SDO/AIA channels also contain contributions from lines of ions that have formation temperatures that are significantly different from the "dominant" ion(s). We investigate the importance of these lines by forward modeling the emission in the SDO/AIA channels with three-dimensional radiative MHD simulations of a model that spans the upper layer of the convection zone to the low corona. The model is highly dynamic. In addition, we pump a steadily increasing magnetic flux into the corona, in order to increase the coronal temperature through the dissipation of magnetic stresses. As a consequence, the model covers different ranges of coronal temperatures as time progresses. The model covers coronal temperatures that are representative of plasma conditions in coronal holes and quiet Sun. The 131, 171, and 304 angstrom AIA passbands are found to be the least influenced by the so-called non-dominant ions, and the emission observed in these channels comes mostly from plasma at temperatures near the formation temperature of the dominant ion(s). On the other hand, the other channels are strongly influenced by the non-dominant ions, and therefore significant emission in these channels comes from plasma at temperatures that are different from the "canonical" values. We have also studied the influence of non-dominant ions on the AIA passbands when different element abundances are assumed (photospheric and coronal), and when the effects of the electron density on the contribution function are taken into account.
C1 [Martinez-Sykora, Juan; De Pontieu, Bart] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
[Martinez-Sykora, Juan; Hansteen, Viggo] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Testa, Paola] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Martinez-Sykora, J (reprint author), Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA.
EM j.m.sykora@astro.uio.no
FU European Community [MEST-CT-2005-020395]; European Commission through
SOLAIRE Network [MTRN-CT-2006-035484]; Spanish Ministry of Research and
Innovation [AYA2007-66502]; NASA [NNX08AL22G, NNX08BA99G, NNM07AA01C];
Lockheed-Martin [SP02H1701R]; High End Computing (HEC) division of NASA
[SMD-07-0434, SMD-08-0743, SMD-09-1128, SMD-09-1336, SMD-10-1622,
SMD-10-1869]; Research Council of Norway [170935/V30]
FX This research has been supported by a Marie Curie Early Stage Research
Training Fellowship of the European Community's Sixth Framework
Programme under contract number MEST-CT-2005-020395: The USO-SP
International School for Solar Physics. Financial support by the
European Commission through the SOLAIRE Network (MTRN-CT-2006-035484)
and by the Spanish Ministry of Research and Innovation through project
AYA2007-66502 is gratefully acknowledged. B. D. P. is supported by NASA
grants NNX08AL22G and NNX08BA99G and NASA contract NNM07AA01C (Hinode).
P. T. was supported by contract SP02H1701R from Lockheed-Martin to the
Smithsonian Astrophysical Observatory. Hinode is a Japanese mission
developed by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC
(UK) as international partners. It is operated in cooperation with ESA
and NSC (Norway). The 3D simulations have been run with the Njord and
Stallo cluster from the Notur project and the Pleiades cluster through
computing grants SMD-07-0434, SMD-08-0743, SMD-09-1128, SMD-09-1336,
SMD-10-1622, and SMD-10-1869 from the High End Computing (HEC) division
of NASA. We thankfully acknowledge the computer and supercomputer
resources of the Research Council of Norway through grant 170935/V30 and
through grants of computing time from the Programme for Supercomputing.
To analyze the data we have used IDL and Vapor
(http://www.vapor.ucar.edu).
NR 28
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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 DEC 10
PY 2011
VL 743
IS 1
AR 23
DI 10.1088/0004-637X/743/1/23
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300023
ER
PT J
AU Myers, PC
AF Myers, Philip C.
TI STAR FORMATION IN DENSE CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM:clouds; stars: formation
ID INITIAL MASS FUNCTION; ORION-NEBULA-CLUSTER; EMBEDDED STELLAR CLUSTERS;
MOLECULAR CLOUD CORES; EVOLUTIONARY SIGNATURES; LUMINOSITY FUNCTIONS;
INTERNAL STRUCTURE; NH3 OBSERVATIONS; DARK CLOUDS; ACCRETION
AB A model of core-clump accretion with equally likely stopping describes star formation in the dense parts of clusters, where models of isolated collapsing cores may not apply. Each core accretes at a constant rate onto its protostar, while the surrounding clump gas accretes as a power of protostar mass. Short accretion flows resemble Shu accretion and make low-mass stars. Long flows resemble reduced Bondi accretion and make massive stars. Accretion stops due to environmental processes of dynamical ejection, gravitational competition, and gas dispersal by stellar feedback, independent of initial core structure. The model matches the field star initial mass function (IMF) from 0.01 to more than 10 solar masses. The core accretion rate and the mean accretion duration set the peak of the IMF, independent of the local Jeans mass. Massive protostars require the longest accretion durations, up to 0.5 Myr. The maximum protostar luminosity in a cluster indicates the mass and age of its oldest protostar. The distribution of protostar luminosities matches those in active star-forming regions if protostars have a constant birthrate but not if their births are coeval. For constant birthrate, the ratio of young stellar objects to protostars indicates the star-forming age of a cluster, typically similar to 1 Myr. The protostar accretion luminosity is typically less than its steady spherical value by a factor of similar to 2, consistent with models of episodic disk accretion.
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 88
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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 DEC 10
PY 2011
VL 743
IS 1
AR 98
DI 10.1088/0004-637X/743/1/98
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300098
ER
PT J
AU Offner, SSR
Lee, EJ
Goodman, AA
Arce, H
AF Offner, Stella S. R.
Lee, Eve J.
Goodman, Alyssa A.
Arce, Hector
TI RADIATION-HYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR OUTFLOWS: SYNTHETIC
OBSERVATIONS AND DATA COMPARISONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: numerical; molecular data; radiative transfer; stars:
formation; stars: winds, outflows
ID YOUNG STELLAR OBJECTS; LOW-MASS STAR; MOLECULAR CLOUDS; SUPERSONIC
TURBULENCE; DRIVEN TURBULENCE; CO OUTFLOWS; JETS; WINDS; EVOLUTION;
ENVELOPE
AB We present results from three-dimensional, self-gravitating, radiation-hydrodynamic simulations of low-mass protostellar outflows. We construct synthetic observations in (12)CO in order to compare with observed outflows and evaluate the effects of beam resolution and outflow orientation on inferred outflow properties. To facilitate the comparison, we develop a quantitative prescription for measuring outflow opening angles. Using this prescription, we demonstrate that, in both simulations and synthetic observations, outflow opening angles broaden with time similarly to observed outflows. However, the interaction between the outflowing gas and the turbulent core envelope produces significant asymmetry between the redshifted and blueshifted outflow lobes. We find that applying a velocity cutoff may result in outflow masses that are underestimated by a factor five or more, and masses derived from optically thick CO emission further underpredict themass of the high-velocity gas by a factor of 5-10. Derived excitation temperatures indicate that outflowing gas is hotter than the ambient gas with temperature rising over time, which is in agreement with the simulation gas temperatures. However, excitation temperatures are otherwise not well correlated with the actual gas temperature.
C1 [Offner, Stella S. R.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lee, Eve J.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3G4, Canada.
[Arce, Hector] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
RP Offner, SSR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM soffner@cfa.harvard.edu
RI Goodman, Alyssa/A-6007-2010;
OI Goodman, Alyssa/0000-0003-1312-0477; Lee, Eve/0000-0002-1228-9820
FU NSF [AST-0901055, AST-0908159]
FX We thank Eric Keto for assistance with MOLLIE and Andrew Cunningham for
technical improvements to ORION. We also thank Tom Robitaille, Chris
Beaumont, Eric Keto, Michelle Borkin, and Ned Ladd for helpful
discussions and the referee Robi Banerjee for helpful comments. This
research has been supported by the NSF through grants AST-0901055 (SSRO)
and AST-0908159 (EJL). The simulations and data analysis were performed
on the Odyssey supercomputing cluster at Harvard University.
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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 DEC 10
PY 2011
VL 743
IS 1
AR 91
DI 10.1088/0004-637X/743/1/91
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300091
ER
PT J
AU Parker, AH
Kavelaars, JJ
Petit, JM
Jones, L
Gladman, B
Parker, J
AF Parker, Alex H.
Kavelaars, J. J.
Petit, Jean-Marc
Jones, Lynne
Gladman, Brett
Parker, Joel
TI CHARACTERIZATION OF SEVEN ULTRA-WIDE TRANS-NEPTUNIAN BINARIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; Kuiper belt: general; planets and satellites: dynamical
evolution and stability; planets and satellites: formation
ID KUIPER-BELT BINARIES; HUBBLE-SPACE-TELESCOPE; MINOR PLANETS;
TRANSNEPTUNIAN BINARIES; SIZE DISTRIBUTION; MUTUAL ORBITS; TIDAL
FRICTION; KOZAI CYCLES; OBJECTS; INCLINATION
AB The low-inclination component of the Classical Kuiper Belt is host to a population of extremely widely separated binaries. These systems are similar to other trans-Neptunian binaries (TNBs) in that the primary and secondary components of each system are of roughly equal size. We have performed an astrometric monitoring campaign of a sample of seven wide-separation, long-period TNBs and present the first-ever well-characterized mutual orbits for each system. The sample contains the most eccentric (2006 CH(69), e(m) = 0.9) and the most widely separated, weakly bound (2001 QW(322), a/R(H) similar or equal to 0.22) binary minor planets known, and also contains the system with lowest-measured mass of any TNB (2000 CF(105), M(sys) similar or equal to 1.85 x 10(17) kg). Four systems orbit in a prograde sense, and three in a retrograde sense. They have a different mutual inclination distribution compared to all other TNBs, preferring low mutual-inclination orbits. These systems have geometric r-band albedos in the range of 0.09-0.3, consistent with radiometric albedo estimates for larger solitary low-inclination Classical Kuiper Belt objects, and we limit the plausible distribution of albedos in this region of the Kuiper Belt. We find that gravitational collapse binary formation models produce an orbital distribution similar to that currently observed, which along with a confluence of other factors supports formation of the cold Classical Kuiper Belt in situ through relatively rapid gravitational collapse rather than slow hierarchical accretion. We show that these binary systems are sensitive to disruption via collisions, and their existence suggests that the size distribution of TNOs at small sizes remains relatively shallow.
C1 [Parker, Alex H.] Univ Victoria, Dept Astron, Victoria, BC, Canada.
[Parker, Alex H.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Kavelaars, J. J.] Natl Res Council Canada, Herzberg Inst Astrophys, Saanich, BC, Canada.
[Petit, Jean-Marc] Observ Besancon, Besancon, France.
[Jones, Lynne] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Gladman, Brett] Univ British Columbia, Dept Astron, Vancouver, BC V5Z 1M9, Canada.
[Parker, Joel] SW Res Inst, Boulder, CO USA.
RP Parker, AH (reprint author), Univ Victoria, Dept Astron, Victoria, BC, Canada.
EM alexhp@uvic.ca
FU NSF-GRFP [DGE-0836694]; Canadian Space Agency
FX We thank Melissa Graham for pointing out that the Malmquist bias lurks
everywhere, and David Nesvorny for providing the results from his
simulations of binary formation. We also thank the Gemini staff for
their technical support of our observing programs. Alex Parker is funded
by the NSF-GRFP award DGE-0836694. This research used the facilities of
the Canadian Astronomy Data Centre operated by the National Research
Council of Canada with the support of the Canadian Space Agency.
NR 50
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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 DEC 10
PY 2011
VL 743
IS 1
AR 1
DI 10.1088/0004-637X/743/1/1
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300001
ER
PT J
AU Schaffer, KK
Crawford, TM
Aird, KA
Benson, BA
Bleem, LE
Carlstrom, JE
Chang, CL
Cho, HM
Crites, AT
de Haan, T
Dobbs, MA
George, EM
Halverson, NW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Ruhl, JE
Shirokoff, E
Spieler, HG
Stalder, B
Staniszewski, Z
Stark, AA
Story, K
Vanderlinde, K
Vieira, JD
Williamson, R
AF Schaffer, K. K.
Crawford, T. M.
Aird, K. A.
Benson, B. A.
Bleem, L. E.
Carlstrom, J. E.
Chang, C. L.
Cho, H. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
George, E. M.
Halverson, N. W.
Holder, G. 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.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Ruhl, J. E.
Shirokoff, E.
Spieler, H. G.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Story, K.
Vanderlinde, K.
Vieira, J. D.
Williamson, R.
TI THE FIRST PUBLIC RELEASE OF SOUTH POLE TELESCOPE DATA: MAPS OF A 95
deg(2) FIELD FROM 2008 OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; methods: data
analysis; surveys
ID MICROWAVE BACKGROUND ANISOTROPIES; ZELDOVICH POWER SPECTRUM; GALAXY
CLUSTERS; SOURCE CATALOG; SUBMILLIMETER; RADIO; SIMULATIONS; PARAMETERS;
COSMOLOGY; SKY
AB The South Pole Telescope (SPT) has nearly completed a 2500 deg(2) survey of the southern sky in three frequency bands. Here, we present the first public release of SPT maps and associated data products. We present arcminute-resolution maps at 150 GHz and 220 GHz of an approximately 95 deg(2) field centered at R. A. 82 degrees.7, decl. -55 degrees. The field was observed to a depth of approximately 17 mu K arcmin at 150 GHz and 41 mu K arcmin at 220 GHz during the 2008 austral winter season. Two variations on map filtering and map projection are presented, one tailored for producing catalogs of galaxy clusters detected through their Sunyaev-Zel'dovich effect signature and one tailored for producing catalogs of emissive sources. We describe the data processing pipeline, and we present instrument response functions, filter transfer functions, and map noise properties. All data products described in this paper are available for download at http://pole.uchicago.edu/public/data/maps/ra5h30dec-55 and from the NASA Legacy Archive for Microwave Background Data Analysis server. This is the first step in the eventual release of data from the full 2500 deg(2) SPT survey.
C1 [Schaffer, K. K.; Crawford, T. M.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crites, A. T.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Schaffer, K. K.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Pryke, C.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Crawford, T. M.; Carlstrom, J. E.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Meyer, S. S.; Story, K.] Univ Chicago, Dept Phys, 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.
[de Haan, T.; Dobbs, M. A.; Holder, G. P.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Joy, M.] NASA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA.
[Lueker, M.; Padin, S.; Staniszewski, Z.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Mohr, J. J.] Excellence Cluster Univ, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.] 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.
[Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Schaffer, KK (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM kschaf2@saic.edu
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; Stark,
Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937, ANT-0130612, AST-1009012,
AST-1009649, MRI-0723073]; NSF Physics Frontier Center [PHY-0114422];
Kavli Foundation; Gordon and Betty Moore Foundation; National Sciences
and Engineering Research Council of Canada; Canada Research Chairs
program; Canadian Institute for Advanced Research; KICP; Alfred P. Sloan
Research Fellowships; NASA [HF-51275.01]; DFG [TR33]; NASA Office of
Space Science
FX The South Pole Telescope is supported by the National Science Foundation
through grants ANT-0638937 and ANT-0130612. Partial support is also
provided by the NSF Physics Frontier Center grant PHY-0114422 to the
Kavli Institute of Cosmological Physics at the University of Chicago,
the Kavli Foundation, and the Gordon and Betty Moore Foundation. The
McGill group acknowledges funding from the National Sciences and
Engineering Research Council of Canada, Canada Research Chairs program,
and the Canadian Institute for Advanced Research. Partial support at
Harvard is provided by NSF grants AST-1009012, AST-1009649, and
MRI-0723073. B. A. B. is supported by a KICP Fellowship. M. D. and N.H.
acknowledge support from Alfred P. Sloan Research Fellowships. R. K.
acknowledges support from NASA Hubble Fellowship grant HF-51275.01.
J.J.M. acknowledges support from the DFG supported Excellence Cluster
Universe and the transregio program TR33: Dark Universe. B. S.
acknowledges partial support from the Brinson Foundation. We acknowledge
the use of the Legacy Archive for Microwave Background Data Analysis
(LAMBDA). Support for LAMBDA is provided by the NASA Office of Space
Science.
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SC Astronomy & Astrophysics
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ER
PT J
AU Servillat, M
Farrell, SA
Lin, DC
Godet, O
Barret, D
Webb, NA
AF Servillat, Mathieu
Farrell, Sean A.
Lin, Dacheng
Godet, Olivier
Barret, Didier
Webb, Natalie A.
TI X-RAY VARIABILITY AND HARDNESS OF ESO 243-49 HLX-1: CLEAR EVIDENCE FOR
SPECTRAL STATE TRANSITIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; X-rays: binaries;
X-rays: individuals (ESO 243-49 HLX-1)
ID MASS BLACK-HOLE; XMM-NEWTON OBSERVATIONS; LIGHT CURVES; LIKELIHOOD
RATIO; GALACTIC NUCLEI; NEARBY GALAXIES; HIGH/SOFT STATE; DOMINANT
STATE; CLUSTER G1; BINARIES
AB The ultraluminous X-ray (ULX) source ESO 243-49 HLX-1, which reaches a maximum luminosity of 10(42) erg s(-1) (0.2-10 keV), currently provides the strongest evidence for the existence of intermediate-mass black holes (IMBHs). To study the spectral variability of the source, we conduct an ongoing monitoring campaign with the Swift X-ray Telescope (XRT), which now spans more than two years. We found that HLX-1 showed two fast rise and exponential decay type outbursts in the Swift XRT light curve with increases in the count rate of a factor similar to 40 separated by 375 +/- 13 days. We obtained new XMM-Newton and Chandra dedicated pointings that were triggered at the lowest and highest luminosities, respectively. From spectral fitting, the unabsorbed luminosities ranged from 1.9 x 10(40) to 1.25 x 10(42) erg s(-1). We confirm here the detection of spectral state transitions from HLX-1 reminiscent of Galactic black hole binaries (GBHBs): at high luminosities, the X-ray spectrum showed a thermal state dominated by a disk component with temperatures of 0.26 keV at most, and at low luminosities the spectrum is dominated by a hard power law with a photon index in the range 1.4-2.1, consistent with a hard state. The source was also observed in a state consistent with the steep power-law state, with a photon index of similar to 3.5. In the thermal state, the luminosity of the disk component appears to scale with the fourth power of the inner disk temperature, which supports the presence of an optically thick, geometrically thin accretion disk. The low fractional variability (rms of 9% +/- 9%) in this state also suggests the presence of a dominant disk. The spectral changes and long-term variability of the source cannot be explained by variations of the beaming angle and are not consistent with the source being in a super-Eddington accretion state as is proposed for most ULX sources with lower luminosities. All this indicates that HLX-1 is an unusual ULX as it is similar to GBHBs, which have non-beamed and sub-Eddington emission, but with luminosities three orders of magnitude higher. In this picture, a lower limit on the mass of the black hole of > 9000 M(circle dot) can be derived, and the relatively low disk temperature in the thermal state also suggests the presence of an IMBH of a few 10(3) M(circle dot).
C1 [Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Farrell, Sean A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Farrell, Sean A.] Univ Sydney, Sch Phys A29, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Lin, Dacheng; Godet, Olivier; Barret, Didier; Webb, Natalie A.] Univ Toulouse 3, Univ Toulouse, Observ Midi Pyrenees, IRAP, F-31062 Toulouse, France.
[Lin, Dacheng; Godet, Olivier; Barret, Didier; Webb, Natalie A.] CNRS, IRAP, F-31028 Toulouse 4, France.
RP Servillat, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA.
EM mservillat@cfa.harvard.edu
FU NASA/Chandra [GO0-11063X, DD0-11050X]; NSF [AST-0909073]; UK Science and
Technology Funding Council; Australian Research Council; Australian
Research Council [DP110102889]; ESA Member States; NASA
FX We are grateful for the comments of the referee which helped us improve
and strengthen the paper. We thank Harvey Tananbaum and the Chandra team
for approving the Chandra DDT observations. M. S. thanks Josh Grindlay
and Jeff McClintock for helpful discussions. 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 and the Australian Research Council. S. A. F.
is the recipient of an Australian Research Council Post Doctoral
Fellowship, funded by grant DP110102889. Based on observations from
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA Member States and NASA. This research has made
use of data obtained from the Chandra Data Archive and software provided
by the Chandra X-ray Center (CXC) in the application packages CIAO,
ChIPS, and Sherpa. This work made use of data supplied by the UK Swift
Science Data Centre at the University of Leicester.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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ER
PT J
AU Silverman, JD
Kampczyk, P
Jahnke, K
Andrae, R
Lilly, SJ
Elvis, M
Civano, F
Mainieri, V
Vignali, C
Zamorani, G
Nair, P
Le Fevre, O
de Ravel, L
Bardelli, S
Bongiorno, A
Bolzonella, M
Cappi, A
Caputi, K
Carollo, CM
Contini, T
Coppa, G
Cucciati, O
de la Torre, S
Franzetti, P
Garilli, B
Halliday, C
Hasinger, G
Iovino, A
Knobel, C
Koekemoer, AM
Kovac, K
Lamareille, F
Le Borgne, JF
Le Brun, V
Maier, C
Mignoli, M
Pello, R
Perez-Montero, E
Ricciardelli, E
Peng, Y
Scodeggio, M
Tanaka, M
Tasca, L
Tresse, L
Vergani, D
Zucca, E
Brusa, M
Cappelluti, N
Comastri, A
Finoguenov, A
Fu, H
Gilli, R
Hao, H
Ho, LC
Salvato, M
AF Silverman, J. D.
Kampczyk, P.
Jahnke, K.
Andrae, R.
Lilly, S. J.
Elvis, M.
Civano, F.
Mainieri, V.
Vignali, C.
Zamorani, G.
Nair, P.
Le Fevre, O.
de Ravel, L.
Bardelli, S.
Bongiorno, A.
Bolzonella, M.
Cappi, A.
Caputi, K.
Carollo, C. M.
Contini, T.
Coppa, G.
Cucciati, O.
de la Torre, S.
Franzetti, P.
Garilli, B.
Halliday, C.
Hasinger, G.
Iovino, A.
Knobel, C.
Koekemoer, A. M.
Kovac, K.
Lamareille, F.
Le Borgne, J-F.
Le Brun, V.
Maier, C.
Mignoli, M.
Pello, R.
Perez-Montero, E.
Ricciardelli, E.
Peng, Y.
Scodeggio, M.
Tanaka, M.
Tasca, L.
Tresse, L.
Vergani, D.
Zucca, E.
Brusa, M.
Cappelluti, N.
Comastri, A.
Finoguenov, A.
Fu, H.
Gilli, R.
Hao, H.
Ho, L. C.
Salvato, M.
TI THE IMPACT OF GALAXY INTERACTIONS ON ACTIVE GALACTIC NUCLEUS ACTIVITY IN
zCOSMOS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: interactions; quasars: general; X-rays:
galaxies
ID SIMILAR-TO 1; SUPERMASSIVE BLACK-HOLES; STELLAR MASS FUNCTION; COSMOS
FIELD. II.; X-RAY SOURCES; STAR-FORMATION; OPTICAL SPECTROSCOPY;
INFRARED GALAXIES; REDSHIFT SURVEY; HOST GALAXIES
AB Close encounters between galaxies are expected to be a viable mechanism, as predicted by numerical simulations, by which accretion onto supermassive black holes can be initiated. To test this scenario, we construct a sample of 562 galaxies (M(*) > 2.5 x 10(10) M(circle dot)) in kinematic pairs over the redshift range 0.25 < z < 1.05 that are more likely to be interacting than a well-matched control sample of 2726 galaxies not identified as being in a pair, both from the zCOSMOS 20k spectroscopic catalog. Galaxies that harbor an active galactic nucleus (AGN) are identified on the basis of their X-ray emission (L(0.5-10) (keV) > 2 x 10(42) erg s(-1)) detected by Chandra. We find a higher fraction of an AGN in galaxies in pairs relative to isolated galaxies of similar stellar mass. Our result is primarily due to an enhancement of AGN activity, by a factor of 1.9 (observed) and 2.6 (intrinsic), for galaxies in pairs of projected separation less than 75 kpc and line-of-sight velocity offset less than 500 km s(-1). This study demonstrates that close kinematic pairs are conducive environments for black hole growth, either indicating a causal physical connection or an inherent relation, such as, to enhanced star formation. In the Appendix, we describe a method for estimating the intrinsic fractions of galaxies (either in pairs or the field) hosting an AGN with confidence intervals, and an excess fraction in pairs. We estimate that 17.8(-7.4)(+8.4)% of all moderate-luminosity AGN activity takes place within galaxies undergoing early stages of interaction that leaves open the question as to what physical processes are responsible for fueling the remaining similar to 80% that may include late-stage mergers.
C1 [Silverman, J. D.; Tanaka, M.] Univ Tokyo, IPMU, Kashiwa, Chiba 2778568, Japan.
[Silverman, J. D.; Kampczyk, P.; Lilly, S. J.; Carollo, C. M.; Knobel, C.; Kovac, K.; Maier, C.; Peng, Y.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Jahnke, K.; Andrae, R.; Hao, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Elvis, M.; Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mainieri, V.] European So Observ, D-85748 Garching, Germany.
[Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Zamorani, G.; Nair, P.; Bardelli, S.; Bolzonella, M.; Cappi, A.; Coppa, G.; Mignoli, M.; Vergani, D.; Zucca, E.; Cappelluti, N.; Comastri, A.; Gilli, R.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Le Fevre, O.; Cucciati, O.; de la Torre, S.; Lamareille, F.; Le Brun, V.; Tresse, L.] Lab Astrophys Marseille, Marseille, France.
[Caputi, K.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Bongiorno, A.; Brusa, M.; Finoguenov, A.] Max Planck Inst Extraterr Phys, D-84571 Garching, Germany.
[Contini, T.; Le Borgne, J-F.; Pello, R.; Perez-Montero, E.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Contini, T.; Le Borgne, J-F.; Pello, R.; Perez-Montero, E.] CNRS, IRAP, F-31400 Toulouse, France.
[Franzetti, P.; Garilli, B.; Salvato, M.] INAF IASF, I-20133 Milan, Italy.
[Halliday, C.] INAF Osservatorio Astron Arcetri, I-50125 Florence, Italy.
[Hasinger, G.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Iovino, A.; Scodeggio, M.; Tasca, L.] INAF Osservatorio Astron Brera, Milan, Italy.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Ricciardelli, E.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Fu, H.] CALTECH, Pasadena, CA 91125 USA.
[Ho, L. C.] Observatories Carnegie Inst Sci, Pasadena, CA 91101 USA.
RP Silverman, JD (reprint author), Univ Tokyo, IPMU, Kashiwa, Chiba 2778568, Japan.
RI Pello, Roser/G-4754-2010; Vignali, Cristian/J-4974-2012; Gilli,
Roberto/P-1110-2015; Bardelli, Sandro/O-9369-2015; Zucca,
Elena/O-9396-2015; Cappi, Alberto/O-9391-2015; Mignoli,
Marco/O-9426-2015; Bolzonella, Micol/O-9495-2015; Comastri,
Andrea/O-9543-2015
OI Zamorani, Giovanni/0000-0002-2318-301X; Koekemoer,
Anton/0000-0002-6610-2048; Perez Montero, E/0000-0003-3985-4882; Brusa,
Marcella/0000-0002-5059-6848; Bongiorno, Angela/0000-0002-0101-6624;
Scodeggio, Marco/0000-0002-2282-5850; Vergani,
Daniela/0000-0003-0898-2216; Jahnke, Knud/0000-0003-3804-2137;
Cappelluti, Nico/0000-0002-1697-186X; Maier,
Christian/0000-0001-6405-2182; Garilli, Bianca/0000-0001-7455-8750;
Vignali, Cristian/0000-0002-8853-9611; Gilli,
Roberto/0000-0001-8121-6177; Iovino, Angela/0000-0001-6958-0304;
Franzetti, Paolo/0000-0002-6986-0127; Bardelli,
Sandro/0000-0002-8900-0298; Zucca, Elena/0000-0002-5845-8132; Cappi,
Alberto/0000-0002-9200-7167; Mignoli, Marco/0000-0002-9087-2835;
Bolzonella, Micol/0000-0003-3278-4607; Comastri,
Andrea/0000-0003-3451-9970
FU World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan; German Science Foundation (DFG); Klaus Tschira Foundation
via Heidelberg Graduate School of Fundamental Physics (HGSFP)
FX The authors appreciate the useful discussions with Charles Steinhardt,
Yen-Ting Lin, and Ed Turner. This work was supported by World Premier
International Research Center Initiative (WPI Initiative), MEXT, Japan.
K.J. is supported by the Emmy Noether Programme by the German Science
Foundation (DFG). R. A. is funded by the Klaus Tschira Foundation via
the Heidelberg Graduate School of Fundamental Physics (HGSFP).
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JI Astrophys. J.
PD DEC 10
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300002
ER
PT J
AU Weisz, DR
Dolphin, AE
Dalcanton, JJ
Skillman, ED
Holtzman, J
Williams, BF
Gilbert, KM
Seth, AC
Cole, A
Gogarten, SM
Rosema, K
Karachentsev, ID
McQuinn, KBW
Zaritsky, D
AF Weisz, Daniel R.
Dolphin, Andrew E.
Dalcanton, Julianne J.
Skillman, Evan D.
Holtzman, Jon
Williams, Benjamin F.
Gilbert, Karoline M.
Seth, Anil C.
Cole, Andrew
Gogarten, Stephanie M.
Rosema, Keith
Karachentsev, Igor D.
McQuinn, Kristen B. W.
Zaritsky, Dennis
TI HOW TYPICAL ARE THE LOCAL GROUP DWARF GALAXIES?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies:
stellar content; Local Group
ID STAR-FORMATION HISTORY; HUBBLE-SPACE-TELESCOPE; STELLAR POPULATIONS; M81
GROUP; IRREGULAR GALAXIES; STRUCTURAL PARAMETERS; NGC 147; SPHEROIDALS;
REIONIZATION; KINEMATICS
AB We compare the cumulative star formation histories (SFHs) of Local Group (LG) dwarf galaxies with those in the volume-limited ACS Nearby Galaxy Survey Treasury (ANGST) sample (D less than or similar to 4 Mpc), in order to understand how typical the LG dwarf galaxies are relative to those in the nearby universe. The SFHs were derived in a uniform manner from high-quality optical color-magnitude diagrams constructed from Hubble Space Telescope imaging. We find that the mean cumulative SFHs of the LG dwarfs are comparable to the mean cumulative SFHs of the ANGST sample for the three different morphological types (dwarf spheroidals/ellipticals: dSph/dE; dwarf irregulars: dI; transition dwarfs: dTrans). We also discuss effects such as population gradients and systematic uncertainties in the stellar models that may influence the derived SFHs. Both the ANGST and LG dwarf galaxies show a consistent and strong morphology-density relationship, emphasizing the importance of environment in the evolution of dwarf galaxies. Specifically, we confirm that dIs are found at lower densities and higher luminosities than dSphs, within this large sample. We also find that dTrans are located in similar environments to those occupied by dwarf irregular galaxies, but have systematically lower luminosities that are more comparable to those of dwarf spheroidals. The similarity of the SFHs and morphology-density relationships of the LG and ANGST dwarf galaxies suggests that the LG dwarfs are a good representation of dwarf galaxies in the local universe.
C1 [Weisz, Daniel R.; Dalcanton, Julianne J.; Williams, Benjamin F.; Gilbert, Karoline M.; Gogarten, Stephanie M.; Rosema, Keith] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Weisz, Daniel R.; Skillman, Evan D.; McQuinn, Kristen B. W.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
[Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85756 USA.
[Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cole, Andrew] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia.
[Karachentsev, Igor D.] Russian Acad Sci, Special Astrophys Observ, Nizhnji Arkhyz 369167, Karachai Circes, Russia.
[Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Weisz, DR (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM dweisz@astro.washington.edu; adolphin@raytheon.com;
jd@astro.washington.edu; skillman@astro.umn.edu; holtz@nmsu.edu;
ben@astro.washington.edu; kgilbert@astro.washington.edu;
aseth@cfa.harvard.edu; andrew.cole@utas.edu.au;
stephanie@astro.washington.edu; krosema@astro.washington.edu;
ikar@luna.sao.ru; kmcquinn@astro.umn.edu; dzaritsky@as.arizona.edu
OI Cole, Andrew/0000-0003-0303-3855; Gogarten,
Stephanie/0000-0002-7231-9745; Weisz, Daniel/0000-0002-6442-6030
FU University of Minnesota; RFBR [10-02-00123]; NASA [HST-HF-51273.01,
GO-10915, DD-11307, GO-11986]; Space Telescope Science Institute; AURA,
Inc., under NASA [NAS5-26555]
FX The authors thank the anonymous referee for a number of insightful
comments that have helped to improve this paper. D. R. W. is grateful
for support from the University of Minnesota Doctoral Dissertation
Fellowship and Penrose Fellowship. I. D. K. is partially supported by
RFBR grant 10-02-00123. Support for K. M. G. is provided by NASA through
Hubble Fellowship grant HST-HF-51273.01 awarded by the Space Telescope
Science Institute. This work is based on observations made with the
NASA/ESA Hubble Space Telescope, obtained from the data archive at the
Space Telescope Science Institute. Support for this work was provided by
NASA through grants GO-10915, DD-11307, and GO-11986 from the Space
Telescope Science Institute, which is operated by AURA, Inc., under NASA
contract NAS5-26555. 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
extensive use of NASA's Astrophysics Data System Bibliographic Services.
NR 51
TC 28
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U1 1
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 DEC 10
PY 2011
VL 743
IS 1
AR 8
DI 10.1088/0004-637X/743/1/8
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300008
ER
PT J
AU Wright, NJ
Drake, JJ
Mamajek, EE
Henry, GW
AF Wright, Nicholas J.
Drake, Jeremy J.
Mamajek, Eric E.
Henry, Gregory W.
TI THE STELLAR-ACTIVITY-ROTATION RELATIONSHIP AND THE EVOLUTION OF STELLAR
DYNAMOS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: coronae; stars: evolution; stars: late-type;
stars: magnetic field; stars: rotation; X-rays: stars
ID X-RAY-EMISSION; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; LOW-MASS STARS;
ALL-SKY SURVEY; M-DWARF STARS; OPEN CLUSTER NGC-2516; YOUNG OPEN
CLUSTER; T-TAURI STARS; SUN-LIKE STARS
AB We present a sample of 824 solar and late-type stars with X-ray luminosities and rotation periods. This is used to study the relationship between rotation and stellar activity and derive a new estimate of the convective turnover time. From an unbiased subset of this sample the power-law slope of the unsaturated regime, L(X)/L(bol) alpha Ro(beta), is fit as beta = -2.70 +/- 0.13. This is inconsistent with the canonical beta = -2 slope to a confidence of 5 sigma, and argues for an additional term in the dynamo number equation. From a simple scaling analysis this implies Delta Omega/Omega alpha Omega(0.7), i.e., the differential rotation of solar-type stars gradually declines as they spin down. Supersaturation is observed for the fastest rotators in our sample and its parametric dependencies are explored. Significant correlations are found with both the corotation radius and the excess polar updraft, the latter theory providing a stronger dependence and being supported by other observations. We estimate mass-dependent empirical thresholds for saturation and supersaturation and map out three regimes of coronal emission. Late F-type stars are shown never to pass through the saturated regime, passing straight from supersaturated to unsaturated X-ray emission. The theoretical threshold for coronal stripping is shown to be significantly different from the empirical saturation threshold (Ro < 0.13), suggesting it is not responsible. Instead we suggest that a different dynamo configuration is at work in stars with saturated coronal emission. This is supported by a correlation between the empirical saturation threshold and the time when stars transition between convective and interface sequences in rotational spin-down models.
C1 [Wright, Nicholas J.; Drake, Jeremy J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mamajek, Eric E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
RP Wright, NJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nwright@cfa.harvard.edu
FU Chandra [AR9-0003X]; NASA [NAS8-39073]; NASA; NSF; Tennessee State
University; State of Tennessee
FX We thank the anonymous referee for a prompt and helpful report that
improved this work. This work has made use of NASA's Astrophysics Data
System, the Simbad and Vizier databases (operated at CDS, Strasbourg,
France) and data from the ROSAT, XMM-Newton, and Chandra X-Ray
Observatory. This work was funded by Chandra Grant AR9-0003X. J.J.D. was
supported by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC)
during the course of this research and thanks the CXC director, Harvey
Tananbaum, and the CXC science team for advice and support. G. W. H.
acknowledges support from NASA, NSF, Tennessee State University, and the
State of Tennessee through its Centers of Excellence program.
NR 163
TC 141
Z9 141
U1 0
U2 3
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 DEC 10
PY 2011
VL 743
IS 1
AR 48
DI 10.1088/0004-637X/743/1/48
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300048
ER
PT J
AU ZuHone, JA
Markevitch, M
Lee, D
AF ZuHone, J. A.
Markevitch, M.
Lee, D.
TI SLOSHING OF THE MAGNETIZED COOL GAS IN THE CORES OF GALAXY CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: intracluster medium; methods: numerical; X-rays:
galaxies: clusters
ID ANISOTROPIC THERMAL CONDUCTION; DIFFUSE RADIO-EMISSION; FARADAY-ROTATION
MAPS; FIELD POWER SPECTRUM; X-RAY-PROPERTIES; COLD FRONTS; COMA CLUSTER;
MAGNETOHYDRODYNAMIC SIMULATIONS; PARTICLE REACCELERATION; INTRACLUSTER
MEDIUM
AB X-ray observations of many clusters of galaxies reveal the presence of edges in surface brightness and temperature, known as "cold fronts." In relaxed clusters with cool cores, these edges have been interpreted as evidence for the "sloshing" of the core gas in the cluster's gravitational potential. The smoothness of these edges has been interpreted as evidence for the stabilizing effect of magnetic fields "draped" around the front surfaces. To check this hypothesis, we perform high-resolution magnetohydrodynamics simulations of magnetized gas sloshing in galaxy clusters initiated by encounters with subclusters. We go beyond previous works on the simulation of cold fronts in a magnetized intracluster medium by simulating their formation in realistic, idealized mergers with high resolution (Delta x similar to 2 kpc). Our simulations sample a parameter space of plausible initial magnetic field strengths and field configurations. In the simulations, we observe strong velocity shears associated with the cold fronts amplifying the magnetic field along the cold front surfaces, increasing the magnetic field strength in these layers by up to an order of magnitude, and boosting the magnetic pressure up to near-equipartition with thermal pressure in some cases. In these layers, the magnetic field becomes strong enough to stabilize the cold fronts against Kelvin-Helmholtz instabilities, resulting in sharp, smooth fronts as those seen in observations of real clusters. These magnetic fields also result in strong suppression of mixing of high-and low-entropy gases in the cluster, seen in our simulations of mergers in the absence of a magnetic field. As a result, the heating of the core due to sloshing is very modest and is unable to stave off a cooling catastrophe.
C1 [ZuHone, J. A.; Markevitch, M.] NASA, Astrophys Sci Div, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[ZuHone, J. A.; Markevitch, M.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Lee, D.] Univ Chicago, Dept Astron, ASC Flash Ctr, Chicago, IL 60637 USA.
RP ZuHone, JA (reprint author), NASA, Astrophys Sci Div, High Energy Astrophys Lab, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
FU NASA; ASC/Alliances Center for Astrophysical Thermonuclear Flashes at
the University of Chicago
FX We thank the anonymous referee for helpful and constructive comments and
suggestions. J.A.Z. thanks Ian Parrish, Bill Forman, Eric Hallman, and
Mateusz Ruszkowski for useful discussions and advice. Calculations were
performed using the computational resources of the Smithsonian
Insitution's Hendron Data Center, Argonne National Laboratory, and the
National Institute for Computational Sciences at the University of
Tennessee. Analysis of the simulation data was carried out using the AMR
analysis and visualization toolset yt (Turk et al. 2011), which is
available for download at http://yt.enzotools.org, and for which Matthew
Turk provided considerable help toward getting it working for the
analysis for this paper. J.A.Z. is supported by the NASA Postdoctoral
Program. The software used in this work was in part developed by the
DOE-supported ASC/Alliances Center for Astrophysical Thermonuclear
Flashes at the University of Chicago.
NR 88
TC 50
Z9 50
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 DEC 10
PY 2011
VL 743
IS 1
AR 16
DI 10.1088/0004-637X/743/1/16
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 853EF
UT WOS:000297408300016
ER
PT J
AU Dawson, RI
Murray-Clay, RA
Fabrycky, DC
AF Dawson, Rebekah I.
Murray-Clay, Ruth A.
Fabrycky, Daniel C.
TI ON THE MISALIGNMENT OF THE DIRECTLY IMAGED PLANET beta PICTORIS b WITH
THE SYSTEM'S WARPED INNER DISK
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planet-disk interactions; planets and satellites: individual (beta
Pictoris b); stars: individual (beta Pictoris)
ID GIANT PLANET; SPACE-TELESCOPE; CORONAGRAPHIC OBSERVATIONS; CIRCUMSTELLAR
DISK; INCLINED ORBIT; DEBRIS DISK; DUST DISK; CLUSTER; INSTABILITY;
ASYMMETRIES
AB The vertical warp in the debris disk beta Pictoris-an inclined inner disk extending into a flat outer disk-has long been interpreted as the signpost of a planet on an inclined orbit. Direct images spanning 2004-2010 have revealed beta Pictoris b, a planet with a mass and orbital distance consistent with this picture. However, it was recently reported that the orbit of planet b is aligned with the flat outer disk, not the inclined inner disk, and thus lacks the inclination to warp the disk. We explore three scenarios for reconciling the apparent misalignment of the directly imaged planet beta Pictoris b with the warped inner disk of beta Pictoris: observational uncertainty, an additional planet, and damping of planet b's inclination. We find that, at the extremes of the uncertainties, the orbit of beta Pictoris b has the inclination necessary to produce the observed warp. We also find that if planet b were aligned with the flat outer disk, it would prevent another planet from creating a warp with the observed properties; therefore planet b itself must be responsible for the warp. Finally, planet b's inclination could have been damped by dynamical friction and still produce the observed disk morphology, but the feasibility of damping depends on disk properties and the presence of other planets. More precise observations of the orbit of planet b and the position angle of the outer disk will allow us to distinguish between the first and third scenarios.
C1 [Dawson, Rebekah I.; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
RP Dawson, RI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rdawson@cfa.harvard.edu
FU NSF [DGE-1144152]; NASA [HF-51272.01]; Harvard FAS Sciences Division
Research Computing Group
FX We thank Michael Fitzgerald, Paul Kalas, and Philippe Thebault for beta
Pictoris insights, and Thayne Currie and an anonymous referee for
helpful comments. R.I.D. acknowledges support by NSF Graduate Research
Fellowship DGE-1144152 and D.C.F. by NASA Hubble Fellowship HF-51272.01.
Simulations were run on the Odyssey cluster supported by the Harvard FAS
Sciences Division Research Computing Group.
NR 31
TC 19
Z9 19
U1 0
U2 10
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 DEC 10
PY 2011
VL 743
IS 1
AR L17
DI 10.1088/2041-8205/743/1/L17
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 852QN
UT WOS:000297372600017
ER
PT J
AU Maitra, D
Miller, JM
Raymond, JC
Reynolds, MT
AF Maitra, Dipankar
Miller, Jon M.
Raymond, John C.
Reynolds, Mark T.
TI A STRONG EMISSION LINE NEAR 24.8 angstrom IN THE X-RAY BINARY SYSTEM
MAXI J0556-332: GRAVITATIONAL REDSHIFT OR UNUSUAL DONOR?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; binaries: general; X-rays: binaries; X-rays:
individual (MAXI J0556-332)
ID REFLECTION GRATING SPECTROMETER; SUBDWARF B-STARS; XMM-NEWTON;
SPECTROSCOPY; COMPANIONS; ABSORPTION; GAS
AB We report the discovery of a strong emission line near 24.8 angstrom (0.5 keV) in the newly discovered X-ray binary system MAXI J0556-332 with the reflection grating spectrometer (RGS) on board the XMM-Newton observatory. The X-ray light curve morphology during these observations is complex and shows occasional dipping behavior. Here we present time-and rate-selected spectra from the RGS and show that this strong emission line is unambiguously present in all the XMM observations. The measured line center is consistent with the Ly alpha transition of N VII in the rest frame. While the spectra contain imprints of absorption lines and edges, there appear to be no other significantly prominent narrow line due to the source itself, thus making the identification of the 24.8 angstrom line uncertain. We discuss possible physical scenarios, including a gravitationally redshifted O VIII Ly alpha line originating at the surface of a neutron star or an unusual donor with an extremely high N/O abundance (>57) relative to solar that may have produced this comparatively strong emission line.
C1 [Maitra, Dipankar; Miller, Jon M.; Reynolds, Mark T.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Maitra, D (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
EM dmaitra@umich.edu
NR 29
TC 3
Z9 3
U1 0
U2 10
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 DEC 10
PY 2011
VL 743
IS 1
AR L11
DI 10.1088/2041-8205/743/1/L11
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 852QN
UT WOS:000297372600011
ER
PT J
AU Oberg, KI
Murray-Clay, R
Bergin, EA
AF Oeberg, Karin I.
Murray-Clay, Ruth
Bergin, Edwin A.
TI THE EFFECTS OF SNOWLINES ON C/O IN PLANETARY ATMOSPHERES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; circumstellar matter; molecular processes; planetary
systems; planet-disk interactions; planets and satellites: atmospheres
ID TRANSITING EXTRASOLAR PLANET; SOLAR NEBULA; PROTOPLANETARY DISKS;
INTERSTELLAR-MEDIUM; THERMAL-DESORPTION; EMISSION-SPECTRUM; WATER-VAPOR;
HD 209458B; SNOW LINE; HR 8799
AB The C/O ratio is predicted to regulate the atmospheric chemistry in hot Jupiters. Recent observations suggest that some exoplanets, e.g., Wasp 12-b, have atmospheric C/O ratios substantially different from the solar value of 0.54. In this Letter, we present a mechanism that can produce such atmospheric deviations from the stellar C/O ratio. In protoplanetary disks, different snowlines of oxygen-and carbon-rich ices, especially water and carbon monoxide, will result in systematic variations in the C/O ratio both in the gas and in the condensed phases. In particular, between the H2O and CO snowlines most oxygen is present in icy grains-the building blocks of planetary cores in the core accretion model-while most carbon remains in the gas phase. This region is coincidental with the giant-planet-forming zone for a range of observed protoplanetary disks. Based on standard core accretion models of planet formation, gas giants that sweep up most of their atmospheres from disk gas outside of the water snowline will have a C/O similar to 1, while atmospheres significantly contaminated by evaporating planetesimals will have a stellar or substellar C/O when formed at the same disk radius. The overall metallicity will also depend on the atmosphere formation mechanism, and exoplanetary atmospheric compositions may therefore provide constraints on where and how a specific planet formed.
C1 [Oeberg, Karin I.; Murray-Clay, Ruth] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM koberg@cfa.harvard.edu
FU NASA [NAS 5-26555]; Space Telescope Science Institute; NSF [1008800]
FX We are grateful for comments from an anonymous referee. Support for
K.I.O. is provided by NASA through a Hubble Fellowship grant awarded by
the Space Telescope Science Institute, operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555. E.A.B. acknowledges support from NSF via grant No. 1008800.
NR 41
TC 113
Z9 115
U1 2
U2 17
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 DEC 10
PY 2011
VL 743
IS 1
AR L16
DI 10.1088/2041-8205/743/1/L16
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 852QN
UT WOS:000297372600016
ER
PT J
AU van Dokkum, PG
Brammer, G
Fumagalli, M
Nelson, E
Franx, M
Rix, HW
Kriek, M
Skelton, RE
Patel, S
Schmidt, KB
Bezanson, R
Bian, FY
da Cunha, E
Erb, DK
Fan, XH
Schreiber, NF
Illingworth, GD
Labbe, I
Lundgren, B
Magee, D
Marchesini, D
McCarthy, P
Muzzin, A
Quadri, R
Steidel, CC
Tal, T
Wake, D
Whitaker, KE
Williams, A
AF van Dokkum, Pieter G.
Brammer, Gabriel
Fumagalli, Mattia
Nelson, Erica
Franx, Marijn
Rix, Hans-Walter
Kriek, Mariska
Skelton, Rosalind E.
Patel, Shannon
Schmidt, Kasper B.
Bezanson, Rachel
Bian, Fuyan
da Cunha, Elisabete
Erb, Dawn K.
Fan, Xiaohui
Schreiber, Natascha Foerster
Illingworth, Garth D.
Labbe, Ivo
Lundgren, Britt
Magee, Dan
Marchesini, Danilo
McCarthy, Patrick
Muzzin, Adam
Quadri, Ryan
Steidel, Charles C.
Tal, Tomer
Wake, David
Whitaker, Katherine E.
Williams, Anna
TI FIRST RESULTS FROM THE 3D-HST SURVEY: THE STRIKING DIVERSITY OF MASSIVE
GALAXIES AT z > 1
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: evolution
ID STAR-FORMATION HISTORIES; STELLAR POPULATION SYNTHESIS; DIGITAL SKY
SURVEY; ULTRA-DEEP-FIELD; SIMILAR-TO 3; QUIESCENT GALAXIES; FORMING
GALAXIES; RED GALAXIES; LUMINOSITY FUNCTIONS; REDSHIFT GALAXIES
AB We present first results from the 3D-HST program, a near-IR spectroscopic survey performed with the Wide Field Camera 3 (WFC3) on the HST. We have used 3D-HST spectra to measure redshifts and Ha equivalent widths (EWH alpha) for a complete, stellar mass-limited sample of 34 galaxies at 1 < z < 1.5 with M-star > 10(11) M-circle dot in the COSMOS, GOODS, and AEGIS fields. We find that a substantial fraction of massive galaxies at this epoch are forming stars at a high rate: the fraction of galaxies with EWH alpha > 10 angstrom is 59%, compared to 10% among Sloan Digital Sky Survey galaxies of similar masses at z = 0.1. Galaxies with weak Ha emission show absorption lines typical of 2-4 Gyr old stellar populations. The structural parameters of the galaxies, derived from the associated WFC3 F140W imaging data, correlate with the presence of H alpha; quiescent galaxies are compact with high Sersic index and high inferred velocity dispersion, whereas star-forming galaxies are typically large two-armed spiral galaxies, with low Sersic index. Some of these star-forming galaxies might be progenitors of the most massive S0 and Sa galaxies. Our results challenge the idea that galaxies at fixed mass form a homogeneous population with small scatter in their properties. Instead, we find that massive galaxies form a highly diverse population at z > 1, in marked contrast to the local universe.
C1 [van Dokkum, Pieter G.; Nelson, Erica; Skelton, Rosalind E.; Bezanson, Rachel; Lundgren, Britt; Muzzin, Adam; Tal, Tomer; Wake, David; Whitaker, Katherine E.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Brammer, Gabriel] European So Observ, Santiago 19, Chile.
[Fumagalli, Mattia; Franx, Marijn; Patel, Shannon; Labbe, Ivo] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Rix, Hans-Walter; Schmidt, Kasper B.; da Cunha, Elisabete] MPIA, D-69117 Heidelberg, Germany.
[Kriek, Mariska] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bian, Fuyan; Fan, Xiaohui] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Erb, Dawn K.] Univ Wisconsin Milwaukee, Dept Phys, Milwaukee, WI 53201 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; Quadri, Ryan] Carnegie Observ, Pasadena, CA 91101 USA.
[Steidel, Charles C.] CALTECH, Pasadena, CA 91125 USA.
[Williams, Anna] Univ Wisconsin Madison, Dept Astron, Madison, WI 53706 USA.
RP van Dokkum, PG (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA.
RI Skelton, Rosalind/S-1845-2016;
OI Skelton, Rosalind/0000-0001-7393-3336; Bezanson,
Rachel/0000-0001-5063-8254
NR 51
TC 54
Z9 54
U1 1
U2 11
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 DEC 10
PY 2011
VL 743
IS 1
AR L15
DI 10.1088/2041-8205/743/1/L15
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 852QN
UT WOS:000297372600015
ER
PT J
AU Tscherbul, TV
Rittenhouse, ST
AF Tscherbul, T. V.
Rittenhouse, Seth T.
TI Three-body radio-frequency association of Efimov trimers
SO PHYSICAL REVIEW A
LA English
DT Article
ID LARGE SCATTERING LENGTH; ATOMS; STATES; SYSTEM; RECOMBINATION;
UNIVERSALITY; COLLISIONS
AB We present a theoretical analysis of rf association of Efimov trimers in a two-component Bose gas with short-range interactions. Using the adiabatic hyperspherical formalism to solve the quantum three-body problem, we obtain universal expressions for three-body rf association rates as a function of the s-wave scattering length a > 0. We find that the association rates scale as a(-2) in the limit of large a, and diverge as a(3)a(ad)(3) whenever an Efimov state crosses the atom-dimer threshold (where a(ad) stands for the atom-dimer scattering length). Our calculations show that trimer formation rates as large as similar to 10(-21) cm(6)/s can be achieved with rf Rabi frequencies on the order of 1 MHz, suggesting that direct rf association is a powerful tool for making and probing few-body quantum states in ultracold atomic gases.
C1 [Tscherbul, T. V.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
[Tscherbul, T. V.; Rittenhouse, Seth T.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Tscherbul, TV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
RI Tscherbul, Timur/K-3286-2014
OI Tscherbul, Timur/0000-0001-5689-040X
FU NSF; Smithsonian Astrophysical Observatory
FX This work was supported by NSF grants to the Harvard-MIT CUA and ITAMP
at Harvard University and the Smithsonian Astrophysical Observatory.
NR 48
TC 6
Z9 6
U1 1
U2 7
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 DEC 9
PY 2011
VL 84
IS 6
AR 062706
DI 10.1103/PhysRevA.84.062706
PG 6
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 860EL
UT WOS:000297931500001
ER
PT J
AU Lemaitre, R
Felder, DL
AF Lemaitre, Rafael
Felder, Darryl L.
TI A new genus of Paguridae (Crustacea: Decapoda: Anomura) for a new
species from the tropical eastern Pacific and Pagurus longimanus Wass,
1963 from the tropical western Atlantic
SO ZOOTAXA
LA English
DT Article
DE Crustacea; Decapoda; Anomura; Paguridae; new genus; Spathapagurus; new
species; Spathapagurus collinae; geminate species; tropical eastern
Pacific
ID HERMIT CRABS CRUSTACEA; FAMILY PAGURIDAE; PAGUROIDEA
AB A new genus, Spathapagurus, is described for S. collinae n. sp. from the tropical eastern Pacific and its geminate species Pagurus longimanus Wass, 1963 from the tropical western Atlantic. These congeners share grossly unequal chelipeds, the right being narrowly spatulate and up to four times longer than the left. The males have short sexual tubes consisting of slight extrusions of the vas deferens from the gonopores, though these short tubes are masked by long, forwardly directed setae. The females lack first pleopods and have unpaired left second to fifth pleopods. The new species is fully described, illustrated, and compared to P. longimanus, herein placed in the new genus. The diagnosis of the latter species is emended and its distribution expanded to include the Caribbean coast of Panama in Central America.
C1 [Lemaitre, Rafael] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Suitland, MD 20746 USA.
[Felder, Darryl L.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA.
[Felder, Darryl L.] Univ Louisiana Lafayette, Lab Crustacean Res, Lafayette, LA 70504 USA.
RP Lemaitre, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM lemaitrr@si.edu; dlf4517@louisiana.edu
FU U.S. National Science Foundation NSF/AToL [EF-0531603]
FX We especially thank Rachel Collin and her support staff at the
Smithsonian Tropical Research Institute who facilitated our access to
study materials and direct participation in several of her research
cruises aboard the R/V Urraca. We are no less grateful to Heather
Bracken-Grissom who participated with Rachel Collin in specifically the
2005 cruise and returned well-preserved hermit crabs and many other
decapods for morphological and molecular analyses. The help of Marcos
Tavares in locating some references published in Brazilian journals is
also acknowledged, as is the assistance of Rose Gulledge in the
electronic mounting of the plates. This study was supported in part by
funding to D. L. Felder from U.S. National Science Foundation NSF/AToL
EF-0531603 for the Decapod Tree of Life project.
NR 36
TC 4
Z9 4
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 DEC 9
PY 2011
IS 3125
BP 39
EP 50
PG 12
WC Zoology
SC Zoology
GA 904UO
UT WOS:000301223600003
ER
PT J
AU Joshi, PS
Malafarina, D
Narayan, R
AF Joshi, Pankaj S.
Malafarina, Daniele
Narayan, Ramesh
TI Equilibrium configurations from gravitational collapse
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID BLACK-HOLE SPIN; NONVANISHING TANGENTIAL STRESSES; VANISHING RADIAL
PRESSURE; NAKED SINGULARITIES; COSMIC CENSORSHIP; SCALAR FIELD;
COSMOLOGICAL CONSTANT; ACCRETION DISK; DUST CLOUD; END STATE
AB We develop here a new procedure within Einstein's theory of gravity to generate equilibrium configurations that result as the final state of gravitational collapse from regular initial conditions. As a simplification, we assume that the collapsing fluid is supported only by tangential pressure. We show that the equilibrium geometries generated by this method form a subset of static solutions to the Einstein equations, and that they can either be regular or develop a naked singularity at the center. When a singularity is present, there are key differences in the properties of stable circular orbits relative to those around a Schwarzschild black hole with the same mass. Therefore, if an accretion disk is present around such a naked singularity it could be observationally distinguished from a disk around a black hole.
C1 [Joshi, Pankaj S.; Malafarina, Daniele] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Joshi, PS (reprint author), Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
EM psj@tifr.res.in; daniele.malafarina@polimi.it; rnarayan@cfa.harvard.edu
RI Malafarina, Daniele/O-2076-2013;
OI Malafarina, Daniele/0000-0002-8100-8797; Narayan,
Ramesh/0000-0002-1919-2730
NR 71
TC 30
Z9 30
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
EI 1361-6382
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD DEC 7
PY 2011
VL 28
IS 23
AR 235018
DI 10.1088/0264-9381/28/23/235018
PG 19
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 865OU
UT WOS:000298321000018
ER
PT J
AU Pyenson, ND
AF Pyenson, Nicholas D.
TI The high fidelity of the cetacean stranding record: insights into
measuring diversity by integrating taphonomy and macroecology
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE taphonomy; diversity; strandings; macroecology; fossil record
ID MOLLUSCAN DEATH ASSEMBLAGES; SP N. CETACEA; ABUNDANCE; WHALES;
POPULATIONS; ZIPHIIDAE; RICHNESS; MIOCENE; MEXICO; SEA
AB Stranded cetaceans have long intrigued naturalists because their causation has escaped singular explanations. Regardless of cause, strandings also represent a sample of the living community, although their fidelity has rarely been quantified. Using commensurate stranding and sighting records compiled from archived datasets representing nearly every major ocean basin, I demonstrated that the cetacean stranding record faithfully reflects patterns of richness and relative abundance in living communities, especially for coastlines greater than 2000 km and latitudinal gradients greater than 4 degrees. Live-dead fidelity metrics from seven different countries indicated that strandings were almost always richer than live surveys; richness also increased with coastline length. Most death assemblages recorded the same ranked relative abundance as living communities, although this correlation decreased in strength and significance at coastline lengths greater than 15 000 km, highlighting the importance of sampling diversity at regional scales. Rarefaction analyses indicated that sampling greater than 10 years generally enhanced the completeness of death assemblages, although protracted temporal sampling did not substitute for sampling over longer coastlines or broader latitudes. Overall, this global live-dead comparison demonstrated that strandings almost always provided better diversity information about extant cetacean communities than live surveys; such archives are therefore relevant for macroecological and palaeobiological studies of cetacean community change through time.
C1 [Pyenson, Nicholas D.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Pyenson, Nicholas D.] Univ Washington, Burke Museum Nat Hist & Culture, Dept Mammal, Seattle, WA 98195 USA.
[Pyenson, Nicholas D.] Univ Washington, Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA.
RP Pyenson, ND (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA.
EM pyensonn@si.edu
FU Natural Sciences and Engineering Research Council of Canada; Smithsonian
Institution
FX I thank the efforts of marine mammal stranding network volunteers across
the globe, whose millions of hours of fieldwork generated the primary
live and dead occurrence datasets. From NOAA's National Marine Fisheries
Service, I thank J. Cordaro (Southwest Regional Office), B. Norberg and
S. A. Norman (Northwest Regional Office), and T. Bowen and M. Garron
(Northeast Regional Office) for assistance with US stranding network
data. The Irish stranding and sightings data are validated by the Irish
Whale and Dolphin Group and are available online. I also warmly
acknowledge A. Frantzis and the Pelagos Cetacean Research Institute for
discussion and access to stranding data from Greece and the Greek
Archipelago. The Department of Conservation and A. van Helden (Museum of
New Zealand, Te Papa Tongarewa) supplied stranding data from New
Zealand. I gratefully acknowledge C. J. Camphuysen and J. Haelters for
access to other national datasets. Comments and suggestions from two
anonymous reviewers improved the quality of this paper. A. K.
Behrensmeyer, R. E. Fordyce, J. A. Goldbogen and J. F. Parham all
provided constructive comments and support. This research was funded in
part by a postdoctoral research fellowship from the Natural Sciences and
Engineering Research Council of Canada and by the Smithsonian
Institution.
NR 43
TC 28
Z9 31
U1 2
U2 24
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 DEC 7
PY 2011
VL 278
IS 1724
BP 3608
EP 3616
DI 10.1098/rspb.2011.0441
PG 9
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 842FS
UT WOS:000296579800020
PM 21525057
ER
PT J
AU Kilburn, VL
Ibanez, R
Green, DM
AF Kilburn, Vanessa L.
Ibanez, Roberto
Green, David M.
TI Reptiles as potential vectors and hosts of the amphibian pathogen
Batrachochytrium dendrobatidis in Panama
SO DISEASES OF AQUATIC ORGANISMS
LA English
DT Article
DE Batrachochytrium dendrobatidis; Chytridiomycosis; Amphibian pathogen;
Reservoir host; Lizard; Snake; Reptilia; Neotropics
ID POPULATION DECLINES; CHYTRID FUNGUS; CLIMATE-CHANGE; NORTHERN
QUEENSLAND; LATIN-AMERICA; PCR ASSAY; CHYTRIDIOMYCOSIS; DISEASE; WATER;
AUSTRALIA
AB Chytridiomycosis, the disease caused by Batrachochytrium dendrobatidis, is considered to be a disease exclusively of amphibians. However, B. dendrobatidis may also be capable of persisting in the environment, and non-amphibian vectors or hosts may contribute to disease transmission. Reptiles living in close proximity to amphibians and sharing similar ecological traits could serve as vectors or reservoir hosts for B. dendrobatidis, harbouring the organism on their skin without succumbing to disease. We surveyed for the presence of B. dendrobatidis DNA among 211 lizards and 8 snakes at 8 sites at varying elevations in Panama where the syntopic amphibians were at pre-epizootic, epizootic or post-epizootic stages of chytridiomycosis. Detection of B. dendrobatidis DNA was done using qPCR analysis. Evidence of the amphibian pathogen was present at varying intensities in 29 of 79 examined Anolis humilis lizards (32%) and 9 of 101 A. lionotus lizards (9%), and in one individual each of the snakes Pliocercus euryzonus, Imantodes cenchoa, and Nothopsis rugosus. In general, B. dendrobatidis DNA prevalence among reptiles was positively correlated with the infection prevalence among co-occurring anuran amphibians at any particular site (r = 0.88, p = 0.004). These reptiles, therefore, may likely be vectors or reservoir hosts for B. dendrobatidis and could serve as disease transmission agents. Although there is no evidence of B. dendrobatidis disease-induced declines in reptiles, cases of coincidence of reptile and amphibian declines suggest this potentiality. Our study is the first to provide evidence of non-amphibian carriers for B. dendrobatidis in a natural Neotropical environment.
C1 [Green, David M.] McGill Univ, Redpath Museum, Montreal, PQ H3A 2K6, Canada.
[Kilburn, Vanessa L.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
[Ibanez, Roberto] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Green, DM (reprint author), McGill Univ, Redpath Museum, 859 Sherbrooke St W, Montreal, PQ H3A 2K6, Canada.
EM david.m.green@mcgill.ca
FU NSERC Canada CGS M; NSERC
FX We thank J. Suraci, J. Ray, G. Reina, A. Crawford, V. Flechas, K.
Turner, D. Turner, S. Oestreicher, E. Trimble, D. Raab, P. McGaw, A.
Kilburn and C. Jaramillo for help in the field; O. Sanjur and E.
Bermingham for advice and support for laboratory work at the STRI Naos
lab in Panama; A. Bramard (Genome Quebec) and C. Brisson for help with
the molecular analyses; and the Autoridad Nacional del Ambiente de
Panama for expediting research permits. This research was supported by
an NSERC Canada CGS M scholarship to V. L. K. and an NSERC Canada
Discovery Grant to D. M. G.
NR 49
TC 20
Z9 20
U1 3
U2 36
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 0177-5103
J9 DIS AQUAT ORGAN
JI Dis. Aquat. Org.
PD DEC 6
PY 2011
VL 97
IS 2
BP 127
EP 134
DI 10.3354/dao02409
PG 8
WC Fisheries; Veterinary Sciences
SC Fisheries; Veterinary Sciences
GA 857FS
UT WOS:000297702900005
PM 22303629
ER
PT J
AU Hines, HM
Counterman, BA
Papa, R
de Moura, PA
Cardoso, MZ
Linares, M
Mallet, J
Reed, RD
Jiggins, CD
Kronforst, MR
McMillan, WO
AF Hines, Heather M.
Counterman, Brian A.
Papa, Riccardo
de Moura, Priscila Albuquerque
Cardoso, Marcio Z.
Linares, Mauricio
Mallet, James
Reed, Robert D.
Jiggins, Chris D.
Kronforst, Marcus R.
McMillan, W. Owen
TI Wing patterning gene redefines the mimetic history of Heliconius
butterflies
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Mullerian mimicry; population genetics; phylogeography
ID SHIFTING BALANCE; MULLERIAN MIMICRY; RACE FORMATION; EVOLUTION;
STICKLEBACKS; DIVERSITY; INFERENCE; AMERICA; COLOR
AB The mimetic butterflies Heliconius erato and Heliconius melpomene have undergone parallel radiations to form a near-identical patchwork of over 20 different wing-pattern races across the Neotropics. Previous molecular phylogenetic work on these radiations has suggested that similar but geographically disjunct color patterns arose multiple times independently in each species. The neutral markers used in these studies, however, can move freely across color pattern boundaries, and therefore might not represent the history of the adaptive traits as accurately as markers linked to color pattern genes. To assess the evolutionary histories across different loci, we compared relationships among races within H. erato and within H. melpomene using a series of unlinked genes, genes linked to color pattern loci, and optix, a gene recently shown to control red color-pattern variation. We found that although unlinked genes partition populations by geographic region, optix had a different history, structuring lineages by red color patterns and supporting a single origin of red-rayed patterns within each species. Genes closely linked (80-250 kb) to optix exhibited only weak associations with color pattern. This study empirically demonstrates the necessity of examining phenotype-determining genomic regions to understand the history of adaptive change in rapidly radiating lineages. With these refined relationships, we resolve a long-standing debate about the origins of the races within each species, supporting the hypothesis that the red-rayed Amazonian pattern evolved recently and expanded, causing disjunctions of more ancestral patterns.
C1 [Hines, Heather M.; McMillan, W. Owen] N Carolina State Univ, Dept Genet, Raleigh, NC 27695 USA.
[Counterman, Brian A.] Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA.
[Papa, Riccardo] Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA.
[Papa, Riccardo] Univ Puerto Rico, Ctr Appl Trop Ecol & Conservat, Rio Piedras, PR 00931 USA.
[de Moura, Priscila Albuquerque; Cardoso, Marcio Z.] Univ Fed Rio Grande do Norte, Dept Bot Ecol & Zool, BR-59072970 Natal, RN, Brazil.
[Linares, Mauricio] Univ Rosario, Fac Ciencias Nat & Matemat, Bogota, Colombia.
[Mallet, James] UCL, Dept Genet Evolut & Environm, London WC1E 6BT, England.
[Mallet, James] Harvard Univ, Dept Organismal & Evolutionary Biol, Cambridge, MA 02138 USA.
[Kronforst, Marcus R.] Harvard Univ, Ctr Syst Biol, Fac Arts & Sci, Cambridge, MA 02138 USA.
[Reed, Robert D.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA.
[Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England.
[McMillan, W. Owen] Smithsonian Trop Res Inst, Balboa, Panama.
RP Hines, HM (reprint author), N Carolina State Univ, Dept Genet, Box 7614, Raleigh, NC 27695 USA.
EM heather_hines@ncsu.edu
RI Jiggins, Chris/B-9960-2008; Reed, Robert/A-2419-2008; Cardoso,
Marcio/D-4683-2009; mallet, james/B-5114-2008; Linares,
Mauricio/I-3509-2016;
OI Jiggins, Chris/0000-0002-7809-062X; Linares,
Mauricio/0000-0002-1021-0226; Mallet, James/0000-0002-3370-0367
FU Ruth L. Kirschstein National Research Service [F32 GM889942];
Fapern/Conselho Nacional de Pesquisas [PPP/2007]; National Institutes of
Health/National Institute of General Medical Sciences [GM068763];
National Science Foundation Division of Environmental Biology (DEB)
[1020355]; Biotechnology and Biological Sciences Research Council
[G006903]; National Science Foundation [DEB-0844244, DEB-0715096]
FX We thank Stephanie Ruzsa, Vincent Izzi, Nicola Chamberlain, and Felix
Araujo-Perez for assistance with sample preparation and sequencing; Matt
Bertone for graphics assistance; Jeff Thorne for analytical advice; and
the Peruvian Ministerio de Agricultura and Instituto Nacional De
Recursos Naturales (004-2008-INRENA-IFFS-DCB and 011756-AG-INRENA), the
Ecuadorian Ministerio del Ambiente Ecuadorian (013-09 IC-FAU-DNB/MA),
and the Brazilian Ministerio do Meio Ambiente (permit 10894-1) for
collection permits. This work was funded by a Ruth L. Kirschstein
National Research Service Award F32 GM889942 (to H.M.H.),
Fapern/Conselho Nacional de Pesquisas Grant PPP/2007 (to M.Z.C.);
National Institutes of Health/National Institute of General Medical
Sciences Grant GM068763 and National Science Foundation Division of
Environmental Biology (DEB) Grant 1020355 (to M.R.K.); Biotechnology and
Biological Sciences Research Council Grant G006903 (to J.M.); and
National Science Foundation Grants DEB-0844244 and DEB-0715096 (to
R.D.R. and W.O.M.).
NR 38
TC 47
Z9 47
U1 0
U2 38
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 DEC 6
PY 2011
VL 108
IS 49
BP 19666
EP 19671
DI 10.1073/pnas.1110096108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 856ZQ
UT WOS:000297683800051
PM 22084094
ER
PT J
AU Santana, SE
Geipel, I
Dumont, ER
Kalka, MB
Kalko, EKV
AF Santana, Sharlene E.
Geipel, Inga
Dumont, Elizabeth R.
Kalka, Margareta B.
Kalko, Elisabeth K. V.
TI All You Can Eat: High Performance Capacity and Plasticity in the Common
Big-Eared Bat, Micronycteris microtis (Chiroptera: Phyllostomidae)
SO PLOS ONE
LA English
DT Article
ID BITE FORCE; FOOD HARDNESS; PANAMA; DIET; ECHOLOCATION; INSECTIVORY;
ASSEMBLAGE; EVOLUTION; BEHAVIOR; FOREST
AB Ecological specialization and resource partitioning are expected to be particularly high in the species-rich communities of tropical vertebrates, yet many species have broader ecological niches than expected. In Neotropical ecosystems, Neotropical leaf-nosed bats (Phyllostomidae) are one of the most ecologically and functionally diverse vertebrate clades. Resource partitioning in phyllostomids might be achieved through differences in the ability to find and process food. We selected Micronycteris microtis, a very small (5-7 g) animalivorous phyllostomid, to explore whether broad resource use is associated with specific morphological, behavioral and performance traits within the phyllostomid radiation. We documented processing of natural prey and measured bite force in free-ranging M. microtis and other sympatric phyllostomids. We found that M. microtis had a remarkably broad diet for prey size and hardness. For the first time, we also report the consumption of vertebrates (lizards), which makes M. microtis the smallest carnivorous bat reported to date. Compared to other phyllostomids, M. microtis had the highest bite force for its size and cranial shape and high performance plasticity. Bite force and cranial shape appear to have evolved rapidly in the M. microtis lineage. High performance capacity and high efficiency in finding motionless prey might be key traits that allow M. microtis, and perhaps other species, to successfully co-exist with other gleaning bats.
C1 [Santana, Sharlene E.] Univ Calif Los Angeles, Ctr Soc & Genet, Los Angeles, CA 90095 USA.
[Santana, Sharlene E.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA.
[Geipel, Inga; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, Ulm, Germany.
[Dumont, Elizabeth R.] Univ Massachusetts, Dept Biol, Amherst, MA 01003 USA.
[Kalka, Margareta B.] Univ Calif Berkeley, Energy & Resources Grp, Berkeley, CA 94720 USA.
[Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Santana, SE (reprint author), Univ Calif Los Angeles, Ctr Soc & Genet, Los Angeles, CA 90095 USA.
EM sesantana@ucla.edu
FU University of Massachusetts; Institute of Experimental Ecology,
University of Ulm; DAAD; NSF [IOB 0447616]; European Union
FX S.E.S. was supported by University of Massachusetts Graduate School
Fellowship and travel funds from the Institute of Experimental Ecology,
University of Ulm; M.B.K. by a DAAD fellowship; E.R.D. by a NSF grant
(IOB 0447616); and G.G. and E.K.V.K. by the European Union project
ChiRoPing. The funders had no role in study design, data collection and
analysis, decision to publish, or preparation of the manuscript.
NR 43
TC 11
Z9 11
U1 2
U2 21
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD DEC 2
PY 2011
VL 6
IS 12
AR e28584
DI 10.1371/journal.pone.0028584
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 863NO
UT WOS:000298171400110
PM 22164308
ER
PT J
AU Langley, HD
AF Langley, Harold D.
TI A Society of Gentlemen: Midshipmen at the U.S. Naval Academy 1845-1861
SO JOURNAL OF THE EARLY REPUBLIC
LA English
DT Book Review
C1 [Langley, Harold D.] Smithsonian Inst, Washington, DC 20560 USA.
[Langley, Harold D.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Langley, HD (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU UNIV PENNSYLVANIA PRESS
PI PHILADELPHIA
PA JOURNALS DIVISION, 3905 SPRUCE STREET, PHILADELPHIA, PA 19104 USA
SN 0275-1275
J9 J EARLY REPUBL
JI J. Early Repub.
PD WIN
PY 2011
VL 31
IS 4
BP 717
EP 720
PG 4
WC History
SC History
GA 949KN
UT WOS:000304575200012
ER
PT J
AU Langley, HD
AF Langley, Harold D.
TI The Long Road to Annapolis: The Founding of the Naval Academy and the
Emerging American Republic
SO JOURNAL OF THE EARLY REPUBLIC
LA English
DT Book Review
C1 [Langley, Harold D.] Smithsonian Inst, Washington, DC 20560 USA.
[Langley, Harold D.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Langley, HD (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 1
PU UNIV PENNSYLVANIA PRESS
PI PHILADELPHIA
PA JOURNALS DIVISION, 3905 SPRUCE STREET, PHILADELPHIA, PA 19104 USA
SN 0275-1275
J9 J EARLY REPUBL
JI J. Early Repub.
PD WIN
PY 2011
VL 31
IS 4
BP 717
EP 720
PG 4
WC History
SC History
GA 949KN
UT WOS:000304575200011
ER
PT J
AU Becker, MH
Harris, RN
Minbiole, KPC
Schwantes, CR
Rollins-Smith, LA
Reinert, LK
Brucker, RM
Domangue, RJ
Gratwicke, B
AF Becker, Matthew H.
Harris, Reid N.
Minbiole, Kevin P. C.
Schwantes, Christian R.
Rollins-Smith, Louise A.
Reinert, Laura K.
Brucker, Robert M.
Domangue, Rickie J.
Gratwicke, Brian
TI Towards a Better Understanding of the Use of Probiotics for Preventing
Chytridiomycosis in Panamanian Golden Frogs
SO ECOHEALTH
LA English
DT Article
DE Batrachochytrium dendrobatidis; Chytridiomycosis; Atelopus zeteki;
Janthinobacterium lividum; probiotic
ID BATRACHOCHYTRIUM-DENDROBATIDIS; JANTHINOBACTERIUM-LIVIDUM; 4-TOED
SALAMANDERS; CUTANEOUS BACTERIA; FACTORIAL-DESIGNS; SKIN BACTERIA;
RANA-MUSCOSA; POPULATION; EXTINCTIONS; DIVERSITY
AB Populations of native Panamanian golden frogs (Atelopus zeteki) have collapsed due to a recent chytridiomycosis epidemic. Reintroduction efforts from captive assurance colonies are unlikely to be successful without the development of methods to control chytridiomycosis in the wild. In an effort to develop a protective treatment regimen, we treated golden frogs with Janthinobacterium lividum, a skin bacterium that has been used to experimentally prevent chytridiomycosis in North American amphibians. Although J. lividum appeared to colonize A. zeteki skin temporarily, it did not prevent or delay mortality in A. zeteki exposed to Batrachochytrium dendrobatidis, the causative agent of chytridiomycosis. After introduction of J. lividum, average bacterial cell counts reached a peak of 1.7 x 10(6) cells per frog similar to 2 weeks after treatment but declined steadily after that. When J. lividum numbers declined to similar to 2.8 x 10(5) cells per frog, B. dendrobatidis infection intensity increased to greater than 13,000 zoospore equivalents per frog. At this point, frogs began to die of chytridiomycosis. Future research will concentrate on isolating and testing antifungal bacterial species from Panama that may be more compatible with Atelopus skin.
C1 [Becker, Matthew H.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA.
[Harris, Reid N.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA.
[Minbiole, Kevin P. C.; Schwantes, Christian R.] James Madison Univ, Dept Chem & Biochem, Harrisonburg, VA 22807 USA.
[Rollins-Smith, Louise A.; Reinert, Laura K.] Vanderbilt Univ, Med Ctr, Dept Pathol, Nashville, TN 37232 USA.
[Rollins-Smith, Louise A.; Reinert, Laura K.] Vanderbilt Univ, Med Ctr, Dept Microbiol & Immunol, Nashville, TN USA.
[Rollins-Smith, Louise A.; Reinert, Laura K.] Vanderbilt Univ, Med Ctr, Dept Pediat, Nashville, TN 37232 USA.
[Rollins-Smith, Louise A.; Brucker, Robert M.] Vanderbilt Univ, Dept Biol Sci, Nashville, TN USA.
[Domangue, Rickie J.] James Madison Univ, Dept Math & Stat, Harrisonburg, VA 22807 USA.
[Gratwicke, Brian] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA.
RP Becker, MH (reprint author), Virginia Tech, Dept Biol Sci, 2119 Derring Hall, Blacksburg, VA 24061 USA.
EM beckermh@vt.edu
RI Brucker, Robert/F-3052-2013
OI Brucker, Robert/0000-0002-0854-848X
FU Anela Kolohe Foundation; Shared Earth Foundation; U.S. Fish and Wildlife
Service; National Science Foundation [0640373, IOS-0619536,
IOS-0843207]; Thomas F. Jeffress and Kate M. Jeffress Memorial Trust
FX We would like to thank the Houston Zoo and the Maryland Zoo in Baltimore
that own all individuals in the Golden Frog Species Survival Plan for
providing the animals. The Fish and Wildlife Service provided permits to
conduct the experiment and IACUC approval was obtained from the
Smithsonian National Zoological Park and the Maryland Zoo in Baltimore.
We are thankful for the technical assistance provided by J. Becker, C.
Crowe, M. Evans, D. Flaherty, W. Lynch, G. Reynolds, E. Smith, L. Ware,
P. Wiggins, and V. Wine. We are grateful for advice from K. Murphy, V.
Poole, K. Zippel, L. Padilla, and T. Walsh in setting up the experiment.
This research was supported by the Anela Kolohe Foundation (B.G.), the
Shared Earth Foundation (B.G.), the U.S. Fish and Wildlife Service as
part of the Panama Amphibian Rescue and Conservation Project (B.G.), the
National Science Foundation grants numbers 0640373 (R.N.H.), IOS-0619536
(L. R-S.), and IOS-0843207 (L.R-S.), and the Thomas F. Jeffress and Kate
M. Jeffress Memorial Trust (K.P.C.M.).
NR 31
TC 25
Z9 25
U1 6
U2 69
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1612-9202
J9 ECOHEALTH
JI EcoHealth
PD DEC
PY 2011
VL 8
IS 4
BP 501
EP 506
DI 10.1007/s10393-012-0743-0
PG 6
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 947QR
UT WOS:000304445100010
PM 22328095
ER
PT J
AU Tipkantha, W
Pukazhenthi, B
Siriaroonrat, B
Thongphakdee, A
Maikaew, U
Thomas, W
Tongthainan, D
Thaeonoen, J
Kamolnorranath, S
Bush, M
Thongtipsiridech, S
AF Tipkantha, Wanlaya
Pukazhenthi, Budhan
Siriaroonrat, Boripat
Thongphakdee, Ampika
Maikaew, Umaporn
Thomas, Warisara
Tongthainan, Daraka
Thaeonoen, Jessada
Kamolnorranath, Sumate
Bush, Mitchell
Thongtipsiridech, Sitthawee
TI Ejaculate Characteristics of Captive Malayan Tapirs (Tapirus indicus)
SO THAI JOURNAL OF VETERINARY MEDICINE
LA English
DT Article
DE Malayan tapir; Semen collection; Seminal traits
ID RHINOCEROS DICERORHINUS-SUMATRENSIS; SUCCESSFUL ARTIFICIAL-INSEMINATION;
HORSES EQUUS-PRZEWALSKII; GENETIC RESOURCE BANKS; DOMESTIC CAT;
MEDETOMIDINE-BUTORPHANOL; ALKALINE-PHOSPHATASE; CONSERVING WILDLIFE;
STALLION SEMEN; ASIAN ELEPHANT
AB The aims of this study were to optimize semen collection by electoejaculation and characterize ejaculate characteristics in Malayan tapir (Tapirus indicus). Eight adult males (4-20 years of age) were anesthetized using a combination of medetomidine HCl (0.012-0.018 mg/kg), bytorphanol tatrate (0.012-0.018 mg/kg), and ketamine HCl (5-7 mg/kg) administered intramuscularly via a dart and subjected to electroejaculation. Ejaculates (milkey-white to yellowish color) were successfully collected from all males. Averages (Mean +/- SD) of the seminal traits (volume, pH, osmolality, sperm concentration, total sperm motility, and viability) were 10.3 +/- 9.4 ml, 7.4 +/- 3.4, 278 +/- 13.3 mOsm, 206.2 +/- 185.4x10(6) spermatozoa 6.7 +/- 2.6% with 39.2 +/- 8.5% intact acrosomes. This is the first study to evaluate semen characteristics and sperm morphology in the Malayan tapirs. Results provide fundamental information essential for development of assisted reproductive technologies in this species.
C1 [Tipkantha, Wanlaya; Siriaroonrat, Boripat; Thongphakdee, Ampika; Kamolnorranath, Sumate] Zool Pk Org, Bur Conservat Res & Educ, Bangkok 10300, Thailand.
[Pukazhenthi, Budhan; Bush, Mitchell] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
[Maikaew, Umaporn; Tongthainan, Daraka; Thaeonoen, Jessada] Khao Kheow Open Zoo, Sriracha 20110, Chonburi, Thailand.
[Thongtipsiridech, Sitthawee] Fac Vet Med, Nakhon Pathom 73140, Thailand.
[Thomas, Warisara] Nakornratchasrima Zoo, Mueng 30000, Nakornratchsrim, Thailand.
[Tipkantha, Wanlaya; Thongtipsiridech, Sitthawee] Kasetsart Univ, Ctr Agr Biotechnol, Nakhon Pathom 73140, Thailand.
[Thongtipsiridech, Sitthawee] Ctr Excellence Agr Biotechnol AG BIO PERDO CHE, Bangkok 10900, Thailand.
[Bush, Mitchell] Adelaide Zool Gardens, Adelaide, SA 5000, Australia.
RP Tipkantha, W (reprint author), Zool Pk Org, Bur Conservat Res & Educ, Bangkok 10300, Thailand.
EM wanlayav62@gmail.com; fvetnit@ku.ac.th
FU Center for Agricultural Biotechnology and the Center of Excellence on
Agricultural Biotechnology (AG-BIO/PERDO-CHE), Kasetsart University;
National Research Council of Thailand; Zoological Park Organization
under Khao Kheow Open Zoo; Zoological Park Organization under Chiang Mai
Zoo; Zoological Park Organization under Nakhonratchasima Zoo; Zoological
Park Organization under Songkhla Zoo
FX This study was supported by the Center for Agricultural Biotechnology
and the Center of Excellence on Agricultural Biotechnology
(AG-BIO/PERDO-CHE), Kasetsart University and was partially funded by the
National Research Council of Thailand. We gratefully thank the zoo
staffs, keepers, scientists and veterinarians of four zoos under the
Zoological Park Organization (Khao Kheow Open Zoo, Chiang Mai Zoo,
Nakhonratchasima Zoo and Songkhla Zoo) for their kind support in this
study.
NR 68
TC 2
Z9 2
U1 2
U2 11
PU CHULALONGKORN UNIV
PI BANGKOK
PA FAC VETERINARY SCI, HENRI DUNANT RD, BANGKOK, 10330, THAILAND
SN 0125-6491
J9 THAI J VET MED
JI Thai J. Vet. Med.
PD DEC
PY 2011
VL 41
IS 4
BP 499
EP 508
PG 10
WC Veterinary Sciences
SC Veterinary Sciences
GA 902IF
UT WOS:000301031100015
ER
PT J
AU Actis, M
Agnetta, G
Aharonian, F
Akhperjanian, A
Aleksic, J
Aliu, E
Allan, D
Allekotte, I
Antico, F
Antonelli, LA
Antoranz, P
Aravantinos, A
Arlen, T
Arnaldi, H
Artmann, S
Asano, K
Asorey, H
Bahr, J
Bais, A
Baixeras, C
Bajtlik, S
Balis, D
Bamba, A
Barbier, C
Barcelo, M
Barnacka, A
Barnstedt, J
de Almeida, UB
Barrio, JA
Basso, S
Bastieri, D
Bauer, C
Becerra, J
Becherini, Y
Bechtol, K
Becker, J
Beckmann, V
Bednarek, W
Behera, B
Beilicke, M
Belluso, M
Benallou, M
Benbow, W
Berdugo, J
Berger, K
Bernardino, T
Bernlor, K
Biland, A
Billotta, S
Bird, T
Birsin, E
Bissaldi, E
Blake, S
Blanch, O
Bobkov, AA
Bogacz, L
Bogdan, M
Boisson, C
Boix, J
Bolmont, J
Bonanno, G
Bonardi, A
Bonev, T
Borkowski, J
Botner, O
Bottani, A
Bourgeat, M
Boutonnet, C
Bouvier, A
Brau-Nogue, S
Braun, I
Bretz, T
Briggs, MS
Brun, P
Brunetti, L
Buckley, H
Bugaev, V
Buhler, R
Bulik, T
Busetto, G
Buson, S
Byrum, K
Cailles, M
Cameron, R
Canestrari, R
Cantu, S
Carmona, E
Carosi, A
Carr, J
Carton, PH
Casiraghi, M
Castarede, H
Catalano, O
Cavazzani, S
Cazaux, S
Cerruti, B
Cerruti, M
Chadwick, M
Chiang, J
Chikawa, M
Cieslar, M
Ciesielska, M
Cillis, A
Clerc, C
Colin, P
Colome, J
Compin, M
Conconi, P
Connaughton, V
Conrad, J
Contreras, JL
Coppi, P
Corlier, M
Corona, P
Corpace, O
Corti, D
Cortina, J
Costantini, H
Cotter, G
Courty, B
Couturier, S
Covino, S
Croston, J
Cusumano, G
Daniel, MK
Dazzi, F
Deangelis, A
del Pozo, ED
Dal Pino, EMD
de Jager, O
Perez, ID
De La Vega, G
De Lotto, B
de Naurois, M
Wilhelmi, ED
de Souza, V
Decerprit, B
Deil, C
Delagnes, E
Deleglise, G
Delgado, C
Dettlaff, T
Di Paolo, A
Di Pierro, F
Diaz, C
Dick, J
Dickinson, H
Digel, SW
Dimitrov, D
Disset, G
Djannati-Ata, A
Doert, M
Domainko, W
Dorner, D
Doro, M
Dournaux, JL
Dravins, D
Drury, L
Dubois, F
Dubois, R
Dubus, G
Dufour, C
Durand, D
Dyks, J
Dyrda, M
Edy, E
Egberts, K
Eleftheriadis, C
Elles, S
Emmanoulopoulos, D
Enomoto, R
Ernenwein, JP
Errando, M
Etchegoyen, A
Falcone, AD
Farakos, K
Farnier, C
Federici, S
Feinstein, F
Ferenc, D
Fillin-Martino, E
Fink, D
Finley, C
Finley, JP
Firpo, R
Florin, D
Fohr, C
Fokitis, E
Font, L
Fontaine, G
Fontana, A
Forster, A
Fortson, L
Fouque, N
Fransson, C
Fraser, GW
Fresnillo, L
Fruck, C
Fujita, Y
Fukazawa, Y
Funk, S
Gabele, W
Gabici, S
Gadola, A
Galante, N
Gallant, Y
Garcia, B
Lopez, RJG
Garrido, D
Garrido, L
Gascon, D
Gasq, C
Gaug, M
Gaweda, J
Geffroy, N
Ghag, C
Ghedina, A
Ghigo, M
Gianakaki, E
Giarrusso, S
Giavitto, G
Giebels, B
Giro, E
Giubilato, P
Glanzman, T
Glicenstein, JF
Gochna, M
Golev, V
Berisso, MG
Gonzalez, A
Gonzalez, F
Granena, F
Graciani, R
Granot, J
Gredig, R
Green, A
Greenshaw, T
Grimm, O
Grube, J
Grudzinska, M
Grygorczuk, J
Guarino, V
Guglielmi, L
Guilloux, F
Gunji, S
Gyuk, G
Hadasch, D
Haefner, D
Hagiwara, R
Hahn, J
Hallgren, A
Hara, S
Hardcastle, MJ
Hassan, T
Haubold, T
Hauser, M
Hayashida, M
Heller, R
Henri, G
Hermann, G
Herrero, A
Hinton, JA
Hoffmann, D
Hofmann, W
Hofverberg, P
Horns, D
Hrupec, D
Huan, H
Huber, B
Huet, JM
Hughes, G
Hultquist, K
Humensky, TB
Huppert, JF
Ibarra, A
Illa, JM
Ingjald, J
Inoue, S
Inoue, Y
Ioka, K
Jablonski, C
Jacholkowska, A
Janiak, M
Jean, P
Jensen, H
Jogler, T
Jung, I
Kaaret, P
Kabuki, S
Kakuwa, J
Kalkuhl, C
Kankanyan, R
Kapala, M
Karastergiou, A
Karczewski, M
Karkar, S
Karlsson, N
Kasperek, J
Katagiri, H
Katarzynski, K
Kawanaka, N
Kedziora, B
Kendziorra, E
Khelifi, B
Kieda, D
Kifune, T
Kihm, T
Klepser, S
Kluzniak, W
Knapp, J
Knappy, AR
Kneiske, T
Knodlseder, J
Kock, F
Kodani, K
Kohri, K
Kokkotas, K
Komin, N
Konopelko, A
Kosack, K
Kossakowski, R
Kostka, P
Kotula, J
Kowal, G
Koziol, J
Krahenbuhl, T
Krause, J
Krawczynski, H
Krennrich, F
Kretzschmann, A
Kubo, H
Kudryavtsev, VA
Kushida, J
La Barbera, N
La Parola, V
La Rosa, G
Lopez, A
Lamanna, G
Laporte, P
Lavalley, C
Le Flour, T
Le Padellec, A
Lenain, JP
Lessio, L
Lieunard, B
Lindfors, E
Liolios, A
Lohse, T
Lombardi, S
Lopatin, A
Lorenz, E
Lubinski, P
Luz, O
Lyard, E
Maccarone, MC
Maccarone, T
Maier, G
Majumdar, P
Maltezos, S
Malkiewicz, P
Mana, C
Manalaysay, A
Maneva, G
Mangano, A
Manigot, P
Marin, J
Mariotti, M
Markoff, S
Martinez, G
Martinez, M
Mastichiadis, A
Matsumoto, H
Mattiazzo, S
Mazin, D
McComb, TJL
McCubbin, N
McHardy, I
Medina, C
Melkumyan, D
Mendes, A
Mertsch, P
Meucci, M
Michalowski, J
Micolon, P
Mineo, T
Mirabal, N
Mirabel, F
Miranda, JM
Mirzoyan, R
Mizuno, T
Moal, B
Moderski, R
Molinari, E
Monteiro, I
Moralejo, A
Morello, C
Mori, K
Motta, G
Mottez, F
Moulin, E
Mukherjee, R
Munar, P
Muraishi, H
Murase, K
Murphy, AS
Nagataki, S
Naito, T
Nakamori, T
Nakayama, K
Naumann, C
Naumann, D
Nayman, P
Nedbal, D
Niedzwiecki, A
Niemiec, J
Nikolaidis, A
Nishijima, K
Nolan, SJ
Nowak, N
O'Brien, PT
Ochoa, I
Ohira, Y
Ohishi, M
Ohka, H
Okumura, A
Olivetto, C
Ong, RA
Orito, R
Orr, M
Osborne, JP
Ostrowski, M
Otero, L
Otte, AN
Ovcharov, E
Oya, I
Ozieblo, A
Paiano, S
Pallota, J
Panazol, JL
Paneque, D
Panter, M
Paoletti, R
Papyan, G
Paredes, JM
Pareschi, G
Parsons, RD
Arribas, MP
Pedaletti, G
Pepato, A
Persic, M
Petrucci, PO
Peyaud, B
Piechocki, W
Pita, S
Pivato, G
Platos, L
Platzer, R
Pogosyan, L
Pohl, M
Pojmanski, G
Ponz, JD
Potter, W
Prandini, E
Preece, R
Prokoph, H
Puhlhofer, G
Punch, M
Quel, E
Quirrenbach, A
Rajda, P
Rando, R
Rataj, M
Raue, M
Reimann, C
Reimann, O
Reimer, A
Reimer, O
Renaud, M
Renner, S
Reymond, JM
Rhode, W
Ribo, M
Ribordy, M
Rico, J
Rieger, F
Ringegni, P
Ripken, J
Ristori, P
Rivoire, S
Rob, L
Rodriguez, S
Roeser, U
Romano, P
Romero, GE
Rosier-Lees, S
Rovero, AC
Roy, F
Royer, S
Rudak, B
Rulten, CB
Ruppel, J
Russo, F
Ryde, F
Sacco, B
Saggion, A
Sahakian, V
Saito, K
Saito, T
Sakaki, N
Salazar, E
Salini, A
Sanchez, F
Conde, MAS
Santangelo, A
Santos, EM
Sanuy, A
Sapozhnikov, L
Sarkar, S
Scalzotto, V
Scapin, V
Scarcioffolo, M
Schanz, T
Schlenstedt, S
Schlickeiser, R
Schmidt, T
Schmoll, J
Schroedter, M
Schultz, C
Schultze, J
Schulz, A
Schwanke, U
Schwarzburg, S
Schweizer, T
Seiradakis, J
Selmane, S
Seweryn, K
Shayduk, M
Shellard, RC
Shibata, T
Sikora, M
Silk, J
Sillanpaa, A
Sitarek, J
Skole, C
Smith, N
Sobczynska, D
Haro, MS
Sol, H
Spanier, F
Spiga, D
Spyrou, S
Stamatescu, V
Stamerra, A
Starling, RLC
Stawarz, L
Steenkamp, R
Stegmann, C
Steiner, S
Stergioulas, N
Sternberger, R
Stinzing, F
Stodulski, M
Straumann, U
Suarez, A
Suchenek, M
Sugawara, R
Sulanke, KH
Sun, S
Supanitsky, AD
Sutcliffe, P
Szanecki, M
Szepieniec, T
Szostek, A
Szymkowiak, A
Tagliaferri, G
Tajima, H
Takahashi, H
Takahashi, K
Takalo, L
Takami, H
Talbot, RG
Tam, PH
Tanaka, M
Tanimori, T
Tavani, M
Tavernet, JP
Tchernin, C
Tejedor, LA
Telezhinsky, I
Temnikov, P
Tenzer, C
Terada, Y
Terrier, R
Teshima, M
Testa, V
Tibaldo, L
Tibolla, O
Tluczykont, M
Peixoto, CJT
Tokanai, F
Tokarz, M
Toma, K
Torres, DF
Tosti, G
Totani, T
Toussenel, F
Vallania, P
Vallejo, G
van der Walt, J
van Eldik, C
Vandenbroucke, J
Vankov, H
Vasileiadis, G
Vassiliev, VV
Vegas, I
Venter, L
Vercellone, S
Veyssiere, C
Vialle, JP
Videla, M
Vincent, P
Vink, J
Vlahakis, N
Vlahos, L
Vogler, P
Vollhardt, A
Volpe, F
Von Gunten, HP
Vorobiov, S
Wagner, S
Wagner, RM
Wagner, B
Wakely, SP
Walter, P
Walter, R
Warwick, R
Wawer, P
Wawrzaszek, R
Webb, N
Wegner, P
Weinstein, A
Weitzel, Q
Welsing, R
Wetteskind, H
White, R
Wierzcholska, A
Wilkinson, MI
Williams, DA
Winde, M
Wischnewski, R
Wisniewski, L
Wolczko, A
Wood, M
Xiong, Q
Yamamoto, T
Yamaoka, K
Yamazaki, R
Yanagita, S
Yoffo, B
Yonetani, M
Yoshida, A
Yoshida, T
Yoshikoshi, T
Zabalza, V
Zagdanski, A
Zajczyk, A
Zdziarski, A
Zech, A
Zietara, K
Ziolkowski, P
Zitelli, V
Zychowski, P
AF Actis, M.
Agnetta, G.
Aharonian, F.
Akhperjanian, A.
Aleksic, J.
Aliu, E.
Allan, D.
Allekotte, I.
Antico, F.
Antonelli, L. A.
Antoranz, P.
Aravantinos, A.
Arlen, T.
Arnaldi, H.
Artmann, S.
Asano, K.
Asorey, H.
Baehr, J.
Bais, A.
Baixeras, C.
Bajtlik, S.
Balis, D.
Bamba, A.
Barbier, C.
Barcelo, M.
Barnacka, A.
Barnstedt, J.
de Almeida, U. Barres
Barrio, J. A.
Basso, S.
Bastieri, D.
Bauer, C.
Becerra, J.
Becherini, Y.
Bechtol, K.
Becker, J.
Beckmann, V.
Bednarek, W.
Behera, B.
Beilicke, M.
Belluso, M.
Benallou, M.
Benbow, W.
Berdugo, J.
Berger, K.
Bernardino, T.
Bernloehr, K.
Biland, A.
Billotta, S.
Bird, T.
Birsin, E.
Bissaldi, E.
Blake, S.
Blanch, O.
Bobkov, A. A.
Bogacz, L.
Bogdan, M.
Boisson, C.
Boix, J.
Bolmont, J.
Bonanno, G.
Bonardi, A.
Bonev, T.
Borkowski, J.
Botner, O.
Bottani, A.
Bourgeat, M.
Boutonnet, C.
Bouvier, A.
Brau-Nogue, S.
Braun, I.
Bretz, T.
Briggs, M. S.
Brun, P.
Brunetti, L.
Buckley, H.
Bugaev, V.
Buehler, R.
Bulik, T.
Busetto, G.
Buson, S.
Byrum, K.
Cailles, M.
Cameron, R.
Canestrari, R.
Cantu, S.
Carmona, E.
Carosi, A.
Carr, J.
Carton, P. H.
Casiraghi, M.
Castarede, H.
Catalano, O.
Cavazzani, S.
Cazaux, S.
Cerruti, B.
Cerruti, M.
Chadwick, M.
Chiang, J.
Chikawa, M.
Cieslar, M.
Ciesielska, M.
Cillis, A.
Clerc, C.
Colin, P.
Colome, J.
Compin, M.
Conconi, P.
Connaughton, V.
Conrad, J.
Contreras, J. L.
Coppi, P.
Corlier, M.
Corona, P.
Corpace, O.
Corti, D.
Cortina, J.
Costantini, H.
Cotter, G.
Courty, B.
Couturier, S.
