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
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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
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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
Seid, MA
Niven, JE
Eberhard, WG
Wcislo, WT
AF Quesada, Rosannette
Triana, Emilia
Vargas, Gloria
Douglass, John K.
Seid, Marc A.
Niven, Jeremy E.
Eberhard, William G.
Wcislo, William T.
TI The allometry of CNS size and consequences of miniaturization in
orb-weaving and cleptoparasitic spiders
SO ARTHROPOD STRUCTURE & DEVELOPMENT
LA English
DT Article
DE Miniaturization; Allometry; Orb-web spiders; cleptoparasitic spiders;
Araneae
ID CENTRAL NERVOUS-SYSTEM; PLETHODONTID SALAMANDERS; KLEPTOPARASITIC
SPIDER; BRAIN SIZE; INSECTS; ARANEAE; BODY; THERIDIIDAE; INFORMATION;
COLEOPTERA
AB Allometric studies of the gross neuroanatomy of adults from nine species of spiders from six web-weaving families (Orbicularia), and nymphs from six of these species, show that very small spiders resemble other small animals in having disproportionately larger central nervous systems (CNSs) relative to body mass when compared with large-bodied forms. Small spiderlings and minute adult spiders have similar relative CNS volumes. The relatively large CNS of a very small spider occupies up to 78% of the cephalothorax volume. The CNSs of very small spiders extend into their coxae, occupying as much as 26% of the profile area of the coxae of an Anapisona simoni spiderling (body mass < 0.005 mg). Such modifications occur both in species with minute adults, and in tiny spiderlings of species with large-bodied adults. In at least one such species, Leucauge mariana, the CNS of the spiderling extends into a prominent ventral bulge of the sternum. Tiny spiders also have reduced neuronal cell body diameters. The adults of nearly all orbicularian spiders weave prey capture webs, as do the spiderlings, beginning with second instar nymphs. Comparable allometric relations occur in adults of both orb-weaving and cleptoparasitic species, indicating that this behavioral difference is not reflected in differences in gross CNS allometry. Published by Elsevier Ltd.
C1 [Quesada, Rosannette; Triana, Emilia; Vargas, Gloria; Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica.
[Quesada, Rosannette; Triana, Emilia; Vargas, Gloria; Douglass, John K.; Seid, Marc A.; Niven, Jeremy E.; Eberhard, William G.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Eberhard, WG (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ Rodrigo Facio, San Pedro, Costa Rica.
EM william.eberhard@gmail.com; WcisloW@si.edu
RI Quesada, Rosannette/E-7947-2015
FU F. H. Levinson Fund; Smithsonian Institution; Smithsonian Tropical
Research Institute's (STRI); Royal Society
FX We thank S. Tierney, A. Smith, N. Strausfeld, and two anonymous
reviewers for help with discussions and comments on the manuscript.
Financial support was provided by the F. H. Levinson Fund, the
Smithsonian Institution's Scholarly Studies Program to WTW (PI), the
Smithsonian Tropical Research Institute's (STRI) "Adelante" Internship
program (to RQ), the Royal Society (to JEN), and general research funds
from STRI to WTW and WGE. We are grateful to the STRI staff for
logistical support, and to the Autoridad Nacional del Medio Ambiente for
collecting and research permits, SE/A-51-10.
NR 47
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U2 17
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1467-8039
J9 ARTHROPOD STRUCT DEV
JI Arthropod Struct. Dev.
PD NOV
PY 2011
VL 40
IS 6
BP 521
EP 529
DI 10.1016/j.asd.2011.07.002
PG 9
WC Entomology
SC Entomology
GA 853KW
UT WOS:000297426200004
PM 22036838
ER
PT J
AU Miller, AW
Minton, MS
Ruiz, GM
AF Miller, A. Whitman
Minton, Mark S.
Ruiz, Gregory M.
TI Geographic Limitations and Regional Differences in Ships' Ballast Water
Management to Reduce Marine Invasions in the Contiguous United States
SO BIOSCIENCE
LA English
DT Article
DE ballast water; shipping; nonnative species; marine invasions; propagule
supply
ID ECOSYSTEMS; PATTERNS; ECOLOGY
AB Marine species are in constant motion in the ballast water and on the hulls of the ships that ply the world's oceans; ships serve as a major vector for biological invasions. Despite federal and state regulations that require ballast water exchange (BWE), particular trade routes impose geographic and temporal constraints on compliance, limiting whether a ship can conduct BWE at the required distance (>= 200 nautical miles) from shore to minimize transfers of coastal organisms. Ships moving across the Americas are largely unable to conduct open-ocean BWE, but instead often conduct exchanges inside coastal waters. Overall, strong differences exist in volumes, geographic sources, and the use of BWE for ballast water discharge among the three major coasts of the contiguous United States. Such patterns suggest important geographic differences in invasion opportunities and also argue for more effective alternative ballast water treatments that can be applied more evenly.
C1 [Miller, A. Whitman; Minton, Mark S.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Miller, AW (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM millerw@si.edu
OI Ruiz, Gregory/0000-0003-2499-441X; Minton, Mark/0000-0002-9439-4930;
Miller, Whitman/0000-0003-0484-182X
FU US Coast Guard
FX Support for this work was provided by the US Coast Guard. We thank all
members of the National Ballast Information Clearinghouse for their
assistance in receiving, processing, and organizing the ballast water
data. We thank Richard Everett and three anonymous reviewers for their
comments and suggestions on the manuscript.
NR 27
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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 NOV
PY 2011
VL 61
IS 11
BP 880
EP 887
DI 10.1525/bio.2011.61.11.7
PG 8
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 853AM
UT WOS:000297398600007
ER
PT J
AU Hong, T
AF Hong, Terry
TI Drifting House
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA.
RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA.
NR 1
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PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD NOV 1
PY 2011
VL 136
IS 18
BP 75
EP 75
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 853PT
UT WOS:000297438900071
ER
PT J
AU Blomme, J
Sarro, LM
O'Donovan, FT
Debosscher, J
Brown, T
Lopez, M
Dubath, P
Rimoldini, L
Charbonneau, D
Dunham, E
Mandushev, G
Ciardi, DR
De Ridder, J
Aerts, C
AF Blomme, J.
Sarro, L. M.
O'Donovan, F. T.
Debosscher, J.
Brown, T.
Lopez, M.
Dubath, P.
Rimoldini, L.
Charbonneau, D.
Dunham, E.
Mandushev, G.
Ciardi, D. R.
De Ridder, J.
Aerts, C.
TI Improved methodology for the automated classification of periodic
variable stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; methods: statistical; techniques: photometric
ID SUPERVISED CLASSIFICATION
AB We present a novel automated methodology to detect and classify periodic variable stars in a large data base of photometric time series. The methods are based on multivariate Bayesian statistics and use a multistage approach. We applied our method to the ground-based data of the Trans-Atlantic Exoplanet Survey (TrES) Lyr1 field, which is also observed by the Kepler satellite, covering similar to 26 000 stars. We found many eclipsing binaries as well as classical non-radial pulsators, such as slowly pulsating B stars, ? Doradus, beta Cephei and d Scuti stars. Also a few classical radial pulsators were found.
C1 [Blomme, J.; Debosscher, J.; De Ridder, J.; Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium.
[Sarro, L. M.] UNED, Dpt Inteligencia Artificial, Madrid 28040, Spain.
[O'Donovan, F. T.] CALTECH, Pasadena, CA 91125 USA.
[Brown, T.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Brown, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Lopez, M.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis, E-28691 Villanueva De La Canada, Spain.
[Dubath, P.; Rimoldini, L.] Observ Geneva, CH-1290 Versoix, Switzerland.
[Charbonneau, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dunham, E.; Mandushev, G.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Ciardi, D. R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Aerts, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegem, Netherlands.
RP Blomme, J (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Heverlee, Belgium.
EM jonas.blomme@ster.kuleuven.be
RI Sarro, Luis/L-8082-2014; O'Donovan, Francis/I-2423-2014;
OI O'Donovan, Francis/0000-0002-4858-6106; Ciardi,
David/0000-0002-5741-3047
FU European Research Council under the European Community [227224];
Research Council of K. U. Leuven [GOA/2008/04]; Fund for Scientific
Research of Flanders [G.0332.06]; Belgian Federal Science Policy Office
[C90309, C90291]; Spanish Ministerio de Educacion y Ciencia
[AYA2005-04286]
FX The research leading to these results has received funding from the
European Research Council under the European Community's Seventh
Framework Programme (FP7/2007-2013)/ERC grant agreement no. 227224
(PROSPERITY), the Research Council of K. U. Leuven (GOA/2008/04), from
the Fund for Scientific Research of Flanders (G.0332.06), the Belgian
Federal Science Policy Office (C90309: CoRoT Data Exploitation, C90291
Gaia-DPAC) and the Spanish Ministerio de Educacion y Ciencia through
grant AYA2005-04286. Public access to the TrES data was provided to the
through the NASA Star and Exoplanet Database (NStED,
http://nsted.ipac.caltech.edu).
NR 13
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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 NOV
PY 2011
VL 418
IS 1
BP 96
EP 106
DI 10.1111/j.1365-2966.2011.19466.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IR
UT WOS:000297045700040
ER
PT J
AU Wright, NJ
Barlow, MJ
Ercolano, B
Rauch, T
AF Wright, N. J.
Barlow, M. J.
Ercolano, B.
Rauch, T.
TI A 3D photoionization model of the extreme planetary nebula NGC 6302
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE planetary nebulae: individual: NGC 6302; ISM: abundances
ID ASYMPTOTIC GIANT BRANCH; INTERMEDIATE-MASS STARS; HUBBLE-TYPE OUTFLOWS;
HEAVY ELEMENT LINES; POST-AGB STARS; HIGH-EXCITATION; ISO SPECTRUM;
X-RAYS; MU-M; CHEMICAL-COMPOSITION
AB We present a 3D photoionization model of the planetary nebula NGC 6302, one of the most complex and enigmatic objects of its kind. Its highly bipolar geometry and dense massive disc, coupled with the very wide range of ions present, from neutral species up to Si8+, make it one of the ultimate challenges to nebular photoionization modelling.
Our MOCASSIN model is composed of an extremely dense geometrically thin circumstellar disc and a large pair of diffuse bipolar lobes, a combination which was necessary to reproduce the observed emission-line spectrum. The masses of these components, 2.2 M-circle dot and 2.5 M-circle dot, respectively, give a total nebular mass of 4.7 M-circle dot, of which 1.8 M-circle dot (39 per cent) is ionized. Discrepancies between our model fit and the observations are attributed to complex density inhomogeneities in the nebula. The potential to resolve such discrepancies with more complex models is confirmed by exploring a range of models introducing small-scale structures. Compared to solar abundances helium is enhanced by 50 per cent, carbon is slightly subsolar, oxygen is solar, and nitrogen is enhanced by a factor of 6. These all imply a significant third dredge-up coupled with hot-bottom burning CN-cycle conversion of dredged-up carbon to nitrogen. Aluminium is also depleted by a factor of 100, consistent with depletion by dust grains.
The central star of NGC 6302 is partly obscured by the opaque circumstellar disc, which is seen almost edge-on, and as such its properties are not well constrained. However, emission from a number of high-ionization 'coronal' lines provides a strong constraint on the form of the high-energy ionizing flux. We model emission from the central star using a series of stellar model atmospheres, the properties of which are constrained from fits to the high-ionization nebular emission lines. Using a solar abundance stellar atmosphere we are unable to fit all of the observed line fluxes, but a substantially better fit was obtained using a 220 000 K hydrogen-deficient stellar atmosphere with log g = 7.0 and L-star = 14 300 L-circle dot. The H-deficient nature of the central star atmosphere suggests that it has undergone some sort of late thermal pulse, and fits to evolutionary tracks imply a central star mass of 0.73-0.82 M-circle dot. Time-scales for these evolutionary tracks suggest the object left the top of the asymptotic giant branch similar to 2100 years ago, in good agreement with studies of the recent mass-loss event that formed one pair of the bipolar lobes. Based on the modelled nebular mass and central star mass we estimate the initial mass of the central star to be 5.5 M-circle dot, in approximate agreement with that derived from evolutionary tracks.
C1 [Wright, N. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wright, N. J.; Barlow, M. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Ercolano, B.] Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
RP Wright, NJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nwright@head.cfa.harvard.edu
RI Barlow, Michael/A-5638-2009
OI Barlow, Michael/0000-0002-3875-1171
FU STFC; BIS; Miracle Consortium; SAO; German Aerospace Center (DLR) [05 OR
0806]
FX The simulations presented in this work were performed in the DiRAC
Facility jointly funded by STFC and the Large Facilities Capital Fund of
BIS. The authors acknowledge support of the STFC funded Miracle
Consortium (part of the DiRAC facility) in providing access to the
University College London (UCL) Legion High Performance Computing
Facility. The authors additionally acknowledge the support of UCL's
Research Computing team with the use of the Legion facility,
particularly Jeremy Yates and Dugan Witherick. This work has also made
use of the CHIANTI data base, a collaborative project involving
researchers at NRL (USA) RAL (UK) and the Universities of: Cambridge
(UK), George Mason (USA) and Florence (Italy).; We are grateful to the
referee, Albert Zijlstra, for a swift and helpful report that has
improved the work presented here. We would also like to thank Pete
Storey, Mikako Matsuura, Jonathan Rawlings and Tim Gledhill for
interesting discussions on this work. NJW acknowledges support from the
STFC and an SAO Pre-doctoral Fellowship. BE acknowledges support from an
STFC Advanced Fellowship. TR was supported by the German Aerospace
Center (DLR) under grant 05 OR 0806.
NR 106
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 418
IS 1
BP 370
EP 389
DI 10.1111/j.1365-2966.2011.19490.x
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IR
UT WOS:000297045700060
ER
PT J
AU Narayanan, D
Krumholz, M
Ostriker, EC
Hernquist, L
AF Narayanan, Desika
Krumholz, Mark
Ostriker, Eve C.
Hernquist, Lars
TI The CO-H2 conversion factor in disc galaxies and mergers
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM: clouds; ISM: molecules; galaxies: interactions; galaxies: ISM;
galaxies: starburst; galaxies: star formation
ID ULTRALUMINOUS INFRARED GALAXIES; GALACTIC MOLECULAR CLOUDS; SUPERMASSIVE
BLACK-HOLES; STAR-FORMING GALAXIES; GAMMA-RAY EMISSION; PARTICLE
HYDRODYNAMICS SIMULATIONS; REDSHIFT SUBMILLIMETER GALAXIES; MODELING CO
EMISSION; AEGIS FIELD GALAXIES; INTERSTELLAR-MEDIUM
AB Relating the observed CO emission from giant molecular clouds (GMCs) to the underlying H2 column density is a long-standing problem in astrophysics. While the Galactic COH2 conversion factor (XCO) appears to be reasonably constant, observations indicate that XCO may be depressed in high surface density starburst environments. Using a multiscale approach, we investigate the dependence of XCO on the galactic environment in numerical simulations of disc galaxies and galaxy mergers. XCO is proportional to the GMC surface density divided by the integrated CO intensity, WCO, and WCO is related to the kinetic temperature and velocity dispersion in the cloud. In disc galaxies (except within the central similar to kpc), the galactic environment is largely unimportant in setting the physical properties of GMCs provided they are gravitationally bound. The temperatures are roughly constant at similar to 10 K due to the balance of CO cooling and cosmic ray heating, giving a nearly constant COH2 conversion factor in discs. In mergers, the velocity dispersion of the gas rises dramatically during coalescence. The gas temperature also rises as it couples well to the warm (similar to 50 K) dust at high densities (n > 104 cm-3). The rise in velocity dispersion and temperature combine to offset the rise in surface density in mergers, causing XCO to drop by a factor of similar to 210 compared to the disc simulation. This model predicts that high-resolution Atacama Large Millimeter/submillimeter Array observations of nearby ultraluminous infrared galaxies should show velocity dispersions of 101102 km s-1, and brightness temperatures comparable to the dust temperatures.
C1 [Narayanan, Desika] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Krumholz, Mark] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ostriker, Eve C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Narayanan, D (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
EM dnarayanan@as.arizona.edu
FU NSF [AST-1009452, AST-0807739, CAREER-0955300, AST-0908185]; Alfred P.
Sloan fellowship; NASA [NNX09AK31G]; Spitzer Space Telescope Theoretical
Research Program; Harvard FAS Research Computing Group
FX This work benefited from discussions had and coding done at the Aspen
Center for Physics. DN would like thank Patrik Jonsson for numerous
helpful conversations regarding adaptive mesh techniques in radiative
transfer modelling, and Rahul Shetty, Andrew Baker, Emanuele Daddi,
Robert Feldmann, Adam Leroy, Padelis Papadopoulos and Erik Rosolowsky
for sharing their knowledge on XCO in galaxies. As always, T.
J. Cox's wisdom was invaluable in understanding the physics associated
with galaxy mergers. The authors thank the referee, Simon Glover, for a
constructive report. Finally, DN would like to thank Rob Kennicutt for
providing the original motivation to pursue this study following an
insightful question at the 2007 Gas Accretion and Star Formation
Workshop in Garching. DN acknowledges support from the NSF via grant
AST-1009452. MK acknowledges support from an Alfred P. Sloan fellowship,
the NSF through grants AST-0807739 and CAREER-0955300 and NASA through
Astrophysics Theory and Fundamental Physics grant NNX09AK31G and a
Spitzer Space Telescope Theoretical Research Program grant. ECO
acknowledges support from the NSF via grant AST-0908185. The simulations
in this paper were run on the Odyssey cluster, supported by the Harvard
FAS Research Computing Group.
NR 159
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 418
IS 1
BP 664
EP 679
DI 10.1111/j.1365-2966.2011.19516.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IR
UT WOS:000297045700085
ER
PT J
AU Kilic, M
Brown, WR
Hermes, JJ
Prieto, CA
Kenyon, SJ
Winget, DE
Winget, KI
AF Kilic, Mukremin
Brown, Warren R.
Hermes, J. J.
Allende Prieto, Carlos
Kenyon, S. J.
Winget, D. E.
Winget, K. I.
TI SDSS J163030.58+423305.8: a 40-min orbital period detached white dwarf
binary
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational waves; binaries: close; stars: individual: SDSS
J163030.58+423305.8; supernovae: general; white dwarfs
ID DIGITAL SKY SURVEY; SPY PROJECT; STARS; EVOLUTION; PROGENITOR;
SUPERNOVAE; DISCOVERY; CATALOG; SYSTEMS; I.
AB We report the discovery of a new detached, double white dwarf (WD) system with an orbital period of 39.8 min. We targeted SDSS J163030.58+423305.8 (hereafter J1630) as part of our radial velocity programme to search for companions around low-mass WDs using the 6.5-m MMT. We detect peak-to-peak radial velocity variations of 576 km s-1. The mass function and optical photometry rule out main-sequence companions. In addition, no millisecond pulsar companions are detected in radio observations. Thus the invisible companion is most likely another WD. Unlike the other 39-min binary SDSS J010657.39-100003.3, follow-up high-speed photometric observations of J1630 obtained at the McDonald 2.1-m telescope do not show significant ellipsoidal variations, indicating a higher primary mass and smaller radius. The absence of eclipses constrain the inclination angle to i= 82 degrees. J1630 contains a pair of WDs, 0.3 M? primary +=0.3 M? invisible secondary, at a separation of =0.32 R. The two WDs will merge in less than 31 Myr. Depending on the core composition of the companion, the merger will form either a single core He-burning subdwarf star or a rapidly rotating massive WD. The gravitational wave strain from J1630 is detectable by instruments like the Laser Interferometer Space Antenna (LISA) within the first year of operation.
C1 [Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Brown, Warren R.; Kenyon, S. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Hermes, J. J.; Winget, D. E.; Winget, K. I.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
RP Kilic, M (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA.
EM kilic@ou.edu
OI Kenyon, Scott/0000-0003-0214-609X
FU NSF [AST-0909107]; Norman Hackerman Advanced Research Programme
[003658-0255-2007, 003658-0252-2009]
FX We thank D. Koester for kindly providing WD model spectra. DEW and JJH
gratefully acknowledge the support of the NSF under grant AST-0909107
and the Norman Hackerman Advanced Research Programme under grants
003658-0255-2007 and 003658-0252-2009.
NR 34
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U1 1
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PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 418
IS 1
BP L157
EP L161
DI 10.1111/j.1745-3933.2011.01165.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IR
UT WOS:000297045700033
ER
PT J
AU Tchekhovskoy, A
Narayan, R
McKinney, JC
AF Tchekhovskoy, Alexander
Narayan, Ramesh
McKinney, Jonathan C.
TI Efficient generation of jets from magnetically arrested accretion on a
rapidly spinning black hole
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; MHD; methods: numerical;
galaxies: jets
ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; ACTIVE GALACTIC NUCLEI;
RELATIVISTIC MAGNETOHYDRODYNAMICS; ELECTROMAGNETIC EXTRACTION; NUMERICAL
SCHEME; COLLAPSING STAR; RADIO-SOURCES; DISKS; ENERGY; FIELD
AB We describe global, 3D, time-dependent, non-radiative, general-relativistic, magnetohydrodynamic simulations of accreting black holes (BHs). The simulations are designed to transport a large amount of magnetic flux to the centre, more than the accreting gas can force into the BH. The excess magnetic flux remains outside the BH, impedes accretion, and leads to a magnetically arrested disc. We find powerful outflows. For a BH with spin parameter a = 0.5, the efficiency with which the accretion system generates outflowing energy in jets and winds is eta approximate to 30 per cent. For a = 0.99, we find eta approximate to 140 per cent, which means that more energy flows out of the BH than flows in. The only way this can happen is by extracting spin energy from the BH. Thus the a = 0.99 simulation represents an unambiguous demonstration, within an astrophysically plausible scenario, of the extraction of net energy from a spinning BH via the PenroseBlandfordZnajek mechanism. We suggest that magnetically arrested accretion might explain observations of active galactic nuclei with apparent eta approximate to few x 100 per cent.
C1 [Tchekhovskoy, Alexander] Princeton Univ, Ctr Theoret Sci, Princeton, NJ 08544 USA.
[Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[McKinney, Jonathan C.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA.
RP Tchekhovskoy, A (reprint author), Princeton Ctr Theoret Sci, Princeton, NJ USA.
EM atchekho@princeton.edu
OI Narayan, Ramesh/0000-0002-1919-2730
FU NSF [AST-1041590]; NASA [NNX11AE16G]; [TG-AST10-0040];
[TG-AST080026N]; [TG-AST080025N]
FX We thank S. Balbus, K. Beckwith, A. Benson, V. Beskin, I. Contopoulos,
L. Foschini, D. Giannios, J. Goodman, I. Igumenshchev, B. Metzger, R.
Penna, R. Rafikov, A. Spitkovsky, J. Stone, F. Tombesi, D. Uzdensky for
discussions. We thank the anonymous referee for useful suggestions. AT
was supported by a Princeton Center for Theoretical Science Fellowship.
AT and RN were supported in part by NSF grant AST-1041590 and NASA grant
NNX11AE16G. We acknowledge support by the NSF through TeraGrid resources
provided by NICS Kraken, where simulations were carried out, NICS
Nautilus, where data were analysed, and NCSA MSS, where data were backed
up, under grant numbers TG-AST10-0040 (AT), TG-AST080026N (RN) and
TG-AST080025N (JCM).
NR 42
TC 208
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U1 2
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 418
IS 1
BP L79
EP L83
DI 10.1111/j.1745-3933.2011.01147.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IR
UT WOS:000297045700017
ER
PT J
AU Nardini, E
Risaliti, G
AF Nardini, E.
Risaliti, G.
TI The effects of X-ray absorption variability in NGC 4395
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: individual: NGC 4395; X-rays: galaxies
ID SEYFERT-1 GALAXY NGC-4395; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS;
EMISSION-LINE; REFLECTION; MODELS; ORIGIN; SOFT
AB We present a new X-ray analysis of the dwarf Seyfert galaxy NGC 4395, based on two archival XMMNewton and Suzaku observations. This source is well known for a series of remarkable properties: one of the smallest estimated black hole masses among active galactic nuclei (AGN) (of the order of similar to 105 M?), intense flux variability on very short time-scales (a few tens of seconds) and an unusually flat X-ray continuum (G similar to 1.4 over the 210 keV energy range). NGC 4395 is also characterized by significant variations of the X-ray spectral shape, and here we show that such behaviour can be explained through the partial occultation by circumnuclear cold absorbers with column densities of similar to 10221023 cm-2. In this scenario, the primary X-ray emission is best reproduced by means of a power law with a standard G similar to 1.8 photon index, consistent with both the spectral slope observed at higher energies and the values typical of local AGN.
C1 [Nardini, E.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
RP Nardini, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM enardini@cfa.harvard.edu
RI XRAY, SUZAKU/A-1808-2009;
OI Risaliti, Guido/0000-0002-3556-977X
FU NASA [NNX08AN48G]
FX This work has been partly supported by NASA grant NNX08AN48G. We thank
the anonymous referee for constructive and useful comments which
significantly improved the content of this paper.
NR 28
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 4
BP 2571
EP 2576
DI 10.1111/j.1365-2966.2011.19423.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IA
UT WOS:000297043900011
ER
PT J
AU Cohen, O
AF Cohen, O.
TI The independency of stellar mass-loss rates on stellar X-ray luminosity
and activity level based on solar X-ray flux and solar wind observations
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: magnetic field; stars: mass-loss; stars: solar-type; stars:
winds; outflows
ID HELIOSPHERIC MAGNETIC-FIELD; ANGULAR-MOMENTUM; STARS; SUN; VLA;
EJECTIONS; ULYSSES
AB Stellar mass-loss rates are an important input ingredient for stellar evolution models since they determine stellar evolution parameters such as stellar spin-down and increase in stellar luminosity through the lifetime of a star. Due to the lack of direct observations of stellar winds from Sun-like stars stellar X-ray luminosity and stellar level of activity are commonly used as a proxy for estimating stellar mass-loss rates. However, such an intuitive activity mass-loss rate relation is not well defined. In this paper, I study the mass-loss rate of the Sun as a function of its activity level. I compare in situ solar wind measurements with the solar activity level represented by the solar X-ray flux. I find no clear dependency of the solar mass flux on solar X-ray flux. Instead, the solar mass-loss rate is scattered around an average value of 2 x 10(-14) M(circle dot)yr(-1). This independency of the mass-loss rate on level of activity can be explained by the fact that the activity level is governed by the large modulations in the solar close magnetic flux, while the mass-loss rate is governed by the rather constant open magnetic flux. I derive a simple expression for stellar mass-loss rates as a function of the stellar ambient weak magnetic field, the stellar radius, the stellar escape velocity and the average height of the Alfven surface. This expression predicts stellar mass-loss rates of 10(-15) to 10(-12) M-circle dot yr(-1) for Sun-like stars.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ocohen@cfa.harvard.edu
OI Cohen, Ofer/0000-0003-3721-0215
FU SHINE through NSF [ATM-0823592]; NASA-LWSTRT [NNG05GM44G]
FX I would like to thank an unknown referee for his/her review. I thank
Jeremy Drake, Vinay Kashyap, Steve Saar, Steven Cranmer and Justin
Kasper for their useful comments and discussion during the preparation
of this article. OC is supported by SHINE through NSF ATM-0823592 grant
and by NASA-LWSTRT grant NNG05GM44G.
NR 50
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U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 4
BP 2592
EP 2600
DI 10.1111/j.1365-2966.2011.19428.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IA
UT WOS:000297043900013
ER
PT J
AU Kassin, SA
Fogarty, L
Goodsall, T
Clarke, FJ
Houghton, RWC
Salter, G
Thatte, N
Tecza, M
Davies, RL
Weiner, BJ
Willmer, CNA
Salim, S
Cooper, MC
Newman, JA
Bundy, K
Conselice, CJ
Koekemoer, AM
Lin, LW
Moustakas, LA
Wang, T
AF Kassin, Susan A.
Fogarty, L.
Goodsall, T.
Clarke, F. J.
Houghton, R. W. C.
Salter, G.
Thatte, N.
Tecza, M.
Davies, Roger L.
Weiner, Benjamin J.
Willmer, C. N. A.
Salim, Samir
Cooper, Michael C.
Newman, Jeffrey A.
Bundy, Kevin
Conselice, C. J.
Koekemoer, A. M.
Lin, Lihwai
Moustakas, Leonidas A.
Wang, Tao
TI Oxford SWIFT integral field spectrograph and multiwavelength
observations of the Eagle galaxy at z=0.77
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: high-redshift; galaxies: interactions; galaxies: irregular;
galaxies: kinematics and dynamics
ID STAR-FORMING GALAXIES; TULLY-FISHER RELATION; SIMILAR-TO 0.6; DATA
REDUCTION SOFTWARE; INITIAL MASS FUNCTION; EXTENDED GROTH STRIP;
TKRS/GOODS-N FIELD; FORMATION RATES; DYNAMICAL EVOLUTION; LUMINOSITY
FUNCTION
AB The Eagle galaxy at a redshift of 0.77 is studied with the Oxford Short Wavelength Integral Field Spectrograph (SWIFT) and multiwavelength data from the All-wavelength Extended Groth strip International Survey (AEGIS). It was chosen from AEGIS because of the bright and extended emission in its slit spectrum. 3D kinematic maps of the Eagle reveal a gradient in velocity dispersion which spans 3575 +/- 10 km s-1 and a rotation velocity of 25 +/- 5 km s-1 uncorrected for inclination. Hubble Space Telescope images suggest it is close to face-on. In comparison with galaxies from AEGIS at similar redshifts, the Eagle is extremely bright and blue in the rest-frame optical, highly star forming, dominated by unobscured star formation and has a low metallicity for its size. This is consistent with its selection. The Eagle is likely undergoing a major merger and is caught in the early stage of a starburst when it has not yet experienced metal enrichment or formed the mass of dust typically found in star-forming galaxies.
C1 [Kassin, Susan A.; Fogarty, L.; Goodsall, T.; Clarke, F. J.; Houghton, R. W. C.; Salter, G.; Thatte, N.; Tecza, M.; Davies, Roger L.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Fogarty, L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Goodsall, T.; Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Salter, G.] Univ New S Wales, Dept Astrophys, Sch Phys, Sydney, NSW 2052, Australia.
[Weiner, Benjamin J.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Salim, Samir] Indiana Univ, Dept Astron, Bloomington, IN 47404 USA.
[Cooper, Michael C.] Univ Calif Irvine, Ctr Galaxy Evolut, Dept Phys & Astron, Irvine, CA 92697 USA.
[Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA USA.
[Bundy, Kevin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94705 USA.
[Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Lin, Lihwai] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Wang, Tao] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kassin, SA (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
EM susan.kassin@nasa.gov
RI Salim, Siti Mawarni/B-7940-2010; Conselice, Christopher/B-4348-2013;
OI Koekemoer, Anton/0000-0002-6610-2048; Salim, Siti
Mawarni/0000-0001-5543-5384; Conselice, Christopher/0000-0003-1949-7638;
Weiner, Benjamin/0000-0001-6065-7483; Moustakas,
Leonidas/0000-0003-3030-2360
FU European Commission [MEXT-CT-2003-002792]; University of Oxford Physics
Department; John Fell OUP Research Fund; Caltech Optical Observatories;
Observational Astrophysics Rolling Grant at Oxford; Oxford Astrophysics
PATT [ST/G004331/1]; NSF [AST00-71198, AST05-07483, AST08-08133];
Balliol College, Oxford; STFC; NASA; NASA ATFP
FX The Oxford SWIFT integral field spectrograph is directly supported by a
Marie Curie Excellence Grant from the European Commission
(MEXT-CT-2003-002792, Team Leader: N. Thatte). It is also supported by
additional funds from the University of Oxford Physics Department and
the John Fell OUP Research Fund. Additional funds to host and support
SWIFT were provided by Caltech Optical Observatories.; Additional
support was provided for by the Observational Astrophysics Rolling Grant
at Oxford and the Oxford Astrophysics PATT Linked Grant ST/G004331/1.
The following NSF grants to the DEEP2 survey are acknowledged:
AST00-71198, AST05-07483 and AST08-08133.; LF would like to acknowledge
the generous support of the Foley-Bejar Scholarship through Balliol
College, Oxford and the support of the STFC.; This work of LAM was
carried out in part at Jet Propulsion Laboratory, California Institute
of Technology, under a contract with NASA. LAM acknowledges support from
the NASA ATFP programme.
NR 70
TC 2
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U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 4
BP 2882
EP 2890
DI 10.1111/j.1365-2966.2011.19449.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IA
UT WOS:000297043900033
ER
PT J
AU Pierini, D
Giodini, S
Finoguenov, A
Bohringer, H
D'Onghia, E
Pratt, GW
Democles, J
Pannella, M
Zibetti, S
Braglia, FG
Verdugo, M
Ziparo, F
Koekemoer, AM
Salvato, M
AF Pierini, D.
Giodini, S.
Finoguenov, A.
Boehringer, H.
D'Onghia, E.
Pratt, G. W.
Democles, J.
Pannella, M.
Zibetti, S.
Braglia, F. G.
Verdugo, M.
Ziparo, F.
Koekemoer, A. M.
Salvato, M.
CA COSMOS Collaboration
TI Two fossil groups of galaxies at z similar to 0.4 in the Cosmic
Evolution Survey: accelerated stellar-mass build-up, different
progenitors
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: groups: general; galaxies: luminosity
function, mass function; X-rays: galaxies: clusters
ID HUBBLE-SPACE-TELESCOPE; STAR-FORMATION RATES; DIGITAL SKY SURVEY;
LUMINOSITY FUNCTION; ELLIPTIC GALAXIES; CLUSTER GALAXIES; SHELL
GALAXIES; RICH CLUSTERS; DARK-MATTER; MILLENNIUM SIMULATION
AB We report on two fossil groups of galaxies at redshifts z= 0.425 and 0.372 discovered in the Cosmic Evolution Survey (COSMOS) area. Selected as X-ray extended sources, they have total masses (M200) equal to 1.9(+/- 0.41) x 1013 and 9.5(+/- 0.42) x 1013 M-circle dot, respectively, as obtained from a recent X-ray luminositymass scaling relation. The lower mass system appears isolated, whereas the other sits in a well-known large-scale structure (LSS) populated by 27 other X-ray emitting groups. The identification as fossil is based on the i-band photometry of all the galaxies with a photometric redshift consistent with that of the group at the 2s confidence level and within a projected groupcentric distance equal to 0.5R200, and iAB= 22.5 mag limited spectroscopy. Both fossil groups exhibit high stellar-to-total mass ratios compared to all the X-ray selected groups of similar mass at 0.3 =z= 0.5 in the COSMOS. At variance with the composite galaxy stellar mass functions (GSMFs) of similarly massive systems, both fossil group GSMFs are dominated by passively evolving galaxies down to Mstars similar to 1010 M-circle dot (according to the galaxy broad-band spectral energy distributions). The relative lack of star-forming galaxies with 1010=Mstars= 1011 M-circle dot is confirmed by the galaxy distribution in the b-r versus i colourmagnitude diagram. Hence, the two fossil groups appear as more mature than the coeval, similarly massive groups. Their overall star formation activity ended rapidly after an accelerated build up of the total stellar mass; no significant infall of galaxies with Mstars= 1010 M-circle dot took place in the last 3 to 6 Gyr. This similarity holds although the two fossil groups are embedded in two very different density environments of the LSS, which suggests that their galaxy populations were shaped by processes that do not depend on the LSS. However, their progenitors may do so. We discuss why the late merging of a compact group is favoured over the early assembly as a formation scenario for the isolated, low-mass fossil group.
C1 [Pierini, D.; Finoguenov, A.; Boehringer, H.; Verdugo, M.; Ziparo, F.; Salvato, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Giodini, S.] Leiden Observ, NL-2300 RA Leiden, Netherlands.
[D'Onghia, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pratt, G. W.; Democles, J.; Pannella, M.] Univ Paris Diderot, CEA Saclay, CNRS,Lab AIM, DAPNIA Serv Astrophys,CEA DSM, F-91191 Gif Sur Yvette, France.
[Zibetti, S.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark.
[Braglia, F. G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Salvato, M.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Salvato, M.] CALTECH, Pasadena, CA 91125 USA.
RP Pierini, D (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
EM dpierini@mpe.mpg.de
OI Koekemoer, Anton/0000-0002-6610-2048
NR 101
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U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 4
BP 2927
EP 2937
DI 10.1111/j.1365-2966.2011.19454.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IA
UT WOS:000297043900037
ER
PT J
AU Sheth, RK
Diaferio, A
AF Sheth, Ravi K.
Diaferio, Antonaldo
TI How unusual are the Shapley supercluster and the Sloan Great Wall?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: analytical; galaxies: clusters: general; dark matter;
large-scale structure of Universe
ID DARK-MATTER HALOES; PROBABILITY-DISTRIBUTION FUNCTION; GAUSSIAN
RANDOM-FIELDS; LARGE-SCALE STRUCTURE; EXCURSION SET MODEL; X-RAY;
PERTURBATION-THEORY; GENERAL MORPHOLOGY; GALAXY CLUSTERS; REDSHIFT
SURVEY
AB We show that extreme value statistics are useful for studying the largest structures in the Universe by using them to assess the significance of two of the most dramatic structures in the local Universe the Shapley supercluster and the Sloan Great Wall. If we assume that the Shapley concentration (volume approximate to 1.2 x 10(5) h(-3) Mpc(3)) evolved from an overdense region in the initial Gaussian fluctuation field, with currently popular choices for the background cosmological model and the shape and amplitude s8 of the initial power spectrum, we estimate that the total mass of the system is within 20 per cent of 1.8 x 1016 h(-1) M-circle dot. Extreme value statistics show that the existence of this massive concentration is not unexpected if the initial fluctuation field was Gaussian, provided there are no other similar objects within a sphere of radius 200 h(-1) Mpc centred on our Galaxy. However, a similar analysis of the Sloan Great Wall, a more distant (z similar to 0.08) and extended concentration of structures (volume similar to 7.2 x 105 h(-3) Mpc3), suggests that it is more unusual. We estimate its total mass to be within 20 per cent of 1.2 x 1017 h(-1) M-circle dot and we find that even if it is the densest such object of its volume within z= 0.2, its existence is difficult to reconcile with the assumption of Gaussian initial conditions if s8 was less than 0.9. This tension can be alleviated if this structure is the densest within the Hubble volume. Finally, we show how extreme value statistics can be used to address the question of how likely it is that an object like the Shapley supercluster exists in the same volume which contains the Sloan Great Wall, finding, again, that Shapley is not particularly unusual. Since it is straightforward to incorporate other models of the initial fluctuation field into our formalism, we expect our approach will allow observations of the largest structures clusters, superclusters and voids to provide relevant constraints on the nature of the primordial fluctuation field.
C1 [Sheth, Ravi K.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Sheth, Ravi K.] Abdus Salam Int Ctr Theoret Phys, I-34151 Trieste, Italy.
[Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy.
[Diaferio, Antonaldo] Ist Nazl Fis Nucl INFN, Sez Torino, I-10125 Turin, Italy.
[Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Sheth, RK (reprint author), Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA.
EM shethrk@physics.upenn.edu; diaferio@ph.unito.it
FU INFN [PD51]; MIUR; NSF-AST [0908241]
FX We thank the INFN exchange program for support, and the Centro di
Ciencias de Benasque 'Pedro Pascual' for hospitality during the summer
of 2008 when most of this work was completed, Jorg Colberg for
encouragement then, Aseem Paranjape for encouragement now, and Stefano
Camera for providing the opportunity for us to meet again and complete
this work. RKS is supported in part by NSF-AST 0908241. AD acknowledges
additional support from the INFN grant PD51 and the PRIN-MIUR-2008 grant
'Matter-antimatter asymmetry, dark matter and dark energy in the LHC
era'. This research has made use of NASA's Astrophysics Data System.
NR 53
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U1 0
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 4
BP 2938
EP 2949
DI 10.1111/j.1365-2966.2011.19453.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848IA
UT WOS:000297043900038
ER
PT J
AU Pogue, MG
AF Pogue, Michael G.
TI Larval Description of Copitarsia incommoda (Lepidoptera: Noctuidae)
SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA
LA English
DT Article
DE Bolivia; Altiplano; invasive species; pest; quinoa
AB The last instar of Copitarsia incommoda (Walker) is described for the first time. Specimens in this study were reared from quinoa (Chenopodium quinoa Willd., Chenopodiaceae), Bolivia, La Paz, 4 km S Viacha, Quipaquipani, 3,880 m. The larva of Copitarsia incommoda is compared with larvae of Copitarsia decolora (Guenee) and Copitarsia corruda Pogue and Simmons.
C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, Washington, DC 20013 USA.
RP Pogue, MG (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, POB 37012,MRC-168, Washington, DC 20013 USA.
EM michael.pogue@ars.usda.gov
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PU ENTOMOLOGICAL SOC AMER
PI LANHAM
PA 10001 DEREKWOOD LANE, STE 100, LANHAM, MD 20706-4876 USA
SN 0013-8746
J9 ANN ENTOMOL SOC AM
JI Ann. Entomol. Soc. Am.
PD NOV
PY 2011
VL 104
IS 6
BP 1292
EP 1296
DI 10.1603/AN10099
PG 5
WC Entomology
SC Entomology
GA 849ZJ
UT WOS:000297163900018
ER
PT J
AU Morowitz, H
Sagan, C
AF Morowitz, Harold
Sagan, Carl
TI Life in the Clouds of Venus?
SO ASTROBIOLOGY
LA English
DT Editorial Material
C1 [Morowitz, Harold] Yale Univ, Dept Mol Biophys, New Haven, CT 06520 USA.
[Sagan, Carl] Smithsonian Astrophys Observ, Harvard Coll Observ, Cambridge, MA USA.
RP Morowitz, H (reprint author), Yale Univ, Dept Mol Biophys, New Haven, CT 06520 USA.
NR 0
TC 0
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U1 5
U2 21
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 NOV
PY 2011
VL 11
IS 9
BP 932
EP 932
PG 1
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 851JK
UT WOS:000297264300010
ER
PT J
AU Zeigler, SL
Neel, MC
Oliveira, L
Raboy, BE
Fagan, WF
AF Zeigler, Sara L. d
Neel, Maile C.
Oliveira, Leonardo
Raboy, Becky E.
Fagan, William F.
TI Conspecific and heterospecific attraction in assessments of functional
connectivity
SO BIODIVERSITY AND CONSERVATION
LA English
DT Article
DE Atlantic forest; Brazil; Circuit theory; Dispersal; Graph theory;
Golden-headed lion tamarin; Wied's marmoset
ID HEADED LION TAMARIN; SOCIAL-INFORMATION USE; LANDSCAPE CONNECTIVITY;
HABITAT PATCHES; LEONTOPITHECUS-CHRYSOMELAS; FRAGMENTED LANDSCAPES;
REPRODUCTIVE SUCCESS; PLANT CONSERVATION; PERCEPTUAL RANGE; FOREST
AB Functional connectivity is known to have an important, positive influence on species persistence. Measurements of functional connectivity traditionally focus on structural attributes of landscapes such as the distance and matrix type between habitat patches as well as on how species interact with those structural attributes. However, we propose that the social behavior of a species, through conspecific and heterospecific attraction, will also impact connectivity by changing how dispersers move with respect to each other and occupied patches. We analyzed functional connectivity patterns using circuit and graph theory for golden-headed lion tamarins (Leontopithecus chrysomelas) in Brazil under three scenarios. In the first scenario, we looked at connectivity without the effects of attraction under varying maximum dispersal distance and ecological movement cost thresholds. In the second scenario, we allowed dispersers to travel over more hostile matrix than they normally would to reach an occupied patch. In the final scenario, we allowed dispersers to move only to occupied patches. We found that, according to the first scenario, range-wide functional landscape connectivity for golden-headed lion tamarins is low at realistic maximum dispersal distance and movement cost thresholds. Incorporating the effects of conspecific or heterospecific attraction would increase functional connectivity, in the case of scenario two, or decrease functional connectivity, in the case of scenario three. Because conspecific/heterospecific attraction can have an impact on movement for some species, this factor should be incorporated in assessments of functional connectivity patterns for social species and others where patch occupancy is likely to influence the movements of dispersers.
C1 [Zeigler, Sara L. d] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA.
[Zeigler, Sara L. d] Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
[Neel, Maile C.] Univ Maryland, Dept Plant Sci & Landscape Architecture, College Pk, MD 20742 USA.
[Oliveira, Leonardo; Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Raboy, Becky E.] Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
[Raboy, Becky E.] Royal Zool Soc Antwerp, Ctr Res & Conservat, Antwerp, Belgium.
RP Zeigler, SL (reprint author), Virginia Tech, Dept Biol Sci, 4095 Derring Hall, Blacksburg, VA 24061 USA.
EM szeig23@vt.edu
RI Oliveira, Leonardo/G-1290-2012
OI Oliveira, Leonardo/0000-0002-1774-0713
FU University of Maryland
FX We thank Brad McRae and Santiago Saura for their quick and enthusiastic
help with the use of their modeling software. Michael Lloyd provided
technical support. Finally, we thank James Dietz, Jennifer Mickelberg,
and Carlos Guidorizzi for sharing their unpublished work and for
providing interesting discussions on lion tamarin movement. Funding was
provided through the Anne G. Wylie Dissertation Fellowship through the
University of Maryland (to S.Z. and L.O.).
NR 73
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U1 5
U2 31
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0960-3115
J9 BIODIVERS CONSERV
JI Biodivers. Conserv.
PD NOV
PY 2011
VL 20
IS 12
BP 2779
EP 2796
DI 10.1007/s10531-011-0107-z
PG 18
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 850MX
UT WOS:000297200000014
ER
PT J
AU Cuk, M
Gladman, BJ
Stewart, ST
AF Cuk, Matija
Gladman, Brett J.
Stewart, Sarah T.
TI Rebuttal to the comment by Malhotra and Strom on "Constraints on the
source of lunar cataclysm impactors"
SO ICARUS
LA English
DT Editorial Material
DE Moon; Moon, Surface; Cratering; Asteroids, Dynamics; Planets, Migration
ID CRATERS; ORIGIN
AB Cuk et al. (Cuk, M. Gladman, B.J., Stewart, S.T. [2010]. Icarus 207 590-594) concluded that the the lunar cataclysm (late heavy bombardment) was recorded in lunar Imbrian era craters, and that their size distribution is different from that of main belt asteroids (which may have been the dominant pre-Imbrian impactors). This result would likely preclude the asteroid belt as the direct source of lunar cataclysm impactors. Malhotra and Strom (Malhotra, R., Strom, R.G. [2011]. Icarus) maintain that the lunar impactor population in the Imbrian era was the same as in Nectarian and pre-Nectarian periods, and this population had a size distribution identical to that of main belt asteroids. In support of this claim, they present an Imbrian size distribution made from two data sets published by Wilhelms et al. (Wilhelms, D.E., Oberbeck, V.R., Aggarwal, H.R. [1978]. Proc. Lunar Sci. Conf. 9, 3735-3762). However, these two data sets cannot be simply combined as they represent areas of different ages and therefore crater densities. Malhotra and Strom (Malhotra, R., Strom, R.G. [2011]. Icarus) differ with the main conclusion of Wilhelms et al. (Wilhelms, D.E., Oberbeck, V.R., Aggarwal, H.R. [1978]. Proc. Lunar Sci. Conf. 9,3735-3762) that the Nectarian and Imbrian crater size distributions were different. We conclude that the available data indicate that the lunar Imbrian-era impactors had a different size distribution from the older ones, with the Imbrian impactor distribution being significantly richer in small impactors than that of older lunar impactors or current main-belt asteroids. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Cuk, Matija] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cuk, Matija; Stewart, Sarah T.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Gladman, Brett J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
RP Cuk, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM cuk@eps.harvard.edu
OI Stewart, Sarah/0000-0001-9606-1593
NR 10
TC 5
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U1 0
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD NOV
PY 2011
VL 216
IS 1
BP 363
EP 365
DI 10.1016/j.icarus.2011.08.011
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 843FQ
UT WOS:000296658100031
ER
PT J
AU Abazajian, KN
Calabrese, E
Cooray, A
De Bernardis, F
Dodelson, S
Friedland, A
Fuller, GM
Hannestad, S
Keating, BG
Linder, EV
Lunardini, C
Melchiorri, A
Miquel, R
Pierpaoli, E
Pritchard, J
Serra, P
Takada, M
Wong, YYY
AF Abazajian, K. N.
Calabrese, E.
Cooray, A.
De Bernardis, F.
Dodelson, S.
Friedland, A.
Fuller, G. M.
Hannestad, S.
Keating, B. G.
Linder, E. V.
Lunardini, C.
Melchiorri, A.
Miquel, R.
Pierpaoli, E.
Pritchard, J.
Serra, P.
Takada, M.
Wong, Y. Y. Y.
TI Cosmological and astrophysical neutrino mass measurements
SO ASTROPARTICLE PHYSICS
LA English
DT Review
DE Neutrinos; Cosmology
ID LYMAN-ALPHA FOREST; DIGITAL SKY SURVEY; EQUATION-OF-STATE; POWER
SPECTRUM; CONCORDANCE MODEL; PRESSURE SUPPORT; DARK-MATTER; PARAMETERS;
REIONIZATION; SIMULATIONS
AB Cosmological and astrophysical measurements provide powerful constraints on neutrino masses complementary to those from accelerators and reactors. Here we provide a guide to these different probes, for each explaining its physical basis, underlying assumptions, current and future reach. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Dodelson, S.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Abazajian, K. N.] Univ Maryland, Dept Phys, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA.
[Calabrese, E.; Melchiorri, A.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Calabrese, E.; Melchiorri, A.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, I-00185 Rome, Italy.
[Cooray, A.; De Bernardis, F.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Dodelson, S.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Dodelson, S.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Friedland, A.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
[Fuller, G. M.; Keating, B. G.] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Hannestad, S.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Linder, E. V.] Berkeley Lab, Berkeley, CA 94720 USA.
[Linder, E. V.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Linder, E. V.] Ewha Womans Univ, Inst Early Universe WCU, Seoul, South Korea.
[Lunardini, C.] Arizona State Univ, Tempe, AZ 85287 USA.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Miquel, R.] Inst Fis Altes Energies, E-08193 Bellaterra, Barcelona, Spain.
[Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
[Pritchard, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Serra, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Takada, M.] Univ Tokyo, IPMU, Chiba 2778582, Japan.
[Wong, Y. Y. Y.] Rhein Westfal TH Aachen, Inst Theoret Teilchenphys & Kosmol, D-52056 Aachen, Germany.
RP Dodelson, S (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM Dodelson@fnal.gov
RI Takada, Masahiro/A-4364-2011; Serra, Paolo/G-9678-2014;
OI Serra, Paolo/0000-0002-7609-3931; Melchiorri,
Alessandro/0000-0001-5326-6003; Pritchard, Jonathan/0000-0003-4127-5353;
Miquel, Ramon/0000-0002-6610-4836; Pierpaoli, Elena/0000-0002-7957-8993
NR 81
TC 85
Z9 85
U1 0
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
J9 ASTROPART PHYS
JI Astropart Phys.
PD NOV
PY 2011
VL 35
IS 4
BP 177
EP 184
DI 10.1016/j.astropartphys.2011.07.002
PG 8
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 846XU
UT WOS:000296937300003
ER
PT J
AU Buchhave, LA
Latham, DW
Carter, JA
Desert, JM
Torres, G
Adams, ER
Bryson, ST
Charbonneau, DB
Ciardi, DR
Kulesa, C
Dupree, AK
Fischer, DA
Fressin, F
Gautier, TN
Gilliland, RL
Howell, SB
Isaacson, H
Jenkins, JM
Marcy, GW
McCarthy, DW
Rowe, JF
Batalha, NM
Borucki, WJ
Brown, TM
Caldwell, DA
Christiansen, JL
Cochran, WD
Deming, D
Dunham, EW
Everett, M
Ford, EB
Fortney, JJ
Geary, JC
Girouard, FR
Haas, MR
Holman, MJ
Horch, E
Klaus, TC
Knutson, HA
Koch, DG
Kolodziejczak, J
Lissauer, JJ
Machalek, P
Mullally, F
Still, MD
Quinn, SN
Seager, S
Thompson, SE
Van Cleve, J
AF Buchhave, Lars A.
Latham, David W.
Carter, Joshua A.
Desert, Jean-Michel
Torres, Guillermo
Adams, Elisabeth R.
Bryson, Stephen T.
Charbonneau, David B.
Ciardi, David R.
Kulesa, Craig
Dupree, Andrea K.
Fischer, Debra A.
Fressin, Francois
Gautier, Thomas N., III
Gilliland, Ronald L.
Howell, Steve B.
Isaacson, Howard
Jenkins, Jon M.
Marcy, Geoffrey W.
McCarthy, Donald W.
Rowe, Jason F.
Batalha, Natalie M.
Borucki, William J.
Brown, Timothy M.
Caldwell, Douglas A.
Christiansen, Jessie L.
Cochran, William D.
Deming, Drake
Dunham, Edward W.
Everett, Mark
Ford, Eric B.
Fortney, Jonathan J.
Geary, John C.
Girouard, Forrest R.
Haas, Michael R.
Holman, Matthew J.
Horch, Elliott
Klaus, Todd C.
Knutson, Heather A.
Koch, David G.
Kolodziejczak, Jeffrey
Lissauer, Jack J.
Machalek, Pavel
Mullally, Fergal
Still, Martin D.
Quinn, Samuel N.
Seager, Sara
Thompson, Susan E.
Van Cleve, Jeffrey
TI KEPLER-14b: A MASSIVE HOT JUPITER TRANSITING AN F STAR IN A CLOSE VISUAL
BINARY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planetary systems; stars: individual (Kepler-14b, KIC 10264660, 2MASS
J19105011+4719589); techniques: photometric; techniques: spectroscopic
ID SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; EXTRASOLAR PLANET;
K-DWARF; STELLAR; MISSION; II.; PARAMETERS; ATMOSPHERE; DISCOVERY
AB We present the discovery of a hot Jupiter transiting an F star in a close visual (0 ''.3 sky projected angular separation) binary system. The dilution of the host star's light by the nearly equal magnitude stellar companion (similar to 0.5 mag fainter) significantly affects the derived planetary parameters, and if left uncorrected, leads to an underestimate of the radius and mass of the planet by 10% and 60%, respectively. Other published exoplanets, which have not been observed with high-resolution imaging, could similarly have unresolved stellar companions and thus have incorrectly derived planetary parameters. Kepler-14b (KOI-98) has a period of P = 6.790 days and, correcting for the dilution, has a mass of M-p = 8.40(-0.34)(+ 0.35) M-J and a radius of R-p = 1.136(-0.054)(+ 0.073) R-J, yielding a mean density of rho(p) = 7.1 +/- 1.1 g cm(-3).
C1 [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
[Latham, David W.; Carter, Joshua A.; Desert, Jean-Michel; Torres, Guillermo; Adams, Elisabeth R.; Charbonneau, David B.; Dupree, Andrea K.; Fressin, Francois; Geary, John C.; Holman, Matthew J.; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91109 USA.
[Kulesa, Craig] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Isaacson, Howard; Marcy, Geoffrey W.; Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Jenkins, Jon M.; Rowe, Jason F.; Caldwell, Douglas A.; Christiansen, Jessie L.; Machalek, Pavel; Mullally, Fergal; Thompson, Susan E.; Van Cleve, Jeffrey] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[McCarthy, Donald W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Girouard, Forrest R.; Klaus, Todd C.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Kolodziejczak, Jeffrey] MSFC, Huntsville, AL 35805 USA.
[Still, Martin D.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Seager, Sara] MIT, Newton, MA 02159 USA.
RP Buchhave, LA (reprint author), Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark.
RI Carter, Joshua/A-8280-2013; Caldwell, Douglas/L-7911-2014;
OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
David/0000-0002-5741-3047; Caldwell, Douglas/0000-0003-1963-9616;
/0000-0001-6545-639X; Fischer, Debra/0000-0003-2221-0861; Fortney,
Jonathan/0000-0002-9843-4354
FU Carlsberg Foundation; NASA's Science Mission Directorate; NASA; NASA
through JPL/Caltech
FX The work of L.A.B. was supported by the Carlsberg Foundation. Funding
for this Discovery Mission is provided by NASA's Science Mission
Directorate. This paper uses observations obtained with 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. This work is also based on observations made with the
Spitzer Space Telescope which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was also provided by NASA through an award
issued by JPL/Caltech.
NR 37
TC 35
Z9 35
U1 0
U2 6
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 NOV
PY 2011
VL 197
IS 1
AR 3
DI 10.1088/0067-0049/197/1/3
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400003
ER
PT J
AU Cochran, WD
Fabrycky, DC
Torres, G
Fressin, F
Desert, JM
Ragozzine, D
Sasselov, D
Fortney, JJ
Rowe, JF
Brugamyer, EJ
Bryson, ST
Carter, JA
Ciardi, DR
Howell, SB
Steffen, JH
Borucki, WJ
Koch, DG
Winn, JN
Welsh, WF
Uddin, K
Tenenbaum, P
Still, M
Seager, S
Quinn, SN
Mullally, F
Miller, N
Marcy, GW
MacQueen, PJ
Lucas, P
Lissauer, JJ
Latham, DW
Knutson, H
Kinemuchi, K
Johnson, JA
Jenkins, JM
Isaacson, H
Howard, A
Horch, E
Holman, MJ
Henze, CE
Haas, MR
Gilliland, RL
Gautier, TN
Ford, EB
Fischer, DA
Everett, M
Endl, M
Demory, BO
Deming, D
Charbonneau, D
Caldwell, D
Buchhave, L
Brown, TM
Batalha, N
AF Cochran, William D.
Fabrycky, Daniel C.
Torres, Guillermo
Fressin, Francois
Desert, Jean-Michel
Ragozzine, Darin
Sasselov, Dimitar
Fortney, Jonathan J.
Rowe, Jason F.
Brugamyer, Erik J.
Bryson, Stephen T.
Carter, Joshua A.
Ciardi, David R.
Howell, Steve B.
Steffen, Jason H.
Borucki, William. J.
Koch, David G.
Winn, Joshua N.
Welsh, William F.
Uddin, Kamal
Tenenbaum, Peter
Still, M.
Seager, Sara
Quinn, Samuel N.
Mullally, F.
Miller, Neil
Marcy, Geoffrey W.
MacQueen, Phillip J.
Lucas, Phillip
Lissauer, Jack J.
Latham, David W.
Knutson, Heather
Kinemuchi, K.
Johnson, John A.
Jenkins, Jon M.
Isaacson, Howard
Howard, Andrew
Horch, Elliott
Holman, Matthew J.
Henze, Christopher E.
Haas, Michael R.
Gilliland, Ronald L.
Gautier, Thomas N., III
Ford, Eric B.
Fischer, Debra A.
Everett, Mark
Endl, Michael
Demory, Brice-Oliver
Deming, Drake
Charbonneau, David
Caldwell, Douglas
Buchhave, Lars
Brown, Timothy M.
Batalha, Natalie
TI KEPLER-18b, c, AND d: A SYSTEM OF THREE PLANETS CONFIRMED BY TRANSIT
TIMING VARIATIONS, LIGHT CURVE VALIDATION, WARM-SPITZER PHOTOMETRY, AND
RADIAL VELOCITY MEASUREMENTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planetary systems; stars: individual (Kepler-18, KIC 8644288, 2MASS
J19521906+4444467); techniques: photometric; techniques: spectroscopic
ID EXOPLANET HD 189733B; SOLAR-TYPE STARS; LOW-DENSITY; INITIAL
CHARACTERISTICS; TERRESTRIAL PLANETS; SECONDARY ECLIPSE;
SPACE-TELESCOPE; BLEND SCENARIOS; TARGET STARS; SUPER-EARTHS
AB We report the detection of three transiting planets around a Sun-like star, which we designate Kepler-18. The transit signals were detected in photometric data from the Kepler satellite, and were confirmed to arise from planets using a combination of large transit-timing variations (TTVs), radial velocity variations, Warm-Spitzer observations, and statistical analysis of false-positive probabilities. The Kepler-18 star has a mass of 0.97M(circle dot), a radius of 1.1R(circle dot), an effective temperature of 5345 K, and an iron abundance of [Fe/H] = +0.19. The planets have orbital periods of approximately 3.5, 7.6, and 14.9 days. The innermost planet "b" is a "super-Earth" with a mass of 6.9 +/- 3.4M(circle plus), a radius of 2.00 +/- 0.10R(circle plus), and a mean density of 4.9 +/- 2.4 g cm(3). The two outer planets "c" and "d" are both low-density Neptune-mass planets. Kepler-18c has a mass of 17.3 +/- 1.9 M-circle plus, a radius of 5.49 +/- 0.26R(circle plus), and a mean density of 0.59 +/- 0.07 g cm(3), while Kepler-18d has a mass of 16.4 +/- 1.4 M-circle plus, a radius of 6.98 +/- 0.33 R-circle plus and a mean density of 0.27 +/- 0.03 g cm(.)(3) Kepler-18c and Kepler-18d have orbital periods near a 2:1 mean-motion resonance, leading to large and readily detected TTVs.
C1 [Cochran, William D.; MacQueen, Phillip J.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Fabrycky, Daniel C.; Fortney, Jonathan J.; Miller, Neil] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Torres, Guillermo; Fressin, Francois; Desert, Jean-Michel; Ragozzine, Darin; Sasselov, Dimitar; Carter, Joshua A.; Quinn, Samuel N.; Latham, David W.; Holman, Matthew J.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brugamyer, Erik J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Winn, Joshua N.; Seager, Sara; Demory, Brice-Oliver] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Uddin, Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Tenenbaum, Peter; Mullally, F.; Jenkins, Jon M.; Caldwell, Douglas] ETI Inst, Mountain View, CA 94043 USA.
[Still, M.; Kinemuchi, K.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Marcy, Geoffrey W.; Knutson, Heather; Isaacson, Howard; Howard, Andrew] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Lucas, Phillip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Johnson, John A.] CALTECH, Dept Astron, Pasadena, CA 91109 USA.
[Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Buchhave, Lars] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
RP Cochran, WD (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
EM wdc@astro.as.utexas.edu; jdesert@cfa.harvard.edu; jwinn@mit.edu;
wfw@kublai.sdsu.edu; kamal.uddin@nasa.gov; Peter.Tenenbaum@nasa.gov;
martin.d.still@nasa.gov; seager@mit.edu; fergal.mullally@nasa.gov;
Karen.Kinemuchi@nasa.gov; johnjohn@astro.caltech.edu;
jjenkins@mail.arc.nasa.gov; horche2@southernct.edu; eford@astro.ufl.edu;
debra.fischer@gmail.com; Douglas.A.Caldwell@nasa.gov;
natalie.m.batalha@nasa.gov
RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell,
Douglas/L-7911-2014; Howard, Andrew/D-4148-2015
OI Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars
A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Demory,
Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X; Fischer,
Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183;
Caldwell, Douglas/0000-0003-1963-9616; Howard,
Andrew/0000-0001-8638-0320
FU NASA's Science Mission Directorate; NASA through JPL/Caltech; W. M. Keck
Foundation; NASA
FX Kepler was competitively selected as the tenth Discovery mission.
Funding for the Kepler Mission is provided by NASA's Science Mission
Directorate. We are deeply grateful for the very hard work of the entire
Kepler team. This research is based in part on observations made with
the Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was provided by NASA through an award issued
by JPL/Caltech. 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
Keck Observatory was made possible by the generous financial support of
the W. M. Keck Foundation.
NR 83
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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JI Astrophys. J. Suppl. Ser.
PD NOV
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400007
ER
PT J
AU Desert, JM
Charbonneau, D
Demory, BO
Ballard, S
Carter, JA
Fortney, JJ
Cochran, WD
Endl, M
Quinn, SN
Isaacson, HT
Fressin, F
Buchhave, LA
Latham, DW
Knutson, HA
Bryson, ST
Torres, G
Rowe, JF
Batalha, NM
Borucki, WJ
Brown, TM
Caldwell, DA
Christiansen, JL
Deming, D
Fabrycky, DC
Ford, EB
Gilliland, RL
Gillon, M
Haas, MR
Jenkins, JM
Kinemuchi, K
Koch, D
Lissauer, JJ
Lucas, P
Mullally, F
MacQueen, PJ
Marcy, GW
Sasselov, DD
Seager, S
Still, M
Tenenbaum, P
Uddin, K
Winn, JN
AF Desert, Jean-Michel
Charbonneau, David
Demory, Brice-Olivier
Ballard, Sarah
Carter, Joshua A.
Fortney, Jonathan J.
Cochran, William D.
Endl, Michael
Quinn, Samuel N.
Isaacson, Howard T.
Fressin, Francois
Buchhave, Lars A.
Latham, David W.
Knutson, Heather A.
Bryson, Stephen T.
Torres, Guillermo
Rowe, Jason F.
Batalha, Natalie M.
Borucki, William J.
Brown, Timothy M.
Caldwell, Douglas A.
Christiansen, Jessie L.
Deming, Drake
Fabrycky, Daniel C.
Ford, Eric B.
Gilliland, Ronald L.
Gillon, Michael
Haas, Michael R.
Jenkins, Jon M.
Kinemuchi, Karen
Koch, David
Lissauer, Jack J.
Lucas, Philip
Mullally, Fergal
MacQueen, Phillip J.
Marcy, Geoffrey W.
Sasselov, Dimitar D.
Seager, Sara
Still, Martin
Tenenbaum, Peter
Uddin, Kamal
Winn, Joshua N.
TI THE HOT-JUPITER KEPLER-17b: DISCOVERY, OBLIQUITY FROM STROBOSCOPIC
STARSPOTS, AND ATMOSPHERIC CHARACTERIZATION
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE eclipses; planetary systems; stars: individual (Kepler-17b, KIC
10619192, 2MASS 19533486+4748540); techniques: photometric
ID EXTRASOLAR GIANT PLANETS; TRANSIT LIGHT-CURVE; HOBBY-EBERLY TELESCOPE;
SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; INITIAL CHARACTERISTICS;
SECONDARY ECLIPSE; THERMAL EMISSION; STELLAR ACTIVITY; SPECTRAL MODELS
AB This paper reports the discovery and characterization of the transiting hot giant exoplanet Kepler-17b. The planet has an orbital period of 1.486 days, and radial velocity measurements from the Hobby-Eberly Telescope show a Doppler signal of 419.5(-15.6)(+13.3) m s(-1). From a transit-based estimate of the host star's mean density, combined with an estimate of the stellar effective temperature T-eff = 5630 +/- 100 from high-resolution spectra, we infer a stellar host mass of 1.06 +/- 0.07 M-circle dot and a stellar radius of 1.02 +/- 0.03 R-circle dot. We estimate the planet mass and radius to be M-P = 2.45 +/- 0.11 M-J and R-P = 1.31 +/- 0.02 R-J. The host star is active, with dark spots that are frequently occulted by the planet. The continuous monitoring of the star reveals a stellar rotation period of 11.89 days, eight times the planet's orbital period; this period ratio produces stroboscopic effects on the occulted starspots. The temporal pattern of these spot-crossing events shows that the planet's orbit is prograde and the star's obliquity is smaller than 15 degrees. We detected planetary occultations of Kepler-17b with both the Kepler and Spitzer Space Telescopes. We use these observations to constrain the eccentricity, e, and find that it is consistent with a circular orbit (e < 0.011). The brightness temperatures of the planet's infrared bandpasses are T-3.6 mu m = 1880 +/- 100 K and T-4.5 mu m = 1770 +/- 150 K. We measure the optical geometric albedo A(g) in the Kepler bandpass and find A(g) = 0.10 +/- 0.02. The observations are best described by atmospheric models for which most of the incident energy is re-radiated away from the day side.
C1 [Desert, Jean-Michel; Charbonneau, David; Ballard, Sarah; Carter, Joshua A.; Quinn, Samuel N.; Fressin, Francois; Latham, David W.; Torres, Guillermo; Lissauer, Jack J.; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Demory, Brice-Olivier; Seager, Sara; Winn, Joshua N.] MIT, Cambridge, MA 02159 USA.
[Fortney, Jonathan J.; Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Isaacson, Howard T.; Knutson, Heather A.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Caldwell, Douglas A.; Jenkins, Jon M.; Mullally, Fergal; Tenenbaum, Peter] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Kinemuchi, Karen; Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lucas, Philip] Univ Hertfordshire, Ctr Astrophyiscs Res, Hatfield AL10 9AB, Herts, England.
[Uddin, Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Desert, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jdesert@cfa.harvard.edu
RI Carter, Joshua/A-8280-2013; Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Fortney,
Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666;
Demory, Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA; NASA through JPL/Caltech; W. M. Keck Foundation
FX This work is also based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. Support
for this work was provided by NASA through an award issued by
JPL/Caltech.; 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 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2011
VL 197
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DI 10.1088/0067-0049/197/1/14
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400014
ER
PT J
AU Desert, JM
Charbonneau, D
Fortney, JJ
Madhusudhan, N
Knutson, HA
Fressin, F
Deming, D
Borucki, WJ
Brown, TM
Caldwell, D
Ford, EB
Gilliland, RL
Latham, DW
Marcy, GW
Seager, S
AF Desert, Jean-Michel
Charbonneau, David
Fortney, Jonathan J.
Madhusudhan, Nikku
Knutson, Heather A.
Fressin, Francois
Deming, Drake
Borucki, William J.
Brown, Timothy M.
Caldwell, Douglas
Ford, Eric B.
Gilliland, Ronald L.
Latham, David W.
Marcy, Geoffrey W.
Seager, Sara
CA Kepler Sci Team
TI THE ATMOSPHERES OF THE HOT-JUPITERS KEPLER-5b AND KEPLER-6b OBSERVED
DURING OCCULTATIONS WITH WARM-SPITZER AND KEPLER
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE eclipses; planetary systems; techniques: photometric
ID EXTRASOLAR GIANT PLANETS; GROUND-BASED DETECTION; INFRARED ARRAY CAMERA;
EXOPLANET HD 189733B; SECONDARY ECLIPSE; THERMAL EMISSION; LIGHT CURVES;
INITIAL CHARACTERISTICS; TEMPERATURE INVERSION; THEORETICAL SPECTRA
AB This paper reports the detection and the measurements of occultations of the two transiting hot giant exoplanets Kepler-5b and Kepler-6b by their parent stars. The observations are obtained in the near-infrared with Warm-Spitzer Space Telescope and at optical wavelengths by combining more than a year of Kepler photometry. The investigation consists of constraining the eccentricities of these systems and of obtaining broadband emergent photometric data for individual planets. For both targets, the occultations are detected at the 3 sigma level at each wavelength with midoccultation times consistent with circular orbits. The brightness temperatures of these planets are deduced from the infrared observations and reach T-Spitzer = 1930 +/- 100 K and T-Spitzer = 1660 +/- 120 K for Kepler-5b and Kepler-6b, respectively. We measure optical geometric albedos A(g) in the Kepler bandpass and find A(g) = 0.12 +/- 0.04 for Kepler-5b and A(g) = 0.11 +/- 0.04 for Kepler-6b, leading to upper an limit for the Bond albedo of A(B) <= 0.17 in both cases. The observations for both planets are best described by models for which most of the incident energy is redistributed on the dayside, with only less than 10% of the absorbed stellar flux redistributed to the nightside of these planets.
C1 [Desert, Jean-Michel; Charbonneau, David; Fressin, Francois; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Madhusudhan, Nikku] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Caldwell, Douglas] SETI Inst, Mountain View, CA 94043 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley Astron Dept, Berkeley, CA 94720 USA.
[Seager, Sara] MIT, Newton, MA 02159 USA.
RP Desert, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jdesert@cfa.harvard.edu
RI Kepler, S. O. /H-5901-2012; Caldwell, Douglas/L-7911-2014;
OI Kepler, S. O. /0000-0002-7470-5703; Caldwell,
Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354;
Charbonneau, David/0000-0002-9003-484X; /0000-0001-6545-639X
FU NASA; NASA through JPL/Caltech; NASA's Science Mission Directorate; W.
M. Keck Foundation
FX We would like to thank Jessie Christiansen, Brice-Olivier Demory, and
Pavel Machaleck for discussions about Kepler photometry, light curves
analysis, and interpretation. Thank you to the Spitzer staff at IPAC and
in particular to Nancy Silbermann for scheduling the observations of
this large program. We would like to thank Jacob Bean for a variety of
useful discussions. 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 would like to thank the many people who generously gave so much
their time to make this Mission a success. Some of the data presented
herein were obtained at the W. M. Keck Observatory, which is
oper-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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SC Astronomy & Astrophysics
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PT J
AU Endl, M
MacQueen, PJ
Cochran, WD
Brugamyer, EJ
Buchhave, LA
Rowe, J
Lucas, P
Isaacson, H
Bryson, S
Howell, SB
Fortney, JJ
Hansen, T
Borucki, WJ
Caldwell, D
Christiansen, JL
Ciardi, DR
Demory, BO
Everett, M
Ford, EB
Haas, MR
Holman, MJ
Horch, E
Jenkins, JM
Koch, DJ
Lissauer, JJ
Machalek, P
Still, M
Welsh, WF
Sanderfer, DT
Seader, SE
Smith, JC
Thompson, SE
Twicken, JD
AF Endl, Michael
MacQueen, Phillip J.
Cochran, William D.
Brugamyer, Erik J.
Buchhave, Lars A.
Rowe, Jason
Lucas, Phillip
Isaacson, Howard
Bryson, Steve
Howell, Steve B.
Fortney, Jonathan J.
Hansen, Terese
Borucki, William J.
Caldwell, Douglas
Christiansen, Jessie L.
Ciardi, David R.
Demory, Brice-Olivier
Everett, Mark
Ford, Eric B.
Haas, Michael R.
Holman, Matthew J.
Horch, Elliott
Jenkins, Jon M.
Koch, David J.
Lissauer, Jack J.
Machalek, Pavel
Still, Martin
Welsh, William F.
Sanderfer, Dwight T.
Seader, Shawn E.
Smith, Jeffrey C.
Thompson, Susan E.
Twicken, Joseph D.
TI KEPLER-15b: A HOT JUPITER ENRICHED IN HEAVY ELEMENTS AND THE FIRST
KEPLER MISSION PLANET CONFIRMED WITH THE HOBBY-EBERLY TELESCOPE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planetary systems; stars: individual (Kepler-15, KOI-128, KIC 11359879,
2MASS J19444814+4908244); techniques: image processing; techniques:
photometric; techniques: radial velocities; techniques: spectroscopic
ID TRANSITING-PLANET; LIGHT CURVES; SPACED DATA; STARS; SPECTROMETER;
PERFORMANCE; EVOLUTION; DISCOVERY; PROGRAM; SCIENCE
AB We report the discovery of Kepler-15b (KOI-128), a new transiting exoplanet detected by NASA's Kepler mission. The transit signal with a period of 4.94 days was detected in the quarter 1 (Q1) Kepler photometry. For the first time, we have used the High Resolution Spectrograph (HRS) at the Hobby-Eberly Telescope (HET) to determine the mass of a Kepler planet via precise radial velocity (RV) measurements. The 24 HET/HRS RVs and 6 additional measurements from the Fibre-fed Echelle Spectrograph spectrograph at the Nordic Optical Telescope reveal a Doppler signal with the same period and phase as the transit ephemeris. We used one HET/HRS spectrum of Kepler-15 taken without the iodine cell to determine accurate stellar parameters. The host star is a metal-rich ([Fe/H] = 0.36 +/- 0.07) G-type main-sequence star with T-eff = 5515 +/- 124 K. The semi-amplitude K of the RV orbit is 78.7(-9.5)(+ 8.5) m s(-1), which yields a planet mass of 0.66 +/- 0.1 M-Jup. The planet has a radius of 0.96 +/- 0.06 R-Jup and a mean bulk density of 0.9 +/- 0.2 g cm(-3). The radius of Kepler-15b is smaller than the majority of transiting planets with similar mass and irradiation level. This suggests that the planet is more enriched in heavy elements than most other transiting giant planets. For Kepler-15b we estimate a heavy element mass of 30-40 M-circle plus.
C1 [Endl, Michael; MacQueen, Phillip J.; Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Brugamyer, Erik J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, Denmark Ctr Star & Planet Format, DK-1168 Copenhagen, Denmark.
[Lucas, Phillip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Demory, Brice-Olivier] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA.
[Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Jenkins, Jon M.; Sanderfer, Dwight T.; Seader, Shawn E.; Smith, Jeffrey C.; Thompson, Susan E.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Machalek, Pavel] SETI Inst, Mountain View, CA 94043 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP Endl, M (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
RI Caldwell, Douglas/L-7911-2014;
OI Demory, Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X;
Caldwell, Douglas/0000-0003-1963-9616; Fortney,
Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666;
Ciardi, David/0000-0002-5741-3047
FU NASA's Science Mission Directorate
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. We thank the hundreds of people who make this mission
successful. The Hobby-Eberly Telescope (HET) is a joint project of the
University of Texas at Austin, the Pennsylvania State University,
Stanford University, Ludwig-Maximilians-Universitat Munchen, and
Georg-August-Universitat at Gottingen. The HET is named in honor of its
principal benefactors, William P. Hobby and Robert E. Eberly. Based in
part on observations made with 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. We also thank the anonymous
referee for many helpful suggestions to improve the manuscript.
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PD NOV
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400013
ER
PT J
AU Ford, EB
Rowe, JF
Fabrycky, DC
Carter, JA
Holman, MJ
Lissauer, JJ
Ragozzine, D
Steffen, JH
Batalha, NM
Borucki, WJ
Bryson, S
Caldwell, DA
Dunham, EW
Gautier, TN
Jenkins, JM
Koch, DG
Li, J
Lucas, P
Marcy, GW
McCauliff, S
Mullally, FR
Quintana, E
Still, M
Tenenbaum, P
Thompson, SE
Twicken, JD
AF Ford, Eric B.
Rowe, Jason F.
Fabrycky, Daniel C.
Carter, Joshua A.
Holman, Matthew J.
Lissauer, Jack J.
Ragozzine, Darin
Steffen, Jason H.
Batalha, Natalie M.
Borucki, William J.
Bryson, Steve
Caldwell, Douglas A.
Dunham, Edward W.
Gautier, Thomas N., III
Jenkins, Jon M.
Koch, David G.
Li, Jie
Lucas, Philip
Marcy, Geoffrey W.
McCauliff, Sean
Mullally, Fergal R.
Quintana, Elisa
Still, Martin
Tenenbaum, Peter
Thompson, Susan E.
Twicken, Joseph D.
TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. I. STATISTICAL ANALYSIS OF THE
FIRST FOUR MONTHS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE methods: statistical; planetary systems; planets and satellites:
detection; planets and satellites: dynamical evolution and stability;
techniques: miscellaneous
ID EXTRASOLAR PLANETS; LIGHT CURVES; LOW-MASS; CANDIDATES; SYSTEM;
DETECTABILITY; EXOMOONS; DENSITY; TRIPLE; STARS
AB The architectures of multiple planet systems can provide valuable constraints on models of planet formation, including orbital migration, and excitation of orbital eccentricities and inclinations. NASA's Kepler mission has identified 1235 transiting planet candidates. The method of transit timing variations (TTVs) has already confirmed seven planets in two planetary systems. We perform a transit timing analysis of the Kepler planet candidates. We find that at least similar to 11% of planet candidates currently suitable for TTV analysis show evidence suggestive of TTVs, representing at least similar to 65 TTV candidates. In all cases, the time span of observations must increase for TTVs to provide strong constraints on planet masses and/or orbits, as expected based on N-body integrations of multiple transiting planet candidate systems (assuming circular and coplanar orbits). We find the fraction of planet candidates showing TTVs in this data set does not vary significantly with the number of transiting planet candidates per star, suggesting significant mutual inclinations and that many stars with a single transiting planet should host additional non-transiting planets. We anticipate that Kepler could confirm (or reject) at least similar to 12 systems with multiple transiting planet candidates via TTVs. Thus, TTVs will provide a powerful tool for confirming transiting planets and characterizing the orbital dynamics of low-mass planets. If Kepler observations were extended to at least seven years, then TTVs would provide much more precise constraints on the dynamics of systems with multiple transiting planets and would become sensitive to planets with orbital periods extending into the habitable zone of solar-type stars.
C1 [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA.
[Rowe, Jason F.; Caldwell, Douglas A.; Jenkins, Jon M.; Li, Jie; Mullally, Fergal R.; Quintana, Elisa; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.] SETI Inst, Mountain View, CA 94043 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Carter, Joshua A.; Holman, Matthew J.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[McCauliff, Sean] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ford, EB (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32111 USA.
EM eford@astro.ufl.edu
RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell,
Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; /0000-0001-6545-639X; Fabrycky,
Daniel/0000-0003-3750-0183
FU National Aeronautics and Space Administration [NNX08AR04G,
HF-51272.01-A, HF-51267.01-A, NAS 5-26555]; National Science Foundation
[0707203]; Space Telescope Science Institute
FX Funding for this mission is provided by NASA's Science Mission
Directorate. We thank the entire Kepler team for the many years of work
that is proving so successful. We thank David Latham for a careful
reading of the manuscript. E.B.F. acknowledges support by the National
Aeronautics and Space Administration under grant NNX08AR04G issued
through the Kepler Participating Scientist Program. This material is
based upon work supported by the National Science Foundation under Grant
No. 0707203. D.C.F. and J.A.C. acknowledge support for this work was
provided by NASA through Hubble Fellowship grants HF-51272.01-A and
HF-51267.01-A awarded by the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Inc., for NASA, under contract NAS 5-26555.
NR 35
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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 NOV
PY 2011
VL 197
IS 1
AR 2
DI 10.1088/0067-0049/197/1/2
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400002
ER
PT J
AU Fortney, JJ
Demory, BO
Desert, JM
Rowe, J
Marcy, GW
Isaacson, H
Buchhave, LA
Ciardi, D
Gautier, TN
Batalha, NM
Caldwell, DA
Bryson, ST
Nutzman, P
Jenkins, JM
Howard, A
Charbonneau, D
Knutson, HA
Howell, SB
Everett, M
Fressin, F
Deming, D
Borucki, WJ
Brown, TM
Ford, EB
Gilliland, RL
Latham, DW
Miller, N
Seager, S
Fischer, DA
Koch, D
Lissauer, JJ
Haas, MR
Still, M
Lucas, P
Gillon, M
Christiansen, JL
Geary, JC
AF Fortney, Jonathan J.
Demory, Brice-Olivier
Desert, Jean-Michel
Rowe, Jason
Marcy, Geoffrey W.
Isaacson, Howard
Buchhave, Lars A.
Ciardi, David
Gautier, Thomas N.
Batalha, Natalie M.
Caldwell, Douglas A.
Bryson, Stephen T.
Nutzman, Philip
Jenkins, Jon M.
Howard, Andrew
Charbonneau, David
Knutson, Heather A.
Howell, Steve B.
Everett, Mark
Fressin, Francois
Deming, Drake
Borucki, William J.
Brown, Timothy M.
Ford, Eric B.
Gilliland, Ronald L.
Latham, David W.
Miller, Neil
Seager, Sara
Fischer, Debra A.
Koch, David
Lissauer, Jack J.
Haas, Michael R.
Still, Martin
Lucas, Philip
Gillon, Michael
Christiansen, Jessie L.
Geary, John C.
TI DISCOVERY AND ATMOSPHERIC CHARACTERIZATION OF GIANT PLANET KEPLER-12b:
AN INFLATED RADIUS OUTLIER
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planets and satellites: atmospheres; stars: individual (Kepler-12,
KOI-20, KIC 11804465); techniques: spectroscopic
ID TRANSITING EXTRASOLAR PLANETS; SPITZER-SPACE-TELESCOPE; EXOPLANET HD
189733B; LIGHT-CURVE PROJECT; B-LIKE PLANETS; HOT JUPITERS; LOW-DENSITY;
INITIAL CHARACTERISTICS; SECONDARY ECLIPSE; THERMAL STRUCTURE
AB We report the discovery of planet Kepler-12b (KOI-20), which at 1.695 +/- 0.030 R-J is among the handful of planets with super-inflated radii above 1.65 R-J. Orbiting its slightly evolved G0 host with a 4.438 day period, this 0.431 +/- 0.041 M-J planet is the least irradiated within this largest-planet-radius group, which has important implications for planetary physics. The planet's inflated radius and low mass lead to a very low density of 0.111 +/- 0.010 g cm(-3). We detect the occultation of the planet at a significance of 3.7 sigma in the Kepler bandpass. This yields a geometric albedo of 0.14 +/- 0.04; the planetary flux is due to a combination of scattered light and emitted thermal flux. We use multiple observations with Warm Spitzer to detect the occultation at 7 sigma and 4 sigma in the 3.6 and 4.5 mu m bandpasses, respectively. The occultation photometry timing is consistent with a circular orbit at e < 0.01 (1s) and e < 0.09 (3 sigma). The occultation detections across the three bands favor an atmospheric model with no dayside temperature inversion. The Kepler occultation detection provides significant leverage, but conclusions regarding temperature structure are preliminary, given our ignorance of opacity sources at optical wavelengths in hot Jupiter atmospheres. If Kepler-12b and HD 209458b, which intercept similar incident stellar fluxes, have the same heavy-element masses, the interior energy source needed to explain the large radius of Kepler-12b is three times larger than that of HD 209458b. This may suggest that more than one radius-inflation mechanism is at work for Kepler-12b or that it is less heavy-element rich than other transiting planets.
C1 [Fortney, Jonathan J.; Nutzman, Philip; Miller, Neil] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Demory, Brice-Olivier; Seager, Sara] MIT, Cambridge, MA 02139 USA.
[Desert, Jean-Michel; Buchhave, Lars A.; Charbonneau, David; Fressin, Francois; Latham, David W.; Geary, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rowe, Jason; Caldwell, Douglas A.; Jenkins, Jon M.; Christiansen, Jessie L.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Marcy, Geoffrey W.; Isaacson, Howard; Howard, Andrew; Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Ciardi, David] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Gautier, Thomas N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Gillon, Michael] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland.
RP Fortney, JJ (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM jfortney@ucolick.org
RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015;
OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars
A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Demory,
Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X; Fischer,
Debra/0000-0003-2221-0861; Howard, Andrew/0000-0001-8638-0320; Fortney,
Jonathan/0000-0002-9843-4354
FU NASA [NNX09AC22G]; NASA's Science Mission Directorate; NASA through
JPL/Caltech
FX J.J.F. acknowledges the support of the Kepler Participating Scientist's
program via NASA grant NNX09AC22G. Kepler was competitively selected as
the tenth Discovery mission. Funding for the Kepler mission is provided
by NASA's Science Mission Directorate. We thank the many people who gave
so generously of their time to make the Kepler mission a success. We
thank Carly Chubak for cross-correlation analyses of the Keck spectra
for companions. This work incorporates 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. Finally, the authors extend special thanks to those of
Hawaiian ancestry on whose sacred mountain of Mauna Kea we are
privileged to be guests. Without their generous hospitality, the Keck
observations presented herein would not have been possible.
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J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2011
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DI 10.1088/0067-0049/197/1/9
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400009
ER
PT J
AU Fressin, F
Torres, G
Desert, JM
Charbonneau, D
Batalha, NM
Fortney, JJ
Rowe, JF
Allen, C
Borucki, WJ
Brown, TM
Bryson, ST
Ciardi, DR
Cochran, WD
Deming, D
Dunham, EW
Fabrycky, DC
Gautier, TN
Gilliland, RL
Henze, CE
Holman, MJ
Howell, SB
Jenkins, JM
Kinemuchi, K
Knutson, H
Koch, DG
Latham, DW
Lissauer, JJ
Marcy, GW
Ragozzine, D
Sasselov, DD
Still, M
Tenenbaum, P
Uddin, K
AF Fressin, Francois
Torres, Guillermo
Desert, Jean-Michel
Charbonneau, David
Batalha, Natalie M.