Covino, S.
Croston, J.
Cusumano, G.
Daniel, M. K.
Dazzi, F.
Deangelis, A.
de Cea del Pozo, E.
Dal Pino, E. M. de Gouveia
de Jager, O.
de la Calle Perez, I.
De La Vega, G.
De Lotto, B.
de Naurois, M.
Wilhelmi, E. de Ona
de Souza, V.
Decerprit, B.
Deil, C.
Delagnes, E.
Deleglise, G.
Delgado, C.
Dettlaff, T.
Di Paolo, A.
Di Pierro, F.
Diaz, C.
Dick, J.
Dickinson, H.
Digel, S. W.
Dimitrov, D.
Disset, G.
Djannati-Ata, A.
Doert, M.
Domainko, W.
Dorner, D.
Doro, M.
Dournaux, J. -L.
Dravins, D.
Drury, L.
Dubois, F.
Dubois, R.
Dubus, G.
Dufour, C.
Durand, D.
Dyks, J.
Dyrda, M.
Edy, E.
Egberts, K.
Eleftheriadis, C.
Elles, S.
Emmanoulopoulos, D.
Enomoto, R.
Ernenwein, J. -P.
Errando, M.
Etchegoyen, A.
Falcone, A. D.
Farakos, K.
Farnier, C.
Federici, S.
Feinstein, F.
Ferenc, D.
Fillin-Martino, E.
Fink, D.
Finley, C.
Finley, J. P.
Firpo, R.
Florin, D.
Foehr, C.
Fokitis, E.
Font, Ll.
Fontaine, G.
Fontana, A.
Foerster, A.
Fortson, L.
Fouque, N.
Fransson, C.
Fraser, G. W.
Fresnillo, L.
Fruck, C.
Fujita, Y.
Fukazawa, Y.
Funk, S.
Gaebele, W.
Gabici, S.
Gadola, A.
Galante, N.
Gallant, Y.
Garcia, B.
Garcia Lopez, R. J.
Garrido, D.
Garrido, L.
Gascon, D.
Gasq, C.
Gaug, M.
Gaweda, J.
Geffroy, N.
Ghag, C.
Ghedina, A.
Ghigo, M.
Gianakaki, E.
Giarrusso, S.
Giavitto, G.
Giebels, B.
Giro, E.
Giubilato, P.
Glanzman, T.
Glicenstein, J. -F.
Gochna, M.
Golev, V.
Gomez Berisso, M.
Gonzalez, A.
Gonzalez, F.
Granena, F.
Graciani, R.
Granot, J.
Gredig, R.
Green, A.
Greenshaw, T.
Grimm, O.
Grube, J.
Grudzinska, M.
Grygorczuk, J.
Guarino, V.
Guglielmi, L.
Guilloux, F.
Gunji, S.
Gyuk, G.
Hadasch, D.
Haefner, D.
Hagiwara, R.
Hahn, J.
Hallgren, A.
Hara, S.
Hardcastle, M. J.
Hassan, T.
Haubold, T.
Hauser, M.
Hayashida, M.
Heller, R.
Henri, G.
Hermann, G.
Herrero, A.
Hinton, J. A.
Hoffmann, D.
Hofmann, W.
Hofverberg, P.
Horns, D.
Hrupec, D.
Huan, H.
Huber, B.
Huet, J. -M.
Hughes, G.
Hultquist, K.
Humensky, T. B.
Huppert, J. -F.
Ibarra, A.
Illa, J. M.
Ingjald, J.
Inoue, S.
Inoue, Y.
Ioka, K.
Jablonski, C.
Jacholkowska, A.
Janiak, M.
Jean, P.
Jensen, H.
Jogler, T.
Jung, I.
Kaaret, P.
Kabuki, S.
Kakuwa, J.
Kalkuhl, C.
Kankanyan, R.
Kapala, M.
Karastergiou, A.
Karczewski, M.
Karkar, S.
Karlsson, N.
Kasperek, J.
Katagiri, H.
Katarzynski, K.
Kawanaka, N.
Kedziora, B.
Kendziorra, E.
Khelifi, B.
Kieda, D.
Kifune, T.
Kihm, T.
Klepser, S.
Kluzniak, W.
Knapp, J.
Knappy, A. R.
Kneiske, T.
Knoedlseder, J.
Koeck, F.
Kodani, K.
Kohri, K.
Kokkotas, K.
Komin, N.
Konopelko, A.
Kosack, K.
Kossakowski, R.
Kostka, P.
Kotula, J.
Kowal, G.
Koziol, J.
Kraehenbuehl, T.
Krause, J.
Krawczynski, H.
Krennrich, F.
Kretzschmann, A.
Kubo, H.
Kudryavtsev, V. A.
Kushida, J.
La Barbera, N.
La Parola, V.
La Rosa, G.
Lopez, A.
Lamanna, G.
Laporte, P.
Lavalley, C.
Le Flour, T.
Le Padellec, A.
Lenain, J. -P.
Lessio, L.
Lieunard, B.
Lindfors, E.
Liolios, A.
Lohse, T.
Lombardi, S.
Lopatin, A.
Lorenz, E.
Lubinski, P.
Luz, O.
Lyard, E.
Maccarone, M. C.
Maccarone, T.
Maier, G.
Majumdar, P.
Maltezos, S.
Malkiewicz, P.
Mana, C.
Manalaysay, A.
Maneva, G.
Mangano, A.
Manigot, P.
Marin, J.
Mariotti, M.
Markoff, S.
Martinez, G.
Martinez, M.
Mastichiadis, A.
Matsumoto, H.
Mattiazzo, S.
Mazin, D.
McComb, T. J. L.
McCubbin, N.
McHardy, I.
Medina, C.
Melkumyan, D.
Mendes, A.
Mertsch, P.
Meucci, M.
Michalowski, J.
Micolon, P.
Mineo, T.
Mirabal, N.
Mirabel, F.
Miranda, J. M.
Mirzoyan, R.
Mizuno, T.
Moal, B.
Moderski, R.
Molinari, E.
Monteiro, I.
Moralejo, A.
Morello, C.
Mori, K.
Motta, G.
Mottez, F.
Moulin, E.
Mukherjee, R.
Munar, P.
Muraishi, H.
Murase, K.
Murphy, A. Stj.
Nagataki, S.
Naito, T.
Nakamori, T.
Nakayama, K.
Naumann, C.
Naumann, D.
Nayman, P.
Nedbal, D.
Niedzwiecki, A.
Niemiec, J.
Nikolaidis, A.
Nishijima, K.
Nolan, S. J.
Nowak, N.
O'Brien, P. T.
Ochoa, I.
Ohira, Y.
Ohishi, M.
Ohka, H.
Okumura, A.
Olivetto, C.
Ong, R. A.
Orito, R.
Orr, M.
Osborne, J. P.
Ostrowski, M.
Otero, L.
Otte, A. N.
Ovcharov, E.
Oya, I.
Ozieblo, A.
Paiano, S.
Pallota, J.
Panazol, J. L.
Paneque, D.
Panter, M.
Paoletti, R.
Papyan, G.
Paredes, J. M.
Pareschi, G.
Parsons, R. D.
Arribas, M. Paz
Pedaletti, G.
Pepato, A.
Persic, M.
Petrucci, P. O.
Peyaud, B.
Piechocki, W.
Pita, S.
Pivato, G.
Platos, L.
Platzer, R.
Pogosyan, L.
Pohl, M.
Pojmanski, G.
Ponz, J. D.
Potter, W.
Prandini, E.
Preece, R.
Prokoph, H.
Puehlhofer, G.
Punch, M.
Quel, E.
Quirrenbach, A.
Rajda, P.
Rando, R.
Rataj, M.
Raue, M.
Reimann, C.
Reimann, O.
Reimer, A.
Reimer, O.
Renaud, M.
Renner, S.
Reymond, J. -M.
Rhode, W.
Ribo, M.
Ribordy, M.
Rico, J.
Rieger, F.
Ringegni, P.
Ripken, J.
Ristori, P.
Rivoire, S.
Rob, L.
Rodriguez, S.
Roeser, U.
Romano, P.
Romero, G. E.
Rosier-Lees, S.
Rovero, A. C.
Roy, F.
Royer, S.
Rudak, B.
Rulten, C. B.
Ruppel, J.
Russo, F.
Ryde, F.
Sacco, B.
Saggion, A.
Sahakian, V.
Saito, K.
Saito, T.
Sakaki, N.
Salazar, E.
Salini, A.
Sanchez, F.
Sanchez Conde, M. A.
Santangelo, A.
Santos, E. M.
Sanuy, A.
Sapozhnikov, L.
Sarkar, S.
Scalzotto, V.
Scapin, V.
Scarcioffolo, M.
Schanz, T.
Schlenstedt, S.
Schlickeiser, R.
Schmidt, T.
Schmoll, J.
Schroedter, M.
Schultz, C.
Schultze, J.
Schulz, A.
Schwanke, U.
Schwarzburg, S.
Schweizer, T.
Seiradakis, J.
Selmane, S.
Seweryn, K.
Shayduk, M.
Shellard, R. C.
Shibata, T.
Sikora, M.
Silk, J.
Sillanpaa, A.
Sitarek, J.
Skole, C.
Smith, N.
Sobczynska, D.
Sofo Haro, M.
Sol, H.
Spanier, F.
Spiga, D.
Spyrou, S.
Stamatescu, V.
Stamerra, A.
Starling, R. L. C.
Stawarz, L.
Steenkamp, R.
Stegmann, C.
Steiner, S.
Stergioulas, N.
Sternberger, R.
Stinzing, F.
Stodulski, M.
Straumann, U.
Suarez, A.
Suchenek, M.
Sugawara, R.
Sulanke, K. H.
Sun, S.
Supanitsky, A. D.
Sutcliffe, P.
Szanecki, M.
Szepieniec, T.
Szostek, A.
Szymkowiak, A.
Tagliaferri, G.
Tajima, H.
Takahashi, H.
Takahashi, K.
Takalo, L.
Takami, H.
Talbot, R. G.
Tam, P. H.
Tanaka, M.
Tanimori, T.
Tavani, M.
Tavernet, J. -P.
Tchernin, C.
Tejedor, L. A.
Telezhinsky, I.
Temnikov, P.
Tenzer, C.
Terada, Y.
Terrier, R.
Teshima, M.
Testa, V.
Tibaldo, L.
Tibolla, O.
Tluczykont, M.
Peixoto, C. J. Todero
Tokanai, F.
Tokarz, M.
Toma, K.
Torres, D. F.
Tosti, G.
Totani, T.
Toussenel, F.
Vallania, P.
Vallejo, G.
van der Walt, J.
van Eldik, C.
Vandenbroucke, J.
Vankov, H.
Vasileiadis, G.
Vassiliev, V. V.
Vegas, I.
Venter, L.
Vercellone, S.
Veyssiere, C.
Vialle, J. P.
Videla, M.
Vincent, P.
Vink, J.
Vlahakis, N.
Vlahos, L.
Vogler, P.
Vollhardt, A.
Volpe, F.
Von Gunten, H. P.
Vorobiov, S.
Wagner, S.
Wagner, R. M.
Wagner, B.
Wakely, S. P.
Walter, P.
Walter, R.
Warwick, R.
Wawer, P.
Wawrzaszek, R.
Webb, N.
Wegner, P.
Weinstein, A.
Weitzel, Q.
Welsing, R.
Wetteskind, H.
White, R.
Wierzcholska, A.
Wilkinson, M. I.
Williams, D. A.
Winde, M.
Wischnewski, R.
Wisniewski, L.
Wolczko, A.
Wood, M.
Xiong, Q.
Yamamoto, T.
Yamaoka, K.
Yamazaki, R.
Yanagita, S.
Yoffo, B.
Yonetani, M.
Yoshida, A.
Yoshida, T.
Yoshikoshi, T.
Zabalza, V.
Zagdanski, A.
Zajczyk, A.
Zdziarski, A.
Zech, A.
Zietara, K.
Ziolkowski, P.
Zitelli, V.
Zychowski, P.
CA CTA Consortium
TI Design concepts for the Cherenkov Telescope Array CTA: an advanced
facility for ground-based high-energy gamma-ray astronomy
SO EXPERIMENTAL ASTRONOMY
LA English
DT Article
DE Ground based gamma ray astronomy; Next generation Cherenkov telescopes;
Design concepts
ID INDUCED AIR-SHOWERS; MAGIC TELESCOPE; COSMIC-RAYS; OPTICAL-SYSTEM; 1ST
DETECTION; RADIATION; TEV; BURSTS; SIMULATION; PARTICLES
AB Ground-based gamma-ray astronomy has had a major breakthrough with the impressive results obtained using systems of imaging atmospheric Cherenkov telescopes. Ground-based gamma-ray astronomy has a huge potential in astrophysics, particle physics and cosmology. CTA is an international initiative to build the next generation instrument, with a factor of 5-10 improvement in sensitivity in the 100 GeV-10 TeV range and the extension to energies well below 100 GeV and above 100 TeV. CTA will consist of two arrays (one in the north, one in the south) for full sky coverage and will be operated as open observatory. The design of CTA is based on currently available technology. This document reports on the status and presents the major design concepts of CTA.
C1 [Hofmann, W.] Heidelberg Univ, CTA Project Off, D-69117 Heidelberg, Germany.
[Allekotte, I.; Arnaldi, H.; Asorey, H.; Gomez Berisso, M.; Sofo Haro, M.] Ctr Atom Bariloche CNEA CONICET IB UNCuyo, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina.
[Cillis, A.; Rovero, A. C.; Supanitsky, A. D.] Inst Astron & Fis Espacio CONICET UBA, Buenos Aires, DF, Argentina.
[Actis, M.; Antico, F.; Bottani, A.; Ochoa, I.; Ringegni, P.; Vallejo, G.] UNLP, Fac Ingn, Dept Aeronaut, UID GEMA, RA-1900 La Plata, Buenos Aires, Argentina.
[De La Vega, G.; Etchegoyen, A.; Garcia, B.; Sanchez, F.; Videla, M.] Inst Tecnol Detecc & Astroparticulas CNEA CONICET, RA-1650 Buenos Aires, DF, Argentina.
[De La Vega, G.; Etchegoyen, A.; Garcia, B.; Sanchez, F.; Videla, M.] Observ Metereol, Mendoza, Argentina.
[Gonzalez, F.; Otero, L.; Pallota, J.; Quel, E.; Ristori, P.] CEILAP CITEDEF CONICET, Villa Martelli, Argentina.
[Romero, G. E.; Suarez, A.] Univ Nacl La Plata, CONICET, CCT La Plata, Inst Argentino Radioastron, RA-1900 La Plata, Buenos Aires, Argentina.
[Romero, G. E.; Suarez, A.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, RA-1900 La Plata, Buenos Aires, Argentina.
[Akhperjanian, A.; Papyan, G.; Pogosyan, L.; Sahakian, V.] Alikhanyan Natl Sci Lab, Yerevan 0036, Armenia.
[Bissaldi, E.; Egberts, K.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Shellard, R. C.] Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, RJ, Brazil.
[Santos, E. M.] Univ Fed Rio de Janeiro, Inst Fis, BR-21941972 Rio De Janeiro, RJ, Brazil.
[Dal Pino, E. M. de Gouveia; Kowal, G.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, Brazil.
[de Souza, V.; Peixoto, C. J. Todero] Univ Sao Paulo, Inst Fis Sao Carlos, BR-13566590 Sao Carlos, SP, Brazil.
[Maneva, G.; Temnikov, P.; Vankov, H.] BAS, Inst Nucl Res & Nucl Energy, BG-1784 Sofia, Bulgaria.
[Golev, V.; Ovcharov, E.] Univ Sofia, Astron Dept, BG-1164 Sofia, Bulgaria.
[Bonev, T.; Dimitrov, D.] Inst Astron, BG-1784 Sofia, Bulgaria.
[Bonev, T.; Dimitrov, D.] NAO, BG-1784 Sofia, Bulgaria.
[Hrupec, D.] Rudjer Boskovic Inst, HR-10000 Zagreb, Croatia.
[Nedbal, D.; Rob, L.] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague 8, Czech Republic.
[Lindfors, E.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland.
[Beckmann, V.; Benallou, M.; Boutonnet, C.; Corlier, M.; Courty, B.; Djannati-Ata, A.; Dufour, C.; Gabici, S.; Guglielmi, L.; Olivetto, C.; Pita, S.; Punch, M.; Selmane, S.; Terrier, R.; Yoffo, B.] APC, F-75205 Paris 13, France.
[Beckmann, V.; Benallou, M.; Boutonnet, C.; Corlier, M.; Courty, B.; Djannati-Ata, A.; Dufour, C.; Gabici, S.; Guglielmi, L.; Olivetto, C.; Pita, S.; Punch, M.; Selmane, S.; Terrier, R.; Yoffo, B.] Univ Paris 07, CEA, Observ Paris, CNRS,UMR 7164, F-75221 Paris 05, France.
[Brun, P.; Carton, P. H.; Cazaux, S.; Corpace, O.; Delagnes, E.; Disset, G.; Durand, D.; Glicenstein, J. -F.; Guilloux, F.; Kosack, K.; Medina, C.; Micolon, P.; Mirabel, F.; Moulin, E.; Peyaud, B.; Reymond, J. -M.; Veyssiere, C.] CEA Saclay, CEA DSM IRFU, F-91191 Gif Sur Yvette, France.
[Brau-Nogue, S.; Jean, P.; Knoedlseder, J.; Le Padellec, A.; Webb, N.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Brau-Nogue, S.; Jean, P.; Knoedlseder, J.; Le Padellec, A.; Webb, N.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Cerruti, B.; Dubus, G.; Henri, G.; Petrucci, P. O.] UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France.
[Akhperjanian, A.; Aravantinos, A.; Bais, A.; Bamba, A.; Barbier, C.; Brunetti, L.; Cailles, M.; Deleglise, G.; Elles, S.; Fouque, N.; Gasq, C.; Geffroy, N.; Komin, N.; Kossakowski, R.; Lamanna, G.; Le Flour, T.; Lieunard, B.; Monteiro, I.; Panazol, J. L.; Rosier-Lees, S.; Vialle, J. P.] Univ Savoie, CNRS IN2P3, Lab Annecy le Vieux Phys Particules, F-74941 Annecy Le Vieux, France.
[Becherini, Y.; Clerc, C.; Couturier, S.; de Naurois, M.; Edy, E.; Fillin-Martino, E.; Fontaine, G.; Giebels, B.; Khelifi, B.; Manigot, P.; Moal, B.; Spyrou, S.] Ecole Polytech, LLR, F-91128 Palaiseau, France.
[Becherini, Y.; Clerc, C.; Couturier, S.; de Naurois, M.; Edy, E.; Fillin-Martino, E.; Fontaine, G.; Giebels, B.; Khelifi, B.; Manigot, P.; Moal, B.; Spyrou, S.] Ecole Polytech, CNRS, UMR 7638, F-91128 Palaiseau, France.
[Bourgeat, M.; Compin, M.; Feinstein, F.; Gallant, Y.; Lavalley, C.; Renaud, M.; Rivoire, S.; Royer, S.; Vasileiadis, G.; Vorobiov, S.] Univ Montpellier 2, CNRS IN2P3, Lab Universe & Particules Montpellier, F-34095 Montpellier 5, France.
[Boisson, C.; Cerruti, M.; Mottez, F.; Roy, F.; Sol, H.; Venter, L.; Zech, A.] Univ Paris Diderot, CNRS, LUTH, Observ Paris, F-92195 Meudon, France.
[Dournaux, J. -L.; Huet, J. -M.; Laporte, P.] Univ Paris Diderot, CNRS, GEPI, Observ Paris, F-92195 Meudon, France.
[Castarede, H.] Univ Paris Diderot, CNRS, UMS, Observ Paris, F-92195 Meudon, France.
[Bolmont, J.; Corona, P.; Huppert, J. -F.; Jacholkowska, A.; Naumann, C.; Nayman, P.; Tavernet, J. -P.; Toussenel, F.; Vincent, P.] Univ Paris 07, Univ Paris 06, LPNHE, F-75252 Paris 5, France.
[Carr, J.; Costantini, H.; Ernenwein, J. -P.; Hoffmann, D.; Karkar, S.; Mendes, A.] Aix Marseille Univ, CNRS IN2P3, CPPM, Aix En Provence, France.
[Artmann, S.; Becker, J.; Schlickeiser, R.] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany.
[Federici, S.; Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Baehr, J.; Behera, B.; Birsin, E.; Decerprit, B.; Federici, S.; Heller, R.; Hughes, G.; Kostka, P.; Kretzschmann, A.; Maier, G.; Melkumyan, D.; Naumann, D.; Arribas, M. Paz; Platzer, R.; Pohl, M.; Prokoph, H.; Ruppel, J.; Schlenstedt, S.; Schmidt, T.; Schultze, J.; Shayduk, M.; Skole, C.; Sternberger, R.; Sulanke, K. H.; Telezhinsky, I.; Wegner, P.; Welsing, R.; Winde, M.; Wischnewski, R.] DESY, D-15738 Zeuthen, Germany.
[Birsin, E.; Lohse, T.; Oya, I.; Schwanke, U.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Doert, M.] TU Dortmund Univ, Dept Phys, D-44227 Dortmund, Germany.
[Jung, I.; Lopatin, A.; Schulz, A.; Stegmann, C.; Stinzing, F.] Univ Erlangen Nurnberg, Phys Inst, D-91058 Erlangen, Germany.
[Horns, D.; Kneiske, T.; Raue, M.; Tluczykont, M.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany.
[Bauer, C.; Bernloehr, K.; Wilhelmi, E. de Ona; Deil, C.; Domainko, W.; Foehr, C.; Foerster, A.; Hahn, J.; Hermann, G.; Hofmann, W.; Hofverberg, P.; Kankanyan, R.; Kihm, T.; Koeck, F.; Panter, M.; Rieger, F.; van Eldik, C.; Volpe, F.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[de Almeida, U. Barres; Colin, P.; Dettlaff, T.; Fink, D.; Fruck, C.; Haefner, D.; Haubold, T.; Jablonski, C.; Jogler, T.; Krause, J.; Lorenz, E.; Mirzoyan, R.; Nowak, N.; Paneque, D.; Reimann, O.; Rodriguez, S.; Saito, K.; Saito, T.; Schweizer, T.; Sun, S.; Takami, H.; Teshima, M.; Wagner, R. M.; Wetteskind, H.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Barnstedt, J.; Bonardi, A.; Dick, J.; Gaebele, W.; Kalkuhl, C.; Kendziorra, E.; Luz, O.; Puehlhofer, G.; Renner, S.; Santangelo, A.; Schanz, T.; Schwarzburg, S.; Tenzer, C.; Vlahakis, N.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany.
[Spanier, F.; Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Bais, A.; Balis, D.; Eleftheriadis, C.; Gianakaki, E.; Kokkotas, K.; Liolios, A.; Nikolaidis, A.; Seiradakis, J.; Stergioulas, N.; Vlahos, L.] Aristotle Univ Thessaloniki, Phys Dept, GR-54124 Thessaloniki, Greece.
[Mastichiadis, A.] Univ Athens, Fac Phys, Dept Astrophys Astron & Mech, GR-15784 Athens, Greece.
[Aravantinos, A.; Farakos, K.; Fokitis, E.; Maltezos, S.] Natl Tech Univ Athens, Dept Phys, Sch Appl Math & Phys Sci, GR-15780 Zografou Attikis, Greece.
[Aharonian, F.; Drury, L.] Dublin Inst Adv Studies, Dublin 2, Ireland.
[Agnetta, G.; Catalano, O.; Cusumano, G.; Giarrusso, S.; La Barbera, N.; La Parola, V.; La Rosa, G.; Maccarone, M. C.; Mangano, A.; Mineo, T.; Romano, P.; Russo, F.; Sacco, B.; Vercellone, S.] INAF Ist Astrofis Spaziale & Fis Cosm Palermo, I-90146 Palermo, Italy.
[Di Pierro, F.; Morello, C.; Vallania, P.] INAF Ist Fis Spazio Interplanetario Torino, I-10133 Turin, Italy.
[Cavazzani, S.; Zitelli, V.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Basso, S.; Canestrari, R.; Cantu, S.; Casiraghi, M.; Conconi, P.; Covino, S.; Ghigo, M.; Motta, G.; Pareschi, G.; Salini, A.; Spiga, D.; Tagliaferri, G.] INAF Osservatorio Astron Brera, I-20121 Milan, Italy.
[Belluso, M.; Billotta, S.; Bonanno, G.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Giro, E.; Lessio, L.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy.
[Antonelli, L. A.; Carosi, A.; Di Paolo, A.; Fontana, A.; Testa, V.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy.
[Tavani, M.] INAF Ist Astrofis Spaziale & Fis Cosm Roma, I-00133 Rome, Italy.
[Ghedina, A.; Molinari, E.; Tosti, G.] Roque de Los Muchachos Astron Observ, INAF Telescopio Nazl Galileo, Garafia 38787, TF, Spain.
[Bastieri, D.; Busetto, G.; Buson, S.; Corti, D.; Doro, M.; Giubilato, P.; Lombardi, S.; Mariotti, M.; Mattiazzo, S.; Paiano, S.; Pepato, A.; Pivato, G.; Prandini, E.; Rando, R.; Saggion, A.; Scalzotto, V.; Scarcioffolo, M.; Schultz, C.; Tibaldo, L.] Univ Padua, I-35131 Padua, Italy.
[Bastieri, D.; Busetto, G.; Buson, S.; Corti, D.; Doro, M.; Giubilato, P.; Lombardi, S.; Mariotti, M.; Mattiazzo, S.; Paiano, S.; Pepato, A.; Pivato, G.; Prandini, E.; Rando, R.; Saggion, A.; Scalzotto, V.; Scarcioffolo, M.; Schultz, C.; Tibaldo, L.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Meucci, M.; Paoletti, R.; Stamerra, A.] Univ Siena, I-53100 Siena, Italy.
[Meucci, M.; Paoletti, R.; Stamerra, A.] INFN Pisa, I-53100 Siena, Italy.
[Dazzi, F.; Deangelis, A.; De Lotto, B.; Scapin, V.] Univ Udine, I-33100 Udine, Italy.
[Deangelis, A.; De Lotto, B.; Persic, M.; Scapin, V.] INFN Sez Trieste, I-33100 Udine, Italy.
[Dazzi, F.] INFN Sez Padova, I-33100 Udine, Italy.
[Persic, M.] Osserv Astron Trieste, I-33100 Udine, Italy.
[Bamba, A.; Sakaki, N.; Shibata, T.; Yamaoka, K.; Yamazaki, R.; Yoshida, A.] Aoyama Gakuin Univ, Dept Phys & Math, Sagamihara, Kanagawa 2525258, Japan.
[Fukazawa, Y.; Kakuwa, J.; Mizuno, T.; Yonetani, M.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan.
[Katagiri, H.; Yanagita, S.; Yoshida, T.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Okumura, A.; Rhode, W.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Ioka, K.; Kawanaka, N.; Kohri, K.; Nakayama, K.; Ohira, Y.; Tanaka, M.] KEK High Energy Accelerator Res Org, Inst Particle & Nucl Studies, Tsukuba, Ibaraki 3050801, Japan.
[Chikawa, M.] Kinki Univ, Dept Phys, Higashiosaka, Osaka 5778502, Japan.
[Muraishi, H.] Kitasato Univ, Sch Allied Hlth Sci, Kanagawa 2288555, Japan.
[Yamamoto, T.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan.
[Hayashida, M.; Inoue, Y.; Totani, T.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Kubo, H.; Tanimori, T.] Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Nagataki, S.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Mori, K.] Miyazaki Univ, Dept Appl Phys, Fac Engn, Miyazaki 8892192, Japan.
[Takahashi, K.] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Matsumoto, H.] Nagoya Univ, KMI Origin Particles & Universe, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Fujita, Y.; Toma, K.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Terada, Y.] Saitama Univ, Sch Sci & Engn, Sakura Ku, Saitama 3388570, Japan.
[Kodani, K.; Kushida, J.; Nishijima, K.] Tokai Univ, Dept Phys, Hiratsuka, Kanagawa 2591292, Japan.
[Kabuki, S.] Tokai Univ Hosp, Isehara, Kanagawa 2591193, Japan.
[Orito, R.; Sugawara, R.] Univ Tokushima, Inst Socio Arts & Sci, Tokushima 7708502, Japan.
[Asano, K.] Tokyo Inst Technol, Grad Sch Sci, Interact Res Ctr Sci, Meguro Ku, Tokyo 1528550, Japan.
[Enomoto, R.; Inoue, S.; Kifune, T.; Murase, K.; Ohishi, M.; Ohka, H.; Teshima, M.; Yoshikoshi, T.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Nakamori, T.] Waseda Univ, Fac Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Gunji, S.; Hagiwara, R.; Tokanai, F.] Yamagata Univ, Yamagata 9908560, Japan.
[Hara, S.; Naito, T.] Yamanashi Gakuin Univ, Fac Management Informat, Kofu, Yamanashi 4008575, Japan.
[Steenkamp, R.] Univ Namibia, Dept Phys, Windhoek, Namibia.
[Vink, J.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands.
[Markoff, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Bednarek, W.; Niedzwiecki, A.; Sitarek, J.; Sobczynska, D.; Szanecki, M.] Univ Lodz, Fac Phys & Appl Comp Sci, PL-90236 Lodz, Poland.
[Bogacz, L.; Koziol, J.; Malkiewicz, P.; Ostrowski, M.; Piechocki, W.; Stawarz, L.; Szostek, A.; Wierzcholska, A.; Zagdanski, A.; Zietara, K.] Jagiellonian Univ, PL-30244 Krakow, Poland.
[Bulik, T.; Cieslar, M.; Gochna, M.; Grudzinska, M.; Kapala, M.; Pojmanski, G.; Suchenek, M.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland.
[Bajtlik, S.; Barnacka, A.; Borkowski, J.; Dyks, J.; Janiak, M.; Kluzniak, W.; Lubinski, P.; Moderski, R.; Rudak, B.; Sikora, M.; Zajczyk, A.; Zdziarski, A.] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Dyrda, M.; Kotula, J.; Michalowski, J.; Niemiec, J.; Stodulski, M.; Ziolkowski, P.; Zychowski, P.] Polish Acad Sci, Inst Nucl Phys, PL-31342 Krakow, Poland.
[Katarzynski, K.] Nicolaus Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland.
[Ciesielska, M.; Grygorczuk, J.; Karczewski, M.; Kedziora, B.; Platos, L.; Rataj, M.; Seweryn, K.; Tokarz, M.; Wawer, P.; Wawrzaszek, R.; Wisniewski, L.] Polish Acad Sci, Space Res Ctr, PL-00716 Warsaw, Poland.
[Kasperek, J.; Rajda, P.; Wolczko, A.] AGH Univ Sci & Technol, Fac Elect Engn Automat Comp Sci & Elect, PL-30059 Krakow, Poland.
[Ozieblo, A.; Szepieniec, T.] Acad Comp Ctr CYFRONET AGH, PL-30950 Krakow, Poland.
[de Jager, O.; van der Walt, J.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa.
[Becerra, J.; Berger, K.; Garcia Lopez, R. J.; Herrero, A.; Sanchez Conde, M. A.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Becerra, J.; Berger, K.; Garcia Lopez, R. J.; Herrero, A.; Sanchez Conde, M. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Berdugo, J.; Carmona, E.; Delgado, C.; Diaz, C.; Gonzalez, A.; Mana, C.; Marin, J.; Martinez, G.] CIEMAT, E-28040 Madrid, Spain.
[Colome, J.; de Cea del Pozo, E.; Hadasch, D.; Pedaletti, G.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Rico, J.; Torres, D. F.] ICREA, Barcelona, Spain.
[Aleksic, J.; Barcelo, M.; Blanch, O.; Boix, J.; Cortina, J.; Firpo, R.; Gaweda, J.; Giavitto, G.; Gonzalez, A.; Granena, F.; Illa, J. M.; Klepser, S.; Lopez, A.; Martinez, M.; Mazin, D.; Moralejo, A.; Rico, J.; Stamatescu, V.] IFAE, E-08193 Barcelona, Spain.
[Baixeras, C.; Doro, M.; Font, Ll.; Garrido, D.; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, E-08193 Barcelona, Spain.
[Munar, P.; Paredes, J. M.; Ribo, M.; Zabalza, V.] Univ Barcelona IEEC UB, ICC, Dept Astron & Meteorol, Barcelona, Spain.
[Garrido, L.; Gascon, D.; Graciani, R.; Sanuy, A.] Univ Barcelona IEEC UB, ICC, Dept Estruct & Constituents Mat, Barcelona, Spain.
[Antoranz, P.; Bernardino, T.; Fresnillo, L.; Miranda, J. M.; Vegas, I.] Univ Complutense Madrid, Dept Elect, E-28040 Madrid, Spain.
[Barrio, J. A.; Contreras, J. L.; Hassan, T.; Mirabal, N.; Salazar, E.; Tejedor, L. A.] Univ Complutense Madrid, Dept FAMN, E-28040 Madrid, Spain.
[de la Calle Perez, I.; Dubois, F.; Ibarra, A.; Ponz, J. D.] ESA, European Space Astron Ctr, INSA, E-28691 Madrid, Spain.
[Dravins, D.; Ingjald, J.; Jensen, H.] Lund Observ, SE-22100 Lund, Sweden.
[Conrad, J.; Dickinson, H.; Finley, C.; Hultquist, K.; Ripken, J.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Fransson, C.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Ryde, F.] Royal Inst Technol, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Botner, O.; Hallgren, A.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Bretz, T.; Ribordy, M.] Ecole Polytech Fed Lausanne, Lab High Energy Phys, CH-1015 Lausanne, Switzerland.
[Biland, A.; Braun, I.; Grimm, O.; Kraehenbuehl, T.; Roeser, U.; Vogler, P.; Von Gunten, H. P.; Weitzel, Q.] ETH, Inst Particle Phys, CH-8093 Zurich, Switzerland.
[Dorner, D.; Farnier, C.; Lenain, J. -P.; Lyard, E.; Walter, R.] Univ Geneva, Observ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland.
[Florin, D.; Gadola, A.; Gredig, R.; Huber, B.; Manalaysay, A.; Steiner, S.; Straumann, U.; Vollhardt, A.] Univ Zurich, Inst Phys, CH-8057 Zurich, Switzerland.
[Schmoll, J.; Talbot, R. G.] Univ Durham, Sci Labs, Dept Phys, Ctr Adv Instrumentat, Durham DH1 3LE, England.
[Blake, S.; Knapp, J.; Parsons, R. D.] Univ Leeds, Sch Phys Astron, Leeds LS2 9JT, W Yorkshire, England.
[Fraser, G. W.; Hinton, J. A.; O'Brien, P. T.; Osborne, J. P.; Starling, R. L. C.; Warwick, R.; White, R.; Wilkinson, M. I.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Greenshaw, T.; Sutcliffe, P.] Univ Liverpool, Oliver Lodge Lab, Liverpool L69 3BX, Merseyside, England.
[Green, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Ghag, C.; Murphy, A. Stj.] Univ Edinburgh, Sch Phys & Astron, Edinburgh EH8 9YL, Midlothian, Scotland.
[Kudryavtsev, V. A.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
[Granot, J.; Hardcastle, M. J.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[McCubbin, N.; Preece, R.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England.
[Bird, T.; Croston, J.; Emmanoulopoulos, D.; Maccarone, T.; McHardy, I.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Cotter, G.; Karastergiou, A.; Mertsch, P.; Potter, W.; Sarkar, S.; Silk, J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Byrum, K.; Guarino, V.; Wagner, B.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Krennrich, F.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Konopelko, A.; Smith, N.; Xiong, Q.] Pittsburg State Unvers, Dept Phys, Pittsburg, KS 66762 USA.
[Bechtol, K.; Buehler, R.; Cameron, R.; Chiang, J.; Digel, S. W.; Dubois, R.; Funk, S.; Glanzman, T.; Sapozhnikov, L.; Vandenbroucke, J.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Bechtol, K.; Buehler, R.; Cameron, R.; Chiang, J.; Digel, S. W.; Dubois, R.; Funk, S.; Glanzman, T.; Sapozhnikov, L.; Vandenbroucke, J.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Benbow, W.; Galante, N.; Schroedter, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Briggs, M. S.; Connaughton, V.] Univ Alabama, Ctr Space Phys & Aeron Res, Huntsville, AL 35805 USA.
[Arlen, T.; Bobkov, A. A.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Bouvier, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Bogdan, M.; Huan, H.; Humensky, T. B.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Beilicke, M.; Buckley, H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Astron Dept, Chicago, IL 60605 USA.
[Falcone, A. D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Finley, J. P.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Ferenc, D.] Univ Calif Davis, Davis, CA 95616 USA.
[Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Coppi, P.; Szymkowiak, A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
RP Hofmann, W (reprint author), Heidelberg Univ, CTA Project Off, D-69117 Heidelberg, Germany.
EM Werner.Hofmann@mpi-hd.mpg.de; martinez@ifae.es
RI Daniel, Michael/A-2903-2010; Komin, Nukri/J-6781-2015; Barrio,
Juan/L-3227-2014; Murase, Kohta/B-2710-2016; Moulin,
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Riccardo/M-7179-2013; Fontaine, Gerard/D-6420-2014; Todero Peixoto,
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FU Ministerio de Ciencia, Tecnologia e Innovacion Productiva (MinCyT);
Comision Nacional de Energia Atomica (CNEA); Consejo Nacional de
Investigaciones Cientificas y Tecnicas (CONICET) Argentina; State
Committee of Science of Armenia; Ministry for Research, France;
CNRS-INSU, France; CNRS-IN2P3, France; CEA, France; Max Planck Society,
Germany; BMBF, Germany; DESY, Germany; Helmholtz Association, Germany;
MIUR, Italy; Netherlands Research School for Astronomy (NOVA);
Netherlands Organization for Scientific Research (NWO); Ministry of
Science and Higher Education, Poland; National Centre for Research and
Development, Poland; MICINN; CPAN, Spain; MultiDark Consolider-Ingenio
programme, Spain; Swedish Research Council, Sweden; Royal Swedish
Academy of Sciences, Sweden; Swiss National Science Foundation (SNSF),
Switzerland; Leverhulme Trust, UK; Royal Society, UK; Science and
Technologies Facilities Council, UK; Durham University, UK; National
Science Foundation; Department of Energy; Argonne National Laboratory;
University of California; University of Chicago; Iowa State University;
Institute for Nuclear and Particle Astrophysics (INPAC-MRPI); Washington
University McDonnell Center for the Space Sciences, USA
FX We gratefully acknowledge financial support from the following agencies
and organisations: Ministerio de Ciencia, Tecnologia e Innovacion
Productiva (MinCyT), Comision Nacional de Energia Atomica (CNEA) and
Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET)
Argentina; State Committee of Science of Armenia; Ministry for Research,
CNRS-INSU, CNRS-IN2P3 and CEA, France; Max Planck Society, BMBF, DESY,
Helmholtz Association, Germany; MIUR, Italy; Netherlands Research School
for Astronomy (NOVA), Netherlands Organization for Scientific Research
(NWO); Ministry of Science and Higher Education and the National Centre
for Research and Development, Poland; MICINN support through the
National R+D+I, CDTI funding plans and the CPAN and MultiDark
Consolider-Ingenio 2010 programme, Spain. Swedish Research Council,
Royal Swedish Academy of Sciences financed, Sweden; Swiss National
Science Foundation (SNSF), Switzerland; Leverhulme Trust, Royal Society,
Science and Technologies Facilities Council, Durham University, UK;
National Science Foundation, Department of Energy, Argonne National
Laboratory, University of California, University of Chicago, Iowa State
University, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI
program), Washington University McDonnell Center for the Space Sciences,
USA.
NR 118
TC 338
Z9 340
U1 11
U2 100
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0922-6435
EI 1572-9508
J9 EXP ASTRON
JI Exp. Astron.
PD DEC
PY 2011
VL 32
IS 3
BP 193
EP 316
DI 10.1007/s10686-011-9247-0
PG 124
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 898VF
UT WOS:000300769700001
ER
PT J
AU Kullander, SO
Roberts, TR
AF Kullander, Sven O.
Roberts, Tyson R.
TI Out of Lake Tanganyika: endemic lake fishes inhabit rapids of the Lukuga
River
SO ICHTHYOLOGICAL EXPLORATION OF FRESHWATERS
LA English
DT Article
ID EAST-AFRICA; HISTORY; LEVEL; AUCHENOGLANIS; SILURIFORMES; TELEOSTEI;
CICHLIDAE; GENUS
AB The Lukuga River is a large permanent river intermittently serving as the only effluent of Lake Tanganyika. For at least the first one hundred km its water is almost pure lake water. Seventy-seven species of fish were collected from six localities along the Lukuga River. Species of cichlids, cyprinids, and clupeids otherwise known only from Lake Tanganyika were identified from rapids in the Lukuga River at Niemba, 100 km from the lake, whereas downstream localities represent a Congo River fish fauna. Cichlid species from Niemba include specialized algal browsers that also occur in the lake (Simochromis babaulti, S. diagramma) and one invertebrate picker representing a new species of a genus (Tanganicodus) otherwise only known from the lake. Other fish species from Niemba include an abundant species of clupeid, Stolothrissa tanganicae, otherwise only known from Lake Tanganyika that has a pelagic mode of life in the lake. These species demonstrate that their adaptations are not necessarily dependent upon the lake habitat. Other endemic taxa occurring at Niemba are known to frequent vegetated shore habitats or river mouths similar to the conditions at the entrance of the Lukuga, viz. Chelnethiops minutus (Cyprinidae), Lates marine (Latidae), Mastacembelus cunningtoni (Mastacembelidae), Astatotilapia burtoni, Ctenochromis herd, Telmatochromis dhonti, and Tylochromis polylepis (Cichlidae). The Lukuga frequently did not serve as an effluent due to weed masses and sand bars building up at the exit, and low water levels of Lake Tanganyika. Since the Lukuga River does not have a permanent connection with Lake Tanganyika we hypothesize that its lake fishes are not temporary occurrences due to occasional spills from the lake. Apparently the Lukuga maintains a stable fish community that is independent of the lake, and may depend more on the flow of the major tributary, the left bank tributary Niemba River, than on outflow from Lake Tanganyika.
C1 [Kullander, Sven O.] Swedish Museum Nat Hist, Dept Vertebrate Zool, SE-10405 Stockholm, Sweden.
[Roberts, Tyson R.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Kullander, SO (reprint author), Swedish Museum Nat Hist, Dept Vertebrate Zool, POB 50007, SE-10405 Stockholm, Sweden.
EM sven.kullander@nrm.se; tysonregalecus@yahoo.com
FU Committee for Research and Exploration of the National Geographic
Society [3291-86]
FX This paper resulted from the second author's project on 'freshwater
ichthyological exploration of tropical Africa' supported by the
Committee for Research and Exploration of the National Geographic
Society (grant 3291-86). The Catalog of Fishes
(http://researcharchive.calacademy.org/research/Ichthyology/catalog/fish
-catmairi.asp) curated by William N. Eschmeyer, FishBase
(http://www.fishbase.org/), and the Biodiversity Heritage Library
(http://www.biodiversitylibrary.org/), have been indispensable resources
in the quest for literature and species information. We thank Lukas
Ruber (BMNH) for valuable comments on the manuscript and on the
identification of the cichlids.
NR 80
TC 5
Z9 5
U1 1
U2 5
PU VERLAG DR FRIEDRICH PFEIL
PI MUNICH
PA WOLFRATSHAUSER STRASSE 27, MUNICH, D-81379, GERMANY
SN 0936-9902
J9 ICHTHYOL EXPLOR FRES
JI Ichthyol. Explor. Freshw.
PD DEC
PY 2011
VL 22
IS 4
BP 355
EP 376
PG 22
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 884OY
UT WOS:000299718600008
ER
PT J
AU Pyenson, ND
Sponberg, SN
AF Pyenson, Nicholas D.
Sponberg, Simon N.
TI Reconstructing Body Size in Extinct Crown Cetacea (Neoceti) Using
Allometry, Phylogenetic Methods and Tests from the Fossil Record
SO JOURNAL OF MAMMALIAN EVOLUTION
LA English
DT Article
DE Cetacea; Fossil record; Body size; Allometry; Independent contrasts;
Partial least squares
ID INDEPENDENT CONTRASTS; STATE RECONSTRUCTION; CONFIDENCE-INTERVALS;
TOOTHED WHALES; CYTOCHROME-B; EVOLUTION; MIOCENE; REGRESSION; RADIATION;
EOCENE
AB Living cetaceans exhibit interspecific size ranging across several orders of magnitude, and rank among the largest vertebrates ever. Details of how cetaceans evolved different body sizes, however, remain obscure, because they lack basic morphological proxies that have been traditionally used in other fossil vertebrates. Here, we reconstruct the body size of extinct crown group cetaceans (Neoceti) using different regression methods on extant skull and length data, in a phylogenetic context. Because most fossil cetaceans are fragmentary, we developed regression equations to predict total length based on cranial metrics that are preserved on most fossil crania. The resultant regression equations are based on a database of skull and length data from most extant lineages of cetaceans (n=45 species; 272 specimens), sampling all living mysticete genera and all major clades of odontocetes. In generating predictive equations, we compared both conventional species data regression and independent contrast regression methods, as well as single trait predictors and a new approach that combines the advantages of a partial least squares (PLS) multivariate regression with independent contrasts. This last approach leverages the predictive power of using multiple correlated proxies. Lastly, we used the rare occurrences of fossil cetaceans with preserved total lengths to test the performance of our predictive equations for reconstructing body size from skull measurements alone. Our results demonstrate that incorporating information about phylogenetic relationships and multiple cranial measures in PLS scaling studies increases the accuracy of reconstructed body size, most notably by reducing prediction intervals by more than 70%. With this empirical foundation, we highlight the outline of major features in the evolution of body size for Neoceti and future opportunities to use these metrics for paleobiological questions.
C1 [Pyenson, Nicholas D.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Pyenson, Nicholas D.] Univ Washington, Burke Museum Nat & Culture, Dept Mammal, Seattle, WA 98195 USA.
[Pyenson, Nicholas D.] Univ Washington, Burke Museum Nat & Culture, Dept Paleontol, Seattle, WA 98195 USA.
[Sponberg, Simon N.] Univ Washington, Dept Biol, Seattle, WA 98195 USA.
RP Pyenson, ND (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, NHB MRC 121,10th & Constitut NW, Washington, DC 20013 USA.
EM PyensonN@si.edu
FU National Science Foundation (NSF); Royal Society of New Zealand; New
Zealand Ministry of Science and Technology; UCMP; Department of
Integrative Biology, University of California, Berkeley; Natural
Sciences and Engineering Research Council of Canada; Smithsonian
Institution; Fannie and John Hertz Foundation
FX For collections visits and assitance, N. D. P. is most grateful to time
and effort of researchers at the following institutions: E. Hoch and
staff at the Conservation Department and Gram Museum of Paleontology; D.
Long and M. Flannery (CAS); O. Lambert (IRNSB); D. Janiger and J. Dynes
(LACM); M. Fornasiero and L. Del Favero (MGPUP); G. Bianucci and C.
Sorbini (MSNTUP); C. de Muizon and V. Bouetel (MNHN); C. Conroy and J.
Patton (MVZ); R. Sabin, L. Tomsett, and P. Jenkins (NHM); A. van Helden
(NMNZ); E. M. G. Fitzgerald (NMV); K. A. Fahy (SBNHM); D. J. Bohaska, C.
W. Potter, and J. G. Mead (USNM); and J. Bradley (UWBM). We are also
extremely grateful for E. P. J. Heizmann (SMNS), who provided crucial
measurements of specimens in Germany. N. D. P. thanks L. G. Barnes and
H. Thomas for collections access and assistance at LACM. T. A. Demere,
R. E. Fordyce, J. A. Goldbogen, M. D. Uhen, and J. Velez-Juarbe provided
helpful comments, discussions and assistance. We also thank two
anonymous reviewers and Editor-in-Chief J. R. Wible for insightful
comments that improved the content of this manuscript. This paper
represents part of a doctoral dissertation completed by N. D. P. in the
Department of Integrative Biology and the Museum of Paleontology at the
University of California, Berkeley; input from committee members D. R.
Lindberg, A. D. Barnosky, J. H. Lipps, W. Alvarez, and G. J. Vermeij
improved the quality of this chapter. C. Nunn, S. Patek, and M. Lahiff
also provided valuable support on multivariate comparative methods.
Portions of this manuscript were written with funding to N. D. P. from:
a National Science Foundation (NSF) Graduate Research Fellowship; a NSF
East Asia and Pacific Summer Institutes fellowship, co-sponsored by the
Royal Society of New Zealand and the New Zealand Ministry of Science and
Technology; the UCMP Remington Kellogg Fund and the Department of
Integrative Biology, University of California, Berkeley; a postdoctoral
research fellowship from the Natural Sciences and Engineering Research
Council of Canada; and from the Smithsonian Institution. Funding for S.
N. S. is from the Fannie and John Hertz Foundation.
NR 101
TC 39
Z9 39
U1 1
U2 11
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1064-7554
EI 1573-7055
J9 J MAMM EVOL
JI J. Mamm. Evol.
PD DEC
PY 2011
VL 18
IS 4
BP 269
EP 288
DI 10.1007/s10914-011-9170-1
PG 20
WC Evolutionary Biology; Zoology
SC Evolutionary Biology; Zoology
GA 893ID
UT WOS:000300348700003
ER
PT J
AU Isaac, B
Isaac, G
AF Isaac, Barbara
Isaac, Gwyneira
TI UNEXPECTED TRAJECTORIES: A HISTORY OF NIUEAN THROWING STONES
SO JOURNAL OF THE POLYNESIAN SOCIETY
LA English
DT Article
DE Niue; throwing stones; missionaries; museum collections
AB Before the arrival of the first missionaries, Niuean warriors fought with stones carefully modified for throwing. This practice, much feared by sailors and missionaries, became a symbol of the primitiveness of the "Savage Island" (Cook 1774). By 1853, following Christian conversion, the practice of throwing stones had come to an end. In so far as it is possible with the limited records available, we reconstruct the original behaviour, as well as the intriguing trajectories the stones took as they left the island and were later collected by and housed in museums. We track this dispersal process, as well as the incorporation of the stones into 19th century anthropological thinking. Today, there is only one stone known on the island, and none are known to have been found in archaeological surveys. This impels us to address the scale of loss represented by these now geographically remote objects of the past.
C1 [Isaac, Gwyneira] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
NR 48
TC 0
Z9 0
U1 1
U2 3
PU POLYNESIAN SOC INC
PI AUCKLAND
PA C/O MAORI STUDIES, UNIV AUCKLAND, PRIVATE BAG, AUCKLAND 92019, NEW
ZEALAND
SN 0032-4000
J9 J POLYNESIAN SOC
JI J. Polyn. Soc.
PD DEC
PY 2011
VL 120
IS 4
BP 369
EP 401
PG 33
WC Anthropology
SC Anthropology
GA 893EA
UT WOS:000300337200004
ER
PT J
AU Hintz, ES
AF Hintz, Eric S.
TI The Power Makers: Steam, Electricity, and the Men Who Invented Modern
America
SO BUSINESS HISTORY REVIEW
LA English
DT Book Review
C1 [Hintz, Eric S.] Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA.
RP Hintz, ES (reprint author), Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 1
U2 1
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0007-6805
J9 BUS HIST REV
JI Bus. Hist. Rev.
PD WIN
PY 2011
VL 85
IS 4
BP 807
EP 812
DI 10.1017/S0007680511001218
PG 6
WC Business; History Of Social Sciences
SC Business & Economics; Social Sciences - Other Topics
GA 883WX
UT WOS:000299666700007
ER
PT J
AU Armstrong, JS
Green, KC
Soon, W
AF Armstrong, J. Scott
Green, Kesten C.
Soon, Willie
TI RESEARCH ON FORECASTING FOR THE MANMADE GLOBAL WARMING ALARM
SO ENERGY & ENVIRONMENT
LA English
DT Article
ID BEAR POPULATION FORECASTS; AUDIT
AB The validity of the manmade global warming alarm requires the support of scientific forecasts of (1) a substantive long-term rise in global mean temperatures in the absence of regulations, (2) serious net harmful effects due to global warming, and (3) cost-effective regulations that would produce net beneficial effects versus alternatives policies, including doing nothing. Without scientific forecasts for all three aspects of the alarm, there is no scientific basis to enact regulations. In effect, the warming alarm is like a three-legged stool: each leg needs to be strong. Despite repeated appeals to global warming alarmists, we have been unable to find scientific forecasts for any of the three legs. We drew upon scientific (evidence-based) forecasting principles to audit the forecasting procedures used to forecast global mean temperatures by the Intergovernmental Panel on Climate Change (IPCC) - leg "1" of the stool. This audit found that the IPCC procedures violated 81% of the 89 relevant forecasting principles. We also audited forecasting procedures, used in two papers, that were written to support regulation regarding the protection of polar bears from global warming - leg "3" of the stool. On average, the forecasting procedures violated 85% of the 90 relevant principles. The warming alarmists have not demonstrated the predictive validity of their procedures. Instead, their argument for predictive validity is based on their claim that nearly all scientists agree with the forecasts. This count of "votes" by scientists is not only an incorrect tally of scientific opinion, it is also, and most importantly, contrary to the scientific method. We conducted a validation test of the IPCC forecasts that were based on the assumption that there would be no regulations. The errors for the IPCC model long-term forecasts (for 91 to 100 years in the future) were 12.6 times larger than those from an evidence-based "no change" model. Based on our own analyses and the documented unscientific behavior of global warming alarmists, we concluded that the global warming alarm is the product of an anti-scientific political movement. Having come to this conclusion, we turned to the "structured analogies" method to forecast the likely outcomes of the warming alarmist movement. In our ongoing study we have, to date, identified 26 similar historical alarmist movements. None of the forecasts behind the analogous alarms proved correct. Twenty-five alarms involved calls for government intervention and the government imposed regulations in 23. None of the 23 interventions was effective and harm was caused by 20 of them. Our findings on the scientific evidence related to global warming forecasts lead to the following recommendations:
1. End government funding for climate change research.
2. End government funding for research predicated on global warming (e.g., alternative energy; CO(2) reduction; habitat loss).
3. End government programs and repeal regulations predicated on global warming.
4. End government support for organizations that lobby or campaign predicated on global warming.
C1 [Armstrong, J. Scott] Univ Penn, Philadelphia, PA 19104 USA.
[Green, Kesten C.] Univ S Australia, Adelaide, SA 5001, Australia.
[Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
RP Armstrong, JS (reprint author), Univ Penn, Philadelphia, PA 19104 USA.
EM armstrong@wharton.upenn.edu
RI Green, Kesten/F-3716-2013
OI Green, Kesten/0000-0001-9122-885X
NR 25
TC 0
Z9 0
U1 5
U2 56
PU MULTI-SCIENCE PUBL CO LTD
PI BRENTWOOD
PA 5 WATES WAY, BRENTWOOD CM15 9TB, ESSEX, ENGLAND
SN 0958-305X
J9 ENERG ENVIRON-UK
JI Energy Environ.
PD DEC
PY 2011
VL 22
IS 8
BP 1091
EP 1104
DI 10.1260/0958-305X.22.8.1091
PG 14
WC Environmental Studies
SC Environmental Sciences & Ecology
GA 871PY
UT WOS:000298751400008
ER
PT J
AU Charbonnier, A
Combet, C
Daniel, M
Funk, S
Hinton, JA
Maurin, D
Power, C
Read, JI
Sarkar, S
Walker, MG
Wilkinson, MI
AF Charbonnier, A.
Combet, C.
Daniel, M.
Funk, S.
Hinton, J. A.
Maurin, D.
Power, C.
Read, J. I.
Sarkar, S.
Walker, M. G.
Wilkinson, M. I.
TI Dark matter profiles and annihilation in dwarf spheroidal galaxies:
prospectives for present and future gamma-ray observatories - I. The
classical dwarf spheroidal galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE astroparticle physics; methods: miscellaneous; galaxies: dwarf;
galaxies: kinematics and dynamics; dark matter; gamma-rays: general
ID MILKY-WAY; NEUTRALINO ANNIHILATION; SPHERICAL GALAXIES; COSMIC-RAYS;
LOCAL GROUP; LEO-I; MASS; MODELS; HALOES; CONSTRAINTS
AB Due to their large dynamical mass-to-light ratios, dwarf spheroidal galaxies (dSphs) are promising targets for the indirect detection of dark matter (DM) in ?-rays. We examine their detectability by present and future ?-ray observatories. The key innovative features of our analysis are as follows: (i) we take into account the angular size of the dSphs; while nearby objects have higher ?-ray flux, their larger angular extent can make them less attractive targets for background-dominated instruments; (ii) we derive DM profiles and the astrophysical J-factor (which parametrizes the expected ?-ray flux, independently of the choice of DM particle model) for the classical dSphs directly from photometric and kinematic data. We assume very little about the DM profile, modelling this as a smooth split-power-law distribution, with and without subclumps; (iii) we use a Markov chain Monte Carlo technique to marginalize over unknown parameters and determine the sensitivity of our derived J-factors to both model and measurement uncertainties; and (iv) we use simulated DM profiles to demonstrate that our J-factor determinations recover the correct solution within our quoted uncertainties.
Our key findings are as follows: (i) subclumps in the dSphs do not usefully boost the signal; (ii) the sensitivity of atmospheric Cherenkov telescopes to dSphs within similar to 20 kpc with cored haloes can be up to similar to 50 times worse than when estimated assuming them to be point-like. Even for the satellite-borne Fermi-Large Area Telescope (Fermi-LAT), the sensitivity is significantly degraded on the relevant angular scales for long exposures; hence, it is vital to consider the angular extent of the dSphs when selecting targets; (iii) no DM profile has been ruled out by current data, but using a prior on the inner DM cusp slope 0 <= gamma prior <= 1 provides J-factor estimates accurate to a factor of a few if an appropriate angular scale is chosen; (iv) the J-factor is best constrained at a critical integration angle alpha(c) = 2r(h)/d (where rh is the half-light radius and d is the distance from the dwarf) and we estimate the corresponding sensitivity of gamma-ray observatories; (v) the 'classical' dSphs can be grouped into three categories: well constrained and promising (Ursa Minor, Sculptor and Draco), well constrained but less promising (Carina, Fornax and Leo I), and poorly constrained (Sextans and Leo II); and (vi) observations of classical dSphs with the Fermi-LAT integrated over the mission lifetime are more promising than observations with the planned Cherenkov Telescope Array for DM particle mass less than or similar to 700 GeV. However, even the Fermi-LAT will not have sufficient integrated signal from the classical dwarfs to detect DM in the 'vanilla' Minimal Supersymmetric Standard Model. Both the Galactic Centre and the 'ultrafaint' dwarfs are likely to be better targets and will be considered in future work.
C1 [Charbonnier, A.; Maurin, D.] Univ Paris 06, Lab Phys Nucl & Hautes Energies, CNRS, IN2P3, F-75252 Paris 05, France.
[Charbonnier, A.; Maurin, D.] Univ Paris 07, Lab Phys Nucl & Hautes Energies, CNRS, IN2P3, F-75252 Paris 05, France.
[Combet, C.; Hinton, J. A.; Maurin, D.; Power, C.; Read, J. I.; Wilkinson, M. I.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Daniel, M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Funk, S.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Funk, S.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Maurin, D.] Univ Grenoble 1, CNRS, IN2P3, Lab Phys Subatom & Cosmol,INPG, F-38026 Grenoble, France.
[Maurin, D.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Power, C.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia.
[Read, J. I.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland.
[Sarkar, S.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England.
[Walker, M. G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Walker, M. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Charbonnier, A (reprint author), Univ Paris 06, Lab Phys Nucl & Hautes Energies, CNRS, IN2P3, 4 Pl Jussieu,Tour 33, F-75252 Paris 05, France.
EM jah85@leicester.ac.uk; dmaurin@lpsc.in2p3.fr; walker@ast.cam.ac.uk
RI Power, Chris/C-2480-2013; Walker, Matthew/P-1777-2014; Funk,
Stefan/B-7629-2015; Daniel, Michael/A-2903-2010; Sarkar,
Subir/G-5978-2011
OI Power, Chris/0000-0002-4003-0904; Walker, Matthew/0000-0003-2496-1925;
Funk, Stefan/0000-0002-2012-0080; Daniel, Michael/0000-0002-8053-7910;
Sarkar, Subir/0000-0002-3542-858X
FU NASA [HST-HF-51283, NAS 5-26555]; Space Telescope Science Institute;
STFC at University of Leicester; STFC; Royal Society; SNF
[PP00P2_128540/1]; EU Research & Training Network 'Unification in the
LHC era' [PITN-GA-2009-237920]; BIS
FX We thank the anonymous referee for careful reading of the manuscript and
useful comments. We thank Walter Dehnen for providing his code for use
in generating artificial dSph data sets. MGW is supported by NASA
through Hubble Fellowship grant HST-HF-51283, 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. CC acknowledges support from an STFC rolling grant at the
University of Leicester. JAH acknowledges the support of an STFC
Advanced Fellowship. MIW acknowledges the Royal Society for support
through a University Research Fellowship. JIR acknowledges support from
SNF grant PP00P2_128540/1. SS acknowledges support by the EU Research &
Training Network 'Unification in the LHC era' (PITN-GA-2009-237920).
Part of this work used the ALICE High Performance Computing Facility at
the University of Leicester. Some resources on ALICE form part of the
DiRAC Facility jointly funded by the STFC and Large Facilities Capital
Fund of BIS.
NR 96
TC 59
Z9 59
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 DEC
PY 2011
VL 418
IS 3
BP 1526
EP 1556
DI 10.1111/j.1365-2966.2011.19387.x
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 862JW
UT WOS:000298088000009
ER
PT J
AU Bogdan, A
Gilfanov, M
AF Bogdan, A.
Gilfanov, M.
TI Unresolved and diffuse components of X-ray emission and X-ray-to-K-band
luminosity ratios in nearby early-type and late-type galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: elliptical and lenticular,cD; galaxies: irregular; galaxies:
spiral; X-rays: galaxies; X-rays: ISM; X-rays: stars
ID HOT GAS; VIRGO CLUSTER; CHANDRA OBSERVATIONS; STELLAR POPULATIONS;
GLOBULAR-CLUSTERS; POINT SOURCES; HOST GALAXY; XMM-NEWTON; NGC 3379;
BINARIES
AB We explore the nature of unresolved X-ray emission in a broad sample of galaxies of all morphological types based on archival Chandra data. After removing bright compact sources, we study L X/L K luminosity ratios of unresolved emission, and compare them with the solar neighbourhood values. We conclude that unresolved emission is determined by four main components, three of which were known before. (i) The population of faint unresolved sources associated with old stellar population: in early-type galaxies, their 210 keV band luminosity scales with the stellar mass with . (ii) The interstellar medium (ISM) with kT similar to 0.20.8 keV present in galaxies of all types: because of the large dispersion in the gas content of galaxies, the size of our sample is insufficient to obtain reliable scaling law for this component. (iii) The population of unresolved young stars and young stellar objects in late-type galaxies: their 210 keV band luminosity scales with the star formation rate with . (iv) In four old and massive Virgo ellipticals (M49, M60, M84, NGC 4636) we find anomalously high X-ray emission in the 210 keV band. Its presence has not been recognized before and its nature is unclear. Although it appears to be stronger in galaxies having stronger ISM component, its existence cannot be explained in terms of an extrapolation of the warm ISM spectrum. Association with Virgo cluster of galaxies suggests that the excess emission may be due to intracluster gas accreted in the gravitational well of a massive galaxy. We investigate this and other possibilities.
C1 [Bogdan, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Bogdan, A.; Gilfanov, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Gilfanov, M.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
RP Bogdan, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM abogdan@cfa.harcard.edu; gilfanov@mpa-garching.mpg.de
FU National Aeronautics and Space Administration; National Science
Foundation
FX The authors thank Bill Forman, Christine Jones and Ralph Kraft for
critical discussions of these results and the anonymous referee for the
careful reading of the manuscript and constructive comments. This
research has made use of Chandra archival data provided by the Chandra
X-ray Center (CXC). The publication makes use of software provided by
the CXC in the application package CIAO. The Spitzer Space Telescope 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.
NR 54
TC 21
Z9 21
U1 0
U2 0
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 DEC
PY 2011
VL 418
IS 3
BP 1901
EP 1912
DI 10.1111/j.1365-2966.2011.19608.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 862JW
UT WOS:000298088000034
ER
PT J
AU Fabian, AC
Sanders, JS
Allen, SW
Canning, REA
Churazov, E
Crawford, CS
Forman, W
GaBany, J
Hlavacek-Larrondo, J
Johnstone, RM
Russell, HR
Reynolds, CS
Salome, P
Taylor, GB
Young, AJ
AF Fabian, A. C.
Sanders, J. S.
Allen, S. W.
Canning, R. E. A.
Churazov, E.
Crawford, C. S.
Forman, W.
GaBany, J.
Hlavacek-Larrondo, J.
Johnstone, R. M.
Russell, H. R.
Reynolds, C. S.
Salome, P.
Taylor, G. B.
Young, A. J.
TI A wide Chandra view of the core of the Perseus cluster
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; galaxies: individual: NGC 1275;
intergalactic medium; X-rays: galaxies
ID GALACTIC NUCLEUS FEEDBACK; X-RAY SPECTROSCOPY; GALAXY CLUSTERS; COLD
FRONTS; EMITTING GAS; RADIO LOBES; BLACK-HOLE; NGC 1275; NGC-1275;
SHOCKS
AB We present new Chandra images of the X-ray emission from the core of the Perseus cluster of galaxies. The total observation time is now 1.4 Ms. New depressions in X-ray surface brightness are discovered to the north of NGC 1275, which we interpret as old rising bubbles. They imply that bubbles are long-lived and do not readily breakup when rising in the hot cluster atmosphere. The existence of a 300 kpc long NNWSSW bubble axis means there cannot be significant transverse large-scale flows exceeding 100 km s-1. Interesting spatial correlations are seen along that axis in early deep radio maps. A semicircular cold front about 100 kpc west of the nucleus is seen. It separates an inner disturbed region dominated by the activity of the active nucleus of NGC 1275 from the outer region where a subcluster merger dominates.
C1 [Fabian, A. C.; Sanders, J. S.; Canning, R. E. A.; Crawford, C. S.; Hlavacek-Larrondo, J.; Johnstone, R. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Allen, S. W.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Churazov, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Forman, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[GaBany, J.] Blackbird 2 Observ, Alder Springs, CA 93602 USA.
[Russell, H. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Salome, P.] CNRS, UMR 8112, Observ Paris, LERMA, F-75014 Paris, France.
[Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Young, A. J.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 3HG, Avon, England.
RP Fabian, AC (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM acf@ast.cam.ac.uk; gbtaylor@unm.edu
RI Churazov, Eugene/A-7783-2013;
OI Sanders, Jeremy/0000-0003-2189-4501
FU Royal Society; National Aeronautics and Space Administration
[GO0-11139X, GO0-11138B, NAS8-03060]; Chandra Guest Observer Program
[GO011138A]; US Department of Energy [DE-AC02-76SF00515]; Canadian Space
Agency
FX We acknowledge financial support from the Royal Society (ACF). JH-L
thanks the Cambridge Trusts and the Natural Sciences and Engineering
Research Council of Canada (NSERC). GBT acknowledges support provided by
the National Aeronautics and Space Administration through Chandra Award
Numbers GO0-11139X and GO0-11138B 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. CSR acknowledges support from
the Chandra Guest Observer Program under grant GO011138A. SWA was
supported in part by the US Department of Energy under contract number
DE-AC02-76SF00515. HRR acknowledges generous financial support from the
Canadian Space Agency Space Science Enhancement Program.
NR 50
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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 DEC
PY 2011
VL 418
IS 4
BP 2154
EP 2164
DI 10.1111/j.1365-2966.2011.19402.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 862JX
UT WOS:000298088100004
ER
PT J
AU Laurino, O
D'Abrusco, R
Longo, G
Riccio, G
AF Laurino, O.
D'Abrusco, R.
Longo, G.
Riccio, G.
TI Astroinformatics of galaxies and quasars: a new general method for
photometric redshifts estimation
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; techniques: photometric; catalogues; surveys;
virtual observatory tools; cosmology: observations
ID DIGITAL SKY SURVEY; ARTIFICIAL NEURAL-NETWORKS; BROAD-BAND PHOTOMETRY;
EARLY DATA RELEASE; 7TH DATA RELEASE; DATA SETS; SDSS; SPACE; SELECTION;
CATALOG
AB With the availability of the huge amounts of data produced by current and future large multiband photometric surveys, photometric redshifts have become a crucial tool for extragalactic astronomy and cosmology. In this paper we present a novel method, called Weak Gated Experts (WGE), which allows us to derive photometric redshifts through a combination of data mining techniques. The WGE, like many other machine learning techniques, is based on the exploitation of a spectroscopic knowledge base composed by sources for which a spectroscopic value of the redshift is available. This method achieves a variance sigma(2)(Delta z) = 2.3 x 10(-4) [sigma(2)(Delta z) = 0.08, where Delta z=Z(phot)-Z(spec)] for the reconstruction of the photometric redshifts for the optical galaxies from the Sloan Digital Sky Survey (SDSS) and for the optical quasars, respectively, while the root mean square (rms) of the Delta z variable distributions for the two experiments is, respectively, equal to 0.021 and 0.35. The WGE provides also a mechanism for the estimation of the accuracy of each photometric redshift. We also present and discuss the catalogues obtained for the optical SDSS galaxies, for the optical candidate quasars extracted from the Data Release 7 of SDSS photometric data set (the sample of SDSS sources on which the accuracy of the reconstruction has been assessed is composed of bright sources, for a subset of which spectroscopic redshifts have been measured) and for optical SDSS candidate quasars observed by GALEX in the ultraviolet range. The WGE method exploits the new technological paradigm provided by the virtual observatory and the emerging field of astroinformatics.
C1 [Laurino, O.] INAF, Astron Observ Trieste, I-34143 Trieste, Italy.
[Laurino, O.; D'Abrusco, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Longo, G.; Riccio, G.] Univ Naples Federico 2, Dept Phys Sci, I-80126 Naples, Italy.
[Longo, G.] CALTECH, Dept Astron, Pasadena, CA 90125 USA.
RP Laurino, O (reprint author), INAF, Astron Observ Trieste, I-34143 Trieste, Italy.
EM olaurino@head.cfa.harvard.edu
RI D'Abrusco, Raffaele/L-2767-2016;
OI D'Abrusco, Raffaele/0000-0003-3073-0605; Riccio,
Giovanni/0000-0002-6594-6820
FU US Virtual Astronomical Observatory; National Science Foundation;
National Aeronautics and Space Administration
FX This work was made possible by the financial support of the US Virtual
Astronomical Observatory, which is sponsored by the National Science
Foundation and the National Aeronautics and Space Administration. This
paper is based on work that took advantage of several technologies the
authors would like to acknowledge. The WGE code is mostly based on the
Fast Artificial Neural Network library.5 Most of the
statistical code is implemented in R,6 while for data
retrieval, analysis and publication, multiple tools, services and
protocols developed by the International Virtual Observatory
Alliance7 were used. In particular, all the catalogues
derived from this publication will be published as standard Cone Search
services through the VODance service hosted at the Italian Center for
Astronomical Archives (IA2), Trieste Astronomical Observatory. TOPCAT
(Taylor 2005) was used extensively in both its desktop version and its
command line counterpart STILTS (Taylor 2006). The authors thank the
anonymous reviewer for insightful comments that have helped to improve
the paper.
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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 DEC
PY 2011
VL 418
IS 4
BP 2165
EP 2195
DI 10.1111/j.1365-2966.2011.19416.x
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 862JX
UT WOS:000298088100005
ER
PT J
AU Mittal, R
O'Dea, CP
Ferland, G
Oonk, JBR
Edge, AC
Canning, REA
Russell, H
Baum, SA
Bohringer, H
Combes, F
Donahue, M
Fabian, AC
Hatch, NA
Hoffer, A
Johnstone, R
McNamara, BR
Salome, P
Tremblay, G
AF Mittal, R.
O'Dea, C. P.
Ferland, G.
Oonk, J. B. R.
Edge, A. C.
Canning, R. E. A.
Russell, H.
Baum, S. A.
Boehringer, H.
Combes, F.
Donahue, M.
Fabian, A. C.
Hatch, N. A.
Hoffer, A.
Johnstone, R.
McNamara, B. R.
Salome, P.
Tremblay, G.
TI Herschel observations of the Centaurus cluster - the dynamics of cold
gas in a cool core
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE photodissociation region (PDR); galaxies: active; galaxies: clusters:
intracluster medium; galaxies: kinematics and dynamics; galaxies: star
formation; infrared: ISM
ID X-RAY SPECTROSCOPY; ACTIVE GALACTIC NUCLEI; POLYCYCLIC
AROMATIC-HYDROCARBONS; FAR-ULTRAVIOLET OBSERVATIONS; MOLECULAR-HYDROGEN
EMISSION; SPITZER-SPACE-TELESCOPE; UNIVERSE GALAXY SURVEY;
STAR-FORMATION; XMM-NEWTON; PHOTODISSOCIATION REGIONS
AB Brightest cluster galaxies (BCGs) in the cores of galaxy clusters have distinctly different properties from other low-redshift massive ellipticals. The majority of the BCGs in cool-core clusters show signs of active star formation. We present observations of NGC 4696, the BCG of the Centaurus galaxy cluster, at far-infrared (FIR) wavelengths with the Herschel space telescope. Using the PACS spectrometer, we detect the two strongest coolants of the interstellar medium, [C Pi] at 157.74 mu m and [O Iota] at 63.18 mu m, and in addition [N Pi] at 121.90 mu m. The [C Pi] emission is extended over a region of 7 kpc with a similar spatial morphology and kinematics to the optical Ha emission. This has the profound implication that the optical hydrogen recombination line, Ha, the optical forbidden lines, [N Pi] lambda 6583 angstrom, the soft X-ray filaments and the FIR [C Pi] line all have the same energy source.
We also detect dust emission using the PACS and SPIRE photometers at all six wavebands. We perform a detailed spectral energy distribution fitting using a two-component modified blackbody function and find a cold 19-K dust component with mass 1.6 x 10(6) M-circle dot and a warm 46-K dust component with mass 4.0 x 10(3) M-circle dot. The total FIR luminosity between 8 and 1000 mu m is 7.5 x 10(8) L-circle dot, which using Kennicutt relation yields a low star formation rate of 0.13 M-circle dot yr(-1). This value is consistent with values derived from other tracers, such as ultraviolet emission. Combining the spectroscopic and photometric results together with optical H alpha, we model emitting clouds consisting of photodissociation regions adjacent to ionized regions. We show that in addition to old and young stellar populations, there is another source of energy, such as cosmic rays, shocks or reconnection diffusion, required to excite the H alpha and [C II] filaments.
C1 [Mittal, R.; Baum, S. A.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA.
[O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA.
[Ferland, G.] Univ Kentucky, Dept Phys, Lexington, KY 40506 USA.
[Oonk, J. B. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Oonk, J. B. R.] Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands.
[Edge, A. C.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England.
[Canning, R. E. A.; Johnstone, R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Russell, H.; McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Boehringer, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Combes, F.; Salome, P.] CNRS, Observ Paris, LERMA, F-75014 Paris, France.
[Donahue, M.; Hoffer, A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Hatch, N. A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada.
[McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Mittal, R (reprint author), Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA.
EM rmittal@astro.rit.edu
OI Hatch, Nina/0000-0001-5600-0534; Edge, Alastair/0000-0002-3398-6916;
Tremblay, Grant/0000-0002-5445-5401; Combes,
Francoise/0000-0003-2658-7893; Ferland, Gary/0000-0003-4503-6333
FU NASA through JPL/Caltech; Canadian Space Agency; STFC; University of
Nottingham; New York Space Grant Consortium; NASA
FX This work is based (in part) on observations made with Herschel, a
European Space Agency Cornerstone Mission with significant participation
by NASA. Support for this work was provided by NASA through an award
issued by JPL/Caltech. We would like to thank the HSC and NHSC
consortium for support with data-reduction pipelines. RM is grateful to
P. Appleton for repeated help with the Herschel analysis and thanks J.
T. Whelan and D. Merritt for comments and discussions. BRMcN and HR
acknowledge generous financial support from the Canadian Space Agency
Space Science Enhancement Programme. NAH thanks STFC and the University
of Nottingham Anne McLaren Fellowship for support. GT acknowledges
support from the New York Space Grant Consortium. This research has made
use of the NASA/IPAC Extragalactic Database (NED) which is operated by
the JPL/Caltech, under contract with NASA. STSDAS is a product of the
Space Telescope Science Institute, which is operated by AURA for NASA.
NR 107
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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 DEC
PY 2011
VL 418
IS 4
BP 2386
EP 2402
DI 10.1111/j.1365-2966.2011.19634.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 862JX
UT WOS:000298088100023
ER
PT J
AU Hallman, EJ
Jeltema, TE
AF Hallman, Eric J.
Jeltema, Tesla E.
TI Structure and turbulence in simulated galaxy clusters and the
implications for the formation of radio haloes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE hydrodynamics; methods: numerical; galaxies: clusters: general;
galaxies: clusters: intracluster medium; cosmology: theory; X-rays:
galaxies: clusters
ID X-RAY-CLUSTERS; COSMOLOGICAL SIMULATIONS; MAGNETIC-FIELDS; DARK-MATTER;
COSMIC-RAYS; EMISSION; EVOLUTION; MERGERS; RELICS; REACCELERATION
AB We track the histories of massive clusters of galaxies formed within a cosmological hydrodynamic simulation. Specifically, we track the time evolution of the energy in random bulk motions of the intracluster medium and X-ray measures of cluster structure and their relationship to cluster mergers. We aim to assess the viability of the turbulent re-acceleration model for the generation of giant radio haloes by comparing the level of turbulent kinetic energy in simulated clusters with the observed properties of radio halo clusters, giving particular attention to the association of radio haloes to clusters with disturbed X-ray structures. The evolution of X-ray cluster structure and turbulence kinetic energy, k, in simulations can then inform us about the expected lifetime of radio haloes and the fraction of clusters as a function of redshift expected to host them. We find strong statistical correlation of disturbed structure measures and the presence of enhancements in k. Specifically, quantitatively disturbed, radio halo-like X-ray morphology in our sample indicates a 92 per cent chance of the cluster in question having k elevated to more than twice its minimum value over the clusters life. The typical lifetime of episodes of elevated turbulence is on the order of 1 Gyr, though these periods can last 5 Gyr or more. This variation reflects the wide range of cluster histories; while some clusters undergo complex and repeated mergers spending a majority of their time in elevated k states, other clusters are relaxed over nearly their entire history. We do not find a bimodal relationship between cluster X-ray luminosity and the total energy in turbulence that might account directly for a bimodal LXP1.4 GHz relation. However, our result may be consistent with the observed bimodality, as here we are not including a full treatment of cosmic ray sources and magnetic fields.
C1 [Hallman, Eric J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jeltema, Tesla E.] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Jeltema, Tesla E.] UCO Lick Observ, Santa Cruz, CA 95064 USA.
RP Hallman, EJ (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
EM ehallman@cfa.harvard.edu
FU Fermi Guest Investigator grant [21077]; NASA [NNX09AT83G]
FX EJH acknowledges the support of Fermi Guest Investigator grant 21077.
EJH also acknowledges very helpful discussions with Rossella Cassano,
Simona Giacintucci, Marcus Brueggen, Brian O'Shea, Sam Skillman and Uri
Keshet. TEJ acknowledges support from NASA grant NNX09AT83G.
Computations described in this work were performed using the ENZO code
developed by the Laboratory for Computational Astrophysics at the
University of California in San Diego (http://lca.ucsd.edu) and by a
community of independent developers from numerous other institutions.
The YT analysis toolkit was developed primarily by Matthew Turk with
contributions from many other developers, to whom we are very grateful.
Computing time was provided by TRAC allocation TG-AST100004. The authors
acknowledge the Texas Advanced Computing Center (TACC) at The University
of Texas at Austin for providing HPC resources that have contributed to
the research results reported within this paper.
URL:http://www.tacc.utexas.edu. EJH acknowledges the WiFi connections
provided by the Massachusetts Bay Transportation Authority's Commuter
Rail (Franklin Line) in enabling significant portions of this work to be
done in transit.
NR 52
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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 DEC
PY 2011
VL 418
IS 4
BP 2467
EP 2480
DI 10.1111/j.1365-2966.2011.19637.x
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 862JX
UT WOS:000298088100029
ER
PT J
AU Hartmann, M
Debattista, VP
Seth, A
Cappellari, M
Quinn, TR
AF Hartmann, Markus
Debattista, Victor P.
Seth, Anil
Cappellari, Michele
Quinn, Thomas R.
TI Constraining the role of star cluster mergers in nuclear cluster
formation: simulations confront integral-field data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: kinematics and dynamics; galaxies:
structure
ID EARLY-TYPE GALAXIES; MASS BLACK-HOLE; SPACE-TELESCOPE OBSERVATIONS;
SURFACE BRIGHTNESS PROFILES; MULTI-GAUSSIAN EXPANSION; DWARF ELLIPTIC
GALAXIES; INNER GALACTIC REGIONS; TO-LIGHT RATIO; SPIRAL GALAXIES;
VIRGO-CLUSTER
AB We present observations and dynamical models of the stellar nuclear clusters (NCs) at the centres of NGC 4244 and M33. We then compare these to an extensive set of simulations testing the importance of purely stellar dynamical mergers on the formation and growth of NCs. Mergers of star clusters are able to produce a wide variety of observed properties, including densities, structural scaling relations, shapes (including the presence of young discs) and even rapid rotation. None the less, difficulties remain, most notably that the second-order kinematic moment of the models is too centrally peaked to match observations. This can be partially remedied by the merger of star clusters on to a pre-existing nuclear disc, but the line-of-sight velocity V is still more slowly rising than in NGC 4244. Our results therefore suggest that purely stellar dynamical mergers cannot form NCs and that gas dissipation is a necessary ingredient for at least similar to 50 per cent of a NCs mass. The negative vertical anisotropy found in NGC 4244, however, requires at least 10 per cent of the mass to have been accreted as stars, since gas dissipation and in situ star formation leads to positive vertical anisotropy.
C1 [Hartmann, Markus; Debattista, Victor P.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Seth, Anil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cappellari, Michele] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Quinn, Thomas R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
RP Hartmann, M (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
EM mhartmann@uclan.ac.uk; vpdebattista@uclan.ac.uk; aseth@cfa.harvard.edu;
cappellari@astro.ox.ac.uk; trq@astro.washington.edu
OI Cappellari, Michele/0000-0002-1283-8420
FU STFC; BIS; Royal Society
FX Part of the simulations in this paper were performed on the COSMOS
Consortium supercomputer within the DIRAC Facility jointly funded by
STFC, the Large Facilities Capital Fund of BIS. Simulations have also
been run at the Arctic Region Supercomputing Center (ARSC) and the High
Performance Computer Facility at the University of Central Lancashire.
We thank Jerry Sellwood for providing us with the multi-mass bulge model
and Jakob Walcher for providing us with his observational data. MH
thanks Chris Brook and Rok Roskar for their support and help. MC
acknowledges support from a Royal Society University Research
Fellowship. We thank Nate Bastian and the anonymous referee for
constructive comments.
NR 117
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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 DEC
PY 2011
VL 418
IS 4
BP 2697
EP 2714
DI 10.1111/j.1365-2966.2011.19659.x
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 862JX
UT WOS:000298088100049
ER
PT J
AU Abergel, A
Ade, PAR
Aghanim, N
Arnaud, M
Ashdown, M
Aumont, J
Baccigalupi, C
Balbi, A
Banday, AJ
Barreiro, RB
Bartlett, JG
Battaner, E
Benabed, K
Benoit, A
Bernard, JP
Bersanelli, M
Bhatia, R
Bock, JJ
Bonaldi, A
Bond, JR
Borrill, J
Bouchet, FR
Boulanger, F
Bucher, M
Burigana, C
Cabella, P
Cardoso, JF
Catalano, A
Cayon, L
Challinor, A
Chamballu, A
Chiang, LY
Chiang, C
Christensen, PR
Colombi, S
Couchot, F
Coulais, A
Crill, BP
Cuttaia, F
Dame, TM
Danese, L
Davies, RD
Davis, RJ
de Bernardis, P
de Gasperis, G
de Rosa, A
de Zotti, G
Delabrouille, J
Delouis, JM
Desert, FX
Dickinson, C
Donzelli, S
Dore, O
Dorl, U
Douspis, M
Dupac, X
Efstathiou, G
Ensslin, TA
Finelli, F
Forni, O
Frailis, M
Franceschi, E
Galeotta, S
Ganga, K
Giard, M
Giardino, G
Giraud-Heraud, Y
Gonzalez-Nuevo, J
Gorski, KM
Gratton, S
Gregorio, A
Grenier, IA
Gruppuso, A
Hansen, FK
Harrison, D
Henrot-Versille, S
Herranz, D
Hildebrandt, SR
Hivon, E
Hobson, M
Holmes, WA
Hovest, W
Hoyland, RJ
Huffenberger, KM
Jaffe, TR
Jaffe, AH
Jones, WC
Juvela, M
Keihanen, E
Keskitalo, R
Kisner, TS
Kneissl, R
Knox, L
Kurki-Suonio, H
Lagache, G
Lahteenmaki, A
Lamarre, JM
Lasenby, A
Laureijs, RJ
Lawrence, CR
Leach, S
Leonardi, R
Leroy, C
Lilje, PB
Linden-Vornle, M
Lopez-Caniego, M
Lubin, PM
Macias-Perez, JF
MacTavish, CJ
Maffei, B
Mandolesi, N
Mann, R
Maris, M
Marshall, DJ
Martinez-Gonzalez, E
Masi, S
Matarrese, S
Matthai, F
Mazzotta, P
McGehee, P
Meinhold, PR
Melchiorri, A
Mendes, L
Mennella, A
Miville-Deschenes, MA
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Murphy, A
Naselsky, P
Natoli, P
Netterfield, CB
Norgaard-Nielsen, HU
Noviello, F
Novikov, D
Novikov, I
Osborne, S
Pajot, F
Paladini, R
Pasian, F
Patanchon, G
Perdereau, O
Perotto, L
Perrotta, F
Piacentini, F
Piat, M
Plaszczynski, S
Pointecouteau, E
Polenta, G
Ponthieu, N
Poutanen, T
Prezeau, G
Prunet, S
Puget, JL
Rachen, JP
Reach, WT
Rebolo, R
Reich, W
Renault, C
Ricciardi, S
Riller, T
Ristorcelli, I
Rocha, G
Rosset, C
Rubino-Martin, JA
Rusholme, B
Sandri, M
Santos, D
Savini, G
Scott, D
Seiffert, MD
Shellard, P
Smoot, GF
Starck, JL
Stivoli, F
Stolyarov, V
Stompor, R
Sudiwala, R
Sygnet, JF
Tauber, JA
Terenzi, L
Toffolatti, L
Tomasi, M
Torre, JP
Tristram, M
Tuovinen, J
Umana, G
Valenziano, L
Varis, J
Vielva, P
Villa, F
Vittorio, N
Wade, LA
Wandelt, BD
Wilkinson, A
Ysard, N
Yvon, D
Zacchei, A
Zonca, A
AF Abergel, A.
Ade, P. A. R.
Aghanim, N.
Arnaud, M.
Ashdown, M.
Aumont, J.
Baccigalupi, C.
Balbi, A.
Banday, A. J.
Barreiro, R. B.
Bartlett, J. G.
Battaner, E.
Benabed, K.
Benoit, A.
Bernard, J-P
Bersanelli, M.
Bhatia, R.
Bock, J. J.
Bonaldi, A.
Bond, J. R.
Borrill, J.
Bouchet, F. R.
Boulanger, F.
Bucher, M.
Burigana, C.
Cabella, P.
Cardoso, J-F
Catalano, A.
Cayon, L.
Challinor, A.
Chamballu, A.
Chiang, L-Y
Chiang, C.
Christensen, P. R.
Colombi, S.
Couchot, F.
Coulais, A.
Crill, B. P.
Cuttaia, F.
Dame, T. M.
Danese, L.
Davies, R. D.
Davis, R. J.
de Bernardis, P.
de Gasperis, G.
de Rosa, A.
de Zotti, G.
Delabrouille, J.
Delouis, J-M
Desert, F-X
Dickinson, C.
Donzelli, S.
Dore, O.
Doerl, U.
Douspis, M.
Dupac, X.
Efstathiou, G.
Ensslin, T. A.
Finelli, F.
Forni, O.
Frailis, M.
Franceschi, E.
Galeotta, S.
Ganga, K.
Giard, M.
Giardino, G.
Giraud-Heraud, Y.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gratton, S.
Gregorio, A.
Grenier, I. A.
Gruppuso, A.
Hansen, F. K.
Harrison, D.
Henrot-Versille, S.
Herranz, D.
Hildebrandt, S. R.
Hivon, E.
Hobson, M.
Holmes, W. A.
Hovest, W.
Hoyland, R. J.
Huffenberger, K. M.
Jaffe, T. R.
Jaffe, A. H.
Jones, W. C.
Juvela, M.
Keihaenen, E.
Keskitalo, R.
Kisner, T. S.
Kneissl, R.
Knox, L.
Kurki-Suonio, H.
Lagache, G.
Lahteenmaki, A.
Lamarre, J-M
Lasenby, A.
Laureijs, R. J.
Lawrence, C. R.
Leach, S.
Leonardi, R.
Leroy, C.
Lilje, P. B.
Linden-Vornle, M.
Lopez-Caniego, M.
Lubin, P. M.
Macias-Perez, J. F.
MacTavish, C. J.
Maffei, B.
Mandolesi, N.
Mann, R.
Maris, M.
Marshall, D. J.
Martinez-Gonzalez, E.
Masi, S.
Matarrese, S.
Matthai, F.
Mazzotta, P.
McGehee, P.
Meinhold, P. R.
Melchiorri, A.
Mendes, L.
Mennella, A.
Miville-Deschenes, M-A
Moneti, A.
Montier, L.
Morgante, G.
Mortlock, D.
Munshi, D.
Murphy, A.
Naselsky, P.
Natoli, P.
Netterfield, C. B.
Norgaard-Nielsen, H. U.
Noviello, F.
Novikov, D.
Novikov, I.
Osborne, S.
Pajot, F.
Paladini, R.
Pasian, F.
Patanchon, G.
Perdereau, O.
Perotto, L.
Perrotta, F.
Piacentini, F.
Piat, M.
Plaszczynski, S.
Pointecouteau, E.
Polenta, G.
Ponthieu, N.
Poutanen, T.
Prezeau, G.
Prunet, S.
Puget, J-L
Rachen, J. P.
Reach, W. T.
Rebolo, R.
Reich, W.
Renault, C.
Ricciardi, S.
Riller, T.
Ristorcelli, I.
Rocha, G.
Rosset, C.
Rubino-Martin, J. A.
Rusholme, B.
Sandri, M.
Santos, D.
Savini, G.
Scott, D.
Seiffert, M. D.
Shellard, P.
Smoot, G. F.
Starck, J-L
Stivoli, F.
Stolyarov, V.
Stompor, R.
Sudiwala, R.
Sygnet, J-F
Tauber, J. A.
Terenzi, L.
Toffolatti, L.
Tomasi, M.
Torre, J-P
Tristram, M.
Tuovinen, J.
Umana, G.
Valenziano, L.
Varis, J.
Vielva, P.
Villa, F.
Vittorio, N.
Wade, L. A.
Wandelt, B. D.
Wilkinson, A.
Ysard, N.
Yvon, D.
Zacchei, A.
Zonca, A.
CA Planck Collaboration
TI Planck early results. XXI. Properties of the interstellar medium in the
Galactic plane
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: general; Galaxy: general; radio continuum: ISM; submillimeter: ISM;
infrared: ISM; radiation mechanisms: general
ID MICROWAVE-ANISOTROPY-PROBE; SPINNING DUST EMISSION; GAMMA-RAY EMISSION;
MILKY-WAY; FOREGROUND EMISSION; INFRARED-EMISSION; WMAP OBSERVATIONS;
MOLECULAR CLOUDS; EXCESS EMISSION; HII-REGIONS
AB Planck has observed the entire sky from 30 GHz to 857 GHz. The observed foreground emission contains contributions from different phases of the interstellar medium (ISM). We have separated the observed Galactic emission into the different gaseous components (atomic, molecular and ionised) in each of a number of Galactocentric rings. This technique provides the necessary information to study dust properties (emissivity, temperature, etc.), as well as other emission mechanisms as a function of Galactic radius. Templates are created for various Galactocentric radii using velocity information from atomic (neutral hydrogen) and molecular ((CO)-C-12) observations. The ionised template is assumed to be traced by free-free emission as observed by WMAP, while 408 MHz emission is used to trace the synchrotron component. Gas emission not traced by the above templates, namely "dark gas", as evidenced using Planck data, is included as an additional template, the first time such a component has been used in this way. These templates are then correlated with each of the Planck frequency bands, as well as with higher frequency data from IRAS and DIRBE along with radio data at 1.4 GHz. The emission per column density of the gas templates allows us to create distinct spectral energy distributions (SEDs) per Galactocentric ring and in each of the gaseous tracers from 1.4 GHz to 25 THz (12 mu m). The resulting SEDs allow us to explore the contribution of various emission mechanisms to the Planck signal. Apart from the thermal dust and free-free emission, we have probed the Galaxy for anomalous (e.g., spinning) dust as well as synchrotron emission. We find the dust opacity in the solar neighbourhood, tau/N-H = 0.92 +/- 0.05x10(-25) cm(2) at 250 mu m, with no significant variation with Galactic radius, even though the dust temperature is seen to vary from over 25 K to under 14 K. Furthermore, we show that anomalous dust emission is present in the atomic, molecular and dark gas phases throughout the Galactic disk. Anomalous emission is not clearly detected in the ionised phase, as free-free emission is seen to dominate. The derived dust propeties associated with the dark gas phase are derived but do not allow us to reveal the nature of this phase. For all environments, the anomalous emission is consistent with rotation from polycyclic aromatic hydrocarbons (PAHs) and, according to our simple model, accounts for (25 +/- 5)% (statistical) of the total emission at 30 GHz.
C1 [Banday, A. J.; Bernard, J-P; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP IRAP, F-31028 Toulouse 4, France.
[Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, ESRIN, Frascati, Italy.
[Bartlett, J. G.; Bucher, M.; Cardoso, J-F; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.; Stompor, R.] Univ Paris 07, CNRS, UMR7164, Paris, France.
[Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Astrophys Grp, Cavendish Lab, Cambridge CB3 0HE, England.
[Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile.
[Bond, J. R.; Miville-Deschenes, M-A] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Banday, A. J.; Bernard, J-P; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; Marshall, D. J.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway.
[Challinor, A.; Shellard, P.] Univ Cambridge, Ctr Math Sci, DAMTP, Cambridge CB3 0WA, England.
[Starck, J-L; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France.
[Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark.
[Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
[Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Juvela, M.; Keihaenen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.; Ysard, N.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Leonardi, R.; Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
[Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Bersanelli, M.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy.
[Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy.
[Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark.
[Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain.
[Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile.
[Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Sci Off, Madrid, Spain.
[Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands.
[Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland.
[Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy.
[Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy.
[Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Bologna, Italy.
[Bersanelli, M.; Donzelli, S.; Tomasi, M.] INAF IASF Milano, Milan, Italy.
[Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France.
[Desert, F-X] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France.
[Chamballu, A.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England.
[Ganga, K.; McGehee, P.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Benoit, A.] Univ Grenoble 1, Inst Neel, CNRS, F-38041 Grenoble, France.
[Abergel, A.; Aghanim, N.; Aumont, J.; Boulanger, F.; Douspis, M.; Lagache, G.; Leroy, C.; Miville-Deschenes, M-A; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J-L; Torre, J-P] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France.
[Benabed, K.; Bouchet, F. R.; Cardoso, J-F; Colombi, S.; Delouis, J-M; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J-F; Wandelt, B. D.] Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, Paris, France.
[Chiang, L-Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Donzelli, S.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Hildebrandt, S. R.; Hoyland, R. J.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain.
[Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain.
[Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Wilkinson, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Catalano, A.; Coulais, A.; Lamarre, J-M] Observ Paris, LERMA, CNRS, F-75014 Paris, France.
[Arnaud, M.; Grenier, I. A.; Starck, J-L] Univ Paris Diderot, Lab AIM, IRFU Serv Astrophys, CEA DSM,CNRS,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Cardoso, J-F] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France.
[Cardoso, J-F] Telecom ParisTech, F-75634 Paris 13, France.
[Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 Grenoble, France.
[Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, Lab Accelerateur Lineaire, CNRS IN2P3, F-91405 Orsay, France.
[Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Rachen, J. P.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland.
[Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland.
[Savini, G.] UCL, Opt Sci Lab, London, England.
[Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Mann, R.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA.
[Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA.
[Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain.
[Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Marshall, DJ (reprint author), Univ Toulouse, UPS OMP IRAP, F-31028 Toulouse 4, France.
EM douglas.marshall@irap.omp.eu
RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015;
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Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov,
Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta,
Pasquale/B-1225-2016; Gregorio, Anna/J-1632-2012; Lopez-Caniego,
Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014; Lahteenmaki,
Anne/L-5987-2013; Vielva, Patricio/F-6745-2014; Toffolatti,
Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Battaner,
Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon,
Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Lilje,
Per/A-2699-2012; de Gasperis, Giancarlo/C-8534-2012
OI Huffenberger, Kevin/0000-0001-7109-0099; Burigana,
Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924;
Ricciardi, Sara/0000-0002-3807-4043; Villa,
Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115;
TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794;
WANDELT, Benjamin/0000-0002-5854-8269; Finelli,
Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott,
Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135;
Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio,
Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri,
Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; de
Bernardis, Paolo/0000-0001-6547-6446; Forni,
Olivier/0000-0001-6772-9689; Morgante, Gianluca/0000-0001-9234-7412;
Maris, Michele/0000-0001-9442-2754; Franceschi,
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NR 89
TC 76
Z9 76
U1 0
U2 7
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 DEC
PY 2011
VL 536
AR A21
DI 10.1051/0004-6361/201116455
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100022
ER
PT J
AU Ade, PAR
Aghanim, N
Arnaud, M
Ashdown, M
Aumont, J
Baccigalupi, C
Balbi, A
Banday, AJ
Barreiro, RB
Bartlett, JG
Battaner, E
Benabed, K
Benoit, A
Bernard, JP
Bersanelli, M
Bhatia, R
Bock, JJ
Bonaldi, A
Bond, JR
Borrill, J
Bouchet, FR
Boulanger, F
Bucher, M
Burigana, C
Cabella, P
Cardoso, JF
Catalano, A
Cayon, L
Challinor, A
Chamballu, A
Chiang, LY
Chiang, C
Christensen, PR
Clements, DL
Colombi, S
Couchot, F
Coulais, A
Crill, BP
Cuttaia, F
Dame, TM
Danese, L
Davies, RD
Davis, RJ
de Bernardis, P
de Gasperis, G
de Rosa, A
de Zotti, G
Delabrouille, J
Delouis, JM
Desert, FX
Dickinson, C
Dobashi, K
Donzelli, S
Dore, O
Dorl, U
Douspis, M
Dupac, X
Efstathiou, G
Ensslin, TA
Eriksen, HK
Falgarone, E
Finelli, F
Forni, O
Fosalba, P
Frailis, M
Franceschi, E
Fukui, Y
Galeotta, S
Ganga, K
Giard, M
Giardino, G
Giraud-Heraud, Y
Gonzalez-Nuevo, J
Gorski, KM
Gratton, S
Gregorio, A
Grenier, IA
Gruppuso, A
Hansen, FK
Harrison, D
Helou, G
Henrot-Versille, S
Herranz, D
Hildebrandt, SR
Hivon, E
Hobson, M
Holmes, WA
Hovest, W
Hoyland, RJ
Huffenberger, KM
Jaffe, AH
Jones, WC
Juvela, M
Kawamura, A
Keihanen, E
Keskitalo, R
Kisner, TS
Kneissl, R
Knox, L
Kurki-Suonio, H
Lagache, G
Lamarre, JM
Lasenby, A
Laureijs, RJ
Lawrence, CR
Leach, S
Leonardi, R
Leroy, C
Lilje, PB
Linden-Vornle, M
Lopez-Caniego, M
Lubin, PM
Macias-Perez, JF
MacTavish, CJ
Maffei, B
Maino, D
Mandolesi, N
Mann, R
Maris, M
Martin, P
Martinez-Gonzalez, E
Masi, S
Matarrese, S
Matthai, F
Mazzotta, P
McGehee, P
Meinhold, PR
Melchiorri, A
Mendes, L
Mennella, A
Miville-Deschenes, MA
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Murphy, A
Naselsky, P
Natoli, P
Netterfield, CB
Norgaard-Nielsen, HU
Noviello, F
Novikov, D
Novikov, I
O'Dwyer, IJ
Onishi, T
Osborne, S
Pajot, F
Paladini, R
Paradis, D
Pasian, F
Patanchon, G
Perdereau, O
Perotto, L
Perrotta, F
Piacentini, F
Piat, M
Plaszczynski, S
Pointecouteau, E
Polenta, G
Ponthieu, N
Poutanen, T
Prezeau, G
Prunet, S
Puget, JL
Reach, WT
Reinecke, M
Renault, C
Ricciardi, S
Riller, T
Ristorcelli, I
Rocha, G
Rosset, C
Rowan-Robinson, M
Rubino-Martin, JA
Rusholme, B
Sandri, M
Santos, D
Savini, G
Scott, D
Seiffert, MD
Shellard, P
Smoot, GF
Starck, JL
Stivoli, F
Stolyarov, V
Stompor, R
Sudiwala, R
Sygnet, JF
Tauber, JA
Terenzi, L
Toffolatti, L
Tomasi, M
Torre, JP
Tristram, M
Tuovinen, J
Umana, G
Valenziano, L
Vielva, P
Villa, F
Vittorio, N
Wade, LA
Wandelt, BD
Wilkinson, A
Yvon, D
Zacchei, A
Zonca, A
AF Ade, P. A. R.
Aghanim, N.
Arnaud, M.
Ashdown, M.
Aumont, J.
Baccigalupi, C.
Balbi, A.
Banday, A. J.
Barreiro, R. B.
Bartlett, J. G.
Battaner, E.
Benabed, K.
Benoit, A.
Bernard, J. -P.
Bersanelli, M.
Bhatia, R.
Bock, J. J.
Bonaldi, A.
Bond, J. R.
Borrill, J.
Bouchet, F. R.
Boulanger, F.
Bucher, M.
Burigana, C.
Cabella, P.
Cardoso, J. -F.
Catalano, A.
Cayon, L.
Challinor, A.
Chamballu, A.
Chiang, L. -Y
Chiang, C.
Christensen, P. R.
Clements, D. L.
Colombi, S.
Couchot, F.
Coulais, A.
Crill, B. P.
Cuttaia, F.
Dame, T. M.
Danese, L.
Davies, R. D.
Davis, R. J.
de Bernardis, P.
de Gasperis, G.
de Rosa, A.
de Zotti, G.
Delabrouille, J.
Delouis, J. -M.
Desert, F. -X.
Dickinson, C.
Dobashi, K.
Donzelli, S.
Dore, O.
Doerl, U.
Douspis, M.
Dupac, X.
Efstathiou, G.
Ensslin, T. A.
Eriksen, H. K.
Falgarone, E.
Finelli, F.
Forni, O.
Fosalba, P.
Frailis, M.
Franceschi, E.
Fukui, Y.
Galeotta, S.
Ganga, K.
Giard, M.
Giardino, G.
Giraud-Heraud, Y.
Gonzalez-Nuevo, J.
Gorski, K. M.
Gratton, S.
Gregorio, A.
Grenier, I. A.
Gruppuso, A.
Hansen, F. K.
Harrison, D.
Helou, G.
Henrot-Versille, S.
Herranz, D.
Hildebrandt, S. R.
Hivon, E.
Hobson, M.
Holmes, W. A.
Hovest, W.
Hoyland, R. J.
Huffenberger, K. M.
Jaffe, A. H.
Jones, W. C.
Juvela, M.
Kawamura, A.
Keihanen, E.
Keskitalo, R.
Kisner, T. S.
Kneissl, R.
Knox, L.
Kurki-Suonio, H.
Lagache, G.
Lamarre, J. -M.
Lasenby, A.
Laureijs, R. J.
Lawrence, C. R.
Leach, S.
Leonardi, R.
Leroy, C.
Lilje, P. B.
Linden-Vornle, M.
Lopez-Caniego, M.
Lubin, P. M.
Macias-Perez, J. F.
MacTavish, C. J.
Maffei, B.
Maino, D.
Mandolesi, N.
Mann, R.
Maris, M.
Martin, P.
Martinez-Gonzalez, E.
Masi, S.
Matarrese, S.
Matthai, F.
Mazzotta, P.
McGehee, P.
Meinhold, P. R.
Melchiorri, A.
Mendes, L.
Mennella, A.
Miville-Deschenes, M. -A.
Moneti, A.
Montier, L.
Morgante, G.
Mortlock, D.
Munshi, D.
Murphy, A.
Naselsky, P.
Natoli, P.
Netterfield, C. B.
Norgaard-Nielsen, H. U.
Noviello, F.
Novikov, D.
Novikov, I.
O'Dwyer, I. J.
Onishi, T.
Osborne, S.
Pajot, F.
Paladini, R.
Paradis, D.
Pasian, F.
Patanchon, G.
Perdereau, O.
Perotto, L.
Perrotta, F.
Piacentini, F.
Piat, M.
Plaszczynski, S.
Pointecouteau, E.
Polenta, G.
Ponthieu, N.
Poutanen, T.
Prezeau, G.
Prunet, S.
Puget, J. -L.
Reach, W. T.
Reinecke, M.
Renault, C.
Ricciardi, S.
Riller, T.
Ristorcelli, I.
Rocha, G.
Rosset, C.
Rowan-Robinson, M.
Rubino-Martin, J. A.
Rusholme, B.
Sandri, M.
Santos, D.
Savini, G.
Scott, D.
Seiffert, M. D.
Shellard, P.
Smoot, G. F.
Starck, J. -L.
Stivoli, F.
Stolyarov, V.
Stompor, R.
Sudiwala, R.
Sygnet, J. -F.
Tauber, J. A.
Terenzi, L.
Toffolatti, L.
Tomasi, M.
Torre, J. -P.
Tristram, M.
Tuovinen, J.
Umana, G.
Valenziano, L.
Vielva, P.
Villa, F.
Vittorio, N.
Wade, L. A.
Wandelt, B. D.
Wilkinson, A.
Yvon, D.
Zacchei, A.
Zonca, A.
CA Planck Collaboration
TI Planck early results. XIX. All-sky temperature and dust optical depth
from Planck and IRAS. Constraints on the "dark gas" in our Galaxy
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE dust, extinction; ISM: clouds; evolution; solar neighborhood; Galaxy:
general; submillimeter: ISM
ID GALACTIC MOLECULAR CLOUDS; SENSITIVITY HI SURVEY; FINAL DATA RELEASE;
MILKY-WAY; INTERSTELLAR-MEDIUM; MAGELLANIC-CLOUD; INFRARED CIRRUS;
SPITZER SURVEY; OUTER GALAXY; GOULD BELT
AB An all sky map of the apparent temperature and optical depth of thermal dust emission is constructed using the Planck-HFI (350 mu m to 2 mm) and IRAS (100 mu m) data. The optical depth maps are correlated with tracers of the atomic (H I) and molecular gas traced by CO. The correlation with the column density of observed gas is linear in the lowest column density regions at high Galactic latitudes. At high N-H, the correlation is consistent with that of the lowest N-H, for a given choice of the CO-to-H-2 conversion factor. In the intermediate N-H range, a departure from linearity is observed, with the dust optical depth in excess of the correlation. This excess emission is attributed to thermal emission by dust associated with a dark gas phase, undetected in the available H I and CO surveys. The 2D spatial distribution of the dark gas in the solar neighbourhood (vertical bar b(II)vertical bar > 10 degrees) is shown to extend around known molecular regions traced by CO. The average dust emissivity in the H I phase in the solar neighbourhood is found to be tau(D)/N-H(tot) = 5.2 x 10(-26) cm(2) at 857 GHz. It follows roughly a power law distribution with a spectral index beta = 1.8 all the way down to 3 mm, although the SED flattens slightly in the millimetre. Taking into account the spectral shape of the dust optical depth, the emissivity is consistent with previous values derived from FIRAS measurements at high latitudes within 10%. The threshold for the existence of the dark gas is found at N-H(tot) = (8.0 +/- 0.58) x 10(20) H cm(-2) (A(V) = 0.4 mag). Assuming the same high frequency emissivity for the dust in the atomic and the molecular phases leads to an average X-CO = (2.54 +/- 0.13) x 10(20) H-2 cm(-2)/(K km s(-1)). The mass of dark gas is found to be 28% of the atomic gas and 118% of the CO emitting gas in the solar neighbourhood. The Galactic latitude distribution shows that its mass fraction is relatively constant down to a few degrees from the Galactic plane. A possible explanation for the dark gas lies in a dark molecular phase, where H-2 survives photodissociation but CO does not. The observed transition for the onset of this phase in the solar neighbourhood (A(V) = 0.4 mag) appears consistent with recent theoretical predictions. It is also possible that up to half of the dark gas could be in atomic form, due to optical depth effects in the Hi measurements.
C1 [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Montier, L.; Paradis, D.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS, OMP, IRAP, F-31028 Toulouse 4, France.
[Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
[Natoli, P.; Polenta, G.] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy.
[Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Catalano, A.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Smoot, G. F.; Stompor, R.] Univ Paris 07, CNRS, UMR7164, Paris, France.
[Ashdown, M.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England.
[Bhatia, R.; Kneissl, R.] ALMA Santiago Cent Off, Santiago, Chile.
[Bond, J. R.; Martin, P.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada.
[Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada.
[Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Leroy, C.; Montier, L.; Paradis, D.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Ganga, K.; McGehee, P.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Bartlett, J. G.; Bock, J. J.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Keskitalo, R.; Lawrence, C. R.; O'Dwyer, I. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Lilje, P. B.] Univ Oslo, Ctr Math Applicat, Oslo, Norway.
[Donzelli, S.; Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway.
[Challinor, A.; Shellard, P.] Univ Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England.
[Starck, J. -L.; Yvon, D.] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France.
[Linden-Vornle, M.; Norgaard-Nielsen, H. U.] Natl Space Inst, DTU Space, Copenhagen, Denmark.
[Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain.
[Dobashi, K.] Tokyo Gakugei Univ, Dept Astron & Earth Sci, Tokyo 1848501, Japan.
[Onishi, T.] Osaka Prefecture Univ, Dept Phys Sci, Grad Sch Sci, Naka Ku, Sakai, Osaka 5998531, Japan.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Juvela, M.; Keihanen, E.; Keskitalo, R.; Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Fukui, Y.; Kawamura, A.] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Chiang, C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Cayon, L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Smoot, G. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Leonardi, R.; Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA.
[Matarrese, S.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[de Bernardis, P.; Masi, S.; Melchiorri, A.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy.
[Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy.
[Natoli, P.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Balbi, A.; Cabella, P.; de Gasperis, G.; Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy.
[Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark.
[Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain.
[Kneissl, R.] European So Observ, ESO Vitacura, Santiago 19, Chile.
[Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain.
[Giardino, G.; Laureijs, R. J.; Leonardi, R.; Tauber, J. A.] Estec, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands.
[Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kurki-Suonio, H.; Poutanen, T.] Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland.
[Umana, G.] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy.
[Bonaldi, A.; de Zotti, G.] Osserv Astron Padova, INAF, Padua, Italy.
[Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Frailis, M.; Galeotta, S.; Maris, M.; Mennella, A.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy.
[Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, Bologna, Italy.
[Bersanelli, M.; Donzelli, S.; Maino, D.; Tomasi, M.] IASF Milano, INAF, Milan, Italy.
[Stivoli, F.] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France.
[Desert, F. -X.] Univ Grenoble 1, CNRS, IPAG, INSU,UMR 5274, F-38041 Grenoble, France.
[Chamballu, A.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France.
[Aghanim, N.; Aumont, J.; Boulanger, F.; Douspis, M.; Lagache, G.; Leroy, C.; Miville-Deschenes, M. -A.; Noviello, F.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Torre, J. -P.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
[Benabed, K.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, Paris, France.
[Fosalba, P.] Fac Ciencies, Inst Ciencies Espai, CSIC, IEEC, Bellaterra 08193, Spain.
[Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Munshi, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Hildebrandt, S. R.; Hoyland, R. J.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain.
[Barreiro, R. B.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, Inst Fis Cantabria, CSIC, E-39005 Santander, Spain.
[Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Wilkinson, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England.
[Catalano, A.; Coulais, A.; Falgarone, E.; Lamarre, J. -M.] Observ Paris, LERMA, CNRS, F-75014 Paris, France.
[Arnaud, M.; Grenier, I. A.; Starck, J. -L.] Univ Paris Diderot, Lab AIM, IRFU, Serv Astrophys,CEA,DSM,CNRS,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France.
[Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France.
[Hildebrandt, S. R.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, CNRS, IN2P3,Inst Natl Polytech Grenoble, F-38026 Grenoble, France.
[Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, Lab Accelerateur Lineaire, IN2P3, F-91405 Orsay, France.
[Borrill, J.; Kisner, T. S.; Smoot, G. F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Banday, A. J.; Doerl, U.; Ensslin, T. A.; Hovest, W.; Matthai, F.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo, Finland.
[Murphy, A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland.
[Savini, G.] UCL, Opt Sci Lab, London, England.
[Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy.
[Mann, R.] Univ Edinburgh, SUPA, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Paladini, R.] Spitzer Sci Ctr, Pasadena, CA USA.
[Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA.
[Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain.
[Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA.
[Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
RP Bernard, JP (reprint author), Univ Toulouse, UPS, OMP, IRAP, F-31028 Toulouse 4, France.
EM Jean-Philippe.Bernard@cesr.fr
RI Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016;
Tomasi, Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov,
Igor/N-5098-2015; Piacentini, Francesco/E-7234-2010; Novikov,
Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Mazzotta,
Pasquale/B-1225-2016; Herranz, Diego/K-9143-2014; Battaner,
Eduardo/P-7019-2014; Barreiro, Rita Belen/N-5442-2014; Yvon,
Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015;
Gonzalez-Nuevo, Joaquin/I-3562-2014; Lilje, Per/A-2699-2012; de
Gasperis, Giancarlo/C-8534-2012; Gregorio, Anna/J-1632-2012;
Lopez-Caniego, Marcos/M-4695-2013; Bouchet, Francois/B-5202-2014;
Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014;
OI WANDELT, Benjamin/0000-0002-5854-8269; Finelli,
Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Frailis,
Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283;
Gregorio, Anna/0000-0003-4028-8785; Polenta,
Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375;
Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger,
Kevin/0000-0001-7109-0099; Scott, Douglas/0000-0002-6878-9840; Masi,
Silvia/0000-0001-5105-1439; Forni, Olivier/0000-0001-6772-9689;
Morgante, Gianluca/0000-0001-9234-7412; Maris,
Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591;
Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227;
Gruppuso, Alessandro/0000-0001-9272-5292; Kurki-Suonio,
Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131;
Piacentini, Francesco/0000-0002-5444-9327; Stolyarov,
Vladislav/0000-0001-8151-828X; Mazzotta, Pasquale/0000-0002-5411-1748;
de Bernardis, Paolo/0000-0001-6547-6446; Rubino-Martin, Jose
Alberto/0000-0001-5289-3021; Valenziano, Luca/0000-0002-1170-0104;
Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita
Belen/0000-0002-6139-4272; Martinez-Gonzalez,
Enrique/0000-0002-0179-8590; Gonzalez-Nuevo,
Joaquin/0000-0003-1354-6822; de Gasperis, Giancarlo/0000-0003-2899-2171;
Vielva, Patricio/0000-0003-0051-272X; Toffolatti,
Luigi/0000-0003-2645-7386; Reach, William/0000-0001-8362-4094; Zacchei,
Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje,
Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416; Burigana,
Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa,
Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115;
TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794
NR 87
TC 158
Z9 158
U1 0
U2 13
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 DEC
PY 2011
VL 536
AR A19
DI 10.1051/0004-6361/201116479
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100020
ER
PT J
AU Robitaille, TP
AF Robitaille, T. P.
TI HYPERION: an open-source parallelized three-dimensional dust continuum
radiative transfer code
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE methods: numerical; radiative transfer; scattering; polarization
ID HERBIG AE/BE STARS; PROTOSTELLAR ENVELOPES; CIRCUMSTELLAR DISKS;
KEPLERIAN DISKS; DIRTY MODEL; SCATTERING; GRAINS; POLARIZATION;
SIMULATIONS; MOCASSIN
AB HYPERION is a new three-dimensional dust continuum Monte-Carlo radiative transfer code that is designed to be as generic as possible, allowing radiative transfer to be computed through a variety of three-dimensional grids. The main part of the code is problem-independent, and only requires an arbitrary three-dimensional density structure, dust properties, the position and properties of the illuminating sources, and parameters controlling the running and output of the code. HYPERION is parallelized, and is shown to scale well to thousands of processes. Two common benchmark models for protoplanetary disks were computed, and the results are found to be in excellent agreement with those from other codes. Finally, to demonstrate the capabilities of the code, dust temperatures, SEDs, and synthetic multi-wavelength images were computed for a dynamical simulation of a low-mass star formation region. HYPERION is being actively developed to include new features, and is publicly available(star star).
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Robitaille, TP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM trobitaille@cfa.harvard.edu
OI Robitaille, Thomas/0000-0002-8642-1329
FU NASA
FX I wish to thank the referee for a careful review and for comments that
helped improve this paper. I also wish to thank C. Pinte and I. Pascucci
for assistance with their respective disk benchmark problems, Stella
Offner for providing the star formation simulation and for useful
discussions and comments, and Barbara Whitney and Kenneth Wood for
helpful discussions and comments. The computations in this paper were
run on the Odyssey cluster supported by the FAS Sciences Division
Research Computing Group. The parallel performance tests were run using
0.7.7 of the code, while the benchmarks problems and the case study
model were computed using version 0.8.4. Support for this work was
provided by NASA through the Spitzer Space Telescope Fellowship Program,
through a contract issued by the Jet Propulsion Laboratory, California
Institute of Technology under a contract with NASA. This research has
made use of NASA's Astrophysics Data System. No photon packets were
harmed in the making of this paper.
NR 48
TC 51
Z9 52
U1 0
U2 6
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD DEC
PY 2011
VL 536
AR A79
DI 10.1051/0004-6361/201117150
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100119
ER
PT J
AU Rolffs, R
Schilke, P
Zhang, Q
Zapata, L
AF Rolffs, R.
Schilke, P.
Zhang, Q.
Zapata, L.
TI Structure of the hot molecular core G10.47+0.03
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: molecules; ISM: structure; ISM: clouds; stars: formation
ID MASSIVE STAR-FORMATION; CONTINUUM OBSERVATIONS; SUBMILLIMETER ARRAY;
COLOGNE DATABASE; HII-REGIONS; II REGIONS; SPECTROSCOPY; RESOLUTION;
CDMS; LINE
AB Context. The physical structure of hot molecular cores, where forming massive stars have heated up dense dust and gas, but have not yet ionized the molecules, poses a prominent challenge in the research of high-mass star formation and astrochemistry.
Aims. We aim at constraining the spatial distribution of density, temperature, velocity field, and chemical abundances in the hot molecular core G10.47+0.03.
Methods. With the SubMillimeter Array (SMA), we obtained high spatial and spectral resolution of a multitude of molecular lines at different frequencies, including at 690 GHz. At 345 GHz, our beam size is 0.3 '', corresponding to 3000 AU. We analyze the data using the three-dimensional dust and line radiative transfer code RADMC-3D for vibrationally excited HCN, and myXCLASS for line identification.
Results. We find hundreds of molecular lines from complex molecules and high excitations. Even vibrationally excited (HCN)-N-15 at 690 GHz is detected. The HCN abundance at high temperatures is very high, on the order of 10(-5) relative to H-2. Absorption against the dust continuum occurs in twelve transitions, whose shape implies an outflow along the line-of-sight. Outside the continuum peak, the line shapes are indicative of infall. Dust continuum and molecular line emission are resolved at 345/355 GHz, revealing central flattening and rapid radial falloff of the density outwards of 104 AU, best reproduced by a Plummer radial profile of the density. No fragmentation is detected, but modeling of the line shapes of vibrationally excited HCN suggests that the density is clumpy.
Conclusions. We conclude that G10.47+0.03 is characterized by beginning of feedback from massive stars, while infall is ongoing. High gas masses (hundreds of M-circle dot) are heated to high temperatures above 300 K, aided by diffusion of radiation in a high-column-density environment. The increased thermal, radiative, turbulent, and wind-driven pressure drives expansion in the central region and is very likely responsible for the central flattening of the density.
C1 [Rolffs, R.; Zapata, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Rolffs, R.; Schilke, P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zapata, L.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico.
RP Rolffs, R (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM rrolffs@mpifr.de; schilke@ph1.uni-koeln.de
OI Zhang, Qizhou/0000-0003-2384-6589
FU Smithsonian Institution; Academia Sinica; International Max Planck
Research School (IMPRS) for Astronomy and Astrophysics
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 (Ho et al. 2004).; We are grateful to Mark Gurwell for
his help with reducing the 690 GHz data, and to Kees Dullemond for
kindly providing us with the RADMC-3D code. R. Rolffs acknowledges
support from the International Max Planck Research School (IMPRS) for
Astronomy and Astrophysics.
NR 28
TC 7
Z9 7
U1 0
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 DEC
PY 2011
VL 536
AR A33
DI 10.1051/0004-6361/201117112
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 867WI
UT WOS:000298485100071
ER
PT J
AU David, B
Geneste, JM
Whear, RL
Delannoy, JJ
Katherine, M
Gunn, RG
Clarkson, C
Plisson, H
Lee, P
Petchey, F
Rowe, C
Barker, B
Lamb, L
Miller, W
Hoerle, S
James, D
Boche, E
Aplin, K
McNiven, IJ
Richards, T
Fairbairn, A
Matthews, J
AF David, Bruno
Geneste, Jean-Michel
Whear, Ray L.
Delannoy, Jean-Jacques
Katherine, Margaret
Gunn, R. G.
Clarkson, Christopher
Plisson, Hugues
Lee, Preston
Petchey, Fiona
Rowe, Cassandra
Barker, Bryce
Lamb, Lara
Miller, Wes
Hoerle, Stephane
James, Daniel
Boche, Elisa
Aplin, Ken
McNiven, Ian J.
Richards, Thomas
Fairbairn, Andrew
Matthews, Jacqueline
TI Nawarla Gabarnmang, a 45,180 +/- 910 cal BP Site in Jawoyn Country,
Southwest Arnhem Land Plateau
SO AUSTRALIAN ARCHAEOLOGY
LA English
DT Article
ID EARLY HUMAN OCCUPATION; NORTHERN-TERRITORY; AUSTRALIA; DATES
AB Recent excavations at Nawarla Gabarnmang in Jawoyn country, southwest Arnhem Land have produced a long sequence of AMS radiocarbon determinations on individual pieces of charcoal reliably associated with stone artefacts dating back to 45,180 +/- 910 cal BP. It represents one of the earliest radiocarbon-dated archaeological sites in Australia. Here we report on initial results.
C1 [David, Bruno; Rowe, Cassandra; James, Daniel; McNiven, Ian J.; Richards, Thomas] Monash Univ, Sch Geog & Environm Sci, Clayton, Vic 3800, Australia.
[Geneste, Jean-Michel; Boche, Elisa] Univ Bordeaux 1, UMR CNRS PACEA 5199, Ctr Natl Prehist, F-33405 Talence, France.
[Whear, Ray L.; Katherine, Margaret; Lee, Preston; Miller, Wes] Jawoyn Assoc Aboriginal Corp, Katherine, NT 0851, Australia.
[Delannoy, Jean-Jacques; Hoerle, Stephane] Univ Savoie, Ctr Interdisciplinaire Sci Montagne, EDYTEM UMR 5204, CNRS Environm Dynam & Terr Montagne, F-73376 Le Bourget Du Lac, France.
[Clarkson, Christopher; Fairbairn, Andrew; Matthews, Jacqueline] Univ Queensland, Sch Social Sci, Brisbane, Qld 4072, Australia.
[Plisson, Hugues] Univ Bordeaux 1, CNRS, UMR PACEA 5199, F-33405 Talence, France.
[Petchey, Fiona] Univ Waikato, Radiocarbon Dating Lab, Hamilton 3240, New Zealand.
[Barker, Bryce; Lamb, Lara] Univ So Queensland, Sch Humanities & Commun, Publ Memory Res Ctr, Toowoomba, Qld 4350, Australia.
[Aplin, Ken] Smithsonian Inst, Div Mammals, Washington, DC 20013 USA.
RP David, B (reprint author), Monash Univ, Sch Geog & Environm Sci, Clayton, Vic 3800, Australia.
EM bruno.david@monash.edu; jean-michel.geneste@culture.gouv.fr;
ray.whear@jawoyn.org; Jean-Jacques.Delannoy@univ-savoie.fr;
gunnb@activ8.net.au; c.clarkson@uq.edu.au;
hugues.plisson@u-bordeaux1.fr; preston.lee@jawoyn.org;
fpetchey@waikato.ac.nz; cassandra.rowe@monash.edu; barker@usq.edu.au;
lamb@usq.edu.au; wes.miller@jawoyn.org; stephane@rockart.wits.ac.za;
daniel.james@monash.edu; elisa.boche@laposte.net; aplin.ken@gmail.com;
ian.mcniven@monash.edu; thomas.richards@monash.edu;
a.fairbairn@uq.edu.au; jacqueline.matthews@uqconnect.edu.au
RI Matthews, Jacqueline/I-4959-2015; Rowe, Cassandra/M-6009-2015;
OI Matthews, Jacqueline/0000-0002-3968-8282; Rowe,
Cassandra/0000-0001-8938-5733; Clarkson, Chris/0000-0002-8938-8974;
David, Bruno/0000-0002-8567-6135
NR 16
TC 12
Z9 12
U1 0
U2 11
PU AUSTRALIAN ARCHAEOLOGICAL ASSOC INC
PI BRISBANE
PA C/O IAN LILLEY (SECRETARY), UNIT ABORIGINAL & TORRES STRAIT ISLANDER
STUDIES, UNIV OF QUEENSLAND, BRISBANE, QLD 4072, AUSTRALIA
SN 0312-2417
J9 AUST ARCHAEOL
JI Austral. Archaeol.
PD DEC
PY 2011
IS 73
BP 73
EP 77
PG 5
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA 872SD
UT WOS:000298828700012
ER
PT J
AU Prathapan, KD
Konstantinov, AS
AF Prathapan, K. D.
Konstantinov, A. S.
TI A NEW SPECIES-GROUP IN APHTHONA CHEVROLAT (COLEOPTERA: CHRYSOMELIDAE)
WITH A DESCRIPTION OF A NEW SPECIES FROM SOUTHERN INDIA
SO COLEOPTERISTS BULLETIN
LA English
DT Article
DE flea beetles; taxonomy; host plants; key to species-groups
AB A new species-group in the flea beetle genus Aphthona Chevrolat is defined and Aphthona yercaudensis Prathapan and Konstantinov, new species, from southern India is described. A key to Aphthona species-groups in the Oriental Region is provided. Herbaceous species of Phyllanthus L. (Euphorbiaceae) are recorded as the host plants of Aphthona bombayensis Scherer.
C1 [Prathapan, K. D.] Kerala Agr Univ, Dept Entomol, Trivandrum 695522, Kerala, India.
[Konstantinov, A. S.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
RP Prathapan, KD (reprint author), Kerala Agr Univ, Dept Entomol, Vellayani PO, Trivandrum 695522, Kerala, India.
EM prathapankd@gmail.com; alex.konstantinov@ars.usda.gov
FU Kerala State Council for Science, Technology and Environment, Trivandrum
FX We are indebted to Anoop P. Balan and A. K. Pradeep for the
identification of the host plants. PKD's work on flea beetles is
supported by the Kerala State Council for Science, Technology and
Environment, Trivandrum. An Ernst Mayr travel grant and a Smithsonian
short-term visitor grant enabled PKD to study the historic flea beetle
collections in the Natural History Museum, London, and the National
Museum of Natural History, Washington, DC. We thank Adelita Linzmeier
(Depto. Zoologia, Universidade Federal do Parana, Curitiba, Brazil),
Allen Norrbom, Jens Prena, and Norman Woodley (Systematic Entomology
Laboratory, USDA, ARS, Washington, DC), and two anonymous reviewers for
valuable comments and suggestions on an earlier version of this
manuscript. USDA is an equal opportunity provider and employer.
NR 8
TC 0
Z9 0
U1 0
U2 3
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 DEC
PY 2011
VL 65
IS 4
BP 329
EP 334
PG 6
WC Entomology
SC Entomology
GA 877NU
UT WOS:000299190000001
ER
PT J
AU Johnson, EI
Wolfe, JD
Ryder, TB
Pyle, P
AF Johnson, Erik I.
Wolfe, Jared D.
Ryder, T. Brandt
Pyle, Peter
TI Modifications to a molt-based ageing system proposed by Wolfe et al.
(2010)
SO JOURNAL OF FIELD ORNITHOLOGY
LA English
DT Article
DE annual cycle; molt cycle; Staffelmauser; tropical birds; W-R-P system
ID AGE
AB Wolfe et al. (2010. Journal of Field Ornithology 81: 186194) proposed a coding system for ageing birds based on the sequence of molts and plumages, which is more practical than a calendar-based system, especially in tropical and southern latitudes where species often breed across 1 January. The WolfeRyderPyle (hereafter, WRP) three-letter system is based on recognition of molt cycle (first, second, third, definitive, and so on) and plumage phase (juvenile, supplemental, formative, alternate, and basic). For example, a bird in First Cycle Formative plumage is coded as FCF. We propose the use of two additional code options that further refine age brackets. First, we suggest the use of an after or A code in place of the C, or cycle code, where an earlier molt cycle or plumage can be ruled out. For example, a bird that exhibits Staffelmauser might be aged as after-third cycle basic, or TAB. Second, we suggest using pre or P in place of the C, or cycle code, when birds are actively molting, such as for birds undergoing the second prebasic molt or SPB. For both codes, we discuss their applicability using examples based on actual banding data. Our proposed codes will improve the utility of the WRP system by better refining age brackets and by expanding its applicability to a diverse array of taxa.
C1 [Johnson, Erik I.; Wolfe, Jared D.] Louisiana State Univ, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA.
[Johnson, Erik I.; Wolfe, Jared D.] Louisiana State Univ, AgCtr, Baton Rouge, LA 70803 USA.
[Ryder, T. Brandt] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20013 USA.
[Pyle, Peter] Inst Bird Populat, Point Reyes Stn, CA 94956 USA.
RP Johnson, EI (reprint author), Louisiana State Univ, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA.
EM ejohn33@lsu.edu
NR 6
TC 4
Z9 4
U1 2
U2 13
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0273-8570
J9 J FIELD ORNITHOL
JI J. Field Ornithol.
PD DEC
PY 2011
VL 82
IS 4
BP 422
EP 424
DI 10.1111/j.1557-9263.2011.00345.x
PG 3
WC Ornithology
SC Zoology
GA 860XT
UT WOS:000297982400008
ER
PT J
AU Kennedy, VS
Breitburg, DL
Christman, MC
Luckenbach, MW
Paynter, K
Kramer, J
Sellner, KG
Dew-Baxter, J
Keller, C
Mann, R
AF Kennedy, Victor S.
Breitburg, Denise L.
Christman, Mary C.
Luckenbach, Mark W.
Paynter, Kennedy
Kramer, Jonathan
Sellner, Kevin G.
Dew-Baxter, Jodi
Keller, Cherie
Mann, Roger
TI LESSONS LEARNED FROM EFFORTS TO RESTORE OYSTER POPULATIONS IN MARYLAND
AND VIRGINIA, 1990 TO 2007
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Article
DE Chesapeake Bay; management; Maryland; monitoring; oyster fishery
restoration; Virginia; Crassostrea virginica
ID CHESAPEAKE BAY; REEF RESTORATION; CRASSOSTREA-VIRGINICA; CONSERVATION;
MANAGEMENT
AB A century-long decline of the fishery for the Eastern oyster Crassostrea virginica (Gmelin, 1791) in Maryland and Virginia stimulated numerous efforts by federal, state, and nongovernmental agencies to restore oyster populations, with limited success. To learn from recent efforts, we analyzed records of restoration and monitoring activities undertaken between 1990 and 2007 by 12 such agencies. Of the 1,037 oyster bars (reefs, beds, or grounds) for which we obtained data, 43% experienced both restoration and monitoring, with the remaining experiencing either restoration or monitoring only. Restoration activities involved adding substrate (shell), transplanting hatchery or wild seed (juvenile oysters), bar cleaning, and bagless dredging. Of these, substrate addition and transplanting seed were common actions, with bar cleaning and bagless dredging relatively uncommon. Limited monitoring efforts, a lack of replicated postrestoration sampling, and the effects of harvest on some restored bars hinders evaluations of the effectiveness of restoration activities. Future restoration activities should have clearly articulated objectives and be coordinated among agencies and across bars, which should also be off limits to fishing. To evaluate restoration efforts, experimental designs should include replication, quantitative sampling, and robust sample sizes, supplemented by pre- and postrestoration monitoring.
C1 [Kennedy, Victor S.] Univ Maryland, Ctr Environm Sci, Horn Point Lab, Cambridge, MD 21613 USA.
[Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Christman, Mary C.] MCC Stat Consulting LLC, Gainesville, FL 32605 USA.
[Luckenbach, Mark W.] Virginia Inst Marine Sci, Eastern Shore Lab, Wachapreague, VA 23480 USA.
[Paynter, Kennedy] Univ Maryland, Chesapeake Biol Lab, Ctr Environm Sci, Solomons, MD 20688 USA.
[Paynter, Kennedy] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Kramer, Jonathan] Univ Syst Maryland, College Pk, MD 20740 USA.
[Sellner, Kevin G.] Chesapeake Res Consortium Inc, Edgewater, MD 21037 USA.
[Dew-Baxter, Jodi] Versar Inc ESM, Columbia, MD 21045 USA.
[Keller, Cherie] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Mann, Roger] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
RP Kennedy, VS (reprint author), Univ Maryland, Ctr Environm Sci, Horn Point Lab, Box 775, Cambridge, MD 21613 USA.
EM kennedy@umces.edu
RI Kennedy, Victor/D-5854-2012; Paynter, Kennedy/F-9717-2013
FU Keith Campbell Foundation; NOAA Chesapeake Bay Office; Keith Campbell
Foundation for the Environment; U.S. Fish and Wildlife Service; Maryland
Sea Grant College Program
FX We gratefully acknowledge Verna Harrison (Keith Campbell Foundation) and
Peyton Robertson (NOAA Chesapeake Bay Office) for support and
encouragement. For contributed data, we thank representatives of the
agencies listed in Table 1, as well as George Abbe, Eric Campbell, A. C.
Carpenter, and James Wesson. Sandy Rodgers provided the figures and Jack
Greer carefully edited the ORET manuscript on which this article is
based. Funding was provided by The Keith Campbell Foundation for the
Environment, the NOAA Chesapeake Bay Office, the U.S. Fish and Wildlife
Service, and the Maryland Sea Grant College Program. UMCES contribution
no. 4542.
NR 28
TC 19
Z9 19
U1 7
U2 46
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD DEC
PY 2011
VL 30
IS 3
BP 719
EP 731
DI 10.2983/035.030.0312
PG 13
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 876WO
UT WOS:000299138700012
ER
PT J
AU Chapman, SK
Feller, IC
AF Chapman, Samantha K.
Feller, Ilka C.
TI Away-field advantage: mangrove seedlings grow best in litter from other
mangrove species
SO OIKOS
LA English
DT Article
ID LEAF-LITTER; PLANT LITTER; NUTRIENT DYNAMICS; DECOMPOSITION; FOREST;
FEEDBACK; DIVERSITY; COMMUNITY; ESTABLISHMENT; GERMINATION
AB Plant community composition can impact ecosystem processes via litter feedbacks. Species variation in litter quality may generate different patterns of nutrient supply for plants that are dependent on litter inputs. However, it is not known whether plants grow faster in their own litter, litter from other species, or in litter mixtures from multiple species. To test whether litter identity and mixture status influenced mangrove seedling growth, biomass allocation, and stoichiometry, we performed mesocosm experiments. Two species of mangrove seedlings, Avicennia germinans, black mangrove and Rhizophora mangle, red mangrove, were exposed to all possible combinations of three mangrove litter types and were isolated from all other nutrient inputs. Litter treatments significantly altered seedling growth. Seedlings from both mangrove species grew most rapidly in litter from a different species rather than their own, irrespective of litter chemical quality, decomposition rate, and nitrogen release. Litter mixtures from white and black mangroves caused black mangroves to grow 65% more than expected. Litter treatments did not impact seedling root:shoot ratios or tissue C:N. Our finding that seedlings grow best in litter from other species may indicate a mechanism that helps sustain the coexistence of dominant species.
C1 [Chapman, Samantha K.] Villanova Univ, Dept Biol, Villanova, PA 19003 USA.
[Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD USA.
RP Chapman, SK (reprint author), Villanova Univ, Dept Biol, Villanova, PA 19003 USA.
EM samantha.chapman@villanova.edu
OI Feller, Ilka/0000-0002-6391-1608
FU Smithsonian Institution; Villanova Univ.
FX A Smithsonian Institution Fellowship and Villanova Univ. funded SKC
during the execution of this project and the preparation of this
manuscript. The scientists and staff at the Smithsonian Marine Station
at Force Pierce, FL provided facilities and assistance for the execution
of this research. We would like to acknowledge Anne Chamberlain for all
her help at every stage of this project. We acknowledge Rainer Feller,
Woody Lee, Jay O'Neill, Jonathan Pahlas, Steve Sanford and Hilary Wilson
for help in the greenhouse and field. J. Adam Langley, Rachel Jones,
Lorae Simpson, Shirley Wang, Antonio Pullano, Kate Devine, Greg Clement,
Kate Shepherd and Bethanne Albert-Bruninga provided helpful feedback on
this manuscript.
NR 54
TC 2
Z9 2
U1 3
U2 33
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0030-1299
J9 OIKOS
JI Oikos
PD DEC
PY 2011
VL 120
IS 12
BP 1880
EP 1888
DI 10.1111/j.1600-0706.2011.19381.x
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 862LS
UT WOS:000298093100013
ER
PT J
AU McSween, HY
Mittlefehldt, DW
Beck, AW
Mayne, RG
McCoy, TJ
AF McSween, Harry Y., Jr.
Mittlefehldt, David W.
Beck, Andrew W.
Mayne, Rhiannon G.
McCoy, Timothy J.
TI HED Meteorites and Their Relationship to the Geology of Vesta and the
Dawn Mission
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Meteorites; Vesta; Asteroid; Eucrite; Diogenite; Howardite
ID EUCRITE PARENT BODY; EARLY SOLAR-SYSTEM; ASTEROID 4 VESTA;
ORTHO-PYROXENE; BASALTIC METEORITES; MN-53-CR-53 SYSTEMATICS; DIOGENITE
METEORITES; THERMAL METAMORPHISM; ISOTOPE SYSTEMATICS; MARTIAN
METEORITES
AB Howardite-eucrite-diogenite (HED) meteorites, thought to be derived from 4 Vesta, provide the best sampling available for any differentiated asteroid. However, deviations in oxygen isotopic composition from a common mass-fractionation line suggest that a few eucrite-like meteorites are from other bodies, or that Vesta was not completely homogenized during differentiation. The petrology and geochemistry of HEDs provide insights into igneous processes that produced a crust composed of basalts, gabbros, and ultramafic cumulate rocks. Although most HED magmas were fractionated, it is unresolved whether some eucrites may have been primary melts. The geochemistry of HEDs indicates that bulk Vesta is depleted in volatile elements and is relatively reduced, but has chondritic refractory element abundances. The compositions of HEDs may favor a magma ocean model, but inconsistencies remain. Geochronology indicates that Vesta accreted and differentiated within the first several million years of solar system history, that magmatism continued over a span of similar to 10 Myr, and that its thermal history extended for perhaps 100 Myr. The protracted cooling history is probably responsible for thermal metamorphism of most HEDs. Impact chronology indicates that Vesta experienced many significant collisions, including during the late heavy bombardment. The age of the huge south pole crater is controversial, but it probably ejected Vestoids and many HEDs. Continued impacts produced a regolith composed of eucrite and diogenite fragments containing only minor exotic materials. HED meteorites serve as ground truth for orbital spectroscopic and chemical analyses by the Dawn spacecraft, and their properties are critical for instrument calibration and interpretation of Vesta's geologic history.
C1 [McSween, Harry Y., Jr.; Beck, Andrew W.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
[McSween, Harry Y., Jr.; Beck, Andrew W.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Mittlefehldt, David W.] NASA, Astromat Res Off, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Mayne, Rhiannon G.] Texas Christian Univ, Dept Geol, Ft Worth, TX 76129 USA.
[McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20546 USA.
RP McSween, HY (reprint author), Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA.
EM mcsween@utk.edu
RI Beck, Andrew/J-7215-2015
OI Beck, Andrew/0000-0003-4455-2299
FU NASA Cosmochemistry [NNG06GG36G, RTOP 344-31-10-18, NNG06GF56G]
FX We acknowledge thoughtful reviews by P. Warren and an anonymous
reviewer. This work was partly supported by NASA Cosmochemistry grants
NNG06GG36G (HYM), RTOP 344-31-10-18 (DWM), and NNG06GF56G (TJM).
NR 156
TC 114
Z9 115
U1 6
U2 54
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
J9 SPACE SCI REV
JI Space Sci. Rev.
PD DEC
PY 2011
VL 163
IS 1-4
BP 141
EP 174
DI 10.1007/s11214-010-9637-z
PG 34
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 875AQ
UT WOS:000299002100009
ER
PT J
AU Woodman, N
AF Woodman, Neal
TI Patterns of morphological variation amongst semifossorial shrews in the
highlands of Guatemala, with the description of a new species (Mammalia,
Soricomorpha, Soricidae)
SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE Blarinini; Central America; Eulipotyphla; humerus; Insectivora; manus;
Soricinae
ID SMALL-EARED SHREW; GENUS CRYPTOTIS; INSECTIVORA
AB Members of the Cryptotis goldmani group of small-eared shrews (Mammalia, Soricomorpha, Soricidae) represent a clade within the genus that is characterized by modifications of the forelimb that include broadened forefeet, elongated and broadened foreclaws, and massive humeri with enlarged processes. These modifications are consistent with greater adaptation to their semifossorial habits than other members of the genus. The species in this group occur discontinuously in temperate highlands from southern Tamaulipas, Mexico, to Honduras. In Guatemala, there are three species: the relatively widespread Cryptotis goodwini and two species (Cryptotis lacertosus, Cryptotis mam) endemic to highland forests in the Sierra de los Cuchumatanes of western Guatemala. Ongoing studies focusing on the relationships of variation in cranial and postcranial skeletal morphology have revealed a fourth species from remnant cloud forest in the Sierra de Yalijux, central Guatemala. In this paper, I describe this new species and characterize its morphology relative to other species in the C. goldmani group and to other species of Cryptotis in Guatemala. In addition, I summarize available details of its habitat and ecology. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 163, 1267-1288. doi: 10.1111/j.1096-3642.2011.00754.x
C1 Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA.
RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA.
EM woodmann@si.edu
OI Woodman, Neal/0000-0003-2689-7373
NR 39
TC 15
Z9 16
U1 0
U2 5
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0024-4082
J9 ZOOL J LINN SOC-LOND
JI Zool. J. Linn. Soc.
PD DEC
PY 2011
VL 163
IS 4
BP 1267
EP 1288
DI 10.1111/j.1096-3642.2011.00754.x
PG 22
WC Zoology
SC Zoology
GA 860KB
UT WOS:000297946100011
ER
PT J
AU Herrera, F
Manchester, SR
Hoot, SB
Wefferling, KM
Carvalho, MR
Jaramillo, C
AF Herrera, Fabiany
Manchester, Steven R.
Hoot, Sara B.
Wefferling, Keir M.
Carvalho, Monica R.
Jaramillo, Carlos
TI PHYTOGEOGRAPHIC IMPLICATIONS OF FOSSIL ENDOCARPS OF MENISPERMACEAE FROM
THE PALEOCENE OF COLOMBIA
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Article
DE Cissampelos; Colombia; endocarps; fossils; paleobiogeography; Paleocene;
rainforest; Stephania
ID NEOTROPICAL RAIN-FOREST; CERREJON FORMATION; AMAZONIAN FORESTS; NORTHERN
COLOMBIA; PHYLOGENY; EVOLUTION; CHLOROPLAST; DISPERSAL; SEQUENCES;
PATAGONIA
AB Premise of the study: Fossil leaves of Menispermaceae were previously described from the Paleocene of Colombia. Because of strong homoplasy of leaf characters, the fossils could not be placed more specifically within recognized clades, and additional data were needed to specify intrafamilial and paleogeographic relationships during the Paleocene.
Methods: Fossil endocarps of Menispermaceae were collected from the Cerrejon Formation, the recently discovered Bogota flora, and Wyoming (similar to 60 Ma). We surveyed the endocarp morphology of almost all extant genera, conducted character optimization, a molecular scaffold analysis, and critically reviewed the related fossil genera.
Key results: Parallel syndromes of fruit characters have appeared in unrelated clades of the family according to current phylogenetic reconstructions. However, mapping selected endocarp characters across those clades that contain horseshoe-shaped endocarps facilitates identification and phylogenetic assessment of the fossils. Three fossil species are recognized. One of them belongs to the extant genus Stephania, which today grows only in Africa and Australasia. Palaeoluna gen. nov. is placed within the pantropical clade composed of extant Stephania, Cissampelos, and Cyclea; this morphogenus is also recognized from the Paleocene of Wyoming. Menispina gen. nov. shows similarity with several unrelated clades.
Conclusions: The new fossils from Colombia reveal a complex paleobiogeographic history of the recognized clades within Menispermaceae, suggesting a more active exchange among neotropical, paleotropical, North American, and European paleo-forests than previously recognized. In addition, the new fossils indicate that neotropical forests were an important biome for the radiation and dispersal of derived lineages in Menispermaceae after the Cretaceous-Paleogene boundary.
C1 [Herrera, Fabiany; Manchester, Steven R.] Univ Florida, Dept Biol, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Herrera, Fabiany; Carvalho, Monica R.; Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Hoot, Sara B.; Wefferling, Keir M.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA.
[Carvalho, Monica R.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
RP Herrera, F (reprint author), Univ Florida, Dept Biol, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
EM fherrera@flmnh.ufl.edu
FU Evolving Earth Foundation; Geological Society of America Foundation;
Asociacion Colombiana de Geologos y Geof sicos del Petroleo-ARES;
Smithsonian Institution; Gary S. Morgan Student Research Award; Lewis &
Clark Foundation-American Philosophical Society; National Science
Foundation (NSF) [EF-0431266, BSR-0743474, DEB-0919071, DEB-0733725,
DEB-0542679]
FX This research was made possible through support from the Evolving Earth
Foundation, the Geological Society of America Foundation, the Asociacion
Colombiana de Geologos y Geof sicos del Petroleo-ARES, The Smithsonian
Institution, the Gary S. Morgan Student Research Award, and the Lewis &
Clark Foundation-American Philosophical Society to F. H., National
Science Foundation (NSF) grants EF-0431266 and BSR-0743474 to S. R. M.,
NSF DEB-0919071 to M. R. C., NSF DEB-0733725 to C.J., and NSF
DEB-0542679 to S. B. H. The authors thank L. Teicher, F. Chavez, and the
geology team at Minas Cerrejon. J. Moreno, E. Cadena, A. Rincon, S.
Moron, G. Bayona, S. L. Wing, J. Bloch, M. I. Barreto, G. Doria, and A.
Rojas for their assistance with the Bogota and Cerrejon field trips; C.
A. Munoz for his hospitality during fieldwork in Bogota. D. Bell (US)
granted access to modern Menispermaceae collections, R. C. Ortiz and F.
Jacques provided helpful discussions about the systematics of the
fossils, and G. Bedoya provided nomenclatural suggestions. Two anonymous
reviewers and T. Lott provided helpful reviews of the manuscript. F. H.
thanks B. Himschoot for support.
NR 51
TC 15
Z9 20
U1 1
U2 7
PU BOTANICAL SOC AMER INC
PI ST LOUIS
PA PO BOX 299, ST LOUIS, MO 63166-0299 USA
SN 0002-9122
J9 AM J BOT
JI Am. J. Bot.
PD DEC
PY 2011
VL 98
IS 12
BP 2004
EP 2017
DI 10.3732/ajb.1000461
PG 14
WC Plant Sciences
SC Plant Sciences
GA 863PB
UT WOS:000298176800024
PM 22114219
ER
PT J
AU Solazzo, C
Heald, S
Ballard, MW
Ashford, DA
DePriest, PT
Koestler, RJ
Collins, MJ
AF Solazzo, Caroline
Heald, Susan
Ballard, Mary W.
Ashford, David A.
DePriest, Paula T.
Koestler, Robert J.
Collins, Matthew J.
TI Proteomics and Coast Salish blankets: a tale of shaggy dogs?
SO ANTIQUITY
LA English
DT Article
DE North America; nineteenth century; Coast Salish; textiles; sheep; goat;
woolly dog
ID FLIGHT MASS-SPECTROMETRY; SPECIES IDENTIFICATION; PATTERN; HAIR
AB Identifying animals to species from relict proteins is a powerful new archaeological tool. Here the authors apply the method to answer questions relating to the Salish of west coast North America. Did they weave their blankets out of dog hair? The proteomic analysis shows that they did, interweaving it with goat, and that the woolly dog was increasingly superseded by sheep in the later nineteenth century.
C1 [Solazzo, Caroline; Collins, Matthew J.] Univ York, BioArCh, Dept Biol, York YO10 5YW, N Yorkshire, England.
[Solazzo, Caroline; Collins, Matthew J.] Univ York, BioArCh, Dept Archaeol, York YO10 5YW, N Yorkshire, England.
[Solazzo, Caroline; Collins, Matthew J.] Univ York, BioArCh, Dept Chem, York YO10 5YW, N Yorkshire, England.
[Solazzo, Caroline; Ballard, Mary W.; DePriest, Paula T.; Koestler, Robert J.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
[Heald, Susan] Natl Museum Amer Indian, CRC, Suitland, MD 20746 USA.
[Ashford, David A.] Univ York, Dept Biol, Technol Facil, Prote & Analyt Biochem Lab, York YO10 5YW, N Yorkshire, England.
[Ashford, David A.] Univ York, Ctr Excellence Mass Spectrometry, York YO10 5YW, N Yorkshire, England.
RP Solazzo, C (reprint author), Univ York, BioArCh, Dept Biol, POB 373, York YO10 5YW, N Yorkshire, England.
EM solazzo.c@gmail.com
NR 39
TC 12
Z9 12
U1 2
U2 12
PU ANTIQUITY
PI YORK
PA KINGS MANOR, YORK YO1 7EP, ENGLAND
SN 0003-598X
J9 ANTIQUITY
JI Antiquity
PD DEC
PY 2011
VL 85
IS 330
BP 1418
EP 1432
PG 15
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA 860OX
UT WOS:000297958700020
ER
PT J
AU Mascaro, J
AF Mascaro, Joseph
TI Earth Similarity Index Provides a Logical Breakpoint for Naming Planets
SO ASTROBIOLOGY
LA English
DT Editorial Material
C1 Smithsonian Trop Res Inst, Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
RP Mascaro, J (reprint author), Smithsonian Trop Res Inst, Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA.
EM jmascaro@stanford.edu
NR 5
TC 0
Z9 0
U1 1
U2 5
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD DEC
PY 2011
VL 11
IS 10
BP 1053
EP 1053
DI 10.1089/ast.2011.0804
PG 1
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 865YA
UT WOS:000298345600009
PM 22185207
ER
PT J
AU Foster, JB
Jackson, JM
Barnes, PJ
Barris, E
Brooks, K
Cunningham, M
Finn, SC
Fuller, GA
Longmore, SN
Mascoop, JL
Peretto, N
Rathborne, J
Sanhueza, P
Schuller, F
Wyrowski, F
AF Foster, Jonathan B.
Jackson, James M.
Barnes, Peter J.
Barris, Elizabeth
Brooks, Kate
Cunningham, Maria
Finn, Susanna C.
Fuller, Gary A.
Longmore, Steve N.
Mascoop, Joshua L.
Peretto, Nicolas
Rathborne, Jill
Sanhueza, Patricio
Schuller, Frederic
Wyrowski, Friedrich
TI THE MILLIMETER ASTRONOMY LEGACY TEAM 90 GHz (MALT90) PILOT SURVEY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE ISM: molecules; stars: formation; stars: massive; surveys
ID INFRARED DARK CLOUDS; STAR-FORMATION; GALACTIC PLANE; CO SURVEY; CORES;
CANDIDATES; TELESCOPE; EMISSION; OUTFLOWS; REGIONS
AB We describe a pilot survey conducted with the Mopra 22 m radio telescope in preparation for the Millimeter Astronomy Legacy Team Survey at 90 GHz (MALT90). We identified 182 candidate dense molecular clumps using six different selection criteria and mapped each source simultaneously in 16 different lines near 90 GHz. We present a summary of the data and describe how the results of the pilot survey shaped the design of the larger MALT90 survey. We motivate our selection of target sources for the main survey based on the pilot detection rates and demonstrate the value of mapping in multiple lines simultaneously at high spectral resolution.
C1 [Foster, Jonathan B.; Jackson, James M.; Barris, Elizabeth; Finn, Susanna C.; Mascoop, Joshua L.; Sanhueza, Patricio] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Barnes, Peter J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Brooks, Kate; Rathborne, Jill] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Cunningham, Maria] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Fuller, Gary A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Longmore, Steve N.] ESO Headquarters, D-85748 Garching, Germany.
[Longmore, Steve N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Peretto, Nicolas] Univ Paris Diderot, CEA, CNRS, Lab AIM,DSM,IRFU,Serv Astrophys,CE Saclay, F-91191 Gif Sur Yvette, France.
[Rathborne, Jill] Univ Chile, Dept Astron, Santiago, Chile.
[Schuller, Frederic; Wyrowski, Friedrich] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
RP Foster, JB (reprint author), Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
EM jbfoster@bu.edu; jackson@bu.edu; peterb@astro.ufl.edu; lizbee@bu.edu;
Kate.Brooks@csiro.au; maria.cunningham@unsw.edu.au; sfinn@bu.edu;
G.Fuller@manchester.ac.uk; slongmor@eso.org; jmascoop@bu.edu;
nicolas.peretto@cea.fr; Jill.Rathborne@csiro.au; patricio@bu.edu;
schuller@mpifr-bonn.mpg.de; wyrowski@mpifr-bonn.mpg.de
OI Brooks, Kate/0000-0001-9373-8992; Cunningham, Maria/0000-0001-7020-6176
FU Commonwealth of Australia; Australian Research Council; University of
New South Wales; University of Sydney; Monash University; National
Aeronautics and Space Administration; NSF [AST-0808001]; University of
New South Wales (UNSW) under the Australian Research Council
FX The Mopra telescope is part of the Australia Telescope and is funded by
the Commonwealth of Australia for operation as National Facility managed
by CSIRO. The UNSW-MOPS Digital Filter Bank used for the observations
with the Mopra telescope was provided with support from the Australian
Research Council, together with the University of New South Wales,
University of Sydney, and Monash University. This research has made use
of the NASA/IPAC Infrared Science Archive (for access to GLIMPSE and
MIPSGAL images), which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. This research has made use of
NASA's Astrophysics Data System Bibliographic Services. J.M.J.
gratefully acknowledges funding support from NSF Grant No. AST-0808001.
The MALT90 project team gratefully acknowledges the use of dense core
positions supplied by ATLASGAL. ATLASGAL is a collaboration between the
Max Planck Gesellschaft (MPG: Max Planck Institute for Radioastronomy,
Bonn and the Max Planck Institute for Astronomy, Heidelberg), the
European Southern Observatory (ESO) and the University of Chile. Thanks
to Anita Titmarsh and the duty astronomers and staff at the Paul Wild
Observatory for their assistance during the observations.; MOPS was
funded in part through a grant instigated by the University of New South
Wales (UNSW) under the Australian Research Council Grants scheme for
Linkage, Infrastructure, Equipment and Facilities (LIEF), and in part by
CSIRO Astronomy and Space Science.
NR 33
TC 47
Z9 47
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 DEC
PY 2011
VL 197
IS 2
AR 25
DI 10.1088/0067-0049/197/2/25
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300011
ER
PT J
AU Grogin, NA
Kocevski, DD
Faber, SM
Ferguson, HC
Koekemoer, AM
Riess, AG
Acquaviva, V
Alexander, DM
Almaini, O
Ashby, MLN
Barden, M
Bell, EF
Bournaud, F
Brown, TM
Caputi, KI
Casertano, S
Cassata, P
Castellano, M
Challis, P
Chary, RR
Cheung, E
Cirasuolo, M
Conselice, CJ
Cooray, AR
Croton, DJ
Daddi, E
Dahlen, T
Dave, R
de Mello, DF
Dekel, A
Dickinson, M
Dolch, T
Donley, JL
Dunlop, JS
Dutton, AA
Elbaz, D
Fazio, GG
Filippenko, AV
Finkelstein, SL
Fontana, A
Gardner, JP
Garnavich, PM
Gawiser, E
Giavalisco, M
Grazian, A
Guo, YC
Hathi, NP
Haussler, B
Hopkins, PF
Huang, JS
Huang, KH
Jha, SW
Kartaltepe, JS
Kirshner, RP
Koo, DC
Lai, K
Lee, KS
Li, WD
Lotz, JM
Lucas, RA
Madau, P
McCarthy, PJ
McGrath, EJ
McIntosh, DH
McLure, RJ
Mobasher, B
Moustakas, LA
Mozena, M
Nandra, K
Newman, JA
Niemi, SM
Noeske, KG
Papovich, CJ
Pentericci, L
Pope, A
Primack, JR
Rajan, A
Ravindranath, S
Reddy, NA
Renzini, A
Rix, HW
Robaina, AR
Rodney, SA
Rosario, DJ
Rosati, P
Salimbeni, S
Scarlata, C
Siana, B
Simard, L
Smidt, J
Somerville, RS
Spinrad, H
Straughn, AN
Strolger, LG
Telford, O
Teplitz, HI
Trump, JR
van der Wel, A
Villforth, C
Wechsler, RH
Weiner, BJ
Wiklind, T
Wild, V
Wilson, G
Wuyts, S
Yan, HJ
Yun, MS
AF Grogin, Norman A.
Kocevski, Dale D.
Faber, S. M.
Ferguson, Henry C.
Koekemoer, Anton M.
Riess, Adam G.
Acquaviva, Viviana
Alexander, David M.
Almaini, Omar
Ashby, Matthew L. N.
Barden, Marco
Bell, Eric F.
Bournaud, Frederic
Brown, Thomas M.
Caputi, Karina I.
Casertano, Stefano
Cassata, Paolo
Castellano, Marco
Challis, Peter
Chary, Ranga-Ram
Cheung, Edmond
Cirasuolo, Michele
Conselice, Christopher J.
Cooray, Asantha Roshan
Croton, Darren J.
Daddi, Emanuele
Dahlen, Tomas
Dave, Romeel
de Mello, Duilia F.
Dekel, Avishai
Dickinson, Mark
Dolch, Timothy
Donley, Jennifer L.
Dunlop, James S.
Dutton, Aaron A.
Elbaz, David
Fazio, Giovanni G.
Filippenko, Alexei V.
Finkelstein, Steven L.
Fontana, Adriano
Gardner, Jonathan P.
Garnavich, Peter M.
Gawiser, Eric
Giavalisco, Mauro
Grazian, Andrea
Guo, Yicheng
Hathi, Nimish P.
Haeussler, Boris
Hopkins, Philip F.
Huang, Jia-Sheng
Huang, Kuang-Han
Jha, Saurabh W.
Kartaltepe, Jeyhan S.
Kirshner, Robert P.
Koo, David C.
Lai, Kamson
Lee, Kyoung-Soo
Li, Weidong
Lotz, Jennifer M.
Lucas, Ray A.
Madau, Piero
McCarthy, Patrick J.
McGrath, Elizabeth J.
McIntosh, Daniel H.
McLure, Ross J.
Mobasher, Bahram
Moustakas, Leonidas A.
Mozena, Mark
Nandra, Kirpal
Newman, Jeffrey A.
Niemi, Sami-Matias
Noeske, Kai G.
Papovich, Casey J.
Pentericci, Laura
Pope, Alexandra
Primack, Joel R.
Rajan, Abhijith
Ravindranath, Swara
Reddy, Naveen A.
Renzini, Alvio
Rix, Hans-Walter
Robaina, Aday R.
Rodney, Steven A.
Rosario, David J.
Rosati, Piero
Salimbeni, Sara
Scarlata, Claudia
Siana, Brian
Simard, Luc
Smidt, Joseph
Somerville, Rachel S.
Spinrad, Hyron
Straughn, Amber N.
Strolger, Louis-Gregory
Telford, Olivia
Teplitz, Harry I.
Trump, Jonathan R.
van der Wel, Arjen
Villforth, Carolin
Wechsler, Risa H.
Weiner, Benjamin J.
Wiklind, Tommy
Wild, Vivienne
Wilson, Grant
Wuyts, Stijn
Yan, Hao-Jing
Yun, Min S.
TI CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY
SURVEY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmology: observations; galaxies: high-redshift
ID HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI;
LYMAN-BREAK GALAXIES; SUPERMASSIVE BLACK-HOLES; EXTENDED GROTH-STRIP;
GOODS-SOUTH FIELD; SIMILAR-TO 7; REST-FRAME ULTRAVIOLET; EARLY RELEASE
SCIENCE
AB The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) is designed to document the first third of galactic evolution, over the approximate redshift (z) range 8-1.5. It will image >250,000 distant galaxies using three separate cameras on the Hubble Space Telescope, from the mid-ultraviolet to the near-infrared, and will find and measure Type Ia supernovae at z > 1.5 to test their accuracy as standardizable candles for cosmology. Five premier multi-wavelength sky regions are selected, each with extensive ancillary data. The use of five widely separated fields mitigates cosmic variance and yields statistically robust and complete samples of galaxies down to a stellar mass of 10(9)M(circle dot) to z approximate to 2, reaching the knee of the ultraviolet luminosity function of galaxies to z approximate to 8. The survey covers approximately 800 arcmin(2) and is divided into two parts. The CANDELS/Deep survey (5 sigma point-source limit H = 27.7 mag) covers similar to 125 arcmin(2) within Great Observatories Origins Deep Survey (GOODS)-N and GOODS-S. The CANDELS/Wide survey includes GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-deep Survey) and covers the full area to a 5 sigma point-source limit of H greater than or similar to 27.0 mag. Together with the Hubble Ultra Deep Fields, the strategy creates a three-tiered "wedding-cake" approach that has proven efficient for extragalactic surveys. Data from the survey are nonproprietary and are useful for a wide variety of science investigations. In this paper, we describe the basic motivations for the survey, the CANDELS team science goals and the resulting observational requirements, the field selection and geometry, and the observing design. The Hubble data processing and products are described in a companion paper.
C1 [Grogin, Norman A.; Ferguson, Henry C.; Koekemoer, Anton M.; Brown, Thomas M.; Casertano, Stefano; Dahlen, Tomas; Donley, Jennifer L.; Huang, Kuang-Han; Lotz, Jennifer M.; Lucas, Ray A.; Niemi, Sami-Matias; Noeske, Kai G.; Rajan, Abhijith; Villforth, Carolin] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kocevski, Dale D.; Faber, S. M.; Cheung, Edmond; Koo, David C.; Lai, Kamson; Madau, Piero; McGrath, Elizabeth J.; Mozena, Mark; Trump, Jonathan R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Lick Observ, UCO, Santa Cruz, CA 95064 USA.
[Riess, Adam G.; Dolch, Timothy; Huang, Kuang-Han; Rodney, Steven A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Acquaviva, Viviana; Gawiser, Eric; Jha, Saurabh W.; Somerville, Rachel S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ USA.
[Alexander, David M.] Univ Durham, Dept Phys, Durham, England.
[Almaini, Omar; Conselice, Christopher J.; Haeussler, Boris] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Ashby, Matthew L. N.; Fazio, Giovanni G.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Barden, Marco] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Bournaud, Frederic; Daddi, Emanuele; Elbaz, David] CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Caputi, Karina I.; Dunlop, James S.; McLure, Ross J.; Wild, Vivienne] Univ Edinburgh, Inst Astron, Edinburgh, Midlothian, Scotland.
[Cassata, Paolo; Giavalisco, Mauro; Guo, Yicheng; Pope, Alexandra; Salimbeni, Sara; Wilson, Grant; Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Castellano, Marco; Fontana, Adriano; Grazian, Andrea; Pentericci, Laura] Osserv Astron Roma, INAF, I-00136 Rome, Italy.
[Challis, Peter] Harvard Coll Observ, Cambridge, MA USA.
[Chary, Ranga-Ram] CALTECH, US Planck Data Ctr, Pasadena, CA 91125 USA.
[Cirasuolo, Michele] UK Astron Technol Ctr, Edinburgh, Midlothian, Scotland.
[Cooray, Asantha Roshan; Smidt, Joseph] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Croton, Darren J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Dave, Romeel; Weiner, Benjamin J.] Univ Arizona, Dept Astron, Tucson, AZ USA.
[de Mello, Duilia F.; Gardner, Jonathan P.; Straughn, Amber N.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
[de Mello, Duilia F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Dickinson, Mark; Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Dutton, Aaron A.] Univ Victoria, Dept Phys & Astron, Victoria, BC, Canada.
[Filippenko, Alexei V.; Hopkins, Philip F.; Li, Weidong; Spinrad, Hyron] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Finkelstein, Steven L.; Papovich, Casey J.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX USA.
[Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Hathi, Nimish P.; McCarthy, Patrick J.] Carnegie Observ, Pasadena, CA USA.
[Huang, Jia-Sheng] Smithsonian Inst Astrophys Observ, Cambridge, MA USA.
[Lee, Kyoung-Soo] Yale Ctr Astron & Astrophys, New Haven, CT USA.
[McIntosh, Daniel H.] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA.
[Mobasher, Bahram; Reddy, Naveen A.; Siana, Brian] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Nandra, Kirpal; Rosario, David J.; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany.
[Newman, Jeffrey A.; Telford, Olivia] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Ravindranath, Swara] Interuniv Ctr Astron & Astrophys, Pune, Maharashtra, India.
[Renzini, Alvio] Osserv Astron Padova, Padua, Italy.
[Rix, Hans-Walter; van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Robaina, Aday R.] Univ Barcelona, Inst Ciencies Cosmos, Barcelona, Spain.
[Rosati, Piero] European So Observ, D-37075 Garching, Germany.
[Scarlata, Claudia] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN USA.
[Scarlata, Claudia] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Simard, Luc] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC, Canada.
[Strolger, Louis-Gregory] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
[Teplitz, Harry I.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Wechsler, Risa H.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Wiklind, Tommy] ESO, ALMA, Santiago, Chile.
[Yan, Hao-Jing] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
RP Grogin, NA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RI Daddi, Emanuele/D-1649-2012; Conselice, Christopher/B-4348-2013;
Bournaud, Frederic/K-1263-2013; Hathi, Nimish/J-7092-2014;
OI fontana, adriano/0000-0003-3820-2823; Koekemoer,
Anton/0000-0002-6610-2048; Brown, Thomas/0000-0002-1793-9968; Bell,
Eric/0000-0002-5564-9873; Moustakas, Leonidas/0000-0003-3030-2360;
Alexander, David/0000-0002-5896-6313; Daddi,
Emanuele/0000-0002-3331-9590; Hathi, Nimish/0000-0001-6145-5090;
Castellano, Marco/0000-0001-9875-8263; Conselice,
Christopher/0000-0003-1949-7638; Cheung, Edmond/0000-0001-8546-1428
FU NASA through the Space Telescope Science Institute [GO-12060, GO-12099];
NASA [NAS5-26555]; ASI-INAF [I/009/10/0]
FX Support for HST Programs GO-12060 and GO-12099 was provided by NASA
through grants from the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS5-26555. A. Fontana acknowledges support
from agreement ASI-INAF I/009/10/0.
NR 226
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U1 6
U2 39
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 DEC
PY 2011
VL 197
IS 2
AR 35
DI 10.1088/0067-0049/197/2/35
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300021
ER
PT J
AU Koekemoer, AM
Faber, SM
Ferguson, HC
Grogin, NA
Kocevski, DD
Koo, DC
Lai, K
Lotz, JM
Lucas, RA
McGrath, EJ
Ogaz, S
Rajan, A
Riess, AG
Rodney, SA
Strolger, L
Casertano, S
Castellano, M
Dahlen, T
Dickinson, M
Dolch, T
Fontana, A
Giavalisco, M
Grazian, A
Guo, YC
Hathi, NP
Huang, KH
van der Wel, A
Yan, HJ
Acquaviva, V
Alexander, DM
Almaini, O
Ashby, MLN
Barden, M
Bell, EF
Bournaud, F
Brown, TM
Caputi, KI
Cassata, P
Challis, PJ
Chary, RR
Cheung, E
Cirasuolo, M
Conselice, CJ
Cooray, AR
Croton, DJ
Daddi, E
Dave, R
de Mello, DF
de Ravel, L
Dekel, A
Donley, JL
Dunlop, JS
Dutton, AA
Elbaz, D
Fazio, GG
Filippenko, AV
Finkelstein, SL
Frazer, C
Gardner, JP
Garnavich, PM
Gawiser, E
Gruetzbauch, R
Hartley, WG
Haussler, B
Herrington, J
Hopkins, PF
Huang, JS
Jha, SW
Johnson, A
Kartaltepe, JS
Khostovan, AA
Kirshner, RP
Lani, C
Lee, KS
Li, WD
Madau, P
McCarthy, PJ
McIntosh, DH
McLure, RJ
McPartland, C
Mobasher, B
Moreira, H
Mortlock, A
Moustakas, LA
Mozena, M
Nandra, K
Newman, JA
Nielsen, JL
Niemi, S
Noeske, KG
Papovich, CJ
Pentericci, L
Pope, A
Primack, JR
Ravindranath, S
Reddy, NA
Renzini, A
Rix, HW
Robaina, AR
Rosario, DJ
Rosati, P
Salimbeni, S
Scarlata, C
Siana, B
Simard, L
Smidt, J
Snyder, D
Somerville, RS
Spinrad, H
Straughn, AN
Telford, O
Teplitz, HI
Trump, JR
Vargas, C
Villforth, C
Wagner, CR
Wandro, P
Wechsler, RH
Weiner, BJ
Wiklind, T
Wild, V
Wilson, G
Wuyts, S
Yun, MS
AF Koekemoer, Anton M.
Faber, S. M.
Ferguson, Henry C.
Grogin, Norman A.
Kocevski, Dale D.
Koo, David C.
Lai, Kamson
Lotz, Jennifer M.
Lucas, Ray A.
McGrath, Elizabeth J.
Ogaz, Sara
Rajan, Abhijith
Riess, Adam G.
Rodney, Steve A.
Strolger, Louis
Casertano, Stefano
Castellano, Marco
Dahlen, Tomas
Dickinson, Mark
Dolch, Timothy
Fontana, Adriano
Giavalisco, Mauro
Grazian, Andrea
Guo, Yicheng
Hathi, Nimish P.
Huang, Kuang-Han
van der Wel, Arjen
Yan, Hao-Jing
Acquaviva, Viviana
Alexander, David M.
Almaini, Omar
Ashby, Matthew L. N.
Barden, Marco
Bell, Eric F.
Bournaud, Frederic
Brown, Thomas M.
Caputi, Karina I.
Cassata, Paolo
Challis, Peter J.
Chary, Ranga-Ram
Cheung, Edmond
Cirasuolo, Michele
Conselice, Christopher J.
Cooray, Asantha Roshan
Croton, Darren J.
Daddi, Emanuele
Dave, Romeel
de Mello, Duilia F.
de Ravel, Loic
Dekel, Avishai
Donley, Jennifer L.
Dunlop, James S.
Dutton, Aaron A.
Elbaz, David
Fazio, Giovanni G.
Filippenko, Alexei V.
Finkelstein, Steven L.
Frazer, Chris
Gardner, Jonathan P.
Garnavich, Peter M.
Gawiser, Eric
Gruetzbauch, Ruth
Hartley, Will G.
Haeussler, Boris
Herrington, Jessica
Hopkins, Philip F.
Huang, Jia-Sheng
Jha, Saurabh W.
Johnson, Andrew
Kartaltepe, Jeyhan S.
Khostovan, Ali A.
Kirshner, Robert P.
Lani, Caterina
Lee, Kyoung-Soo
Li, Weidong
Madau, Piero
McCarthy, Patrick J.
McIntosh, Daniel H.
McLure, Ross J.
McPartland, Conor
Mobasher, Bahram
Moreira, Heidi
Mortlock, Alice
Moustakas, Leonidas A.
Mozena, Mark
Nandra, Kirpal
Newman, Jeffrey A.
Nielsen, Jennifer L.
Niemi, Sami
Noeske, Kai G.
Papovich, Casey J.
Pentericci, Laura
Pope, Alexandra
Primack, Joel R.
Ravindranath, Swara
Reddy, Naveen A.
Renzini, Alvio
Rix, Hans-Walter
Robaina, Aday R.
Rosario, David J.
Rosati, Piero
Salimbeni, Sara
Scarlata, Claudia
Siana, Brian
Simard, Luc
Smidt, Joseph
Snyder, Diana
Somerville, Rachel S.
Spinrad, Hyron
Straughn, Amber N.
Telford, Olivia
Teplitz, Harry I.
Trump, Jonathan R.
Vargas, Carlos
Villforth, Carolin
Wagner, Cory R.
Wandro, Pat
Wechsler, Risa H.
Weiner, Benjamin J.
Wiklind, Tommy
Wild, Vivienne
Wilson, Grant
Wuyts, Stijn
Yun, Min S.
TI CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY
SURVEY-THE HUBBLE SPACE TELESCOPE OBSERVATIONS, IMAGING DATA PRODUCTS,
AND MOSAICS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE cosmology: observations; galaxies: high-redshift
ID STAR-FORMING GALAXIES; INTEGRAL FIELD SPECTROSCOPY; PROBE WMAP
OBSERVATIONS; UV LUMINOSITY FUNCTIONS; EXTENDED GROTH STRIP; EARLY DATA
RELEASE; HIGH-REDSHIFT; MASSIVE GALAXIES; IA SUPERNOVAE; SKY SURVEY
AB This paper describes the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). This survey is designed to document the evolution of galaxies and black holes at z approximate to 1.5-8, and to study Type Ia supernovae at z > 1.5. Five premier multi-wavelength sky regions are selected, each with extensive multi-wavelength observations. The primary CANDELS data consist of imaging obtained in the Wide Field Camera 3 infrared channel (WFC3/IR) and the WFC3 ultraviolet/optical channel, along with the Advanced Camera for Surveys (ACS). The CANDELS/Deep survey covers similar to 125 arcmin(2) within GOODS-N and GOODS-S, while the remainder consists of the CANDELS/Wide survey, achieving a total of similar to 800 arcmin(2) across GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-Deep Survey). We summarize the observational aspects of the survey as motivated by the scientific goals and present a detailed description of the data reduction procedures and products from the survey. Our data reduction methods utilize the most up-to-date calibration files and image combination procedures. We have paid special attention to correcting a range of instrumental effects, including charge transfer efficiency degradation for ACS, removal of electronic bias-striping present in ACS data after Servicing Mission 4, and persistence effects and other artifacts in WFC3/IR. For each field, we release mosaics for individual epochs and eventual mosaics containing data from all epochs combined, to facilitate photometric variability studies and the deepest possible photometry. A more detailed overview of the science goals and observational design of the survey are presented in a companion paper.
C1 [Koekemoer, Anton M.; Ferguson, Henry C.; Grogin, Norman A.; Lotz, Jennifer M.; Lucas, Ray A.; Ogaz, Sara; Rajan, Abhijith; Casertano, Stefano; Dahlen, Tomas; Huang, Kuang-Han; Brown, Thomas M.; Donley, Jennifer L.; Niemi, Sami; Noeske, Kai G.; Somerville, Rachel S.; Villforth, Carolin; Wiklind, Tommy] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Faber, S. M.; Kocevski, Dale D.; Koo, David C.; Lai, Kamson; McGrath, Elizabeth J.; Cheung, Edmond; Johnson, Andrew; Madau, Piero; McPartland, Conor; Mozena, Mark; Primack, Joel R.; Rosario, David J.; Snyder, Diana; Trump, Jonathan R.; Wandro, Pat] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Riess, Adam G.; Rodney, Steve A.; Dolch, Timothy; Huang, Kuang-Han; Kartaltepe, Jeyhan S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Strolger, Louis] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42101 USA.
[Castellano, Marco; Fontana, Adriano; Grazian, Andrea; Pentericci, Laura] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Dickinson, Mark; Pope, Alexandra; Reddy, Naveen A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Giavalisco, Mauro; Guo, Yicheng; Cassata, Paolo; Salimbeni, Sara; Wilson, Grant; Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Hathi, Nimish P.; McCarthy, Patrick J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[van der Wel, Arjen; Rix, Hans-Walter; Rosati, Piero] European So Observ, D-85748 Garching, Germany.
[Yan, Hao-Jing] Ohio State Univ, Res Fdn, Columbus, OH 43210 USA.
[Acquaviva, Viviana; Gawiser, Eric; Jha, Saurabh W.; Moreira, Heidi; Vargas, Carlos] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Alexander, David M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Almaini, Omar; Conselice, Christopher J.; Gruetzbauch, Ruth; Hartley, Will G.; Haeussler, Boris; Lani, Caterina; Mortlock, Alice] Univ Nottingham, Nottingham NG7 2RD, England.
[Ashby, Matthew L. N.; Fazio, Giovanni G.; Kirshner, Robert P.; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Barden, Marco] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
[Bell, Eric F.; Herrington, Jessica] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Bournaud, Frederic; Daddi, Emanuele] CEA, F-91191 Gif Sur Yvette, France.
[Bournaud, Frederic; Daddi, Emanuele] Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Caputi, Karina I.; Cirasuolo, Michele] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Challis, Peter J.] Harvard Coll Observ, Cambridge, MA USA.
[Cooray, Asantha Roshan; Frazer, Chris; Khostovan, Ali A.; Smidt, Joseph] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA.
[Croton, Darren J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Dave, Romeel; Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[de Mello, Duilia F.; Gardner, Jonathan P.; Straughn, Amber N.] NASA, Goddard Space Flight Ctr, Lab Observat Cosmol, Greenbelt, MD 20771 USA.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Dutton, Aaron A.] Univ Victoria, Victoria, BC, Canada.
[Elbaz, David] CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Filippenko, Alexei V.; Hopkins, Philip F.; Li, Weidong; Spinrad, Hyron] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Finkelstein, Steven L.; Papovich, Casey J.] Texas A&M Res Fdn, College Stn, TX 77843 USA.
[Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Huang, Jia-Sheng] Smithsonian Inst Astrophys Observ, Cambridge, MA USA.
[Lee, Kyoung-Soo] Yale Ctr Astron & Astrophys, New Haven, CT USA.
[McIntosh, Daniel H.; Nielsen, Jennifer L.; Wagner, Cory R.] Univ Missouri Kansas City, Dept Phys, Kansas City, MO 64110 USA.
[Mobasher, Bahram] UC Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nandra, Kirpal] Univ London Imperial Coll Sci Technol & Med, London, England.
[Newman, Jeffrey A.; Telford, Olivia] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Newman, Jeffrey A.] PITT PAC, Pittsburgh, PA USA.
[Ravindranath, Swara] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Renzini, Alvio] Osserv Astron Padova, Padua, Italy.
[Robaina, Aday R.] IEEC, Inst Ciencies Cosmos, ICC UB, Barcelona 08028, Spain.
[Wechsler, Risa H.] Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Wechsler, Risa H.] SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
RP Koekemoer, AM (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RI Daddi, Emanuele/D-1649-2012; Conselice, Christopher/B-4348-2013;
Bournaud, Frederic/K-1263-2013; Hathi, Nimish/J-7092-2014;
OI Koekemoer, Anton/0000-0002-6610-2048; Brown, Thomas/0000-0002-1793-9968;
Bell, Eric/0000-0002-5564-9873; Daddi, Emanuele/0000-0002-3331-9590;
Hathi, Nimish/0000-0001-6145-5090; Conselice,
Christopher/0000-0003-1949-7638; Cheung, Edmond/0000-0001-8546-1428;
Moustakas, Leonidas/0000-0003-3030-2360; fontana,
adriano/0000-0003-3820-2823
FU NASA through the Space Telescope Science Institute [GO-12060, GO-12099];
NASA [NAS5-26555]
FX We thank the referee for very helpful and valuable comments on this
manuscript. We also thank our Program Coordinators, Tricia Royle and
Beth Perriello, along with the rest of the Hubble planning team, for
their efforts to schedule this challenging program. The WFC3 team has
made substantial contributions to the program by calibrating and
characterizing the instrument and have provided much useful advice.
Rychard Bouwens provided helpful input on the observing strategy for the
CANDELS/Deep survey. John Mackenty suggested using 2 x 2 on-chip binning
for the UV observations, which will significantly improve the
signal-to-noise ratio of those observations. The CANDELS observations
would not have been possible without the contributions of hundreds of
other individuals to the Hubble missions and the development and
installation of new instruments. Support for HST Programs GO-12060 and
GO-12099 (the SN component) is provided by NASA through a grant from the
Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555.
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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 DEC
PY 2011
VL 197
IS 2
AR 36
DI 10.1088/0067-0049/197/2/36
PG 36
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300022
ER
PT J
AU Massaro, F
Harris, DE
Cheung, CC
AF Massaro, F.
Harris, D. E.
Cheung, C. C.
TI LARGE-SCALE EXTRAGALACTIC JETS IN THE CHANDRA ERA. I. DATA REDUCTION AND
ANALYSIS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: active; galaxies: jets; radio continuum: galaxies; radiation
mechanisms: non-thermal; relativistic processes; X-rays: galaxies
ID X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE;
MAGNETIC-FIELD STRENGTHS; EXTENDED RADIO JETS; HOT-SPOTS; DEEP CHANDRA;
COMPLETE SAMPLE; QUASAR JETS; XMM-NEWTON
AB In this paper, we report the first stages of an investigation into the X-ray properties of extragalactic jets. Our approach is to subject all sources for which X-ray emission has been detected by Chandra to uniform reduction procedures. Using Chandra archival data for 106 such sources, we measure X-ray fluxes in three bands and compare these to radio fluxes. We discuss the sample, the reduction methods, and present first results for the ratio of X-ray to radio flux for jet knots and hotspots. In particular, we apply statistical tests to various distributions of key observational parameters to evaluate differences between the different classes of sources. Subsequent papers will deal with various ramifications such as considerations of how well the observational data fulfill expectations of the different radiation processes proposed for the knots of FRI radio galaxies and quasars.
C1 [Massaro, F.; Harris, D. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
RP Massaro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Massaro, Francesco/L-9102-2016
OI Massaro, Francesco/0000-0002-1704-9850
FU National Science Foundation; Commonwealth of Australia; Fondazione
Angelo Della Riccia at SAO; NASA [AR6-7013X, NAS8-39073, GO8-9114A,
NNX10AD50G]; Foundation BLANCEFLOR Boncompagni-Ludovisi, n'ee Bildt
FX Several radio maps were downloaded from the NVAS (NRAO VLA Archive
Survey) and from the MERLIN archive. The National Radio Astronomy
Observatory is operated by Associated Universities, Inc., under contract
with the National Science Foundation. MERLIN is a National Facility
operated by the University of Manchester at Jodrell Bank Observatory on
behalf of STFC. The Australia Telescope is funded by the Commonwealth of
Australia for operation as a National Facility managed by CSIRO. This
research has made use of data obtained through the High Energy
Astrophysics Science Archive Research Center Online Service, provided by
the NASA/Goddard Space Flight Center.; F.M. acknowledges the Fondazione
Angelo Della Riccia for the grant awarded him to support his research at
SAO during 2011. The XJET Web site is partially supported by NASA grant
AR6-7013X and NASA contract NAS8-39073. The work at SAO was supported by
NASA-GRANTS GO8-9114A and NNX10AD50G. F. M. acknowledges the Foundation
BLANCEFLOR Boncompagni-Ludovisi, n'ee Bildt for the grants awarded him
in 2009 and in 2010 to support his research at SAO.
NR 97
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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 DEC
PY 2011
VL 197
IS 2
AR 24
DI 10.1088/0067-0049/197/2/24
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300010
ER
PT J
AU Schwarz, GJ
Ness, JU
Osborne, JP
Page, KL
Evans, PA
Beardmore, AP
Walter, FM
Helton, LA
Woodward, CE
Bode, M
Starrfield, S
Drake, JJ
AF Schwarz, Greg J.
Ness, Jan-Uwe
Osborne, J. P.
Page, K. L.
Evans, P. A.
Beardmore, A. P.
Walter, Frederick M.
Helton, L. Andrew
Woodward, Charles E.
Bode, Mike
Starrfield, Sumner
Drake, Jeremy J.
TI SWIFT X-RAY OBSERVATIONS OF CLASSICAL NOVAE. II. THE SUPER SOFT SOURCE
SAMPLE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE novae, cataclysmic variables; ultraviolet: stars; X-rays: stars
ID INTERMEDIATE POLAR CANDIDATE; EXPANDING NEBULAR REMNANT; XMM-NEWTON
OBSERVATIONS; HIGH-SPEED PHOTOMETRY; V1974 CYGNI 1992; MIRA V407 CYG;
RS-OPHIUCHI; SPECTRAL EVOLUTION; RECURRENT NOVAE; 2006 OUTBURST
AB The Swift gamma-ray burst satellite is an excellent facility for studying novae. Its rapid response time and sensitive X-ray detector provides an unparalleled opportunity to investigate the previously poorly sampled evolution of novae in the X-ray regime. This paper presents Swift observations of 52 Galactic/Magellanic Cloud novae. We included the X-Ray Telescope (0.3-10 keV) instrument count rates and the UltraViolet and Optical Telescope (1700-8000 angstrom) filter photometry. Also included in the analysis are the publicly available pointed observations of 10 additional novae the X-ray archives. This is the largest X-ray sample of Galactic/Magellanic Cloud novae yet assembled and consists of 26 novae with Super Soft X-ray emission, 19 from Swift observations. The data set shows that the faster novae have an early hard X-ray phase that is usually missing in slower novae. The Super Soft X-ray phase occurs earlier and does not last as long in fast novae compared to slower novae. All the Swift novae with sufficient observations show that novae are highly variable with rapid variability and different periodicities. In the majority of cases, nuclear burning ceases less than three years after the outburst begins. Previous relationships, such as the nuclear burning duration versus t(2) or the expansion velocity of the eject and nuclear burning duration versus the orbital period, are shown to be poorly correlated with the full sample indicating that additional factors beyond the white dwarf mass and binary separation play important roles in the evolution of a nova outburst. Finally, we confirm two optical phenomena that are correlated with strong, soft X-ray emission which can be used to further increase the efficiency of X-ray campaigns.
C1 [Schwarz, Greg J.] Amer Astron Soc, Washington, DC 20009 USA.
[Ness, Jan-Uwe] ESAC, XMM Newton Sci Operat Ctr, Madrid 28691, Spain.
[Osborne, J. P.; Page, K. L.; Evans, P. A.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Walter, Frederick M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Helton, L. Andrew] NASA, SOFIA Sci Ctr, USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Woodward, Charles E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Bode, Mike] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Starrfield, Sumner] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Drake, Jeremy J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Schwarz, GJ (reprint author), Amer Astron Soc, 2000 Florida Ave NW,Suite 400, Washington, DC 20009 USA.
EM Greg.Schwarz@aas.org
OI Schwarz, Gregory/0000-0002-0786-7307
FU NASA [NNH08ZDA001N1, NAS8-39073]; STFC; NSF
FX This research has made use of data obtained from NASA's Swift satellite.
We thank Neil Gehrels and the Swift team for generous allotments of ToO
and fill in time. Funding support from NASA NNH08ZDA001N1. Stony Brook
University's initial participation in the SMARTS consortium was made
possible by generous contributions from the Dean of Arts and Sciences,
the Provost, and the Vice President for Research of Stony Brook
University. We acknowledge with thanks the variable star observations
from the AAVSO International Database contributed by observers worldwide
and used in this research. J.P.O., K. P., P. E. and A. B. acknowledge
the support of the STFC. S. S. acknowledges partial support from NASA
and NSF grants to ASU. J.J.D. was supported by NASA contract NAS8-39073
to the Chandra X-ray Center.
NR 315
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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 DEC
PY 2011
VL 197
IS 2
AR 31
DI 10.1088/0067-0049/197/2/31
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300017
ER
PT J
AU Strader, J
Romanowsky, AJ
Brodie, JP
Spitler, LR
Beasley, MA
Arnold, JA
Tamura, N
Sharples, RM
Arimoto, N
AF Strader, Jay
Romanowsky, Aaron J.
Brodie, Jean P.
Spitler, Lee R.
Beasley, Michael A.
Arnold, Jacob A.
Tamura, Naoyuki
Sharples, Ray M.
Arimoto, Nobuo
TI WIDE-FIELD PRECISION KINEMATICS OF THE M87 GLOBULAR CLUSTER SYSTEM
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE dark matter; galaxies: elliptical and lenticular, cD; galaxies:
individual (M87); galaxies: kinematics and dynamics; galaxies: star
clusters: general; globular clusters: general
ID EARLY-TYPE GALAXIES; COMPACT DWARF GALAXIES; ACS-VIRGO-CLUSTER;
DARK-MATTER HALOS; SUPERMASSIVE BLACK-HOLE; EXTENDED STAR-CLUSTERS; M60
NGC 4649; ELLIPTIC GALAXIES; X-RAY; FORNAX CLUSTER
AB We present the most extensive combined photometric and spectroscopic study to date of the enormous globular cluster (GC) system around M87, the central giant elliptical galaxy in the nearby Virgo Cluster. Using observations from DEIMOS and the Low Resolution Imaging Spectrometer at Keck, and Hectospec on the Multiple Mirror Telescope, we derive new, precise radial velocities for 451 GCs around M87, with projected radii from similar to 5 to 185 kpc. We combine these measurements with literature data for a total sample of 737 objects, which we use for a re-examination of the kinematics of the GC system of M87. The velocities are analyzed in the context of archival wide-field photometry and a novel Hubble Space Telescope catalog of half-light radii, which includes sizes for 344 spectroscopically confirmed clusters. We use this unique catalog to identify 18 new candidate ultracompact dwarfs and to help clarify the relationship between these objects and true GCs. We find much lower values for the outer velocity dispersion and rotation of the GC system than in earlier papers and also differ from previous work in seeing no evidence for a transition in the inner halo to a potential dominated by the Virgo Cluster, nor for a truncation of the stellar halo. We find little kinematical evidence for an intergalactic GC population. Aided by the precision of the new velocity measurements, we see significant evidence for kinematical substructure over a wide range of radii, indicating that M87 is in active assembly. A simple, scale-free analysis finds less dark matter within similar to 85 kpc than in other recent work, reducing the tension between X-ray and optical results. In general, out to a projected radius of similar to 150 kpc, our data are consistent with the notion that M87 is not dynamically coupled to the Virgo Cluster; the core of Virgo may be in the earliest stages of assembly.
C1 [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Romanowsky, Aaron J.; Brodie, Jean P.; Beasley, Michael A.; Arnold, Jacob A.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Spitler, Lee R.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Beasley, Michael A.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Tamura, Naoyuki] Natl Inst Nat Sci, Natl Astron Observ Japan, Hilo, HI 96720 USA.
[Sharples, Ray M.] Univ Durham, Dept Phys, Durham, England.
[Arimoto, Nobuo] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
RP Strader, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jstrader@cfa.harvard.edu
RI Spitler, Lee/A-9867-2013; Sharples, Ray/N-7309-2013
OI Spitler, Lee/0000-0001-5185-9876; Sharples, Ray/0000-0003-3449-8583
FU NASA [NAS5-26555]; NSF [AST-0808099, AST-0909237, AST-1101733,
AST-1109878]; Canadian Space Agency; W. M. Keck Foundation; Smithsonian
Astrophysical Observatory; National Science Foundation at the Kavli
Institute for Theoretical Physics [NSF PHY05-51164]
FX This paper is dedicated to the memory of John P. Huchra, a fearless
pioneer in the spectroscopic study of M87 GCs. Special thanks to Karl
Gebhardt and Jeremy Murphy for extensive discussions and for providing
their results in advance of publications. We also thank Magda Arnaboldi,
Michele Cappellari, Payel Das, Juan Madrid, and Soeren Larsen for
providing their results in electronic form, and Jurg Diemand and Chris
Mihos for helpful comments. We thank Nelson Caldwell for his assistance
with the Hectospec observations, and Jason X. Prochaska and Kate Rubin
for software help. J.S. was supported by NASA through a Hubble
Fellowship, administered by the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in
Astronomy, Incorporated, under NASA contract NAS5-26555. J.B. and A.J.R.
acknowledge support from the NSF through grants AST-0808099,
AST-0909237, AST-1101733, and AST-1109878. This research used the
facilities of the Canadian Astronomy Data Centre operated by the
National Research Council of Canada with the support of the Canadian
Space Agency. Much of the data presented herein were obtained at the W.
M. Keck Observatory, which is operated as a scientific partnership among
the California Institute of Technology, the University of California,
and the National Aeronautics and Space Administration. The Observatory
was made possible by the generous financial support of the W. M. Keck
Foundation. Observations reported here were obtained at the MMT
Observatory, a joint facility of the Smithsonian Institution and the
University of Arizona. This paper was based in part on data collected at
Subaru Telescope, which is operated by the National Astronomical
Observatory of Japan. This paper uses data products produced by the OIR
Telescope Data Center, supported by the Smithsonian Astrophysical
Observatory. This research was supported in part by the National Science
Foundation under grant no. NSF PHY05-51164 while at the Kavli Institute
for Theoretical Physics.
NR 223
TC 94
Z9 94
U1 1
U2 5
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 DEC
PY 2011
VL 197
IS 2
AR 33
DI 10.1088/0067-0049/197/2/33
PG 49
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 864MN
UT WOS:000298244300019
ER
PT J
AU Zoogman, P
Jacob, DJ
Chance, K
Zhang, L
Le Sager, P
Fiore, AM
Eldering, A
Liu, X
Natraj, V
Kulawik, SS
AF Zoogman, Peter
Jacob, Daniel J.
Chance, Kelly
Zhang, Lin
Le Sager, Philippe
Fiore, Arlene M.
Eldering, Annmarie
Liu, Xiong
Natraj, Vijay
Kulawik, Susan S.
TI Ozone air quality measurement requirements for a geostationary satellite
mission
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Air quality; Ozone; Kalman filter; Assimilation; Remote sensing
ID TROPOSPHERIC OZONE; MONITORING INSTRUMENT; POLLUTION INFLUENCES;
UNITED-STATES; CHEMISTRY; PROFILES; MODELS; TES
AB We conduct an Observing System Simulation Experiment (OSSE) to test the ability of geostationary satellite measurements of ozone in different spectral regions to constrain surface ozone concentrations through data assimilation. Our purpose is to define instrument requirements for the NASA GEO-CAPE geostationary air quality mission over North America. We consider instruments using different spectral combinations of UV (290-340 nm), Vis (560-620 nm), and thermal IR (TIR, 9.6 mu m). Hourly ozone data from the MOZART global 3-D chemical transport model (CTM) are taken as the "true" atmosphere to be sampled by the instruments for July 2001. The resulting synthetic data are assimilated in the GEOS-Chem CTM using a Kalman filter. The MOZART and GEOS-Chem CTMs have independent heritages and use different assimilated meteorological data sets for the same period, making for an objective OSSE. We show that hourly observations of ozone from geostationary orbit improve the assimilation considerably relative to daily observation from low earth orbit, and that broad observation over the ocean is unnecessary if the objective is to constrain surface ozone distribution over land. We also show that there is little propagation of ozone information from the free troposphere to the surface, so that instrument sensitivity in the boundary layer is essential. UV + Vis and UV + TIR spectral combinations improve greatly the information on surface ozone relative to UV alone. UV + TIR is preferable under high-sensitivity conditions with strong thermal contrast at the surface, but UV + Vis is preferable under low-sensitivity conditions. Assimilation of data from a UV + Vis + TIR instrument reduces the GEOS-Chem error for surface ozone by a factor of two. Observation in the TIR is critical to obtain ozone information in the upper troposphere relevant to climate forcing. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Zoogman, Peter; Jacob, Daniel J.; Zhang, Lin] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Jacob, Daniel J.; Le Sager, Philippe] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Chance, Kelly; Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fiore, Arlene M.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Eldering, Annmarie; Natraj, Vijay; Kulawik, Susan S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Zoogman, P (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA.
EM zoogman@fas.harvard.edu
RI Zhang, Lin/A-6729-2008; Chem, GEOS/C-5595-2014; Zhang, Lin/H-9801-2014;
Liu, Xiong/P-7186-2014;
OI Zhang, Lin/0000-0003-2383-8431; Liu, Xiong/0000-0003-2939-574X; Zoogman,
Peter/0000-0002-8848-4999; Chance, Kelly/0000-0002-7339-7577
FU NASA; NASA Earth Science Division, Flight Directorate
FX This work was supported by the NASA Atmospheric Composition and Modeling
Program, by the NASA Earth Science Division, Flight Directorate, and by
a NASA Earth and Space Science Fellowship to Peter Zoogman.
NR 36
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U1 3
U2 23
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD DEC
PY 2011
VL 45
IS 39
BP 7143
EP 7150
DI 10.1016/j.atmosenv.2011.05.058
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 862UU
UT WOS:000298120400016
ER
PT J
AU Natraj, V
Liu, X
Kulawik, S
Chance, K
Chatfield, R
Edwards, DP
Eldering, A
Francis, G
Kurosu, T
Pickering, K
Spurr, R
Worden, H
AF Natraj, Vijay
Liu, Xiong
Kulawik, Susan
Chance, Kelly
Chatfield, Robert
Edwards, David P.
Eldering, Annmarie
Francis, Gene
Kurosu, Thomas
Pickering, Kenneth
Spurr, Robert
Worden, Helen
TI Multi-spectral sensitivity studies for the retrieval of tropospheric and
lowermost tropospheric ozone from simulated clear-sky GEO-CAPE
measurements
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Multi-spectral; Ozone; Retrieval; Sensitivity; Troposphere;
Geostationary platform; GEO-CAPE
ID MOLECULAR SPECTROSCOPIC DATABASE; RADIATIVE-TRANSFER; MONITORING
INSTRUMENT; PROFILE RETRIEVALS; NADIR RETRIEVALS; AIR-QUALITY;
SATELLITE; POLARIZATION; TES; OBJECTIVES
AB One of the important science requirements of the Geostationary Coastal and Air Pollution Events (GEO-CAPE) mission is to be able to measure ozone with two degrees of freedom in the troposphere and sensitivity in the lowest 2 km (lowermost troposphere, LMT), in order to characterize air quality and boundary layer transport of pollution. Currently available remote sensing techniques utilize backscattered solar ultraviolet (UV) radiances or thermal infrared (TIR) emissions to perform ozone retrievals. However, in the TIR, measurement sensitivity to the LMT requires high thermal contrast between the Earth's surface and the near-surface (tens to hundreds of meters above surface) atmosphere, while in the UV, the measurement sensitivity to the LMT is low because of Rayleigh scattering. In this paper, we explore the feasibility of using multi-spectral intensity measurements in the UV, visible (VIS), mid infrared (MIR) and TIR, and polarization measurements in the UV/VIS, to improve tropospheric and lowermost tropospheric ozone retrievals.
Simulations for 16 cloud and aerosol free atmospheric profiles spanning a range of ozone mixing ratios indicate that adding VIS measurements to UV measurements significantly enhances the sensitivity to lowermost tropospheric ozone, but only makes a slight improvement to the total degrees of freedom for signal (DFS). On the other hand, the combination of UV and TIR significantly improves the total DFS as well as the lowermost tropospheric DFS.