Fortney, Jonathan J.
Rowe, Jason F.
Allen, Christopher
Borucki, William J.
Brown, Timothy M.
Bryson, Stephen T.
Ciardi, David R.
Cochran, William D.
Deming, Drake
Dunham, Edward W.
Fabrycky, Daniel C.
Gautier, Thomas N., III
Gilliland, Ronald L.
Henze, Christopher E.
Holman, Matthew J.
Howell, Steve B.
Jenkins, Jon M.
Kinemuchi, Karen
Knutson, Heather
Koch, David G.
Latham, David W.
Lissauer, Jack J.
Marcy, Geoffrey W.
Ragozzine, Darin
Sasselov, Dimitar D.
Still, Martin
Tenenbaum, Peter
Uddin, Kamal
TI KEPLER-10 c: A 2.2 EARTH RADIUS TRANSITING PLANET IN A MULTIPLE SYSTEM
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: eclipsing; planetary systems; stars: individual (Kepler-10,
KOI-072, KIC 11904151); stars: statistics
ID SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; LOW-MASS; OBSERVATIONAL
EVIDENCE; SECONDARY ECLIPSE; BLEND SCENARIOS; LIGHT CURVES; WARM
SPITZER; CANDIDATES; ATMOSPHERE
AB The Kepler mission has recently announced the discovery of Kepler-10 b, the smallest exoplanet discovered to date and the first rocky planet found by the spacecraft. A second, 45 day period transit-like signal present in the photometry from the first eight months of data could not be confirmed as being caused by a planet at the time of that announcement. Here we apply the light curve modeling technique known as BLENDER to explore the possibility that the signal might be due to an astrophysical false positive (blend). To aid in this analysis we report the observation of two transits with the Spitzer Space Telescope at 4.5 mu m. When combined, they yield a transit depth of 344 +/- 85 ppm that is consistent with the depth in the Kepler passband (376 +/- 9 ppm, ignoring limb darkening), which rules out blends with an eclipsing binary of a significantly different color than the target. Using these observations along with other constraints from high-resolution imaging and spectroscopy, we are able to exclude the vast majority of possible false positives. We assess the likelihood of the remaining blends, and arrive conservatively at a false alarm rate of 1.6 x 10(-5) that is small enough to validate the candidate as a planet (designated Kepler-10 c) with a very high level of confidence. The radius of this object is measured to be R-p = 2.227(-0.057)(+ 0.052) R-circle plus (in which the error includes the uncertainty in the stellar properties), but currently available radial-velocity measurements only place an upper limit on its mass of about 20 M-circle plus. Kepler-10 c represents another example (with Kepler-9 d and Kepler-11 g) of statistical "validation" of a transiting exoplanet, as opposed to the usual "confirmation" that can take place when the Doppler signal is detected or transit timing variations are measured. It is anticipated that many of Kepler's smaller candidates will receive a similar treatment since dynamical confirmation may be difficult or impractical with the sensitivity of current instrumentation.
C1 [Fressin, Francois; Torres, Guillermo; Desert, Jean-Michel; Charbonneau, David; Holman, Matthew J.; Latham, David W.; Ragozzine, Darin; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
[Fortney, Jonathan J.; Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Allen, Christopher; Tenenbaum, Peter; Uddin, Kamal] Uddin Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Ciardi, David R.; Koch, David G.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Jenkins, Jon M.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kinemuchi, Karen; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
[Knutson, Heather; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ffressin@cfa.harvard.edu
RI Ragozzine, Darin/C-4926-2013;
OI Fortney, Jonathan/0000-0002-9843-4354; Ciardi,
David/0000-0002-5741-3047; Charbonneau, David/0000-0002-9003-484X;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA through JPL/Caltech; NASA
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. This research has made use of the facilities at the NASA
Advanced Supercomputing Division (NASA Ames Research Center), and is
based also 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. We thank
Mukremin Kilic and Rosanne Di Stefano for helpful discussions about
white dwarfs, and the anonymous referee for constructive comments.
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JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2011
VL 197
IS 1
AR 5
DI 10.1088/0067-0049/197/1/5
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400005
ER
PT J
AU Lissauer, JJ
Ragozzine, D
Fabrycky, DC
Steffen, JH
Ford, EB
Jenkins, JM
Shporer, A
Holman, MJ
Rowe, JF
Quintana, EV
Batalha, NM
Borucki, WJ
Bryson, ST
Caldwell, DA
Carter, JA
Ciardi, D
Dunham, EW
Fortney, JJ
Gautier, TN
Howell, SB
Koch, DG
Latham, DW
Marcy, GW
Morehead, RC
Sasselov, D
AF Lissauer, Jack J.
Ragozzine, Darin
Fabrycky, Daniel C.
Steffen, Jason H.
Ford, Eric B.
Jenkins, Jon M.
Shporer, Avi
Holman, Matthew J.
Rowe, Jason F.
Quintana, Elisa V.
Batalha, Natalie M.
Borucki, William J.
Bryson, Stephen T.
Caldwell, Douglas A.
Carter, Joshua A.
Ciardi, David
Dunham, Edward W.
Fortney, Jonathan J.
Gautier, Thomas N., III
Howell, Steve B.
Koch, David G.
Latham, David W.
Marcy, Geoffrey W.
Morehead, Robert C.
Sasselov, Dimitar
TI ARCHITECTURE AND DYNAMICS OF KEPLER'S CANDIDATE MULTIPLE TRANSITING
PLANET SYSTEMS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE celestial mechanics; planets and satellites: dynamical evolution and
stability; planets and satellites: fundamental parameters; planets and
satellites: general; planetary systems
ID HOT SUPER-EARTHS; 1ST 4 MONTHS; EXTRASOLAR PLANETS; ORBITAL
ECCENTRICITIES; SOLAR-SYSTEM; HARPS SEARCH; LIGHT CURVES; SHORT-PERIOD;
LOW-MASS; RESONANCES
AB About one-third of the similar to 1200 transiting planet candidates detected in the first four months of Kepler data are members of multiple candidate systems. There are 115 target stars with two candidate transiting planets, 45 with three, 8 with four, and 1 each with five and six. We characterize the dynamical properties of these candidate multi-planet systems. The distribution of observed period ratios shows that the vast majority of candidate pairs are neither in nor near low-order mean-motion resonances. Nonetheless, there are small but statistically significant excesses of candidate pairs both in resonance and spaced slightly too far apart to be in resonance, particularly near the 2:1 resonance. We find that virtually all candidate systems are stable, as tested by numerical integrations that assume a nominal mass-radius relationship. Several considerations strongly suggest that the vast majority of these multi-candidate systems are true planetary systems. Using the observed multiplicity frequencies, we find that a single population of planetary systems that matches the higher multiplicities underpredicts the number of singly transiting systems. We provide constraints on the true multiplicity and mutual inclination distribution of the multi-candidate systems, revealing a population of systems with multiple super-Earth-size and Neptune-size planets with low to moderate mutual inclinations.
C1 [Lissauer, Jack J.; Jenkins, Jon M.; Rowe, Jason F.; Quintana, Elisa V.; Caldwell, Douglas A.; Morehead, Robert C.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ragozzine, Darin; Holman, Matthew J.; Carter, Joshua A.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabrycky, Daniel C.; Fortney, Jonathan J.; Latham, David W.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Ford, Eric B.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Ciardi, David] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Lissauer, JJ (reprint author), NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM Jack.Lissauer@nasa.gov
RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell,
Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Fortney,
Jonathan/0000-0002-9843-4354; Ciardi, David/0000-0002-5741-3047;
/0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [HF-51272.01-A, HF-51267.01-A];
STScI [NAS 5-26555]
FX Kepler was competitively selected as NASA's tenth Discovery mission.
Funding for this mission is provided by NASA's Science Mission
Directorate. The authors thank the many people who gave so generously of
their time to make the Kepler mission a success. D.C.F. and J.A.C.
acknowledge NASA support through Hubble Fellowship grants HF-51272.01-A
and HF-51267.01-A, respectively, awarded by STScI, operated by AURA
under contract NAS 5-26555. We thank Bill Cochran, Avi Loeb, Hanno Rein,
Subo Dong, and Bill Welsh for valuable discussions and Kevin Zahnle, Tom
Greene, Andrew Youdin, and an anonymous reviewer for constructive
comments on the manuscript. Numerical integrations to test the stability
of nominal planetary systems were run on the supercomputer Pleiades at
University of California, Santa Cruz.
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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 NOV
PY 2011
VL 197
IS 1
AR 8
DI 10.1088/0067-0049/197/1/8
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400008
ER
PT J
AU Moorhead, AV
Ford, EB
Morehead, RC
Rowe, J
Borucki, WJ
Batalha, NM
Bryson, ST
Caldwell, DA
Fabrycky, DC
Gautier, TN
Koch, DG
Holman, MJ
Jenkins, J
Li, J
Lissauer, JJ
Lucas, P
Marcy, GW
Quinn, SN
Quintana, E
Ragozzine, D
Shporer, A
Still, M
Torres, G
AF Moorhead, Althea V.
Ford, Eric B.
Morehead, Robert C.
Rowe, Jason
Borucki, William J.
Batalha, Natalie M.
Bryson, Stephen T.
Caldwell, Douglas A.
Fabrycky, Daniel C.
Gautier, Thomas N., III
Koch, David G.
Holman, Matthew J.
Jenkins, Jonm.
Li, Jie
Lissauer, Jack J.
Lucas, Philip
Marcy, Geoffrey W.
Quinn, Samuel N.
Quintana, Elisa
Ragozzine, Darin
Shporer, Avi
Still, Martin
Torres, Guillermo
TI THE DISTRIBUTION OF TRANSIT DURATIONS FOR KEPLER PLANET CANDIDATES AND
IMPLICATIONS FOR THEIR ORBITAL ECCENTRICITIES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE planets and satellites: fundamental parameters
ID 1ST 4 MONTHS; EXTRASOLAR PLANETS; LIGHT CURVES; TIMING VARIATIONS; HOT
JUPITERS; SUPER-EARTHS; BINARY; SCATTERING; SYSTEMS; STARS
AB Doppler planet searches have discovered that giant planets follow orbits with a wide range of orbital eccentricities, revolutionizing theories of planet formation. The discovery of hundreds of exoplanet candidates by NASA's Kepler mission enables astronomers to characterize the eccentricity distribution of small exoplanets. Measuring the eccentricity of individual planets is only practical in favorable cases that are amenable to complementary techniques (e.g., radial velocities, transit timing variations, occultation photometry). Yet even in the absence of individual eccentricities, it is possible to study the distribution of eccentricities based on the distribution of transit durations (relative to the maximum transit duration for a circular orbit). We analyze the transit duration distribution of Kepler planet candidates. We find that for host stars with T-eff > 5100K we cannot invert this to infer the eccentricity distribution at this time due to uncertainties and possible systematics in the host star densities. With this limitation in mind, we compare the observed transit duration distribution with models to rule out extreme distributions. If we assume a Rayleigh eccentricity distribution for Kepler planet candidates, then we find best fits with a mean eccentricity of 0.1-0.25 for host stars with T-eff <= 5100 K. We compare the transit duration distribution for different subsets of Kepler planet candidates and discuss tentative trends with planetary radius and multiplicity. High-precision spectroscopic follow-up observations for a large sample of host stars will be required to confirm which trends are real and which are the results of systematic errors in stellar radii. Finally, we identify planet candidates that must be eccentric or have a significantly underestimated stellar radius.
C1 [Moorhead, Althea V.; Ford, Eric B.; Morehead, Robert C.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
[Rowe, Jason; Caldwell, Douglas A.; Jenkins, Jonm.; Li, Jie; Quintana, Elisa] SETI Inst, Mountain View, CA 94043 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Holman, Matthew J.; Quinn, Samuel N.; Ragozzine, Darin; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Marcy, Geoffrey W.; Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Shporer, Avi] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Moorhead, AV (reprint author), Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA.
EM altheam@astro.ufl.edu
RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; /0000-0001-6545-639X; Fabrycky,
Daniel/0000-0003-3750-0183
FU National Aeronautics and Space Administration [NNX08AR04G]; NASA's
Science Mission Directorate
FX We thank Bill Cochran, Dave Latham, and Tim Brown for their many helpful
suggestions and the latter two for their assistance with the Kepler
Input Catalog, on which this work relies. We thank the entire Kepler
team for the many years of work that is proving so successful. This
material is based on work supported by the National Aeronautics and
Space Administration under grant NNX08AR04G issued through the Kepler
Participating Scientist Program. Funding for this mission is provided by
NASA's Science Mission Directorate.
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J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2011
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DI 10.1088/0067-0049/197/1/1
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400001
ER
PT J
AU Welsh, WF
Orosz, JA
Aerts, C
Brown, TM
Brugamyer, E
Cochran, WD
Gilliland, RL
Guzik, JA
Kurtz, DW
Latham, DW
Marcy, GW
Quinn, SN
Zima, W
Allen, C
Batalha, NM
Bryson, S
Buchhave, LA
Caldwell, DA
Gautier, TN
Howell, SB
Kinemuchi, K
Ibrahim, KA
Isaacson, H
Jenkins, JM
Prsa, A
Still, M
Street, R
Wohler, B
Koch, DG
Borucki, WJ
AF Welsh, William F.
Orosz, Jerome A.
Aerts, Conny
Brown, Timothy M.
Brugamyer, Erik
Cochran, William D.
Gilliland, Ronald L.
Guzik, Joyce Ann
Kurtz, D. W.
Latham, David W.
Marcy, Geoffrey W.
Quinn, Samuel N.
Zima, Wolfgang
Allen, Christopher
Batalha, Natalie M.
Bryson, Steve
Buchhave, Lars A.
Caldwell, Douglas A.
Gautier, Thomas N., III
Howell, Steve B.
Kinemuchi, K.
Ibrahim, Khadeejah A.
Isaacson, Howard
Jenkins, Jon M.
Prsa, Andrej
Still, Martin
Street, Rachel
Wohler, Bill
Koch, David G.
Borucki, William J.
TI KOI-54: THE KEPLER DISCOVERY OF TIDALLY EXCITED PULSATIONS AND
BRIGHTENINGS IN A HIGHLY ECCENTRIC BINARY
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: close; binaries: spectroscopic; stars: individual (KID
8112039, HD 187091, 2MASS J19461553+4356513); stars: oscillations;
stars: variables: general
ID CLOSE BINARIES; INITIAL CHARACTERISTICS; SPECTROSCOPIC BINARIES; ORBITAL
PARAMETERS; CADENCE DATA; STELLAR; SYSTEMS; EVOLUTION; OPACITIES;
SCIENCE
AB Kepler observations of the star HD 187091 (KIC 8112039, hereafter KOI-54) revealed a remarkable light curve exhibiting sharp periodic brightening events every 41.8 days with a superimposed set of oscillations forming a beating pattern in phase with the brightenings. Spectroscopic observations revealed that this is a binary star with a highly eccentric orbit, e = 0.83. We are able to match the Kepler light curve and radial velocities with a nearly face-on (i = 5 degrees.5) binary star model in which the brightening events are caused by tidal distortion and irradiation of nearly identical A stars during their close periastron passage. The two dominant oscillations in the light curve, responsible for the beating pattern, have frequencies that are the 91st and 90th harmonic of the orbital frequency. The power spectrum of the light curve, after removing the binary star brightening component, reveals a large number of pulsations, 30 of which have a signal-to-noise ratio greater than or similar to 7. Nearly all of these pulsations have frequencies that are either integer multiples of the orbital frequency or are tidally split multiples of the orbital frequency. This pattern of frequencies unambiguously establishes the pulsations as resonances between the dynamic tides at periastron and the free oscillation modes of one or both of the stars. KOI-54 is only the fourth star to show such a phenomenon and is by far the richest in terms of excited modes.
C1 [Welsh, William F.; Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Aerts, Conny; Zima, Wolfgang] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Aerts, Conny; Zima, Wolfgang] Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Brown, Timothy M.; Street, Rachel] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Brown, Timothy M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Brugamyer, Erik; Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Brugamyer, Erik; Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Guzik, Joyce Ann] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England.
[Latham, David W.; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Allen, Christopher; Ibrahim, Khadeejah A.; Wohler, Bill] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
[Caldwell, Douglas A.; Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kinemuchi, K.; Still, Martin] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
RP Welsh, WF (reprint author), San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
EM wfw@sciences.sdsu.edu
RI Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars
A./0000-0003-1605-5666
FU NASA, Science Mission Directorate; NASA [NNX08AR14G]; European Research
Council under the European Community [227224]; W.M. Keck Foundation
FX Kepler was selected as the 10th mission of the Discovery Program.
Funding for this mission is provided by NASA, Science Mission
Directorate. The authors acknowledge support from the Kepler
Participating Scientists Program via NASA grant NNX08AR14G. C.A. and
W.Z. received funding from the European Research Council under the
European Community's Seventh Framework Programme (FP7/2007-2013)/ERC
grant agreement No. 227224 (PROSPERITY). 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. We thank Gur Windmiller
for general assistance and for a careful reading of this manuscript. We
especially thank the many members of the Kepler team whose hard work
made these observation possible. Finally, we thank the anonymous referee
for a thorough review of this paper.
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EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD NOV
PY 2011
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PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 846BO
UT WOS:000296872400004
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PT J
AU Beckman, NG
Muller-Landau, HC
AF Beckman, Noelle G.
Muller-Landau, Helene C.
TI Linking fruit traits to variation in predispersal vertebrate seed
predation, insect seed predation, and pathogen attack
SO ECOLOGY
LA English
DT Article
DE fruit development; fruit morphology; germination; Janzen-Connell
effects; natural enemies; Panama; plant traits; predispersal seed
mortality; seed survival
ID MOIST TROPICAL FOREST; DISPERSAL; PLANT; SIZE; TREE; GERMINATION;
DIVERSITY; HERBIVORY; DEFENSE; DISEASE
AB The importance of vertebrates, invertebrates, and pathogens for plant communities has long been recognized, but their absolute and relative importance in early recruitment of multiple coexisting tropical plant species has not been quantified. Further, little is known about the relationship of fruit traits to seed mortality due to natural enemies in tropical plants. To investigate the influences of vertebrates, invertebrates, and pathogens on reproduction of seven canopy plant species varying in fruit traits, we quantified reductions in fruit development and seed germination due to vertebrates, invertebrates, and fungal pathogens through experimental removal of these enemies using canopy exclosures, insecticide, and fungicide, respectively. We also measured morphological fruit traits hypothesized to mediate interactions of plants with natural enemies of seeds. Vertebrates, invertebrates, and fungi differentially affected predispersal seed mortality depending on the plant species. Fruit morphology explained some variation among species; species with larger fruit and less physical protection surrounding seeds exhibited greater negative effects of fungi on fruit development and germination and experienced reduced seed survival integrated over fruit development and germination in response to vertebrates. Within species, variation in seed size also contributed to variation in natural enemy effects on seed viability. Further, seedling growth was higher for seeds that developed in vertebrate exclosures for Anacardium excelsum and under the fungicide treatment for Castilla elastica, suggesting that predispersal effects of natural enemies may carry through to the seedling stage. This is the first experimental test of the relative effects of vertebrates, invertebrates, and pathogens on seed survival in the canopy. This study motivates further investigation to determine the generality of our results for plant communities. If there is strong variation in natural enemy attack among species related to differences in fruit morphology, then quantification of fruit traits will aid in predicting the outcomes of interactions between plants and their natural enemies. This is particularly important in tropical forests, where high species diversity makes it logistically impossible to study every plant life history stage of every species.
C1 [Beckman, Noelle G.; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Unit 9100, Dpo, AA 34002 USA.
[Beckman, Noelle G.] Univ Minnesota Twin Cities, St Paul, MN 55108 USA.
RP Beckman, NG (reprint author), Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA.
EM nbeckman2@unl.edu
RI Beckman, Noelle/E-5554-2011
OI Beckman, Noelle/0000-0001-5822-0610
FU National Science Foundation; University of Minnesota Graduate School;
University of Minnesota Department of Ecology, Evolution and Behavior;
Smithsonian Tropical Research Institute; Bell Museum of Natural History;
HSBC
FX We thank Jim Dalling, Linda Kinkel, Claudia Neuhauser, David Tilman,
Sunshine Van Bael, Marta Vargas, Sandford Weisberg, and S. J. Wright for
invaluable advice. We thank Rebeca Acosta, Matt Certo, Sophia
Christoforides, Amy Dickson, Reina Heinz, Bernardo Lopez, Christopher
Moore, and Serica Zwack for field and laboratory assistance. The
Smithsonian Tropical Research Institute provided logistical support. We
are grateful for the financial support of the National Science
Foundation (Graduate Research Fellowship to N. G. Beckman), the
University of Minnesota Graduate School (Doctoral Dissertation
Fellowship and International Research Grant to N. G. Beckman), the
University of Minnesota Department of Ecology, Evolution and Behavior
(Block Grant to N. G. Beckman), the Smithsonian Tropical Research
Institute (Supplementary Award to N. G. Beckman), the Bell Museum of
Natural History (Dayton Natural History Fund to N. G. Beckman), and the
HSBC Climate Partnership (H. C. Muller-Landau).
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PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 0012-9658
J9 ECOLOGY
JI Ecology
PD NOV
PY 2011
VL 92
IS 11
BP 2131
EP 2140
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 840GB
UT WOS:000296426000014
PM 22164837
ER
PT J
AU Wang, XG
Wiegand, T
Wolf, A
Howe, R
Davies, SJ
Hao, ZQ
AF Wang, Xugao
Wiegand, Thorsten
Wolf, Amy
Howe, Robert
Davies, Stuart J.
Hao, Zhanqing
TI Spatial patterns of tree species richness in two temperate forests
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE aggregation; Changbaishan; determinants of plant community diversity and
structure; habitat heterogeneity; Possion processes; temperate forest;
Thomas processes; Wabikon
ID AREA RELATIONSHIP; RAIN-FOREST; HABITAT ASSOCIATIONS; NORTHEASTERN
CHINA; TROPICAL FORESTS; POINT PATTERNS; BETA-DIVERSITY; SOIL CHEMISTRY;
NEUTRAL THEORY; DISTRIBUTIONS
AB 1. The relative contribution of external vs. internal clustering mechanisms for determining community structure and its manifestations has been the subject of a continuous debate, but few attempts have been made to examine their single and joint effects in a compound process model.
2. In this study, we tested four a priori hypotheses on the relative importance of habitat heterogeneity (topography and soil) and internal clustering mechanisms such as dispersal limitation on the species- area relationship (SAR) in two fully mapped 25-ha plots of temperate forests in the Changbaishan (CBS) Nature Reserve, China, and the Chequamegon-Nicolet National Forest in Wisconsin, USA.
3. We used the distance decay curve to test the generality of the results obtained for the SAR. To find out if the relative importance of internal and external clustering mechanisms changed with life stage, we conducted separate analyses for small, large and all trees.
4. Model selection favoured the most complex hypothesis that assumed an influence of both habitat heterogeneity and internal clustering on SAR and the distance decay curve. For the CBS plot, which shows weak topographical structuring, models were consistent with data only if soil factors were included into assessment of habitat heterogeneity. At the Wabikon plot, we could not test soil variables, but inclusion of topographical variables substantially improved the fit of the distance decay curve.
5. In general, the results of the SAR agreed with those of the distance decay curve, but the latter was sensitive to positive habitat-mediated species associations. The SAR, but not distance decay, distinguished among competing hypotheses for the community of large trees at CBS, where species exhibited only weak clustering.
6. Contrary to our expectations, we did not find substantial differences in the relative importance of internal and external clustering mechanisms with life stage.
7. Synthesis. Our analysis of spatial community structure for two relatively diverse temperate forests revealed that the factors governing spatial community structure may not substantially differ from those in highly diverse tropical forests. This result adds to our understanding of the ecological processes underlying the spatial diversity structure in natural forest communities.
C1 [Wang, Xugao; Hao, Zhanqing] Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110164, Peoples R China.
[Wiegand, Thorsten] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04301 Leipzig, Germany.
[Wolf, Amy; Howe, Robert] Univ Wisconsin, Dept Nat & Appl Sci, Green Bay, WI 54311 USA.
[Davies, Stuart J.] Harvard Univ, Ctr Trop Forest Sci, Boston, MA 02131 USA.
[Davies, Stuart J.] Smithsonian Trop Res Inst, Boston, MA 02131 USA.
RP Hao, ZQ (reprint author), Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110164, Peoples R China.
EM hzq@iae.ac.cn
RI wang, xugao/B-1111-2015; Wiegand, Thorsten/H-5877-2016
OI wang, xugao/0000-0003-1207-8852; Wiegand, Thorsten/0000-0002-3721-2248
FU Chinese Academy of Sciences [KZCX2-YW-QN402, KSCX2-EW-Z-5,
KZCX2-EW-401]; National Natural Science Foundation of China [40971286];
National Key Technologies R&D Program of China [2008BAC39B02]; ERC
[233066]; Center for Tropical Forest Science of the Smithsonian Tropical
Research Institute; HSBC; Cofrin Center for Biodiversity
FX We thank the CBS and Wabikon plot census and data management teams, the
latter including many student assistants from the University of
Wisconsin-Green Bay. In particular, we thank Buhang Li, Ji Ye, Fei Lin,
Zuoqiang Yuan, Xuejiao Bai, Liwei Wang and Dingliang Xing for their
field work and data collection in the CBS plot. At the Wabikon plot,
Gary Fewless, Kathryn Corio and Juniper Sundance were instrumental in
collecting and managing the data. This study was sponsored by the
Knowledge Innovation Program of the Chinese Academy of Sciences
(KZCX2-YW-QN402, KSCX2-EW-Z-5 and KZCX2-EW-401), the National Natural
Science Foundation of China (40971286) and the National Key Technologies
R&D Program of China (2008BAC39B02). The ERC advanced grant 233066
supported travelling of X.W. The Center for Tropical Forest Science of
the Smithsonian Tropical Research Institute and the HSBC Climate
Partnership provided support for X.W. and for establishment of the
Wabikon Plot. Primary funding for the Wabikon Plot was provided by the
Cofrin Center for Biodiversity with additional support from the
Department of Natural and Applied Sciences at the University of
Wisconsin-Green Bay. We are grateful for permission and important
logistic contributions by the U.S. Forest Service, particularly
Chequamegon-Nicolet National Forest ecologists Linda Parker and Steven
Janke. Other significant contributors to the project include Richard
Condit, Steve Dhein and Kimberlee McKeefry.
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SN 0022-0477
J9 J ECOL
JI J. Ecol.
PD NOV
PY 2011
VL 99
IS 6
BP 1382
EP 1393
DI 10.1111/j.1365-2745.2011.01857.x
PG 12
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 840FR
UT WOS:000296425000009
ER
PT J
AU Kanagaraj, R
Wiegand, T
Comita, LS
Huth, A
AF Kanagaraj, Rajapandian
Wiegand, Thorsten
Comita, Liza S.
Huth, Andreas
TI Tropical tree species assemblages in topographical habitats change in
time and with life stage
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE environmental heterogeneity; habitat preference; multivariate regression
tree analysis; plant population and community dynamics; regeneration
niche; species assemblages; topography; tropical forest diversity
ID MULTIVARIATE REGRESSION TREES; BORNEAN RAIN-FOREST; NEOTROPICAL FOREST;
DENSITY-DEPENDENCE; SOIL NUTRIENTS; BETA DIVERSITY; ASSOCIATIONS;
ABUNDANCE; PATTERNS; NICHE
AB 1. Recent studies have documented shifts in habitat associations of single tropical tree species from one life stage to the next. However, the community-level consequences of such shifts have not been investigated, and it is not clear whether they would amplify, neutralize or completely alter habitat structuring during the transitions to the adult community.
2. We compared habitat-driven species assemblages at three life stages (i.e. recruitment, juvenile and reproductive stages) and six censuses for tree and shrub species in a fully censused 50-ha plot of Panamanian lowland forest. Habitat types were determined using multivariate regression trees that group areas with similar species composition (i.e. species assemblages) according to their topographical characteristics.
3. Three topographical variables (a topographical wetness index, slope and elevation) were major determinants of species assemblages. When analysing individuals of all life stages together, we found a distinct and temporally consistent structuring of the plot into four dominant habitat types (low and high plateaus, slope and swamp) which was consistent with previous classifications. Basically, the same habitat structuring emerged for the juvenile communities of individual censuses. However, recruits showed a weak and temporally inconsistent habitat structuring.
4. A notable homogenization in species assemblages occurred during the transition from juvenile to reproductive, through both a reduction in the number of species assemblages (in 3 censuses, one large reproductive assemblage covered 93% of the plot, and in others, an additional slope habitat emerged) and a reduction in the classification error. Overall, habitat structuring became noisier and weaker over the 25 years of the study.
5. Synthesis. Our results suggest that mortality processes during the transition from recruits to juveniles must enhance the signal of habitat structuring. However, during the transition to the reproductive stage, species may have lost the advantage of being in the habitat with which they had become associated, or the quality of habitat changed during their life span because of larger climatic changes. The homogeneous assemblages of the reproductive stage could be interpreted as support for neutral theories, but further research is required to unravel the mechanisms behind these intriguing observations.
C1 [Kanagaraj, Rajapandian; Wiegand, Thorsten; Huth, Andreas] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04318 Leipzig, Germany.
[Comita, Liza S.] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA.
[Comita, Liza S.] Smithsonian Trop Res Inst, Balboa Ancon, Panama.
RP Kanagaraj, R (reprint author), UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, Permoserst 15, D-04318 Leipzig, Germany.
EM rajapandian.kanagaraj@ufz.de
RI Kanagaraj, Rajapandian/D-4972-2015; Wiegand, Thorsten/H-5877-2016
OI Wiegand, Thorsten/0000-0002-3721-2248
FU National Science Foundation; Center for Tropical Forest Science;
Smithsonian Tropical Research Institute; John D. and Catherine T.
MacArthur Foundation; Mellon Foundation; Celera Foundation; ERC
[233066]; National Center for Ecological Analysis and Synthesis; U.S.
NSF [EF-0553768]; University of California, Santa Barbara; State of
California
FX The BCI forest dynamics research project was made possible by National
Science Foundation grants to Stephen P. Hubbell, 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. R.K and
A.H were supported by the ERC advanced grant 233066 to T.W. L.S.C
acknowledges the support of a postdoctoral fellowship from the National
Center for Ecological Analysis and Synthesis, a Center funded by U.S.
NSF (Grant #EF-0553768), the University of California, Santa Barbara,
and the State of California. Two anonymous reviewers provided helpful
suggestions for improving the manuscript.
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SN 0022-0477
J9 J ECOL
JI J. Ecol.
PD NOV
PY 2011
VL 99
IS 6
BP 1441
EP 1452
DI 10.1111/j.1365-2745.2011.01878.x
PG 12
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 840FR
UT WOS:000296425000015
ER
PT J
AU Churchill, CKC
Strong, EE
Foighil, DO
AF Churchill, Celia K. C.
Strong, Ellen E.
Foighil, Diarmaid O.
TI HITCHHIKING JUVENILES IN THE RARE NEUSTONIC GASTROPOD RECLUZIA CF.
JEHENNEI (JANTHINIDAE)
SO JOURNAL OF MOLLUSCAN STUDIES
LA English
DT Article
ID CAENOGASTROPODA MOLLUSCA GASTROPODA; DWARF MALES; HERMAPHRODITISM;
MORPHOLOGY; CARPENTER; BIVALVIA
C1 [Churchill, Celia K. C.; Foighil, Diarmaid O.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA.
[Churchill, Celia K. C.; Foighil, Diarmaid O.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA.
[Strong, Ellen E.] Smithsonian Inst, Washington, DC 20013 USA.
RP Churchill, CKC (reprint author), Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA.
EM celia.churchill@gmail.com
FU Smithsonian Predoctoral Fellowship; NSF [OCE 0850625]; National
Geographic Society [8601-09]
FX We wish to acknowledge Jochen Gerber and Rudiger Bieler of the Field
Museum of Natural History for the loaned specimen (FMNH reg. no.
328104), which was collected during the BivATOL Moreton Bay Expedition
(2008). SEM was performed at the University of Michigan Electron
Microbeam Analysis Laboratory. Denis Riek photographed live specimens
and John Megahan provided the illustration in Figure 1B. Supplementary
Material is included with the permissions of Phil Colman and Des Beechey
(Editor, Australian Shell News). Funding for this research comes from a
Smithsonian Predoctoral Fellowship award to C.K.C.C., and NSF award OCE
0850625 and National Geographic Society award 8601-09 to D.OF.
NR 31
TC 5
Z9 5
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0260-1230
J9 J MOLLUS STUD
JI J. Molluscan Stud.
PD NOV
PY 2011
VL 77
BP 441
EP 444
DI 10.1093/mollus/eyr020
PN 4
PG 4
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 842US
UT WOS:000296627100013
ER
PT J
AU Alves-Brito, A
Hau, GKT
Forbes, DA
Spitler, LR
Strader, J
Brodie, JP
Rhode, KL
AF Alves-Brito, Alan
Hau, George K. T.
Forbes, Duncan A.
Spitler, Lee R.
Strader, Jay
Brodie, Jean P.
Rhode, Katherine L.
TI Spectra of globular clusters in the Sombrero galaxy: evidence for
spectroscopic metallicity bimodality
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE globular clusters: general; galaxies: individual: Sombrero (M104, NGC
4594); galaxies: star clusters: general
ID COLOR-MAGNITUDE RELATION; STELLAR POPULATIONS; ELLIPTIC GALAXIES;
WIDE-FIELD; BLUE TILT; SYSTEMS; PHOTOMETRY; VIRGO; M87; DISTRIBUTIONS
AB We present a large sample of over 200 integrated-light spectra of confirmed globular clusters (GCs) associated with the Sombrero (M104) galaxy taken with the Deep Imaging Multi-Object Spectrograph (DEIMOS) instrument on the Keck telescope. A significant fraction of the spectra have signal-to-noise ratio levels high enough to allow measurements of GC metallicities using the method of Brodie & Huchra. We find a distribution of spectroscopic metallicities in the range -2.2 < [Fe/H] < + 0.1 that is bimodal, with peaks at [Fe/H] similar to -1.4 and -0.6. Thus, the GC system of the Sombrero galaxy, like a few other galaxies now studied in detail, reveals a bimodal spectroscopic metallicity distribution supporting the long-held belief that colour bimodality reflects two metallicity subpopulations. This further suggests that the transformation from optical colour to metallicity for old stellar populations, such as GCs, is not strongly non-linear. We also explore the radial and magnitude distribution with metallicity for GC subpopulations but small number statistics prevent any clear trends in these distributions.
C1 [Alves-Brito, Alan; Hau, George K. T.; Forbes, Duncan A.; Spitler, Lee R.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Alves-Brito, Alan] Dept Astron & Astrofis, PUC, Santiago 7820436, Chile.
[Hau, George K. T.] European So Observ, Santiago 6670191, Chile.
[Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02144 USA.
[Brodie, Jean P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Rhode, Katherine L.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA.
RP Alves-Brito, A (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
EM abrito@astro.puc.cl
RI Spitler, Lee/A-9867-2013; Alves-Brito, Alan/J-2430-2013
OI Spitler, Lee/0000-0001-5185-9876;
FU CNPq [200227/2008-4]; FONDE-CYT [3100013]; ARC; NSF [AST-0917706,
AST-0909237, AST-0071048, AST-0808099]; JPL/Caltech [1310512]
FX AAB acknowledges CNPq (PDE, 200227/2008-4) and FONDE-CYT (3100013) for
financial support. GKTH, DAF and LRS thank ARC for financial support. JS
acknowledges support from NSF grants AST-0917706 and AST-0909237. We are
grateful to Caroline Foster and Bill Harris for useful discussions and
suggestions. We thank an anonymous referee for useful comments and
suggestions. Support for this work was provided by award 1310512, issued
by JPL/Caltech. The analysis pipeline used to reduce the DEIMOS data was
developed at UC Berkeley with support from NSF grant AST-0071048. This
work was supported by the National Science Foundation through grant
AST-0808099. We thank Steve Zepf for his help in supplying an object
list of globular candidates, and Arunav Kundu for his help with
astrometry.
NR 49
TC 26
Z9 27
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 3
BP 1823
EP 1838
DI 10.1111/j.1365-2966.2011.19368.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HX
UT WOS:000297043600014
ER
PT J
AU Rani, B
Gupta, AC
Bachev, R
Strigachev, A
Semkov, E
D'Ammando, F
Wiita, PJ
Gurwell, MA
Ovcharov, E
Mihov, B
Boeva, S
Peneva, S
AF Rani, Bindu
Gupta, Alok C.
Bachev, R.
Strigachev, A.
Semkov, E.
D'Ammando, F.
Wiita, P. J.
Gurwell, M. A.
Ovcharov, E.
Mihov, B.
Boeva, S.
Peneva, S.
TI Spectral energy distribution variation in BL Lacs and flat spectrum
radio quasars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; galaxies: active; BL Lacertae
objects: general
ID OBJECT S5 0716+714; GAMMA-RAY FLARE; OPTICAL INTRADAY VARIABILITY;
ACTIVE GALACTIC NUCLEI; LOG-PARABOLIC SPECTRA; LARGE-AREA TELESCOPE;
LACERTAE OBJECTS; MULTIWAVELENGTH OBSERVATIONS; WEBT CAMPAIGN;
EXTRAGALACTIC SOURCES
AB We present the results of our study of spectral energy distributions (SEDs) of a sample of 10 low- to intermediate-synchrotron-peaked blazars. We investigate some of the physical parameters most likely responsible for the observed short-term variations in blazars. To do so, we focus on the study of changes in the SEDs of blazars corresponding to changes in their respective optical fluxes. We model the observed spectra of blazars from radio to optical frequencies using a synchrotron model that entails a log-parabolic distribution of electron energies. A significant correlation among the two fitted spectral parameters (a, b) of log-parabolic curves and a negative trend among the peak frequency and spectral curvature parameter, b, emphasize that the SEDs of blazars are fitted well by log-parabolic curves. On considering each model parameter that could be responsible for changes in the observed SEDs of these blazars, we find that changes in the jet Doppler factors are most important.
C1 [Rani, Bindu; Gupta, Alok C.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, India.
[Rani, Bindu; Gupta, Alok C.] DDU Gorakhpur Univ, Dept Phys, Gorakhpur 273009, Uttar Pradesh, India.
[Rani, Bindu; Bachev, R.; Strigachev, A.; Semkov, E.; Mihov, B.; Boeva, S.; Peneva, S.] Bulgarian Acad Sci, Inst Astron, Sofia 1784, Bulgaria.
[Rani, Bindu; Bachev, R.; Strigachev, A.; Semkov, E.; Mihov, B.; Boeva, S.; Peneva, S.] Bulgarian Acad Sci, Natl Astron Observ, Sofia 1784, Bulgaria.
[D'Ammando, F.] INAF IASF Palermo, I-90146 Palermo, Italy.
[Wiita, P. J.] Coll New Jersey, Dept Phys, Ewing, NJ 08628 USA.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ovcharov, E.] Univ Sofia, Dept Astron, Sofia 1164, Bulgaria.
RP Rani, B (reprint author), Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, India.
EM bindu@aries.res.in
OI Wiita, Paul/0000-0002-1029-3746
FU Bulgarian Ministry of Education and Sciences [BIn - 13/09, DO 02-85,
DO02-340/08]; Indo-Bulgaria bilateral scientific exchange project
INT/Bulgaria [B-5/08]; DST, India; University of Michigan; National
Science Foundation [AST-0607523]; Smithsonian Institution; Academia
Sinica
FX We thank the referee, Dr Paolo Giommi, for several helpful suggestions.
BR is thankful to Professor D. C. Srivastava for his valuable
suggestions and encouragements and to Mr Ravi Joshi for help while
finalizing the text. This research was partially supported by Scientific
Research Fund of the Bulgarian Ministry of Education and Sciences (BIn -
13/09, DO 02-85 and DO02-340/08) and by Indo-Bulgaria bilateral
scientific exchange project INT/Bulgaria/B-5/08 funded by DST, India. RB
and AS acknowledge the kind hospitality of ARIES, Nainital, India. This
research has made use of data from the University of Michigan Radio
Astronomy Observatory which has been supported by the University of
Michigan and by a series of grants from the National Science Foundation,
most recently AST-0607523. BR is very grateful to Margo Aller for
providing the data at radio frequencies. 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. We used these data in
our research. The Australia Telescope Compact Array is part of the
Australia Telescope which is funded by the Commonwealth of Australia for
operation as a National Facility managed by CSIRO. The efforts of ATNF
staff in maintaining the ATCA calibrator data base
(http://www.narrabri.atnf.csiro.au/calibrators/) are gratefully
acknowledged. SMARTS data are made available by Yale University at
http://www.astro.yale.edu/smarts/fermi through Fermi GI grant 011283.
NR 87
TC 10
Z9 10
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 3
BP 1881
EP 1890
DI 10.1111/j.1365-2966.2011.19373.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HX
UT WOS:000297043600018
ER
PT J
AU Margutti, R
Chincarini, G
Granot, J
Guidorzi, C
Berger, E
Bernardini, MG
Gehrels, N
Soderberg, AM
Stamatikos, M
Zaninoni, E
AF Margutti, R.
Chincarini, G.
Granot, J.
Guidorzi, C.
Berger, E.
Bernardini, M. G.
Gehrels, N.
Soderberg, A. M.
Stamatikos, M.
Zaninoni, E.
TI X-ray flare candidates in short gamma-ray bursts
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: non-thermal; gamma-ray burst: general
ID LAG-LUMINOSITY RELATION; AFTERGLOW LIGHT CURVES; EXTENDED EMISSION;
TELESCOPE OBSERVATIONS; TEMPORAL PROPERTIES; PROMPT EMISSION; PEAK
LUMINOSITY; HOST GALAXIES; NEUTRON-STARS; SWIFT
AB We present the first systematic study of X-ray flare candidates in short gamma-ray bursts (SGRBs) exploiting the large 6-year Swift data base with the aim to constrain the physical nature of such fluctuations. We find that flare candidates appear in different types of SGRB host galaxy environments and show no clear correlation with the X-ray afterglow lifetime; flare candidates are detected both in SGRBs with a bright extended emission in the soft gamma-rays and in SGRBs which do not show such component. We furthermore show that SGRB X-ray flare candidates only partially share the set of observational properties of long GRB (LGRB) flares. In particular, the main parameter driving the duration evolution of X-ray variability episodes in both classes is found to be the elapsed time from the explosion, with very limited dependence on the different progenitors, environments, central engine lifetimes, prompt variability time-scales and energy budgets. On the contrary, SGRB flare candidates significantly differ from LGRB flares in terms of peak luminosity, isotropic energy, flare-to-prompt luminosity ratio and relative variability flux. However, these differences disappear when the central engine time-scales and energy budget are accounted for, suggesting that (i) flare candidates and prompt pulses in SGRBs likely have a common origin; (ii) similar dissipation and/or emission mechanisms are responsible for the prompt and flare emission in LGRBs and SGRBs, with SGRBs being less energetic albeit faster evolving versions of the long class. Finally, we show that in strict analogy to the SGRB prompt emission, flares candidates fall off the lag-luminosity relation defined by LGRBs, thus strengthening the SGRB flare-prompt pulse connection.
C1 [Margutti, R.; Chincarini, G.; Bernardini, M. G.; Zaninoni, E.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Margutti, R.; Berger, E.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chincarini, G.] Univ Milano Bicocca, Dip Fis G Occhialini, I-20126 Milan, Italy.
[Granot, J.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Granot, J.] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Granot, J.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Guidorzi, C.] Univ Ferrara, Dept Phys, I-44122 Ferarra, Italy.
[Gehrels, N.; Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Zaninoni, E.] Univ Padua, Dip Astron, I-35122 Padua, Italy.
RP Margutti, R (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Italy.
EM raffaella.margutti@brera.inaf.it
RI Gehrels, Neil/D-2971-2012
FU ASI [SWIFT I/011/07/0]; Ministry of University and Research of Italy
[PRIN MIUR 2007TNYZXL]; MAE (Ministry of Exterior); University of Milano
Bicocca, Italy; ERC
FX We thank the anonymous referee for helpful suggestions that improved the
quality of this work. RM thanks Lorenzo Amati for sharing his data
before publication. This work is supported by ASI grant SWIFT
I/011/07/0, by the Ministry of University and Research of Italy (PRIN
MIUR 2007TNYZXL), by MAE (Ministry of Exterior), by the University of
Milano Bicocca, Italy and by the ERC advanced research grant 'GRBs'.
NR 77
TC 27
Z9 28
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD NOV
PY 2011
VL 417
IS 3
BP 2144
EP 2160
DI 10.1111/j.1365-2966.2011.19397.x
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HX
UT WOS:000297043600035
ER
PT J
AU Perkins, SL
Martinsen, ES
Falk, BG
AF Perkins, S. L.
Martinsen, E. S.
Falk, B. G.
TI Do molecules matter more than morphology? Promises and pitfalls in
parasites
SO PARASITOLOGY
LA English
DT Article
DE Integrated taxonomy; molecular systematics; cryptic species
ID INTERNAL TRANSCRIBED SPACER-1; ANIMAL MITOCHONDRIAL-DNA; CHAIN-REACTION
PRIMERS; AVIAN BLOOD PARASITES; RNA GENE-SEQUENCES; MALARIA PARASITES;
HOST-SPECIFICITY; CYTOCHROME-B; PLASMODIUM-FALCIPARUM; CRYPTIC DIVERSITY
AB Systematics involves resolving both the taxonomy and phylogenetic placement of organisms. We review the advantages and disadvantages of the two kinds of information commonly used for such inferences - morphological and molecular data - as applied to the systematics of metazoan parasites generally, with special attention to the malaria parasites. The problems that potentially confound the use of morphology in parasites include challenges to consistent specimen preservation, plasticity of features depending on hosts or other environmental factors, and morphological convergence. Molecular characters such as DNA sequences present an alternative data source and are particularly useful when not all the parasite's life stages are present or when parasitaemia is low. Nonetheless, molecular data can bring challenges that include troublesome DNA isolation, paralogous gene copies, difficulty in developing molecular markers, and preferential amplification in mixed species infections. Given the differential benefits and shortcomings of both molecular and morphological characters, both should be implemented in parasite taxonomy and phylogenetics.
C1 [Perkins, S. L.; Falk, B. G.] Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA.
[Martinsen, E. S.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
[Falk, B. G.] Amer Museum Nat Hist, Richard Gilder Grad Sch, New York, NY 10024 USA.
RP Perkins, SL (reprint author), Amer Museum Nat Hist, Sackler Inst Comparat Genom, Cent Pk W & 79th St, New York, NY 10024 USA.
EM perkins@amnh.org
OI Perkins, Susan/0000-0002-5400-5662
NR 103
TC 32
Z9 33
U1 2
U2 36
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0031-1820
EI 1469-8161
J9 PARASITOLOGY
JI Parasitology
PD NOV
PY 2011
VL 138
IS 13
BP 1664
EP 1674
DI 10.1017/S0031182011000679
PG 11
WC Parasitology
SC Parasitology
GA 847JY
UT WOS:000296970400003
PM 21729351
ER
PT J
AU Zarowiecki, M
Loaiza, JR
Conn, JE
AF Zarowiecki, Magdalena
Loaiza, Jose R.
Conn, Jan E.
TI Towards a new role for vector systematics in parasite control
SO PARASITOLOGY
LA English
DT Article
DE Species complex; speciation; biogeography; vector systematics
ID ALBITARSIS COMPLEX DIPTERA; MULTILOCUS GENOTYPE DATA; ANOPHELES-GAMBIAE;
SPECIES DELIMITATION; GENE-FLOW; MALARIA VECTOR; POPULATION-STRUCTURE;
SOUTHEAST-ASIA; COMPARATIVE SUSCEPTIBILITY; LEUCOSPHYRUS GROUP
AB Vector systematics research is being transformed by the recent development of theoretical, experimental and analytical methods, as well as conceptual insights into speciation and reconstruction of evolutionary history. We review this progress using examples from the mosquito genus Anopheles. The conclusion is that recent progress, particularly in the development of better tools for understanding evolutionary history, makes systematics much more informative for vector control purposes, and has increasing potential to inform and improve targeted vector control programmes.
C1 [Zarowiecki, Magdalena] Nat Hist Museum, Dept Zool, London SW7 5BD, England.
[Loaiza, Jose R.] Univ Panama, Programa Ctr Amer Maestria Entomol Vicerrectoria, Panama City, Panama.
[Loaiza, Jose R.] Smithsonian Trop Res Inst, Unit 0948, Balboa Ancon, Panama.
[Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Griffin Lab, Slingerlands, NY USA.
[Conn, Jan E.] SUNY Albany, Sch Publ Hlth, Dept Biomed Sci, Albany, NY 12222 USA.
RP Zarowiecki, M (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England.
EM mz3@sanger.ac.uk
OI Zarowiecki, Magdalena/0000-0001-6102-7731; Conn, Jan/0000-0002-5301-7020
FU Natural History Museum
FX This work was supported by the Natural History Museum (M.Z., Prize
Studentship).
NR 93
TC 4
Z9 5
U1 1
U2 9
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0031-1820
EI 1469-8161
J9 PARASITOLOGY
JI Parasitology
PD NOV
PY 2011
VL 138
IS 13
BP 1723
EP 1729
DI 10.1017/S003118201100062X
PG 7
WC Parasitology
SC Parasitology
GA 847JY
UT WOS:000296970400007
PM 21679487
ER
PT J
AU Ibanez-Mejia, M
Ruiz, J
Valencia, VA
Cardona, A
Gehrels, GE
Mora, AR
AF Ibanez-Mejia, Mauricio
Ruiz, Joaquin
Valencia, Victor A.
Cardona, Agustin
Gehrels, George E.
Mora, Andres R.
TI The Putumayo Orogen of Amazonia and its implications for Rodinia
reconstructions: New U-Pb geochronological insights into the Proterozoic
tectonic evolution of northwestern South America
SO PRECAMBRIAN RESEARCH
LA English
DT Article
DE South America; Amazonia; Putumayo Orogen; Rodinia; Grenville; U-Pb
geochronology
ID NEOPROTEROZOIC ACTIVE MARGIN; EASTERN GRENVILLE PROVINCE; NORTHERN
OAXACAN COMPLEX; LARGE OCEAN BASINS; COLOMBIAN ANDES; LLANO UPLIFT;
ZIRCON GEOCHRONOLOGY; SVECONORWEGIAN PROVINCE; GUICHICOVI COMPLEX; U/PB
GEOCHRONOLOGY
AB Outcrops of late Meso- to early Neoproterozoic crust in northwestern South America are restricted to isolated exposures of basement inliers within the northern Andes of Colombia, Peru and Venezuela. However, evidence for the existence of an autochthonous Stenian-Tonian belt in northern Amazonia that is undisturbed by Andean orogenesis has not been recognized so far. Here we report similar to 1200 new single-zircon U-Pb geochronological analyses from 19 Proterozoic rock samples of northwestern South America collected from the Garzon and Las Minas Andean cordilleran inliers, drill-core samples from the foreland basin basement, and outcrops of cratonic Amazonia in eastern Colombia (western Guyana shield). Our new geochronological results document the existence of a previously unrecognized Meso- to Neoproterozoic orogenic belt buried under the north Andean foreland basins, herein termed the Putumayo Orogen, which has implications for Proterozoic tectonic reconstructions of Amazonia during the assembly of the supercontinent Rodinia. Based on the interpretations of new and pre-existing data, we propose a three-stage tectonometamorphic evolution for this orogenic segment characterized by: (1) development of a pericratonic fringing-arc system outboard of Amazonia's leading margin during Mesoproterozoic time from similar to 1.3 to 1.1 Ga, where the protoliths for metaigneous and metavolcanosedimentary units of the Colombian and Mexican inliers would have originated in a commonly evolving Colombian-Oaxaquian fringing-arc system; (2) amphibolite-grade metamorphism and migmatization between ca. 1.05 and 1.01 Ga by inferred amalgamation of these parautochtonous arc terranes onto the continental margin, and (3) granulite-grade metamorphism at similar to 0.99 Ga during continent-continent collision related to Rodinia final assembly. Along with additional paleogeographic constraints, this new geochronological framework suggests that the final metamorphic phase of the Putumayo Orogen was likely the result of collisional interactions with the Sveconorwegian province of Baltica, in contrast to previously proposed models that place this margin of Amazonia as the conjugate of the Grenville province of Laurentia. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Ibanez-Mejia, Mauricio; Ruiz, Joaquin; Gehrels, George E.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[Valencia, Victor A.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
[Cardona, Agustin] Smithsonian Trop Res Inst, Balboa, Panama.
[Mora, Andres R.] ECOPETROL, Inst Colombiano Petr ICP, Santander, Spain.
RP Ibanez-Mejia, M (reprint author), Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
EM ibanezm@email.arizona.edu
OI Ibanez-Mejia, Mauricio/0000-0002-7839-2425
FU Ecopetrol-ICP; GSA [9184-09]; Chevron-Texaco through University of
Arizona; NSF-EAR [0443387, 0732436]
FX This research benefited from funding provided to M.I. by Ecopetrol-ICP,
the GSA student Grant #9184-09 and a Chevron-Texaco summer Grant through
the University of Arizona. The Laserchron center is partially funded by
NSF-EAR Grants #0443387 and #0732436. The authors would like to thank
the Colombian Instituto Nacional del Petroleo (ICP-ECOPETROL) and the
Litoteca Nacional de Colombia for allowing access to the core samples.
M.I. would specially like to thank Monica Carvalho for help with figure
elaboration, Camilo Bustamante for assistance during fieldwork, Kendra
Murray for editorial improvements and Ana Milena Rangel for assistance
during core sampling at the Litoteca Nacional. Insightful comments from
reviewers Alan Collins and David Chew as well as the editorial
assistance of Peter Cawood are greatly appreciated as they helped
improve the final version of this manuscript. This paper is specially
dedicated to the memory of Prof. Dr. Thomas Van der Hammen for his
pioneering contributions on the geology of Colombia and the Amazonas
region.
NR 118
TC 37
Z9 38
U1 0
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0301-9268
J9 PRECAMBRIAN RES
JI Precambrian Res.
PD NOV
PY 2011
VL 191
IS 1-2
BP 58
EP 77
DI 10.1016/j.precamres.2011.09.005
PG 20
WC Geosciences, Multidisciplinary
SC Geology
GA 848VM
UT WOS:000297083200004
ER
PT J
AU Unghire, JM
Sutton-Grier, AE
Flanagan, NE
Richardson, CJ
AF Unghire, Joshua M.
Sutton-Grier, Ariana E.
Flanagan, Neal E.
Richardson, Curtis J.
TI Spatial Impacts of Stream and Wetland Restoration on Riparian Soil
Properties in the North Carolina Piedmont
SO RESTORATION ECOLOGY
LA English
DT Article
DE floodplain; geostatistics; kriging; soil organic matter; spatial
variability
ID PAIRED NATURAL WETLANDS; ECOSYSTEM DEVELOPMENT; VARIABILITY; ECOLOGY;
DENITRIFICATION; BIODIVERSITY; SCALE; MARSH
AB Hydric soil development of riparian wetlands is primarily influenced by the hydrologic connection between the floodplains and the stream channel. Often, the goal of riparian restoration is to revitalize this connectivity through a restructuring of the stream channel and the floodplain; however, the effects of this restructuring on the physical and spatial characteristics of soil properties are rarely considered. The objective of this study was to quantify the impacts of restoration efforts on the spatial characteristics of soil properties by means of a pre- and post-restoration comparison. We determined that the spatial patterns of soil organic matter (SOM) and exchangeable phosphorus (P(ex)) appeared less variable in the years following restoration than in the years before restoration. Mean SOM significantly decreased after restoration, whereas mean P(ex) significantly increased. The spatial characteristics and mean concentrations of NO(2)-NO(3) did not differ much between sampling dates. The loss of this spatial patterning in SOM and P(ex) and the decrease in SOM pools may represent negative impacts of restoration on important ecosystem characteristics. This study demonstrates that soil properties and spatial patterns can be negatively affected by restoration activities potentially hindering ecosystem development and function.
C1 [Unghire, Joshua M.; Flanagan, Neal E.; Richardson, Curtis J.] Duke Univ, Nicholas Sch Environm, Wetland Ctr, Durham, NC 27708 USA.
[Sutton-Grier, Ariana E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Unghire, JM (reprint author), 806 Parkwood Ave,Floor 2, Annapolis, MD 21403 USA.
EM JMUnghire@alumni.duke.edu
OI Sutton-Grier, Ariana/0000-0002-1242-7728
FU Duke University Wetlands Center (DUWC)
FX This research was supported by the Duke University Wetlands Center
(DUWC) endowment fund, Curtis J. Richardson, Director. Invaluable
laboratory support was provided by Wes Willis of the DUWC. In addition,
we want to thank Song Qian for his guidance with statistical analysis.
Also, a special thanks to Jean Still, Joe Williams, Mengchi Ho, Brian
Roberts, and Wyatt Hartman for laboratory and field assistance.
NR 44
TC 9
Z9 9
U1 3
U2 32
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1061-2971
J9 RESTOR ECOL
JI Restor. Ecol.
PD NOV
PY 2011
VL 19
IS 6
BP 738
EP 746
DI 10.1111/j.1526-100X.2010.00726.x
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 848TS
UT WOS:000297078600010
ER
PT J
AU Baresch, A
Smith, JAC
Winter, K
Valerio, AL
Jaramillo, C
AF Baresch, Andres
Smith, J. Andrew C.
Winter, Klaus
Lucia Valerio, Ana
Jaramillo, Carlos
TI KARATOPHYLLUM BROMELIOIDES LD GOMEZ REVISITED: A PROBABLE FOSSIL CAM
BROMELIAD
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Article
DE Aechmea magdalenae; Bromeliaceae; CAM photosynthesis; Karatophyllum
bromelioides; leaf morphology; travertine
ID HISTORICAL BIOGEOGRAPHY; ADAPTIVE RADIATION; AECHMEA-MAGDALENAE; GROWTH;
PHOTOSYNTHESIS; PHYLOGENY; PANAMA; ZONE
AB Premise of the study: The fossil leaf Karatophyllum bromelioides L. D. Gomez found in Costa Rica was proposed by Gomez (1972) to belong to the Bromeliaceae and to date from the middle Tertiary. If the age and affinity of this specimen were proven to be correct, it would constitute the oldest record of this large and ecologically diverse monocotyledonous family.
Key results: Morphological features of the fossil (leaf dimensions, marginal spines, cuticular traces) indicate a close affinity with the extant bromeliad Aechmea magdalenae (Andre) Andre ex Baker. Leaf thickness (1.6 mm at maximum) suggests that K. bromelioides L. D. Gomez performed CAM photosynthesis. The geological information does not corroborate the estimated age and location of the specimen; the fossil is suggested to be of more recent origin.
Conclusions: The affinity of this fossil to Bromeliaceae was confirmed, but the uncertainties surrounding its age and collection locality mitigate against its use in inferences concerning the evolutionary history of the family.
C1 [Baresch, Andres; Winter, Klaus; Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Smith, J. Andrew C.] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England.
[Lucia Valerio, Ana] Museo Nacl Costa Rica, Dept Hist Nat, San Jose, Costa Rica.
RP Baresch, A (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA.
EM ba.andres@gmail.com
FU U.S. National Science Foundation [0966884, EAR 0824299, EAR 0418042];
Mark Tupper Fellowship; Ricardo Perez SA; Smithsonian Tropical Research
Institute
FX Financial support for this investigation was provided by the U.S.
National Science Foundation Partnerships in International Research and
Education grant 0966884 (OISE, EAR, DRL), EAR 0824299, and EAR 0418042,
the Mark Tupper Fellowship, Ricardo Perez SA, and the Smithsonian
Tropical Research Institute. The authors thank Jorge Aranda and Aurelio
Virgo for assistance and Camilla Crifo, Judy Jernstedt, John G. Conran,
and an anonymous reviewer for useful comments and reviews of the
manuscript.
NR 25
TC 2
Z9 2
U1 0
U2 4
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 NOV
PY 2011
VL 98
IS 11
BP 1905
EP 1908
DI 10.3732/ajb.1100261
PG 4
WC Plant Sciences
SC Plant Sciences
GA 844PU
UT WOS:000296760500026
PM 22034484
ER
PT J
AU Bedell, M
Villaume, A
Weiss, L
Sliski, D
Strelnitski, V
Walker, G
Williams, J
Henden, A
Krajci, T
AF Bedell, Megan
Villaume, Alexa
Weiss, Lauren
Sliski, David
Strelnitski, Vladimir
Walker, Gary
Williams, Jedediyah
Henden, Arne
Krajci, Tom
TI MONITORING H alpha EMISSION AND CONTINUUM OF UXORs: RR Tauri
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; methods: observational; stars: individual (RR
Tauri); stars: pre-main sequence; stars: variables: general
ID HERBIG AE/BE STARS; YOUNG STARS; VARIABILITY; PHOTOMETRY; CATALOG; DISKS
AB The Maria Mitchell Observatory, in collaboration with the Astrokolkhoz Observatory, started a program of photometric monitoring of UX Ori-type stars (UXORs) with narrowband interference filters (IFs; augmented with the traditional broadband filters) aimed at separating the H alpha emission variations from those of the continuum. We present the method of separation and the first results for RR Tau obtained in two seasons, each roughly 100 days long (2010 Winter-Spring and 2010 Fall-2011 Spring). We confirm the conclusion from previous studies that the H alpha emission in this star is less variable than the continuum. Although some correlation between the two is not excluded, the amplitude of H alpha variations is much smaller (factors of 3-5) than that of the continuum. These results are compatible with Grinin's model of UXORs, which postulates the presence of small obscuring circumstellar clouds as the cause of the continuum fading, as well as the presence of a circumstellar reflection/emission nebula, larger than the star and the obscuring clouds, which is responsible for H alpha emission and the effect of the "color reversal" in deep minima. However, the results of both our broadband and narrowband photometry indicate that the obscuration model may be insufficient to explain all of the observations. Disk accretion, the presence of stellar or (proto) planetary companion(s), as well as the intrinsic variations of the star, may contribute to the observed light variations. We argue, in particular, that the H alpha emission may be more closely correlated with the intrinsic variations of the star than with the much stronger observed variations caused by the cloud obscuration. If this hypothesis is correct, the close monitoring of H alpha emission with IFs, accessible to small-size telescopes, may become an important tool in studying the physical nature of the UXORs' central stars.
C1 [Bedell, Megan; Villaume, Alexa; Weiss, Lauren; Sliski, David; Strelnitski, Vladimir; Walker, Gary; Williams, Jedediyah] Maria Mitchell Observ, Nantucket, MA 02554 USA.
[Bedell, Megan] Haverford Coll, Haverford, PA 19041 USA.
[Villaume, Alexa] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Weiss, Lauren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Weiss, Lauren] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Henden, Arne] AAVSO, Cambridge, MA 02138 USA.
[Krajci, Tom] Astrokolkhoz Observ, Cloudcroft, NM 88317 USA.
RP Bedell, M (reprint author), Maria Mitchell Observ, 4 Vestal St, Nantucket, MA 02554 USA.
FU NSF REU [AST-0851892]; Maria Mitchell Association; MMA; NSF; Keenan
Foundation
FX The major part of this project was accomplished by the MMO REU interns
M.B., A.V., and L.W., who thank the support from the NSF REU grant
AST-0851892 and from the Maria Mitchell Association. D.S. thanks the
support by the MMA and its Presidential Award for Excellence in Science,
Mathematics and Engineering Mentoring. The MMO observations were
performed on its new 24 inch telescope; the authors thank the NSF PREST
program, the Keenan Foundation, and numerous individual donors whose
financial support made the purchasing and running of this instrument
possible. Authors also thank the referee for a valuable suggestion about
possible parallels in physics of UXORs and T Tau stars.
NR 15
TC 0
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2011
VL 142
IS 5
AR 164
DI 10.1088/0004-6256/142/5/164
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844VH
UT WOS:000296777000021
ER
PT J
AU Drake, JJ
Ball, B
Eldridge, JJ
Ness, JU
Stancliffe, RJ
AF Drake, Jeremy J.
Ball, B.
Eldridge, John J.
Ness, J. -U.
Stancliffe, Richard J.
TI CLOSE TO THE DREDGE: PRECISE X-RAY C AND N ABUNDANCES IN lambda
ANDROMEDA AND ITS PRECOCIOUS RED GIANT BRANCH MIXING PROBLEM
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE stars: abundances; stars: activity; stars: coronae; stars: evolution;
stars: late-type; X-rays: stars
ID LOW-MASS STARS; CARBON-ISOTOPE RATIOS; METAL-POOR STARS; OLD DISK
GIANTS; CHEMICAL-COMPOSITION; STELLAR MODELS; RGB-STARS; THERMOHALINE
CONVECTION; EVOLUTIONARY SEQUENCE; NITROGEN ABUNDANCES
AB Chandra LETG+HRC-S and XMM-Newton RGS spectra of H-like C and N lines formed in the corona of the primary star of the RS CVn-type binary lambda And, a mildly metal-poor G8 III-IV first ascent giant that completed dredge-up similar to 50 Myr ago, have been used to make a precise measurement of its surface C/N ratio. We obtain the formal result [C/N] = 0.03 +/- 0.07, which is typical of old disk giants and in agreement with standard dredge-up theory for stars less than or similar to 1 M-circle dot. In contrast, these stars as a group, including lambda And, have C-12/C-13 less than or similar to 20, which is much lower than standard model predictions. We show that the abundances of the old disk giants are consistent with models including thermohaline mixing that begins at the red giant branch luminosity function "bump." Instead, lambda And indicates that the C-12/C-13 anomaly can be present immediately following dredge-up, contrary to current models of extra mixing on the red giant branch. In the context of other recent C and N abundance results for RS CVn-type binaries it seems likely that the anomaly is associated with either strong magnetic activity, fast rotation, or both, rather than close binarity itself.
C1 [Drake, Jeremy J.; Ball, B.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Eldridge, John J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Ness, J. -U.] SRE OAX, XMM Newton Observ SOC, European Space Agcy, Madrid 28691, Spain.
[Stancliffe, Richard J.] Monash Univ, Ctr Stellar & Planetary Astrophys, Sch Math Sci, Melbourne, Vic 3800, Australia.
RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS-3,60 Garden St, Cambridge, MA 02138 USA.
EM jdrake@cfa.harvard.edu; jje@ast.cam.ac.uk; Jan-Uwe.Ness@sciops.esa.int;
richard.stancliffe@monash.edu
FU NASA AISRP; NASA [NAS8-39073]; Chandra X-ray Center [AR4-5002X]; CXC
science team
FX We thank the NASA AISRP for providing financial assistance for the
development of the PINTofALE package. J.J.D. was supported by NASA
contract NAS8-39073 to the Chandra X-ray Center during the course of
this research. B. B. was supported by Chandra award number AR4-5002X
issued by the Chandra X-ray Center. J.J.D. thanks H. Tananbaum and the
CXC science team for advice and support.
NR 80
TC 2
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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 NOV
PY 2011
VL 142
IS 5
AR 144
DI 10.1088/0004-6256/142/5/144
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844VH
UT WOS:000296777000001
ER
PT J
AU Lyo, AR
Ohashi, N
Qi, CH
Wilner, DJ
Su, YN
AF Lyo, A-Ran
Ohashi, Nagayoshi
Qi, Chunhua
Wilner, David J.
Su, Yu-Nung
TI MILLIMETER OBSERVATIONS OF THE TRANSITION DISK AROUND HD 135344B (SAO
206462)
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planetary systems; protoplanetary disks; stars: pre-main sequence
ID MAIN-SEQUENCE STARS; VEGA-EXCESS STARS; HERBIG AE STARS; PROTOPLANETARY
DISK; CIRCUMSTELLAR DISKS; MOLECULAR DISK; YOUNG STARS; CO EMISSION;
DUST; SUBMILLIMETER
AB We present similar to 1 '' resolution 1.3 mm dust continuum and spectral line ((CO)-C-12 and (CO)-C-13 J = 2-1) observations of the transitional disk system HD 135344B obtained with the Submillimeter Array. The disk shows a Keplerian rotation pattern with an inclination of similar to 11 degrees, based on the spatially and spectrally resolved (CO)-C-12 and (CO)-C-13 emission. The data show clear evidence for both dust and gas surface density reductions in the inner region of the disk (radius less than or similar to 50 AU) from the continuum and (CO)-C-13 J = 2-1 data, respectively. The presence of this inner cavity in both the dust and gas is more consistent with clearing by giant planet formation than by photoevaporation or by grain growth. There is also an indication of global CO gas depletion in the disk, as the mass estimated from (CO)-C-13 emission (similar to 3.8 x 10(-4) M-circle dot) is about two orders of magnitude lower than that derived from the 1.3mm continuum (similar to 2.8 x 10(-2) M-circle dot).
C1 [Lyo, A-Ran] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Ohashi, Nagayoshi; Su, Yu-Nung] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Qi, Chunhua; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
RP Lyo, AR (reprint author), Korea Astron & Space Sci Inst, 61-1 Hwaam Dong, Taejon 305348, South Korea.
EM arl@kasi.re.kr
FU Smithsonian Institution; Academia Sinica
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.
NR 35
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2011
VL 142
IS 5
AR 151
DI 10.1088/0004-6256/142/5/151
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844VH
UT WOS:000296777000008
ER
PT J
AU Stencel, RE
Kloppenborg, BK
Wall, RE
Hopkins, JL
Howell, SB
Hoard, DW
Rayner, J
Bus, S
Tokunaga, A
Sitko, ML
Bradford, S
Russell, RW
Lynch, DK
Hammel, H
Whitney, B
Orton, G
Yanamandra-Fisher, P
Hora, JL
Hinz, P
Hoffmann, W
Skemer, A
AF Stencel, Robert E.
Kloppenborg, Brian K.
Wall, Randall E., Jr.
Hopkins, Jeffrey L.
Howell, Steve B.
Hoard, D. W.
Rayner, John
Bus, Schelte
Tokunaga, Alan
Sitko, Michael L.
Bradford, Suellen
Russell, Ray W.
Lynch, David K.
Hammel, Heidi
Whitney, Barbara
Orton, Glenn
Yanamandra-Fisher, Padma
Hora, Joseph L.
Hinz, Philip
Hoffmann, William
Skemer, Andrew
TI INFRARED STUDIES OF EPSILON AURIGAE IN ECLIPSE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; protoplanetary disks; stars: individual (epsilon
Aurigae)
ID SPITZER-SPACE-TELESCOPE; ABSORPTION-LINES; ARRAY CAMERA; SECONDARY;
SYSTEM; STARS; DISK; SPECTROGRAPH; ULTRAVIOLET; PHOTOMETRY
AB We report here on a series of medium resolution spectro-photometric observations of the enigmatic long period eclipsing binary epsilon Aurigae, during its eclipse interval of 2009-2011, using near-infrared spectra obtained with SpeX on tHe Infrared Telescope Facility (IRTF), mid-infrared spectra obtained with BASS on AOES and IRTF, MIRSI on IRTF, and MIRAC4 on the MMT, along with mid-infrared photometry using MIRSI on IRTF and MIRAC4 on the MMT, plus 1995-2000 timeframe published photometry and data obtained with Denver's TNTCAM2 at WIRO. The goals of these observations included: (1) comparing eclipse depths with prior eclipse data, (2) confirming the re-appearance of CO absorption bands at and after mid-eclipse, associated with sublimation in the disk, (3) seeking evidence for any mid-infrared solid state spectral features from particles in the disk, and (4) providing evidence that the externally irradiated disk has azimuthal temperature differences. IR eclipse depths appear similar to those observed during the most recent (1983) eclipse, although evidence for post-mid-eclipse disk temperature increase is present, due to F star heated portions of the disk coming into view. Molecular CO absorption returned 57 days after nominal mid-eclipse, but was not detected at mid-eclipse plus 34 days, narrowing the association with differentially heated sub-regions in the disk. Transient He I 10830A absorption was detected at mid-eclipse, persisting for at least 90 days thereafter, providing a diagnostic for the hot central region. The lack of solid-state features in Spitzer Infrared Spectrograph, BASS, and MIRAC spectra to date suggests the dominance of large particles (micron-sized) in the disk. Based on these observations, mid-infrared studies out of eclipse can directly monitor and map the disk thermal changes, and better constrain disk opacity and thermal conductivity.
C1 [Stencel, Robert E.; Kloppenborg, Brian K.; Wall, Randall E., Jr.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Hopkins, Jeffrey L.] Hopkins Phoenix Observ, Phoenix, AZ 85033 USA.
[Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Rayner, John; Bus, Schelte; Tokunaga, Alan] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Sitko, Michael L.; Bradford, Suellen] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Sitko, Michael L.; Bradford, Suellen; Hammel, Heidi; Whitney, Barbara] Space Sci Inst, Boulder, CO 80301 USA.
[Russell, Ray W.; Lynch, David K.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Orton, Glenn; Yanamandra-Fisher, Padma] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hinz, Philip; Hoffmann, William; Skemer, Andrew] Univ Arizona, Steward Observ, Dept Astron, Tucson, AZ 85721 USA.
RP Stencel, RE (reprint author), Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
EM rstencel@du.edu
OI Skemer, Andrew/0000-0001-6098-3924; Hora, Joseph/0000-0002-5599-4650
FU bequest of William Herschel Womble; astronomy at the University of
Denver; NSF [AST 97-24506, AST 10-16678, JPL RSA 1414715]; NASA ADP
[NNX09AC73G]; The Aerospace Corporation; National Aeronautics and Space
Administration, Science Mission Directorate [NNX-08AE38A]
FX This work was supported in part by the bequest of William Herschel
Womble in support of astronomy at the University of Denver, by NSF
grants AST 97-24506 and AST 10-16678, and JPL RSA 1414715 to the
University of Denver, by NASA ADP grant NNX09AC73G to the University of
Cincinnati, and by The Aerospace Corporation's Independent Research and
Development Program. Observations reported here were obtained in part as
Visiting Astronomers at the Infrared Telescope Facility, which is
operated by the University of Hawaii under Cooperative Agreement
NNX-08AE38A with the National Aeronautics and Space Administration,
Science Mission Directorate, Planetary Astronomy Program. Observations
reported here were obtained in part at the MMT Observatory, a joint
facility of the Smithsonian Institution and the University of Arizona.
Observations were also obtained in part at the University of Wyoming's
Infrared Observatory (WIRO), involving access for which we are grateful.
The first author thanks Dana Backman for the encouragement to obtain
mid-IR data during the mid-1990s, and the many observers involved in
those and all the data reported here. We also thank Jeff Hopkins, Brian
McCandless, Thomas Rutherford, and the AAVSO for access to their visual
observation records.
NR 37
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD NOV
PY 2011
VL 142
IS 5
AR 174
DI 10.1088/0004-6256/142/5/174
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844VH
UT WOS:000296777000031
ER
PT J
AU Beaumont, CN
Williams, JP
Goodman, AA
AF Beaumont, Christopher N.
Williams, Jonathan P.
Goodman, Alyssa A.
TI CLASSIFYING STRUCTURES IN THE INTERSTELLAR MEDIUM WITH SUPPORT VECTOR
MACHINES: THE G16.05-0.57 SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (G16.05-0.57, M17); ISM: supernova remnants;
techniques: image processing
ID PRINCIPAL COMPONENT ANALYSIS; CLASSIFICATION; EXTRACTION; ALGORITHM;
EMISSION; OUTFLOWS; PERSEUS; CLOUDS; CO
AB We apply Support Vector Machines (SVMs)-a machine learning algorithm-to the task of classifying structures in the interstellar medium (ISM). As a case study, we present a position-position-velocity (PPV) data cube of (12)CO J = 3-2 emission toward G16.05-0.57, a supernova remnant that lies behind the M17 molecular cloud. Despite the fact that these two objects partially overlap in PPV space, the two structures can easily be distinguished by eye based on their distinct morphologies. The SVM algorithm is able to infer these morphological distinctions, and associate individual pixels with each object at >90% accuracy. This case study suggests that similar techniques may be applicable to classifying other structures in the ISM-a task that has thus far proven difficult to automate.
C1 [Beaumont, Christopher N.; Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Beaumont, Christopher N.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Beaumont, CN (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM beaumont@ifa.hawaii.edu
RI Goodman, Alyssa/A-6007-2010;
OI Goodman, Alyssa/0000-0003-1312-0477; Williams,
Jonathan/0000-0001-5058-695X
FU NSF [AST-0908159]
FX We are grateful to C. Brogan for sharing her 20 cm data of G16.05-0.57,
and to K. Binsted for discussions regarding this manuscript. We also
thank the anonymous referee for his or her careful feedback. J.P.W.
acknowledges support from NSF. This material is based upon work
supported by the National Science Foundation under Grant No.
AST-0908159.
NR 32
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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 NOV 1
PY 2011
VL 741
IS 1
AR 14
DI 10.1088/0004-637X/741/1/14
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000014
ER
PT J
AU Cranmer, SR
Saar, SH
AF Cranmer, Steven R.
Saar, Steven H.
TI TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL
STARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: coronae; stars: late-type; stars: magnetic field; stars:
mass-loss; stars: winds, outflows; turbulence
ID MAIN-SEQUENCE STARS; HORIZONTAL-BRANCH STARS; ANGULAR-MOMENTUM LOSS;
SOLAR-LIKE STARS; FUNDAMENTAL STELLAR PARAMETERS; ROTATION-ACTIVITY
CORRELATION; PHOTOSPHERIC MAGNETIC-FIELD; HERTZSPRUNG-RUSSELL DIAGRAM;
WAVE ENERGY-SPECTRA; LOW-GRAVITY STARS
AB The basic mechanisms responsible for producing winds from cool, late-type stars are still largely unknown. We take inspiration from recent progress in understanding solar wind acceleration to develop a physically motivated model of the time-steady mass loss rates of cool main-sequence stars and evolved giants. This model follows the energy flux of magnetohydrodynamic turbulence from a subsurface convection zone to its eventual dissipation and escape through open magnetic flux tubes. We show how Alfven waves and turbulence can produce winds in either a hot corona or a cool extended chromosphere, and we specify the conditions that determine whether or not coronal heating occurs. These models do not utilize arbitrary normalization factors, but instead predict the mass loss rate directly from a star's fundamental properties. We take account of stellar magnetic activity by extending standard age-activity-rotation indicators to include the evolution of the filling factor of strong photospheric magnetic fields. We compared the predicted mass loss rates with observed values for 47 stars and found significantly better agreement than was obtained from the popular scaling laws of Reimers, Schroder, and Cuntz. The algorithm used to compute cool-star mass loss rates is provided as a self-contained and efficient computer code. We anticipate that the results from this kind of model can be incorporated straightforwardly into stellar evolution calculations and population synthesis techniques.
C1 [Cranmer, Steven R.; Saar, Steven H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM scranmer@cfa.harvard.edu; ssaar@cfa.harvard.edu
FU Smithsonian Institution Research Endowment; National Aeronautics and
Space Administration (NASA) [NNX09AB27G, NNX10AC11G]
FX The authors gratefully acknowledge Nancy Brickhouse, Andrea Dupree,
Adriaan van Ballegooijen, Stan Owocki, Ofer Cohen, and the anonymous
referee for many valuable discussions. This work was supported by the
Sprague Fund of the Smithsonian Institution Research Endowment, and by
the National Aeronautics and Space Administration (NASA) under grants
NNX09AB27G and NNX10AC11G to the Smithsonian Astrophysical Observatory.
This research made extensive use of NASA's Astrophysics Data System and
the SIMBAD database operated at CDS, Strasbourg, France. This research
has also made use of the NASA/IPAC/NExScI Star and Exoplanet Database
(NStED), which is operated by the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA.
NR 242
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U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2011
VL 741
IS 1
AR 54
DI 10.1088/0004-637X/741/1/54
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SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000054
ER
PT J
AU Fox, OD
Chevalier, RA
Skrutskie, MF
Soderberg, AM
Filippenko, AV
Ganeshalingam, M
Silverman, JM
Smith, N
Steele, TN
AF Fox, Ori D.
Chevalier, Roger A.
Skrutskie, Michael F.
Soderberg, Alicia M.
Filippenko, Alexei V.
Ganeshalingam, Mohan
Silverman, Jeffrey M.
Smith, Nathan
Steele, Thea N.
TI A SPITZER SURVEY FOR DUST IN TYPE IIn SUPERNOVAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; dust, extinction; infrared: stars; stars:
mass-loss; stars: winds, outflows; supernovae: general
ID CORE-COLLAPSE SUPERNOVAE; LUMINOUS BLUE VARIABLES; WOLF-RAYET STARS;
MASSIVE STARS; INFRARED ECHO; CIRCUMSTELLAR INTERACTION;
SPACE-TELESCOPE; SN 2005IP; PRESUPERNOVA EVOLUTION; RADIO-EMISSION
AB Recent observations suggest that Type IIn supernovae (SNe IIn) may exhibit late-time (>100 days) infrared (IR) emission from warm dust more than other types of core-collapse SNe. Mid-IR observations, which span the peak of the thermal spectral energy distribution, provide useful constraints on the properties of the dust and, ultimately, the circumstellar environment, explosion mechanism, and progenitor system. Due to the low SN IIn rate (<10% of all core-collapse SNe), few IR observations exist for this subclass. The handful of isolated studies, however, show late-time IR emission from warm dust that, in some cases, extends for five or six years post-discovery. While previous Spitzer/IRAC surveys have searched for dust in SNe, none have targeted the Type IIn subclass. This paper presents results from a warm Spitzer/IRAC survey of the positions of all 68 known SNe IIn within a distance of 250 Mpc between 1999 and 2008 that have remained unobserved by Spitzer more than 100 days post-discovery. The detection of late-time emission from 10 targets (similar to 15%) nearly doubles the database of existing mid-IR observations of SNe IIn. Although optical spectra show evidence for new dust formation in some cases, the data show that in most cases the likely origin of the mid-IR emission is pre-existing dust, which is continuously heated by optical emission generated by ongoing circumstellar interaction between the forward shock and circumstellar medium. Furthermore, an emerging trend suggests that these SNe decline at similar to 1000-2000 days post-discovery once the forward shock overruns the dust shell. The mass-loss rates associated with these dust shells are consistent with luminous blue variable progenitors.
C1 [Fox, Ori D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Chevalier, Roger A.; Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Filippenko, Alexei V.; Ganeshalingam, Mohan; Silverman, Jeffrey M.; Smith, Nathan; Steele, Thea N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Smith, Nathan] Steward Observ, Dept Astron, Tucson, AZ 85721 USA.
RP Fox, OD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM ori.d.fox@nasa.gov
FU NASA; NSF [AST-0807727, AST-0908886]; TABASGO Foundation; W. M. Keck
Foundation; Bill and Marina Kast
FX This work is based on observations made with the Spitzer Space Telescope
(PID 60122), 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. O.D.F. is grateful for support from the NASA Postdoctoral
Program (NPP). R.A.C. was supported by NSF grant AST-0807727. A.V.F. is
grateful for the support of NSF grant AST-0908886 and the TABASGO
Foundation. J.M.S. thanks Marc J. Staley for a graduate fellowship. 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
NASA; the observatory was made possible by the generous financial
support of the W. M. Keck Foundation. The Kast spectrograph on the Lick
3 m Shane telescope was funded by a gift from Bill and Marina Kast. We
thank the staffs of the Lick and Keck Observatories for their assistance
with the observations. We are also grateful to many students and
postdocs who helped take and reduce the optical spectra.
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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 1
PY 2011
VL 741
IS 1
AR 7
DI 10.1088/0004-637X/741/1/7
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000007
ER
PT J
AU MacLachlan, JM
Matthews, LD
Wood, K
Gallagher, JS
AF MacLachlan, J. M.
Matthews, L. D.
Wood, K.
Gallagher, J. S.
TI THE STABILITY OF LOW SURFACE BRIGHTNESS DISKS BASED ON MULTI-WAVELENGTH
MODELING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: ISM; galaxies: spiral; radiative transfer
ID EDGE-ON GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; TELESCOPE ADVANCED
CAMERA; CARLO RADIATION TRANSFER; INFRARED EXTINCTION LAW; HI IMAGING
OBSERVATIONS; DIFFUSE IONIZED-GAS; SPIRAL GALAXIES; STAR-FORMATION; NGC
4244
AB To investigate the structure and composition of the dusty interstellar medium (ISM) of low surface brightness (LSB) disk galaxies, we have used multi-wavelength photometry to construct spectral energy distributions for three low-mass, edge-on LSB galaxies (V-rot = 88-105 km s(-1)). We use Monte Carlo radiation transfer codes that include the effects of transiently heated small grains and polycyclic aromatic hydrocarbon molecules to model and interpret the data. We find that, unlike the high surface brightness galaxies previously modeled, the dust disks appear to have scale heights equal to or exceeding their stellar scale heights. This result supports the findings of previous studies that low-mass disk galaxies have dust scale heights comparable to their stellar scale heights and suggests that the cold ISM of low-mass, LSB disk galaxies may be stable against fragmentation and gravitational collapse. This may help to explain the lack of observed dust lanes in edge-on LSB galaxies and their low current star formation rates. Dust masses are found in the range (1.16-2.38) x 10(6) M-circle dot, corresponding to face-on (edge-on), V-band, optical depths 0.034 less than or similar to tau(face) less than or similar to 0.106 (0.69 less than or similar to tau(eq) less than or similar to 1.99).
C1 [MacLachlan, J. M.; Wood, K.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Matthews, L. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gallagher, J. S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
RP MacLachlan, JM (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
EM jmm55@st-andrews.ac.uk
FU Jet Propulsion Laboratory (JPL) [1279242]; National Aeronautic and Space
Administration (NASA) [1407]; 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;
American Museum of Natural History; Astrophysical Institute Potsdam;
University of Basel; University of Cambridge; Case Western Reserve
University; University of Chicago; Drexel University; Fermilab;
Institute for Advanced Study; Japan Participation Group; Johns Hopkins
University; Joint Institute for Nuclear Astrophysics; Kavli Institute
for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese
Academy of Sciences (LAMOST), Los Alamos National Laboratory;
Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for
Astrophysics (MPA); New Mexico State University; Ohio State University;
University of Pittsburgh; University of Portsmouth; Princeton
University; United States Naval Observatory; University of Washington
FX Financial support for this work was provided to L.D.M. through contract
1279242 from the Jet Propulsion Laboratory (JPL). This work is based in
part on observations from the Spitzer Space Telescope, operated by JPL,
California Institute of Technology, under contract 1407 with the
National Aeronautic and Space Administration (NASA).; Funding for the
SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation,
the Participating Institutions, the National Science Foundation, the
U.S. Department of Energy, 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 NOV 1
PY 2011
VL 741
IS 1
AR 6
DI 10.1088/0004-637X/741/1/6
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000006
ER
PT J
AU McLean, M
Berger, E
Irwin, J
Forbrich, J
Reiners, A
AF McLean, M.
Berger, E.
Irwin, J.
Forbrich, J.
Reiners, A.