The analysis presented here is a necessary and important first step for defining spectral regions that can meet the GEO-CAPE measurement requirements, and subsequently, the requirements for instrumentation. In this work, the principle of multi-spectral retrievals has been extended from previously published literature and we show that the UV + VIS, UV + TIR and UV + VIS + TIR combinations have the potential to meet the GEO-CAPE measurement requirements for tropospheric ozone. Our analysis includes errors from water and surface properties: further analysis is needed to include temperature, additional gas interferents, clouds, aerosols and more realistic surface properties. These simulations must be run on a much larger dataset, followed by OSSEs (Observing System Simulation Experiments), where simulated retrievals are assimilated into chemical-transport models, to quantitatively assess the impact of the proposed measurements for constraining the spatiotemporal distribution of ozone in the LMT for basic science studies and applications such as air quality forecasts. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Natraj, Vijay; Kulawik, Susan; Eldering, Annmarie; Kurosu, Thomas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chatfield, Robert] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Edwards, David P.; Francis, Gene; Worden, Helen] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Pickering, Kenneth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Spurr, Robert] RT Solut Inc, Cambridge, MA 02138 USA.
RP Natraj, V (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Vijay.Natraj@jpl.nasa.gov
RI Pickering, Kenneth/E-6274-2012; Liu, Xiong/P-7186-2014;
OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577
FU Earth Science Division of the NASA Science Mission Directorate; Aura OMI
project; National Science Foundation
FX A portion of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology. Funding for this effort was provided
by the Earth Science Division of the NASA Science Mission Directorate.
X.L. was funded by the Aura OMI project. The National Center for
Atmospheric Research is sponsored by the National Science Foundation.
The authors would like to thank the two anonymous reviewers for their
insightful suggestions that undoubtedly improved the quality of the
paper.
NR 89
TC 32
Z9 33
U1 1
U2 25
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD DEC
PY 2011
VL 45
IS 39
BP 7151
EP 7165
DI 10.1016/j.atmosenv.2011.09.014
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 862UU
UT WOS:000298120400017
ER
PT J
AU Peterson, K
Birkmeyer, P
Dudley, R
Fearing, RS
AF Peterson, K.
Birkmeyer, P.
Dudley, R.
Fearing, R. S.
TI A wing-assisted running robot and implications for avian flight
evolution
SO BIOINSPIRATION & BIOMIMETICS
LA English
DT Article
ID ARCHAEOPTERYX; LOCOMOTION; ORIGINS; STROKE; BIRDS; MODEL
AB DASH+Wings is a small hexapedal winged robot that uses flapping wings to increase its locomotion capabilities. To examine the effects of flapping wings, multiple experimental controls for the same locomotor platform are provided by wing removal, by the use of inertially similar lateral spars, and by passive rather than actively flapping wings. We used accelerometers and high-speed cameras to measure the performance of this hybrid robot in both horizontal running and while ascending inclines. To examine consequences of wing flapping for aerial performance, we measured lift and drag forces on the robot at constant airspeeds and body orientations in a wind tunnel; we also determined equilibrium glide performance in free flight. The addition of flapping wings increased the maximum horizontal running speed from 0.68 to 1.29 m s(-1), and also increased the maximum incline angle of ascent from 5.6 degrees to 16.9 degrees. Free flight measurements show a decrease of 10.3 degrees in equilibrium glide slope between the flapping and gliding robot. In air, flapping improved the mean lift: drag ratio of the robot compared to gliding at all measured body orientations and airspeeds. Low-amplitude wing flapping thus provides advantages in both cursorial and aerial locomotion. We note that current support for the diverse theories of avian flight origins derive from limited fossil evidence, the adult behavior of extant flying birds, and developmental stages of already volant taxa. By contrast, addition of wings to a cursorial robot allows direct evaluation of the consequences of wing flapping for locomotor performance in both running and flying.
C1 [Peterson, K.; Birkmeyer, P.; Fearing, R. S.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA.
[Dudley, R.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Dudley, R.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Peterson, K (reprint author), Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA.
EM kevincp@eecs.berkeley.edu; paulb@eecs.berkeley.edu; wings@berkeley.edu;
ronf@eecs.berkeley.edu
FU NSF Center of Integrated Nanomechanical Systems; United States Army
Research Laboratory under the Micro Autonomous Science and Technology
Collaborative Technology Alliance; NSF [IOS-0837866]
FX Thanks to Dennis Evangelista for his assistance with gathering wind
tunnel measurements, David Larson for measuring the wind tunnel
turbulence and Cameron Rose for his assistance with the free-flight
measurements. This work was supported by the NSF Center of Integrated
Nanomechanical Systems (PB) and the United States Army Research
Laboratory under the Micro Autonomous Science and Technology
Collaborative Technology Alliance (KP and RF) and NSF IOS-0837866 (RD).
NR 24
TC 20
Z9 20
U1 2
U2 70
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-3182
J9 BIOINSPIR BIOMIM
JI Bioinspir. Biomim.
PD DEC
PY 2011
VL 6
IS 4
AR 046008
DI 10.1088/1748-3182/6/4/046008
PG 8
WC Engineering, Multidisciplinary; Materials Science, Biomaterials;
Robotics
SC Engineering; Materials Science; Robotics
GA 863CF
UT WOS:000298139700015
PM 22004831
ER
PT J
AU DeVorkin, DH
Neufeld, MJ
AF DeVorkin, David H.
Neufeld, Michael J.
TI Space artifact or Nazi weapon? Displaying the Smithsonian's V-2 missile,
1976-2011
SO ENDEAVOUR
LA English
DT Article
C1 [Neufeld, Michael J.] Smithsonian Inst, NASM Space Hist Div, Natl Air & Space Museum, Washington, DC 20013 USA.
RP Neufeld, MJ (reprint author), Smithsonian Inst, NASM Space Hist Div, Natl Air & Space Museum, MRC 311,POB 37012, Washington, DC 20013 USA.
EM devorkind@si.edu; neufeldm@si.edu
NR 24
TC 4
Z9 4
U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0160-9327
J9 ENDEAVOUR
JI Endeavour
PD DEC
PY 2011
VL 35
IS 4
SI SI
BP 187
EP 195
DI 10.1016/j.endeavour.2011.08.003
PG 9
WC History & Philosophy Of Science; Multidisciplinary Sciences
SC History & Philosophy of Science; Science & Technology - Other Topics
GA 869AV
UT WOS:000298568900009
PM 21868096
ER
PT J
AU France, CAM
Giaccai, JA
Cano, N
AF France, Christine A. M.
Giaccai, Jennifer A.
Cano, Nadia
TI The effects of PVAc treatment and organic solvent removal on delta C-13,
delta N-15, and delta O-18 values of collagen and hydroxyapatite in a
modern bone
SO JOURNAL OF ARCHAEOLOGICAL SCIENCE
LA English
DT Article
DE Stable isotopes; Bone; Collagen; Hydroxyapatite; Polyvinyl acetate; PVAc
ID OXYGEN-ISOTOPE COMPOSITIONS; STABLE-ISOTOPES; DIETARY RECONSTRUCTION;
TROPHIC RELATIONSHIPS; NITROGEN; CARBON; PHOSPHATE; PRESERVATION;
DIAGENESIS; PHYSIOLOGY
AB The stable isotopic analysis of archaeological and paleontological bones has become a common method to examine questions of ecology, climate, and physiology. As researchers addressing such questions incorporate museum collections in their studies, it is necessary to understand the isotopic effects of common preservation techniques utilized in such collections to ensure the preservation of original isotopic values. This study examines the effects of PVAc glue (polyvinyl acetate) applied in acetone solution and the subsequent removal of PVAc using various organic solvents on the delta C-13 and delta N-15 values of extracted bone collagen, the delta C-13 and delta O-18 values of carbonate in bone hydroxyapatite, and the delta O-18 values of phosphate in hydroxyapatite. The data demonstrate that isotopic values in the collagen and phosphate are unaffected by any combination of PVAc treatment and solvent application. The carbonates show little variation in delta C-13 values, but exhibit variable delta O-18 values upon exposure to the PVAc solution. It is here suggested that delta O-18 values from carbonates in PVAc-treated bones do not retain an original isotopic value and should not be included in future studies. Published by Elsevier
C1 [France, Christine A. M.; Giaccai, Jennifer A.; Cano, Nadia] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA.
RP France, CAM (reprint author), Smithsonian Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM francec@si.edu
FU Smithsonian Institution
FX The authors wish to acknowledge the three anonymous reviewers of this
manuscript and their helpful comments which greatly improved its
quality. Analyses were provided with assistance of staff in the
Smithsonian OUSS/MCI Stable Isotope Mass Spectrometry Laboratory and the
Smithsonian MCI GC-MS Laboratory. Funding provided by the Smithsonian
Institution.
NR 44
TC 5
Z9 5
U1 3
U2 21
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 DEC
PY 2011
VL 38
IS 12
BP 3387
EP 3393
DI 10.1016/j.jas.2011.07.024
PG 7
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 852UZ
UT WOS:000297384300019
ER
PT J
AU Speakman, RJ
Little, NC
Creel, D
Miller, MR
Inanez, JG
AF Speakman, Robert J.
Little, Nicole C.
Creel, Darrell
Miller, Myles R.
Inanez, Javier G.
TI Sourcing ceramics with portable XRF spectrometers? A comparison with
INAA using Mimbres pottery from the American Southwest
SO JOURNAL OF ARCHAEOLOGICAL SCIENCE
LA English
DT Article
DE Portable and handheld XRF; INAA; mu XRF; Mimbres and Jornada pottery
ID RAY-FLUORESCENCE SPECTROMETRY; SOUTHERN PERU; IODIDE DETECTOR; SILICATE
ROCKS; EDXRF ANALYSIS; EL-HIBEH; FIELD; PROVENANCE; ARTIFACTS; ISLANDS
AB Seventy-five intact Mimbres and Jornada pottery sherds from the American Southwest were analyzed by portable XRF and instrumental neutron activation analysis (INAA). Examination of the data demonstrates that INAA and portable XRF results for elements common to both analyses can be used to construct similar compositional groups. When individual compositional groups are compared to one another, it is apparent that unambiguous separation of compositional groups is challenging by portable XRF given (1) the limited number of key discriminating elements that can be measured relative to INAA, and (2) the relative analytical precision and accuracy of portable XRF for measurements of intact heterogeneous ceramics. We conclude that sourcing intact ceramics by portable XRF is challenging and that bulk analytical measurements, such as INAA, remain a better approach for sourcing archaeological pottery. Published by Elsevier Ltd.
C1 [Speakman, Robert J.; Little, Nicole C.; Inanez, Javier G.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
[Creel, Darrell] Univ Texas Austin, Texas Archaeol Res Lab, Austin, TX 78712 USA.
[Miller, Myles R.] Geomarine Inc, El Paso, TX 77912 USA.
[Inanez, Javier G.] Univ Barcelona, Dept Prehist Hist Antiga & Arqueol, Barcelona 08001, Catalonia, Spain.
RP Speakman, RJ (reprint author), Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
EM Speakmanj@si.edu
RI Little, Nicole/L-6420-2015;
OI Little, Nicole/0000-0002-9533-3187; Inanez, Javier/0000-0002-1411-8099;
Speakman, Robert/0000-0003-2063-154X
FU NSF; European Commission [PIOF-GA-2008-223319]
FX We acknowledge all the Southwestern archaeologists who have submitted
Mimbres, Jornada, and related ceramics for INAA at Texas A&M and MURR.
Steve Shackley, Mike Glascock, Steven LeBlanc, and three anonymous
reviewers are thanked for their thoughtful comments and criticisms of an
earlier draft of this paper. INAA analyses were conducted at the
University of Missouri Research Reactor and subsidized by various NSF
grants awarded to Glascock and colleagues. JGI is indebted to the
support of the Marie Curie International Outgoing Fellowships program,
endorsed by the European Commission ("ARCHSYMB", PIOF-GA-2008-223319).
NR 46
TC 47
Z9 47
U1 2
U2 33
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 DEC
PY 2011
VL 38
IS 12
BP 3483
EP 3496
DI 10.1016/j.jas.2011.08.011
PG 14
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 852UZ
UT WOS:000297384300029
ER
PT J
AU Long, WC
Grow, JN
Majoris, JE
Hines, AH
AF Long, W. Christopher
Grow, Jacob N.
Majoris, John E.
Hines, Anson H.
TI Effects of anthropogenic shoreline hardening and invasion by Phragmites
australis on habitat quality for juvenile blue crabs (Callinectes
sapidus)
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Blue crab; Callinectes sapidus; Phragmites australis; Predation;
Shoreline development; Spartina
ID CORDGRASS SPARTINA-ALTERNIFLORA; CHESAPEAKE-BAY; COMMON REED;
SALT-MARSH; SHALLOW-WATER; FUNDULUS-HETEROCLITUS; BENTHIC COMMUNITIES;
ESTUARINE HABITATS; TEMPORAL VARIATION; TIDAL MARSHES
AB Unvegetated, shallow water habitats adjacent to marshes are an important nursery for juvenile blue crabs. Callinectes sapidus, in Chesapeake Bay. Alteration of the shoreline, either through the replacement of marshes with anthropogenic structures, such as riprap and bulkheads, or through the replacement of the native marsh grass Spartina sp. (Spartina) with the invasive Phragmites australis (Phragmites), may affect the value of this habitat as a nursery. In this study, we compared the effects of four common shoreline types, bulkheads, riprap, Phragmites marshes, and Spartina marshes, on food availability, feeding, growth, and survival of juvenile blue crabs in adjacent subtidal areas, as well as on the abundance and size of predators in the South River, Maryland. Sites with each shoreline type were randomly selected. We used benthic cores to sample macrobenthic prey and performed gut content analysis on caged crabs to examine food availability and feeding. Growth was estimated using caged crabs. Survival was assayed with a tethering experiment and predators were sampled with a seine net. Riprap had a lower abundance of macrofaunal prey, and the macrofaunal community differed from both marsh types in that it had it had smaller an more opportunistic species such as nematodes and small polychaetes compared to more bivalves and larger polychaetes at the marsh sites; however, gut contents and growth did not vary among shoreline types. Predation pressure on juvenile blue crabs was highest at bulkhead sites and lowest at riprap. Predator abundance did not vary among the shoreline types, though piscine predators were smaller in size near Spartina marshes compared to the other shorelines. We conclude that shoreline hardening substantially reduced the value of shoreline habitats for juvenile blue crabs, but that Spartina and Phragmites are functionally equivalent. Published by Elsevier B.V.
C1 [Long, W. Christopher; Grow, Jacob N.; Majoris, John E.; Hines, Anson H.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Long, WC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM chris.long@noaa.gov
RI Long, William/C-7074-2009
OI Long, William/0000-0002-7095-1245
FU NOAA Chesapeake Bay Program Office; Marine Science Network from the
Smithsonian; Wabash College through the Wabash-SERC
FX We thank M. Kramer, M. Goodison, R. Aguilar, and D. Long for help with
field work. We thank M. Kramer and H. Soulen for help with sorting and
identifying benthic organisms in the laboratory. Critical comments on
earlier versions of this paper by J. Long, R. Foy, and two anonymous
reviewers substantially improved the manuscript. Hatchery crabs were
provided by Dr. Yonathan Zohar and Oded Zmora, University of Maryland,
Biotechnology Institute, Center of Marine Biotechnology. Funding for
this research came from the NOAA Chesapeake Bay Program Office to the
Blue Crab Advanced Research Consortium including funding for JM. WCL was
supported by a Marine Science Network Fellowship from the Smithsonian.
JG was supported by Wabash College through the Wabash-SERC internship
program. The findings and conclusions in the paper are those of the
authors and do not necessarily represent the views of the National
Marine Fisheries Service, NOAA. [SS]
NR 58
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U1 3
U2 31
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD DEC 1
PY 2011
VL 409
IS 1-2
BP 215
EP 222
DI 10.1016/j.jembe.2011.08.024
PG 8
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 866EK
UT WOS:000298363100027
ER
PT J
AU Capogrosso-Sansone, B
Kuklov, AB
AF Capogrosso-Sansone, B.
Kuklov, A. B.
TI Superfluidity of Flexible Chains of Polar Molecules
SO JOURNAL OF LOW TEMPERATURE PHYSICS
LA English
DT Article
DE Dipolar interaction; Optical lattices; Polar molecules; Multilayers;
Quantum phase transitions
ID INSULATOR; PHASE; GAS
AB We study quantum chains formed in a gas of polar bosonic molecules confined in a stack of N identical one-and two-dimensional optical lattice layers, with molecular dipole moments aligned perpendicularly to the layers. Quantum Monte Carlo simulations of a single chain reveal its quantum roughening transition. The case of finite in-layer density of molecules is analyzed within the J-current model approximation, and it is found that N-layered molecular superfluid phase can undergo a quantum phase transition to a rough chain superfluid. A theorem is proven that no superfluidity of chains with length shorter than N is possible. The scheme for detecting the chain formation is proposed.
C1 [Kuklov, A. B.] CUNY, CSI, Dept Engn Sci & Phys, Staten Isl, NY 10314 USA.
[Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
RP Kuklov, AB (reprint author), CUNY, CSI, Dept Engn Sci & Phys, Staten Isl, NY 10314 USA.
EM bcapogrosso@cfa.harvard.edu; Anatoly.Kuklov@csi.cuny.edu
FU Institute for Theoretical Atomic, Molecular and Optical Physics (ITAMP);
National Science Foundation [PHY1005527]; CUNY PSC [63071-0041]; CUNY
HPCC under NSF [CNS-0855217, CNS-0958379]
FX Authors are grateful to Y.E. Lozovik, N.V. Prokof'ev, B.V. Svistunov and
M. Troyer for stimulating discussions and to D. Jin for discussing
experimental aspects. One of us (A.B.K.) is thankful to KITPC at
Beijing, KITP at Santa Barbara and Nordita for hospitality. This work
was supported by the Institute for Theoretical Atomic, Molecular and
Optical Physics (ITAMP), and the National Science Foundation under Grant
No. PHY1005527, CUNY PSC grant 63071-0041 and by a grant of computer
time from the CUNY HPCC under NSF Grants CNS-0855217 and CNS-0958379.
NR 33
TC 9
Z9 9
U1 0
U2 2
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 DEC
PY 2011
VL 165
IS 5-6
SI SI
BP 213
EP 226
DI 10.1007/s10909-011-0386-5
PG 14
WC Physics, Applied; Physics, Condensed Matter
SC Physics
GA 865TP
UT WOS:000298333500004
ER
PT J
AU Black, PA
Trent, AM
Bauman, JE
Farnsworth, RJ
Monfort, SL
AF Black, Peter A.
Trent, Ava M.
Bauman, Joan E.
Farnsworth, Ralph J.
Monfort, Steven L.
TI FECAL STEROID ANALYSIS FOR EVALUATING OVARIAN FUNCTION IN THE GREATER
KUDU (TRAGELAPHUS STREPSICEROS) AND LESSER KUDU (TRAGELAPHUS IMBERBIS)
SO JOURNAL OF ZOO AND WILDLIFE MEDICINE
LA English
DT Article
DE Fecal hormones; greater kudu; lesser kudu; progesterone metabolites;
Tragelaphus
ID SCIMITAR-HORNED ORYX; ARTIFICIAL-INSEMINATION; PREGNANCY DIAGNOSIS;
REPRODUCTIVE STATUS; ESTROUS-CYCLE; DAMMAH; SYNCHRONIZATION;
METABOLITES; PROGESTINS; ESTROGENS
AB Seasonal reproductive-endocrine norms have not been described for the genus Tragelaphus, which consists of seven species of African antelope. Longitudinal patterns of progesterone metabolite excretion were assessed by radioimmunoassays in fecal samples collected noninvasively (three to seven samples per week) from greater kudu (Tragelaphus strepsiceros, n = 4) and lesser kudu (Tragelaphus imberbis, n = 4). Progesterone metabolite excretion patterns revealed seasonal estrous cycles in both species, and discrimination of pregnant versus nonpregnant females was achieved in lesser kudu. These data reveal the value of fecal progesterone metabolites for establishing reproductive-endocrine norms in both zoo-maintained and free-living antelopes of the genus Tragelaphus.
C1 [Monfort, Steven L.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
[Bauman, Joan E.] St Louis Zoo, St Louis, MO 63110 USA.
[Black, Peter A.; Trent, Ava M.; Farnsworth, Ralph J.] Univ Minnesota, Coll Vet Med, St Paul, MN 55108 USA.
RP Black, PA (reprint author), Busch Gardens, 3605 E Bougainvillea Ave, Tampa, FL 33612 USA.
EM peter.black@buschgardens.com
NR 31
TC 2
Z9 2
U1 0
U2 8
PU AMER ASSOC ZOO VETERINARIANS
PI YULEE
PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA
SN 1042-7260
J9 J ZOO WILDLIFE MED
JI J. Zoo Wildl. Med.
PD DEC
PY 2011
VL 42
IS 4
BP 558
EP 564
PG 7
WC Veterinary Sciences
SC Veterinary Sciences
GA 867FJ
UT WOS:000298440000003
PM 22204048
ER
PT J
AU Whattam, SA
Cho, M
Smith, IEM
AF Whattam, Scott A.
Cho, Moonsup
Smith, Ian E. M.
TI Magmatic peridotites and pyroxenites, Andong Ultramafic Complex, Korea:
Geochemical evidence for supra-subduction zone formation and extensive
melt-rock interaction
SO LITHOS
LA English
DT Article
DE South Korea; Ultramafic magmas; Peridotite; Melt-rock reaction;
Supra-subduction zone (SSZ); Volcanic arc
ID LITHOSPHERIC MANTLE BENEATH; MID-ATLANTIC RIDGE; EAST PACIFIC RISE;
RONDA PERIDOTITE; SOUTH-KOREA; TRACE-ELEMENT; TECTONIC IMPLICATIONS;
LHERZOLITE MASSIF; SUBCONTINENTAL LITHOSPHERE; RECRYSTALLIZATION FRONT
AB The Andong Ultramafic Complex (AUC) mainly comprises peridotites (wehrlites +/- plagioclase or spinel; or plagioclase + spinel) and related serpentinites with subordinate low-Al pyroxenites (clinopyroxenites, orthopyroxenites, and websterites). These rocks are compositionally similar to sub-continental lithospheric mantle peridotites and pyroxenites. Wehrlites formed predominantly by fractional crystallization processes within supra-subduction zone magmas and the pyroxenites are generally consistent with segregation and accumulation in similar magmas. Bulk rock ratios of Al2O3/SiO2 (0.01-0.03) and MgO/SiO2 (up to >1) exhibited by the wehrlites and serpentinites indicate crystallization from a refractory source that underwent high degrees of melt extraction. Spinel chemistry confirms this and demonstrates that wehrlite and clinoproxenite protoliths underwent approximately 20-23% and 12-15% partial melting, respectively. Wehrlites and serpentinites also preserve evidence of extensive melt-peridotite interaction manifest as bulk rock SiO2-depletions and FeOt-enrichments relative to mantle residua as well as low Mg# (0.39-0.45) spinels with variable Ti contents but constant Cr# (0.42-0.47). These features are identical to those of 'impregnated' plagioclase-peridotites of abyssal and sub-continental environments and compositional trends in spinel space imply reaction between secondary. MORB-like melts saturated in olivine + clinopyroxene or olivine and a harzburgitic protolith. High olivine:pyroxene (similar to 3:1) and clinopyroxene:orthopyroxene ratios of the wehrlites coupled with chemical data dictate that reactions entailed orthopyroxene dissolution and olivine recrystallization. All AUC rock types exhibit primitive mantle-normalized incompatible element signatures characterized by LILE-enrichments, high fluid-mobile/immobile element ratios (Sr/Nd, Ba/La and Pb/Ce >> 1) and prominent HFSE (Nb, Zr, and Ti) depletions indicative of generation in a sub-arc environment within a supra-subduction zone system. A candidate for the associated arc-system is the one responsible for nearby arc-related Jurassic granitoids. Southeast-directed thrusting along the Andong Fault System may account for subsequent emplacement of the AUC into the Gyeongsang Basin. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Whattam, Scott A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Cho, Moonsup] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151747, South Korea.
[Smith, Ian E. M.] Univ Auckland, Dept Geol, Auckland, New Zealand.
RP Whattam, SA (reprint author), Korea Univ, Dept Earth & Environm Sci, Seoul 136701, South Korea.
EM sawhatta@gmail.com
OI Whattam, Scott/0000-0001-9193-9002; Smith, Ian/0000-0001-8473-3372
FU NRF-MEST [2010-0000296]; Seoul National University
FX Editor A. Kerr and reviewers S. Arai and O. Parlak are thanked for
detailed and constructive comments which greatly aided in revision of
the original version of the manuscript. M. Lee, SNU probe technician, is
thanked for her assistance in the operation of and acquisition of data
from the JEOL 8900 electron microprobe. Y. Lee is thanked for assistance
in the field and J.K. Kim for assistance in data manipulation. S.A.
Whattam thanks R.J. Stern for comments and ideas related to this study.
This work was supported in part by a NRF-MEST grant 2010-0000296 to M.
Cho and a postdoctoral fellowship to S.A. Whattam via the Brain Korea
(BK) 21 grant, Seoul National University.
NR 114
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U1 2
U2 13
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0024-4937
J9 LITHOS
JI Lithos
PD DEC
PY 2011
VL 127
IS 3-4
BP 599
EP 618
DI 10.1016/j.lithos.2011.06.013
PG 20
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 868HH
UT WOS:000298513800015
ER
PT J
AU Clark, JL
Skog, LE
Barrie, FR
AF Clark, John L.
Skog, Laurence E.
Barrie, Fred R.
TI Novae Gesneriaceae Neotropicarum XVII: New Combinations and
Typifications
SO NOVON
LA English
DT Article
DE Alloplectus; Amalophyllon; Colombia; Columnea; Costa Rica; Dalbergaria;
Ecuador; Gesneriaceae; Panama; Pentadenia; Peru; Resia; Venezuela
ID GASTERANTHUS GESNERIACEAE; ECUADOR
AB Fieldwork and current research projects in Central and South America on the Gesneriaceae have shown that nomenclatural and taxonomic changes are needed. The Ecuadorian endemic species Columnea albovinosa (M. Freiberg) J. L. Clark & L. E. Skog is transferred from Dalbergaria Tussac. The name Pentadenia lutea M. Freiberg is synonymized with C. angustata (Wiehler) L. E. Skog. Amalophyllon ecuadoranum (Wiehler) J. L. Clark, comb. nov., is recognized as a species distinct from A. divaricatum (Poepp.) Boggan, L. E. Skog & Roalson. The application of the name C. serrata (Klotzsch ex Oerst..) Hanst. is stabilized by the designation of a neotype. The new name Drymonia ovatifolia J. L. Clark is made for the species Nautilocalyx dressleri Wiehler. Resia bracteata, a name originally published without a Latin diagnosis, is here validly published as R. bracteata J. L. Clark & L. E. Skog.
C1 [Clark, John L.] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA.
[Clark, John L.; Skog, Laurence E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
[Barrie, Fred R.] Missouri Bot Garden, St Louis, MO 63166 USA.
RP Clark, JL (reprint author), Field Museum Nat Hist, Dept Bot, 1400 S Lake Shore Dr, Chicago, IL 60605 USA.
EM jlc@ua.edu; skogl@si.edu; fbarrie@fieldmuseum.org
FU National Science Foundation [DEB-0841958, DEB-0949169]
FX Funding for this project came from the National Science Foundation
(DEB-0841958, DEB-0949169) to John L. Clark. We thank Marcela Mora and
Laura Clavijo for providing the Spanish translation of the abstract;
Barry Hammel (MO/INB) for providing the image of the neotype of Columnea
serrata; Christian Feuillet (US) for providing the Latin diagnosis for
Resia bracteata: Kanchi N. Gandhi (HUH) for providing guidance on
nomenclature; Marina Gaslac Galoc (Jefatura del Bosque de Proteccion
Alto Mayo), Juan Perez (Guardeparque del Bosque de Proteccion Alto
Mayo), and Miguel Chocce (Universidad Nacional Mayor de San Marcos) for
facilitating our research in northern Peru; three anonymous reviewers
and Harry Luther for providing helpful comments on an early version of
the manuscript; and James Di Loreto (Smithsonian Institution NMNH
Imaging) for providing images in Figure 1.
NR 14
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U1 0
U2 1
PU MISSOURI BOTANICAL GARDEN
PI ST LOUIS
PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA
SN 1055-3177
J9 NOVON
JI Novon
PD DEC
PY 2011
VL 21
IS 4
BP 413
EP 423
DI 10.3417/2011002
PG 11
WC Plant Sciences
SC Plant Sciences
GA 874FU
UT WOS:000298941600004
ER
PT J
AU Rhodes, EA
Evans, LG
Nittler, LR
Starr, RD
Sprague, AL
Lawrence, DJ
Mccoy, TJ
Stockstill-Cahill, KR
Goldsten, JO
Peplowski, PN
Hamara, DK
Boynton, WV
Solomon, SC
AF Rhodes, Edgar A.
Evans, Larry G.
Nittler, Larry R.
Starr, Richard D.
Sprague, Ann L.
Lawrence, David J.
Mccoy, Timothy J.
Stockstill-Cahill, Karen R.
Goldsten, John O.
Peplowski, Patrick N.
Hamara, David K.
Boynton, William V.
Solomon, Sean C.
TI Analysis of MESSENGER Gamma-Ray Spectrometer data from the Mercury
flybys
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Gamma-ray spectrometry; Elemental abundances; MESSENGER
ID SURFACE; SPECTROSCOPY
AB During its three flybys of Mercury, the MESSENGER spacecraft made the first detection of gamma-ray emission from the planet's surface. With a closest approach distance of similar to 200 km, the flybys provided an opportunity to measure elemental abundances of Mercury's near-equatorial regions, which will not be visited at low altitude during MESSENGER's orbital mission phase. Despite being limited by low planetary photon flux, sufficient counts were accumulated during the first two flybys to estimate bounds on abundances for some elements having relatively strong gamma-ray spectral peaks, including Si, Fe, Ti, K, and Th. Only for Si is the standard deviation sigma sufficiently small to conclude that this element was detected with 99% confidence. Iron and potassium are detected at the 2 - sigma (95% confidence) level, whereas only upper bounds on Ti and Th can be determined. Relative to a Si abundance assumed to be 18 weight percent (wt%), 2 - sigma upper bounds have been estimated as 9.7 wt% for Fe, 7.0 wt% for Ti, 0.087 wt% for K, and 2.2 ppm for Th. The relatively low upper bound on K rules out some previously suggested models for surface composition for the regions sampled. Upper bounds on Fe/Si and Ti/Si ratios are generally consistent with Ti and Fe abundances estimated from the analysis of measurements by the MESSENGER Neutron Spectrometer during the flybys but are also permissive of much lower concentrations. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Rhodes, Edgar A.; Lawrence, David J.; Goldsten, John O.; Peplowski, Patrick N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA.
[Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Starr, Richard D.] Catholic Univ Amer, Washington, DC 20064 USA.
[Sprague, Ann L.; Hamara, David K.; Boynton, William V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Mccoy, Timothy J.; Stockstill-Cahill, Karen R.] Smithsonian Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Rhodes, EA (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM Ed.Rhodes@jhuapl.edu
RI Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015
OI Peplowski, Patrick/0000-0001-7154-8143; Lawrence,
David/0000-0002-7696-6667
FU NASA [NASW-00002, NAS5-97271]
FX Several of the authors acknowledge support from NASA's MESSENGER
Participating Scientist Program. The MESSENGER project is supported by
the NASA Discovery Program under contracts NASW-00002 to the Carnegie
Institution of Washington and NAS5-97271 to the Johns Hopkins University
Applied Physics Laboratory.
NR 21
TC 9
Z9 9
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC
PY 2011
VL 59
IS 15
SI SI
BP 1829
EP 1841
DI 10.1016/j.pss.2011.07.018
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800002
ER
PT J
AU Preusker, F
Oberst, J
Head, JW
Watters, TR
Robinson, MS
Zuber, MT
Solomon, SC
AF Preusker, Frank
Oberst, Juergen
Head, James W.
Watters, Thomas R.
Robinson, Mark S.
Zuber, Maria T.
Solomon, Sean C.
TI Stereo topographic models of Mercury after three MESSENGER flybys
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; MESSENGER; Topography; Digital terrain models
ID EXPRESS HRSC DATA; IMAGES; BASIN
AB From photogrammetric analysis of stereo images of Mercury obtained during three MESSENGER flybys, we have produced three digital terrain models (DTMs) that have a grid spacing of 1 km and together cover 30% of the planet's surface. The terrain models provide a rich source of information on the morphology of Mercury's surface, including details of tectonic scarp systems as well as impact craters and basins. More than 400 craters larger than 15 km in diameter are included in the models. Additionally, the models provide important test cases for the analysis of stereo image data to be collected during MESSENGER's orbital mission phase. Small lateral offsets and differences in trends between stereo DTMs and laser altimeter profiles may be due to remaining errors in spacecraft position, instrument pointing, or Mercury coordinate knowledge. Such errors should be resolved during the orbital mission phase, when more joint analyses of data and detailed orbit modeling will be possible. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Preusker, Frank; Oberst, Juergen] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Preusker, F (reprint author), German Aerosp Ctr DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
EM Frank.Preusker@dlr.de
FU NASA [NASW-00002, NAS5-97271]
FX We thank Carolyn Ernst for helpful comments that improved an earlier
version of this manuscript. The MESSENGER project is supported by the
NASA Discovery Program under contracts NASW-00002 to the Carnegie
Institution of Washington and NAS5-97271 to the Johns Hopkins University
Applied Physics Laboratory.
NR 17
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U1 0
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC
PY 2011
VL 59
IS 15
SI SI
BP 1910
EP 1917
DI 10.1016/j.pss.2011.07.005
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800008
ER
PT J
AU Strom, RG
Banks, ME
Chapman, CR
Fassett, CI
Forde, JA
Head, JW
Merline, WJ
Prockter, LM
Solomon, SC
AF Strom, Robert G.
Banks, Maria E.
Chapman, Clark R.
Fassett, Caleb I.
Forde, Jeffrey A.
Head, James W., III
Merline, William J.
Prockter, Louise M.
Solomon, Sean C.
TI Mercury crater statistics from MESSENGER flybys: Implications for
stratigraphy and resurfacing history
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mercury; Cratering; Volcanism; MESSENGER
ID VOLCANISM; ORIGIN; PLANETS; PLAINS; IMPACT; EARTH
AB The primary crater population on Mercury has been modified by volcanism and secondary craters. Two phases of volcanism are recognized. One volcanic episode that produced widespread intercrater plains occurred during the period of the Late Heavy Bombardment and markedly altered the surface in many areas. The second episode is typified by the smooth plains interior and exterior to the Caloris basin, both of which have a different crater size-frequency distribution than the intercrater plains, consistent with a cratering record dominated by a younger population of impactors. These two phases may have overlapped as parts of a continuous period of volcanism during which the volcanic flux tended to decrease with time. The youngest age of smooth plains volcanism cannot yet be determined, but at least small expanses of plains are substantially younger than the plains associated with the Caloris basin. The spatial and temporal variations of volcanic resurfacing events can be used to reconstruct Mercury's geologic history from images and compositional and topographic data to be acquired during the orbital phase of the MESSENGER mission. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Banks, Maria E.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Chapman, Clark R.; Merline, William J.] SW Res Inst, Boulder, CO 80302 USA.
[Fassett, Caleb I.; Head, James W., III] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Forde, Jeffrey A.] Microsoft Corp, Redmond, WA 98052 USA.
[Prockter, Louise M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
RP Strom, RG (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM rstrom@lpl.arizona.edu
OI Fassett, Caleb/0000-0001-9155-3804
NR 23
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U1 0
U2 15
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD DEC
PY 2011
VL 59
IS 15
SI SI
BP 1960
EP 1967
DI 10.1016/j.pss.2011.03.018
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 871FH
UT WOS:000298722800013
ER
PT J
AU Kuznetsova, E
Yelin, SF
Cote, R
AF Kuznetsova, Elena
Yelin, S. F.
Cote, Robin
TI An atom-molecule platform for quantum computing
SO QUANTUM INFORMATION PROCESSING
LA English
DT Article
DE Neutral atom quantum computing; Polar molecules; Optical lattices;
Dipole-dipole interaction
ID OPTICAL LATTICES; RYDBERG BLOCKADE; POLAR-MOLECULES
AB We propose a combined atom-molecule system for quantum information processing in individual traps, such as provided by optical lattices. In this platform, different species of atoms-one atom carrying a qubit and the other enabling the interaction-are used to store and process quantum information via intermediate molecular states. We show how gates, initialization, and read out operations could be implemented using this approach. In particular, we describe in some detail the implementation of a two-qubit phase gate in which a pair of atoms is transferred into the ground rovibrational state of a polar molecule with a large dipole moment, thus allowing atoms transferred into molecules to interact via their dipole-dipole interaction. We also discuss how the reverse process could be used as a non-destructive readout tool of molecular qubit states. Finally, we generalize these ideas to use a decoherence-free subspace for qubit encoding to minimize the decoherence due to magnetic field fluctuations. In this case, qubits will be encoded into field-insensitive states of two identical atoms, while a third atom of a different species will be used to realize a phase gate.
C1 [Kuznetsova, Elena; Yelin, S. F.; Cote, Robin] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Kuznetsova, Elena; Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Cote, R (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
EM lenak@phys.uconn.edu; rcote@phys.uconn.edu
FU National Science Foundation; Air Force Office of Scientific Research
FX The authors gratefully acknowledge financial support from National
Science Foundation and Air Force Office of Scientific Research.
NR 53
TC 2
Z9 2
U1 0
U2 4
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1570-0755
J9 QUANTUM INF PROCESS
JI Quantum Inf. Process.
PD DEC
PY 2011
VL 10
IS 6
SI SI
BP 821
EP 838
DI 10.1007/s11128-011-0308-0
PG 18
WC Physics, Multidisciplinary; Physics, Mathematical
SC Physics
GA 875MF
UT WOS:000299033800006
ER
PT J
AU Weimer, H
Muller, M
Buchler, HP
Lesanovsky, I
AF Weimer, H.
Mueller, M.
Buechler, H. P.
Lesanovsky, I.
TI Digital quantum simulation with Rydberg atoms
SO QUANTUM INFORMATION PROCESSING
LA English
DT Article
DE Quantum simulator; Digital quantum simulation; Rydberg atoms;
Dissipative dynamics
ID MOTT INSULATOR; TRAPPED IONS; OPTICAL LATTICE; NEUTRAL ATOMS; SYSTEMS;
COMPUTER; COMPUTATION; TRANSITION; SUPERFLUID; PHYSICS
AB We discuss in detail the implementation of an open-system quantum simulator with Rydberg states of neutral atoms held in an optical lattice. Our scheme allows one to realize both coherent as well as dissipative dynamics of complex spin models involving many-body interactions and constraints. The central building block of the simulation scheme is constituted by a mesoscopic Rydberg gate that permits the entanglement of several atoms in an efficient, robust and quick protocol. In addition, optical pumping on ancillary atoms provides the dissipative ingredient for engineering the coupling between the system and a tailored environment. As an illustration, we discuss how the simulator enables the simulation of coherent evolution of quantum spin models such as the two-dimensional Heisenberg model and Kitaev's toric code, which involves four-body spin interactions. We moreover show that in principle also the simulation of lattice fermions can be achieved. As an example for controlled dissipative dynamics, we discuss ground state cooling of frustration-free spin Hamiltonians.
C1 [Lesanovsky, I.] Univ Nottingham, Midlands Ultracold Atom Res Ctr MUARC, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Buechler, H. P.] Univ Stuttgart, Inst Theoret Phys 3, Stuttgart, Germany.
[Mueller, M.] Univ Complutense, Dept Fis Teor 1, E-28040 Madrid, Spain.
[Mueller, M.] Univ Innsbruck, Inst Quantenopt & Quanteninformat Osterreichische, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Weimer, H.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Weimer, H.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
RP Lesanovsky, I (reprint author), Univ Nottingham, Midlands Ultracold Atom Res Ctr MUARC, Sch Phys & Astron, Nottingham NG7 2RD, England.
EM hweimer@cfa.harvard.edu; igor.lesanovsky@nottingham.ac.uk
RI Muller, Markus/I-6530-2012; Lesanovsky, Igor/J-6012-2015
OI Lesanovsky, Igor/0000-0001-9660-9467
FU National Science Foundation; German Academic Exchange Service (DAAD);
EPSRC; Austrian Science Fund (FOQUS); European Commission (AQUTE);
Institute of Quantum Information
FX H.W. 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 Postdoc Program of the German Academic
Exchange Service (DAAD). I. L acknowledges funding by EPSRC. M. M.
acknowledges support by the Austrian Science Fund (FOQUS), the European
Commission (AQUTE) and the Institute of Quantum Information.
NR 55
TC 29
Z9 29
U1 2
U2 17
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1570-0755
J9 QUANTUM INF PROCESS
JI Quantum Inf. Process.
PD DEC
PY 2011
VL 10
IS 6
SI SI
BP 885
EP 906
DI 10.1007/s11128-011-0303-5
PG 22
WC Physics, Multidisciplinary; Physics, Mathematical
SC Physics
GA 875MF
UT WOS:000299033800009
ER
PT J
AU Romaschenko, K
Peterson, PM
Soreng, RJ
Futorna, O
Susanna, A
AF Romaschenko, Konstantin
Peterson, Paul M.
Soreng, Robert J.
Futorna, Oksana
Susanna, Alfonso
TI Phylogenetics of Piptatherum s.l. (Poaceae: Stipeae): Evidence for a new
genus, Piptatheropsis, and resurrection of Patis
SO TAXON
LA English
DT Article
DE classification; lemma micromorphology; plastid DNA sequences; phylogeny;
Pooideae
ID SEQUENCES; GRAMINEAE; CLASSIFICATION; INFERENCE; MRBAYES; NUCLEAR; TREES
AB Historically, there has been taxonomic confusion among agrostologists regarding the short-spikeleted Stipeae. We refer to these as the Oryzopsis/Piplatherum complex which consists of short-spikeleted species with coriaceous to cartilaginous and often caducous-awned lemmas, and Florets with a blunt callus. We conducted a phylogenetic analysis of 53 species that have been associated with this complex using four plastid regions (ndtF, rp132-trnL., rps16-trnK, rps16 intron) in combination with lemma micromorphology to infer evolutionary relationships. Piplatherum as currently circumscribed is polyphyletic and is found in live strongly supported chides in our maximum likelihood tree. Based on our phylogenetic and morphological evidence we recognize a Eurasian Piptatherum s.str., propose a new genus, Piptatheropsis, to include five North American species. and resurrect the genus Patis to include three species, two from Eurasia and one from North America. We provide morphological descriptions of Paris, Piptatherum, and Piptatheropsis, and provide keys to the genera and species of the Oryzopsis/Piplatherum complex. The following new combinations are made: Pails bursa, Pails raccemosa, Piptatheropsis canadensis, Piptatheropsis exigua, Piptatheropsis micrantha, Piptatheropsis pungens, Piptatheropsis shoshoneana, Piptatheruni brachycladum, a id Piptatherum kopetdagense.
C1 [Romaschenko, Konstantin; Peterson, Paul M.; Soreng, Robert J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
[Romaschenko, Konstantin; Susanna, Alfonso] Bot Inst Barcelona CSIC ICUB, Lab Mol Systemat, Barcelona 08038, Spain.
[Futorna, Oksana] Natl Acad Sci Ukraine, MG Kholodny Inst Bot, UA-01601 Kiev, Ukraine.
RP Peterson, PM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
EM peterson@si.edu
RI Susanna, Alfonso/C-1683-2013; Romaschenko, Konstantin/K-3096-2014
OI Susanna, Alfonso/0000-0003-4717-9063; Romaschenko,
Konstantin/0000-0002-7248-4193
FU Smithsonian Institution; Scholarly Studies Program; Atherton Seidell
Foundation; Biodiversity Surveys and Inventories Program; National
Museum of Natural History; Laboratory of Analytical Biology (LAB);
National Geographic Society Committee for Research and Exploration
[8087-06]; Fulbright Scholar Program; Komarov Botanical Institute;
Russian Academy of Sciences
FX We thank the following organizations and people: the Smithsonian
Institution's Restricted Endowment Fund, the Scholarly Studies Program,
Research Opportunities, Atherton Seidell Foundation, Biodiversity
Surveys and Inventories Program, National Museum of Natural
History-Small Grants, and Laboratory of Analytical Biology (LAB) all for
financial support; Lee Weigt, Gabriel Johnson, Jeffrey Hunt, David
Erickson, Kenneth Wurdack, and Andrea Ormon for support and consultation
while working at LAB; the National Geographic Society Committee for
Research and Exploration (grant number 8087-06) for field and laboratory
support; the Fulbright Scholar Program to KR for a research visit to the
Smithsonian Institution; the Komarov Botanical Institute, Russian
Academy of Sciences for the opportunity to work with herbarium
collections, and Nikolay Tzvelev and Dmitry Geltman for consultation and
permitting us to sample Stipeae specimens; the herbarium of University
of Copenhagen for providing samples of Stipa keniensis; Yakov Didukh,
Asuncion Cano Echevarria, Oscar Tovar Serpa, Dorita Susanibar Cruz,
Maria Isabel La Torre Acuy, Jenny Vanessa Rojas Fox, Isidoro Sanchez
Vega, Socorro Gonzalez Elizondo, Nancy Refulio Rodriguez, Diego Leonel
Salariato, Adela Maria Panizza, Fernando Zuloaga, and Stephan Beck for
help with our field expeditions to Ukraine, Peru, Bolivia, and
Argentina; Samuel Pyke for providing us with samples from North African
specimens; Jeffery Saarela and the herbarium of Brigham Young University
for help with sampling some North American species; Christian Feuillet
and Alain Touwaide for correcting the Latin description; and Lynn Clark
and three anonymous reviewers for suggesting improvements to the
manuscript.
NR 62
TC 8
Z9 10
U1 1
U2 6
PU INT ASSOC PLANT TAXONOMY
PI VIENNA
PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA
SN 0040-0262
J9 TAXON
JI Taxon
PD DEC
PY 2011
VL 60
IS 6
BP 1703
EP 1716
PG 14
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 867JY
UT WOS:000298451900015
ER
PT J
AU Olson, SL
Rauzon, MJ
AF Olson, Storrs L.
Rauzon, Mark J.
TI THE EXTINCT WAKE ISLAND RAIL GALLIRALLUS WAKENSIS: A COMPREHENSIVE
SPECIES ACCOUNT BASED ON MUSEUM SPECIMENS AND ARCHIVAL RECORDS
SO WILSON JOURNAL OF ORNITHOLOGY
LA English
DT Article
ID SEA-LEVEL; ARCHAEOLOGICAL SITES; LATE PLEISTOCENE; RALLIDAE; BERMUDA;
EVOLUTION; BIRDS; FLIGHTLESSNESS; AVES
AB A review of all available specimens and the discovery of many unpublished life history notes allows a much more complete picture of the morphology and behavior of the extinct Wake Island Rail (Gallirallus wakensis). The breeding season of the species may have been environmentally influenced but, under favorable conditions, there may have been two broods per year. Small groups of birds engaged in cooperative nesting and prolonged parental care and feeding of the young. probably in part to defend the eggs and young from hermit crabs (Coenobita) and rats (Ranus). The smallest species of its genus. the Wake Island Rail was able to co-exist with Pacific rats (Ranus exulans). Extinction of the rail occurred between 1942 and 1945 as a result of direct predation by thousands of starving Japanese troops and habitat destruction resulting from military alterations and aerial bombardment. Received 8 February 2011. Accepted 4 June 2011.
C1 [Olson, Storrs L.] Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA.
[Rauzon, Mark J.] Laney Coll, Dept Geog, Oakland, CA 94607 USA.
RP Olson, SL (reprint author), Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, POB 37012, Washington, DC 20013 USA.
EM olsons@si.edu
NR 80
TC 1
Z9 1
U1 0
U2 4
PU WILSON ORNITHOLOGICAL SOC
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA
SN 1559-4491
EI 1938-5447
J9 WILSON J ORNITHOL
JI Wilson J. Ornithol.
PD DEC
PY 2011
VL 123
IS 4
BP 663
EP 689
PG 27
WC Ornithology
SC Zoology
GA 865MH
UT WOS:000298314500001
ER
PT J
AU Morrison, SA
Sillett, TS
Ghalambor, CK
Fitzpatrick, JW
Graber, DM
Bakker, VJ
Bowman, R
Collins, CT
Collins, PW
Delaney, KS
Doak, DF
Koenig, WD
Laughrin, L
Lieberman, AA
Marzluff, JM
Reynolds, MD
Scott, JM
Stallcup, JA
Vickers, W
Boyce, WM
AF Morrison, Scott A.
Sillett, T. Scott
Ghalambor, Cameron K.
Fitzpatrick, John W.
Graber, David M.
Bakker, Victoria J.
Bowman, Reed
Collins, Charles T.
Collins, Paul W.
Delaney, Kathleen Semple
Doak, Daniel F.
Koenig, Walter D.
Laughrin, Lyndal
Lieberman, Alan A.
Marzluff, John M.
Reynolds, Mark D.
Scott, J. Michael
Stallcup, Jerre Ann
Vickers, Winston
Boyce, Walter M.
TI Proactive Conservation Management of an Island-endemic Bird Species in
the Face of Global Change
SO BIOSCIENCE
LA English
DT Article
DE Aphelocoma insularis; climate adaptation; conservation-reliant species;
ecosystem engineer; translocation
ID WEST-NILE-VIRUS; APHELOCOMA-INSULARIS; CLIMATE-CHANGE; SCRUB-JAYS;
CALIFORNIA; COASTAL; SEED
AB Biodiversity conservation in an era of global change and scarce funding benefits from approaches that simultaneously solve multiple problems. Here, we discuss conservation management of the island scrub-jay (Aphelocoma insularis), the only island-endemic passerine species in the continental United States, which is currently restricted to 250-square-kilometer Santa Cruz Island, California. Although the species is not listed as threatened by state or federal agencies, its viability is nonetheless threatened on multiple fronts. We discuss management actions that could reduce extinction risk, including vaccination, captive propagation, biosecurity measures, and establishing a second free-living population on a neighboring island. Establishing a second population on Santa Rosa Island may have the added benefit of accelerating the restoration and enhancing the resilience of that island's currently highly degraded ecosystem. The proactive management framework for island scrub-jays presented here illustrates how strategies for species protection, ecosystem restoration, and adaptation to and mitigation of climate change can converge into an integrated solution.
C1 [Morrison, Scott A.] Nature Conservancy, San Francisco, CA USA.
[Sillett, T. Scott] Smithsonian Conservat Biol Inst, Washington, DC USA.
[Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA.
[Fitzpatrick, John W.; Koenig, Walter D.] Cornell Univ, Cornell Lab Ornithol, Ithaca, NY USA.
[Fitzpatrick, John W.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY USA.
[Graber, David M.] Natl Pk Serv, Oakland, CA USA.
[Bakker, Victoria J.] James Madison Univ, Harrisonburg, VA 22807 USA.
[Bowman, Reed] Archbold Biol Stn, Venus, FL USA.
[Collins, Charles T.] Calif State Univ Long Beach, Dept Biol Sci, Long Beach, CA 90840 USA.
[Collins, Paul W.] Santa Barbara Museum Nat Hist, Santa Barbara, CA USA.
[Delaney, Kathleen Semple] Univ Calif Los Angeles, Los Angeles, CA USA.
[Doak, Daniel F.] Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA.
[Doak, Daniel F.] Univ Wyoming, Program Ecol, Laramie, WY 82071 USA.
[Koenig, Walter D.] Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA.
[Laughrin, Lyndal] Univ Calif Santa Barbara, Univ Calif Nat Reserve Syst Santa Cruz Isl Reserv, Santa Barbara, CA 93106 USA.
[Lieberman, Alan A.] San Diego Zoo Inst Conservat Res, Escondido, CA USA.
[Marzluff, John M.] Univ Washington, Seattle, WA 98195 USA.
[Reynolds, Mark D.] Nat Conservancys Calif Chapter, San Francisco, CA USA.
[Reynolds, Mark D.] San Francisco State Univ, San Francisco, CA USA.
[Scott, J. Michael] Univ Idaho, Moscow, ID 83843 USA.
[Stallcup, Jerre Ann] Conservat Biol Inst, Corvallis, OR USA.
[Vickers, Winston; Boyce, Walter M.] Univ Calif Davis, Wildlife Hlth Ctr, Sch Vet Med, Davis, CA 95616 USA.
RP Morrison, SA (reprint author), Nature Conservancy, San Francisco, CA USA.
EM smorrison@tnc.org
OI Koenig, Walter/0000-0001-6207-1427
NR 44
TC 12
Z9 12
U1 4
U2 45
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 DEC
PY 2011
VL 61
IS 12
BP 1013
EP 1021
DI 10.1525/bio.2011.61.12.11
PG 9
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 860QC
UT WOS:000297961800011
ER
PT J
AU Zhang, SC
Kuntner, M
Li, DQ
AF Zhang, Shichang
Kuntner, Matjaz
Li, Daiqin
TI Mate binding: male adaptation to sexual conflict in the golden orb-web
spider (Nephilidae: Nephila pilipes)
SO ANIMAL BEHAVIOUR
LA English
DT Article
DE Nephila pilipes; orb-web spider; sexual cannibalism; sexual conflict;
sexual selection; sexual size dimorphism; tactile communication
ID CANNIBALISTIC SPIDER; GENITAL MUTILATION; WIDOW SPIDER; BEHAVIOR;
FEMALES; ARANEAE; COEVOLUTION; EVOLUTION; COURTSHIP; DURATION
AB To counter female resistance to mating and cannibalism, males of many animal species have evolved a variety of behavioural adaptations. Here we investigated a novel copulatory courtship behaviour, mate binding, in which the male deposits fine silk onto the female's body in between copulation bouts, in an orb-web nephilid spider, Nephila pilipes. We hypothesized that mate binding might reduce female aggressiveness and sexual cannibalism and that both tactile and chemical cues play a role. We performed a series of mating trials, in which we blocked (1) the females' tactile perception, (2) the females' chemoreceptors, and (3) both types of communication. We also manipulated male spinnerets and thus male silk production. As predicted, mate binding reduced both female resistance to repeated mating and levels of sexual cannibalism. Our results suggest that both tactile and chemical cues are crucial for mate binding to succeed in rendering females less aggressive, but that tactile cues are more important. We conclude that mate binding prolongs total copulation duration, whereby the male maximizes his paternity. Therefore, mate binding may serve as a mechanism countering sexual conflict over repeated mating and sexual cannibalism. (C) 2011 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved.
C1 [Zhang, Shichang; Li, Daiqin] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore.
[Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, SI-1001 Ljubljana, Slovenia.
[Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA.
[Li, Daiqin] Hubei Univ, Coll Life Sci, Wuhan, Peoples R China.
RP Li, DQ (reprint author), Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore.
EM dbslidq@nus.edu.sg
RI Li, Daiqin/D-6922-2013
OI Li, Daiqin/0000-0001-8269-7734
FU Ministry of Education (MOE) [R-154-000-435-112]; Slovenian Research
Agency [J1-2063, 1000-10-720023]; National Park Board of Singapore
[NP/RP9860-1]
FX This study was supported by a grant from the Ministry of Education (MOE)
Academic Research Fund (AcRF) to D. L. (R-154-000-435-112) and in part
by the Slovenian Research Agency, grants J1-2063 and 1000-10-720023 to
M. K. We thank Goh Poh Moi for the maintenance of house flies and
National Park Board of Singapore for a research permit (Permit No:
NP/RP9860-1).
NR 49
TC 12
Z9 12
U1 1
U2 44
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0003-3472
J9 ANIM BEHAV
JI Anim. Behav.
PD DEC
PY 2011
VL 82
IS 6
BP 1299
EP 1304
DI 10.1016/j.anbehav.2011.09.010
PG 6
WC Behavioral Sciences; Zoology
SC Behavioral Sciences; Zoology
GA 859FY
UT WOS:000297863500010
ER
PT J
AU Rijsdijk, KF
Zinke, J
de Louw, PGB
Hume, JP
van der Plicht, H
Hooghiemstra, H
Meijer, HJM
Vonhof, HB
Porch, N
Florens, FBV
Baider, C
van Geel, B
Brinkkemper, J
Vernimmen, T
Janoo, A
AF Rijsdijk, Kenneth F.
Zinke, Jens
de Louw, Perry G. B.
Hume, Julian P.
van der Plicht, Hans (J)
Hooghiemstra, Henry
Meijer, Hanneke J. M.
Vonhof, Hubert B.
Porch, Nick
Florens, F. B. Vincent
Baider, Claudia
van Geel, Bas
Brinkkemper, Joost
Vernimmen, Tamara
Janoo, Anwar
TI Mid-Holocene (4200 kyr BP) mass mortalities in Mauritius (Mascarenes):
Insular vertebrates resilient to climatic extremes but vulnerable to
human impact
SO HOLOCENE
LA English
DT Article
DE climate change; dodo; insular vertebrates; mass mortality; megadrought;
palaeoecology; speleothems; volcanic islands
ID LAST GLACIAL MAXIMUM; SEA-LEVEL RISE; INDIAN-OCEAN;
ENVIRONMENTAL-CHANGES; HOLOCENE CLIMATE; AFRICAN TROPICS; PACIFIC;
EASTERN; EXTINCTIONS; VARIABILITY
AB In the light of the currently increasing drought frequency and water scarcity on oceanic islands, it is crucial for the conservation of threatened insular vertebrates to assess how they will be affected. A 4000 yr old fossil assemblage in the Mare Aux Songes (MAS), southwest Mauritius, Mascarene Islands, contains bones of 100000+ individual vertebrates, dominated by two species of giant tortoises Cylindraspis triserrata and C. inepta, the dodo Raphus cucullatus, and 20 other vertebrate species (Rijsdijk, Hume, Bunnik, Florens, Baider, Shapiro et al. (2009) Mid-Holocene vertebrate bone Concentration-Lagerstatte on oceanic island Mauritius provides a window into the ecosystem of the dodo (Raphus cucullatus). Quaternary Science Reviews 28: 14-24). Nine radiocarbon dates of bones statistically overlap and suggest mass mortality occurred between 4235 and 4100 cal. yr BP. The mortality period coincides with a widely recognized megadrought event. Our multidisciplinary investigations combining geological, paleontological and hydrological evidence suggests the lake was located in a dry coastal setting and had desiccated during this period. Oxygen isotope data from a Uranium-series dated stalagmite from Rodrigues, an island 560 km east of Mauritius, supports this scenario by showing frequently alternating dry and wet periods lasting for decades between 4122 and 2260 cal. yr BP. An extreme drought resulted in falling water-tables at MAS and elsewhere on the island, perhaps deprived these insular vertebrates of fresh water, which led to natural mass mortalities and possibly to extirpations. In spite of these events, all insular species survived until at least the seventeenth century, confirming their resistance to climatic extremes. Despite this, the generally exponential increase of combined human impacts on islands including loss of geodiversity, habitats, and stocks of fresh water, there will be less environmental safe-haven options for insular endemic and native vertebrates during future megadrought conditions; and therefore will be more prone to extinction.
C1 [Rijsdijk, Kenneth F.; Meijer, Hanneke J. M.; Vernimmen, Tamara] NCB Naturalis, NL-2300 RA Leiden, Netherlands.
[Rijsdijk, Kenneth F.; Hooghiemstra, Henry; van Geel, Bas; Brinkkemper, Joost] Univ Amsterdam, NL-1012 WX Amsterdam, Netherlands.
[Zinke, Jens; Vonhof, Hubert B.] Vrije Univ Amsterdam, Amsterdam, Netherlands.
[de Louw, Perry G. B.] Subsurface & Groundwater Syst Unit, Deltares, Netherlands.
[Hume, Julian P.] Nat Hist Museum, London, England.
[van der Plicht, Hans (J)] Univ Groningen, NL-9700 AB Groningen, Netherlands.
[van der Plicht, Hans (J)] Leiden Univ, NL-2300 RA Leiden, Netherlands.
[Meijer, Hanneke J. M.] Smithsonian Inst, Washington, DC 20560 USA.
[Porch, Nick] Deakin Univ, Geelong, Vic 3217, Australia.
[Florens, F. B. Vincent; Janoo, Anwar] Univ Mauritius, Reduit, Mauritius.
[Baider, Claudia] Mauritius Sugar Ind Res Inst, Reduit, Mauritius.
RP Rijsdijk, KF (reprint author), NCB Naturalis, POB 9517, NL-2300 RA Leiden, Netherlands.
EM rijsdijk@naturalis.nl
RI Meijer, Hanneke/A-1912-2013; Zinke, Jens/G-5026-2011;
OI Meijer, Hanneke/0000-0001-7066-6869; Zinke, Jens/0000-0002-0634-8281;
Rijsdijk, kenneth/0000-0002-0943-2577; Baider,
Claudia/0000-0002-2203-2076; Vonhof, Hubert/0000-0002-0897-8244;
Florens, Francois Benjamin Vincent/0000-0002-1720-5438
FU Omnicane; World Wildlife Fund; Gen Foundation; Percy Sladen Centenary
Fund; Treub Stichting for interdisciplinary research in the tropics,
Deltares; Geological Survey of the Netherlands-TNO
FX We thank the staff of the The Francois Leguat Giant Tortoise and Cave
Reserve, and Shoals Rodrigues for logistical support during field
sampling of the stalagmite in La Vierge Cave. We thank J. Hellstrom from
the University of Melbourne (Australia) for providing the U/Th datings
on the stalagmite from La Vierge cave. We also thank Suzan Warmerdam,
Charlotte Spliethoff and Alexander Prick from the VU University
Amsterdam for sampling and analytical support for the stable isotope
measurements of the stalagmites. We thank Leo Kriegsman and Menno
Schilthuizen, and four anonymous reviewers for their insightful feedback
on earlier versions of this manuscript. We thank John de Vos for
discussions in the field and Astrid Kromhout and Nico Staring for
stimulating feedback. We thank Omnicane, World Wildlife Fund, Gen
Foundation, Percy Sladen Centenary Fund, the Treub Stichting for
interdisciplinary research in the tropics, Deltares and The Geological
Survey of the Netherlands-TNO for financing the field work in 2007.
NR 76
TC 14
Z9 14
U1 0
U2 38
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0959-6836
J9 HOLOCENE
JI Holocene
PD DEC
PY 2011
VL 21
IS 8
BP 1179
EP 1194
DI 10.1177/0959683611405236
PG 16
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 857YE
UT WOS:000297760600001
ER
PT J
AU Dudley, R
Yanoviak, SP
AF Dudley, Robert
Yanoviak, Stephen P.
TI Animal Aloft: The Origins of Aerial Behavior and Flight
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Article
ID SURFACE-SKIMMING STONEFLIES; DINOSAUR MICRORAPTOR-GUI; INSECT FLIGHT;
LOCOMOTOR PERFORMANCE; EVOLUTIONARY ORIGIN; TERRESTRIAL ARTHROPODS;
GLIDING PERFORMANCE; GIANT INTERNEURONS; VERTEBRATE FLIGHT; FLYING
SQUIRRELS
AB Diverse taxa of animals exhibit remarkable aerial capacities, including jumping, mid-air righting, parachuting, gliding, landing, controlled maneuvers, and flapping flight. The origin of flapping wings in hexapods and in 3 separate lineages of vertebrates (pterosaurs, bats, and birds) greatly facilitated subsequent diversification of lineages, but both the paleobiological context and the possible selective pressures for the evolution of wings remain contentious. Larvae of various arboreal hemimetabolous insects, as well as many adult canopy ants, demonstrate the capacity for directed aerial descent in the absence of wings. Aerial control in the ancestrally wingless archaeognathans suggests that flight behavior preceded the origins of wings in hexapods. In evolutionary terms, the use of winglets and partial wings to effect aerial righting and maneuvers could select for enhanced appendicular motions, and ultimately lead to powered flight. Flight behaviors that involve neither flapping nor wings are likely to be much more widespread than is currently recognized. Further characterization of the sensory and biomechanical mechanisms used by these aerially capable taxa can potentially assist in reconstruction of ancestral winged morphologies and facilitate our understanding of the origins of flight.
C1 [Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama.
[Yanoviak, Stephen P.] Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA.
RP Dudley, R (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
EM wings@berkeley.edu
FU National Science Foundation [IOS-0837866, IOS-0843120]; SICB Divisions
of Animal Behavior, Comparative Biomechanics, and Vertebrate Morphology
FX We thank the SICB Divisions of Animal Behavior, Comparative
Biomechanics, and Vertebrate Morphology for funding this symposium. Marc
Badger, Sofia Chang, Dennis Evangelista, Erica Kim, Mimi Koehl, Jim
McGuire, Yonatan Munk, Victor Ortega, Kevin Peterson, Nir Sapir, Marta
Wolf, and Yu Zeng kindly provided comments on the manuscript. We also
thank two anonymous reviewers for additional suggestions.; National
Science Foundation (IOS-0837866 to R. D. and IOS-0843120 to S.P.Y.).
NR 132
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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 DEC
PY 2011
VL 51
IS 6
BP 926
EP 936
DI 10.1093/icb/icr002
PG 11
WC Zoology
SC Zoology
GA 852SC
UT WOS:000297376800008
PM 21558180
ER
PT J
AU Jusufi, A
Zeng, Y
Full, RJ
Dudley, R
AF Jusufi, Ardian
Zeng, Yu
Full, Robert J.
Dudley, Robert
TI Aerial Righting Reflexes in Flightless Animals
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Article
ID POSTNATAL-DEVELOPMENT; VISUAL MODULATION; ALBINO-RATS; INSECT;
PERFORMANCE; ROTATIONS; WALKING
AB Animals that fall upside down typically engage in an aerial righting response so as to reorient dorsoventrally. This behavior can be preparatory to gliding or other controlled aerial behaviors and is ultimately necessary for a successful landing. Aerial righting reflexes have been described historically in various mammals such as cats, guinea pigs, rabbits, rats, and primates. The mechanisms whereby such righting can be accomplished depend on the size of the animal and on anatomical features associated with motion of the limbs and body. Here we apply a comparative approach to the study of aerial righting to explore the diverse strategies used for reorientation in midair. We discuss data for two species of lizards, the gecko Hemidactylus platyurus and the anole Anolis carolinensis, as well as for the first instar of the stick insect Extatosoma tiaratum, to illustrate size-dependence of this phenomenon and its relevance to subsequent aerial performance in parachuting and gliding animals. Geckos can use rotation of their large tails to reorient their bodies via conservation of angular momentum. Lizards with tails well exceeding snout-vent length, and correspondingly large tail inertia to body inertia ratios, are more effective at creating midair reorientation maneuvers. Moreover, experiments with stick insects, weighing an order of magnitude less than the lizards, suggest that aerodynamic torques acting on the limbs and body may play a dominant role in the righting process for small invertebrates. Both inertial and aerodynamic effects, therefore, can play a role in the control of aerial righting. We propose that aerial righting reflexes are widespread among arboreal vertebrates and arthropods and that they represent an important initial adaptation in the evolution of controlled aerial behavior.
C1 [Jusufi, Ardian; Zeng, Yu; Full, Robert J.; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama.
RP Jusufi, A (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
EM ardianj@berkeley.edu
FU SICB Divisions of Animal Behavior, Comparative Biomechanics, and
Vertebrate Morphology; Swiss National Science Foundation; Berkeley Sigma
Xi grant; National Science Foundation [IOS-0837866]
FX We thank the SICB Divisions of Animal Behavior, Comparative
Biomechanics, and Vertebrate Morphology for funding this symposium. We
thank Thomas Libby, Steve Vogel, and Daniel Kawano for for valuable
insights. We also thank Hal Heatwole and two anonymous reviewers for
additional suggestions.; Swiss National Science Foundation Fellowship
for Prospective Researchers (to A.J.); a Berkeley Sigma Xi grant (to
Y.Z.); National Science Foundation (IOS-0837866 to R. D.).
NR 40
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U2 30
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 DEC
PY 2011
VL 51
IS 6
BP 937
EP 943
DI 10.1093/icb/icr114
PG 7
WC Zoology
SC Zoology
GA 852SC
UT WOS:000297376800009
PM 21930662
ER
PT J
AU Riley, S
AF Riley, Sheila
TI The Darlings
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Riley, Sheila] Smithsonian Inst Lib, Washington, DC 20560 USA.
RP Riley, S (reprint author), Smithsonian Inst Lib, 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 DEC
PY 2011
VL 136
IS 20
BP 112
EP 112
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 859XT
UT WOS:000297909800066
ER
PT J
AU Castaneda, MD
de Queiroz, K
AF Castaneda, Maria del Rosario
de Queiroz, Kevin
TI Phylogenetic relationships of the Dactyloa clade of Anolis lizards based
on nuclear and mitochondrial DNA sequence data
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE Anolis; Dactyloa; Phylogenetics; South America; Taxonomy
ID SPECIES GROUP SAURIA; MOLECULAR PHYLOGENETICS; IGUANIAN LIZARDS;
MORPHOLOGICAL DIVERSIFICATION; HISTORICAL BIOGEOGRAPHY;
BAYESIAN-INFERENCE; LESSER-ANTILLES; TREE SELECTION; ROQUET GROUP;
COSTA-RICA
AB The Dactyloa clade, one of two major subgroups of mainland Anolis lizards, is distributed from Costa Rica to Peru, including the Amazon region and the southern Lesser Antilles. We estimated the phylogenetic relationships within Dactyloa based on mitochondrial (ND2, five transfer-RNAs, COI) and nuclear (RAG1) gene regions using likelihood and Bayesian methods under different partition strategies. In addition, we tested the monophyly of five previously recognized groups within Dactyloa. The data strongly support the monophyly of Dactyloa and five major clades: eastern, latifrons, Phenacosaurus, roquet and western, each of which exhibits a coherent geographic range. Relationships among the five major clades are less clear: support for basal nodes within Dactyloa is weak and some contradictory relationships are supported by different datasets and/or phylogenetic methods. Of the previously recognized subgroups within Dactyloa, only the roquet series consistently passed the topology tests applied. The monophyly of the aequatorialis, latifrons (as traditionally circumscribed) and punctatus series was strongly rejected, and the monophyly of Phenacosaurus (as traditionally circumscribed) yielded mixed results. The results of the phylogenetic analyses suggest the need for a revised taxonomy and have implications for the biogeography and tempo of the Dactyloa radiation. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Castaneda, Maria del Rosario] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA.
[Castaneda, Maria del Rosario; de Queiroz, Kevin] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
RP Castaneda, MD (reprint author), Smithsonian Inst, Div Amphibians & Reptiles, POB 37012,MRC 162, Washington, DC 20013 USA.
EM castanedar@si.edu
FU George Washington University; Sigma-Xi (GWU Chapter); Cosmos Club
Foundation; Laboratories of Analytical Biology at the Smithsonian
Institution
FX James Clark, James Schulte, and Omar Torres-Carvajal provided help with
data collection, analyses and earlier versions of this paper. This
research was partially funded by The George Washington University,
Sigma-Xi (GWU Chapter), Cosmos Club Foundation (Young Scholars Award)
and the Laboratories of Analytical Biology at the Smithsonian
Institution. Many thanks to those who provided tissues: Tito Barros,
Wesley Chun, Luis A. Coloma (Universidad Catolica de Quito-QCAZ),
Richard Glor, Jonathan Losos, Roy McDiarmid, Kirsten Nicholson, Vivian
Paez (Universidad de Antioquia-MHUA) and James Schulte. For assistance
in the field the first author would like to thank Fernando Ayala, Tito
Barros, Eduardo Castaneda, Wesley Chun, Paul D.A. Gutierrez, Juan Pablo
Hurtado, Gustavo A. London, Juan L. Parra, Gilson Rivas and Julian
Velasco. Jonathan B. Losos helped track down locality data for some of
the sequences obtained from GenBank. Derrick Zwickl provided help with
site-likelihood estimations in GARLI. The Instituto Humboldt (thanks to
Fernando Gast and Mauricio Alvarez) facilitated permits in Colombia. In
Venezuela, access to tissue samples was granted under the access to
genetic resources permit between the IVIC-MINAMB; Tito Barros (MBLUZ),
associate researcher of IVIC, loaned the tissues. Cristiano Moreira
helped in preparing the distribution map. Laboratory work was performed
at the Laboratories of Analytical Biology-Smithsonian Institution
(thanks to Lee Weight) and Universidad de Los Andes, Colombia.
NR 93
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U1 1
U2 13
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 DEC
PY 2011
VL 61
IS 3
BP 784
EP 800
DI 10.1016/j.ympev.2011.07.004
PG 17
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 852WG
UT WOS:000297387600017
ER
PT J
AU Potts, R
AF Potts, Richard
TI EVOLUTION Big brains explained
SO NATURE
LA English
DT Editorial Material
C1 Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA.
RP Potts, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA.
EM pottsr@si.edu
NR 5
TC 9
Z9 9
U1 2
U2 31
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD DEC 1
PY 2011
VL 480
IS 7375
BP 43
EP 44
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 861PO
UT WOS:000298031900026
PM 22129720
ER
PT J
AU Aliu, E
Aune, T
Beilicke, M
Benbow, W
Bottcher, M
Bouvier, A
Bradbury, SM
Buckley, JH
Bugaev, V
Cannon, A
Cesarini, A
Ciupik, L
Connolly, MP
Cui, W
Decerprit, G
Dickherber, R
Duke, C
Errando, M
Falcone, A
Feng, Q
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Godambe, S
Griffin, S
Grube, J
Gyuk, G
Hanna, D
Hivick, B
Holder, J
Huan, H
Hughes, G
Hui, CM
Humensky, TB
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Krawczynski, H
Krennrich, F
Maier, G
Majumdar, P
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Nelson, T
Ong, RA
Orr, M
Otte, AN
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
Sembroski, GH
Skole, C
Smith, AW
Staszak, D
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Tyler, J
Varlotta, A
Vassiliev, VV
Wakely, SP
Weekes, TC
Weinstein, A
Williams, DA
Zitzer, B
Ciprini, S
Fumagalli, M
Kaplan, K
Paneque, D
Prochaska, JX
AF Aliu, E.
Aune, T.
Beilicke, M.
Benbow, W.
Boettcher, M.
Bouvier, A.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Cannon, A.
Cesarini, A.
Ciupik, L.
Connolly, M. P.
Cui, W.
Decerprit, G.
Dickherber, R.
Duke, C.
Errando, M.
Falcone, A.
Feng, Q.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gillanders, G. H.
Godambe, S.
Griffin, S.
Grube, J.
Gyuk, G.
Hanna, D.
Hivick, B.
Holder, J.
Huan, H.
Hughes, G.
Hui, C. M.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Nelson, T.
Ong, R. A.
Orr, M.
Otte, A. 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.
Sembroski, G. H.
Skole, C.
Smith, A. W.
Staszak, D.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Tyler, J.
Varlotta, A.
Vassiliev, V. V.
Wakely, S. P.
Weekes, T. C.
Weinstein, A.
Williams, D. A.
Zitzer, B.
Ciprini, S.
Fumagalli, M.
Kaplan, K.
Paneque, D.
Prochaska, J. X.
CA VERITAS Collaboration
TI MULTIWAVELENGTH OBSERVATIONS OF THE PREVIOUSLY UNIDENTIFIED BLAZAR RX
J0648.7+1516
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (RX J0648.7+1516, 1FGL J0648.8+1516, VER
J0648+152); gamma rays: galaxies
ID LARGE-AREA TELESCOPE; BL-LACERTAE OBJECTS; ALL-SKY SURVEY;
PARTICLE-ACCELERATION; SOURCE CATALOG; RAY; VERITAS; MISSION
AB We report on the VERITAS discovery of very high energy (VHE) gamma-ray emission above 200 GeV from the high-frequency-peaked BL Lac (HBL) object RX J0648.7+1516 (GB J0648+1516), associated with 1FGL J0648.8+1516. The photon spectrum above 200 GeV is fitted by a power law dN/dE = F-0(E/E-0)(-Gamma) with a photon index Gamma of 4.4 +/- 0.8(stat) +/- 0.3(syst) and a flux normalization F-0 of (2.3 +/- 0.5(stat) +/- 1.2(sys)) x 10(-11) TeV-1 cm(-2) s(-1) with E-0 = 300 GeV. No VHE variability is detected during VERITAS observations of RX J0648.7+1516 between 2010 March 4 and April 15. Following the VHE discovery, the optical identification and spectroscopic redshift were obtained using the Shane 3 m Telescope at the Lick Observatory, showing the unidentified object to be a BL Lac type with a redshift of z = 0.179. Broadband multiwavelength observations contemporaneous with the VERITAS exposure period can be used to subclassify the blazar as an HBL object, including data from the MDM observatory, Swift-UVOT, and X-Ray Telescope, and continuous monitoring at photon energies above 1 GeV from the Fermi Large Area Telescope (LAT). We find that in the absence of undetected, high-energy rapid variability, the one-zone synchrotron self-Compton (SSC) model overproduces the high-energy gamma-ray emission measured by the Fermi-LAT over 2.3 years. The spectral energy distribution can be parameterized satisfactorily with an external-Compton or lepto-hadronic model, which have two and six additional free parameters, respectively, compared to the one-zone SSC model.
C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 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.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Galante, N.; Roache, E.; Theiling, M.; Weekes, T. C.; Kaplan, K.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Boettcher, M.; Hivick, B.] 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.
[Cannon, A.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Connolly, M. P.; Gillanders, G. H.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Feng, Q.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Decerprit, G.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Skole, C.] DESY, D-15738 Zeuthen, Germany.
[Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Holder, J.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Huan, H.; Humensky, T. B.; Park, N.; Reyes, L. C.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[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, Dept Phys, Baltimore, MD 21250 USA.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Pohl, M.; Ruppel, J.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Ciprini, S.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Fumagalli, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Prochaska, J. X.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
EM afurniss@ucsc.edu; miki@ucolick.org; dpaneque@mppmu.mpg.de
RI Fumagalli, Michele/K-9510-2015;
OI Fumagalli, Michele/0000-0001-6676-3842; Cui, Wei/0000-0002-6324-5772;
Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794
FU US Department of Energy; NSERC in Canada; Science Foundation Ireland
(SFI ) [10/RFP/AST2748]; STFC in the UK; NASA [NNX10AF89G]; Fermi
[NNX09AU18G]; NSF [AST-0548180]; US National Science Foundation;
Smithsonian Institution
FX VERITAS is supported by the US Department of Energy, US National Science
Foundation, and Smithsonian Institution, by NSERC in Canada, by Science
Foundation Ireland (SFI 10/RFP/AST2748), and STFC in the UK. We
acknowledge the excellent work of the technical support staff at the
FLWO and at the collaborating institutions. This work was also supported
by NASA grants from the Swift (NNX10AF89G) and Fermi (NNX09AU18G) Guest
Investigator programs.; J.X.P. acknowledges funding through an NSF
CAREER grant (AST-0548180).
NR 33
TC 22
Z9 23
U1 0
U2 3
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 DEC 1
PY 2011
VL 742
IS 2
AR 127
DI 10.1088/0004-637X/742/2/127
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900067
ER
PT J
AU Arce, HG
Borkin, MA
Goodman, AA
Pineda, JE
Beaumont, CN
AF Arce, Hector G.
Borkin, Michelle A.
Goodman, Alyssa A.
Pineda, Jaime E.
Beaumont, Christopher N.
TI A BUBBLING NEARBY MOLECULAR CLOUD: COMPLETE SHELLS IN PERSEUS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: bubbles; ISM: individual objects (Perseus); stars: formation;
stars: pre-main sequence; stars: winds, outflows; turbulence
ID T-TAURI STARS; YOUNG STELLAR OBJECTS; SPITZER IRS SPECTRA; LOW-MASS
PROTOSTARS; SUN-LIKE STARS; FORMING REGIONS; COLLIMATED OUTFLOWS;
INTERSTELLAR CLOUDS; TURBULENCE DRIVEN; CLUSTER IC-348
AB We present a study of the shells (and bubbles) in the Perseus molecular cloud using the COMPLETE survey large-scale (CO)-C-12(1-0) and (CO)-C-13(1-0) maps. The 12 shells reported here are spread throughout most of the Perseus cloud and have circular or arc-like morphologies with a range in radius of about 0.1-3 pc. Most of them have not been detected before most likely because maps of the region lacked the coverage and resolution needed to distinguish them. The majority of the shells are coincident with infrared nebulosity of similar shape and have a candidate powering source near the center. We suggest that they are formed by the interaction of spherical or very wide angle winds powered by young stars inside or near the Perseus molecular cloud-a cloud that is commonly considered to be forming mostly low-mass stars. Two of the 12 shells are powered by high-mass stars close to the cloud, while the others appear to be powered by low-or intermediate-mass stars in the cloud. We argue that winds with a mass loss rate of about 10(-8) to 10(-6) M-circle dot yr(-1) are required to produce the observed shells. Our estimates indicate that the energy input rate from these stellar winds is similar to the turbulence dissipation rate. We conclude that in Perseus the total energy input from both collimated protostellar outflows and powerful spherical winds from young stars is sufficient to maintain the turbulence in the molecular cloud. Large-scale molecular line and IR continuum maps of a sample of clouds will help determine the frequency of this phenomenon in other star-forming regions.
C1 [Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Borkin, Michelle A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pineda, Jaime E.] ESO, D-85748 Garching, Germany.
[Pineda, Jaime E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Beaumont, Christopher N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
RP Arce, HG (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA.
EM hector.arce@yale.edu; michelle_borkin@harvard.edu;
agoodman@cfa.harvard.edu; jaime.pineda@manchester.ac.uk;
beaumont@ifa.hawaii.edu
RI Pineda, Jaime/J-7405-2013; Goodman, Alyssa/A-6007-2010
OI Pineda, Jaime/0000-0002-3972-1978; Goodman, Alyssa/0000-0003-1312-0477
FU Initiative in Innovative Computing at Harvard; NSF [AST-0401568,
AST-0845619, AST-0908159, AST-0407172]
FX We thank the rest of the COMPLETE team, and especially Mark Heyer, for
their help with the acquisition and reduction of the data. We also thank
Chris McKee and Chris Maztner for their discussion on winds, and Kelle
Cruz for her help on colors of very low mass stars. Comments and
suggestions from the anonymous referee helped improve the paper. Our
gratitude goes to the Initiative in Innovative Computing at Harvard for
their support of the Astronomical Medicine Project. H. G. A. was
partially funded by NSF awards AST-0401568 and AST-0845619 while
conducting this study. This material is also based on work supported by
NSF grant AST-0908159 to A. A. G. The COMPLETE Survey of Star Forming
Regions is supported by NSF grant no. AST-0407172. H. G. A. is very
grateful to the Universidad de Chile and University of Illinois,
Urbana-Champaign astronomy departments for their kind hospitality while
much of this work was conducted.
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JI Astrophys. J.
PD DEC 1
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900045
ER
PT J
AU Assef, RJ
Denney, KD
Kochanek, CS
Peterson, BM
Kozeowski, S
Ageorges, N
Barrows, RS
Buschkamp, P
Dietrich, M
Falco, E
Feiz, C
Gemperlein, H
Germeroth, A
Grier, CJ
Hofmann, R
Juette, M
Khan, R
Kilic, M
Knierim, V
Laun, W
Lederer, R
Lehmitz, M
Lenzen, R
Mall, U
Madsen, KK
Mandel, H
Martini, P
Mathur, S
Mogren, K
Mueller, P
Naranjo, V
Pasquali, A
Polsterer, K
Pogge, RW
Quirrenbach, A
Seifert, W
Stern, D
Shappee, B
Storz, C
Van Saders, J
Weiser, P
Zhang, D
AF Assef, R. J.
Denney, K. D.
Kochanek, C. S.
Peterson, B. M.
Kozeowski, S.
Ageorges, N.
Barrows, R. S.
Buschkamp, P.
Dietrich, M.
Falco, E.
Feiz, C.
Gemperlein, H.
Germeroth, A.
Grier, C. J.
Hofmann, R.
Juette, M.
Khan, R.
Kilic, M.
Knierim, V.
Laun, W.
Lederer, R.
Lehmitz, M.
Lenzen, R.
Mall, U.
Madsen, K. K.
Mandel, H.
Martini, P.
Mathur, S.
Mogren, K.
Mueller, P.
Naranjo, V.
Pasquali, A.
Polsterer, K.
Pogge, R. W.
Quirrenbach, A.
Seifert, W.
Stern, D.
Shappee, B.
Storz, C.
Van Saders, J.
Weiser, P.
Zhang, D.
TI BLACK HOLE MASS ESTIMATES BASED ON CIV ARE CONSISTENT WITH THOSE BASED
ON THE BALMER LINES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; gravitational lensing: strong; quasars: emission lines
ID ACTIVE GALACTIC NUCLEI; NEAR-INFRARED SPECTROSCOPY; QUASI-STELLAR
OBJECTS; EARLY-TYPE GALAXIES; DIGITAL-SKY-SURVEY; EMISSION-LINE; BROAD
EMISSION; HIGH-REDSHIFT; GRAVITATIONAL LENSES; VELOCITY DISPERSION
AB Using a sample of high-redshift lensed quasars from the CASTLES project with observed-frame ultraviolet or optical and near-infrared spectra, we have searched for possible biases between supermassive black hole (BH) mass estimates based on the C IV, H alpha, and H beta broad emission lines. Our sample is based upon that of Greene, Peng, & Ludwig, expanded with new near-IR spectroscopic observations, consistently analyzed high signal-to-noise ratio (S/N) optical spectra, and consistent continuum luminosity estimates at 5100 angstrom. We find that BH mass estimates based on the full width at half-maximum (FWHM) of C IV show a systematic offset with respect to those obtained from the line dispersion, sigma(l), of the same emission line, but not with those obtained from the FWHM of H alpha and H beta. The magnitude of the offset depends on the treatment of the He II and Fe II emission blended with C IV, but there is little scatter for any fixed measurement prescription. While we otherwise find no systematic offsets between C IV and Balmer line mass estimates, we do find that the residuals between them are strongly correlated with the ratio of the UV and optical continuum luminosities. This means that much of the dispersion in previous comparisons of C IV and H beta BH mass estimates are due to the continuum luminosities rather than to any properties of the lines. Removing this dependency reduces the scatter between the UV- and optical-based BH mass estimates by a factor of approximately two, from roughly 0.35 to 0.18 dex. The dispersion is smallest when comparing the C IV sigma(l) mass estimate, after removing the offset from the FWHM estimates, and either Balmer line mass estimate. The correlation with the continuum slope is likely due to a combination of reddening, host contamination, and object-dependent SED shapes. When we add additional heterogeneous measurements from the literature, the results are unchanged. Moreover, in a trial observation of a remaining outlier, the origin of the deviation is clearly due to unrecognized absorption in a low S/N spectrum. This not only highlights the importance of the quality of the observations, but also raises the question whether cases like this one are common in the literature, further biasing comparisons between C IV and other broad emission lines.
C1 [Assef, R. J.; Denney, K. D.; Kochanek, C. S.; Peterson, B. M.; Kozeowski, S.; Dietrich, M.; Grier, C. J.; Khan, R.; Martini, P.; Mathur, S.; Mogren, K.; Pogge, R. W.; Shappee, B.; Van Saders, J.; Zhang, D.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Assef, R. J.; Denney, K. D.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Kochanek, C. S.; Peterson, B. M.; Martini, P.; Mathur, S.; Pogge, R. W.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Ageorges, N.; Buschkamp, P.; Gemperlein, H.; Hofmann, R.; Lederer, R.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Barrows, R. S.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA.
[Falco, E.; Kilic, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Feiz, C.; Germeroth, A.; Mandel, H.; Mueller, P.; Quirrenbach, A.] Heidelberg Univ, ZAH, D-69117 Heidelberg, Germany.
[Juette, M.; Knierim, V.; Polsterer, K.] Astron Inst Ruhr Univ, D-44780 Bochum, Germany.
[Laun, W.; Lehmitz, M.; Lenzen, R.; Mall, U.; Naranjo, V.; Pasquali, A.; Storz, C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Madsen, K. K.] CALTECH, Pasadena, CA 91125 USA.
[Weiser, P.] Fachhsch Tech & Gestaltung, D-68163 Mannheim, Germany.
RP Assef, RJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
EM rjassef@astronomy.ohio-state.edu
RI Peterson, Bradley/G-8226-2012; Kozlowski, Szymon/G-4799-2013; Khan,
Rubab/F-9455-2015
OI Kozlowski, Szymon/0000-0003-4084-880X; Khan, Rubab/0000-0001-5100-5168
FU NASA at the Jet Propulsion Laboratory; NASA; NSF [AST-0708082,
AST-1009756, AST-1008882, AST-0705170]
FX We thank Jenny E. Greene, Christopher Onken, Chien Y. Peng, Kristen
Sellgren, Marianne Vestergaard, and Linda Watson for their help and
suggestions that improved our work. We thank F. Courbin, E. Mediavilla,
V. Motta, L. J. Goicoechea, S. Sluse, J. L. Tonry, L. Wisotzki, and J.
Munoz for sending us their optical spectra of Q2237+030, SDSS1138+0314,
Q0957+561, HE1104-1805, B1422+231, and SBS0909+532. We thank F. Harrison
for helping us obtain an optical spectrum of SDSS1151+0340. We also
thank all the people in the LUCIFER science demonstration time team who
did not participate directly in this work. We thank the anonymous
referee for suggestions that helped improve our work. R. J. A. was
supported in part by an appointment to the NASA Postdoctoral Program at
the Jet Propulsion Laboratory, administered by Oak Ridge Associated
Universities through a contract with NASA. C. S. K. is supported by NSF
grants AST-0708082 and AST-1009756. B. M. P., M. D., and R. W. P. are
supported by NSF grant AST-1008882. P. M. is supported by NSF grant
AST-0705170. 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.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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UT WOS:000297211900033
ER
PT J
AU Bakos, GA
Hartman, J
Torres, G
Latham, DW
Kovacs, G
Noyes, RW
Fischer, DA
Johnson, JA
Marcy, GW
Howard, AW
Kipping, D
Esquerdo, GA
Shporer, A
Beky, B
Buchhave, LA
Perumpilly, G
Everett, M
Sasselov, DD
Stefanik, RP
Lazar, J
Papp, I
Sari, P
AF Bakos, G. A.
Hartman, J.
Torres, G.
Latham, D. W.
Kovacs, Geza
Noyes, R. W.
Fischer, D. A.
Johnson, J. A.
Marcy, G. W.
Howard, A. W.
Kipping, D.
Esquerdo, G. A.
Shporer, A.
Beky, B.
Buchhave, L. A.
Perumpilly, G.
Everett, M.
Sasselov, D. D.
Stefanik, R. P.
Lazar, J.
Papp, I.
Sari, P.
TI HAT-P-20b-HAT-P-23b: FOUR MASSIVE TRANSITING EXTRASOLAR PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: individual (HAT-P-20, HAT-P-21, HAT-P-22, HAT-P-23); techniques:
photometric; techniques: spectroscopic
ID SOLAR-TYPE STAR; HOT JUPITERS; BRIGHT STAR; K-DWARF; ECCENTRIC ORBIT;
GIANT PLANETS; BROWN DWARFS; KEPLER FIELD; EXOPLANETS; SYSTEMS
AB We report the discovery of four relatively massive (2-7M(J)) transiting extrasolar planets. HAT-P-20b orbits the moderately bright V = 11.339 K3 dwarf star GSC 1910-00239 on a circular orbit, with a period P = 2.875317 +/- 0.000004 days, transit epoch T-c = 2455080.92661 +/- 0.00021 (BJD(UTC)), and transit duration 0.0770 +/- 0.0008 days. The host star has a mass of 0.76 +/- 0.03 M-circle dot, radius of 0.69 +/- 0.02 R-circle dot, effective temperature 4595 +/- 80 K, and metallicity [Fe/H] = +0.35 +/- 0.08. The planetary companion has a mass of 7.246 +/- 0.187 M-J and a radius of 0.867 +/- 0.033 R-J yielding a mean density of 13.78 +/- 1.50 g cm(-3). HAT-P-21b orbits the V = 11.685 G3 dwarf star GSC 3013-01229 on an eccentric (e = 0.228 +/- 0.016) orbit, with a period P = 4.124481 +/- 0.000007 days, transit epoch T-c = 2454996.41312 +/- 0.00069, and transit duration 0.1530 +/- 0.0027 days. The host star has a mass of 0.95 +/- 0.04 M-circle dot, radius of 1.10 +/- 0.08 R-circle dot, effective temperature 5588 +/- 80 K, and metallicity [Fe/H] = +0.01 +/- 0.08. The planetary companion has a mass of 4.063 +/- 0.161 M-J and a radius of 1.024 +/- 0.092 R-J yielding a mean density of 4.68(-0.99)(+1.59) g cm(-3). HAT-P-21b is a borderline object between the pM and pL class planets, and the transits occur near apastron. HAT-P-22b orbits the bright V = 9.732 G5 dwarf star HD 233731 on a circular orbit, with a period P = 3.212220 +/- 0.000009 days, transit epoch T-c = 2454930.22001 +/- 0.00025, and transit duration 0.1196 +/- 0.0014 days. The host star has a mass of 0.92 +/- 0.03 M-circle dot, radius of 1.04 +/- 0.04 R-circle dot, effective temperature 5302 +/- 80 K, and metallicity [Fe/H] = +0.24 +/- 0.08. The planet has a mass of 2.147 +/- 0.061 M-J and a compact radius of 1.080 +/- 0.058 R-J yielding a mean density of 2.11(-0.29)(+0.40) g cm(-3). The host star also harbors an M-dwarf companion at a wide separation. Finally, HAT-P-23b orbits the V = 12.432 G0 dwarf star GSC 1632-01396 on a close to circular orbit, with a period P = 1.212884 +/- 0.000002 days, transit epoch T-c = 2454852.26464 +/- 0.00018, and transit duration 0.0908 +/- 0.0007 days. The host star has a mass of 1.13 +/- 0.04 M-circle dot, radius of 1.20 +/- 0.07 R-circle dot, effective temperature 5905 +/- 80 K, and metallicity [Fe/H] = + 0.15 +/- 0.04. The planetary companion has a mass of 2.090 +/- 0.111 M-J and a radius of 1.368 +/- 0.090 R-J yielding a mean density of 1.01 +/- 0.18 g cm(-3). HAT-P-23b is an inflated and massive hot Jupiter on a very short period orbit, and has one of the shortest characteristic infall times (7.5(-1.8)(+2.9) Myr) before it gets engulfed by the star.
C1 [Bakos, G. A.; Hartman, J.; Torres, G.; Latham, D. W.; Noyes, R. W.; Kipping, D.; Esquerdo, G. A.; Beky, B.; Perumpilly, G.; Everett, M.; Sasselov, D. D.; Stefanik, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary.
[Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Fischer, D. A.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA.
[Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Marcy, G. W.; Howard, A. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kipping, D.] UCL, Dept Phys, London WC1E 6BT, England.
[Shporer, A.] LCOGT, Santa Barbara, CA USA.
[Shporer, A.] UC Santa Barbara, Dept Phys, Santa Barbara, CA USA.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary.
RP Bakos, GA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM gbakos@cfa.harvard.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars
A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166; Fischer,
Debra/0000-0003-2221-0861
FU NOAO; NASA
FX 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. Keck time has been granted by NOAO and NASA.
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JI Astrophys. J.
PD DEC 1
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SC Astronomy & Astrophysics
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UT WOS:000297211900056
ER
PT J
AU Binder, B
Williams, BF
Eracleous, M
Garcia, MR
Anderson, SF
Gaetz, TJ
AF Binder, B.
Williams, B. F.
Eracleous, M.
Garcia, M. R.
Anderson, S. F.
Gaetz, T. J.
TI A DEEP CHANDRA OBSERVATION OF THE WOLF-RAYET plus BLACK HOLE BINARY NGC
300 X-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars: Wolf-Rayet; X-rays: binaries
ID QUASI-PERIODIC OSCILLATIONS; SOURCE POPULATION; LMC X-3; MASS;
ACCRETION; FREQUENCY; TRANSITIONS; GALAXIES; MODELS; STARS
AB We have obtained a 63 ks Chandra ACIS-I observation of the Wolf-Rayet + black hole binary NGC 300 X-1. We measure rapid low-amplitude variability in the 0.35-8 keV light curve. The power density spectrum has a power-law index gamma = 1.02 +/- 0.15 consistent with an accreting black hole in a steep power-law state. When compared to previous studies of NGC 300 X-1 performed with XMM-Newton, we find the source at the low end of the previously measured 0.3-10 keV luminosity. The spectrum of NGC 300 X-1 is dominated by a power law (Gamma = 2.0 +/- 0.3) with a contribution at low energies by a thermal component. We estimate the 0.3-10 keV luminosity to be 2.6(-1.0)(+0.8) x 10(38) erg s(-1). The timing and spectroscopic properties of NGC 300 X-1 are consistent with being in a steep power-law state, similar to earlier observations performed with XMM-Newton. We additionally compare our observations to known high-mass X-ray binaries and ultraluminous X-ray sources, and find the properties of NGC 300 X-1 are most consistent with black hole high-mass X-ray binaries.
C1 [Binder, B.; Williams, B. F.; Anderson, S. F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Eracleous, M.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Eracleous, M.] Penn State Univ, Ctr Gravitat Wave Phys, Davey Lab 525, University Pk, PA 16802 USA.
[Garcia, M. R.; Gaetz, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Binder, B (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
FU Chandra [GO1-12118X]; NASA [NAS8-03060]
FX The authors thank the anonymous referee for the many helpful comments
which significantly improved this manuscript. B.B. and B.F.W.
acknowledge support from Chandra grant GO1-12118X. M.R.G. and T.J.G.
acknowledge support of NASA Contract NAS8-03060.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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JI Astrophys. J.
PD DEC 1
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AR 128
DI 10.1088/0004-637X/742/2/128
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SC Astronomy & Astrophysics
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UT WOS:000297211900068
ER
PT J
AU Foley, RJ
Sanders, NE
Kirshner, RP
AF Foley, Ryan J.
Sanders, Nathan E.
Kirshner, Robert P.
TI VELOCITY EVOLUTION AND THE INTRINSIC COLOR OF TYPE Ia SUPERNOVAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE distance scale; dust, extinction; supernovae: general
ID HUBBLE-SPACE-TELESCOPE; BVRI LIGHT CURVES; WIDTH-LUMINOSITY RELATION;
DARK ENERGY; SPECTRAL EVOLUTION; SPECTROSCOPIC OBSERVATIONS; OPTICAL
SPECTROSCOPY; LEGACY SURVEY; DECLINE RATE; SN
AB To understand how best to use observations of Type Ia supernovae (SNe Ia) to obtain precise and accurate distances, we investigate the relations between spectra of SNe Ia and their intrinsic colors. Using a sample of 1630 optical spectra of 255 SNe, based primarily on data from the CfA Supernova Program, we examine how the velocity evolution and line strengths of Si II lambda 6355 and Ca II H&K are related to the B - V color at peak brightness. We find that the maximum-light velocity of Si II lambda 6355 and Ca II H&K and the maximum-light pseudo-equivalent width of Si II lambda 6355 are correlated with intrinsic color, with intrinsic color having a linear relation with the Si II lambda 6355 measurements. Ca II H&K does not have a linear relation with intrinsic color, but lower-velocity SNe tend to be intrinsically bluer. Combining the spectroscopic measurements does not improve intrinsic color inference. The intrinsic color scatter is larger for higher-velocity SNe Ia-even after removing a linear trend with velocity-indicating that lower-velocity SNe Ia are more "standard crayons." Employing information derived from SN Ia spectra has the potential to improve the measurements of extragalactic distances and the cosmological properties inferred from them.
C1 [Foley, Ryan J.; Sanders, Nathan E.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rfoley@cfa.harvard.edu
FU Clay Fellowship; National Science Foundation [AST09-07903]
FX R.J.F. is supported by a Clay Fellowship. N.E.S. is supported by the
National Science Foundation through a Graduate Research Fellowship.
Supernova studies at the Harvard College Observatory are supported by
NSF grant AST09-07903.
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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 DEC 1
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SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900029
ER
PT J
AU Fuentes, CI
Trilling, DE
Holman, MJ
AF Fuentes, Cesar I.
Trilling, David E.
Holman, Matthew J.
TI DYNAMICALLY EXCITED OUTER SOLAR SYSTEM OBJECTS IN THE HUBBLE SPACE
TELESCOPE ARCHIVE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Kuiper belt: general; planets and satellites: formation
ID KUIPER-BELT OBJECTS; TRANS-NEPTUNIAN OBJECTS; SIZE DISTRIBUTION;
LUMINOSITY FUNCTION; INCLINATION DISTRIBUTION; SEARCH; BODIES
AB We present the faintest mid-ecliptic latitude survey in the second part of Hubble Space Telescope archival search for outer solar system bodies. We report the discovery of 28 new trans-Neptunian objects and one small centaur (R similar to 2 km) in the band 5 degrees-20 degrees off the ecliptic. The inclination distribution of these excited objects is consistent with the distribution derived from brighter ecliptic surveys. We suggest that the size and inclination distribution should be estimated consistently using suitable surveys with calibrated search algorithms and reliable orbital information.