TI PERIODIC RADIO EMISSION FROM THE M7 DWARF 2MASS J13142039+1320011:
IMPLICATIONS FOR THE MAGNETIC FIELD TOPOLOGY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radio continuum: stars; stars: activity; stars: low-mass; stars:
magnetic field
ID LOW-MASS STARS; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS;
ELECTRON-CYCLOTRON MASER; FULLY CONVECTIVE STARS; LSPM-NORTH CATALOG;
LARGE-SCALE; ULTRACOOL DWARF; BROWN DWARFS; DUST CLOUDS; X-RAY
AB We present multi-epoch radio and optical observations of the M7 dwarf 2MASS J13142039+1320011. We detect a similar to 1 mJy source at 1.43, 4.86, 8.46, and 22.5 GHz, making it the most luminous radio emission over the widest frequency range detected from an ultracool dwarf to date. A 10 hr Very Large Array observation reveals that the radio emission varies sinusoidally with a period of 3.89 +/- 0.05 hr, and an amplitude of approximate to 30% at 4.86 GHz and approximate to 20% at 8.46 GHz. The periodicity is also seen in circular polarization, where at 4.86 GHz the polarization reverses helicity from left-to right-handed in phase with the total intensity. An archival detection in the Faint Images of the Radio Sky at Twenty Centimeters survey indicates that the radio emission has been stable for at least a decade. We also detect periodic photometric variability in several optical filters with a period of 3.79 hr and measure a rotation velocity of v sin i = 45 +/- 5 km s(-1), in good agreement with the radio and optical periods. The subtle difference in radio and optical periods may be due to differential rotation, with Delta Omega approximate to 1 rad day(-1) between the equation and poles. The period and rotation velocity allow us to place a lower limit on the radius of the source of greater than or similar to 0.13 R-circle dot, about 30% larger than theoretical expectations. The properties of the radio emission can be explained with a simple model of a magnetic dipole misaligned relative to the stellar rotation axis, with the sinusoidal variations and helicity reversal due to the rotation of the magnetic poles relative to our line of sight. The long-term stability of the radio emission indicates that the magnetic field (and hence the dynamo) is stable on a much longer timescale than the convective turnover time of similar to 0.2 yr. If the radio emission is due to gyrosynchrotron emission the inferred magnetic field strength is similar to 0.1 kG, while the electron cyclotron maser process requires a field of at least 8 kG.
C1 [McLean, M.; Berger, E.; Irwin, J.; Forbrich, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Reiners, A.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
RP McLean, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU National Science Foundation [AST-1008361, AST-0807690]; David and Lucile
Packard Fellowship for Science and Engineering; DFG [RE 1664/4-1]
FX The authors acknowledge assistance from Philip Nutzman, Zachory Berta,
and Peter Challis. E. B. acknowledges support for this work from the
National Science Foundation under grant AST-1008361. J.I. gratefully
acknowledges funding for the MEarth project from the David and Lucile
Packard Fellowship for Science and Engineering (awarded to David
Charbonneau), and support from the National Science Foundation under
grant number AST-0807690. A. R. received research funding from the DFG
as an Emmy Noether fellow (RE 1664/4-1). This paper includes data
gathered with the 6.5 m Magellan Telescopes located at Las Campanas
Observatory, Chile.
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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 1
PY 2011
VL 741
IS 1
AR 27
DI 10.1088/0004-637X/741/1/27
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000027
ER
PT J
AU Starikova, S
Cool, R
Eisenstein, D
Forman, W
Jones, C
Hickox, R
Kenter, A
Kochanek, C
Kravtsov, A
Murray, SS
Vikhlinin, A
AF Starikova, S.
Cool, R.
Eisenstein, D.
Forman, W.
Jones, C.
Hickox, R.
Kenter, A.
Kochanek, C.
Kravtsov, A.
Murray, S. S.
Vikhlinin, A.
TI CONSTRAINING HALO OCCUPATION PROPERTIES OF X-RAY ACTIVE GALACTIC NUCLEI
USING CLUSTERING OF CHANDRA SOURCES IN THE BOOTES SURVEY REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: statistics; large-scale structure of
universe; X-rays: galaxies
ID CROSS-CORRELATION FUNCTION; SUPERMASSIVE BLACK-HOLES; LUMINOUS RED
GALAXIES; DIGITAL SKY SURVEY; SPATIAL CORRELATION-FUNCTION;
REDSHIFT-SPACE DISTORTIONS; DARK-MATTER HALOES; ANALYTIC MODEL;
NUMERICAL SIMULATIONS; ANGULAR-CORRELATION
AB We present one of the most precise measurements to date of the spatial clustering of X-ray-selected active galactic nuclei (AGNs) using a sample derived from the Chandra X-ray Observatory survey in the Bootes field. The real-space two-point correlation function over a redshift interval from z = 0.17 to z similar to 3 is well described by the power law,. xi(r) = (r/r(0))-(gamma), for comoving separations r less than or similar to 20 h(-1) Mpc. We find gamma = 1.84 +/- 0.12 and gamma(0) consistent with no redshift trend within the sample (varying between r(0) = 5.5 +/- 0.6 h(-1) Mpc for < z > = 0.37 and r(0) = 6.9 +/- 1.0 h(-1) Mpc for < z > = 1.28). Furthermore, we are able to measure the projections of the two-point correlation function both on the sky plane and in the line of sight. We use these measurements to show that the Chandra/Bootes AGNs are predominantly located at the centers of dark matter halos with circular velocity v(max) > 320 km s(-1) or M(180) > 4.1 x 10(12) h(-1) M(circle dot), and tend to avoid satellite galaxies in halos of this or higher mass. The halo occupation properties inferred from the clustering properties of Chandra/Bootes AGNs-the mass scale of the parent dark matter halos, the lack of significant redshift evolution of the clustering length, and the low satellite fraction-are broadly consistent with the Hopkins et al. scenario of quasar activity triggered by mergers of similarly sized galaxies.
C1 [Starikova, S.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Starikova, S.; Eisenstein, D.; Forman, W.; Jones, C.; Kenter, A.; Murray, S. S.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cool, R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hickox, R.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Kochanek, C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Kravtsov, A.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, E Fermi Inst, Chicago, IL 60637 USA.
[Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Vikhlinin, A.] Space Res Inst IKI, Moscow, Russia.
RP Starikova, S (reprint author), Univ Padua, Dipartimento Astron, Vicolo Osservatorio 2, I-35122 Padua, Italy.
OI Forman, William/0000-0002-9478-1682
FU Smithsonian Institution and NASA [NAS8-39073, NAS8-03060]; NSF
[AST-0708154]; NASA [NAG5-13274]; Kavli Institute for Cosmological
Physics at the University of Chicago [NSF PHY-0551142]
FX This work was supported by the Smithsonian Institution and NASA through
contracts NAS8-39073 and NAS8-03060 (CXC). A.K. is supported by NSF
grant AST-0708154, by NASA grant NAG5-13274, and by the Kavli Institute
for Cosmological Physics at the University of Chicago through grant NSF
PHY-0551142 and an endowment from the Kavli Foundation. We thank O.
Gnedin and A. Franceschini for useful discussions and comments.
Facilities: CXO, MMT
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD NOV 1
PY 2011
VL 741
IS 1
AR 15
DI 10.1088/0004-637X/741/1/15
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844TA
UT WOS:000296769000015
ER
PT J
AU Evans, DA
Summers, AC
Hardcastle, MJ
Kraft, RP
Gandhi, P
Croston, JH
Lee, JC
AF Evans, D. A.
Summers, A. C.
Hardcastle, M. J.
Kraft, R. P.
Gandhi, P.
Croston, J. H.
Lee, J. C.
TI THE SUZAKU VIEW OF THE DISK-JET CONNECTION IN THE LOW-EXCITATION RADIO
GALAXY NGC 6251
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 6251); galaxies: jets;
X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATIONS; X-RAY; FR-I; NGC-6251;
CHANDRA; ENVIRONMENT; DICHOTOMY; ACCRETION; SAMPLE
AB We present results from an 87 ks Suzaku observation of the canonical low-excitation radio galaxy (LERG) NGC6251. We have previously suggested that LERGs violate conventional active galactic nucleus unification schemes: they may lack an obscuring torus and are likely to accrete in a radiatively inefficient manner, with almost all of the energy released by the accretion process being channeled into powerful jets. We model the 0.5-20 keV Suzaku spectrum with a single power law of photon index Gamma = 1.82(-0.05)(+0.04) , together with two collisionally ionized plasma models whose parameters are consistent with the known galaxy- and group-scale thermal emission. Our observations confirm that there are no signatures of obscured, accretion-related X-ray emission in NGC 6251, and we show that the luminosity of any such component must be substantially sub-Eddington in nature.
C1 [Evans, D. A.; Kraft, R. P.; Lee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Evans, D. A.; Summers, A. C.] Elon Univ, Dept Phys, Elon, NC 27244 USA.
[Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England.
[Gandhi, P.] Japan Aerosp Explorat Agcy, ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
RP Evans, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Hardcastle, Martin/E-2264-2012; XRAY, SUZAKU/A-1808-2009
OI Hardcastle, Martin/0000-0003-4223-1117;
FU NASA [NNX11AD34G]; Jet Propulsion Laboratory, California Institute of
Technology, under NASA
FX We thank the anonymous referee for providing constructive comments.
D.A.E. gratefully acknowledges financial support for this work from NASA
under grant number NNX11AD34G. This research has made use of data
obtained from the Suzaku satellite, a collaborative mission between the
space agencies of Japan (JAXA) and the USA (NASA). This research has
also used the NASA/IPAC Extragalactic Database (NED) which is operated
by the Jet Propulsion Laboratory, California Institute of Technology,
under contract with NASA.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD NOV 1
PY 2011
VL 741
IS 1
AR L4
DI 10.1088/2041-8205/741/1/L4
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844NC
UT WOS:000296753000004
ER
PT J
AU Long, DM
DeLuca, EE
Gallagher, PT
AF Long, David M.
DeLuca, Edward E.
Gallagher, Peter T.
TI THE WAVE PROPERTIES OF CORONAL BRIGHT FRONTS OBSERVED USING SDO/AIA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: magnetic topology; waves
ID EXTREME-ULTRAVIOLET WAVE; EIT WAVES; MASS EJECTION; SOLAR CORONA; QUIET
SUN; PROPAGATING DISTURBANCE; QUADRATURE OBSERVATIONS; SOHO/EIT
OBSERVATIONS; MORETON WAVES; MHD WAVES
AB Coronal bright fronts (CBFs) are large-scale wavefronts that propagate through the solar corona at hundreds of kilometers per second. While their kinematics have been studied in detail, many questions remain regarding the temporal evolution of their amplitude and pulse width. Here, contemporaneous high cadence, multi-thermal observations of the solar corona from the Solar Dynamic Observatory (SDO) and Solar TErrestrial RElations Observatory (STEREO) spacecraft are used to determine the kinematics and expansion rate of a CBF wavefront observed on 2010 August 14. The CBF was found to have a lower initial velocity with weaker deceleration in STEREO observations compared to SDO observations (similar to 340 km s(-1) and -72 m s(-2) as opposed to similar to 410 km s(-1) and -279 m s(-2)). The CBF kinematics from SDO were found to be highly passband-dependent, with an initial velocity ranging from 379 +/- 12 km s(-1) to 460 +/- 28 km s(-1) and acceleration ranging from -128 +/- 28 m s(-2) to -431 +/- 86 m s(-2) in the 335 angstrom and 304 angstrom passbands, respectively. These kinematics were used to estimate a quiet coronal magnetic field strength range of similar to 1-2 G. Significant pulse broadening was also observed, with expansion rates of similar to 130 km s(-1) (STEREO) and similar to 220 km s(-1) (SDO). By treating the CBF as a linear superposition of sinusoidal waves within a Gaussian envelope, the resulting dispersion rate of the pulse was found to be similar to 8-13 Mm(2) s(-1). These results are indicative of a fast-mode magnetoacoustic wave pulse propagating through an inhomogeneous medium.
C1 [Long, David M.; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Long, David M.; Gallagher, Peter T.] Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland.
RP Long, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM longda@tcd.ie
RI Long, David/J-3227-2013; DeLuca, Edward/L-7534-2013; Gallagher,
Peter/C-7717-2011
OI Long, David/0000-0003-3137-0277; DeLuca, Edward/0000-0001-7416-2895;
Gallagher, Peter/0000-0001-9745-0400
FU Irish Research Council for Science, Engineering and Technology (IRCSET)
FX D.M.L. is a 2010-2011 Pre-Doctoral Fellow at the Harvard-Smithsonian
Center for Astrophysics, and carried out some of this work while a
Government of Ireland Scholar supported by the Irish Research Council
for Science, Engineering and Technology (IRCSET). We thank S.
Patsourakos, R. T. J. McAteer, D. S. Bloomfield, and J. Raymond for
useful discussions, and the anonymous referee whose comments helped to
improve this Letter.
NR 41
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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 1
PY 2011
VL 741
IS 1
AR L21
DI 10.1088/2041-8205/741/1/L21
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844NC
UT WOS:000296753000021
ER
PT J
AU Pillitteri, I
Gunther, HM
Wolk, SJ
Kashyap, VL
Cohen, O
AF Pillitteri, I.
Guenther, H. M.
Wolk, S. J.
Kashyap, V. L.
Cohen, O.
TI X-RAY ACTIVITY PHASED WITH PLANET MOTION IN HD 189733?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; stars: activity; stars: coronae; stars: individual
(HD189733); X-rays: stars
ID STELLAR ACTIVITY ENHANCEMENT; EXTRASOLAR GIANT PLANETS;
PROXIMA-CENTAURI; ATOMIC DATABASE; EMISSION-LINES; HOT JUPITERS;
XMM-NEWTON; STARS; SPECTROSCOPY; ACCRETION
AB We report on the follow-up XMM-Newton observation of the planet-hosting star HD 189733 we obtained in 2011 April. We observe a flare just after the secondary transit of the hot Jupiter. This event shares the same phase and many of the characteristics of the flare we observed in 2009. We suggest that a systematic interaction between planet and stellar magnetic fields when the planet passes close to active regions on the star can lead to periodic variability phased with planetary motion. By means of high-resolution X-ray spectroscopy with the Reflection Grating Spectrometer on board XMM-Newton, we determine that the corona of this star is unusually dense.
C1 [Pillitteri, I.; Guenther, H. M.; Wolk, S. J.; Kashyap, V. L.; Cohen, O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Pillitteri, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Pillitteri, Ignazio/L-1549-2016;
OI Pillitteri, Ignazio/0000-0003-4948-6550; Gunther, Hans
Moritz/0000-0003-4243-2840; Wolk, Scott/0000-0002-0826-9261; Cohen,
Ofer/0000-0003-3721-0215
FU XMM [NNX09AP46G]; NASA [NAS8-03060, NAS8-39073]; NASA LWSTRT
[NNG05GM44G]
FX The XMM-Newton guest investigator program supported I.P. and H.M.G.
through grant NNX09AP46G. S.J.W. was supported by NASA Contract
NAS8-03060 to the Chandra Science Center. V.K. acknowledges CXC NASA
Contract NAS8-39073 and O.C. acknowledges NASA LWSTRT Grant NNG05GM44G.
NR 28
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U1 0
U2 6
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 1
PY 2011
VL 741
IS 1
AR L18
DI 10.1088/2041-8205/741/1/L18
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844NC
UT WOS:000296753000018
ER
PT J
AU Winn, JN
Albrecht, S
Johnson, JA
Torres, G
Cochran, WD
Marcy, GW
Howard, AW
Isaacson, H
Fischer, D
Doyle, L
Welsh, W
Carter, JA
Fabrycky, DC
Ragozzine, D
Quinn, SN
Shporer, A
Howell, SB
Latham, DW
Orosz, J
Prsa, A
Slawson, RW
Borucki, WJ
Koch, D
Barclay, T
Boss, AP
Christensen-Dalsgaard, J
Girouard, FR
Jenkins, J
Klaus, TC
Meibom, S
Morris, RL
Sasselov, D
Still, M
Van Cleve, J
AF Winn, Joshua N.
Albrecht, Simon
Johnson, John Asher
Torres, Guillermo
Cochran, William D.
Marcy, Geoffrey W.
Howard, Andrew W.
Isaacson, Howard
Fischer, Debra
Doyle, Laurance
Welsh, William
Carter, Joshua A.
Fabrycky, Daniel C.
Ragozzine, Darin
Quinn, Samuel N.
Shporer, Avi
Howell, Steve B.
Latham, David W.
Orosz, Jerome
Prsa, Andrej
Slawson, Robert W.
Borucki, William J.
Koch, David
Barclay, Thomas
Boss, Alan P.
Christensen-Dalsgaard, Jorgen
Girouard, Forrest R.
Jenkins, Jon
Klaus, Todd C.
Meibom, Soren
Morris, Robert L.
Sasselov, Dimitar
Still, Martin
Van Cleve, Jeffrey
TI SPIN-ORBIT ALIGNMENT FOR THE CIRCUMBINARY PLANET HOST KEPLER-16 A
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: general; planets and satellites: formation; stars: individual
(Kepler-16 A, KIC 12644769); stars: low-mass; stars: rotation
ID LOWER MAIN-SEQUENCE; CLOSE BINARY-SYSTEMS; LOW-MASS STARS; ECLIPSING
BINARY; ABSOLUTE DIMENSIONS; EVOLUTIONARY MODELS; HIERARCHICAL TRIPLE;
BROWN DWARF; ROTATION; STELLAR
AB Kepler-16 is an eccentric low-mass eclipsing binary with a circumbinary transiting planet. Here, we investigate the angular momentum of the primary star, based on Kepler photometry and Keck spectroscopy. The primary star's rotation period is 35.1 +/- 1.0 days, and its projected obliquity with respect to the stellar binary orbit is 1.degrees 6 +/- 2.degrees 4. Therefore, the three largest sources of angular momentum-the stellar orbit, the planetary orbit, and the primary's rotation-are all closely aligned. This finding supports a formation scenario involving accretion from a single disk. Alternatively, tides may have realigned the stars despite their relatively wide separation (0.2 AU), a hypothesis that is supported by the agreement between the measured rotation period and the "pseudosynchronous" period of tidal evolution theory. The rotation period, chromospheric activity level, and fractional light variations suggest a main-sequence age of 2-4 Gyr. Evolutionary models of low-mass stars can match the observed masses and radii of the primary and secondary stars to within about 3%.
C1 [Winn, Joshua N.; Albrecht, Simon] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Winn, Joshua N.; Albrecht, Simon] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Johnson, John Asher] NASA Exoplanet Sci Inst NExScI, Pasadena, CA USA.
[Torres, Guillermo; Carter, Joshua A.; Ragozzine, Darin; Quinn, Samuel N.; Latham, David W.; Meibom, Soren; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Doyle, Laurance; Slawson, Robert W.; Jenkins, Jon; Morris, Robert L.; Van Cleve, Jeffrey] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA.
[Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Welsh, William; Orosz, Jerome] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Boss, Alan P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Christensen-Dalsgaard, Jorgen] Aarhus Univ, Danish AsteroSeismol Ctr, DK-8000 Aarhus C, Denmark.
[Christensen-Dalsgaard, Jorgen] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Girouard, Forrest R.; Klaus, Todd C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.
RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Howard,
Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Barclay, Thomas/0000-0001-7139-2724;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA [NNX09AB33G]; NSF [AST-1007992]; W. M. Keck Foundation
FX We thank Brice-Olivier Demory, Nevin Weinberg, and Jamie Lloyd for
helpful discussions. Work by J.N.W. and S.A. was supported by NASA
Origins award NNX09AB33G. G.T. acknowledges partial support from the NSF
through grant AST-1007992. Funding for the Kepler Discovery mission is
provided by NASA's Science Mission Directorate. The W. M. Keck
Observatory is operated as a scientific partnership among the California
Institute of Technology, the University of California, and the National
Aeronautics and Space Administration, and was made possible by the
generous financial support of the W. M. Keck Foundation. We extend
special thanks to those of Hawaiian ancestry on whose sacred mountain of
Mauna Kea we are privileged to be guests.
NR 47
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U1 1
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 1
PY 2011
VL 741
IS 1
AR L1
DI 10.1088/2041-8205/741/1/L1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844NC
UT WOS:000296753000001
ER
PT J
AU Brickhouse, NS
AF Brickhouse, Nancy S.
TI Magnetic accretion onto young stars
SO ASTROPHYSICS AND SPACE SCIENCE
LA English
DT Article
DE Accretion; Atomic physics; Magnetic fields; Stars: individual (TW
Hydrae); Techniques: spectroscopic; X-rays: stars
ID CLASSICAL T-TAURI; EMISSION-LINE DIAGNOSTICS; MAGNETOSPHERIC ACCRETION;
DISK ACCRETION; HYDRAE; CHANDRA; PLASMA
AB Young T Tauri stars exhibit strong solar-type magnetic activity, with extremely high temperature coronae and energetic flares. In a few systems discovered with Chandra and XMM-Newton there is also evidence for X-ray emission produced by shocks associated with magnetically channeled accretion. A recent 489 ksec Chandra HETG/ACIS-S observation of the classical T Tauri star TW Hydrae has provided a wealth of spectroscopic diagnostics not available in lower signal-to-noise ratio observations. Using line ratios for electron temperature, electron density, and column density we have found that the shock produced by the accelerating material in the accretion stream behaves as predicted by standard theory. However, the properties of the post-shock plasma differ substantially from the predictions of standard 1D shock models (Brickhouse et al. in Astrophys. J. 710:1835, 2010). The accretion process apparently heats the stellar atmosphere up to soft X-ray emitting temperatures, providing hot ions to populate the magnetic corona, in loops, stellar wind, and/or jets. This gas is highly turbulent, as evidenced by non-thermal line broadening. The observed properties of the accretion-fed corona should constrain theoretical models of an accretion-driven dynamo.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Brickhouse, NS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM nbrickhouse@cfa.harvard.edu
OI Brickhouse, Nancy/0000-0002-8704-4473
FU NASA [Chandra GO7-8018X, NAS8-03060]
FX The author acknowledges collaborators S. R. Cranmer, A. K. Dupree,
G.J.M. Luna, and S.J. Wolk. This work was supported by Chandra GO7-8018X
from NASA to the Smithsonian Astrophysical Observatory (SAO) and by NASA
contract NAS8-03060 to SAO for the Chandra X-ray Center.
NR 23
TC 0
Z9 0
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0004-640X
J9 ASTROPHYS SPACE SCI
JI Astrophys. Space Sci.
PD NOV
PY 2011
VL 336
IS 1
BP 75
EP 79
DI 10.1007/s10509-010-0562-0
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844EZ
UT WOS:000296731800013
ER
PT J
AU Simpson, C
Kiessling, W
Mewis, H
Baron-Szabo, RC
Muller, J
AF Simpson, Carl
Kiessling, Wolfgang
Mewis, Heike
Baron-Szabo, Rosemarie C.
Mueller, Johannes
TI EVOLUTIONARY DIVERSIFICATION OF REEF CORALS: A COMPARISON OF THE
MOLECULAR AND FOSSIL RECORDS
SO EVOLUTION
LA English
DT Article
DE Diversification; extinction; fossils; molecular phylogenies; reef
corals; speciation
ID MARINE DIVERSITY; EXTINCTION RISK; RATES; PHYLOGENIES; ORIGINATION;
SPECIATION; SCLERACTINIA; MITOCHONDRIAL; RADIATIONS; MODELS
AB Understanding historical patterns of diversity dynamics is of paramount importance for many evolutionary questions. The fossil record has long been the only source of information on patterns of diversification, but the molecular record, derived from time-calibrated phylogenies, is becoming an important additional resource. Both fossil and molecular approaches have shortcomings and biases. These have been well studied for fossil data but much less so for molecular data and empirical comparisons between approaches are lacking. Here, we compare the patterns of diversification derived from fossil and molecular data in scleractinian reef coral species. We also assess the robustness of molecular diversification rates to poor taxon sampling. We find that the temporal pattern of molecular diversification rates is robust to incomplete sampling when rates are calculated per interval. The major obstacle of molecular methods is that rate estimates are distorted because diversification rates can never be negative, whereas the fossil record suffers from incomplete preservation and inconsistent taxonomy. Nevertheless, the molecular pattern of diversification is comparable to the pattern we observe in the fossil record, with the timing of major diversification pulses coinciding in each dataset. For example, both agree that the end-Triassic coral extinction was a catastrophic bottleneck in scleractinian evolution.
C1 [Simpson, Carl; Kiessling, Wolfgang; Mewis, Heike; Mueller, Johannes] Humboldt Univ, Museum Nat Kunde, Leibniz Inst, D-10115 Berlin, Germany.
[Baron-Szabo, Rosemarie C.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA.
RP Simpson, C (reprint author), Humboldt Univ, Museum Nat Kunde, Leibniz Inst, D-10115 Berlin, Germany.
EM carl.simpson@mfn-berlin.de; wolfgang.kiessling@mfn-berlin.de;
heike.mewis@mfn-berlin.de; actinacis@hotmail.com;
Johannes.mueller@mfn-berlin.de
RI Kiessling, Wolfgang/E-2259-2015; Muller, Johannes/A-6293-2017
OI Muller, Johannes/0000-0001-5801-856X
FU VolkswagenStiftung; DFG [KI 806/7-1]
FX We thank U. Merkel for contributing substantially to the coral
occurrence data and P. Harnik for comments. We also thank G. Hunt, A.
Miller, and two anonymous referees for constructive reviews. This work
was supported by the VolkswagenStiftung and DFG project # KI 806/7-1.
This is Paleobiology Database publication #135.
NR 56
TC 20
Z9 20
U1 2
U2 35
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0014-3820
J9 EVOLUTION
JI Evolution
PD NOV
PY 2011
VL 65
IS 11
BP 3274
EP 3284
DI 10.1111/j.1558-5646.2011.01365.x
PG 11
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 843VK
UT WOS:000296702800020
PM 22023591
ER
PT J
AU Higgins, L
Coddington, J
Goodnight, C
Kuntner, M
AF Higgins, Linden
Coddington, Jonathan
Goodnight, Charles
Kuntner, Matjaz
TI Testing ecological and developmental hypotheses of mean and variation in
adult size in nephilid orb-weaving spiders
SO EVOLUTIONARY ECOLOGY
LA English
DT Article
DE Female gigantism; Sexual size dimorphism; Nephilidae; Nephila;
Nephilengys
ID DWARF MALE SPIDERS; MALE BODY-SIZE; SEXUAL-DIMORPHISM; PHENOTYPIC
PLASTICITY; CONFIDENCE-INTERVALS; DEVELOPMENT TIME; REACTION NORMS;
SEASON LENGTH; GIANT FEMALE; CLAVIPES
AB Fecundity selection has been hypothesized to drive the evolution of female gigantism in the orb-weaving family Nephilidae. Several species of these spiders also exhibit large amounts of variation in size at maturity in one or both sexes. In this article, we attempt to detect correlations of mean and variation in adult size at a phylogenetic scale between the sexes and with latitude. We tested six predictions derived from three broad developmental, ecological, and age structure hypotheses, using independent contrasts and a recent species-level nephilid phylogeny as well as least squares and other conventional statistics: 1. In both sexes, species with larger mean size will have greater variation in size; 2. Males and females will show correlated changes in mean size and of variation in size; 3. In both sexes, mean size will be negatively correlated with the midpoint of the latitudinal range; 4. In both sexes, tropical species will be more variable; 5. In both sexes, more widespread species will be more variable; 6. Variation in male size will be positively correlated with mean female size. In no cases were male and female development correlated, suggesting that in this lineage male and female body size evolve independently. The only significant trend detected was a positive phylogenetic correlation between variation in female size and latitude, the opposite of prediction 4. Power tests showed that in all tests of the ecological hypothesis, sample sizes were more than adequate to detect significant trends, if present. Our results suggest that evolutionary trends in juvenile development among species are too weak to be detectable in such data sets.
C1 [Higgins, Linden; Goodnight, Charles] Univ Vermont, Dept Biol, Burlington, VT 05405 USA.
[Coddington, Jonathan] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Ljubljana, Slovenia.
RP Higgins, L (reprint author), Univ Vermont, Dept Biol, Burlington, VT 05405 USA.
EM Linden.Higgins@uvm.edu; coddington@si.edu; Charles.Goodnight@uvm.edu;
kuntner@gmail.com
FU US National Science Foundation [INT-1235778, DEB-9712353, EAR-0228699];
Slovenian Research Agency [Z1-7082-0618, BI-US/06-07-026]; European
Commission [MIRG-CT-2005 036536]
FX We are grateful to many people for help in the preparation of this
manuscript, especially numerous patient curators. Financial support
during the collection of data and preparation of the manuscript came
from the US National Science Foundation with grants to LEH (INT-1235778)
and JC (PEET grant DEB-9712353 and EAR-0228699), from the Slovenian
Research Agency to MK and JC (ARRS grants Z1-7082-0618, BI-US/06-07-026)
and the European Commission's 6th FP to MK (MIRG-CT-2005 036536). From
the Smithsonian NMNH, D. DeRoche helped with the specimen management and
K. Darrow prepared all the figures. Specimen measurements and data entry
were done in part by M. Gregoric. (Ljubljana) and A. Gallant Bernstein,
J. Madden, R. Webber, B. Mulcahey and S. Wanamaker at UVM. Additional
data were graciously contributed by J. Schneider, M. Elgar, and H.
Japyassu. T. Garland and P. Midford helped us navigate the intricacies
of PDAP within Mesquite. Conversations with K. Pickett also aided in our
understanding of the statistics employed in these analyses. Comments
from several anonymous reviewers were very helpful in preparation of the
final manuscript.
NR 58
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U1 2
U2 19
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0269-7653
J9 EVOL ECOL
JI Evol. Ecol.
PD NOV
PY 2011
VL 25
IS 6
BP 1289
EP 1306
DI 10.1007/s10682-011-9475-9
PG 18
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 834RV
UT WOS:000295982300008
ER
PT J
AU Ivanenko, VN
Defaye, D
Segonzac, M
Khripounoff, A
Sarrazin, J
Ferrari, FD
AF Ivanenko, Viatcheslav N.
Defaye, Danielle
Segonzac, Michel
Khripounoff, Alexis
Sarrazin, Jozee
Ferrari, Frank D.
TI A new species of Exrima, synonymy of four species of Aphotopontius,
Stygiopontius and Rhogobius, and record of first copepodid stage of
Dirivultidae (Copepoda: Siphonostomatoida) from deep-sea hydrothermal
vents of the East Pacific Rise (13 degrees N)
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
DE Copepoda; Siphonostomatoida; Dirivultidae; new species; synonymy; new
records; deep-sea; hydrothermal vents; East Pacific Rise; Mid-Atlantic
Ridge
ID MID-ATLANTIC RIDGE; N-SP COPEPODA; NORTHEASTERN PACIFIC; COLD SEEPS;
FAMILY; WATER; ASTEROCHERIDAE; HARPACTICOIDA; SITES; GENUS
AB Females of the new species Exrima walteri sp. nov. were found in sediment trap samples deployed over different sites of the East Pacific Rise (13 degrees N) at 2600 m depth. Four traps were deposited during the HOPE99 cruise (1999) and recovered during the AMISTAD (1999) cruise on the research vessel 'L'Atalante'. The new species is distinguished from congeners, E. singula Humes, 1987 and E. dolichopus Humes, 1987, by the following derived characters: first somite of the urosome with 3 (one dorsal and two lateral) stout conical extensions; distal endopodal segment on the swimming leg 4 broad. In addition, many specimens of copepodids I and lecithotrophic nauplii, identified as belonging to Dirivultidae gen. sp., were found in the samples of all sediment traps. This is the first record of copepodids I and of a nauplius of dirivultids from the Pacific Ocean. Study of type and additional material collected during different Ifremer cruises at different vent sites (HERO91, EXOMAR, PHARE and MoMARETO) required synonymy of four species of Aphotopontius Humes, 1987, Stygiopontius Humes, 1987 and Rhogobius Humes, 1987. Aphotopontius rapunculus Humes and Segonzac, 1998 is transferred to the genus Rhogobius because it possesses all presumed derived attributes of this genus: last abdominal somite with lobes at sides of anal operculum; second segment of antennal endopod elongate and slender. A new study of the type material suggests that: Aphotopontius temperatus Humes, 1997 is a synonym of A. atlanteus Humes, 1996; Stygiopontius lumiger Humes, 1989 is a synonym of S. sentifer Humes, 1987 while S. bulbisetiger Humes, 1996 is a synonym of S. pectinatus Humes, 1987. Females of the three synonymized species were found to be sub-adult females at copepodid V. Leg 6 on these specimens is one seta located dorsolaterally on the posterior part of the genital somite. This position for leg 6 is unknown for copepodid V of other siphonostomatoids whose leg 6 is located ventrally at copepodid V; the dorsolateral position is presumed derived and shared by the dirivultid genera Aphotopontius Humes, 1987 and Stygiopontius Humes, 1987. A new key to the Dirivultidae genera is presented.
C1 [Ivanenko, Viatcheslav N.] Moscow MV Lomonosov State Univ, Dept Invertebrate Zool, Fac Biol, Moscow 119899, Russia.
[Defaye, Danielle; Segonzac, Michel] Museum Natl Hist Nat, Dept Milieux & Peuplements Aquat, UMR 7208, F-75005 Paris, France.
[Khripounoff, Alexis; Sarrazin, Jozee] IFREMER, Dept Etude Ecosyst Profonds, Lab Environm Profond, Ctr Brest, F-29280 Plouzane, France.
[Ferrari, Frank D.] Smithsonian Inst, IZ MSC, Natl Museum Nat Hist, Suitland, MD 20746 USA.
RP Ivanenko, VN (reprint author), Moscow MV Lomonosov State Univ, Dept Invertebrate Zool, Fac Biol, Moscow 119899, Russia.
EM ivanenko@mail.bio.msu.ru
RI Ivanenko, Viatcheslav/B-8198-2008; MNHN/CNRS/UPMC/IRD, UMR
BOREA/B-2312-2012
OI Ivanenko, Viatcheslav/0000-0003-1255-0491;
FU Museum National d'Histoire Naturelle and Ifremer (France); Smithsonian
Institution (USA); Russian Foundation for Basic Research
[09-04-01523-a]; Ministry of Education and Science of the Russian
Federation [02.740.11.0280, H1291, 02.740.11.0875]; AMORES [MAST3 CT
95-0040]; EXOCET/D
FX The authors are indebted to the chief scientists of the cruises HERO91
(chief scientist Daniel Desbruyeres), AMISTAD (chief scientist Christian
Jeanthon), HOPE99 (chief scientist Francois Lallier), PHARE
(chief scientist Nadine Le Bris), EXOMAR (chief scientist Anne Godfroy),
and MoMARETO (chief scientists Jozee Sarrazin and Pierre-Marie
Sarradin); the crews of the research vessels 'Nadir', 'L'Atalante' and
'Pourquoi Pas?' and of the manned submersible 'Nautile', and the
remotely operated vehicle 'Victor 6000'. The cruises were supported by
European programmes AMORES (MAST3 CT 95-0040) and EXOCET/D. Philippe
Crassous (Ifremer DEEP) prepared sampling arrays; Patrick Briand
(Ifremer DEEP) provided sorted material and data obtained during
colonization experiments. This work was supported by grants from the
Museum National d'Histoire Naturelle and Ifremer (France), Smithsonian
Institution (USA), the Russian Foundation for Basic Research
(09-04-01523-a), and the Ministry of Education and Science of the
Russian Federation (02.740.11.0280, H1291, 02.740.11.0875).
NR 35
TC 2
Z9 2
U1 0
U2 8
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0025-3154
EI 1469-7769
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD NOV
PY 2011
VL 91
IS 7
BP 1547
EP 1559
DI 10.1017/S0025315411000178
PG 13
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 837VI
UT WOS:000296233300016
ER
PT J
AU Cardoso, NA
Le Pendu, Y
Lapenta, MJ
Raboy, BE
AF Cardoso, Nayara A.
Le Pendu, Yvonnick
Lapenta, Marina J.
Raboy, Becky E.
TI Frugivory patterns and seed dispersal by golden-headed lion tamarins
(Leontopithecus chrysomelas) in Una Biological Reserve, Bahia, Brazil
SO MAMMALIA
LA English
DT Article
DE Atlantic forest; frugivory; Leontopithecus chrysomelas; primates; seed
dispersal; South America
ID SAGUINUS-FUSCICOLLIS; SOUTHEASTERN BRAZIL; SYMPATRIC PRIMATES;
ALOUATTA-SENICULUS; ATLANTIC FOREST; SOUTHERN BAHIA; RAIN-FOREST;
MONKEYS; BLACK; GERMINATION
AB This study identified fruit species eaten by Leontopithecus chrysomelas (golden-headed lion tamarins; GHLTs) and related their consumption to seed dispersal. Two GHLT groups were monitored from September 2006 through August 2007 in Una Biological Reserve, Bahia, Brazil. GHLTs consumed fruit from 71 species, preferred mature fruit and swallowed the seeds of most species (76.8%). Smaller seeds were swallowed and larger seeds were generally discarded. GHLTs defecated in low quantities and more than 50% of the faeces contained seeds from only one species. Most faeces were deposited far from the parental tree (>20m) and only 24.2% under the parental tree. The defecation pattern of L. chrysomelas could reduce competition between seeds and facilitate the establishment of seedlings from the most consumed species. Faeces were deposited widely throughout home ranges and away from a seed's parental tree increasing the chances that seeds reach favourable environments and avoid competition with other seedlings. Additionally, defecations also occurred in the same habitat type as a seed's parental tree, keeping species within their typical habitat. GHLTs in Una Biological Reserve were efficient dispersers and might play an important role in the maintenance of floristic composition and regeneration of habitat.
C1 [Cardoso, Nayara A.; Le Pendu, Yvonnick] Univ Estadual Santa Cruz, Dept Biol, BR-45662900 Ilheus, Bahia, Brazil.
[Lapenta, Marina J.] Inst Pri Matas Conservcao Biodiversidade, BR-30140970 Belo Horizonte, MG, Brazil.
[Raboy, Becky E.] Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
RP Cardoso, NA (reprint author), Univ Estadual Santa Cruz, Dept Biol, Rodovia Ilheus Itabuna,Km 16, BR-45662900 Ilheus, Bahia, Brazil.
EM nayara_cardoso@yahoo.com.br
RI Le Pendu, Yvonnick/B-3463-2008
FU FAPESB [1629/2006]
FX Field work was carried out within the infrastructure of the
Golden-Headed Lion Tamarin Project (PIs B.E. Raboy and J.M. Dietz). We
thank the Instituto de Estudos Socioambientais do Sul da Bahia (IESB)
and Universidade Estadual de Santa Cruz (UESC)-Zoology Postgraduate
Program for providing institutional and logistic support. We thank IBAMA
for the permission to work in Una Biological Reserve (Licence number
12279-1) and FAPESB for the scholarship grant to N.A. Cardoso (Term
1629/2006). We are extremely grateful to Gilvan Gomes Mota and Jiomario
dos Santos Souza for their field assistance and to James Dietz, Lilian
Catenacci, Kristel De Vleeschouwer, Leonardo Neves and Carlos Guidorizzi
for their assistance with GHLT captures and/or processing during the
study period.
NR 63
TC 3
Z9 3
U1 4
U2 33
PU WALTER DE GRUYTER & CO
PI BERLIN
PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY
SN 0025-1461
J9 MAMMALIA
JI Mammalia
PD NOV
PY 2011
VL 75
IS 4
BP 327
EP 337
DI 10.1515/MAMM.2011.042
PG 11
WC Zoology
SC Zoology
GA 844RQ
UT WOS:000296765400003
ER
PT J
AU Pre, CG
Culver, SJ
Mallinson, DJ
Farrell, KM
Corbett, DR
Horton, BP
Hillier, C
Riggs, SR
Snyder, SW
Buzas, MA
AF Pre, Candace Grand
Culver, Stephen J.
Mallinson, David J.
Farrell, Kathleen M.
Corbett, D. Reide
Horton, Benjamin P.
Hillier, Caroline
Riggs, Stanley R.
Snyder, Scott W.
Buzas, Martin A.
TI Rapid Holocene coastal change revealed by high-resolution
micropaleontological analysis, Pamlico Sound, North Carolina, USA
SO QUATERNARY RESEARCH
LA English
DT Article
DE Foraminifera; Diatoms; Holocene; Paleoenvironments
ID RADIOCARBON AGE CALIBRATION; RECENT ENVIRONMENTAL-CHANGE; CAL KYR BP;
OUTER BANKS; BENTHIC FORAMINIFERA; ALBEMARLE EMBAYMENT; UNITED-STATES;
CLIMATE; RECORD; ISLAND
AB Foraminiferal analyses of 404 contiguous samples, supported by diatom, lithologic, geochronologic and seismic data, reveal both rapid and gradual Holocene paleoenvironmental changes in an 8.21-m vibracore taken from southern Pamlico Sound, North Carolina. Data record initial flooding of a latest Pleistocene river drainage and the formation of an estuary 9000 yr ago. Estuarine conditions were punctuated by two intervals of marine influence from approximately 4100 to 3700 and 1150 to 500 cal yr BP. Foraminiferal assemblages in the muddy sand facies that accumulated during these intervals contain many well-preserved benthic foraminiferal species, which occur today in open marine settings as deep as the mid shelf, and significant numbers of well-preserved planktonic foraminifera, some typical of Gulf Stream waters. We postulate that these marine-influenced units resulted from temporary destruction of the southern Outer Banks barrier islands by hurricanes. The second increase in marine influence is coeval with increased rate of sea-level rise and a peak in Atlantic tropical cyclone activity during the Medieval Climate Anomaly. This high-resolution analysis demonstrates the range of environmental variability and the rapidity of coastal change that can result from the interplay of changing climate, sea level and geomorphology in an estuarine setting. (C) 2011 University of Washington. Published by Elsevier Inc. All rights reserved.
C1 [Pre, Candace Grand; Culver, Stephen J.; Mallinson, David J.; Corbett, D. Reide; Riggs, Stanley R.; Snyder, Scott W.] E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA.
[Pre, Candace Grand; Horton, Benjamin P.] Univ Penn, Sea Level Res Lab, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA.
[Farrell, Kathleen M.] N Carolina Geol Survey, Raleigh Field Off & Core Repository, Raleigh, NC 27699 USA.
[Corbett, D. Reide] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA.
[Hillier, Caroline] Argos Ecol Ltd, Annfield Plain, Durham DH9 7XN, England.
[Buzas, Martin A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
RP Culver, SJ (reprint author), E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA.
EM culvers@ecu.edu
FU Cushman Foundation; U.S. Geological Survey [02ERAG0044]; American
Chemical Society
FX We thank I. Abbene, D. Ames, J. Foley, J. Jett, M. Hale, K. McDowell, L
Metger, J. Ricardo, J. Rosenberger, C. Smith, D. Twamley, D. Vance, J.
Watson and J. Woods for their assistance. The efforts of Stephen
Gallagher and an anonymous reviewer are greatly appreciated. The Cushman
Foundation and the U.S. Geological Survey (cooperative agreement
02ERAG0044) provided funding for this project. Acknowledgement is also
made to the donors of The American Chemical Society Petroleum Research
Fund for partial support of this research.
NR 68
TC 7
Z9 7
U1 2
U2 30
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0033-5894
J9 QUATERNARY RES
JI Quat. Res.
PD NOV
PY 2011
VL 76
IS 3
BP 319
EP 334
DI 10.1016/j.yqres.2011.06.012
PG 16
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 843LA
UT WOS:000296672100004
ER
PT J
AU Gowaty, PA
AF Gowaty, Patricia Adair
TI What is sexual selection and the short herstory of female trait
variation
SO BEHAVIORAL ECOLOGY
LA English
DT Editorial Material
DE sexual selection
ID BLUEBIRDS SIALIA-SIALIS; DECREASE OFFSPRING VIABILITY; EASTERN
BLUEBIRDS; MATE PREFERENCES; REPRODUCTIVE COMPENSATION;
ANAS-PLATYRHYNCHOS; CONSTRAINTS; AGGRESSION; HYPOTHESIS; MALLARDS
C1 [Gowaty, Patricia Adair] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Gowaty, Patricia Adair] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA 90095 USA.
[Gowaty, Patricia Adair] Smithsonian Trop Res Inst, Unit 9100, DPO, AA 34002 USA.
RP Gowaty, PA (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr S, Los Angeles, CA 90095 USA.
EM gowaty@eeb.ucla.edu
NR 16
TC 1
Z9 1
U1 9
U2 37
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1045-2249
J9 BEHAV ECOL
JI Behav. Ecol.
PD NOV-DEC
PY 2011
VL 22
IS 6
BP 1146
EP 1147
DI 10.1093/beheco/arr113
PG 2
WC Behavioral Sciences; Biology; Ecology; Zoology
SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics;
Environmental Sciences & Ecology; Zoology
GA 838MB
UT WOS:000296295000007
ER
PT J
AU Knudsen, E
Linden, A
Both, C
Jonzen, N
Pulido, F
Saino, N
Sutherland, WJ
Bach, LA
Coppack, T
Ergon, T
Gienapp, P
Gill, JA
Gordo, O
Hedenstroom, A
Lehikoinen, E
Marra, PP
Moller, AP
Nilsson, ALK
Peron, G
Ranta, E
Rubolini, D
Sparks, TH
Spina, F
Studds, CE
Saether, SA
Tryjanowski, P
Stenseth, NC
AF Knudsen, Endre
Linden, Andreas
Both, Christiaan
Jonzen, Niclas
Pulido, Francisco
Saino, Nicola
Sutherland, William J.
Bach, Lars A.
Coppack, Timothy
Ergon, Torbjorn
Gienapp, Phillip
Gill, Jennifer A.
Gordo, Oscar
Hedenstrom, Anders
Lehikoinen, Esa
Marra, Peter P.
Moller, Anders P.
Nilsson, Anna L. K.
Peron, Guillaume
Ranta, Esa
Rubolini, Diego
Sparks, Tim H.
Spina, Fernando
Studds, Colin E.
Saether, Stein A.
Tryjanowski, Piotr
Stenseth, Nils Chr.
TI Challenging claims in the study of migratory birds and climate change
SO BIOLOGICAL REVIEWS
LA English
DT Article
DE bird migration; climate change; phenology; annual life cycle;
match-mismatch; endogenous control; phenotypic plasticity;
microevolutionary change; population trends; integrative biology
ID NORTH-ATLANTIC OSCILLATION; LONG-DISTANCE MIGRANTS; SPRING ARRIVAL
DATES; TERM POPULATION DECLINES; STORKS CICONIA-CICONIA; WEST-AFRICAN
RAINFALL; AVIAN MIGRATION; NATURAL-SELECTION; AMERICAN BIRDS; BARN
SWALLOW
AB Recent shifts in phenology in response to climate change are well established but often poorly understood. Many animals integrate climate change across a spatially and temporally dispersed annual life cycle, and effects are modulated by ecological interactions, evolutionary change and endogenous control mechanisms. Here we assess and discuss key statements emerging from the rapidly developing study of changing spring phenology in migratory birds. These well-studied organisms have been instrumental for understanding climate-change effects, but research is developing rapidly and there is a need to attack the big issues rather than risking affirmative science. Although we agree poorly on the support for most claims, agreement regarding the knowledge basis enables consensus regarding broad patterns and likely causes. Empirical data needed for disentangling mechanisms are still scarce, and consequences at a population level and on community composition remain unclear. With increasing knowledge, the overall support ('consensus view') for a claim increased and between-researcher variability in support ('expert opinions') decreased, indicating the importance of assessing and communicating the knowledge basis. A proper integration across biological disciplines seems essential for the field's transition from affirming patterns to understanding mechanisms and making robust predictions regarding future consequences of shifting phenologies.
C1 [Knudsen, Endre; Ergon, Torbjorn; Nilsson, Anna L. K.; Saether, Stein A.; Stenseth, Nils Chr.] Univ Oslo, CEES, Dept Biol, NO-0316 Oslo, Norway.
[Linden, Andreas; Ranta, Esa] Univ Helsinki, Dept Biol & Environm Sci, Integrat Ecol Unit, FIN-00014 Helsinki, Finland.
[Both, Christiaan] Univ Groningen, Ctr Ecol & Evolutionary Studies, Anim Ecol Grp, NL-9750 AA Haren, Netherlands.
[Jonzen, Niclas; Hedenstrom, Anders] Lund Univ, Dept Biol, SE-22362 Lund, Sweden.
[Pulido, Francisco; Gordo, Oscar] Univ Complutense Madrid, Dept Zool & Phys Anthropol, Fac Biol, E-28040 Madrid, Spain.
[Saino, Nicola; Rubolini, Diego] Univ Milan, Dipartimento Biol, I-20133 Milan, Italy.
[Sutherland, William J.] Univ Cambridge, Dept Zool, Conservat Sci Grp, Cambridge CB2 3EJ, England.
[Bach, Lars A.] Lund Univ, Dept Theoret Ecol, SE-22362 Lund, Sweden.
[Coppack, Timothy] Univ Zurich, Zool Museum, CH-8057 Zurich, Switzerland.
[Gienapp, Phillip] Univ Helsinki, Dept Biol & Environm Sci, Ecol Genet Res Unit, FIN-00014 Helsinki, Finland.
[Gill, Jennifer A.] Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England.
[Lehikoinen, Esa] Univ Turku, Sect Ecol, Turku 20014, Finland.
[Marra, Peter P.; Studds, Colin E.] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
[Moller, Anders P.] Univ Paris 11, Lab Ecol Syst & Evolut, F-91405 Orsay, France.
[Peron, Guillaume] CNRS, Ctr Ecol Fonct & Evolut, Equipe Biometrie & Biol Populat, UMR 5175, F-34293 Montpellier, France.
[Sparks, Tim H.; Tryjanowski, Piotr] Poznan Univ Life Sci, Inst Zool, PL-60625 Poznan, Poland.
[Spina, Fernando] Ist Super Protez Ric Ambientale, I-40064 Ozzano Dell Emilia, Italy.
RP Stenseth, NC (reprint author), Univ Oslo, CEES, Dept Biol, POB 1066 Blindern, NO-0316 Oslo, Norway.
EM n.c.stenseth@bio.uio.no
RI Both, Christiaan/E-6459-2011; Studds, Colin/C-3701-2012; Pulido,
Francisco/C-6697-2012; Coppack, Timothy/D-1204-2010; Gordo,
Oscar/A-4701-2013; Sutherland, William/B-1291-2013; PERON,
Guillaume/C-5379-2013; Gienapp, Phillip/A-2261-2014; Gill,
Jennifer/A-7759-2008; Hedenstrom, Anders/F-5377-2010; Evolution and
Conservation Biology, UCM Group /K-9382-2014; Rubolini,
Diego/F-2851-2011; Lehikoinen, Esa /I-6128-2013; Stenseth, Nils
Chr./G-5212-2016; Linden, Andreas/D-9315-2017;
OI Pulido, Francisco/0000-0002-2430-8080; Gordo, Oscar/0000-0003-3766-0566;
Gienapp, Phillip/0000-0002-9368-8769; Hedenstrom,
Anders/0000-0002-1757-0945; Rubolini, Diego/0000-0003-2703-5783;
Lehikoinen, Esa /0000-0002-6932-3604; Stenseth, Nils
Chr./0000-0002-1591-5399; Linden, Andreas/0000-0002-5548-2671; Linden,
Anthony/0000-0002-9343-9180; Bach, Lars A./0000-0001-8610-7834;
Sutherland, William/0000-0002-6498-0437; Sparks,
Tim/0000-0003-4382-7051; Nilsson, Anna/0000-0002-5609-4988; Saino,
Nicola/0000-0002-0230-3967
FU NordForsk through the Nordic Centre of Excellence EcoClim
FX E.K., A.L., N.J., L.B., T.E., N.C.S. and two meetings were partially
funded by NordForsk through the Nordic Centre of Excellence EcoClim. We
thank collaborators and field workers inside and outside academia for
thought-provoking long-term data and discussions, and the reviewers for
comments and suggestions that helped improve the manuscript.
NR 237
TC 124
Z9 125
U1 20
U2 256
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1464-7931
EI 1469-185X
J9 BIOL REV
JI Biol. Rev.
PD NOV
PY 2011
VL 86
IS 4
BP 928
EP 946
DI 10.1111/j.1469-185X.2011.00179.x
PG 19
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 840XL
UT WOS:000296475300010
PM 21489123
ER
PT J
AU Mascaro, J
Litton, CM
Hughes, RF
Uowolo, A
Schnitzer, SA
AF Mascaro, Joseph
Litton, Creighton M.
Hughes, R. Flint
Uowolo, Amanda
Schnitzer, Stefan A.
TI Minimizing Bias in Biomass Allometry: Model Selection and
Log-transformation of Data
SO BIOTROPICA
LA English
DT Article
DE allometry; Hawai'i; heteroscedasticity; linear regression; nonlinear
regression analysis; Psidium cattleianum
ID LOGARITHMIC TRANSFORMATION; FORESTS; HAWAII; INVASION; PLANTS
AB Nonlinear regression is increasingly used to develop allometric equations for forest biomass estimation (i.e., as opposed to the traditional approach of log-transformation followed by linear regression). Most statistical software packages, however, assume additive errors by default, violating a key assumption of allometric theory and possibly producing spurious models. Here, we show that such models may bias stand-level biomass estimates by up to 100 percent in young forests, and we present an alternative nonlinear fitting approach that conforms with allometric theory.
C1 [Mascaro, Joseph] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 96025 USA.
[Mascaro, Joseph; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama.
[Mascaro, Joseph; Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53211 USA.
[Litton, Creighton M.] Univ Hawaii Manoa, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA.
[Hughes, R. Flint; Uowolo, Amanda] US Forest Serv, Inst Pacific Isl Forestry, USDA, Hilo, HI 96720 USA.
RP Mascaro, J (reprint author), Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 96025 USA.
EM jmascaro@stanford.edu
OI Schnitzer, Stefan/0000-0002-2715-9455
FU Applied Ecological Services Inc.; NSF; UWM; National Science Foundation
[DEB-0816486]
FX Jim Baldwin (USFS-PSW) provided assistance fitting models. J. Mascaro
was supported by a grant from Applied Ecological Services Inc., an NSF
Graduate Research Fellowship, and a UWM Golda Meir Library Scholar
Award. Additional support was provided by a grant from the National
Science Foundation to C. M. Litton (DEB-0816486). Comments from four
anonymous reviewers improved this manuscript.
NR 17
TC 27
Z9 29
U1 8
U2 37
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0006-3606
J9 BIOTROPICA
JI Biotropica
PD NOV
PY 2011
VL 43
IS 6
BP 649
EP 653
DI 10.1111/j.1744-7429.2011.00798.x
PG 5
WC Ecology
SC Environmental Sciences & Ecology
GA 846NF
UT WOS:000296909800001
ER
PT J
AU Yanoviak, SP
Berghoff, SM
Linsenmair, KE
Zotz, G
AF Yanoviak, Stephen P.
Berghoff, Stefanie M.
Linsenmair, K. Eduard
Zotz, Gerhard
TI Effects of an Epiphytic Orchid on Arboreal Ant Community Structure in
Panama
SO BIOTROPICA
LA English
DT Article
DE Annona glabra; Caularthron bilamellatum; myrmecophyte; tropical forest
ID TROPICAL RAIN-FOREST; SPECIES-DIVERSITY; ANNONA-GLABRA; CANOPY;
ABUNDANCE; NECTAR; INVERTEBRATES; ASSEMBLAGES; HYMENOPTERA; FORMICIDAE
AB Epiphytes are conspicuous structural elements of tropical forest canopies. Individual tree crowns in lowland forests may support more than 30 ant species, yet we know little about the effects of epiphytes on ant diversity. We examined the composition of arboreal ant communities on Annona glabra trees and their interactions with the epiphytic orchid Caularthron bilamellatum in Panama. We surveyed the ants on 73 trees (45 with C. bilamellatum and 28 lacking epiphytes) and recorded their nest sites and behavioral dominance at baits. We found a total of 49 ant species (in 20 genera), ranging 1-9 species per tree. Trees with C. bilamellatum had higher average (+SD) ant species richness (4.2 + 2.28) than trees without epiphytes (2.7 + 1.21). Hollow pseudobulbs (PBs) of C. bilamellatum were used as nest sites by 32 ant species, but only 43 percent of suitable PBs were occupied. Ant species richness increased with PB abundance in trees, but nest sites did not appear to be a limiting resource on A. glabra. We detected no close association between ants and the orchid. We conclude that higher ant species richness in the presence of the orchid is due to bottom-up effects, especially the year-round supply of extrafloral nectar. The structure of ant communities on A. glabra partly reflects interference competition among behaviorally dominant species and stochastic factors, as observed in other forests.
C1 [Yanoviak, Stephen P.] Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA.
[Berghoff, Stefanie M.; Linsenmair, K. Eduard] Univ Wurzburg, Theodor Boveri Inst, Dept Anim Ecol & Trop Biol, D-97074 Wurzburg, Germany.
[Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, D-26111 Oldenburg, Germany.
[Zotz, Gerhard] Smithsonian Trop Res Inst, Balboa, Panama.
RP Yanoviak, SP (reprint author), Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA.
EM spyanoviak@ualr.edu
FU University of Wurzburg (HSPIII); National Science Foundation
[IOS-0843120]
FX Critical input from Jack Longino and two anonymous reviewers improved
this paper. Comments from Ulrich Simon provided the inspiration for this
project and Jack Longino assisted with ant identifications. Oris
Acevedo, Hans Peter Heckrodt, Sabine Armsen, and the staff of the
Smithsonian Tropical Research Institute provided logistical support.
This work was supported by grants from the University of Wurzburg
(HSPIII) to SMB and the National Science Foundation (IOS-0843120) to
SPY.
NR 58
TC 9
Z9 9
U1 2
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0006-3606
EI 1744-7429
J9 BIOTROPICA
JI Biotropica
PD NOV
PY 2011
VL 43
IS 6
BP 731
EP 737
DI 10.1111/j.1744-7429.2011.00764.x
PG 7
WC Ecology
SC Environmental Sciences & Ecology
GA 846NF
UT WOS:000296909800011
ER
PT J
AU Farris, DW
Jaramillo, C
Bayona, G
Restrepo-Moreno, SA
Montes, C
Cardona, A
Mora, A
Speakman, RJ
Glascock, MD
Valencia, V
AF Farris, David W.
Jaramillo, Carlos
Bayona, German
Restrepo-Moreno, Sergio A.
Montes, Camilo
Cardona, Agustin
Mora, Andres
Speakman, Robert J.
Glascock, Michael D.
Valencia, Victor
TI Fracturing of the Panamanian Isthmus during initial collision with South
America
SO GEOLOGY
LA English
DT Article
ID NORTHERN ANDES; GEOCHEMICAL EVOLUTION; EASTERN CORDILLERA; WESTERN
PANAMA; LAND-BRIDGE; ARC; DEFORMATION; COLOMBIA; PLATE; STRATIGRAPHY
AB Tectonic collision between South America and Panama began at 23-25 Ma. The collision is significant because it ultimately led to development of the Panamanian Isthmus, which in turn had wide-ranging oceanic, climatic, biologic, and tectonic implications. Within the Panama Canal Zone, volcanic activity transitioned from hydrous mantle-wedge-derived arc magmatism to localized extensional arc magmatism at 24 Ma, and overall marks a permanent change in arc evolution. We interpret the arc geochemical change to result from fracturing of the Panama block during initial collision with South America. Fracturing of the Panama block led to localized crustal extension, normal faulting, sedimentary basin formation, and extensional magmatism in the Canal Basin and Bocas del Toro. Synchronous with this change, both Panama and inboard South America experienced a broad episode of exhumation indicated by ( U-Th)/He and fission-track thermochronology coupled with changing geographic patterns of sedimentary deposition in the Colombian Eastern Cordillera and Llanos Basin. Such observations allow for construction of a new tectonic model of the South America-Panama collision, northern Andes uplift and Panama orocline formation. Finally, synchroneity of Panama arc chemical changes and linked uplift indicates that onset of collision and Isthmus formation began earlier than commonly assumed.
C1 [Farris, David W.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Jaramillo, Carlos; Bayona, German; Restrepo-Moreno, Sergio A.; Montes, Camilo; Cardona, Agustin] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
[Bayona, German; Montes, Camilo; Cardona, Agustin] Corp Geol ARES, Bogota, Colombia.
[Restrepo-Moreno, Sergio A.] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA.
[Mora, Andres] Ecopetrol, Inst Colombiano Petr, Bucaramanga, Colombia.
[Speakman, Robert J.] Museum Conservat Inst, Smithsonian Inst, Washington, DC 20012 USA.
[Glascock, Michael D.] Univ Missouri, Archaeometry Lab, Columbia, MO 65211 USA.
[Valencia, Victor] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
RP Farris, DW (reprint author), Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
OI Glascock, Michael D./0000-0003-0686-7556; Speakman,
Robert/0000-0003-2063-154X; Montes, Camilo/0000-0002-3553-0787
FU National Science Foundation (NSF) [0966884, DEB-0733725]; Smithsonian
Institution; Panama Canal Authority; National Geographic; SENACYT;
Ricardo Perez SA
FX This contribution to the Panama Canal Project (PCP) was supported by
National Science Foundation (NSF) PIRE grant 0966884 (OISE, EAR, DRL).
Funding also came from NSF grant DEB-0733725, the Smithsonian
Institution, the Panama Canal Authority, Mr. Mark Tupper, the National
Geographic, SENACYT, and Ricardo Perez SA. Thanks go to the Panama Canal
Authority, Ministerio de Industria y Comercio, Odebretch, and to the
Kuna Congress and Nation for access and logistical help.
NR 34
TC 110
Z9 112
U1 8
U2 52
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD NOV
PY 2011
VL 39
IS 11
BP 1007
EP 1010
DI 10.1130/G32237.1
PG 4
WC Geology
SC Geology
GA 842OA
UT WOS:000296607600006
ER
PT J
AU Lucking, R
Schulz, K
Crespo, A
Nash, TH
Lumbsch, HT
AF Luecking, Robert
Schulz, Katja
Crespo, Ana
Nash, Thomas H.
Lumbsch, H. Thorsten
TI The Encyclopedia of Life (EOL) as a scientific resource and outreach
medium applied to the lichen family Parmeliaceae (Ascomycota:
Lecanorales)
SO LICHENOLOGIST
LA English
DT Article
DE BioSync; Index Fungorum; Hypogymnia; Menegazzia; Parmotrema
ID COMMUNICATION; FUTURE
AB A brief discussion of the Encyclopedia of Life and the LifeDesks websites as a means to assemble and publish species pages and taxonomic information on the internet, for both the scientific community and the public, is provided. The lichen family Parmeliaceae is the first large group of lichenized fungi for which a concerted effort is currently being undertaken to produce substantial content for the EOL.
C1 [Luecking, Robert; Lumbsch, H. Thorsten] Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA.
[Schulz, Katja] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA.
[Crespo, Ana] Univ Complutense Madrid, Fac Farm, Dept Biol Vegetal 2, E-28040 Madrid, Spain.
[Nash, Thomas H.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA.
RP Lucking, R (reprint author), Field Museum Nat Hist, Dept Bot, 1400 S Lake Shore Dr, Chicago, IL 60605 USA.
EM rlucking@fieldmuseum.org
RI Lumbsch, Thorsten/K-3573-2012; Crespo, Ana/N-6236-2014;
OI Lumbsch, Thorsten/0000-0003-1512-835X; Crespo, Ana/0000-0002-5271-0157;
Schulz, Katja/0000-0001-7134-3324
NR 31
TC 1
Z9 1
U1 0
U2 1
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND
SN 0024-2829
J9 LICHENOLOGIST
JI Lichenologist
PD NOV
PY 2011
VL 43
BP 503
EP 510
DI 10.1017/S0024282911000168
PN 6
PG 8
WC Plant Sciences; Mycology
SC Plant Sciences; Mycology
GA 841IL
UT WOS:000296505900002
ER
PT J
AU Kerr, KCR
AF Kerr, Kevin C. R.
TI Searching for evidence of selection in avian DNA barcodes
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Article
DE birds; cytochrome c oxidase; DNA barcode; mitochondrial DNA; purifying
selection; selective sweep
ID ANIMAL MITOCHONDRIAL-DNA; CYTOCHROME-C-OXIDASE; NONNEUTRAL EVOLUTION;
NATURAL-SELECTION; POPULATION-SIZE; BIRDS; POLYMORPHISM; NEUTRALITY;
GENE; INTROGRESSION
AB The barcode of life project has assembled a tremendous number of mitochondrial cytochrome c oxidase I (COI) sequences. Although these sequences were gathered to develop a DNA-based system for species identification, it has been suggested that further biological inferences may also be derived from this wealth of data. Recurrent selective sweeps have been invoked as an evolutionary mechanism to explain limited intraspecific COI diversity, particularly in birds, but this hypothesis has not been formally tested. In this study, I collated COI sequences from previous barcoding studies on birds and tested them for evidence of selection. Using this expanded data set, I re-examined the relationships between intraspecific diversity and interspecific divergence and sampling effort, respectively. I employed the McDonald-Kreitman test to test for neutrality in sequence evolution between closely related pairs of species. Because amino acid sequences were generally constrained between closely related pairs, I also included broader intra-order comparisons to quantify patterns of protein variation in avian COI sequences. Lastly, using 22 published whole mitochondrial genomes, I compared the evolutionary rate of COI against the other 12 protein-coding mitochondrial genes to assess intragenomic variability. I found no conclusive evidence of selective sweeps. Most evidence pointed to an overall trend of strong purifying selection and functional constraint. The COI protein did vary across the class Aves, but to a very limited extent. COI was the least variable gene in the mitochondrial genome, suggesting that other genes might be more informative for probing factors constraining mitochondrial variation within species.
C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA.
RP Kerr, KCR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA.
EM kerrkc@si.edu
RI Kerr, Kevin/B-8510-2013
OI Kerr, Kevin/0000-0002-6784-3884
FU Ontario Graduate Scholarship; University of Guelph; NSERC; Genome Canada
FX This work was funded by an Ontario Graduate Scholarship and through the
author's thesis advisor at the University of Guelph, Paul Hebert, by
grants from NSERC and Genome Canada. I thank Justin Schonfeld for the
computational support necessary to produce the secondary structure
predictions. I thank Teresa Crease, Steve Lougheed and Paul Hebert for
helpful input and discussion. I thank Beren Robinson and Lee-Ann Hayek
for providing assistance with statistical methods. I also thank three
anonymous reviewers for comments on an earlier version of this
manuscript.
NR 58
TC 14
Z9 14
U1 0
U2 15
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1755-098X
J9 MOL ECOL RESOUR
JI Mol. Ecol. Resour.
PD NOV
PY 2011
VL 11
IS 6
BP 1045
EP 1055
DI 10.1111/j.1755-0998.2011.03049.x
PG 11
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 840EN
UT WOS:000296421200013
PM 21777399
ER
PT J
AU Richter, DD
Bacon, AR
Mobley, ML
Richardson, CJ
Andrews, SS
West, L
Wills, S
Billings, S
Cambardella, CA
Cavallaro, N
DeMeester, JE
Franzluebbers, AJ
Grandy, AS
Grunwald, S
Gruver, J
Hartshorn, AS
Janzen, H
Kramer, MG
Ladha, JK
Lajtha, K
Liles, GC
Markewitz, D
Megonigal, PJ
Mermut, AR
Rasmussen, C
Robinson, DA
Smith, P
Stiles, CA
Tate, RL
Thompson, A
Tugel, AJ
van Es, H
Yaalon, D
Zobeck, TM
AF Richter, Daniel deB
Bacon, Allan R.
Mobley, Megan L.
Richardson, Curtis J.
Andrews, Susan S.
West, Larry
Wills, Skye
Billings, Sharon
Cambardella, Cynthia A.
Cavallaro, Nancy
DeMeester, Julie E.
Franzluebbers, Alan J.
Grandy, A. Stuart
Grunwald, Sabine
Gruver, Joel
Hartshorn, Anthony S.
Janzen, Henry
Kramer, Marc G.
Ladha, Jagdish K.
Lajtha, Kate
Liles, Garrett C.
Markewitz, Daniel
Megonigal, Patrick J.
Mermut, Ahmet R.
Rasmussen, Craig
Robinson, David A.
Smith, Pete
Stiles, Cynthia A.
Tate, Robert L., III
Thompson, Aaron
Tugel, Arlene J.
van Es, Harold
Yaalon, Dan
Zobeck, Ted M.
TI Human-Soil Relations are Changing Rapidly: Proposals from SSSA's
Cross-Divisional Soil Change Working Group
SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL
LA English
DT Article
ID ECOSYSTEM SERVICES; FRAMEWORK; SCIENCE; AGRICULTURE; MANAGEMENT;
TRANSFORMATION; PERSPECTIVE; MITIGATION; DIVERSITY; AMERICA
AB A number of scientists have named our age the Anthropocene because humanity is globally affecting Earth systems, including the soil. Global soil change raises important questions about the future of soil, the environment, and human society. Although many soil scientists strive to understand human forcings as integral to soil genesis, there remains an explicit need for a science of anthropedology to detail how humanity is a fully fledged soil-forming factor and to understand how soil change affects human well being. The development and maturation of anthropedology is critical to achieving land-use sustainability and needs to be nurtured by all soil disciplines, with inputs from allied sciences and the humanities,. The Soil Science Society of America (SSSA) has recently approved a cross-divisional Working Group on Soil Change, which aims to advance the basic and applied science of anthropedology, to facilitate networks of scientists, long-term soil field studies, and regional databases and modeling, and to engage in new modes of communications about human-soil relations. We challenge all interested parties, especially young scientists and students, to contribute to these activities and help grow soil science in the Anthropocene.
C1 [Richter, Daniel deB; Bacon, Allan R.; Mobley, Megan L.; Richardson, Curtis J.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Andrews, Susan S.; West, Larry; Wills, Skye] USDA NRCS, Natl Soil Survey Ctr, Lincoln, NE 68508 USA.
[Billings, Sharon] Univ Kansas, Kansas Biol Survey, Dep Ecol & Evolutionary Biol, Lawrence, KS 66047 USA.
[Cambardella, Cynthia A.] USDA ARS, Natl Lab Agr & Environm, Ames, IA 50011 USA.
[Cavallaro, Nancy] Natl Inst Food & Agr, USDA, Washington, DC 20024 USA.
[Franzluebbers, Alan J.] USDA ARS, J Phil Campbell Sr Nat Resource Conservat Ctr, Watkinsville, GA 30677 USA.
[Grandy, A. Stuart] Univ New Hampshire, Dep Nat Resources & Environm, Durham, NH 03824 USA.
[Grunwald, Sabine] Univ Florida, Soil & Water Sci Dep, Gainesville, FL 32611 USA.
[Gruver, Joel] Western Illinois Univ, Sch Agr, Macomb, IL 61455 USA.
[Hartshorn, Anthony S.] James Madison Univ, Dep Geol & Environm Sci, Harrisonburg, VA 22807 USA.
[Janzen, Henry] Agr & Agri Food Canada, Lethbridge Res Ctr, Lethbridge, AB T1J 4B1, Canada.
[Kramer, Marc G.] USDA Forest Serv, Portland, OR 97204 USA.
[Ladha, Jagdish K.] IRRI, New Delhi 110012, India.
[Lajtha, Kate] Oregon State Univ, Dep Crop & Soil Sci, Corvallis, OR 97331 USA.
[Liles, Garrett C.] Univ Calif Davis, Dep Land Air & Water Resources, Davis, CA 95616 USA.
[Markewitz, Daniel] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA.
[Megonigal, Patrick J.] Smithsonian Inst, Smithsonian Environm Res Ctr, Washington, DC 20013 USA.
[Mermut, Ahmet R.] Univ Saskatchewan, Dep Soil Sci, Saskatoon, SK S7N 5A2, Canada.
[Rasmussen, Craig] Univ Arizona, Dep Soil Water & Environm Sci, Tucson, AZ 85721 USA.
[Robinson, David A.] Environm Ctr Wales, Ctr Ecol & Hydrol, Bangor LL57 2UW, Gwynedd, Wales.
[Smith, Pete] Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland.
[Stiles, Cynthia A.] USDA NRCS, Pacific Isl Area State Off, Honolulu, HI 96850 USA.
[Tate, Robert L., III] Rutgers State Univ, Dep Environm Sci, New Brunswick, NJ 08901 USA.
[Thompson, Aaron] Univ Georgia, Dep Crop & Soil Sci, Athens, GA 30602 USA.
[Tugel, Arlene J.] USDA NRCS, Las Cruces, NM 88003 USA.
[van Es, Harold] Cornell Univ, Dep Crop & Soil Sci, Ithaca, NY 14853 USA.
[Yaalon, Dan] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel.
[Zobeck, Ted M.] USDA ARS, Cropping Syst Res Lab, Lubbock, TX 79415 USA.
RP Richter, DD (reprint author), Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
EM drichter@duke.edu
RI Robinson, David/A-6287-2010; Zobeck, Ted/A-6126-2012; Billings,
Sharon/I-5115-2013; Smith, Pete/G-1041-2010;
OI Robinson, David/0000-0001-7290-4867; Billings,
Sharon/0000-0003-1611-526X; Smith, Pete/0000-0002-3784-1124; Hartshorn,
Anthony/0000-0002-0004-5749
NR 85
TC 27
Z9 27
U1 4
U2 40
PU SOIL SCI SOC AMER
PI MADISON
PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA
SN 0361-5995
J9 SOIL SCI SOC AM J
JI Soil Sci. Soc. Am. J.
PD NOV
PY 2011
VL 75
IS 6
BP 2079
EP 2084
DI 10.2136/sssaj2011.0124
PG 6
WC Soil Science
SC Agriculture
GA 841ZK
UT WOS:000296553600005
ER
PT J
AU de Rivera, CE
Steves, BP
Fofonoff, PW
Hines, AH
Ruiz, GM
AF de Rivera, Catherine E.
Steves, Brian P.
Fofonoff, Paul W.
Hines, Anson H.
Ruiz, Gregory M.
TI Potential for high-latitude marine invasions along western North America
SO DIVERSITY AND DISTRIBUTIONS
LA English
DT Article
DE Abiotic resistance; Amphibalanus improvisus; biological invasions;
Carcinus maenas; environmental niche model; Littorina saxatilis; Styela
clava
ID SPECIES GEOGRAPHIC DISTRIBUTIONS; GLOBAL CLIMATE-CHANGE; CRAB
CARCINUS-MAENAS; LITTORINA-SAXATILIS; DISTRIBUTION MODELS; NICHE SHIFT;
PROPAGULE PRESSURE; INTRODUCED CRAB; PLANT INVASIONS; RANGE SHIFTS
AB Aim High-latitude regions host many fewer non-native species than temperate ones. The low invasion loads of these colder regions may change with increases in human-mediated propagule supply. We test the hypothesis that colonization by non-native species that have already invaded temperate shorelines would be precluded by environmental conditions if they were introduced to Alaska and other high-latitude regions by shipping or other vectors.
Location Pacific coast of North America as well as coastal oceans world-wide.
Methods Using 16 habitat descriptors in ecological niche models, we characterized the conditions throughout the native and introduced distributions of four marine species (Amphibalanus improvisus, Carcinus maenas, Littorina saxatilis and Styela clava) that have invaded multiple global regions to test the extent to which suitable conditions for these species exist in Alaska and other high-latitude regions under current and predicted future climate scenarios.
Results Models projected environmental match for all four species in many areas beyond their present range limits, suggesting that Alaska and other high-latitude shorelines are currently vulnerable to invasion by non-native species that occur in lower latitudes.
Main conclusions Given current and possibly increasing human-mediated species transfers and suitable environmental conditions that exist now and with projected warming, policy and management efforts are urgently needed to minimize invasion opportunities at high latitudes.
C1 [de Rivera, Catherine E.; Steves, Brian P.; Fofonoff, Paul W.; Hines, Anson H.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[de Rivera, Catherine E.; Steves, Brian P.; Ruiz, Gregory M.] Portland State Univ, Aquat Bioinvas Res & Policy Inst, Portland, OR 97207 USA.
RP de Rivera, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM derivera@pdx.edu
OI Ruiz, Gregory/0000-0003-2499-441X
FU Prince William Sound Regional Citizen's Advisory Council; U.S. Fish and
Wildlife Service
FX We thank Lisa Ka'aihue, Denny Lassuy, Bob Piorkowski and Linda Shaw for
comments. We also benefited from discussions with Chad Hewitt and
Whitman Miller. This project was funded by a grant to GMR, AHH and CED
from the Prince William Sound Regional Citizen's Advisory Council and by
U.S. Fish and Wildlife Service.
NR 75
TC 27
Z9 27
U1 3
U2 46
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1366-9516
J9 DIVERS DISTRIB
JI Divers. Distrib.
PD NOV
PY 2011
VL 17
IS 6
BP 1198
EP 1209
DI 10.1111/j.1472-4642.2011.00790.x
PG 12
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 836TG
UT WOS:000296134800012
ER
PT J
AU Visser, MD
Muller-Landau, HC
Wright, SJ
Rutten, G
Jansen, PA
AF Visser, Marco D.
Muller-Landau, Helene C.
Wright, S. Joseph
Rutten, Gemma
Jansen, Patrick A.
TI Tri-trophic interactions affect density dependence of seed fate in a
tropical forest palm
SO ECOLOGY LETTERS
LA English
DT Article
DE Attalea butyracea; Barro Colorado Island; enemies hypothesis; negative
density dependence; seed predation; specialization; species coexistence;
species diversity; trophic cascade; tropical forest
ID BARRO-COLORADO ISLAND; JANZEN-CONNELL MODEL; RAIN-FOREST;
SPECIES-DIVERSITY; NEOTROPICAL TREE; BRUCHID BEETLES; PLANT DIVERSITY;
PARENT PALM; DISPERSAL; PREDATION
AB Natural enemies, especially host-specific enemies, are hypothesised to facilitate the coexistence of plant species by disproportionately inflicting more damage at increasing host abundance. However, few studies have assessed such Janzen-Connell mechanisms on a scale relevant for coexistence and no study has evaluated potential top-down influences on the specialized pests. We quantified seed predation by specialist invertebrates and generalist vertebrates, as well as larval predation on these invertebrates, for the Neotropical palm Attalea butyracea across ten 4-ha plots spanning 20-fold variation in palm density. As palm density increased, seed attack by bruchid beetles increased, whereas seed predation by rodents held constant. But because rodent predation on bruchid larvae increased disproportionately with increasing palm density, bruchid emergence rates and total seed predation by rodents and bruchids combined were both density-independent. Our results demonstrate that top-down effects can limit the potential of host-specific insects to induce negative-density dependence in plant populations.
C1 [Visser, Marco D.; Muller-Landau, Helene C.; Wright, S. Joseph; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Visser, Marco D.; Jansen, Patrick A.] Univ Wageningen & Res Ctr, Forest Ecol & Forest Management Grp, Wageningen, Netherlands.
[Visser, Marco D.] Radboud Univ Nijmegen, Inst Water & Wetland Res, Dept Expt Plant Ecol, NL-6525 AJ Nijmegen, Netherlands.
[Rutten, Gemma] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland.
[Rutten, Gemma; Jansen, Patrick A.] Univ Groningen, Community & Conservat Ecol Grp, NL-9700 CC Groningen, Netherlands.
RP Visser, MD (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama.
EM m.visser@science.ru.nl
RI Wright, Stuart/M-3311-2013; Jansen, Patrick/G-2545-2015
OI Wright, Stuart/0000-0003-4260-5676; Jansen, Patrick/0000-0002-4660-0314
FU Smithsonian Tropical Research Institute; HSBC; David and Lucile Packard
Foundation; Netherlands Organization for Scientific Research
FX We thank Eric Oriel Vasquez, Christoph Gahr and Femke Maes for their
help in the field and laboratory, Carol Garzon-Lopez and Stephanie
Bohlman for providing the BCI crown maps, and Robert Holt, Rob Klinger
and two anonymous reviewers for helpful comments. We gratefully
acknowledge the financial support of the Smithsonian Tropical Research
Institute (MDV), the HSBC Climate Partnership (HCM), the David and
Lucile Packard Foundation (HCM) and the Netherlands Organization for
Scientific Research (PAJ).
NR 49
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U1 2
U2 40
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 NOV
PY 2011
VL 14
IS 11
BP 1093
EP 1100
DI 10.1111/j.1461-0248.2011.01677.x
PG 8
WC Ecology
SC Environmental Sciences & Ecology
GA 838CB
UT WOS:000296263200003
PM 21899693
ER
PT J
AU Hosaka, T
Yumoto, T
Chen, YY
Sun, IF
Wright, SJ
Noor, NSM
AF Hosaka, Tetsuro
Yumoto, Takakazu
Chen, Yu-Yun
Sun, I-Fang
Wright, S. Joseph
Noor, Nur Supardi Md
TI Abundance of insect seed predators and intensity of seed predation on
Shorea (Dipterocarpaceae) in two consecutive masting events in
Peninsular Malaysia
SO JOURNAL OF TROPICAL ECOLOGY
LA English
DT Article
DE Alcidodes; Andrioplecta; Dipterocarpaceae; general flowering;
Nanophyidae; population dynamics; predator satiation; pre-dispersal seed
predator; Shorea
ID RAIN-FOREST; BEETLES; PATTERNS; SARAWAK; BORNEO
C1 [Hosaka, Tetsuro] Kyoto Univ, Grad Sch Agr, Kyoto 6068502, Japan.
[Yumoto, Takakazu] Res Inst Humanity & Nat, Kyoto 6038047, Japan.
[Chen, Yu-Yun] Natl Tsing Hua Univ, Hsinchu 300, Taiwan.
[Sun, I-Fang] Tunghai Univ, Ctr Trop Ecol & Biodivers, Taichung 40704, Taiwan.
[Wright, S. Joseph] Smithsonian Trop Res Inst, Ancon, Panama.
[Noor, Nur Supardi Md] Forest Res Inst Malaysia, Kepong 52109, Selangor, Malaysia.
RP Hosaka, T (reprint author), Hiroshima Univ, Grad Sch Integrated Arts & Sci, Kagamiyama 1-7-1, Higashihiroshima 7398521, Japan.
EM hosaka@hiroshima-u.ac.jp
RI Yumoto, Takakazu/B-6215-2013; Wright, Stuart/M-3311-2013
OI Wright, Stuart/0000-0003-4260-5676
FU FRIM; National Institute for Environmental Studies, Japan [E-4];
Ministry of Education, Culture, Sports, Science and Technology of Japan;
US NSF [DEB-0108388]
FX We are grateful to Dr Laurence G. Kirton of the Forest Research
Institute of Malaysia (FRIM) for permission to conduct the research in
Pasoh. Special thanks are due to Dr Mamoru Kanzaki, Dr Naoya Osawa
(Kyoto University) and Dr Toshinori Okuda (Hiroshima University) for
their kind support. Dr Hiroaki Kojima and Mr Junnosuke Kanto (Tokyo
University of Agriculture) identified weevils and Dr Furumi Komai (Osaka
University of Arts) identified moths. This study was partly supported by
a joint research project of FRIM and the National Institute for
Environmental Studies, Japan: Grant No. E-4, Global Environmental
Research Program, Ministry of Education, Culture, Sports, Science and
Technology of Japan. Flower and seed rain data collection was supported
by the US NSF grant DEB-0108388 awarded to S. P. Hubbell and S. J.
Wright.
NR 23
TC 4
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U1 2
U2 29
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0266-4674
J9 J TROP ECOL
JI J. Trop. Ecol.
PD NOV
PY 2011
VL 27
BP 651
EP 655
DI 10.1017/S0266467411000393
PN 6
PG 5
WC Ecology
SC Environmental Sciences & Ecology
GA 837MS
UT WOS:000296208500011
ER
PT J
AU Fleischer, RC
AF Fleischer, Robert C.
TI Ladies and gentes: Maternally inherited DNA and ancient honeyguide host
races
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Editorial Material
ID MOLOTHRUS-BONARIENSIS; CUCKOO
C1 Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA.
RP Fleischer, RC (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20013 USA.
EM fleischerr@si.edu
NR 13
TC 1
Z9 1
U1 1
U2 24
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 1
PY 2011
VL 108
IS 44
BP 17859
EP 17860
DI 10.1073/pnas.1115041108
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 839NH
UT WOS:000296373400007
PM 22006330
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI Simple Pleasures
SO SMITHSONIAN
LA English
DT Article
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 NOV
PY 2011
VL 42
IS 7
BP 28
EP +
PG 3
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 837FS
UT WOS:000296177100013
ER
PT J
AU Osborn, KJ
Haddock, SHD
Rouse, GW
AF Osborn, Karen J.
Haddock, Steven H. D.
Rouse, Greg W.
TI Swima (Annelida, Acrocirridae), holopelagic worms from the deep Pacific
SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE Celebes Sea; Cirratuliformia; deep-sea; gelata; midwater; pelagic; Swima
bombiviridis; Swima fulgida sp nov.; Swima tawitawiensis sp nov.
ID FLABELLIGERIDAE ANNELIDA; POLYCHAETA; SUBSTITUTION; SEDENTARIA; MODEL
AB Two new species of Swima, a recently established genus of annelid worms, are introduced, one from deep water off the North American West Coast and the other from the Philippines. The acrocirrid genus now contains three named species, Swima bombiviridis, Swima fulgida sp. nov., and Swima tawitawiensis sp. nov. Swima are holopelagic, occurring only in the water column, and thus far have only been observed below 2700 m. The worms are relatively large, sometimes reaching over 30 mm in length and 5 mm in width. They have gelatinous bodies and fans of long swimming chaetae, which are flattened into paddles in S. tawitawiensis sp. nov. Members of Swima are distinguished from other swimming acrocirrids by their transparent bodies, single medial subulate branchiae, and simple nuchal organs that do not skirt the bases of lateral subulate branchiae. Swima fulgida sp. nov. is distinguished from other members of the genus by its darkly pigmented anterior gut, whereas S. tawitawiensis sp. nov. is distinguished by possessing three subulate head appendages instead of just one and by the shape of its noto- and neurochaetae. Swima species possess four pairs of elliptical, transformed segmental branchiae that produce green bioluminescence when autotomized. These 'bombs' were observed in various states of regeneration on a single individual. Swima are neutrally buoyant, often observed hanging immobile in the water column, and are active, agile swimmers. Although not previously documented in the literature, these worms are not rare in the deep water column. Since the worms were first noticed in 2001, they have been observed on more than half of the Monterey Bay Aquarium Research Institute's midwater remotely operated vehicle dives that went to sufficient depth. The discovery of Swima underscores our lack of knowledge of deep pelagic fauna. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 163, 663-678. doi: 10.1111/j.1096-3642.2011.00727.x
C1 [Osborn, Karen J.; Rouse, Greg W.] Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Haddock, Steven H. D.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA.
RP Osborn, KJ (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20052 USA.
EM osbornk@si.edu
RI Rouse, Greg/F-2611-2010;
OI Rouse, Greg/0000-0001-9036-9263; Osborn, Karen/0000-0002-4226-9257
FU Scripps Institution of Oceanography; University of California; David and
Lucile Packard Foundation; National Geographic Society; National Oceanic
and Atmospheric Administration; Woods Hole Oceanographic Institution
FX We would like to thank Bruce Robison of the Monterey Bay Aquarium
Research Institute for ship time made available for observation and
collection of several specimens. Thanks go to Larry Madin of Woods Hole
Oceanographic Institution, the science party, and crew aboard the R/V
Hydrographer Presbitero for their work in the Celebes Sea, for the
foresight to collect, photograph, and preserve for morphology and
molecular work the single specimen of S. tawitawiensis considered here.
Thanks go to the crew of the R/V Western Flyer, the pilots of the ROVs
Tiburon and Doc Ricketts, and the MBARI video lab staff for their
dedication to deep-sea exploration. We also thank Cynthia Claxton (UC
Irvine) for advice regarding Latin usage and form, although any errors
are the sole responsibility of the authors. Evelyn York's expertise on
the SEM was much appreciated. Scripps Institution of Oceanography funded
K. J. O. and G. W. R. and the University of California President's
Postdoctoral Fellowship supported K. J. O. The David and Lucile Packard
Foundation provided funding to the Monterey Bay Aquarium Research
Institute. The National Geographic Society, National Oceanic and
Atmospheric Administration, and Woods Hole Oceanographic Institution
provided funding for the Celebes Sea Expedition.