C1 [Fuentes, Cesar I.; Trilling, David E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA.
[Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Fuentes, CI (reprint author), No Arizona Univ, Dept Phys & Astron, POB 6010, Flagstaff, AZ 86011 USA.
EM cesar.i.fuentes@nau.edu
RI Fuentes, Cesar /G-7506-2016
FU NASA through the Space Telescope Science Institute; NASA [NAS 5-26555]
FX Support for program 11778 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
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DI 10.1088/0004-637X/742/2/118
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SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900058
ER
PT J
AU Gou, LJ
McClintock, JE
Reid, MJ
Orosz, JA
Steiner, JF
Narayan, R
Xiang, JG
Remillard, RA
Arnaud, KA
Davis, SW
AF Gou, Lijun
McClintock, Jeffrey E.
Reid, Mark J.
Orosz, Jerome A.
Steiner, James F.
Narayan, Ramesh
Xiang, Jingen
Remillard, Ronald A.
Arnaud, Keith A.
Davis, Shane W.
TI THE EXTREME SPIN OF THE BLACK HOLE IN CYGNUS X-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; stars: individual
(Cygnus X-1); X-rays: binaries
ID X-RAY BINARIES; CONTINUUM-FITTING METHOD; ACCRETION DISK MODELS; DWARF
NOVA OUTBURSTS; EMISSION-LINES; INNER-DISK; SOFT STATE; LMC X-1; MASS;
REFLECTION
AB The compact primary in the X-ray binary Cygnus X-1 was the first black hole to be established via dynamical observations. We have recently determined accurate values for its mass and distance, and for the orbital inclination angle of the binary. Building on these results, which are based on our favored (asynchronous) dynamical model, we have measured the radius of the inner edge of the black hole's accretion disk by fitting its thermal continuum spectrum to a fully relativistic model of a thin accretion disk. Assuming that the spin axis of the black hole is aligned with the orbital angular momentum vector, we have determined that Cygnus X-1 contains a near-extreme Kerr black hole with a spin parameter a(*) > 0.95 (3 sigma). For a less probable (synchronous) dynamical model, we find a(*) > 0.92 (3 sigma). In our analysis, we include the uncertainties in black hole mass, orbital inclination angle, and distance, and we also include the uncertainty in the calibration of the absolute flux via the Crab. These four sources of uncertainty totally dominate the error budget. The uncertainties introduced by the thin-disk model we employ are particularly small in this case given the extreme spin of the black hole and the disk's low luminosity.
C1 [Gou, Lijun; McClintock, Jeffrey E.; Reid, Mark J.; Steiner, James F.; Narayan, Ramesh; Xiang, Jingen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Arnaud, Keith A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Arnaud, Keith A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Davis, Shane W.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
RP Gou, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Narayan, Ramesh/0000-0002-1919-2730
FU NASA [DD0-11049X, DD1-12054X, NNX11AD08G]; Smithsonian Endowment Funds
FX We thank an anonymous referee for very helpful and constructive
comments. We are grateful to Director H. Tanananbaum and Project
Scientist T. Strohmayer for granting us, respectively, Chandra and RXTE
observing time. We thank H. Marshall, M. Nowak, and N. Schulz for help
in planning the Chandra observations, and M. Hanke, M. Nowak, and J.
Wilms for discussions on X-ray data analysis. The research has made use
of data obtained from the High Energy Astrophysics Science Archive
Research Center (HEASARC) at NASA/Goddard Space Flight Center. L. G.
thanks the Harvard FAS Sciences Division Research Computing Group for
their technical support on the Odyssey cluster. J. E. M. acknowledges
support from NASA grants DD0-11049X, DD1-12054X, and NNX11AD08G, and the
Smithsonian Endowment Funds.
NR 80
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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 DEC 1
PY 2011
VL 742
IS 2
AR 85
DI 10.1088/0004-637X/742/2/85
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900025
ER
PT J
AU Irwin, JM
Quinn, SN
Berta, ZK
Latham, DW
Torres, G
Burke, CJ
Charbonneau, D
Dittmann, J
Esquerdo, GA
Stefanik, RP
Oksanen, A
Buchhave, LA
Nutzman, P
Berlind, P
Calkins, ML
Falco, EE
AF Irwin, Jonathan M.
Quinn, Samuel N.
Berta, Zachory K.
Latham, David W.
Torres, Guillermo
Burke, Christopher J.
Charbonneau, David
Dittmann, Jason
Esquerdo, Gilbert A.
Stefanik, Robert P.
Oksanen, Arto
Buchhave, Lars A.
Nutzman, Philip
Berlind, Perry
Calkins, Michael L.
Falco, Emilio E.
TI LSPM J1112+7626: DETECTION OF A 41 DAY M-DWARF ECLIPSING BINARY FROM THE
MEARTH TRANSIT SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; stars: low-mass
ID LOW-MASS STARS; DIGITAL SKY SURVEY; STELLAR ATMOSPHERE MODELS; LOWER
MAIN-SEQUENCE; LIMB-DARKENING LAW; FIELD M-DWARFS; CM-DRACONIS; ACCURATE
MASSES; DATA RELEASE; ABSOLUTE DIMENSIONS
AB We report the detection of eclipses in LSPM J1112+7626, which we find to be a moderately bright (I-C = 12.14 +/- 0.05) very low mass binary system with an orbital period of 41.03236 +/- 0.00002 days, and component masses M-1 = 0.395 +/- 0.002 M-circle dot and M-2 = 0.275 +/- 0.001 M-circle dot in an eccentric (e = 0.239 +/- 0.002) orbit. A 65 day out-of-eclipse modulation of approximately 2% peak-to-peak amplitude is seen in I-band, which is probably due to rotational modulation of photospheric spots on one of the binary components. This paper presents the discovery and characterization of the object, including radial velocities sufficient to determine both component masses to better than 1% precision, and a photometric solution. We find that the sum of the component radii, which is much better determined than the individual radii, is inflated by 3.8(-0.5)(+0.9)% compared to the theoretical model predictions, depending on the age and metallicity assumed. These results demonstrate that the difficulties in reproducing observed M-dwarf eclipsing binary radii with theoretical models are not confined to systems with very short orbital periods. This object promises to be a fruitful testing ground for the hypothesized link between inflated radii in M-dwarfs and activity.
C1 [Irwin, Jonathan M.; Quinn, Samuel N.; Berta, Zachory K.; Latham, David W.; Torres, Guillermo; Burke, Christopher J.; Charbonneau, David; Dittmann, Jason; Esquerdo, Gilbert A.; Stefanik, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Oksanen, Arto] Hankasalmi Observ, FI-40270 Palokka, Finland.
[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.
[Nutzman, Philip] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Berlind, Perry; Calkins, Michael L.; Falco, Emilio E.] Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
RP Irwin, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jirwin@cfa.harvard.edu
OI Berta-Thompson, Zachory/0000-0002-3321-4924; Buchhave, Lars
A./0000-0003-1605-5666; Charbonneau, David/0000-0002-9003-484X
FU David and Lucile Packard Fellowship for Science and Engineering;
National Science Foundation (NSF) [AST-0807690, AST-1007992]; NASA
[NCC2-1390]; Space Telescope Science Institute under U.S. Government
[NAG W-2166]; Alfred P. Sloan Foundation; U.S. Department of Energy;
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; United States Naval Observatory;
University of Washington
FX The MEarth team gratefully acknowledges funding from the David and
Lucile Packard Fellowship for Science and Engineering (awarded to D.C.)
and the National Science Foundation (NSF) under grant number
AST-0807690. S.N.Q., D.W.L., and G.A.E. acknowledge partial support from
the NASA Kepler mission under cooperative agreement NCC2-1390, and G.T.
acknowledges partial support from NSF grant AST-1007992. We thank
Allyson Bieryla for assistance with the Clay telescope observations,
David Kipping for discussions of appropriate priors for use in Monte
Carlo simulations, Eric Mamajek for compiling and maintaining the "Basic
Astronomical Data for the Sun" page, Todd Vaccaro for clarification of
the parameters of LP 133-373, Andrew West for discussions of M-dwarf
activity, and Edo Berger and the 2011 Harvard Astronomy 100
undergraduate class for assistance with the FAST observations. The
anonymous referee is thanked for a prompt and helpful report that
improved the manuscript. The MEarth team is greatly indebted to the
staff at the Fred Lawrence Whipple Observatory for their efforts in
construction and maintenance of the facility, and thank Wayne Peters,
Ted Groner, Karen Erdman-Myres, Grace Alegria, Rodger Harris, Bob
Hutchins, Dave Martina, Dennis Jankovsky, and Tom Welsh for their
support.; This research has made extensive use of data products from the
Two Micron All Sky Survey, which is a joint project of the University of
Massachusetts and the Infrared Processing and Analysis Center/California
Institute of Technology, funded by NASA and the NSF, NASA's Astrophysics
Data System (ADS) bibliographic services, and the SIMBAD database,
operated at CDS, Strasbourg, France. The Digitized Sky Surveys were
produced at the Space Telescope Science Institute under U.S. Government
grant NAG W-2166. The images of these surveys are based on photographic
data obtained using the Oschin Schmidt Telescope on Palomar Mountain and
the UK Schmidt Telescope. The plates were processed into the present
compressed digital form with the permission of these institutions.;
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/. The SDSS is managed by the
Astrophysical Research Consortium for the Participating Institutions.
The Participating Institutions are the American Museum of Natural
History, Astrophysical Institute Potsdam, University of Basel,
University of Cambridge, Case Western Reserve University, University of
Chicago, Drexel University, Fermilab, the Institute for Advanced Study,
the Japan Participation Group, Johns Hopkins University, the Joint
Institute for Nuclear Astrophysics, the Kavli Institute for Particle
Astrophysics and Cosmology, the Korean Scientist Group, the Chinese
Academy of Sciences (LAMOST), Los Alamos National Laboratory, the
Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for
Astrophysics (MPA), New Mexico State University, Ohio State University,
University of Pittsburgh, University of Portsmouth, Princeton
University, the United States Naval Observatory, and the University of
Washington.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2011
VL 742
IS 2
AR 123
DI 10.1088/0004-637X/742/2/123
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900063
ER
PT J
AU Lotz, JM
Jonsson, P
Cox, TJ
Croton, D
Primack, JR
Somerville, RS
Stewart, K
AF Lotz, Jennifer M.
Jonsson, Patrik
Cox, T. J.
Croton, Darren
Primack, Joel R.
Somerville, Rachel S.
Stewart, Kyle
TI THE MAJOR AND MINOR GALAXY MERGER RATES AT z < 1.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: interactions;
galaxies: structure
ID STAR-FORMING GALAXIES; HIGH-REDSHIFT GALAXIES; DARK-MATTER HALOES; VLT
DEEP SURVEY; SIMILAR-TO 1; SUPERMASSIVE BLACK-HOLES; MASS ASSEMBLY
HISTORIES; ACTIVE GALACTIC NUCLEI; EXTENDED GROTH STRIP; DIGITAL SKY
SURVEY
AB Calculating the galaxy merger rate requires both a census of galaxies identified as merger candidates and a cosmologically averaged "observability" timescale < T-obs(z)> for identifying galaxy mergers. While many have counted galaxy mergers using a variety of techniques, < T-obs(z)> for these techniques have been poorly constrained. We address this problem by calibrating three merger rate estimators with a suite of hydrodynamic merger simulations and three galaxy formation models. We estimate < T-obs(z)> for (1) close galaxy pairs with a range of projected separations, (2) the morphology indicator G - M-20, and (3) the morphology indicator asymmetry Lambda A. Then, we apply these timescales to the observed merger fractions at z < 1.5 from the recent literature. When our physically motivated timescales are adopted, the observed galaxy merger rates become largely consistent. The remaining differences between the galaxy merger rates are explained by the differences in the ranges of the mass ratio measured by different techniques and differing parent galaxy selection. The major merger rate per unit comoving volume for samples selected with constant number density evolves much more strongly with redshift (alpha (1 + z)(+3.0 +/- 1.1)) than samples selected with constant stellar mass or passively evolving luminosity (alpha (1 + z)(+0.1 +/- 0.4)). We calculate the minor merger rate (1:4 < M-sat/M-primary less than or similar to 1:10) by subtracting the major merger rate from close pairs from the "total" merger rate determined by G - M-20. The implied minor merger rate is similar to 3 times the major merger rate at z similar to 0.7 and shows little evolution with redshift.
C1 [Lotz, Jennifer M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Lotz, Jennifer M.; Somerville, Rachel S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Jonsson, Patrik] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cox, T. J.] Carnegie Observ, Pasadena, CA USA.
[Croton, Darren] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Somerville, Rachel S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Stewart, Kyle] Jet Prop Lab, Pasadena, CA USA.
RP Lotz, JM (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA.
EM lotz@stsci.edu
FU NOAO; W. M. Keck Foundation; Australian Government; Office of Science of
the U.S. Department of Energy
FX We thank L. Lin, L. de Ravel, J. Kartaltepe, and Y. Shi for sending us
detailed versions of their data and calculations. We thank N. Scoville,
K. Bundy, P. Hopkins, and the anonymous referee for helpful comments on
earlier version of this manuscript. We acknowledge the use of S. Salim's
measurements of the stellar masses for galaxies in the Extended Groth
Strip. J. M. L. acknowledges support from the NOAO Leo Goldberg
Fellowship. P. J. was supported by a grant from the W. M. Keck
Foundation. D. C. acknowledges receipt of a QEII Fellowship by the
Australian Government. This research used computational resources of the
NASA Advanced Supercomputing Division (NAS) and the National Energy
Research Scientific Computing Center (NERSC), which is supported by the
Office of Science of the U.S. Department of Energy.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2011
VL 742
IS 2
DI 10.1088/0004-637X/742/2/103
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900043
ER
PT J
AU Munoz, JA
Mediavilla, E
Kochanek, CS
Falco, EE
Mosquera, AM
AF Munoz, J. A.
Mediavilla, E.
Kochanek, C. S.
Falco, E. E.
Mosquera, A. M.
TI A STUDY OF GRAVITATIONAL LENS CHROMATICITY WITH THE HUBBLE SPACE
TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; cosmology: observations; dust, extinction;
galaxies: ISM; gravitational lensing: micro
ID LINE QSO H1413+1143; OPTICAL-TIME DELAY; QUASAR PG 1115+080; EXTINCTION
CURVES; ACCRETION DISK; ULTRAVIOLET EXTINCTION; SYSTEM B1600+434; LIGHT
CURVES; GALAXIES; HE-1104-1805
AB We report Hubble Space Telescope observations of six gravitational lenses with the Advanced Camera for Surveys. We measured the flux ratios between the lensed images in seven filters from 8140 angstrom to 2200 angstrom. In three of the systems, HE0512-3329, B1600+434, and H1413 + 117, we were able to construct UV extinction curves partially overlapping the 2175 angstrom feature and characterize the properties of the dust relative to the Galaxy and the Magellanic Clouds. In HE1104-1804, we detect chromatic microlensing and use it to study the physical properties of the quasar accretion disk. For a Gaussian model of the disk exp(-r(2)/2r(s)(2) ), scaling with wavelength as r(s) alpha lambda(p), we estimate r(s) (lambda 3363) = 4(-2)(+4) (7 +/- 4) light days and p = 1.1 +/- 0.6 (1.0 +/- 0.6) for a logarithmic (linear) prior on r(s). The remaining two systems, FBQ0951+2635 and SBS1520+530, yielded no useful estimates of extinction or chromatic microlensing.
C1 [Munoz, J. A.; Mosquera, A. M.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
[Mediavilla, E.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Kochanek, C. S.; Mosquera, A. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Falco, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Munoz, JA (reprint author), Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
EM jmunoz@uv.es
FU European Community [MRTN-CT-2004-505183]; Spanish Ministerio de
Educacion y Ciencias [AYA2007-67342-C03-01/03, AYA2010-21741-C03/02];
Generalitat Valenciana [PROMETEO/2009/64, APOSTD/2010/030]; NSF
[AST-1009756]; NASA [NAS 5-26555]
FX This research was supported by the European Community's Sixth Framework
Marie Curie Research Training Network Programme, Contract No.
MRTN-CT-2004-505183 "ANGLES," and by the Spanish Ministerio de Educacion
y Ciencias (grants AYA2007-67342-C03-01/03 and AYA2010-21741-C03/02).
J.A.M. is also supported by the Generalitat Valenciana with the grant
PROMETEO/2009/64. A. M. M. is also supported by Generalitat Valenciana,
grant APOSTD/2010/030. C. S. K. is supported in part by NSF grant
AST-1009756. These observations are associated with program GO-9896.;
Based on observations made with the NASA/ESA Hubble Space Telescope. The
Space Telescope Science Institute is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555.
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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 DEC 1
PY 2011
VL 742
IS 2
AR 67
DI 10.1088/0004-637X/742/2/67
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900007
ER
PT J
AU Orosz, JA
McClintock, JE
Aufdenberg, JP
Remillard, RA
Reid, MJ
Narayan, R
Gou, LJ
AF Orosz, Jerome A.
McClintock, Jeffrey E.
Aufdenberg, Jason P.
Remillard, Ronald A.
Reid, Mark J.
Narayan, Ramesh
Gou, Lijun
TI THE MASS OF THE BLACK HOLE IN CYGNUS X-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; black hole physics; stars: individual (Cygnus X-1);
X-rays: binaries
ID BLANKETED MODEL ATMOSPHERES; BROAD-BAND SPECTRUM; X-RAY; LIGHT-CURVE;
BINARY; STAR
AB Cygnus X-1 is a binary star system that is comprised of a black hole and a massive giant companion star in a tight orbit. Building on our accurate distance measurement reported in the preceding paper, we first determine the radius of the companion star, thereby constraining the scale of the binary system. To obtain a full dynamical model of the binary, we use an extensive collection of optical photometric and spectroscopic data taken from the literature. By using all of the available observational constraints, we show that the orbit is slightly eccentric (both the radial velocity and photometric data independently confirm this result) and that the companion star rotates roughly 1.4 times its pseudosynchronous value. We find a black hole mass of M = 14.8 +/- 1.0 M-circle dot, a companion mass of M-opt = 19.2 +/- 1.9M(circle dot), and the angle of inclination of the orbital plane to our line of sight of i = 27.1 +/- 0.8 deg.
C1 [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[McClintock, Jeffrey E.; Reid, Mark J.; Narayan, Ramesh; Gou, Lijun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Aufdenberg, Jason P.] Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL 32114 USA.
[Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Orosz, JA (reprint author), San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
EM orosz@sciences.sdsu.edu; jem@cfa.harvard.edu; aufded93@erau.edu;
rr@space.mit.edu; reid@cfa.harvard.edu; narayan@cfa.harvard.edu;
lgou@cfa.harvard.edu
OI Narayan, Ramesh/0000-0002-1919-2730
FU NASA [NNX11AD08G]
FX We thank Catherine Brocksopp for sending us the optical light curves.
The work of J.E.M. was supported in part by NASA grant NNX11AD08G. This
research has made use of NASA's Astrophysics Data System.
NR 36
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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 DEC 1
PY 2011
VL 742
IS 2
AR 84
DI 10.1088/0004-637X/742/2/84
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900024
ER
PT J
AU Reid, MJ
McClintock, JE
Narayan, R
Gou, LJ
Remillard, RA
Orosz, JA
AF Reid, Mark J.
McClintock, Jeffrey E.
Narayan, Ramesh
Gou, Lijun
Remillard, Ronald A.
Orosz, Jerome A.
TI THE TRIGONOMETRIC PARALLAX OF CYGNUS X-1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; black hole physics; stars: distances; stars: individual
(Cygnus X-1); X-rays: binaries
ID BLACK-HOLE; STELLAR ORBITS; DISTANCE; BINARY; GALAXY; MILKY; MASS
AB We report a direct and accurate measurement of the distance to the X-ray binary Cygnus X-1, which contains the first black hole to be discovered. The distance of 1.86(-0.11)(+0.12) kpc was obtained from a trigonometric parallax measurement using the Very Long Baseline Array. The position measurements are also sensitive to the 5.6 day binary orbit and we determine the orbit to be clockwise on the sky. We also measured the proper motion of Cygnus X-1 which, when coupled to the distance and Doppler shift, gives the three-dimensional space motion of the system. When corrected for differential Galactic rotation, the non-circular (peculiar) motion of the binary is only about 21 km s(-1), indicating that the binary did not experience a large "kick" at formation.
C1 [Reid, Mark J.; McClintock, Jeffrey E.; Narayan, Ramesh; Gou, Lijun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Narayan, Ramesh/0000-0002-1919-2730
NR 28
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2011
VL 742
IS 2
AR 83
DI 10.1088/0004-637X/742/2/83
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900023
ER
PT J
AU Salvato, M
Ilbert, O
Hasinger, G
Rau, A
Civano, F
Zamorani, G
Brusa, M
Elvis, M
Vignali, C
Aussel, H
Comastri, A
Fiore, F
Le Floc'h, E
Mainieri, V
Bardelli, S
Bolzonella, M
Bongiorno, A
Capak, P
Caputi, K
Cappelluti, N
Carollo, CM
Contini, T
Garilli, B
Iovino, A
Fotopoulou, S
Fruscione, A
Gilli, R
Halliday, C
Kneib, JP
Kakazu, Y
Kartaltepe, JS
Koekemoer, AM
Kovac, K
Ideue, Y
Ikeda, H
Impey, CD
Le Fevre, O
Lamareille, F
Lanzuisi, G
Le Borgne, JF
Le Brun, V
Lilly, S
Maier, C
Manohar, S
Masters, D
McCracken, H
Messias, H
Mignoli, M
Mobasher, B
Nagao, T
Pello, R
Puccetti, S
Perez-Montero, E
Renzini, A
Sargent, M
Sanders, DB
Scodeggio, M
Scoville, N
Shopbell, P
Silvermann, J
Taniguchi, Y
Tasca, L
Tresse, L
Trump, JR
Zucca, E
AF Salvato, M.
Ilbert, O.
Hasinger, G.
Rau, A.
Civano, F.
Zamorani, G.
Brusa, M.
Elvis, M.
Vignali, C.
Aussel, H.
Comastri, A.
Fiore, F.
Le Floc'h, E.
Mainieri, V.
Bardelli, S.
Bolzonella, M.
Bongiorno, A.
Capak, P.
Caputi, K.
Cappelluti, N.
Carollo, C. M.
Contini, T.
Garilli, B.
Iovino, A.
Fotopoulou, S.
Fruscione, A.
Gilli, R.
Halliday, C.
Kneib, J. -P.
Kakazu, Y.
Kartaltepe, J. S.
Koekemoer, A. M.
Kovac, K.
Ideue, Y.
Ikeda, H.
Impey, C. D.
Le Fevre, O.
Lamareille, F.
Lanzuisi, G.
Le Borgne, J. -F.
Le Brun, V.
Lilly, S.
Maier, C.
Manohar, S.
Masters, D.
McCracken, H.
Messias, H.
Mignoli, M.
Mobasher, B.
Nagao, T.
Pello, R.
Puccetti, S.
Perez-Montero, E.
Renzini, A.
Sargent, M.
Sanders, D. B.
Scodeggio, M.
Scoville, N.
Shopbell, P.
Silvermann, J.
Taniguchi, Y.
Tasca, L.
Tresse, L.
Trump, J. R.
Zucca, E.
TI DISSECTING PHOTOMETRIC REDSHIFT FOR ACTIVE GALACTIC NUCLEUS USING XMM-
AND CHANDRA-COSMOS SAMPLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: distances and redshifts; methods: data
analysis; surveys; techniques: photometric; X-rays: galaxies
ID SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES; EXTENDED GROTH
STRIP; DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; DEEP-FIELD; LUMINOSITY
FUNCTION; MULTICOLOR CLASSIFICATION; LEGACY SURVEY; S-COSMOS
AB In this paper, we release accurate photometric redshifts for 1692 counterparts to Chandra sources in the central square degree of the Cosmic Evolution Survey (COSMOS) field. The availability of a large training set of spectroscopic redshifts that extends to faint magnitudes enabled photometric redshifts comparable to the highest quality results presently available for normal galaxies. We demonstrate that morphologically extended, faint X-ray sources without optical variability are more accurately described by a library of normal galaxies (corrected for emission lines) than by active galactic nucleus (AGN) dominated templates, even if these sources have AGN-like X-ray luminosities. Preselecting the library on the bases of the source properties allowed us to reach an accuracy sigma(Delta z/(1+zspec)) similar to 0.015 with a fraction of outliers of 5.8% for the entire Chandra-COSMOS sample. In addition, we release revised photometric redshifts for the 1735 optical counterparts of the XMM-detected sources over the entire 2 deg(2) of COSMOS. For 248 sources, our updated photometric redshift differs from the previous release by Delta z > 0.2. These changes are predominantly due to the inclusion of newly available deep H-band photometry (H-AB = 24 mag). We illustrate once again the importance of a spectroscopic training sample and how an assumption about the nature of a source together, with the number and the depth of the available bands, influences the accuracy of the photometric redshifts determined for AGN. These considerations should be kept in mind when defining the observational strategies of upcoming large surveys targeting AGNs, such as eROSITA at X-ray energies and the Australian Square Kilometre Array Pathfinder Evolutionary Map of the Universe in the radio band.
C1 [Salvato, M.; Hasinger, G.; Fotopoulou, S.] Max Planck Inst Plasma Phys & Excellence Cluster, D-85748 Garching, Germany.
[Ilbert, O.; Kneib, J. -P.; Le Fevre, O.; Tasca, L.; Tresse, L.] Univ Aix Marseille 1, CNRS, Lab Astrophys Marseille, UMR 6110, F-13388 Marseille 13, France.
[Hasinger, G.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Rau, A.; Brusa, M.; Bongiorno, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Civano, F.; Elvis, M.; Fruscione, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zamorani, G.; Vignali, C.; Comastri, A.; Bardelli, S.; Bolzonella, M.; Cappelluti, N.; Gilli, R.; Mignoli, M.; Zucca, E.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Aussel, H.; Le Floc'h, E.; Sargent, M.] Univ Paris Diderot, CEA DSM CNRS, IRFU SAp, F-91191 Gif Sur Yvette, France.
[Fiore, F.] INAF Osservatorio Astron Roma, Monteporzio Roma, Italy.
[Mainieri, V.] European So Observ, D-85748 Garching, Germany.
[Capak, P.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Caputi, K.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Carollo, C. M.; Lilly, S.; Maier, C.] ETH, Dept Phys, CH-8093 Zurich, Switzerland.
[Contini, T.; Lamareille, F.; Le Borgne, J. -F.; Le Brun, V.; Pello, R.; Perez-Montero, E.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Lamareille, F.; Le Borgne, J. -F.; Le Brun, V.; Pello, R.; Perez-Montero, E.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Garilli, B.; Iovino, A.; Scodeggio, M.] INAF IASF Milano, Milan, Italy.
[Halliday, C.] Osserv Astrofis Arcetri, I-50125 Florence, Italy.
[Kartaltepe, J. S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kovac, K.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Ideue, Y.; Ikeda, H.; Nagao, T.] Ehime Univ, Grad Sch Sci & Engn, Matsuyama, Ehime 7908577, Japan.
[Impey, C. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Lanzuisi, G.; Masters, D.] INAF IASF Bologna, I-40129 Bologna, Italy.
[McCracken, H.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Messias, H.] Univ Lisbon, Observ Astron Lisboa, Ctr Astron & Astrofis, P-1349018 Lisbon, Portugal.
[Mobasher, B.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92508 USA.
[Nagao, T.] Kyoto Univ, Hakubi Project, Kyoto 6068502, Japan.
[Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Perez-Montero, E.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Renzini, A.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Silvermann, J.] Univ Tokyo, IPMU, Chiba 2778568, Japan.
[Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan.
[Trump, J. R.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
RP Salvato, M (reprint author), Max Planck Inst Plasma Phys & Excellence Cluster, D-85748 Garching, Germany.
EM mara.salvato@ipp.mpg.de
RI Pello, Roser/G-4754-2010; Vignali, Cristian/J-4974-2012; Lanzuisi,
Giorgio/K-4378-2013; Kneib, Jean-Paul/A-7919-2015; Zucca,
Elena/O-9396-2015; Bardelli, Sandro/O-9369-2015; Mignoli,
Marco/O-9426-2015; Bolzonella, Micol/O-9495-2015; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015;
OI Zamorani, Giovanni/0000-0002-2318-301X; Koekemoer,
Anton/0000-0002-6610-2048; Perez Montero, E/0000-0003-3985-4882; Brusa,
Marcella/0000-0002-5059-6848; Puccetti, Simonetta/0000-0002-2734-7835;
Fiore, Fabrizio/0000-0002-4031-4157; Bongiorno,
Angela/0000-0002-0101-6624; Scodeggio, Marco/0000-0002-2282-5850;
Cappelluti, Nico/0000-0002-1697-186X; Maier,
Christian/0000-0001-6405-2182; Garilli, Bianca/0000-0001-7455-8750;
Vignali, Cristian/0000-0002-8853-9611; Lanzuisi,
Giorgio/0000-0001-9094-0984; Kneib, Jean-Paul/0000-0002-4616-4989;
Zucca, Elena/0000-0002-5845-8132; Bardelli, Sandro/0000-0002-8900-0298;
Mignoli, Marco/0000-0002-9087-2835; Bolzonella,
Micol/0000-0003-3278-4607; Comastri, Andrea/0000-0003-3451-9970; Gilli,
Roberto/0000-0001-8121-6177; Fotopoulou, Sotiria/0000-0002-9686-254X;
Iovino, Angela/0000-0001-6958-0304
FU National Aeronautics Space Administration [NAS8-03060, NAS 5-26555,
1407]; ESA Member States; European Southern Observatory, Chile [175.
A-0839]; Kitt Peak National Observatory; Cerro Tololo Inter-American
Observatory; National Optical Astronomy Observatory; German Deutsche
Forschungsgemeinschaft, DFG Leibniz Prize [FKZ HA 1850/28-1]; NASA
Chandra [GO7-8136A]; Blancheflor Boncompagni Ludovisi foundation;
Smithsonian Scholarly Studies; [ASI-INAF I/009/10/0]
FX Based on observations 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. Also based on observations with the NASA/ESA Hubble Space
Telescope, obtained at the Space Telescope Science Institute, which is
operated by AURA Inc., under NASA contract NAS 5-26555. Also based on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology, under
NASA contract 1407. Also based on data collected at the Subaru
Telescope, which is operated by the National Astronomical Observatory of
Japan; the XMM-Newton, an ESA science mission with instruments and
contributions directly funded by ESA Member States and NASA; the
European Southern Observatory under Large Program 175. A-0839, Chile;
the Kitt Peak National Observatory, Cerro Tololo Inter-American
Observatory and the National Optical Astronomy Observatory, which are
operated by the Association of Universities for Research in Astronomy,
Inc. (AURA), under cooperative agreement with the National Science
Foundation; the Canada-France-Hawaii Telescope with MegaPrime/MegaCam
operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the NRC
and CADC of Canada, the CNRS of France, TERAPIX, and the University of
Hawaii.; We gratefully acknowledge the contributions of the entire
COSMOS collaboration consisting of more than 100 scientists. More
information about the COSMOS survey is available at
http://www.astro.caltech.edu/similar to cosmos. We also acknowledge the
use of STILTS and TOPCAT tools (Taylor 2005). We acknowledge the
anonymous referee for helpful comments that improved the paper. M. S.
and G. H. acknowledge support by the German Deutsche
Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1). F. C. was
supported in part by NASA Chandra grant No. GO7-8136A, the Blancheflor
Boncompagni Ludovisi foundation, and the Smithsonian Scholarly Studies.
A. C., C. V., N.C., and F. F. acknowledge financial contribution from
agreement ASI-INAF I/009/10/0.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2011
VL 742
IS 2
AR 61
DI 10.1088/0004-637X/742/2/61
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900001
ER
PT J
AU van der Wel, A
Straughn, AN
Rix, HW
Finkelstein, SL
Koekemoer, AM
Weiner, BJ
Wuyts, S
Bell, EF
Faber, SM
Trump, JR
Koo, DC
Ferguson, HC
Scarlata, C
Hathi, NP
Dunlop, JS
Newman, JA
Dickinson, M
Jahnke, K
Salmon, BW
de Mello, DF
Kocevski, DD
Lai, K
Grogin, NA
Rodney, SA
Guo, YC
McGrath, EJ
Lee, KS
Barro, G
Huang, KH
Riess, AG
Ashby, MLN
Willner, SP
AF van der Wel, A.
Straughn, A. N.
Rix, H. -W.
Finkelstein, S. L.
Koekemoer, A. M.
Weiner, B. J.
Wuyts, S.
Bell, E. F.
Faber, S. M.
Trump, J. R.
Koo, D. C.
Ferguson, H. C.
Scarlata, C.
Hathi, N. P.
Dunlop, J. S.
Newman, J. A.
Dickinson, M.
Jahnke, K.
Salmon, B. W.
de Mello, D. F.
Kocevski, D. D.
Lai, K.
Grogin, N. A.
Rodney, S. A.
Guo, Yicheng
McGrath, E. J.
Lee, K. -S.
Barro, G.
Huang, K. -H.
Riess, A. G.
Ashby, M. L. N.
Willner, S. P.
TI EXTREME EMISSION-LINE GALAXIES IN CANDELS: BROADBAND-SELECTED,
STARBURSTING DWARF GALAXIES AT z > 1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies:
high-redshift; galaxies: starburst
ID EARLY RELEASE SCIENCE; LY-ALPHA EMITTERS; ORIGINS DEEP SURVEY; GREEN PEA
GALAXIES; STAR-FORMATION; FORMATION HISTORIES; MASS FUNCTION; LOCAL
VOLUME; FIELD; EVOLUTION
AB We identify an abundant population of extreme emission-line galaxies (EELGs) at redshift z similar to 1.7 in the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey imaging from Hubble Space Telescope/Wide Field Camera 3 (HST/WFC3). Sixty-nine EELG candidates are selected by the large contribution of exceptionally bright emission lines to their near-infrared broadband magnitudes. Supported by spectroscopic confirmation of strong [OIII] emission lines-with rest-frame equivalent widths similar to 1000 angstrom-in the four candidates that have HST/WFC3 grism observations, we conclude that these objects are galaxies with similar to 10(8) M-circle dot in stellar mass, undergoing an enormous starburst phase with M-*/(M) over dot(*) of only similar to 15 Myr. These bursts may cause outflows that are strong enough to produce cored dark matter profiles in low-mass galaxies. The individual star formation rates and the comoving number density (3.7 x 10(-4) Mpc(-3)) can produce in similar to 4 Gyr much of the stellar mass density that is presently contained in 10(8)-10(9) M-circle dot dwarf galaxies. Therefore, our observations provide a strong indication that many or even most of the stars in present-day dwarf galaxies formed in strong, short-lived bursts, mostly at z > 1.
C1 [van der Wel, A.; Rix, H. -W.; Jahnke, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Straughn, A. N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Finkelstein, S. L.; Salmon, B. W.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Koekemoer, A. M.; Ferguson, H. C.; Grogin, N. A.; Riess, A. G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Weiner, B. J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Wuyts, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bell, E. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Faber, S. M.; Trump, J. R.; Koo, D. C.; Kocevski, D. D.; Lai, K.; McGrath, E. J.; Barro, G.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Scarlata, C.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Hathi, N. P.] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
[Dunlop, J. S.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Newman, J. A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Dickinson, M.] Natl Optic Astron Observ, Tucson, AZ 85719 USA.
[de Mello, D. F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[de Mello, D. F.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Rodney, S. A.; Huang, K. -H.; Riess, A. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Guo, Yicheng] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Lee, K. -S.] Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA.
[Ashby, M. L. N.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP van der Wel, A (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM vdwel@mpia.de
RI Hathi, Nimish/J-7092-2014;
OI Hathi, Nimish/0000-0001-6145-5090; Koekemoer, Anton/0000-0002-6610-2048;
Bell, Eric/0000-0002-5564-9873
FU HST [GO-12060]; NSF [AST 08-08133]
FX A.v.d.W. thanks the following people for useful feedback and stimulating
discussions: Greg Stinson, Andrea Maccio, Brent Groves, Dan Weisz, Joe
Hennawi, Kate Rubin, Sharon Meidt, and Marijn Franx. S.M.F., J.R.T.,
D.C.K., D.D.K., K.L., and E.G.M. acknowledge funding through HST
GO-12060 and NSF AST 08-08133.
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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 DEC 1
PY 2011
VL 742
IS 2
AR 111
DI 10.1088/0004-637X/742/2/111
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900051
ER
PT J
AU Zhu, GT
Zaw, I
Blanton, MR
Greenhill, LJ
AF Zhu, Guangtun
Zaw, Ingyin
Blanton, Michael R.
Greenhill, Lincoln J.
TI OPTICAL PROPERTIES OF HOST GALAXIES OF EXTRAGALACTIC NUCLEAR WATER
MASERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: nuclei; galaxies: Seyfert; masers; radio
lines: galaxies
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; STELLAR VELOCITY
DISPERSIONS; SUPERMASSIVE BLACK-HOLES; DWARF SEYFERT NUCLEI; MASS
ACCRETION RATE; H2O MASERS; X-RAY; NEARBY GALAXIES; BRIGHT GALAXIES
AB We study the optical properties of the host galaxies of nuclear 22 GHz (lambda = 1.35 cm) water masers. To do so, we cross-match the galaxy sample surveyed for water maser emission (123 detections and 3806 non-detections) with the Sloan Digital Sky Survey (SDSS) low-redshift galaxy sample (z < 0.05). Out of 1636 galaxies with SDSS photometry, we identify 48 detections; out of the 1063 galaxies that also have SDSS spectroscopy, we identify 33 detections. We find that maser detection rate is higher at higher optical luminosity (M(B)), larger velocity dispersion (sigma), and higher [O III] lambda 5007 luminosity, with [O III] lambda 5007 being the dominant factor. These detection rates are essentially the result of the correlations of isotropic maser luminosity with all three of these variables. These correlations are natural if maser strength increases with central black hole mass and the level of active galactic nucleus (AGN) activity. We also find that the detection rate is higher in galaxies with higher extinction. Based on these results, we propose that maser surveys seeking to efficiently find masers should rank AGN targets by extinction-corrected [O III] lambda 5007 flux when available. This prioritizationwould improve maser detection efficiency, from an overall similar to 3% without pre-selection to similar to 16% for the strongest intrinsic [O III] lambda 5007 emitters, by a factor of similar to 5.
C1 [Zhu, Guangtun; Zaw, Ingyin; Blanton, Michael R.] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA.
[Zaw, Ingyin] New York Univ Abu Dhabi, New York, NY 10276 USA.
[Greenhill, Lincoln J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Zhu, GT (reprint author), NYU, Ctr Cosmol & Particle Phys, Dept Phys, 4 Washington Pl, New York, NY 10003 USA.
EM gz323@nyu.edu
RI Zhu, Guangtun/C-8552-2012;
OI Zhu, Guangtun/0000-0002-7574-8078
FU NSF [AST-0607701, 06-FLEX06-0030, NNX09AC85G, NNX09AC95G]; Spitzer
[G05-AR-50443]; Alfred P. Sloan Foundation; Participating Institutions;
National Science Foundation; U.S. Department of Energy; National
Aeronautics and Space Administration; Japanese Monbukagakusho; Max
Planck Society; Higher Education Funding Council for England
FX The authors acknowledge funding support from NSF grant AST-0607701, NASA
grants 06-FLEX06-0030, NNX09AC85G, and NNX09AC95G, and Spitzer grant
G05-AR-50443.; 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 72
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 1
PY 2011
VL 742
IS 2
AR 73
DI 10.1088/0004-637X/742/2/73
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 850QM
UT WOS:000297211900013
ER
PT J
AU Schmid, M
Hothorn, T
Maloney, KO
Weller, DE
Potapov, S
AF Schmid, Matthias
Hothorn, Torsten
Maloney, Kelly O.
Weller, Donald E.
Potapov, Sergej
TI Geoadditive regression modeling of stream biological condition
SO ENVIRONMENTAL AND ECOLOGICAL STATISTICS
LA English
DT Article
DE Proportional odds model; Gradient boosting; Geoadditive regression;
Stream biological condition; Maryland Biological Streams Survey
ID VARIABLE SELECTION; BIOTIC INTEGRITY; FISH ASSEMBLAGES; RIVER CONTINUUM;
UNITED-STATES; LAND-COVER; LANDSCAPE; CLASSIFICATION; MARYLAND; HABITAT
AB Indices of biotic integrity have become an established tool to quantify the condition of small non-tidal streams and their watersheds. To investigate the effects of watershed characteristics on stream biological condition, we present a new technique for regressing IBIs on watershed-specific explanatory variables. Since IBIs are typically evaluated on an ordinal scale, our method is based on the proportional odds model for ordinal outcomes. To avoid overfitting, we do not use classical maximum likelihood estimation but a component-wise functional gradient boosting approach. Because component-wise gradient boosting has an intrinsic mechanism for variable selection and model choice, determinants of biotic integrity can be identified. In addition, the method offers a relatively simple way to account for spatial correlation in ecological data. An analysis of the Maryland Biological Streams Survey shows that nonlinear effects of predictor variables on stream condition can be quantified while, in addition, accurate predictions of biological condition at unsurveyed locations are obtained.
C1 [Schmid, Matthias; Potapov, Sergej] Univ Erlangen Nurnberg, Inst Med Informat Biometrie & Epidemiol, D-91054 Erlangen, Germany.
[Hothorn, Torsten] Univ Munich, Inst Stat, D-80539 Munich, Germany.
[Maloney, Kelly O.; Weller, Donald E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Schmid, M (reprint author), Univ Erlangen Nurnberg, Inst Med Informat Biometrie & Epidemiol, Waldstr 6, D-91054 Erlangen, Germany.
EM matthias.schmid@imbe.med.uni-erlangen.de
RI Hothorn, Torsten/A-3639-2010;
OI Hothorn, Torsten/0000-0001-8301-0471; Weller, Donald/0000-0002-7629-5437
FU Deutsche Forschungsgemeinschaft (DFG) [HO 3242/1-3]; Interdisciplinary
Center for Clinical Research (IZKF) at the University Hospital of the
University of Erlangen-Nuremberg [J11]; Smithsonian Institution; US
Environmental Protection Agency National Center for Environmental
Research (NCER) Science [R831369]
FX The work of Matthias Schmid and Torsten Hothorn was supported by
Deutsche Forschungsgemeinschaft (DFG), grant HO 3242/1-3, and by the
Interdisciplinary Center for Clinical Research (IZKF) at the University
Hospital of the University of Erlangen-Nuremberg (Project J11). We thank
the Maryland Department of Natural Resources for providing data from
their Maryland Biological Stream Survey (MBSS). Funding for this project
was provided by a Smithsonian Institution Post-Doctoral Fellowship
awarded to KOM and by the US Environmental Protection Agency National
Center for Environmental Research (NCER) Science to Achieve Results
(STAR), grant #R831369. We thank the editor and two anonymous reviewers
for helpful comments and suggestions.
NR 60
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PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1352-8505
J9 ENVIRON ECOL STAT
JI Environ. Ecol. Stat.
PD DEC
PY 2011
VL 18
IS 4
BP 709
EP 733
DI 10.1007/s10651-010-0158-4
PG 25
WC Environmental Sciences; Mathematics, Interdisciplinary Applications;
Statistics & Probability
SC Environmental Sciences & Ecology; Mathematics
GA 852IK
UT WOS:000297351000007
ER
PT J
AU Hassler, SK
Lark, RM
Milne, AE
Elsenbeer, H
AF Hassler, S. K.
Lark, R. M.
Milne, A. E.
Elsenbeer, H.
TI Exploring the variation in soil saturated hydraulic conductivity under a
tropical rainforest using the wavelet transform
SO EUROPEAN JOURNAL OF SOIL SCIENCE
LA English
DT Article
ID PEDOTRANSFER FUNCTIONS; SPATIAL VARIABILITY; RETENTION; DEGRADATION;
MANAGEMENT; INFERENCE
AB Saturated hydraulic conductivity (Ks) of the soil is a key variable in the water cycle. For the humid tropics, information about spatial scales of Ks and their relation to soil types deduced from soil map units is of interest, as soil maps are often the only available data source for modelling. We examined the influence of soil map units on the mean and variation in Ks along a transect in a tropical rainforest using undisturbed soil cores at 06 and 612 cm depth. The Ks means were estimated with a linear mixed model fitted by residual maximum likelihood (REML), and the spatial variation in Ks was investigated with the maximum overlap discrete wavelet packet transform (MODWPT). The mean values of Ks did not differ between soil map units. The best wavelet packet basis for Ks at 06 cm showed stationarity at high frequencies, suggesting uniform small-scale influences such as bioturbation. There were substantial contributions to wavelet packet variance over the range of spatial frequencies and a pronounced low frequency peak corresponding approximately to the scale of soil map units. However, in the relevant frequency intervals no significant changes in wavelet packet variance were detected. We conclude that near-surface Ks is not dominated by static, soil-inherent properties for the examined range of soils. Several indicators from the wavelet packet analysis hint at the more dominant dynamic influence of biotic processes, which should be kept in mind when modelling soil hydraulic properties on the basis of soil maps.
C1 [Hassler, S. K.; Elsenbeer, H.] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany.
[Lark, R. M.; Milne, A. E.] Rothamsted Res, Harpenden AL5 2JQ, Herts, England.
[Elsenbeer, H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Hassler, SK (reprint author), Univ Potsdam, Inst Earth & Environm Sci, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany.
EM sibylle.hassler@uni-potsdam.de
RI Lark, Richard/G-6744-2012; Hassler, Sibylle/N-6342-2013;
OI Lark, Richard/0000-0003-2571-8521; Hassler, Sibylle/0000-0001-5411-8491;
Milne, Alice/0000-0002-4509-0578
FU DAAD (German Academic Exchange Service); Panama Canal Authority (ACP);
National Environmental Authority of Panama (ANAM); Smithsonian Tropical
Research Institute (STRI); HSBC; STRI; ACP; Frank Levinson family
foundation; Motta family foundation; Biotechnology and Biological
Sciences Research Council (BBSRC)
FX Sibylle Hassler was partially supported by the DAAD (German Academic
Exchange Service) and by the Agua Salud Project (ASP), which is a
collaboration of the Panama Canal Authority (ACP), the National
Environmental Authority of Panama (ANAM) and the Smithsonian Tropical
Research Institute (STRI). The ASP is financially supported by the HSBC
climate partnership, with additional funding from STRI, ACP, the Frank
Levinson family foundation, and the Motta family foundation. The
contributions of Murray Lark and Alice Milne were funded under
Rothamsted Research's programme in Computational and Mathematical
Biology, which is funded by the Biotechnology and Biological Sciences
Research Council (BBSRC).
NR 39
TC 7
Z9 7
U1 0
U2 18
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1351-0754
J9 EUR J SOIL SCI
JI Eur. J. Soil Sci.
PD DEC
PY 2011
VL 62
IS 6
BP 891
EP 901
DI 10.1111/j.1365-2389.2011.01400.x
PG 11
WC Soil Science
SC Agriculture
GA 850OX
UT WOS:000297206100011
ER
PT J
AU Benedict, GF
McArthur, BE
Feast, MW
Barnes, TG
Harrison, TE
Bean, JL
Menzies, JW
Chaboyer, B
Fossati, L
Nesvacil, N
Smith, HA
Kolenberg, K
Laney, CD
Kochukhov, O
Nelan, EP
Shulyak, DV
Taylor, D
Freedman, WL
AF Benedict, G. Fritz
McArthur, Barbara E.
Feast, Michael W.
Barnes, Thomas G.
Harrison, Thomas E.
Bean, Jacob L.
Menzies, John W.
Chaboyer, Brian
Fossati, Luca
Nesvacil, Nicole
Smith, Horace A.
Kolenberg, Katrien
Laney, C. D.
Kochukhov, Oleg
Nelan, Edmund P.
Shulyak, D. V.
Taylor, Denise
Freedman, Wendy L.
TI DISTANCE SCALE ZERO POINTS FROM GALACTIC RR LYRAE STAR PARALLAXES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE astrometry; stars: distances; stars: variables: RR Lyrae
ID HUBBLE-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; PERIOD-LUMINOSITY
RELATIONS; GLOBULAR-CLUSTER DISTANCES; HORIZONTAL-BRANCH STARS;
VARIABLE-STARS; TRIGONOMETRIC PARALLAXES; HIPPARCOS-PARALLAXES; ABSOLUTE
MAGNITUDE; PROPER MOTIONS
AB We present new absolute trigonometric parallaxes and proper motions for seven Population II variable stars-five RR Lyr variables: RZ Cep, XZ Cyg, SU Dra, RR Lyr, and UV Oct; and two type 2 Cepheids: VY Pyx and kappa Pav. We obtained these results with astrometric data from Fine Guidance Sensors, white-light interferometers on Hubble Space Telescope. We find absolute parallaxes in milliseconds of arc: RZ Cep, 2.12 +/- 0.16 mas; XZ Cyg, 1.67 +/- 0.17 mas; SU Dra, 1.42 +/- 0.16 mas; RR Lyr, 3.77 +/- 0.13 mas; UV Oct, 1.71 +/- 0.10 mas; VY Pyx, 6.44 +/- 0.23 mas; and. Pav, 5.57 +/- 0.28 mas; an average sigma(pi)/pi = 5.4%. With these parallaxes, we compute absolute magnitudes in V and K bandpasses corrected for interstellar extinction and Lutz-Kelker-Hanson bias. Using these RR Lyrae variable star absolute magnitudes, we then derive zero points for M-V-[Fe/H] and M-K-[Fe/H]-log P relations. The technique of reduced parallaxes corroborates these results. We employ our new results to determine distances and ages of several Galactic globular clusters and the distance of the Large Magellanic Cloud. The latter is close to that previously derived from Classical Cepheids uncorrected for any metallicity effect, indicating that any such effect is small. We also discuss the somewhat puzzling results obtained for our two type 2 Cepheids.
C1 [Benedict, G. Fritz; McArthur, Barbara E.; Barnes, Thomas G.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Feast, Michael W.] Univ Cape Town, Dept Astron, Ctr Astrophys Cosmol & Gravitat, ZA-7701 Rondebosch, South Africa.
[Feast, Michael W.; Menzies, John W.; Laney, C. D.] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Harrison, Thomas E.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
[Bean, Jacob L.; Kolenberg, Katrien] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chaboyer, Brian] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Fossati, Luca] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Nesvacil, Nicole; Kolenberg, Katrien] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Nesvacil, Nicole] Med Univ Vienna, Dept Radiotherapy, A-1090 Vienna, Austria.
[Smith, Horace A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Laney, C. D.] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA.
[Kochukhov, Oleg] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Nelan, Edmund P.; Taylor, Denise] STScI, Baltimore, MD 21218 USA.
[Shulyak, D. V.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Freedman, Wendy L.] Carnegie Inst Washington, Pasadena, CA 91101 USA.
RP Benedict, GF (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
OI Chaboyer, Brian/0000-0003-3096-4161; Nesvacil,
Nicole/0000-0002-7920-7754
FU NASA from the Space Telescope Science Institute [GO-11211, GO-11789];
NASA [NAS5-26555]; NSF; NASA's Astrophysics Data System Abstract
Service; STFC; Knut and Alice Wallenberg Foundation; Swedish Research
Council; Deutsche Forschungsgemeinschaft (DFG) [RE1664/7-1]; Austrian
FWF [T359, P19962]; National Research Foundation (NRF) of South Africa
FX Support for this work was provided by NASA through grants GO-11211 and
GO-11789 from the Space Telescope Science Institute, which is operated
by AURA, Inc., under NASA contract NAS5-26555. This paper uses
observations made at the SAAO, and observations obtained with the Apache
Point Observatory 3.5-meter telescope, which is owned and operated by
the Astrophysical Research Consortium. This paper uses observations made
at the Cerro Tololo Observatory 4 m telescope. Cerro Tololo is also
operated by AURA. T. E. H. thanks the SMARTS crew for obtaining
photometry of the VY Pyx and UV Oct fields after three weathered-out
failed attempts by T. E. H. This publication makes use of data products
from the Two Micron All Sky Survey, which is a joint project of the
University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by NASA and the NSF.
This research has made use of the SIMBAD database, operated at CDS,
Strasbourg, France; the NASA/IPAC Extragalactic Database (NED), which is
operated by JPL, California Institute of Technology, under contract with
the NASA; and NASA's Astrophysics Data System Abstract Service. This
material is based in part upon work by T. G. B. while serving at the
National Science Foundation. 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.
This work is supported by an STFC Rolling Grant (L. F.). O.K. is a Royal
Swedish Academy of Sciences Research Fellow supported by grants from the
Knut and Alice Wallenberg Foundation and the Swedish Research Council.
D. S. acknowledges support received from the Deutsche
Forschungsgemeinschaft (DFG) Research Grant RE1664/7-1. K. K., L. F.,
and N.N. are supported by Austrian FWF grants T359 and P19962. M. W. F.
and J.W.M. thank the National Research Foundation (NRF) of South Africa
for financial support. G. F. B. thanks Debbie Winegarten, whose able
assistance with other matters freed me to devote necessary time to this
project. Finally, we thank an anonymous referee for careful reading and
extensive constructive criticism that materially improved the
presentation and discussion.
NR 107
TC 51
Z9 51
U1 0
U2 4
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 DEC
PY 2011
VL 142
IS 6
AR 187
DI 10.1088/0004-6256/142/6/187
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 851FT
UT WOS:000297254500009
ER
PT J
AU Brodie, JP
Romanowsky, AJ
Strader, J
Forbes, DA
AF Brodie, Jean P.
Romanowsky, Aaron J.
Strader, Jay
Forbes, Duncan A.
TI THE RELATIONSHIPS AMONG COMPACT STELLAR SYSTEMS: A FRESH VIEW OF
ULTRACOMPACT DWARFS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: individual (M87); galaxies: nuclei; galaxies:
star clusters: general; galaxies: structure; globular clusters: general
ID GLOBULAR-CLUSTER SYSTEM; HUBBLE-SPACE-TELESCOPE; EARLY-TYPE GALAXIES;
EXTENDED STAR-CLUSTERS; OUTER GALACTIC HALO; FORNAX CLUSTER;
VIRGO-CLUSTER; NGC 5128; DARK-MATTER; ELLIPTIC GALAXIES
AB We use a combined imaging and spectroscopic survey of the nearby central cluster galaxy, M87, to assemble a sample of 34 confirmed ultracompact dwarfs (UCDs) with half-light radii of greater than or similar to 10 pc measured from Hubble Space Telescope images. This doubles the existing sample in M87, making it the largest such sample for any galaxy, while extending the detection of UCDs to unprecedentedly low luminosities (M-V = -9). With this expanded sample, we find no correlation between size and luminosity, in contrast to previous suggestions, and no general correlation between size and galactocentric distance. We explore the relationships between UCDs, less luminous extended clusters (including faint fuzzies), globular clusters (GCs), as well as early-type galaxies and their nuclei, assembling an extensive new catalog of sizes and luminosities for stellar systems. Most of the M87 UCDs follow a tight color-magnitude relation, offset from the metal-poor GCs. This, along with kinematical differences, demonstrates that most UCDs are a distinct population from normal GCs, and not simply a continuation to larger sizes and higher luminosities. The UCD color-magnitude trend couples closely with that for Virgo dwarf elliptical nuclei. We conclude that the M87 UCDs are predominantly stripped nuclei. The brightest and reddest UCDs may be the remnant nuclei of more massive galaxies while a subset of the faintest UCDs may be tidally limited and related to more compact star clusters. In the broader context of galaxy assembly, blue UCDs may trace halo build-up by accretion of low-mass satellites, while red UCDs may be markers of metal-rich bulge formation in larger galaxies.
C1 [Brodie, Jean P.; Romanowsky, Aaron J.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Forbes, Duncan A.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
RP Brodie, JP (reprint author), Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
EM brodie@ucolick.org
FU Smithsonian Astrophysical Observatory; National Science Foundation
[AST-0808099, AST-0909237, AST-1101733, AST-1109878]; Australian
Government's innovation statement, Backing Australia's Ability
FX We thank Kristin Chiboucas, Soren Larsen, Juan Madrid, and Ingo Misgeld
for providing their data in electronic form; Holger Baumgardt, Kenji
Bekki, Mark Gieles, Sheila Kannappan, Pavel Kroupa, and Mark Norris for
helpful conversations; and an anonymous referee for constructive
suggestions. Some of the observations reported here were obtained at the
MMT Observatory, a joint facility of the Smithsonian Institution and the
University of Arizona. This paper uses data products produced by the OIR
Telescope Data Center, supported by the Smithsonian Astrophysical
Observatory. Much of the data presented herein were obtained at the W.
M. Keck Observatory, which is operated as a scientific partnership among
the California Institute of Technology, the University of California and
the National Aeronautics and Space Administration. Based on observations
made with the NASA/ESA Hubble Space Telescope, and obtained from the
Hubble Legacy Archive, which is a collaboration between the Space
Telescope Science Institute (STScI/NASA), the Space Telescope European
Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data
Centre (CADC/NRC/CSA). This work was supported by the National Science
Foundation through grants AST-0808099, AST-0909237, AST-1101733, and
AST-1109878. We acknowledge financial support from the Access to Major
Research Facilities Programme, a component of the International Science
Linkages Programme established under the Australian Government's
innovation statement, Backing Australia's Ability.
NR 150
TC 83
Z9 83
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 DEC
PY 2011
VL 142
IS 6
AR 199
DI 10.1088/0004-6256/142/6/199
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 851FT
UT WOS:000297254500021
ER
PT J
AU Chomiuk, L
Povich, MS
AF Chomiuk, Laura
Povich, Matthew S.
TI TOWARD A UNIFICATION OF STAR FORMATION RATE DETERMINATIONS IN THE MILKY
WAY AND OTHER GALAXIES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: star formation; Galaxy: fundamental parameters; H II regions;
ISM: supernova remnants
ID INITIAL MASS FUNCTION; SPECTRAL ENERGY-DISTRIBUTION; FORMATION RATE
INDICATOR; YOUNG STELLAR OBJECTS; X-RAY BINARIES; M-CIRCLE-DOT;
SUPERNOVA-REMNANTS; LUMINOSITY FUNCTION; FORMING GALAXIES; FORMATION
HISTORY
AB The star formation rate (SFR) of the Milky Way remains poorly known, with often-quoted values ranging from 1 to 10 M-circle dot yr(-1). This situation persists despite the potential for the Milky Way to serve as the ultimate SFR calibrator for external galaxies. We show that various estimates for the Galactic SFR are consistent with one another once they have been normalized to the same initial mass function (IMF) and massive star models, converging to 1.9 +/- 0.4 M-circle dot yr(-1). However, standard SFR diagnostics are vulnerable to systematics founded in the use of indirect observational tracers sensitive only to high-mass stars. We find that absolute SFRs measured using resolved low/intermediate-mass stellar populations in Galactic H II regions are systematically higher by factors of similar to 2-3 compared with calibrations for SFRs measured from mid-IR and radio emission. We discuss some potential explanations for this discrepancy and conclude that it could be allayed if (1) the power-law slope of the IMF for intermediate-mass (1.5M(circle dot) < m < 5M(circle dot)) stars were steeper than the Salpeter slope or (2) a correction factor was applied to the extragalactic 24 mu m SFR calibrations to account for the duration of star formation in individual mid-IR-bright H II regions relative to the lifetimes of O stars. Finally, we present some approaches for testing whether a Galactic SFR of similar to 2M(circle dot) yr(-1) is consistent with what we would measure if we could view the Milky Way as external observers. Using luminous radio supernova remnants and X-ray point sources, we find that the Milky Way deviates from expectations at the 1 sigma-3 sigma level, hinting that perhaps the Galactic SFR is overestimated or extragalactic SFRs need to be revised upward.
C1 [Chomiuk, Laura] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Chomiuk, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Povich, Matthew S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Chomiuk, L (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
EM lchomiuk@cfa.harvard.edu; povich@astro.psu.edu
FU NSF [AST-0901646, AST-0708002]; Associated Universities, Inc.
FX We thank Ed Churchwell, Dave Green, Leisa Townsley, and Eric Wilcots for
their support and useful insights. We are also grateful to our referee,
Neal J. Evans II, for his improvements to this work. M. S. P. is
supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship
under award AST-0901646. L. C. is a Jansky Fellow of the National Radio
Astronomy Observatory. She is also grateful for the support of NSF grant
AST-0708002. The National Radio Astronomy Observatory is a facility of
the National Science Foundation operated under cooperative agreement by
Associated Universities, Inc.
NR 139
TC 96
Z9 96
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 DEC
PY 2011
VL 142
IS 6
AR 197
DI 10.1088/0004-6256/142/6/197
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 851FT
UT WOS:000297254500019
ER
PT J
AU Nantais, JB
Huchra, JP
Zezas, A
Gazeas, K
Strader, J
AF Nantais, Julie B.
Huchra, John P.
Zezas, Andreas
Gazeas, Kosmas
Strader, Jay
TI HUBBLE SPACE TELESCOPE PHOTOMETRY OF GLOBULAR CLUSTERS IN M81
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M81); galaxies: spiral; galaxies: star clusters:
general; galaxies: stellar content
ID EXTRAGALACTIC DISTANCE SCALE; COMPACT STAR-CLUSTERS; EARLY-TYPE
GALAXIES; SOMBRERO GALAXY; KEY PROJECT; STRUCTURAL PARAMETERS;
LUMINOSITY FUNCTION; SIZE DIFFERENCE; ADVANCED CAMERA; SYSTEMS
AB We perform aperture photometry and profile fitting on 419 globular cluster (GC) candidates with m(V) <= 23 mag identified in Hubble Space Telescope/Advanced Camera for Surveys BVI imaging, and estimate the effective radii of the clusters. We identify 85 previously known spectroscopically confirmed clusters, and newly identify 136 objects as good cluster candidates within the 3 sigma color and size ranges defined by the spectroscopically confirmed clusters, yielding a total of 221 probable GCs. The luminosity function peak for the 221 probable GCs with estimated total dereddening applied is V similar to (20.26 +/- 0.13) mag, corresponding to a distance of similar to 3.7 +/- 0.3 Mpc. The blue and red GC candidates, and the metal-rich and metal-poor spectroscopically confirmed clusters, respectively, are similar in half-light radius. Red confirmed clusters are about 6% larger in median half-light radius than blue confirmed clusters, and red and blue good GC candidates are nearly identical in half-light radius. The total population of confirmed and "good" candidates shows an increase in half-light radius as a function of galactocentric distance.
C1 [Nantais, Julie B.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Huchra, John P.; Zezas, Andreas; Gazeas, Kosmas; Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zezas, Andreas] Univ Crete, Dept Phys, Iraklion, Greece.
[Zezas, Andreas] Fdn Res & Technol, Inst Elect Struct & Laser, Iraklion, Greece.
RP Nantais, JB (reprint author), Univ Concepcion, Dept Astron, Av Esteban Iturra S-N Barrio Univ Casilla 160-C, Concepcion, Chile.
RI Zezas, Andreas/C-7543-2011
OI Zezas, Andreas/0000-0001-8952-676X
FU NASA from the Space Telescope Science Institute [GO-10250, GO-10584];
National Science Foundation [AST 05077229]; NASA from the GALEX
[NNG06GD33G]; Harvard College Observatory; Marie Curie Reintegration
Grant [224878]; Chilean Centro de Excelencia en Astrofisica y
Tecnologias Afines (CATA); [ASTROSPACE 206464]
FX This research was supported by the NASA grants GO-10250 and GO-10584
from the Space Telescope Science Institute, the National Science
Foundation grant AST 05077229, and the NASA grant NNG06GD33G from the
GALEX Guest Observers Program. We also thank the staff of the Harvard
College Observatory for their support. Astrophysics research in Crete is
supported by grant ASTROSPACE 206464. A.Z. acknowledges support from the
Marie Curie Reintegration Grant 224878. J.N. gratefully acknowledges
support from the Chilean Centro de Excelencia en Astrofisica y
Tecnologias Afines (CATA).
NR 56
TC 8
Z9 8
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD DEC
PY 2011
VL 142
IS 6
AR 183
DI 10.1088/0004-6256/142/6/183
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 851FT
UT WOS:000297254500005
ER
PT J
AU Cleveland, CC
Townsend, AR
Taylor, P
Alvarez-Clare, S
Bustamante, MMC
Chuyong, G
Dobrowski, SZ
Grierson, P
Harms, KE
Houlton, BZ
Marklein, A
Parton, W
Porder, S
Reed, SC
Sierra, CA
Silver, WL
Tanner, EVJ
Wieder, WR
AF Cleveland, Cory C.
Townsend, Alan R.
Taylor, Philip
Alvarez-Clare, Silvia
Bustamante, Mercedes M. C.
Chuyong, George
Dobrowski, Solomon Z.
Grierson, Pauline
Harms, Kyle E.
Houlton, Benjamin Z.
Marklein, Alison
Parton, William
Porder, Stephen
Reed, Sasha C.
Sierra, Carlos A.
Silver, Whendee L.
Tanner, Edmund V. J.
Wieder, William R.
TI Relationships among net primary productivity, nutrients and climate in
tropical rain forest: a pan-tropical analysis (vol 14, pg 939, 2011)
SO ECOLOGY LETTERS
LA English
DT Correction
ID MULU-NATIONAL-PARK; SOIL-PHOSPHORUS FRACTIONATION;
LUQUILLO-EXPERIMENTAL-FOREST; LEAF-LITTER DECOMPOSITION; LOWLAND
AMAZONIAN FOREST; HAWAIIAN MONTANE FOREST; BARRO-COLORADO ISLAND; INDIAN
WESTERN GHATS; BRAZILIAN AMAZON; PRECIPITATION GRADIENT
C1 [Cleveland, Cory C.] Univ Montana, Dept Ecosyst & Conservat Sci, Missoula, MT 59812 USA.
[Townsend, Alan R.] Univ Colorado, Dept Ecol & Evolutionary Biol, Environm Studies Program, Boulder, CO 80309 USA.
[Townsend, Alan R.; Taylor, Philip; Wieder, William R.] Univ Colorado, INSTAAR, Boulder, CO 80309 USA.
[Alvarez-Clare, Silvia] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Alvarez-Clare, Silvia] Univ Florida, Sch Nat Resources & Environm, Gainesville, FL 32611 USA.
[Bustamante, Mercedes M. C.] Univ Brasilia, Dept Ecol, Brasilia, DF, Brazil.
[Chuyong, George] Univ Buea, Dept Plant & Anim Sci, Buea, Cameroon.
[Dobrowski, Solomon Z.] Univ Montana, Dept Forest Management, Missoula, MT 59812 USA.
[Grierson, Pauline] Univ Western Australia, Sch Plant Biol M090, Crawley, WA 6016, Australia.
[Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Harms, Kyle E.] Smithsonian Trop Res Inst, Panama City, Panama.
[Houlton, Benjamin Z.; Marklein, Alison] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
[Parton, William] Colorado State Univ, Nat Resource Ecol Lab, Ft Collins, CO 80523 USA.
[Porder, Stephen] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA.
[Reed, Sasha C.] US Geol Survey, SW Biol Sci Ctr, Moab, UT 84532 USA.
[Sierra, Carlos A.] Max Planck Inst Biogeochem, Dept Biol Proc, D-07745 Jena, Germany.
[Silver, Whendee L.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
[Tanner, Edmund V. J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England.
RP Cleveland, CC (reprint author), Univ Montana, Dept Ecosyst & Conservat Sci, Missoula, MT 59812 USA.
EM cory.cleveland@umontana.edu
RI Grierson, Pauline/A-9240-2008; Silver, Whendee/H-1118-2012; Marklein,
Alison/I-3255-2016; Bustamante, Mercedes/H-7597-2015
OI Grierson, Pauline/0000-0003-2135-0272; Marklein,
Alison/0000-0002-0865-5816; Bustamante, Mercedes/0000-0003-1008-452X
NR 157
TC 10
Z9 14
U1 4
U2 65
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1461-023X
J9 ECOL LETT
JI Ecol. Lett.
PD DEC
PY 2011
VL 14
IS 12
BP 1313
EP 1317
DI 10.1111/j.1461-0248.2011.01711.x
PG 5
WC Ecology
SC Environmental Sciences & Ecology
GA 849TG
UT WOS:000297147500014
ER
PT J
AU Diefendorf, AF
Freeman, KH
Wing, SL
Graham, HV
AF Diefendorf, Aaron F.
Freeman, Katherine H.
Wing, Scott L.
Graham, Heather V.
TI Production of n-alkyl lipids in living plants and implications for the
geologic past
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID HYDROGEN ISOTOPIC COMPOSITION; COMPOUND-SPECIFIC DELTA-C-13; EOCENE
THERMAL MAXIMUM; CUTICULAR WAXES; ORGANIC-MATTER; CHEMICAL-COMPOSITION;
CONSTRUCTION COSTS; EPICUTICULAR WAXES; MODERN ANGIOSPERMS; VEGETATION
CHANGE
AB Leaf waxes (i.e., n-alkyl lipids or n-alkanes) are land-plant biomarkers widely used to reconstruct changes in climate and the carbon isotopic composition of the atmosphere. There is little information available, however, on how the production of leaf waxes by different kinds of plants might influence the abundance and isotopic composition of n-alkanes in sedimentary archives. This lack of information increases uncertainty in interpreting n-alkyl lipid abundance and delta(13)C signals in ancient settings. We provide here n-alkyl abundance distributions and carbon isotope fractionation data for deciduous and evergreen angiosperm and gymnosperm leaves from 46 tree species, representing 24 families. n-Alkane abundances are significantly higher in angiosperms than gymnosperms; many of the gymnosperm species investigated did not produce any n-alkanes. On average, deciduous angiosperms produce 200 times more n-alkanes than deciduous gymnosperms. Although differences between angiosperms and gymnosperms dominate the variance in n-alkane abundance, leaf life-span is also important, with higher n-alkane abundances in longer-lived leaves. n-Alkanol abundances covary with n-alkanes, but n-alkanoic acids have similar abundances across all plant groups. Isotopic fractionation between leaf tissue and individual alkanes (epsilon(lipid)) varies by as much as 10 parts per thousand among different chain lengths. Overall, epsilon(lipid) values are slightly lower (-4.5 parts per thousand) for angiosperm than for gymnosperm (-2.5 parts per thousand) n-alkanes. Angiosperms commonly express slightly higher Delta(leaf) (photosynthetic discrimination) relative to gymnosperms under similar growth conditions. As a result, angiosperm n-alkanes are expected to be generally 3-5 parts per thousand more depleted in (13)C relative to gymnosperm alkanes for the same locality. Differences in n-alkane production indicate the biomarker record will largely (but not exclusively) reflect angiosperms if both groups were present, and also that evergreen plants will likely be overrepresented compared with deciduous ones. We apply our modern lipid abundance patterns and epsilon(lipid) results to constrain the magnitude of the carbon isotope excursion (CIE) at the onset of the Paleocene-Eocene Thermal Maximum (55.8 Ma). When Bighorn Basin (WY) sediment n-alkanes are interpreted in context of floral changes and modern n-alkane production estimates for angiosperms and gymnosperms, the CIE is greater in magnitude (similar to 5.6 parts per thousand) by similar to 1 parts per thousand compared to previous estimates that do not take into account n-alkane production. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Diefendorf, Aaron F.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA.
[Freeman, Katherine H.; Graham, Heather V.] 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, POB 210013, Cincinnati, OH 45221 USA.
EM aaron.diefendorf@uc.edu
RI Freeman, Katherine/H-5140-2011;
OI Freeman, Katherine/0000-0002-3350-7671; Wing, Scott/0000-0002-2954-8905
FU National Science Foundation [EAR-0844212, DGE-9972759]; Penn State
Biogeochemical Research Initiative for Education (BRIE)
FX We thank Laurie Eccles for laboratory preparation, Kevin Mueller and
Emily Diefendorf for sample collection assistance, and Denny Walizer for
technical support. We also thank two anonymous reviewers, Rienk
Smittenberg and Associate Editor Josef Werne for their helpful
suggestions. 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 Integrative Graduate Education
and Research Traineeship (IGERT Grant DGE-9972759).
NR 66
TC 73
Z9 75
U1 3
U2 64
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 DEC 1
PY 2011
VL 75
IS 23
BP 7472
EP 7485
DI 10.1016/j.gca.2011.09.028
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 850RE
UT WOS:000297214400006
ER
PT J
AU Miguel, Y
Kaltenegger, L
Fegley, B
Schaefer, L
AF Miguel, Y.
Kaltenegger, L.
Fegley, B., Jr.
Schaefer, L.
TI COMPOSITIONS OF HOT SUPER-EARTH ATMOSPHERES: EXPLORING KEPLER CANDIDATES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrobiology; atmospheric effects; planets and satellites: atmospheres;
planets and satellites: composition
ID THERMODYNAMIC MODEL; GIANT PLANETS; HD 209458B; LOW-ALBEDO;
VAPORIZATION; PHOTOMETRY; EXOPLANETS; OXIDE; IO
AB This paper outlines a simple approach to evaluate the atmospheric composition of hot rocky planets by assuming different types of planetary composition and using corresponding model calculations. To explore hot atmospheres above 1000 K, we model the vaporization of silicate magma and estimate the range of atmospheric compositions according to the planet's radius and semi-major axis for the Kepler 2011 February data release. Our results show five atmospheric types for hot, rocky super-Earth atmospheres, strongly dependent on the initial composition and the planet's distance to the star. We provide a simple set of parameters that can be used to evaluate atmospheric compositions for current and future candidates provided by the Kepler mission and other searches.
C1 [Miguel, Y.; Kaltenegger, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Kaltenegger, L.; Schaefer, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fegley, B., Jr.] Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO 63130 USA.
[Fegley, B., Jr.] Washington Univ, Mc Donnell Ctr Space Sci, St Louis, MO 63130 USA.
RP Miguel, Y (reprint author), Max Planck Inst Astron, Koenigstuhl 17, D-69117 Heidelberg, Germany.
EM miguel@mpia-hd.mpg.de
FU DFG [ENP Ka 3142/1-1]
FX We are grateful to Wade Henning, Dimitar Sasselov, and Tilman Spohn for
stimulating discussions. Y.M. and L. K. acknowledge DFG funding ENP Ka
3142/1-1.
NR 31
TC 20
Z9 20
U1 1
U2 14
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 DEC 1
PY 2011
VL 742
IS 2
AR L19
DI 10.1088/2041-8205/742/2/L19
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846SY
UT WOS:000296924700003
ER
PT J
AU Hintz, ES
AF Hintz, Eric S.
TI The Post-Heroic Generation: American Independent Inventors, 1900-1950
SO ENTERPRISE & SOCIETY
LA English
DT Article
ID HISTORY
AB By World War I, the public (and later, many historians) had come to believe that teams of anonymous scientists in corporate research and development (R&D) laboratories had displaced "heroic" individual inventors like Thomas Edison and Alexander Graham Bell as the wellspring of innovation. However, the first half of the twentieth century was actually a long transitional period when lesser known independents like Chester Carlson (Xerox copier), Earl Tupper (Tupperware), Samuel Ruben (Duracell batteries), and Edwin Land (Polaroid camera) continued to make notable contributions to the overall context of innovation. Accordingly, my dissertation considers the changing fortunes of American independent inventors from approximately 1900 to 1950, a period of expanding corporate R&D, the Great Depression, and two world wars. Contrary to most interpretations of this period, I argue that individual, "post-heroic" inventors remained an important, though less visible, source of inventions in the early twentieth century.
C1 Natl Museum Amer Hist, Lemelson Ctr, Washington, DC 20013 USA.
[Hintz, Eric S.] Smithsonian Inst, Natl Museum Amer Hist, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA.
RP Hintz, ES (reprint author), Natl Museum Amer Hist, Lemelson Ctr, POB 37012,MRC 604, Washington, DC 20013 USA.
EM hintze@si.edu
NR 46
TC 1
Z9 1
U1 1
U2 12
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1467-2227
J9 ENTERP SOC
JI Enterp. Soc
PD DEC
PY 2011
VL 12
IS 4
BP 732
EP 748
DI 10.1093/es/khr039
PG 17
WC Business; History Of Social Sciences
SC Business & Economics; Social Sciences - Other Topics
GA 838US
UT WOS:000296318400003
ER
PT J
AU Marten-Rodriguez, S
Kress, WJ
Temeles, EJ
Melendez-Ackerman, E
AF Marten-Rodriguez, Silvana
Kress, W. John
Temeles, Ethan J.
Melendez-Ackerman, Elvia
TI Plant-pollinator interactions and floral convergence in two species of
Heliconia from the Caribbean Islands
SO OECOLOGIA
LA English
DT Article
DE Convergent evolution; Heliconia; Hummingbird; Islands; Pollination
ID TROPICAL HUMMINGBIRD; ECOLOGICAL CAUSATION; SEXUAL-DIMORPHISM;
ADAPTATION; POPULATIONS; EVOLUTION; SHAPE; SIZE
AB Variation in interspecific interactions across geographic space is a potential driver of diversification and local adaptation. This study quantitatively examined variation in floral phenotypes and pollinator service of Heliconia bihai and H. caribaea across three Antillean islands. The prediction was that floral characters would correspond to the major pollinators of these species on each island. Analysis of floral phenotypes revealed convergence among species and populations of Heliconia from the Greater Antilles. All populations of H. caribaea were similar, characterized by long nectar chambers and short corolla tubes. In contrast, H. bihai populations were strongly divergent: on Dominica, H. bihai had flowers with short nectar chambers and long corollas, whereas on Hispaniola, H. bihai flowers resembled those of H. caribaea with longer nectar chambers and shorter corolla tubes. Morphological variation in floral traits corresponded with geographic differences or similarities in the major pollinators on each island. The Hispaniolan mango, Anthracothorax dominicus, is the principal pollinator of both H. bihai and H. caribaea on Hispaniola; thus, the similarity of floral phenotypes between Heliconia species suggests parallel selective regimes imposed by the principal pollinator. Likewise, divergence between H. bihai populations from Dominica and Hispaniola corresponded with differences in the pollinators visiting this species on the two islands. The study highlights the putative importance of pollinator-mediated selection as driving floral convergence and the evolution of locally-adapted plant variants across a geographic mosaic of pollinator species.
C1 [Marten-Rodriguez, Silvana; Kress, W. John] Natl Museum Nat Hist, Dept Bot, MRC 166, Smithsonian Inst, Washington, DC 20013 USA.
[Temeles, Ethan J.] Amherst Coll, Dept Biol, Amherst, MA 01002 USA.
[Melendez-Ackerman, Elvia] Univ Puerto Rico Rio Piedras, Inst Trop Ecosyst Studies, San Juan, PR 00936 USA.
RP Marten-Rodriguez, S (reprint author), Inst Ecol, Dept Biol Evolutiva, AC Ap Postal 63, Xalapa 91070, Veracruz, Mexico.
EM smartenr@gmail.com
FU Depto de Recursos Naturales y Ambientales in Puerto Rico; Secretaria de
Estado de Medio Ambiente y Recursos Naturales in the Dominican Republic;
Smithsonian Institution; NSF [DEB 0614218]
FX The authors thank T. Clase, A. Cherenfant, J. Fumero, N. Marten, B.
Peguero, R. Perez, R. Rodriguez, N. Ruiz and M. Vindas for assistance
conducting field work. The authors thank P. Acevedo for discussion of
ideas and providing useful botanical information, and I. Lopez for
generating the distribution map. V. Gowda, S. Johnson, and three
anonymous reviewers provided insightful comments on earlier versions of
this manuscript. Logistic support for fieldwork was provided by Jardin
Botanico Nacional de Santo Domingo in Dominican Republic, and El Verde
Field Station in Puerto Rico. Research permits were awarded by Depto de
Recursos Naturales y Ambientales in Puerto Rico, and by the Secretaria
de Estado de Medio Ambiente y Recursos Naturales in the Dominican
Republic, and experiments complied with the current laws of those
countries. Funding was provided by Smithsonian Institution grant to SMR,
NSF Grant DEB 0614218 to E. Temeles and W.J. Kress.
NR 37
TC 9
Z9 9
U1 3
U2 43
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD DEC
PY 2011
VL 167
IS 4
BP 1075
EP 1083
DI 10.1007/s00442-011-2043-8
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 849OB
UT WOS:000297133800019
PM 21792557
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI New Angles
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 DEC
PY 2011
VL 42
IS 8
BP 30
EP 30
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 850WS
UT WOS:000297230900012
ER
PT J
AU Lasso, E
Dalling, JW
Bermingham, E
AF Lasso, E.
Dalling, J. W.
Bermingham, E.
TI Strong spatial genetic structure in five tropical Piper species: should
the Baker-Fedorov hypothesis be revived for tropical shrubs?
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE AFLP; Barro Colorado Island; Clonal reproduction; Gene flow; Piperaceae
ID FRAGMENT LENGTH POLYMORPHISM; RAIN-FOREST TREES; SEED DISPERSAL; POLLEN
DISPERSAL; NEOTROPICAL TREE; BREEDING SYSTEMS; LATITUDINAL GRADIENTS;
POPULATION-STRUCTURE; MOLECULAR EVOLUTION; NATURAL-POPULATIONS
AB Fifty years ago, Baker and Fedorov proposed that the high species diversity of tropical forests could arise from the combined effects of inbreeding and genetic drift leading to population differentiation and eventually to sympatric speciation. Decades of research, however have failed to support the Baker-Fedorov hypothesis (BFH), and it has now been discarded in favor of a paradigm where most trees are self-incompatible or strongly outcrossing, and where long-distance pollen dispersal prevents population drift. Here, we propose that several hyper-diverse genera of tropical herbs and shrubs, including Piper (>1,000 species), may provide an exception. Species in this genus often have aggregated, high-density populations with self-compatible breeding systems; characteristics which the BFH would predict lead to high local genetic differentiation. We test this prediction for five Piper species on Barro Colorado Island, Panama, using Amplified Fragment Length Polymorphism (AFLP) markers. All species showed strong genetic structure at both fine- and large-spatial scales. Over short distances (200-750 m) populations showed significant genetic differentiation (Fst 0.11-0.46, P < 0.05), with values of spatial genetic structure that exceed those reported for other tropical tree species (Sp = 0.03-0.136). This genetic structure probably results from the combined effects of limited seed and pollen dispersal, clonal spread, and selfing. These processes are likely to have facilitated the diversification of populations in response to local natural selection or genetic drift and may explain the remarkable diversity of this rich genus.
C1 [Lasso, E.; Dalling, J. W.; Bermingham, E.] Smithsonian Trop Res Inst, Panama City, Panama.
[Lasso, E.] Univ Los Andes, Dept Ciencias Biol, Bogota 4976, Colombia.
[Dalling, J. W.] Univ Illinois, Urbana, IL 61801 USA.
RP Lasso, E (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama.
EM lassoe@si.edu
OI Lasso, Eloisa/0000-0003-4586-8674
FU STRI; NSF [DEB 05-08471]; University of Illinois; SENACYT-IFARHU
FX We thank F. Jones for revising earlier draft of this manuscript. Thanks
to O. Sanjur, M. Gonzales, G. Grajales, R. Reina and C. Vergara for all
their support and help in the lab, and to D. Kikuchi for help with
fieldwork. Financial support for this work came from a STRI short-term
and a predoctoral fellowship, a dissertation Improvement Grant-NSF
(grant DEB 05-08471), the Francis M. and Harlie M. Clark Research
Support Grant from University of Illinois, and a SENACYT-IFARHU doctoral
fellowship.
NR 105
TC 10
Z9 10
U1 0
U2 22
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD DEC
PY 2011
VL 1
IS 4
DI 10.1002/ece3.40
PG 15
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA 055TV
UT WOS:000312441500006
PM 22393518
ER
PT J
AU Hartke, TR
Koenemann, S
Yager, J
AF Hartke, Tamara R.
Koenemann, Stefan
Yager, Jill
TI Speleonectes williamsi, a new species of Remipedia (Crustacea) from the
Bahamas
SO ZOOTAXA
LA English
DT Article
DE remipede; cryptic species; pseudo-cryptic species; glands;
Speleonectidae
ID TURKS-AND-CAICOS; ANCHIALINE CAVES; GENUS
AB We describe a new species of the genus Speleonectes (Crustacea, Remipedia, Nectiopoda) from an anchialine cave on Grand Bahama Island in the northern Bahamas. Speleonectes williamsi n. sp. is morphologically highly similar to Speleonectes emersoni from the Dominican Republic. However, morphological differences between the two species were detected in dissected body parts, such as the setal patterns of the antennae and trunk limbs, the terminal claws of maxillae and maxillipeds, and the frontal filaments.
C1 [Hartke, Tamara R.] Univ Vet Med Hannover, Inst Anim Ecol & Cell Biol, D-30559 Hannover, Germany.
[Hartke, Tamara R.] Northeastern Univ, Dept Biol, Boston, MA 02115 USA.
[Koenemann, Stefan] Univ Siegen, Sect Biol Sci & Technol, D-57068 Siegen, Germany.
[Yager, Jill] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
RP Hartke, TR (reprint author), Univ Vet Med Hannover, Inst Anim Ecol & Cell Biol, Bunteweg 17D, D-30559 Hannover, Germany.
EM trhartke@gmail.com; koene-mann@biologie.uni-siegen.de;
jill.yager@gmail.com
RI Hartke, Tamara/I-2579-2013
OI Hartke, Tamara/0000-0002-5422-5251
FU German Research Foundation [DFG KO 3483/1]
FX We thank Jan Mohr for drawings and a first morphological description of
the new species in German, and Scott Whittaker of the Scanning Electron
Microscopy Lab and the staff in Lab 5 of the Museum Support Center at
NMNH, Smithsonian. This study was supported by a grant from the German
Research Foundation to S. Koenemann (DFG KO 3483/1).
NR 11
TC 2
Z9 2
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 DEC 1
PY 2011
IS 3115
BP 21
EP 28
PG 8
WC Zoology
SC Zoology
GA 861TV
UT WOS:000298043000002
ER
PT J
AU Andrews, BJ
Manga, M
AF Andrews, Benjamin J.
Manga, Michael
TI Effects of topography on pyroclastic density current runout and
formation of coignimbrites
SO GEOLOGY
LA English
DT Article
ID ASH FLOWS; IGNIMBRITE; TRANSPORT; VOLCANO; ALASKA; THERMODYNAMICS;
EMPLACEMENT; DEPOSITION; DYNAMICS; MOBILITY
AB Laboratory experiments of dilute mixtures of warm talc powder in air simulate dilute pyroclastic density currents (PDCs) and show the effects of topography on current runout, buoyancy reversal, and liftoff into buoyant plumes. The densimetric and thermal Richardson, Froude, Stokes, and settling numbers for our experiments match those of natural PDCs. The laboratory currents are fully turbulent, although the experiments have lower Reynolds numbers than PDCs. In sum, our experiments are dynamically similar to natural currents. Comparisons of currents traversing flat topography or encountering barriers show that runout distance is not significantly reduced for currents that traverse barriers with height <1.5 times the current thickness, but currents do not pass taller barriers. Buoyancy reversals occur in most currents, resulting in liftoff and generation of a buoyant plume. Liftoff occurs near the maximum runout distance for currents traveling over flat topography, but is focused near or above barriers for currents that encounter barriers. Notably, plume formation above barriers can result in reversal of flow direction downstream of the obstruction as portions of the current flow back and feed the rising plume.
C1 [Andrews, Benjamin J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20004 USA.
[Manga, Michael] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
RP Andrews, BJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 1000 Constitut Ave NW, Washington, DC 20004 USA.
RI Manga, Michael/D-3847-2013;
OI Manga, Michael/0000-0003-3286-4682
FU National Science Foundation (NSF) [EAR-0847366, EAR-080954]
FX William Gange provided assistance running many experiments. Stuart
Foster helped build the experimental apparatus. Bill Dietrich and
Leonard Sklar provided space at the Richmond Field Station. Andrews was
supported by a National Science Foundation (NSF) Earth Sciences
Postdoctoral Fellowship (EAR-0847366). Manga was supported by NSF grant
EAR-080954. Thoughtful comments by G. Valentine, A. Burgisser, and one
anonymous reviewer helped improve this paper.
NR 17
TC 21
Z9 21
U1 0
U2 14
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD DEC
PY 2011
VL 39
IS 12
BP 1099
EP 1102
DI 10.1130/G32226.1
PG 4
WC Geology
SC Geology
GA 844ZZ
UT WOS:000296793900003
ER
PT J
AU Villeneuve, PJ
Goldberg, MS
Burnett, RT
van Donkelaar, A
Chen, H
Martin, RV
AF Villeneuve, Paul J.
Goldberg, Mark S.
Burnett, Richard T.
van Donkelaar, Aaron
Chen, Hong
Martin, Randall V.
TI Associations between cigarette smoking, obesity, sociodemographic
characteristics and remote-sensing-derived estimates of ambient PM2.5:
results from a Canadian population-based survey
SO OCCUPATIONAL AND ENVIRONMENTAL MEDICINE
LA English
DT Article
ID PARTICULATE AIR-POLLUTION; LONG-TERM EXPOSURE; NITROGEN-DIOXIDE;
NORWEGIAN MEN; UNITED-STATES; LUNG-CANCER; LOS-ANGELES; MORTALITY;
POLLUTANTS; DISEASE
AB Objectives Long-term exposure to ambient fine particles (PM2.5) has been shown to increase mortality. Variables measured on the same spatial scales of air pollution may confound associations, and so the authors' objectives were to evaluate the associations between PM2.5 and individual-level measures of smoking, obesity and sociodemographic status. The authors present an approach to evaluate the impact that uncontrolled confounding from smoking may have on associations between PM2.5 and mortality.
Methods Individual-level behavioural and sociodemographic data were obtained from a 2003 national survey of 122 548 Canadians. Estimates of ground-level PM2.5 at a resolution of 10 x 10 km between 2001 and 2006 were derived from satellite remote sensing. Exposures were assigned to the residence of the participants at the time of the survey. Differences in the prevalence of smoking across concentrations of PM2.5 and RRs drawn from the literature were used to model the bias on rate ratios.
Results Participants in areas with higher concentrations of PM2.5 had a higher income and educational attainment, smoked less and were more likely immigrants. Smoking had a negative confounding effect on the associations between PM2.5 and mortality. To compensate for this bias, for a 10 mu g/m(3) increase in PM2.5, mortality from lung cancer and heart disease in the referent exposure group needed to be increased by 6.9% and 3.2%, respectively.
Conclusions Associations were found between sociodemographic and lifestyle characteristics and PM2.5 at a resolution of 10 x 10 km. The authors present a model to adjust for uncontrolled confounding of smoking that can be readily adapted to exposures measured at different spatial resolutions.
C1 [Villeneuve, Paul J.; Burnett, Richard T.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0K9, Canada.
[Villeneuve, Paul J.] Univ Toronto, Dalla Lana Sch Publ Hlth, Div Occupat & Environm Hlth, Toronto, ON, Canada.
[Goldberg, Mark S.] McGill Univ, Dept Med, Montreal, PQ, Canada.
[Goldberg, Mark S.] McGill Univ, Ctr Hlth, Res Inst, Div Clin Epidemiol, Montreal, PQ, Canada.
[van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Chen, Hong] McGill Univ, Dept Epidemiol & Biostat, Montreal, PQ, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Villeneuve, PJ (reprint author), Hlth Canada, Populat Studies Div, 50 Columbine Driveway,Room 165,PL0801A, Ottawa, ON K1A 0K9, Canada.
EM paul_villeneuve@hc-sc.gc.ca
RI Martin, Randall/C-1205-2014
OI Martin, Randall/0000-0003-2632-8402
FU Health Canada
FX Health Canada provided funding for this study.
NR 49
TC 18
Z9 18
U1 1
U2 13
PU BMJ PUBLISHING GROUP
PI LONDON
PA BRITISH MED ASSOC HOUSE, TAVISTOCK SQUARE, LONDON WC1H 9JR, ENGLAND
SN 1351-0711
EI 1470-7926
J9 OCCUP ENVIRON MED
JI Occup. Environ. Med.
PD DEC
PY 2011
VL 68
IS 12
BP 920
EP 927
DI 10.1136/oem.2010.062521
PG 8
WC Public, Environmental & Occupational Health
SC Public, Environmental & Occupational Health
GA 845AG
UT WOS:000296794600011
PM 21610265
ER
PT J
AU Velinsky, DJ
Riedel, GF
Ashley, JTF
Cornwell, JC
AF Velinsky, David J.
Riedel, Gerhardt F.
Ashley, Jeffrey T. F.
Cornwell, Jeffrey C.
TI Historical contamination of the Anacostia River, Washington, DC
SO ENVIRONMENTAL MONITORING AND ASSESSMENT
LA English
DT Article
DE Anacostia River; Washington DC; Sediment cores; Trace elements; Organic
contaminants; Dating
ID POLYCYCLIC AROMATIC-HYDROCARBONS; CHESAPEAKE BAY; ESTUARINE SEDIMENTS;
ORGANIC CONTAMINANTS; LAKE-SEDIMENTS; POLYCHLORINATED-BIPHENYLS;
ANAEROBIC MICROORGANISMS; BIOGEOCHEMICAL CONTROL; TRACE-ELEMENTS;
UNITED-STATES
AB The tidal Anacostia River in Washington DC has long been impacted by various sources of chemical pollution over the past 200 years. To explore more recent inputs of various chemicals, six sediment cores were collected for dating and chemical analysis in the downstream section of the tidal Anacostia River. Profiles of contaminants in sediment cores can be useful in determining management direction and effectiveness of pollution controls over time. There were two main objectives for this investigation: (1) determine current sediment contaminant levels; (2) determine a historical perspective of the sediment changes in contamination using (137)Cs and (210)Pb dating. The determination of an age-depth relationship using (210)Pb and (137)Cs dating gave somewhat different results, suggesting that the assumptions of (210)Pb dating were not met. Using the (137)Cs horizon allowed an assignment of approximate sediment accumulation rates and hence an age-depth relationship to contaminant events in the upper portions of the cores. Total PAHs showed higher concentrations at depth and lower surface concentrations. In the upper sections, PAHs were a mixture of combustion and petrogenic sources, while at depth the signature appeared to be of natural origins. Total PCBs, DDTs and chlordane concentrations showed a maximum in recent sediments, decreasing towards the surface. PCBs had lower molecular weight congeners near the surface and higher molecular weights at depth. A phthalate ester, DEHP, appeared in the mid 1940-1950s, and decreased towards the surface. Trace elements fell roughly into three groups. Fe, Mn, and As were in approximately constant proportion to Al, except in some deeper, sandy sediments, where they showed enrichments linked to redox conditions. Ag, Cd, Cu, Hg, Pb, and Zn had low concentrations in the deepest sediments, high concentrations at mid-depths, and declines to intermediate levels at the surface. Ni and Cr followed neither of these patterns closely. We observed that many contaminants appeared in the Anacostia sediments at various times, and reached relatively high concentrations in the past, but are now showing declines in loadings. In some cases, such as PCBs, DDT, chlordane, and Pb from leaded gasoline, these declines can be clearly linked to the discontinuation of their use for environmental reasons. For other contaminants (e.g., PAHs, DEHP, selected metals) these declines are more likely the result of changes in production, usage and waste control.
C1 [Velinsky, David J.; Ashley, Jeffrey T. F.] Acad Nat Sci, Patrick Ctr Environm Res, Philadelphia, PA 19103 USA.
[Riedel, Gerhardt F.] Smithsonian Environm Res Ctr, Edgewater, MD 20137 USA.
[Ashley, Jeffrey T. F.] Philadelphia Univ, Sch Sci & Hlth, Philadelphia, PA 19144 USA.
[Cornwell, Jeffrey C.] Univ Maryland, UMCES Horn Point Lab, Cambridge, MD 21613 USA.
RP Velinsky, DJ (reprint author), Acad Nat Sci, Patrick Ctr Environm Res, 1900 Benjamin Franklin Pkwy, Philadelphia, PA 19103 USA.
EM velinsky@ansp.org; riedelf@si.edu; ashleyj@philau.edu;
cornwell@hpl.umces.edu
RI Cornwell, Jeffrey/R-5506-2016
OI Cornwell, Jeffrey/0000-0001-7111-2489
NR 68
TC 8
Z9 8
U1 1
U2 33
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-6369
J9 ENVIRON MONIT ASSESS
JI Environ. Monit. Assess.
PD DEC
PY 2011
VL 183
IS 1-4
BP 307
EP 328
DI 10.1007/s10661-011-1923-z
PG 22
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 835UW
UT WOS:000296062700022
PM 21404015
ER
PT J
AU Cho, S
Zwick, A
Regier, JC
Mitter, C
Cummings, MP
Yao, JX
Du, ZL
Zhao, H
Kawahara, AY
Weller, S
Davis, DR
Baixeras, J
Brown, JW
Parr, C
AF Cho, Soowon
Zwick, Andreas
Regier, Jerome C.
Mitter, Charles
Cummings, Michael P.
Yao, Jianxiu
Du, Zaile
Zhao, Hong
Kawahara, Akito Y.
Weller, Susan
Davis, Donald R.
Baixeras, Joaquin
Brown, John W.
Parr, Cynthia
TI Can Deliberately Incomplete Gene Sample Augmentation Improve a Phylogeny
Estimate for the Advanced Moths and Butterflies (Hexapoda: Lepidoptera)?
SO SYSTEMATIC BIOLOGY
LA English
DT Article
DE Ditrysia; gene sampling; Hexapoda; Lepidoptera; missing data; molecular
phylogenetics; nuclear genes; taxon sampling
ID CODON-SUBSTITUTION MODELS; PROTEIN-CODING SEQUENCES; MISSING DATA;
NUCLEAR GENES; AMINO-ACID; DATA SETS; TAXA; EVOLUTION; ACCURACY; LIFE
AB This paper addresses the question of whether one can economically improve the robustness of a molecular phylogeny estimate by increasing gene sampling in only a subset of taxa, without having the analysis invalidated by artifacts arising from large blocks of missing data. Our case study stems from an ongoing effort to resolve poorly understood deeper relationships in the large clade Ditrysia ( > 150,000 species) of the insect order Lepidoptera (butterflies and moths). Seeking to remedy the overall weak support for deeper divergences in an initial study based on five nuclear genes (6.6 kb) in 123 exemplars, we nearly tripled the total gene sample (to 26 genes, 18.4 kb) but only in a third (41) of the taxa. The resulting partially augmented data matrix (45% intentionally missing data) consistently increased bootstrap support for groupings previously identified in the five-gene (nearly) complete matrix, while introducing no contradictory groupings of the kind that missing data have been predicted to produce. Our results add to growing evidence that data sets differing substantially in gene and taxon sampling can often be safely and profitably combined. The strongest overall support for nodes above the family level came from including all nucleotide changes, while partitioning sites into sets undergoing mostly nonsynonymous versus mostly synonymous change. In contrast, support for the deepest node for which any persuasive molecular evidence has yet emerged (78-85% bootstrap) was weak or nonexistent unless synonymous change was entirely excluded, a result plausibly attributed to compositional heterogeneity. This node (Gelechioidea + Apoditrysia), tentatively proposed by previous authors on the basis of four morphological synapomorphies, is the first major subset of ditrysian superfamilies to receive strong statistical support in any phylogenetic study. A "more-genes-only" data set (41 taxax26 genes) also gave strong signal for a second deep grouping (Macrolepidoptera) that was obscured, but not strongly contradicted, in more taxon-rich analyses.
C1 [Cho, Soowon; Mitter, Charles; Kawahara, Akito Y.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Zwick, Andreas; Regier, Jerome C.; Yao, Jianxiu; Du, Zaile; Zhao, Hong] Univ Maryland, Inst Biotechnol, Ctr Biosyst Res, College Pk, MD 20742 USA.
[Cummings, Michael P.] Univ Maryland, Lab Mol Evolut, Ctr Bioinformat & Computat Biol, College Pk, MD 20742 USA.
[Weller, Susan] Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA.
[Davis, Donald R.] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA.
[Baixeras, Joaquin] Univ Valencia, Cavanilles Inst Biodivers & Evolutionary Biol, Valencia, Spain.
[Brown, John W.] ARS, Systemat Entomol Lab, USDA, Beltsville, MD 20705 USA.