NR 34
TC 5
Z9 5
U1 1
U2 16
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-4082
J9 ZOOL J LINN SOC-LOND
JI Zool. J. Linn. Soc.
PD NOV
PY 2011
VL 163
IS 3
BP 663
EP 678
DI 10.1111/j.1096-3642.2011.00727.x
PG 16
WC Zoology
SC Zoology
GA 838BK
UT WOS:000296261300001
ER
PT J
AU Liu, Q
Triplett, JK
Wen, J
Peterson, PM
AF Liu, Qing
Triplett, Jimmy K.
Wen, Jun
Peterson, Paul M.
TI Allotetraploid origin and divergence in Eleusine (Chloridoideae,
Poaceae): evidence from low-copy nuclear gene phylogenies and a plastid
gene chronogram
SO ANNALS OF BOTANY
LA English
DT Article
DE Allotetraploid origin; chloroplast markers; East Africa; Eleusine;
low-copy nuclear markers; phylogeny; Poaceae
ID IN-SITU HYBRIDIZATION; FINGER MILLET; TRITICEAE GRAMINEAE; C-4
PHOTOSYNTHESIS; GENOME; DNA; EVOLUTIONARY; SEQUENCE; WILD; GRASSLANDS
AB Background and Aims Eleusine (Poaceae) is a small genus of the subfamily Chloridoideae exhibiting considerable morphological and ecological diversity in East Africa and the Americas. The interspecific phylogenetic relationships of Eleusine are investigated in order to identify its allotetraploid origin, and a chronogram is estimated to infer temporal relationships between palaeoenvironment changes and divergence of Eleusine in East Africa.
Methods Two low-copy nuclear (LCN) markers, Pepc4 and EF-1 alpha, were analysed using parsimony, likelihood and Bayesian approaches. A chronogram of Eleusine was inferred from a combined data set of six plastid DNA markers (ndhA intron, ndhF, rps16-trnK, rps16 intron, rps3, and rpl32-trnL) using the Bayesian dating method.
Key Results The monophyly of Eleusine is strongly supported by sequence data from two LCN markers. In the cpDNA phylogeny, three tetraploid species (E. africana, E. coracana and E. kigeziensis) share a common ancestor with the E. indica-E. tristachya clade, which is considered a source of maternal parents for allotetraploids. Two homoeologous loci are isolated from three tetraploid species in the Pepc4 phylogeny, and the maternal parents receive further support. The A-type EF-1 alpha sequences possess three characters, i.e. a large number of variations of intron 2; clade E-A distantly diverged from clade E-B and other diploid species; and seven deletions in intron 2, implying a possible derivation through a gene duplication event. The crown age of Eleusine and the allotetraploid lineage are 3.89 million years ago (mya) and 1.40 mya, respectively.
Conclusions The molecular data support independent allotetraploid origins for E. kigeziensis and the E. africana-E. coracana clade. Both events may have involved diploids E. indica and E. tristachya as the maternal parents, but the paternal parents remain unidentified. The habitat-specific hypothesis is proposed to explain the divergence of Eleusine and its allotetraploid lineage.
C1 [Liu, Qing] Chinese Acad Sci, Key Lab Plant Resources Conservat & Sustainable U, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China.
[Triplett, Jimmy K.] Jacksonville State Univ, Dept Biol, Jacksonville, AL 36265 USA.
[Wen, Jun; Peterson, Paul M.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Liu, Q (reprint author), Chinese Acad Sci, Key Lab Plant Resources Conservat & Sustainable U, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China.
EM liuqing@scib.ac.cn; peterson@si.edu
FU National Geographic Society Committee for Research and Exploration
[8087-06]; Smithsonian Institution, National Natural Science Foundation
of China [30700043]; China Scholarship Council [2008491004]; Key
Laboratory of Plant Resources Conservation and Sustainable Utilization
of Chinese Academy of Sciences [200922]; Chinese Academy of Sciences
[KSCX2-EW-J-28]
FX We thank USDA-Beltsville National Germplasm System, ILRI-Addis Ababa and
J. Travis Columbus for help with caryopsis and leaf collection; Lee
Weigt, Jeffery Hunt, Rong Li and Xinwei Xu for help in the laboratory;
Robert J. Soreng, Dianxiang Zhang, Gabriel Johnson and Tieyao Tu for
helpful discussions; and six anonymous reviewers for their constructive
comments that improved the manuscript. This work was supported by the
National Geographic Society Committee for Research and Exploration
(grant no. 8087-06), the Smithsonian Institution's Small Grants Program,
National Natural Science Foundation of China (no. 30700043), the China
Scholarship Council Awards (no. 2008491004), the Key Laboratory of Plant
Resources Conservation and Sustainable Utilization of Chinese Academy of
Sciences (no. 200922) and the Knowledge Innovation Program of the
Chinese Academy of Sciences (no. KSCX2-EW-J-28).
NR 77
TC 12
Z9 13
U1 3
U2 26
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0305-7364
J9 ANN BOT-LONDON
JI Ann. Bot.
PD NOV
PY 2011
VL 108
IS 7
BP 1287
EP 1298
DI 10.1093/aob/mcr231
PG 12
WC Plant Sciences
SC Plant Sciences
GA 836GN
UT WOS:000296098900007
PM 21880659
ER
PT J
AU O'Meara, C
Baez, GP
AF O'Meara, Carolyn
Perez Baez, Gabriela
TI Spatial frames of reference in Mesoamerican languages
SO LANGUAGE SCIENCES
LA English
DT Article
DE Mesoamerican languages; Frames of reference; Spatial semantics; Semantic
typology; Spatial reference; Language and cognition
ID LINGUISTIC RELATIVITY; SPACE ORIENTATION; SEMANTIC TYPOLOGY; BODY;
COGNITION; TABLES; PARTS; SHAPE
AB This article presents the conceptual and methodological framework for the special issue Frames of reference in Mesoamerican languages, which reports on the use of frames of reference (FoRs) in eight Mesoamerican languages and two non-Mesoamerican control languages. The papers included here are a result of the ongoing collaborative project Spatial language and cognition in Mesoamerica. This article provides a background to the study of FoRs, the research methodology used cross-linguistically, the classification that serves as the basis for the coding of cross-linguistic data, and a preview of the articles in the special issue. Published by Elsevier Ltd.
C1 [Perez Baez, Gabriela] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA.
[O'Meara, Carolyn] Univ Nacl Autonoma Mexico, Inst Invest Filol, Seminario Lenguas Indigenas, Mexico City 04510, DF, Mexico.
RP Baez, GP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012, Washington, DC 20013 USA.
EM perezbaezg@si.edu
NR 70
TC 17
Z9 17
U1 0
U2 8
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0388-0001
J9 LANG SCI
JI Lang. Sci.
PD NOV
PY 2011
VL 33
IS 6
SI SI
BP 837
EP 852
DI 10.1016/j.langsci.2011.06.013
PG 16
WC Linguistics; Language & Linguistics
SC Linguistics
GA 836LK
UT WOS:000296113000001
ER
PT J
AU Baez, GP
AF Perez Baez, Gabriela
TI Spatial frames of reference preferences in Juchitan Zapotec
SO LANGUAGE SCIENCES
LA English
DT Article
DE Zapotec languages; Mesoamerican languages; Spatial frames of reference;
Semantic typology; Linguistic relativity
ID COGNITION; TYPOLOGY; LANGUAGE; SHAPE
AB This article reports on spatial frames of reference (FoRs) preferences in Juchiteco (Zapotec, Otomanguean). The data show that speakers exhibit a strong preference for the absolute and object-centered FoRs, both observer-independent, and overall disfavor most other FoR types. Of particular interest is the limited use of the relative (observer-dependent) FoR. This is relevant in a language such as Juchiteco, which has a productive meronymic (part-naming) system, as it supports the hypothesis put forth by the Spatial Language and Cognition in Mesoamerica project that productive meronymy correlates with a bias against the use of the relative FoR. Published by Elsevier Ltd.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA.
RP Baez, GP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012, Washington, DC 20013 USA.
EM perezbaezg@si.edu
NR 47
TC 2
Z9 2
U1 0
U2 3
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0388-0001
J9 LANG SCI
JI Lang. Sci.
PD NOV
PY 2011
VL 33
IS 6
SI SI
BP 943
EP 960
DI 10.1016/j.langsci.2011.06.012
PG 18
WC Linguistics; Language & Linguistics
SC Linguistics
GA 836LK
UT WOS:000296113000006
ER
PT J
AU Montaser, R
Paul, VJ
Luesch, H
AF Montaser, Rana
Paul, Valerie J.
Luesch, Hendrik
TI Pitipeptolides C-F, antimycobacterial cyclodepsipeptides from the marine
cyanobacterium Lyngbya majuscula from Guam
SO PHYTOCHEMISTRY
LA English
DT Article
DE Marine cyanobacteria; Lyngbya majuscula; Pitipeptolides; Cytotoxin;
Antimycobacterial activity
ID NATURAL-PRODUCTS
AB Pitipeptolides A (1) and B (2) are cyclic depsipeptides isolated from the marine cyanobacterium Lyngbya majuscula from Piti Bomb Holes, Guam. Additional analogues have now been isolated by revisiting larger collections of the same cyanobacterium. The four identified analogues, pitipeptolides C-F (3-6), are the tetrahydro analogue (3), an analogue with a lower degree of methylation (4) as well as two homologues (5 and 6) of pitipeptolide A. Their structures were elucidated using 20 NMR experiments, chiral HPLC analysis and comparison with pitipeptolide A. The identified analogues showed weaker cytotoxic activities compared to the two major parent compounds, pitipeptolides A (1) and B (2), against HT-29 colon adenocarcinoma and MCF7 breast cancer cells. On the other hand, pitipeptolide F (6) was the most potent pitipeptolide in a disc diffusion assay against Mycobacterium tuberculosis. The latter finding suggests that the structure of pitipeptolides could be optimized for selective antibacterial activity. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Montaser, Rana; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA.
[Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.
RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA.
EM luesch@cop.ufl.edu
FU National Institutes of Health, NIGMS [P41GM086210]
FX This research was supported by the National Institutes of Health, NIGMS
Grant P41GM086210. We thank J. R. Rocca for technical assistance with
NMR data acquisition. This is contribution 852 from the Smithsonian
Marine Station.
NR 16
TC 15
Z9 15
U1 3
U2 21
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0031-9422
J9 PHYTOCHEMISTRY
JI Phytochemistry
PD NOV
PY 2011
VL 72
IS 16
BP 2068
EP 2074
DI 10.1016/j.phytochem.2011.07.014
PG 7
WC Biochemistry & Molecular Biology; Plant Sciences
SC Biochemistry & Molecular Biology; Plant Sciences
GA 834HJ
UT WOS:000295950100017
PM 21843895
ER
PT J
AU Zotz, G
Schmidt, G
Mikona, C
AF Zotz, G.
Schmidt, G.
Mikona, C.
TI What is the proximate cause for size-dependent ecophysiological
differences in vascular epiphytes?
SO PLANT BIOLOGY
LA English
DT Article
DE Bromeliaceae; nutrient limitation; ontogenetic drift; Orchidaceae;
photosynthesis; rain forest; size dependency; specific leaf area
ID PLANT SIZE; WATER RELATIONS; TREE HEIGHT; CARBON GAIN; GROWTH;
PHOTOSYNTHESIS; BROMELIADS; CONSEQUENCES; NITROGEN; ORCHID
AB Size-related variation in physiological parameters as diverse as photosynthetic capacity, abscisic acid relationships or the relative water deficit at stomatal closure have been reported for a large number of vascular epiphytes, but the proximate mechanism behind these observations has not been identified. We test four possible reasons for size-related changes in photosynthetic capacity, leaf-N content and specific leaf area: (i) plant size itself, (ii) plant age or developmental stage, (iii) previous nutrition, or (iv) previous water regime. A suite of study species and approaches were used: a 'natural experiment' with the orchid Polystachya foliosa; an experimental field study with another orchid, Dimerandra emarginata; and a study under controlled conditions with the tank bromeliad, Vriesea sanguinolenta. Neither size, age nor differences in water supply caused differences in leaf N and photosynthetic capacity, while low supply of nutrients yielded, and high supply with nutrients completely removed, size-related trends. The observed size-related trends are thus a consequence of in situ differences in nutrient acquisition. Arguably, the improved nutrient status of larger plants under natural conditions results from larger tanks, holding moisture for increasingly longer intervals, which allows longer periods of decomposition of detritus and of nutrient uptake.
C1 [Zotz, G.] Carl von Ossietzky Univ Oldenburg, Inst Biol Umweltwissensch, AG Funkt Okol, D-26111 Oldenburg, Germany.
[Zotz, G.] Smithsonian Trop Res Inst, Balboa, Panama.
[Schmidt, G.; Mikona, C.] Univ Wurzburg, Lehrstuhl Bot 2, D-8700 Wurzburg, Germany.
RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Inst Biol Umweltwissensch, AG Funkt Okol, Postfach 2503, D-26111 Oldenburg, Germany.
EM gerhard.zotz@uni-oldenburg.de
FU Deutsche Forschungsgemeinschaft [Sonderforschungsbereich 251]
FX This research was supported by a grant from the Deutsche
Forschungsgemeinschaft (Sonderforschungsbereich 251). Cord Mikona
received generous support from the Wilhelm-v. Gwinner Foundation,
Munich, Germany. Thanks also to Edgardo Garrido and Vera Thomas for
assistance in the field and to Frida Reisberg, Wurzburg, for CHN
analysis. Sabine Armsen, Wurzburg, supplied data from her unpublished
Master's thesis. Comments by three anonymous reviewers and Diane Byers,
Normal, USA, on earlier versions helped to improve the manuscript.
Finally, we thank the Republic of Panama for making its natural
resources available for study.
NR 39
TC 3
Z9 3
U1 1
U2 21
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1435-8603
J9 PLANT BIOLOGY
JI Plant Biol.
PD NOV
PY 2011
VL 13
IS 6
BP 902
EP 908
DI 10.1111/j.1438-8677.2011.00460.x
PG 7
WC Plant Sciences
SC Plant Sciences
GA 835JD
UT WOS:000296031800011
PM 21973121
ER
PT J
AU Kleiman, DG
AF Kleiman, Devra G.
TI Canid Mating Systems, Social Behavior, Parental Care and Ontogeny: Are
they Flexible?
SO BEHAVIOR GENETICS
LA English
DT Article
DE Monogamy; Behavioral plasticity; Canids; Sociality; Reproductive
behavior
ID DOG SPEOTHOS-VENATICUS; CRAB-EATING FOX; WOLF CHRYSOCYON-BRACHYURUS;
BUSH DOG; MANED WOLF
AB Benson Ginsburg's early studies of canid socialization and wolf social and reproductive behavior were focused, in part, on the degree to which there was flexibility in social development and specifically whether there was a critical period during development after which wolf pups could not be socialized to humans. My focus was the degree to which differences in canid ecology and social structure were correlated with differences in the plasticity of social and reproductive behavior, including development. Canid species are unusual among the Mammalia in being primarily monogamous. Males may play an indirect or direct role in parental care, depending on a species degree of sociality. Canid species also differ in developmental parameters, and reproductive suppression is common in the group-living pack hunters. I review comparative studies of the social and reproductive behavior of three South American canids which vary in their degree of sociality and explore the degree to which the species are ecologically and socially flexible.
C1 Smithsonian Natl Zool Pk, Div Conservat & Sci, Washington, DC 20008 USA.
RP Kleiman, DG (reprint author), Smithsonian Natl Zool Pk, Div Conservat & Sci, Washington, DC 20008 USA.
FU Smithsonian Research Foundation; NIMH [27241-03]
FX I would like to thank Benson Ginsburg for giving me a start in canid
research and supporting my interests so completely. Without the
opportunities he provided, my career would have gone in a very different
direction. I also wish to thank George and Mary Rabb for introducing me
to the complexities of life within a wolf pack. I would also like to
thank those colleagues that contributed so much to the canid studies,
especially: Maxeen Biben, Chuck Brady, James Dietz, John Eisenberg,
Ingrid Porton, and Melissa Rodden. These studies were supported by
grants from the Smithsonian Research Foundation and NIMH 27241-03.
NR 34
TC 9
Z9 9
U1 8
U2 126
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0001-8244
EI 1573-3297
J9 BEHAV GENET
JI Behav. Genet.
PD NOV
PY 2011
VL 41
IS 6
SI SI
BP 803
EP 809
DI 10.1007/s10519-011-9459-0
PG 7
WC Behavioral Sciences; Genetics & Heredity; Psychology, Multidisciplinary
SC Behavioral Sciences; Genetics & Heredity; Psychology
GA 826BO
UT WOS:000295326600004
PM 21487689
ER
PT J
AU Purdy, BA
Jones, KS
Mecholsky, JJ
Bourne, G
Hulbert, RC
MacFadden, BJ
Church, KL
Warren, MW
Jorstad, TF
Stanford, DJ
Wachowiak, MJ
Speakman, RJ
AF Purdy, Barbara A.
Jones, Kevin S.
Mecholsky, John J.
Bourne, Gerald
Hulbert, Richard C., Jr.
MacFadden, Bruce J.
Church, Krista L.
Warren, Michael W.
Jorstad, Thomas F.
Stanford, Dennis J.
Wachowiak, Melvin J.
Speakman, Robert J.
TI Earliest art in the Americas: incised image of a proboscidean on a
mineralized extinct animal bone from Vero Beach, Florida
SO JOURNAL OF ARCHAEOLOGICAL SCIENCE
LA English
DT Article
DE Old Vero site; Incised art; Terminal Pleistocene; Mammoth; Mastodon
ID NORTH-AMERICA; BUTCHERY
AB A fragmented fossil bone incised with the figure of a proboscidean was recently found at Vero Beach, Florida near the location where Late Pleistocene fauna and human bones were recovered from 1913 to 1916. This engraving may represent the oldest and only existing example of Terminal Pleistocene art depicting a proboscidean in the Americas. Because of the uniqueness, rarity, and potential antiquity of this specimen, caution demanded that a variety of tests be used in an attempt to verify its authenticity. The mineralized bone was identified as mammoth, mastodon, or giant sloth. Rare earth element analysis was consistent with the fossil bone being ancient and originating at or near the Old Vero site (8-IR-9). Forensic analysis suggests the markings on the bone are not recent. Optical microscopy results show no discontinuity in coloration between the carved grooves and the surrounding material indicating that both surfaces aged simultaneously. Scanning electron microscopy (SEM) revealed that the edges of the inscription are worn and show no signs of being incised recently or that the grooves were made with metal tools. In addition, the backscattered SEM images suggest there is no discontinuity in the distribution of light and heavy elements between the scribed region and the surrounding bone indicating that both surfaces aged in the same environment. This is very different from an intentional mark made on the bone for comparison. Energy dispersive x-ray spectroscopy (EDXS) shows that the surface contains significant amounts of calcium, phosphorus, oxygen, and carbon typical of a mineralized bone surface. Examination of a cast and mold of the incised bone by Reflectance Transformation Imaging (RTI) also provided no evidence that the engraving was made recently. All of these results are consistent with the mammoth engraving being authentic. Published by Elsevier Ltd.
C1 [Wachowiak, Melvin J.; Speakman, Robert J.] Museum Support Ctr, Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
[Purdy, Barbara A.; Warren, Michael W.] Univ Florida, Dept Anthropol, Gainesville, FL 32611 USA.
[Jones, Kevin S.; Mecholsky, John J.; Bourne, Gerald] Univ Florida, Dept Mat Sci & Engn, Gainesville, FL 32611 USA.
[Hulbert, Richard C., Jr.; MacFadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Church, Krista L.] Univ Texas Austin, Dept Anthropol, Austin, TX 78712 USA.
[Jorstad, Thomas F.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Stanford, Dennis J.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Speakman, RJ (reprint author), Museum Support Ctr, Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM speakmanj@si.edu
RI Bourne, Gerald/B-7219-2008;
OI Bourne, Gerald/0000-0001-6977-2138; Hulbert,
Richard/0000-0002-2242-4256; Speakman, Robert/0000-0003-2063-154X
NR 33
TC 14
Z9 14
U1 2
U2 7
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 NOV
PY 2011
VL 38
IS 11
BP 2908
EP 2913
DI 10.1016/j.jas.2011.05.022
PG 6
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 829CI
UT WOS:000295552600005
ER
PT J
AU McRae, SB
AF McRae, Susan B.
TI Conspecific brood parasitism in the tropics: an experimental
investigation of host responses in common moorhens and American purple
gallinules
SO ECOLOGY AND EVOLUTION
LA English
DT Article
DE Breeding synchrony; egg rejection; Gallinula chloropus; intraspecific
brood parasitism; Porphyrula martinica; Rallidae; seasonality;
neotropics; wetlands
ID INTRASPECIFIC NEST PARASITISM; COOTS FULICA-AMERICANA; EGG
DISCRIMINATION; SEXUAL SELECTION; REED WARBLERS; WOOD DUCKS; OWN EGGS;
BIRDS; RECOGNITION; EVOLUTION
AB Species occupying a broad latitudinal range may show greater phenotypic plasticity in behavior than species with smaller ranges or more specific habitat requirements. This study investigates for the first time the occurrence of conspecific brood parasitism (CBP) in sympatric tropical populations of the common moorhen (Gallinula chloropus pauxilla Bangs) and the American purple gallinule (Porphyrula martinica L.). CBP occurred in at least 20% (N = 76) of common moorhen nests on the Rio Chagres in Panama. Half (N = 20) of the parasitic eggs were accepted, but 10 were destroyed or ejected from host nests. Introductions of experimental eggs into nests revealed hosts were more likely to accept parasitism later in the host's laying period and during incubation, consistent with expectation of an adaptive response. CBP was not detected in a small sympatric population of American purple gallinules. Members of this population did not eject experimental eggs, suggesting a lack of experience with costly CBP. Contrasting ecological factors help explain why these two species of rail (Family Rallidae) differ in regard to CBP. Purple gallinule territories were sparse, owing to the distribution of preferred habitat. Moorhens flocked outside of the breeding season. They nested more synchronously, at higher densities, and primarily in ephemeral floating vegetation. Further, moorhens suffered a rate of nest loss nearly double that of American purple gallinules, and this increased over the course of the breeding season. Moorhen clutches were larger on average, and more variable in size than those of purple gallinules. Reproductive effort and rate (seasonality) constitute important life history differences between these species that may constrain the evolution of reproductive tactics. Comparing these sympatric populations, and others differing in life-history traits and ecological constraints, highlights the role of risk management in the evolution of CBP.
C1 [McRae, Susan B.] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA.
[McRae, Susan B.] Smithsonian Trop Res Inst, Panama City, Panama.
RP McRae, SB (reprint author), E Carolina Univ, Dept Biol, Greenville, NC 27858 USA.
EM mcraes@ecu.edu
FU Smithsonian Postdoctoral Research Fellowship
FX Funded by Smithsonian Postdoctoral Research Fellowship.
NR 51
TC 5
Z9 6
U1 2
U2 24
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2045-7758
J9 ECOL EVOL
JI Ecol. Evol.
PD NOV
PY 2011
VL 1
IS 3
BP 317
EP 329
DI 10.1002/ece3.26
PG 13
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA 055TQ
UT WOS:000312441000005
PM 22393503
ER
PT J
AU Megill, ND
Pavicic, M
AF Megill, Norman D.
Pavicic, Mladen
TI Kochen-Specker Sets and Generalized Orthoarguesian Equations
SO ANNALES HENRI POINCARE
LA English
DT Article
ID LATTICES
AB We prove that the 7oa class (equational variety) of generalized orthoarguesian lattices is properly included in all noa classes for n < 7. This result strengthens the conjecture that any generalized orthoarguesian equation is strictly stronger than those of lower orders. The result emerged from our recent analysis of whether three-dimensional Kochen-Specker sets can be represented by Greechie lattices, which are a kind of orthomodular lattice.
C1 [Megill, Norman D.] Boston Informat Grp, Lexington, MA 02420 USA.
[Pavicic, Mladen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pavicic, Mladen] Harvard Univ, Inst Theoret Atom Mol & Optic Phys, Dept Phys, Cambridge, MA 02138 USA.
[Pavicic, Mladen] Univ Zagreb, Fac Civil Engn, Phys Chair, Zagreb 41000, Croatia.
RP Megill, ND (reprint author), Boston Informat Grp, 19 Locke Ln, Lexington, MA 02420 USA.
EM nm@alum.mit.edu; pavicic@grad.hr
FU US National Science Foundation through Institute for Theoretical Atomic,
Molecular, and Optical Physics (ITAMP) at Harvard University;
Smithsonian Astrophysical Observatory; Ministry of Science, Education,
and Sport of Croatia [082-0982562-3160]
FX One of us (M. P.) would like to thank his host Hossein Sadeghpour for
support during his stay at ITAMP. His stay was supported by the US
National Science Foundation through a grant for the Institute for
Theoretical Atomic, Molecular, and Optical Physics (ITAMP) at Harvard
University and Smithsonian Astrophysical Observatory and the Ministry of
Science, Education, and Sport of Croatia through the project No.
082-0982562-3160. His part of computation was supported the University
Computing Centre (at cluster Isabella) of the University of Zagreb and
by the Croatian National Grid Infrastructure.
NR 20
TC 1
Z9 1
U1 1
U2 3
PU SPRINGER BASEL AG
PI BASEL
PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND
SN 1424-0637
EI 1424-0661
J9 ANN HENRI POINCARE
JI Ann. Henri Poincare
PD NOV
PY 2011
VL 12
IS 7
BP 1417
EP 1429
DI 10.1007/s00023-011-0109-0
PG 13
WC Physics, Multidisciplinary; Physics, Particles & Fields; Physics,
Mathematical
SC Physics
GA 828RE
UT WOS:000295519300005
ER
PT J
AU van Donkelaar, A
Martin, RV
Levy, RC
da Silva, AM
Krzyzanowski, M
Chubarova, NE
Semutnikova, E
Cohen, AJ
AF van Donkelaar, Aaron
Martin, Randall V.
Levy, Robert C.
da Silva, Arlindo M.
Krzyzanowski, Michal
Chubarova, Natalia E.
Semutnikova, Eugenia
Cohen, Aaron J.
TI Satellite-based estimates of ground-level fine particulate matter during
extreme events: A case study of the Moscow fires in 2010
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE MODIS; PM(2.5); Moscow wildfires; Aerosol optical depth
ID AEROSOL OPTICAL-THICKNESS; UNITED-STATES; CHEMISTRY; MORTALITY;
TRANSPORT; POLLUTION; HEALTH; DEPTH; CHINA; LAND
AB We estimate fine particulate matter (PM(2.5)) concentrations daily using MODIS satellite observations of aerosol optical depth (AOD) for a major biomass burning event around Moscow during summer 2010. Evaluation of MODIS AOD with the Moscow AERONET site supports a MODIS-AOD error estimate of +/-(0.05 + 0.2 x AOD) for this event. However, since the smoke was often thick (AOD > 4.0) and spatially variable, the standard MODIS algorithm incorrectly identifies some aerosol as cloud. We test relaxed cloud screening criteria that increase MODIS coverage by 21% and find excellent agreement with coincident operational retrievals (r(2) = 0.994, slope = 1.01) with no evidence of false aerosol detection. We relate the resultant MODIS AOD to PM(2.5) using aerosol vertical profiles from the GEOS-Chem chemical transport model. Our estimates are in good agreement with PM(2.5) values estimated from in-situ PM(10) (r(2) = 0.85, slope = 1.06), and we find that the relationship between AOD and PM2.5 is insensitive to uncertainties in biomass burning emissions. The satellite-derived and in-situ values both indicate that peak daily mean concentrations of approximately 600 mu g m(-3) occurred on August 7, 2010 in the Moscow region of the Russian Federation. We estimate that exposure to air pollution from the Moscow wildfires may have caused hundreds of excess deaths. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Krzyzanowski, Michal] WHO, European Ctr Environm & Hlth, Reg Off Europe, Bonn, Germany.
[Chubarova, Natalia E.] Moscow MV Lomonosov State Univ, Dept Geog, Moscow, Russia.
[Semutnikova, Eugenia] Mosecomonitoring, State Environm Org, Moscow, Russia.
[Cohen, Aaron J.] Hlth Effects Inst, Boston, MA USA.
RP van Donkelaar, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, 6300 Coburg Rd, Halifax, NS B3H 3J5, Canada.
EM aaron.van.Donkelaar@dal.ca; randall.martin@dal.ca;
robert.c.levy@nasa.gov; arlindo.m.dasilva@nasa.gov;
mkr@ecehbonn.euro.who.int; chubarova@imp.kiae.ru; info@mosecom.ru;
acohen@healtheffects.org
RI da Silva, Arlindo/D-6301-2012; Levy, Robert/M-7764-2013; Martin,
Randall/C-1205-2014; Chem, GEOS/C-5595-2014
OI da Silva, Arlindo/0000-0002-3381-4030; Levy, Robert/0000-0002-8933-5303;
Martin, Randall/0000-0003-2632-8402;
FU Natural Science and Engineering Research Council of Canada (NSERC);
Killam Trust
FX This work was supported by the Natural Science and Engineering Research
Council of Canada (NSERC) and the Killam Trust.
NR 48
TC 48
Z9 50
U1 1
U2 32
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 NOV
PY 2011
VL 45
IS 34
BP 6225
EP 6232
DI 10.1016/j.atmosenv.2011.07.068
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 831UU
UT WOS:000295757400016
ER
PT J
AU Whattam, SA
Stern, RJ
AF Whattam, Scott A.
Stern, Robert J.
TI The 'subduction initiation rule': a key for linking ophiolites,
intra-oceanic forearcs, and subduction initiation
SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY
LA English
DT Article
DE Ophiolites; Forearcs; Intra-oceanic arcs; Subduction initiation; Tethys;
Izu-Bonin-Marianas arc
ID VOLCANIC-ROCKS; TETHYAN OPHIOLITES; TRENCH ROLLBACK; OMAN OPHIOLITE;
OCEANIC-CRUST; ACCRETION; EVOLUTION; ZONE; ALBANIA; GEOCHEMISTRY
AB We establish the 'subduction initiation rule' (SIR) which predicts that most ophiolites form during subduction initiation (SI) and that the diagnostic magmatic chemostratigraphic progression for SIR ophiolites is from less to more HFSE-depleted and LILE-enriched compositions. This chemostratigraphic evolution reflects formation of what ultimately becomes forearc lithosphere as a result of mantle melting that is progressively influenced by subduction zone enrichment during SI. The magmatic chemostratigraphic progression for the Izu-Bonin-Mariana (IBM) forearc and most Tethyan ophiolites is specifically from MORB-like to arc-like (volcanic arc basalts or VAB +/- A boninites or BON) because SI progressed until establishment of a mature subduction zone. MORB-like lavas result from decompression melting of upwelling asthenosphere and are the first magmatic expression of SI. The contribution of fluids from dehydrating oceanic crust and sediments on the sinking slab is negligible in early SI, but continued melting results in a depleted, harzburgitic residue that is progressively metasomatized by fluids from the sinking slab; subsequent partial melting of this residue yields 'typical' SSZ-like lavas in the latter stages of SI. If SI is arrested early, e.g., as a result of collision, 'MORB-only' ophiolites might be expected. Consequently, MORB- and SSZ-only ophiolites may represent end-members of the SI ophiolite spectrum. The chemostratigraphic similarity of the Mariana forearc with that of ophiolites that follow the SIR intimates that a model linking such ophiolites, oceanic forearcs, and SI is globally applicable.
C1 [Whattam, Scott A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Stern, Robert J.] Univ Texas Dallas, Geosci Dept, Dallas, TX 75083 USA.
RP Whattam, SA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama.
EM whattams@si.edu
OI Whattam, Scott/0000-0001-9193-9002
FU National Science Foundation
FX RJS thanks many of his colleagues who helped him over the years
understand what happens during subduction initiation, including Sherm
Bloomer, Yildirim Dilek, Mike Gurnis, Osamu Ishizuka, Yas Ohara, Hadi
Shafaii Moghadem, Julian Pearce, Mark Reagan, and John Shervais. These
insights would not have been possible without support from the National
Science Foundation.
NR 70
TC 71
Z9 73
U1 10
U2 55
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0010-7999
J9 CONTRIB MINERAL PETR
JI Contrib. Mineral. Petrol.
PD NOV
PY 2011
VL 162
IS 5
BP 1031
EP 1045
DI 10.1007/s00410-011-0638-z
PG 15
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 830SN
UT WOS:000295677500009
ER
PT J
AU Rick, TC
DeLong, RL
Erlandson, JM
Braje, TJ
Jones, TL
Arnold, JE
Des Lauriers, MR
Hildebrandt, WR
Kennett, DJ
Vellanoweth, RL
Wake, TA
AF Rick, Torben C.
DeLong, Robert L.
Erlandson, Jon M.
Braje, Todd J.
Jones, Terry L.
Arnold, Jeanne E.
Des Lauriers, Matthew R.
Hildebrandt, William R.
Kennett, Douglas J.
Vellanoweth, Rene L.
Wake, Thomas A.
TI Where were the northern elephant seals? Holocene archaeology and
biogeography of Mirounga angustirostris
SO HOLOCENE
LA English
DT Article
DE historical ecology; human-environmental interactions; marine
conservation; Pacific Coast; pinniped; Phocidae
ID SOUTHERN NORTHWEST COAST; SAN-MIGUEL ISLAND; POPULATION BOTTLENECK;
CALIFORNIA; PACIFIC; AMERICA; OREGON; EXTINCTION; RESPONSES; EXAMPLES
AB Driven to the brink of extinction during the nineteenth century commercial fur and oil trade, northern elephant seal (NES, Mirounga angustirostris) populations now exceed 100 000 animals in the northeast Pacific from Alaska to Baja California. Because little is known about the biogeography and ecology of NES prior to the mid-nineteenth century, we synthesize and analyze the occurrence of NES remains in North American archaeological sites. Comparing these archaeological data with modern biogeographical, genetic, and behavioral data, we provide a trans-Holocene perspective on NES distribution and abundance. Compared with other pinnipeds, NES bones are relatively rare throughout the Holocene, even in California where they currently breed in large numbers. Low numbers of NES north of California match contemporary NES distribution, but extremely low occurrences in California suggest their abundance in this area was very different during the Holocene than today. We propose four hypotheses to explain this discrepancy, concluding that ancient human settlement and other activities may have displaced NES from many of their preferred modern habitats during much of the Holocene.
C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA.
[Erlandson, Jon M.; Kennett, Douglas J.] Univ Oregon, Eugene, OR 97403 USA.
[Braje, Todd J.] San Diego State Univ, San Diego, CA 92182 USA.
[Jones, Terry L.] California Polytech State Univ, San Luis Obispo, CA USA.
[Arnold, Jeanne E.; Wake, Thomas A.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Des Lauriers, Matthew R.] Calif State Univ Northridge, Northridge, CA 91330 USA.
[Vellanoweth, Rene L.] Calif State Univ Los Angeles, Los Angeles, CA USA.
RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA.
EM rickt@si.edu
RI Kennett, Douglas/I-7613-2015;
OI Kennett, Douglas/0000-0001-5133-9010; Erlandson, Jon/0000-0002-4705-4319
FU Channel Islands National Park; Western National Parks Association;
National Science Foundation; our home institutions
FX This paper is dedicated to the late Phillip L. Walker, friend, mentor,
and colleague, who helped shape our thinking on numerous topics,
including ancient interactions between humans and pinnipeds. Our work on
the Channel Islands has been supported by Channel Islands National Park,
the Western National Parks Association, the National Science Foundation,
and our home institutions. Finally, we thank Arlene Rosen and two
anonymous reviewers for constructive comments that greatly improved this
manuscript.
NR 67
TC 6
Z9 6
U1 1
U2 23
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 NOV
PY 2011
VL 21
IS 7
BP 1159
EP 1166
DI 10.1177/0959683611400463
PG 8
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 825ZF
UT WOS:000295320200013
ER
PT J
AU Cardoso, P
Erwin, TL
Borges, PAV
New, TR
AF Cardoso, Pedro
Erwin, Terry L.
Borges, Paulo A. V.
New, Tim R.
TI The seven impediments in invertebrate conservation and how to overcome
them
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE Conservation priorities; Ecosystem services; Extinction; Information
shortfalls; Science funding; Species diversity
ID WILLINGNESS-TO-PAY; BIODIVERSITY CONSERVATION; ECOSYSTEM SERVICES; RED
LIST; AGRICULTURAL LANDSCAPES; SPECIES CONSERVATION; INSECT
CONSERVATION; TROPICAL FORESTS; CITIZEN SCIENCE; EXTINCTION
AB Despite their high diversity and importance for humankind, invertebrates are often neglected in biodiversity conservation policies. We identify seven impediments to their effective protection: (1) invertebrates and their ecological services are mostly unknown to the general public (the public dilemma); (2) policy-makers and stakeholders are mostly unaware of invertebrate conservation problems (the political dilemma); (3) basic science on invertebrates is scarce and underfunded (the scientific dilemma); (4) most species are undescribed (the Linnean shortfall); (5) the distribution of described species is mostly unknown (the Wallacean shortfall); (6) the abundance of species and their changes in space and time are unknown (the Prestonian shortfall); (7) species ways of life and sensitivities to habitat change are largely unknown (the Hutchinsonian shortfall).
Numerous recent developments in taxonomy, inventorying, monitoring, data compilation, statistical analysis and science communication facilitate overcoming these impediments in both policy and practice. We suggest as possible solutions for the public dilemma: better public information and marketing. For the political dilemma: red-listing, legal priority listing and inclusion in environmental impact assessment studies. For the scientific dilemma: parataxonomy, citizen science programs and biodiversity informatics. For the Linnean shortfall: biodiversity surrogacy, increased support for taxonomy and advances in taxonomic publications. For the Wallacean shortfall: funding of inventories, compilation of data in public repositories and species distribution modeling. For the Prestonian shortfall: standardized protocols for inventorying and monitoring, widespread use of analogous protocols and increased support for natural history collections. For the Hutchinsonian shortfall: identifying good indicator taxa and studying extinction rates by indirect evidence. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Cardoso, Pedro; Borges, Paulo A. V.] Univ Acores, Azorean Biodivers Grp CITA A, Dept Ciencias Agr, P-9700042 Angra Do Heroismo, Portugal.
[Cardoso, Pedro; Erwin, Terry L.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
[New, Tim R.] La Trobe Univ, Dept Zool, Bundoora, Vic 3086, Australia.
RP Cardoso, P (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, Dept Ciencias Agr, Rua Capitao Joao Avila, P-9700042 Angra Do Heroismo, Portugal.
EM pcardoso@ennor.org
RI Borges, Paulo/B-2780-2008; Cardoso, Pedro/A-8820-2008
OI Borges, Paulo/0000-0002-8448-7623; Cardoso, Pedro/0000-0001-8119-9960
FU Portuguese Foundation for Science and Technology [SFRH/BPD/40688/2007,
FCT - PTDC/BIA-BEC/104571/2008, FCT - PTDC/BIA-BEC/100182/2008]
FX We thank J. Hortal, S. Ribeiro and A.S. Pullin for suggestions and
fruitful discussions around the subject. P.C. and P.A.V.B. are supported
by the Portuguese Foundation for Science and Technology
(SFRH/BPD/40688/2007; FCT - PTDC/BIA-BEC/104571/2008; FCT -
PTDC/BIA-BEC/100182/2008).
NR 125
TC 143
Z9 150
U1 18
U2 171
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0006-3207
EI 1873-2917
J9 BIOL CONSERV
JI Biol. Conserv.
PD NOV
PY 2011
VL 144
IS 11
BP 2647
EP 2655
DI 10.1016/j.biocon.2011.07.024
PG 9
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 827QL
UT WOS:000295442900013
ER
PT J
AU Greco, MK
Welz, PM
Siegrist, M
Ferguson, SJ
Gallmann, P
Roubik, DW
Engel, MS
AF Greco, M. K.
Welz, P. M.
Siegrist, M.
Ferguson, S. J.
Gallmann, P.
Roubik, D. W.
Engel, M. S.
TI Description of an ancient social bee trapped in amber using diagnostic
radioentomology
SO INSECTES SOCIAUX
LA English
DT Article
DE Proplebeia; Stingless bees; Diagnostic radioentomology; Miocene;
Burdigalian; MicroCT; Amber
ID TRIGONA-HYPOGEA HYMENOPTERA; RAY SYNCHROTRON MICROTOMOGRAPHY;
XYLOCOPA-PUBESCENS SPINOLA; DOMINICAN AMBER; PROVENTRICULAR STRUCTURE;
COMPUTERIZED-TOMOGRAPHY; PHYLOGENETIC ANALYSIS; HIGH-RESOLUTION;
STINGLESS BEE; CARPENTER BEE
AB The application of non-invasive imaging technologies using X-radiation (diagnostic radioentomology, 'DR') is demonstrated for the study of amber-entombed social bees. Here, we examine the external and internal morphology of an Early Miocene (Burdigalian) stingless bee (Apinae: Meliponini) from the Dominican Republic using non-destructive X-ray microtomography analysis. The study permits the accurate reconstruction of features otherwise obscured or impossible to visualize without destroying the sample and allows diagnosis of the specimen as a new species, Proplebeia adbita Greco and Engel.
C1 [Greco, M. K.] Univ Bath, Dept Elect & Elect Engn, INVERT Grp, Bath BA2 7AY, Avon, England.
[Greco, M. K.] Univ Bern, Dept Klin Vet Med, Vetsuisse Fak, CH-3001 Bern, Switzerland.
[Gallmann, P.] Swiss Bee Res Ctr, Agroscope Liebefeld Posieux Res Stn ALP, CH-3033 Bern, Switzerland.
[Welz, P. M.; Ferguson, S. J.] Univ Bern, Inst Surg Technol & Biomech, CH-3014 Bern, Switzerland.
[Siegrist, M.] Univ Bern, Dept Clin Res, Bone Biol Grp, CH-3010 Bern, Switzerland.
[Roubik, D. W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Engel, M. S.] Univ Kansas, Div Entomol Paleoentomol, Dept Ecol & Evolutionary Biol, Nat Hist Museum, Lawrence, KS 66049 USA.
[Engel, M. S.] Amer Museum Nat Hist, Div Invertebrate Zool Entomol, New York, NY 10024 USA.
RP Greco, MK (reprint author), Univ Bern, Dept Klin Vet Med, Vetsuisse Fak, CH-3001 Bern, Switzerland.
EM M.K.Greco@bath.ac.uk
RI Ferguson, Stephen/A-4118-2012; Engel, Michael/C-5461-2012;
OI Engel, Michael/0000-0003-3067-077X; Greco, Mark/0000-0002-2136-5127
NR 65
TC 5
Z9 7
U1 0
U2 13
PU SPRINGER BASEL AG
PI BASEL
PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND
SN 0020-1812
EI 1420-9098
J9 INSECT SOC
JI Insect. Soc.
PD NOV
PY 2011
VL 58
IS 4
BP 487
EP 494
DI 10.1007/s00040-011-0168-8
PG 8
WC Entomology
SC Entomology
GA 819JK
UT WOS:000294821000008
ER
PT J
AU Stolarski, J
Kitahara, MV
Miller, DJ
Cairns, SD
Mazur, M
Meibom, A
AF Stolarski, Jaroslaw
Kitahara, Marcelo V.
Miller, David J.
Cairns, Stephen D.
Mazur, Maciej
Meibom, Anders
TI The ancient evolutionary origins of Scleractinia revealed by
azooxanthellate corals
SO BMC EVOLUTIONARY BIOLOGY
LA English
DT Article
ID WATER CORALS; MITOCHONDRIAL; PHYLOGENY; SKELETON; AMPLIFICATION;
ORDOVICIAN; ANTHOZOA; SCOTLAND; SUGGEST; PRIMERS
AB Background: Scleractinian corals are currently a focus of major interest because of their ecological importance and the uncertain fate of coral reefs in the face of increasing anthropogenic pressure. Despite this, remarkably little is known about the evolutionary origins of corals. The Scleractinia suddenly appear in the fossil record about 240 Ma, but the range of morphological variation seen in these Middle Triassic fossils is comparable to that of modern scleractinians, implying much earlier origins that have so far remained elusive. A significant weakness in reconstruction(s) of early coral evolution is that deep-sea corals have been poorly represented in molecular phylogenetic analyses.
Results: By adding new data from a large and representative range of deep-water species to existing molecular datasets and applying a relaxed molecular clock, we show that two exclusively deep-sea families, the Gardineriidae and Micrabaciidae, diverged prior to the Complexa/Robusta coral split around 425 Ma, thereby pushing the evolutionary origin of scleractinian corals deep into the Paleozoic.
Conclusions: The early divergence and distinctive morphologies of the extant gardineriid and micrabaciid corals suggest a link with Ordovician "scleractiniamorph" fossils that were previously assumed to represent extinct anthozoan skeletonized lineages. Therefore, scleractinian corals most likely evolved from Paleozoic soft-bodied ancestors. Modern shallow-water Scleractinia, which are dependent on symbionts, appear to have had several independent origins from solitary, non-symbiotic precursors. The Scleractinia have survived periods of massive climate change in the past, suggesting that as a lineage they may be less vulnerable to future changes than often assumed.
C1 [Stolarski, Jaroslaw] Polish Acad Sci, Inst Paleobiol, PL-00818 Warsaw, Poland.
[Kitahara, Marcelo V.; Miller, David J.] James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia.
[Kitahara, Marcelo V.; Miller, David J.] James Cook Univ, Coral Genom Grp, Townsville, Qld 4811, Australia.
[Cairns, Stephen D.] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Mazur, Maciej] Univ Warsaw, Dept Chem, Lab Electrochem, PL-02093 Warsaw, Poland.
[Meibom, Anders] LMCM, Museum Natl Hist Nat, UMR 7202, F-75005 Paris, France.
RP Stolarski, J (reprint author), Polish Acad Sci, Inst Paleobiol, Twarda 51-55, PL-00818 Warsaw, Poland.
EM stolacy@twarda.pan.pl
RI Kitahara, Marcelo/D-5560-2011; Manager, MEEL/C-4732-2015
FU Polish Ministry of Science and Higher Education [N307-015733]; European
Research Council [246749]; Australian Research Council (ARC) via the ARC
Centre of Excellence for Coral Reef Studies (ARC CoE); Coordination for
the Improvement of Higher Level Personnel (CAPES); Fisheries Research
and Development Corporation (FRDC); Australian Government Department of
Environment, Water, Heritage and the Arts; Australian CSIRO
(Commonwealth Scientific and Industrial Research Organization)
FX This work was supported in part by the Polish Ministry of Science and
Higher Education (project N307-015733) to JS, the European Research
Council through Advanced Grant 246749 (BIOCARB) to AM, the Australian
Research Council (ARC) via the ARC Centre of Excellence for Coral Reef
Studies (ARC CoE) to DJM, and PhD scholarship support for MVK via
Coordination for the Improvement of Higher Level Personnel (CAPES). The
authors also thank Nancy Knowlton, Eldon Ball and Sylvain Foret for
their valuable comments on drafts of the manuscript. We would also like
to acknowledge all the Smithsonian Institution invertebrate collection
staff (NMNH) for sending the New Caledonian material to Australia,
especially Paul Greenhall. Special thanks are due to all Museum of
Tropical Queensland staff (MTQ-Queensland), especially Carden Wallace,
Barbara Done for use of facilities at the Museum of Tropical Queensland.
We also thank Philippe Bouchet (MNHN) who generously loaned the New
Caledonian material from the Paris Museum to the Smithsonian
Institution, and Bertrand Richer de Forges and IRD-Noumea staff and
collaborators for their great effort in collecting and preserving the
New Caledonian specimens examined in the present study. We extend our
gratitude to Felicity McEnnulty (CSIRO) for the loan the Australian
specimens examined in the present study, which were collected with
funding from the Fisheries Research and Development Corporation (FRDC),
Environment Australia (now the Australian Government Department of
Environment, Water, Heritage and the Arts), and by the Australian CSIRO
(Commonwealth Scientific and Industrial Research Organization) Wealth
from Oceans Flagship with the assistance of the Australian Government
Department of the Environment, Water, Heritage and the Arts.
NR 53
TC 67
Z9 67
U1 4
U2 53
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2148
J9 BMC EVOL BIOL
JI BMC Evol. Biol.
PD OCT 28
PY 2011
VL 11
AR 316
DI 10.1186/1471-2148-11-316
PG 10
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA 852LD
UT WOS:000297358500001
PM 22034946
ER
PT J
AU Loos, M
Elsenbeer, H
AF Loos, Martin
Elsenbeer, Helmut
TI Topographic controls on overland flow generation in a forest - An
ensemble tree approach
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Overland Bow; Tropical rainforest; Random Forest; Spatial scale; Digital
Elevation Model; Topography
ID TROPICAL RAIN-FOREST; DIGITAL TERRAIN MODELS; SOIL-MOISTURE; HYDRAULIC
CONDUCTIVITY; HYDROLOGICAL PROCESSES; STORMFLOW GENERATION;
DEPRESSION-STORAGE; EROSION PROCESSES; CATCHMENT; WATER
AB Overland flow is an important hydrological pathway in many forests of the humid tropics. Its generation is subject to topographic controls at differing spatial scales. Our objective was to identify such controls on the occurrence of overland flow in a lowland tropical rainforest. To this end, we installed 95 overland flow detectors (OFDs) in four nested subcatchments of the Lutzito catchment on Barro Colorado Island, Panama, and monitored the frequency of overland flow occurrence during 18 rainfall events at each OFD location temporal frequency. For each such location, we derived three non-digital terrain attributes and 17 digital ones, of which 15 were based on Digital Elevation Models (DEMs) of three different resolutions. These attributes then served as input into a Random Forest ensemble tree model to elucidate the importance and partial and joint dependencies of topographic controls for overland flow occurrence.
Lutzito features a high median temporal frequency in overland flow occurrence of 0.421 among OFD locations. However, spatial temporal frequencies of overland flow occurrence vary strongly among these locations and the subcatchments of Lutzito catchment. This variability is best explained by (1) microtopography, (2) coarse terrain sloping and (3) various measures of distance-to-channel, with the contribution of all other terrain attributes being small. Microtopographic features such as concentrated flowlines and wash areas produce highest temporal frequencies, whereas the occurrence of overland flow drops sharply for flow distances and terrain sloping beyond certain threshold values.
Our study contributes to understanding both the spatial controls on overland flow generation and the limitations of terrain attributes for the spatially explicit prediction of overland flow frequencies. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Loos, Martin; Elsenbeer, Helmut] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany.
[Elsenbeer, Helmut] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Loos, M (reprint author), Dr Gebauer Str 40, D-55411 Bingen, Germany.
EM martin.loos@alumni.uni-potsdam.de
FU German Academic Exchange Service (DAAD)
FX This study was funded by the German Academic Exchange Service (DAAD).
The Smithsonian Tropical Research Institute kindly provided rainfall
data and research facilities. Further financial and logistical support
was provided by Ursula and Jurgen Loos. We appreciate the thoughtful and
constructive comments by an anonymous reviewer.
NR 84
TC 15
Z9 16
U1 4
U2 24
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
J9 J HYDROL
JI J. Hydrol.
PD OCT 28
PY 2011
VL 409
IS 1-2
BP 94
EP 103
DI 10.1016/j.jhydrol.2011.08.002
PG 10
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 842LT
UT WOS:000296601600008
ER
PT J
AU Tscherbul, TV
Klos, J
Buchachenko, AA
AF Tscherbul, T. V.
Klos, J.
Buchachenko, A. A.
TI Ultracold spin-polarized mixtures of (2)Sigma molecules with S-state
atoms: Collisional stability and implications for sympathetic cooling
SO PHYSICAL REVIEW A
LA English
DT Article
AB The prospects of sympathetic cooling of polar molecules with magnetically cotrapped alkali-metal atoms are generally considered poor due to strongly anisotropic atom-molecule interactions leading to large spin relaxation rates. Using rigorous quantum scattering calculations based on ab initio interaction potentials, we show that inelastic spin relaxation in low-temperature collisions of CaH((2)Sigma) molecules with Li and Mg atoms occurs at a slow rate despite the strongly anisotropic interactions. This unexpected result, which we rationalize using multichannel quantum-defect theory, opens up the possibility of sympathetic cooling of polar (2)Sigma molecules with alkali-metal atoms in a magnetic trap and with alkaline-earth-metal atoms in an optical dipole trap.
C1 [Tscherbul, T. V.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
[Tscherbul, T. V.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Klos, J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA.
[Buchachenko, A. A.] Moscow MV Lomonosov State Univ, Dept Chem, RU-119991 Moscow, Russia.
RP Tscherbul, TV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
EM tshcherb@cfa.harvard.edu
RI Buchachenko, Alexei/C-8452-2012; Klos, Jacek/A-6457-2008; Tscherbul,
Timur/K-3286-2014
OI Buchachenko, Alexei/0000-0003-0701-5531; Klos,
Jacek/0000-0002-7407-303X; Tscherbul, Timur/0000-0001-5689-040X
FU NSF [CHE-0848110]; RFBR [03-11-00081]
FX We thank H.-I Lu, M. J. Wright, and J. M. Doyle for discussions and A.
Dalgarno and J. F. E. Croft for helpful comments on the manuscript. This
work was supported by NSF grants to the Harvard-MIT CUA and ITAMP at
Harvard University and the Smithsonian Astrophysical Observatory. A. A.
B. and J. K. acknowledge support from RFBR (project No. 03-11-00081) and
the NSF (Grant No. CHE-0848110 to M. H. Alexander).
NR 40
TC 15
Z9 15
U1 0
U2 8
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 OCT 28
PY 2011
VL 84
IS 4
AR 040701
DI 10.1103/PhysRevA.84.040701
PG 5
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 838JJ
UT WOS:000296284300001
ER
PT J
AU Helgen, KM
AF Helgen, Kristofer M.
TI The Mammal Family Tree
SO SCIENCE
LA English
DT Editorial Material
C1 Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA.
RP Helgen, KM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, MRC 108,POB 37012, Washington, DC 20013 USA.
EM helgenk@si.edu
NR 11
TC 6
Z9 7
U1 3
U2 30
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 OCT 28
PY 2011
VL 334
IS 6055
BP 458
EP 459
DI 10.1126/science.1214544
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 837UR
UT WOS:000296230500027
PM 22034419
ER
PT J
AU Benjamin, SP
AF Benjamin, Suresh P.
TI Phylogenetics and comparative morphology of crab spiders (Araneae:
Dionycha, Thomisidae)
SO ZOOTAXA
LA English
DT Article
DE Arachnida; Biodiversity; Character weighting; Cladistics; Color change
behavior; implied weights; sampling bias
ID MISUMENA-VATIA; CHEMICAL ATTRACTION; CLADISTIC-ANALYSIS; REVISION;
GENUS; PHILODROMIDAE; SALTICIDAE; ARANEOIDEA; ARACHNIDA; PARSIMONY
AB The higher-level phylogenetic relationships of crab spiders (Thomisidae) are studied from morphological data. 33 taxa are coded for 74 characters (53 binary and 21 multistate). Several analyses using equal, successive and implied weights were carried out. The most parsimonious tree obtained by analysis with successive and implied weights is put forward as the preferred hypothesis of thomisid relationships (length 222 steps, CI 0.74, RI 0.83). Thomisidae emerge monophyletic in all analyses, supported by four unambiguous synapomorphies. It is now apparent that thomisid taxa have been mostly defined on the basis of plesiomorphic character states. A number of taxonomic changes, including the description of new taxa are proposed and the evolution of diverse behaviors of thomisids is studied in light of the new phylogenetic result. Color change behavior evolved once within the family, but eye arrangement patterns of the median ocular quadrangle, thought to be diagnostic for many genera, evolved as much as 10 times independently. The following new species are described: Borboropactus nyerere sp. nov., Cebrenninus srivijaya sp. nov., Geraesta lehtineni sp. nov. and Geraesta mkwawa sp. nov. The following new generic synonymies are proposed: Bucranium O. P.-Cambridge, 1881 = Aphantochilus O. P.-Cambridge, 1870; Sanmenia Song and Kim, 1992 = Pharta Thorell, 1891 and Cupa Strand, 1906 = Epidius Thorell, 1877. The following species are synonymized: Regillus divergens Hogg, 1914 and Borboropactus hainanus Song, 1993 = Borboropactus bituberculatus Simon, 1884 syn. nov., Epidius ganxiensis (Yin, Peng & Kim, 1999) = Epidius rubropictus Simon, 1909 syn. nov., Geraesta bilobata Simon, 1897 = Geraesta hirta Simon, 1889 syn. nov., Sanmenia kohi Ono, 1995 = Pharta bimaculata Thorell, 1891 syn. nov. and Sanmenia zhengi (Ono & Song, 1986) = Pharta brevipalpus (Simon, 1903) syn. nov. The following new combinations are proposed: Aphantochilus taurifrons (O. P.-Cambridge, 1881) comb. nov., Epidius typicus (Bosenberg & Strand, 1906) comb. nov., Pharta brevipalpus (Simon, 1903) comb. nov., Pharta gongshan (Yang, Zhu and Song, 2006) comb. nov., Pharta nigra (Tang, Griswold & Peng, 2009) comb. nov. and Pharta tengchong (Tang, Griswold & Yin, 2009) comb. nov.
C1 [Benjamin, Suresh P.] Inst Fundamental Studies, Kandy, Sri Lanka.
[Benjamin, Suresh P.] Smithsonian Inst, Natl Museum Nat Hist MRC 105, Dept Entomol, Washington, DC 20013 USA.
RP Benjamin, SP (reprint author), Inst Fundamental Studies, Hantana Rd, Kandy, Sri Lanka.
EM suresh.benjamin@gmail.com
FU Smithsonian Institution; Institute of Fundamental Studies
FX This study was mainly funded by a Smithsonian Institution postdoctoral
fellowship. Additional funding came from Institute of Fundamental
Studies. Thanks to the following individuals for spider specimens:
Fernando Alvarez, David Court, Gustavo Hormiga, Cristian Grismado,
Charles Haddad, Stephen Lew, Lara Lopardo and Tang Guo. Thanks to the
following curators for granting access to collections under their care:
Jonathan Coddington and Dana M. De Roche (USNM), Jason Dunlop (MNHU),
Charles Griswold (CAS), Peter Jager (SMF), Rudy Jocque (MRAC), Torbjorn
Kronestedt (SMNH), Christine Rollard and Elise-Anne Leguin (MNHN), Peter
Schwendinger (MHNG). David Court and Martin Ramirez improved earlier
drafts of this manuscript. Thanks to two anonymous reviewers and
Christoph Muster for providing critical comments. The SEMs were taken at
the Smithsonian's National Museum of Natural History Scanning Electron
Microscope Facility with assistance from Scott Whittaker.
NR 117
TC 19
Z9 21
U1 2
U2 6
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 OCT 28
PY 2011
IS 3080
BP 1
EP 108
PG 108
WC Zoology
SC Zoology
GA 846CR
UT WOS:000296875300001
ER
PT J
AU Gallegos, CL
Werdell, PJ
McClain, CR
AF Gallegos, Charles L.
Werdell, P. Jeremy
McClain, Charles R.
TI Long-term changes in light scattering in Chesapeake Bay inferred from
Secchi depth, light attenuation, and remote sensing measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID EXOPOLYMER PARTICLES TEP; INHERENT OPTICAL-PROPERTIES; DISSOLVED
ORGANIC-MATTER; INFRARED SPECTRAL REGION; OCEANIC WATERS; MARINE
PARTICLES; COASTAL WATERS; ABSORPTION-COEFFICIENTS; NATURAL
PHYTOPLANKTON; BACKSCATTERING RATIO
AB The relationship between the Secchi depth (Z(SD)) and the diffuse attenuation coefficient for photosynthetically active radiation (K-d(PAR)), and in particular the product of the two, Z(SD)center dot K-d(PAR), is governed primarily by the ratio of light scattering to absorption. We analyzed measurements of Z(SD) and K-d(PAR) at main stem stations in Chesapeake Bay and found that the Z(SD)center dot K-d(PAR) product has declined at rates varying from 0.020 to 0.033 yr(-1) over the 17 to 25 years of measurement, implying that there has been a long-term increase in the scattering-to-absorption ratio. Remote sensing reflectance at the green wavelength most relevant to Z(SD) and K-d(PAR) in these waters, R-rs(555), did not exhibit an increasing trend over the 10 years of available measurements. To reconcile the observations we constructed a bio-optical model to calculate Z(SD), K-d(PAR), Z(SD)center dot K-d(PAR), and R-rs(555) as a function of light attenuating substances and their mass-specific absorption and scattering coefficients. When simulations were based exclusively on changes in concentrations of light attenuating substances, a declining trend in Z(SD)center dot K-d entailed an increasing trend in R-rs(555), contrary to observations. To simulate both decreasing Z(SD center dot)K(d)(PAR) and stationary R-rs(555), it was necessary to allow for a declining trend in the ratio of backscattering to total scattering. Within our simulations, this was accomplished by increasing the relative proportion of organic detritus with high mass-specific scattering and low backscattering ratio. An alternative explanation not explicitly modeled is an increasing tendency for the particulate matter to occur in large aggregates. Data to discriminate between these alternatives are not available.
C1 [Gallegos, Charles L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Werdell, P. Jeremy; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Ocean Ecol Branch, Greenbelt, MD 20771 USA.
RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM gallegosc@si.edu
RI Werdell, Jeremy/D-8265-2012;
OI Gallegos, Charles/0000-0001-5112-0166
NR 75
TC 20
Z9 20
U1 0
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD OCT 27
PY 2011
VL 116
AR C00H08
DI 10.1029/2011JC007160
PG 19
WC Oceanography
SC Oceanography
GA 838YH
UT WOS:000296329800003
ER
PT J
AU Gregoric, M
Agnarsson, I
Blackledge, TA
Kuntner, M
AF Gregoric, Matjaz
Agnarsson, Ingi
Blackledge, Todd A.
Kuntner, Matjaz
TI How Did the Spider Cross the River? Behavioral Adaptations for
River-Bridging Webs in Caerostris darwini (Araneae: Araneidae)
SO PLOS ONE
LA English
DT Article
ID ORB-WEAVING SPIDERS; PHYLOGENY; EVOLUTION; CONSTRUCTION; ULOBORIDAE;
SIZE; DIVERSIFICATION; TETRAGNATHIDAE; THERIDIIDAE; COEVOLUTION
AB Background: Interspecific coevolution is well described, but we know significantly less about how multiple traits coevolve within a species, particularly between behavioral traits and biomechanical properties of animals' "extended phenotypes''. In orb weaving spiders, coevolution of spider behavior with ecological and physical traits of their webs is expected. Darwin's bark spider (Caerostris darwini) bridges large water bodies, building the largest known orb webs utilizing the toughest known silk. Here, we examine C. darwini web building behaviors to establish how bridge lines are formed over water. We also test the prediction that this spider's unique web ecology and architecture coevolved with new web building behaviors.
Methodology: We observed C. darwini in its natural habitat and filmed web building. We observed 90 web building events, and compared web building behaviors to other species of orb web spiders.
Conclusions: Caerostris darwini uses a unique set of behaviors, some unknown in other spiders, to construct its enormous webs. First, the spiders release unusually large amounts of bridging silk into the air, which is then carried downwind, across the water body, establishing bridge lines. Second, the spiders perform almost no web site exploration. Third, they construct the orb capture area below the initial bridge line. In contrast to all known orb-weavers, the web hub is therefore not part of the initial bridge line but is instead built de novo. Fourth, the orb contains two types of radial threads, with those in the upper half of the web doubled. These unique behaviors result in a giant, yet rather simplified web. Our results continue to build evidence for the coevolution of behavioral (web building), ecological (web microhabitat) and biomaterial (silk biomechanics) traits that combined allow C. darwini to occupy a unique niche among spiders.
C1 [Gregoric, Matjaz; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Ljubljana, Slovenia.
[Agnarsson, Ingi] Univ Puerto Rico, Dept Biol, San Juan, PR 00936 USA.
[Blackledge, Todd A.] Univ Akron, Dept Biol, Integrated Biosci Program, Akron, OH 44325 USA.
[Agnarsson, Ingi; Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan 430062, Hubei, Peoples R China.
RP Gregoric, M (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Ljubljana, Slovenia.
EM matjaz.gregoric@gmail.com
FU National Geographic [8655-09]; Slovenian Research Agency [P1-0236,
J1-2063]; National Science Foundation [IOS-0745379]
FX This is the second contribution resulting from the 2010 Madagascar
expedition, funded by National Geographic (grant 8655-09 to Dr.
Agnarsson, Dr. Kuntner and Dr. Blackledge). Additional funding came from
the Slovenian Research Agency (grants P1-0236, J1-2063 to Dr. Kuntner)
and National Science Foundation (IOS-0745379 to Dr. Blackledge). The
funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 52
TC 9
Z9 9
U1 3
U2 29
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 OCT 26
PY 2011
VL 6
IS 10
AR e26847
DI 10.1371/journal.pone.0026847
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 841NR
UT WOS:000296519600065
PM 22046378
ER
PT J
AU Oka, M
Phan, TD
Eastwood, JP
Angelopoulos, V
Murphy, NA
Oieroset, M
Miyashita, Y
Fujimoto, M
McFadden, J
Larson, D
AF Oka, M.
Phan, T. -D.
Eastwood, J. P.
Angelopoulos, V.
Murphy, N. A.
Oieroset, M.
Miyashita, Y.
Fujimoto, M.
McFadden, J.
Larson, D.
TI Magnetic reconnection X-line retreat associated with dipolarization of
the Earth's magnetosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID NEUTRAL LINE; SUBSTORM EXPANSION; CURRENT DISRUPTION; MAGNETOTAIL;
RECOVERY; ONSET; EVENT; FIELD; TAIL
AB Magnetic reconnection is the key process of plasma transport in the Earth's magnetotail. The 'X-line' where magnetic field lines reconnect often moves away from the Earth. However, the precise cause of the X-line motion remains unclear. Here we present data from five THEMIS probes positioned along the Sun-Earth line and show that a tailward retreat motion of the X-line (detected by the outermost probe P1) occurred when the dipolarized inner magnetosphere started to return to a more stretched, tail-like configuration (observed by the inner probes P3, P4, and P5). At an intermediate location (P2), the total pressure was increasing. These observations are consistent with the idea that the pressure increase in the inner magnetosphere eventually causes the X-line to retreat tailward. Citation: Oka, M., T.-D. Phan, J. P. Eastwood, V. Angelopoulos, N. A. Murphy, M. Oieroset, Y. Miyashita, M. Fujimoto, J. McFadden, and D. Larson (2011), Magnetic reconnection X-line retreat associated with dipolarization of the Earth's magnetosphere, Geophys. Res. Lett., 38, L20105, doi:10.1029/2011GL049350.
C1 [Oka, M.; Phan, T. -D.; Oieroset, M.; McFadden, J.; Larson, D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Eastwood, J. P.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England.
[Angelopoulos, V.] Univ Calif Los Angeles, IGPP, ESS, Los Angeles, CA 90095 USA.
[Murphy, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Miyashita, Y.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Fujimoto, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
RP Oka, M (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM moka@ssl.berkeley.edu
RI NASA MMS, Science Team/J-5393-2013;
OI NASA MMS, Science Team/0000-0002-9504-5214; Oka,
Mitsuo/0000-0003-2191-1025; Murphy, Nicholas/0000-0001-6628-8033
FU NSF [ATM-0503374]; NASA at UC Berkeley [NNX08AO83G]; Imperial College
London; NASA [NNX11AB61G]
FX The authors acknowledge helpful discussions with M. Cartwright. We also
acknowledge K. H. Glassmeier and his group at Technical University of
Braunschweig for providing the magnetometer data (FGM). We made
extensive use of the software (TDAS) developed by the THEMIS team as
well as the Coordinated Data Analysis Web of NASA. This research was
funded by NSF grant ATM-0503374 and NASA grant NNX08AO83G at UC
Berkeley. JPE holds an STFC Advanced Fellowship at Imperial College
London. NAM is supported by NASA grant NNX11AB61G.
NR 27
TC 17
Z9 17
U1 0
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD OCT 26
PY 2011
VL 38
AR L20105
DI 10.1029/2011GL049350
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 839CT
UT WOS:000296343000005
ER
PT J
AU Peer, BD
Kuehn, MJ
Rothstein, SI
Fleischer, RC
AF Peer, Brian D.
Kuehn, Michael J.
Rothstein, Stephen I.
Fleischer, Robert C.
TI Persistence of host defence behaviour in the absence of avian brood
parasitism
SO BIOLOGY LETTERS
LA English
DT Article
DE brood parasitism; coevolution; egg rejection; molecular clock; relaxed
selection
ID COWBIRD PARASITISM; COEVOLUTION; CUCKOO; DISCRIMINATION
AB The fate of host defensive behaviour in the absence of selection from brood parasitism is critical to long-term host-parasite coevolution. We investigated whether New World Bohemian waxwings Bombycilla garrulus that are allopatric from brown-headed cowbird Molothrus ater and common cuckoo Cuculus canorus parasitism have retained egg rejection behaviour. We found that egg rejection was expressed by 100 per cent of Bohemian waxwings. Our phylogeny revealed that Bohemian and Japanese waxwings Bombycilla japonica were sister taxa, and this clade was sister to the cedar waxwing Bombycilla cedrorum. In addition, there was support for a split between Old and New World Bohemian waxwings. Our molecular clock estimates suggest that egg rejection may have been retained for 2.8-3.0 Myr since NewWorld Bohemian waxwings inherited it from their common ancestor with the rejecter cedar waxwings. These results support the 'single trajectory' model of host-brood parasite coevolution that once hosts evolve defences, they are retained, forcing parasites to become more specialized over time.
C1 [Peer, Brian D.; Fleischer, Robert C.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA.
[Peer, Brian D.; Kuehn, Michael J.; Rothstein, Stephen I.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[Peer, Brian D.] Western Illinois Univ, Dept Sci Biol, Macomb, IL 61455 USA.
[Kuehn, Michael J.] Western Fdn Vertebrate Zool, Camarillo, CA 93012 USA.
RP Peer, BD (reprint author), Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA.
EM bd-peer@wiu.edu
FU Western Illinois University; N.S.F. [0078139]
FX This research was supported by N.S.F. grant 0078139 awarded to S.I.R.,
R.C.F. and B.D.P. B.D.P. and R.C.F. were supported by a Faculty
Mentoring grant from Western Illinois University while preparing the
article.
NR 24
TC 18
Z9 20
U1 3
U2 26
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 1744-9561
EI 1744-957X
J9 BIOL LETTERS
JI Biol. Lett.
PD OCT 23
PY 2011
VL 7
IS 5
BP 670
EP 673
DI 10.1098/rsbl.2011.0268
PG 4
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 818QE
UT WOS:000294768400011
PM 21493623
ER
PT J
AU Yunes, N
Kocsis, B
Loeb, A
Haiman, Z
AF Yunes, Nicolas
Kocsis, Bence
Loeb, Abraham
Haiman, Zoltan
TI Imprint of Accretion Disk-Induced Migration on Gravitational Waves from
Extreme Mass Ratio Inspirals
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ACTIVE GALACTIC NUCLEI; STANDARD SIRENS; BLACK-HOLES; PLANET MIGRATION;
MHD TURBULENCE; VISCOSITY; LISA; SATELLITES; BINARIES; STARS
AB We study the effects of a thin gaseous accretion disk on the inspiral of a stellar-mass black hole into a supermassive black hole. We construct a phenomenological angular momentum transport equation that reproduces known disk effects. Disk torques modify the gravitational wave phase evolution to detectable levels with LISA for reasonable disk parameters. The Fourier transform of disk-modified waveforms acquires a correction with a different frequency trend than post-Newtonian vacuum terms. Such inspirals could be used to detect accretion disks with LISA and to probe their physical parameters.
C1 [Yunes, Nicolas] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Yunes, Nicolas] MIT Kavli Inst, Cambridge, MA 02139 USA.
[Yunes, Nicolas; Kocsis, Bence; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Haiman, Zoltan] Columbia Univ, Dept Astron, New York, NY 10027 USA.
RP Yunes, N (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RI Kocsis, Bence/C-3061-2013
OI Kocsis, Bence/0000-0002-4865-7517
FU NASA [PF9-00063, PF0-110080, NAS8-03060, NNX08AL43G, NNA09DB30A,
NNX08AH35G]; NSF [AST-0907890]; Hungarian National Office for Research
and Technology (NKTH); Hungarian Research Fund (OTKA) [68228]
FX B. K. and N. Y. acknowledge support from the NASA through Einstein
Fellowship PF9-00063 and PF0-110080 issued by the Chandra X-ray
Observatory, operated by the SAO, on behalf of NASA under NAS8-03060. A.
L. acknowledges support from NSF grant AST-0907890 and NASA grants
NNX08AL43G and NNA09DB30A, Z. H. from the Polanyi Program of the
Hungarian National Office for Research and Technology (NKTH) and from
NASA grant NNX08AH35G, and B. K. from the Hungarian Research Fund (OTKA)
grant 68228.
NR 38
TC 28
Z9 28
U1 0
U2 0
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 OCT 21
PY 2011
VL 107
IS 17
AR 171103
DI 10.1103/PhysRevLett.107.171103
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 847PN
UT WOS:000296985000001
PM 22107500
ER
PT J
AU Hong, J
Allen, B
Grindlay, J
Barthelemy, S
Baker, R
Garson, A
Krawczynski, H
Apple, J
Cleveland, WH
AF Hong, J.
Allen, B.
Grindlay, J.
Barthelemy, S.
Baker, R.
Garson, A.
Krawczynski, H.
Apple, J.
Cleveland, W. H.
TI Flight performance of an advanced CZT imaging detector in a
balloon-borne wide-field hard X-ray telescope-ProtoEXIST1
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE Hard X-ray imaging; CdZnTe; Coded-aperture imaging
AB We successfully carried out the first high-altitude balloon flight of a wide-field hard X-ray coded-aperture telescope ProtoEXIST1, which was launched from the Columbia Scientific Balloon Facility at Ft. Sumner, New Mexico on October 9, 2009. ProtoEXIST1 is the first implementation of an advanced CdZnTe (CZT) imaging detector in our ongoing program to establish the technology required for next generation wide-field hard X-ray telescopes such as the High Energy Telescope (HET) in the Energetic X-ray Imaging Survey Telescope (EXIST). The CZT detector plane in ProtoEXIST1 consists of an 8 x 8 array of closely tiled 2 cm x 2 cm x 0.5 cm thick pixellated CZT crystals, each with 8 x 8 pixels, mounted on a set of readout electronics boards and covering a 256 cm(2) active area with 2.5 mm pixels. A tungsten mask, mounted at 90 cm above the detector provides shadowgrams of X-ray sources in the 30-600 keV band for imaging, allowing a fully coded field of view of 9 degrees x 9 degrees (and 19 degrees x 19 degrees for 50% coding fraction) with an angular resolution of 20'. In order to reduce the background radiation, the detector is surrounded by semi-graded (Pb/Sn/Cu) passive shields on the four sides all the way to the mask. On the back side, a 26 cm x 26 cm x 2 cm CsI(Na) active shield provides signals to tag charged particle induced events as well as greater than or similar to 100 keV background photons from below. The flight duration was only about 7.5 h due to strong winds (60 knots) at float altitude (38-39 km). Throughout the flight, the CZT detector performed excellently. The telescope observed Cyg X-1, a bright black hole binary system, for similar to 1 h at the end of the flight. Despite a few problems with the pointing and aspect systems that caused the telescope to track about 6.4 degrees off the target, the analysis of the Cyg X-1 data revealed an X-ray source at 7.2 sigma in the 30-100 key energy band at the expected location from the optical images taken by the onboard daytime star camera. The success of this first flight is very encouraging for the future development of the advanced CZT imaging detectors (ProtoEXIST2, with 0.6 mm pixels), which will take advantage of the modularization architecture employed in ProtoEXIST1. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Hong, J.; Allen, B.; Grindlay, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Barthelemy, S.; Baker, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Garson, A.; Krawczynski, H.] Washington Univ, St Louis, MO 63130 USA.
[Garson, A.; Krawczynski, H.] McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Apple, J.; Cleveland, W. H.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Apple, J.; Cleveland, W. H.] Univ Space Res Assoc, Huntsville, AL 35812 USA.
RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jaesub@head.cfa.harvard.edu
FU NASA [NNG06WC12G, NNXO9AD76G, NNX10AJ56G]
FX This work was supported by NASA Grants NNG06WC12G and NNXO9AD76G to
Harvard University, and NASA Grant NNX10AJ56G to Washington University
in St. Louis. We thank M. Burke (SAO engineering), N. Gehrels (GSFC), K.
Dietz, C.M. Benson, B. Ramsey (MSFC), D. Huie (University of Alabama
Hunsville), W.R. Cook and F. Harrison (Caltech) for their support in the
development and assembly of the ProtoEXIST1 detector, telescope and
gondola. We also thank the McDonnell Center for the Space Sciences for
their support in the active CsI shield assembly, and the NASA CSBF
balloon launching team for their excellent support.
NR 18
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD OCT 21
PY 2011
VL 654
IS 1
BP 361
EP 372
DI 10.1016/j.nima.2011.07.025
PG 12
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 831XT
UT WOS:000295765100051
ER
PT J
AU Hogerheijde, MR
Bergin, EA
Brinch, C
Cleeves, LI
Fogel, JKJ
Blake, GA
Dominik, C
Lis, DC
Melnick, G
Neufeld, D
Panic, O
Pearson, JC
Kristensen, L
Yildiz, UA
van Dishoeck, EF
AF Hogerheijde, Michiel R.
Bergin, Edwin A.
Brinch, Christian
Cleeves, L. Ilsedore
Fogel, Jeffrey K. J.
Blake, Geoffrey A.
Dominik, Carsten
Lis, Dariusz C.
Melnick, Gary
Neufeld, David
Panic, Olja
Pearson, John C.
Kristensen, Lars
Yildiz, Umut A.
van Dishoeck, Ewine F.
TI Detection of the Water Reservoir in a Forming Planetary System
SO SCIENCE
LA English
DT Article
ID T TAURI STARS; PROTOPLANETARY DISKS; HERSCHEL; LINES; ICE; INTERSTELLAR;
EMISSION; SURFACE; REGION; GRAINS
AB Icy bodies may have delivered the oceans to the early Earth, yet little is known about water in the ice-dominated regions of extrasolar planet-forming disks. The Heterodyne Instrument for the Far-Infrared on board the Herschel Space Observatory has detected emission lines from both spin isomers of cold water vapor from the disk around the young star TW Hydrae. This water vapor likely originates from ice-coated solids near the disk surface, hinting at a water ice reservoir equivalent to several thousand Earth oceans in mass. The water's ortho-to-para ratio falls well below that of solar system comets, suggesting that comets contain heterogeneous ice mixtures collected across the entire solar nebula during the early stages of planetary birth.
C1 [Hogerheijde, Michiel R.; Brinch, Christian; Kristensen, Lars; Yildiz, Umut A.; van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Bergin, Edwin A.; Cleeves, L. Ilsedore; Fogel, Jeffrey K. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Dominik, Carsten] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Lis, Dariusz C.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Melnick, Gary] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Neufeld, David] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Panic, Olja] European So Observ, D-85748 Garching, Germany.
[Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
RP Hogerheijde, MR (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM michiel@strw.leidenuniv.nl
RI Kristensen, Lars/F-4774-2011; Yildiz, Umut/C-5257-2011; Brinch,
Christian/G-5157-2015
OI Kristensen, Lars/0000-0003-1159-3721; Yildiz, Umut/0000-0001-6197-2864;
Brinch, Christian/0000-0002-5074-7183
FU Nederlandse Organisatie voor Wetenschappelijk Onderzoek [639.042.404];
NSF [0707777]; NASA
FX Herschel is a European Space Agency space observatory with science
instruments provided by European-led principal investigator consortia
and with important participation from NASA. This work was partially
supported by Nederlandse Organisatie voor Wetenschappelijk Onderzoek
grant 639.042.404, NSF grant 0707777, and, as part of the NASA Herschel
HIFI guaranteed time program, NASA. The data presented here are archived
at the Herschel Science Archive, http://archives.esac.esa.int/hda/ui,
under OBSID 1342198337 and 1342201585.
NR 24
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U1 4
U2 18
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 OCT 21
PY 2011
VL 334
IS 6054
BP 338
EP 340
DI 10.1126/science.1208931
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 835RC
UT WOS:000296052500042
PM 22021851
ER
PT J
AU Cox, P
Krips, M
Neri, R
Omont, A
Gusten, R
Menten, KM
Wyrowski, F
Weiss, A
Beelen, A
Gurwell, MA
Dannerbauer, H
Ivison, RJ
Negrello, M
Aretxaga, I
Hughes, DH
Auld, R
Baes, M
Blundell, R
Buttiglione, S
Cava, A
Cooray, A
Dariush, A
Dunne, L
Dye, S
Eales, SA
Frayer, D
Fritz, J
Gavazzi, R
Hopwood, R
Ibar, E
Jarvis, M
Maddox, S
Michallowski, M
Pascale, E
Pohlen, M
Rigby, E
Smith, DJB
Swinbank, AM
Temi, P
Valtchanov, I
van der Werf, P
de Zotti, G
AF Cox, P.
Krips, M.
Neri, R.
Omont, A.
Guesten, R.
Menten, K. M.
Wyrowski, F.
Weiss, A.
Beelen, A.
Gurwell, M. A.
Dannerbauer, H.
Ivison, R. J.
Negrello, M.
Aretxaga, I.
Hughes, D. H.
Auld, R.
Baes, M.
Blundell, R.
Buttiglione, S.
Cava, A.
Cooray, A.
Dariush, A.
Dunne, L.
Dye, S.
Eales, S. A.
Frayer, D.
Fritz, J.
Gavazzi, R.
Hopwood, R.
Ibar, E.
Jarvis, M.
Maddox, S.
Michallowski, M.
Pascale, E.
Pohlen, M.
Rigby, E.
Smith, D. J. B.
Swinbank, A. M.
Temi, P.
Valtchanov, I.
van der Werf, P.
de Zotti, G.
TI GAS AND DUST IN A SUBMILLIMETER GALAXY AT z=4.24 FROM THE HERSCHEL ATLAS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: high-redshift;
galaxies: individual (ID 141); galaxies: starburst; submillimeter:
galaxies
ID ULTRALUMINOUS INFRARED GALAXIES; ISO-LWS SPECTROSCOPY; MICRON LINE
DEFICIT; STAR-FORMATION; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; ATOMIC
CARBON; MU-M; MOLECULAR GAS; PHYSICAL CONDITIONS
AB We report ground-based follow-up observations of the exceptional source, ID 141, one of the brightest sources detected so far in the Herschel Astrophysical Terahertz Large Area Survey cosmological survey. ID 141 was observed using the IRAM 30 m telescope and Plateau de Bure interferometer (PdBI), the Submillimeter Array, and the Atacama Pathfinder Experiment submillimeter telescope to measure the dust continuum and emission lines of the main isotope of carbon monoxide and carbon ([C I] and [C II]). The detection of strong CO emission lines with the PdBI confirms that ID 141 is at high redshift (z = 4.243 +/- 0.001). The strength of the continuum and emission lines suggests that ID 141 is gravitationally lensed. The width (Delta V-FWHM similar to 800 km s(-1)) and asymmetric profiles of the CO and carbon lines indicate orbital motion in a disk or a merger. The properties derived for ID 141 are compatible with an ultraluminous (L-FIR similar to (8.5 +/- 0.3) x 10(13) mu(-1)(L) L-circle dot, where mu L is the amplification factor), dense (n approximate to 10(4) cm(-3)), and warm (T-kin approximate to 40 K) starburst galaxy, with an estimated star formation rate of (0.7-1.7) x 10(4) mu(-1)(L) M-circle dot yr(-1). The carbon emission lines indicate a dense (n approximate to 10(4) cm(-3)) photon-dominated region, illuminated by a far-UV radiation field a few thousand times more intense than that in our Galaxy. In conclusion, the physical properties of the high-z galaxy ID 141 are remarkably similar to those of local ultraluminous infrared galaxies.
C1 [Cox, P.; Krips, M.; Neri, R.] IRAM, F-38406 St Martin Dheres, France.
[Omont, A.; Gavazzi, R.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France.
[Omont, A.; Gavazzi, R.] CNRS, UMR7095, F-75014 Paris, France.
[Guesten, R.; Menten, K. M.; Wyrowski, F.; Weiss, A.] MPIfR, D-53121 Bonn, Germany.
[Beelen, A.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Gurwell, M. A.; Blundell, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dannerbauer, H.] CEA DSM CNRS Univ Paris Diderot, DAPNIA Serv Astrophys, CEA Saclay, AIM, F-91191 Gif Sur Yvette, France.
[Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Michallowski, M.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Negrello, M.; Hopwood, R.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico.
[Auld, R.; Dariush, A.; Eales, S. A.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Buttiglione, S.; Jarvis, M.; de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Buttiglione, S.; Jarvis, M.; de Zotti, G.] SISSA, I-34136 Trieste, Italy.
[Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran.
[Dunne, L.; Dye, S.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Swinbank, A. M.] Univ Durham, Inst Computat Cosmol, Durham DH1 3EE, England.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[Valtchanov, I.] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Cox, P (reprint author), IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France.
EM cox@iram.fr
RI Baes, Maarten/I-6985-2013; Ivison, R./G-4450-2011; Cava,
Antonio/C-5274-2017;
OI Baes, Maarten/0000-0002-3930-2757; Ivison, R./0000-0001-5118-1313; Cava,
Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X; Dye,
Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X
FU NASA through JPL; Centre National de la Recherche Scientifique (France);
Max-Planck Gesellschaft (Germany); Instituto Geografico Nacional
(Spain); Smithsonian Institution; Academia Sinica; CONACyT [39953-F];
[ASI-INAF I009/10/0]
FX The results described in this paper are based on observations obtained
with Herschel, an ESA space observatory with science instruments
provided by European-led Principal Investigator consortia and with
important participation from NASA. US participants in H-ATLAS
acknowledge support from NASA through a contract from JPL. The
ground-based follow-up observations were obtained at the following
facilities. The 30 m telescope and the PdBI of IRAM that is funded by
the Centre National de la Recherche Scientifique (France), the
Max-Planck Gesellschaft (Germany), and the Instituto Geografico Nacional
(Spain). APEX is a collaboration between the Max-Planck-Institut fur
Radioastronomie, the European Southern Observatory, and the Onsala Space
Observatory. The Submillimeter Array (SMA) is a joint project between
the Smithsonian Astrophysical Observatory and the Academia Sinica
Institute of Astronomy and Astrophysics and is funded by the Smithsonian
Institution and the Academia Sinica. Part of this study was supported by
financial contribution from the agreement ASI-INAF I009/10/0 and by
CONACyT grant 39953-F.