RP Mitter, C (reprint author), Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
EM cmitter@umd.edu
RI Parr, Cynthia/E-8013-2010; Baixeras, Joaquin/L-1734-2014; Zwick,
Andreas/A-5735-2015
OI Parr, Cynthia/0000-0002-8870-7099; Baixeras,
Joaquin/0000-0002-6092-0496;
FU US National Science Foundation [0531626, 0531769, DEB 0515699]; Spanish
Government (Ministerio de Ciencia e Innovacion) [CGL2008-00605]
FX Financial support was provided by the US National Science Foundation's
Assembling the Tree of Life program, award numbers 0531626 and 0531769;
the Spanish Government (Ministerio de Ciencia e Innovacion)
(CGL2008-00605 to J.B.); US National Science Foundation (DEB 0515699 to
D. H. Janzen).
NR 55
TC 50
Z9 51
U1 4
U2 27
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1063-5157
EI 1076-836X
J9 SYST BIOL
JI Syst. Biol.
PD DEC
PY 2011
VL 60
IS 6
BP 782
EP 796
DI 10.1093/sysbio/syr079
PG 15
WC Evolutionary Biology
SC Evolutionary Biology
GA 836ZO
UT WOS:000296159900004
PM 21840842
ER
PT J
AU de Queiroz, K
Donoghue, MJ
AF de Queiroz, Kevin
Donoghue, Michael J.
TI Phylogenetic Nomenclature, Three-Taxon Statements, and Unnecessary Name
Changes
SO SYSTEMATIC BIOLOGY
LA English
DT Article
ID BIOLOGICAL NOMENCLATURE; PHYLOCODE
C1 [de Queiroz, Kevin] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Donoghue, Michael J.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA.
[Donoghue, Michael J.] Yale Univ, Peabody Museum Nat Hist, New Haven, CT 06520 USA.
RP de Queiroz, K (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Amphibians & Reptiles, NHB, POB 37012,W-200,MRC 162, Washington, DC 20013 USA.
EM dequeirozk@si.edu
FU Yale Institute for Biospheric Studies
FX The Yale Institute for Biospheric Studies awarded a fellowship to K.d.Q.
that facilitated interactions with M.J.D. in the preparation of this
article. The fellowship was funded by Edward P. Bass.
NR 13
TC 4
Z9 4
U1 2
U2 17
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1063-5157
J9 SYST BIOL
JI Syst. Biol.
PD DEC
PY 2011
VL 60
IS 6
BP 887
EP 892
DI 10.1093/sysbio/syr070
PG 6
WC Evolutionary Biology
SC Evolutionary Biology
GA 836ZO
UT WOS:000296159900013
PM 21865335
ER
PT J
AU Sheehy, D
AF Sheehy, Daniel
TI Bess Lomax Hawes (1921-2009) Obituary
SO JOURNAL OF AMERICAN FOLKLORE
LA English
DT Biographical-Item
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Sheehy, D (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER FOLKLORE SOC
PI ARLINGTON
PA 4350 NORTH FAIRFAX DR, STE 640, ARLINGTON, VA 22203 USA
SN 0021-8715
J9 J AM FOLKLORE
JI J. Am. Folk.
PD WIN
PY 2011
VL 124
IS 491
BP 85
EP 88
PG 4
WC Folklore
SC Arts & Humanities - Other Topics
GA 718ZJ
UT WOS:000287165000008
ER
PT J
AU Green, WA
Hunt, G
Wing, SL
DiMichele, WA
AF Green, Walton A.
Hunt, Gene
Wing, Scott L.
DiMichele, William A.
TI Does extinction wield an axe or pruning shears? How interactions between
phylogeny and ecology affect patterns of extinction
SO PALEOBIOLOGY
LA English
DT Article
ID MASS EXTINCTIONS; TAXONOMIC SELECTIVITY; CRETACEOUS MOLLUSKS; GEOGRAPHIC
RANGE; EAST GREENLAND; ILLINOIS BASIN; FOSSIL RECORD; SPECIES-LEVEL;
EVOLUTIONARY; BOUNDARY
AB Extinctions are caused by environmental and ecological change but are recognized and measured in the fossil record by the disappearance of clades or lineages. If the ecological preferences of lineages or taxa are weakly congruent with their phylogenetic relationships, even large ecological perturbations are unlikely to drive major clades extinct because the factors that eliminate some species are unlikely to affect close relatives with different ecological preferences. In contrast, if phylogenetic relatedness and ecological preferences are congruent, then ecological perturbations can more easily cause extinctions of large clades. In order to quantify this effect, we used a computer model to simulate the diversification and extinction of clades based on ecological criteria. By varying the parameters of the model, we explored (1) the relationship between the extinction probability for a clade of a given size (number of terminals) and the overall intensity of extinction (the proportion of the terminals that go extinct), and (2) the congruence between ecological traits of the terminals and their phylogenetic relationships. Data from two extinctions (planktonic foraminifera at the Eocene/Oligocene boundary and vascular land plants at the Middle/Late Pennsylvanian boundary) show phylogenetic clustering of both ecological traits and extinction probability and demonstrate the interaction of these factors. The disappearance of large clades is observed in the fossil record, but our model suggests that it is very improbable without both high overall extinction intensities and high congruence between ecology and phylogeny.
C1 [Green, Walton A.; Hunt, Gene; Wing, Scott L.; DiMichele, William A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Green, WA (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, 26 Oxford St, Cambridge, MA 02138 USA.
EM wagreen@bricol.net
RI Hunt, Gene/B-3783-2010; DiMichele, William/K-4301-2012;
OI Hunt, Gene/0000-0001-6430-5020; Wing, Scott/0000-0002-2954-8905
FU Smithsonian Institution
FX We would like to thank B. Huber for assistance with compiling the
phylogeny of foraminifera; N. Atkins, K. Black, A. Janevski, and M.
McKinney for helpful comments on the manuscript; and the Smithsonian
Institution for financial support. This is publication number 228 of the
Smithsonian Evolution of Terrestrial Ecosystems Program.
NR 91
TC 12
Z9 12
U1 3
U2 15
PU PALEONTOLOGICAL SOC INC
PI LAWRENCE
PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA
SN 0094-8373
J9 PALEOBIOLOGY
JI Paleobiology
PD WIN
PY 2011
VL 37
IS 1
BP 72
EP 91
DI 10.1666/09078.1
PG 20
WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology
SC Biodiversity & Conservation; Environmental Sciences & Ecology;
Evolutionary Biology; Paleontology
GA 707KT
UT WOS:000286286000004
ER
PT J
AU Melott, AL
Bambach, RK
AF Melott, Adrian L.
Bambach, Richard K.
TI A ubiquitous similar to 62-Myr periodic fluctuation superimposed on
general trends in fossil biodiversity. I. Documentation
SO PALEOBIOLOGY
LA English
DT Article
ID UNEVENLY SPACED DATA; TIME-SERIES ANALYSIS; SPECTRAL-ANALYSIS; MASS
EXTINCTIONS; GAUSS-VANICEK; DIVERSITY; DIVERSIFICATION; HISTORY; CYCLES;
RECORD
AB We use Fourier analysis and related techniques to investigate the question of periodicities in fossil biodiversity. These techniques are able to identify cycles superimposed on the long-term trends of the Phanerozoic. We review prior results and analyze data previously reduced and published. Joint time-series analysis of various reductions of the Sepkoski Data, Paleobiology Database, and Fossil Record 2 indicate the same periodicity in biodiversity of marine animals at 62 Myr. We have not found this periodicity in the terrestrial fossil record. We have found that the signal strength decreases with time because of the accumulation of apparently "resistant" long-lived genera. The existence of a 62-Myr periodicity despite very different treatment of systematic error, particularly sampling-strength biases, in all three major databases strongly argues for its reality in the fossil record.
C1 [Melott, Adrian L.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bambach, Richard K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
RP Melott, AL (reprint author), Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
EM melott@ku.edu; richard.bambach@verizon.net
FU American Astronomical Society; NASA [NNX09AM85G]
FX We thank J. Alroy, M. Benton, and S. Peters for providing some of the
data which we analyze herein. Two referees provided extremely helpful
suggestions on presentation, and Don Johnson provided the illustration
for Figure 1. We are grateful to the American Astronomical Society for
the sponsorship of the 2007 Honolulu multidisciplinary Splinter Meeting
at which discussions leading to this project took place. Research
support at the University of Kansas was provided by the NASA Program
Astrobiology: Exobiology and Evolutionary Biology, under grant number
NNX09AM85G. This is Paleobiology Database official publication number
120.
NR 31
TC 17
Z9 17
U1 1
U2 5
PU PALEONTOLOGICAL SOC INC
PI LAWRENCE
PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA
SN 0094-8373
J9 PALEOBIOLOGY
JI Paleobiology
PD WIN
PY 2011
VL 37
IS 1
BP 92
EP 112
DI 10.1666/09054.1
PG 21
WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology
SC Biodiversity & Conservation; Environmental Sciences & Ecology;
Evolutionary Biology; Paleontology
GA 707KT
UT WOS:000286286000005
ER
PT J
AU Biesold, SE
Ritz, D
Gloza-Rausch, F
Wollny, R
Drexler, JF
Corman, VM
Kalko, EKV
Oppong, S
Drosten, C
Muller, MA
AF Biesold, Susanne E.
Ritz, Daniel
Gloza-Rausch, Florian
Wollny, Robert
Drexler, Jan Felix
Corman, Victor M.
Kalko, Elisabeth K. V.
Oppong, Samuel
Drosten, Christian
Mueller, Marcel A.
TI Type I Interferon Reaction to Viral Infection in Interferon-Competent,
Immortalized Cell Lines from the African Fruit Bat Eidolon helvum
SO PLOS ONE
LA English
DT Article
ID TOLL-LIKE RECEPTORS; PTEROPUS-GIGANTEUS; GENE-EXPRESSION; RESERVOIR
HOSTS; VIRUS-INFECTION; SINDBIS VIRUS; MARBURG VIRUS; V-PROTEIN; ASSAY;
EVOLUTION
AB Bats harbor several highly pathogenic zoonotic viruses including Rabies, Marburg, and henipaviruses, without overt clinical symptoms in the animals. It has been suspected that bats might have evolved particularly effective mechanisms to suppress viral replication. Here, we investigated interferon (IFN) response, -induction, -secretion and -signaling in epithelial-like cells of the relevant and abundant African fruit bat species, Eidolon helvum (E. helvum). Immortalized cell lines were generated; their potential to induce and react on IFN was confirmed, and biological assays were adapted to application in bat cell cultures, enabling comparison of landmark IFN properties with that of common mammalian cell lines. E. helvum cells were fully capable of reacting to viral and artificial IFN stimuli. E. helvum cells showed highest IFN mRNA induction, highly productive IFN protein secretion, and evidence of efficient IFN stimulated gene induction. In an Alphavirus infection model, O'nyong-nyong virus exhibited strong IFN induction but evaded the IFN response by translational rather than transcriptional shutoff, similar to other Alphavirus infections. These novel IFN-competent cell lines will allow comparative research on zoonotic, bat-borne viruses in order to model mechanisms of viral maintenance and emergence in bat reservoirs.
C1 [Biesold, Susanne E.; Ritz, Daniel; Gloza-Rausch, Florian; Wollny, Robert; Drexler, Jan Felix; Corman, Victor M.; Drosten, Christian; Mueller, Marcel A.] Univ Bonn, Inst Virol, Med Ctr, Bonn, Germany.
[Gloza-Rausch, Florian] Noctalis, Ctr Bat Protect & Informat, Bad Segeberg, Germany.
[Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, Ulm, Germany.
[Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama.
[Oppong, Samuel] Kwame Nkrumah Univ Sci & Technol, Kumasi, Ghana.
RP Biesold, SE (reprint author), Univ Bonn, Inst Virol, Med Ctr, Bonn, Germany.
EM drosten@virology-bonn.de
RI Drexler, Jan Felix/C-1004-2014;
OI Mueller, Marcel/0000-0003-2242-5117; Corman, Victor
Max/0000-0002-3605-0136
FU German Ministry of Education [SARS II 01KI1005A]; European Commission
[228292, 223498]
FX This work was supported by the German Ministry of Education (project
code SARS II 01KI1005A) and grants from the European Commission
(contracts FP7-EVA number 228292 and FP7-EMPERIE number 223498). The
funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 54
TC 30
Z9 30
U1 0
U2 10
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD NOV 30
PY 2011
VL 6
IS 11
AR e28131
DI 10.1371/journal.pone.0028131
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 863MI
UT WOS:000298168100039
PM 22140523
ER
PT J
AU Araki, N
Moini, M
AF Araki, Naoko
Moini, Mehdi
TI Age estimation of museum wool textiles from Ovis aries using deamidation
rates utilizing matrix-assisted laser desorption/ionization
time-of-flight mass spectrometry
SO RAPID COMMUNICATIONS IN MASS SPECTROMETRY
LA English
DT Article
ID PROTEIN DEAMIDATION; RESIDUES; ACID
AB Cultural heritage contains a large number of precious proteinaceous specimens, such as wool and silk textiles, leather objects, paper, paint, coatings, binders (and associated adhesives), etc. To minimize the degradation of and to preserve these artifacts, it is desirable to understand the fundamental factors that cause their degradation, to identify the deterioration markers that determine their degradation stage and their age, and to use technologies that can provide this information rapidly while consuming a minimal amount of sample. There are several forces that cause protein degradation, including amino acid racemization, protein deamidation, and protein truncation. The purpose of this paper is to study protein deamidation using matrix-assisted laser desorption/ionization mass spectrometry (MALDI-MS) for high-throughput dating of museums wool specimens. For proof of concept, several well-dated sheep's wool textiles from museum collections were analyzed. For wool samples aged from the present to similar to 400 years ago, the deamidation of two asparagine-containing peptides obtained from the tryptic digest of sheep wool were found to behave linearly in time, indicating that they could act as a potential biomarker of aging for wool samples. Copyright (C) 2011 John Wiley & Sons, Ltd.
C1 [Moini, Mehdi] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
[Araki, Naoko] Texas State Univ, Dept Chem & Biochem, San Marcos, TX USA.
RP Moini, M (reprint author), Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM moinim@si.edu
NR 26
TC 9
Z9 9
U1 0
U2 10
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0951-4198
J9 RAPID COMMUN MASS SP
JI Rapid Commun. Mass Spectrom.
PD NOV 30
PY 2011
VL 25
IS 22
BP 3396
EP 3400
DI 10.1002/rcm.5237
PG 5
WC Biochemical Research Methods; Chemistry, Analytical; Spectroscopy
SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy
GA 847ZL
UT WOS:000297015300004
PM 22002692
ER
PT J
AU MacPherson, GJ
Thiemens, MH
AF MacPherson, Glenn J.
Thiemens, Mark H.
TI Cosmochemistry: Understanding the Solar System through analysis of
extraterrestrial materials
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
ID METEORITES; OXYGEN; NEBULA; INCLUSIONS; CHONDRITE; ALLENDE; ORIGIN;
GASES; AGE
AB Cosmochemistry is the chemical analysis of extraterrestrial materials. This term generally is taken to mean laboratory analysis, which is the cosmochemistry gold standard because of the ability for repeated analysis under highly controlled conditions using the most advanced instrumentation unhindered by limitations in power, space, or environment. Over the past 40 y, advances in technology have enabled telescopic and spacecraft instruments to provide important data that significantly complement the laboratory data. In this special edition, recent advances in the state of the art of cosmochemistry are presented, which range from instrumental analysis of meteorites to theoretical-computational and astronomical observations.
C1 [MacPherson, Glenn J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Thiemens, Mark H.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
RP MacPherson, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
EM macphers@si.edu; mthiemens@ucsd.edu
NR 31
TC 3
Z9 3
U1 0
U2 11
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 NOV 29
PY 2011
VL 108
IS 48
BP 19130
EP 19134
DI 10.1073/pnas.1111493108
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 853ZB
UT WOS:000297463100015
PM 22128323
ER
PT J
AU MacPherson, GJ
Boss, A
AF MacPherson, Glenn J.
Boss, Alan
TI Cosmochemical evidence for astrophysical processes during the formation
of our solar system
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE cosmochemistry; solar system origin
ID ALUMINUM-RICH INCLUSIONS; ISOTOPIC ANOMALIES; ALLENDE METEORITE;
INTERPLANETARY DUST; INTERSTELLAR GRAINS; COMET 81P/WILD-2;
CALCIUM-RICH; CHONDRITES; ABUNDANCES; ELEMENTS
AB Through the laboratory study of ancient solar system materials such as meteorites and comet dust, we can recognize evidence for the same star-formation processes in our own solar system as those that we can observe now through telescopes in nearby star-forming regions. High temperature grains formed in the innermost region of the solar system ended up much farther out in the solar system, not only the asteroid belt but even in the comet accretion region, suggesting a huge and efficient process of mass transport. Bi-polar outflows, turbulent diffusion, and marginal gravitational instability are the likely mechanisms for this transport. The presence of short-lived radionuclides in the early solar system, especially (60)Fe, (26)Al, and (41)Ca, requires a nearby supernova shortly before our solar system was formed, suggesting that the Sun was formed in a massive star-forming region similar to Orion or Carina. Solar system formation may have been "triggered" by ionizing radiation originating from massive O and B stars at the center of an expanding HII bubble, one of which may have later provided the supernova source for the short-lived radionuclides. Alternatively, a supernova shock wave may have simultaneously triggered the collapse and injected the short-lived radionuclides. Because the Sun formed in a region where many other stars were forming more or less contemporaneously, the bi-polar outflows from all such stars enriched the local region in interstellar silicate and oxide dust. This may explain several observed anomalies in the meteorite record: a near absence of detectable (no extreme isotopic properties) presolar silicate grains and a dichotomy in the isotope record between (26)Al and nucleosynthetic (nonradiogenic) anomalies.
C1 [MacPherson, Glenn J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Boss, Alan] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
RP MacPherson, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
EM macphers@si.edu
FU National Aeronautics and Space Administration (NASA) [NNX11AD43G,
NNX09AF62G]; NASA Astrobiology Institute [NNA09DA81A]
FX We thank Dr. Ann Nguyen for providing Fig. 5, Drs. John Bradley and
Larry Nittler for helpful discussions, and two anonymous reviewers for
very constructive suggestions that greatly improved the paper. G.J.M.
would like to acknowledge the pioneering work of G. Herbig, who long ago
considered the possibility that bipolar outflow from young stars might
be an important source of interstellar dust. This work was supported by
National Aeronautics and Space Administration (NASA) Grants NNX11AD43G
(to G.J.M.; Cosmochemistry program), NNX09AF62G (to A.P.B.; Origins of
Solar Systems), and NASA Astrobiology Institute NNA09DA81A (to A.P.B.).
NR 54
TC 12
Z9 12
U1 1
U2 10
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 NOV 29
PY 2011
VL 108
IS 48
BP 19152
EP 19158
DI 10.1073/pnas.1110051108
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 853ZB
UT WOS:000297463100019
PM 22106251
ER
PT J
AU McCoy, TJ
Corrigan, CM
Herd, CDK
AF McCoy, Timothy J.
Corrigan, Catherine M.
Herd, Christopher D. K.
TI Combining meteorites and missions to explore Mars
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
ID ALLAN HILLS 84001; MARTIAN METEORITE; SNC METEORITES; FRACTIONAL
CRYSTALLIZATION; DIFFERENTIATION HISTORY; ISOTOPIC SYSTEMATICS;
SHERGOTTY METEORITE; BASALTIC METEORITES; MERIDIANI-PLANUM; OXYGEN
FUGACITY
AB Laboratory studies of meteorites and robotic exploration of Mars reveal scant atmosphere, no evidence of plate tectonics, past evidence for abundant water, and a protracted igneous evolution. Despite indirect hints, direct evidence of a martian origin came with the discovery of trapped atmospheric gases in one meteorite. Since then, the study of martian meteorites and findings from missions have been linked. Although the meteorite source locations are unknown, impact ejection modeling and spectral mapping of Mars suggest derivation from small craters in terrains of Amazonian to Hesperian age. Whereas most martian meteorites are young (< 1.3 Ga), the spread of whole rock isotopic compositions results from crystallization of a magma ocean > 4.5 Ga and formation of enriched and depleted reservoirs. However, the history inferred from martian meteorites conflicts with results from recent Mars missions, calling into doubt whether the igneous histor y inferred from the meteorites is applicable to Mars as a whole. Allan Hills 84001 dates to 4.09 Ga and contains fluid-deposited carbonates. Accompanying debate about the mechanism and temperature of origin of the carbonates came several features suggestive of past microbial life in the carbonates. Although highly disputed, the suggestion spurred interest in habitable extreme environments on Earth and throughout the Solar System. A flotilla of subsequent spacecraft has redefined Mars from a volcanic planet to a hydrologically active planet that may have harbored life. Understanding the history and habitability of Mars depends on understanding the coupling of the atmosphere, surface, and subsurface. Sample return that brings back direct evidence from these diverse reservoirs is essential.
C1 [McCoy, Timothy J.; Corrigan, Catherine M.; Herd, Christopher D. K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Herd, Christopher D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
RP McCoy, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th & Constitut Ave NW, Washington, DC 20560 USA.
EM mccoyt@si.edu
NR 69
TC 13
Z9 13
U1 3
U2 21
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 NOV 29
PY 2011
VL 108
IS 48
BP 19159
EP 19164
DI 10.1073/pnas.1013478108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 853ZB
UT WOS:000297463100020
PM 21969535
ER
PT J
AU Morita, SI
AF Morita, Shelah I.
TI Repeatability and precision in proboscis length measurements for long
proboscid flies
SO ZOOTAXA
LA English
DT Article
DE Proboscis; long-tongued fly; Tabanidae; Nemestrinidae; measurement;
morphology; co-divergence; pollination ecology
ID FLY POLLINATION SYSTEM; SOUTHERN AFRICA; IPOMOPSIS-AGGREGATA;
BOMBYLIIDAE DIPTERA; GLADIOLUS IRIDACEAE; MEDIATED SELECTION; SOAPBERRY
BUG; FLOWERS; MORPHOLOGY; RADIATION
AB Methods for measuring proboscides in long-tongued fly pollinators are examined with respect to fly morphology and behavior. Most ecological studies aim to measure the functional proboscis length as a response or predictor variable. Here I suggest a proxy for this, the Maximum Functional Length (MFL), obtained by combining the lengths of the prementum and labrum. I also quantify errors in proboscis measurements due to a lack of consideration of the extensible ventral rostral membrane (VRM). Results show that naive measurements allow for substantial unrepeatable variation (mean: 7mm; maximum 14mm).
C1 [Morita, Shelah I.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA.
RP Morita, SI (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20560 USA.
EM moritas@si.edu
FU U.S. Department of State; US National Science Foundation [NSF:OISE-IRFP
0701336, DEB 0138288]; US NSF PEET [DEB 0731528]
FX I would like to thank my Smithsonian NMNH interns, Nora Underwood, and
Elizabeth Brandt, for assistance with measurements, to S. Johnson and
the Johnson Lab for unfailing support, and to B. Anderson for
invigorating discussion. Also, I am grateful for comments and
suggestions provided by Matthew Buffington, Kevin Holston, and Bradley
Sinclair, and one anonymous reviewer which significantly improved
earlier version of the manuscript. Funding was provided by grants to the
author from the Fulbright U.S. Scholar Program to South Africa (U.S.
Department of State), and the US National Science Foundation
(NSF:OISE-IRFP 0701336; DEB 0138288), and by support from US NSF PEET
Grant DEB 0731528 (Tabanid PEET).
NR 56
TC 2
Z9 2
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 NOV 29
PY 2011
IS 3112
BP 49
EP 58
PG 10
WC Zoology
SC Zoology
GA 861TK
UT WOS:000298041900003
ER
PT J
AU Pyle, JA
Warwick, NJ
Harris, NRP
Abas, MR
Archibald, AT
Ashfold, MJ
Ashworth, K
Barkley, MP
Carver, GD
Chance, K
Dorsey, JR
Fowler, D
Gonzi, S
Gostlow, B
Hewitt, CN
Kurosu, TP
Lee, JD
Langford, SB
Mills, G
Moller, S
MacKenzie, AR
Manning, AJ
Misztal, P
Nadzir, MSM
Nemitz, E
Newton, HM
O'Brien, LM
Ong, S
Oram, D
Palmer, PI
Peng, LK
Phang, SM
Pike, R
Pugh, TAM
Rahman, NA
Robinson, AD
Sentian, J
Abu Samah, A
Skiba, U
Ung, HE
Yong, SE
Young, PJ
AF Pyle, J. A.
Warwick, N. J.
Harris, N. R. P.
Abas, Mohd Radzi
Archibald, A. T.
Ashfold, M. J.
Ashworth, K.
Barkley, Michael P.
Carver, G. D.
Chance, K.
Dorsey, J. R.
Fowler, D.
Gonzi, S.
Gostlow, B.
Hewitt, C. N.
Kurosu, T. P.
Lee, J. D.
Langford, S. B.
Mills, G.
Moller, S.
MacKenzie, A. R.
Manning, A. J.
Misztal, P.
Nadzir, Mohd Shahrul Mohd
Nemitz, E.
Newton, H. M.
O'Brien, L. M.
Ong, Simon
Oram, D.
Palmer, P. I.
Peng, Leong Kok
Phang, Siew Moi
Pike, R.
Pugh, T. A. M.
Rahman, Noorsaadah Abdul
Robinson, A. D.
Sentian, J.
Abu Samah, Azizan
Skiba, U.
Ung, Huan Eng
Yong, Sei Eng
Young, P. J.
TI The impact of local surface changes in Borneo on atmospheric composition
at wider spatial scales: coastal processes, land-use change and air
quality
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE tropospheric ozone; biogenic organic compounds; rainforest; isoprene;
atmospheric modelling
ID TROPICAL RAIN-FOREST; MARINE BOUNDARY-LAYER; TERRESTRIAL ISOPRENE
EMISSIONS; VOLATILE ORGANIC-COMPOUNDS; OZONE DESTRUCTION;
ATLANTIC-OCEAN; BOX MODEL; EAST; TROPOSPHERE; GASES
AB We present results from the OP3 campaign in Sabah during 2008 that allowus to study the impact of local emission changes over Borneo on atmospheric composition at the regional and wider scale. OP3 constituent data provide an important constraint on model performance. Treatment of boundary layer processes is highlighted as an important area of model uncertainty. Model studies of land-use change confirm earlier work, indicating that further changes to intensive oil palm agriculture in South East Asia, and the tropics in general, could have important impacts on air quality, with the biggest factor being the concomitant changes in NOx emissions. With the model scenarios used here, local increases in ozone of around 50 per cent could occur. We also report measurements of short-lived brominated compounds around Sabah suggesting that oceanic (and, especially, coastal) emission sources dominate locally. The concentration of bromine in short-lived halocarbons measured at the surface during OP3 amounted to about 7 ppt, setting an upper limit on the amount of these species that can reach the lower stratosphere.
C1 [Pyle, J. A.; Warwick, N. J.; Harris, N. R. P.; Archibald, A. T.; Ashfold, M. J.; Carver, G. D.; Gostlow, B.; O'Brien, L. M.; Pike, R.; Robinson, A. D.; Young, P. J.] Univ Cambridge, Dept Chem, Cambridge CB2 1EW, England.
[Ashworth, K.; Hewitt, C. N.; Langford, S. B.; MacKenzie, A. R.; Pugh, T. A. M.] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England.
[Barkley, Michael P.; Gonzi, S.; Palmer, P. I.] Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JW, Midlothian, Scotland.
[Barkley, Michael P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Chance, K.; Kurosu, T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dorsey, J. R.] Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester M13 3PL, Lancs, England.
[Fowler, D.; Misztal, P.; Nemitz, E.; Skiba, U.] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland.
[Lee, J. D.; Moller, S.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England.
[Manning, A. J.] Met Off, Exeter, Devon, England.
[Misztal, P.] Univ Edinburgh, Dept Chem, Edinburgh EH8 9YL, Midlothian, Scotland.
[Abas, Mohd Radzi; Nadzir, Mohd Shahrul Mohd; Phang, Siew Moi; Abu Samah, Azizan] Univ Malaya, Inst Ocean & Earth Sci, Kuala Lumpur 50603, Malaysia.
[Rahman, Noorsaadah Abdul] Univ Malaya, Dept Chem, Kuala Lumpur 50603, Malaysia.
[Mills, G.; Newton, H. M.; Oram, D.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Ong, Simon; Ung, Huan Eng] Global Satria Life Sci Lab, Tawau 91000, Sabah, Malaysia.
[Peng, Leong Kok; Yong, Sei Eng] Ketua Stesen GAW Lembah Danum, Malaysian Meteorol Dept, Tawau 91011, Sabah, Malaysia.
[Sentian, J.] Univ Malaysia Sabah, Sch Sci & Technol, Kota Kinabalu, Malaysia.
[Young, P. J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Young, P. J.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
EM john.pyle@atm.ch.cam.ac.uk
RI Phang, Siew Moi/A-7653-2008; Manager, CSD Publications/B-2789-2015;
Pugh, Thomas/A-3790-2010; Young, Paul/E-8739-2010; Abd-Rahman,
Noorsaadah/B-9291-2010; Misztal, Pawel/B-8371-2009; Nemitz,
Eiko/I-6121-2012; Skiba, Ute/I-6441-2012; Ashworth, Kirsti/A-7742-2013;
fowler, david/B-5446-2010; Ashworth, Kirsti/N-4550-2013; Palmer,
Paul/F-7008-2010; ABAS, MHD RADZI/B-9002-2010; Hewitt, Charles
Nicholas/B-1219-2009; HJ ABU SAMAH, AZIZAN/B-8295-2010
OI Pugh, Thomas/0000-0002-6242-7371; Ashfold, Matthew/0000-0002-2191-1554;
Archibald, Alexander/0000-0001-9302-4180; Chance,
Kelly/0000-0002-7339-7577; Moller, Sarah/0000-0003-4923-9509; Harris,
Neil/0000-0003-1256-3006; Young, Paul/0000-0002-5608-8887; Abd-Rahman,
Noorsaadah/0000-0001-5847-8961; Misztal, Pawel/0000-0003-1060-1750;
Nemitz, Eiko/0000-0002-1765-6298; fowler, david/0000-0002-2999-2627;
Ashworth, Kirsti/0000-0001-5627-3014; Hewitt, Charles
Nicholas/0000-0001-7973-2666;
FU NCAS; British Council; NERC [NE/G014655/1, NE/D002117/1, NE/E011233/1]
FX We thank the Malaysian and Sabah Governments for their permission to
conduct research in Malaysia; the Malaysian Meteorological Department
(MMD, now Met Malaysia) for access to the Bukit Atur Global Atmosphere
Watch station and their long-term ozone record. For all their assistance
with the fieldwork, we gratefully acknowledge: Waidi Sinun of Yayasan
Sabah and his staff; Dr Glen Reynolds and his staff at the Royal
Society's Danum Valley Research Centre; the ground staff, engineers,
scientists and pilots of the UK Natural Environment Research Council/UK
Meteorological Office's BAe 146-301 large atmospheric research aircraft
(FAAM); and the rest of the OP3 project team for their individual and
collective efforts. This research was funded by NCAS, by NERC under the
OP3 (grant ref: NE/D002117/1) and ACES (grant ref: NE/E011233/1)
projects. This work was also supported by a British Council PMI2 grant.
N.R.P.H. thanks NERC for his Advanced Fellowship (NE/G014655/1). We
acknowledge data from AATSR World Fire Atlas from the Data User Element
of the European Space Agency. This paper constitutes Publication no. 513
of the Royal Society South East Asia Rainforest Research Programme.
NR 74
TC 10
Z9 10
U1 2
U2 37
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8436
EI 1471-2970
J9 PHILOS T R SOC B
JI Philos. Trans. R. Soc. B-Biol. Sci.
PD NOV 27
PY 2011
VL 366
IS 1582
BP 3210
EP 3224
DI 10.1098/rstb.2011.0060
PG 15
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 841ZZ
UT WOS:000296555900005
PM 22006963
ER
PT J
AU Ewers, RM
Didham, RK
Fahrig, L
Ferraz, G
Hector, A
Holt, RD
Kapos, V
Reynolds, G
Sinun, W
Snaddon, JL
Turner, EC
AF Ewers, Robert M.
Didham, Raphael K.
Fahrig, Lenore
Ferraz, Goncalo
Hector, Andy
Holt, Robert D.
Kapos, Valerie
Reynolds, Glen
Sinun, Waidi
Snaddon, Jake L.
Turner, Edgar C.
TI A large-scale forest fragmentation experiment: the Stability of Altered
Forest Ecosystems Project
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE Biological Dynamics of Forest Fragments Project; Calling Lake
Fragmentation Experiment; deforestation; hierarchical sampling design;
Savannah River Site Corridor Experiment; Wog Wog Habitat Fragmentation
Experiment
ID HABITAT FRAGMENTATION; SPECIES RICHNESS; BIODIVERSITY; CONSERVATION;
LANDSCAPE; OIL; RESPONSES; EXTINCTIONS; CORRIDOR; DYNAMICS
AB Opportunities to conduct large-scale field experiments are rare, but provide a unique opportunity to reveal the complex processes that operate within natural ecosystems. Here, we review the design of existing, large-scale forest fragmentation experiments. Based on this review, we develop a design for the Stability of Altered Forest Ecosystems (SAFE) Project, a new forest fragmentation experiment to be located in the lowland tropical forests of Borneo (Sabah, Malaysia). The SAFE Project represents an advance on existing experiments in that it: (i) allows discrimination of the effects of landscape-level forest cover from patch-level processes; (ii) is designed to facilitate the unification of a wide range of data types on ecological patterns and processes that operate over a wide range of spatial scales; (iii) has greater replication than existing experiments; (iv) incorporates an experimental manipulation of riparian corridors; and (v) embeds the experimentally fragmented landscape within a wider gradient of land-use intensity than do existing projects. The SAFE Project represents an opportunity for ecologists across disciplines to participate in a large initiative designed to generate a broad understanding of the ecological impacts of tropical forest modification.
C1 [Ewers, Robert M.; Turner, Edgar C.] Univ London Imperial Coll Sci Technol & Med, Dept Life Sci, Ascot SL5 7PY, Berks, England.
[Didham, Raphael K.] Univ Western Australia, Sch Anim Biol, Crawley, WA 6009, Australia.
[Didham, Raphael K.] CSIRO Ecosyst Serv, Ctr Environm & Life Sci, Floreat, WA 6014, Australia.
[Didham, Raphael K.] Univ Canterbury, Sch Biol Sci, Christchurch 1, New Zealand.
[Fahrig, Lenore] Carleton Univ, Ottawa Carleton Inst Biol, Ottawa, ON K1S 5B6, Canada.
[Ferraz, Goncalo] Inst Nacl de Pesquisas da Amazonia, Smithsonian Trop Res Inst, Biol Dynam Forest Fragments Project, BR-69011 Manaus, AM, Brazil.
[Ferraz, Goncalo] Smithsonian Trop Res Inst, Balboa, Panama.
[Hector, Andy; Snaddon, Jake L.] Univ Zurich, Inst Evolutionary Biol & Environm Studies, CH-8057 Zurich, Switzerland.
[Holt, Robert D.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Kapos, Valerie] World Conservat Monitoring Ctr WCMW, UNEP, Cambridge CB3 0DL, England.
[Kapos, Valerie; Snaddon, Jake L.; Turner, Edgar C.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England.
[Reynolds, Glen] Royal Soc SE Asia Rainforest Res Programme SEARRP, Danum Valley Field Ctr, Lahad Datu 91112, Sabah, Malaysia.
[Sinun, Waidi] Yayasan Sabah Grp, Conservat & Environm Management Div, Kota Kinabalu 88817, Sabah, Malaysia.
RP Ewers, RM (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Life Sci, Silwood Pk Campus,Buckhurst Rd, Ascot SL5 7PY, Berks, England.
EM r.ewers@imperial.ac.uk
RI Didham, Raphael/B-5953-2011; Hector, Andrew/H-4199-2011; Kapos,
Valerie/G-3136-2010; Snaddon, Jake/C-8800-2011;
OI Hector, Andrew/0000-0002-1309-7716; Kapos, Valerie/0000-0002-5739-8262;
Turner, Edgar/0000-0003-2715-2234
FU NERC Centre for Population Biology; Sime Darby Foundation
FX We thank the Sime Darby Foundation, the Sabah Foundation, BentaWawasan
and the Sabah Forestry Department for their generous support of the SAFE
Project. Mick Crawley, Charles Godfray, Bill Laurance, Georgina Mace and
Stuart Pimm provided valuable advice on the project design. This paper
arose from a workshop sponsored by the NERC Centre for Population
Biology. The SAFE Project is funded by the Sime Darby Foundation.
Researchers are invited to take advantage of the SAFE study sites and,
if interested, should visit the project website (www.safeproject.net).
This paper constitutes Publication Number A/580 of the Royal Society
South East Asia Rainforest Research Programme.
NR 52
TC 56
Z9 58
U1 14
U2 97
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8436
J9 PHILOS T R SOC B
JI Philos. Trans. R. Soc. B-Biol. Sci.
PD NOV 27
PY 2011
VL 366
IS 1582
BP 3292
EP 3302
DI 10.1098/rstb.2011.0049
PG 11
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 841ZZ
UT WOS:000296555900011
PM 22006969
ER
PT J
AU Li, W
Pohl, T
Rost, JM
Rittenhouse, ST
Sadeghpour, HR
Nipper, J
Butscher, B
Balewski, JB
Bendkowsky, V
Low, R
Pfau, T
AF Li, W.
Pohl, T.
Rost, J. M.
Rittenhouse, Seth T.
Sadeghpour, H. R.
Nipper, J.
Butscher, B.
Balewski, J. B.
Bendkowsky, V.
Loew, R.
Pfau, T.
TI A Homonuclear Molecule with a Permanent Electric Dipole Moment
SO SCIENCE
LA English
DT Article
ID RANGE RYDBERG MOLECULES; PENDULAR STATES; ORIENTATION; COLLISIONS;
PULSES; DIMERS; FIELDS; POLAR; ATOM
AB Permanent electric dipole moments in molecules require a breaking of parity symmetry. Conventionally, this symmetry breaking relies on the presence of heteronuclear constituents. We report the observation of a permanent electric dipole moment in a homonuclear molecule in which the binding is based on asymmetric electronic excitation between the atoms. These exotic molecules consist of a ground-state rubidium (Rb) atom bound inside a second Rb atom electronically excited to a high-lying Rydberg state. Detailed calculations predict appreciable dipole moments on the order of 1 Debye, in excellent agreement with the observations.
C1 [Rittenhouse, Seth T.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA.
[Li, W.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Li, W.; Pohl, T.; Rost, J. M.] Max Planck Inst Phys Komplexer Syst, D-01187 Dresden, Germany.
[Nipper, J.; Butscher, B.; Balewski, J. B.; Bendkowsky, V.; Loew, R.; Pfau, T.] Univ Stuttgart, Inst Phys, D-70569 Stuttgart, Germany.
RP Sadeghpour, HR (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, 60 Garden St, Cambridge, MA 02138 USA.
EM hrs@cfa.harvard.edu
RI Pfau, Tilman/G-1774-2011; Li, Weibin/E-6807-2011; Pohl,
Thomas/B-5133-2013; Loew, Robert/I-8206-2014;
OI Rost, Jan M./0000-0002-8306-1743
FU NSF through ITAMP [0653021]; Harvard Department of Physics; Smithsonian
Astrophysical Observatory; European Union; Deutsche
Forschungsgemeinschaft [SFB/TRR21, PF 381/4-2]
FX We thank J. Feist and P. Julienne for useful discussions in the
preparation of this work and L. Kukota for her assistance. Supported by
NSF grant 0653021 through ITAMP, the Harvard Department of Physics, and
the Smithsonian Astrophysical Observatory (S. T. R. and H. R. S.), a
European Union Marie Curie Fellowship (W. L.), and the Deutsche
Forschungsgemeinschaft within SFB/TRR21 and the project PF 381/4-2.
NR 30
TC 60
Z9 60
U1 2
U2 26
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 NOV 25
PY 2011
VL 334
IS 6059
BP 1110
EP 1114
DI 10.1126/science.1211255
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 852AF
UT WOS:000297313900044
PM 22116881
ER
PT J
AU LaPolla, JS
Brady, SG
Shattuck, SO
AF LaPolla, John S.
Brady, Sean G.
Shattuck, Steven O.
TI Monograph of Nylanderia (Hymenoptera: Formicidae) of the World: An
introduction to the systematics and biology of the genus
SO ZOOTAXA
LA English
DT Article
DE Formicidae; Nylanderia; Paraparatrechina; Paratrechina; Prenolepis
genus-group; taxonomy
ID TAXONOMIC REVISION; ANTS HYMENOPTERA; CRAZY ANT
AB This paper serves as an introduction to a world monographic series addressing the species-level taxonomy of the ant genus Nylanderia. This series will consist of several regionally based taxonomic revisions. The systematics and biology of Nylanderia are discussed in a global context, and a diagnosis of the genus is given. Several morphological features, which are considered putative synapomorphies for the genus, are provided. Morphological descriptions of all three castes (workers, queens, and males) are provided and discussed.
C1 [LaPolla, John S.] Towson Univ, Dept Biol Sci, Towson, MD 21252 USA.
[Brady, Sean G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA.
[Shattuck, Steven O.] CSIRO Ecosyst Sci, Australian Natl Insect Collect, Canberra, ACT, Australia.
RP LaPolla, JS (reprint author), Towson Univ, Dept Biol Sci, Towson, MD 21252 USA.
FU National Science Foundation [DEB-0743542]; National Museum of Natural
History [177]
FX We thank Eugenia Okonski for assistance with specimen preparations and
Scott Whittaker for assistance with the SEM. James Trager provided
interesting discussions regarding the use of macrosetae versus
macrochaetae in Nylanderia and provided valuable comments on a draft of
this manuscript. Jack Longino and two anonymous reviewers provided
helpful comments that greatly improved the manuscript. We thank Alex
Wild for the use of his photographs. This research was supported by the
National Science Foundation under grant no. DEB-0743542. This is number
177 in the National Museum of Natural History's Biological Diversity of
the Guiana Shield Program publication series.
NR 21
TC 11
Z9 12
U1 3
U2 5
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 NOV 25
PY 2011
IS 3110
BP 1
EP 9
PG 9
WC Zoology
SC Zoology
GA 852DL
UT WOS:000297328000001
ER
PT J
AU Takei, D
Ness, JU
Tsujimoto, M
Kitamoto, S
Drake, JJ
Osborne, JP
Takahashi, H
Kinugasa, K
AF Takei, Dai
Ness, Jan-Uwe
Tsujimoto, Masahiro
Kitamoto, Shunji
Drake, Jeremy J.
Osborne, Julian P.
Takahashi, Hiromitsu
Kinugasa, Kenzo
TI X-Ray Study of Rekindled Accretion in the Classical Nova V2491 Cygni
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE stars: individual (Nova Cygni 2008 number 2, V2491 Cygni); stars: novae,
cataclysmic variables; X-rays: stars
ID MAGNETIC CATACLYSMIC VARIABLES; PHOTON IMAGING CAMERA; BOARD XMM-NEWTON;
RS-OPHIUCHI; SWIFT OBSERVATIONS; LINE DIAGNOSTICS; 2006 OUTBURST; V382
VELORUM; DWARF NOVAE; BLAST WAVE
AB We conducted an X-ray spectroscopic study of the classical nova V2491 Cygni using our target-of-opportunity observation data with the Suzaku and XMM-Newton satellites as well as archived data with the Swift satellite. Medium-resolution (R similar to 10-50) spectra were obtained using the X-ray CCD spectrometers at several post-nova epochs on days 9, 29, 40, 50, and 60-150 in addition to a pre-nova interval between days 322 and 100, all relative to the time when the classical nova was spotted. We found remarkable changes in the time series of the spectra: (a) In the pre-nova phase and on day 9, the 6.7 keV emission line from Fe XXV was significantly detected. (b) On day 29, no such emission line was found. (c) On day 40, the 6.7 keV emission line emerged again. (d) On days 50 and 60-150, three emission lines at 6.4, 6.7, and 7.0 keV, respectively, from quasi-neutral Fe, Fe XXV, and Fe XXVI were found. Statistically significant changes of the Fe K line intensities were confirmed between days 29 and 50. Based on these phenomena, we conclude that: (1) the post-nova evolution can be divided into two different phases, (2) ejecta is responsible for the X-ray emission in the earlier phase, while rekindled accretion is responsible for the later phase, and (3) the accretion process is considered to be reestablished as early as day 50 when the quasi-neutral Fe emission line emerged, which is a common signature of accretion from magnetic cataclysmic variables.
C1 [Takei, Dai; Kitamoto, Shunji] Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo 1718501, Japan.
[Takei, Dai] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Ness, Jan-Uwe] European Space Agcy, XMM Newton Observ SOC, SRE OAX, Madrid 28691, Spain.
[Tsujimoto, Masahiro; Drake, Jeremy J.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Osborne, Julian P.] Univ Leicester, Dept Phys & Astron, Leicester LE8 9DX, Leics, England.
[Takahashi, Hiromitsu] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Kinugasa, Kenzo] Gunma Astron Observ, Gunma 3770702, Japan.
RP Takei, D (reprint author), Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan.
EM takei@ast.rikkyo.ac.jp
RI XRAY, SUZAKU/A-1808-2009
FU Japan Society for the Promotion of Science (JSPS); NASA [NAS8-39073];
Science and Technology Facilities Council (STFC)
FX D. T. is financially supported by the Japan Society for the Promotion of
Science (JSPS). J. J. D. was supported by the NASA contract NAS8-39073
to the Chandra X-ray Observatory Center (CXC). J. P. O. acknowledges the
support of the Science and Technology Facilities Council (STFC).
NR 97
TC 1
Z9 1
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 NOV 25
PY 2011
VL 63
SI 3
BP S729
EP S738
DI 10.1093/pasj/63.sp3.S729
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 877OM
UT WOS:000299191800011
ER
PT J
AU Yamaguchi, H
Koyama, K
Uchida, H
AF Yamaguchi, Hiroya
Koyama, Katsuji
Uchida, Hiroyuki
TI Suzaku View of the Supernova Remnant RCW 86: X-Ray Studies of
Newly-Discovered Fe-Rich Ejecta
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE ISM: individual (RCW 86); supernova remnants; X-rays: spectra
ID IA SUPERNOVAE; PROGENITOR SYSTEMS; EMISSION; SPECTROSCOPY; SHELL;
IONIZATION; MODELS; SHOCK; ACCELERATION; ABUNDANCES
AB We report on results of imaging and spectral analysis of the supernova remnant (SNR) RCW 86 observed with Suzaku. The SNR is known to exhibit K-shell emission of low ionized Fe, possibly originating from supernova ejecta. We revealed the global distribution of the Fe-rich plasma in the entire remnant, for the first time; the Fe-K emission was clearly detected from the west, north, and south regions, in addition to the X-ray brighter shells of southwest and northeast, where the presence of the Fe-rich ejecta has already been reported. The spectrum of each region is well represented by a three-component model consisting of low- and high-temperature thermal plasmas and non-thermal emission. The lower-temperature component, with elemental abundances of near the solar values, likely originates from the forward shocked interstellar medium, while the Fe-rich ejecta is described by the hotter plasma. From the morphologies of the forward and reverse shocks in the west region, the total ejecta mass is estimated to be 1-2 M-circle dot for the typical explosion energy of similar to 1 x 10(51) erg. The integrated flux of the Fe-K emission from the entire SNR roughly corresponds to a total Fe mass of about 1 M-circle dot. Both of these estimates suggest a Type la supernova origin of this SNR. We also find possible evidence of an Fe-rich clump located beyond the forward-shock front in the north rim, which is reminiscent of ejecta knots observed in the Tycho and Vela SNRs.
C1 [Yamaguchi, Hiroya] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Yamaguchi, Hiroya] RIKEN, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan.
[Koyama, Katsuji; Uchida, Hiroyuki] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan.
RP Yamaguchi, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM hyamaguchi@head.cfa.harvard.edu
RI XRAY, SUZAKU/A-1808-2009
FU NASA [NNXOAC71G]; Japan Society for the Promotion of Science (JSPS);
Ministry of Education, Culture, Sports, Science and Technology (MEXT)
[20654019]
FX The authors deeply appreciate a number of constructive suggestions from
the anonymous referee. We also thank to Drs. Adam Foster and Randall K.
Smith for providing useful information about AtomDB, and Drs. Patrick O.
Slane and Daniel Patnaude for stimulating discussions. Dr. Midori Ozawa
largely contributed to planning the mapping observation of RCW 86 using
Suzaku. H.Y. acknowledges funding from NASA ADP grant NNXOAC71G. H.Y.
and H.U. are supported by Japan Society for the Promotion of Science
(JSPS) Research Fellowship for Research Abroad and Young Scientists,
respectively. K.K. is supported by the Challenging Exploratory Research
program (No. 20654019) of the Ministry of Education, Culture, Sports,
Science and Technology (MEXT).
NR 50
TC 7
Z9 7
U1 0
U2 0
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 NOV 25
PY 2011
VL 63
SI 3
BP S837
EP S848
DI 10.1093/pasj/63.sp3.S837
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 877OM
UT WOS:000299191800021
ER
PT J
AU Loreau, J
Ryabchenko, S
Dalgarno, A
Vaeck, N
AF Loreau, J.
Ryabchenko, S.
Dalgarno, A.
Vaeck, N.
TI Isotope effect in charge-transfer collisions of H with He+
SO PHYSICAL REVIEW A
LA English
DT Article
ID ION-ATOM COLLISIONS; EXCHANGE PROCESSES; ELECTRON-CAPTURE; HYDROGEN;
PLASMAS; HELIUM
AB We present a theoretical study of the isotope effect arising from the replacement of H by T in the charge-transfer collision H(n = 2) + He+(1s) at low energy. Using a quasimolecular approach and a time-dependent wave-packet method, we compute the cross sections for the reaction including the effects of the nonadiabatic radial and rotational couplings. For H(2s) + He+(1s) collisions, we find a strong isotope effect at energies below 1 eV/amu for both singlet and triplet states. We find a much smaller isotopic dependence of the cross section for H(2p) + He+(1s) collisions in triplet states, and no isotope effect in singlet states. We explain the isotope effect on the basis of the potential energy curves and the nonadiabatic couplings, and we evaluate the importance of the isotope effect on the charge-transfer rate coefficients.
C1 [Loreau, J.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
[Ryabchenko, S.] No Arctic Fed Univ, Arkhangelsk 163002, Russia.
[Ryabchenko, S.; Vaeck, N.] Univ Libre Bruxelles, Lab Chim Quant & Photophys, B-1050 Brussels, Belgium.
RP Loreau, J (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, 60 Garden St, Cambridge, MA 02138 USA.
EM nvaeck@ulb.ac.be
RI Ryabchenko, Sergey/B-1720-2012;
OI Ryabchenko, Sergey/0000-0003-1415-1603; Loreau,
Jerome/0000-0002-6142-1509
FU Belgian American Educational Foundation; ARC (ATMOS); IISN; FRFC from
the F.R.S.-FNRS
FX J.L. acknowledges the support of the Belgian American Educational
Foundation. N.V. acknowledges financial support from the ARC (ATMOS),
IISN, and FRFC programs from the F.R.S.-FNRS.
NR 25
TC 7
Z9 7
U1 1
U2 17
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 NOV 22
PY 2011
VL 84
IS 5
AR 052720
DI 10.1103/PhysRevA.84.052720
PG 6
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 851TC
UT WOS:000297292800009
ER
PT J
AU Studds, CE
Marra, PP
AF Studds, Colin E.
Marra, Peter P.
TI Rainfall-induced changes in food availability modify the spring
departure programme of a migratory bird
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE American redstart; climate change; ecological constraint;
microevolution; phenotypic plasticity; Setophaga ruticilla
ID CLIMATE-CHANGE; ARRIVAL DATE; PHENOTYPIC PLASTICITY; ECOLOGICAL
CONDITIONS; SETOPHAGA-RUTICILLA; NONBREEDING SEASON; AMERICAN REDSTARTS;
ANNUAL CYCLE; SONGBIRD; WINTER
AB Climatic warming has intensified selection for earlier reproduction in many organisms, but potential constraints imposed by climate change outside the breeding period have received little attention. Migratory birds provide an ideal model for exploring such constraints because they face warming temperatures on temperate breeding grounds and declining rainfall on many tropical non-breeding areas. Here, we use longitudinal data on spring departure dates of American redstarts (Setophaga ruticilla) to show that annual variation in tropical rainfall and food resources are associated with marked change in the timing of spring departure of the same individuals among years. This finding challenges the idea that photoperiod alone regulates the onset of migration, providing evidence that intensifying drought in the tropical winter could hinder adaptive responses to climatic warming in the temperate zone.
C1 [Studds, Colin E.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
RP Studds, CE (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
EM studdsc@si.edu
RI Studds, Colin/C-3701-2012
FU Cosmos Club Foundation; Wilson Ornithological Society; Smithsonian
Predoctoral Fellowship Programme; National Science Foundation
FX We are grateful to numerous assistants for their dedicated work in the
field. The Cosmos Club Foundation, the Wilson Ornithological Society,
the Smithsonian Predoctoral Fellowship Programme (CES) and the National
Science Foundation (PPM) provided funding this work. We thank the
Petroleum Corporation of Jamaica for permission to conduct this research
at the Font Hill Nature Preserve, and Yvette Strong and Andrea Donaldson
of the Jamaica National Environment and Planning Agency for their
cooperation.
NR 42
TC 81
Z9 81
U1 2
U2 74
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8452
J9 P ROY SOC B-BIOL SCI
JI Proc. R. Soc. B-Biol. Sci.
PD NOV 22
PY 2011
VL 278
IS 1723
BP 3437
EP 3443
DI 10.1098/rspb.2011.0332
PG 7
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 838KW
UT WOS:000296290400016
PM 21450737
ER
PT J
AU Sues, HD
Nesbitt, SJ
Berman, DS
Henrici, AC
AF Sues, Hans-Dieter
Nesbitt, Sterling J.
Berman, David S.
Henrici, Amy C.
TI A late-surviving basal theropod dinosaur from the latest Triassic of
North America
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE Dinosauria; Theropoda; Late Triassic; Chinle Formation; New Mexico
ID EARLY EVOLUTION; ISCHIGUALASTO FORMATION; ARGENTINA; ORIGIN; SAURISCHIA;
SKELETON; SAUROPODOMORPHA; ARCHOSAURS; RADIATION; ONTOGENY
AB The oldest theropod dinosaurs are known from the Carnian of Argentina and Brazil. However, the evolutionary diversification of this group after its initial radiation but prior to the Triassic-Jurassic boundary is still poorly understood because of a sparse fossil record near that boundary. Here, we report on a new basal theropod, Daemonosaurus chauliodus gen. et sp. nov., from the latest Triassic 'siltstone member' of the Chinle Formation of the Coelophysis Quarry at Ghost Ranch, New Mexico. Based on a comprehensive phylogenetic analysis, Daemonosaurus is more closely related to coeval neotheropods (e. g. Coelophysis bauri) than to Herrerasauridae and Eoraptor. The skeletal structure of Daemonosaurus and the recently discovered Tawa bridge a morphological gap between Eoraptor and Herrerasauridae on one hand and neotheropods on the other, providing additional support for the theropod affinities of both Eoraptor and Herrerasauridae and demonstrating that lineages from the initial radiation of Dinosauria persisted until the end of the Triassic. Various features of the skull of Daemonosaurus, including the procumbent dentary and premaxillary teeth and greatly enlarged premaxillary and anterior maxillary teeth, clearly set this taxon apart from coeval neotheropods and demonstrate unexpected disparity in cranial shape among theropod dinosaurs just prior to the end of the Triassic.
C1 [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Nesbitt, Sterling J.] Univ Washington, Dept Biol, Seattle, WA 98195 USA.
[Berman, David S.; Henrici, Amy C.] Carnegie Museum Nat Hist, Sect Vertebrate Paleontol, Pittsburgh, PA 15213 USA.
RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA.
EM suesh@si.edu
FU Natural Sciences and Engineering Research Council (NSERC) of Canada
FX Robert M. Sullivan (State Museum of Pennsylvania, Harrisburg) initially
drew the authors' attention to the specimen. Diane Scott (University of
Toronto at Mississauga) skillfully prepared this specimen; an Operating
Grant from the Natural Sciences and Engineering Research Council (NSERC)
of Canada to H.-D.S. supported her work. We thank Sarah Werning
(University of California at Berkeley) and Mark Loewen (University of
Utah) for providing comparative measurements for some theropod skulls
and the late Chip Clark (National Museum of Natural History) for the
photographs used in figure 1. We gratefully acknowledge discussions with
Randall B. Irmis (University of Utah) concerning theropod phylogeny and
character evolution and helpful comments from Nicholas R. Longrich (Yale
University) and two anonymous referees.
NR 32
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U1 0
U2 10
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 NOV 22
PY 2011
VL 278
IS 1723
BP 3459
EP 3464
DI 10.1098/rspb.2011.0410
PG 6
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 838KW
UT WOS:000296290400019
PM 21490016
ER
PT J
AU Latch, EK
Boarman, WI
Walde, A
Fleischer, RC
AF Latch, Emily K.
Boarman, William I.
Walde, Andrew
Fleischer, Robert C.
TI Fine-Scale Analysis Reveals Cryptic Landscape Genetic Structure in
Desert Tortoises
SO PLOS ONE
LA English
DT Article
ID SPATIAL AUTOCORRELATION ANALYSIS; NORTH-AMERICAN TORTOISES; MULTILOCUS
GENOTYPE DATA; PARTIAL MANTEL TESTS; FALSE DISCOVERY RATE;
GOPHERUS-AGASSIZII; POPULATION-STRUCTURE; MOJAVE DESERT; PHYLOGEOGRAPHIC
PATTERNS; MICROSATELLITE LOCI
AB Characterizing the effects of landscape features on genetic variation is essential for understanding how landscapes shape patterns of gene flow and spatial genetic structure of populations. Most landscape genetics studies have focused on patterns of gene flow at a regional scale. However, the genetic structure of populations at a local scale may be influenced by a unique suite of landscape variables that have little bearing on connectivity patterns observed at broader spatial scales. We investigated fine-scale spatial patterns of genetic variation and gene flow in relation to features of the landscape in desert tortoise (Gopherus agassizii), using 859 tortoises genotyped at 16 microsatellite loci with associated data on geographic location, sex, elevation, slope, and soil type, and spatial relationship to putative barriers (power lines, roads). We used spatially explicit and non-explicit Bayesian clustering algorithms to partition the sample into discrete clusters, and characterize the relationships between genetic distance and ecological variables to identify factors with the greatest influence on gene flow at a local scale. Desert tortoises exhibit weak genetic structure at a local scale, and we identified two subpopulations across the study area. Although genetic differentiation between the subpopulations was low, our landscape genetic analysis identified both natural (slope) and anthropogenic (roads) landscape variables that have significantly influenced gene flow within this local population. We show that desert tortoise movements at a local scale are influenced by features of the landscape, and that these features are different than those that influence gene flow at larger scales. Our findings are important for desert tortoise conservation and management, particularly in light of recent translocation efforts in the region. More generally, our results indicate that recent landscape changes can affect gene flow at a local scale and that their effects can be detected almost immediately.
C1 [Latch, Emily K.] Univ Wisconsin, Dept Biol Sci, Behav & Mol Ecol Res Grp, Milwaukee, WI 53201 USA.
[Latch, Emily K.; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA.
[Boarman, William I.] Conservat Sci Res & Consulting, Spring Valley, VA USA.
[Walde, Andrew] Walde Res & Environm Consulting, Atascadero, CA USA.
RP Latch, EK (reprint author), Univ Wisconsin, Dept Biol Sci, Behav & Mol Ecol Res Grp, POB 413, Milwaukee, WI 53201 USA.
EM latch@uwm.edu
FU United States Department of Defense [W9124J-0-c-0011]
FX The United States Department of Defense funded this work through a grant
to the ITS Corporation, reference code W9124J-0-c-0011. The funders had
no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.
NR 88
TC 15
Z9 15
U1 2
U2 39
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD NOV 21
PY 2011
VL 6
IS 11
AR e27794
DI 10.1371/journal.pone.0027794
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 858IO
UT WOS:000297789900020
PM 22132143
ER
PT J
AU Popescu, EM
AF Popescu, Eugeniu M.
TI Analysis of Kelvin Probe operational models with application to SR-POEM
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID MICROSCOPE; LISA
AB We present a study of several models on which Kelvin Probe (KP) instruments with flat and spherical tips rely for operation and for the determination of the contact potential difference (CPD). The study is part of the development of a high-performance KP instrument that will be used in investigations of the patch effect for the sounding rocket principle of equivalence measurement experiment. Using covariance analysis for each model we investigate its performance as imposed by the Cramer-Rao bounds and the biases introduced in the estimation of the CPD, as well as its applicability to instrument control.
C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Popescu, EM (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St,MS-63, Cambridge, MA 02138 USA.
EM epopescu@cfa.harvard.edu
RI Popescu, Eugeniu/B-7342-2012
FU NASA [NNX08AO04G]
FX This work was supported by the NASA grant NNX08AO04G. The author would
like to thank Robert D Reasenberg and Bijunath R Patla (SAO-CfA) for
useful discussions and suggestions, as well as James P Cowin (PNNL) for
in-depth discussions on the operation of KP instruments.
NR 15
TC 0
Z9 0
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD NOV 21
PY 2011
VL 28
IS 22
AR 225005
DI 10.1088/0264-9381/28/22/225005
PG 14
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 846AN
UT WOS:000296869700006
ER
PT J
AU Reasenberg, RD
Phillips, JD
Popescu, EM
AF Reasenberg, Robert D.
Phillips, James D.
Popescu, Eugeniu M.
TI Test masses for the G-POEM test of the weak equivalence principle
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID GAUGE; EARTH; SPACE
AB We describe the design of the test masses that are used in the 'ground-based principle of equivalence measurement' test of the weak equivalence principle. The main features of the design are the incorporation of corner cubes and the use of mass removal and replacement to create pairs of test masses with different test substances. The corner cubes allow for the vertical separation of the test masses to be measured with picometer accuracy by SAO's unique tracking frequency laser gauge, while the mass removal and replacement operations are arranged so that the test masses incorporating different test substances have nominally identical gravitational properties.
C1 [Reasenberg, Robert D.; Phillips, James D.; Popescu, Eugeniu M.] 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,MS-63, Cambridge, MA 02138 USA.
EM reasenberg@cfa.harvard.edu
RI Popescu, Eugeniu/B-7342-2012
FU NASA SMD [NNC04GB30G, NNX07AI11G, NNX08AO04G]
FX This work was supported in part by the NASA SMD through grants
NNC04GB30G (past) and NNX07AI11G and NNX08AO04G (present). Additional
support came from the Smithsonian.
NR 21
TC 1
Z9 1
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD NOV 21
PY 2011
VL 28
IS 22
AR 225001
DI 10.1088/0264-9381/28/22/225001
PG 7
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 846AN
UT WOS:000296869700002
ER
PT J
AU Buckley-Geer, EJ
Lin, H
Drabek, ER
Allam, SS
Tucker, DL
Armstrong, R
Barkhouse, WA
Bertin, E
Brodwin, M
Desai, S
Frieman, JA
Hansen, SM
High, FW
Mohr, JJ
Lin, YT
Ngeow, CC
Rest, A
Smith, RC
Song, J
Zenteno, A
AF Buckley-Geer, E. J.
Lin, H.
Drabek, E. R.
Allam, S. S.
Tucker, D. L.
Armstrong, R.
Barkhouse, W. A.
Bertin, E.
Brodwin, M.
Desai, S.
Frieman, J. A.
Hansen, S. M.
High, F. W.
Mohr, J. J.
Lin, Y-T
Ngeow, C-C
Rest, A.
Smith, R. C.
Song, J.
Zenteno, A.
TI THE SERENDIPITOUS OBSERVATION OF A GRAVITATIONALLY LENSED GALAXY AT
z=0.9057 FROM THE BLANCO COSMOLOGY SURVEY: THE ELLIOT ARC
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: high-redshift; gravitational lensing: strong; gravitational
lensing: weak
ID DIGITAL SKY SURVEY; XMM-NEWTON OBSERVATION; DARK-MATTER; STAR-FORMATION;
RICHNESS RELATION; LEGACY SURVEY; CLUSTER; WEAK; MASS; MAXBCG
AB We report on the serendipitous discovery in the Blanco Cosmology Survey (BCS) imaging data of a z = 0.9057 galaxy that is being strongly lensed by a massive galaxy cluster at a redshift of z = 0.3838. The lens (BCS J2352-5452) was discovered while examining i- and z-band images being acquired in 2006 October during a BCS observing run. Follow-up spectroscopic observations with the Gemini Multi-Object Spectrograph instrument on the Gemini-South 8 m telescope confirmed the lensing nature of this system. Using weak-plus-strong lensing, velocity dispersion, cluster richness N-200, and fitting to a Navarro-Frenk-White (NFW) cluster mass density profile, we have made three independent estimates of the mass M-200 which are all very consistent with each other. The combination of the results from the three methods gives M-200 = (5.1 +/- 1.3) x 10(14) M-circle dot, which is fully consistent with the individual measurements. The final NFW concentration c(200) from the combined fit is c(200) = 5.4(1.1)(+1.4) We have compared our measurements of M-200 and c(200) with predictions for (1) clusters from ACDM simulations, (2) lensing-selected clusters from simulations, and (3) a real sample of cluster lenses. We find that we are most compatible with the predictions for ACDM simulations for lensing clusters, and we see no evidence based on this one system for an increased concentration compared to ACDM. Finally, using the flux measured from the [O-II]3727 line we have determined the star formation rate of the source galaxy and find it to be rather modest given the assumed lens magnification.
C1 [Buckley-Geer, E. J.; Lin, H.; Drabek, E. R.; Allam, S. S.; Tucker, D. L.; Frieman, J. A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Drabek, E. R.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Armstrong, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Barkhouse, W. A.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA.
[Bertin, E.] Univ Paris 06, Inst Astrophys Paris, UMR CNRS 7095, F-75014 Paris, France.
[Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Desai, S.; Ngeow, C-C] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Frieman, J. A.; High, F. W.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Hansen, S. M.] Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA.
[Hansen, S. M.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
[Mohr, J. J.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Lin, Y-T] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Lin, Y-T] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Ngeow, C-C] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taiwan.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Smith, R. C.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile.
[Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
RP Buckley-Geer, EJ (reprint author), Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA.
OI Tucker, Douglas/0000-0001-7211-5729
FU HST; NASA [11167]; Space Telescope Science Institute; Association of
Universities for Research in Astronomy, Inc., under NASA [NAS5-26555];
Excellence Cluster Universe in Garching; W. M. Keck Foundation; Fermi
Research Alliance, LLC [DE-AC02-07CH11359]; United States Department of
Energy
FX S.S.A. acknowledges support from an HST Grant. Support of program No.
11167 was provided by NASA through a grant from the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS5-26555.; A.Z.
and J.J.M. acknowledge the support of the Excellence Cluster Universe in
Garching. Support for M. B. was provided by the W. M. Keck Foundation.;
Fermilab is operated by Fermi Research Alliance, LLC under Contract No.
DE-AC02-07CH11359 with the United States Department of Energy.
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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 NOV 20
PY 2011
VL 742
IS 1
AR 48
DI 10.1088/0004-637X/742/1/48
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400048
ER
PT J
AU Dunham, MM
Chen, XP
Arce, HG
Bourke, TL
Schnee, S
Enoch, ML
AF Dunham, Michael M.
Chen, Xuepeng
Arce, Hector G.
Bourke, Tyler L.
Schnee, Scott
Enoch, Melissa L.
TI DETECTION OF A BIPOLAR MOLECULAR OUTFLOW DRIVEN BY A CANDIDATE FIRST
HYDROSTATIC CORE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (Per-Bolo 58); ISM: jets and outflows; stars:
formation; stars: low-mass
ID SPITZER-SPACE-TELESCOPE; STAR-FORMING REGIONS; PROTOSTELLAR CORES; DENSE
CORE; C2D SURVEY; SUBMILLIMETER ARRAY; INTERSTELLAR CLOUDS; LINE
FORMATION; HH 211; PERSEUS
AB We present new 230 GHz Submillimeter Array observations of the candidate first hydrostatic core Per-Bolo 58. We report the detection of a 1.3 mm continuum source and a bipolar molecular outflow, both centered on the position of the candidate first hydrostatic core. The continuum detection has a total flux density of 26.6 +/- 4.0 mJy, from which we calculate a total (gas and dust) mass of 0.11 +/- 0.05 M-circle dot and a mean number density of 2.0 +/- 1.6 x 10(7) cm(-3). There is some evidence for the existence of an unresolved component in the continuum detection, but longer-baseline observations are required in order to confirm the presence of this component and determine whether its origin lies in a circumstellar disk or in the dense inner envelope. The bipolar molecular outflow is observed along a nearly due east-west axis. The outflow is slow (characteristic velocity of 2.9 km s(-1)), shows a jet-like morphology (opening semi-angles similar to 8 degrees for both lobes), and extends to the edges of the primary beam. We calculate the kinematic and dynamic properties of the outflow in the standard manner and compare them to several other protostars and candidate first hydrostatic cores with similarly low luminosities. We discuss the evidence both in support of and against the possibility that Per-Bolo 58 is a first hydrostatic core, and we outline future work needed to further evaluate the evolutionary status of this object.
C1 [Dunham, Michael M.; Chen, Xuepeng; Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Schnee, Scott] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Enoch, Melissa L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Dunham, MM (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA.
EM michael.dunham@yale.edu
FU Smithsonian Institution; Academia Sinica; NSF [AST-0845619]; NASA
[NXX09AB89G]
FX The authors extend their gratitude to the anonymous referee for comments
and suggestions that have improved the quality of this work. We also
thank the SMA staff for executing these observations as part of the
queue schedule, and Charlie Qi for his assistance with MIR and MIRIAD.
This work is based primarily on observations obtained with the
Submillimeter Array, a joint project between the Smithsonian
Astrophysical Observatory and the Academia Sinica Institute of Astronomy
and Astrophysics and funded by the Smithsonian Institution and the
Academia Sinica. This research has made use of NASA's Astrophysics Data
System (ADS) Abstract Service and of the SIMBAD database, operated at
CDS, Strasbourg, France. Support for this work was provided by the NSF
through grant AST-0845619 to H.G.A. T.L.B. acknowledges support from
NASA Origins grant NXX09AB89G.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
VL 742
IS 1
AR 1
DI 10.1088/0004-637X/742/1/1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400001
ER
PT J
AU Elias-Rosa, N
Van Dyk, SD
Li, WD
Silverman, JM
Foley, RJ
Ganeshalingam, M
Mauerhan, JC
Kankare, E
Jha, S
Filippenko, AV
Beckman, JE
Berger, E
Cuillandre, JC
Smith, N
AF Elias-Rosa, Nancy
Van Dyk, Schuyler D.
Li, Weidong
Silverman, Jeffrey M.
Foley, Ryan J.
Ganeshalingam, Mohan
Mauerhan, Jon C.
Kankare, Erkki
Jha, Saurabh
Filippenko, Alexei V.
Beckman, John E.
Berger, Edo
Cuillandre, Jean-Charles
Smith, Nathan
TI THE MASSIVE PROGENITOR OF THE POSSIBLE TYPE II-LINEAR SUPERNOVA 2009hd
IN MESSIER 66
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 3627); stars: evolution; supernovae: general;
supernovae: individual (SN 2009hd)
ID EXPANDING PHOTOSPHERE METHOD; SN 2008S; INFRARED OBSERVATIONS; STELLAR
PHOTOMETRY; IA SUPERNOVA; P SUPERNOVAE; LIGHT CURVES; SPECTROSCOPY;
EVOLUTION; 1999EM
AB We present early- and late-time photometric and spectroscopic observations of supernova (SN) 2009hd in the nearby spiral galaxy NGC 3627 (M66). This SN is one of the closest to us in recent years and provides an uncommon opportunity to observe and study the nature of SNe. However, the object was heavily obscured by dust, rendering it unusually faint in the optical given its proximity. We find that the observed properties of SN 2009hd support its classification as a possible Type II-Linear SN (SN II-L), a relatively rare subclass of core-collapse SNe. High-precision relative astrometry has been employed to attempt to identify an SN progenitor candidate, based on a pixel-by-pixel comparison between Hubble Space Telescope (HST) F555W and F814W images of the SN site prior to explosion and at late times. A progenitor candidate is identified in the F814W images only; this object is undetected in F555W. Significant uncertainty exists in the astrometry, such that we cannot definitively identify this object as the SN progenitor. Via insertion of artificial stars into the pre-SN HST images, we are able to constrain the progenitor's properties to those of a possible supergiant, with intrinsic absolute magnitude M-F555W(0) greater than or similar to -7.6 mag and intrinsic color (V - I)(0) greater than or similar to 0.99 mag. The magnitude and color limits are consistent with a luminous red supergiant (RSG); however, they also allow for the possibility that the star could have been more yellow than red. From a comparison with theoretical massive-star evolutionary tracks which include rotation and pulsationally enhanced mass loss, we can place a conservative upper limit on the initial mass for the progenitor of M-ini less than or similar to 20 M-circle dot. If the actual mass of the progenitor is near the upper range allowed by our derived mass limit, then it would be consistent with that for the identified progenitors of the SN II-L 2009kr and the high-luminosity SN II-Plateau (II-P) 2008cn. The progenitors of these three SNe may possibly bridge the gap between lower-mass RSGs that explode as SNe II-P and luminous blue variables, or more extreme RSGs, from which the more exotic SNe II-narrow may arise. Very late time imaging of the SN 2009hd site may provide us with more clues regarding the true nature of its progenitor.
C1 [Elias-Rosa, Nancy; Van Dyk, Schuyler D.; Mauerhan, Jon C.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Elias-Rosa, Nancy; Li, Weidong; Silverman, Jeffrey M.; Ganeshalingam, Mohan; Filippenko, Alexei V.; Smith, Nathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Elias-Rosa, Nancy] Fac Ciencies, Inst Ciencies LOEspai IEEC CSIC, Bellaterra 08193, Spain.
[Foley, Ryan J.; Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kankare, Erkki] Univ Turku, Dept Phys & Astron, Tuorla Observ, Piikkio 21500, Finland.
[Kankare, Erkki] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Spain.
[Jha, Saurabh] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Beckman, John E.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Beckman, John E.] CSIC, Madrid, Spain.
[Cuillandre, Jean-Charles] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA.
[Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Elias-Rosa, N (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
EM nelias@ice.csic.es
RI Elias-Rosa, Nancy/D-3759-2014;
OI Elias-Rosa, Nancy/0000-0002-1381-9125; Van Dyk,
Schuyler/0000-0001-9038-9950
FU NASA [NAS 05-26555]; UK Science and Technology Facilities Council; W. M.
Keck Foundation; MICINN [AYA08-1839/ESP]; ESF EUROCORES Program
[EUI2009-04170]; Generalitat de Catalunya; EU; National Science
Foundation [AST-0908886]; TABASGO Foundation; Space Telescope Science
Institute [AR-11248, AR-12126, GO-11575]
FX This research is based in part on observations made with the NASA/ESA
Hubble Space Telescope, obtained from the Data Archive at the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy (AURA), Inc., under NASA contract
NAS 05-26555; the SMARTS Consortium 1.3 m telescope located at Cerro
Tololo Inter-American Observatory (CTIO), Chile; the 1.5 m telescope
located at Palomar Observatory; the Liverpool Telescope operated on the
island of La Palma by Liverpool John Moores University in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
de Canarias with financial support from the UK Science and Technology
Facilities Council; the Nordic Optical Telescope, operated on the island
of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in
the Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofisica de Canarias; the 6.5 m Magellan Clay and Baade telescopes
located at Las Campanas Observatory, Chile; and the W. M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
NASA, with generous financial support from the W. M. Keck Foundation. We
are grateful to the staffs at these observatories for their excellent
assistance with the observations.; N.E.R. thanks Stefano Benetti and
Alberto Noriega-Crespo for useful discussions and Avet Harutyunyan for
his help. Many of the spectra used here for comparison were obtained
from the Padova-Asiago Supernova Archive (ASA). This work 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. This work has been supported by the MICINN grant
AYA08-1839/ESP, by the ESF EUROCORES Program EuroGENESIS (MICINN grant
EUI2009-04170), by SGR grants of the Generalitat de Catalunya, and by
EU-FEDER funds.; The research of A.V.F.'s supernova group has been
generously supported by National Science Foundation grant AST-0908886
and the TABASGO Foundation, as well as by NASA through grants AR-11248,
AR-12126, and GO-11575 from the Space Telescope Science Institute, which
is operated by AURA, Inc., under NASA contract NAS 5-26555.
NR 81
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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 NOV 20
PY 2011
VL 742
IS 1
AR 6
DI 10.1088/0004-637X/742/1/6
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400006
ER
PT J
AU Grav, T
Mainzer, AK
Bauer, J
Masiero, J
Spahr, T
McMillan, RS
Walker, R
Cutri, R
Wright, E
Eisenhardt, PRM
Blauvelt, E
DeBaun, E
Elsbury, D
Gautier, T
Gomillion, S
Hand, E
Wilkins, A
AF Grav, T.
Mainzer, A. K.
Bauer, J.
Masiero, J.
Spahr, T.
McMillan, R. S.
Walker, R.
Cutri, R.
Wright, E.
Eisenhardt, P. R. M.
Blauvelt, E.
DeBaun, E.
Elsbury, D.
Gautier, T.
Gomillion, S.
Hand, E.
Wilkins, A.
TI WISE/NEOWISE OBSERVATIONS OF THE JOVIAN TROJANS: PRELIMINARY RESULTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; minor planets, asteroids: general; surveys
ID INFRARED-SURVEY-EXPLORER; NEAR-EARTH ASTEROIDS; SOLAR-SYSTEM;
SPECTROSCOPIC SURVEY; SIZE DISTRIBUTION; THERMAL-MODEL; JUPITER; ORIGIN;
POPULATION; PHOTOMETRY
AB We present the preliminary analysis of over 1739 known and 349 candidate Jovian Trojans observed by the NEOWISE component of the Wide-field Infrared Survey Explorer (WISE). With this survey the available diameters, albedos, and beaming parameters for the Jovian Trojans have been increased by more than an order of magnitude compared to previous surveys. We find that the Jovian Trojan population is very homogenous for sizes larger than similar to 10 km (close to the detection limit of WISE for these objects). The observed sample consists almost exclusively of low albedo objects, having a mean albedo value of 0.07 +/- 0.03. The beaming parameter was also derived for a large fraction of the observed sample, and it is also very homogenous with an observed mean value of 0.88 +/- 0.13. Preliminary debiasing of the survey shows that our observed sample is consistent with the leading cloud containing more objects than the trailing cloud. We estimate the fraction to be N(leading)/N(trailing) similar to 1.4 +/- 0.2, lower than the 1.6 +/- 0.1 value derived by Szabo et al.
C1 [Grav, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Mainzer, A. K.; Bauer, J.; Masiero, J.; Eisenhardt, P. R. M.; Blauvelt, E.; DeBaun, E.; Elsbury, D.; Gautier, T.; Gomillion, S.; Hand, E.; Wilkins, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J.; Cutri, R.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[McMillan, R. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Walker, R.] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Wright, E.] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA.
[Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Grav, T (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM tgrav@pha.jhu.edu
OI Blauvelt, Erin/0000-0002-2944-5818; 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 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 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
VL 742
IS 1
AR 40
DI 10.1088/0004-637X/742/1/40
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400040
ER
PT J
AU Hartman, JD
Bakos, GA
Torres, G
Latham, DW
Kovacs, G
Beky, B
Quinn, SN
Mazeh, T
Shporer, A
Marcy, GW
Howard, AW
Fischer, DA
Johnson, JA
Esquerdo, GA
Noyes, RW
Sasselov, DD
Stefanik, RP
Fernandez, JM
Szklenar, T
Lazar, J
Papp, I
Sari, P
AF Hartman, J. D.
Bakos, G. A.
Torres, G.
Latham, D. W.
Kovacs, Geza
Beky, B.
Quinn, S. N.
Mazeh, T.
Shporer, A.
Marcy, G. W.
Howard, A. W.
Fischer, D. A.
Johnson, J. A.
Esquerdo, G. A.
Noyes, R. W.
Sasselov, D. D.
Stefanik, R. P.
Fernandez, J. M.
Szklenar, T.
Lazar, J.
Papp, I.
Sari, P.
TI HAT-P-32b AND HAT-P-33b: TWO HIGHLY INFLATED HOT JUPITERS TRANSITING
HIGH-JITTER STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HAT-P-32, GSC 3281-00800,
HAT-P-33, GSC 2461-00988); techniques: photometric; techniques:
spectroscopic
ID EXTRASOLAR PLANETS; ECCENTRIC ORBIT; ECLIPSING BINARIES; GIANT PLANETS;
MAGNETIC ACTIVITY; SPECTRAL-ANALYSIS; TIDAL EVOLUTION; BLEND SCENARIOS;
MASSIVE PLANET; OPEN CLUSTERS
AB We report the discovery of two exoplanets transiting high-jitter stars. HAT-P-32b orbits the bright V = 11.289 late-F-early-G dwarf star GSC 3281-00800, with a period P = 2.150008 +/- 0.000001 d. The stellar and planetary masses and radii depend on the eccentricity of the system, which is poorly constrained due to the high-velocity jitter (similar to 80 m s(-1)). Assuming a circular orbit, the star has a mass of 1.16 +/- 0.04 M-circle dot and radius of 1.22 +/- 0.02 R-circle dot, while the planet has a mass of 0.860 +/- 0.164 M-J and a radius of 1.789 +/- 0.025 R-J. The second planet, HAT-P-33b, orbits the bright V = 11.188 late-F dwarf star GSC 2461-00988, with a period P = 3.474474 +/- 0.000001 d. As for HAT-P-32, the stellar and planetary masses and radii of HAT-P-33 depend on the eccentricity, which is poorly constrained due to the high jitter (similar to 50 m s(-1)). In this case, spectral line bisector spans (BSs) are significantly anti-correlated with the radial velocity residuals, and we are able to use this correlation to reduce the residual rms to similar to 35ms(-1). We find that the star has a mass of 1.38 +/- 0.04 M-circle dot and a radius of 1.64 +/- 0.03 R-circle dot while the planet has a mass of 0.762 +/- 0.101 M-J and a radius of 1.686 +/- 0.045 R-J for an assumed circular orbit. Due to the large BS variations exhibited by both stars we rely on detailed modeling of the photometric light curves to rule out blend scenarios. Both planets are among the largest radii transiting planets discovered to date.
C1 [Hartman, J. D.; Bakos, G. A.; Torres, G.; Latham, D. W.; Beky, B.; Quinn, S. N.; Esquerdo, G. A.; Noyes, R. W.; Sasselov, D. D.; Stefanik, R. P.; Szklenar, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary.
[Mazeh, T.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Shporer, A.] LCOGT, Santa Barbara, CA USA.
[Shporer, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Marcy, G. W.; Howard, A. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Fernandez, J. M.] Univ Gottingen, Inst Astrophys, Gottingen, Germany.
[Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary.
RP Hartman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM gbakos@cfa.harvard.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Hartman, Joel/0000-0001-8732-6166;
Fischer, Debra/0000-0003-2221-0861
FU NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G, N128Hr, N145Hr, N049Hr,
N018Hr, N167Hr, N029Hr]; SAO IRD grants; NSF [AST-0702843, AST-0702821];
Kepler Mission under NASA [NCC2-1390]; Hungarian Scientific Research
Foundation (OTKA) [K-81373]; NOAO [A285Hr, A146Hr, A201Hr, A289Hr,
G329Hr]
FX HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G
and SAO IR&D grants. Works of G.A.B. and J. J. were supported by the
Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program
(AST-0702843 and AST-0702821, respectively). G. T. acknowledges partial
support from NASA grant NNX09AF59G. We acknowledge partial support also
from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (PI:
D. W. L.). 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 (A285Hr, A146Hr, A201Hr,
A289Hr), NASA (N128Hr, N145Hr, N049Hr, N018Hr, N167Hr, N029Hr), and the
NOAO Gemini/Keck time-exchange program (G329Hr). We gratefully
acknowledge F. Bouchy, F. Pont, and the SOPHIE team for their efforts in
gathering OHP/SOPHIE observations of HAT-P-33.
NR 79
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
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IS 1
AR 59
DI 10.1088/0004-637X/742/1/59
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400059
ER
PT J
AU Hollek, JK
Frebel, A
Roederer, IU
Sneden, C
Shetrone, M
Beers, TC
Kang, SJ
Thom, C
AF Hollek, Julie K.
Frebel, Anna
Roederer, Ian U.
Sneden, Christopher
Shetrone, Matthew
Beers, Timothy C.
Kang, Sung-ju
Thom, Christopher
TI THE CHEMICAL ABUNDANCES OF STARS IN THE HALO (CASH) PROJECT. II. A
SAMPLE OF 14 EXTREMELY METAL-POOR STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: halo; methods: data analysis; stars: abundances; stars:
atmospheres; stars: Population II
ID HOBBY-EBERLY TELESCOPE; NEUTRON-CAPTURE ELEMENTS; RED GIANT BRANCH;
EARLY GALAXY; HAMBURG/ESO SURVEY; 1ST STARS; SPECTROSCOPIC ANALYSIS;
STELLAR ARCHAEOLOGY; SPITE PLATEAU; SURVEY HERES
AB We present a comprehensive abundance analysis of 20 elements for 16 new low-metallicity stars from the Chemical Abundances of Stars in the Halo (CASH) project. The abundances have been derived from both Hobby-Eberly Telescope High Resolution Spectrograph snapshot spectra (R similar to 15,000) and corresponding high-resolution (R similar to 35,000) Magellan Inamori Kyocera Echelle spectra. The stars span a metallicity range from [Fe/H] from -2.9 to -3.9, including four new stars with [Fe/H] < -3.7. We find four stars to be carbon-enhanced metal-poor (CEMP) stars, confirming the trend of increasing [C/Fe] abundance ratios with decreasing metallicity. Two of these objects can be classified as CEMP-no stars, adding to the growing number of these objects at [Fe/H]< -3. We also find four neutron-capture-enhanced stars in the sample, one of which has [Eu/Fe] of 0.8 with clear r-process signatures. These pilot sample stars are the most metal-poor ([Fe/H] less than or similar to -3.0) of the brightest stars included in CASH and are used to calibrate a newly developed, automated stellar parameter and abundance determination pipeline. This code will be used for the entire similar to 500 star CASH snapshot sample. We find that the pipeline results are statistically identical for snapshot spectra when compared to a traditional, manual analysis from a high-resolution spectrum.
C1 [Hollek, Julie K.; Sneden, Christopher; Shetrone, Matthew] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Frebel, Anna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Roederer, Ian U.] Carnegie Observat, Pasadena, CA 91101 USA.
[Shetrone, Matthew] Univ Texas, McDonald Observ, Ft Davis, TX 78734 USA.
[Beers, Timothy C.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Beers, Timothy C.] Michigan State Univ, JINA, E Lansing, MI 48824 USA.
[Kang, Sung-ju] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Thom, Christopher] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Hollek, JK (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM julie@astro.as.utexas.edu; afrebel@cfa.harvard.edu;
iur@obs.carnegiescience.edu; chris@astro.as.utexas.edu;
shetrone@astro.as.utexas.edu; beers@pa.msu.edu; sjkang@iastate.edu;
cthom@stsci.edu
FU Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA)
[PHY 02-16783, PHY 0822648]; Carnegie Institution of Washington; NSF
[AST-0908978]
FX The Hobby-Eberly Telescope (HET) is a joint project of the University of
Texas at Austin, the Pennsylvania State University, Stanford University,
Ludwig-Maximilians-Universitt Mnchen, and Georg-August-Universitt
Gttingen. The HET is named in honor of its principal benefactors,
William P. Hobby and Robert E. Eberly. We are grateful to the
Hobby-Eberly staff for their assistance in obtaining the data collected
for this paper. We thank John Norris and Norbert Christlieb for their
valuable contributions to the discovery of the bright metal-poor stars
analyzed here. J.K.H. and T. C. B. acknowledge partial support through
grants PHY 02-16783 and PHY 0822648: Physics Frontier Center/Joint
Institute for Nuclear Astrophysics (JINA). A. F. acknowledges support of
a Clay Fellowship administered by the Smithsonian Astrophysical
Observatory. I. U. R. is supported by the Carnegie Institution of
Washington through the Carnegie Observatories Fellowship. C. S. is
supported through NSF grant AST-0908978.
NR 74
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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 NOV 20
PY 2011
VL 742
IS 1
AR 54
DI 10.1088/0004-637X/742/1/54
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400054
ER
PT J
AU Sicilia-Aguilar, A
Henning, T
Dullemond, CP
Patel, N
Juhasz, A
Bouwman, J
Sturm, B
AF Sicilia-Aguilar, Aurora
Henning, Thomas
Dullemond, Cornelis P.
Patel, Nimesh
Juhasz, Attila
Bouwman, Jeroen
Sturm, Bernhard
TI DUST PROPERTIES AND DISK STRUCTURE OF EVOLVED PROTOPLANETARY DISKS IN
Cep OB2: GRAIN GROWTH, SETTLING, GAS AND DUST MASS, AND INSIDE-OUT
EVOLUTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE open clusters and associations: individual (Cep OB2); protoplanetary
disks; stars: late-type; stars: pre-main sequence
ID T-TAURI STARS; SPITZER-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS;
INTERSTELLAR SILICATE MINERALOGY; INFRARED SPECTROGRAPH SURVEY; GIANT
PLANET FORMATION; YOUNG STELLAR OBJECTS; HERBIG AE/BE SYSTEMS;
MAIN-SEQUENCE STARS; NE-II EMISSION
AB We present Spitzer/Infrared Spectrograph spectra of 31 T Tauri stars (TTS) and IRAM/1.3 mm observations for 34 low-and intermediate-mass stars in the Cep OB2 region. Including our previously published data, we analyze 56 TTS and 3 intermediate-mass stars with silicate features in Tr 37 (similar to 4 Myr) and NGC 7160 (similar to 12 Myr). The silicate emission features are well reproduced with a mixture of amorphous (with olivine, forsterite, and silica stoichiometry) and crystalline grains (forsterite, enstatite). We explore grain size and disk structure using radiative transfer disk models, finding that most objects have suffered substantial evolution (grain growth, settling). About half of the disks show inside-out evolution, with either dust-cleared inner holes or a radially dependent dust distribution, typically with larger grains and more settling in the innermost disk. The typical strong silicate features nevertheless require the presence of small dust grains, and could be explained by differential settling according to grain size, anomalous dust distributions, and/or optically thin dust populations within disk gaps. M-type stars tend to have weaker silicate emission and steeper spectral energy distributions than K-type objects. The inferred low dust masses are in a strong contrast with the relatively high gas accretion rates, suggesting global grain growth and/or an anomalous gas-to-dust ratio. Transition disks in the Cep OB2 region display strongly processed grains, suggesting that they are dominated by dust evolution and settling. Finally, the presence of rare but remarkable disks with strong accretion at old ages reveals that some very massive disks may still survive to grain growth, gravitational instabilities, and planet formation.
C1 [Sicilia-Aguilar, Aurora; Henning, Thomas; Dullemond, Cornelis P.; Bouwman, Jeroen; Sturm, Bernhard] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Sicilia-Aguilar, Aurora] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain.
[Dullemond, Cornelis P.] Univ Heidelberg, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany.
[Patel, Nimesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Juhasz, Attila] Leiden Observ, NL-2333 CA Leiden, Netherlands.
RP Sicilia-Aguilar, A (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM sicilia@mpia.de
OI Dullemond, Cornelis/0000-0002-7078-5910
FU Deutsche Forschungsgemeinschaft (DFG) [SI1486/1-1]; National Aeronautics
and Space Administration; National Science Foundation
FX We thank R. Zylka for his help with the IRAM observations and data
reduction, in particular, his MOPSIC scripts. We are also indebted to F.
Lahuis for his helpwith the reduction of high-resolution IRS spectra,
and the Spitzer Science Center Helpdesk for their help with the MOPEX
software. We also thank A. Martinez-Sansigre and V. Roccatagliata for
their participation in the IRAM observations, and the referee for the
careful report that helped to clarify our paper. A. S.-A. acknowledges
support from the Deutsche Forschungsgemeinschaft (DFG) grant SI1486/1-1.
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. It also
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 110
TC 24
Z9 25
U1 0
U2 3
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 NOV 20
PY 2011
VL 742
IS 1
AR 39
DI 10.1088/0004-637X/742/1/39
PG 35
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400039
ER
PT J
AU Walker, MG
Penarrubia, J
AF Walker, Matthew G.
Penarrubia, Jorge
TI A METHOD FOR MEASURING (SLOPES OF) THE MASS PROFILES OF DWARF SPHEROIDAL
GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: dwarf; galaxies: fundamental parameters;
galaxies: kinematics and dynamics
ID DARK-MATTER HALOS; CA II TRIPLET; MILKY-WAY SATELLITES; SURFACE
BRIGHTNESS GALAXIES; UNIVERSAL DENSITY PROFILE; TO-LIGHT RATIOS; LOCAL
GROUP; PROPER MOTIONS; RADIAL-VELOCITIES; URSA-MINOR
AB We introduce a method for measuring the slopes of mass profiles within dwarf spheroidal (dSph) galaxies directly from stellar spectroscopic data and without adopting a dark matter halo model. Our method combines two recent results: (1) spherically symmetric, equilibrium Jeans models imply that the product of half-light radius and (squared) stellar velocity dispersion provides an estimate of the mass enclosed within the half-light radius of a dSph stellar component, and (2) some dSphs have chemodynamically distinct stellar subcomponents that independently trace the same gravitational potential. We devise a statistical method that uses measurements of stellar positions, velocities, and spectral indices to distinguish two dSph stellar subcomponents and to estimate their individual half-light radii and velocity dispersions. For a dSph with two detected stellar subcomponents, we obtain estimates of masses enclosed at two discrete points in the same mass profile, immediately defining a slope. Applied to published spectroscopic data, our method distinguishes stellar subcomponents in the Fornax and Sculptor dSphs, for which we measure slopes Gamma equivalent to Delta log M/Delta log r = 2.61(-0.37)(+0.43) and Gamma = 2.95(-0.39)(+0.51), respectively. These values are consistent with "cores" of constant density within the central few hundred parsecs of each galaxy and rule out "cuspy" Navarro-Frenk-White (NFW) profiles (d log M/d log r <= 2 at all radii) with a significance greater than or similar to 96% and greater than or similar to 99%, respectively. Tests with synthetic data indicate that our method tends systematically to overestimate the mass of the inner stellar subcomponent to a greater degree than that of the outer stellar subcomponent, and therefore to underestimate the slope Gamma (implying that the stated NFW exclusion levels are conservative).
C1 [Walker, Matthew G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Walker, Matthew G.; Penarrubia, Jorge] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP Walker, MG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mwalker@cfa.harvard.edu
RI Walker, Matthew/P-1777-2014
OI Walker, Matthew/0000-0003-2496-1925
FU Institute of Astronomy (IoA), Cambridge; STFC; NASA [HST-HF-51283.01-A];
Space Telescope Science Institute [NAS5-26555]
FX M.G.W.'s debts to Mario Mateo and Ed Olszewski are immeasurable. On
behalf of the Dwarf Investigative Network (DwaIN), we are grateful to
Mark Wilkinson for providing synthetic data sets which we used to
perform initial tests of our method. We thank Gerry Gilmore and
colleagues at the Institute of Astronomy (IoA), Cambridge, for support
and inspiration. We thank Alan McConnachie, Justin Read, George Lake,
and John Magorrian for helpful discussions and comments. We thank
Bodhisattva Sen for guidance regarding statistical issues. We thank the
anonymous referee for suggestions that helped to improve this
manuscript. We thank the IoA for inviting us to teach a graduate seminar
on Dwarf Galaxies and Cosmology during Winter 2010, when the ideas
developed here were formed. M.G.W. and J.P. acknowledge support from the
STFC-funded Galaxy Formation and Evolution programme at the IoA. M.G.W.
is currently supported by NASA through Hubble Fellowship grant
HST-HF-51283.01-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 NAS5-26555.
NR 124
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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 NOV 20
PY 2011
VL 742
IS 1
AR 20
DI 10.1088/0004-637X/742/1/20
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400020
ER
PT J
AU Wang, JF
Fabbiano, G
Elvis, M
Risaliti, G
Karovska, M
Zezas, A
Mundell, CG
Dumas, G
Schinnerer, E
AF Wang, Junfeng
Fabbiano, Giuseppina
Elvis, Martin
Risaliti, Guido
Karovska, Margarita
Zezas, Andreas
Mundell, Carole G.
Dumas, Gaelle
Schinnerer, Eva
TI A DEEP CHANDRA ACIS STUDY OF NGC 4151. III. THE LINE EMISSION AND
SPECTRAL ANALYSIS OF THE IONIZATION CONE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 4151); galaxies: ISM; galaxies: Seyfert; ISM:
jets and outflows; X-rays: galaxies
ID SOFT-X-RAY; SEYFERT-GALAXY NGC-4151; ACTIVE GALACTIC NUCLEUS; H-I;
GEMINI NIFS; MASS OUTFLOWS; WARM OUTFLOW; GAS-DYNAMICS; RADIO JET; MRK
573
AB This paper is the third in a series in which we present deep Chandra ACIS-S imaging spectroscopy of the Seyfert 1 galaxy NGC 4151, devoted to study its complex circumnuclear X-ray emission. Emission features in the soft X-ray spectrum of the bright extended emission (L0.3-2 keV similar to 10(40) erg s(-1)) at r > 130 pc (2 '') are consistent with blended brighter O VII, O VIII, and Ne IX lines seen in the Chandra HETGS and XMM-Newton RGS spectra below 2 keV. We construct emission line images of these features and find good morphological correlations with the narrow-line region clouds mapped in [O III] lambda 5007. Self-consistent photoionization models provide good descriptions of the spectra of the large-scale emission, as well as resolved structures, supporting the dominant role of nuclear photoionization, although displacement of optical and X-ray features implies a more complex medium. Collisionally ionized emission is estimated to be less than or similar to 12% of the extended emission. Presence of both low- and high-ionization spectral components and extended emission in the X-ray image perpendicular to the bicone indicates leakage of nuclear ionization, likely filtered through warm absorbers, instead of being blocked by a continuous obscuring torus. The ratios of [O III]/soft X-ray flux are approximately constant (similar to 15) for the 1.5 kpc radius spanned by these measurements, indicating similar relative contributions from the low- and high-ionization gas phases at different radial distances from the nucleus. If the [O III] and X-ray emission arise from a single photoionized medium, this further implies an outflow with a wind-like density profile. Using spatially resolved X-ray features, we estimate that the mass outflow rate in NGC 4151 is similar to 2 M-circle dot yr(-1) at 130 pc and the kinematic power of the ionized outflow is 1.7 x 10(41) erg s(-1), approximately 0.3% of the bolometric luminosity of the active nucleus in NGC 4151.
C1 [Wang, Junfeng; Fabbiano, Giuseppina; Elvis, Martin; Risaliti, Guido; Karovska, Margarita; Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Risaliti, Guido] INAF Arcetri Observ, I-50125 Florence, Italy.
[Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece.
[Mundell, Carole G.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Dumas, Gaelle; Schinnerer, Eva] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Wang, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM juwang@cfa.harvard.edu
RI Zezas, Andreas/C-7543-2011;
OI Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X;
Schinnerer, Eva/0000-0002-3933-7677
FU NASA [GO8-9101X, GO1-12009X, NAS8-03060, NAS5-26555]; CXC; Royal Society
and Research Councils UK; DFG [SCH 536/4-1, SCH 536/4-2, SPP 1177.]
FX We thank the anonymous referee for providing us with detailed and
constructive comments that have improved the clarity of this manuscript.
This work is supported by NASA grants GO8-9101X and GO1-12009X. We
acknowledge support from the CXC, which is operated by the Smithsonian
Astrophysical Observatory (SAO) for and on behalf of NASA under Contract
NAS8-03060. C. G. M. acknowledges financial support from the Royal
Society and Research Councils UK. G. D. was supported by DFG grants SCH
536/4-1 and SCH 536/4-2 as part of SPP 1177. J.W. thanks T. Kallman, G.
Ferland, S. Bianchi, A. Marinucci, and S. Chakravorty for advice on
photoionization modeling. This research has made use of data obtained
from the Chandra Data Archive, and software provided by the CXC in the
application packages CIAO and Sherpa. Some of the data presented in this
paper were obtained from the Multimission Archive at the Space Telescope
Science Institute (MAST). STScI is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract
NAS5-26555.