NR 69
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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 OCT 20
PY 2011
VL 740
IS 2
AR 63
DI 10.1088/0004-637X/740/2/63
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900013
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
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: photometry; supernovae: general
ID DIGITAL SKY SURVEY; STELLAR POPULATION SYNTHESIS; INITIAL MASS FUNCTION;
LIGHT-CURVE SHAPES; STAR-FORMATION; HUBBLE DIAGRAM; LOCAL UNIVERSE;
SN-IA; METALLICITY; LUMINOSITY
AB We improve estimates of the stellar mass and mass-weighted average age of Type Ia supernova (SN Ia) host galaxies by combining UV and near-IR photometry with optical photometry in our analysis. Using 206 SNe Ia drawn from the full three-year Sloan Digital Sky Survey (SDSS-II) Supernova Survey (median redshift of z approximate to 0.2) and multi-wavelength host-galaxy photometry from SDSS, the Galaxy Evolution Explorer, and the United Kingdom Infrared Telescope Infrared Deep Sky Survey, we present evidence of a correlation (1.9 sigma confidence level) between the residuals of SNe Ia about the best-fit Hubble relation and the mass-weighted average age of their host galaxies. The trend is such that older galaxies host SNe Ia that are brighter than average after standard light-curve corrections are made. We also confirm, at the 3.0 sigma level, the trend seen by previous studies that more massive galaxies often host brighter SNe Ia after light-curve 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] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Rondebosch, 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
OI Bassett, Bruce/0000-0001-7700-1069
FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department
of Energy; National Aeronautics and Space Administration [NNX09AC75G];
Japanese Monbukagakusho; Max Planck Society; Higher Education Funding
Council for England; American Museum of Natural History; Astrophysical
Institute Potsdam; University of Basel; Cambridge University; 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 (MPA);
Max-Planck-Institute for Astrophysics (MPIA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington; W. M. Keck Foundation
FX Funding for the creation and distribution of 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, Cambridge University, 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 (MPA), the
Max-Planck-Institute for Astrophysics (MPIA), 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.; This work is based in
part on observations made at the following telescopes. The Hobby-Eberly
Telescope (HET) is a joint project of the University of Texas at Austin,
the Pennsylvania State University, Stanford University,
Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat
Gottingen. The HET is named in honor of its principal benefactors,
William P. Hobby and Robert E. Eberly. The Marcario Low-Resolution
Spectrograph is named for Mike Marcario of High Lonesome Optics, who
fabricated several optical elements for the instrument but died before
its completion; it is a joint project of the Hobby-Eberly Telescope
partnership and the Instituto de Astronomia de la Universidad Nacional
Autonomade Mexico. The Apache Point Observatory 3.5 m telescope is owned
and operated by the Astrophysical Research Consortium. We thank the
observatory director, Suzanne Hawley, and site manager, Bruce Gillespie,
for their support of this project. The Subaru Telescope is operated by
the National Astronomical Observatory of Japan. The William Herschel
Telescope is operated by the Isaac Newton Group on the island of La
Palma in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofisica de Canarias. The W. M. Keck Observatory is
operated as a scientific partnership among the California Institute of
Technology, the University of California, and the National Aeronautics
and Space Administration; the observatory was made possible by the
generous financial support of the W. M. Keck Foundation.; This work was
funded by the NASA ADP Program NNX09AC75G.
NR 61
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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 OCT 20
PY 2011
VL 740
IS 2
AR 92
DI 10.1088/0004-637X/740/2/92
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900042
ER
PT J
AU Hajian, A
Acquaviva, V
Ade, PAR
Aguirre, P
Amiri, M
Appel, JW
Barrientos, LF
Battistelli, ES
Bond, JR
Brown, B
Burger, B
Chervenak, J
Das, S
Devlin, MJ
Dicker, SR
Doriese, WB
Dunkley, J
Dunner, R
Essinger-Hileman, T
Fisher, RP
Fowler, JW
Halpern, M
Hasselfield, M
Hernandez-Monteagudo, C
Hilton, GC
Hilton, M
Hincks, AD
Hlozek, R
Huffenberger, KM
Hughes, DH
Hughes, JP
Infante, L
Irwin, KD
Juin, JB
Kaul, M
Klein, J
Kosowsky, A
Lau, JM
Limon, M
Lin, YT
Lupton, RH
Marriage, TA
Marsden, D
Mauskopf, P
Menanteau, F
Moodley, K
Moseley, H
Netterfield, CB
Niemack, MD
Nolta, MR
Page, LA
Parker, L
Partridge, B
Reid, B
Sehgal, N
Sherwin, BD
Sievers, J
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Thornton, R
Trac, H
Tucker, C
Warne, R
Wollack, E
Zhao, Y
AF Hajian, Amir
Acquaviva, Viviana
Ade, Peter A. R.
Aguirre, Paula
Amiri, Mandana
Appel, John William
Felipe Barrientos, L.
Battistelli, Elia S.
Bond, John R.
Brown, Ben
Burger, Bryce
Chervenak, Jay
Das, Sudeep
Devlin, Mark J.
Dicker, Simon R.
Doriese, W. Bertrand
Dunkley, Joanna
Duenner, Rolando
Essinger-Hileman, Thomas
Fisher, Ryan P.
Fowler, Joseph W.
Halpern, Mark
Hasselfield, Matthew
Hernandez-Monteagudo, Carlos
Hilton, Gene C.
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Huffenberger, Kevin M.
Hughes, David H.
Hughes, John P.
Infante, Leopoldo
Irwin, Kent D.
Baptiste Juin, Jean
Kaul, Madhuri
Klein, Jeff
Kosowsky, Arthur
Lau, Judy M.
Limon, Michele
Lin, Yen-Ting
Lupton, Robert H.
Marriage, Tobias A.
Marsden, Danica
Mauskopf, Phil
Menanteau, Felipe
Moodley, Kavilan
Moseley, Harvey
Netterfield, Calvin B.
Niemack, Michael D.
Nolta, Michael R.
Page, Lyman A.
Parker, Lucas
Partridge, Bruce
Reid, Beth
Sehgal, Neelima
Sherwin, Blake D.
Sievers, Jon
Spergel, David N.
Staggs, Suzanne T.
Swetz, Daniel S.
Switzer, Eric R.
Thornton, Robert
Trac, Hy
Tucker, Carole
Warne, Ryan
Wollack, Ed
Zhao, Yue
TI THE ATACAMA COSMOLOGY TELESCOPE: CALIBRATION WITH THE WILKINSON
MICROWAVE ANISOTROPY PROBE USING CROSS-CORRELATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; methods: data
analysis; methods: statistical
ID BACKGROUND POWER SPECTRUM; WMAP OBSERVATIONS; 148 GHZ; GALAXY CLUSTERS;
BEAM PROFILES; ARRAY CAMERA; 2003 FLIGHT; TEMPERATURE; MAPS;
POLARIZATION
AB We present a new calibration method based on cross-correlations with the Wilkinson Microwave Anisotropy Probe (WMAP) and apply it to data from the Atacama Cosmology Telescope (ACT). ACT's observing strategy and map-making procedure allows an unbiased reconstruction of the modes in the maps over a wide range of multipoles. By directly matching the ACT maps to WMAP observations in the multipole range of 400 < l < 1000, we determine the absolute calibration with an uncertainty of 2% in temperature. The precise measurement of the calibration error directly impacts the uncertainties in the cosmological parameters estimated from the ACT power spectra. We also present a combined map based on ACT and WMAP data that has a high signal-to-noise ratio over a wide range of multipoles.
C1 [Hajian, Amir; Bond, John R.; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Hajian, Amir; Acquaviva, Viviana; Das, Sudeep; Dunkley, Joanna; Lin, Yen-Ting; Lupton, Robert H.; Marriage, Tobias A.; Spergel, David N.; Trac, Hy] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hajian, Amir; Appel, John William; Das, Sudeep; Dunkley, Joanna; Duenner, Rolando; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hincks, Adam D.; Lau, Judy M.; Limon, Michele; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.; Zhao, Yue] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Acquaviva, Viviana; Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aguirre, Paula; Felipe Barrientos, L.; Infante, Leopoldo; Baptiste Juin, Jean; Lin, Yen-Ting] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Chervenak, Jay; Moseley, Harvey; Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
[Devlin, Mark J.; Dicker, Simon R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Marsden, Danica; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Doriese, W. Bertrand; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Cape Town, South Africa.
[Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Hughes, David H.] INAOE, Puebla, Mexico.
[Lau, Judy M.; Sehgal, Neelima] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Limon, Michele] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan.
[Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Reid, Beth] Univ Barcelona, ICREA, Barcelona 08028, Spain.
[Reid, Beth] Univ Barcelona, ICC, Barcelona 08028, Spain.
[Switzer, Eric R.] Kavli Inst Cosmol Phys, Lab Astrophys & Space Res, Chicago, IL 60637 USA.
[Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
[Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hajian, A (reprint author), Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew
James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Huffenberger, Kevin/0000-0001-7109-0099; Sievers,
Jonathan/0000-0001-6903-5074; Limon, Michele/0000-0002-5900-2698
FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
PIRE-0507768]; Princeton University; University of Pennsylvania; Canada
Foundation for Innovation under the auspices of Compute Canada;
Government of Ontario; Ontario Research Fund-Research Excellence;
University of Toronto; NASA [NNX08AH30G]; Natural Science and
Engineering Research Council of Canada (NSERC); NSF [AST-0546035,
AST-0606975]; FONDAP Centro de Astrofisica; CONICYT; MECESUP; Fundacion
Andes; NSF Physics Frontier Center [PHY-0114422]; South African National
Research Foundation (NRF); Meraka Institute; South African Square
Kilometer Array (SKA) Project; RCUK; Berkeley Center for Cosmological
Physics; World Premier International Research Center Initiative, MEXT,
Japan; U.S. Department of Energy [DE-AC3-76SF00515]; NASA Office of
Space Science
FX This work was supported by the U.S. National Science Foundation through
awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731,
and PIRE-0507768. Funding was also provided by Princeton University and
the University of Pennsylvania. The PIRE program made possible exchanges
between Chile, South Africa, Spain, and the United States that enabled
this research program. Computations were performed on the GPC
supercomputer at the SciNet HPC Consortium. SciNet is funded by the
Canada Foundation for Innovation under the auspices of Compute Canada;
the Government of Ontario; Ontario Research Fund-Research Excellence;
and the University of Toronto.; A. H., V. A., S. D., and T. A. M. were
supported through NASA grant NNX08AH30G. A. D. H. received additional
support from a Natural Science and Engineering Research Council of
Canada (NSERC) PGS-D scholarship. A. K. and B. P. were partially
supported through NSF AST-0546035 and AST-0606975, respectively, for
work on ACT. L. I. acknowledge partial support from FONDAP Centro de
Astrofisica. R. D. was supported by CONICYT, MECESUP, and Fundacion
Andes. E. R. S. acknowledges support by NSF Physics Frontier Center
grant PHY-0114422 to the Kavli Institute of Cosmological Physics. K.M.,
M. Hilton, and R. W. received financial support from the South African
National Research Foundation (NRF), the Meraka Institute via funding for
the South African Centre for High Performance Computing (CHPC), and the
South African Square Kilometer Array (SKA) Project. J.D. received
support from an RCUK Fellowship. R. H. received funding from the Rhodes
Trust. We thank Norm Jarosik for useful discussions and his
contributions. S.D. acknowledges support from the Berkeley Center for
Cosmological Physics. Y.-T.L. acknowledges support from the World
Premier International Research Center Initiative, MEXT, Japan. N.S. is
supported by the U.S. Department of Energy contract to SLAC No.
DE-AC3-76SF00515. 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. The data will be made
public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web
site (http://www.physics.princeton.edu/act/). Some of the results in
this paper have been derived using the HEALPix (Gorski et al. 2005)
package.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
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DI 10.1088/0004-637X/740/2/86
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900036
ER
PT J
AU Leier, D
Ferreras, I
Saha, P
Falco, EE
AF Leier, Dominik
Ferreras, Ignacio
Saha, Prasenjit
Falco, Emilio E.
TI RESOLVING THE BARYON-FRACTION PROFILE IN LENSING GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: elliptical and lenticular, cD; galaxies: stellar
content; gravitational lensing: strong
ID INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; DARK-MATTER HALOES; TO-LIGHT
RATIOS; LINE-OF-SIGHT; GRAVITATIONAL LENS; ELLIPTIC GALAXIES; STELLAR
MASS; BLACK-HOLES; FUNDAMENTAL PLANE
AB The study of the distribution of baryonic matter within dark halos enriches our understanding of galaxy formation. We show the radial dependence of stellar baryon-fraction curves derived for 21 lensing galaxies from the CfA-Arizona Space Telescope LEns Survey (CASTLES) by means of stellar population synthesis and pixel-based mass reconstruction. The sample covers a stellar mass range of M-s similar or equal to 2 x 10(9)-3 x 10(11) M-circle dot (solar masses) which corresponds to a total enclosed mass range of M-L similar or equal to 7 x 10(9)-3 x 10(12) M-circle dot on radial scales from 0.25 R-e to 5 R-e (effective radii). By examining the M-s and M-L dependence on radial distance to the center of each galaxy, we find that there are pairs of lenses on small to intermediate mass scales which approach at large radii the same values for their enclosed total mass but exhibit very different stellar masses and stellar baryon fractions. This peculiar behavior subsides for the most massive lensing galaxies. All the baryon-fraction profiles show that the dark matter halo overtakes the stellar content between 1.5 and 2.5R(e). At 3R(e) most of the stellar component is enclosed. We find evidence for a stellar baryon fraction steadily declining over the full mass range. Furthermore, we shed light on the Fundamental Plane puzzle by showing that the slope of the M-L(< R)-to-M-s ( T10) BROWN DWARF IN A BINARY SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; binaries: general; brown dwarfs; infrared: stars;
techniques: high angular resolution
ID STAR ADAPTIVE OPTICS; EXTRASOLAR GIANT PLANETS; EXOPLANET HOST STAR;
INFRARED FILTER SET; MID-T DWARFS; DYNAMICAL MASS; EVOLUTIONARY MODELS;
SPECTRAL CLASSIFICATION; PHYSICAL-PROPERTIES; L/T TRANSITION
AB We have identified CFBDSIR J1458+1013 as a 0 ''.11 (2.6 AU) physical binary using Keck laser guide star adaptive optics imaging and have measured a distance of 23.1 +/- 2.4 pc to the system based on near-IR parallax data from the Canada-France-Hawaii Telescope. The integrated-light near-IR spectrum indicates a spectral type of T9.5, and model atmospheres suggest a slightly higher temperature and surface gravity than the T10 dwarf UGPS J0722-05. Thus, CFBDSIR J1458+1013AB is the coolest brown dwarf binary found to date. Its secondary component has an absolute H-band magnitude that is 1.9 +/- 0.3 mag fainter than UGPS J0722-05, giving an inferred spectral type of >T10. The secondary's bolometric luminosity of similar to 2 x 10(-7) L-circle dot makes it the least luminous known brown dwarf by a factor of 4-5. By comparing to evolutionary models and T9-T10 objects, we estimate a temperature of 370 +/- 40 K and a mass of 6-15 M-Jup for CFBDSIR J1458+1013B. At such extremes, atmospheric models predict the onset of novel photospheric processes, namely, the appearance of water clouds and the removal of strong alkali lines, but their impact on the emergent spectrum is highly uncertain. Our photometry shows that strong CH4 absorption persists in the H band, the J - K color is bluer than the latest known T dwarfs but not as blue as predicted by current models, and the J - H color delineates a possible inflection in the blueward trend for the latest T dwarfs. Given its low luminosity, atypical colors, and cold temperature, CFBDSIR J1458+1013B is a promising candidate for the hypothesized Y spectral class. However, regardless of its ultimate classification, CFBDSIR J1458+1013AB provides a new benchmark for measuring the properties of brown dwarfs and gas-giant planets, testing substellar models, and constraining the low-mass limit for star formation.
C1 [Liu, Michael C.; Bowler, Brendan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Delorme, Philippe; Forveille, Thierry; Delfosse, Xavier] UJF Grenoble 1, CNRS, IPAG, UMR 5274,INSU, F-38041 Grenoble, France.
[Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Albert, Loic] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA.
[Artigau, Etienne] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Artigau, Etienne] Univ Montreal, Observ Mt Megant, Montreal, PQ H3C 3J7, Canada.
[Reyle, Celine] Univ Franche Comte, Observ Besancon, Inst Utinam, CNRS,UMR 6213, F-25010 Besancon, France.
RP Liu, MC (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM mliu@ifa.hawaii.edu
FU W. M. Keck Foundation; NSF [AST-0507833, AST-0909222]; NASA
[HF-51271.01-A, NAS 5-26555]; Space Telescope Science Institute
FX 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.; It is a pleasure to thank Jim Lyke, Gary Punawai, Cynthia
Wilburn, and the Keck Observatory staff for assistance with the LGS AO
observing and the staffs of CFHT and VLT for carrying out the queue
imaging and spectroscopy. We thank Sandy Leggett and Didier Saumon for
making published results readily available and thank Kathleen Brandt for
assistance while this paper was being written. Our research has employed
the 2MASS data products; NASA's Astrophysical Data System; the SIMBAD
database operated at CDS, Strasbourg, France; and the SpeX Prism
Spectral Libraries maintained by Adam Burgasser at
http://www.browndwarfs.org/spexprism. M.C.L., T.J.D., and B.P.B.
acknowledge support for this work from NSF grants AST-0507833 and
AST-0909222. Support for this work to T.J.D. was partially provided by
NASA through Hubble Fellowship grant HF-51271.01-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555. Finally, the authors wish to recognize and acknowledge the
very significant cultural role and reverence that the summit of Mauna
Kea has always had within the indigenous Hawaiian community. We are most
fortunate to have the opportunity to conduct observations from this
mountain.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
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DI 10.1088/0004-637X/740/2/108
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900058
ER
PT J
AU Lynch, BJ
Reinard, AA
Mulligan, T
Reeves, KK
Rakowski, CE
Allred, JC
Li, Y
Laming, JM
MacNeice, PJ
Linker, JA
AF Lynch, B. J.
Reinard, A. A.
Mulligan, T.
Reeves, K. K.
Rakowski, C. E.
Allred, J. C.
Li, Y.
Laming, J. M.
MacNeice, P. J.
Linker, J. A.
TI IONIC COMPOSITION STRUCTURE OF CORONAL MASS EJECTIONS IN AXISYMMETRIC
MAGNETOHYDRODYNAMIC MODELS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; magnetohydrodynamics (MHD); Sun: corona; Sun:
coronal mass ejections (CMEs); Sun: flares; Sun: heliosphere
ID INTER-PLANETARY SHOCK; SLOW SOLAR-WIND; CHARGE STATES;
ELECTRON-TEMPERATURE; COMPOSITION SPECTROMETER; MAGNETIC-STRUCTURE; FLUX
CANCELLATION; SOHO OBSERVATIONS; IONIZATION STATE; 1 AU
AB We present the ionic charge state composition structure derived from axisymmetric MHD simulations of coronal mass ejections (CMEs), initiated via the flux-cancellation and magnetic breakout mechanisms. The flux-cancellation CME simulation is run on the Magnetohydrodynamics-on-A-Sphere code developed at Predictive Sciences, Inc., and the magnetic breakout CME simulation is run on ARC7 developed at NASA GSFC. Both MHD codes include field-aligned thermal conduction, radiative losses, and coronal heating terms which make the energy equations sufficient to calculate reasonable temperatures associated with the steady-state solar wind and model the eruptive flare heating during CME formation and eruption. We systematically track a grid of Lagrangian plasma parcels through the simulation data and calculate the coronal density and temperature history of the plasma in and around the CME magnetic flux ropes. The simulation data are then used to integrate the continuity equations for the ionic charge states of several heavy ion species under the assumption that they act as passive tracers in the MHD flow. We construct two-dimensional spatial distributions of commonly measured ionic charge state ratios in carbon, oxygen, silicon, and iron that are typically elevated in interplanetary coronal mass ejection (ICME) plasma. We find that the slower CME eruption has relatively enhanced ionic charge states and the faster CME eruption shows basically no enhancement in charge states-which is the opposite trend to what is seen in the in situ ICME observations. The primary cause of the difference in the ionic charge states in the two simulations is not due to the different CME initiation mechanisms per se. Rather, the difference lies in their respective implementation of the coronal heating which governs the steady-state solar wind, density and temperature profiles, the duration of the connectivity of the CME to the eruptive flare current sheet, and the contribution of the flare-heated plasma associated with the reconnection jet outflow into the ejecta. Despite the limitations inherent in the first attempt at this novel procedure, the simulation results provide strong evidence in support of the conclusion that enhanced heavy ion charge states within CMEs are a direct consequence of flare heating in the low corona. We also discuss future improvements through combining numerical CME modeling with quantitative ionic charge state calculations.
C1 [Lynch, B. J.; Li, Y.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Reinard, A. A.] NOAA Space Weather Predict Ctr, Boulder, CO 80505 USA.
[Mulligan, T.] Aerosp Corp, Dept Space Sci, Los Angeles, CA 90009 USA.
[Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rakowski, C. E.; Laming, J. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Allred, J. C.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
[MacNeice, P. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Linker, J. A.] Predict Sci Inc, San Diego, CA 92121 USA.
RP Lynch, BJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM blynch@ssl.berkeley.edu; alysha.reinard@noaa.gov;
tamitha.mulligan@aero.org; kreeves@cfa.harvard.edu;
c.rakowski@nrl.navy.mil; jca32@drexel.edu; yanli@ssl.berkeley.edu;
j.laming@nrl.navy.mil; peter.j.macneice@nasa.gov; linkerj@presci.com
RI Lynch, Benjamin/B-1300-2013; Reinard, Alysha/H-7808-2013; Reeves,
Katharine/P-9163-2014; Allred, Joel/C-9550-2012; MacNeice,
Peter/F-5587-2012
OI Reinard, Alysha/0000-0003-0304-2989; Lynch,
Benjamin/0000-0001-6886-855X;
FU NASA [HTP NNX08AI56G NNX11AJ65G, NASA HGI NNX08AJ04G, SRT NNX08AH54G,
HGI NNG08EK62I, TRT NNG04GN00G]; Office of Naval Research; NSF [SHINE
ATM0752257]
FX B.J.L. thanks S. K. Antiochos and G. H. Fisher for helpful discussion
during the preparation of the manuscript. This collaborative research
was made possible with support from NASA's Heliosphysics Theory, Guest
Investigator, Living With a Star, and SR&T programs, as well as the NSF
SHINE program, the Office of Naval Research, and the Center for
Integrated Space Weather Modeling (an NSF Science and Technology
Center). B.J.L. and Y.L. acknowledge support from NASA HTP NNX08AI56G
NNX11AJ65G, and NASA HGI NNX08AJ04G; A.A.R. and T.L.M. acknowledge NASA
SR&T NNX08AH54G; C.E.R. and J.M.L. acknowledge NASA HGI NNG08EK62I and
basic research funds of the Office of Naval Research; K.K.R.
acknowledges NSF SHINE ATM0752257; and J.C.A. and P.J.M. acknowledge
support from NASA TR&T NNG04GN00G.
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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 OCT 20
PY 2011
VL 740
IS 2
AR 112
DI 10.1088/0004-637X/740/2/112
PG 15
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SC Astronomy & Astrophysics
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UT WOS:000296762900062
ER
PT J
AU Ma, CJ
McNamara, BR
Nulsen, PEJ
Schaffer, R
Vikhlinin, A
AF Ma, C-J
McNamara, B. R.
Nulsen, P. E. J.
Schaffer, R.
Vikhlinin, A.
TI AVERAGE HEATING RATE OF HOT ATMOSPHERES IN DISTANT CLUSTERS BY RADIO
ACTIVE GALACTIC NUCLEUS: EVIDENCE FOR CONTINUOUS ACTIVE GALACTIC NUCLEUS
HEATING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: intracluster medium;
quasars: general; radio continuum: galaxies; X-rays: galaxies: clusters
ID X-RAY CAVITIES; DEEP CHANDRA OBSERVATION; GALAXY CLUSTERS; COOLING
FLOWS; INTRACLUSTER MEDIUM; LUMINOSITY FUNCTION; THERMAL CONDUCTION;
GASEOUS ATMOSPHERE; REDSHIFT EVOLUTION; NEARBY CLUSTERS
AB We examine atmospheric heating by radio active galactic nuclei (AGNs) in distant X-ray clusters by cross correlating clusters selected from the 400 Square Degree (400SD) X-ray Cluster survey with radio sources in the NRAO VLA Sky Survey. Roughly 30% of the clusters show radio emission above a flux threshold of 3 mJy within a projected radius of 250 kpc. The radio emission is presumably associated with the brightest cluster galaxy. The mechanical jet power for each radio source was determined using scaling relations between radio power and cavity (mechanical) power determined for nearby clusters, groups, and galaxies with hot atmospheres containing X-ray cavities. The average jet power of central radio AGNs is approximately 2 x 10(44) erg s(-1). We find no significant correlation between radio power, and hence mechanical jet power, and the X-ray luminosities of clusters in the redshift range 0.1-0.6. This implies that the mechanical heating rate per particle is higher in lower mass, lower X-ray luminosity clusters. The jet power averaged over the sample corresponds to an atmospheric heating of approximately 0.2 keV per particle within R-500. Assuming the current AGN heating rate does not evolve but remains constant to redshifts of 2, the heating rate per particle would rise by a factor of two. We find that the energy injected from radio AGNs contribute substantially to the excess entropy in hot atmospheres needed to break self-similarity in cluster scaling relations. The detection frequency of radio AGNs is inconsistent with the presence of strong cooling flows in 400SD clusters, but does not exclude weak cooling flows. It is unclear whether central AGNs in 400SD clusters are maintained by feedback at the base of a cooling flow. Atmospheric heating by radio AGNs may retard the development of strong cooling flows at early epochs.
C1 [Ma, C-J; McNamara, B. R.; Schaffer, R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Ma, C-J; McNamara, B. R.; Nulsen, P. E. J.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Vikhlinin, A.] Space Res Inst IKI, Moscow, Russia.
RP Ma, CJ (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada.
OI Nulsen, Paul/0000-0003-0297-4493
FU Chandra Large Project [G09-0140X]; NASA [NAS8-03060]
FX C.-J.M. and B.R.M. are supported by Chandra Large Project Grant
G09-0140X. B.R.M. acknowledges generous support from the Natural
Sciences and Engineering Research Council of Canada. P.E.J.N. was
supported by NASA grant NAS8-03060.
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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 OCT 20
PY 2011
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AR 51
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SC Astronomy & Astrophysics
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UT WOS:000296762900001
ER
PT J
AU Oberg, KI
Boogert, ACA
Pontoppidan, KM
van den Broek, S
van Dishoeck, EF
Bottinelli, S
Blake, GA
Evans, NJ
AF Oeberg, Karin I.
Boogert, A. C. Adwin
Pontoppidan, Klaus M.
van den Broek, Saskia
van Dishoeck, Ewine F.
Bottinelli, Sandrine
Blake, Geoffrey A.
Evans, Neal J., II
TI THE SPITZER ICE LEGACY: ICE EVOLUTION FROM CORES TO PROTOSTARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; circumstellar matter; infrared: ISM; ISM: abundances;
ISM: lines and bands; ISM: molecules; molecular processes; stars:
formation
ID YOUNG STELLAR OBJECTS; LOW-MASS STARS; INTERSTELLAR GRAIN MANTLES; VLT
SPECTROSCOPIC SURVEY; MU-M; MOLECULAR CLOUDS; DENSE CLOUDS; INFRARED
OBSERVATIONS; GALACTIC-CENTER; UPPER LIMITS
AB Ices regulate much of the chemistry during star formation and account for up to 80% of the available oxygen and carbon. In this paper, we use the Spitzer c2d Legacy ice survey, complimented with data sets on ices in cloud cores and high-mass protostars, to determine standard ice abundances and to present a coherent picture of the evolution of ices during low-and high-mass star formation. The median ice composition H2O:CO:CO2:CH3OH:NH3:CH4:XCN is 100:29:29:3:5:5:0.3 and 100:13:13:4:5:2:0.6 toward low-and high-mass protostars, respectively, and 100:31:38:4:-:-:- in cloud cores. In the low-mass sample, the ice abundances with respect to H2O of CH4, NH3, and the component of CO2 mixed with H2O typically vary by <25%, indicative of co-formation with H2O. In contrast, some CO and CO2 ice components, XCN, and CH3OH vary by factors 2-10 between the lower and upper quartile. The XCN band correlates with CO, consistent with its OCN- identification. The origin(s) of the different levels of ice abundance variations are constrained by comparing ice inventories toward different types of protostars and background stars, through ice mapping, analysis of cloud-to-cloud variations, and ice (anti-)correlations. Based on the analysis, the first ice formation phase is driven by hydrogenation of atoms, which results in an H2O-dominated ice. At later prestellar times, CO freezes out and variations in CO freezeout levels and the subsequent CO-based chemistry can explain most of the observed ice abundance variations. The last important ice evolution stage is thermal and UV processing around protostars, resulting in CO desorption, ice segregation, and the formation of complex organic molecules. The distribution of cometary ice abundances is consistent with the idea that most cometary ices have a protostellar origin.
C1 [Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA.
[Boogert, A. C. Adwin] CALTECH, IPAC, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA.
[Pontoppidan, Klaus M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Oeberg, Karin I.; van den Broek, Saskia; van Dishoeck, Ewine F.; Bottinelli, Sandrine] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Bottinelli, Sandrine] CNRS, UMR 5187, CESR, F-31028 Toulouse 4, France.
[Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany.
RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA.
FU NASA [NAS 5-26555, 1224608, 1230779, 1407]; Space Telescope Science
Institute; Netherlands Organization for Scientific Research (NWO); W. M.
Keck Foundation
FX 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. Astrochemistry in Leiden is supported
by SPINOZA grant of the Netherlands Organization for Scientific Research
(NWO). Support for this work, part of the Spitzer Space Telescope Legacy
Science Program, was provided by NASA through contracts 1224608 and
1230779 issued by the Jet Propulsion Laboratory, California Institute of
Technology under NASA contract 1407. The W. M. Keck Observatory is
operated as a scientific partnership among the California Institute of
Technology, the University of California, and the National Aeronautics
and Space Administration, and was made possible by the generous
financial support of the W. M. Keck Foundation. The authors recognize
the cultural role and reverence that the summit of Mauna Kea has within
the indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. We acknowledge
helpful comments from an anonymous referee.
NR 82
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U1 3
U2 35
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 OCT 20
PY 2011
VL 740
IS 2
AR 109
DI 10.1088/0004-637X/740/2/109
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900059
ER
PT J
AU Qi, CH
D'Alessio, P
Oberg, KI
Wilner, DJ
Hughes, AM
Andrews, SM
Ayala, S
AF Qi, Chunhua
D'Alessio, Paola
Oeberg, Karin I.
Wilner, David J.
Hughes, A. Meredith
Andrews, Sean M.
Ayala, Sandra
TI RESOLVING THE CO SNOW LINE IN THE DISK AROUND HD 163296
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; ISM: abundances; planetary systems; protoplanetary
disks; radio lines: stars; stars: individual (HD 163296); techniques:
interferometric
ID HERBIG AE/BE STARS; MAIN-SEQUENCE STARS; T TAURI STARS; PROTOPLANETARY
DISKS; ACCRETION DISKS; CIRCUMSTELLAR DISKS; YOUNG OBJECTS; AE STARS;
DM-TAU; SUBMILLIMETER ARRAY
AB We report Submillimeter Array observations of CO (J = 2-1, 3-2, and 6-5) and its isotopologues ((CO)-C-13 J = 2-1, (CO)-O-18 J = 2-1, and (CO)-O-17 J = 3-2) in the disk around the Herbig Ae star HD 163296 at similar to 2 '' (250 AU) resolution, and interpret these data in the framework of a model that constrains the radial and vertical location of the line emission regions. First, we develop a physically self-consistent accretion disk model with an exponentially tapered edge that matches the spectral energy distribution and spatially resolved millimeter dust continuum emission. Then, we refine the vertical structure of the model using wide range of excitation conditions sampled by the CO lines, in particular the rarely observed J = 6-5 transition. By fitting (CO)-C-13 data in this structure, we further constrain the vertical distribution of CO to lie between a lower boundary below which CO freezes out onto dust grains (T less than or similar to 19 K) and an upper boundary above which CO can be photodissociated (the hydrogen column density from the disk surface is less than or similar to 10(21) cm(-2)). The freezeout at 19 K leads to a significant drop in the gas-phase CO column density beyond a radius of similar to 155 AU, a "CO snow line" that we directly resolve. By fitting the abundances of all CO isotopologues, we derive isotopic ratios of C-12/C-13, O-16/O-18, and O-18/O-17 that are consistent with quiescent interstellar gas-phase values. This detailed model of the HD 163296 disk demonstrates the potential of a staged, parametric technique for constructing unified gas and dust structure models and constraining the distribution of molecular abundances using resolved multi-transition, multi-isotope observations.
C1 [Qi, Chunhua; Oeberg, Karin I.; Wilner, David J.; Hughes, A. Meredith; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[D'Alessio, Paola; Ayala, Sandra] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico.
[Hughes, A. Meredith] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Qi, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA.
EM cqi@cfa.harvard.edu; p.dalessio@crya.unam.mx; koberg@cfa.harvard.edu;
dwilner@cfa.harvard.edu; mhughes@cfa.harvard.edu;
sandrews@cfa.harvard.edu; sayala2001@gmail.com
FU NASA [NAS 5-26555]; Space Telescope Science Institute; Miller Institute
for Basic Research in Science; NASA Origins of Solar Systems
[NNX11AK63G]
FX We thank Edwin Bergin, Eugene Chiang, and Jeremy Drake for beneficial
conversations, and a referee for constructive comments on the paper.
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. Support for A. M. H. is provided by a
fellowship from the Miller Institute for Basic Research in Science. We
acknowledge NASA Origins of Solar Systems grant No. NNX11AK63G.
NR 77
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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
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 20
PY 2011
VL 740
IS 2
AR 84
DI 10.1088/0004-637X/740/2/84
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900034
ER
PT J
AU Zhu, L
Zhao, JH
Wright, MCH
AF Zhu, Lei
Zhao, Jun-Hui
Wright, M. C. H.
TI OUTFLOW, INFALL, AND PROTOSTARS IN THE STAR-FORMING CORE W3-SE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: jets and outflows; ISM: kinematics and dynamics; ISM:
molecules; radio lines: ISM
ID NGC-1333 IRAS-4; PROTOSTELLAR INFALL; NGC 1333-IRAS2; CANDIDATES;
ENVELOPE; MOTIONS; SYSTEM; MASS; DISK; JET
AB We report new results on outflow and infall in the star-forming cores W3-SE SMA-1 and SMA-2 based on analysis of similar to 2 ''.5 resolution observations of the molecular lines HCN(3-2), HCO+(3-2), N2H+(3-2), and CH3OH(5(2,3)-4(1,3)) with the Submillimeter Array (SMA). A high-velocity bipolar outflow originating from the protostellar core SMA-1 was observed in the HCN(3-2) line, with a projected outflow axis at a position angle of 48 degrees. The detection of the outflow is confirmed from other molecular lines. An inverse P-Cygni profile in the HCN(3-2) line toward SMA-1 suggests that at least one of the double cores accretes matter from the molecular core. A filamentary structure in the molecular gas surrounds SMA-1 and SMA-2. Based on the SMA observations, our analysis suggests that the double pre-stellar cores SMA-1 and SMA-2 result from fragmentation in the collapsing massive molecular core W3-SE, and it is likely that they are forming intermediate-to high-mass stars which will be new members of a star cluster in the W3-SE region.
C1 [Zhu, Lei] Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
[Zhu, Lei; 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 Zhu, L (reprint author), Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
EM lzhu@cfa.harvard.edu; jzhao@cfa.harvard.edu
FU SAO; NSFC [10873019]; Smithsonian Institution; Academia Sinica
FX We are grateful to the staff of the SMA and CARMA telescopes who make
these observations possible. We also thank the anonymous referee for his
detailed comments and questions which have significantly improved the
presentation of these results. We thank Wu Y. for the suggestions and
discussions in forming the idea of this paper, selecting the research
targets and providing the single-dish data of the targets, suggesting
the suitable molecular probes, as well as the discussions in the
analysis of the results. L.Z. is supported by the SAO pre-doctoral
program during this research, and he is also supported by Grant 10873019
at NSFC when staying at Peking University.; The Submillimeter Array is a
joint project between the Smithsonian Astrophysical Observatory and the
Academia Sinica Institute of Astronomy and Astrophysics and is funded by
the Smithsonian Institution and the Academia Sinica.
NR 25
TC 4
Z9 4
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 OCT 20
PY 2011
VL 740
IS 2
AR 114
DI 10.1088/0004-637X/740/2/114
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844QR
UT WOS:000296762900064
ER
PT J
AU Foster, AR
Testa, P
AF Foster, Adam R.
Testa, Paola
TI Fe IX CALCULATIONS FOR THE SOLAR DYNAMICS OBSERVATORY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE atomic data; Sun: UV radiation
ID ATOMIC DATA; EMISSION-LINES; HYDROGEN; ELEMENTS; RATES; IONS
AB New calculations of the energy levels, radiative transition rates, and collisional excitation rates of Fe IX have been carried out using the Flexible Atomic Code, paying close attention to experimentally identified levels and extending existing calculations to higher energy levels. For lower levels, R-matrix collisional excitation rates from earlier work have been used. Significant emission is predicted by these calculations in the 5f-3d transitions, which will impact analysis of Solar Dynamics Observatory Atmospheric Imaging Assembly observations using the 94 angstrom filter.
C1 [Foster, Adam R.; Testa, Paola] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Foster, AR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM afoster@cfa.harvard.edu
FU NASA ADP [NNX09AC71G]; Lockheed-Martin [SP02H1701R]
FX A.R.F. acknowledges funding from NASA ADP grant NNX09AC71G. P. T. has
been supported by contract SP02H1701R from Lockheed-Martin to SAO.
NR 22
TC 16
Z9 16
U1 0
U2 6
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 OCT 20
PY 2011
VL 740
IS 2
AR L52
DI 10.1088/2041-8205/740/2/L52
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844MZ
UT WOS:000296752600021
ER
PT J
AU Liu, MC
Deacon, NR
Magnier, EA
Dupuy, TJ
Aller, KM
Bowler, BP
Redstone, J
Goldman, B
Burgett, WS
Chambers, KC
Hodapp, KW
Kaiser, N
Kudritzki, RP
Morgan, JS
Price, PA
Tonry, JL
Wainscoat, RJ
AF Liu, Michael C.
Deacon, Niall R.
Magnier, Eugene A.
Dupuy, Trent J.
Aller, Kimberly M.
Bowler, Brendan P.
Redstone, Joshua
Goldman, Bertrand
Burgett, W. S.
Chambers, K. C.
Hodapp, K. W.
Kaiser, N.
Kudritzki, R-P
Morgan, J. S.
Price, P. A.
Tonry, J. L.
Wainscoat, R. J.
TI A SEARCH FOR HIGH PROPER MOTION T DWARFS WITH Pan-STARRS1+2MASS+WISE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE brown dwarfs; proper motions; solar neighborhood; surveys
ID INFRARED SURVEY EXPLORER; COOL BROWN DWARF; SKY SURVEY; 2MASS;
TRANSITION; BENCHMARK; BINARIES; WISE; MASS; SPECTROGRAPH
AB We have searched approximate to 8200 deg(2) for high proper motion (approximate to 0.'' 5-2.'' 7 year(-1)) T dwarfs by combining first-epoch data from the Pan-STARRS1 (PS1) 3 pi Survey, the Two Micron All Sky Survey (2MASS) All-Sky Point Source Catalog, and the WISE Preliminary Data Release. We identified two high proper motion objects with the very red (W1 - W2) colors characteristic of T dwarfs, one being the known T7.5 dwarf GJ 570D. Near-IR spectroscopy of the other object (PSO J043.5395+02.3995 equivalent to WISEP J025409.45+022359.1) reveals a spectral type of T8, leading to a photometric distance of 7.2 +/- 0.7 pc. The 2.'' 56 year(-1) proper motion of PSO J043.5+02 is the second highest among field T dwarfs, corresponding to a tangential velocity of 87 +/- 8 km s(-1). According to the Besan, con galaxy model, this velocity indicates that its galactic membership is probably in the thin disk, with the thick disk an unlikely possibility. Such membership is in accord with the near-IR spectrum, which points to a surface gravity (age) and metallicity typical of the field population. We combine 2MASS, Sloan Digital Sky Survey, WISE, and PS1 astrometry to derive a preliminary parallax of 171 +/- 45 mas (5.8(-1.2)(+2.0) pc), the first such measurement using PS1 data. The proximity and brightness of PSO J043.5+02 will facilitate future characterization of its atmosphere, variability, multiplicity, distance, and kinematics. The modest number of candidates from our search suggests that the immediate (similar to 10 pc) solar neighborhood does not contain a large reservoir of undiscovered T dwarfs earlier than about T8.
C1 [Liu, Michael C.; Deacon, Niall R.; Magnier, Eugene A.; Aller, Kimberly M.; Bowler, Brendan P.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kaiser, N.; Kudritzki, R-P; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Redstone, Joshua] Facebook, Palo Alto, CA 94304 USA.
[Goldman, Bertrand] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Liu, MC (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
OI Chambers, Kenneth /0000-0001-6965-7789
FU National Aeronautics and Space Administration [NNX-08AE38A]; NSF
[AST-0507833, AST09-09222, AST-0709460]; AFRL [FA9451-06-2-0338]; DFG
[Sonderforschungsbereich 881]
FX Visiting Astronomer at the Infrared Telescope Facility, which is
operated by the University of Hawaii under Cooperative Agreement no.
NNX-08AE38A with the National Aeronautics and Space Administration,
Science Mission Directorate, Planetary Astronomy Program.; The
Pan-STARRS1 surveys have been made possible by the Institute for
Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the
institutions of the Pan-STARRS1 Science Consortium
(http://www.ps1sc.org), and NASA. Our research has employed the WISE,
SDSS-III, and 2MASS data products; NASA's Astrophysical Data System; the
SIMBAD database; the M, L, and T dwarf compendium housed at
DwarfArchives.org; and the SpeX Prism Spectral Libraries. This research
was supported by NSF Grants AST-0507833 and AST09-09222 (awarded to
MCL), AST-0709460 (awarded to EAM), AFRL Cooperative Agreement
FA9451-06-2-0338, and DFG-Sonderforschungsbereich 881 "The Milky Way."
Finally, the authors wish to recognize the very significant cultural
role that the summit of Mauna Kea has always had within the indigenous
Hawaiian community. We are most fortunate to conduct observations from
this mountain.
NR 46
TC 26
Z9 26
U1 0
U2 6
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 OCT 20
PY 2011
VL 740
IS 2
AR L32
DI 10.1088/2041-8205/740/2/L32
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 844MZ
UT WOS:000296752600001
ER
PT J
AU Hill, EM
Davis, JL
Tamisiea, ME
Ponte, RM
Vinogradova, NT
AF Hill, Emma M.
Davis, James L.
Tamisiea, Mark E.
Ponte, Rui M.
Vinogradova, Nadya T.
TI Using a spatially realistic load model to assess impacts of Alaskan
glacier ice loss on sea level
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
ID GRAVITY-FIELD; MASS CHANGES; OCEAN MASS; AGE EARTH; GRACE; SURFACE;
TRENDS; UPLIFT; FLUX
AB Ice loss from glaciers results in highly nonuniform patterns of sea level change due to the effects of self-attraction and loading. To quantify these spatial effects, it is necessary to obtain an ice load model that is both spatially realistic and regionally complete. We demonstrate a technique to produce such a model for the Alaskan glaciers by combining mass balance rates from a Gravity Recovery and Climate Experiment (GRACE) mascon solution with realistic glacier geometries. This load model can be used to solve the "sea level equation" to determine gravitationally self-consistent sea level and gravity rates. The model predicts a significant drop in relative sea level in the near field of the glaciers, with coastal rates of around -9 mm/yr (compared to a global average rise of 0.2 mm/yr) and significant differences to those predicted by a coarser model. The magnitude and sensitivity of these near-field rates imply that the near-field tide gauge records could contain significant information about the spatial distribution of ice loss. Comparison of model gravity rates with an independently produced, spherical harmonic, GRACE solution verifies that our technique can successfully capture the mass changes estimated in the mascon solution within our higher-resolution model. Finally, we use our ice load model to examine the possibility of detecting the effects of ice loss in estimates of ocean bottom pressure (OBP) from GRACE. We use the model to simulate the effects of GRACE signal leakage and show that the OBP signal from leakage has a similar pattern to, but larger amplitude than, the sea level "fingerprint" expected from ice loss.
C1 [Hill, Emma M.; Davis, James L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hill, Emma M.] Nanyang Technol Univ, Earth Observ Singapore, Singapore 639798, Singapore.
[Davis, James L.] Columbia Univ, Lamont Doherty Earth Observ, Earth Inst, Palisades, NY 10964 USA.
[Tamisiea, Mark E.] Natl Oceanog Ctr, Liverpool L3 5DA, Merseyside, England.
[Ponte, Rui M.; Vinogradova, Nadya T.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
RP Hill, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ehill@ntu.edu.sg; jdavis@ldeo.columbia.edu; mtam@noc.ac.uk;
rponte@aer.com; nvinogra@aer.com
RI Davis, James/D-8766-2013; Hill, Emma/B-7037-2011;
OI Davis, James/0000-0003-3057-477X; Hill, Emma/0000-0003-0231-5818; Ponte,
Rui/0000-0001-7206-6461
FU NASA [NNX08AJ79G, NNX07AM77G, NNX11AC14G, NNX11AB97G]; Earth Observatory
of Singapore (EOS) [32]; NERC
FX This work was supported by NASA grants NNX08AJ79G, NNX07AM77G,
NNX11AC14G, and NNX11AB97G. E. M. H. was partially supported by the
Earth Observatory of Singapore (EOS number 32). M. E. T. was funded by
NERC as part of Oceans 2025. We are grateful to Scott Luthcke for
providing the bounding box coordinates for his published mascon results
and to Katherine Quinn for useful discussions. Our routine uses the
Generic Mapping Tools [Wessel and Smith, 1998]. The manuscript was
significantly improved by reviews from Chris Larsen, two anonymous
reviewers, and the Associate Editor.
NR 37
TC 4
Z9 4
U1 2
U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD OCT 20
PY 2011
VL 116
AR B10407
DI 10.1029/2011JB008339
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 836XK
UT WOS:000296151500002
ER
PT J
AU Munroe, TA
Tyler, J
Tunnicliffe, V
AF Munroe, Thomas A.
Tyler, Jennifer
Tunnicliffe, Verena
TI Description and biological observations on a new species of deepwater
symphurine tonguefish (Pleuronectiformes: Cynoglossidae: Symphurus)
collected at Volcano-19, Tonga Arc, West Pacific Ocean
SO ZOOTAXA
LA English
DT Article
DE taxonomy; deep-sea flatfish; tongue sole; hydrothermal vents; volcanic
arcs; seamounts; reversed asymmetry; species description; ocelli
AB Symphurus maculopinnis n. sp., described on a single specimen (USNM 398820; 84.4 mm SL), was collected by a remotely operated vehicle (ROV) exploring a hydrothermal vent area located at 561 m on Volcano-19, Tonga Arc, West Pacific (24 degrees 48.439' S, 177 degrees 0.009' W). This new species is distinctive and readily diagnosed from congeners by the following combination of characters: 1-2-2-2-1 pattern of interdigitation of dorsal proximal pterygiophores and neural spines (ID pattern), 14 caudal-fin rays, 3+6 abdominal vertebrae, 49 total vertebrae, 89 scales in a longitudinal row, 92 dorsal-fin rays, 77 anal-fin rays, blunt squarish snout, thick blind-side lips with conspicuous plicae, and conspicuous ocellated (sometimes partially) spots on posterior dorsal and anal fins. Among Symphurus, only S. ocellatus von Bonde, collected at deepwater locations off East Africa, features a similar ID pattern, 14 caudal-fin rays and spots on the posterior dorsal and anal fins. Symphurus maculopinnis differs distinctly from S. ocellatus in its lower and non-overlapping meristic features (49 vs. 54-56 total vertebrae; 92 vs. 97-103 dorsal-fin rays; and 77 vs. 85-89 anal-fin rays), its squarish (vs. pointed) snout, and thick, plicated blind-side lower lip (vs. thin, non-plicated blind-side lower lip). Additional specimens (N= 56) of S. maculopinnis observed and filmed in situ near active venting sites located between ca. 433-561 m on Volcano-19 provide the basis for behavioral and ecological information recorded for the species. Videotapes reveal one individual of S. maculopinnis featuring reversed (dextral) asymmetry from that typical (sinistral) for members of the Cynoglossidae. Specimens with reversed asymmetry are relatively rare in this family and this S. maculopinnis represents only the second known reversed individual among the approximately 42 species of deep-sea (> 200 m) Symphurus.
C1 [Munroe, Thomas A.] Smithsonian Inst, Natl Systemat Lab, Natl Marine Fisheries Serv, NOAA,Natl Museum Nat Hist, Washington, DC 20013 USA.
[Tyler, Jennifer; Tunnicliffe, Verena] Univ Victoria, Dept Biol, Victoria, BC V8W 3N5, Canada.
RP Munroe, TA (reprint author), Smithsonian Inst, Natl Systemat Lab, Natl Marine Fisheries Serv, NOAA,Natl Museum Nat Hist, POB 37012,WC-57,MRC-153, Washington, DC 20013 USA.
EM munroet@si.edu; jentyler24@gmail.com; verenat@uvic.ca
RI Tunnicliffe, Verena/D-1056-2014
FU NSERC Canada
FX L. Willis provided radiographs of the holotype and L. Willis and M.
Nizinski provided radiographs of specimens used in the comparisons. J.
Clayton and D. Smith assisted with accessioning and cataloguing the
holotype. J. Rose compiled the videotape of specimens filmed in situ at
Volcano-19 and provided field data associated with the holotype; C.
Marzec and M. Benson assisted with publishing and archiving the
tonguefish video to the Smithsonian Institution's Ocean Portal website;
C. Ames assisted with making video grabs from video tapes. S. Raredon
provided photographs of the holotype. Appreciation is extended to
curators and collection staff who provided assistance locating
specimens, providing catalogue information, or who arranged for loan of
specimens used in this study. We acknowledge the field team who
collected and filmed this species during the SO192-2 MANGO Expedition,
particularly S. K. Juniper and C. Stevens; expedition co-chiefs were U.
Schwarz-Schampera and M. Hannington with R/V Sonne and ROV ROPOS.
Collection of this specimen was made possible by funding provided to V.
Tunnicliffe by NSERC Canada.
NR 18
TC 7
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U1 0
U2 3
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1175-5326
EI 1175-5334
J9 ZOOTAXA
JI Zootaxa
PD OCT 18
PY 2011
IS 3061
BP 53
EP 66
PG 14
WC Zoology
SC Zoology
GA 833ZY
UT WOS:000295926300003
ER
PT J
AU Osinski, GR
Tornabene, LL
Grieve, RAF
AF Osinski, Gordon R.
Tornabene, Livio L.
Grieve, Richard A. F.
TI Impact ejecta emplacement on terrestrial planets
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE impact cratering; impact ejecta; Mars; Moon
ID CRATERING RECORD; OBLIQUE IMPACTS; LAYERED EJECTA; DEVON ISLAND; MELT
ROCKS; RIES; MARS; GERMANY; FLOWS; VENUS
AB Impact cratering is one of the most fundamental processes responsible for shaping the surfaces of solid planetary bodies. One of the principal characteristics of impact events is the formation and emplacement of ejecta deposits, an understanding of which is critical for planetary exploration. Current models of ejecta emplacement, however, do not account for several important observations of ejecta deposits on the terrestrial planets, in particular, the presence of more than one layer of ejecta. Furthermore, there is also no universal model for the origin and emplacement of ejecta on different planetary bodies. We present a unifying working hypothesis for the origin and emplacement of ejecta on the terrestrial planets, in which the ejecta are emplaced in a multi-stage process. The generation of the continuous ejecta blanket occurs during the excavation stage of cratering, via the conventional ballistic sedimentation and radial flow model. This is followed by the emplacement of more melt-rich, ground-hugging flows - the "surface melt flow" phase during the terminal stages of crater excavation and the modification stage of crater formation. Minor fallback occurs during the final stages of crater formation. Several factors will affect the final morphology and character of ejecta deposits. The volatile content and cohesiveness of the uppermost target rocks will significantly affect the runout distance of the ballistically emplaced continuous ejecta blanket, with impact angle also influencing the overall geometry of the deposits (e.g., the production of the characteristic butterfly pattern seen in very oblique impacts). Ejecta deposited during the surface melt flow stage is influenced by several factors, most importantly planetary gravity, surface temperature, and the physical properties of the target rocks. Topography and angle of impact play important roles in determining the final distribution of surface melt flow ejecta deposits with respect to the source crater. This working hypothesis of ballistic sedimentation and surface melt flow provides a framework in which observations of ejecta at impact craters can be compared and placed in the context of the respective terrestrial planets. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Osinski, Gordon R.; Grieve, Richard A. F.] Univ Western Ontario, Dept Earth Sci Phys & Astron, London, ON N6A 5B7, Canada.
[Tornabene, Livio L.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Grieve, Richard A. F.] Nat Resources Canada, Earth Sci Sector, Ottawa, ON K1A 0E8, Canada.
RP Osinski, GR (reprint author), Univ Western Ontario, Dept Earth Sci Phys & Astron, 1151 Richmond St, London, ON N6A 5B7, Canada.
EM gosinski@uwo.ca
FU Natural Sciences and Engineering Research Council of Canada (NSERC); MDA
Space Missions; Canadian Space Agency (CSA); CSA Canadian Analogue
Research Network (CARN)
FX G.R.O. is supported by the Natural Sciences and Engineering Research
Council of Canada (NSERC) Industrial Research Chair in Planetary Geology
sponsored by MDA Space Missions and the Canadian Space Agency (CSA).
Funding from the NSERC Discovery Grant and the CSA Canadian Analogue
Research Network (CARN) programs is gratefully acknowledged. Sarah
Stewart-Mukhopadhyay and an anonymous reviewer are thanked for their
detailed and constructive reviews.
NR 99
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Z9 72
U1 2
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD OCT 15
PY 2011
VL 310
IS 3-4
BP 167
EP 181
DI 10.1016/j.epsl.2011.08.012
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 864XJ
UT WOS:000298273500001
ER
PT J
AU Reeder, LA
Erlandson, JM
Rick, TC
AF Reeder, Leslie A.
Erlandson, Jon M.
Rick, Torben C.
TI Younger Dryas environments and human adaptations on the West Coast of
the United States and Baja California
SO QUATERNARY INTERNATIONAL
LA English
DT Article
ID LATE QUATERNARY VEGETATION; GULF-OF-CALIFORNIA; SANTA-BARBARA BASIN;
SOUTHWESTERN COLUMBIA BASIN; LAST GLACIAL MAXIMUM; SCALE CLIMATE-CHANGE;
BATTLE GROUND LAKE; SEA-LEVEL RECORD; NORTH-AMERICA; CURRENT SYSTEM
AB On the Pacific Coast of the United States and Baja California, the Younger Dryas was one component of dynamic Late Pleistocene and Holocene environmental changes. Changing climate, sea level rise, and shifting shorelines created ecological challenges for ancient coastal peoples and daunting challenges for archaeologists searching for early coastal sites. This paper reviews the evidence for ecological change in this 'West Coast' region, including shoreline changes that may have submerged or destroyed archaeological sites from this time period. Examining the regional record of human occupation dating to the Younger Dryas, well-dated coastal sites are limited to California's Northern Channel Islands and Isla Cedros off Baja California. A small number of fluted points found in coastal areas may also date to the Younger Dryas, but their context and chronology is not well defined. Review of the implications of these two data sets considers whether the early but discontinuous Younger Dryas archaeological record from the West Coast might result from a migration of maritime peoples from Northeast Asia into the Americas. (C) 2011 Elsevier Ltd and INQUA. All rights reserved.
C1 [Reeder, Leslie A.] So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA.
[Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA.
[Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA.
[Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA.
RP Reeder, LA (reprint author), So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA.
EM lreeder@smu.edu
OI Erlandson, Jon/0000-0002-4705-4319
NR 155
TC 2
Z9 2
U1 2
U2 22
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1040-6182
J9 QUATERN INT
JI Quat. Int.
PD OCT 15
PY 2011
VL 242
IS 2
BP 463
EP 478
DI 10.1016/j.quaint.2011.04.016
PG 16
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 827NZ
UT WOS:000295436500017
ER
PT J
AU van Breugel, M
Ransijn, J
Craven, D
Bongers, F
Hall, JS
AF van Breugel, Michiel
Ransijn, Johannes
Craven, Dylan
Bongers, Frans
Hall, Jefferson S.
TI Estimating carbon stock in secondary forests: Decisions and
uncertainties associated with allometric biomass models
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Carbon; Tree allometry; Biomass; Secondary succession; Tropical forest
ID ABOVEGROUND TREE BIOMASS; TROPICAL RAIN-FOREST; WOOD DENSITY;
CLIMATE-CHANGE; FUNCTIONAL-GROUPS; BRAZILIAN AMAZON; LANDSCAPE-SCALE;
LAND-USE; DEFORESTATION; EQUATIONS
AB Secondary forests are a major terrestrial carbon sink and reliable estimates of their carbon stocks are pivotal for understanding the global carbon balance and initiatives to mitigate CO2 emissions through forest management and reforestation. A common method to quantify carbon stocks in forests is the use of allometric regression models to convert forest inventory data to estimates of aboveground biomass (AGO). The use of allometric models implies decisions on the selection of extant models or the development of a local model, the predictor variables included in the selected model, and the number of trees and species for destructive biomass measurements. We assess uncertainties associated with these decisions using data from 94 secondary forest plots in central Panama and 244 harvested trees belonging to 26 locally abundant species. AGB estimates from species-specific models were used to assess relative errors of estimates from multispecies models. To reduce uncertainty in the estimation of plot AGO, including wood specific gravity (WSG) in the model was more important than the number of trees used for model fitting. However, decreasing the number of trees increased uncertainty of landscape-level AGB estimates substantially, while including WSG had limited effects on the accuracy of the landscape-level estimates. Predictions of stand and landscape AGB varied strongly among models, making model choice an important source of uncertainty. Local models provided more accurate AGB estimates than foreign models, but high variability in carbon stocks across the landscape implies that developing local models is only justified when landscape sampling is sufficiently intensive. (C) 2011 Elsevier B.V. All rights reserved.
C1 [van Breugel, Michiel; Ransijn, Johannes; Craven, Dylan; Hall, Jefferson S.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa, Ancon, Panama.
[Ransijn, Johannes; Bongers, Frans] Wageningen Univ, Forest Ecol & Forest Management Grp, Ctr Ecosyst Studies, NL-6700 AA Wageningen, Netherlands.
[Ransijn, Johannes] Univ Copenhagen, DK-1958 Frederiksberg C, Denmark.
[Craven, Dylan] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
RP van Breugel, M (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Av Roosevelt 401, Balboa, Ancon, Panama.
EM mvbreugel@gmail.com
RI Craven, Dylan/K-2717-2012; Ransijn, Johannes/D-5324-2015;
OI Craven, Dylan/0000-0003-3940-833X; Ransijn,
Johannes/0000-0003-0416-2210; van Breugel, Michiel/0000-0003-2778-7803
FU HSBC; STRI; ACP; Frank Levinson Family Foundation; Motta Family
Foundation; Secretaria Nacional de Ciencia, Tecnologia e Innovacion
(SENACYT) of Panama
FX This paper is a scientific contribution to the Agua Salud Project (ASP),
collaboration among the Smithsonian Tropical Research Institute, the
Panama Canal Authority (ACP) and the National Environmental Authority of
Panama (ANAM). The ASP is supported by the HSBC climate partnership,
STRI, the ACP, the Frank Levinson Family Foundation and the Motta Family
Foundation. This study was supported by an Anonymous Donor and the
Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) of
Panama. We thank Daniela Weber and Federico Davis for logistical
support, Yuriza Guerrero, Johana Balbuena, Miguel Nunez, Guillermo
Fernandez, Fernando Garcia, Carlos Diaz, Anabel Rivas, Jenny Calvo,
Manuel Valdes and Gregorio Sala for their help in the collection of
field data, Christian Salas and two anonymous reviewers for their
valuable comments and Joe Wright for providing data on wood specific
gravity. Finally, JR thanks Michele Abene, Adriana Cromer and Gillian
Paul for their support and companionship during the field work period.
NR 60
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U1 7
U2 87
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD OCT 15
PY 2011
VL 262
IS 8
BP 1648
EP 1657
DI 10.1016/j.foreco.2011.07.018
PG 10
WC Forestry
SC Forestry
GA 825QN
UT WOS:000295297300034
ER
PT J
AU Baeza, JA
Bolanos, JA
Hernandez, JE
Lira, C
Lopez, R
AF Antonio Baeza, J.
Bolanos, Juan A.
Hernandez, Jesus E.
Lira, Carlos
Lopez, Regulo
TI Monogamy does not last long in Pontonia mexicana, a symbiotic shrimp of
the amber pen-shell Pinna carnea from the southeastern Caribbean Sea
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Caridea; Monogamy; Promiscuity; Symbiosis; Venezuela
ID CRAB INACHUS-PHALANGIUM; SOCIAL MONOGAMY; SNAPPING SHRIMP; EVOLUTIONARY
CONSEQUENCES; HOST CHARACTERISTICS; MATING TACTICS; LIFE-HISTORY;
DECAPODA; ANEMONE; DIMORPHISM
AB Theory suggests that symbiotic species should be monogamous and form long-lasting heterosexual pairs in/on hosts when inhabiting scarce and small hosts in environments where predation risk away from hosts is high (e.g., tropical subtidal). This prediction was tested with Pontonia mexicana which inhabits the relatively small and scarce amber pen-shell Pinna carnea in the tropical Caribbean. In agreement with theory, P. mexicana were found dwelling as heterosexual pairs in the mantle cavity of pen-shell individuals with more frequency than expected by chance alone. However, additional observations suggested that male-female pairing of P. mexicana does not last long. First, males paired with females that were close to molt and become sexually receptive more frequently than expected by chance alone. In monogamous species in which pairing appears to be long lasting, males occur with females in the same host, independent of the reproductive condition of the female. Second, the body size of paired shrimps was poorly correlated and the relationship between host and shrimp body size was weak. If males and females of P. mexicana were staying within host individuals for long periods of time, a tight correlation between host and shrimp size and between males and females in a pair would have been found. Lastly, sexual dimorphism in terms of cheliped size was evident; males invested considerably more resources to this body structure compared to females. In monogamous species in which pairing appears to be long-term, sexual dimorphism is low or absent given that sexual selection is weak in this mating system. Overall, our data suggests that monogamy in P. mexicana does not last long and that males switch among host individuals in search of receptive females. Manipulative experiments are necessary to understand the conditions favoring short- and long-term monogamy in symbiotic crustaceans. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Antonio Baeza, J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23435 USA.
[Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
[Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile.
[Bolanos, Juan A.; Hernandez, Jesus E.; Lira, Carlos; Lopez, Regulo] Univ Oriente, Nucleo Nueva Esparta, Escuela Ciencias Aplicadas Mar, Grp Invest Carcinol, Isla Margarita, Venezuela.
RP Baeza, JA (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23435 USA.
EM baezaa@si.edu
OI Baeza, Juan Antonio/0000-0002-2573-6773
FU Smithsonian Marine Station (SMS); Smithsonian Tropical Research
Institute (STRI)
FX JAB (SI) is grateful for the support from a Smithsonian Marine Station
(SMS) Postdoctoral Fellowship and a Smithsonian Tropical Research
Institute (STRI) Postdoctoral Fellowship. We appreciate the help from
several students attending the course "Behavior of Marine Invertebrates"
held during 2008 at the Escuela de Ciencias Aplicadas del Mar, Nucleo
Nueva Esparta, Universidad de Oriente, for their help during the
different steps of sampling, measurement, and data analysis. Dr. M.
Soledad Fuentes at NOAA, Milford, CT gently provided access to
statistical software and support. This is contribution number 859 of the
Smithsonian Marine Station at Fort Pierce. [SS]
NR 46
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U1 0
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
EI 1879-1697
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD OCT 15
PY 2011
VL 407
IS 1
BP 41
EP 47
DI 10.1016/j.jembe.2011.07.011
PG 7
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 825RG
UT WOS:000295299200007
ER
PT J
AU Clark, MA
Joo, B
Kennedy, AD
Silva, PJ
AF Clark, M. A.
Joo, Balint
Kennedy, A. D.
Silva, P. J.
TI Improving dynamical lattice QCD simulations through integrator tuning
using Poisson brackets and a force-gradient integrator
SO PHYSICAL REVIEW D
LA English
DT Article
AB We show how the integrators used for the molecular dynamics step of the Hybrid Monte Carlo algorithm can be further improved. These integrators not only approximately conserve some Hamiltonian H but conserve exactly a nearby shadow Hamiltonian (H) over tilde. This property allows for a new tuning method of the molecular dynamics integrator and also allows for a new class of integrators (force-gradient integrators) which is expected to reduce significantly the computational cost of future large-scale gauge field ensemble generation.
C1 [Silva, P. J.] Univ Coimbra, Ctr Fis Computac, P-3000 Coimbra, Portugal.
[Clark, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Joo, Balint] Jefferson Lab, Newport News, VA 23606 USA.
[Kennedy, A. D.] Univ Edinburgh, Tait Inst, Edinburgh EH9 3JZ, Midlothian, Scotland.
[Kennedy, A. D.] Univ Edinburgh, SUPA, Sch Phys & Astron, Edinburgh EH9 3JZ, Midlothian, Scotland.
RP Silva, PJ (reprint author), Univ Coimbra, Ctr Fis Computac, P-3000 Coimbra, Portugal.
EM psilva@teor.fis.uc.pt
RI Silva, Paulo/H-8270-2013
OI Silva, Paulo/0000-0002-3658-2319
FU FCT [SFRH/BPD/40998/2007, PTDC/FIS/100968/2008]; U.S. DOE
[DE-FC02-06ER41440, DE-FC02-06ER41449, DE-AC05-060R23177]; NSF
[PHY-0835713, OCI-1060067]
FX P.J.S. acknowledges support from FCT via Grant No. SFRH/BPD/40998/2007
and Project No. PTDC/FIS/100968/2008. B.J. acknowledges funding through
U.S. DOE Grants No. DE-FC02-06ER41440, No. DE-FC02-06ER41449 (SciDAC),
and No. DE-AC05-060R23177 under which Jefferson Science Associates LLC
manages and operates the Jefferson Lab. M.A.C. acknowledges support from
the NSF via PHY-0835713 and OCI-1060067. The numerical results have been
obtained using the Chroma library [10]. Simulations have been carried
out in Iridis (University of Southampton) and Centaurus (University of
Coimbra) High Performance Computing facilities.
NR 10
TC 3
Z9 3
U1 0
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD OCT 14
PY 2011
VL 84
IS 7
AR 071502
DI 10.1103/PhysRevD.84.071502
PG 5
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 841UX
UT WOS:000296541500002
ER
PT J
AU Trefzger, C
Menotti, C
Capogrosso-Sansone, B
Lewenstein, M
AF Trefzger, C.
Menotti, C.
Capogrosso-Sansone, B.
Lewenstein, M.
TI Ultracold dipolar gases in optical lattices
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
ID BOSE-EINSTEIN CONDENSATE; MONTE-CARLO; ATOMS; MOLECULES; BOSONS;
TRANSITION; SUPERFLUID; COLLAPSE; STATE; MODEL
AB This tutorial is a theoretical work, in which we study the physics of ultra-cold dipolar bosonic gases in optical lattices. Such gases consist of bosonic atoms or molecules that interact via dipolar forces, and that are cooled below the quantum degeneracy temperature, typically in the nK range. When such a degenerate quantum gas is loaded into an optical lattice produced by standing waves of laser light, new kinds of physical phenomena occur. Then, these systems realize extended Hubbard-type models, and can be brought to a strongly correlated regime. The physical properties of such gases, dominated by the long-range, anisotropic dipole-dipole interactions, are discussed using the mean-field approximations and exact quantum Monte Carlo techniques (the worm algorithm).
C1 [Trefzger, C.; Menotti, C.; Lewenstein, M.] ICFO Inst Ciencies Foton, Barcelona 08860, Spain.
[Menotti, C.] Univ Trent, INO CNR BEC Ctr, I-38123 Povo, Italy.
[Menotti, C.] Univ Trent, Dipartimento Fis, I-38123 Povo, Italy.
[Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
[Lewenstein, M.] ICREA, Barcelona 08010, Spain.
RP Trefzger, C (reprint author), ICFO Inst Ciencies Foton, Mediterranean Technol Pk, Barcelona 08860, Spain.
EM christian.trefzger@lkb.ens.fr
RI Lewenstein, Maciej/I-1337-2014
OI Lewenstein, Maciej/0000-0002-0210-7800
FU Spanish MEC [FIS2008-00784]; EU; ERC
FX This tutorial was supported by Spanish MEC(FIS2008-00784, QOIT), EU
projects AQUTE and NAMEQUAM, and ERC grant QUAGATUA. ML acknowledges
also Alexander von Humboldt Stiftung and Hamburg Prize for Theoretical
Physics. It is a great pleasure for us to thank everybody in the Quantum
Optics Theory Group of ICFO for interesting discussions. We are
especially grateful to K Rzazewski, who invited us to write this paper.
CT thanks C Menotti, and M Lewenstein for their constant support, and
patience, they showed him during these years, the result of which is not
only in this work. CT thanks B Capogrosso-Sansone and G Pupillo for
their guide in the quantum Monte Carlo work, and Peter Zoller for the
kind hospitality in Innsbruck. This work was partially written at the
Indian Association for the Cultivation of Science, in Calcutta, while CT
was visiting K Sengupta. The warm hospitality he showed him is unique,
and CT thanks him together with everybody in the Theoretical Physics
Department.
NR 87
TC 55
Z9 55
U1 2
U2 18
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD OCT 14
PY 2011
VL 44
IS 19
AR 193001
DI 10.1088/0953-4075/44/19/193001
PG 31
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 824QO
UT WOS:000295217300005
ER
PT J
AU Plaisance, L
Caley, MJ
Brainard, RE
Knowlton, N
AF Plaisance, Laetitia
Caley, M. Julian
Brainard, Russell E.
Knowlton, Nancy
TI The Diversity of Coral Reefs: What Are We Missing?
SO PLOS ONE
LA English
DT Article
ID BIOLOGICAL IDENTIFICATIONS; BIODIVERSITY HOTSPOTS; MARINE BIODIVERSITY;
SPECIES RICHNESS; EXTINCTION RISK; CLIMATE-CHANGE; DNA BARCODES; OCEAN;
INVERTEBRATES; CONSERVATION
AB Tropical reefs shelter one quarter to one third of all marine species but one third of the coral species that construct reefs are now at risk of extinction. Because traditional methods for assessing reef diversity are extremely time consuming, taxonomic expertise for many groups is lacking, and marine organisms are thought to be less vulnerable to extinction, most discussions of reef conservation focus on maintenance of ecosystem services rather than biodiversity loss. In this study involving the three major oceans with reef growth, we provide new biodiversity estimates based on quantitative sampling and DNA barcoding. We focus on crustaceans, which are the second most diverse group of marine metazoans. We show exceptionally high numbers of crustacean species associated with coral reefs relative to sampling effort (525 species from a combined, globally distributed sample area of 6.3 m(2)). The high prevalence of rare species (38% encountered only once), the low level of spatial overlap (81% found in only one locality) and the biogeographic patterns of diversity detected (Indo-West Pacific > Central Pacific > Caribbean) are consistent with results from traditional survey methods, making this approach a reliable and efficient method for assessing and monitoring biodiversity. The finding of such large numbers of species in a small total area suggests that coral reef diversity is seriously under-detected using traditional survey methods, and by implication, underestimated.
C1 [Plaisance, Laetitia; Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Plaisance, Laetitia; Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA.
[Caley, M. Julian] Australian Inst Marine Sci, Townsville, Qld 4810, Australia.
[Brainard, Russell E.] Natl Ocean & Atmospher Adm Fisheries, Pacific Islands Fisheries Sci Ctr, Coral Reef Ecosyst Div, Honolulu, HI USA.
RP Plaisance, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
EM plaisancel@si.edu
FU Alfred P. Sloan Foundation; Census of Marine Life; Census of Coral
Reefs; BHP Billiton (Australia)
FX This work was supported by the Alfred P. Sloan Foundation, Census of
Marine Life, Census of Coral Reefs, and BHP Billiton (Australia). The
funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 30
TC 34
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U1 4
U2 61
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 OCT 13
PY 2011
VL 6
IS 10
AR e25026
DI 10.1371/journal.pone.0025026
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 834QT
UT WOS:000295978600008
PM 22022371
ER
PT J
AU Churchill, CKC
Foighil, DO
Strong, EE
Gittenberger, A
AF Churchill, Celia K. C.
Foighil, Diarmaid O.
Strong, Ellen E.
Gittenberger, Adriaan
TI Females floated first in bubble-rafting snails
SO CURRENT BIOLOGY
LA English
DT Letter
C1 [Churchill, Celia K. C.; Foighil, Diarmaid O.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA.
[Churchill, Celia K. C.; Foighil, Diarmaid O.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA.
[Strong, Ellen E.] Smithsonian Inst, Washington, DC 20013 USA.
[Gittenberger, Adriaan] Netherlands Ctr Biodivers Naturalis, NL-2300 RA Leiden, Netherlands.
[Gittenberger, Adriaan] Leiden Univ, Inst Biol, NL-2300 RA Leiden, Netherlands.
[Gittenberger, Adriaan] Leiden BioSci Pk, GiMaRIS, NL-2333 CA Leiden, Netherlands.
RP Churchill, CKC (reprint author), Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA.
EM celia.churchill@gmail.com
NR 10
TC 5
Z9 5
U1 0
U2 11
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 OCT 11
PY 2011
VL 21
IS 19
BP R802
EP R803
DI 10.1016/j.cub.2011.08.011
PG 2
WC Biochemistry & Molecular Biology; Cell Biology
SC Biochemistry & Molecular Biology; Cell Biology
GA 833QI
UT WOS:000295899600004
PM 21996498
ER
PT J
AU Hughes, AM
Wilner, DJ
Andrews, SM
Williams, JP
Su, KYL
Murray-Clay, RA
Qi, CH
AF Hughes, A. Meredith
Wilner, David J.
Andrews, Sean M.
Williams, Jonathan P.
Su, Kate Y. L.
Murray-Clay, Ruth A.
Qi, Chunhua
TI RESOLVED SUBMILLIMETER OBSERVATIONS OF THE HR 8799 AND HD 107146 DEBRIS
DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; planet-disk interactions;
stars: individual (HD 107146, HR 8799)
ID SOLAR-TYPE STARS; PLANETARY SYSTEM; KUIPER-BELT; VEGA-LIKE; DUST;
EVOLUTION; MASS; PHOTOMETRY; MORPHOLOGY; STABILITY
AB We present 880 mu m Submillimeter Array observations of the debris disks around the young solar analog HD 107146 and the multiple-planet host star HR 8799, at an angular resolution of 3 '' and 6 '', respectively. We spatially resolve the inner edge of the disk around HR 8799 for the first time. While the data are not sensitive enough (with rms noise of 1 mJy) to constrain the system geometry, we demonstrate that a model by Su et al. based on the spectral energy distribution (SED) with an inner radius of 150 AU predicts the spatially resolved data well. Furthermore, by modeling simultaneously the SED and visibilities, we demonstrate that the dust is distributed in a broad (of order 100 AU) annulus rather than a narrow ring. We also model the observed SED and visibilities for the HD 107146 debris disk and generate a model of the dust emission that extends in a broad band between 50 and 170 AU from the star. We perform an a posteriori comparison with existing 1.3 mm CARMA observations and demonstrate that a smooth, axisymmetric model reproduces all of the available millimeter-wavelength data well.
C1 [Hughes, A. Meredith] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Wilner, David J.; Andrews, Sean M.; Murray-Clay, Ruth A.; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Su, Kate Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Hughes, AM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM mhughes@astro.berkeley.edu
OI Williams, Jonathan/0000-0001-5058-695X; Su, Kate/0000-0002-3532-5580
FU Miller Institute for Basic Research in Science
FX The authors are grateful to Stuartt Corder and John Carpenter for
sharing their HD 107146 CARMA data. We also thank Eugene Chiang for
constructive comments on the paper. A.M.H. is supported by a fellowship
from the Miller Institute for Basic Research in Science.
NR 56
TC 37
Z9 37
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 OCT 10
PY 2011
VL 740
IS 1
AR 38
DI 10.1088/0004-637X/740/1/38
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825FL
UT WOS:000295256500038
ER
PT J
AU Kratter, KM
Murray-Clay, RA
AF Kratter, Kaitlin M.
Murray-Clay, Ruth A.
TI FRAGMENT PRODUCTION AND SURVIVAL IN IRRADIATED DISKS: A COMPREHENSIVE
COOLING CRITERION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; planetary systems; protoplanetary disks
ID GRAVITATING ACCRETION DISCS; GIANT PLANET FORMATION; PROTOSTELLAR DISKS;
STAR-FORMATION; LOW-MASS; PROTOPLANETARY DISCS; EPISODIC ACCRETION;
LAYERED ACCRETION; INSTABILITY; STABILITY
AB Accretion disks that become gravitationally unstable can fragment into stellar or substellar companions. The formation and survival of these fragments depends on the precarious balance between self-gravity, internal pressure, tidal shearing, and rotation. Disk fragmentation depends on two key factors: (1) whether the disk can get to the fragmentation boundary of Q = 1 and (2) whether fragments can survive for many orbital periods. Previous work suggests that to reach Q = 1, and have fragments survive, a disk must cool on an orbital timescale. Here we show that disks heated primarily by external irradiation always satisfy the standard cooling time criterion. Thus, even though irradiation heats disks and makes them more stable in general, once they reach the fragmentation boundary, they fragment more easily. We derive a new cooling criterion that determines fragment survival and calculate a pressure-modified Hill radius, which sets the maximum size of pressure-supported objects in a Keplerian disk. We conclude that fragmentation in protostellar disks might occur at slightly smaller radii than previously thought and recommend tests for future simulations that will better predict the outcome of fragmentation in real disks.
C1 [Kratter, Kaitlin M.; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kratter, KM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
EM kkratter@cfa.harvard.edu
FU Institute for Theory and Computation through the Harvard College
Observatory
FX We thank the referee for detailed comments that improved this work. We
also acknowledge Phil Armitage, Charles Gammie, Chris Matzner, and Ken
Rice for useful conversations and for comments on an early version of
this manuscript. K. M. K. is supported by an Institute for Theory and
Computation Postdoctoral Fellowship through the Harvard College
Observatory.
NR 44
TC 33
Z9 33
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
IS 1
AR 1
DI 10.1088/0004-637X/740/1/1
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825FL
UT WOS:000295256500001
ER
PT J
AU Luo, B
Brandt, WN
Xue, YQ
Alexander, DM
Brusa, M
Bauer, FE
Comastri, A
Fabian, AC
Gilli, R
Lehmer, BD
Rafferty, DA
Schneider, DP
Vignali, C
AF Luo, B.
Brandt, W. N.
Xue, Y. Q.
Alexander, D. M.
Brusa, M.
Bauer, F. E.
Comastri, A.
Fabian, A. C.
Gilli, R.
Lehmer, B. D.
Rafferty, D. A.
Schneider, D. P.
Vignali, C.
TI REVEALING A POPULATION OF HEAVILY OBSCURED ACTIVE GALACTIC NUCLEI AT z
approximate to 0.5-1 IN THE CHANDRA DEEP FIELD-SOUTH
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; galaxies: active; galaxies: photometry;
galaxies: starburst; infrared: galaxies; X-rays: galaxies
ID STAR-FORMATION RATE; ULTRALUMINOUS INFRARED GALAXIES; COMPTON-THICK AGN;
X-RAY-EMISSION; POINT-SOURCE CATALOGS; MS SOURCE CATALOGS; PHOTOMETRIC
REDSHIFTS; FORMING GALAXIES; NEARBY GALAXIES; STELLAR-MASS
AB Heavily obscured (NH greater than or similar to 3 x 10(23) cm(-2)) active galactic nuclei (AGNs) not detected even in the deepest X-ray surveys are often considered to be comparably numerous to the unobscured and moderately obscured AGNs. Such sources are required to fit the cosmic X-ray background (XRB) emission in the 10-30 keV band. We identify a numerically significant population of heavily obscured AGNs at z approximate to 0.5-1 in the Chandra Deep Field-South (CDF-S) and Extended Chandra Deep Field-South by selecting 242 X-ray undetected objects with infrared-based star-formation rates (SFRs) substantially higher (a factor of 3.2 or more) than their SFRs determined from the UV after correcting for dust extinction. An X-ray stacking analysis of 23 candidates in the central CDF-S region using the 4 Ms Chandra data reveals a hard X-ray signal with an effective power-law photon index of Gamma = 0.6(-0.4)(+ 0.3), indicating a significant contribution from obscured AGNs. Based on Monte Carlo simulations, we conclude that 74% +/- 25% of the selected galaxies host obscured AGNs, within which approximate to 95% are heavily obscured and approximate to 80% are Compton-thick (CT; N-H > 1.5 x 10(24) cm(-2)). The heavily obscured objects in our sample are of moderate intrinsic X-ray luminosity (approximate to(0.9-4) x 10(42) erg s(-1) in the 2-10 keV band). The space density of the CT AGNs is (1.6 +/- 0.5) x 10(-4) Mpc(-3). The z approximate to 0.5-1 CT objects studied here are expected to contribute approximate to 1% of the total XRB flux in the 10-30 keV band, and they account for approximate to 5%-15% of the emission in this energy band expected from all CT AGNs according to population-synthesis models. In the 6-8 keV band, the stacked signal of the 23 heavily obscured candidates accounts for <5% of the unresolved XRB flux, while the unresolved approximate to 25% of the XRB in this band can probably be explained by a stacking analysis of the X-ray undetected optical galaxies in the CDF-S (a 2.5 sigma stacked signal). We discuss prospects to identify such heavily obscured objects using future hard X-ray observatories.
C1 [Luo, B.; Brandt, W. N.; Xue, Y. Q.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Luo, B.; Brandt, W. N.; Xue, Y. Q.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Luo, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Brusa, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Comastri, A.; Gilli, R.] INAF Osservatorio Astron Bologna, Bologna, Italy.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Lehmer, B. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rafferty, D. A.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Vignali, C.] Univ Bologna, Dipartimento Astron, Bologna, Italy.
RP Luo, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
RI Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015;
OI Vignali, Cristian/0000-0002-8853-9611; Brandt,
William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970;
Gilli, Roberto/0000-0001-8121-6177; Alexander, David/0000-0002-5896-6313
FU CXC [SP1-12007A, G09-0134A]; NASA [NNX10AC99G]; Science and Technology
Facilities Council; ASI/INAF [I/009/10/0]
FX We acknowledge financial support from CXC grant SP1-12007A (B.L.,
W.N.B., Y.Q.X.), CXC grant G09-0134A (B. L., W.N.B., Y.Q.X.), NASA ADP
grant NNX10AC99G (W.N.B.), the Science and Technology Facilities Council
(D.M.A.), and ASI/INAF grant I/009/10/0 (A.C., C.V., R.G.). We are
grateful to T. Yaqoob and K. D. Murphy for providing support for the
MYTORUS model and making available the data for our desired half-opening
angle. We thank A. T. Steffen for helpful discussions. We also thank the
referee for carefully reviewing the manuscript and providing helpful
comments that improved this work.
NR 126
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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 OCT 10
PY 2011
VL 740
IS 1
AR 37
DI 10.1088/0004-637X/740/1/37
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825FL
UT WOS:000295256500037
ER
PT J
AU Oberg, KI
van der Marel, N
Kristensen, LE
van Dishoeck, EF
AF Oeberg, Karin I.
van der Marel, Nienke
Kristensen, Lars E.
van Dishoeck, Ewine F.
TI COMPLEX MOLECULES TOWARD LOW-MASS PROTOSTARS: THE SERPENS CORE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; astrochemistry; ISM: abundances; ISM: molecules
ID STAR-FORMING REGIONS; ORGANIC-MOLECULES; IRAS 16293-2422; HOT CORINOS;
CHEMISTRY; IRAS-16293-2422; ICES; PHOTODESORPTION; OUTFLOW; L1157
AB Gas-phase complex organic molecules are commonly detected toward high-mass protostellar hot cores. Detections toward low-mass protostars and outflows are comparatively rare, and a larger sample is the key to investigate how the chemistry responds to its environment. Guided by the prediction that complex organic molecules form in CH3OH-rich ices and thermally or non-thermally evaporate with CH3OH, we have identified three sight lines in the Serpens core-SMM1, SMM4, and SMM4-W-which are likely to be rich in complex organics. Using the IRAM 30 m telescope, narrow lines (FWHM of 1-2 km s(-1)) of CH3CHO and CH3OCH3 are detected toward all sources, HCOOCH3 toward SMM1 and SMM4-W, and C2H5OH not at all. Beam-averaged abundances of individual complex organics range between 0.6% and 10% with respect to CH3OH when the CH3OH rotational temperature is applied. The summed complex organic abundances also vary by an order of magnitude, with the richest chemistry toward the most luminous protostar SMM1. The range of abundances compare well with other beam-averaged observations of low-mass sources. Complex organic abundances are of the same order of magnitude toward low-mass protostars and high-mass hot cores, but HCOOCH3 is relatively more important toward low-mass protostars. This is consistent with a sequential ice photochemistry, dominated by CHO-containing products at low temperatures and early times.
C1 [Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[van der Marel, Nienke; Kristensen, Lars E.; van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, MS 42,60 Garden St, Cambridge, MA 02138 USA.
RI Kristensen, Lars/F-4774-2011
OI Kristensen, Lars/0000-0003-1159-3721
FU INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA [NAS 5-26555];
European Community [R113CT 2003 5058187]; Netherlands Organization for
Scientific Research (NWO)
FX Based on observations carried out with the IRAM 30 m telescope. IRAM is
supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).; We are
grateful to the IRAM staff for their assistance and to an anonymous
referee for helpful comments. Support for K.I.O. is provided by NASA
through 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.
Astrochemistry in Leiden is supported by a SPINOZA grant of the
Netherlands Organization for Scientific Research (NWO). This work has
benefited from research funding from the European Community's sixth
Framework Programme under RadioNet R113CT 2003 5058187.
NR 27
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U1 2
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 OCT 10
PY 2011
VL 740
IS 1
AR 14
DI 10.1088/0004-637X/740/1/14
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825FL
UT WOS:000295256500014
ER
PT J
AU Winebarger, AR
Schmelz, JT
Warren, HP
Saar, SH
Kashyap, VL
AF Winebarger, Amy R.
Schmelz, Joan T.
Warren, Harry P.
Saar, Steve H.
Kashyap, Vinay L.
TI USING A DIFFERENTIAL EMISSION MEASURE AND DENSITY MEASUREMENTS IN AN
ACTIVE REGION CORE TO TEST A STEADY HEATING MODEL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona
ID X-RAY TELESCOPE; ULTRAVIOLET IMAGING SPECTROMETER; SOLAR-B SATELLITE;
CORONAL LOOPS; TEMPERATURE DISTRIBUTION; SOHO EIT; HINODE; MOSS; TRACE;
MISSION
AB The frequency of heating events in the corona is an important constraint on the coronal heating mechanisms. Observations indicate that the intensities and velocities measured in active region cores are effectively steady, suggesting that heating events occur rapidly enough to keep high-temperature active region loops close to equilibrium. In this paper, we couple observations of active region (AR) 10955 made with the X-Ray Telescope and the EUV Imaging Spectrometer on board Hinode to test a simple steady heating model. First we calculate the differential emission measure (DEM) of the apex region of the loops in the active region core. We find the DEM to be broad and peaked around 3 MK. We then determine the densities in the corresponding footpoint regions. Using potential field extrapolations to approximate the loop lengths and the density-sensitive line ratios to infer the magnitude of the heating, we build a steady heating model for the active region core and find that we can match the general properties of the observed DEM for the temperature range of 6.3 < log T < 6.7. This model, for the first time, accounts for the base pressure, loop length, and distribution of apex temperatures of the core loops. We find that the density-sensitive spectral line intensities and the bulk of the hot emission in the active region core are consistent with steady heating. We also find, however, that the steady heating model cannot address the emission observed at lower temperatures. This emission may be due to foreground or background structures, or may indicate that the heating in the core is more complicated. Different heating scenarios must be tested to determine if they have the same level of agreement.
C1 [Winebarger, Amy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Schmelz, Joan T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
[Warren, Harry P.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Saar, Steve H.; Kashyap, Vinay L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA.
EM amy.r.winebarger@nasa.gov
FU NSF; NASA/SAO
FX A.R.W. was supported by an NSF Career grant. Solar physics research at
the University of Memphis is supported by a Hinode subcontract from
NASA/SAO. A. R. W. thanks Mark Weber for many enlightening conversations
on differential emission measures.
NR 56
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 10
PY 2011
VL 740
IS 1
AR 2
DI 10.1088/0004-637X/740/1/2
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 825FL
UT WOS:000295256500002
ER
PT J
AU Mulcahy, DG
Beckstead, TH
Sites, JW
AF Mulcahy, Daniel G.
Beckstead, Thomas H.
Sites, Jack W., Jr.
TI Molecular Systematics of the Leptodeirini (Colubroidea: Dipsadidae)
Revisited: Species-tree Analyses and Multi-locus Data
SO COPEIA
LA English
DT Article
ID AMERICAN XENODONTINE SNAKES; GENE-TREE; PHYLOGENETIC ANALYSIS;
MAXIMUM-LIKELIHOOD; MITOCHONDRIAL-DNA; COLUBRID SNAKE; DIPSAS-INDICA;
SEQUENCES; SERPENTES; LIZARDS
AB Cat-eyed snakes (Leptodeira) were thought to be closely related to nightsnakes (Hypsiglena and Pseudoleptodeira) based on morphology and immunological data, which allied these genera with blunt-headed vine snakes (Imantodes) and the Cloud Forest Snake (Cryophis hallbergi). We collected sequence data from six protein-encoding nuclear loci (SLC30A1, ZEB2, FSHR, NTF3, DNAH3, and PNN; 4149 bp) and additional mtDNA data (nad5; 955 bp) added to published cob and nad4 (total 2387 bp mtDNA) from these and other rear-fanged, mildly venomous snakes that prey on vertebrates (frogs and lizards) and from several other dipsadine genera (Dipsas, Sibon, and Atractus) that prey on invertebrates (goo-eaters). We analyzed relationships using concatenation and a coalescent species-tree method. When analyzed separately, using either concatenation or coalescent methods, nuclear data support a different overall topology from the mtDNA data. Like the mtDNA data, the nuclear data support the Leptodeira + Imantodes relationship, but instead place this clade more closely to the goo-eaters, with the nightsnakes as the basal divergence in the group. When the data are combined in concatenation analyses, the more variable mtDNA data appear to overwhelm the nuclear data, but not under the coalescent model.
C1 [Mulcahy, Daniel G.] Smithsonian Inst, Museum Support Ctr LAB, Suitland, MD 20746 USA.
[Mulcahy, Daniel G.; Beckstead, Thomas H.; Sites, Jack W., Jr.] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA.
[Mulcahy, Daniel G.; Beckstead, Thomas H.; Sites, Jack W., Jr.] Brigham Young Univ, Bean Life Sci Museum, Provo, UT 84602 USA.
RP Mulcahy, DG (reprint author), Smithsonian Inst, Museum Support Ctr LAB, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM MulcahyD@si.edu; tombeckstead@gmail.com; jack_sites@byu.edu
FU BYU; BYU Department of Biology; NSF [EF-0334966]
FX This work was funded by a BYU Mentoring Environment Grant (MEG; Office
of Research and Creative Activities), the BYU Department of Biology, and
by NSF Assembling the Tree of Life-Deep Scaly project (sub-award
EF-0334966) to JWS, Jr. W. B. Simison at the California Academy of
Sciences allowed extended use of their PhyloCluster. K. de Queiroz
provided additional computational resources at the Smithsonian
Institution. F. Fontanel la and H. Bracken, both at BYU provided useful
discussion and comments on the manuscript. The following institutions
and individuals provided tissue loans: KU (W. E. Duellman), LSU (D.
Dittman), MVZ (J. McGuire), L. Canseco-Marquez, E. Greenbaum, J.
Mendelson, III, T. Papenfuss, and O. Robles-Romero.
NR 68
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Z9 6
U1 1
U2 5
PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS
PI MIAMI
PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200
SW 8TH STREET, MIAMI, FL 33199 USA
SN 0045-8511
EI 1938-5110
J9 COPEIA
JI Copeia
PD OCT 10
PY 2011
IS 3
BP 407
EP 417
DI 10.1643/CH-10-058
PG 11
WC Zoology
SC Zoology
GA 833BD
UT WOS:000295855900008
ER
PT J
AU Csengeri, T
Bontemps, S
Schneider, N
Motte, F
Gueth, F
Hora, JL
AF Csengeri, T.
Bontemps, S.
Schneider, N.
Motte, F.
Gueth, F.
Hora, J. L.
TI CONVERGENT FLOWS AND LOW-VELOCITY SHOCKS IN DR21(OH)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: kinematics and dynamics; stars: formation
ID MOLECULAR CLOUD EVOLUTION; STAR-FORMATION; COMPLEX-MOLECULES; MASER
EMISSION; CYGNUS-X; CONTINUUM; CLUSTER; CORE; GAS; FRAGMENTATION
AB DR21(OH) is a pc-scale massive, similar to 7000 M-circle dot clump hosting three massive dense cores (MDCs) at an early stage of their evolution. We present a high angular resolution mosaic, covering similar to 70 '' x 100 '', with the IRAM Plateau de Bure Interferometer at 3 mm to trace the dust continuum emission and the N2H+ (J = 1-0) and CH3CN (J = 5-4) molecular emission. The cold, dense gas traced by the compact emission in N2H+ is associated with the three MDCs and shows several velocity components toward each MDC. These velocity components reveal local shears in the velocity fields which are best interpreted as convergent flows. Moreover, we report the detection of weak extended emission from CH3CN at the position of the N2H+ velocity shears. We propose that this extended CH3CN emission is tracing warm gas associated with the low-velocity shocks expected at the location of convergence of the flows where velocity shears are observed. This is the first detection of low-velocity shocks associated with small (subparsec) scale convergent flows which are proposed to be at the origin of the densest structures and of the formation of (high-mass) stars. In addition, we propose that MDCs may be active sites of star formation for more than a crossing time as they continuously receive material from larger scale flows as suggested by the global picture of dynamical, gravity-driven evolution of massive clumps which is favored by the present observations.
C1 [Csengeri, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Csengeri, T.; Schneider, N.; Motte, F.] Univ Paris Diderot, CNRS, CEA Saclay, Lab AIM Paris Saclay,CEA INSU,IRFU SAp, F-91191 Gif Sur Yvette, France.
[Bontemps, S.] Univ Bordeaux 1, CNRS, OASU LAB UMR5804, F-33270 Floirac, France.
[Gueth, F.] IRAM, F-38406 St Martin Dheres, France.
[Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Csengeri, T (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM ctimea@mpifr-bonn.mpg.de
FU FP6 Marie-Curie Research Training Network Constellation: the origin of
stellar masses [MRTN-CT-2006-035890]; ANR (Agence Nationale pour la
Recherche) [ANR-08-BLAN-0241]; INSU/CNRS (France); MPG (Germany); IGN
(Spain)
FX T. Csengeri acknowledges support from the FP6 Marie-Curie Research
Training Network Constellation: the origin of stellar masses
(MRTN-CT-2006-035890). This work was also supported by the ANR (Agence
Nationale pour la Recherche) project PROBeS, number ANR-08-BLAN-0241.;
IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).
NR 34
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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 OCT 10
PY 2011
VL 740
IS 1
AR L5
DI 10.1088/2041-8205/740/1/L5
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 824OH
UT WOS:000295210900005
ER
PT J
AU McIntosh, SW
Kiefer, KK
Leamon, RJ
Kasper, JC
Stevens, ML
AF McIntosh, Scott W.
Kiefer, Kandace K.
Leamon, Robert J.
Kasper, Justin C.
Stevens, Michael L.
TI SOLAR CYCLE VARIATIONS IN THE ELEMENTAL ABUNDANCE OF HELIUM AND
FRACTIONATION OF IRON IN THE FAST SOLAR WIND: INDICATORS OF AN EVOLVING
ENERGETIC RELEASE OF MASS FROM THE LOWER SOLAR ATMOSPHERE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE solar wind; Sun: chromosphere; Sun: corona; Sun: heliosphere; Sun:
surface magnetism; Sun: transition region
ID ALFVENIC WAVES; CORONA; SPEED; POWER
AB We present and discuss the strong correspondence between evolution of the emission length scale in the lower transition region and in situ measurements of the fast solar wind composition during the most recent solar minimum. We combine recent analyses demonstrating the variance in the (supergranular) network emission length scale measured by the Solar and Heliospheric Observatory (and STEREO) with that of the helium abundance (from Wind) and the degree of iron fractionation in the solar wind (from the Advanced Composition Explorer and Ulysses). The net picture developing is one where a decrease in the helium abundance and the degree of iron fractionation (approaching values expected of the photosphere) in the fast wind indicate a significant change in the process loading material into the fast solar wind during the recent solar minimum. This result is compounded by a study of the helium abundance during the space age using the NASA OMNI database, which shows a slowly decaying amount of helium being driven into the heliosphere over the course of several solar cycles.
C1 [McIntosh, Scott W.; Kiefer, Kandace K.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Kiefer, Kandace K.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47906 USA.
[Leamon, Robert J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
[Kasper, Justin C.; Stevens, Michael L.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP McIntosh, SW (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA.
RI Kasper, Justin/D-1152-2010
OI Kasper, Justin/0000-0002-7077-930X
FU NSF [ATM-0541567, ATM-0925177]; NASA [NNG06GC89G, NNX08AL22G,
NNX08AH45G]; National Science Foundation
FX S.W.M. is supported by NSF ATM-0541567 (ATM-0925177), NASA grants
NNG06GC89G, NNX08AL22G, and NNX08AH45G. K3 visited HAO in the
summer of 2011 supported by the NSF Research Experience for
Undergraduates (REU) program-we greatly appreciate the organization and
commitment of the CU/LASP REU program administration group. In addition,
we thank Joe Gurman for valuable comments, the Ulysses/SWICS and
ACE/SWICS instrument teams for the effort taken to distribute and
document the ion composition they serve to the community, and likewise
to the OMNI database staff for their continued effort to preserve an
essential physical record. NCAR is sponsored by the National Science
Foundation.
NR 26
TC 9
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U1 0
U2 8
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 OCT 10
PY 2011
VL 740
IS 1
AR L23
DI 10.1088/2041-8205/740/1/L23
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 824OH
UT WOS:000295210900023
ER
PT J
AU Viti, S
Jimenez-Serra, I
Yates, JA
Codella, C
Vasta, M
Caselli, P
Lefloch, B
Ceccarelli, C
AF Viti, S.
Jimenez-Serra, I.
Yates, J. A.
Codella, C.
Vasta, M.
Caselli, P.
Lefloch, B.
Ceccarelli, C.
TI L1157-B1: WATER AND AMMONIA AS DIAGNOSTICS OF SHOCK TEMPERATURE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual objects (L1157); ISM: jets and outflows; ISM: molecules;
stars: formation
ID C-TYPE SHOCKS; CHESS SPECTRAL SURVEY; MOLECULAR CLOUDS; INTERSTELLAR
AMMONIA; TEMPORAL EVOLUTION; RADIATIVE-TRANSFER; OUTFLOW L1157;
EMISSION; WAVES; CORES
AB We investigate the origin and nature of the profiles of water and ammonia observed toward the L1157-B1 clump as part of the HIFI CHESS survey using a new code coupling a gas-grain chemical model with a parametric shock model. First results from the unbiased survey reveal different molecular components at different excitation conditions coexisting in the B1 bow shock structure, with NH3, H2CO, and CH3OH emitting only at relatively low outflow velocities whereas H2O shows bright emission at high velocities. Our model suggests that these differences are purely chemical and can be explained by the presence of a C-type shock whose maximum temperature must be close to 4000 K along the B1 clump.
C1 [Viti, S.; Yates, J. A.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Codella, C.; Vasta, M.; Caselli, P.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Lefloch, B.; Ceccarelli, C.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France.
[Lefloch, B.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain.
RP Viti, S (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
EM sv@star.ucl.ac.uk
OI Codella, Claudio/0000-0003-1514-3074
FU Smithsonian Astrophysical Observatory
FX I.J.-S. acknowledges the Smithsonian Astrophysical Observatory for the
support provided through a SMA fellowship.
NR 41
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD OCT 10
PY 2011
VL 740
IS 1
AR L3
DI 10.1088/2041-8205/740/1/L3
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 824OH
UT WOS:000295210900003
ER
PT J
AU Aliu, E
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bouvier, A
Bradbury, SM
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Christiansen, JL
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickherber, R
Duke, C
Errando, M
Falcone, A
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gibbs, K
Gillanders, GH
Godambe, S
Griffin, S
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Huan, H
Hughes, G
Hui, CM
Humensky, TB
Imran, A
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Krawczynski, H
Krennrich, F
Lang, MJ
Lyutikov, M
Madhavan, AS
Maier, G
Majumdar, P
McArthur, S
McCann, A
McCutcheon, M
Moriarty, P
Mukherjee, R
Nunez, P
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
Pizlo, F
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
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Tyler, J
Varlotta, A
Vassiliev, VV
Vincent, S
Vivier, M
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Williams, DA
Zitzer, B
AF Aliu, E.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Bouvier, A.
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.
Dickherber, R.
Duke, C.
Errando, M.
Falcone, A.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gibbs, K.
Gillanders, G. H.
Godambe, S.
Griffin, S.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Holder, J.
Huan, H.
Hughes, G.
Hui, C. M.
Humensky, T. B.
Imran, A.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
Lyutikov, M.
Madhavan, A. S.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
McCutcheon, M.
Moriarty, P.
Mukherjee, R.
Nunez, P.
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
Pizlo, F.
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.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Tyler, J.
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.
Zitzer, B.
CA VERITAS Collaboration
TI Detection of Pulsed Gamma Rays Above 100 GeV from the Crab Pulsar
SO SCIENCE
LA English
DT Article
ID HIGH-ENERGY EMISSION; AREA TELESCOPE; OUTER MAGNETOSPHERE; MILLISECOND
PULSARS; LIGHT CURVES; SLOT GAPS; NEBULA; RADIATION; TEV; CATALOG
AB We report the detection of pulsed gamma rays from the Crab pulsar at energies above 100 giga-electron volts (GeV) with the Very Energetic Radiation Imaging Telescope Array System (VERITAS) array of atmospheric Cherenkov telescopes. The detection cannot be explained on the basis of current pulsar models. The photon spectrum of pulsed emission between 100 mega-electron volts and 400 GeV is described by a broken power law that is statistically preferred over a power law with an exponential cutoff. It is unlikely that the observation can be explained by invoking curvature radiation as the origin of the observed gamma rays above 100 GeV. Our findings require that these gamma rays be produced more than 10 stellar radii from the neutron star.
C1 [Griffin, S.; Guenette, R.; Hanna, D.; McCann, A.; McCutcheon, M.; Ragan, K.; Staszak, D.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 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.
[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.; Gibbs, K.; Perkins, J. S.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Byrum, K.; Smith, A. W.; Zitzer, B.] 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.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Christiansen, J. L.] 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.; Lyutikov, M.; Pizlo, F.; Sembroski, G. H.; Theiling, M.; 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.; Nunez, P.; 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.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Huan, H.; Humensky, T. B.; Park, N.; Reyes, L. C.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.] DESY, D-15738 Zeuthen, Germany.
[Imran, A.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Gall, D.; 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.
[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, Dept Phys, New York, NY 10027 USA.
RP McCann, A (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
EM mccann@hep.physics.mcgill.ca; nepomuk.otte@gmail.com;
schroedter@veritas.sao.arizona.edu
OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610;
Ward, John E/0000-0003-1973-0794; Otte, Adam
Nepomuk/0000-0002-5955-6383; Lang, Mark/0000-0003-4641-4201
FU U.S. Department of Energy; NSF; Smithsonian Institution; Natural
Sciences and Engineering Research Council of Canada; Science Foundation
Ireland (SFI) [10/RFP/AST2748]; Science and Technology Facilities
Council in the United Kingdom; Alexander von Humboldt Foundation
FX This research is supported by grants from the U.S. Department of Energy,
NSF, and the Smithsonian Institution; by Natural Sciences and
Engineering Research Council of Canada; by Science Foundation Ireland
(SFI 10/RFP/AST2748); and by the Science and Technology Facilities
Council in the United Kingdom. We acknowledge the excellent work of the
technical support staff at the Fred Lawrence Whipple Observatory and at
the collaborating institutions in the construction and operation of the
instrument. A.N.O. was supported in part by a Feodor-Lynen fellowship of
the Alexander von Humboldt Foundation. We are grateful to M. Roberts and
A. Lyne for providing us with Crab-pulsar ephemerides before the public
ones became available.
NR 32
TC 83
Z9 84
U1 1
U2 6
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 OCT 7
PY 2011
VL 334
IS 6052
BP 69
EP 72
DI 10.1126/science.1208192
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 829KW
UT WOS:000295580300040
ER
PT J
AU Cassoff, RM
Moore, KM
McLellan, WA
Barco, SG
Rotstein, DS
Moore, MJ
AF Cassoff, Rachel M.
Moore, Kathleen M.
McLellan, William A.
Barco, Susan G.
Rotstein, David S.
Moore, Michael J.
TI Lethal entanglement in baleen whales
SO DISEASES OF AQUATIC ORGANISMS
LA English
DT Article
DE Baleen whales; Entanglement; Mortality; Cetacean; Strandings; Fishing
gear; Necropsy; Northwestern Atlantic
ID ATLANTIC RIGHT WHALES; WESTERN NORTH-ATLANTIC; MEGAPTERA-NOVAEANGLIAE;
EUBALAENA-GLACIALIS; HUMPBACK WHALES; BALAENOPTERA-ACUTOROSTRATA;
CYAMIDS CRUSTACEA; BOWHEAD WHALE; MINKE WHALE; INJURIES
AB Understanding the scenarios whereby fishing gear entanglement of large whales induces mortality is important for the development of mitigation strategies. Here we present a series of 21 cases involving 4 species of baleen whales in the NW Atlantic, describing the available sighting history, necropsy observations, and subsequent data analyses that enabled the compilation of the manners in which entanglement can be lethal. The single acute cause of entanglement mortality identified was drowning from entanglement involving multiple body parts, with the animal's inability to surface. More protracted causes of death included impaired foraging during entanglement, resulting in starvation after many months; systemic infection arising from open, unresolved entanglement wounds; and hemorrhage or debilitation due to severe gear-related damage to tissues. Serious gear-induced injury can include laceration of large vessels, occlusion of the nares, embedding of line in growing bone, and massive periosteal proliferation of new bone in an attempt to wall off constricting, encircling lines. These data show that baleen whale entanglement is not only a major issue for the conservation of some baleen whale populations, but is also a major concern for the welfare of each affected individual.
C1 [Moore, Michael J.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
[Cassoff, Rachel M.] Univ Penn, Sch Vet Med, Philadelphia, PA 19104 USA.
[Moore, Kathleen M.] Int Fund Anim Welf, Yarmouth Port, MA 02675 USA.
[McLellan, William A.] Univ N Carolina, Wilmington, NC 28403 USA.
[Barco, Susan G.] Virginia Aquarium & Marine Sci Ctr, Stranding Response Program, Virginia Beach, VA 23451 USA.
[Rotstein, David S.] Smithsonian Museum Support Ctr, Osteoprep Lab, Suitland, MD 20746 USA.
[Moore, Michael J.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
RP Moore, MJ (reprint author), Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA.
EM mmoore@whoi.edu
RI Moore, Michael/E-1707-2015
OI Moore, Michael/0000-0003-3074-6631
FU NOAA [NA09OAR4320129]
FX The authors thank the many stranding responders on the North American
east coast who have contributed hugely to this dataset. Right whale data
were accessed with permission from the North Atlantic Right Whale
Consortium necropsy and sightings databases. This case report analysis
was supported in part by NOAA Cooperative Agreement No. NA09OAR4320129.
Stranding response was supported by multiple NOAA Prescott awards to UNC
Wilmington, Virginia Aquarium & Marine Science Center, the Cape Cod
Stranding Network and Woods Hole Oceanographic Institution (WHOI). NOAA
contracts for right whale necropsy were held by WHOI.
NR 43
TC 39
Z9 43
U1 10
U2 51
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 OCT 6
PY 2011
VL 96
IS 3
BP 175
EP 185
DI 10.3354/dao02385
PG 11
WC Fisheries; Veterinary Sciences
SC Fisheries; Veterinary Sciences
GA 831GF
UT WOS:000295716200001
PM 22132496
ER
PT J
AU Bean, J
AF Bean, Jacob
TI EXTRASOLAR PLANETS Homing in on another Earth
SO NATURE
LA English
DT Editorial Material
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Bean, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jbean@cfa.harvard.edu
NR 4
TC 5
Z9 5
U1 0
U2 0
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD OCT 6
PY 2011
VL 478
IS 7367
BP 41
EP 42
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 829JN
UT WOS:000295575400027
PM 21964338
ER
PT J
AU Grego, L
AF Grego, Laura
TI Security in Space: What Is at Stake and How Do We Move Forward?
SO ASIAN PERSPECTIVE
LA English
DT Article
DE space security; antisatellite capability; space debris; international
security
ID DEBRIS
AB In recent decades, satellites have become increasingly important in the economic, civil, and military spheres. At the same time, space has become more crowded with satellites and the debris from their use, and many more states have become spacefaring. However, the legal and normative regime has not kept pace with these changes. Recent trends and events-including demonstrations of antisatellite (ASAT) capability, a collision between satellites, and a dramatic increase in dangerous space debris-make clear that the space environment needs more protection, that satellites face growing risks, and that space activities may be a potential source of mistrust and tension between countries. While voluntary confidence-building and transparency measures can help solve some of these issues, more substantive engagement is required to keep space safe and secure into the future.
C1 [Grego, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
EM lgrego@ucsusa.org
NR 13
TC 1
Z9 1
U1 1
U2 1
PU KYUNGNAM UNIV, INST FAR EASTERN STUDIES
PI SEOUL
PA 28-42 SAMCHUNG-DONG, CHONGRO-KU, SEOUL, 110-230, SOUTH KOREA
SN 0258-9184
J9 ASIAN PERSPECT-SEOUL
JI Asian Perspec.
PD OCT-DEC
PY 2011
VL 35
IS 4
SI SI
BP 503
EP 520
PG 18
WC International Relations
SC International Relations
GA 862DA
UT WOS:000298068800002
ER
PT J
AU Wise, MA
Brown, CD
AF Wise, Michael A.
Brown, Cathleen D.
TI Chemical composition of coexisting columbite-group minerals and
cassiterite from the Black Mountain pegmatite, Maine
SO EUROPEAN JOURNAL OF MINERALOGY
LA English
DT Article
DE cassiterite; columbite-group minerals; pegmatite; Black Mountain; Maine
ID ELEMENT GRANITIC PEGMATITES; OXIDE MINERALS; NIOBIUM-TANTALUM;
SOUTH-DAKOTA; TA-BEARING; NB-BEARING; GEOCHEMISTRY; WODGINITE; TRENDS;
FRACTIONATION
AB Detailed examination of hand samples and backscatter electron images of Nb-, Ta-, Sn-oxide minerals from the Black Mountain pegmatite has revealed the presence of discrete crystals, as well as cassiterite-hosted micrograins of columbite-group minerals (CGM). Micrograins and discrete grains of CGM show a wide range of Mn/(Mn + Fe) values, but only the micrograins have limited Ta/(Ta + Nb) values. Trace amounts of Ti, Sc, Fe(3+) and Sn are common in both generations of CGM, but their total rarely exceeds 1.0 oxide wt%. The chemistry of the host cassiterite is relatively homogeneous and pure; the total concentration of FeO, MnO, Nb(2)O(5), Ta(2)O(5) and TiO(2) rarely exceeds 2.0 wt%.
While discrete CGM grains show weak progressive zonation and minor replacement, micrograins display complex oscillatory zonation, resorption and/or replacement textures. Textural evidence suggests that the micrograins crystallized after the formation of discrete grains of columbite and cassiterite. On the whole, both discrete crystals and micrograins of CGM show increasing Mn/(Mn + Fe) with fractionation as commonly observed in F-enriched granitic pegmatites. Micrograins of CGM typically show higher Ta/(Ta + Nb) values compared to their discrete crystal counterparts. Textural characteristics of CGM micrograins are inconsistent with an origin by exsolution, and instead, indicate primary precipitation.
C1 [Wise, Michael A.; Brown, Cathleen D.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Wise, MA (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM wisem@si.edu
FU Sprague fund; Smithsonian Institution
FX This study was made possible by the Sprague fund and laboratory support
of the Smithsonian Institution. We gratefully thank Joe Martin of
Rumford, Maine for providing access to the Black Mountain pegmatite and
T. S. Ercit and T. Martin for their invaluable discussions regarding
columbite inclusions in cassiterite. The authors thank W. Simmons, M.
Novak, P. Cerny and Y. Thibault for constructive criticisms which led to
considerable improvements of this manuscript.
NR 41
TC 3
Z9 3
U1 0
U2 11
PU E SCHWEIZERBARTSCHE VERLAGS
PI STUTTGART
PA NAEGELE U OBERMILLER, SCIENCE PUBLISHERS, JOHANNESSTRASSE 3A, D 70176
STUTTGART, GERMANY
SN 0935-1221
J9 EUR J MINERAL
JI Eur. J. Mineral.
PD OCT
PY 2011
VL 23
IS 5
BP 817
EP 828
DI 10.1127/0935-1221/2011/0023-2102
PG 12
WC Mineralogy
SC Mineralogy
GA 861SB
UT WOS:000298038400011
ER
PT J
AU Santymire, RM
Brown, JL
Stewart, RA
Santymire, RC
Wildt, DE
Howard, J
AF Santymire, Rachel M.
Brown, Janine L.
Stewart, Rosemary A.
Santymire, Robb C.
Wildt, David E.
Howard, JoGayle
TI Reproductive gonadal steroidogenic activity in the fishing cat
(Prionailurus viverrinus) assessed by fecal steroid analyses
SO ANIMAL REPRODUCTION SCIENCE
LA English
DT Article
DE Fe lid reproduction; Seasonality; Estrous cycle; Ovulation
ID INTRAUTERINE ARTIFICIAL-INSEMINATION; NORMAL ESTROUS-CYCLE; LEOPARD
NEOFELIS-NEBULOSA; PUMA FELIS-CONCOLOR; LION PANTHERA-LEO; OVARIAN
ACTIVITY; SEXUAL-BEHAVIOR; EXOGENOUS GONADOTROPINS; SERUM
CONCENTRATIONS; CLOUDED LEOPARD
AB Non-invasive fecal steroid analyses were used to characterize gonadal activity in the fishing cat (Prionailurus viverrinus). Estrogen, progestagen and androgen metabolites were quantified in fecal samples collected for 12 months from four males and 10 females housed at seven North American zoological institutions. Male reproductive hormone concentrations did not vary (P > 0.05) among season, and estrogen cycles were observed year-round in females and averaged (+/- SEM) 19.9 +/- 1.0 days. Mean peak estrogen concentration during estrus (460.0 +/- 72.6 ng/g feces) was five-fold higher than baseline (87.3 +/- 14.0 ng/g feces). Five of seven females (71.4%) housed alone or with another female demonstrated spontaneous luteal activity (apparent ovulation without copulation), with mean progestagen concentration (20.3 +/- 4.7 mu g/g feces), increasing nearly five-fold above baseline (4.1 +/- 0.8 mu g/g feces). The non-pregnant luteal phase averaged 32.9 +/- 2.5 days (n = 13). One female delivered kittens 70 days after natural mating with fecal progestagen concentrations averaging 51.2 +/- 5.2 mu g/g feces. Two additional females were administered exogenous gonadotropins (150 IU eCG; 100 IU hCG), which caused hyper-elevated concentrations of fecal estrogen and progestagen (plus ovulation). Results indicate that: (1) male and female fishing cats managed in North American zoos are reproductively active year round; (2) 71.4% of females experienced spontaneous ovulation; and (3) females are responsive to exogenous gonadotropins for ovulation induction, but a regimen that produces a normative ovarian steroidogenic response needs to be identified. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Santymire, Rachel M.; Brown, Janine L.; Stewart, Rosemary A.; Santymire, Robb C.; Wildt, David E.; Howard, JoGayle] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Ctr Species Survival, Front Royal, VA 22630 USA.
RP Santymire, RM (reprint author), Lincoln Pk Zoo,2001 N Clark St, Chicago, IL 60614 USA.
EM rsantymire@lpzoo.org
FU Morris Animal Foundation
FX This study was supported by the Morris Animal Foundation. The authors
thank the animal care staff and management of the partner zoological
institutions (Minnesota Zoological Garden, Cincinnati Zoo & Botanical
Garden, Sacramento Zoo, San Francisco Zoological Gardens, Happy Hollow
Zoo, Oklahoma City Zoological Park, and San Antonio Zoological Gardens
and Aquarium) for participation in the study and dedication on fecal
sample collections. We thank Dr. Bill Swanson and the animal care and
veterinary staff at the Cincinnati Zoo & Botanical Garden for
administering exogenous gonadotropins (eCG and hCG) to two female
fishing cats. We also thank Claudia Sanchez and Nicole Abbondanza at the
National Zoo's Endocrine Research Laboratories for excellent technical
assistance. Additionally, we thank Dr. Eric Lonsdorf at Lincoln Park Zoo
for assistance with statistical analyses.
NR 55
TC 9
Z9 9
U1 1
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-4320
J9 ANIM REPROD SCI
JI Anim. Reprod. Sci.
PD OCT
PY 2011
VL 128
IS 1-4
BP 60
EP 72
DI 10.1016/j.anireprosci.2011.09.001
PG 13
WC Agriculture, Dairy & Animal Science; Reproductive Biology
SC Agriculture; Reproductive Biology
GA 859RF
UT WOS:000297892800008
PM 21975304
ER
PT J
AU Ryder, TB
Fox, JW
Marra, PP
AF Ryder, Thomas B.
Fox, James W.
Marra, Peter P.
TI ESTIMATING MIGRATORY CONNECTIVITY OF GRAY CATBIRDS (DUMETELLA
CAROLINENSIS) USING GEOLOCATOR AND MARK-RECAPTURE DATA (vol 128, pg 448,
2011)
SO AUK
LA English
DT Correction
C1 [Ryder, Thomas B.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
[Fox, James W.] British Antarctic Survey, Nat Environm Res Council, Cambridge CB3 0ET, England.
RP Ryder, TB (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, POB 37012-MRC5503, Washington, DC 20008 USA.
EM rydert@si.edu
NR 1
TC 0
Z9 0
U1 1
U2 19
PU AMER ORNITHOLOGISTS UNION
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0004-8038
J9 AUK
JI AUK
PD OCT
PY 2011
VL 128
IS 4
BP 810
EP 810
DI 10.1525/auk.2011.128.4.810
PG 1
WC Ornithology
SC Zoology
GA 859JM
UT WOS:000297872700026
ER
PT J
AU Graur, O
Poznanski, D
Maoz, D
Yasuda, N
Totani, T
Fukugita, M
Filippenko, AV
Foley, RJ
Silverman, JM
Gal-Yam, A
Horesh, A
Jannuzi, BT
AF Graur, O.
Poznanski, D.
Maoz, D.
Yasuda, N.
Totani, T.
Fukugita, M.
Filippenko, A. V.
Foley, R. J.
Silverman, J. M.
Gal-Yam, A.
Horesh, A.
Jannuzi, B. T.
TI Supernovae in the Subaru Deep Field: the rate and delay-time
distribution of Type Ia supernovae out to redshift 2
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: observational; surveys; supernovae: general; galaxies:
distances and redshifts
ID DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES;
LYMAN-BREAK GALAXIES; CORE-COLLAPSE SUPERNOVAE; WHITE-DWARF BINARY;
GAMMA-RAY BURSTS; LUMINOSITY FUNCTIONS; LEGACY SURVEY; LIGHT CURVES
AB The Type Ia supernova (SN Ia) rate, when compared to the cosmic star formation history (SFH), can be used to derive the delay-time distribution (DTD; the hypothetical SN Ia rate versus time following a brief burst of star formation) of SNe Ia, which can distinguish among progenitor models. We present the results of a supernova (SN) survey in the Subaru Deep Field (SDF). Over a period of 3 years, we have observed the SDF on four independent epochs with Suprime-Cam on the Subaru 8.2-m telescope, with two nights of exposure per epoch, in the R, i'and z' bands. We have discovered 150 SNe out to redshift z 2. Using 11 photometric bands from the observer-frame far-ultraviolet to the near-infrared, we derive photometric redshifts for the SN host galaxies (for 24 we also have spectroscopic redshifts). This information is combined with the SN photometry to determine the type and redshift distribution of the SN sample. Our final sample includes 28 SNe Ia in the range 1.0 < z < 1.5 and 10 in the range 1.5 < z < 2.0. As our survey is largely insensitive to core-collapse SNe (CC SNe) at z > 1, most of the events found in this range are likely SNe Ia. Our SN Ia rate measurements are consistent with those derived from the Hubble Space Telescope (HST) Great Observatories Origins Deep Survey (GOODS) sample, but the overall uncertainty of our 1.5 < z < 2.0 measurement is a factor of 2 smaller, of 3550 per cent. Based on this sample, we find that the SN Ia rate evolution levels off at 1.0 < z < 2.0, but shows no sign of declining. Combining our SN Ia rate measurements and those from the literature, and comparing to a wide range of possible SFHs, the best-fitting DTD (with a reduced ?2= 0.7) is a power law of the form ?(t) ?t beta, with index beta=-1.1 +/- 0.1 (statistical) +/- 0.17 (systematic). This result is consistent with other recent DTD measurements at various redshifts and environments, and is in agreement with a generic prediction of the double-degenerate progenitor scenario for SNe Ia. Most single-degenerate models predict different DTDs. By combining the contribution from CC SNe, based on the wide range of SFHs, with that from SNe Ia, calculated with the best-fitting DTD, we predict that the mean present-day cosmic iron abundance is in the range ZFe= (0.090.37) ZFe, ?. We further predict that the high-z SN searches now beginning with HST will discover 211 SNe Ia at z > 2.
C1 [Graur, O.; Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Poznanski, D.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Poznanski, D.; Filippenko, A. V.; Foley, R. J.; Silverman, J. M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Yasuda, N.; Fukugita, M.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Totani, T.] Kyoto Univ, Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gal-Yam, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel.
[Horesh, A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
RP Graur, O (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
EM orgraur@wise.tau.ac.il
RI Yasuda, Naoki/A-4355-2011; Horesh, Assaf/O-9873-2016;
OI Horesh, Assaf/0000-0002-5936-1156; Graur, Or/0000-0002-4391-6137
FU Israel Science Foundation; Israel Science Foundation (ISF); Einstein
Fellowship; US Department of Energy [DE-FG02-06ER06-04]; NSF
[AST-0908886]; TABASGO Foundation; Department of Energy
[DE-FG0-08ER41563]; Clay fellowship; Marie Curie IRG
FX DM acknowledges support by a grant from the Israel Science Foundation
(ISF). DP is supported by an Einstein Fellowship, and by the US
Department of Energy Scientific Discovery through Advanced Computing
(SciDAC) programme under contract DE-FG02-06ER06-04. AVF is grateful for
the financial support of NSF grant AST-0908886, the TABASGO Foundation
and Department of Energy grant DE-FG0-08ER41563. RJF is supported by a
Clay fellowship. AG is supported by an FP7/Marie Curie IRG fellowship
and a grant from the ISF.
NR 177
TC 61
Z9 61
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 2
BP 916
EP 940
DI 10.1111/j.1365-2966.2011.19287.x
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HR
UT WOS:000297043000008
ER
PT J
AU Angus, GW
Diaferio, A
AF Angus, G. W.
Diaferio, Antonaldo
TI The abundance of galaxy clusters in modified Newtonian dynamics:
cosmological simulations with massive neutrinos
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: formation; cosmology: theory; dark matter; large-scale
structure of Universe
ID MICROWAVE BACKGROUND ANISOTROPIES; POWER-SPECTRUM; BULLET CLUSTER;
DARK-MATTER; LAMBDA-CDM; MOND; EXISTENCE; GRAVITY; HALOS; SCALE
AB We present a new particle mesh cosmological N-body code for accurately solving the modified Poisson equation of the quasi-linear formulation of modified Newtonian dynamics (MOND). We generate initial conditions for the Angus cosmological model, which is identical to ? cold dark matter (?CDM) except that the CDM is switched for a single species of thermal sterile neutrinos. We set the initial conditions at z= 250 for a (512 Mpc h-1)3 box with 2563 particles, and we evolve them down to z= 0. We clearly demonstrate the ability of MOND to develop the large-scale structure in a hot dark matter cosmology and contradict the naive expectation that MOND cannot form galaxy clusters. We find that the correct order of magnitude of X-ray clusters (with TX > 4.5 keV) can be formed, but that we overpredict the number of very rich clusters and seriously underpredict the number of lower mass clusters. We present evidence that suggests the density profiles of our simulated clusters are compatible with those of the observed X-ray clusters in MOND. As a last test, we computed the relative velocity between pairs of haloes within 10 Mpc and find that pairs with velocities larger than 3000 km s-1, like the bullet cluster, can form without difficulty.
C1 [Angus, G. W.] Univ Cape Town, Astrophys Cosmol & Grav Ctr, ZA-7700 Rondebosch, South Africa.
[Angus, G. W.; Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy.
[Angus, G. W.; Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Angus, GW (reprint author), Univ Cape Town, Astrophys Cosmol & Grav Ctr, Private Bag X3, ZA-7700 Rondebosch, South Africa.
EM angus.gz@gmail.com
FU National Research Foundation of South Africa; NRF; University of Torino;
Regione Piemonte; INFN [PD51]; PRIN-MIUR [2008NEBK003]
FX GWA's research is supported by the National Research Foundation of South
Africa and in particular the NRF special award for Y-rated researchers
is gratefully acknowledged. AD's research is supported by the University
of Torino and Regione Piemonte. Partial support is acknowledged from the
INFN grant PD51 and PRIN-MIUR-2008 grant '2008NEBK003'
'Matter-antimatter asymmetry, dark matter and dark energy in the LHC
era'. We appreciate comments from Silvio Bonometto, Tom Zlosnik, Martin
Feix, Benoit Famaey, Gianfranco Gentile and Kurt van der Heyden.
Finally, we thank the referee for valuable comments that greatly
strengthened the paper.
NR 51
TC 23
Z9 23
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 2
BP 941
EP 949
DI 10.1111/j.1365-2966.2011.19321.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HR
UT WOS:000297043000009
ER
PT J
AU Blondin, S
Kasen, D
Ropke, FK
Kirshner, RP
Mandel, KS
AF Blondin, Stephane
Kasen, Daniel
Roepke, Friedrich K.
Kirshner, Robert P.
Mandel, Kaisey S.
TI Confronting 2D delayed-detonation models with light curves and spectra
of Type Ia supernovae
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: general
ID FAILED DEFLAGRATION MODEL; HIGH-VELOCITY FEATURES; MAXIMUM LIGHT;
THERMONUCLEAR SUPERNOVAE; OPTICAL SPECTROSCOPY; IMPROVED DISTANCES;
EQUIVALENT WIDTHS; SNE-IA; DIVERSITY; EXPLOSION
AB We compare models for Type Ia supernova (SN Ia) light curves and spectra with an extensive set of observations. The models come from a recent survey of 44 two-dimensional delayed-detonation models computed by Kasen et al., each viewed from multiple directions. The data include optical light curves of 251 SNe Ia, some of which have near-infrared observations, and 2231 low-dispersion spectra from the Center for Astrophysics, plus data from the literature. These allow us to compare a wide range of SN Ia models with observations for a wide range of luminosities and decline rates. The analysis uses standard techniques employed by observers, including MLCS2k2, SALT2 and SNooPy for light-curve analysis, and the Supernova Identification (snid) code of Blondin & Tonry for spectroscopic comparisons to assess how well the models match the data. The ability to use the tools developed for observational data directly on the models marks a significant step forward in the realism of the models. We show that the models that match observed spectra best lie systematically on the observed widthluminosity relation. Conversely, we reject six models with highly asymmetric ignition conditions and a large amount (?1 M?) of synthesized 56Ni that yield poor matches to observed SN Ia spectra. More subtle features of the comparison include the general difficulty of the models to match the U-band flux at early times, caused by hot ionized ejecta that affect the subsequent redistribution of flux at longer wavelengths. The models have systematically higher velocities than the observed spectra at maximum light, as inferred from the Si ii ?6355 line. We examine ways in which the asymptotic kinetic energy of the explosion affects both the predicted velocity and velocity gradient in the Si ii and Ca ii lines. Models with an asymmetric distribution of 56Ni are found to result in a larger variation of photometric and spectroscopic properties with viewing angle, regardless of the initial ignition setup. We discuss more generally whether highly anisotropic ignition conditions are ruled out by observations, and how detailed comparisons between models and observations involving both light curves and spectra can lead to a better understanding of SN Ia explosion mechanisms.
C1 [Blondin, Stephane] Univ Aix Marseille, CNRS, CPPM, IN2P3, F-13288 Marseille 9, France.
[Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Kasen, Daniel] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Nucl Sci, Berkeley, CA 94720 USA.
[Roepke, Friedrich K.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Roepke, Friedrich K.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Kirshner, Robert P.; Mandel, Kaisey S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Blondin, S (reprint author), Univ Aix Marseille, CNRS, CPPM, IN2P3, 163 Ave Luminy, F-13288 Marseille 9, France.
EM blondin@cppm.in2p3.fr
OI Ropke, Friedrich/0000-0002-4460-0097
FU DOE [DE-FC02-06ER41438]; ORNL; NERSC; Deutsche Forschungsgemeinschaft
[RO 3676/1-1]; NSF [AST 09-07903]
FX SB acknowledges useful discussions with Luc Dessart, Ryan Foley, Alexei
Khokhlov and Masaomi Tanaka. This research has been supported by the DOE
SciDAC Program (DE-FC02-06ER41438). Computing time was provided by ORNL
through an INCITE award and by NERSC. The work of FKR is supported by
the Deutsche Forschungsgemeinschaft via the Emmy Noether programme (RO
3676/1-1). Support for supernova research at Harvard University,
including the CfA Supernova Archive, is provided in part by NSF grant
AST 09-07903.
NR 91
TC 30
Z9 30
U1 0
U2 2
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 2
BP 1280
EP 1302
DI 10.1111/j.1365-2966.2011.19345.x
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 848HR
UT WOS:000297043000031
ER
PT J
AU Koch, F
Smith, DR
AF Koch, Frank
Smith, David R.
TI A NEW SPECIES OF CALIROA (HYMENOPTERA: TENTHREDINIDAE) FROM SOUTH AFRICA
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Symphyta; Heterarthrinae; Caliroini; Afromontane Region; Limpopo
Province; Mpumalanga Province
AB Caliroa blanki, n. sp., the first native species of Caliroa from the Afrotropical Region, is described from South Africa. Differences in wing venation from usual Caliroa species and provisional placement in Caliroa are discussed. Discussion and records for the invasive Caliroa cerasi (L.) in South Africa are given. A distribution map is provided for both species.
C1 [Koch, Frank] Humboldt Univ, Museum Nat Kunde, Inst Systemat Zool, D-10115 Berlin, Germany.
[Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
RP Koch, F (reprint author), Humboldt Univ, Museum Nat Kunde, Inst Systemat Zool, Invalidenstr 43, D-10115 Berlin, Germany.
EM frank.koch@mfn-berlin.de; dave.smith@ars.usda.gov
FU German Research Foundation [445 SUA-113/8/1-3]; International Bureau of
the Federal Ministry of Education and Research at the Project Management
Agency c/o German Aerospace Center (DLR) [SUA 08/058]
FX We are most grateful to the following for allowing examination of
specimens in their care: C. D. Eardley (PPRI); M. Kruger (TMSA). The
German Research Foundation (445 SUA-113/8/1-3) and the International
Bureau of the Federal Ministry of Education and Research at the Project
Management Agency c/o German Aerospace Center (DLR) (SUA 08/058) are
gratefully acknowledged for providing a research grant. Mike Picker
(ZUCT) provided information on C. cerasi. Michele Touchet, Systematic
Entomology Laboratory, USDA, Washington, DC, helped with images 1-8. We
thank the following for review of the manuscript: H. Goulet, Agriculture
Canada, Ottawa, and A. S. Konstantinov and T. J. Henry, Systematic
Entomology Laboratory, USDA, Washington, DC. USDA is an equal
opportunity provider and employer.
NR 11
TC 0
Z9 0
U1 0
U2 1
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD OCT
PY 2011
VL 113
IS 4
BP 442
EP 450
DI 10.4289/0013-8797.113.4.442
PG 9
WC Entomology
SC Entomology
GA 853QA
UT WOS:000297439600005
ER
PT J
AU Kula, RR
Marsh, PM
AF Kula, Robert R.
Marsh, Paul M.
TI DORYCTINAE (HYMENOPTERA: BRACONIDAE) OF KONZA PRAIRIE EXCLUDING SPECIES
OF HETEROSPILUS HALIDAY
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE biodiversity; conservation; Flint Hills; gallery forest; Great Plains;
Kansas; Nearctic; tallgrass prairie
ID NEARCTIC DORYCTINAE; COLEOPTERA BUPRESTIDAE; NORTH-AMERICA; SPATHIUS
NEES; LELUTHIA
AB The results of a survey of Doryctinae (Hymenoptera: Braconidae), excluding species of Heterospilus Haliday, at Konza Prairie near Manhattan, Kansas are reported. Eleven sites representing prairie and woodland/wetland areas, including gallery forest, were sampled in 2001 and 2005 using Malaise and canopy traps. Topographic trap placement included lowland, midslope, and upland areas. Twenty-four species were collected, including 18 in 2001 and 16 in 2005. Twenty-three of the 24 species were collected from the woodland/wetland sites, including 19 from gallery forest sites; five of the 24 species were collected from the prairie sites. Rhaconotus fasciatus (Ashmead) was the most abundant species in 2001 (n = 13); Callihormius bifasciatus (Ashmead) and Coiba jeffersoni Kula were the most abundant species in 2005 (n = 10). The following new species are described: Doryctes xanthogaster Kula and Marsh, Doryctes xanthosoma Kula and Marsh, Doryctinus zolnerowichi Kula and Marsh, and Pambolidea dollari Kula and Marsh. Glyptocolastes caryae (Ashmead), status revised is removed from synonymy with Glyptocolastes rugulosus (Cresson), the type species for Doryctinus Roman. The latter species is transferred to Acrophasmus Enderlein, resulting in Acrophasmus as a new synonym of Doryctinus. Synonymy of the aforementioned genera results in the following nomenclatural changes: Doryctinus amazonicus (Roman), new combination; Doryctinus arizonensis (Marsh), new combination; Doryctinus atriventris (Cresson), new combination; Doryctinus butleri (Marsh), new combination; Doryctinus costaricensis (Marsh), new combination; Doryctinus erugatus (Marsh), new combination; Doryctinus exilis (Enderlein), new combination; Doryctinus ferrugineus (Marsh), new combination; Doryctinus gauldi (Marsh), new combination; Doryctinus immigrans (Beardsley), new combination; Doryctinus maeandrius (Enderlein), new combination; Doryctinus marshi Greenbaum, revised combination; Doryctinus rubronotum (Marsh), new combination; Doryctinus rugulosus (Cresson), revised combination; Doryctinus scobiciae (Marsh), new combination; and Doryctinus secundus (Muesebeck and Walkley), new combination. Doryctes infuscus Marsh is a new synonym of Doryctes rufipes (Provancher), Pioscelus wichitus (Viereck) is a new synonym of Pioscelus borealis (Ashmead), and Rhaconotus graciliformis (Viereck) is a new synonym of R. fasciatus. The following species are first records for Kansas: C. bifasciatus, Dendrosoter sulcatus Muesebeck, D. rufipes, D. ferrugineus, Ecphylus hypothenemi Ashmead, Ecphylus rohweri Muesebeck, Ontsira mellipes (Ashmead), and Rhaconotus canadensis Marsh.
C1 [Kula, Robert R.] ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
RP Kula, RR (reprint author), ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA.
EM Robert.Kula@ars.usda.gov; swampy@wildblue.net
NR 73
TC 6
Z9 6
U1 0
U2 5
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD OCT
PY 2011
VL 113
IS 4
BP 451
EP 491
DI 10.4289/0013-8797.113.4.451
PG 41
WC Entomology
SC Entomology
GA 853QA
UT WOS:000297439600006
ER
PT J
AU Pogue, MG
AF Pogue, Michael G.
TI USING GENITALIA CHARACTERS AND MITOCHONDRIAL COI SEQUENCES TO PLACE
"LEUCOCHLAENA" HIPPARIS (DRUCE) IN SPODOPTERA GUENEE (LEPIDOPTERA:
NOCTUIDAE)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE DNA barcode region; morphology; taxonomy
ID DNA BARCODES; SKIPPER BUTTERFLIES; GENUS
AB The species "Leucochlaena" hipparis (Druce) belongs in the genus Spodoptera based on morphological characters of the male and female genitalia, as well as maximum parsimony and maximum likelihood analysis of the 658 bp "barcode" region of cytochrome oxidae (COI). Adult and male and female genitalia are illustrated. Cladograms are included to illustrate the placement of "Leucochlaena" hipparis within Spodoptera.
C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, Washington, DC 20013 USA.
RP Pogue, MG (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, POB 37012,MRC 168, Washington, DC 20013 USA.
EM michael.pogue@ars.usda.gov
NR 25
TC 1
Z9 2
U1 0
U2 2
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD OCT
PY 2011
VL 113
IS 4
BP 497
EP 507
DI 10.4289/0013-8797.113.4.497
PG 11
WC Entomology
SC Entomology
GA 853QA
UT WOS:000297439600008
ER
PT J
AU Smith, DR
Tripotin, P
AF Smith, Davto R.
Tripotin, Pierre
TI AULACIDAE (HYMENOPTERA) OF KOREA, WITH NOTES ON THEIR BIOLOGY
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE parasitic wasps; Asia; Cerambycidae; Buprestidae; Xiphydriidae
ID FAMILY AULACIDAE; XIPHYDRIIDAE; EVANIOIDEA
AB Five species of Aulacidae are recorded from Korea: Aulacus salicius Sun and Sheng, 2007, Pristaulacus insularis Konishi, 1990, Pristaulacus intermedius Uchida, 1932, Pristaulacus kostylevi Alekseev,1986, and Pristaulacus jirisani Smith and Tripotin, new species. All except P intermedius represent new country records. A key to species and a diagnosis of each species are provided. Collection notes are given for each species, indicating that Xiphydria palaeanarctica Semenov (Hymenoptera: Xiphydriidae) is the host for A. salicius, and Cerambycidae and possibly Buprestidae (Coleoptera) are the hosts for the Pristaulacus species.
C1 [Smith, Davto R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA.
EM dave.smith@ars.usda.gov; p_tripotin@hotmail.com
NR 12
TC 1
Z9 3
U1 0
U2 1
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD OCT
PY 2011
VL 113
IS 4
BP 519
EP 530
DI 10.4289/0013-8797.113.4.519
PG 12
WC Entomology
SC Entomology
GA 853QA
UT WOS:000297439600010
ER
PT J
AU Rowcliffe, JM
Carbone, C
Jansen, PA
Kays, R
Kranstauber, B
AF Rowcliffe, J. Marcus
Carbone, Chris
Jansen, Patrick A.
Kays, Roland
Kranstauber, Bart
TI Quantifying the sensitivity of camera traps: an adapted distance
sampling approach
SO METHODS IN ECOLOGY AND EVOLUTION
LA English
DT Article
DE abundance estimation; animal density; camera detection zone; detection
probability; passive infrared motion sensor; Random Encounter Model
ID NEOTROPICAL FORESTS; PHOTOGRAPHIC RATES; ESTIMATE DENSITIES; CRYPTIC
MAMMALS; POPULATION; TIGERS; LANDSCAPE; DESIGN; BIRDS
AB 1. Abundance estimation is a pervasive goal in ecology. The rate of detection by motion-sensitive camera traps can, in principle, provide information on the abundance of many species of terrestrial vertebrates that are otherwise difficult to survey. The random encounter model (REM, Rowcliffe 2008) provides a means estimating abundance from camera trap rate but requires camera sensitivity to be quantified.
2. Here, we develop a method to estimate the area effectively monitored by cameras, which is one of the most important codeterminants of detection rate. Our method borrows from distance sampling theory, applying detection function models to data on the position (distance and angle relative to the camera) where the animals are first detected. Testing the reliability of this approach through simulation, we find that bias depends on the effective detection angle assumed but was generally low at less than 5% for realistic angles typical of camera traps.
3. We adapted standard detection functions to allow for the possibility of smaller animals passing beneath the field of view close to the camera, resulting in reduced detection probability within that zone. Using a further simulation to test this approach, we find that detection distance can be estimated with little or no bias if detection probability is certain for at least some distance from the camera.
4. Applying this method to a 1-year camera trapping data set from Barro Colorado Island, Panama, we show that effective detection distance is related strongly positively to species body mass and weakly negatively to species average speed of movement. There was also a strong seasonal effect, with shorter detection distance during the wet season. Effective detection angle is related more weakly to species body mass, and again strongly to season, with a wider angle in the wet season.
5. This method represents an important step towards practical application of the REM, including abundance estimation for relatively small (< 1 kg) species.
C1 [Rowcliffe, J. Marcus; Carbone, Chris] ZSL Inst Zool, London NW1 4RY, England.
[Jansen, Patrick A.; Kays, Roland] Smithsonian Trop Res Inst, Balboa, Panama.
[Jansen, Patrick A.] Wageningen Univ, Ctr Ecosyst Studies, Wageningen, Netherlands.
[Kays, Roland] New York State Museum & Sci Serv, Albany, NY USA.
[Kranstauber, Bart] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany.
RP Rowcliffe, JM (reprint author), ZSL Inst Zool, Regents Pk, London NW1 4RY, England.
EM marcus.rowcliffe@ioz.ac.uk
RI Jansen, Patrick/G-2545-2015
OI Jansen, Patrick/0000-0002-4660-0314
FU NSF [DEB 0717071]; British Ecological Society; Netherlands Foundation of
Scientific Research [NWO-ALW863-07-008]
FX We thank Nadia Sitas, Anthony Turner, Daniel Rasmussen and Lennart
Suselbeek for assistance in the field and the Smithsonian Tropical
Research Institute, especially Oris Acevedo, for general logistical
support. Required permits for the work described in this paper were
obtained from the Autoridad Nacional del Ambiente, Panama, and the
Smithsonian Tropical Research Institute. We are indebted to three
referees for their insightful and supportive comments, in particular
Steve Buckland. The work was funded by NSF (DEB 0717071) and the British
Ecological Society. PAJ was funded by the Netherlands Foundation of
Scientific Research (NWO-ALW863-07-008).
NR 29
TC 33
Z9 39
U1 9
U2 118
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2041-210X
J9 METHODS ECOL EVOL
JI Methods Ecol. Evol.
PD OCT
PY 2011
VL 2
IS 5
BP 464
EP 476
DI 10.1111/j.2041-210X.2011.00094.x
PG 13
WC Ecology
SC Environmental Sciences & Ecology
GA 852CI
UT WOS:000297323700005
ER
PT J
AU Piperno, DR
AF Piperno, Dolores R.
TI The Origins of Plant Cultivation and Domestication in the New World
Tropics Patterns, Process, and New Developments
SO CURRENT ANTHROPOLOGY
LA English
DT Article
ID BALSAS RIVER VALLEY; REAL-ALTO SITE; STARCH GRAINS; NORTHERN PERU;
AGRICULTURAL ORIGINS; MANIHOT-ESCULENTA; PHYLOGENETIC-RELATIONSHIPS;
TERMINAL PLEISTOCENE; BEHAVIORAL ECOLOGY; PHYTOLITH EVIDENCE
AB The New World tropical forest is now considered to be an early and independent cradle of agriculture. As in other areas of the world, our understanding of this issue has been significantly advanced by a steady stream of archaeobotanical, paleoecological, and molecular/genetic data. Also importantly, a renewed focus on formulating testable theories and explanations for the transition from foraging to food production has led to applications from subdisciplines of ecology, economy, and evolution not previously applied to agricultural origins. Most recently, the integration of formerly separated disciplines, such as developmental and evolutionary biology, is causing reconsiderations of how novel phenotypes, including domesticated species, originate and the influence of artificial selection on the domestication process. It is becoming clear that the more interesting question may be the origins of plant cultivation rather than the origins of agriculture. This paper reviews this body of evidence and assesses current views about how and why domestication and plant food production arose.
C1 Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeol, Washington, DC 20560 USA.
RP Piperno, DR (reprint author), Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeol, 10th St & Constitut Ave, Washington, DC 20560 USA.
EM pipernod@si.edu
NR 121
TC 46
Z9 47
U1 8
U2 62
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0011-3204
J9 CURR ANTHROPOL
JI Curr. Anthropol.
PD OCT
PY 2011
VL 52
SU 4
BP S453
EP S470
DI 10.1086/659998
PG 18
WC Anthropology
SC Anthropology
GA 842NO
UT WOS:000296606400019
ER
PT J
AU Smith, BD
AF Smith, Bruce D.
TI The Cultural Context of Plant Domestication in Eastern North America
SO CURRENT ANTHROPOLOGY
LA English
DT Article
ID MISSISSIPPI RIVER VALLEY; NICHE CONSTRUCTION; MIDDLE TENNESSEE; DATES;
FIBS; SITE; BP
AB The timing and sequence of the independent domestication of indigenous eastern North American seed plants (Cucurbita pepo, Helianthus annuus, Iva annua, Chenopodium berlandieri) and the subsequent development of a crop complex are discussed within a broader environmental and cultural context. The settlements that have yielded the earliest record of eastern domesticates are all small and situated in resource-rich lower-order river valley corridors within oak-savannah and oak-hickory forest regions. Well-preserved floral and faunal assemblages indicate continued substantial reliance on a wide range of wild species with no evidence of resource depletion. Similarly, there is no indication of landscape packing in terms of high site density in these resource-rich river valleys, calling into question developmental models of domestication and agricultural origins that rely on population pressure or resource imbalance as causal factors.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA.
RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012, Washington, DC 20013 USA.
EM smithb@si.edu
NR 62
TC 15
Z9 15
U1 8
U2 31
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0011-3204
J9 CURR ANTHROPOL
JI Curr. Anthropol.
PD OCT
PY 2011
VL 52
SU 4
BP S471
EP S484
DI 10.1086/659645
PG 14
WC Anthropology
SC Anthropology
GA 842NO
UT WOS:000296606400020
ER
PT J
AU Zeder, MA
AF Zeder, Melinda A.
TI The Origins of Agriculture in the Near East
SO CURRENT ANTHROPOLOGY
LA English
DT Article
ID MITOCHONDRIAL-DNA ANALYSIS; BARLEY HORDEUM-VULGARE; DOMESTIC GOATS;
PHYLOGEOGRAPHIC STRUCTURE; CATTLE DOMESTICATION; ANIMAL DOMESTICATION;
WHEAT DOMESTICATION; NICHE CONSTRUCTION; TETRAPLOID WHEATS; PIG
DOMESTICATION
AB The emerging picture of plant and animal domestication and agricultural origins in the Near East is dramatically different from that drawn 16 years ago in a landmark article by Bar-Yosef and Meadow. While in 1995 there appeared to have been at least a 1,500-year gap between plant and animal domestication, it now seems that both occurred at roughly the same time, with initial management of morphologically wild future plant and animal domesticates reaching back to at least 11,500 cal BP, if not earlier. A focus on the southern Levant as the core area for crop domestication and diffusion has been replaced by a more pluralistic view that sees domestication of various crops and livestock occurring, sometimes multiple times in the same species, across the entire region. Morphological change can no longer be held to be a leading-edge indicator of domestication. Instead, it appears that a long period of increasingly intensive human management preceded the manifestation of archaeologically detectable morphological change in managed crops and livestock. Agriculture in the Near East arose in the context of broad-based systematic human efforts at modifying local environments and biotic communities to encourage plant and animal resources of economic interest. This process took place across the entire Fertile Crescent during a period of dramatic post-Pleistocene climate and environmental change with considerable regional variation in the scope and intensity of these activities as well as in the range of resources being manipulated.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA.
RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, MRC 112, Washington, DC 20013 USA.
EM zederm@si.edu
NR 115
TC 82
Z9 82
U1 9
U2 83
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0011-3204
J9 CURR ANTHROPOL
JI Curr. Anthropol.
PD OCT
PY 2011
VL 52
SU 4
BP S221
EP S235
DI 10.1086/659307
PG 15
WC Anthropology
SC Anthropology
GA 842NO
UT WOS:000296606400006
ER
PT J
AU Soon, W
Dutta, K
Legates, DR
Velasco, V
Zhang, WJ
AF Soon, Willie
Dutta, Koushik
Legates, David R.
Velasco, Victor
Zhang, WeiJia
TI Variation in surface air temperature of China during the 20th century
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Total solar irradiance; Sunshine duration; Surface air temperature;
Circum-global teleconnection
ID ASIAN SUMMER MONSOON; NORTH-ATLANTIC OSCILLATION; SOLAR-RADIATION
CHANGES; YANGTZE-RIVER VALLEY; LONG-TERM TREND; ATMOSPHERIC CIRCULATION;
SUNSHINE DURATION; UNITED-STATES; TELECONNECTION PATTERNS; CLIMATE
VARIABILITY
AB The 20th century surface air temperature (SAT) records of China from various sources are analyzed using data which include the recently released Twentieth Century Reanalysis Project dataset. Two key features of the Chinese records are confirmed: (1) significant 1920s and 1940s warming in the temperature records, and (2) evidence for a persistent multidecadal modulation of the Chinese surface temperature records in co-variations with both incoming solar radiation at the top of the atmosphere as well as the modulated solar radiation reaching ground surface. New evidence is presented for this Sun-climate link for the instrumental record from 1880 to 2002. Additionally, two non-local physical aspects of solar radiation-induced modulation of the Chinese SAT record are documented and discussed.
Teleconnections that provide a persistent and systematic modulation of the temperature response of the Tibetan Plateau and/or the tropospheric air column above the Eurasian continent (e.g., 30 degrees N-70 degrees N; 0 degrees-120 degrees E) are described. These teleconnections may originate from the solar irradiance-Arctic-North Atlantic overturning circulation mechanism proposed by Soon (2009). Also considered is the modulation of large-scale land-sea thermal contrasts both in terms of meridional and zonal gradients between the subtropical western Pacific and mid-latitude North Pacific and the continental landmass of China. The Circum-global teleconnection (CGT) pattern of summer circulation of Ding and Wang (2005) provides a physical framework for study of the Sun-climate connection over East Asia. Our results highlight the importance of solar radiation reaching the ground and the concomitant importance of changes in atmospheric transparency or cloudiness or both in motivating a true physical explanation of any Sun-climate connection. We conclude that ground surface solar radiation is an important modulating factor for Chinese SAT changes on multidecadal to centennial timescales. Therefore, a comprehensive view of local and remote factors of climate change in China must take account of this as well as other natural and anthropogenic forcings. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dutta, Koushik] Univ Minnesota, Large Lakes Observ, Duluth, MN 55812 USA.
[Legates, David R.] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA.
[Velasco, Victor] Univ Nacl Autonoma Mexico, Inst Geofis, Dept Invest Solares & Planetarias, Mexico City 04510, DF, Mexico.
[Zhang, WeiJia] Peking Univ, Dept Phys, Beijing 100871, Peoples R China.
RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM wsoon@cfa.harvard.edu
RI Dutta, Koushik/F-9371-2010;
OI Dutta, Koushik/0000-0002-5976-7965; Velasco, Victor/0000-0002-0100-8878
NR 163
TC 19
Z9 21
U1 3
U2 26
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
EI 1879-1824
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD OCT
PY 2011
VL 73
IS 16
BP 2331
EP 2344
DI 10.1016/j.jastp.2011.07.007
PG 14
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 849QY
UT WOS:000297141400008
ER
PT J
AU Diaferio, A
Ostorero, L
Cardone, V
AF Diaferio, Antonaldo
Ostorero, Luisa
Cardone, Vincenzo
TI Gamma-ray bursts as cosmological probes: Lambda CDM vs. conformal
gravity
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE modified gravity; gamma ray burst experiments; dark energy experiments;
supernova type Ia - standard candles
ID GALACTIC ROTATION CURVES; BAYES FACTORS; STANDARD CANDLES; MODEL
SELECTION; DARK ENERGY; COSMIC ACCELERATION; HUBBLE DIAGRAM; IA
SUPERNOVAE; LUMINOSITY; CONSTANT
AB Lambda CDM, for the currently preferred cosmological density Omega(0) and cosmological constant Omega(Lambda), predicts that the Universe expansion decelerates from early times to redshift z approximate to 0.9 and accelerates at later times. On the contrary, the cosmological model based on conformal gravity predicts that the cosmic expansion has always been accelerating. To distinguish between these two very different cosmologies, we resort to gamma-ray bursts (GRBs), which have been suggested to probe the Universe expansion history at z > 1, where identified type Ia supernovae (SNe) are rare. We use the full Bayesian approach to infer the cosmological parameters and the additional parameters required to describe the GRB data available in the literature. For the first time, we use GRBs as cosmological probes without any prior information from other data. In addition, when we combine the GRB samples with SNe, our approach neatly avoids all the inconsistencies of most numerous previous methods that are plagued by the so-called circularity problem. In fact, when analyzed properly, current data are consistent with distance moduli of GRBs and SNe that can respectively be, in a variant of conformal gravity, similar to 15 and similar to 3 magnitudes fainter than in Lambda CDM. Our results indicate that the currently available SN and GRB samples are accommodated equally well by both Lambda CDM and conformal gravity and do not exclude a continuous accelerated expansion. We conclude that GRBs are currently far from being effective cosmological probes, as they are unable to distinguish between these two very different expansion histories.
C1 [Diaferio, Antonaldo; Ostorero, Luisa] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy.
[Diaferio, Antonaldo; Ostorero, Luisa] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Diaferio, Antonaldo; Ostorero, Luisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ostorero, Luisa] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Ostorero, Luisa; Cardone, Vincenzo] Osserv Astron Roma, INAF, I-00040 Rome, Italy.
RP Diaferio, A (reprint author), Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Via P Giuria 1, I-10125 Turin, Italy.
EM diaferio@ph.unito.it; ostorero@ph.unito.it; winnyenodrac@gmail.com
FU INFN [PD51]; PRIN-MIUR [2008NR3EBK_003]; L'OREAL-UNESCO; ASI [I/016/07/0
COFIS]
FX We sincerely thank Johannes Buchner and Michael Gruberbauer for
developing their superb code APEMoST and making it available to the
community (apemost.sourceforge.net). We also are particularly grateful
to Johannes Buchner and Stefano Andreon for intense and enlightening
correspondence on Bayesian statistics. Stefano Andreon is also
acknoweldged for a very stimulating seminar, delivered in Torino, on
Bayesian statistics applied to astrophysics that inspired this work. We
finally thank Margaret Geller, Xiao-Li Meng and the JCAP Editor, Carl
Akerlof, for valuable suggestions on the presentation of our results.
Support from the INFN grant PD51 and the PRIN-MIUR-2008 grant
2008NR3EBK_003 "Matter-antimatter asymmetry, dark matter and dark energy
in the LHC era" is gratefully acknowledged. LO also acknowledges support
from a 2009 National Fellowship "L'OREAL Italia Per le Donne e la
Scienza" of the L'OREAL-UNESCO program "For Women in Science" and
partial support from the ASI Contract No. I/016/07/0 COFIS. This
research has made use of NASA's Astrophysics Data System.
NR 87
TC 9
Z9 9
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD OCT
PY 2011
IS 10
AR 008
DI 10.1088/1475-7516/2011/10/008
PG 31
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 844SM
UT WOS:000296767600008
ER
PT J
AU Xie, L
Wen, J
Li, LQ
AF Xie, Lei
Wen, Jun
Li, Liang-Qian
TI Phylogenetic Analyses of Clematis (Ranunculaceae) based on Sequences of
Nuclear Ribosomal ITS and Three Plastid Regions
SO SYSTEMATIC BOTANY
LA English
DT Article
DE Clematis; divergence times; molecular phylogeny; Ranunculaceae; species
radiation
ID INDIAN-OCEAN BASIN; TIBETAN PLATEAU; POLYSCIAS ARALIACEAE;
NORTHERN-HEMISPHERE; VASCULAR ANATOMY; DNA-SEQUENCES; BIOGEOGRAPHY;
EVOLUTION; GENUS; CHLOROPLAST
AB Clematis, a largely temperate genus of vines and lianas, consists of approximately 300 species. Based on a sampling of about 75 species, sequences of the nrITS, the plastid atpB-rbcL spacer, psbA-trnH-trnQ spacer, and rpoB-trnC spacer regions were analyzed using parsimony, maximum likelihood, and Bayesian inference methods. Analyses of the combined data set by the three methods yielded similar topologies. Previously recognized genera including Archiclematis and Naravelia are nested within Clematis, supporting the merging of these genera within Clematis. Ten major clades with various levels of support were detected in the combined analyses. Our results in general do not support previous infrageneric classifications based on morphological characters and suggest significant convergence in floral and vegetative characters in Clematis. Several clades were resolved as regional geographic groups. Bayesian dating suggests a relatively ancient origin of the genus in the Oligocene, yet a relatively recent species radiation of the crown Clematis in the Miocene. Geologic and climatic changes in the late Tertiary to Quaternary are perhaps important for the speciation of Clematis, especially in eastern Asia. Long-distance dispersal of the fruits by wind, water, and/or animals and strong environmental adaptability, are proposed as the main mechanisms for the current cosmopolitan distribution and high species diversity of Clematis.
C1 [Xie, Lei; Wen, Jun; Li, Liang-Qian] Chinese Acad Sci, State Key Lab Systemat & Evolutionary Bot, Inst Bot, Beijing 100093, Peoples R China.
[Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Wen, J (reprint author), Chinese Acad Sci, State Key Lab Systemat & Evolutionary Bot, Inst Bot, Beijing 100093, Peoples R China.
EM wenj@si.edu; lqli@ibcas.ac.cn
FU John D. and Catherine T. MacArthur Foundation; National Natural Science
Foundation of China [30870146]; National Museum of Natural History;
Smithsonian Institution
FX We are grateful to Prof. Wang Wen-Tsai for identifying specimens and for
his invaluable comments on the manuscript. We thank S. Manchester and C.
Anderson for discussions of fossil records and calibration methods. This
study was supported by the John D. and Catherine T. MacArthur Foundation
(to J. Wen, R. Ree, and G. Mueller), the National Natural Science
Foundation of China, Grant No. 30870146, the small grants of the
National Museum of Natural History, and the endowment grants of the
Smithsonian Institution. Laboratory work was conducted in the Laboratory
of Analytical Biology of the National Museum of Natural History of the
Smithsonian Institution. We are grateful to Elvira Horandl, Lawrence
Janeway, and Quentin Luke for their kind assistance collecting tissue
samples.
NR 117
TC 18
Z9 20
U1 3
U2 25
PU AMER SOC PLANT TAXONOMISTS
PI LARAMIE
PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071
USA
SN 0363-6445
EI 1548-2324
J9 SYST BOT
JI Syst. Bot.
PD OCT-DEC
PY 2011
VL 36
IS 4
BP 907
EP 921
DI 10.1600/036364411X604921
PG 15
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 850GK
UT WOS:000297182900010
ER
PT J
AU Smith, BC
AF Smith, Barbara Clark
TI Beyond the "Economic"
SO WILLIAM AND MARY QUARTERLY
LA English
DT Article
C1 Smithsonian Inst, Natl Museum Amer Hist, Div Polit Hist, Washington, DC 20560 USA.
RP Smith, BC (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Div Polit Hist, Washington, DC 20560 USA.
NR 6
TC 1
Z9 1
U1 0
U2 0
PU INST EARLY AMER HIST CULT
PI WILLIAMSBURG
PA BOX 220, WILLIAMSBURG, VA 23187 USA
SN 0043-5597
J9 WILLIAM MARY QUART
JI William Mary Q.
PD OCT
PY 2011
VL 68
IS 4
BP 639
EP 643
DI 10.5309/willmaryquar.68.4.0639
PG 5
WC History
SC History
GA 847QN
UT WOS:000296987700009
ER
PT J
AU Wendler, I
Huber, BT
MacLeod, KG
Wendler, JE
AF Wendler, Ines
Huber, Brian T.
MacLeod, Kenneth G.
Wendler, Jens E.
TI EARLY EVOLUTIONARY HISTORY OF TUBULOGENERINA AND COLOMIA, WITH NEW
SPECIES FROM THE TURONIAN OF EAST AFRICA
SO JOURNAL OF FORAMINIFERAL RESEARCH
LA English
DT Article
ID CARBON ISOTOPIC FRACTIONATION; LIVE BENTHIC FORAMINIFERA; SEDIMENTS
AB Two new species, Tuhulogeneriaa turonica and Colomia africana, are described from the Turonian of Tanzania, and the genus Colomia is emended. The genus Tubulogenerina was originally thought to have originated in Europe in the early Eocene. Our discovery of T. turorrica indicates that the roots of the genus reach back to the middle Cretaceous, and argues against a previous conclusion that it originated in temperate European regions. A tropical/subtropical site of origination would be consistent with the observation that most Tuba logo:cram species inhabited warm, shallow-water environments. Tubulogenerina turonica has a relatively simple morphology, suitable as a starting point for morphological trends in the genus during the Cenozoic, thus supporting its status as a plausible ancestral species.
In clay-rich middle Cretaceous sediments from Tanzania, foraminifera are exceptionally well preserved, and assemblages include a number of aragonitic taxa, including Colomia africana. This new species is distinguished from others of the genus by its aperture and toothplate structure and its dominantly biserial test without a well-developed uniserial growth stage. Morphologic similarities, however, indicate the close evolutionary relationship with other species of Colomia, so the genus is emended accordingly. Sufficient numbers of C. africana were found in multiple samples to characterize its stable carbon and oxygen isotope values relative to another aragonitic species (Epistomina chapmani) and calcitic species (Bertthelina berthelini) from the same material. Results show an expected offset between calcitic and aragonitic tests that is partially explained by differential fractionation factors, but suggests vital or microhabitat effects contribute to values measured on C. africana.
C1 [Wendler, Ines; Wendler, Jens E.] Univ Bremen, Dept Geol Sci, D-28334 Bremen, Germany.
[Wendler, Ines; Huber, Brian T.; Wendler, Jens E.] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[MacLeod, Kenneth G.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA.
RP Wendler, I (reprint author), Univ Bremen, Dept Geol Sci, POB 330 440, D-28334 Bremen, Germany.
EM flatter@uni-bremen.de
RI MacLeod, Kenneth/C-4042-2017
OI MacLeod, Kenneth/0000-0002-6016-0837
FU Smithsonian Natural History Research Experiences Program; National
Science Foundation [EAR 0642993]; Smithsonian Walcott Fund and
Scholoarly Studies grants
FX This paper benefitted from helpful comments and suggestions from Laia
Alegret and an anonymous reviewer. We also thank Ken Finger and Mimi
Katz for their editorial suggestions. The authors are very grateful for
the assistance of Sarah Ehlinger, Carlos Rodriguez-Russo, Shannon
Haynes, Carlos Peredo, and Joshua Johnson with foraminifer picking, we
thank Erin Jacobs for her help with digital image editing, and we
acknowledge the support of summer student internships from the
Smithsonian Natural History Research Experiences Program. We also thank
Tim Rose and the Smithsonian's Department of Mineral Sciences for access
to their cathodoluminescene microscope. Fieldwork, drilling, and
laboratory expenses were funded by a National Science Foundation grant
to National Science Foundation grant to BTH and KGM (EAR 0642993) and
Smithsonian Walcott Fund and Scholoarly Studies grants to BTH.
NR 22
TC 10
Z9 11
U1 0
U2 3
PU CUSHMAN FOUNDATION FORAMINIFERAL RES
PI CAMBRIDGE
PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST,
HARVARD UNIV, CAMBRIDGE, MA 02138 USA
SN 0096-1191
J9 J FORAMIN RES
JI J. Foraminifer. Res.
PD OCT
PY 2011
VL 41
IS 4
BP 384
EP 400
PG 17
WC Paleontology
SC Paleontology
GA 847AB
UT WOS:000296943200007
ER
PT J
AU Thompson, JR
Foster, DR
Scheller, R
Kittredge, D
AF Thompson, Jonathan R.
Foster, David R.
Scheller, Robert
Kittredge, David
TI The influence of land use and climate change on forest biomass and
composition in Massachusetts, USA
SO ECOLOGICAL APPLICATIONS
LA English
DT Article
DE aboveground biomass; climate change; current trends; forest carbon
sequestration; future scenarios; Massachusetts; USA; landscape inertia;
landscape simulation; land use legacies; old-growth forest
ID NORTHEASTERN NORTH-AMERICA; LANDSCAPE SIMULATION-MODEL; EASTERN
UNITED-STATES; NEW-ENGLAND; ABOVEGROUND BIOMASS; CANOPY NITROGEN; CARBON
STORAGE; WATER YIELD; USE HISTORY; MANAGEMENT
AB Land use and climate change have complex and interacting effects on naturally dynamic forest landscapes. To anticipate and adapt to these changes, it is necessary to understand their individual and aggregate impacts on forest growth and composition. We conducted a simulation experiment to evaluate regional forest change in Massachusetts, USA over the next 50 years (2010-2060). Our objective was to estimate, assuming a linear continuation of recent trends, the relative and interactive influence of continued growth and succession, climate change, forest conversion to developed uses, and timber harvest on live aboveground biomass (AGB) and tree species composition. We examined 20 years of land use records in relation to social and biophysical explanatory variables and used regression trees to create "probability-of-conversion" and "probability-of-harvest" zones. We incorporated this information into a spatially interactive forest landscape simulator to examine forest dynamics as they were affected by land use and climate change. We conducted simulations in a full-factorial design and found that continued forest growth and succession had the largest effect on AGB, increasing stores from 181.83 Tg to 309.56 Tg over 50 years. The increase varied from 49% to 112% depending on the ecoregion within the state. Compared to simulations with no climate or land use, forest conversion reduced gains in AGB by 23.18 Tg (or 18%) over 50 years. Timber harvests reduced gains in AGB by 5.23 Tg (4%). Climate change (temperature and precipitation) increased gains in AGB by 17.3 Tg (13.5%). Pinus strobus and Acer rubrum were ranked first and second, respectively, in terms of total AGB throughout all simulations. Climate change reinforced the dominance of those two species. Timber harvest reduced Quercus rubra from 10.8% to 9.4% of total AGB, but otherwise had little effect on composition. Forest conversion was generally indiscriminate in terms of species removal. Under the naive assumption that future land use patterns will resemble the recent past, we conclude that continued forest growth and recovery will be the dominant mechanism driving forest dynamics over the next 50 years, and that while climate change may enhance growth rates, this will be more than offset by land use, primarily forest conversion to developed uses.
C1 [Thompson, Jonathan R.] Smithsonian Conservat Biol Inst, Smithsonian Inst, Front Royal, VA 22630 USA.
[Thompson, Jonathan R.; Foster, David R.; Kittredge, David] Harvard Univ, Petersham, MA 01366 USA.
[Scheller, Robert] Portland State Univ, Portland, OR 97207 USA.
[Kittredge, David] Univ Massachusetts, Dept Nat Resource Conservat, Amherst, MA 01003 USA.
RP Thompson, JR (reprint author), Smithsonian Conservat Biol Inst, Smithsonian Inst, 1500 Remount Rd, Front Royal, VA 22630 USA.
EM thompsonjr@si.edu
RI Scheller, Robert/B-3135-2009
FU NSF [DEB-9411975]
FX We thank Dunbar Carpenter for technical help. Funding for this research
was provided by NSF Grant DEB-9411975 to the Harvard Forest, Long Term
Ecological Research (LTER) program.
NR 95
TC 48
Z9 50
U1 9
U2 79
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1051-0761
J9 ECOL APPL
JI Ecol. Appl.
PD OCT
PY 2011
VL 21
IS 7
BP 2425
EP 2444
PG 20
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 836UP
UT WOS:000296139200007
PM 22073633
ER
PT J
AU Blakeslee, AMH
Canning-Clode, J
Lind, EM
Quilez-Badia, G
AF Blakeslee, April M. H.
Canning-Clode, Joao
Lind, Eric M.
Quilez-Badia, Gemma
TI Biological invasions in the 21st century: Ecological impacts,
predictions, and management across land and sea Introduction
SO ENVIRONMENTAL RESEARCH
LA English
DT Editorial Material
C1 [Blakeslee, April M. H.] Long Isl Univ, Dept Biol, Brookville, NY USA.
[Blakeslee, April M. H.; Canning-Clode, Joao; Lind, Eric M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Canning-Clode, Joao] CIMAR CIIMAR Ctr Marine & Environm Res, Oporto, Portugal.
[Lind, Eric M.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA.
[Quilez-Badia, Gemma] World Wildlife Fund Nat Mediterranean Program Off, Barcelona, Spain.
RP Blakeslee, AMH (reprint author), Long Isl Univ, Dept Biol, CW Post Campus, Brookville, NY USA.
EM April.Blakeslee@liu.edu
RI Canning Clode, Joao/G-5142-2011; Scientific output, CIIMAR/E-5122-2012
OI Canning Clode, Joao/0000-0003-2143-6535; Scientific output,
CIIMAR/0000-0001-6270-2153
NR 6
TC 0
Z9 0
U1 0
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0013-9351
J9 ENVIRON RES
JI Environ. Res.
PD OCT
PY 2011
VL 111
IS 7
SI SI
BP 891
EP 892
DI 10.1016/j.envres.2011.09.005
PG 2
WC Environmental Sciences; Public, Environmental & Occupational Health
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health
GA 830LY
UT WOS:000295659700001
PM 21958957
ER
PT J
AU McKenzie, LA
Brooks, R
Johnston, EL
AF McKenzie, Louise A.
Brooks, Rob
Johnston, Emma L.
TI Heritable pollution tolerance in a marine invader
SO ENVIRONMENTAL RESEARCH
LA English
DT Article
DE Non-indigenous species; Copper; Offspring size; Maternal provisioning;
Heavy metal pollution
ID POLYCHAETE NEREIS-DIVERSICOLOR; ECOLOGICAL TIME-SCALES; LIFE-HISTORY;
HEAVY-METALS; WATERSIPORA-SUBTORQUATA; CONTAMINATED ESTUARIES;
DIFFERENTIAL TOLERANCE; PHENOTYPIC PLASTICITY; ANTIFOULING PAINT; RAPID
EVOLUTION
AB The global spread of fouling invasive species is continuing despite the use of antifouling biocides. Furthermore, previous evidence suggests that non-indigenous species introduced via hull fouling may be capable of adapting to metal-polluted environments. Using a laboratory based toxicity assay, we investigated tolerance to copper in the non-indigenous bryozoan Watersipora subtorquata from four source populations. Individual colonies were collected from four sites within Port Hacking (Sydney, Australia) and their offspring exposed to a range of copper concentrations. This approach, using a fullsib, split-family design, tests for a genotype by environment (G x E) interaction. Settlement and complete metamorphosis (recruitment) were measured as ecologically relevant endpoints. Larval sizes were also measured for each colony. Successful recruitment was significantly reduced by the highest copper concentration of 80 mu g L(-1). While there was no difference in pollution tolerance between sites, there was a significant G x E interaction, with large variation in the response of colony offspring within sites. Larval size differed significantly both between sites and between colonies and was positively correlated with tolerance. The high level of variation in copper tolerance between colonies suggests that there is considerable potential within populations to adapt to elevated copper levels, as tolerance is a heritable trait. Also, colonies that produce large larvae are more tolerant to copper, suggesting that tolerance may be a direct consequence of larger size. (C) 2011 Elsevier Inc. All rights reserved.
C1 Univ New S Wales, Evolut & Ecol Res Ctr, Sydney, NSW 2052, Australia.
Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia.
RP McKenzie, LA (reprint author), Smithsonian Environm Res Ctr, Marine Invas Lab, POB 28, Edgewater, MD 21037 USA.
EM mckenziel@si.edu.au; rob.brooks@unsw.edu.au; e.johnston@unsw.edu.au
RI Brooks, Robert/A-1251-2008; Johnston, Emma/B-7210-2009
OI Brooks, Robert/0000-0001-6926-0781; Johnston, Emma/0000-0002-2117-366X
FU Australian Government; Australian Research Council
FX We are grateful to Subtidal Ecology and Ecotoxicology laboratory members
for assistance in the field. The authors were supported by the
Australian Government and Australian Research Council through Research
Fellowships, Postgraduate Awards and Grants. We thank Alistair Poore for
comments which improved earlier draughts of this article.
NR 83
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U1 1
U2 48
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0013-9351
J9 ENVIRON RES
JI Environ. Res.
PD OCT
PY 2011
VL 111
IS 7
SI SI
BP 926
EP 932
DI 10.1016/j.envres.2010.12.007
PG 7
WC Environmental Sciences; Public, Environmental & Occupational Health
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health
GA 830LY
UT WOS:000295659700006
PM 21295292
ER
PT J
AU Bisson, IA
Butler, LK
Hayden, TJ
Kelley, P
Adelman, JS
Romero, LM
Wikelski, MC
AF Bisson, I. -A.
Butler, L. K.
Hayden, T. J.
Kelley, P.
Adelman, J. S.
Romero, L. M.
Wikelski, M. C.
TI Energetic response to human disturbance in an endangered songbird
SO ANIMAL CONSERVATION
LA English
DT Article
DE human disturbance; heart rate telemetry; energy expenditure; endangered
songbirds; fast life histories; vireo
ID HEART-RATE; ADRENOCORTICAL RESPONSES; STRESS-RESPONSE; EXPENDITURE;
PENGUINS; BEHAVIOR; BIRDS; REPRODUCTION; METABOLISM; TELEMETRY
AB Physiological changes in response to environmental stressors can reveal cryptic effects of disturbance that can potentially lead to species decline. However, such responses may vary with life history. We used heart rate telemetry to continuously and instantaneously measure energy expenditure in response to human-mediated disturbance in a free-living breeding population of the endangered [International Union for Conservation of Nature, vulnerable] black-capped vireo Vireo atricapilla (n = 10). Heart rate predicted 84% of energy expenditure as determined by respirometry (n = 3). Each bird mounted with a 0.5 g heart rate transmitter were subjected to standardized disturbance trials for 1 or 4 h during the day, and for 1 h at night. Only 1-h daytime disturbances elicited an increase in heart rate but this was not significant when compared with control no-disturbance periods. Our findings suggest that black-capped vireos quickly acclimate to a limited amount of human disturbance during the breeding season, which may be an adaptive response for any 'fast-living' species with a short life span and a short and synchronized breeding season. Because similar results were reported for another fast-living species, the common white-eyed vireo Vireo griseus, we suggest that life-history traits are stronger predictors of short-term physiological responses to disturbances than population status.