NR 77
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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 NOV 20
PY 2011
VL 742
IS 1
AR 23
DI 10.1088/0004-637X/742/1/23
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400023
ER
PT J
AU Youdin, AN
AF Youdin, Andrew N.
TI THE EXOPLANET CENSUS: A GENERAL METHOD APPLIED TO KEPLER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: statistical; planetary systems; planets and satellites:
detection; planets and satellites: dynamical evolution and stability;
planets and satellites: formation
ID EXTRASOLAR PLANETS; GRAVITATIONAL-INSTABILITY; PLANETESIMAL FORMATION;
LOW-MASS; METALLICITY; CANDIDATES; COMPANION; SOLAR; STAR
AB We develop a general method to fit the underlying planetary distribution function (PLDF) to exoplanet survey data. This maximum likelihood method accommodates more than one planet per star and any number of planet or target star properties. We apply the method to announced Kepler planet candidates that transit solar-type stars. The Kepler team's estimates of the detection efficiency are used and are shown to agree with theoretical predictions for an ideal transit survey. The PLDF is fit to a joint power law in planet radius, down to 0.5 R(circle plus), and orbital period, up to 50 days. The estimated number of planets per star in this sample is similar to 0.7-1.4, where the range covers systematic uncertainties in the detection efficiency. To analyze trends in the PLDF we consider four planet samples, divided between shorter and longer periods at 7 days and between large and small radii at 3 R(circle plus). The size distribution changes appreciably between these four samples, revealing a relative deficit of similar to 3 R(circle plus). planets at the shortest periods. This deficit is suggestive of preferential evaporation and sublimation of Neptune-and Saturn-like planets. If the trend and explanation hold, it would be spectacular observational support of the core accretion and migration hypotheses, and would allow refinement of these theories.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Youdin, AN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-16, Cambridge, MA 02138 USA.
RI Youdin, Andrew/C-1596-2013
OI Youdin, Andrew/0000-0002-3644-8726
FU NASA [NNX10AF35G]; Smithsonian Institute
FX Scott Kenyon's advice and encouragement made this paper possible. I
thank Kevin Schlaufman for making Tables 1 and 2 of Borucki et al.
(2011) available in ascii format at http://www.ucolick.org/similar to
kcs/research/planets/kepler_table.dat. I am very grateful to Elisabeth
Adams, Jean-Michel Desert, Andrew Howard, Matt Holman, Jonathan Irwin,
and Darin Ragozzine for insightful discussions and to all responsible
for maintaining the venue of these conversations: the daily SSP coffee
at the CfA. This project was supported by the NASA Astrophysics Theory
Program and Origins of Solar Systems Program through grant NNX10AF35G
and by endowment funds of the Smithsonian Institute.
NR 34
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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 NOV 20
PY 2011
VL 742
IS 1
AR 38
DI 10.1088/0004-637X/742/1/38
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400038
ER
PT J
AU Zhao, JH
Wright, MCH
AF Zhao, Jun-Hui
Wright, M. C. H.
TI SAGITTARIUS B2 MAIN: A CLUSTER OF ULTRA-COMPACT H-II REGIONS AND MASSIVE
PROTOSTELLAR CORES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: center; H II regions; ISM: individual objects (Sgr B2); radio
continuum: ISM; radio lines: ISM; stars: formation
ID STAR-FORMING REGION; GRAVITATIONAL COLLAPSE; COMPETITIVE ACCRETION;
RECOMBINATION LINES; CONTINUUM OBSERVATIONS; MOLECULAR CLOUDS; UPPER
LIMIT; PARAMETERS; TURBULENT; HYDROGEN
AB The ionized core in the Sgr B2 Main star-forming region was imaged using the Submillimeter Array archival data observed for the H26 alpha line and continuum emission at 0.86 mm with an angular resolution 0.'' 3. Eight hyper-compact H26a emission sources were detected with a typical size in the range of 1.6-20 x 10(2) AU and electron density of 0.3-3 x 10(7) cm(-3), corresponding to the emission measure 0.4-8.4 x 10(10) cm(-6) pc. The H26 alpha line fluxes from the eight hyper-compact H II sources imply that the ionization for each of the sources must be powered by a Lyman continuum flux from an O star or a cluster of B stars. The most luminous H26a source among the eight detected sources requires an O6 star that appears to be embedded in the ultra-compact H II region F3. In addition, similar to 23 compact continuum emission sources were also detected within the central 5 '' x 3 '' (similar to 0.2 pc) region. Under the assumption of a power-law distribution for the dust temperature, with the observed brightness temperature of the dust emission we determined the physical properties of the submillimeter emission sources, showing that the molecular densities are in the range of 1-10 x 10(8) cm(-3), surface densities between 13 and 150 g cm(-2), and total gas masses in the range from 5 to greater than or similar to 200 M-circle dot, which are one or two orders of magnitude greater than the corresponding values of the Bonnor-Ebert mass. With a mean free-fall timescale of 2 x 10(3) years, each of the massive protostellar cores is undergoing gravitational collapse to form new massive stars in the Sgr B2 Main core.
C1 [Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wright, M. C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Zhao, JH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jzhao@cfa.harvard.edu
NR 57
TC 1
Z9 1
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 20
PY 2011
VL 742
IS 1
AR 50
DI 10.1088/0004-637X/742/1/50
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844WW
UT WOS:000296783400050
ER
PT J
AU Andrews, SM
Rosenfeld, KA
Wilner, DJ
Bremer, M
AF Andrews, Sean M.
Rosenfeld, Katherine A.
Wilner, David J.
Bremer, Michael
TI A CLOSER LOOK AT THE LkCa 15 PROTOPLANETARY DISK
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; planet-disk interactions; protoplanetary disks;
stars: individual (LkCa 15); submillimeter: planetary systems
ID TRANSITIONAL DISKS; CIRCUMSTELLAR DISKS; GIANT PLANET; YOUNG; EVOLUTION;
MIGRATION; GAP; MWC-480; SYSTEMS; HOLES
AB We present 870 mu m observations of dust continuum emission from the LkCa 15 protoplanetary disk at high angular resolution (with a characteristic scale of 0 ''.25 = 35 AU), obtained with the IRAM Plateau de Bure interferometer and supplemented by slightly lower resolution observations from the Submillimeter Array. We fit these data with simple morphological models to characterize the spectacular ring-like emission structure of this disk. Our analysis indicates that a small amount of 870 mu m dust emission (similar to 5 mJy) originates inside a large (40-50 AU radius) low optical depth cavity. This result can be interpreted either in the context of an abrupt decrease by a factor of similar to 5 in the radial distribution of millimeter-sized dust grains or as indirect evidence for a gap in the disk, in agreement with previous inferences from the unresolved infrared spectrum and scattered light images. A preliminary model focused on the latter possibility suggests the presence of a low-mass (planetary) companion, having properties commensurate with those inferred from the recent discovery of LkCa 15b.
C1 [Andrews, Sean M.; Rosenfeld, Katherine A.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bremer, Michael] IRAM, F-38406 St Martin Dheres, France.
RP Andrews, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Smithsonian Institution;
Academia Sinica
FX We are very grateful to Adam Kraus for his advice and for kindly sharing
results prior to publication. This article is based on observations
carried out with the IRAM Plateau de Bure Interferometer and the
Submillimeter Array. IRAM is supported by INSU/CNRS (France), MPG
(Germany), and IGN (Spain). 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.
NR 32
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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 NOV 20
PY 2011
VL 742
IS 1
AR L5
DI 10.1088/2041-8205/742/1/L5
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QY
UT WOS:000296763600005
ER
PT J
AU Huang, JS
Zheng, XZ
Rigopoulou, D
Magdis, G
Fazio, GG
Wang, T
AF Huang, J. -S.
Zheng, X. Z.
Rigopoulou, D.
Magdis, G.
Fazio, G. G.
Wang, T.
TI FOUR IRAC SOURCES WITH AN EXTREMELY RED H - [3.6] COLOR: PASSIVE OR
DUSTY GALAXIES AT z > 4.5?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: evolution; galaxies: formation;
galaxies: high-redshift; infrared: galaxies
ID NEAR-INFRARED OBSERVATIONS; STAR-FORMING GALAXIES; Z-SIMILAR-TO-6
QUASARS; SPECTROSCOPY; DEEP; ULTRAVIOLET; CONSTRAINTS; POPULATION;
RESOLUTION; OBJECTS
AB We report the detection of four IRAC sources in the GOODS-South field with an extremely red color of H - [3.6] > 4.5. The four sources are not detected in the deep Hubble Space Telescope WFC3 H-band image with H-limit = 28.3 mag. We find that only three types of SED templates can produce such a red H -[3.6] color: a very dusty SED with the Calzetti extinction of A(V) = 16 mag at z = 0.8; a very dusty SED with the SMC extinction of AV = 8 mag at z = 2.0-2.2; and an 1 Gyr SSP with A(V) similar to 0.8 at z = 5.7. We argue that these sources are unlikely dusty galaxies at z <= 2.2 based on absent strong MIPS 24 mu m emission. The old stellar population model at z > 4.5 remains a possible solution for the 4 sources. At z > 4.5, these sources have stellar masses of log(M-*/M-circle dot) = 10.6-11.2. One source, ERS-1, is also a type-II X-ray QSO with L2-8 (keV) = 1.6 x 10(44) er gs(-1). One of the four sources is an X-ray QSO and another one is a HyperLIRG, suggesting a galaxy-merging scenario for the formation of these massive galaxies at high redshifts.
C1 [Huang, J. -S.; Fazio, G. G.; Wang, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zheng, X. Z.] Acad Sinica, Purple Mt Observ, Nanjing 210008, Jiangsu Provinc, Peoples R China.
[Rigopoulou, D.; Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Wang, T.] Nanjing Univ, Dept Astron, Nanjing 210008, Jiangsu Provinc, Peoples R China.
RP Huang, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Magdis, Georgios/C-7295-2014
OI Magdis, Georgios/0000-0002-4872-2294
FU NASA [1407, NAS 5-26555]
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, and with
the NASA/ESA HST obtained at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS 5-26555.
NR 48
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U1 0
U2 10
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 NOV 20
PY 2011
VL 742
IS 1
AR L13
DI 10.1088/2041-8205/742/1/L13
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QY
UT WOS:000296763600013
ER
PT J
AU Lorenzen, ED
Nogues-Bravo, D
Orlando, L
Weinstock, J
Binladen, J
Marske, KA
Ugan, A
Borregaard, MK
Gilbert, MTP
Nielsen, R
Ho, SYW
Goebel, T
Graf, KE
Byers, D
Stenderup, JT
Rasmussen, M
Campos, PF
Leonard, JA
Koepfli, KP
Froese, D
Zazula, G
Stafford, TW
Aaris-Sorensen, K
Batra, P
Haywood, AM
Singarayer, JS
Valdes, PJ
Boeskorov, G
Burns, JA
Davydov, SP
Haile, J
Jenkins, DL
Kosintsev, P
Kuznetsova, T
Lai, XL
Martin, LD
McDonald, HG
Mol, D
Meldgaard, M
Munch, K
Stephan, E
Sablin, M
Sommer, RS
Sipko, T
Scott, E
Suchard, MA
Tikhonov, A
Willerslev, R
Wayne, RK
Cooper, A
Hofreiter, M
Sher, A
Shapiro, B
Rahbek, C
Willerslev, E
AF Lorenzen, Eline D.
Nogues-Bravo, David
Orlando, Ludovic
Weinstock, Jaco
Binladen, Jonas
Marske, Katharine A.
Ugan, Andrew
Borregaard, Michael K.
Gilbert, M. Thomas P.
Nielsen, Rasmus
Ho, Simon Y. W.
Goebel, Ted
Graf, Kelly E.
Byers, David
Stenderup, Jesper T.
Rasmussen, Morten
Campos, Paula F.
Leonard, Jennifer A.
Koepfli, Klaus-Peter
Froese, Duane
Zazula, Grant
Stafford, Thomas W., Jr.
Aaris-Sorensen, Kim
Batra, Persaram
Haywood, Alan M.
Singarayer, Joy S.
Valdes, Paul J.
Boeskorov, Gennady
Burns, James A.
Davydov, Sergey P.
Haile, James
Jenkins, Dennis L.
Kosintsev, Pavel
Kuznetsova, Tatyana
Lai, Xulong
Martin, Larry D.
McDonald, H. Gregory
Mol, Dick
Meldgaard, Morten
Munch, Kasper
Stephan, Elisabeth
Sablin, Mikhail
Sommer, Robert S.
Sipko, Taras
Scott, Eric
Suchard, Marc A.
Tikhonov, Alexei
Willerslev, Rane
Wayne, Robert K.
Cooper, Alan
Hofreiter, Michael
Sher, Andrei
Shapiro, Beth
Rahbek, Carsten
Willerslev, Eske
TI Species-specific responses of Late Quaternary megafauna to climate and
humans
SO NATURE
LA English
DT Article
ID PLEISTOCENE EXTINCTIONS; POPULATION-DYNAMICS; WOOLLY MAMMOTHS; STEPPE;
INFERENCE; PATTERNS; AMERICA; DECLINE; RECORD; CANADA
AB Despite decades of research, the roles of climate and humans in driving the dramatic extinctions of large-bodied mammals during the Late Quaternary period remain contentious. Here we use ancient DNA, species distribution models and the human fossil record to elucidate how climate and humans shaped the demographic history of woolly rhinoceros, woolly mammoth, wild horse, reindeer, bison and musk ox. We show that climate has been a major driver of population change over the past 50,000 years. However, each species responds differently to the effects of climatic shifts, habitat redistribution and human encroachment. Although climate change alone can explain the extinction of some species, such as Eurasian musk ox and woolly rhinoceros, a combination of climatic and anthropogenic effects appears to be responsible for the extinction of others, including Eurasian steppe bison and wild horse. We find no genetic signature or any distinctive range dynamics distinguishing extinct from surviving species, emphasizing the challenges associated with predicting future responses of extant mammals to climate and human-mediated habitat change.
C1 [Lorenzen, Eline D.; Orlando, Ludovic; Weinstock, Jaco; Binladen, Jonas; Gilbert, M. Thomas P.; Stenderup, Jesper T.; Rasmussen, Morten; Campos, Paula F.; Stafford, Thomas W., Jr.; Aaris-Sorensen, Kim; Haile, James; Meldgaard, Morten; Willerslev, Eske] Univ Copenhagen, Ctr GeoGenet, DK-1350 Copenhagen K, Denmark.
[Nogues-Bravo, David; Marske, Katharine A.; Borregaard, Michael K.; Rahbek, Carsten] Univ Copenhagen, Dept Biol, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark.
[Ugan, Andrew] Smithsonian Trop Res Inst, Ancon, Punama, Panama.
[Nielsen, Rasmus] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Nielsen, Rasmus] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA.
[Nielsen, Rasmus] Univ Copenhagen, Dept Biol, DK-2200 Copenhagen, Denmark.
[Ho, Simon Y. W.] Univ Sydney, Sch Biol Sci, Sydney, NSW 2006, Australia.
[Goebel, Ted; Graf, Kelly E.] Texas A&M Univ, Dept Anthropol, Ctr Study Amer 1, College Stn, TX 77843 USA.
[Byers, David] Missouri State Univ, Dept Sociol & Anthropol, Springfield, MO 65807 USA.
[Leonard, Jennifer A.] Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden.
[Leonard, Jennifer A.] EBD CSIC, Conservat & Evolutionary Genet Grp, Seville 41092, Spain.
[Koepfli, Klaus-Peter; Wayne, Robert K.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Koepfli, Klaus-Peter] NCI, Lab Genom Divers, Frederick, MD 21702 USA.
[Froese, Duane] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
[Zazula, Grant] Govt Yukon, Dept Tourism & Culture, Yukon Palaeontol Program, Whitehorse, YT Y1A 2C6, Canada.
[Stafford, Thomas W., Jr.] Stafford Res Inc, Lafayette, CO 80026 USA.
[Batra, Persaram] Mt Holyoke Coll, Dept Earth & Environm, S Hadley, MA 01075 USA.
[Haywood, Alan M.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Singarayer, Joy S.; Valdes, Paul J.] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Boeskorov, Gennady] Russian Acad Sci, Siberian Branch, Diamond & Precious Met Geol Inst, Yakutsk 677891, Russia.
[Burns, James A.] Royal Alberta Museum, Edmonton, AB T5N 0M6, Canada.
[Burns, James A.] Manitoba Museum, Winnipeg, MB R3B 0N2, Canada.
[Davydov, Sergey P.] Russian Acad Sci, Far E Branch, Pacific Inst Geog, NE Sci Stn, Chersky 678830, Russia.
[Jenkins, Dennis L.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA.
[Kosintsev, Pavel] Russian Acad Sci, Ural Branch, Inst Plant & Anim Ecol, Ekaterinburg 620144, Russia.
[Kuznetsova, Tatyana] Moscow MV Lomonosov State Univ, Moscow 119899, Russia.
[Lai, Xulong] China Univ Geosci, State Key Lab Biogeol & Environm Geol, Wuhan 430074, Hubei, Peoples R China.
[Martin, Larry D.] Univ Kansas, Museum Nat Hist, Lawrence, KS 66045 USA.
[McDonald, H. Gregory] Natl Pk Serv, Pk Museum Management Program, Ft Collins, CO 80525 USA.
[Mol, Dick] Nat Hist Museum, Rotterdam, Netherlands.
[Munch, Kasper] Aarhus Univ, BiRC, DK-8000 Aarhus C, Denmark.
[Stephan, Elisabeth] Landesamt Denkmalpflege, Regierungsprasidium Stuttgart, D-78467 Constance, Germany.
[Sablin, Mikhail; Tikhonov, Alexei] Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia.
[Sommer, Robert S.] Univ Kiel, Inst Nat & Resource Conservat, Dept Landscape Ecol, D-24098 Kiel, Germany.
[Sipko, Taras; Sher, Andrei] Russian Acad Sci, Inst Ecol & Evolut, Moscow 119071, Russia.
[Scott, Eric] San Bernardino Cty Museum, Div Geol Sci, Redlands, CA 92374 USA.
[Suchard, Marc A.] Univ Calif Los Angeles, David Geffen Sch Med, Dept Biomath Genet, Los Angeles, CA 90095 USA.
[Suchard, Marc A.] Univ Calif Los Angeles, David Geffen Sch Med, Dept Human Genet, Los Angeles, CA 90095 USA.
[Suchard, Marc A.] Univ Calif Los Angeles, Sch Publ Hlth, Dept Biostat, Los Angeles, CA 90095 USA.
[Willerslev, Rane] Univ Oslo, Museum Cultural Hist, N-0130 Oslo, Norway.
[Cooper, Alan] Univ Adelaide, Australian Ctr Ancient DNA, Adelaide, SA 5005, Australia.
[Hofreiter, Michael] Univ York, Dept Biol, Area 2, York YO10 5DD, N Yorkshire, England.
[Shapiro, Beth] Penn State Univ, Dept Biol, University Pk, PA 16802 USA.
[Ugan, Andrew] Univ Utah, Dept Anthropol, Salt Lake City, UT 84112 USA.
[Ugan, Andrew] Museo Hist Nat San Rafael, Mendoza, Argentina.
RP Willerslev, E (reprint author), Univ Copenhagen, Ctr GeoGenet, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark.
EM ewillerslev@snm.ku.dk
RI CSIC, EBD Donana/C-4157-2011; Borregaard, Michael/B-8442-2008; Leonard,
Jennifer/A-7894-2010; publist, CMEC/C-3010-2012; Hofreiter,
Michael/A-3996-2017; publicationpage, cmec/B-4405-2017; Munch,
Kasper/A-1434-2010; Ho, Simon/A-8417-2008; Campos, Paula/B-1634-2010;
Koroleva, Olga/C-1306-2012; Cooper, Alan/E-8171-2012; Lorenzen,
Eline/D-1442-2012; Orlando, Ludovic/A-8932-2013; Gilbert,
Marcus/A-8936-2013; Nielsen, Rasmus/D-4405-2009; Valdes,
Paul/C-4129-2013; Rahbek, Carsten/D-9372-2013; Rahbek,
Carsten/L-1129-2013; Marske, Katharine/J-5962-2014;
OI CSIC, EBD Donana/0000-0003-4318-6602; Borregaard,
Michael/0000-0002-8146-8435; Leonard, Jennifer/0000-0003-0291-7819;
Hofreiter, Michael/0000-0003-0441-4705; Sablin,
Mikhail/0000-0002-2773-7454; Munch, Kasper/0000-0003-2880-6252; Ho,
Simon/0000-0002-0361-2307; Campos, Paula/0000-0003-1285-4671; Cooper,
Alan/0000-0002-7738-7851; Lorenzen, Eline/0000-0002-6353-2819; Orlando,
Ludovic/0000-0003-3936-1850; Gilbert, Marcus/0000-0002-5805-7195;
Nielsen, Rasmus/0000-0003-0513-6591; Marske,
Katharine/0000-0002-9837-9367; Shapiro, Beth/0000-0002-2733-7776
FU Leverhulme Trust [F/757/A]; McDonald Grants and Awards Fund; NSF
[ARC-0909456]; Danish National Research Foundation; Lundbeck Foundation;
Danish Council for Independent Research; US National Science Foundation
FX This paper is in memory of our friend and colleague Andrei Sher, who was
a contributor to this study. Dr Sher died unexpectedly, but his major
contributions to the field of Quaternary science will be remembered and
appreciated for many years. We are grateful to A. Lister and T. Stuart
for guidance and discussions. We thank T. B. Brandt, B. Hockett and A.
Telka for laboratory help and samples, and L. M. R. Thrane for his work
on the megafauna locality database. Data taken from the Stage 3 project
were partly funded by grant F/757/A from the Leverhulme Trust, and a
grant from the McDonald Grants and Awards Fund. B. S. was supported by
NSF ARC-0909456. We acknowledge the Danish National Research Foundation,
the Lundbeck Foundation, the Danish Council for Independent Research and
the US National Science Foundation for financial support.
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PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD NOV 17
PY 2011
VL 479
IS 7373
BP 359
EP U195
DI 10.1038/nature10574
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 848OA
UT WOS:000297059700037
PM 22048313
ER
PT J
AU Lee, X
Goulden, ML
Hollinger, DY
Barr, A
Black, TA
Bohrer, G
Bracho, R
Drake, B
Goldstein, A
Gu, LH
Katul, G
Kolb, T
Law, BE
Margolis, H
Meyers, T
Monson, R
Munger, W
Oren, R
Kyaw, TPU
Richardson, AD
Schmid, HP
Staebler, R
Wofsy, S
Zhao, L
AF Lee, Xuhui
Goulden, Michael L.
Hollinger, David Y.
Barr, Alan
Black, T. Andrew
Bohrer, Gil
Bracho, Rosvel
Drake, Bert
Goldstein, Allen
Gu, Lianhong
Katul, Gabriel
Kolb, Thomas
Law, Beverly E.
Margolis, Hank
Meyers, Tilden
Monson, Russell
Munger, William
Oren, Ram
Kyaw Tha Paw U
Richardson, Andrew D.
Schmid, Hans Peter
Staebler, Ralf
Wofsy, Steven
Zhao, Lei
TI Observed increase in local cooling effect of deforestation at higher
latitudes
SO NATURE
LA English
DT Article
ID SCALE DEFORESTATION; GLOBAL CLIMATE; BOREAL FOREST; LAND-USE;
VEGETATION; ENERGY; EXCHANGE; ALBEDO; WATER
AB Deforestation in mid-to high latitudes is hypothesized to have the potential to cool the Earth's surface by altering biophysical processes(1-3). In climate models of continental-scale land clearing, the cooling is triggered by increases in surface albedo and is reinforced by a land albedo-sea ice feedback(4,5). This feedback is crucial in the model predictions; without it other biophysical processes may overwhelm the albedo effect to generate warming instead(5). Ongoing land-use activities, such as land management for climate mitigation, are occurring at local scales (hectares) presumably too small to generate the feedback, and it is not known whether the intrinsic biophysical mechanism on its own can change the surface temperature in a consistent manner(6,7). Nor has the effect of deforestation on climate been demonstrated over large areas from direct observations. Here we show that surface air temperature is lower in open land than in nearby forested land. The effect is 0.85 +/- 0.44 K (mean +/- one standard deviation) northwards of 45 degrees N and 0.21 +/- 0.53 K southwards. Below 35 degrees N there is weak evidence that deforestation leads to warming. Results are based on comparisons of temperature at forested eddy covariance towers in the USA and Canada and, as a proxy for small areas of cleared land, nearby surface weather stations. Night-time temperature changes unrelated to changes in surface albedo are an important contributor to the overall cooling effect. The observed latitudinal dependence is consistent with theoretical expectation of changes in energy loss from convection and radiation across latitudes in both the daytime and night-time phase of the diurnal cycle, the latter of which remains uncertain in climate models(8).
C1 [Lee, Xuhui; Zhao, Lei] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
[Goulden, Michael L.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Hollinger, David Y.] US Forest Serv, USDA, No Res Stn, Durham, NH 03824 USA.
[Barr, Alan] Environm Canada, Div Climate Res, Saskatoon, SK S7N 3H5, Canada.
[Black, T. Andrew] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada.
[Bohrer, Gil] Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA.
[Bracho, Rosvel] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA.
[Drake, Bert] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Goldstein, Allen] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
[Gu, Lianhong] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA.
[Katul, Gabriel; Oren, Ram] Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA.
[Kolb, Thomas] No Arizona Univ, Sch Forestry, Flagstaff, AZ 86011 USA.
[Law, Beverly E.] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Margolis, Hank] Univ Laval, Fac Foresterie Geog & Geomat, Ctr Etud Foret, Quebec City, PQ G1V 0A6, Canada.
[Meyers, Tilden] NOAA ARL ATDD, Oak Ridge, TN 37830 USA.
[Monson, Russell] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
[Munger, William; Wofsy, Steven] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Kyaw Tha Paw U] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
[Richardson, Andrew D.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Schmid, Hans Peter] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-82467 Garmisch Partenkirchen, Germany.
[Staebler, Ralf] Environm Canada, Proc Res Sect, Toronto, ON M3H 5T4, Canada.
RP Lee, X (reprint author), Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
EM xuhui.lee@yale.edu
RI Goldstein, Allen/A-6857-2011; Gu, Lianhong/H-8241-2014; Law,
Beverly/G-3882-2010; Richardson, Andrew/F-5691-2011; Katul,
Gabriel/A-7210-2008; Hollinger, David/G-7185-2012; Schmid, Hans
Peter/I-1224-2012; Bohrer, Gil/A-9731-2008; Garmisch-Pa,
Ifu/H-9902-2014; Barr, Alan/H-9939-2014; Meyers, Tilden/C-6633-2016;
OI Goldstein, Allen/0000-0003-4014-4896; Gu, Lianhong/0000-0001-5756-8738;
Law, Beverly/0000-0002-1605-1203; Richardson,
Andrew/0000-0002-0148-6714; Katul, Gabriel/0000-0001-9768-3693; Schmid,
Hans Peter/0000-0001-9076-4466; Bohrer, Gil/0000-0002-9209-9540
FU US Department of Energy; Yale University Climate and Energy Institute
FX The data collection and analysis were supported in part by grants from
the US Department of Energy and by a Yale University Climate and Energy
Institute grant. We thank D. Fitzjarrald and R. Sakai for providing the
data for the KM77 tropical site and C. von Randow for providing the
friction velocity data for FLUXNET cluster e.
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PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD NOV 17
PY 2011
VL 479
IS 7373
BP 384
EP 387
DI 10.1038/nature10588
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 848OA
UT WOS:000297059700042
PM 22094699
ER
PT J
AU Meickle, T
Gunasekera, SP
Liu, YX
Luesch, H
Paul, VJ
AF Meickle, Theresa
Gunasekera, Sarath P.
Liu, Yanxia
Luesch, Hendrik
Paul, Valerie J.
TI Porpoisamides A and B, two novel epimeric cyclic depsipeptides from a
Florida Keys collection of Lyngbya sp.
SO BIOORGANIC & MEDICINAL CHEMISTRY
LA English
DT Article
DE Cyanobacteria; Lyngbya majuscula; Depsipeptides; Porpoisamide
ID AMINO-ACIDS; MARINE CYANOBACTERIA; NATURAL-PRODUCTS; CYCLODEPSIPEPTIDES;
CONFIGURATION; SPECTROMETRY; CONFERVOIDES; MAJUSCULA
AB NMR-guided fractionation of a non-polar extract of a Florida Keys collection of Lyngbya sp. resulted in the isolation of two novel epimeric cyclic depsipeptides, porpoisamides A (1) and B (2). The planar structures of these compounds were determined using NMR spectroscopic techniques. The absolute configurations of amino and hydroxy acid subunits were assigned by enantioselective HPLC analysis. These compounds showed weak cytotoxicity towards HCT-116 colorectal carcinoma and U2OS osteosarcoma cells. The porpoisamides are a unique pair of cyclic depsipeptides that are epimeric at C-2 of the beta-amino acid, 3-amino-2-methyloctanoic acid. Published by Elsevier Ltd.
C1 [Meickle, Theresa; Gunasekera, Sarath P.; Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.
[Meickle, Theresa] Florida Atlantic Univ, Dept Chem, Boca Raton, FL 33431 USA.
[Liu, Yanxia; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA.
RP Paul, VJ (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM paul@si.edu
FU National Institutes of Health, NIGMS [P41GM086210]
FX This research was supported by the National Institutes of Health, NIGMS
Grant P41GM086210. We are grateful for the use of the 600 MHz NMR
spectrometer at Harbor Branch Oceanographic Institute at Florida
Atlantic University. We also thank the Florida Atlantic University,
Jupiter Campus, for use of their polarimeter and infrared spectrometer.
HRMS analyses were performed at the UCR Mass Spectrometry Facility,
Department of Chemistry, University of California at Riverside. This is
contribution # 849 of the Smithsonian Marine Station at Fort Pierce.
NR 16
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U1 1
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0968-0896
J9 BIOORGAN MED CHEM
JI Bioorg. Med. Chem.
PD NOV 15
PY 2011
VL 19
IS 22
BP 6576
EP 6580
DI 10.1016/j.bmc.2011.05.051
PG 5
WC Biochemistry & Molecular Biology; Chemistry, Medicinal; Chemistry,
Organic
SC Biochemistry & Molecular Biology; Pharmacology & Pharmacy; Chemistry
GA 841TI
UT WOS:000296535900004
PM 21705224
ER
PT J
AU McCoy, TJ
Walker, RJ
Goldstein, JI
Yang, J
McDonough, WF
Rumble, D
Chabot, NL
Ash, RD
Corrigan, CM
Michael, JR
Kotula, PG
AF McCoy, T. J.
Walker, R. J.
Goldstein, J. I.
Yang, J.
McDonough, W. F.
Rumble, D.
Chabot, N. L.
Ash, R. D.
Corrigan, C. M.
Michael, J. R.
Kotula, P. G.
TI Group IVA irons: New constraints on the crystallization and cooling
history of an asteroidal core with a complex history
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID SILICATE PARTITION-COEFFICIENTS; OXYGEN-ISOTOPE ANALYSIS; SIDEROPHILE
ELEMENTS; RE-187-OS-187 SYSTEMATICS; SOLAR-SYSTEM; PARENT BODY;
STONY-IRON; THERMAL EVOLUTION; MASS-SPECTROMETRY; METEORITES
AB We report analyses of 14 group IVA iron meteorites, and the ungrouped but possibly related, Elephant Moraine (EET) 83230, for siderophile elements by laser ablation ICP-MS and isotope dilution. EET was also analyzed for oxygen isotopic composition and metallographic structure, and Fuzzy Creek, currently the IVA with the highest Ni concentration, was analyzed for metallographic structure. Highly siderophile elements (HSE) Re, Os and Ir concentrations vary by nearly three orders of magnitude over the entire range of IVA irons, while Ru, Pt and Pd vary by less than factors of five. Chondrite normalized abundances of HSE form nested patterns consistent with progressive crystal-liquid fractionation. Attempts to collectively model the HSE abundances resulting from fractional crystallization achieved best results for 3 wt.% S, compared to 0.5 or 9 wt.% S. Consistent with prior studies, concentrations of HSE and other refractory siderophile elements estimated for the bulk IVA core and its parent body are in generally chondritic proportions. Projected abundances of Pd and Au, relative to more refractory HSE, are slightly elevated and modestly differ from L/LL chondrites, which some have linked with group IVA, based on oxygen isotope similarities.
Abundance trends for the moderately volatile and siderophile element Ga cannot be adequately modeled for any S concentration, the cause of which remains enigmatic. Further, concentrations of some moderately volatile and siderophile elements indicate marked, progressive depletions in the IVA system. However, if the IVA core began crystallization with similar to 3 wt.% S, depletions of more volatile elements cannot be explained as a result of prior volatilization/condensation processes. The initial IVA core had an approximately chondritic Ni/Co ratio, but a fractionated Fe/Ni ratio of similar to 10, indicates an Fe-depleted core. This composition is most easily accounted for by assuming that the surrounding silicate shell was enriched in iron, consistent with an oxidized parent body. The depletions in Ga may reflect decreased siderophilic behavior in a relatively oxidized body, and more favorable partitioning into the silicate portion of the parent body.
Phosphate inclusions in EET show Delta(17)O values within the range measured for silicates in IVA iron meteorites. EET has a typical ataxitic microstructure with precipitates of kamacite within a matrix of plessite. Chemical and isotopic evidence for a genetic relation between EET and group IVA is strong, but the high Ni content and the newly determined, rapid cooling rate of this meteorite show that it should continue to be classified as ungrouped. Previously reported metallographic cooling rates for IVA iron meteorites have been interpreted to indicate an inwardly crystallizing, similar to 150 km radius metallic body with little or no silicate mantle. Hence, the IVA group was likely formed as a mass of molten metal separated from a much larger parent body that was broken apart by a large impact. Given the apparent genetic relation with IVA, EET was most likely generated via crystal-liquid fractionation in another, smaller body spawned from the same initial liquid during the impact event that generated the IVA body. Published by Elsevier Ltd.
C1 [McCoy, T. J.; Corrigan, C. M.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Walker, R. J.; McDonough, W. F.; Ash, R. D.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA.
[Goldstein, J. I.; Yang, J.] Univ Massachusetts, Engn Lab 313, Dept Mech & Ind Engn, Amherst, MA 01003 USA.
[Rumble, D.] Geophys Lab, Washington, DC 20015 USA.
[Chabot, N. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Michael, J. R.; Kotula, P. G.] Sandia Natl Labs, Mat Characterizat Dept, Albuquerque, NM 87185 USA.
RP McCoy, TJ (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM mccoyt@si.edu
RI Kotula, Paul/A-7657-2011; McDonough, William/C-4791-2009; Chabot,
Nancy/F-5384-2015; McDonough, William/I-7720-2012; Walker,
Richard/K-6869-2016
OI Kotula, Paul/0000-0002-7521-2759; McDonough,
William/0000-0001-9154-3673; Chabot, Nancy/0000-0001-8628-3176;
McDonough, William/0000-0001-9154-3673; Walker,
Richard/0000-0003-0348-2407
FU NASA [NNG06GF56G, NNX07AM29G, NNX10AG94G, NNX08AG53G, NNX09AG90G,
NNX08AH76G]
FX Funding for this work was provided by NASA Grants NNG06GF56G (to
T.J.M.), NNX07AM29G and NNX10AG94G (to R.J.W.), NNX08AG53G (to J.I.G.),
NNX09AG90G (to N.L.C.) and NNX08AH76G (to W. F. M.) which is gratefully
acknowledged. The authors thank Janne Blichert-Toft for the sample of
Muonionalusta.
NR 73
TC 28
Z9 28
U1 2
U2 33
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 NOV 15
PY 2011
VL 75
IS 22
BP 6821
EP 6843
DI 10.1016/j.gca.2011.09.006
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 842FQ
UT WOS:000296579600006
ER
PT J
AU Cernusak, LA
Hutley, LB
Beringer, J
Holtum, JAM
Turner, BL
AF Cernusak, Lucas A.
Hutley, Lindsay B.
Beringer, Jason
Holtum, Joseph A. M.
Turner, Benjamin L.
TI Photosynthetic physiology of eucalypts along a sub-continental rainfall
gradient in northern Australia
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Carbon-isotope discrimination; Leaf mass per area; Photosynthetic
capacity; Rainfall gradient; Savanna
ID CARBON-ISOTOPE DISCRIMINATION; WATER-USE EFFICIENCY; TROPICAL PIONEER
TREE; 2 COMMON GARDENS; STOMATAL CONDUCTANCE; MESOPHYLL CONDUCTANCE;
TRANSPIRATION EFFICIENCY; NITROGEN NUTRITION; BIOCHEMICAL-MODEL; CO2
ASSIMILATION
AB Leaf-level photosynthetic parameters of species in the closely related genera Eucalyptus and Corymbia were assessed along a strong rainfall gradient in northern Australia. Both instantaneous gas exchange measurements and leaf carbon isotope discrimination indicated little variation in intercellular CO(2) concentrations during photosynthesis (c(i)) in response to a decrease in mean annual precipitation from similar to 1700 mm to similar to 300 mm. Correlation between stomatal conductance and photosynthetic capacity contributed toward the maintenance of relatively constant c(i) among the sampled leaves, when assessed at ambient CO(2) concentration and photon irradiance similar to full sunlight. Leaf mass per area was the most plastic leaf trait along the rainfall gradient, showing a linear increase in response to decreasing mean annual precipitation. The maximum Rubisco carboxylation velocity, V(cmax), expressed on a leaf-area basis, showed a modest increase in response to decreasing rainfall. This modest increase in V(cmax) was associated with the strongly expressed increase in leaf mass per area. These results suggest that variation in ecosystem-level gas exchange during the dry season in north-Australian savannas will likely be dominated by changes in leaf area index in response to increasing aridity, rather than by changes in photosynthetic performance per unit leaf area. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Cernusak, Lucas A.; Hutley, Lindsay B.] Charles Darwin Univ, Sch Environm & Life Sci, Darwin, NT 0909, Australia.
[Hutley, Lindsay B.] Charles Darwin Univ, Sch Environm Res, Darwin, NT 0909, Australia.
[Beringer, Jason] Monash Univ, Sch Geog & Environm Sci, Clayton, Vic 3800, Australia.
[Holtum, Joseph A. M.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia.
[Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Cernusak, LA (reprint author), Charles Darwin Univ, Sch Environm & Life Sci, Darwin, NT 0909, Australia.
EM lcernusak@gmail.com
RI Turner, Benjamin/E-5940-2011; Hutley, Lindsay/A-7925-2011; Holtum,
Joseph/B-3063-2012; Cernusak, Lucas/A-6859-2011; Research ID, CTBCC
/O-3564-2014; Beringer, Jason/B-8528-2008
OI Turner, Benjamin/0000-0002-6585-0722; Hutley,
Lindsay/0000-0001-5533-9886; Holtum, Joseph/0000-0001-6568-8019;
Cernusak, Lucas/0000-0002-7575-5526; Beringer, Jason/0000-0002-4619-8361
FU Australian Research Council [DP0344744, DP0772981, DP0771427]
FX Financial support for this research was provided by two Discovery grants
from the Australian Research Council (DP0344744 and DP0772981). Lucas A.
Cernusak was supported by a Post-doctoral Fellowship provided by the
Australian Research Council (DP0771427). We are grateful to the NT
Government and landowners who kindly provided access to their properties
and resources (Theona Station, Newcastle Waters Station, Nenen Station,
and the NT Governement' s Douglas Daly Research Farm). We thank David
Ellsworth (University of Western Sydney) for the loan of a portable
photosynthesis system for use during the measurement campaign.
NR 76
TC 28
Z9 29
U1 6
U2 60
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD NOV 15
PY 2011
VL 151
IS 11
SI SI
BP 1462
EP 1470
DI 10.1016/j.agrformet.2011.01.006
PG 9
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA 825TT
UT WOS:000295305700006
ER
PT J
AU Weimer, H
Buchler, HP
AF Weimer, Hendrik
Buechler, Hans Peter
TI In situ measurement of the dynamic structure factor in ultracold quantum
gases
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
ID BOSE-EINSTEIN CONDENSATE; INTERACTING FERMI GAS; CAVITY
AB We propose an experimental setup to efficiently measure the dynamic structure factor of ultracold quantum gases. Our method uses the interaction of the trapped atomic system with two different cavity modes, which are driven by external laser fields. By measuring the output fields of the cavity, the dynamic structure factor of the atomic system can be determined. In contrast to previous approaches, the atomic system is not destroyed during the measurement process.
C1 [Weimer, Hendrik; Buechler, Hans Peter] Univ Stuttgart, Inst Theoret Phys 3, D-70550 Stuttgart, Germany.
[Weimer, Hendrik] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Weimer, Hendrik] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Weimer, H (reprint author), Univ Stuttgart, Inst Theoret Phys 3, D-70550 Stuttgart, Germany.
EM hweimer@cfa.harvard.edu
FU Army Research Office; DARPA OLE; Deutsche Forschungsgemeinschaft (DFG)
[SFB/TRR 21]; National Science Foundation; German Academic Exchange
Service (DAAD)
FX We thank R Low for fruitful discussions on the experimental parameters.
This work was supported by a grant from the Army Research Office with
funding from the DARPA OLE program, by the Deutsche
Forschungsgemeinschaft (DFG) within SFB/TRR 21, 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 Postdoc
Program of the German Academic Exchange Service (DAAD).
NR 23
TC 4
Z9 4
U1 0
U2 1
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 NOV 14
PY 2011
VL 13
AR 113018
DI 10.1088/1367-2630/13/11/113018
PG 9
WC Physics, Multidisciplinary
SC Physics
GA 855PG
UT WOS:000297576100001
ER
PT J
AU Loreau, J
Lecointre, J
Urbain, X
Vaeck, N
AF Loreau, J.
Lecointre, J.
Urbain, X.
Vaeck, N.
TI Rovibrational analysis of the XUV photodissociation of HeH+ ions
SO PHYSICAL REVIEW A
LA English
DT Article
ID SINGLET SIGMA-STATES; MOLECULAR ION; CONFIGURATION-INTERACTION; SPECTRA;
PI
AB We investigate the dynamics of the photodissociation of the helium hydride ion HeH+ by XUV radiation with the aim to establish a detailed comparison with a recent experimental work carried out at the FLASH free electron laser using both vibrationally hot and cold ions. We determine the corresponding rovibrational distributions using a dissociative charge transfer setup and the same source conditions as in the FLASH experiment. Using a nonadiabatic time-dependent wave-packet method, we calculate the partial photodissociation cross sections for the n = 1-3 coupled electronic states of HeH+. We find good agreement with the experiment for the cross section into the He + H+ dissociative channel. On the other hand, we show that the experimental observation of the importance of the electronic states with n > 3 cannot be well explained theoretically, especially for cold (v = 0) ions. We find a good agreement with the experiment on the relative contribution of the Sigma and Pi states to the cross section for the He+ + H channel, but only a qualitative one for the He + H+ channel. We discuss the factors that could explain the remaining discrepancies between theory and experiment.
C1 [Loreau, J.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
[Lecointre, J.; Urbain, X.] Catholic Univ Louvain, Inst Condensed Matter & Nanosci, B-1348 Louvain, Belgium.
[Vaeck, N.] Univ Libre Bruxelles, Lab Chim Quant & Photophys, B-1050 Brussels, Belgium.
RP Loreau, J (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
EM jloreau@cfa.harvard.edu; julien.lecointre@uclouvain.be;
xavier.urbain@uclouvain.be; nvaeck@ulb.ac.be
OI Loreau, Jerome/0000-0002-6142-1509
FU Fund for Scientific Research (FRS-FNRS) under Interuniversity Institute
for Nuclear Sciences [4.4504.10]; Action de Recherche Concertee (ATMOS);
Fonds de la Recherche Fondamentale; Belgian American Educational
Foundation
FX We thank H. B. Pedersen for providing us the conditions of operation of
the ion source used in the FLASH experiment. We are also grateful to M.
Desouter-Lecomte, D. Lauvergnat, and Y. Justum for their help with the
computer codes. We acknowledge financial support from the Fund for
Scientific Research (FRS-FNRS) under Interuniversity Institute for
Nuclear Sciences Contract No. 4.4504.10 and from the Action de Recherche
Concertee (ATMOS) and Fonds de la Recherche Fondamentale Collective
programs. J. Loreau is supported by the Belgian American Educational
Foundation.
NR 33
TC 5
Z9 5
U1 1
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 NOV 14
PY 2011
VL 84
IS 5
AR 053412
DI 10.1103/PhysRevA.84.053412
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 848ZV
UT WOS:000297094500010
ER
PT J
AU Kusumi, K
Kulathinal, RJ
Abzhanov, A
Boissinot, S
Crawford, NG
Faircloth, BC
Glenn, TC
Janes, DE
Losos, JB
Menke, DB
Poe, S
Sanger, TJ
Schneider, CJ
Stapley, J
Wade, J
Wilson-Rawls, J
AF Kusumi, Kenro
Kulathinal, Rob J.
Abzhanov, Arhat
Boissinot, Stephane
Crawford, Nicholas G.
Faircloth, Brant C.
Glenn, Travis C.
Janes, Daniel E.
Losos, Jonathan B.
Menke, Douglas B.
Poe, Steven
Sanger, Thomas J.
Schneider, Christopher J.
Stapley, Jessica
Wade, Juli
Wilson-Rawls, Jeanne
TI Developing a community-based genetic nomenclature for anole lizards
SO BMC GENOMICS
LA English
DT Article
ID EUKARYOTIC TRANSPOSABLE ELEMENTS; UNIFIED CLASSIFICATION-SYSTEM;
MULTIPLE SEQUENCE ALIGNMENT; HORIZONTAL TRANSFER; POPULATION GENOMICS;
MAXIMUM-LIKELIHOOD; PHYLOGENETIC TREES; DATABASE; BROWSER; MAMMALS
AB Background: Comparative studies of amniotes have been hindered by a dearth of reptilian molecular sequences. With the genomic assembly of the green anole, Anolis carolinensis available, non-avian reptilian genes can now be compared to mammalian, avian, and amphibian homologs. Furthermore, with more than 350 extant species in the genus Anolis, anoles are an unparalleled example of tetrapod genetic diversity and divergence. As an important ecological, genetic and now genomic reference, it is imperative to develop a standardized Anolis gene nomenclature alongside associated vocabularies and other useful metrics.
Results: Here we report the formation of the Anolis Gene Nomenclature Committee (AGNC) and propose a standardized evolutionary characterization code that will help researchers to define gene orthology and paralogy with tetrapod homologs, provide a system for naming novel genes in Anolis and other reptiles, furnish abbreviations to facilitate comparative studies among the Anolis species and related iguanid squamates, and classify the geographical origins of Anolis subpopulations.
Conclusions: This report has been generated in close consultation with members of the Anolis and genomic research communities, and using public database resources including NCBI and Ensembl. Updates will continue to be regularly posted to new research community websites such as lizardbase. We anticipate that this standardized gene nomenclature will facilitate the accessibility of reptilian sequences for comparative studies among tetrapods and will further serve as a template for other communities in their sequencing and annotation initiatives.
C1 [Kusumi, Kenro; Wilson-Rawls, Jeanne] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA.
[Kulathinal, Rob J.] Temple Univ, Dept Biol, Philadelphia, PA 19122 USA.
[Abzhanov, Arhat; Janes, Daniel E.; Losos, Jonathan B.; Sanger, Thomas J.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Boissinot, Stephane] CUNY, Dept Biol, Queens Coll, Flushing, NY 11367 USA.
[Crawford, Nicholas G.; Schneider, Christopher J.] Boston Univ, Dept Biol, Boston, MA 02215 USA.
[Faircloth, Brant C.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Glenn, Travis C.] Univ Georgia, Dept Environm Hlth Sci, Athens, GA 30602 USA.
[Losos, Jonathan B.; Sanger, Thomas J.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA.
[Menke, Douglas B.] Univ Georgia, Dept Genet, Athens, GA 30602 USA.
[Poe, Steven] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
[Stapley, Jessica] Smithsonian Trop Res Inst, Dpo, AA 34002 USA.
[Wade, Juli] Michigan State Univ, Dept Psychol, E Lansing, MI 48824 USA.
[Wade, Juli] Michigan State Univ, Dept Zool, E Lansing, MI 48824 USA.
RP Kusumi, K (reprint author), Arizona State Univ, Sch Life Sci, POB 874501, Tempe, AZ 85287 USA.
EM kenro.kusumi@asu.edu; robkulathinal@temple.edu
RI Kusumi, Kenro/J-2626-2012; Stapley, Jessica/B-3858-2010; wade,
juli/F-4993-2012;
OI Kusumi, Kenro/0000-0002-1458-4540; Faircloth, Brant/0000-0002-1943-0217
FU NSF [IOS 0742833, DEB-0844624, DEB-1011544, DEB-1119734, MCB-0817687];
NIH [RR031305]; Arizona Biomedical Research Commission
FX The committee would like to thank the following individuals for helpful
discussions: Janet Weber, Manfred Grabherr, Jessica Alfoldi, Federica di
Palma, Sudhir Kumar, Fiona McCarthy, Tonia Hsieh, Alan Rawls, and
Rebecca Fisher. We thank Karla Moeller for permission to reproduce the
image used for the cover page. Anolis genome-related research is
supported by the NSF (IOS 0742833, JW; DEB-0844624, SP; DEB-1011544 and
DEB-1119734, CJS), NIH (RR031305, KK and JW-R) and Arizona Biomedical
Research Commission (KK). Postdoctoral support (DEJ) was provided by the
National Science Foundation (MCB-0817687).
NR 40
TC 12
Z9 12
U1 1
U2 13
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2164
J9 BMC GENOMICS
JI BMC Genomics
PD NOV 11
PY 2011
VL 12
AR 554
DI 10.1186/1471-2164-12-554
PG 13
WC Biotechnology & Applied Microbiology; Genetics & Heredity
SC Biotechnology & Applied Microbiology; Genetics & Heredity
GA 869HR
UT WOS:000298589500001
PM 22077994
ER
PT J
AU Maruca, BA
Kasper, JC
Bale, SD
AF Maruca, B. A.
Kasper, J. C.
Bale, S. D.
TI What Are the Relative Roles of Heating and Cooling in Generating Solar
Wind Temperature Anisotropies?
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID HOT ACCRETION FLOWS; VELOCITY DISTRIBUTIONS; PLASMA; INSTABILITY;
COLLISIONS; TURBULENCE; PROTONS
AB Temperature anisotropy in the solar wind results from a combination of mechanisms of anisotropic heating (e.g., cyclotron-resonant heating and dissipation of kinetic Alfven waves) and cooling (e.g., Chew-Goldberger-Low double-adiabatic expansion). In contrast, anisotropy-driven instabilities such as the cyclotron, mirror, and firehose instabilities limit the allowable departure of the plasma from isotropy. This study used data from the Faraday cups on the Wind spacecraft to examine scalar temperature and temperature components of protons. Plasma unstable to the mirror or firehose instability was found to be about 3-4 times hotter than stable plasma. Since anisotropy-driven instabilities are not understood to heat the plasma, these results suggest that heating processes are more effective than cooling processes at creating and maintaining proton temperature anisotropy in the solar wind.
C1 [Maruca, B. A.; Kasper, J. C.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Maruca, B. A.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bale, S. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
RP Maruca, BA (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
EM bmaruca@cfa.harvard.edu
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 NASA [NNX08AW07G]
FX J. C. K. and B. A. M. thank S. Cranmer, S. P. Gary, M. L. Stevens, R.
Narayan, and J. Raymond for discussions. Analysis of Wind observations
is supported by NASA Grant No. NNX08AW07G. This research has made use of
the SAO/NASA Astrophysics Data System (ADS).
NR 32
TC 57
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U1 0
U2 3
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 NOV 11
PY 2011
VL 107
IS 20
AR 201101
DI 10.1103/PhysRevLett.107.201101
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 849OA
UT WOS:000297133700002
PM 22181718
ER
PT J
AU Adams, ER
Lopez-Morales, M
Elliot, JL
Seager, S
Osip, DJ
Holman, MJ
Winn, JN
Hoyer, S
Rojo, P
AF Adams, E. R.
Lopez-Morales, M.
Elliot, J. L.
Seager, S.
Osip, D. J.
Holman, M. J.
Winn, J. N.
Hoyer, S.
Rojo, P.
TI TWENTY-ONE NEW LIGHT CURVES OF OGLE-TR-56b: NEW SYSTEM PARAMETERS AND
LIMITS ON TIMING VARIATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (OGLE-TR-56)
ID TRANSITING PLANET OGLE-TR-56B; STELLAR ATMOSPHERE MODELS; LIMB-DARKENING
LAW; DECONVOLUTION PHOTOMETRY; EXTRASOLAR PLANETS; IMAGE SUBTRACTION;
SURFACE GRAVITIES; HIGH-SPEED; STAR; OCCULTATION
AB Although OGLE-TR-56b was the second transiting exoplanet discovered, only one light curve, observed in 2006, has been published besides the discovery data. We present 21 light curves of 19 different transits observed between 2003 July and 2009 July with the Magellan Telescopes and Gemini South. The combined analysis of the new light curves confirms a slightly inflated planetary radius relative to model predictions, with R(p) = 1.378 +/- 0.090 R(J). However, the values found for the transit duration, semimajor axis, and inclination values differ significantly from the previous result, likely due to systematic errors. The new semimajor axis and inclination, a = 0.01942 +/- 0.00015 AU and i = 73.degrees 72 +/- 0.degrees 18, are smaller than previously reported, while the total duration, T(14) = 7931 +/- 38 s, is 18 minutes longer. The transit midtimes have errors from 23 s to several minutes, and no evidence is seen for transit midtime or duration variations. Similarly, no change is seen in the orbital period, implying a nominal stellar tidal decay factor of Q(*) = 107, with a 3 sigma lower limit of 10(5.7).
C1 [Adams, E. R.; Holman, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Adams, E. R.; Elliot, J. L.; Seager, S.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Lopez-Morales, M.] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, E-08193 Barcelona, Spain.
[Lopez-Morales, M.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Elliot, J. L.; Seager, S.; Winn, J. N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Elliot, J. L.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Osip, D. J.] Carnegie Observ, Las Campanas Observ, La Serena, Chile.
[Hoyer, S.; Rojo, P.] Univ Chile, Dept Astron, Santiago, Chile.
RP Adams, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Rojo, Patricio/I-5765-2016
FU NASA [NNX07AN63G, HF-01210.01-A/HF-51233.01, NAS5-26555]
FX E.R.A. received support from NASA Origins grant NNX07AN63G. M.L.M.
acknowledges support for parts of this work from NASA through Hubble
Fellowship grant HF-01210.01-A/HF-51233.01 awarded by the STScI, which
is operated by the AURA, Inc. for NASA, under contract NAS5-26555. This
paper makes use of observations made with the European Southern
Observatory telescopes and obtained from the ESO/ST-ECF Science Archive
Facility. We thank Paul Schechter for observing a transit of OGLE-TR-56b
as part of MIT's Magellan queue; Brian Taylor and Paul Schechter for
their tireless instrument support; and Georgi Mandushev for assistance
with image subtraction.
NR 38
TC 10
Z9 10
U1 0
U2 3
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 NOV 10
PY 2011
VL 741
IS 2
AR 102
DI 10.1088/0004-637X/741/2/102
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500035
ER
PT J
AU Bischoff, C
Brizius, A
Buder, I
Chinone, Y
Cleary, K
Dumoulin, RN
Kusaka, A
Monsalve, R
Naess, SK
Newburgh, LB
Reeves, R
Smith, KM
Wehus, IK
Zuntz, JA
Zwart, JTL
Bronfman, L
Bustos, R
Church, SE
Dickinson, C
Eriksen, HK
Ferreira, PG
Gaier, T
Gundersen, JO
Hasegawa, M
Hazumi, M
Huffenberger, KM
Jones, ME
Kangaslahti, P
Kapner, DJ
Lawrence, CR
Limon, M
May, J
McMahon, JJ
Miller, AD
Nguyen, H
Nixon, GW
Pearson, TJ
Piccirillo, L
Radford, SJE
Readhead, ACS
Richards, JL
Samtleben, D
Seiffert, M
Shepherd, MC
Staggs, ST
Tajima, O
Thompson, KL
Vanderlinde, K
Williamson, R
Winstein, B
AF Bischoff, C.
Brizius, A.
Buder, I.
Chinone, Y.
Cleary, K.
Dumoulin, R. N.
Kusaka, A.
Monsalve, R.
Naess, S. K.
Newburgh, L. B.
Reeves, R.
Smith, K. M.
Wehus, I. K.
Zuntz, J. A.
Zwart, J. T. L.
Bronfman, L.
Bustos, R.
Church, S. E.
Dickinson, C.
Eriksen, H. K.
Ferreira, P. G.
Gaier, T.
Gundersen, J. O.
Hasegawa, M.
Hazumi, M.
Huffenberger, K. M.
Jones, M. E.
Kangaslahti, P.
Kapner, D. J.
Lawrence, C. R.
Limon, M.
May, J.
McMahon, J. J.
Miller, A. D.
Nguyen, H.
Nixon, G. W.
Pearson, T. J.
Piccirillo, L.
Radford, S. J. E.
Readhead, A. C. S.
Richards, J. L.
Samtleben, D.
Seiffert, M.
Shepherd, M. C.
Staggs, S. T.
Tajima, O.
Thompson, K. L.
Vanderlinde, K.
Williamson, R.
Winstein, B.
CA QUIET Collaboration
TI FIRST SEASON QUIET OBSERVATIONS: MEASUREMENTS OF COSMIC MICROWAVE
BACKGROUND POLARIZATION POWER SPECTRA AT 43 GHz IN THE MULTIPOLE RANGE
25 <= l <= 475
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; gravitational
waves; inflation; polarization
ID PROBE WMAP OBSERVATIONS; PERSEUS MOLECULAR-COMPLEX; MAPS; BOOMERANG;
EMISSION; TEMPERATURE; CALIBRATION; COVARIANCE; ANTENNAS; DESIGN
AB The Q/U Imaging ExperimenT (QUIET) employs coherent receivers at 43 GHz and 94 GHz, operating on the Chajnantor plateau in the Atacama Desert in Chile, to measure the anisotropy in the polarization of the cosmic microwave background (CMB). QUIET primarily targets the B modes from primordial gravitational waves. The combination of these frequencies gives sensitivity to foreground contributions from diffuse Galactic synchrotron radiation. Between 2008 October and 2010 December, over 10,000 hr of data were collected, first with the 19 element 43 GHz array (3458 hr) and then with the 90 element 94 GHz array. Each array observes the same four fields, selected for low foregrounds, together covering approximate to 1000 deg(2). This paper reports initial results from the 43 GHz receiver, which has an array sensitivity to CMB fluctuations of 69 mu K root s. The data were extensively studied with a large suite of null tests before the power spectra, determined with two independent pipelines, were examined. Analysis choices, including data selection, were modified until the null tests passed. Cross-correlating maps with different telescope pointings is used to eliminate a bias. This paper reports the EE, BB, and EB power spectra in the multipole range l = 25-475. With the exception of the lowest multipole bin for one of the fields, where a polarized foreground, consistent with Galactic synchrotron radiation, is detected with 3 sigma significance, the E-mode spectrum is consistent with the Lambda CDM model, confirming the only previous detection of the first acoustic peak. The B-mode spectrum is consistent with zero, leading to a measurement of the tensor-to-scalar ratio of r = 0.35(-0.87)(+1.06). The combination of a new time-stream "double-demodulation" technique, side-fed Dragonian optics, natural sky rotation, and frequent boresight rotation leads to the lowest level of systematic contamination in the B-mode power so far reported, below the level of r = 0.1.
C1 [Bischoff, C.; Brizius, A.; Buder, I.; Kusaka, A.; Smith, K. M.; Kapner, D. J.; Tajima, O.; Vanderlinde, K.; Winstein, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brizius, A.; Samtleben, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Chinone, Y.; Hasegawa, M.; Hazumi, M.; Tajima, O.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan.
[Chinone, Y.] Tohoku Univ, Astron Inst, Grad Sch Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Cleary, K.; Reeves, R.; Pearson, T. J.; Radford, S. J. E.; Readhead, A. C. S.; Richards, J. L.; Shepherd, M. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Dumoulin, R. N.; Newburgh, L. B.; Zwart, J. T. L.; Limon, M.; Miller, A. D.; Williamson, R.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Dumoulin, R. N.; Newburgh, L. B.; Zwart, J. T. L.; Limon, M.; Miller, A. D.; Williamson, R.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Monsalve, R.; Bustos, R.; Gundersen, J. O.; Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA.
[Naess, S. K.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
[Wehus, I. K.] Univ Oslo, Dept Phys, N-0316 Oslo, Norway.
[Zuntz, J. A.; Jones, M. E.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Zuntz, J. A.] Oxford Martin Sch, Oxford OX1 3BD, England.
[Zuntz, J. A.] UCL, Dept Phys & Astron, London WC1E, England.
[Bronfman, L.; Bustos, R.; May, J.] Univ Chile, Dept Astron, Santiago, Chile.
[Bustos, R.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Church, S. E.; Thompson, K. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Church, S. E.; Thompson, K. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Dickinson, C.; Piccirillo, L.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Eriksen, H. K.] Univ Oslo, Ctr Math Applicat, N-0316 Oslo, Norway.
[Gaier, T.; Kangaslahti, P.; Lawrence, C. R.; Seiffert, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Nguyen, H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Nixon, G. W.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Bischoff, C.; Brizius, A.; Buder, I.; Kusaka, A.; Smith, K. M.; Kapner, D. J.; Tajima, O.; Vanderlinde, K.; Winstein, B.] Univ Chicago, Kavli Inst Cosmol Phys, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
RP Bischoff, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 43, Cambridge, MA 02138 USA.
EM akito@kicp.uchicago.edu
RI Bronfman, Leonardo/H-9544-2013; Reeves, Rodrigo/H-2812-2014; Williamson,
Ross/H-1734-2015; Pearson, Timothy/N-2376-2015;
OI Bronfman, Leonardo/0000-0002-9574-8454; Reeves,
Rodrigo/0000-0001-5704-271X; Williamson, Ross/0000-0002-6945-2975;
Limon, Michele/0000-0002-5900-2698; Pearson,
Timothy/0000-0001-5213-6231; Bischoff, Colin/0000-0001-9185-6514; Zwart,
Jonathan/0000-0002-4967-946X
FU NSF [AST-0506648, PHY-0355328, AST-0448909, AST-1010016, PHY-0551142];
KAKENHI [20244041, 20740158, 21111002]; PRODEX [C90284]; KIPAC
Enterprise; Strategic Alliance for the Implementation of New
Technologies (SAINT); Fermilab; Kavli Institute for Cosmological
Physics; University of Chicago; National Aeronautics and Space
Administration; JPL; STFC; ERC IRG; Beecroft Institute of Particle
Astrophysics and Cosmology; Oxford Martin School; Science and Technology
Facilities Council; CONICYT [PFB-06]; ALMA-Conicyt [31080022, 31070015];
Sloan foundation
FX Support for the QUIET instrument and operation comes through the NSF
cooperative agreement AST-0506648. Support was also provided by NSF
awards PHY-0355328, AST-0448909, AST-1010016, and PHY-0551142; KAKENHI
20244041, 20740158, and 21111002; PRODEX C90284; a KIPAC Enterprise
grant; and by the Strategic Alliance for the Implementation of New
Technologies (SAINT).; Some work was performed on the Joint
Fermilab-KICP Supercomputing Cluster, supported by grants from Fermilab,
the Kavli Institute for Cosmological Physics, and the University of
Chicago. Some work was performed on the Titan Cluster, owned and
maintained by the University of Oslo and NOTUR (the Norwegian High
Performance Computing Consortium), and on the Central Computing System,
owned and operated by the Computing Research Center at KEK. Portions of
this work were performed at the Jet Propulsion Laboratory (JPL) and
California Institute of Technology, operating under a contract with the
National Aeronautics and Space Administration. The Q-band polarimeter
modules were developed using funding from the JPL R&TD program.; C.D.
acknowledges an STFC Advanced Fellowship and an ERC IRG grant under FP7.
P. G. F. and J.A.Z. gratefully acknowledge the support of the Beecroft
Institute of Particle Astrophysics and Cosmology, the Oxford Martin
School, and the Science and Technology Facilities Council. L. B., R. B.,
and J.M. acknowledge support from CONICYT project Basal PFB-06. R. B.
acknowledges support from ALMA-Conicyt 31080022 and 31070015. A. D. M.
acknowledges a Sloan foundation fellowship.; PWV measurements were
provided by the Atacama Pathfinder Experiment (APEX). We thank CONICYT
for granting permission to operate within the Chajnantor Scientific
Preserve in Chile, and ALMA for providing site infrastructure support.
Field operations were based at the Don Esteban facility run by
Astro-Norte. We are particularly indebted to the engineers and
technician who maintained and operated the telescope: Jose Cortes,
Cristobal Jara, Freddy Munoz, and Carlos Verdugo.; In addition, we
acknowledge the following people for their assistance in the instrument
design, construction, commissioning, operation, and in data analysis:
Augusto Gutierrez Aitken, Colin Baines, Phil Bannister, Hannah Barker,
Matthew R. Becker, Alex Blein, Mircea Bogdan, April Campbell, Anushya
Chandra, Sea Moon Cho, Emma Curry, Maire Daly, Richard Davis, Fritz
Dejongh, Joy Didier, Greg Dooley, Hans Eide, Will Grainger, Jonathon
Goh, Peter Hamlington, Takeo Higuchi, Seth Hillbrand, Christian Holler,
Ben Hooberman, Kathryn D. Huff, William Imbriale, Koji Ishidoshiro,
Eiichiro Komatsu, Jostein Kristiansen, Richard Lai, Erik Leitch, Kelly
Lepo, Martha Malin, MarkMcCulloch, Oliver Montes, David Moore, Makoto
Nagai, Ian O'Dwyer, Stephen Osborne, Stephen Padin, Felipe Pedreros,
Ashley Perko, Alan Robinson, Jacklyn Sanders, Dale Sanford, Mary Soria,
Alex Sugarbaker, David Sutton, Matias Vidal, Liza Volkova, Edward
Wollack, Stephanie Xenos, and Mark Zaskowski.
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JI Astrophys. J.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500044
ER
PT J
AU Civano, F
Brusa, M
Comastri, A
Elvis, M
Salvato, M
Zamorani, G
Capak, P
Fiore, F
Gilli, R
Hao, H
Ikeda, H
Kakazu, Y
Kartaltepe, JS
Masters, D
Miyaji, T
Mignoli, M
Puccetti, S
Shankar, F
Silverman, J
Vignali, C
Zezas, A
Koekemoer, AM
AF Civano, F.
Brusa, M.
Comastri, A.
Elvis, M.
Salvato, M.
Zamorani, G.
Capak, P.
Fiore, F.
Gilli, R.
Hao, H.
Ikeda, H.
Kakazu, Y.
Kartaltepe, J. S.
Masters, D.
Miyaji, T.
Mignoli, M.
Puccetti, S.
Shankar, F.
Silverman, J.
Vignali, C.
Zezas, A.
Koekemoer, A. M.
TI THE POPULATION OF HIGH-REDSHIFT ACTIVE GALACTIC NUCLEI IN THE
CHANDRA-COSMOS SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE evolution; galaxies: active; surveys; X-rays: galaxies
ID QUASAR LUMINOSITY FUNCTION; SUPERMASSIVE BLACK-HOLES; DEEP FIELD-SOUTH;
SIMILAR-TO 4; DIGITAL-SKY-SURVEY; LY-ALPHA EMITTERS; FAINT END;
STAR-FORMATION; SPACE DENSITY; EVOLUTION
AB We present the high-redshift (3 < z < 5.3) 0.5-2 keV number counts and the 2-10 keV (rest-frame) space density of X-ray-selected active galactic nuclei (AGNs) detected in the Chandra Cosmic Evolution Survey. The sample comprises 81 X-ray-detected sources with available spectroscopic (31) and photometric (50) redshifts plus 20 sources with a formal z(phot) < 3 but with a broad photometric redshift probability distribution, such that z(phot) + 1 sigma > 3. Eighty-one sources are selected in the 0.5-2 keV band, fourteen are selected in the 2-10 keV and six in the 0.5-10 keV bands. We sample the high-luminosity (log L((2-10 keV)) > 44.15 erg s(-1)) space density up to z similar to 5 and a fainter luminosity range (43.5 erg s(-1) < log L((2-10 keV)) < 44.15 erg s(-1)) than previous studies, up to z = 3.5. We weighted the contribution to the number counts and the space density of the sources with photometric redshift by using their probability of being at z > 3. We find that the space density of high-luminosity AGNs declines exponentially at all the redshifts, confirming the trend observed for optically selected quasars. At lower luminosity, the measured space density is not conclusive, and a larger sample of faint sources is needed. Comparisons with optical luminosity functions and black hole formation models are presented together with prospects for future surveys.
C1 [Civano, F.; Elvis, M.; Hao, H.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brusa, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Comastri, A.; Zamorani, G.; Gilli, R.; Mignoli, M.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Salvato, M.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Capak, P.; Kakazu, Y.; Masters, D.] CALTECH, Pasadena, CA 91125 USA.
[Fiore, F.] INAF Osservatorio Astron Roma, Rome, Italy.
[Ikeda, H.] Ehime Univ, Grad Sch Sci & Engn, Matsuyama, Ehime 7908577, Japan.
[Kartaltepe, J. S.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Masters, D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Miyaji, T.] Univ Nacl Autonoma Mexico Ensenada, Inst Astron, Ensenada 22860, Baja California, Mexico.
[Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy.
[Shankar, F.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Silverman, J.] Univ Tokyo, IPMU, Chiba 2778568, Japan.
[Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Civano, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Vignali, Cristian/J-4974-2012; Mignoli, Marco/O-9426-2015; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; Zezas,
Andreas/C-7543-2011;
OI Vignali, Cristian/0000-0002-8853-9611; Koekemoer,
Anton/0000-0002-6610-2048; Mignoli, Marco/0000-0002-9087-2835; Comastri,
Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Zezas,
Andreas/0000-0001-8952-676X; Puccetti, Simonetta/0000-0002-2734-7835;
Zamorani, Giovanni/0000-0002-2318-301X; Brusa,
Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157
FU NASA [GO7-8136A]; Blancheflor Boncompagni Ludovisi foundation;
Smithsonian Scholarly Studies; Alexander von Humboldt Foundation;
ASI/INAF [I/009/10/0, I/088/06]
FX The authors thank the referee for suggestions which improved this
paper's content. The authors thank J. Aird and E. Glikman for sharing
their luminosity functions, and G. Risaliti, R. D'Abrusco, and A.
Goulding for useful discussions. This work was supported in part by NASA
Chandra grant No. GO7-8136A (M.E., F.C., H.H.), the Blancheflor
Boncompagni Ludovisi foundation (F.C.) and the Smithsonian Scholarly
Studies (F.C.). F.S. acknowledges the Alexander von Humboldt Foundation
for support. In Italy this work is supported by ASI/INAF contracts
I/009/10/0 and I/088/06.
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SN 0004-637X
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JI Astrophys. J.
PD NOV 10
PY 2011
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PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500024
ER
PT J
AU Conroy, C
Loeb, A
Spergel, DN
AF Conroy, Charlie
Loeb, Abraham
Spergel, David N.
TI EVIDENCE AGAINST DARK MATTER HALOS SURROUNDING THE GLOBULAR CLUSTERS
MGC1 AND NGC 2419
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; globular clusters: general
ID RANDOM GRAVITATIONAL ENCOUNTERS; YOUNG STAR-CLUSTERS; SPIRAL GALAXIES;
MILKY-WAY; STELLAR POPULATIONS; ANTENNAE GALAXIES; SPHERICAL SYSTEMS;
EVOLUTION; ORIGIN; NUCLEI
AB The conjecture that the ancient globular clusters (GCs) formed at the center of their own dark matter (DM) halos was first proposed by Peebles in 1984 and has recently been revived to explain the puzzling abundance patterns observed within many GCs. In this paper, we demonstrate that the outer stellar density profile of isolated GCs is very sensitive to the presence of an extended dark halo. The GCs NGC 2419, located at 90 kpc from the center of our Galaxy, and MGC1, located at similar to 200 kpc from the center of M31, are ideal laboratories for testing the scenario that GCs formed at the centers of massive dark halos. Comparing analytic models to observations of these GCs, we conclude that these GCs cannot be embedded within dark halos with a virial mass greater than 10(6) M-circle dot, or, equivalently, the DM halo-mass-to-stellar mass ratio must be M-DM/M-* < 1. If these GCs have indeed orbited within weak tidal fields throughout their lifetimes, then these limits imply that these GCs did not form within their own dark halos. Recent observations of an extended stellar halo in the GC NGC 1851 are also interpreted in the context of our analytic models. Implications of these results for the formation of GCs are briefly discussed.
C1 [Conroy, Charlie; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Conroy, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Spergel, David/A-4410-2011
FU NSF [AST-0907890, AST-0707731]; NASA [NNX08AK43G, NNA09DB30A]
FX We thank Dougal Mackey for providing his data on MGC1, Jay Strader for
fruitful conversations, and Dougal Mackey and Scott Tremaine for
comments on an earlier draft. The referee is thanked for insightful
comments that improved the quality of the manuscript. This work made
extensive use of the NASA Astrophysics Data System and of the astro-ph
preprint archive at arXiv.org, and was supported in part by NSF grants
AST-0907890 and AST-0707731 and NASA grants NNX08AK43G and NNA09DB30A.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
VL 741
IS 2
AR 72
DI 10.1088/0004-637X/741/2/72
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500005
ER
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
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general; gamma-ray burst: general
ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; EXTRAGALACTIC DISTANCE
SCALE; STRIPPED-ENVELOPE SUPERNOVAE; RICH CIRCUMSTELLAR MEDIUM;
TELESCOPE KEY PROJECT; 25 APRIL 1998; IA SUPERNOVAE; IC SUPERNOVAE;
OBSERVATIONAL CONSTRAINTS
AB We present detailed optical photometry for 25 Type Ibc supernovae (SNe Ibc) within d approximate to 150 Mpc obtained with the robotic Palomar 60 inch telescope in 2004-2007. This study represents the first uniform, systematic, and statistical sample of multi-band SNe Ibc light curves available to date. We correct the light curves for host galaxy extinction using a new technique based on the photometric color evolution, namely, we show that the (V - R) color of extinction-corrected SNe Ibc at Delta t approximate to 10 days after V-band maximum is tightly distributed, <(V - R)(V10)> = 0.26 +/- 0.06 mag. Using this technique, we find that SNe Ibc typically suffer from significant host galaxy extinction, < E(B - V)> approximate to 0.4 mag. A comparison of the extinction-corrected light curves for helium-rich (Type Ib) and helium-poor (Type Ic) SNe reveals that they are statistically indistinguishable, both in luminosity and decline rate. We report peak absolute magnitudes of < M(R)> = -17.9 +/- 0.9 mag and < M(R)> = -18.3 +/- 0.6 mag for SNe Ib and Ic, respectively. Focusing on the broad-lined (BL) SNe Ic, we find that they are more luminous than the normal SNe Ibc sample, < M(R)> = -19.0 +/- 1.1 mag, with a probability of only 1.6% that they are drawn from the same population of explosions. By comparing the peak absolute magnitudes of SNe Ic-BL with those inferred for local engine-driven explosions (GRB-SN 1998bw, XRF-SN 2006aj, and SN 2009bb) we find a 25% probability that relativistic SNe are drawn from the overall SNe Ic-BL population. Finally, we fit analytic models to the light curves to derive typical (56)Ni masses of M(Ni) approximate to 0.2 and 0.5 M(circle dot) for SNe Ibc and SNe Ic-BL, respectively. With reasonable assumptions for the photospheric velocities, we further extract kinetic energy and ejecta mass values of M(ej) approximate to 2 M(circle dot) and E(K) approximate to 10(51) erg for SNe Ibc, while for SNe Ic-BL we find higher values, M(ej) approximate to 5 M(circle dot) and E(K) approximate to 10(52) erg. We discuss the implications for the progenitors of SNe Ibc and their relation to those of engine-driven explosions.
C1 [Drout, Maria R.; Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Drout, Maria R.] Univ Cambridge Churchill Coll, Cambridge CB3 0DS, England.
[Gal-Yam, Avishay; Arcavi, Iair; Green, Yoav] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Fac Phys, 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, Cambridge, MA 02138 USA.
RI Green, Yoav/L-5874-2015
OI Green, Yoav/0000-0002-0809-6575
FU National Science Foundation (NSF) [AST-1009571, AST-0401479]; Department
of Defense [0754568]; Smithsonian Institution; Israeli Science
Foundation (ISF); EU; Gruber Awards
FX M.R.D. 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 0754568 and by the Smithsonian
Institution. The work of A.G. is supported by grants from the Israeli
Science Foundation (ISF), an EU/FP7 Marie Curie IRG Fellowship and a
research grant from the Gruber Awards. S.B.C acknowledges generous
support from Gary and Cynthia Bengier and the Richard and Rhoda Goldman
Foundation. The work of D.C.L. is supported by National Science
Foundation (NSF) grant AST-1009571. D.C.L. is grateful for an NSF
Astronomy and Astrophysics Postdoctoral Fellowship under award
AST-0401479, during which part of this work was completed.
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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 NOV 10
PY 2011
VL 741
IS 2
AR 97
DI 10.1088/0004-637X/741/2/97
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500030
ER
PT J
AU Dunham, MK
Rosolowsky, E
Evans, NJ
Cyganowski, C
Urquhart, JS
AF Dunham, Miranda K.
Rosolowsky, Erik
Evans, Neal J., II
Cyganowski, Claudia
Urquhart, James S.
TI THE BOLOCAM GALACTIC PLANE SURVEY. VII. CHARACTERIZING THE PROPERTIES OF
MASSIVE STAR-FORMING REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: clouds; ISM: molecules; stars: formation
ID INFRARED-DARK CLOUDS; KINEMATIC DISTANCE AMBIGUITY; NARROW
SELF-ABSORPTION; H-II REGIONS; MOLECULAR CLOUDS; PHYSICAL-PROPERTIES;
DENSE CORES; RING SURVEY; DUST CONTINUUM; MILKY-WAY
AB We present the results of a Green Bank Telescope survey of NH(3)(1,1), (2,2), (3,3) lines toward 631 Bolocam Galactic Plane Survey (BGPS) sources at a range of Galactic longitudes in the inner Galaxy. We have detected the NH(3)(1,1) line toward 72% of our targets (456), demonstrating that the high column density features identified in the BGPS and other continuum surveys accurately predict the presence of dense gas. We have determined kinematic distances and resolved the distance ambiguity for all BGPS sources detected in NH(3). The BGPS sources trace the locations of the Scutum and Sagittarius spiral arms, with the number of sources peaking between R(Gal) similar to 4 and 5 kpc. We measure the physical properties of each source and find that depending on the distance, BGPS sources are primarily clumps, with some cores and clouds. We have examined the physical properties as a function of Galactocentric distance, and find a mean gas kinetic temperature of 15.6 K, and that the NH(3) column density and abundance decrease by nearly an order of magnitude between R(Gal) similar to 3 and 11 kpc. Comparing sources at similar distances demonstrates that the physical properties are indistinguishable, which suggests a similarity in clump structure across the Galactic disk. We have also compared the BGPS sources to criteria for efficient star formation presented independently by Heiderman et al. and Lada et al., and for massive star formation presented by Kauffmann et al. Forty-eight percent of our sample should be forming stars (including massive stars) with high efficiency, and 87% contain subregions that should be efficiently forming stars. Indeed, we find that 67% of the sample exhibit signs of star formation activity based on an association with a mid-infrared source.
C1 [Dunham, Miranda K.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Dunham, Miranda K.; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Rosolowsky, Erik] Univ British Columbia, Dept Phys & Astron, Kelowna, BC V1V 1V7, Canada.
[Cyganowski, Claudia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Urquhart, James S.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
RP Dunham, MK (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA.
EM miranda.dunham@yale.edu
FU National Science Foundation [AST-0708403, AST-0607793, AST-1003134,
AST-0808119, AST-9800334, AST-0098562, AST-0100793]; National Radio
Astronomy Observatory (NRAO) [GSSP09-0004]; Natural Sciences and
Engineering Research Council Canada; Science and Technology Facilities
Council of the UK; Canadian Space Agency; CSIRO OCE
FX The authors thank the anonymous referee for constructive comments, C.
Figura and L. Morgan for the NH3 observations they have
provided for this work, as well as T. Robitaille and M. M. Dunham for
many enlightening conversations. The BGPS is supported by the National
Science Foundation through NSF grant AST-0708403. M.K.D. and N.J.E. were
supported by NSF grant AST-0607793 to the University of Texas at Austin.
M. K. D. was additionally supported by a grant from the National Radio
Astronomy Observatory (NRAO) Student Observing Support Program, award
number GSSP09-0004. The NRAO is a facility of the National Science
Foundation, operated under cooperative agreement by Associated
Universities, Inc. E. R. is supported by a Discovery Grant from the
Natural Sciences and Engineering Research Council Canada. C.J.C. is
supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship
under award AST-1003134 and also acknowledges support from NSF grant
AST-0808119. J.S.U. is supported by a CSIRO OCE postdoctoral grant. This
paper made use of information from the RedMSXSource (RMS) survey
database at www.ast.leeds.ac.uk/RMS, which was constructed with support
from the Science and Technology Facilities Council of the UK. This
publication makes use of molecular line data from the Boston
University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project
of Boston University and Five College Radio Astronomy Observatory,
funded by the National Science Foundation under grants AST-9800334,
AST-0098562, and AST-0100793. This research used the facilities of the
Canadian Astronomy Data Centre operated by the National Research Council
of Canada with the support of the Canadian Space Agency.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
VL 741
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AR 110
DI 10.1088/0004-637X/741/2/110
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500043
ER
PT J
AU Gupta, RR
D'Andrea, CB
Sako, M
Conroy, C
Smith, M
Bassett, B
Frieman, JA
Garnavich, PM
Jha, SW
Kessler, R
Lampeitl, H
Marriner, J
Nichol, RC
Schneider, DP
AF Gupta, Ravi R.
D'Andrea, Chris B.
Sako, Masao
Conroy, Charlie
Smith, Mathew
Bassett, Bruce
Frieman, Joshua A.
Garnavich, Peter M.
Jha, Saurabh W.
Kessler, Richard
Lampeitl, Hubert
Marriner, John
Nichol, Robert C.
Schneider, Donald P.
TI IMPROVED CONSTRAINTS ON TYPE Ia SUPERNOVA HOST GALAXY PROPERTIES USING
MULTI-WAVELENGTH PHOTOMETRY AND THEIR CORRELATIONS WITH SUPERNOVA
PROPERTIES (vol 740, pg 92, 2011)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Gupta, Ravi R.; D'Andrea, Chris B.; Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Smith, Mathew] Univ Cape Town, Dept Math & Appl Math, ACGC, 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.; Kessler, Richard] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Frieman, Joshua A.; Marriner, John] Fermilab Natl Accelerator Lab, 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.
[Kessler, Richard] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Lampeitl, Hubert; Nichol, Robert C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
RP Gupta, RR (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
EM ravgupta@physics.upenn.edu
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
VL 741
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DI 10.1088/0004-637X/741/2/127
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500060
ER
PT J
AU Lidz, A
Furlanetto, SR
Oh, SP
Aguirre, J
Chang, TC
Dore, O
Pritchard, JR
AF Lidz, Adam
Furlanetto, Steven R.
Oh, S. Peng
Aguirre, James
Chang, Tzu-Ching
Dore, Olivier
Pritchard, Jonathan R.
TI INTENSITY MAPPING WITH CARBON MONOXIDE EMISSION LINES AND THE REDSHIFTED
21 cm LINE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: theory; intergalactic medium; large-scale structure of
universe
ID MURCHISON-WIDEFIELD-ARRAY; MOLECULAR GAS; INTERGALACTIC MEDIUM;
STAR-FORMATION; HYDROGEN REIONIZATION; DARK-MATTER; PROBING
REIONIZATION; IONIZING EMISSIVITY; COSMIC EVOLUTION; ALPHA EMITTERS
AB We quantify the prospects for using emission lines from rotational transitions of the CO molecule to perform an "intensity mapping" observation at high redshift during the Epoch of Reionization (EoR). The aim of CO intensity mapping is to observe the combined CO emission from many unresolved galaxies, to measure the spatial fluctuations in this emission, and to use this as a tracer of large-scale structure at very early times in the history of our universe. This measurement would help determine the properties of molecular clouds-the sites of star formation-in the very galaxies that reionize the universe. We further consider the possibility of cross-correlating CO intensity maps with future observations of the redshifted 21 cm line. The cross spectrum is less sensitive to foreground contamination than the auto power spectra, and can therefore help confirm the high-redshift origin of each signal. Furthermore, the cross spectrum measurement would help extract key information about the EoR, especially regarding the size distribution of ionized regions. We discuss uncertainties in predicting the CO signal at high redshift, and discuss strategies for improving these predictions. Under favorable assumptions and feasible specifications for a CO survey mapping the CO(2-1) and CO(1-0) lines, the power spectrum of CO emission fluctuations and its cross spectrum with future 21 cm measurements from the Murchison Widefield Array are detectable at high significance.
C1 [Lidz, Adam; Aguirre, James] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Furlanetto, Steven R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Oh, S. Peng] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Chang, Tzu-Ching] Acad Sinica, IAA, Taipei 115, Taiwan.
[Dore, Olivier] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dore, Olivier] CALTECH, Pasadena, CA 91125 USA.
[Pritchard, Jonathan R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lidz, A (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
EM alidz@sas.upenn.edu
OI Pritchard, Jonathan/0000-0003-4127-5353
FU David and Lucile Packard Foundation; Alfred P. Sloan Foundation; NASA;
NASA Lunar Science Institute [NNA09DB30A]; NSF [AST 0908480]
FX We thank Matt McQuinn for providing the reionization simulations used in
this analysis and for comments on a draft. We are also grateful to Mark
Krumholz and the anonymous referee for helpful remarks that have
improved this paper. This work was initiated at the summer 2010 Aspen 21
cm cosmology meeting. This meeting and a subsequent meeting at the Keck
Institute for Space Sciences helped fuel this work, and we acknowledge
useful conversations with the participants of these meetings. We are
especially grateful to Judd Bowman as a co-organizer of both of these
meetings. S.R.F. was partially supported by the David and Lucile Packard
Foundation, by the Alfred P. Sloan Foundation, and by NASA through the
LUNAR program. The LUNAR consortium (http://lunar.colorado.edu),
headquartered at the University of Colorado, is funded by the NASA Lunar
Science Institute (via Cooperative Agreement NNA09DB30A) to investigate
concepts for astrophysical observatories on the Moon. S.P.O.
acknowledges NSF grant AST 0908480 for support. Part of the research
described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
VL 741
IS 2
AR 70
DI 10.1088/0004-637X/741/2/70
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500003
ER
PT J
AU Mainzer, A
Grav, T
Masiero, J
Hand, E
Bauer, J
Tholen, D
McMillan, RS
Spahr, T
Cutri, RM
Wright, E
Watkins, J
Mo, W
Maleszewski, C
AF Mainzer, A.
Grav, T.
Masiero, J.
Hand, E.
Bauer, J.
Tholen, D.
McMillan, R. S.
Spahr, T.
Cutri, R. M.
Wright, E.
Watkins, J.
Mo, W.
Maleszewski, C.
TI NEOWISE STUDIES OF SPECTROPHOTOMETRICALLY CLASSIFIED ASTEROIDS:
PRELIMINARY RESULTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; minor planets, asteroids: general; surveys
ID NEAR-EARTH ASTEROIDS; THERMAL-MODEL CALIBRATION;
INFRARED-SURVEY-EXPLORER; SPECTROSCOPIC SURVEY; MINOR PLANETS;
POPULATION; RADIOMETRY; PHOTOMETRY; TAXONOMY; OBJECTS
AB The NEOWISE data set offers the opportunity to study the variations in albedo for asteroid classification schemes based on visible and near-infrared observations for a large sample of minor planets. We have determined the albedos for nearly 1900 asteroids classified by the Tholen, Bus, and Bus-DeMeo taxonomic classification schemes. We find that the S-complex spans a broad range of bright albedos, partially overlapping the low albedo C-complex at small sizes. As expected, the X-complex covers a wide range of albedos. The multiwavelength infrared coverage provided by NEOWISE allows determination of the reflectivity at 3.4 and 4.6 mu m relative to the visible albedo. The direct computation of the reflectivity at 3.4 and 4.6 mu m enables a new means of comparing the various taxonomic classes. Although C, B, D, and T asteroids all have similarly low visible albedos, the D and T types can be distinguished from the C and B types by examining their relative reflectance at 3.4 and 4.6 mu m. All of the albedo distributions are strongly affected by selection biases against small, low albedo objects, as all objects selected for taxonomic classification were chosen according to their visible light brightness. Due to these strong selection biases, we are unable to determine whether or not there are correlations between size, albedo, and space weathering. We argue that the current set of classified asteroids makes any such correlations difficult to verify. A sample of taxonomically classified asteroids drawn without significant albedo bias is needed in order to perform such an analysis.
C1 [Mainzer, A.; Masiero, J.; Hand, E.; Bauer, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.; Mo, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bauer, J.; Cutri, R. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Tholen, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[McMillan, R. S.; Maleszewski, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[Wright, E.] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA.
[Watkins, J.] 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.
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 Widefield 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 gratefully acknowledge
the extraordinary services specific to NEOWISE contributed by the
International Astronomical Union's MPC, operated by the
Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for
Astronomical Telegrams, operated by Harvard University. We thank the
paper's referee, Prof. Richard Binzel, for his helpful contributions. 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.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
VL 741
IS 2
AR 90
DI 10.1088/0004-637X/741/2/90
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500023
ER
PT J
AU Mandushev, G
Quinn, SN
Buchhave, LA
Dunham, EW
Rabus, M
Oetiker, B
Latham, DW
Charbonneau, D
Brown, TM
Belmonte, JA
O'Donovan, FT
AF Mandushev, Georgi
Quinn, Samuel N.
Buchhave, Lars A.
Dunham, Edward W.
Rabus, Markus
Oetiker, Brian
Latham, David W.
Charbonneau, David
Brown, Timothy M.
Belmonte, Juan A.
O'Donovan, Francis T.
TI TrES-5: A MASSIVE JUPITER-SIZED PLANET TRANSITING A COOL G DWARF
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; techniques: photometric; techniques: radial
velocities; techniques: spectroscopic
ID HOT JUPITERS; BRIGHT STAR; BROWN DWARF; STELLAR; PARAMETERS; COMPANION;
BINARIES
AB We report the discovery of TrES-5, a massive hot Jupiter that transits the star GSC 03949-00967 every 1.48 days. From spectroscopy of the star we estimate a stellar effective temperature of T(eff) = 5171 +/- 36 K, and from high-precision B, R, and I photometry of the transit we constrain the ratio of the semimajor axis a and the stellar radius R(star) to be a/R(star) = 6.07 +/- 0.14. We compare these values to model stellar isochrones to obtain a stellar mass of M(star) = 0.893 +/- 0.024 M(circle dot). Based on this estimate and the photometric time series, we constrain the stellar radius to be R(star) = 0.866 +/- 0.013 R(circle dot) and the planet radius to be R(p) = 1.209 +/- 0.021 R(J). We model our radial-velocity data assuming a circular orbit and find a planetary mass of 1.778 +/- 0.063 M(J). Our radial-velocity observations rule out line-bisector variations that would indicate a specious detection resulting from a blend of an eclipsing binary system. TrES-5 orbits one of the faintest stars with transiting planets found to date from the ground and demonstrates that precise photometry and followup spectroscopy are possible, albeit challenging, even for such faint stars.
C1 [Mandushev, Georgi; Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Quinn, Samuel N.; Latham, David W.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Rabus, Markus] Ponticia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Rabus, Markus; Belmonte, Juan A.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Oetiker, Brian] Sam Houston State Univ, Dept Phys, Huntsville, TX 77340 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Belmonte, Juan A.] Univ La Laguna, Dept Astrofis, Tenerife, Spain.
[O'Donovan, Francis T.] Ab Initio Software, Lexington, MA 02421 USA.
RP Mandushev, G (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
EM gmand@lowell.edu
RI O'Donovan, Francis/I-2423-2014;
OI O'Donovan, Francis/0000-0002-4858-6106; Buchhave, Lars
A./0000-0003-1605-5666; Charbonneau, David/0000-0002-9003-484X
FU NASA [NNG04GN74G, NNG04LG89G, NNG05GI57G, NNG05GJ29G, NNH05AB88I,
N4G5-12229]; NASA Kepler mission [NCC2-1390]; ALMA-CONICYT [31090015,
31080021]; National Science Foundation
FX We thank Travis Barman for useful discussions. This paper is based on
work supported in part by NASA grants NNG04GN74G, NNG04LG89G,
NNG05GI57G, NNG05GJ29G, and NNH05AB88I through the Origins of Solar
Systems Program, and NASA Planetary Major Equipment grant N4G5-12229. We
acknowledge support from the NASA Kepler mission under cooperative
agreement NCC2-1390, and M. R. acknowledges support from ALMA-CONICYT
projects 31090015 and 31080021. This publication makes use of data
products from the Two Micron All Sky Survey, which is a joint project of
the University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by NASA and the
National Science Foundation.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 10
PY 2011
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DI 10.1088/0004-637X/741/2/114
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500047
ER
PT J
AU Masiero, JR
Mainzer, AK
Grav, T
Bauer, JM
Cutri, RM
Dailey, J
Eisenhardt, PRM
McMillan, RS
Spahr, TB
Skrutskie, MF
Tholen, D
Walker, RG
Wright, EL
DeBaun, E
Elsbury, D
Gautier, T
Gomillion, S
Wilkins, A
AF Masiero, Joseph R.
Mainzer, A. K.
Grav, T.
Bauer, J. M.
Cutri, R. M.
Dailey, J.
Eisenhardt, P. R. M.
McMillan, R. S.
Spahr, T. B.
Skrutskie, M. F.
Tholen, D.
Walker, R. G.
Wright, E. L.
DeBaun, E.
Elsbury, D.
Gautier, T.
Gomillion, S.
Wilkins, A.
TI MAIN BELT ASTEROIDS WITH WISE/NEOWISE. I. PRELIMINARY ALBEDOS AND
DIAMETERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: general; minor planets, asteroids: general
ID INFRARED-SURVEY-EXPLORER; NEAR-EARTH ASTEROIDS; DIGITAL SKY SURVEY;
THERMAL-MODEL; SIZE DISTRIBUTIONS; SPACE-TELESCOPE; 298 BAPTISTINA; K/T
IMPACTOR; 2 PALLAS; FAMILIES
AB We present initial results from the Wide-field Infrared Survey Explorer (WISE), a four-band all-sky thermal infrared survey that produces data well suited for measuring the physical properties of asteroids, and the NEOWISE enhancement to the WISE mission allowing for detailed study of solar system objects. Using a NEATM thermal model fitting routine, we compute diameters for over 100,000 Main Belt asteroids from their IR thermal flux, with errors better than 10%. We then incorporate literature values of visible measurements (in the form of the H absolute magnitude) to determine albedos. Using these data we investigate the albedo and diameter distributions of the Main Belt. As observed previously, we find a change in the average albedo when comparing the inner, middle, and outer portions of the Main Belt. We also confirm that the albedo distribution of each region is strongly bimodal. We observe groupings of objects with similar albedos in regions of the Main Belt associated with dynamical breakup families. Asteroid families typically show a characteristic albedo for all members, but there are notable exceptions to this. This paper is the first look at the Main Belt asteroids in the WISE data, and only represents the preliminary, observed raw size, and albedo distributions for the populations considered. These distributions are subject to survey biases inherent to the NEOWISE data set and cannot yet be interpreted as describing the true populations; the debiased size and albedo distributions will be the subject of the next paper in this series.
C1 [Masiero, Joseph R.; Mainzer, A. K.; Bauer, J. M.; Eisenhardt, P. R. M.; DeBaun, E.; Elsbury, D.; Gautier, T.; Gomillion, S.; Wilkins, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bauer, J. M.; Cutri, R. M.; Dailey, J.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[McMillan, R. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[Skrutskie, M. F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Tholen, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Walker, R. G.] Monterey Inst Res Astron, Monterey, CA USA.
[Wright, E. L.] UCLA Astron, Los Angeles, CA 90095 USA.
[DeBaun, E.] Dartmouth Coll, Hanover, NH 03755 USA.
[Elsbury, D.] Notre Dame High Sch, Sherman Oaks, CA 91423 USA.
[Gautier, T.] Flintridge Preparatory Sch, La Canada Flintridge, CA 91101 USA.
[Gomillion, S.] Embry Riddle Aeronaut Univ, Daytona Beach, FL 32114 USA.
[Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Masiero, JR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Joseph.Masiero@jpl.nasa.gov
OI Masiero, Joseph/0000-0003-2638-720X
FU NASA; Planetary Science Division of the National Aeronautics and Space
Administration
FX We thank the anonymous referee for the helpful comments and suggestions
that led to the improvement of this manuscript. J.R.M. was supported by
an appointment to the NASA Postdoctoral Program at JPL, administered by
Oak Ridge Associated Universities through a contract with NASA. J.R.M.
thanks M. Delbo and M. Mueller for providing access to their thermal
modeling code which was helpful in early test cases. 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. 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. We thank the
worldwide community of dedicated amateur and professional astronomers
devoted to minor planet follow-up observations. We are deeply grateful
for the outstanding contributions of all members of the WISE and NEOWISE
teams.
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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 NOV 10
PY 2011
VL 741
IS 2
AR 68
DI 10.1088/0004-637X/741/2/68
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500001
ER
PT J
AU Okabe, N
Bourdin, H
Mazzotta, P
Maurogordato, S
AF Okabe, N.
Bourdin, H.
Mazzotta, P.
Maurogordato, S.
TI SUBARU WEAK-LENSING STUDY OF A2163: BIMODAL MASS STRUCTURE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; dark matter; galaxies: clusters: general;
gravitational lensing: weak; X-rays: galaxies: clusters; X-rays:
individual (A2163)
ID ABELL GALAXY CLUSTER; NFW DENSITY PROFILE; X-RAY; DARK-MATTER; SCALING
RELATIONS; SPHERICAL GALAXIES; MERGER EVENTS; RADIO HALOS; XMM-NEWTON;
SIMULATIONS
AB We present a weak-lensing analysis of the merging cluster A2163 using Subaru/Suprime-Cam and CFHT/Mega-Cam data and discuss the dynamics of this cluster merger, based on complementary weak-lensing, X-ray, and optical spectroscopic data sets. From two-dimensional multi-component weak-lensing analysis, we reveal that the cluster mass distribution is well described by three main components including the two-component main cluster A2163-A with mass ratio 1: 8, and its cluster satellite A2163-B. The bimodal mass distribution in A2163-A is similar to the galaxy density distribution, but appears as spatially segregated from the brightest X-ray emitting gas region. We discuss the possible origins of this gas-dark-matter offset and suggest the gas core of the A2163-A subcluster has been stripped away by ram pressure from its dark matter component. The survival of this gas core from the tidal forces exerted by the main cluster lets us infer a subcluster accretion with a non-zero impact parameter. Dominated by the most massive component of A2163-A, the mass distribution of A2163 is well described by a universal Navarro-Frenk-White profile as shown by a one-dimensional tangential shear analysis, while the singular-isothermal sphere profile is strongly ruled out. Comparing this cluster mass profile with profiles derived assuming intracluster medium hydrostatic equilibrium ( H. E.) in two opposite regions of the cluster atmosphere has allowed us to confirm the prediction of a departure from H. E. in the eastern cluster side, presumably due to shock heating. Yielding a cluster mass estimate of M(500) = 11.18(-1.46)(+1.64) x 10(14) h(-1) M(circle dot), our mass profile confirms the exceptionally high mass of A2163, consistent with previous analyses relying on the cluster dynamical analysis and Y(X) mass proxy.
C1 [Okabe, N.] Acad Sinica Inst Astron & Astrophys ASIAA, Taipei 10617, Taiwan.
[Bourdin, H.; Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Mazzotta, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Maurogordato, S.] Univ Nice, CNRS, Lab Cassiopee, Observ Cote Azur,UMR 6202, F-06304 Nice 4, France.
RP Okabe, N (reprint author), Acad Sinica Inst Astron & Astrophys ASIAA, POB 23-141, Taipei 10617, Taiwan.