C1 [Bisson, I. -A.; Adelman, J. S.; Wikelski, M. C.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA.
[Butler, L. K.; Romero, L. M.] Tufts Univ, Dept Biol, Medford, MA 02155 USA.
[Hayden, T. J.] Engineer Res & Dev Ctr, Champaign, IL USA.
[Kelley, P.] Severn Elect, Annapolis, MD USA.
RP Bisson, IA (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, POB 37102,MRC 5503, Washington, DC 20013 USA.
EM BissonI@si.edu
RI Kelley, Paul/C-9155-2016
FU Department of Defense through the US Army Corps of Engineers, Engineer
Research and Development Center [CS-1396, W9132T-05-C-0023]
FX We thank J.L. Granger, S. Lovell, A. Whitley, J. Ferrer, C. Pekins, D.
Cimprich, The Nature Conservancy (Fort Hood Chapter) and the Fort Hood
Natural Resources Management Branch for their assistance in the field.
We are also grateful for valuable comments on the paper from two
anonymous reviewers. This project was supported by the Department of
Defense, Strategic Environmental Research and Development Program,
Project CS-1396, through the US Army Corps of Engineers, Engineer
Research and Development Center, contract #W9132T-05-C-0023. Research
activities were conducted in accordance with all applicable Federal and
State of Texas wildlife and endangered species permits.
NR 44
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U1 2
U2 24
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1367-9430
J9 ANIM CONSERV
JI Anim. Conserv.
PD OCT
PY 2011
VL 14
IS 5
BP 484
EP 491
DI 10.1111/j.1469-1795.2011.00447.x
PG 8
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 846JX
UT WOS:000296894900006
ER
PT J
AU Bel, MC
Rodriguez, J
D'Avanzo, P
Russell, DM
Tomsick, J
Corbel, S
Lewis, FW
Rahoui, F
Buxton, M
Goldoni, P
Kuulkers, E
AF Bel, M. Cadolle
Rodriguez, J.
D'Avanzo, P.
Russell, D. M.
Tomsick, J.
Corbel, S.
Lewis, F. W.
Rahoui, F.
Buxton, M.
Goldoni, P.
Kuulkers, E.
TI Overview of an extensive multi-wavelength study of GX 339-4 during the
2010 outburst
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE black hole physics; stars: individual: GX 339-4; gamma rays: general;
X-rays: binaries; infrared: general; radio continuum: general
ID X-RAY BINARIES; BLACK-HOLE BINARIES; HIGH-ENERGY OBSERVATIONS; LOW/HARD
STATE; GAMMA-RAY; ACCRETION DISK; COMPACT JET; LOW-LUMINOSITY; XTE
J1550-564; LIGHT CURVES
AB Context. The microquasar GX 339-4 experienced a new outburst in 2010: it was observed simultaneously at various wavelengths from radio up to soft gamma-rays. We focus on observations that are quasi-simultaneous with those made with the INTEGRAL and RXTE satellites: these were collected in 2010 March-April during our INTEGRAL target of opportunity programme, and during some of the other INTEGRAL observing programmes with GX 339-4 in the field-of-view.
Aims. X-ray transients are extreme systems that often harbour a black hole, and are known to emit throughout the whole electromagnetic spectrum when in outburst. The goals of our programme are to understand the evolution of the physical processes close to the black hole and to study the connections between the accretion and ejection.
Methods. We analysed radio, NIR, optical, UV, X-ray and soft gamma-ray observations. We studied the source evolution in detail by producing light curves, hardness-intensity diagrams and spectra. We fitted the broadband data with phenomenological, then physical, models to study the emission coming from the distinct components.
Results. Based on the energy spectra, the source evolved from the canonical hard state to the canonical soft state. The source showed X-ray spectral variations that were correlated with changes in radio, NIR and optical emission. The bolometric flux increased from 0.8 to 2.9 x 10(-8) erg cm(-2) s(-1) while the relative flux and contribution of the hot medium decreased on the average. Reprocessing in the disc was likely to be strong at the end of our observations.
Conclusions. The source showed a behaviour similar to that of previous outbursts, with some small deviations in the hard X-ray parameter evolution. The radio, NIR and optical emission from jets was detected and observed to fade as the source softened. The results are discussed within the context of disc and jet models.
C1 [Bel, M. Cadolle; Kuulkers, E.] ISOC, ESAC, Madrid, Spain.
[Rodriguez, J.; Corbel, S.] Univ Paris Diderot, CNRS, UMR 7158, Lab AIM,CEA DSM,IRFU SAp, Gif Sur Yvette, France.
[D'Avanzo, P.] Osserv Astron Brera, INAF, Merate, Italy.
[Russell, D. M.] Univ Amsterdam, Anton Pannekoek Inst, NL-1012 WX Amsterdam, Netherlands.
[Tomsick, J.] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA.
[Lewis, F. W.] Univ Glamorgan, Faulkes Telescope Project, Pontypridd CF37 1DL, M Glam, Wales.
[Rahoui, F.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Rahoui, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
[Buxton, M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Goldoni, P.] Univ Paris Diderot, IRFU SAp, CNRS, UMR 7164,Lab APC,CEA DSM, Paris, France.
RP Bel, MC (reprint author), ISOC, ESAC, Madrid, Spain.
EM Marion.Cadolle@sciops.esa.int
OI Rodriguez, Jerome/0000-0002-4151-4468
FU ESA member states; Faculty of the European Space Astronomy Center
(ESAC); European Community [ITN 215212]; NASA [NNX08AW35G]
FX We thank the referee for his/her helpful comments that improved our
manuscript. We thank the INTEGRAL, Swift and RXTE mission planners for
programming the ToO observations described in the paper. The present
work is partly based on observations with INTEGRAL, and ESA project with
instruments and science data centre funded by ESA member states
(especially the PI countries: Denmark, France, Germany, Italy,
Switzerland, Spain), and Poland, and with the participation of Russia
and the USA, and on observations with RXTE. The NRAO is a facility of
the National Science Foundation operated under cooperative agreement by
Associated Universities, Inc. M.C.B. acknowledges support from the
Faculty of the European Space Astronomy Center (ESAC) and L. Prat's
comments. JR acknowledges partial funding from the European Community's
Seventh Framework Programme (FP7/2007-2013) under grant agreement number
ITN 215212 "Black Hole Universe". JAT acknowledges partial support from
NASA under Swift Guest Observer grant NNX08AW35G. The FT North and South
are maintained and operated by Las Cumbres Observatory Global Telescope
Network. This research has made use of the NASA Astrophysics Data System
Abstract Service and of the SIMBAD database, operated at the CDS,
Strasbourg, France.
NR 92
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR A119
DI 10.1051/0004-6361/201117684
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800136
ER
PT J
AU Ferrari, C
Intema, HT
Orru, E
Govoni, F
Murgia, M
Mason, B
Bourdin, H
Asad, KM
Mazzotta, P
Wise, MW
Mroczkowski, T
Croston, JH
AF Ferrari, C.
Intema, H. T.
Orru, E.
Govoni, F.
Murgia, M.
Mason, B.
Bourdin, H.
Asad, K. M.
Mazzotta, P.
Wise, M. W.
Mroczkowski, T.
Croston, J. H.
TI Discovery of the correspondence between intra-cluster radio emission and
a high pressure region detected through the Sunyaev-Zel'dovich effect
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: clusters: individual: RX J1347-1145; radio continuum:
galaxies; X-rays: galaxies: clusters; cosmic background radiation
ID GALAXY CLUSTERS; RX J1347.5-1145; PARTICLE REACCELERATION; SHOCK-WAVES;
SKY SURVEY; CORE; PLASMA; HALOS; GAS
AB We analyzed new 237 MHz and 614 MHz GMRT data of the most X-ray luminous galaxy cluster, RXJ1347-1145. Our radio results are compared with the MUSTANG 90 GHz Sunyaev-Zel'dovich effect map and with re-processed Chandra and XMM-Newton archival data of this cluster. We point out for the first time in an unambiguous way the correspondence between a radio excess in a diffuse intra-cluster radio source and a hot region detected through both Sunyaev-Zel'dovich effect and X-ray observations. Our result indicates that electron re-acceleration in the excess emission of the radio mini-halo at the center of RXJ1347-1145 is most likely related to a shock front propagating into the intra-cluster medium.
C1 [Ferrari, C.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Cassiopee, Nice, France.
[Intema, H. T.; Mason, B.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Orru, E.] Radboud Univ Nijmegen, NL-6525 AJ Nijmegen, Netherlands.
[Govoni, F.; Murgia, M.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Ca, Italy.
[Bourdin, H.; Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Mazzotta, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wise, M. W.] ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands.
[Mroczkowski, T.] Univ Penn, Philadelphia, PA 19104 USA.
[Mroczkowski, T.] NASA, Washington, DC USA.
[Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
RP Ferrari, C (reprint author), Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Cassiopee, Nice, France.
EM chiara.ferrari@oca.eu
RI Mazzotta, Pasquale/B-1225-2016;
OI Mroczkowski, Tony/0000-0003-3816-5372; Mazzotta,
Pasquale/0000-0002-5411-1748; Murgia, Matteo/0000-0002-4800-0806;
Govoni, Federica/0000-0003-3644-3084
FU Agence Nationale de la Recherche [ANR-09-JCJC-0001-01]; BQR program of
Observatoire de la Cote d'Azur; Laboratoire Cassiopee [UMR 6202]
FX We thank the anonymous referee for her/his useful comments. We are
grateful to Giulia Macario for helpful suggestions in the radio data
reduction phase. We warmly thank Monique Arnaud for very useful
discussions. We would like to thank the staff of the GMRT that made
these observations possible. GMRT is run by the National Centre for
Radio Astrophysics of the Tata Institute of Fundamental Research. CF
acknowledges financial support by the "Agence Nationale de la Recherche"
through grant ANR-09-JCJC-0001-01. This work was supported by the BQR
program of Observatoire de la Cote d'Azur and by Laboratoire Cassiopee
(UMR 6202).
NR 27
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR L12
DI 10.1051/0004-6361/201117788
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800146
ER
PT J
AU Jorgensen, JK
Bourke, TL
Luong, QN
Takakuwa, S
AF Jorgensen, J. K.
Bourke, T. L.
Luong, Q. Nguyen
Takakuwa, S.
TI Arcsecond resolution images of the chemical structure of the low-mass
protostar IRAS 16293-2422 An overview of a large molecular line survey
from the Submillimeter Array
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE circumstellar matter; ISM: molecules; stars: formation; ISM: jets and
outflows; submillimeter: ISM; ISM: individual objects: IRAS 16293-2422
ID STAR-FORMATION; HOT CORE; COLOGNE DATABASE; IRAS-16293-2422; ENVELOPES;
ABUNDANCES; EVOLUTION; SPECTROSCOPY; CHEMISTRY; OUTFLOWS
AB It remains a key challenge to establish the molecular content of different components of low-mass protostars, like their envelopes and disks, and how this depends on the evolutionary stage and/or environment of the young stars. Observations at submillimeter wavelengths provide a direct possibility to study the chemical composition of low-mass protostars through transitions probing temperatures up to a few hundred K in the gas surrounding these sources. This paper presents a large molecular line survey of the deeply embedded protostellar binary IRAS 16293-2422 from the Submillimeter Array (SMA) - including images of individual lines down to approximate to 1.5- 3" (190-380 AU) resolution. More than 500 individual transitions are identified related to 54 molecular species (including isotopologues) probing temperatures up to about 550 K. Strong chemical differences are found between the two components in the protostellar system with a separation between, in particular, the sulfur- and nitrogen-bearing species and oxygen-bearing complex organics. The action of protostellar outflow on the ambient envelope material is seen in images of CO and SiO and appear to influence a number of other species, including (deuterated) water, HDO. The effects of cold gas-phase chemistry is directly imaged through maps of CO, N2D+ and DCO+, showing enhancements of first DCO+ and subsequently N2D+ in the outer envelope where CO freezes-out on dust grains.
C1 [Jorgensen, J. K.] Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, DK-2100 Copenhagen O, Denmark.
[Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark.
[Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Luong, Q. Nguyen] IRFU Serv Astrophys, CEA DSM, Lab AIM, F-91191 Gif Sur Yvette, France.
[Luong, Q. Nguyen] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Takakuwa, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
RP Jorgensen, JK (reprint author), Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
EM jeskj@nbi.dk
FU Smithsonian Institution; Lundbeck foundation; Danish National Research
Foundation; University of Copenhagen; Bonn International Graduate School
of Physics and Astronomy (BIGS); Argelander Institut fur Astronomie;
Academia Sinica
FX We would like to thank the anonymous referee for a number of good
suggestions helping to improve the presentation of this survey. This
paper is based on data from the Submillimeter Array: 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. It is a pleasure to thank everybody involved with the
Submillimeter Array for the continued development of this observatory.
The research of J.K.J. was supported by a Junior Group Leader Fellowship
from the Lundbeck foundation. Research at Centre for Star and Planet
Formation is funded by the Danish National Research Foundation and the
University of Copenhagen's programme of excellence. Quang Nguyen Luong's
research at Bonn University was supported by a M.Sc. fellowship from
Bonn International Graduate School of Physics and Astronomy (BIGS) and
Argelander Institut fur Astronomie.
NR 39
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR A100
DI 10.1051/0004-6361/201117139
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800060
ER
PT J
AU Kaastra, JS
Petrucci, PO
Cappi, M
Arav, N
Behar, E
Bianchi, S
Bloom, J
Blustin, AJ
Branduardi-Raymont, G
Costantini, E
Dadina, M
Detmers, RG
Ebrero, J
Jonker, PG
Klein, C
Kriss, GA
Lubinski, P
Malzac, J
Mehdipour, M
Paltani, S
Pinto, C
Ponti, G
Ratti, EM
Smith, RAN
Steenbrugge, KC
de Vries, CP
AF Kaastra, J. S.
Petrucci, P-O.
Cappi, M.
Arav, N.
Behar, E.
Bianchi, S.
Bloom, J.
Blustin, A. J.
Branduardi-Raymont, G.
Costantini, E.
Dadina, M.
Detmers, R. G.
Ebrero, J.
Jonker, P. G.
Klein, C.
Kriss, G. A.
Lubinski, P.
Malzac, J.
Mehdipour, M.
Paltani, S.
Pinto, C.
Ponti, G.
Ratti, E. M.
Smith, R. A. N.
Steenbrugge, K. C.
de Vries, C. P.
TI Multiwavelength campaign on Mrk 509 I. Variability and spectral energy
distribution
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; quasars: absorption lines; X-rays: general
ID ACTIVE GALACTIC NUCLEI; GALAXY MARKARIAN 509; X-RAY SPECTROSCOPY;
REFLECTION GRATING SPECTROMETER; QUASAR OUTFLOW CONTRIBUTION; SEYFERT
TYPE-1 GALAXIES; EMISSION-LINE SPECTRA; XMM-NEWTON; ABSORPTION-LINES;
PHYSICAL CONDITIONS
AB Context. Active galactic nuclei (AGN) show a wealth of interesting physical processes, some of which are poorly understood. In a broader context, they play an important role in processes that are far beyond their immediate surroundings, owing to the high emitted power.
Aims. We want to address a number of open questions, including the location and physics of the outflow from AGN, the nature of the continuum emission, the geometry and physical state of the X-ray broad emission line region, the Fe-K line complex, the metal abundances of the nucleus, and finally the interstellar medium of our own Galaxy as seen through the signatures it imprints on the X-ray and UV spectra of AGN.
Methods. We study one of the best targets for these aims, the Seyfert 1 galaxy Mrk 509 with a multiwavelength campaign using five satellites (XMM-Newton, INTEGRAL, Chandra, HST, and Swift) and two ground-based facilities (WHT and PAIRITEL). Our observations cover more than five decades in frequency, from 2 mu m to 200 keV. The combination of high-resolution spectroscopy and time variability allows us to disentangle and study the different components. Our campaign covers 100 days from September to December 2009, and is centred on a simultaneous set of deep XMM-Newton and INTEGRAL observations with regular time intervals, spanning seven weeks.
Results. We obtain a continuous light curve in the X-ray and UV band, showing a strong, up to 60% flux increase in the soft X-ray band during the three weeks in the middle of our deepest monitoring campaign, and which is correlated with an enhancement of the UV flux. This allows us to study the time evolution of the continuum and the outflow. By stacking the observations, we have also obtained one of the best X-ray and UV spectra of a Seyfert galaxy ever obtained. In this paper we also study the effects of the spectral energy distribution (SED) that we obtained on the photo-ionisation equilibrium. Thanks to our broad-band coverage, uncertainties on the SED do not strongly affect the determination of this equilibrium.
Conclusions. Here we present our very successful campaign and in a series of subsequent papers we will elaborate on different aspects of our study.
C1 [Kaastra, J. S.; Costantini, E.; Detmers, R. G.; Ebrero, J.; Jonker, P. G.; Pinto, C.; Ratti, E. M.; de Vries, C. P.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Kaastra, J. S.; Detmers, R. G.] Univ Utrecht, Sterrenkundig Inst, NL-3508 TA Utrecht, Netherlands.
[Petrucci, P-O.] CNRS INSU, UMR 5274, IPAG, UJF Grenoble 1, F-38041 Grenoble, France.
[Cappi, M.; Dadina, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Arav, N.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Behar, E.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel.
[Bianchi, S.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy.
[Bloom, J.; Klein, C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Blustin, A. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Branduardi-Raymont, G.; Mehdipour, M.; Smith, R. A. N.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jonker, P. G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Kriss, G. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lubinski, P.] Ctr Astron M Kopernika, PL-87100 Torun, Poland.
[Malzac, J.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Malzac, J.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Paltani, S.] Univ Geneva, Astron Observ, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland.
[Ponti, G.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Steenbrugge, K. C.] Univ Catolica Norte, Inst Astron, Antofagasta, Chile.
[Steenbrugge, K. C.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
RP Kaastra, JS (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
EM j.s.kaastra@sron.nl
RI Bianchi, Stefano/B-4804-2010; Cappi, Massimo/F-4813-2015;
OI Bianchi, Stefano/0000-0002-4622-4240; Cappi,
Massimo/0000-0001-6966-8920; Dadina, Mauro/0000-0002-7858-7564
FU ESA Member States; USA (NASA); NWO, the Netherlands Organization for
Scientific Research; CNES; French GDR PCHE; ASI-INAF [I/088/06/0];
NASA/XMM [NNX09AR01G]; NASA through Space Telescope Science Institute;
ISF; STFC; Polish MNiSW [NN203065933, 362/1/N-INTEGRAL/2008/09/0]; UK
Science & Technology Facilities Council (STFC); EU
[FP7-PEOPLE-2009-IEF-254279]; Comite Mixto ESO - Gobierno de Chile; NASA
[NAS5-26555]
FX This work is based on observations obtained with XMM-Newton, an ESA
science mission with instruments and contributions directly funded by
ESA Member States and the USA (NASA). It is also based on observations
with INTEGRAL, an ESA project with instrument and science data centre
funded by ESA member states (especially the PI countries: Denmark,
France, Germany, Italy, Switzerland, Spain), Czech Republic, and Poland
and with the participation of Russia and the USA. This work made use of
data supplied by the UK Swift Science Data Centre at the University if
Leicester. SRON is supported financially by NWO, the Netherlands
Organization for Scientific Research. J.S. Kaastra thanks the PI of
Swift, Neil Gehrels, for approving the TOO observations, and the duty
scientists at the William Herschel Telescope for performing the service
observations. P.-O. Petrucci acknowledges financial support from CNES
and the French GDR PCHE. M. Cappi, M. Dadina, S. Bianchi, and G. Ponti
acknowledge financial support from contract ASI-INAF n. I/088/06/0. N.
Arav and G. Kriss gratefully acknowledge support from NASA/XMM-Newton
Guest Investigator grant NNX09AR01G. Support for HST Program number
12022 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. E.
Behar was supported by a grant from the ISF. A. Blustin acknowledges the
support of a STFC Postdoctoral Fellowship. P. Lubinski has been
supported by the Polish MNiSW grants NN203065933 and
362/1/N-INTEGRAL/2008/09/0. M. Mehdipour acknowledges the support of a
PhD studentship awarded by the UK Science & Technology Facilities
Council (STFC). G. Ponti acknowledges support via an EU Marie Curie
Intra-European Fellowship under contract No. FP7-PEOPLE-2009-IEF-254279.
K. Steenbrugge acknowledges the support of Comite Mixto ESO - Gobierno
de Chile.
NR 132
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PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR A36
DI 10.1051/0004-6361/201116869
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800029
ER
PT J
AU Lusso, E
Comastri, A
Vignali, C
Zamorani, G
Treister, E
Sanders, D
Bolzonella, M
Bongiorno, A
Brusa, M
Civano, F
Gilli, R
Mainieri, V
Nair, P
Aller, MC
Carollo, M
Koekemoer, AM
Merloni, A
Trump, JR
AF Lusso, E.
Comastri, A.
Vignali, C.
Zamorani, G.
Treister, E.
Sanders, D.
Bolzonella, M.
Bongiorno, A.
Brusa, M.
Civano, F.
Gilli, R.
Mainieri, V.
Nair, P.
Aller, M. C.
Carollo, M.
Koekemoer, A. M.
Merloni, A.
Trump, J. R.
TI The bolometric output and host-galaxy properties of obscured AGN in the
XMM-COSMOS survey
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE methods: statistical; quasars: general; galaxies: active; Galaxy:
general; X-rays: general
ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES;
WIDE-FIELD SURVEY; SPECTRAL ENERGY-DISTRIBUTION; HUBBLE-SPACE-TELESCOPE;
X-RAY-EMISSION; SIMILAR-TO 1; LUMINOSITY FUNCTION; MAGNITUDE RELATION
AB We present a study of the multi-wavelength properties, from the mid-infrared to the hard X-rays, of a sample of 255 spectroscopically identified X-ray selected type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) are computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. We calculate bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using a multi-component modeling to properly disentangle the emission associated to stellar light from that due to black hole accretion. For 90% of the sample we also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). We find that on average type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, we confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10(10) solar masses.
C1 [Lusso, E.; Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Lusso, E.; Comastri, A.; Vignali, C.; Zamorani, G.; Bolzonella, M.; Gilli, R.; Nair, P.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy.
[Treister, E.; Sanders, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Bongiorno, A.; Brusa, M.; Merloni, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Merloni, A.] TUM, D-85748 Garching, Germany.
[Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mainieri, V.] ESO, D-85748 Garching, Germany.
[Aller, M. C.; Carollo, M.] ETH, Dept Phys, CH-8093 Zurich, Switzerland.
[Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Trump, J. R.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Lusso, E (reprint author), Univ Bologna, Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy.
EM elisabeta.lusso2@unibo.it
RI Vignali, Cristian/J-4974-2012; 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; Vignali, Cristian/0000-0002-8853-9611;
Bolzonella, Micol/0000-0003-3278-4607; Brusa,
Marcella/0000-0002-5059-6848; Comastri, Andrea/0000-0003-3451-9970;
Gilli, Roberto/0000-0001-8121-6177; Bongiorno,
Angela/0000-0002-0101-6624
FU ASI-INAF [I/009/10/0, I/088/06, ASI/COFIS/WP3110I/026/07/0];
Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur
Luft und Raumfahrt; Max-Planck society; NASA [PF8-90055, NAS8-03060];
University of Bologna
FX We gratefully thank B. Simmons for her useful comments and suggestions.
In Italy, the XMM-COSMOS project is supported by ASI-INAF grants
I/009/10/0, I/088/06 and ASI/COFIS/WP3110I/026/07/0. Elisabeta Lusso
gratefully acknowledges financial support from the Marco Polo program,
University of Bologna. In Germany the XMM-Newton project is supported by
the Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur
Luft und Raumfahrt and the Max-Planck society. Support for the work of
E.T. was provided by NASA through Chandra Postdoctoral Fellowship Award
grant number PF8-90055, issued by the Chandra X-ray Observatory Center,
which is operated by the Smithsonian Astrophysical Observatory for and
on behalf of NASA under contract NAS8-03060. The entire COSMOS
collaboration is gratefully acknowledged.
NR 88
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U1 0
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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 OCT
PY 2011
VL 534
AR A110
DI 10.1051/0004-6361/201117175
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800064
ER
PT J
AU Raiteri, CM
Villata, M
Aller, MF
Gurwell, MA
Kurtanidze, OM
Lahteenmaki, A
Larionov, VM
Romano, P
Vercellone, S
Agudo, I
Aller, HD
Arkharov, AA
Bach, U
Benitez, E
Berdyugin, A
Blinov, DA
Borisova, EV
Bottcher, M
Calle, OJAB
Buemi, CS
Calcidese, P
Carosati, D
Casas, R
Chen, WP
Efimova, NV
Gomez, JL
Gusbar, C
Hawkins, K
Heidt, J
Hiriart, D
Hsiao, HY
Jordan, B
Jorstad, SG
Joshi, M
Kimeridze, GN
Koptelova, E
Konstantinova, TS
Kopatskaya, EN
Kurtanidze, SO
Larionova, EG
Larionova, LV
Leto, P
Li, Y
Ligustri, R
Lindfors, E
Lister, M
Marscher, AP
Molina, SN
Morozova, DA
Nieppola, E
Nikolashvili, MG
Nilsson, K
Palma, N
Pasanen, M
Reinthal, R
Roberts, V
Ros, JA
Roustazadeh, P
Sadun, AC
Sakamoto, T
Schwartz, RD
Sigua, LA
Sillanpaa, A
Takalo, LO
Tammi, J
Taylor, B
Tornikoski, M
Trigilio, C
Troitsky, IS
Umana, G
Volvach, A
Yuldasheva, TA
AF Raiteri, C. M.
Villata, M.
Aller, M. F.
Gurwell, M. A.
Kurtanidze, O. M.
Lahteenmaki, A.
Larionov, V. M.
Romano, P.
Vercellone, S.
Agudo, I.
Aller, H. D.
Arkharov, A. A.
Bach, U.
Benitez, E.
Berdyugin, A.
Blinov, D. A.
Borisova, E. V.
Casas, R.
Calle, O. J. A. Bravo
Buemi, C. S.
Calcidese, P.
Carosati, D.
Casas, R.
Chen, W-P.
Efimova, N. V.
Gomez, J. L.
Gusbar, C.
Hawkins, K.
Heidt, J.
Hiriart, D.
Hsiao, H. Y.
Jordan, B.
Jorstad, S. G.
Joshi, M.
Kimeridze, G. N.
Koptelova, E.
Konstantinova, T. S.
Kopatskaya, E. N.
Kurtanidze, S. O.
Larionova, E. G.
Larionova, L. V.
Leto, P.
Li, Y.
Ligustri, R.
Lindfors, E.
Lister, M.
Marscher, A. P.
Molina, S. N.
Morozova, D. A.
Nieppola, E.
Nikolashvili, M. G.
Nilsson, K.
Palma, N.
Pasanen, M.
Reinthal, R.
Roberts, V.
Ros, J. A.
Roustazadeh, P.
Sadun, A. C.
Sakamoto, T.
Schwartz, R. D.
Sigua, L. A.
Sillanpaa, A.
Takalo, L. O.
Tammi, J.
Taylor, B.
Tornikoski, M.
Trigilio, C.
Troitsky, I. S.
Umana, G.
Volvach, A.
Yuldasheva, T. A.
TI The long-lasting activity of 3C 454.3 GASP-WEBT and satellite
observations in 2008-2010
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; quasars: general; quasars: individual: 3C 454.3;
galaxies: jets
ID SPACE-TELESCOPE OBSERVATIONS; GAMMA-RAY FLARE; GALACTIC NUCLEI;
BL-LACERTAE; BLAZAR 3C-454.3; MULTIWAVELENGTH OBSERVATIONS; INFRARED
OBSERVATIONS; RADIO VARIABILITY; AGILE DETECTION; CRAZY-DIAMOND
AB Context. The blazar 3C 454.3 is one of the most active sources from the radio to the gamma-ray frequencies observed in the past few years.
Aims. We present multiwavelength observations of this source from April 2008 to March 2010. The radio to optical data are mostly from the GASP-WEBT, UV and X-ray data from Swift, and gamma-ray data from the AGILE and Fermi satellites. The aim is to understand the connection among emissions at different frequencies and to derive information on the emitting jet.
Methods. Light curves in 18 bands were carefully assembled to study flux variability correlations. We improved the calibration of optical-UV data from the UVOT and OM instruments and estimated the Ly alpha flux to disentangle the contributions from different components in this spectral region.
Results. The observations reveal prominent variability above 8 GHz. In the optical-UV band, the variability amplitude decreases with increasing frequency due to a steadier radiation from both a broad line region and an accretion disc. The optical flux reaches nearly the same levels in the 2008-2009 and 2009-2010 observing seasons; the mm one shows similar behaviour, whereas the gamma and X-ray flux levels rise in the second period. Two prominent gamma-ray flares in mid 2008 and late 2009 show a double-peaked structure, with a variable gamma/optical flux ratio. The X-ray flux variations seem to follow the gamma-ray and optical ones by about 0.5 and 1 d, respectively.
Conclusions. We interpret the multifrequency behaviour in terms of an inhomogeneous curved jet, where synchrotron radiation of increasing wavelength is produced in progressively outer and wider jet regions, which can change their orientation in time. In particular, we assume that the long-term variability is due to this geometrical effect. By combining the optical and mm light curves to fit the gamma and X-ray ones, we find that the gamma (X-ray) emission may be explained by inverse-Comptonisation of synchrotron optical (IR) photons by their parent relativistic electrons (SSC process). A slight, variable misalignment between the synchrotron and Comptonisation zones would explain the increased gamma and X-ray flux levels in 2009-2010, as well as the change in the gamma/optical flux ratio during the outbursts peaks. The time delays of the X-ray flux changes after the gamma, and optical ones are consistent with the proposed scenario.
C1 [Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, Turin, Italy.
[Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kurtanidze, O. M.; Kimeridze, G. N.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, Abastumani, Rep of Georgia.
[Lahteenmaki, A.; Nieppola, E.; Tammi, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Kylmala, Finland.
[Larionov, V. M.; Blinov, D. A.; Borisova, E. V.; Calle, O. J. A. Bravo; Efimova, N. V.; Jorstad, S. G.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.; Yuldasheva, T. A.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia.
[Larionov, V. M.; Arkharov, A. A.; Efimova, N. V.] Pulkovo Observ, St Petersburg, Russia.
[Larionov, V. M.; Blinov, D. A.] St Petersburg Branch, Isaac Newton Inst Chile, St Petersburg, Russia.
[Romano, P.; Vercellone, S.] INAF IASF Palermo, Palermo, Italy.
[Agudo, I.; Gomez, J. L.; Molina, S. N.] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Agudo, I.; Jorstad, S. G.; Joshi, M.; Marscher, A. P.; Taylor, B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Bach, U.] Max Planck Inst Radioastron, D-5300 Bonn, Germany.
[Benitez, E.; Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Berdyugin, A.; Lindfors, E.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, Piikkio, Finland.
[Casas, R.; Gusbar, C.; Hawkins, K.; Li, Y.; Palma, N.; Roberts, V.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA.
[Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, Catania, Italy.
[Calcidese, P.] Osservatorio Astron Reg Autonoma Valle dAosta, St Barthelemy, Italy.
[Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain.
[Carosati, D.] TNG Fdn Galileo Galilei, INAF, La Palma, Spain.
[Casas, R.] Inst Ciencies Espai CSIC IEEC, Barcelona, Spain.
[Casas, R.; Ros, J. A.] Agrupacio Astron Sabadell, Sabadell, Spain.
[Chen, W-P.; Hsiao, H. Y.; Koptelova, E.] Natl Cent Univ, Grad Inst, Jhongli, Taiwan.
[Heidt, J.] Landessternwarte Heidelberg Konigstuhl, ZAH, Heidelberg, Germany.
[Hsiao, H. Y.] Natl Cent Univ, Lulin Observ, Jhongli, Taiwan.
[Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin, Ireland.
[Koptelova, E.] Natl Taiwan Univ, Dept Phys, Taipei, Taiwan.
[Ligustri, R.] Circolo Astrofili Talmassons, Talmassons, Italy.
[Lister, M.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Nieppola, E.; Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio, Finland.
[Palma, N.] Univ Nacl Autonoma Honduras, Fac Ciencias Espaciales, Tegucigalpa Mdc, Honduras.
[Sadun, A. C.] Univ Colorado Denver, Dept Phys, Denver, CO USA.
[Sakamoto, T.] NASA, Ctr Res & Explorat Space Sci & Technol, GSFC, Greenbelt, MD USA.
[Schwartz, R. D.] Galaxy View Observ, Sequim, WA USA.
[Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Volvach, A.] Crimean Astrophys Observ, Radio Astron Lab, Crimea, Ukraine.
RP Raiteri, CM (reprint author), Osserv Astron Torino, INAF, Turin, Italy.
EM raiteri@oato.inaf.it; villata@oato.inaf.it
RI Kurtanidze, Omar/J-6237-2014; Molina, Sol Natalia/F-9968-2015; Agudo,
Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Larionov,
Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova,
Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad,
Svetlana/H-6913-2013; Efimova, Natalia/I-2196-2013; Blinov,
Dmitry/G-9925-2013; Lahteenmaki, Anne/L-5987-2013; Grishina,
Tatiana/H-6873-2013;
OI Molina, Sol Natalia/0000-0002-4112-2157; Agudo,
Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Larionov,
Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X;
Larionova, Elena/0000-0002-2471-6500; Troitskiy,
Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453;
Efimova, Natalia/0000-0002-8071-4753; Blinov,
Dmitry/0000-0003-0611-5784; Grishina, Tatiana/0000-0002-3953-6676;
Villata, Massimo/0000-0003-1743-6946; Larionova,
Liudmila/0000-0002-0274-1481; Leto, Paolo/0000-0003-4864-2806;
Vercellone, Stefano/0000-0003-1163-1396; Raiteri, Claudia
Maria/0000-0003-1784-2784
FU ASI-INAF I/009/10/0; Russian RFBR foundation [09-02-00092]; Georgian
National Science Foundation [GNSF/ST08/4-404]; Academy of Finland
[212656, 210338, 121148]; NASA [NNX09AU16G, NNX10AP16G, NNX08AV65G,
NNX08AV61G, NNX09AT99G]; NSF [AST-0607523, AST-0907893]; University of
Michigan; MICIIN (Spain) [AYA2010-14844]; CEIC (Andalucia)
[P09-FQM-4784]; Smithsonian Institution; Academia Sinica; BU; Lowell
Observatory
FX C.M.R. is grateful to Stefania Rasetti from the Torino Observatory
Computer Centre for her assistance. We thank the Fermi-LAT team for
providing Fermi data. We acknowledge the use of public data from the
Swift data archive. We acknowledge financial contribution from the
agreement ASI-INAF I/009/10/0. St.-Petersburg University team
acknowledges support from Russian RFBR foundation via grant 09-02-00092.
Abastumani Observatory team acknowledges financial support by the
Georgian National Science Foundation through grant GNSF/ST08/4-404. The
Metsahovi team acknowledges the support from the Academy of Finland to
our observing projects (numbers 212656, 210338, 121148, and others). The
University of Michigan team acknowledges financial support through the
NASA Fermi grants NNX09AU16G, NNX10AP16G, and NSF grant AST-0607523. The
operation of UMRAO is funded by the University of Michigan. This paper
is partly based on observations carried out at the German-Spanish Calar
Alto Observatory, which is jointly operated by the MPIA and the
IAA-CSIC. Acquisition of the MAPCAT data is supported in part by MICIIN
(Spain) grant and AYA2010-14844, and by CEIC (Andalucia) grant
P09-FQM-4784. Partly based on observations with the Medicina and Noto
telescopes operated by INAF - Istituto di Radioastronomia. This research
has made use of NASA's Astrophysics Data System and of the XRT Data
Analysis Software (XRTDAS) developed under the responsibility of the ASI
Science Data Center (ASDC), Italy. This research has made use of data
from the MOJAVE database that is maintained by the MOJAVE team (Lister
et al. 2009). The Submillimeter Array is a joint project between the
Smithsonian Astrophysical Observatory and the Academia Sinica Institute
of Astronomy and Astrophysics and is funded by the Smithsonian
Institution and the Academia Sinica. The research at Boston U. was
supported by NSF grant AST-0907893 and NASA Fermi GI grants NNX08AV65G,
NNX08AV61G, and NNX09AT99G. The PRISM camera at Lowell Observatory was
developed by K. Janes et al. at BU and Lowell Observatory, with funding
from the NSF, BU, and Lowell Observatory.
NR 67
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U2 9
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD OCT
PY 2011
VL 534
AR A87
DI 10.1051/0004-6361/201117026
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800047
ER
PT J
AU Stiele, H
Pietsch, W
Haberl, F
Hatzidimitriou, D
Barnard, R
Williams, BF
Kong, AKH
Kolb, U
AF Stiele, H.
Pietsch, W.
Haberl, F.
Hatzidimitriou, D.
Barnard, R.
Williams, B. F.
Kong, A. K. H.
Kolb, U.
TI The deep XMM-Newton Survey of M 31
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: individual: M 31; X-rays: galaxies
ID X-RAY SOURCES; HUBBLE-SPACE-TELESCOPE; SUPERNOVA REMNANT CANDIDATES;
COLOR-MAGNITUDE DIAGRAMS; CURRENTLY FORMING STARS; DISK CLUSTER
POPULATION; HIGH-RESOLUTION CAMERA; SMALL-MAGELLANIC-CLOUD; M31
GLOBULAR-CLUSTERS; CHANDRA ACIS SURVEY
AB Aims. The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, obtaining a luminosity lower limit similar to 10(35) erg s(-1) in the 0.2-4.5 keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D-25 ellipse. The main goal of the paper is to study the X-ray source population of M 31.
Methods. An X-ray catalogue of 1897 sources was created, with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared, and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries.
Results. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as is expected for an HMXB containing a neutron star primary.
Conclusions. While our survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help classify these sources.
C1 [Stiele, H.; Pietsch, W.; Haberl, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Hatzidimitriou, D.] Univ Athens, Fac Phys, Dept Astrophys Astron & Mech, Athens 15784, Greece.
[Hatzidimitriou, D.] Fdn Res & Technol, IESL, Iraklion 71110, Greece.
[Barnard, R.; Kolb, U.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Barnard, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Williams, B. F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.
[Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.
RP Stiele, H (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
EM holger.stiele@brera.inaf.it
RI Hatzidimitriou, Despina/A-3732-2015;
OI Haberl, Frank/0000-0002-0107-5237
FU ESA Member States; NASA; National Aeronautics and Space Administration;
National Science Foundation; Bundesministerium fur Wirtschaft und
Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR) [FKZ 50
OX 0001, FKZ 50 OR 0405]; Max-Planck Society
FX Based on observations obtained with XMM-Newton, an ESA science mission
with instruments and contributions directly funded by ESA Member States
and NASA.; This publication makes use of the USNOFS Image and Catalogue
Archive operated by the United States Naval Observatory, Flagstaff
Station (http://www.nofs.navy.mil/data/fchpix/), 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, of the SIMBAD database, operated at CDS, Strasbourg, France,
and 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. The
XMM-Newton project is supported by the Bundesministerium fur Wirtschaft
und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR, FKZ
50 OX 0001) and the Max-Planck Society. HS acknowledges support by the
Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur
Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 0405).
NR 129
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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 OCT
PY 2011
VL 534
AR A55
DI 10.1051/0004-6361/201015270
PG 51
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 841ZS
UT WOS:000296554800005
ER
PT J
AU Poffenbarger, HJ
Needelman, BA
Megonigal, JP
AF Poffenbarger, Hanna J.
Needelman, Brian A.
Megonigal, J. Patrick
TI Salinity Influence on Methane Emissions from Tidal Marshes
SO WETLANDS
LA English
DT Article
DE Carbon sequestration; Sulfate reduction; Methane flux; Porewater
ID SALT-MARSH; SULFATE REDUCTION; VERTICAL ACCRETION; NATURAL WETLANDS;
CARBON-DIOXIDE; RIVER ESTUARY; ELEVATED CO2; PORE-WATER; FLUXES;
METHANOGENESIS
AB The relationship between methane emissions and salinity is not well understood in tidal marshes, leading to uncertainty about the net effect of marsh conservation and restoration on greenhouse gas balance. We used published and unpublished field data to investigate the relationships between tidal marsh methane emissions, salinity, and porewater concentrations of methane and sulfate, then used these relationships to consider the balance between methane emissions and soil carbon sequestration. Polyhaline tidal marshes (salinity > 18) had significantly lower methane emissions (mean +/- sd = 1 +/- 2 gm(-2) yr(-1)) than other marshes, and can be expected to decrease radiative forcing when created or restored. There was no significant difference in methane emissions from fresh (salinity=0-0.5) and mesohaline (5-18) marshes (42 +/- 76 and 16 +/- 11 gm(-2) yr(-1), respectively), while oligohaline (0.5-5) marshes had the highest and most variable methane emissions (150 +/- 221 gm(-2) yr(-1)). Annual methane emissions were modeled using a linear fit of salinity against log-transformed methane flux (log(CH4) - -0.056 x salinity + 1: 38; r(2) = 0.52; p < 0.0001). Managers interested in using marshes as greenhouse gas sinks can assume negligible methane emissions in polyhaline systems, but need to estimate or monitor methane emissions in lower-salinity marshes.
C1 [Poffenbarger, Hanna J.; Needelman, Brian A.] Univ Maryland, Dept Environm Sci & Technol, College Pk, MD 20742 USA.
[Megonigal, J. Patrick] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Needelman, BA (reprint author), Univ Maryland, Dept Environm Sci & Technol, 1109 HJ Patterson Hall, College Pk, MD 20742 USA.
EM bneed@umd.edu; megonigalp@si.edu
FU Maryland Department of Natural Resources
FX We thank Andrew Baldwin, Raymond Crew, Emily Hutchins, Miriam Meyers,
Nicholas Mudd, Jim Duls, Caitlin Megonigal and U.S. Fish and Wildlife
Service staff at the Blackwater Natural Wildlife Refuge. This work was
supported by funding from the Maryland Department of Natural Resources
Power Plant Research Program.
NR 50
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U1 10
U2 119
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0277-5212
J9 WETLANDS
JI Wetlands
PD OCT
PY 2011
VL 31
IS 5
BP 831
EP 842
DI 10.1007/s13157-011-0197-0
PG 12
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 843TJ
UT WOS:000296695200002
ER
PT J
AU Lazo-Wasem, EA
Pinou, T
de Niz, AP
Feuerstein, A
AF Lazo-Wasem, Eric A.
Pinou, Theodora
de Niz, Alejandro Pena
Feuerstein, Amanda
TI Epibionts Associated with the Nesting Marine Turtles Lepidochelys
olivacea and Chelonia mydas in Jalisco, Mexico: A Review and Field Guide
SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY
LA English
DT Article
ID LOGGERHEAD SEA-TURTLES; COPEPODA HARPACTICOIDA; BARNACLES CIRRIPEDIA;
CARETTA-CARETTA; COMMENSAL; ATLANTIC; PLANES; STOMATOLEPAS;
TESTUDINARIA; CALIFORNIA
AB The diversity and frequency of epibiota collected over three years (2001, 2002, 2008) from sea turtles (Lepidochelys olivacea and Chelonia mydas) nesting on Teopa Beach in Jalisco State, Mexico, are described. This diversity is compared to epibiotic assemblages procured from these same turtle species nesting on other Mexican beaches, and the role these turtles play in the conservation and dispersal of these epibiota is discussed. Given the increased awareness of epibionts and the desire of many researchers to make positive identifications, specific diagnoses, photographs and a collecting protocol will serve as a basic aid to the collection and accurate identification of epibionts found on turtles living along the Pacific coast of Mexico.
C1 [Lazo-Wasem, Eric A.] Yale Univ, Div Invertebrate Zool, Peabody Museum Nat Hist, New Haven, CT 06520 USA.
[Pinou, Theodora; Feuerstein, Amanda] Western Connecticut State Univ, Dept Biol & Environm Sci, Danbury, CT 06810 USA.
[de Niz, Alejandro Pena] Ctr Protecc & Conservac Tortugas Marinas Playa Te, Municipio De La Huerta 48894, Jalisco, Mexico.
[Feuerstein, Amanda] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
RP Lazo-Wasem, EA (reprint author), Yale Univ, Div Invertebrate Zool, Peabody Museum Nat Hist, New Haven, CT 06520 USA.
EM eric.lazo-wasem@yale.edu
FU Yale College; Yale Peabody Museum
FX We thank Melissa Salgado, Damon Nakamura and Laura Smowle for their help
with fieldwork; these students were supported by the Yale College
Studies in the Environment Program. Further support for M. Salgado was
received from the Yale Class of 1954, and L. Smowle received additional
support from the Environmental Engineering Yale Summer Program.
Fieldwork by A. Feuerstein was supported by the Yale Peabody Museum
Summer Internship Program (2008). Additional support was provided by
Connecticut State University-AAUP to T. Pinou. The Brignone family of
Costa Careyes, Jalisco, Mexico, generously provided field and logistical
support, and access to beaches where the study was conducted, and helped
arrange lodging for two of us (E.A. Lazo-Wasem and A. Feuerstein) during
the 2008 field season. Also, the family of A. Pena de Niz, especially
his wife Dulce, provided considerable general assistance to A.
Feuerstein while she lived in Jalisco during the summer of 2008. We
thank our colleagues at the University of Guadalajara for their
assistant at Campamento La Gloria. Ivan Sazima (Universidade Estadual de
Campinas) generously supplied the diagnostic characters to distinguish
remoras. Suggestions by reviewers Adam Baldinger (Museum of Comparative
Zoology, Harvard University), Christopher Boyko (Dowling College),
Michael Frick (Gainesville, Florida) and John Zardus (The Citadel)
greatly improved the manuscript. Lourdes Rojas (Yale Peabody Museum)
helped with many iterations of the data tables and Daniel Drew (Yale
Peabody Museum) pointed out valuable references for historical accounts
of remora.
NR 55
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U1 2
U2 13
PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV
PI NEW HAVEN
PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA
SN 0079-032X
J9 B PEABODY MUS NAT HI
JI Bull. Peabody Mus. Natl. Hist.
PD OCT
PY 2011
VL 52
IS 2
BP 221
EP 240
PG 20
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 837QM
UT WOS:000296218300003
ER
PT J
AU Corrigan, C
AF Corrigan, Cari
TI ANTARCTICA: THE BEST PLACE ON EARTH TO COLLECT METEORITES
SO ELEMENTS
LA English
DT Editorial Material
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Corrigan, C (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 1
U2 2
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 1811-5209
J9 ELEMENTS
JI Elements
PD OCT
PY 2011
VL 7
IS 5
BP 296
EP 296
PG 1
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 838QY
UT WOS:000296308500003
ER
PT J
AU Smith, KM
Zaldarriaga, M
AF Smith, Kendrick M.
Zaldarriaga, Matias
TI Algorithms for bispectra: forecasting, optimal analysis and simulation
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE cosmic background radiation; early Universe; inflation
ID MICROWAVE BACKGROUND MAPS; PROBE WMAP OBSERVATIONS; POWER SPECTRUM;
NON-GAUSSIANITY; ANISOTROPIES; REIONIZATION
AB We propose a factorizability ansatz for angular bispectra which permits fast algorithms for forecasting, analysis and simulation, yet is general enough to encompass many interesting cosmic microwave background (CMB) bispectra. We describe a suite of general algorithms which apply to any bispectrum which can be represented in factorizable form. First, we present algorithms for Fisher matrix forecasts and the related problem of optimizing the factorizable representation, giving a Fisher forecast for Planck as an example. We show that the CMB can give independent constraints on the amplitude of primordial bispectra of both local and equilateral shape as well as those created by secondary anisotropies. We also show that the integrated Sachs-Wolfe (ISW)-lensing bispectrum should be detected by Planck and could bias estimates of the local type of non-Gaussianity if not properly accounted for. Second, we implement a bispectrum estimator which is fully optimal in the presence of sky cuts and inhomogeneous noise, extends the generality of fast estimators which have been limited to a few specific forms of the bispectrum and improves the running time of existing implementations by several orders of magnitude. Third, we give an algorithm for simulating random, weakly non-Gaussian maps with prescribed power spectrum and factorizable bispectrum.
C1 [Smith, Kendrick M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Smith, Kendrick M.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Zaldarriaga, Matias] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Zaldarriaga, Matias] Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA.
RP Smith, KM (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
EM kmsmith@astro.princeton.edu
FU Kavli Institure for Cosmological Physics [NSF PHY-0114422]; Packard and
Sloan foundations [NSF AST-0506556, NASA NNG05GG84G]
FX We would like to thank Wayne Hu, Dragan Huterer, Michele Liguori, Eugene
Lim and Bruce Winstein for useful discussions. We acknowledge the use of
the FFTW, LAPACK, CAMB and HEALPiX software packages. KMS was supported
by the Kavli Institure for Cosmological Physics through the grant NSF
PHY-0114422. MZ was supported by the Packard and Sloan foundations, NSF
AST-0506556 and NASA NNG05GG84G.
NR 50
TC 54
Z9 54
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP 2
EP 19
DI 10.1111/j.1365-2966.2010.18175.x
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300023
ER
PT J
AU McDonald, I
van Loon, JT
Sloan, GC
Dupree, AK
Zijlstra, AA
Boyer, ML
Gehrz, RD
Evans, A
Woodward, CE
Johnson, CI
AF McDonald, I.
van Loon, J. Th.
Sloan, G. C.
Dupree, A. K.
Zijlstra, A. A.
Boyer, M. L.
Gehrz, R. D.
Evans, A.
Woodward, C. E.
Johnson, C. I.
TI Spitzer spectra of evolved stars in omega Centauri and their
low-metallicity dust production
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: AGB and post-AGB; circumstellar matter; stars: mass-loss; stars:
winds, outflows; globular clusters: general; infrared: stars
ID RED-GIANT-BRANCH; GALACTIC GLOBULAR-CLUSTERS; MASS-LOSS;
OPTICAL-PROPERTIES; SPACE-TELESCOPE; STELLAR POPULATIONS;
INTERSTELLAR-MEDIUM; CIRCUMSTELLAR DUST; MODEL ATMOSPHERES; MAGELLANIC
CLOUDS
AB Dust production is explored around 14 metal-poor ([Fe/H] = -1.91 to -0.98) giant stars in the Galactic globular cluster omega Centauri using new Spitzer Infrared Spectrograph spectra. This sample includes the cluster's post-asymptotic giant branch (AGB) and carbon stars and is thus the first representative spectral study of dust production in a metal-poor ([Fe/H] < -1) population. Only the more metal-rich stars V6 and V17 ([Fe/H]= -1.08, -1.06) exhibit silicate emission, while the five other stars with mid-infrared excess show only a featureless continuum which we argue is caused by metallic iron dust grains. We examine the metallicity of V42, and find it is likely part of the metal-rich population ([Fe/H] similar to -0.8). Aside from the post-AGB star V1, we find no star from the cluster's bulk, metal-poor ([Fe/H] < -1.5) population - including the carbon stars - to be producing detectable amounts of dust. We compare the dust production to the stars' H alpha line profiles obtained at the Magellan/Clay telescope at Las Campanas Observatory, finding pulsation shocking in the strongest pulsators (V6, V17 and V42), but evidence of outflow in all other stars. We conclude that the onset of dust production does not signify a fundamental change in the material leaving the star. Our data add to a growing body of evidence that metallic iron dominates dust production in metal-poor, oxygen-rich stars, but that dust is probably not the primary accelerant of winds in this mass-metallicity regime.
C1 [McDonald, I.; Zijlstra, A. A.] Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[McDonald, I.; van Loon, J. Th.; Evans, A.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Boyer, M. L.] STScI, Baltimore, MD 21218 USA.
[Gehrz, R. D.; Woodward, C. E.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
[Johnson, C. I.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP McDonald, I (reprint author), Jodrell Bank, Ctr Astrophys, Alan Turing Bldg, Manchester M13 9PL, Lancs, England.
EM mcdonald@jb.man.ac.uk
FU NASA; United States Air Force; National Science Foundation
[AST-1003201]; NASA JPL/Spitzer
FX RDG was supported by NASA and the United States Air Force. CEW was
supported in part by the National Science Foundation and NASA
JPL/Spitzer grants awarded to the University of Minnesota. CIJ was
supported by the National Science Foundation under award No.
AST-1003201.
NR 76
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U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP 20
EP 31
DI 10.1111/j.1365-2966.2011.18963.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300024
ER
PT J
AU Risaliti, G
Nardini, E
Elvis, M
Brenneman, L
Salvati, M
AF Risaliti, G.
Nardini, E.
Elvis, M.
Brenneman, L.
Salvati, M.
TI Probing general relativistic effects during active galactic nuclei X-ray
eclipses
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE relativistic processes; galaxies: active
ID BLACK-HOLE; ACCRETION DISK; NGC 1365; LINE; GALAXIES; SPECTROSCOPY;
TRANSITIONS; MCG-6-30-15; ABSORPTION; ABSORBER
AB Long X-ray observations of bright active galactic nuclei (AGN) show that X-ray eclipses, with durations from a few hours to a few days, are rather common. This opens up a new window of opportunity in the search for signatures of relativistic effects in AGN: an obscuring cloud covers/uncovers different parts of the accretion disc at different times, allowing a direct check of the expected pattern of disc emission. In particular, the combination of gravitational redshift and relativistic Doppler boosting should imply strong differences between the receding and approaching parts of an inclined thin disc. At present, these effects may be already detectable with a 'lucky' XMM-Newton or Suzaku observation of a complete eclipse by a Compton-thick cloud (a rare, but not impossible-to-see event). In the future, higher sensitivity observatories will be able to perform these tests easily on tens of AGN. This will provide a powerful and direct way to test extreme gravity, and to probe the structure of AGN in the close vicinity of the central black holes.
C1 [Risaliti, G.; Salvati, M.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Risaliti, G.; Elvis, M.; Brenneman, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Nardini, E.] Univ Florence, Dipartimento Fis Astron, I-50125 Florence, Italy.
RP Risaliti, G (reprint author), INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy.
EM grisaliti@cfa.harvard.edu
RI XRAY, SUZAKU/A-1808-2009;
OI Risaliti, Guido/0000-0002-3556-977X
FU [NASA NNX08AN48G]
FX This work has been partly supported by grants NASA NNX08AN48G.
NR 29
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP 178
EP 183
DI 10.1111/j.1365-2966.2011.19055.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300031
ER
PT J
AU Sobolewska, MA
Papadakis, IE
Done, C
Malzac, J
AF Sobolewska, M. A.
Papadakis, I. E.
Done, C.
Malzac, J.
TI Evidence for a change in the X-ray radiation mechanism in the hard state
of Galactic black holes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; X-rays: binaries
ID BROAD-BAND SPECTRUM; ADVECTION-DOMINATED ACCRETION; NOVA-MUSCAE 1991;
SGR-A-ASTERISK; GX 339-4; XTE J1550-564; GAMMA-RAY; OUTBURST DECAY;
LOW/HARD STATE; NEUTRON-STARS
AB We present results on the spectral variability of two Galactic black hole X-ray binaries, GRO J1655-40 and GX 339-4, in the hard state. We confirm a transition in behaviour of the photon index with luminosity, such that the well-known decrease in X-ray photon index with decreasing luminosity only continues down to L-bol similar to 0.01L(E). Below this point, the photon index increases again. For Comptonization models, this implies that the ratio of the Compton luminosity to seed photon luminosity, l(h)/l(s), changes with bolometric luminosity, consistent with a scenario where seed photons change from cyclo-synchrotron at the lowest luminosities to those from a truncated disc. Alternatively, the transition could mark the point below which the non-thermal jet starts to dominate, or where reprocessed photons replace the viscous photons in an outflowing corona model.
C1 [Sobolewska, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sobolewska, M. A.; Papadakis, I. E.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Crete, Greece.
[Sobolewska, M. A.; Papadakis, I. E.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
[Sobolewska, M. A.; Papadakis, I. E.] Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece.
[Done, C.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Malzac, J.] Univ Toulouse, Toulouse, France.
[Malzac, J.] UPS OMP, Toulouse, France.
[Malzac, J.] IRAP, F-31028 Toulouse 4, France.
[Malzac, J.] CNRS, F-31028 Toulouse 4, France.
RP Sobolewska, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM msobolewska@cfa.harvard.edu
RI Papadakis, Iossif/C-3235-2011; done, chris/D-4605-2016
OI done, chris/0000-0002-1065-7239
FU Chandra grant [GO8-9125A]; Marie-Curie ToK Fellowship
[MTKD-CT-2006-039965]; EU FP7-REGPOT [206469]; GdR PCHE in France
FX Wewould like to thank the anonymous referee for helpful comments and
suggestions. MS acknowledges support from a Chandra grant GO8-9125A and
a Marie-Curie ToK Fellowship number MTKD-CT-2006-039965. IEP
acknowledges support from the EU FP7-REGPOT 206469 grant. This work was
partially supported by the GdR PCHE in France.
NR 70
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JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP 280
EP 288
DI 10.1111/j.1365-2966.2011.19209.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300039
ER
PT J
AU Alsubai, KA
Parley, NR
Bramich, DM
West, RG
Sorensen, PM
Cameron, AC
Latham, DW
Horne, K
Anderson, DR
Bakos, GA
Brown, DJA
Buchhave, LA
Esquerdo, GA
Everett, ME
Furesz, G
Hartman, JD
Hellier, C
Miller, GM
Pollacco, D
Quinn, SN
Smith, JC
Stefanik, RP
Szentgyorgyi, A
AF Alsubai, K. A.
Parley, N. R.
Bramich, D. M.
West, R. G.
Sorensen, P. M.
Cameron, A. Collier
Latham, D. W.
Horne, K.
Anderson, D. R.
Bakos, G. A.
Brown, D. J. A.
Buchhave, L. A.
Esquerdo, G. A.
Everett, M. E.
Furesz, G.
Hartman, J. D.
Hellier, C.
Miller, G. M.
Pollacco, D.
Quinn, S. N.
Smith, J. C.
Stefanik, R. P.
Szentgyorgyi, A.
TI Qatar-1b: a hot Jupiter orbiting a metal-rich K dwarf star
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: photometric; techniques: radial velocities; techniques:
spectroscopic; stars: individual: Qatar-1; planetary systems
ID M-J PLANET; LIGHT CURVES; SPECTROSCOPIC BINARIES; EXTRASOLAR PLANETS;
TRANSIT SEARCHES; ALGORITHM; FIELD; CANDIDATES
AB We report the discovery and initial characterization of Qatar-1b, a hot Jupiter-orbiting metal-rich K dwarf star, the first planet discovered by the Qatar Exoplanet Survey. We describe the strategy used to select candidate transiting planets from photometry generated by the Qatar Exoplanet Survey camera array. We examine the rate of astrophysical and other false positives found during the spectroscopic reconnaissance of the initial batch of candidates. A simultaneous fit to the follow-up radial velocities and photometry of Qatar-1b yields a planetary mass of 1.09 +/- 0.08 M-J and a radius of 1.16 +/- 0.05 R-J. The orbital period and separation are 1.420 033 +/- 0.000 016 d and 0.023 43 +/- 0.000 26 au for an orbit assumed to be circular. The stellar density, effective temperature and rotation rate indicate an age greater than 4 Gyr for the system.
C1 [Alsubai, K. A.] Qatar Fdn, Doha, Qatar.
[Parley, N. R.; Cameron, A. Collier; Horne, K.; Brown, D. J. A.; Miller, G. M.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[West, R. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Sorensen, P. M.] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Santa Cruz De T, Spain.
[Latham, D. W.; Bakos, G. A.; Esquerdo, G. A.; Furesz, G.; Hartman, J. D.; Quinn, S. N.; Stefanik, R. P.; Szentgyorgyi, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Anderson, D. R.; Hellier, C.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Everett, M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Pollacco, D.] Queens Univ, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Smith, J. C.] Hidden Loft Observ, Tucson, AZ 85755 USA.
RP Alsubai, KA (reprint author), Qatar Fdn, POB 5825, Doha, Qatar.
EM kalsubai@qf.org.qa
OI Buchhave, Lars A./0000-0003-1605-5666; Cameron,
Andrew/0000-0002-8863-7828; Hartman, Joel/0000-0001-8732-6166
FU Spanoptic Ltd of Glenrothes
FX This research has made use of the ESO Data Archive, the NASA
Astrophysics Data System and the VizieR catalogue access tool, CDS,
Strasbourg, France. The high quality of the JGT photometry reported in
this paper owes much to recent telescope upgrades made possible by a
generous grant from Spanoptic Ltd of Glenrothes, and carried out with
inspired technical effort by Mark Ross, Chris Booth, Roger Stapleton and
David Steven. We thank the anonymous referee for several insightful
suggestions for improving the clarity of the manuscript and the
interpretation of the results.
NR 30
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PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP 709
EP 716
DI 10.1111/j.1365-2966.2011.19316.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300078
ER
PT J
AU Kipping, DM
Spiegel, DS
AF Kipping, David M.
Spiegel, David S.
TI Detection of visible light from the darkest world
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: photometric; stars: individual: TrES-2
ID IRRADIATED GIANT PLANETS; HOT JUPITER; THERMAL INVERSIONS; KEPLER-FIELD;
ATMOSPHERES; ALBEDO; TRES-2; PHOTOMETRY; EMISSION; BINARY
AB We present the detection of visible light from the planet TrES-2b, the darkest exoplanet currently known. By analysis of the orbital photometry from publicly available Kepler data (0.4-0.9 mu m), we determine a day-night contrast amplitude of 6.5 +/- 1.9 ppm (parts per million), constituting the lowest amplitude orbital phase variation discovered. The signal is detected to 3.7 sigma confidence and persists in six different methods of modelling the data and thus appears robust. In contrast, we are unable to detect ellipsoidal variations or beaming effects, but we do provide confidence intervals for these terms. If the day-night contrast is interpreted as being due to scattering, it corresponds to a geometric albedo of A(g) = 0.0253 +/- 0.0072. However, our models indicate that there is a significant emission component to dayside brightness, and the true albedo is even lower (<1 per cent). By combining our measurement with Spitzer and ground-based data, we show that a model with moderate redistribution (P-n similar or equal to 0.3) and moderate extra optical opacity (kappa' similar or equal to 0.3-0.4) provide a compatible explanation to the data.
C1 [Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Spiegel, David S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dkipping@cfa.harvard.edu
FU Smithsonian Institute
FX We thank the Kepler Science Team, especially the DAWG, for making the
data used here available. Thanks to A. Burrows, M. Nikku and the
anonymous referee for helpful comments, and I. Hubeny and A. Burrows for
the development and continued maintenance of COOLTLUSTY and associated
opacity data base. DMK is supported by Smithsonian Institute Restricted
Endowment Funds.
NR 25
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP L88
EP L92
DI 10.1111/j.1745-3933.2011.01127.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300019
ER
PT J
AU McKernan, B
Ford, KES
Lyra, W
Perets, HB
Winter, LM
Yaqoob, T
AF McKernan, B.
Ford, K. E. S.
Lyra, W.
Perets, H. B.
Winter, L. M.
Yaqoob, T.
TI On rapid migration and accretion within discs around supermassive black
holes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accreation, accreation discs; planet-disc interactions; stars:
kinematics and dynamics; galaxies: active; galaxies: nuclei; quasars:
general
ID ACTIVE GALACTIC NUCLEI; III PLANETARY MIGRATION; SOFT-X-RAY; NUMERICAL
SIMULATIONS; STELLAR REMNANTS; STAR-FORMATION; MASS; GALAXIES; CLUSTER;
EXCESS
AB Galactic nuclei should contain a cluster of stars and compact objects in the vicinity of the central supermassive black hole due to stellar evolution, minor mergers and gravitational dynamical friction. By analogy with protoplanetary migration, nuclear cluster objects (NCOs) can migrate in the accretion discs that power active galactic nuclei (AGN) by exchanging angular momentum with disc gas. Here we show that an individual NCO undergoing runaway outward migration comparable to type III protoplanetary migration can generate an accretion rate corresponding to Seyfert AGN or quasar luminosities. Multiple migrating NCOs in an AGN disc can dominate traditional viscous disc accretion, and at large disc radii, ensemble NCO migration and accretion could provide sufficient heating to prevent the gravitational instability from consuming disc gas in star formation. The magnitude and energy of the X-ray soft excess observed at similar to 0.1-1 keV in Seyfert AGN could be explained by a small population of similar to 10(2)-10(3) accreting stellar mass black holes or a few ULXs. NCO migration and accretion in AGN discs are therefore extremely important mechanisms to add to realistic models of AGN discs.
C1 [McKernan, B.; Ford, K. E. S.] CUNY, Borough Manhattan Community Coll, Dept Sci, New York, NY 10007 USA.
[McKernan, B.; Ford, K. E. S.; Lyra, W.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[McKernan, B.; Ford, K. E. S.] CUNY, Grad Ctr, New York, NY 10016 USA.
[Perets, H. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Winter, L. M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA.
[Yaqoob, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP McKernan, B (reprint author), CUNY, Borough Manhattan Community Coll, Dept Sci, New York, NY 10007 USA.
EM bmckernan@amnh.org
RI Perets, Hagai/K-9605-2015
OI Perets, Hagai/0000-0002-5004-199X
NR 45
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SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP L103
EP L107
DI 10.1111/j.1745-3933.2011.01132.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300022
ER
PT J
AU Russell, HR
van Weeren, RJ
Edge, AC
McNamara, BR
Sanders, JS
Fabian, AC
Baum, SA
Canning, REA
Donahue, M
O'Dea, CP
AF Russell, H. R.
van Weeren, R. J.
Edge, A. C.
McNamara, B. R.
Sanders, J. S.
Fabian, A. C.
Baum, S. A.
Canning, R. E. A.
Donahue, M.
O'Dea, C. P.
TI A merger mystery: no extended radio emission in the merging cluster
Abell 2146
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE general: clusters: general; galaxies: clusters: individual: A2146; radio
continuum: general
ID X-RAY-EMISSION; VLA SKY SURVEY; GALAXY CLUSTERS; COMA CLUSTER;
COSMIC-RAYS; PARTICLE-ACCELERATION; NONTHERMAL EMISSION; RELIC
CANDIDATES; SHOCK-WAVES; DARK-MATTER
AB We present a new 400 ks Chandra X-ray observation and a Giant Metrewave Radio Telescope (GMRT) radio observation at 325 MHz of the merging galaxy cluster Abell 2146. The Chandra observation reveals detailed structure associated with the major merger event including the Mach M = 2.1 +/- 0.2 bow shock located ahead of the dense subcluster core and the first known example of an upstream shock (M = 1.6 +/- 0.1). Surprisingly, the deep GMRT observation at 325MHz does not detect any extended radio emission associated with either shock front. All other merging galaxy clusters with X-ray-detected shock fronts, including the Bullet cluster, Abell 520, Abell 754 and Abell 2744, and clusters with candidate shock fronts have detected radio relics or radio halo edges coincident with the shocks. We consider several possible factors which could affect the formation of radio relics, including the shock strength and the presence of a pre-existing electron population, but do not find a favourable explanation for this result. We calculate a 3 sigma upper limit of 13 mJy on extended radio emission, which is significantly below the radio power expected by the observed P-radio-L-X correlation for merging systems. The lack of an extended radio halo in Abell 2146 maybe due to the low cluster mass relative to the majority of merging galaxy clusters with detected radio haloes.
C1 [Russell, H. R.; McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[van Weeren, R. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada.
[McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sanders, J. S.; Fabian, A. C.; Canning, R. E. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Baum, S. A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
[Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA.
RP Russell, HR (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
EM helen.russell@uwaterloo.ca
OI Edge, Alastair/0000-0002-3398-6916; Sanders, Jeremy/0000-0003-2189-4501;
van Weeren, Reinout/0000-0002-0587-1660
FU Canadian Space Agency; Royal Society; Royal Netherlands Academy of Arts
and Sciences; STFC
FX HRR and BRM acknowledge generous financial support from the Canadian
Space Agency Space Science Enhancement Program. ACF thanks the Royal
Society for support. RJvW and REAC acknowledge funding from the Royal
Netherlands Academy of Arts and Sciences and the STFC, respectively. The
GMRT is operated by the National Centre for Radio Astrophysics (NCRA).
The authors are grateful to the GMRT Director and staff for the award of
time and executing the observations. HRR thanks David Green, Julie
Hlavacek-Larrondo, Roderick Johnstone and Grant Tremblay for helpful
discussions. We also thank the referee and Gianfranco Brunetti for
helpful comments that improved this letter.
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JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP L1
EP L5
DI 10.1111/j.1745-3933.2011.01098.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300001
ER
PT J
AU Steffen, JH
Quinn, SN
Borucki, WJ
Brugamyer, E
Bryson, ST
Buchhave, LA
Cochran, WD
Endl, M
Fabrycky, DC
Ford, EB
Holman, MJ
Jenkins, J
Koch, D
Latham, DW
MacQueen, P
Mullally, F
Prsa, A
Ragozzine, D
Rowe, JF
Sanderfer, DT
Seader, SE
Short, D
Shporer, A
Thompson, SE
Torres, G
Twicken, JD
Welsh, WF
Windmiller, G
AF Steffen, J. H.
Quinn, S. N.
Borucki, W. J.
Brugamyer, E.
Bryson, S. T.
Buchhave, L. A.
Cochran, W. D.
Endl, M.
Fabrycky, D. C.
Ford, E. B.
Holman, M. J.
Jenkins, J.
Koch, D.
Latham, D. W.
MacQueen, P.
Mullally, F.
Prsa, A.
Ragozzine, D.
Rowe, J. F.
Sanderfer, D. T.
Seader, S. E.
Short, D.
Shporer, A.
Thompson, S. E.
Torres, G.
Twicken, J. D.
Welsh, W. F.
Windmiller, G.
TI The architecture of the hierarchical triple star KOI 928 from eclipse
timing variations seen in Kepler photometry
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: eclipsing
ID LIGHT CURVES; LOW-MASS; PLANETS; SYSTEM; GIANT
AB We present a hierarchical triple star system (KIC 9140402) where a low-mass eclipsing binary orbits a more massive third star. The orbital period of the binary (4.988 29 d) is determined by the eclipse times seen in photometry from NASA's Kepler spacecraft. The periodically changing tidal field, due to the eccentric orbit of the binary about the tertiary, causes a change in the orbital period of the binary. The resulting eclipse timing variations provide insight into the dynamics and architecture of this system and allow the inference of the total mass of the binary (0.424 +/- 0.017M(circle dot)) and the orbital parameters of the binary about the central star.
C1 [Steffen, J. H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Quinn, S. N.; Holman, M. J.; Latham, D. W.; Ragozzine, D.; Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Borucki, W. J.; Bryson, S. T.; Jenkins, J.; Koch, D.; Mullally, F.; Rowe, J. F.; Sanderfer, D. T.; Seader, S. E.; Thompson, S. E.; Twicken, J. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brugamyer, E.; Cochran, W. D.; Endl, M.; MacQueen, P.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Fabrycky, D. C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ford, E. B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Jenkins, J.; Mullally, F.; Seader, S. E.; Thompson, S. E.; Twicken, J. D.] SETI Inst, Mountain View, CA 94043 USA.
[Prsa, A.] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Short, D.; Welsh, W. F.; Windmiller, G.] San Diego State Univ, San Diego, CA 92182 USA.
[Shporer, A.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
RP Steffen, JH (reprint author), Fermilab Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA.
EM jsteffen@fnal.gov
RI Steffen, Jason/A-4320-2013; Ragozzine, Darin/C-4926-2013;
OI Buchhave, Lars A./0000-0003-1605-5666; Fabrycky,
Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [HF-51272.01-A, HF-51267.01-A];
STScI; AURA [NAS 5-26555]
FX Kepler is NASA's 10th Discovery mission with funding provided by NASA's
Science Mission Directorate. DCF acknowledges NASA support through
Hubble Fellowship grants #HF-51272.01-A and #HF-51267.01-A awarded by
STScI and operated by AURA under contract NAS 5-26555.
NR 22
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PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 417
IS 1
BP L31
EP L35
DI 10.1111/j.1745-3933.2011.01114.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 838GV
UT WOS:000296276300007
ER
PT J
AU Grindlay, J
Hong, J
Allen, B
Barthelmy, S
Baker, R
AF Grindlay, J.
Hong, J.
Allen, B.
Barthelmy, S.
Baker, R.
TI Development of tiled imaging CZT detectors for sensitive wide-field hard
X-ray surveys to EXIST
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE CZT detectors; Pixellated CZT; Coded aperture telescopes; Black holes;
Wide-field surveys
ID BURST
AB Motivated by the proposed EXIST mission, a "medium-class" space observatory to survey black holes and the Early Universe proposed to the 2010 NAS/NRC Astronomy and Astrophysics Decadal Survey, we have developed the first "large" area 256 cm(2) close-tiled (0.6 mm gaps) hard X-ray (20-600 key) imaging detector employing pixelated (2.5 mm) CdZnTe (CZT) detectors, each 2 x 2 x 0.5 cm(3). We summarize the design, development and operation of this detector array (8 x 8 CZTs) and its performance as the imager for a coded aperture telescope on a high altitude (40 km) balloon flight in October, 2009, as the ProtoEXIST1 payload. We then outline our current development of a second-generation imager, ProtoEXIST2, with 0.6 mm pixels on a 32 x 32 array on each CZT, and how it will lead to the ultimate imaging system needed for EXIST. Other applications of this technology will also be mentioned. (C) 2010 Elsevier B.V. All rights reserved.
C1 [Grindlay, J.; Hong, J.; Allen, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Barthelmy, S.; Baker, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Grindlay, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM josh@head.cfa.harvard.edu
RI Barthelmy, Scott/D-2943-2012
FU NASA [NNG06WC12G, NN09AD76G]
FX This work is supported in part by NASA APRA Grants NNG06WC12G and
NN09AD76G.
NR 7
TC 6
Z9 6
U1 2
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD OCT 1
PY 2011
VL 652
IS 1
BP 671
EP 673
DI 10.1016/j.nima.2010.09.160
PG 3
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 831XS
UT WOS:000295765000162
ER
PT J
AU Kijbunchoo, N
Clayton, GC
Vieux, TC
Dickerman, N
Hillwig, TC
Welch, DL
Pagnotta, A
Tang, SM
Grindlay, JE
Henden, A
AF Kijbunchoo, Nutsinee
Clayton, Geoffrey C.
Vieux, Timothy C.
Dickerman, N.
Hillwig, T. C.
Welch, D. L.
Pagnotta, Ashley
Tang, Sumin
Grindlay, J. E.
Henden, A.
TI NSV 11154 Is a New R Coronae Borealis Star
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID CARBON STARS; PHOTOMETRY; DATABASE; EROS-2
AB NSV 11154 has been confirmed as a new member of the rare hydrogen-deficient R Coronae Borealis (RCB) stars based on new photometric and spectroscopic data. Using new photometry, as well as archival plates from the Harvard archive, we have constructed the historical light curve of NSV 11154 from 1896 to the present. The light curve shows the sudden, deep, irregularly spaced declines characteristic of RCB stars. The visible spectrum is typical of a cool (T-eff less than or similar to 5000 K) RCB star, showing no hydrogen lines, strong C-2 Swan bands, and no evidence of C-13. In addition, the star shows small pulsations that are typical of an RCB star and an infrared excess due to circumstellar dust, with a temperature of similar to 800 K. The distance to NSV 11154 is estimated to be similar to 14.5 kpc. RCB stars are very rare in the Galaxy, so each additional star is important to population studies leading to a better understanding the origins of these mysterious stars. Among the known sample of RCB stars, NSV 11154 is unusual in that it lies well above the Galactic plane (5 kpc) and away from the Galactic center, which suggests that its parent population is neither thick disk nor bulge.
C1 [Kijbunchoo, Nutsinee; Clayton, Geoffrey C.; Vieux, Timothy C.; Dickerman, N.; Pagnotta, Ashley] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Hillwig, T. C.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA.
[Welch, D. L.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
[Tang, Sumin; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Henden, A.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA.
RP Kijbunchoo, N (reprint author), Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
EM nkijbu1@tigers.lsu.edu; gclayton@fenway.phys.lsu.edu;
tvieux1@tigers.lsu.edu; todd.hillwig@valpo.edu;
welch@physics.mcmaster.ca; pagnotta@phys.lsu.edu; stang@cfa.harvard.edu;
josh@head.cfa.harvard.edu; arne@aavso.org
FU NSF [AST-0407380, AST-0909073]; Cornel and Cynthia K. Sarosdy Fund
FX This article used data from Digital Access to a Sky Century at Harvard
(DASCH), supported by NSF grants AST-0407380 and AST-0909073, as well as
by the Cornel and Cynthia K. Sarosdy Fund.
NR 24
TC 4
Z9 4
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD OCT
PY 2011
VL 123
IS 908
BP 1149
EP 1155
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 840XK
UT WOS:000296475200002
ER
PT J
AU Szentgyorgyi, A
Furesz, G
Cheimets, P
Conroy, M
Eng, R
Fabricant, D
Fata, R
Gauron, T
Geary, J
McLeod, B
Zajac, J
Amato, S
Bergner, H
Caldwell, N
Dupree, A
Goddard, R
Johnston, E
Meibom, S
Mink, D
Pieri, M
Roll, J
Tokarz, S
Wyatt, W
Epps, H
Hartmann, L
Meszaros, S
AF Szentgyorgyi, Andrew
Furesz, Gabor
Cheimets, Peter
Conroy, Maureen
Eng, Roger
Fabricant, Daniel
Fata, Robert
Gauron, Thomas
Geary, John
McLeod, Brian
Zajac, Joseph
Amato, Stephen
Bergner, Henry
Caldwell, Nelson
Dupree, Andrea
Goddard, Richard
Johnston, Everett
Meibom, Soeren
Mink, Douglas
Pieri, Mario
Roll, John
Tokarz, Susan
Wyatt, William
Epps, Harland
Hartmann, Lee
Meszaros, Szabolcz
TI Hectochelle: A Multiobject Optical Echelle Spectrograph for the MMT
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID MOUNTING LARGE LENSES; RED GIANT STARS; CHROMOSPHERIC ACTIVITY;
CROSS-DISPERSION; CONVERTED MMT; MASS OUTFLOW; FIBER; SPECTROSCOPY;
INSTRUMENTS
AB The Hectochelle is an optical band, fiber-fed, multiobject echelle spectrograph deployed at the MMT Observatory on Mount Hopkins, Arizona. The optical fibers that feed the Hectochelle are positioned by the Hectospec robot positioner on the MMT f/5 focal surface, and the Hectochelle shares an optical fiber feed system with the Hectospec, a moderate-dispersion spectrograph that is collocated with the Hectochelle. Hectochelle can record up to 240 spectra simultaneously at a resolution of 38,000. Spectra cover a single diffractive order that is approximately 150 angstrom wide. The total potential operating passband of the Hectochelle extends from 3800 A to 9000 angstrom. Operated in conjunction with the MMT f/5 secondary, the MMT wide-field corrector, and the atmospheric dispersion compensator, the patrol field is 10 in diameter and the individual fiber slits are 1.5 '' in diameter. The throughput of the combined telescope, fiber feed, and spectrograph is measured to be 6.1% at 5275 angstrom, exclusive of atmospheric extinction. A 20 minute observation of a V = 15 F-type star yields a signal-to-noise ratio of 35 per resolution element. Hectochelle had first light 2003 December 4 and continues to be operated at the MMT today.
C1 [Szentgyorgyi, Andrew; Furesz, Gabor; Cheimets, Peter; Conroy, Maureen; Eng, Roger; Fabricant, Daniel; Fata, Robert; Gauron, Thomas; Geary, John; McLeod, Brian; Zajac, Joseph; Amato, Stephen; Bergner, Henry; Caldwell, Nelson; Dupree, Andrea; Goddard, Richard; Johnston, Everett; Meibom, Soeren; Mink, Douglas; Pieri, Mario; Roll, John; Tokarz, Susan; Wyatt, William] Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, Cambridge, MA 02138 USA.
[Epps, Harland] Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA.
[Hartmann, Lee] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Meszaros, Szabolcz] Univ Szeged, Dept Opt & Quantum Elect, Szeged, Hungary.
RP Szentgyorgyi, A (reprint author), Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, 60 Garden St, Cambridge, MA 02138 USA.
RI Meszaros, Szabolcs/N-2287-2014
OI Meszaros, Szabolcs/0000-0001-8237-5209
FU MMT instrument team; MMT; Whipple
FX We are grateful for the contributions and support of the entire MMT
instrument team and students and of the MMT and Whipple Observatory
staff. We thank Kevin Bennett, David Bosworth, David Boyd, Daniel
Blanco, William Brymer, David Caldwell, Shawn Callahan, Florine
Collette, Emilio Falco, Craig Foltz, Art Gentile, Charles Hughes,
Everett Johnston, Sheila Kannappan, Frank Licata, Steve Nichols, Dale
Noll, Ricardo Ortiz, Tim Pickering, Frank Rivera, Phil Ritz, Cory
Sassaman, Gary Schmidt, Dennis Smith, Ken Van Horn, David Weaver, Grant
Williams and J. T. Williams. We thank the Robot positioner operators
Perry Berlind and Mike Calkins and the MMT operators Mike Alegria,
Alejandra Milone, and John McAfee. We are grateful to the efforts of the
Harvard College Observatory Model Shop led by Larry Knowles. We thank
Robert Dew and Diane Nutter of Cleveland Crystals and John Hoose of
Richardson Grating Laboratory.
NR 35
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Z9 16
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD OCT
PY 2011
VL 123
IS 908
BP 1188
EP 1209
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 840XK
UT WOS:000296475200006
ER
PT J
AU Lu, JM
Li, DZ
Lutz, S
Soejima, A
Yi, TS
Wen, J
AF Lu, Jin-Mei
Li, De-Zhu
Lutz, Sue
Soejima, Akiko
Yi, Tingshuang
Wen, Jun
TI BIOGEOGRAPHIC DISJUNCTION BETWEEN EASTERN ASIA AND NORTH AMERICA IN THE
ADIANTUM PEDATUM COMPLEX (PTERIDACEAE)
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Article
DE Adiantum pedatum; biogeography; eastern Asia; eastern North America;
North America; intercontinental disjunction; phylogeny; Pteridaceae
ID BAYESIAN PHYLOGENETIC INFERENCE; HISTORICAL BIOGEOGRAPHY; CHLOROPLAST
DNA; POLYSTICHUM DRYOPTERIDACEAE; MOLECULAR DIVERGENCE; FERN
BIOGEOGRAPHY; GEOGRAPHIC RANGE; MAIDENHAIR FERN; EVOLUTION; HEMISPHERE
AB Premise of the study: Biogeographic analyses of ferns with an eastern Asian-North American disjunction are few. The Adiantum pedatum complex has such a disjunct distribution. The monophyly of the complex needs to be tested and diversification history of the four species needs to be reconstructed.
Methods: Plastid (atpA, atpB, rbcL, trnL-F, and rps4-trnS) sequences of 100 accessions representing the biogeographic diversity of Adiantum were analyzed with parsimony and Bayesian inference. Biogeography of the Adiantum pedatum complex was inferred using programs DIVA and LAGRANGE. Divergence times of clades were estimated with the program BEAST.
Key results: The A. pedatum complex is monophyletic and sister to the eastern Asian A. edentulum. Accessions of A. pedatum do not form a clade; instead three subgroups are recognizable. The clade of A. aleuticum and A. viridimontanum is nested within A. pedatum. The Asian A. myriosorum is sister to the A. pedatum-A. aleuticum clade. Both DIVA and LAGRANGE analyses suggest an eastern Asian origin of the A. pedatum complex. The age of the crown A. pedatum complex is dated to be at 4.27 (2.24-6.57) million years ago.
Conclusions: The currently recognized eastern Asian-North American disjunct species A. pedatum needs to be segregated into three species, corresponding to populations in eastern North America, China, and Japan. The eastern Asian-North American disjunction in the complex is inferred to be the result of two intercontinental migrations, one from eastern Asia into North America in the late Tertiary and the other from North America back to eastern Asia in the Pleistocene.
C1 [Lu, Jin-Mei; Lutz, Sue; Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA.
[Lu, Jin-Mei; Li, De-Zhu] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China.
[Lu, Jin-Mei; Li, De-Zhu; Yi, Tingshuang] Germplasm Bank Wild Species, Plant Germplasm & Genom Ctr, Kunming 650204, Yunnan, Peoples R China.
[Soejima, Akiko] Kumamoto Univ, Grad Sch Sci & Technol, Kumamoto 8608555, Japan.
RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA.
EM wenj@si.edu
OI li, de zhu/0000-0002-4990-724X
FU John D. and Catherine T. MacArthur Foundation; National Basic Research
Program of China (973 Program) [2007CB411601]; National Natural Science
Foundation of China [30828001, 31070199, 30800063]; Chinese Academy of
Sciences [2010KIBA02, 2009-LSF-GBOWS-01]; SRF for ROCS, SEM
FX The study was supported by grants from the John D. and Catherine T.
MacArthur Foundation (to J. Wen, R. Ree, and G. Mueller), National Basic
Research Program of China (973 Program, grant no. 2007CB411601), the
National Natural Science Foundation of China (grant nos. 30828001,
31070199, and 30800063), the Project of Knowledge Innovation Program of
the Chinese Academy of Sciences (grant no. 2010KIBA02), the Research
Fund for the Large-Scale Scientific Facilities of the Chinese Academy of
Sciences (grant no. 2009-LSF-GBOWS-01), and the project sponsored by SRF
for ROCS, SEM.
NR 93
TC 19
Z9 20
U1 3
U2 21
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 OCT
PY 2011
VL 98
IS 10
BP 1680
EP 1693
DI 10.3732/ajb.1100125
PG 14
WC Plant Sciences
SC Plant Sciences
GA 833ME
UT WOS:000295888800023
PM 21965133
ER
PT J
AU Bruna, EM
de Andrade, AS
AF Bruna, Emilio M.
de Andrade, Ana Segalin
TI EDGE EFFECTS ON GROWTH AND BIOMASS PARTITIONING OF AN AMAZONIAN
UNDERSTORY HERB (HELICONIA ACUMINATA; HELICONIACEAE)
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Article
DE biomass allocation; common garden; forest fragmentation; Heliconiaceae;
Heliconia acuminata; leaf area ratio; relative growth rate; specific
leaf area
ID TROPICAL RAIN-FOREST; PAST LAND-USE; PHENOTYPIC PLASTICITY; SPATIAL
HETEROGENEITY; PLANT-POPULATIONS; HABITAT FRAGMENTATION; CONTRASTING
HABITATS; GENOTYPIC VARIATION; LIGHT ENVIRONMENTS; SECONDARY FORESTS
AB Premise: After deforestation, environmental changes in the remaining forest fragments are often most intense near the forest edge, but few studies have evaluated plant growth or plasticity of plant growth in response to edge effects.
Methods: In a 2-year common garden experiment, we compared biomass allocation and growth of Heliconia acuminata with identical genotypes grown in 50 x 35 m common gardens on a 25-year-old edge and in a forest interior site.
Key results: Genetically identical plants transplanted to the forest edge and understory exhibited different patterns of growth and biomass allocation. However, individuals with identical genotypes in the same garden often had very different responses. Plants on forest edges also had higher growth rates and increased biomass at the end of the experiment, almost certainly due to the increased light on the forest edge.
Conclusions: With over 70 000 km of forest edge created annually in the Brazilian Amazon, phenotypic plasticity may play an important role in mediating plant responses to these novel environmental conditions.
C1 [Bruna, Emilio M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA.
[Bruna, Emilio M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA.
[Bruna, Emilio M.; de Andrade, Ana Segalin] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, AM, Brazil.