EM okabe@asiaa.sinica.edu.tw
RI Mazzotta, Pasquale/B-1225-2016
OI Mazzotta, Pasquale/0000-0002-5411-1748
FU NASA [NNX09AP45G, NNX09AP36G]; ASI-INAF [I/088/06/0, I/009/10/0]
FX N.O. acknowledges Yoichi Oyama, Keiichi Umetsu, Motoki Kino, Keiichi
Asada, Makoto Inoue, and Alberto Cappi for helpful discussions. We thank
the anonymous referee for the useful comments that led to improvement of
the manuscript. We also thank G. Soucail for giving us CFHT g'-band
data. We are also grateful to N. Kaiser for developing the publicly
available IMCAT package. H. B. and P. M. acknowledge support by NASA
grants NNX09AP45G and NNX09AP36G and grants ASI-INAF I/088/06/0 and
ASI-INAF I/009/10/0.
NR 59
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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 NOV 10
PY 2011
VL 741
IS 2
AR 116
DI 10.1088/0004-637X/741/2/116
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500049
ER
PT J
AU Owers, MS
Nulsen, PEJ
Couch, WJ
AF Owers, Matt S.
Nulsen, Paul E. J.
Couch, Warrick J.
TI MINOR MERGER-INDUCED COLD FRONTS IN ABELL 2142 AND RXJ1720.1+2638
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (Abell 2142, RXJ1720.1+2638); X-rays:
galaxies: clusters
ID XMM-NEWTON OBSERVATIONS; DIGITAL SKY SURVEY; X-RAY DATA; GALAXY
CLUSTERS; CHANDRA OBSERVATION; VORONOI TESSELLATIONS; MERGING CLUSTERS;
RICH CLUSTERS; CORE; GAS
AB We present evidence for the existence of substructure in the "relaxed appearing" cold front clusters Abell 2142 and RXJ1720.1+2638. The detection of these substructures was made possible by comprehensive multi-object optical spectroscopy obtained with the Hectospec and DEep Imaging Multi-Object Spectrograph instruments on the 6.5 m MMT and 10 m Keck II telescope, respectively. These observations produced 956 and 400 spectroscopically confirmed cluster members within a projected radius of 3 Mpc from the centers of A2142 and RXJ1720.1+2638, respectively. The substructure manifests itself as local peaks in the spatial distribution of member galaxies and also as regions of localized velocity substructure. For both Abell 2142 and RXJ1720.1+2638, we identify group-scale substructures which, when considering the morphology of the cold fronts and the time since pericentric passage of a perturber estimated from the cold front radii, could plausibly have perturbed the cluster cores and generated the cold fronts observed in Chandra images. The results presented here are consistent with cold fronts being the result of merger activity and with cold fronts in relaxed appearing clusters being due to minor merger activity.
C1 [Owers, Matt S.; Couch, Warrick J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Nulsen, Paul E. J.] 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@astro.swin.edu.au
OI Owers, Matt/0000-0002-2879-1663; Nulsen, Paul/0000-0003-0297-4493
FU Australian Research Council; Commonwealth of Australia; NASA
[NAS8-03060]; W. M. Keck Foundation
FX We thank Michael Cooper and Jeffrey Newman for their help with spec2d.
M.S.O. and W.J.C. gratefully acknowledge the financial support of an
Australian Research Council Discovery Project grant throughout the
course of this work. M.S.O. and W.J.C. acknowledge travel support from
the Australian Nuclear Science and Technology Organisation's access to
major research facilities program which is supported by the Commonwealth
of Australia under the International Science Linkages program. P.E.J.N.
was partly supported by NASA grant NAS8-03060. We acknowledge the Keck
data used in this paper was obtained through the Swinburne Time
Allocation Committee for Keck (STACK). 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. Some of the observations reported here
were obtained at the MMT Observatory, a joint facility of the
Smithsonian Institution and the University of Arizona. We thank the MMT
operators and queue-schedule mode scientists for their help during
observations and the staff at the Harvard-Smithsonian Center for
Astrophysics Telescope Data Center for reducing the Hectospec data.;
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 58
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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 NOV 10
PY 2011
VL 741
IS 2
AR 122
DI 10.1088/0004-637X/741/2/122
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500055
ER
PT J
AU Rangelov, B
Prestwich, AH
Chandar, R
AF Rangelov, Blagoy
Prestwich, Andrea H.
Chandar, Rupali
TI THE CONNECTION BETWEEN X-RAY BINARIES AND STAR CLUSTERS IN NGC 4449
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; galaxies: individual (NGC 4449); galaxies: star
clusters: general; stars: evolution
ID IRREGULAR GALAXY NGC-4449; TELESCOPE ADVANCED CAMERA; PHOTOMETRIC
PERFORMANCE; INTERSTELLAR EXTINCTION; CHANDRA OBSERVATIONS; ANTENNAE
GALAXIES; MASS FUNCTION; FIELD; CALIBRATION; EVOLUTION
AB We present 23 candidate X-ray binaries with luminosities down to 1.8 x 10(36) erg s(-1), in the nearby starburst galaxy NGC 4449, from observations totaling 105 ks taken with the ACIS-S instrument on the Chandra Space Telescope. We determine count rates, luminosities, and colors for each source, and perform spectral fits for sources with sufficient counts. We also compile a new catalog of 129 compact star clusters in NGC 4449 from high-resolution, multi-band optical images taken with the Hubble Space Telescope, doubling the number of clusters known in this galaxy. The UBVI, H alpha luminosities of each cluster are compared with predictions from stellar evolution models to estimate their ages and masses. We find strong evidence for a population of very young massive, black hole binaries, which comprise nearly 50% of the detected X-ray binaries in NGC 4449. Approximately a third of these remain within their parent star clusters, which formed tau less than or similar to 6-8 Myr ago, while others have likely been ejected from their parent clusters. We also find evidence for a population of somewhat older X-ray binaries, including both supergiant and Be-binaries, which appear to be associated with somewhat older tau approximate to 100-400 Myr star clusters, and one X-ray binary in an ancient (tau approximate to 10 Gyr) globular cluster. Our results suggest that detailed information on star clusters can significantly improve constraints on X-ray binary populations in star-forming galaxies.
C1 [Rangelov, Blagoy; Chandar, Rupali] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Prestwich, Andrea H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Rangelov, B (reprint author), Univ Toledo, Dept Phys & Astron, 2801 W Bancroft St, Toledo, OH 43606 USA.
EM blagoy.rangelov@gmail.com
FU NASA [NAS8-39073, AR8-9010]
FX We thank the anonymous referee, whose careful reading and helpful
suggestions significantly improved our manuscript. This work was
supported by NASA contract NAS8-39073 (CXC) and NASA AR8-9010.
NR 46
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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 NOV 10
PY 2011
VL 741
IS 2
AR 86
DI 10.1088/0004-637X/741/2/86
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500019
ER
PT J
AU Rathborne, JM
Garay, G
Jackson, JM
Longmore, S
Zhang, Q
Simon, R
AF Rathborne, J. M.
Garay, G.
Jackson, J. M.
Longmore, S.
Zhang, Q.
Simon, R.
TI HOT MOLECULAR CORES IN INFRARED DARK CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; radio lines: ISM; stars: formation; submillimeter: ISM
ID MASSIVE STAR-FORMATION; PROTOSTELLAR CANDIDATES; SUBMILLIMETER ARRAY;
HIGH-RESOLUTION; CO OUTFLOWS; DISCOVERY; EMISSION; SEARCH; REGION;
SAMPLE
AB We present high angular resolution continuum images and molecular line spectra obtained at 345 GHz with the Submillimeter Array (SMA) toward two massive cores that lie within Infrared Dark Clouds (IRDCs): G034.43+00.24 MM1 and G024.33+00.11 MM1. Both of these cores contain bright, unresolved (<2 '') objects that have previously been imaged in the millimeter/submillimeter continuum with the Institut de RadioAstronomie Millimetrique (IRAM) Plateau de Bure Interferometer and SMA and show complex molecular line chemistry. The new, higher angular resolution SMA continuum images reveal that both cores contain massive (8, 26 M(circle dot)), unresolved (0 ''.6; similar to 3000 AU) continuum emission features and emission from many complex molecular transitions, which confirm that these are hot molecular cores, an early stage in the formation of a high-mass star. Because these hot cores are located within IRDCs, they may well represent the very earliest phases in the formation of high-mass protostars and, hence, their detailed study may reveal the initial conditions within high-mass star-forming cores, before they are shredded apart by stellar winds and radiation.
C1 [Rathborne, J. M.; Garay, G.] Univ Chile, Dept Astron, Santiago, Chile.
[Jackson, J. M.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Longmore, S.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Simon, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
RP Rathborne, JM (reprint author), CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia.
EM rathborn@das.uchile.cl; guido@das.uchile.cl; jackson@bu.edu;
slongmore@cfa.harvard.edu; qzhang@cfa.harvard.edu;
simonr@ph1.uni-koeln.de
RI Garay, Guido/H-8840-2013;
OI Garay, Guido/0000-0003-1649-7958; Zhang, Qizhou/0000-0003-2384-6589
FU CONICYT [15010003]; BASAL [PFB-06]; US National Science Foundation
[AST-0808001]
FX This research made use of the myXCLASS program
(http://www.astro.uni-koeln.de/projects/schilke/XCLASS), which accesses
the CDMS (http://www.cdms.de) and JPL (http://spec.jpl.nasa.gov)
molecular data bases. Special thanks go to Peter Schilke for making
xclass available to us and especially Sebastien Maret for help
installing mySQL and xclass. Thanks to Debra Shepherd for making her
12CO data available to us and to Keping Qiu for help with the
CH3CN fitting. G.G. acknowledges support from CONICYT through
projects FONDAP No. 15010003 and BASAL PFB-06. This work was supported
in part by the US National Science Foundation by grant AST-0808001.
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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 NOV 10
PY 2011
VL 741
IS 2
AR 120
DI 10.1088/0004-637X/741/2/120
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500053
ER
PT J
AU Snyder, GF
Cox, TJ
Hayward, CC
Hernquist, L
Jonsson, P
AF Snyder, Gregory F.
Cox, Thomas J.
Hayward, Christopher C.
Hernquist, Lars
Jonsson, Patrik
TI K+A GALAXIES AS THE AFTERMATH OF GAS-RICH MERGERS: SIMULATING THE
EVOLUTION OF GALAXIES AS SEEN BY SPECTROSCOPIC SURVEYS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: interactions; galaxies: starburst;
methods: numerical
ID SUPERMASSIVE BLACK-HOLES; POST-STARBURST GALAXIES; ACTIVE GALACTIC
NUCLEI; PARTICLE HYDRODYNAMICS SIMULATIONS; REDSHIFT SUBMILLIMETER
GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; QUASAR LUMINOSITY FUNCTION;
DIGITAL SKY SURVEY; SIMILAR-TO 2; STAR-FORMATION
AB Models of poststarburst (or "K+A") galaxies are constructed by combining fully three-dimensional hydrodynamic simulations of galaxy mergers with radiative transfer calculations of dust attenuation. Spectral line catalogs are generated automatically from moderate-resolution optical spectra calculated as a function of merger progress in each of a large suite of simulations. The mass, gas fraction, orbital parameters, and mass ratio of the merging galaxies are varied systematically, showing that the lifetime and properties of the K+A phase are strong functions of the merger scenario. K+A durations are generally less than or similar to 0.1-0.3 Gyr, significantly shorter than the commonly assumed 1 Gyr, which is obtained only in rare cases, owing to a wide variation in star formation histories resulting from different orbital and progenitor configurations. Combined with empirical merger rates, the model lifetimes predict rapidly rising K+A fractions as a function of redshift that are consistent with results of large spectroscopic surveys, resolving tension between the observed K+A abundance and that predicted when one assumes the K+A duration is the lifetime of A stars (similar to 1 Gyr). These simulated spectra are spatially resolved on scales of about 1 kpc, and indicate that a centrally concentrated starburst causes the Balmer absorption strengths to increase toward the central few kiloparsecs of the remnant. The effects of dust attenuation, viewing angle, and aperture bias on our models are analyzed. In some cases, the K+A features are longer-lived and more pronounced when active galactic nucleus (AGN) feedback removes dust from the center, uncovering the young stars formed during the burst. In this picture, the K+A phase begins during or shortly after the bright starburst/AGN phase in violent mergers, and thus offers a unique opportunity to study the effects of quasar and star formation feedback on the gas reservoir and evolution of the remnant. Analytic fitting formulae are provided for the estimates of K+A incidence as a function of merger scenario.
C1 [Snyder, Gregory F.; Hayward, Christopher C.; Hernquist, Lars; Jonsson, Patrik] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cox, Thomas J.] Carnegie Observ, Pasadena, CA 91101 USA.
RP Snyder, GF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Hayward, Christopher/I-4756-2012
OI Hayward, Christopher/0000-0003-4073-3236
FU W. M. Keck Foundation; FAS Research Computing Group at Harvard
University
FX G.F.S. gratefully acknowledges helpful discussions with Gurtina Besla,
Elena D'Onghia, Tomotsugu Goto, Daniel McIntosh, Desika Narayanan, Paul
Torrey, Vivienne Wild, Ann Zabludoff, and Dennis Zaritsky at various
points of this work. P.J. acknowledges support from the W. M. Keck
Foundation. We thank the anonymous referee for numerous essential
suggestions. The computations in this paper were run on the Odyssey
cluster supported by the FAS Research Computing Group at Harvard
University.
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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 NOV 10
PY 2011
VL 741
IS 2
AR 77
DI 10.1088/0004-637X/741/2/77
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500010
ER
PT J
AU Williams, BJ
Blair, WP
Blondin, JM
Borkowski, KJ
Ghavamian, P
Long, KS
Raymond, JC
Reynolds, SP
Rho, J
Winkler, PF
AF Williams, Brian J.
Blair, William P.
Blondin, John M.
Borkowski, Kazimierz J.
Ghavamian, Parviz
Long, Knox S.
Raymond, John C.
Reynolds, Stephen P.
Rho, Jeonghee
Winkler, P. Frank
TI RCW 86: A TYPE Ia SUPERNOVA IN A WIND-BLOWN BUBBLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; dust, extinction; ISM: supernova remnants
ID LARGE-MAGELLANIC-CLOUD; X-RAY SPECTROSCOPY; HIGH-RESOLUTION
SPECTROSCOPY; BALMER-DOMINATED SHOCKS; SPITZER-SPACE-TELESCOPE; DUST
DESTRUCTION; REMNANT RCW-86; CYGNUS LOOP; NONRADIATIVE SHOCK; SUZAKU
OBSERVATION
AB We report results from a multi-wavelength analysis of the Galactic supernova remnant RCW 86, the proposed remnant of the supernova of 185 A. D. We show new infrared observations from the Spitzer Space Telescope and the Wide-Field Infrared Survey Explorer, where the entire shell is detected at 24 and 22 mu m. We fit the infrared flux ratios with models of collisionally heated ambient dust, finding post-shock gas densities in the non-radiative shocks of 2.4 and 2.0 cm(-3) in the southwest (SW) and northwest (NW) portions of the remnant, respectively. The Balmer-dominated shocks around the periphery of the shell, large amount of iron in the X-ray-emitting ejecta, and lack of a compact remnant support a Type Ia origin for this remnant. From hydrodynamic simulations, the observed characteristics of RCW 86 are successfully reproduced by an off-center explosion in a low-density cavity carved by the progenitor system. This would make RCW 86 the first known case of a Type Ia supernova in a wind-blown bubble. The fast shocks (>3000 km s(-1)) observed in the northeast are propagating in the low-density bubble, where the shock is just beginning to encounter the shell, while the slower shocks elsewhere have already encountered the bubble wall. The diffuse nature of the synchrotron emission in the SW and NW is due to electrons that were accelerated early in the lifetime of the remnant, when the shock was still in the bubble. Electrons in a bubble could produce gamma rays by inverse-Compton scattering. The wind-blown bubble scenario requires a single-degenerate progenitor, which should leave behind a companion star.
C1 [Williams, Brian J.; Blondin, John M.; Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Ghavamian, Parviz; Long, Knox S.] STScI, Baltimore, MD 21218 USA.
[Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rho, Jeonghee] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
RP Williams, BJ (reprint author), N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
EM bjwilli2@ncsu.edu
FU JPL RSA [1378047]; NSF [AST-0708224]; NASA [NNX11AB14G]; NASA
FX We acknowledge support from Spitzer Guest Observer Grants JPL RSA
1378047, NSF Theory Grant AST-0708224, and NASA Astrophysics Data and
Analysis Program Grant NNX11AB14G. 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 has made use of software provided by
the Chandra X-ray Center (CXC) in the application package CIAO. Support
for this work was provided by NASA through an award issued by
JPL/Caltech.
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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 NOV 10
PY 2011
VL 741
IS 2
AR 96
DI 10.1088/0004-637X/741/2/96
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TT
UT WOS:000296771500029
ER
PT J
AU Jedlicka, JA
Greenberg, R
Letourneau, DK
AF Jedlicka, Julie A.
Greenberg, Russell
Letourneau, Deborah K.
TI Avian Conservation Practices Strengthen Ecosystem Services in California
Vineyards
SO PLOS ONE
LA English
DT Article
ID REDUCE CATERPILLAR DAMAGE; APPLE ORCHARDS; COFFEE FARMS; GREAT TITS; SUN
COFFEE; PREDATORS; BIRDS; PEST; BIODIVERSITY; SHADE
AB Insectivorous Western Bluebirds (Sialia mexicana) occupy vineyard nest boxes established by California winegrape growers who want to encourage avian conservation. Experimentally, the provision of available nest sites serves as an alternative to exclosure methods for isolating the potential ecosystem services provided by foraging birds. We compared the abundance and species richness of avian foragers and removal rates of sentinel prey in treatments with songbird nest boxes and controls without nest boxes. The average species richness of avian insectivores increased by over 50 percent compared to controls. Insectivorous bird density nearly quadrupled, primarily due to a tenfold increase in Western Bluebird abundance. In contrast, there was no significant difference in the abundance of omnivorous or granivorous bird species some of which opportunistically forage on grapes. In a sentinel prey experiment, 2.4 times more live beet armyworms (Spodoptera exigua) were removed in the nest box treatment than in the control. As an estimate of the maximum foraging services provided by insectivorous birds, we found that larval removal rates measured immediately below occupied boxes averaged 3.5 times greater than in the control. Consequently the presence of Western Bluebirds in vineyard nest boxes strengthened ecosystem services to winegrape growers, illustrating a benefit of agroecological conservation practices. Predator addition and sentinel prey experiments lack some disadvantages of predator exclusion experiments and were robust methodologies for detecting ecosystem services.
C1 [Jedlicka, Julie A.; Letourneau, Deborah K.] Univ Calif Santa Cruz, Dept Environm Studies, Santa Cruz, CA 95064 USA.
[Greenberg, Russell] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA.
RP Jedlicka, JA (reprint author), Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
EM julie.jedlicka@gmail.com
FU The Organic Farming Research Foundation; Animal Behavior Society; Wilson
Ornithological Society; Smithsonian Migratory Bird Center; Annie's
Sustainable Agriculture Graduate Scholarship; Environmental Studies
Department at University of California Santa Cruz
FX Funding for this research was provided by: The Organic Farming Research
Foundation (http://ofrf.org); Animal Behavior Society
(http://animalbehaviorsociety.org); Wilson Ornithological Society
(http://www.wilsonsociety.org); Smithsonian Migratory Bird Center
(http://nationalzoo.si.edu/scbi/migratorybirds/default.cfm); Annie's
Sustainable Agriculture Graduate Scholarship
(http://www.annies.com/sustainable_agriculture_scholarship); and the
Environmental Studies Department at University of California Santa Cruz
(http://envs.ucsc.edu). The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 58
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U2 73
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD NOV 9
PY 2011
VL 6
IS 11
AR e27347
DI 10.1371/journal.pone.0027347
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 852II
UT WOS:000297350800046
PM 22096555
ER
PT J
AU Choi, S
Onofrio, R
Sundaram, B
AF Choi, Stephen
Onofrio, Roberto
Sundaram, Bala
TI Optimized sympathetic cooling of atomic mixtures via fast adiabatic
strategies
SO PHYSICAL REVIEW A
LA English
DT Article
ID DEPENDENT HARMONIC-OSCILLATOR; QUANTUM-SYSTEMS; FERMI GASES
AB We discuss fast frictionless cooling techniques in the framework of sympathetic cooling of cold atomic mixtures. It is argued that optimal cooling of an atomic species-in which the deepest quantum degeneracy regime is achieved-may be obtained by means of sympathetic cooling with another species whose trapping frequency is dynamically changed to maintain constancy of the Lewis-Riesenfeld adiabatic invariant. Advantages and limitations of this cooling strategy are discussed, with particular regard to the possibility of cooling Fermi gases to a deeper degenerate regime.
C1 [Choi, Stephen; Onofrio, Roberto; Sundaram, Bala] Univ Massachusetts, Dept Phys, Boston, MA 02125 USA.
[Onofrio, Roberto] Univ Padua, Dipartimento Fis Galileo Galilei, I-35131 Padua, Italy.
[Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA.
RP Choi, S (reprint author), Univ Massachusetts, Dept Phys, Boston, MA 02125 USA.
RI Sundaram, Bala/A-6532-2010
OI Sundaram, Bala/0000-0002-1728-704X
NR 24
TC 28
Z9 28
U1 0
U2 5
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 NOV 9
PY 2011
VL 84
IS 5
AR 051601
DI 10.1103/PhysRevA.84.051601
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 845VD
UT WOS:000296851100002
ER
PT J
AU Lerner, HRL
Meyer, M
James, HF
Hofreiter, M
Fleischer, RC
AF Lerner, Heather R. L.
Meyer, Matthias
James, Helen F.
Hofreiter, Michael
Fleischer, Robert C.
TI Multilocus Resolution of Phylogeny and Timescale in the Extant Adaptive
Radiation of Hawaiian Honeycreepers
SO CURRENT BIOLOGY
LA English
DT Article
ID MOLECULAR CLOCK; GENE TREES; EVOLUTION; DIVERGENCE; BIRDS;
DIVERSIFICATION; ISLANDS; RATES
AB Evolutionary theory has gained tremendous insight from studies of adaptive radiations. High rates of speciation, morphological divergence, and hybridization, combined with low sequence variability, however, have prevented phylogenetic reconstruction for many radiations. The Hawaiian honeycreepers are an exceptional adaptive radiation, with high phenotypic diversity and speciation that occurred within the geologically constrained setting of the Hawaiian Islands. Here we analyze a new data set of 13 nuclear loci and pyrosequencing of mitochondrial genomes that resolves the Hawaiian honeycreeper phylogeny. We show that they are a sister taxon to Eurasian rosefinches (Carpodacus) and probably came to Hawaii from Asia. We use island ages to calibrate DNA substitution rates, which vary substantially among gene regions, and calculate divergence times, showing that the radiation began roughly when the oldest of the current large Hawaiian Islands (Kauai and Niihau) formed, similar to 5.7 million years ago (mya). We show that most of the lineages that gave rise to distinctive morphologies diverged after Oahu emerged (4.0-3.7 mya) but before the formation of Maui and adjacent islands (2.4-1.9 mya). Thus, the formation of Oahu, and subsequent cycles of colonization and speciation between Kauai and Oahu, played key roles in generating the morphological diversity of the extant honeycreepers.
C1 [Lerner, Heather R. L.; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA.
[Lerner, Heather R. L.; James, Helen F.; Fleischer, Robert C.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Meyer, Matthias; Hofreiter, Michael] Max Planck Inst Evolutionary Anthropol, D-04103 Leipzig, Germany.
[James, Helen F.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Hofreiter, Michael] Univ York, Dept Biol, York YO10 5DD, N Yorkshire, England.
RP Lerner, HRL (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk,POB 37012,MRC 5513, Washington, DC 20013 USA.
EM hlerner@gmail.com
RI Hofreiter, Michael/A-3996-2017
OI Hofreiter, Michael/0000-0003-0441-4705
FU National Science Foundation [DEB-0643291]; Smithsonian Institution
Center for Conservation and Evolutionary Genetics; Smithsonian Scholarly
Studies Program; Max Planck Society
FX We would like to thank those who contributed tissues and the museum
curators and collection managers (see Supplemental Information) who have
accommodated us. We thank Nancy Rotzel, Joshua Miller, Zachary Sanford,
and the Max Planck Institute for Evolutionary Anthropology for
assistance in the lab. Remco Bouckart, Joseph Heled, Matthew Kweskin,
and Michael Lerner provided technical support. Jack Jeffrey permitted
our use of his stunning Hawaiian honeycreeper photographs in Figure 2,
and H. Douglas Pratt provided the lovely cover art. Support for this
research was provided by National Science Foundation DEB-0643291, the
Smithsonian Institution Center for Conservation and Evolutionary
Genetics, the Smithsonian Scholarly Studies Program, and the Max Planck
Society.
NR 33
TC 143
Z9 143
U1 23
U2 134
PU CELL PRESS
PI CAMBRIDGE
PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA
SN 0960-9822
J9 CURR BIOL
JI Curr. Biol.
PD NOV 8
PY 2011
VL 21
IS 21
BP 1838
EP 1844
DI 10.1016/j.cub.2011.09.039
PG 7
WC Biochemistry & Molecular Biology; Cell Biology
SC Biochemistry & Molecular Biology; Cell Biology
GA 849QG
UT WOS:000297139600024
PM 22018543
ER
PT J
AU Loreau, J
Zhang, P
Dalgarno, A
AF Loreau, Jerome
Zhang, Peng
Dalgarno, Alexander
TI Elastic scattering and rotational excitation of nitrogen molecules by
sodium atoms
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
DE atom-molecule collisions; coupled cluster calculations; excited states;
molecular moments; nitrogen; polarisability; potential energy surfaces;
rotational states; rotational-vibrational energy transfer; sodium
ID COUPLED-CLUSTER THEORY; COMPOUND STATE RESONANCES; GAUSSIAN-BASIS SETS;
POLARIZATION PROPAGATOR; CROSS-SECTIONS; ENERGIES; POLARIZABILITIES;
FREQUENCY; HYDROGEN; MODEL
AB A quantal study of the rotational excitation of nitrogen molecules by sodium atoms is carried out. We present the two-dimensional potential energy surface of the NaN2 complex, with the N-2 molecule treated as a rigid rotor. The interaction potential is computed using the spin unrestricted coupled-cluster method with single, double, and perturbative triple excitations (UCCSD(T)). The long-range part of the potential is constructed from the dynamic electric dipole polarizabilities of Na and N-2. The total, differential, and momentum transfer cross sections for rotationally elastic and inelastic transitions are calculated using the close-coupling approach for energies between 5 cm(-1) and 1500 cm(-1). The collisional and momentum transfer rate coefficients are calculated for temperatures between 100K and 300 K, corresponding to the conditions under which Na-N-2 collisions occur in the mesosphere. (C) 2011 American Institute of Physics. [doi:10.1063/1.3653983]
C1 [Loreau, Jerome; Zhang, Peng; Dalgarno, Alexander] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 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 We thank D. Budker, R. Holzlohner and their collaborators for useful
discussions. J.L. is supported by a fellowship from the Belgian American
Educational Foundation. 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 31
TC 8
Z9 8
U1 0
U2 4
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 NOV 7
PY 2011
VL 135
IS 17
AR 174301
DI 10.1063/1.3653983
PG 9
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 844FO
UT WOS:000296733300012
PM 22070297
ER
PT J
AU Asher, RJ
Helgen, KM
AF Asher, Robert J.
Helgen, Kristofer M.
TI High level Mammalian taxonomy: a response to Hedges (2011)
SO ZOOTAXA
LA English
DT Letter
C1 [Asher, Robert J.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England.
[Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Asher, RJ (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England.
NR 6
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 NOV 7
PY 2011
IS 3092
BP 63
EP 64
PG 2
WC Zoology
SC Zoology
GA 882HP
UT WOS:000299554700005
ER
PT J
AU Hietz, P
Turner, BL
Wanek, W
Richter, A
Nock, CA
Wright, SJ
AF Hietz, Peter
Turner, Benjamin L.
Wanek, Wolfgang
Richter, Andreas
Nock, Charles A.
Wright, S. Joseph
TI Long-Term Change in the Nitrogen Cycle of Tropical Forests
SO SCIENCE
LA English
DT Article
ID N DEPOSITION; CONSEQUENCES; DELTA-N-15; ABUNDANCE; FOLIAR; LOSSES;
TRENDS; IMPACT; FUTURE
AB Deposition of reactive nitrogen (N) from human activities has large effects on temperate forests where low natural N availability limits productivity but is not known to affect tropical forests where natural N availability is often much greater. Leaf N and the ratio of N isotopes (delta N-15) increased substantially in a moist forest in Panama between similar to 1968 and 2007, as did tree-ring delta N-15 in a dry forest in Thailand over the past century. A decade of fertilization of a nearby Panamanian forest with N caused similar increases in leaf N and delta N-15. Therefore, our results indicate regional increases in N availability due to anthropogenic N deposition. Atmospheric nitrogen dioxide measurements and increased emissions of anthropogenic reactive N over tropical land areas suggest that these changes are widespread in tropical forests.
C1 [Hietz, Peter] Univ Nat Resources & Life Sci, Inst Bot, A-1180 Vienna, Austria.
[Turner, Benjamin L.; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Wanek, Wolfgang] Univ Vienna, Dept Chem Ecol & Ecosyst Res, A-1090 Vienna, Austria.
[Richter, Andreas] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany.
[Nock, Charles A.] Univ Quebec, Dept Sci Biol, Ctr Etud Foret, Montreal, PQ H3C 3P8, Canada.
RP Hietz, P (reprint author), Univ Nat Resources & Life Sci, Inst Bot, Gregor Mendel Str 33, A-1180 Vienna, Austria.
EM peter.hietz@boku.ac.at
RI Turner, Benjamin/E-5940-2011; Wanek, Wolfgang/E-7001-2012; Richter,
Andreas/C-4971-2008; Wright, Stuart/M-3311-2013;
OI Turner, Benjamin/0000-0002-6585-0722; Wanek,
Wolfgang/0000-0003-2178-8258; Richter, Andreas/0000-0003-3339-212X;
Wright, Stuart/0000-0003-4260-5676; Hietz, Peter/0000-0002-0458-6593
FU F. H. Levinson Fund; Austrian Science Fund [P19507-B17]
FX We thank D. Agudo, T. Romero, U. Hietz-Seifert, and M. Watzka for
laboratory support and the F. H. Levinson Fund and the Austrian Science
Fund (grant P19507-B17) for funding. P. H. took herbarium and wood
samples and analyzed the leaf, wood, and N emission data; S.J.W.
provided 2007 leaves; B. L. T. analyzed 2007 leaves; W. W. analyzed
herbarium leaves and wood; C. A. N. synchronized wood cores; A. R.
analyzed satellite data; and P. H., B. L. T., and S.J.W. wrote the
manuscript. All authors contributed to the discussion of the data. Leaf
and wood data are available from P. H.; NO2 satellite data
are available from A.R.
NR 25
TC 103
Z9 107
U1 11
U2 160
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 NOV 4
PY 2011
VL 334
IS 6056
BP 664
EP 666
DI 10.1126/science.1211979
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 841EG
UT WOS:000296494700053
PM 22053047
ER
PT J
AU Aplin, KP
Suzuki, H
Chinen, AA
Chesser, RT
ten Have, J
Donnellan, SC
Austin, J
Frost, A
Gonzalez, JP
Herbreteau, V
Catzeflis, F
Soubrier, J
Fang, YP
Robins, J
Matisoo-Smith, E
Bastos, ADS
Maryanto, I
Sinaga, MH
Denys, C
Van den Bussche, RA
Conroy, C
Rowe, K
Cooper, A
AF Aplin, Ken P.
Suzuki, Hitoshi
Chinen, Alejandro A.
Chesser, R. Terry
ten Have, Jose
Donnellan, Stephen C.
Austin, Jeremy
Frost, Angela
Gonzalez, Jean Paul
Herbreteau, Vincent
Catzeflis, Francois
Soubrier, Julien
Fang, Yin-Ping
Robins, Judith
Matisoo-Smith, Elizabeth
Bastos, Amanda D. S.
Maryanto, Ibnu
Sinaga, Martua H.
Denys, Christiane
Van den Bussche, Ronald A.
Conroy, Chris
Rowe, Kevin
Cooper, Alan
TI Multiple Geographic Origins of Commensalism and Complex Dispersal
History of Black Rats
SO PLOS ONE
LA English
DT Article
ID RATTUS SENSU-LATO; POPULATION-GROWTH; EVOLUTIONARY RELATIONSHIPS;
STATISTICAL TESTS; MITOCHONDRIAL-DNA; MOLECULAR CLOCKS; LATE
PLEISTOCENE; TIME DEPENDENCY; GENE-SEQUENCES; MADAGASCAR
AB The Black Rat (Rattus rattus) spread out of Asia to become one of the world's worst agricultural and urban pests, and a reservoir or vector of numerous zoonotic diseases, including the devastating plague. Despite the global scale and inestimable cost of their impacts on both human livelihoods and natural ecosystems, little is known of the global genetic diversity of Black Rats, the timing and directions of their historical dispersals, and the risks associated with contemporary movements. We surveyed mitochondrial DNA of Black Rats collected across their global range as a first step towards obtaining an historical genetic perspective on this socioeconomically important group of rodents. We found a strong phylogeographic pattern with well-differentiated lineages of Black Rats native to South Asia, the Himalayan region, southern Indochina, and northern Indochina to East Asia, and a diversification that probably commenced in the early Middle Pleistocene. We also identified two other currently recognised species of Rattus as potential derivatives of a paraphyletic R. rattus. Three of the four phylogenetic lineage units within R. rattus show clear genetic signatures of major population expansion in prehistoric times, and the distribution of particular haplogroups mirrors archaeologically and historically documented patterns of human dispersal and trade. Commensalism clearly arose multiple times in R. rattus and in widely separated geographic regions, and this may account for apparent regionalism in their associated pathogens. Our findings represent an important step towards deeper understanding the complex and influential relationship that has developed between Black Rats and humans, and invite a thorough re-examination of host-pathogen associations among Black Rats.
C1 [Aplin, Ken P.; Frost, Angela] CSIRO Ecosystem Sci, Australian Natl Wildlife Collect, Canberra, ACT, Australia.
[Suzuki, Hitoshi; Chinen, Alejandro A.] Hokkaido Univ, Grad Sch Environm Earth Sci, Sapporo, Hokkaido 060, Japan.
[Chesser, R. Terry] Smithsonian Inst, Div Birds, Washington, DC 20560 USA.
[ten Have, Jose] Off Gene Technol Regulator, Canberra, ACT, Australia.
[Donnellan, Stephen C.] Univ Adelaide, S Australian Museum, Adelaide, SA, Australia.
[Donnellan, Stephen C.] Univ Adelaide, Australian Ctr Evolutionary Biol & Biodivers, Adelaide, SA, Australia.
[Austin, Jeremy; Soubrier, Julien; Cooper, Alan] Univ Adelaide, Australian Ctr Ancient DNA, Adelaide, SA, Australia.
[Gonzalez, Jean Paul; Herbreteau, Vincent] Mahidol Univ, Inst Rech Dev, Res Unit 178, Ctr Vectors & Vector Dis,Fac Sci, Nakhon Pathom, Thailand.
[Catzeflis, Francois] Univ Montpellier 2, Inst Sci Evolut, Lab Paleontol Phylogenie & Paleobiol, Montpellier, France.
[Fang, Yin-Ping] Natl Chiayi Univ, Dept Biol Resources, Chiayi, Taiwan.
[Robins, Judith] Univ Auckland, Dept Anthropol, Auckland 1, New Zealand.
[Matisoo-Smith, Elizabeth] Univ Otago, Dept Anat & Struct Biol, Dunedin, New Zealand.
[Bastos, Amanda D. S.] Univ Pretoria, Mammal Res Inst, Dept Zool & Entomol, ZA-0002 Pretoria, South Africa.
[Maryanto, Ibnu; Sinaga, Martua H.] Indonesian Inst Sci LIPI, Cibinong, West Java, Indonesia.
[Denys, Christiane] Museum Natl Hist Nat, Dept Systemat & Evolut, F-75231 Paris, France.
[Van den Bussche, Ronald A.] Oklahoma State Univ, Dept Zool, Stillwater, OK 74078 USA.
[Conroy, Chris; Rowe, Kevin] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA.
[Maryanto, Ibnu; Sinaga, Martua H.] Museum Bogoriense, Cibinong, West Java, Indonesia.
RP Aplin, KP (reprint author), CSIRO Ecosystem Sci, Australian Natl Wildlife Collect, Canberra, ACT, Australia.
EM aplin.ken@gmail.com
RI Bastos, Armanda/B-6357-2009; Austin, Jeremy/F-8729-2010; Cooper,
Alan/E-8171-2012; Suzuki, Hitoshi/F-8539-2012; Donnellan,
Stephen/F-2442-2013; Herbreteau, Vincent/L-4411-2013; Soubrier,
Julien/B-9951-2014;
OI Bastos, Armanda/0000-0002-9223-4204; Austin, Jeremy/0000-0003-4244-2942;
Cooper, Alan/0000-0002-7738-7851; Suzuki, Hitoshi/0000-0003-4426-385X;
Donnellan, Stephen/0000-0002-5448-3226; Herbreteau,
Vincent/0000-0003-1762-6336; Soubrier, Julien/0000-0001-9350-7369;
Gonzalez, Jean-Paul/0000-0003-3063-1770
FU Australian Centre for International Agricultural Research (ACIAR);
Australian Government; Department for International Development(DfID)
[R8190]; National Science Council; Council of Agriculture, Republic of
China; European Commission's INCO-DEV [(ICA4-CT2002-10056]
FX Funding support that allowed KA and AF to collect samples in Myanmar,
Vietnam, Laos and Cambodia was provided by Australian Centre for
International Agricultural Research (ACIAR - (http://aciar.gov.au/) and
AusAID (http://www.ausaid.gov.au/), funding agencies of the Australian
Government. Collecting by KA in Bangladesh was supported by Department
for International Development(DfID) grants through the Poverty
Elimination through Rice Research Assistance and Crop Protection
Programme programmes. Y-PF was supported by grants from the National
Science Council (http://web1.nsc.gov.tw/) and the Council of Agriculture
(http://eng.coa.gov.tw/), Republic of China. AB was supported by DFID
(project number R8190) and the European Commission's INCO-DEV programme
(ICA4-CT2002-10056: Ratzooman - http://www.nri.org/ratzooman). CD's
collecting in Guinea was supported by the European Commission's INCO-DEV
programme (project 'TREATCONTROL'). The funders had no role in study
design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 100
TC 67
Z9 73
U1 6
U2 54
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 NOV 2
PY 2011
VL 6
IS 11
AR e26357
DI 10.1371/journal.pone.0026357
PG 20
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 849WB
UT WOS:000297154900019
PM 22073158
ER
PT J
AU Fisher, R
Knowlton, N
Brainard, RE
Caley, MJ
AF Fisher, Rebecca
Knowlton, Nancy
Brainard, Russell E.
Caley, M. Julian
TI Differences among Major Taxa in the Extent of Ecological Knowledge
across Four Major Ecosystems
SO PLOS ONE
LA English
DT Article
ID CORAL-REEF ECOSYSTEMS; MARINE ECOSYSTEMS; SPECIES RICHNESS; SEAGRASS
MEADOWS; BIODIVERSITY; RESILIENCE; DIVERSITY; FUTURE; ASSEMBLAGES;
MANAGEMENT
AB Existing knowledge shapes our understanding of ecosystems and is critical for ecosystem-based management of the world's natural resources. Typically this knowledge is biased among taxa, with some taxa far better studied than others, but the extent of this bias is poorly known. In conjunction with the publically available World Registry of Marine Species database (WoRMS) and one of the world's premier electronic scientific literature databases (Web of Science (R)), a text mining approach is used to examine the distribution of existing ecological knowledge among taxa in coral reef, mangrove, seagrass and kelp bed ecosystems. We found that for each of these ecosystems, most research has been limited to a few groups of organisms. While this bias clearly reflects the perceived importance of some taxa as commercially or ecologically valuable, the relative lack of research of other taxonomic groups highlights the problem that some key taxa and associated ecosystem processes they affect may be poorly understood or completely ignored. The approach outlined here could be applied to any type of ecosystem for analyzing previous research effort and identifying knowledge gaps in order to improve ecosystem-based conservation and management.
C1 [Fisher, Rebecca] Australian Inst Marine Sci, UWA Oceans Inst, Crawley, WA, Australia.
[Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA.
[Brainard, Russell E.] Natl Marine Fisheries Serv, Coral Reef Ecosyst Div, Pacific Isl Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, Honolulu, HI USA.
[Caley, M. Julian] Australian Inst Marine Sci, Townsville, Qld 4810, Australia.
RP Fisher, R (reprint author), Australian Inst Marine Sci, UWA Oceans Inst, Crawley, WA, Australia.
EM r.fisher@aims.gov.au
OI Fisher, Rebecca/0000-0001-5148-6731
FU BHP Billiton through CReefs Australia
FX This work was funded by BHP Billiton through CReefs Australia, a
partnership between BHP Billiton, the Great Barrier Reef Foundation, the
Census of Marine Life and the Australian Institute of Marine Science
(AIMS). CReefs Australia is a node of the Census of Coral Reef
Ecosystems (CReefs), a project of the Census of Marine Life. The funders
had no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.
NR 48
TC 6
Z9 6
U1 2
U2 24
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD NOV 2
PY 2011
VL 6
IS 11
AR e26556
DI 10.1371/journal.pone.0026556
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 849WB
UT WOS:000297154900024
PM 22073172
ER
PT J
AU Wood, B
Leakey, M
AF Wood, Bernard
Leakey, Meave
TI The Omo-Turkana Basin Fossil Hominins and Their Contribution to Our
Understanding of Human Evolution in Africa
SO EVOLUTIONARY ANTHROPOLOGY
LA English
DT Article
DE Australopithecus; Homo; Paranthropus; taxonomy; East Africa
ID LOWER PLEISTOCENE HOMINIDS; MODERN HUMAN ORIGINS; LATE PLIOCENE HOMO;
WEST LAKE TURKANA; KNM-WT 17000; AUSTRALOPITHECUS-BOISEI; OLDUVAI-GORGE;
EAST-RUDOLF; PLIOPLEISTOCENE HOMINID; PARANTHROPUS-BOISEI
AB The Omo-Turkana Basin, including the hominin fossil sites around Lake Turkana and the sites along the lower reaches of the Omo River, has made and continues to make an important contribution to improving our murky understanding of human evolution. This review highlights the various ways the Omo-Turkana Basin fossil record has contributed to, and continues to challenge, interpretations of human evolution. Despite many diagrams that look suspiciously like comprehensive hypotheses about human evolutionary history, any sensible paleoanthropologist knows that the early hominin fossil record is too meager to do anything other than offer very provisional statements about hominin taxonomy and phylogeny. If history tells us anything, it is that we still have much to learn about the hominin clade. Thus, we summarize the current state of knowledge of the hominin species represented at the Omo-Turkana Basin sites. We then focus on three specific topics for which the fossil evidence is especially relevant: the origin and nature of Paranthropus; the origin and nature of early Homo; and the ongoing debate about whether the pattern of human evolution is more consistent with speciation by cladogenesis, with greater taxonomic diversity or with speciation by anagenetic transformation, resulting in less taxonomic diversity and a more linear interpretation of human evolutionary history. (C) Wiley Periodicals, Inc.
C1 [Wood, Bernard] George Washington Univ, Washington, DC 20052 USA.
[Wood, Bernard] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Leakey, Meave] SUNY Stony Brook, Dept Anthropol, New York, NY USA.
RP Wood, B (reprint author), George Washington Univ, Washington, DC 20052 USA.
EM bernardawood@gmail.com; meaveleakey@gmail.com
NR 130
TC 25
Z9 27
U1 4
U2 36
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1060-1538
J9 EVOL ANTHROPOL
JI Evol. Anthropol.
PD NOV-DEC
PY 2011
VL 20
IS 6
SI SI
BP 264
EP 292
DI 10.1002/evan.20335
PG 29
WC Anthropology
SC Anthropology
GA 862LA
UT WOS:000298091000010
PM 22170695
ER
PT J
AU Broersen, S
Vink, J
Kaastra, J
Raymond, J
AF Broersen, S.
Vink, J.
Kaastra, J.
Raymond, J.
TI The high resolution X-ray spectrum of SNR 0506-68 using XMM-Newton
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: supernova remnants; supernovae: general
ID LARGE-MAGELLANIC-CLOUD; SUPERNOVA REMNANT N23; IONIZATION EQUILIBRIUM;
DISCOVERY; EMISSION; ELEMENTS; PLASMA; SUZAKU; SPECTROSCOPY; DIAGNOSTICS
AB Aims. We study the supernova remnant 0506-68 in order to obtain detailed information about, among other things, the ionisation state and age of the ionised plasma.
Methods. Using the Reflection Grating Spectrometer (RGS) onboard the XMM-Newton satellite we are able to take detailed spectra of the remnant. In addition, we use the MOS data to obtain spectral information at higher energies.
Results. The spectrum shows signs of recombination and we derive the conditions for which the remnant and SNR in general are able to cool rapidly enough to become over-ionised. The elemental abundances found are mostly in agreement with the mean LMC abundances. Our models and calculations favour the lower age estimate mentioned in the literature of similar to 4000 year.
C1 [Broersen, S.; Vink, J.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands.
[Kaastra, J.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands.
[Raymond, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Broersen, S (reprint author), Univ Utrecht, Astron Inst, Postbus 80000, NL-3508 TA Utrecht, Netherlands.
EM s.broersen@astro-uu.nl
FU NWO, The Netherlands Organisation for Scientific Research; ESA Member
States; USA (NASA)
FX The authors thank the anonymous referee for their positive and useful
comments. We would like to acknowledge D. Kosenko and T. van Werkhoven
for useful input. S. B. and SRON are supported financially by NWO, The
Netherlands Organisation for Scientific Research. The results presented
are 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).
NR 24
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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 NOV
PY 2011
VL 535
AR A11
DI 10.1051/0004-6361/201117390
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 858YY
UT WOS:000297841200023
ER
PT J
AU Lombardi, M
Alves, J
Lada, CJ
AF Lombardi, M.
Alves, J.
Lada, C. J.
TI 2MASS wide field extinction maps IV. The Orion, Monoceros R2, Rosette,
and Canis Major star forming regions
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: clouds; ISM: structure; dust, extinction; methods: statistical
ID MOLECULAR CLOUDS; COLUMN-DENSITY; NGC 2244; PROBABILITY-DISTRIBUTION;
SUPERSONIC TURBULENCE; REFLECTION NEBULAE; INTRINSIC COLORS; DARK CLOUD;
IC 5146; PHOTOMETRY
AB We present a near-infrared extinction map of a large region (approximately 2200 deg(2)) covering the Orion, the Monoceros R2, the Rosette, and the Canis Major molecular clouds. We used robust and optimal methods to map the dust column density in the near-infrared (NICER and NICEST) towards similar to 19 million stars of the Two Micron All Sky Survey (2MASS) point source catalog. Over the relevant regions of the field, we reached a 1-sigma error of 0.03 mag in the K-band extinction with a resolution of 3 arcmin. We measured the cloud distances by comparing the observed density of foreground stars with the prediction of galactic models, thus obtaining d(OrionA) = (371 +/- 10) pc, d(OrionB) = (398 +/- 12) pc, d(MonR2) = (905 +/- 37) pc, d(Rosette) = (1330 +/- 48) pc, and d(CMa) = (1150 +/- 64) pc, values that compare very well independent estimates.
C1 [Lombardi, M.] Univ Milan, Dept Phys, I-20133 Milan, Italy.
[Alves, J.] Univ Vienna, A-1180 Vienna, Austria.
[Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lombardi, M (reprint author), Univ Milan, Dept Phys, Via Celoria 16, I-20133 Milan, Italy.
EM marco.lombardi@unimi.it
OI LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921
FU National Aeronautics and Space Administration
FX This research has made use of the 2MASS archive, provided by 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. Additionally, this
research has made use of the SIMBAD database, operated at CDS,
Strasbourg, France.
NR 49
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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 NOV
PY 2011
VL 535
AR A16
DI 10.1051/0004-6361/20116915
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 858YY
UT WOS:000297841200028
ER
PT J
AU Mainieri, V
Bongiorno, A
Merloni, A
Aller, M
Carollo, M
Iwasawa, K
Koekemoer, AM
Mignoli, M
Silverman, JD
Bolzonella, M
Brusa, M
Comastri, A
Gilli, R
Halliday, C
Ilbert, O
Lusso, E
Salvato, M
Vignali, C
Zamorani, G
Contini, T
Kneib, JP
Le Fevre, O
Lilly, S
Renzini, A
Scodeggio, M
Balestra, I
Bardelli, S
Caputi, K
Coppa, G
Cucciati, O
de la Torre, S
de Ravel, L
Franzetti, P
Garilli, B
Iovino, A
Kampczyk, P
Knobel, C
Kovac, K
Lamareille, F
Le Borgne, JF
Le Brun, V
Maier, C
Nair, P
Pello, R
Peng, Y
Montero, EP
Pozzetti, L
Ricciardelli, E
Tanaka, M
Tasca, L
Tresse, L
Vergani, D
Zucca, E
Aussel, H
Capak, P
Cappelluti, N
Elvis, M
Fiore, F
Hasinger, G
Impey, C
Le Floc'h, E
Scoville, N
Taniguchi, Y
Trump, J
AF Mainieri, V.
Bongiorno, A.
Merloni, A.
Aller, M.
Carollo, M.
Iwasawa, K.
Koekemoer, A. M.
Mignoli, M.
Silverman, J. D.
Bolzonella, M.
Brusa, M.
Comastri, A.
Gilli, R.
Halliday, C.
Ilbert, O.
Lusso, E.
Salvato, M.
Vignali, C.
Zamorani, G.
Contini, T.
Kneib, J. -P.
Le Fevre, O.
Lilly, S.
Renzini, A.
Scodeggio, M.
Balestra, I.
Bardelli, S.
Caputi, K.
Coppa, G.
Cucciati, O.
de la Torre, S.
de Ravel, L.
Franzetti, P.
Garilli, B.
Iovino, A.
Kampczyk, P.
Knobel, C.
Kovac, K.
Lamareille, F.
Le Borgne, J. -F.
Le Brun, V.
Maier, C.
Nair, P.
Pello, R.
Peng, Y.
Montero, E. Perez
Pozzetti, L.
Ricciardelli, E.
Tanaka, M.
Tasca, L.
Tresse, L.
Vergani, D.
Zucca, E.
Aussel, H.
Capak, P.
Cappelluti, N.
Elvis, M.
Fiore, F.
Hasinger, G.
Impey, C.
Le Floc'h, E.
Scoville, N.
Taniguchi, Y.
Trump, J.
TI Black hole accretion and host galaxies of obscured quasars in XMM-COSMOS
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE quasars: general; galaxies: active; galaxies: nuclei; X-rays: general;
galaxies: star formation
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; DEEP
FIELD-SOUTH; SPECTRAL ENERGY-DISTRIBUTIONS; POWERFUL RADIO GALAXIES;
HUBBLE-SPACE-TELESCOPE; STELLAR MASS DENSITY; EARLY DATA RELEASE;
X-RAY-ABSORPTION
AB Aims. We explore the connection between black hole growth at the center of obscured quasars selected from the XMM-COSMOS survey and the physical properties of their host galaxies. We study a bolometric regime (< L-bol > = 8 x 10(45) erg s(-1)) where several theoretical models invoke major galaxy mergers as the main fueling channel for black hole accretion.
Methods. To derive robust estimates of the host galaxy properties, we use an SED fitting technique to distinguish the AGN and host galaxy emission. We evaluate the effect on galaxy properties estimates of being unable to remove the nuclear emission from the SED. The superb multiwavelength coverage of the COSMOS field allows us to obtain reliable estimates of the total stellar masses and star formation rates (SFRs) of the hosts. We supplement this information with a morphological analysis of the ACS/HST images, optical spectroscopy, and an X-ray spectral analysis.
Results. We confirm that obscured quasars mainly reside in massive galaxies (M-* > 10(10) M-circle dot) and that the fraction of galaxies hosting such powerful quasars monotonically increases with the stellar mass. We stress the limitation of the use of rest-frame color-magnitude diagrams as a diagnostic tool for studying galaxy evolution and inferring the influence that AGN activity can have on such a process. We instead use the correlation between SFR and stellar mass found for star-forming galaxies to discuss the physical properties of the hosts. We find that at z similar to 1, approximate to 62% of Type-2 QSOs hosts are actively forming stars and that their rates are comparable to those measured for normal star-forming galaxies. The fraction of star-forming hosts increases with redshift: approximate to 71% at z similar to 2, and 100% at z similar to 3. We also find that the evolution from z similar to 1 to z similar to 3 of the specific SFR of the Type-2 QSO hosts is in excellent agreement with that measured for star-forming galaxies. From the morphological analysis, we conclude that most of the objects are bulge-dominated galaxies, and that only a few of them exhibit signs of recent mergers or disks. Finally, bulge-dominated galaxies tend to host Type-2 QSOs with low Eddington ratios (lambda < 0.1), while disk-dominated or merging galaxies have at their centers BHs accreting at high Eddington ratios (lambda > 0.1).
C1 [Mainieri, V.] ESO, D-85748 Garching, Germany.
[Bongiorno, A.; Merloni, A.; Brusa, M.; Balestra, I.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Merloni, A.] TUM, D-85748 Garching, Germany.
[Aller, M.; Carollo, M.; Lilly, S.; Kampczyk, P.; Knobel, C.; Maier, C.; Peng, Y.] ETH, Inst Astron, CH-8093 Zurich, Switzerland.
[Iwasawa, K.] Univ Barcelona, IEEC, ICREA, E-08028 Barcelona, Spain.
[Iwasawa, K.] Univ Barcelona, IEEC, ICC, E-08028 Barcelona, Spain.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Mignoli, M.; Bolzonella, M.; Comastri, A.; Gilli, R.; Lusso, E.; Zamorani, G.; Bardelli, S.; Coppa, G.; Nair, P.; Pozzetti, L.; Vergani, D.; Zucca, E.; Cappelluti, N.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Silverman, J. D.; Tanaka, M.] Univ Tokyo, IPMU, Kashiwa, Chiba 2778568, Japan.
[Halliday, C.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Ilbert, O.; Kneib, J. -P.; Le Fevre, O.; de Ravel, L.; Le Brun, V.; Tasca, L.; Tresse, L.] Astrophys Lab, Marseille, France.
[Lusso, E.; Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Salvato, M.; Hasinger, G.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Contini, T.; Lamareille, F.; Le Borgne, J. -F.; Pello, R.; Montero, E. Perez] Univ Toulouse, Lab Astrophys Toulouse Tarbes, CNRS, F-31400 Toulouse, France.
[Renzini, A.; Ricciardelli, E.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Scodeggio, M.; Cucciati, O.; Franzetti, P.; Garilli, B.] IASF Milano, INAF, Milan, Italy.
[Caputi, K.; de la Torre, S.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Iovino, A.] Osserv Astron Brera, INAF, Milan, Italy.
[Kovac, K.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Capak, P.; Scoville, N.] CALTECH, Pasadena, CA 91125 USA.
[Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Impey, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Fiore, F.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy.
[Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan.
[Trump, J.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA.
[Aussel, H.] Univ Paris 07, CEA, CNRS, AIM,Unite Mixte Rech,UMR 158, Paris, France.
[Le Floc'h, E.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
RP Mainieri, V (reprint author), ESO, Karl Schwarschild Str 2, D-85748 Garching, Germany.
EM vmainier@eso.org
RI Pello, Roser/G-4754-2010; Vignali, Cristian/J-4974-2012; Kneib,
Jean-Paul/A-7919-2015; Bardelli, Sandro/O-9369-2015; Zucca,
Elena/O-9396-2015; Mignoli, Marco/O-9426-2015; Bolzonella,
Micol/O-9495-2015; Comastri, Andrea/O-9543-2015; Gilli,
Roberto/P-1110-2015;
OI Koekemoer, Anton/0000-0002-6610-2048; Perez Montero,
E/0000-0003-3985-4882; Brusa, Marcella/0000-0002-5059-6848; Fiore,
Fabrizio/0000-0002-4031-4157; Balestra, Italo/0000-0001-9660-894X;
Bongiorno, Angela/0000-0002-0101-6624; Scodeggio,
Marco/0000-0002-2282-5850; Franzetti, Paolo/0000-0002-6986-0127;
Vergani, Daniela/0000-0003-0898-2216; Maier,
Christian/0000-0001-6405-2182; Garilli, Bianca/0000-0001-7455-8750;
Zamorani, Giovanni/0000-0002-2318-301X; Vignali,
Cristian/0000-0002-8853-9611; Kneib, Jean-Paul/0000-0002-4616-4989;
Bardelli, Sandro/0000-0002-8900-0298; Zucca, Elena/0000-0002-5845-8132;
Mignoli, Marco/0000-0002-9087-2835; Bolzonella,
Micol/0000-0003-3278-4607; Comastri, Andrea/0000-0003-3451-9970; Gilli,
Roberto/0000-0001-8121-6177; Iovino, Angela/0000-0001-6958-0304;
Pozzetti, Lucia/0000-0001-7085-0412
FU zCOSMOS [175.A-0839]; ESA; US (NASA); NASA [NAS 5-26555]; Italian Space
Agency (ASI) [ASI-INAF I/088/06/0, I/009/10/0]; German Deutsche
Forschungsgemeinschaft, DFG [FKZ HA 1850/28-1]
FX We are grateful to Hagai Netzer for inspiring discussions and to Giulia
Rodighiero for providing the Herschel curves in Fig. 9 in electronic
format. We thank the referee, Montse Villar-Martin, for a careful
reading of the manuscript and useful comments. This work is based on
observations made with ESO Telescopes at the La Silla/Paranal
Observatories under the zCOSMOS Large Programme 175.A-0839; the
XMM-Newton satellite, an ESA science mission with instruments and
contributions directly funded by ESA Member States and the US (NASA);
the Magellan Telescope, operated by the Carnegie Observatorie and the
MMT Observatory, a joint facility of the University of Arizona and the
Smithsonian Institution; the Subaru Telescope, operated by the National
Astronomical Observatory of Japan; and the NASA/ESA Hubble Space
Telescope, operated at the Space Telescope Science Institute, which is
operated by AURA Inc, under NASA contract NAS 5-26555. Support from the
Italian Space Agency (ASI) under the contracts ASI-INAF I/088/06/0 and
I/009/10/0 is acknowledged. G. H. and M. S. acknowledge support by the
German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA
1850/28-1).
NR 162
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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 NOV
PY 2011
VL 535
AR A80
DI 10.1051/0004-6361/201117259
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 858YY
UT WOS:000297841200092
ER
PT J
AU Kays, R
Tilak, S
Crofoot, M
Fountain, T
Obando, D
Ortega, A
Kuemmeth, F
Mandel, J
Swenson, G
Lambert, T
Hirsch, B
Wikelski, M
AF Kays, Roland
Tilak, Sameer
Crofoot, Margaret
Fountain, Tony
Obando, Daniel
Ortega, Alejandro
Kuemmeth, Franz
Mandel, Jamie
Swenson, George
Lambert, Thomas
Hirsch, Ben
Wikelski, Martin
TI Tracking Animal Location and Activity with an Automated Radio Telemetry
System in a Tropical Rainforest
SO COMPUTER JOURNAL
LA English
DT Article
DE sensor networks; animal tracking; environmental observing systems
ID AGOUTI DASYPROCTA-PUNCTATA; PREDATION; LOCALIZATION; DISPERSAL;
MOVEMENTS; SURVIVAL; ROBOTS; RISK; WILD
AB How do animals use their habitat? Where do they go and what do they do? These basic questions are key not only to understanding a species' ecology and evolution, but also for addressing many of the environmental challenges we currently face, including problems posed by invasive species, the spread of zoonotic diseases and declines in wildlife populations due to anthropogenic climate and land-use changes. Monitoring the movements and activities of wild animals can be difficult, especially when the species in question are small, cryptic or move over large areas. In this paper, we describe an Automated Radio-Telemetry System (ARTS) that we designed and built on Barro Colorado Island (BCI), Panama to overcome these challenges. We describe the hardware and software we used to implement the ARTS, and discuss the scientific successes we have had using the system, as well as the logistical challenges we faced in maintaining the system in real-world, rainforest conditions. The ARTS uses automated radio-telemetry receivers mounted on 40-m towers topped with arrays of directional antennas to track the activity and location of radio-collared study animals, 24 h a day, 7 days a week. These receiving units are connected by a wireless network to a server housed in the laboratory on BCI, making these data available in real time to researchers via a web-accessible database. As long as study animals are within the range of the towers, the ARTS system collects data more frequently than typical animal-borne global positioning system collars (similar to 12 locations/h) with lower accuracy (approximately 50 m) but at much reduced cost per tag (similar to 10X less expensive). The geographic range of ARTS, like all VHF telemetry, is affected by the size of the radio-tag as well as its position in the forest (e. g. tags in the canopy transmit farther than those on the forest floor). We present a model of signal propagation based on landscape conditions, which quantifies these effects and identifies sources of interference, including weather events and human activity. ARTS has been used to track 374 individual animals from 38 species, including 17 mammal species, 12 birds, 7 reptiles or amphibians, as well as two species of plant seeds. These data elucidate the spatio-temporal dynamics of animal activity and movement at the site and have produced numerous peer-reviewed publications, student theses, magazine articles, educational programs and film documentaries. These data are also relevant to long-term population monitoring and conservation plans. Both the successes and the failures of the ARTS system are applicable to broader sensor network applications and are valuable for advancing sensor network research.
C1 [Kays, Roland; Hirsch, Ben] New York State Museum & Sci Serv, Albany, NY USA.
[Kays, Roland; Crofoot, Margaret; Obando, Daniel; Ortega, Alejandro; Hirsch, Ben; Wikelski, Martin] Smithsonian Trop Res Inst, Balboa, Panama.
[Tilak, Sameer; Fountain, Tony] Univ Calif San Diego, Calif Inst Telecommun & Informat Technol Calit2, San Diego, CA 92103 USA.
[Crofoot, Margaret; Wikelski, Martin] Max Plank Inst Ornithol, Radolfzell am Bodensee, Germany.
[Kuemmeth, Franz] E Obs, Gruenwald, Germany.
[Mandel, Jamie] Princeton Univ, Princeton, NJ 08544 USA.
[Swenson, George] Univ Illinois, Urbana, IL 61801 USA.
[Lambert, Thomas] Frostburg State Univ, Frostburg, MD 21532 USA.
RP Kays, R (reprint author), New York State Museum & Sci Serv, Albany, NY USA.
EM rkays@mail.nysed.gov
FU US National Science Foundation [0756920, 0201307]; Smithsonian Tropical
Research Institute; Frank Levinson Family Foundation; National
Geographic Society
FX This work was partially supported by the US National Science Foundation
(Award Number: 0756920, 0201307), Smithsonian Tropical Research
Institute, Frank Levinson Family Foundation and National Geographic
Society.
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0010-4620
J9 COMPUT J
JI Comput. J.
PD NOV
PY 2011
VL 54
IS 12
BP 1931
EP 1948
DI 10.1093/comjnl/bxr072
PG 18
WC Computer Science, Hardware & Architecture; Computer Science, Information
Systems; Computer Science, Software Engineering; Computer Science,
Theory & Methods
SC Computer Science
GA 866MX
UT WOS:000298386300002
ER
PT J
AU Miller, MJ
Lelevier, MJ
Bermingham, E
Klicka, JT
Escalante, P
Winker, K
AF Miller, Matthew J.
Lelevier, Michael J.
Bermingham, Eldredge
Klicka, John T.
Escalante, Patricia
Winker, Kevin
TI PHYLOGEOGRAPHY OF THE RUFOUS-TAILED HUMMINGBIRD (AMAZILIA TZACATL)
SO CONDOR
LA English
DT Article
DE Amazilia tzacatl; Middle America; mitochondrial DNA; phylogeography;
Rufous-tailed Hummingbird; secondary contact
ID DNA POLYMORPHISM; ATLANTIC FOREST; DENDROCOLAPTIDAE; EVOLUTION; BIRD;
DIVERSIFICATION; BIOGEOGRAPHY; SYSTEMATICS; DIVERGENCE; HISTORY
AB The Rufous-tailed Hummingbird (Amazilia tzacatl) is a common resident of the neotropical lowlands of Middle America and northern South America. The Escudo Hummingbird (A. t. handleyi), the most distinctive of the five subspecies of A. tzacatl, is endemic to Isla Escudo in Caribbean western Panama. Mitochondrial DNA (mtDNA) sequence variation from across most of the species' range showed five well-defined but shallow clades (maximum uncorrected distance 2.4%) that only partially agreed with subspecific taxonomy. A widespread Middle American clade ranges from southeastern Mexico to central Caribbean Panama and includes birds collected on the Bocas del Toro archipelago. The Escudo Hummingbird fell within this clade and was slightly differentiated (two unique substitutions; uncorrected distance similar to 0.2-0.5%). Two additional clades occur in the Pacific regions of southern Middle America. A fourth clade is endemic to eastern Panama (eastern Panama and Darien provinces); a fifth is found in northwestern South America and in Darien. Secondary contact between clades occurs at three sites: between clades I and III in northwestern Costa Rica, between clades I and II in western Panama, and between clades IV and V near the Panama-Colombia border. The last case is likely due to recent expansion into the region from two directions. Thus the history of Amazilia tzacatl demonstrates a tendency for the formation of monophyletic mtDNA clades, likely as the result of geographic isolation, but also a propensity for secondary contact of these clades, a phenomenon recovered in many other phylogeographic studies of neotropical birds.
C1 [Miller, Matthew J.; Lelevier, Michael J.; Winker, Kevin] Univ Alaska Museum, Fairbanks, AK 99775 USA.
[Miller, Matthew J.; Lelevier, Michael J.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama.
[Klicka, John T.] Univ Nevada, Barrick Museum Nat Hist, Las Vegas, NV 89154 USA.
[Escalante, Patricia] Univ Nacl Autonoma Mexico, Inst Biol, Mexico City 04511, DF, Mexico.
RP Miller, MJ (reprint author), Univ Alaska Museum, 907 Yukon Dr, Fairbanks, AK 99775 USA.
EM millerma@si.edu
RI Winker, Kevin/M-2042-2014; Escalante, Patricia/B-8704-2014;
OI Winker, Kevin/0000-0002-8985-8104; Escalante,
Patricia/0000-0002-5531-263X; Miller, Matthew/0000-0002-2939-0239
FU University of Alaska Museum; Smithsonian Tropical Research Institute; U.
S. National Science Foundation [INT-9403053]; Consejo Nacional de
Ciencia y Tecnologia of Mexico [E120]; U.S. Department of Agriculture
[SCA 58-6612-2-217]; National Institute of Health's Fogarty
International Center [U01TW006634]; STRI Bird Collection team
FX We thank the collectors and institutions that made tissues available and
the permitting agencies of Ecuador, Panama, Costa Rica, Nicaragua,
Honduras, Belize, and Mexico for approving specimen collection. The
University of Alaska Museum and the Smithsonian Tropical Research
Institute supported our work, along with the U. S. National Science
Foundation (INT-9403053), Consejo Nacional de Ciencia y Tecnologia of
Mexico (E120), the U.S. Department of Agriculture (SCA 58-6612-2-217),
and the National Institute of Health's Fogarty International Center
(U01TW006634). We thank Marco Gandasegui and Ancon Expeditions for
access to the Cana Field Station and Mike and Terri Andrews and the
Tropic Star Lodge for logistical support and access to the Rio Pinas. We
thank M. A. Gonzales, E. Humphries, J. M. Maley, and P. Guitton-Mayerma
for laboratory assistance. We thank O. Sanjur and the STRI Bird
Collection team for logistical support throughout the project.
NR 55
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U1 2
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PU COOPER ORNITHOLOGICAL SOC
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0010-5422
J9 CONDOR
JI Condor
PD NOV
PY 2011
VL 113
IS 4
BP 806
EP 816
DI 10.1525/cond.2011.100226
PG 11
WC Ornithology
SC Zoology
GA 862YJ
UT WOS:000298129700011
ER
PT J
AU Tonra, CM
Marra, PP
Holberton, RL
AF Tonra, Christopher M.
Marra, Peter P.
Holberton, Rebecca L.
TI Migration phenology and winter habitat quality are related to
circulating androgen in a long-distance migratory bird
SO JOURNAL OF AVIAN BIOLOGY
LA English
DT Article
ID WHITE-CROWNED SPARROWS; NON-BREEDING SEASON; EXPERIMENTALLY ELEVATED
TESTOSTERONE; STONECHATS SAXICOLA-TORQUATA; RUFOUS-COLLARED SPARROWS;
AVIAN LIFE HISTORIES; DARK-EYED JUNCOS; ZONOTRICHIA-CAPENSIS;
SETOPHAGA-RUTICILLA; BODY CONDITION
AB In migratory birds, the timing of departure from wintering grounds is often dependant on the quality of habitat on an individual's territory and may influence individual fitness, resulting in an interaction of life history stages across large geographical distances. American redstart Setophaga ruticilla males who overwinter in high quality habitats arrive early to breed and subsequently produce more offspring than late arrivers. Since many migratory species overlap vernal migration with the physiological transition to breeding, we examined if breeding preparation plays a role in this seasonal interaction. We tested the hypothesis that early arriving male redstarts from high quality winter habitats are in superior breeding condition by simultaneously measuring winter habitat quality (stable-carbon isotopes) and breeding preparation (circulating androgen, cloacal protuberance (CP) diameter) upon arrival at breeding grounds. Compared with late arrivers, early arriving males were from higher quality winter habitats and had higher androgen, but smaller CPs. Males arriving with higher androgen were in more advanced physiological migratory condition, as measured by haematocrit. Early arrivers were more likely to successfully breed, but there was no significant relationship between androgen upon arrival and breeding success. One possible explanation for these relationships is that androgen measured during arrival is most relevant in a migratory context, such that birds with high androgen may benefit from effects on migratory condition, positively influencing fitness through earlier arrival.
C1 [Tonra, Christopher M.; Holberton, Rebecca L.] Univ Maine, Lab Avian Biol, Sch Biol & Ecol, Orono, ME 04469 USA.
[Tonra, Christopher M.; Marra, Peter P.; Holberton, Rebecca L.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
RP Tonra, CM (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
EM tonrac@si.edu
RI Tonra, Christopher/B-1620-2013
FU National Science Foundation [0649679, 0615701]; American Ornithologist
Union; American Museum of Natural History; Cooper Ornithological Society
FX This research was funded by grants awarded to PPM (0649679) and RLH
(0615701) from the National Science Foundation and to CMT from the
American Ornithologist Union Student Research Award, the American Museum
of Natural History Frank M. Chapman Award, and the Cooper Ornithological
Society Joseph Grinnell Student Research Award. We are grateful to Cord
Dorcey, Doug Perez, Stephanie Sult, and especially Mark Thomas for
assistance in the field and Nora Diggs, Greg Henkes, and Kayla Porcelli
for assistance in the laboratory. For logistical support at our field
site and frequent discussions of the phenomena addressed in this study
we thank Dick Holmes, Sara Kaiser, Nick Rodenhouse, Scott Sillett, and
the Hubbard Brook Research Foundation. We thank Bill Glanz, Matt
Reudink, Colin Studds, members of the UMaine Lab of Avian Biology
reading group for comments on an earlier draft of this manuscript. Our
research was approved by the Univ. of Maine Inst. Animal Care and Use
Committee (protocol A2006-07-04) and was in compliance with United
States law.
NR 69
TC 22
Z9 23
U1 1
U2 43
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0908-8857
J9 J AVIAN BIOL
JI J. Avian Biol.
PD NOV
PY 2011
VL 42
IS 5
BP 397
EP 404
DI 10.1111/j.1600-048X.2011.05333.x
PG 8
WC Ornithology
SC Zoology
GA 854PE
UT WOS:000297505900003
ER
PT J
AU Braje, TJ
Rick, TC
Erlandson, JM
Anderson, M
DeLong, RL
AF Braje, Todd J.
Rick, Torben C.
Erlandson, Jon M.
Anderson, Megan
DeLong, Robert L.
TI Conflicts in natural and cultural resource management: Archaeological
site disturbances by seals and sea lions on California's Northern
Channel Islands
SO JOURNAL OF FIELD ARCHAEOLOGY
LA English
DT Article
DE seals; sea lions; coastal erosion; archaeological conservation; Channel
Islands
ID SAN-MIGUEL ISLAND; AQUATIC ADAPTATIONS; SOUTH-AFRICA; EROSION; COAST;
SETTLEMENT; PACIFIC; AMERICA
AB California's Channel Islands currently have around 150,000 breeding seals and sea lions (pinnipeds). Driven to near extinction by 20th-century exploitation, many pinniped populations have recovered dramatically under federal and state management and continue to expand in number and distribution. Some of these pinniped populations are damaging or destroying coastal archaeological sites as they establish new breeding and haul-out areas-places occupied between periods of foraging activity-on upland landforms. We use archaeological excavations from a prehistoric village on San Miguel Island to illustrate the adverse effects pinnipeds can have on archaeological sites. Estimates based on excavations at Otter Point suggest that in one year nearly 10,000 kg of shellfish remains, 840,000 animal bones, and 1700 formal artifacts were lost to erosion caused by the activities of seals and sea lions. Our study documents potential conflicts between natural and cultural resource management suggesting the need for collaborative efforts between archaeologists and biologists to balance the conservation of both resources.
C1 [Braje, Todd J.] San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA.
[Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA.
[Anderson, Megan] Humboldt State Univ, Arcata, CA 95521 USA.
[DeLong, Robert L.] NOAA, Natl Marine Mammal Lab, Alaska Fisheries Sci Ctr, Calif Current Ecosyst Program, Seattle, WA USA.
RP Braje, TJ (reprint author), San Diego State Univ, Dept Anthropol, 5500 Campanile Dr, San Diego, CA 92182 USA.
EM tbraje@mail.sdsu.edu
OI Erlandson, Jon/0000-0002-4705-4319
NR 55
TC 2
Z9 2
U1 1
U2 12
PU MANEY PUBLISHING
PI LEEDS
PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND
SN 0093-4690
J9 J FIELD ARCHAEOL
JI J. Field Archaeol.
PD NOV
PY 2011
VL 36
IS 4
BP 312
EP 321
DI 10.1179/009346911X13200731373863
PG 10
WC Archaeology
SC Archaeology
GA 863DX
UT WOS:000298144100005
ER
PT J
AU Chambouvet, A
Laabir, M
Sengco, M
Vaquer, A
Guillou, L
AF Chambouvet, Aurelie
Laabir, Mohamed
Sengco, Mario
Vaquer, Andre
Guillou, Laure
TI Genetic diversity of Amoebophryidae (Syndiniales) during Alexandrium
catenella/tamarense (Dinophyceae) blooms in the Thau lagoon
(Mediterranean Sea, France)
SO RESEARCH IN MICROBIOLOGY
LA English
DT Article
DE Dinoflagellate; Parasite; Invasive species
ID TAMARENSE COMPLEX DINOPHYCEAE; HOST-SPECIFICITY; CHESAPEAKE BAY;
CATENELLA; POPULATIONS; PARASITISM; SEQUENCES; PACIFIC
AB During toxic spring and fall blooms produced by the dinoflagellate Alexandrium in the Thau lagoon (Mediterranean Sea), we monitored the presence of Amoebophryidae (Syndiniales), a group of parasites virulent toward a wide range of dinoflagellate hosts. A PCR-biased approach unveiled the presence of at least 10 different parasitic groups during Alexandrium proliferation. However, fluorescent in situ hybridization failed to reveal parasitic infection inside Alexandrium cells in field populations. In contrast, several co-occurring, less abundant thecate dinofiagellate species were infected by Amoebophryidae, showing up to 10% of infected cells. We concluded that Alexandrium populations were not infected by these local parasites, at least during our survey. In order to check this resistance capacity on a more global scale, we cross-infected several Alexandrium strains isolated from the Thau lagoon with one strain of the parasite Amoebophrya sp. originating from Salt Pond, MA, USA. All of these hosts were strongly infected by the North American parasite, leading to the conclusion that blooming Alexandrium in the Thau lagoon were not particularly resistant to this kind of parasite. These results provide additional evidence that dinofiagellates may become invasive when they successfully escaped their natural enemies in time and/or space (the "enemy release" hypothesis). (C) 2011 Institut Pasteur. Published by Elsevier Masson SAS. All rights reserved.
C1 [Chambouvet, Aurelie; Guillou, Laure] Univ Paris 06, CNRS, UMR 7144, Biol Stn, F-29680 Roscoff, France.
[Laabir, Mohamed; Vaquer, Andre] CNRS, UM2 Ecosyst Lagunaires, UMR 5119, F-34095 Montpellier 05, France.
[Sengco, Mario] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Guillou, L (reprint author), Univ Paris 06, CNRS, UMR 7144, Biol Stn, Pl G Teissier, F-29680 Roscoff, France.
EM a.chambouvet@gmail.com; Mohamed.Laabir@univ-montp2.fr;
mario.sengco@gmail.com; Andre.Vaquer@univ-montp2.fr;
lguillou@sb-roscoff.fr
FU French programs EC2CO; ANR AQUAPARADOX
FX We are grateful to Annie Pastoureaud (Ifremer, Sete) for her help during
sampling and for use of her cruise facilities. We also thank Anne-Laure
Sauvadet for her help in phylogenetic analysis and we are indebted to
Morgan Perennou from Ouest-Genopole for sequencing operations. This work
was supported by the French programs EC2CO (2006-2008) and the ANR
AQUAPARADOX.
NR 32
TC 13
Z9 14
U1 1
U2 22
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0923-2508
J9 RES MICROBIOL
JI Res. Microbiol.
PD NOV
PY 2011
VL 162
IS 9
SI SI
BP 959
EP 968
DI 10.1016/j.resmic.2011.03.002
PG 10
WC Microbiology
SC Microbiology
GA 862VB
UT WOS:000298121100017
PM 21392576
ER
PT J
AU Neufeld, MJ
AF Neufeld, Michael J.
TI Falling to Earth: An Apollo 15 Astronaut's Journey
SO SPACE POLICY
LA English
DT Book Review
C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA.
RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA.
EM NeufeldM@si.edu
NR 1
TC 0
Z9 0
U1 1
U2 1
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0265-9646
J9 SPACE POLICY
JI Space Policy
PD NOV
PY 2011
VL 27
IS 4
BP 253
EP 254
DI 10.1016/j.spacepol.2011.09.003
PG 2
WC International Relations; Social Sciences, Interdisciplinary
SC International Relations; Social Sciences - Other Topics
GA 867PC
UT WOS:000298465300012
ER
PT J
AU Dow, TL
Holaskova, I
Brown, JL
AF Dow, T. L.
Holaskova, I.
Brown, J. L.
TI Results of the third reproductive assessment survey of north American
Asian (Elephas maximus) and African (Loxodonta africana) female
elephants
SO ZOO BIOLOGY
LA English
DT Article
DE ovarian cyclicity; hormones; reproduction; acyclicity; ultrasound;
progestagens
ID OVARIAN ACTIVITY; MANAGEMENT; BEHAVIOR; POPULATION; HORMONE; TOOL
AB A written survey assessed reproductive status of female Asian and African elephants in AZA/SSP facilities in 2008, and data were compared to surveys conducted in 2002 and 2005. Results showed that ovarian acyclicity rates across the surveys remained unchanged for Asian (13.3, 10.9 and 11.1%) and African (22.1, 31.2 and 30.5%) elephants, respectively (P>0.05), but were higher overall for African compared to Asian elephants (P<0.05). In 2008, the percentages of Asian and African elephants with irregular cycles (14.3 and 15.8%) and irregular + no cycles (25.4 and 46.4%) was similar to 2005 (7.6 and 11.8%; 18.5 and 43.0%), but were increased compared to 2002 (2.6 and 5.2%; 16.0 and 27.3%), respectively (P<0.05). For both species, ovarian acyclicity increased with age (P<0.05). Reproductive tract pathologies did not account for the majority of acyclicity, although rates were higher in noncycling females (P<0.05). Bull presence was associated with increased cyclicity rates (P<0.05) for Asian (92.5 vs. 58.3%) and African (64.9 vs. 57.8%) elephants compared to females at facilities with no male, respectively. Cyclicity rates were higher for Asian (86.8 vs. 65.2%) and African (67.9 vs. 56.7%) elephants managed in free compared to protected contact programs (P<0.05), respectively. Geographical facility location had no effect on cyclicity (P>0.05). In summary, incidence of ovarian cycle problems continues to predominantly affect African elephants. Although percentages of acyclicity did not increase between 2005 and 2008, 42.2% Asian and 30.2% African females were no longer being hormonally monitored; thus, reproductive cycle abnormalities could be worse than current data suggest. Zoo Biol 30:699711, 2011. (c) 2011 Wiley Periodicals, Inc.
C1 [Dow, T. L.; Brown, J. L.] Smithsonian Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA.
[Dow, T. L.; Holaskova, I.] W Virginia Univ, Dept Anim & Nutr Sci, Morgantown, WV 26506 USA.
RP Brown, JL (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA.
EM brownjan@si.edu
NR 34
TC 14
Z9 14
U1 3
U2 16
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0733-3188
J9 ZOO BIOL
JI Zoo Biol.
PD NOV-DEC
PY 2011
VL 30
IS 6
BP 699
EP 711
DI 10.1002/zoo.20377
PG 13
WC Veterinary Sciences; Zoology
SC Veterinary Sciences; Zoology
GA 864PZ
UT WOS:000298253500010
PM 21319213
ER
PT J
AU Forget, PM
Jordano, P
Lambert, JE
Bohning-Gaese, K
Traveset, A
Wright, SJ
AF Forget, Pierre-Michel
Jordano, Pedro
Lambert, Joanna E.
Boehning-Gaese, Katrin
Traveset, Anna
Joseph Wright, S.
TI Frugivores and seed dispersal (1985-2010); the 'seeds' dispersed,
established and matured
SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY
LA English
DT Editorial Material
ID TROPICAL FORESTS; ECOSYSTEM SERVICES; CONSEQUENCES; REGENERATION; BIRDS;
CONSERVATION; RECRUITMENT; MECHANISMS; ANIMALS; AFRICA
C1 [Forget, Pierre-Michel] Museum Natl Hist Nat, UMR 7179, F-91800 Brunoy, France.
[Jordano, Pedro] Estn Biol Donana EBD CSIC, Integrat Ecol Grp, E-41092 Seville, Spain.
[Lambert, Joanna E.] Univ Texas San Antonio, Dept Ecol Anthropol, San Antonio, TX 78249 USA.
[Boehning-Gaese, Katrin] Goethe Univ, Dept Biol Sci, D-60323 Frankfurt, Germany.
[Boehning-Gaese, Katrin] Biodivers & Climate Res Ctr BiK F, D-60325 Frankfurt, Germany.
[Traveset, Anna] Inst Mediterrani Estudis Avancats CSIC UIB, Esporles Mallorca 07190, Illes Balears, Spain.
[Joseph Wright, S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Forget, PM (reprint author), Museum Natl Hist Nat, UMR 7179, 1 Ave Petit Chateau, F-91800 Brunoy, France.
EM pmf@mnhn.fr
RI Biodiversity & Climate Res Ctr, BiK-F/C-4266-2012; Forget,
Pierre-Michel/B-4355-2009; Jordano, Pedro/A-5162-2008; Jordano,
Pedro/B-6678-2014; Wright, Stuart/M-3311-2013; CSIC, EBD
Donana/C-4157-2011
OI Forget, Pierre-Michel/0000-0002-9252-974X; Jordano,
Pedro/0000-0003-2142-9116; Jordano, Pedro/0000-0003-2142-9116; Wright,
Stuart/0000-0003-4260-5676; CSIC, EBD Donana/0000-0003-4318-6602
NR 74
TC 12
Z9 12
U1 3
U2 34
PU GAUTHIER-VILLARS/EDITIONS ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75015 PARIS, FRANCE
SN 1146-609X
EI 1873-6238
J9 ACTA OECOL
JI Acta Oecol.-Int. J. Ecol.
PD NOV-DEC
PY 2011
VL 37
IS 6
SI SI
BP 517
EP 520
DI 10.1016/j.actao.2011.09.008
PG 4
WC Ecology
SC Environmental Sciences & Ecology
GA 860NU
UT WOS:000297955800001
ER
PT J
AU Fleming, TH
Kress, WJ
AF Fleming, Theodore H.
Kress, W. John
TI A brief history of fruits and frugivores
SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY
LA English
DT Article
DE Coevolution; Fruits; Frugivores; Phylogenies
ID FLOWERING PLANTS; FLESHY FRUITS; SEED SIZE; DISPERSAL; DIVERSITY;
EVOLUTION; ANGIOSPERMS; PHYLOGENY; SEQUENCES; BATS
AB In this paper we briefly review the evolutionary history of the mutualistic interaction between angiosperms that produce fleshy fruits and their major consumers: frugivorous birds and mammals. Fleshy fruits eaten by these vertebrates are widely distributed throughout angiosperm phylogeny. Similarly, a frugivorous diet has evolved independently many times in birds and mammals. Bird dispersal is more common than mammal-dispersal in all lineages of angiosperms, and we suggest that the evolution of bird fruits may have facilitated the evolution of frugivory in primates. The diets of fruit-eating bats overlap less with those of other kinds of frugivorous vertebrates. With a few exceptions, most families producing vertebrate-dispersed fruit appeared substantially earlier in earth history than families of their vertebrate consumers. It is likely that major radiations of these plants and animals have occurred in the past 30 Ma, in part driven by geological changes and also by the foraging behavior of frugivores in topographically complex landscapes. Overall, this mutualistic interaction has had many evolutionary and ecological consequences for tropical plants and animals for most of the Cenozoic Era. Loss of frugivores and their dispersal services will have a strong negative impact on the ecological and evolutionary dynamics of tropical and subtropical communities. (C) 2011 Elsevier Masson SAS. All rights reserved.
C1 [Fleming, Theodore H.] Univ Miami, Tucson, AZ USA.
[Fleming, Theodore H.] Univ Arizona, Tucson, AZ USA.
[Kress, W. John] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA.
RP Fleming, TH (reprint author), 6211 N Camino Corozal, Tucson, AZ 85704 USA.
EM tedfleming@dakotacom.net
NR 53
TC 42
Z9 45
U1 11
U2 103
PU GAUTHIER-VILLARS/EDITIONS ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75015 PARIS, FRANCE
SN 1146-609X
J9 ACTA OECOL
JI Acta Oecol.-Int. J. Ecol.
PD NOV-DEC
PY 2011
VL 37
IS 6
SI SI
BP 521
EP 530
DI 10.1016/j.actao.2011.01.016
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 860NU
UT WOS:000297955800002
ER
PT J
AU Kays, R
Jansen, PA
Knecht, EMH
Vohwinkel, R
Wikelski, M
AF Kays, Roland
Jansen, Patrick A.
Knecht, Elise M. H.
Vohwinkel, Reinhard
Wikelski, Martin
TI The effect of feeding time on dispersal of Virola seeds by toucans
determined from GPS tracking and accelerometers
SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY
LA English
DT Article
DE Seed dispersal kernel; Regurgitation time; GPS tracking; Accelerometer;
Tropical forests
ID SPATIAL-PATTERNS; ANIMAL MOVEMENT; FOREST; ECOLOGY; MODELS; PANAMA;
BIRDS; WILD; FRUGIVORE; BEHAVIOR
AB Seed dispersal is critical to understanding forest dynamics but is hard to study because tracking seeds is difficult. Even for the best-studied dispersal system of the Neotropics, Virola nobilis, the dispersal kernel remains unknown. We combined high-resolution GPS/3D-acceleration bird tracking, seed-retention experiments, and field observations to quantify dispersal of V. nobilis by their principal dispersers, Ramphastos toucans. We inferred feeding events from movement data, and then estimated spatio-temporally explicit seed-dispersal kernels. Wild toucans moved an average of 1.8 km d(-1) with two distinct activity peaks. Seed retention time in captive toucans averaged 25.5 min (range 4-98 min). Estimated seed dispersal distance averaged 144 +/- 147 m, with a 56% likelihood of dispersal >100 m, two times further than the behaviour-naive estimate from the same data. Dispersal was furthest for seeds ingested in the morning, and increased with seed retention time, but only up to 60 min after feeding. Our study supports the long-standing hypothesis that toucans are excellent dispersers of Virola seeds. To maximize seed dispersal distances trees should ripen fruit in the morning when birds move the most, and produce fruits with gut-processing times around 60 min. Our study demonstrates how new tracking technology can yield nuanced seed dispersal kernels for animals that cannot be directly observed. (C) 2011 Elsevier Masson SAS. All rights reserved.
C1 [Kays, Roland] New York State Museum & Sci Serv, Albany, NY USA.
[Kays, Roland; Jansen, Patrick A.; Wikelski, Martin] Smithsonian Trop Res Inst, Balboa, Panama.
[Jansen, Patrick A.; Knecht, Elise M. H.] Wageningen Univ, Ctr Ecosyst Studies, Wageningen, Netherlands.
[Jansen, Patrick A.] Univ Groningen, Ctr Ecol & Evolutionary Studies, Haren, Netherlands.
[Vohwinkel, Reinhard] Avifaunist Untersuchungen, D-42553 Velbert, Nordrhein Westf, Germany.
[Wikelski, Martin] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell Am Bodensee, Germany.
[Wikelski, Martin] Univ Konstanz, Chair Ornithol, D-78457 Constance, Germany.
RP Kays, R (reprint author), New York State Museum & Sci Serv, 3140 CEC, Albany, NY USA.
EM rkays@mail.nysed.gov
RI Jansen, Patrick/G-2545-2015
OI Jansen, Patrick/0000-0002-4660-0314
FU Netherlands Organisation for Scientific Research [W84-584, 863-07-008];
National Science Foundation [NSF-DEB 0717071]; Max Planck Institute for
Ornithology
FX We thank Renee Seidler, Lars Sluiter, Niels Rattenborg, Christian
Ziegler, and Bryson Voirin for their assistance in the field, Halit
Khoshen from Summit Botanical Gardens and Harald Schmidt and colleagues
from Rotterdam Zoo for help with captive toucans, Wolfgang Heidrich,
Franz Kuemmeth, Bart Kranstauber Daniel Obando and Alexandro Ortega for
technical support, and the Smithsonian Tropical Research Institute and
Autoridad Nacional del Ambiente de Panama for administrative support.
Thanks to Edgar Perez and the Gamboa resort hotel for allowing us to
work on their properties. This study was supported by funding from the
Netherlands Organisation for Scientific Research (grants W84-584 and
863-07-008 to P.A.J.), the National Science Foundation (NSF-DEB 0717071
to R.K.), and the Max Planck Institute for Ornithology.
NR 47
TC 21
Z9 21
U1 4
U2 55
PU GAUTHIER-VILLARS/EDITIONS ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75015 PARIS, FRANCE
SN 1146-609X
J9 ACTA OECOL
JI Acta Oecol.-Int. J. Ecol.
PD NOV-DEC
PY 2011
VL 37
IS 6
SI SI
BP 625
EP 631
DI 10.1016/j.actao.2011.06.007
PG 7
WC Ecology
SC Environmental Sciences & Ecology
GA 860NU
UT WOS:000297955800013
ER
PT J
AU Keil, K
Mccoy, TJ
Wilson, L
Barrat, JA
Rumble, D
Meier, MMM
Wieler, R
Huss, GR
AF Keil, Klaus
McCoy, Timothy J.
Wilson, Lionel
Barrat, Jean-Alix
Rumble, Doug
Meier, Matthias M. M.
Wieler, Rainer
Huss, Gary R.
TI A composite Fe, Ni-FeS and enstatite-forsterite-diopside-glass
vitrophyre clast in the Larkman Nunatak 04316 aubrite: Origin by
pyroclastic volcanism
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID OXYGEN-ISOTOPE RATIOS; RARE-EARTH-ELEMENT; PARENT BODY; EXPLOSIVE
ERUPTIONS; COSMOGENIC NUCLIDES; MELT MIGRATION; CORE FORMATION;
SOLAR-SYSTEM; CHONDRITES; METEORITES
AB We studied the mineralogy, petrology, and bulk, trace element, oxygen, and noble gas isotopic compositions of a composite clast approximately 20 mm in diameter discovered in the Larkman Nunatak (LAR) 04316 aubrite regolith breccia. The clast consists of two lithologies: One is a quench-textured intergrowth of troilite with spottily zoned metallic Fe, Ni which forms a dendritic or cellular structure. The approximately 30 mu m spacings between the Fe, Ni arms yield an estimated cooling rate of this lithology of approximately 25-30 degrees C s(-1). The other is a quench-textured enstatite-forsterite-diopside-glass vitrophyre lithology. The composition of the clast suggests that it formed at an exceptionally high degree of partial melting, perhaps approaching complete melting, and that the melts from which the composite clast crystallized were quenched from a temperature of approximately 1380-1400 degrees C at a rate of approximately 25-30 degrees C s(-1). The association of the two lithologies in a composite clast allows, for the first time, an estimation of the cooling rate of a silicate vitrophyre in an aubrite of approximately 25-30 degrees C s(-1). While we cannot completely rule out an impact origin of the clast, we present what we consider is very strong evidence that this composite clast is one of the elusive pyroclasts produced during pyroclastic volcanism on the aubrite parent body (Wilson and Keil 1991). We further suggest that this clast was not ejected into space but retained on the aubrite parent body by virtue of the relatively large size of the clast of approximately 20 mm. Our modeling, taking into account the size of the clast, suggests that the aubrite parent body must have been between approximately 40 and 100 km in diameter, and that the melt from which the clast crystallized must have contained an estimated maximum range of allowed volatile mass fractions between approximately 500 and approximately 4500 ppm.
C1 [Keil, Klaus; Wilson, Lionel; Huss, Gary R.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
[Wilson, Lionel] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England.
[Barrat, Jean-Alix] UBOIUEM, CNRS UMR Domaines Ocean 6538, F-29280 Plouzane, France.
[Rumble, Doug] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA.
[Meier, Matthias M. M.; Wieler, Rainer] Swiss Fed Inst Technol, Inst Geochem & Petr, CH-8092 Zurich, Switzerland.
RP Keil, K (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
EM keil@hawaii.edu
RI Jean-Alix, BARRAT/F-8035-2012; Wieler, Rainer/A-1355-2010; Barrat,
Jean-Alix/C-8416-2017;
OI Wieler, Rainer/0000-0001-5666-7494; Barrat,
Jean-Alix/0000-0003-3158-3109; Meier, Matthias/0000-0002-7179-4173
FU NASA [NNX08AE08G, NNG06GF56G, NNX08AG58G, NNX07AI48G]; Swiss Science
Foundation
FX We thank Kevin Righter and the staff of the Meteorite Processing
Laboratory at NASA's L. B. Johnson Space Center for providing Fig. 1 and
the carefully selected and well-documented samples of the various
lithologies of LAR 04316. At the University of Hawai'i, we thank Eric
Hellebrand for his expert assistance with the electron probe
microanalyses, Deon Van Niekerk for the modal analysis of the Fe,Ni-FeS
clast, Sasha Krot for his assistance with the X-ray maps, and Ed Scott
for insightful discussions of the origin of the zoned metal. We thank
Ian Franchi, James Day, and an anonymous reviewer for constructive
reviews that helped improve the manuscript considerably. We are grateful
to Kees Welten of the University of California, Berkeley for providing
his unpublished CRE age of LAR 04316. This work was supported in part by
NASA Cosmochemistry grants NNX08AE08G (K. Keil, PI), NNG06GF56G (T.
McCoy, PI), NNX08AG58G (G. R. Huss, PI), NNX07AI48G (D. Rumble, PI), and
by the Swiss Science Foundation (R. Wieler, PI). This is a Hawai'i
Institute of Geophysics and Planetology publication No. 8211 and School
of Ocean and Earth Science and Technology Publication no. 8300.
NR 73
TC 7
Z9 7
U1 0
U2 8
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD NOV
PY 2011
VL 46
IS 11
BP 1719
EP 1741
DI 10.1111/j.1945-5100.2011.01261.x
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 853GQ
UT WOS:000297414600009
ER
PT J
AU Wall, AJ
Mathur, R
Post, JE
Heaney, PJ
AF Wall, Andrew J.
Mathur, Ryan
Post, Jeffrey E.
Heaney, Peter J.
TI Cu isotope fractionation during bornite dissolution: An in situ X-ray
diffraction analysis
SO ORE GEOLOGY REVIEWS
LA English
DT Review
DE Copper isotope fractionation; Bornite; Synchrotron XRD
ID SOURCE MASS-SPECTROMETRY; UNITED-STATES; SE AUSTRALIA; AU DEPOSIT;
COPPER; RATIOS; MINERALIZATION; CHALCOCITE; PORPHYRY; ACID
AB Low-temperature ore deposits exhibit a large variation in delta(65)Cu (similar to 12 parts per thousand), and this range has been attributed, in part, to isotope fractionation during weathering reactions of primary minerals such as chalcocite and chalcopyrite. Here, we examine the fractionation of Cu isotopes during dissolution of another important Cu ore mineral, bornite, using a novel approach that combines time-resolved X-ray diffraction (XRD) and isotope analysis of reaction products. During the initial stages of bornite oxidative dissolution by ferric sulfate (<5 mol% of total Cu leached), dissolved Cu was enriched in isotopically heavy Cu ((65)Cu) relative to the solid, with an average apparent isotope fractionation (Delta(aq-min) = delta(65)Cu(aq)-delta(65)Cu(min)(0)) of 2.20 +/- 0.25 parts per thousand. When >20 mol% Cu was leached from the solid, the difference between the Cu isotope composition of the aqueous and mineral phases approached zero, with Delta(0)(aq-min) values ranging from -0.21 +/- 0.61 parts per thousand to 0.92 +/- 0.25 parts per thousand. XRD analysis allowed us to correlate changes in the atomic structure of bornite with the apparent isotope fractionation as the dissolution reaction progressed. These data revealed that the greatest degree of apparent fractionation is accompanied by a steep contraction in the unit-cell volume, which we identified as a transition from stoichiometric to non-stoichiometric bornite. We propose that the initially high A(aq-min) values result from isotopically heavy Cu ((65)Cu) concentrating within Cu(2+) during dissolution. The decrease in the apparent isotope fractionation as the reaction progresses occurs from the distillation of isotopically heavy Cu ((65)Cu) during dissolution or kinetic isotope effects associated with the depletion of Cu from the surfaces of bornite particles. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Wall, Andrew J.; Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Mathur, Ryan] Juniata Coll, Dept Geol, Huntingdon, PA 16652 USA.
[Post, Jeffrey E.] Smithsonian NMNH, Dept Mineral Sci, Washington, DC 20013 USA.
RP Wall, AJ (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
EM awall@psu.edu
FU NSF [EAR07-45374, NSF CHE04-31328]; Center for Environmental Kinetics
Analysis (CEKA); DOE; Mineralogical Society of America; Geological
Society of America; U.S. Department of Energy, Division of Materials
Sciences and Division of Chemical Sciences [DE-AC02-98CH10886]; U.S.
Department of Energy, Office of Science, Office of Basic Energy Sciences
[DE-AC02-06CH11357]
FX Funding for this research was provided by NSF grant EAR07-45374, the
Center for Environmental Kinetics Analysis (CEKA), an NSF- and
DOE-sponsored Environmental Molecular Science Institute (NSF
CHE04-31328), the Edward H. Kraus Crystallographic Research Fund of the
Mineralogical Society of America, and by a Geological Society of America
Graduate Student Research Grant. This research was carried out at two
synchrotron sources: 1) the National Synchrotron Light Source,
Brookhaven National Laboratory, which is supported by the U.S.
Department of Energy, Division of Materials Sciences and Division of
Chemical Sciences, under Contract No. DE-AC02-98CH10886: and 2) the
Advanced Photon Source at Argonne National Laboratory, which is
supported by the U.S. Department of Energy, Office of Science, Office of
Basic Energy Sciences, under Contract No. DE-AC02-06CH11357. We thank
the three anonymous reviewers whose comments improved
NR 49
TC 18
Z9 21
U1 3
U2 30
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-1368
J9 ORE GEOL REV
JI Ore Geol. Rev.
PD NOV
PY 2011
VL 42
IS 1
SI SI
BP 62
EP 70
DI 10.1016/j.oregeorev.2011.01.001
PG 9
WC Geology; Mineralogy; Mining & Mineral Processing
SC Geology; Mineralogy; Mining & Mineral Processing
GA 858FS
UT WOS:000297781900006
ER
PT J
AU Quesada, R
Triana, E
Vargas, G
Douglass, JK