[Bruna, Emilio M.; de Andrade, Ana Segalin] Smithsonian Trop Res Inst, BR-69011970 Manaus, AM, Brazil.
RP Bruna, EM (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, POB 110430, Gainesville, FL 32611 USA.
EM embruna@ufl.edu
RI Bruna, Emilio/H-2769-2012
OI Bruna, Emilio/0000-0003-3381-8477
FU NSF [DEB-0309819]; Biological Dynamics of Forest Fragments Project
(BDFFP)
FX The authors thank J. Ewel, K. Kitajima, and two anonymous reviewers for
helpful discussions and comments on the manuscript. A. M dos Reis and O.
Ferreira da Silva provided assistance in the field, and financial
support was provided by NSF Grant DEB-0309819 and the Biological
Dynamics of Forest Fragments Project (BDFFP). This is publication number
584 in the BDFFP Technical Series. The data for the analyses in this
article are archived with Data Dryad under record numbers
doi:10.5061/dryad.553hc134
NR 62
TC 2
Z9 2
U1 2
U2 34
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 OCT
PY 2011
VL 98
IS 10
BP 1727
EP 1734
DI 10.3732/ajb.1000290
PG 8
WC Plant Sciences
SC Plant Sciences
GA 833ME
UT WOS:000295888800026
PM 21965134
ER
PT J
AU Kuffner, IB
Hickey, TD
Paul, VJ
Morrison, JM
Walters, LJ
Grablow, KR
Turner, T
Parish, ER
AF Kuffner, Ilsa B.
Hickey, T. Don
Paul, Valerie J.
Morrison, Jennifer M.
Walters, Linda J.
Grablow, Katie R.
Turner, Teresa
Parish, Edward R.
TI HALF-DEAD COLONIES OF MONTASTRAEA ANNULARIS RELEASE VIABLE GAMETES ON A
DEGRADED REEF IN THE US VIRGIN ISLANDS
SO BULLETIN OF MARINE SCIENCE
LA English
DT Editorial Material
C1 [Kuffner, Ilsa B.; Hickey, T. Don; Morrison, Jennifer M.] US Geol Survey, St Petersburg, FL 33701 USA.
[Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
[Walters, Linda J.; Grablow, Katie R.] Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA.
[Turner, Teresa; Parish, Edward R.] Univ Virgin Isl, Div Sci & Math, St Thomas, VI 00802 USA.
RP Kuffner, IB (reprint author), US Geol Survey, 600 4th St S, St Petersburg, FL 33701 USA.
EM ikuffner@usgs.gov
OI Kuffner, Ilsa/0000-0001-8804-7847
NR 1
TC 1
Z9 1
U1 0
U2 4
PU ROSENSTIEL SCH MAR ATMOS SCI
PI MIAMI
PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA
SN 0007-4977
J9 B MAR SCI
JI Bull. Mar. Sci.
PD OCT
PY 2011
VL 87
IS 4
BP 855
EP 856
DI 10.5343/bms.2010.1103
PG 2
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 835ZA
UT WOS:000296074600007
ER
PT J
AU Weber, CF
Zak, DR
Hungate, BA
Jackson, RB
Vilgalys, R
Evans, RD
Schadt, CW
Megonigal, JP
Kuske, CR
AF Weber, Carolyn F.
Zak, Donald R.
Hungate, Bruce A.
Jackson, Robert B.
Vilgalys, Rytas
Evans, R. David
Schadt, Christopher W.
Megonigal, J. Patrick
Kuske, Cheryl R.
TI Responses of soil cellulolytic fungal communities to elevated
atmospheric CO2 are complex and variable across five ecosystems
SO ENVIRONMENTAL MICROBIOLOGY
LA English
DT Article
ID SCRUB-OAK ECOSYSTEM; MOJAVE DESERT SOILS; LITTER DECOMPOSITION;
CARBON-DIOXIDE; ABOVEGROUND BIOMASS; MICROBIAL BIOMASS; MODEL ECOSYSTEM;
NITROGEN; FOREST; O-3
AB Elevated atmospheric CO2 generally increases plant productivity and subsequently increases the availability of cellulose in soil to microbial decomposers. As key cellulose degraders, soil fungi are likely to be one of the most impacted and responsive microbial groups to elevated atmospheric CO2. To investigate the impacts of ecosystem type and elevated atmospheric CO2 on cellulolytic fungal communities, we sequenced 10 677 cbhI gene fragments encoding the catalytic subunit of cellobiohydrolase I, across five distinct terrestrial ecosystem experiments after a decade of exposure to elevated CO2. The cbhI composition of each ecosystem was distinct, as supported by weighted Unifrac analyses (all P-values; < 0.001), with few operational taxonomic units (OTUs) being shared across ecosystems. Using a 114-member cbhI sequence database compiled from known fungi, less than 1% of the environmental sequences could be classified at the family level indicating that cellulolytic fungi in situ are likely dominated by novel fungi or known fungi that are not yet recognized as cellulose degraders. Shifts in fungal cbhI composition and richness that were correlated with elevated CO2 exposure varied across the ecosystems. In aspen plantation and desert creosote bush soils, cbhI gene richness was significantly higher after exposure to elevated CO2 (550 mu mol mol(-1)) than under ambient CO2 (360 mmol mol(-1) CO2). In contrast, while the richness was not altered, the relative abundance of dominant OTUs in desert soil crusts was significantly shifted. This suggests that responses are complex, vary across different ecosystems and, in at least one case, are OTU-specific. Collectively, our results document the complexity of cellulolytic fungal communities in multiple terrestrial ecosystems and the variability of their responses to long-term exposure to elevated atmospheric CO2.
C1 [Weber, Carolyn F.; Kuske, Cheryl R.] Los Alamos Natl Lab, Biosci Div, Los Alamos, NM 87545 USA.
[Zak, Donald R.] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA.
[Zak, Donald R.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA.
[Hungate, Bruce A.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA.
[Hungate, Bruce A.] No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA.
[Jackson, Robert B.; Vilgalys, Rytas] Duke Univ, Dept Biol, Durham, NC 27708 USA.
[Jackson, Robert B.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA.
[Evans, R. David] Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA.
[Schadt, Christopher W.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA.
[Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Washington, DC 20013 USA.
RP Kuske, CR (reprint author), Los Alamos Natl Lab, Biosci Div, POB 1663, Los Alamos, NM 87545 USA.
EM kuske@lanl.gov
RI Zak, Donald/C-6004-2012; Hungate, Bruce/F-8991-2011; Schadt,
Christopher/B-7143-2008
OI Hungate, Bruce/0000-0002-7337-1887; Schadt,
Christopher/0000-0001-8759-2448
FU US Department of Energy Biological and Environmental Research
[2010LANLF260]; DOE [2009LANLE660]; DOE Joint Genome Institute
FX This project was funded by the US Department of Energy Biological and
Environmental Research Program (SFA#2010LANLF260 to C.R.K.) and the DOE
Program for Ecosystem Research (Grant #2009LANLE660 to C. R. K.). Sanger
DNA sequencing was conducted at Los Alamos National Laboratory, by the
DOE Joint Genome Institute. We wish to thank Kuan-Liang Liu, Gary Xie
and John Knepper for providing data analysis advice and writing perl
scripts for data analysis and parsing, as well as Lawrence Ticknor for
statistical consulting. We also wish to thank Andrea Porras-Alfaro
(Western Illinois University), Terri M. Porter (McMaster University),
Michael S. Fitzsimons (LANL) and Lynn F. Weber for gifts of fungal
cultures or sporocarps as well as Benjamin Wolfe (Harvard University)
for providing unpublished cbhI sequence data to add to our database. La
Verne Gallegos-Graves (LANL), Jennifer Price (LANL) and Asli Unal (LANL)
provided excellent technical support. We also thank multiple people at
the different field sites for helping collect field samples.
NR 45
TC 22
Z9 22
U1 7
U2 38
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1462-2912
J9 ENVIRON MICROBIOL
JI Environ. Microbiol.
PD OCT
PY 2011
VL 13
IS 10
BP 2778
EP 2793
DI 10.1111/j.1462-2920.2011.02548.x
PG 16
WC Microbiology
SC Microbiology
GA 834OK
UT WOS:000295971300014
PM 21883796
ER
PT J
AU Estrada, C
Schulz, S
Yildizhan, S
Gilbert, LE
AF Estrada, Catalina
Schulz, Stefan
Yildizhan, Selma
Gilbert, Lawrence E.
TI SEXUAL SELECTION DRIVES THE EVOLUTION OF ANTIAPHRODISIAC PHEROMONES IN
BUTTERFLIES
SO EVOLUTION
LA English
DT Article
DE Female mating receptivity; Heliconius; male-male competition; male
control on female reproduction; sexual conflict; signal evolution
ID SEMINAL FLUID PROTEINS; HELICONIUS BUTTERFLIES; DROSOPHILA-MELANOGASTER;
CHEMICAL COMMUNICATION; PHYLOGENETIC SIGNAL; SPERM PRECEDENCE;
MATING-BEHAVIOR; FEMALE FITNESS; LEPIDOPTERA; CONFLICT
AB Competition for mates has resulted in sophisticated mechanisms of male control over female reproduction. Antiaphrodisiacs are pheromones transferred from males to females during mating that reduce attractiveness of females to subsequent courting males. Antiaphrodisiacs generally help unreceptive females reduce male harassment. However, lack of control over pheromone release by females and male control over the amount transferred provides males an opportunity to use antiaphrodisiacs to delay remating by females that have returned to a receptive state. We propose a model for the evolution of antiaphrodisiacs under the influence of intrasexual selection, and determine whether changes in this signal in 11 species of Heliconius butterflies are consistent with two predictions of the model. First, we find that as predicted, male-contributed chemical mixtures are complex and highly variable across species, with limited phylogenetic signal. Second, differences in rates of evolution in pheromone composition between two major clades of Heliconius are as expected: the clade with a greater potential for male-male competition (polyandrous) shows a faster rate of divergence than the one with typically monoandrous mating system. Taken together, our results provide evidence that for females, antiaphrodisiacs can be both honest signals of receptivity (helping reduce harassment) and chastity belts (a male-imposed reduction in remating).
C1 [Estrada, Catalina; Gilbert, Lawrence E.] Univ Texas Austin, Brackenridge Field Lab, Austin, TX 78712 USA.
[Schulz, Stefan; Yildizhan, Selma] Tech Univ Carolo Wilhelmina Braunschweig, Inst Organ Chem, D-38106 Braunschweig, Germany.
[Estrada, Catalina; Gilbert, Lawrence E.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
RP Estrada, C (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092 Balboa, Ancon, Panama.
EM estradac@si.edu
FU National Science Foundation; Office of International Science and
Engineering [0608167]; Animal Behavior Society; Lepidoptera Research
Foundation; Section of Integrative Biology of the University of Texas;
Fonds der chemischen Industrie; UT Austin
FX We thank J. Jamtsho, J. Crutchfield, G. Crutchfield, T. Alexander, S.
Marout, A. Wartenberg, K. Busby, C. Strickland, for their help with
butterfly rearing and maintenance of greenhouse facilities at Patterson
Laboratory and the Brackenridge Field Laboratory. We are also grateful
to S. Mikheyev and J. C. Santos for advice in data analysis, S. Pawar,
G. Grether, C. Anderson, N. Losin, K. Deere, and three anonymous
reviewers for comments on the manuscript, and M. Beltran for providing
phylogenetic distances. This work was funded by the National Science
Foundation and the Office of International Science and Engineering under
grant No 0608167, Animal Behavior Society, Lepidoptera Research
Foundation, the Section of Integrative Biology of the University of
Texas, and Fonds der chemischen Industrie. The insects were imported to
the USA under permits to LEG from USDA APHIS. We thank A. Vega for
assistance with Costa Rican research, collecting and exportation permits
and staff of P. N. Corcovado for facilitating fieldwork. Austin
insectary facilities (LEG) were developed through funding from NSF and
UT Austin.
NR 80
TC 21
Z9 21
U1 2
U2 61
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0014-3820
J9 EVOLUTION
JI Evolution
PD OCT
PY 2011
VL 65
IS 10
BP 2843
EP 2854
DI 10.1111/j.1558-5646.2011.01352.x
PG 12
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 828RZ
UT WOS:000295521600012
PM 21967426
ER
PT J
AU Derryberry, EP
Claramunt, S
Derryberry, G
Chesser, RT
Cracraft, J
Aleixo, A
Perez-Eman, J
Remsen, JV
Brumfield, RT
AF Derryberry, Elizabeth P.
Claramunt, Santiago
Derryberry, Graham
Chesser, R. Terry
Cracraft, Joel
Aleixo, Alexandre
Perez-Eman, Jorge
Remsen, J. V., Jr.
Brumfield, Robb T.
TI LINEAGE DIVERSIFICATION AND MORPHOLOGICAL EVOLUTION IN A LARGE-SCALE
CONTINENTAL RADIATION: THE NEOTROPICAL OVENBIRDS AND WOODCREEPERS (AVES:
FURNARIIDAE)
SO EVOLUTION
LA English
DT Article
DE Morphological Evolution; Phylogenetics; Adaptive Radiation
ID DENSITY-DEPENDENT DIVERSIFICATION; ADAPTIVE RADIATION; MOLECULAR
PHYLOGENIES; ECOLOGICAL OPPORTUNITY; CLADE DIVERSIFICATION;
GEOGRAPHIC-VARIATION; SPECIES RICHNESS; EXTINCTION RATES; FOSSIL RECORD;
HIGHER TAXA
AB Patterns of diversification in species-rich clades provide insight into the processes that generate biological diversity. We tested different models of lineage and phenotypic diversification in an exceptional continental radiation, the ovenbird family Furnariidae, using the most complete species-level phylogenetic hypothesis produced to date for a major avian clade (97% of 293 species). We found that the Furnariidae exhibit nearly constant rates of lineage accumulation but show evidence of constrained morphological evolution. This pattern of sustained high rates of speciation despite limitations on phenotypic evolution contrasts with the results of most previous studies of evolutionary radiations, which have found a pattern of decelerating diversity-dependent lineage accumulation coupled with decelerating or constrained phenotypic evolution. Our results suggest that lineage accumulation in tropical continental radiations may not be as limited by ecological opportunities as in temperate or island radiations. More studies examining patterns of both lineage and phenotypic diversification are needed to understand the often complex tempo and mode of evolutionary radiations on continents.
C1 [Derryberry, Elizabeth P.; Claramunt, Santiago; Remsen, J. V., Jr.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Derryberry, Graham] BioComp Asheville, Asheville, NC 28803 USA.
[Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA.
[Cracraft, Joel] Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA.
[Aleixo, Alexandre] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil.
[Perez-Eman, Jorge] Cent Univ Venezuela, Inst Zool & Ecol Trop, Caracas 1041A, Venezuela.
[Perez-Eman, Jorge] Colecc Ornitol Phelps, Caracas 1010A, Venezuela.
RP Derryberry, EP (reprint author), Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
EM brumfld@lsu.edu
RI Aleixo, Alexandre/L-3135-2013;
OI Brumfield, Robb/0000-0003-2307-0688
FU NSF [DBI-0400797, DEB-0543562, EAR-0228693]; NSF-RTG (Univ. of Arizona);
Univ. of Arizona; CNPq (Brazil) [310593/2009-3, 574008/2008-0,
476212/2007-3]; Sigma Xi
FX We thank M. E. Alfaro, R. E. Ricklefs, C. D. Cadena, and two anonymous
reviewers for helpful comments on earlier drafts of the manuscript. We
thank numerous collectors, including C. M. Milensky, and institutions
for providing tissue samples (see Table S1) and C. Burney, G. Bravo, C.
D. Cadena, A. Cuervo, J. Maley, and L. Naka for sequence data for this
project. G. Bravo, J. M. Brown, J. W. Brown, L. Harmon, C. Heibl, W.
Pfeiffer, J. McCormack, D. Rabosky, A. Rambaut, and M. Tingley provided
code, analysis assistance, and discussion concerning analyses. This
research was supported in part by NSF grants DBI-0400797 and DEB-0543562
to RTB, NSF AToL grant EAR-0228693 to JC, Frank M. Chapman (AMNH) and
NSF-RTG (Univ. of Arizona) postdoctoral fellowships and a
faculty/research small grant (Univ. of Arizona) to RTC, CNPq (Brazil)
grants 310593/2009-3, 574008/2008-0, and 476212/2007-3 to AA, and a
Sigma Xi Grant-in-Aid of Research to SC. Any use of trade, product, or
firm names is for descriptive purposes only and does not imply
endorsement by the U.S. Government.
NR 90
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U1 10
U2 77
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0014-3820
J9 EVOLUTION
JI Evolution
PD OCT
PY 2011
VL 65
IS 10
BP 2973
EP 2986
DI 10.1111/j.1558-5646.2011.01374.x
PG 14
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 828RZ
UT WOS:000295521600022
PM 21967436
ER
PT J
AU Steppan, SJ
Kenagy, GJ
Zawadzki, C
Robles, R
Lyapunova, EA
Hoffmann, RS
AF Steppan, Scott J.
Kenagy, G. J.
Zawadzki, Christopher
Robles, Rafael
Lyapunova, Elena A.
Hoffmann, Robert S.
TI Molecular data resolve placement of the Olympic marmot and estimate
dates of trans-Beringian interchange
SO JOURNAL OF MAMMALOGY
LA English
DT Article
DE cytochrome b; historical biogeography; Marmota olympus; phylogeny; RAG1
ID VANCOUVER-ISLAND MARMOT; MORPHOLOGICAL EVOLUTION; GEOMETRIC
MORPHOMETRICS; RODENTIA; SCIURIDAE; PHYLOGENY; CRANIUM; DIFFERENTIATION;
SPERMOPHILUS; SYSTEMATICS
AB We reinvestigated the phylogeny of all 15 species of Marmota to resolve a conflict between 2 published analyses, one by Kruckenhauser et al. and another by Steppan et al., regarding the Olympic marmot (M. olympus) and to improve resolution in the genus. We acquired fresh samples of M. olympus, combined all available data on mitochondrial DNA (cytochrome b [Cytb] and ND3/ND4), new sequences for ND3/ND4, and 2,000 base pairs (bp) of the nuclear RAG1 gene. All analyses indicate that M. olympus is a much older, rather than more recent, offshoot of the widespread hoary marmot (M. caligata) or Vancouver Island marmot (M. vancouverensis). The mitochondrial data and some RAG1 results are largely congruent, but RAG1 differs on several points, including: the subgenus Marmota appears paraphyletic to Petromarmota, with reciprocally monophyletic Palearctic and Nearctic clades; and the long-tailed marmot (M. caudata) and Menzbier's marmot (M. menzbieri) are not sister species, suggesting mitochondrial introgression. Asia was colonized by Marmota from North America at approximately 4.6 million years ago (mya), followed by rapid diversification of several major lineages. M. olympus diverged from the M. caligata-M. vancouverensis lineage at approximately 2.6 mya, whereas M. vancouverensis and M. caligata diverged at only about 0.4-1.2 mya. M. olympus might have survived in isolation on the Olympic Peninsula in a nunatak refugium throughout a series of glacial maxima.
C1 [Steppan, Scott J.; Zawadzki, Christopher; Robles, Rafael] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA.
[Kenagy, G. J.] Univ Washington, Burke Museum, Seattle, WA 98195 USA.
[Kenagy, G. J.] Univ Washington, Dept Biol, Seattle, WA 98195 USA.
[Lyapunova, Elena A.] Russian Acad Sci, Inst Dev Biol, Moscow, Russia.
[Hoffmann, Robert S.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Steppan, SJ (reprint author), Florida State Univ, Dept Biol Sci, B-157, Tallahassee, FL 32306 USA.
EM steppan@bio.fsu.edu
RI Robles, Rafael/F-1967-2010; Lyapunova, Elena/A-4696-2016
FU National Science Foundation [DEB-9221504, DEB-0918982]; Smithsonian
Institution; Institute of Developmental Biology, Russian Academy of
Sciences, Moscow; Northwest Plateau Institute of Biology, Chinese
Academy of Sciences, Xining; Division of Mammals, National Museum of
Natural History, Smithsonian Institution, Washington, D.C.
FX This paper is dedicated to our friend and colleague Bob Hoffmann, who
died before completion of the manuscript. We thank S. Miller in the
Florida State University sequencing facility for the DNA sequencing, A.
B. Thistle for editorial revisions to this manuscript, and an anonymous
reviewer for constructive comments. Field research was supported by the
Institute of Developmental Biology, Russian Academy of Sciences, Moscow,
the Northwest Plateau Institute of Biology, Chinese Academy of Sciences,
Xining, and by the Division of Mammals, National Museum of Natural
History, Smithsonian Institution, Washington, D.C. We thank Drs. W.
Arnold and T. Ruff of the Research Institute of Wildlife Ecology,
University of Veterinary Medicine, Vienna, Austria; J. Cook of the
University of Alaska; P. Tongiori of the Department of Animal Biology,
University of Modena, Italy; and D. Hafner of the New Mexico Museum of
Natural History for loans of frozen tissue. We also thank A. Bryant of
the Vancouver Island Marmot recovery team for supplying blood samples.
Collecting in Eurasia was funded in part from National Science
Foundation grant DEB-9221504 to Drs. R. Harrison and P. Sherman, Cornell
University (RSH and E. Yensen, coinvestigators). Laboratory work was
supported by a Smithsonian Institution Scholarly Studies Grant to SJS
and RSH and National Science Foundation grant DEB-0918982 to SJS.
NR 37
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U1 0
U2 26
PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS
PI LAWRENCE
PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA
SN 0022-2372
J9 J MAMMAL
JI J. Mammal.
PD OCT
PY 2011
VL 92
IS 5
BP 1028
EP 1037
DI 10.1644/10-MAMM-A-272.1
PG 10
WC Zoology
SC Zoology
GA 835FR
UT WOS:000296021600012
ER
PT J
AU Bozarth, CA
Hailer, F
Rockwood, LL
Edwards, CW
Maldonado, JE
AF Bozarth, Christine A.
Hailer, Frank
Rockwood, Larry L.
Edwards, Cody W.
Maldonado, Jesus E.
TI Coyote colonization of northern Virginia and admixture with Great Lakes
wolves
SO JOURNAL OF MAMMALOGY
LA English
DT Article
DE Canis latrans; colonization; control region; coyote; eastern United
States; Great Lakes wolf
ID MITOCHONDRIAL-DNA PHYLOGEOGRAPHY; BEARS URSUS-AMERICANUS; GRAY WOLF;
INTERFERENCE COMPETITION; GENETIC-CHARACTERIZATION; NORTHEASTERN
COYOTES; POPULATION HISTORY; EASTERN COYOTES; HABITAT USE; RED WOLVES
AB Ecological invasions of generalist species often are facilitated by anthropogenic disturbance. Coyotes (Canis latrans) have benefitted from anthropogenic changes to North American ecosystems and have experienced a dramatic range expansion since the early 19th century. The region east of the Mississippi River has been colonized via 2 routes that have converged in the mid-Atlantic region during the past few decades. Coyotes using the northern route of expansion show molecular evidence of admixture with the Great Lakes wolf (GLW). We used noninvasive molecular techniques to detect the geographic origins of the recent coyote colonization of northern Virginia as a representative of the mid-Atlantic region and to detect signatures of admixture with GLWs. Of 455 individual canid scats screened, we sequenced a variable 282-base pair fragment of the mitochondrial control region from 126 coyote scats, assigned individual identities to samples using 6 microsatellite loci, and conducted phylogeographic analyses by comparing our sequences to previously published haplotypes. In 39 individuals identified in our scat surveys we detected 7 mitochondrial DNA haplotypes, all of which have been previously reported in diverse surrounding geographic localities. Phylogeographic analyses indicate multiple sources of colonization of northern Virginia. One common haplotype detected in northern Virginia is of wolf origin, indicating the presence of admixed coyotes and GLWs from the north.
C1 [Bozarth, Christine A.; Hailer, Frank; Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA.
[Bozarth, Christine A.; Rockwood, Larry L.; Edwards, Cody W.; Maldonado, Jesus E.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA.
[Maldonado, Jesus E.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Bozarth, CA (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA.
EM bozarthc@si.edu
RI Hailer, Frank/C-9114-2012
OI Hailer, Frank/0000-0002-2340-1726
FU Naval Facilities Engineering Command Washington [N40080-08-LTC-0001]
FX Financial and logistical assistance was provided by Naval Facilities
Engineering Command Washington Cooperative Agreement N40080-08-LTC-0001
for Coyote Population Study at MCBQ, the Smithsonian Conservation
Biology Institute Center for Conservation and Evolutionary Genetics, and
the Smithsonian Institution National Museum of Natural History. We thank
T. Stamps, C. Himmelberger, K. Robinson, N. Rotzel, and L. Lakeman for
samples, assistance, and guidance. We also thank S. Lance and J. Leonard
for providing haplotype data from their studies.
NR 80
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U1 3
U2 33
PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS
PI LAWRENCE
PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA
SN 0022-2372
EI 1545-1542
J9 J MAMMAL
JI J. Mammal.
PD OCT
PY 2011
VL 92
IS 5
BP 1070
EP 1080
DI 10.1644/10-MAMM-A-223.1
PG 11
WC Zoology
SC Zoology
GA 835FR
UT WOS:000296021600016
ER
PT J
AU Shik, JZ
Kaspari, M
Yanoviak, SP
AF Shik, Jonathan Z.
Kaspari, Michael
Yanoviak, Stephen P.
TI Preliminary Assessment of Metabolic Costs of the Nematode Myrmeconema
neotropicum on its Host, the Tropical Ant Cephalotes atratus
SO JOURNAL OF PARASITOLOGY
LA English
DT Article
ID ENERGETIC COST; PARASITISM
AB The parasitic nematode Myrmeconema neotropicum infects workers of the neotropical arboreal ant Cephalotes atratus. Infected ants exhibit altered behavior, e.g., reduced aggression and slower tempo, as well as physical traits, e.g., gaster changes from shiny black to bright red. These changes are thought to induce fruit mimicry and attract frugivorous birds, which are the presumed paratenic hosts for the nematodes. We used respirometry to measure the energetic costs of nematode infection, testing the prediction of higher metabolic rates for infected workers maintaining both ant and nematode biomass. Contrary to this prediction, infected workers had lower mass-specific metabolic rates than uninfected workers. Parasites are limited to the gasters (abdomens) of adult ants, and infected gasters had 57% more mass, but 37% lower metabolic rates, compared to uninfected glisters. These results use a metabolic currency to measure, in vivo, the energetic costs of parasitism, and they shed light on the complex co-evolutionary relationship between host and parasite.
C1 [Shik, Jonathan Z.; Kaspari, Michael] Univ Oklahoma, Dept Zool, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA.
[Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama.
[Yanoviak, Stephen P.] Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA.
RP Shik, JZ (reprint author), N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA.
EM jonathan.shik@gmail.com
OI Kaspari, Michael/0000-0002-9717-5768
FU National Science Foundation [DEB-0842038, IOS 0843120]
FX We thank Oris Acevedo, Belkys Jimenez, and the staff of the Smithsonian
Tropical Research Institute for logistical support. This project was
funded by the National Science Foundation under the grants DEB-0842038
to M.K., and IOS 0843120 to S.P.Y.
NR 17
TC 4
Z9 4
U1 5
U2 42
PU AMER SOC PARASITOLOGISTS
PI LAWRENCE
PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA
SN 0022-3395
J9 J PARASITOL
JI J. Parasitol.
PD OCT
PY 2011
VL 97
IS 5
BP 958
EP 959
DI 10.1645/GE-2735.1
PG 2
WC Parasitology
SC Parasitology
GA 834HP
UT WOS:000295950700039
PM 21506804
ER
PT J
AU Fontanella, JE
Fish, FE
Rybczynski, N
Nweeia, MT
Ketten, DR
AF Fontanella, Janet E.
Fish, Frank E.
Rybczynski, Natalia
Nweeia, Martin T.
Ketten, Darlene R.
TI Three-dimensional geometry of the narwhal (Monodon monoceros) flukes in
relation to hydrodynamics
SO MARINE MAMMAL SCIENCE
LA English
DT Article
ID CETACEAN FLUKES; PERFORMANCE; EFFICIENCY; MOVEMENTS; BEHAVIOR
C1 [Fontanella, Janet E.; Fish, Frank E.] W Chester Univ, Dept Biol, W Chester, PA 19383 USA.
[Rybczynski, Natalia] Canadian Museum Nat, Ottawa, ON K1P 6P4, Canada.
[Nweeia, Martin T.] Harvard Univ, Sch Dent Med, Boston, MA 02115 USA.
[Nweeia, Martin T.] Smithsonian Inst, Washington, DC 20227 USA.
[Ketten, Darlene R.] Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA.
[Ketten, Darlene R.] Harvard Univ, Sch Med, Dept Otol & Laryngol, Boston, MA 02114 USA.
RP Fish, FE (reprint author), W Chester Univ, Dept Biol, W Chester, PA 19383 USA.
EM ffish@wcupa.edu
FU National Science Foundation [IOS-0640185]; CMN; Office of Naval
Research; Harvard University
FX We are indebted to Julie Arruda and Scott Cramer of Woods Hole
Oceanographic Institution (WHOI) for assistance with transfers and CT
scanning of the narwhal flukes and for assistance from James G. Mead and
Charles W. Potter of the Marine Mammal Program of the Natural History
Museum of the Smithsonian Institution, and Lisa-Marie Leclerc and
Jaypootie Kooneeliusie. Sanja Hinic-Frlog assisted NR with
transportation of the flukes from the CMN to WHOI. Kamal Khidas and
Peter Frank (CMN) provided much help with the paper work and
accessioning. The hunters' and trappers' organization of Qikiqtarjuaq
are gratefully acknowledged. We are extremely grateful to Kristin Laidre
for providing information on narwhals, which aided in the analysis of
our data. The transport of all materials was in accordance with CITES
permits. This work was funded in part by grants from the National
Science Foundation (IOS-0640185) to FEF, by CMN funding to NR, by the
Office of Naval Research to DRK, and by Harvard University to MTN.
NR 28
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U1 3
U2 19
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0824-0469
EI 1748-7692
J9 MAR MAMMAL SCI
JI Mar. Mamm. Sci.
PD OCT
PY 2011
VL 27
IS 4
BP 889
EP 898
DI 10.1111/j.1748-7692.2010.00439.x
PG 10
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 834DC
UT WOS:000295938200020
ER
PT J
AU Huang, L
Shcherbakov, RV
AF Huang, Lei
Shcherbakov, Roman V.
TI Faraday conversion and rotation in uniformly magnetized relativistic
plasmas
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE plasmas; polarization; radiation mechanisms: general; radiative
transfer; Galaxy: centre
ID SAGITTARIUS-A-ASTERISK; SYNCHROTRON RADIATION; CIRCULAR-POLARIZATION;
LINEAR-POLARIZATION; RESPONSE TENSOR; ACCRETION FLOW; THERMAL PLASMA;
MODELS
AB We provide precise fitting formulae for Faraday conversion and rotation coefficients in uniformly magnetized relativistic plasmas. The formulae are immediately applicable to rotation measure and circular polarization (CP) production in jets and hot accretion flows. We show the recipe and results for arbitrary isotropic particle distributions, in particular thermal and power law. The exact Faraday conversion coefficient is found to approach zero with the increasing particle energy. The non-linear corrections of Faraday conversion and rotation coefficients are found essential for reliable CP interpretation of Sagittarius A*.
C1 [Huang, Lei] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China.
[Huang, Lei] Chinese Acad Sci, Key Lab Radio Astron, Shanghai 200030, Peoples R China.
[Shcherbakov, Roman V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Huang, L (reprint author), Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China.
EM muduri@shao.ac.cn
RI he, shuyi/K-2082-2014
FU National Natural Science Foundation of China [10625314, 10633010,
10821302]; Chinese Academy of Sciences [KJCX2-YW-T03]; National Key
Basic Research Development Program of China [2007CB815405]; CAS/SAFEA;
China Postdoctoral Science Foundation [20090450822]; Academia Sinica;
NASA [NNX08AX04H, NNX11AE16G]
FX The authors are grateful to Prof. Makoto Inoue, Dr Rohta Takahashi and
Prof. Ramesh Narayan for useful suggestions. The comments of the
anonymous referee helped us to improve the presentation of findings.
This work was supported in part by the National Natural Science
Foundation of China (grants 10625314, 10633010 and 10821302), the
Knowledge Innovation Program of the Chinese Academy of Sciences (Grant
No. KJCX2-YW-T03), the National Key Basic Research Development Program
of China (No. 2007CB815405) and the CAS/SAFEA International Partnership
Program for Creative Research Teams. LH acknowledges the support by the
China Postdoctoral Science Foundation (grant 20090450822) and Regular
Postdoctoral Research Fellowship in Academia Sinica. RVS acknowledges
the support by NASA grants NNX08AX04H and NNX11AE16G.
NR 25
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U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 416
IS 4
BP 2574
EP 2592
DI 10.1111/j.1365-2966.2011.19207.x
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 829OJ
UT WOS:000295592600015
ER
PT J
AU O'Sullivan, E
Worrall, DM
Birkinshaw, M
Trinchieri, G
Wolter, A
Zezas, A
Giacintucci, S
AF O'Sullivan, E.
Worrall, D. M.
Birkinshaw, M.
Trinchieri, G.
Wolter, A.
Zezas, A.
Giacintucci, S.
TI Interaction between the intergalactic medium and central radio source in
the NGC 4261 group of galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: individual: 3C 270; galaxies: individual:
NGC4261; intergalactic medium; X-rays: galaxies
ID DEEP CHANDRA OBSERVATION; X-RAY LUMINOSITY; ACTIVE GALACTIC NUCLEUS;
HUBBLE-SPACE-TELESCOPE; XMM-NEWTON OBSERVATION; ELLIPTIC GALAXIES;
STAR-FORMATION; HOT GAS; BLACK-HOLE; JET POWER
AB Using observations from the Chandra and XMM-Newton X-ray observatories, we examine the interaction between the intragroup medium and central radio source in the nearby NGC 4261 galaxy group. We confirm the presence of cavities associated with the radio lobes and estimate their enthalpy to be similar to 2.4 x 10(58) erg. The mechanical power output of the jets is >= 10(43) erg s(-1), at least a factor of 60 greater than the cooling luminosity in the region the lobes inhabit. We identify rims of compressed gas enclosing the lobes, but find no statistically significant temperature difference between them and their surroundings, suggesting that the lobe expansion velocity is approximately sonic (M <= 1.05). The apparent pressure of the radio lobes, based on the synchrotron minimum energy density argument, is a factor of 5 lower than that of the intragroup medium. Pressure balance could be achieved if the entrainment of thermal gas provided additional non-radiating particles in the lobe plasma, but the energy required to heat these particles would be similar to 20 per cent of the mechanical energy output of the radio source. NGC 4261 has a relatively compact cool core, which should probably be categorized as a galactic corona. The corona is capable of fuelling the active nucleus for considerably longer than the inferred source lifetime, but can be only inefficiently heated by the active galactic nucleus (AGN) or conduction. The expansion of the radio lobes has affected the structure of the gas in the galaxy, compressing and moving the material of the corona without causing significant shock heating, and expelling gas from the immediate neighbourhood of the jets. We discuss the possible implications of this environment for the duration of the AGN outburst and consider mechanisms which might lead to the cessation of nuclear activity.
C1 [O'Sullivan, E.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[O'Sullivan, E.; Zezas, A.; Giacintucci, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Worrall, D. M.; Birkinshaw, M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Trinchieri, G.; Wolter, A.] Osserv Astron Brera, I-20121 Milan, Italy.
[Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece.
[Zezas, A.] Fdn Res & Technol Hela, IESL, Iraklion 7110, Greece.
[Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP O'Sullivan, E (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
EM ejos@star.sr.bham.ac.uk
RI Zezas, Andreas/C-7543-2011;
OI Zezas, Andreas/0000-0001-8952-676X; Wolter, Anna/0000-0001-5840-9835;
O'Sullivan, Ewan/0000-0002-5671-6900; Trinchieri,
Ginevra/0000-0002-0227-502X
FU National Aeronautics and Space Administration [G08-9094X, NAS8-03060];
ESA Member States; NASA; European Community under the Marie Curie
Research Training Network; EU [206469]; Agenzia Spaziale Italiana
[ASI-INAF I/009/10/0]
FX The authors thank the anonymous referee for several useful suggestions,
and P. Bonfini for providing optical data for NGC 4261. EO'S thanks A.
Sanderson for useful discussions of the X-ray analysis. Support for this
work was provided by the National Aeronautics and Space Administration
through Chandra Award Number G08-9094X issued by the Chandra X-ray
Observatory Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of the National Aeronautics and Space
Administration under contract NAS8-03060. This work is partially based
on observations obtained with XMM-Newton, an ESA science mission with
instruments and contributions directly funded by ESA Member States and
NASA. This work has used data from the VLA. EO'S acknowledges the
support of the European Community under the Marie Curie Research
Training Network. Space Astrophysics in Crete is partly supported by EU
FP7 Capacities GA No. 206469. GT and AW acknowledge support from the
Agenzia Spaziale Italiana through grant ASI-INAF I/009/10/0. We
acknowledge the usage of the HyperLeda data base
(http://leda.univ-lyon1.fr).
NR 98
TC 18
Z9 18
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD OCT
PY 2011
VL 416
IS 4
BP 2916
EP 2931
DI 10.1111/j.1365-2966.2011.19239.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 829OJ
UT WOS:000295592600039
ER
PT J
AU Toscano, MA
Peltier, WR
Drummond, R
AF Toscano, Marguerite A.
Peltier, W. Richard
Drummond, Rosemarie
TI ICE-5G and ICE-6G models of postglacial relative sea-level history
applied to the Holocene coral reef record of northeastern St Croix,
U.S.V.I.: investigating the influence of rotational feedback on GIA
processes at tropical latitudes
SO QUATERNARY SCIENCE REVIEWS
LA English
DT Article
DE Holocene sea-level rise; St. Croix; USVI; Coral reef record; Geophysical
sea-level models; Rotational feedback; Latitudinal extent of proglacial
forebulge
ID GLACIAL-ISOSTATIC-ADJUSTMENT; VIRGIN-ISLANDS; PUERTO-RICO; MANTLE
VISCOSITY; VM2 MODEL; EARTH; ATLANTIC; MAXIMUM; BARBADOS; PLATFORM
AB Fossil coral reefs along the northeastern coast of St Croix in the Caribbean Sea provide an 8000 year record of dated and interpreted Holocene sea-level change. We herein compare this record with the predictions of models of glacio-hydro-isostatic adjustment for St Croix and for additional sites at similar latitudes in the Greater and Lesser Antilles region. RSL predictions are based upon the model ICE-5G (VM2), and with a modified model ICE-6G (VM5A), both including and excluding the influence of rotational feedback. Misfits between the modeled sea levels and the local geologic data are most apparent for models without rotational feedback, particularly in the prediction of a +2 to +4 m unsupported mid-Holocene misfit at similar to 4 ka, as well as a small-amplitude highstand that extends from 2.5 to 1.5 ka. Incorporation of the influence of rotational feedback provides the best fit to the data, largely eliminating the unsupported mid-Holocene misfit between the data field and the sea-level histories predicted by the models without rotational feedback, and fitting data older than 5 kyr more closely than a previously published latitudinally-averaged sea-level curve for the western Atlantic. The St Croix data therefore demonstrate that rotational influence extends at least 27 degrees further south from its 45 degrees N mid-latitude extremum along the US east coast, and identifies tropical latitudes as influenced by proglacial forebulge collapse. Implications for reef-based sea-level reconstruction include the ability to accurately model sea levels at specific tropical sites with partial Holocene chronologies using the ICE-6G (VM5A) model with rotational feedback. Latitudinally-averaged sea-level curves are therefore of limited use in understanding the relative importance of contributing physical influences on postglacial sea-level history. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Toscano, Marguerite A.] NMNH, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA.
[Peltier, W. Richard; Drummond, Rosemarie] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
RP Toscano, MA (reprint author), NMNH, Smithsonian Inst, Dept Paleobiol, POB 37012,MRC-121, Washington, DC 20013 USA.
EM toscanom@si.edu; peltier@atmosp.physics.utoronto.ca;
rmarie@atmosp.physics.utoronto.ca
RI Peltier, William/A-1102-2008
FU NSF [0921879]; Smithsonian Institution, Department of Paleobiology;
Canadian Foundation for Climate and Atmospheric Sciences; consortium of
Canadian universities; NSERC [A9627]
FX NSF grant 0921879 and the Smithsonian Institution, Department of
Paleobiology provided support to MAT. This paper is a contribution to
the work of the Polar Climate Stability Network which has been sponsored
by the Canadian Foundation for Climate and Atmospheric Sciences and by a
consortium of Canadian universities as well as NSERC Discovery Grant
A9627 to WRP. Computations have been performed on the SciNet facility
for High Performance Computation which an element of the Compute Canada
HPC platform. Ian Macintyre, Ian Shennan and one anonymous reviewer
provided important assistance in improving the manuscript.
NR 70
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U1 0
U2 10
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0277-3791
J9 QUATERNARY SCI REV
JI Quat. Sci. Rev.
PD OCT
PY 2011
VL 30
IS 21-22
BP 3032
EP 3042
DI 10.1016/j.quascirev.2011.07.018
PG 11
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 830NK
UT WOS:000295663500012
ER
PT J
AU Hintz, E
AF Hintz, Eric
TI Edison's Electric Light: The Art of Invention
SO TECHNOLOGY AND CULTURE
LA English
DT Book Review
C1 [Hintz, Eric] Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA.
RP Hintz, E (reprint author), Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 1
U2 2
PU JOHNS HOPKINS UNIV PRESS
PI BALTIMORE
PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD
21218-4363 USA
SN 0040-165X
J9 TECHNOL CULT
JI Technol. Cult.
PD OCT
PY 2011
VL 52
IS 4
BP 829
EP 831
PG 3
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 836MW
UT WOS:000296116800022
ER
PT J
AU Stine, JK
AF Stine, Jeffrey K.
TI The Nature of New York: An Environmental History of the Empire State
SO TECHNOLOGY AND CULTURE
LA English
DT Book Review
C1 [Stine, Jeffrey K.] Natl Museum Amer Hist, Smithsonian Inst, Div Med & Sci, Washington, DC 20560 USA.
RP Stine, JK (reprint author), Natl Museum Amer Hist, Smithsonian Inst, Div Med & Sci, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU JOHNS HOPKINS UNIV PRESS
PI BALTIMORE
PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD
21218-4363 USA
SN 0040-165X
J9 TECHNOL CULT
JI Technol. Cult.
PD OCT
PY 2011
VL 52
IS 4
BP 838
EP 840
PG 3
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 836MW
UT WOS:000296116800027
ER
PT J
AU Moini, M
Klauenberg, K
Ballard, M
AF Moini, Mehdi
Klauenberg, Kathryn
Ballard, Mary
TI Dating Silk By Capillary Electrophoresis Mass Spectrometry
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID ASPARTIC-ACID RACEMIZATION; AMINO-ACIDS; CHROMATOGRAPHY; PRESERVATION
AB A new capillary electrophoresis mass spectrometry (CE-MS) technique is introduced for age estimation of silk textiles based on amino acid racemization rates. With an L to D conversion half-life of similar to 2500 years for silk (B. mari) aspartic acid, the technique is capable of dating silk textiles ranging in age from several decades to a few-thousand-years-old. Analysis required only similar to 100 mu g or less of silk fiber. Except for a 2 h acid hydrolysis at 110 degrees C, no other sample preparation is required. The CE-MS analysis takes similar to 20 min, consumes only nanoliters of the amino acid mixture, and provides both amino acid composition profiles and D/L ratios for similar to 11 amino acids.
C1 [Moini, Mehdi; Klauenberg, Kathryn; Ballard, Mary] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
RP Moini, M (reprint author), Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM MoiniM@si.edu
FU Smithsonian's Museum Conservation Institute
FX We wish to thank the Smithsonian's Museum Conservation Institute
Director and Deputy Director, Drs. Robert J. Koestler and Paula T.
DePriest, for their support of this project. We also wish to thank
several curators and conservators who have provided expertise as well as
silk samples: Dr. Sumru Kordy and Ms. Esther Methe of the Textile
Museum; Dr. James C. Y. Watt and Ms. Joyce Denney of the Metropolitan
Museum of Art; Dr. Blythe McCarthy of the Smithsonian's Freer and Sadder
Galleries; Ms. Laura Mina of the Smithsonian Museum Conservation
Institute; Ms. Phyllis Magidson of the Museum of the City of New York;
Ms. Jennifer Jones and Ms. Suzanne Thomassen-Krauss of the National
Museum of American History; and Dr. Katja Schmitz-von Ledebur from the
Kunsthistoriches Museum, Vienna, Austria. We also wish to thank intern
Casey Kohnhorst for her assistance in proteomics analysis of silk acid
hydrolysates.
NR 31
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U2 22
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
J9 ANAL CHEM
JI Anal. Chem.
PD OCT 1
PY 2011
VL 83
IS 19
BP 7577
EP 7581
DI 10.1021/ac201746u
PG 5
WC Chemistry, Analytical
SC Chemistry
GA 825SY
UT WOS:000295303600050
PM 21913691
ER
PT J
AU Boyer, ML
Srinivasan, S
van Loon, JT
McDonald, I
Meixner, M
Zaritsky, D
Gordon, KD
Kemper, F
Babler, B
Block, M
Bracker, S
Engelbracht, CW
Hora, J
Indebetouw, R
Meade, M
Misselt, K
Robitaille, T
Sewillo, M
Shiao, B
Whitney, B
AF Boyer, Martha L.
Srinivasan, Sundar
van Loon, Jacco Th.
McDonald, Iain
Meixner, Margaret
Zaritsky, Dennis
Gordon, Karl D.
Kemper, F.
Babler, Brian
Block, Miwa
Bracker, Steve
Engelbracht, Charles W.
Hora, Joe
Indebetouw, Remy
Meade, Marilyn
Misselt, Karl
Robitaille, Thomas
Sewillo, Marta
Shiao, Bernie
Whitney, Barbara
TI SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW
METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). II. COOL EVOLVED STARS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; Magellanic Clouds; stars: AGB and post-AGB; stars:
carbon; stars: mass-loss; supergiants
ID ASYMPTOTIC GIANT BRANCH; SPITZER-SPACE-TELESCOPE; MASS-LOSS RATES; RICH
AGB-STARS; DWARF IRREGULAR GALAXIES; NEAR-INFRARED PHOTOMETRY; YOUNG
STELLAR OBJECTS; CLUSTER 47 TUCANAE; LOCAL GROUP DWARFS; EXTRINSIC
S-STARS
AB We investigate the infrared (IR) properties of cool, evolved stars in the Small Magellanic Cloud (SMC), including the red giant branch (RGB) stars and the dust-producing red supergiant (RSG) and asymptotic giant branch (AGB) stars using observations from the Spitzer Space Telescope Legacy program entitled "Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity SMC," or SAGE-SMC. The survey includes, for the first time, full spatial coverage of the SMC bar, wing, and tail regions at IR wavelengths (3.6-160 mu m). We identify evolved stars using a combination of near-IR and mid-IR photometry and point out a new feature in the mid-IR color-magnitude diagram that may be due to particularly dusty O-rich AGB stars. We find that the RSG and AGB stars each contribute approximate to 20% of the global SMC flux (extended + point-source) at 3.6 mu m, which emphasizes the importance of both stellar types to the integrated flux of distant metal-poor galaxies. The equivalent SAGE survey of the higher-metallicity Large Magellanic Cloud (SAGE-LMC) allows us to explore the influence of metallicity on dust production. We find that the SMC RSG stars are less likely to produce a large amount of dust (as indicated by the [3.6] - [8] color). There is a higher fraction of carbon-rich stars in the SMC, and these stars appear to reach colors as red as their LMC counterparts, indicating that C-rich dust forms efficiently in both galaxies. A preliminary estimate of the dust production in AGB and RSG stars reveals that the extreme C-rich AGB stars dominate the dust input in both galaxies, and that the O-rich stars may play a larger role in the LMC than in the SMC.
C1 [Boyer, Martha L.; Meixner, Margaret; Gordon, Karl D.; Shiao, Bernie] STScI, Baltimore, MD 21218 USA.
[Srinivasan, Sundar] CNRS, Inst Astrophys Paris, UPR 341, F-75014 Paris, France.
[van Loon, Jacco Th.] Univ Keele, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[McDonald, Iain; Kemper, F.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Zaritsky, Dennis; Block, Miwa; Engelbracht, Charles W.; Misselt, Karl] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Babler, Brian; Bracker, Steve; Meade, Marilyn; Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Hora, Joe; Robitaille, Thomas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Sewillo, Marta] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Boyer, ML (reprint author), STScI, Baltimore, MD 21218 USA.
EM mboyer@stsci.edu
RI Kemper, Francisca/D-8688-2011;
OI Kemper, Francisca/0000-0003-2743-8240; Babler,
Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650; Robitaille,
Thomas/0000-0002-8642-1329
FU NASA [1309827, 1340964]
FX This work is supported by NASA via JPL contracts 1309827 and 1340964. We
thank the anonymous referee for thoughtful remarks.
NR 144
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2011
VL 142
IS 4
AR 103
DI 10.1088/0004-6256/142/4/103
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500007
ER
PT J
AU Brown, TM
Latham, DW
Everett, ME
Esquerdo, GA
AF Brown, Timothy M.
Latham, David W.
Everett, Mark E.
Esquerdo, Gilbert A.
TI KEPLER INPUT CATALOG: PHOTOMETRIC CALIBRATION AND STELLAR CLASSIFICATION
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE catalogs; methods: data analysis; surveys; techniques: photometric
ID DIGITAL SKY SURVEY; DATA RELEASE; STARS; EXTINCTION; SPECTRA; SYSTEM;
RADIUS; FIELD; MASS; M67
AB We describe the photometric calibration and stellar classification methods used by the Stellar Classification Project to produce the Kepler Input Catalog (KIC). The KIC is a catalog containing photometric and physical data for sources in the Kepler mission field of view; it is used by the mission to select optimal targets. Four of the visible-light (g, r, i, z) magnitudes used in the KIC are tied to Sloan Digital Sky Survey magnitudes; the fifth (D51) is an AB magnitude calibrated to be consistent with Castelli & Kurucz (CK) model atmosphere fluxes. We derived atmospheric extinction corrections from hourly observations of secondary standard fields within the Kepler field of view. For these filters and extinction estimates, repeatability of absolute photometry for stars brighter than magnitude 15 is typically 2%. We estimated stellar parameters {T(eff), log(g), log(Z), E(B-V)} using Bayesian posterior probability maximization to match observed colors to CK stellar atmosphere models. We applied Bayesian priors describing the distribution of solar-neighborhood stars in the color-magnitude diagram, in log(Z), and in height above the galactic plane. Several comparisons with samples of stars classified by other means indicate that for 4500 K <= T(eff) <= 6500 K, our classifications are reliable within about +/- 200 K and 0.4 dex in log(g) for dwarfs, with somewhat larger log(g) uncertainties for giants. It is difficult to assess the reliability of our log(Z) estimates, but there is reason to suspect that it is poor, particularly at extreme T(eff). Comparisons between the CK models and observed colors are generally satisfactory with some exceptions, notably for stars cooler than 4500 K. Of great importance for the Kepler mission, for T(eff) <= 5400 K, comparison with asteroseismic results shows that the distinction between main-sequence stars and giants is reliable with about 98% confidence. Larger errors in log(g) occur for warmer stars, for which our filter set provides inadequate gravity diagnostics. The KIC is available through the MAST data archive.
C1 [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Latham, David W.; Esquerdo, Gilbert A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85721 USA.
RP Brown, TM (reprint author), Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
EM tbrown@lcogt.net; latham@cfa.harvard.edu; everett@noao.edu;
gesquerd@cfa.harvard.edu
FU NASA [NNX10AG02A]; National Science Foundation; NASA with the
Smithsonian Astrophysical Observatory [NCC-1390]
FX We are grateful to the Mt. Hopkins support and observing staff,
especially Carl Hergenrother, for his tireless work obtaining the
necessary observations. We also thank Dave Monet, for his indispensable
help in implementing the KIC astrometry methods, and for federating the
SCP with other catalogs that carry essential information. We thank Steve
Howell, for helping to define our photometric approach in the project's
early days. We thank Geoff Marcy, Howard Isaacson, Debra Fischer, Bill
Cochran, Sam Quinn, Lars Buchhave, Mike Endl, and Phillip MacQueen for
the use of their spectra and spectral analysis of Kepler target stars.
We also thank Saskia Hekker, Bill Chaplin, Ronald Gilliland, and dozens
of members of the Kepler Asteroseismic Consortium for making their
seismic data available before publication. We are deeply grateful to the
Kepler Science Team and everyone connected with the Kepler mission, for
keeping the mission running smoothly, and for providing the amazing
Kepler photometric data, the promise of which was the inspiration for
the current work. We thank Jeffrey Scargle for a careful reading of an
early version of this work, and Don Kolinski for extensive software
development help. T.M.B. acknowledges support from NASA Grant Number
NNX10AG02A, and thanks HAO/NCAR and Las Cumbres Observatory Global
Telescope for patience and support while this work was being done. The
National Center for Atmospheric Research is supported by the National
Science Foundation. We are grateful to the Kepler mission for partial
support of the photometric observations under NASA Cooperative Agreement
NCC-1390 with the Smithsonian Astrophysical Observatory.
NR 37
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2011
VL 142
IS 4
AR 112
DI 10.1088/0004-6256/142/4/112
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500016
ER
PT J
AU Etxaluze, M
Smith, HA
Tolls, V
Stark, AA
Gonzalez-Alfonso, E
AF Etxaluze, M.
Smith, Howard A.
Tolls, V.
Stark, A. A.
Gonzalez-Alfonso, E.
TI THE GALACTIC CENTER IN THE FAR-INFRARED
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE dust, extinction; Galaxy: center; infrared: ISM; ISM: individual objects
(Sgr A*)
ID CIRCUMNUCLEAR DISK; MOLECULAR CLOUDS; TEMPERATURE-DEPENDENCE; STELLAR
ORBITS; STAR-FORMATION; CENTER REGION; BLACK-HOLE; ISO-LWS; DUST; GALAXY
AB We analyze the far-infrared dust emission from the Galactic center region, including the circumnuclear disk (CND) and other structures, using Herschel PACS and SPIRE photometric observations. These Herschel data are complemented by unpublished observations by the Infrared Space Observatory Long Wavelength Spectrometer (ISO-LWS), which used parallel mode scans to obtain photometric images of the region with a larger beam than Herschel but with a complementary wavelength coverage and more frequent sampling with 10 detectors observing at 10 different wavelengths in the range from 46 mu m to 180 mu m, where the emission peaks. We also include data from the Midcourse Space Experiment at 21.3 mu m for completeness. We model the combined ISO-LWS continuum plus Herschel PACS and SPIRE photometric data toward the central 2 pc in Sagittarius A* (Sgr A*), a region that includes the CND. We find that the far-infrared spectral energy distribution is best represented by a continuum that is the sum of three gray body curves from dust at temperatures of 90, 44.5, and 23 K. We obtain temperature and molecular hydrogen column density maps of the region. We estimate the mass of the inner part of the CND to be similar to 5.0 x 10(4) M(circle dot), with luminosities: L(cavity) similar to 2.2 x 10(6) L(circle dot) and LCND similar to 1.5 x 10(6) L(circle dot) in the central 2 pc radius around Sgr A*. We find from the Herschel and ISO data that the cold component of the dust dominates the total dust mass, with a contribution of similar to 3.2 x 10(4) M(circle dot); this important cold material had escaped the notice of earlier studies that relied on shorter wavelength observations. The hotter component disagrees with some earlier estimates, but is consistent with measured gas temperatures and with models that imply shock heating or turbulent effects are at work. We find that the dust grain sizes apparently change widely across the region, perhaps in response to the temperature variations, and we map that distribution.
C1 [Etxaluze, M.; Smith, Howard A.; Tolls, V.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gonzalez-Alfonso, E.] Univ Alcala de Henares, Alcala De Henares 28801, Spain.
[Gonzalez-Alfonso, E.] CfA, Alcala De Henares 28801, Spain.
RP Etxaluze, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM metxaluz@cfa.harvard.edu
OI Stark, Antony/0000-0002-2718-9996
FU NASA [NNX10AD83G]
FX We thank the referee for his or her careful reading of the paper, and
for the useful comments made. We are very grateful to Tanya Lim for her
suggestions on the treatment of the ISO-LWS parallel mode data. This
work was supported in part by NASA Grant NNX10AD83G. The ISO-LWS LIA is
a joint development of the ISO-LWS Instrument Team at Rutherford
Appleton Laboratory and the Infrared Processing and Analysis Center
(IPAC/Caltech, USA). HIPE is a joint development by the Herschel Science
Ground Segment Consortium consisting of ESA, the NASA Herschel Science
Center, and the HIFI, PACS, and SPIRE consortia.
NR 47
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD OCT
PY 2011
VL 142
IS 4
AR 134
DI 10.1088/0004-6256/142/4/134
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500038
ER
PT J
AU Fernandez-Lopez, M
Girart, JM
Curiel, S
Gomez, Y
Ho, PTP
Patel, N
AF Fernandez-Lopez, M.
Girart, J. M.
Curiel, S.
Gomez, Y.
Ho, P. T. P.
Patel, N.
TI A ROTATING MOLECULAR DISK TOWARD IRAS 18162-2048, THE EXCITING SOURCE OF
HH 80-81
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (GGD27, IRAS 18162-2048, HH 80-81); stars:
formation; submillimeter: ISM
ID HERBIG-HARO OBJECTS; MASSIVE STAR-FORMATION; ULTRACOMPACT HII-REGIONS;
LARGE PROPER MOTIONS; THERMAL RADIO JET; HOT CORES; INTERFEROMETRIC
OBSERVATIONS; MILLIMETER OBSERVATIONS; COLLISIONAL FORMATION;
SUBMILLIMETER ARRAY
AB We present several molecular line emission arcsecond and subarcsecond observations obtained with the Submillimeter Array in the direction of the massive protostar IRAS 18162-2048, the exciting source of HH 80-81. The data clearly indicate the presence of a compact (radius approximate to 425-850 AU) SO2 structure, enveloping the more compact (radius less than or similar to 150 AU) 1.4 mm dust emission (reported in a previous paper). The emission spatially coincides with the position of the prominent thermal radio jet which terminates at the HH 80-81 and HH 80N Herbig-Haro objects. Furthermore, the molecular emission is elongated in the direction perpendicular to the axis of the thermal radio jet, suggesting a disk-like structure. We derive a total dynamic mass (disk-like structure and protostar) of 11-15 M-circle dot. The SO2 spectral line data also allow us to constrain the structure temperature between 120 and 160 K and the volume density greater than or similar to 2 x 10(9) cm(-3). We also find that such a rotating flattened system could be unstable due to gravitational disturbances. The data from (CO)-O-17 line emission show a dense core within this star-forming region. Additionally, the H2CO and SO emissions appear clumpy and trace the disk-like structure, a possible interaction between a molecular core and the outflows, and in part, the cavity walls excavated by the thermal radio jet.
C1 [Fernandez-Lopez, M.; Curiel, S.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Girart, J. M.] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Bellaterra 08193, Catalunya, Spain.
[Gomez, Y.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico.
[Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Ho, P. T. P.; Patel, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Fernandez-Lopez, M (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico.
EM manferna@gmail.com; girart@ieec.cat; scuriel@astroscu.unam.mx;
y.gomez@astrosmo.unam.mx
RI Girart, Josep/O-1638-2014
OI Girart, Josep/0000-0002-3829-5591
FU DGAP-UNAM, Mexico; Spanish MICINN [AYA2008-06189-C03]; Catalan AGAUR
[2009SGR1172]; CONACyT, Mexico [60581]; CONACyT [80769, 49947-F]
FX We thank all members of the SMA staff who made these observations
possible. M.F.L. acknowledges financial support from DGAP-UNAM, Mexico.
J.M.G. is supported by the Spanish MICINN AYA2008-06189-C03 and the
Catalan AGAUR 2009SGR1172 grants. S.C. and M.F.L. acknowledge support
from CONACyT grant 60581, Mexico. S.C. and M.F.L. thank the hospitality
of the Institut de Ciencies de l'Espai (CSIC-IEEC), Bellaterra,
Catalunya, Spain. Y.G. acknowledges support from CONACyT grants 80769
and 49947-F.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD OCT
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VL 142
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AR 97
DI 10.1088/0004-6256/142/4/97
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500001
ER
PT J
AU Geller, MJ
Diaferio, A
Kurtz, MJ
AF Geller, Margaret J.
Diaferio, Antonaldo
Kurtz, Michael J.
TI MAPPING THE UNIVERSE: THE 2010 RUSSELL LECTURE
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: clusters: general; large-scale
structure of universe
ID FIBER-FED SPECTROGRAPH; REGION NEARBY SURVEY; DIGITAL SKY SURVEY; GALAXY
CLUSTERS; RICH CLUSTERS; MASS PROFILES; REDSHIFT SURVEY; INFALL
PATTERNS; HECTOSPEC; EVOLUTION
AB Redshift surveys are a powerful tool of modern cosmology. We discuss two aspects of their power to map the distribution of mass and light in the universe: (1) measuring the mass distribution extending into the infall regions of rich clusters and (2) applying deep redshift surveys to the selection of clusters of galaxies and to the identification of very large structures (Great Walls). We preview the HectoMAP project, a redshift survey with median redshift z = 0.34 covering 50 deg(2) to r = 21. We emphasize the importance and power of spectroscopy for exploring and understanding the nature and evolution of structure in the universe.
C1 [Geller, Margaret J.; Kurtz, Michael J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy.
[Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM mgeller@cfa.harvard.edu; adiaferio@cfa.harvard.edu;
mkurtz@cfa.harvard.edu
RI KURTZ, Michael /B-3890-2009;
OI Kurtz, Michael/0000-0002-6949-0090
FU Smithsonian Institution; Smithsonian Fellowship; INFN [PD51];
[2008NR3EBK]
FX The Smithsonian Institution supports the research of Margaret Geller and
Michael Kurtz, and during 2010-2011, a Smithsonian Fellowship partially
supported Antonaldo Diaferio. INFN grant PD51 and the PRIN-MIUR-2008
grant 2008NR3EBK also support Antonaldo Diaferio.
NR 51
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
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DI 10.1088/0004-6256/142/4/133
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SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500037
ER
PT J
AU Gordon, KD
Meixner, M
Meade, MR
Whitney, B
Engelbracht, C
Bot, C
Boyer, ML
Lawton, B
Sewilo, M
Babler, B
Bernard, JP
Bracker, S
Block, M
Blum, R
Bolatto, A
Bonanos, A
Harris, J
Hora, JL
Indebetouw, R
Misselt, K
Reach, W
Shiao, B
Tielens, X
Carlson, L
Churchwell, E
Clayton, GC
Chen, CHR
Cohen, M
Fukui, Y
Gorjian, V
Hony, S
Israel, FP
Kawamura, A
Kemper, F
Leroy, A
Li, A
Madden, S
Marble, AR
McDonald, I
Mizuno, A
Mizuno, N
Muller, E
Oliveira, JM
Olsen, K
Onishi, T
Paladini, R
Paradis, D
Points, S
Robitaille, T
Rubin, D
Sandstrom, K
Sato, S
Shibai, H
Simon, JD
Smith, LJ
Srinivasan, S
Vijh, U
Van Dyk, S
van Loon, JT
Zaritsky, D
AF Gordon, K. D.
Meixner, M.
Meade, M. R.
Whitney, B.
Engelbracht, C.
Bot, C.
Boyer, M. L.
Lawton, B.
Sewilo, M.
Babler, B.
Bernard, J. -P.
Bracker, S.
Block, M.
Blum, R.
Bolatto, A.
Bonanos, A.
Harris, J.
Hora, J. L.
Indebetouw, R.
Misselt, K.
Reach, W.
Shiao, B.
Tielens, X.
Carlson, L.
Churchwell, E.
Clayton, G. C.
Chen, C. -H. R.
Cohen, M.
Fukui, Y.
Gorjian, V.
Hony, S.
Israel, F. P.
Kawamura, A.
Kemper, F.
Leroy, A.
Li, A.
Madden, S.
Marble, A. R.
McDonald, I.
Mizuno, A.
Mizuno, N.
Muller, E.
Oliveira, J. M.
Olsen, K.
Onishi, T.
Paladini, R.
Paradis, D.
Points, S.
Robitaille, T.
Rubin, D.
Sandstrom, K.
Sato, S.
Shibai, H.
Simon, J. D.
Smith, L. J.
Srinivasan, S.
Vijh, U.
Van Dyk, S.
van Loon, J. Th
Zaritsky, D.
TI SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW
METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). I. OVERVIEW
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: individual (SMC)
ID SPITZER-SPACE-TELESCOPE; MULTIBAND IMAGING PHOTOMETER; INFRARED ARRAY
CAMERA; MASS-LOSS RETURN; SPECTRAL IRRADIANCE CALIBRATION; YOUNG STELLAR
OBJECTS; GIANT BRANCH STARS; 24 MU-M; ABSOLUTE CALIBRATION; EVOLVED
STARS
AB The Small Magellanic Cloud (SMC) provides a unique laboratory for the study of the lifecycle of dust given its low metallicity (similar to 1/5 solar) and relative proximity (similar to 60 kpc). This motivated the SAGE-SMC (Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity Small Magellanic Cloud) Spitzer Legacy program with the specific goals of studying the amount and type of dust in the present interstellar medium, the sources of dust in the winds of evolved stars, and how much dust is consumed in star formation. This program mapped the full SMC (30 deg(2)) including the body, wing, and tail in seven bands from 3.6 to 160 mu m using IRAC and MIPS on the Spitzer Space Telescope. The data were reduced and mosaicked, and the point sources were measured using customized routines specific for large surveys. We have made the resulting mosaics and point-source catalogs available to the community. The infrared colors of the SMC are compared to those of other nearby galaxies and the 8 mu m/24 mu m ratio is somewhat lower than the average and the 70 mu m/160 mu m ratio is somewhat higher than the average. The global infrared spectral energy distribution (SED) shows that the SMC has approximately 1/3 the aromatic emission/polycyclic aromatic hydrocarbon abundance of most nearby galaxies. Infrared color-magnitude diagrams are given illustrating the distribution of different asymptotic giant branch stars and the locations of young stellar objects. Finally, the average SED of H II/star formation regions is compared to the equivalent Large Magellanic Cloud average H II/star formation region SED. These preliminary results will be expanded in detail in subsequent papers.
C1 [Gordon, K. D.; Meixner, M.; Boyer, M. L.; Lawton, B.; Shiao, B.; Smith, L. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Meade, M. R.; Whitney, B.; Babler, B.; Bracker, S.; Churchwell, E.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Whitney, B.] Space Sci Inst, Boulder, CO 80301 USA.
[Engelbracht, C.; Block, M.; Misselt, K.; Marble, A. R.; Zaritsky, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bot, C.] Univ Strasbourg, Ctr Donnees Astron Strasbourg CDS, UMR 7550, F-67000 Strasbourg, France.
[Sewilo, M.; Carlson, L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bernard, J. -P.] Univ Toulouse, UPS, CESR, F-31028 Toulouse 4, France.
[Blum, R.; Harris, J.; Olsen, K.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Bolatto, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bonanos, A.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece.
[Hora, J. L.; Robitaille, T.] Harvard Smithsonian, CfA, Cambridge, MA 02138 USA.
[Indebetouw, R.; Reach, W.; Paladini, R.; Paradis, D.; Van Dyk, S.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Indebetouw, R.; Leroy, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Tielens, X.; Israel, F. P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
[Chen, C. -H. R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Cohen, M.] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Fukui, Y.; Kawamura, A.; Mizuno, A.; Mizuno, N.; Muller, E.; Onishi, T.; Sato, S.; Shibai, H.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Gorjian, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hony, S.; Madden, S.; Rubin, D.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Kawamura, A.; Muller, E.] Natl Astron Observ Japan, ALMA J Project Off, Tokyo 1818588, Japan.
[Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Kemper, F.; van Loon, J. Th] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Li, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Marble, A. R.] Natl Solar Observ, Tucson, AZ 85719 USA.
[McDonald, I.; Oliveira, J. M.] Univ Keele, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England.
[Points, S.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile.
[Sandstrom, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Simon, J. D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Smith, L. J.] European Space Agcy, Res & Sci Support Dept, Baltimore, MD 21218 USA.
[Srinivasan, S.] Inst Astrophys, F-75014 Paris, France.
[Vijh, U.] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA.
RP Gordon, KD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RI Kemper, Francisca/D-8688-2011; Bonanos, Alceste/K-5392-2013;
OI Kemper, Francisca/0000-0003-2743-8240; Bonanos,
Alceste/0000-0003-2851-1905; Bot, Caroline/0000-0001-6118-2985; Babler,
Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650; Reach,
William/0000-0001-8362-4094; Robitaille, Thomas/0000-0002-8642-1329; Van
Dyk, Schuyler/0000-0001-9038-9950
FU NASA [1340964, 1407]
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under NASA contract 1407. Support for
this work was provided by NASA through Contract Number 1340964 issued by
JPL/Caltech.
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SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
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DI 10.1088/0004-6256/142/4/102
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500006
ER
PT J
AU Petit, JM
Kavelaars, JJ
Gladman, BJ
Jones, RL
Parker, JW
Van Laerhoven, C
Nicholson, P
Mars, G
Rousselot, P
Mousis, O
Marsden, B
Bieryla, A
Taylor, M
Ashby, MLN
Benavidez, P
Bagatin, AC
Bernabeu, G
AF Petit, J-M
Kavelaars, J. J.
Gladman, B. J.
Jones, R. L.
Parker, J. Wm
Van Laerhoven, C.
Nicholson, P.
Mars, G.
Rousselot, P.
Mousis, O.
Marsden, B.
Bieryla, A.
Taylor, M.
Ashby, M. L. N.
Benavidez, P.
Campo Bagatin, A.
Bernabeu, G.
TI THE CANADA-FRANCE ECLIPTIC PLANE SURVEY-FULL DATA RELEASE: THE ORBITAL
STRUCTURE OF THE KUIPER BELT
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE Kuiper Belt: general; surveys
ID TRANS-NEPTUNIAN OBJECTS; TURBULENT PROTOPLANETARY DISKS; EXTENDED
SCATTERED DISK; SOLAR-SYSTEM; COLLISIONAL FAMILY; SIZE DISTRIBUTION;
DYNAMICAL CLASSIFICATION; LUMINOSITY FUNCTION; GLOBAL EVOLUTION;
HAWAII-TELESCOPE
AB We report the orbital distribution of the trans-Neptunian objects (TNOs) discovered during the Canada-France Ecliptic Plane Survey (CFEPS), whose discovery phase ran from early 2003 until early 2007. The follow-up observations started just after the first discoveries and extended until late 2009. We obtained characterized observations of 321 deg(2) of sky to depths in the range g similar to 23.5-24.4 AB mag. We provide a database of 169 TNOs with high-precision dynamical classification and known discovery efficiency. Using this database, we find that the classical belt is a complex region with sub-structures that go beyond the usual splitting of inner (interior to 3:2 mean-motion resonance [MMR]), main (between 3: 2 and 2: 1 MMR), and outer (exterior to 2:1 MMR). The main classical belt (a = 40-47 AU) needs to be modeled with at least three components: the "hot" component with a wide inclination distribution and two "cold" components (stirred and kernel) with much narrower inclination distributions. The hot component must have a significantly shallower absolute magnitude (H-g) distribution than the other two components. With 95% confidence, there are 8000(-1600)(+1800) objects in the main belt with H-g <= 8.0, of which 50% are from the hot component, 40% from the stirred component, and 10% from the kernel; the hot component's fraction drops rapidly with increasing Hg. Because of this, the apparent population fractions depend on the depth and ecliptic latitude of a trans-Neptunian survey. The stirred and kernel components are limited to only a portion of the main belt, while we find that the hot component is consistent with a smooth extension throughout the inner, main, and outer regions of the classical belt; in fact, the inner and outer belts are consistent with containing only hot-component objects. The H-g <= 8.0 TNO population estimates are 400 for the inner belt and 10,000 for the outer belt to within a factor of two (95% confidence). We show how the CFEPS Survey Simulator can be used to compare a cosmogonic model for the orbital element distribution to the real Kuiper Belt.
C1 [Petit, J-M; Rousselot, P.; Mousis, O.] Observ Besancon, CNRS UMR 6213, Inst UTINAM, F-25010 Besancon, France.
[Petit, J-M; Gladman, B. J.; Jones, R. L.; Van Laerhoven, C.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Kavelaars, J. J.; Jones, R. L.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Parker, J. Wm; Bieryla, A.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA.
[Van Laerhoven, C.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Nicholson, P.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Mars, G.] Observ Cote Azur, F-06304 Nice 4, France.
[Marsden, B.; Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Taylor, M.; Bernabeu, G.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada.
[Benavidez, P.; Campo Bagatin, A.] Univ Alicante, EPSA, Dept Fis Ingn Sistemas & Teoria Senal, E-03080 Alicante, Spain.
RP Petit, JM (reprint author), Observ Besancon, CNRS UMR 6213, Inst UTINAM, BP 1615, F-25010 Besancon, France.
RI Bernabeu, Guillermo/L-4703-2014; Campo Bagatin, Adriano/L-2809-2014;
OI Bernabeu, Guillermo/0000-0001-5695-0900; Campo Bagatin,
Adriano/0000-0001-9840-2216; Taylor, Matthew/0000-0003-3009-4928
FU Natural Sciences and Engineering Research Council of Canada; Canadian
Foundation for Innovation; National Research Council of Canada; NASA
[NNG04GI29G]
FX This research was supported by funding from the Natural Sciences and
Engineering Research Council of Canada, the Canadian Foundation for
Innovation, the National Research Council of Canada, and NASA Planetary
Astronomy Program NNG04GI29G. This project could not have been a success
without the dedicated staff of the Canada-France-Hawaii telescope as
well as the assistance of the skilled telescope operators at KPNO and
Mount Palomar.
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JI Astron. J.
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PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822JY
UT WOS:000295042500035
ER
PT J
AU Kokkin, DL
Brunken, S
Young, KH
Patel, NA
Gottlieb, CA
Thaddeus, P
McCarthy, MC
AF Kokkin, D. L.
Bruenken, S.
Young, K. H.
Patel, N. A.
Gottlieb, C. A.
Thaddeus, P.
McCarthy, M. C.
TI THE ROTATIONAL SPECTRA OF (SiC2)-Si-29 AND (SiC2)-Si-30
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE ISM: molecules; line: identification; molecular data; radio lines: ISM;
submillimeter: ISM
ID SILICON DICARBIDE SIC2; LINE SURVEY; MOLECULAR-SPECTROSCOPY; LABORATORY
MEASUREMENT; COLOGNE DATABASE; EXCITED-STATE; IRC+10216; ENVELOPE;
RESOLUTION; CDMS
AB The rotational spectra of (SiC2)-Si-29 and (SiC2)-Si-30, two silicon isotopic species of the abundant astronomical ring (SiC2)-Si-28, have been characterized in the millimeter band between 140 and 360 GHz in a low pressure discharge through SiH4, C2H2, and Ar. Precise rotational and centrifugal distortion constants have been derived for both species by fitting a standard asymmetric top Hamiltonian to 38 a-type transitions of (SiC2)-Si-29 and 35 of (SiC2)-Si-30; the data sets include transitions up to K-a = 8 and at least J = 16. With these new measurements in hand, the most intense radio transitions of both species either have been measured or can now be predicted to better than 1 km s(-1) in equivalent radial velocity up to 500 GHz, more than adequate accuracy for spectral line identifications in circumstellar shells of evolved carbon stars such as IRC+10216 where SiC2 is conspicuous. More than 10 new lines of (SiC2)-Si-29 and (SiC2)-Si-30 have been identified between 295 and 354 GHz in the interferometric spectral line survey of IRC+10216 with the Submillimeter Array.
C1 [Kokkin, D. L.] Univ Sydney, Sch Chem, Sydney, NSW 2006, Australia.
[Kokkin, D. L.; Bruenken, S.; Young, K. H.; Patel, N. A.; Gottlieb, C. A.; Thaddeus, P.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bruenken, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
RP Kokkin, DL (reprint author), Univ Sydney, Sch Chem, Sydney, NSW 2006, Australia.
EM dkokkin@cfa.harvard.edu
RI Brunken, Sandra/B-1880-2010;
OI Brunken, Sandra/0000-0001-7175-4828; McCarthy,
Michael/0000-0001-9142-0008
FU NASA [NNX08AE05G]; University of Sydney; Harvard College Observatory
FX This work is supported by NASA grant NNX08AE05G. D.L.K. thanks the
University of Sydney for a University Postgraduate Award. S.B. is
grateful to the Harvard College Observatory for a Menzel fellowship.
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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 OCT
PY 2011
VL 196
IS 2
AR 17
DI 10.1088/0067-0049/196/2/17
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 832XR
UT WOS:000295844500003
ER
PT J
AU Kettenring, KM
McCormick, MK
Baron, HM
Whigham, DF
AF Kettenring, Karin M.
McCormick, Melissa K.
Baron, Heather M.
Whigham, Dennis F.
TI Mechanisms of Phragmites australis invasion: feedbacks among genetic
diversity, nutrients, and sexual reproduction
SO JOURNAL OF APPLIED ECOLOGY
LA English
DT Article
DE allee effect; anthropogenic development; common reed; cross-pollination;
nitrogen; phosphorus; seed viability; superior genotypes
ID COMMON REED; CHESAPEAKE BAY; SALT MARSHES; SPARTINA-ALTERNIFLORA;
BIOLOGICAL INVASIONS; CRYPTIC INVASION; NORTH-AMERICA; PLANT; NITROGEN;
SPREAD
AB 1. A fundamental challenge to invasion ecology is to determine what factors cause an exotic species to spread rapidly long after the initial introduction. The increase of a resource (e. g. nitrogen) could trigger an expansion, but in other instances, species have overcome biological limitations (e. g. an Allee effect) like accumulating sufficient genetic diversity for successful reproduction. Understanding the ecological mechanisms governing plant invasions, such as nutrient enrichment or Allee effects, can be used to improve invasive plant management.
2. We used the invasive, introduced grass Phragmites australis as a model to evaluate the role of nutrient enrichment and Allee effects in invasion. Based on recent studies that demonstrated the importance of sexual reproduction in this plant's spread, we chose to focus our efforts on reproductive output. We examined the effects of patch-level genetic diversity on viable seed production across watersheds of the Chesapeake Bay, USA, with differing levels of anthropogenic development (a proxy for nutrient enrichment). In an outdoor mesocosm experiment, we treated Phragmites plants originating from forested and developed watersheds with elevated vs. ambient nutrients and cross vs. self-pollination and determined the effects on viable seed, floret and inflorescence production.
3. The proportion of viable seeds produced at field sites varied widely and was not directly related to watershed development. Instead, seed viability was positively related to patch-level genetic diversity, and patches in more developed watersheds had higher genetic diversity. Also, plants in larger patches produced a higher proportion of viable seeds. In the mesocosm experiment, seed viability was substantially higher for out-crossed plants. Elevated nutrients resulted in greater floret and inflorescence production, particularly for plants originating from developed vs. forested watersheds.
4. These findings have important management implications: small populations should be controlled before they accumulate sufficient genetic variation for prolific viable seed production, and landscape-scale nutrient management could further limit reproductive output.
5. Synthesis and applications. Our research shows how nutrient enrichment and a weak Allee effect can interact across multiple scales to impact invasion success and how understanding the ecological mechanisms governing plant invasions can be used to better inform invasive plant management.
C1 [Kettenring, Karin M.] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA.
[Kettenring, Karin M.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA.
[Kettenring, Karin M.; McCormick, Melissa K.; Baron, Heather M.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Baron, Heather M.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
RP Kettenring, KM (reprint author), Utah State Univ, Ctr Ecol, 5210 Old Main Hill, Logan, UT 84322 USA.
EM karin.kettenring@usu.edu
OI Whigham, Dennis/0000-0003-1488-820X
FU EPA STAR [692105]; Smithsonian Work-learn internship; Smithsonian
Postdoctoral Fellowship
FX We thank J. O'Neill, C. Laine, J. Baker for lab assistance; L. Meyerson
for pollination advice; S. Durham for statistical advice; and J. Beder,
R. Downard, S. Galatowitsch, E. Hazelton, D. Menuz, K. Mercer for
manuscript feedback. This research was funded by EPA STAR grant # 692105
to D. Wardrop; a Smithsonian Work-learn internship to H. M. B.; and a
Smithsonian Postdoctoral Fellowship to K.M.K.
NR 59
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U1 8
U2 72
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0021-8901
J9 J APPL ECOL
JI J. Appl. Ecol.
PD OCT
PY 2011
VL 48
IS 5
BP 1305
EP 1313
DI 10.1111/j.1365-2664.2011.02024.x
PG 9
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 823BA
UT WOS:000295095100027
ER
PT J
AU Kibii, JM
Clarke, RJ
Tocheri, MW
AF Kibii, Job M.
Clarke, Ron J.
Tocheri, Matthew W.
TI A hominin scaphoid from Sterkfontein, Member 4: Morphological
description and first comparative phenetic 3D analyses
SO JOURNAL OF HUMAN EVOLUTION
LA English
DT Editorial Material
DE Australopithecus; Wrist bone; Thumb; Carpal arch
ID SOUTH-AFRICA; OLDUVAI GORGE; AUSTRALOPITHECUS-ANAMENSIS; FOOT BONES;
HAND; EVOLUTION; PLIOCENE; SHAPE; SIZE; MORPHOMETRICS
C1 [Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20013 USA.
[Kibii, Job M.; Clarke, Ron J.] Univ Witwatersrand, Sch Anat Sci, Johannesburg, South Africa.
[Kibii, Job M.; Clarke, Ron J.] Univ Witwatersrand, Inst Human Evolut, ZA-2050 Johannesburg, South Africa.
RP Tocheri, MW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, 10th & Constitut Ave NW, Washington, DC 20013 USA.
EM tocherim@si.edu
OI Tocheri, Matthew/0000-0001-7600-8998
NR 48
TC 2
Z9 2
U1 1
U2 8
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0047-2484
J9 J HUM EVOL
JI J. Hum. Evol.
PD OCT
PY 2011
VL 61
IS 4
BP 510
EP 517
DI 10.1016/j.jhevol.2011.06.001
PG 8
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA 828LR
UT WOS:000295503000013
PM 21788062
ER
PT J
AU Hanner, R
Floyd, R
Bernard, A
Collette, BB
Shivji, M
AF Hanner, Robert
Floyd, Robin
Bernard, Andrea
Collette, Bruce B.
Shivji, Mahmood
TI DNA barcoding of billfishes
SO MITOCHONDRIAL DNA
LA English
DT Article
DE COI; rhodopsin; mitochondrial DNA; species delimitation
ID MITOCHONDRIAL-DNA; IDENTIFICATION; MARLIN; SPEARFISH; SEQUENCES;
NUCLEAR; FISHES; GENE; LIFE; PCR
AB DNA barcoding is a method promising fast and accurate identification of animal species based on the sequencing of the mitochondrial c oxidase subunit (COI) gene. In this study, we explore the prospects for DNA barcoding in one particular fish group, the billfishes (suborder Xiphioidei-swordfish, marlins, spearfishes, and sailfish). We sequenced the mitochondrial COI gene from 296 individuals from the 10 currently recognized species of billfishes, and combined these data with a further 57 sequences from previously published projects. We also sequenced the rhodopsin gene from a subset of 72 individuals to allow comparison of mitochondrial results against a nuclear marker. Five of the 10 species are readily distinguishable by COI barcodes. Of the rest, the striped marlin (Kajikia audax) and white marlin (K. albida) show highly similar sequences and are not unambiguously distinguishable by barcodes alone, likewise are the three spearfishes Tetrapturus angustirostris, T. belone, and T. pfluegeri. We discuss the taxonomic status of these species groups in light of our and other data, molecular and morphological.
C1 [Hanner, Robert; Floyd, Robin] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada.
[Hanner, Robert; Floyd, Robin] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada.
[Bernard, Andrea; Shivji, Mahmood] Nova SE Univ, Oceanog Ctr, Guy Harvey Res Inst, Dania, FL 33004 USA.
[Collette, Bruce B.] Natl Museum Nat Hist, Smithsonian Inst, Natl Marine Fisheries Serv Systemat Lab, MRC 0153, Washington, DC 20560 USA.
RP Hanner, R (reprint author), Univ Guelph, Biodivers Inst Ontario, 50 Stone Rd E, Guelph, ON N1G 2W1, Canada.
EM rhanner@uoguelph.ca
FU Canadian Barcode of Life Network from Genome Canada (through the Ontario
Genomics Institute); NSERC
FX This work was supported through funding to the Canadian Barcode of Life
Network from Genome Canada (through the Ontario Genomics Institute),
NSERC, and other sponsors listed at http://www.BOLNET.ca; and
additionally by operational funds to the Guy Harvey Research Institute,
AFTCO, Inc., and an NSERC postgraduate fellowship (AB). We thank L.
Beerkircher, J. Graves, J. McDowell, E. Prince, J. Serafy, and D.
Snodgrass for providing tissue samples and Eugene Wong for assistance in
the laboratory. We are grateful to Johanne Fischer of the FAO for
granting permission to use images from their catalog (Nakamura 1985) for
the first figure in our study. The authors report no conflicts of
interest. The authors alone are responsible for the content and writing
of the paper.
NR 46
TC 12
Z9 13
U1 1
U2 12
PU INFORMA HEALTHCARE
PI LONDON
PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND
SN 1940-1736
EI 1940-1744
J9 MITOCHONDR DNA
JI Mitochondrial DNA
PD OCT
PY 2011
VL 22
SU 1
BP 27
EP 36
DI 10.3109/19401736.2011.596833
PG 10
WC Genetics & Heredity
SC Genetics & Heredity
GA 831JJ
UT WOS:000295726100006
PM 21980985
ER
PT J
AU Moran, JM
AF Moran, James M.
TI John Peter Huchra Obituary
SO PHYSICS TODAY
LA English
DT Biographical-Item
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Moran, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0031-9228
J9 PHYS TODAY
JI Phys. Today
PD OCT
PY 2011
VL 64
IS 10
BP 66
EP 66
PG 1
WC Physics, Multidisciplinary
SC Physics
GA 833PS
UT WOS:000295898000023
ER
PT J
AU Elvis, M
McDowell, J
Hoffman, JA
Binzel, RP
AF Elvis, Martin
McDowell, Jonathan
Hoffman, Jeffrey A.
Binzel, Richard P.
TI Ultra-low delta-v objects and the human exploration of asteroids
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Human exploration; Asteroids; Surveys
ID TELESCOPE
AB Missions to near-Earth objects (NEOs) are key destinations in NASA's new 'Flexible Path' approach. NEOs are also of interest for science, for the hazards they pose, and for their resources. We emphasize the importance of ultra-low delta-v from LEO to NEO rendezvous as a target selection criterion, as this choice can greatly increase the payload to the NEO. Few such ultra-low delta-v NEOs are currently known; only 65 of the 6699 known NEOs (March 2010) have delta-v < 4.5 km/s, 2/3 of typical LEO-NEO delta-v. Even these are small and hard to recover. Other criteria - short transit times, long launch windows, a robust abort capability, and a safe environment for proximity operations - will further limit the list of accessible objects. Potentially there is at least an order of magnitude more ultra-low delta-v NEOs, but finding them all on a short enough timescale (before 2025) requires a dedicated survey in the optical or mid-IR, optimally from a Venus-like orbit because of the short synodic period for NEOs in that orbit, plus long arc determination of their orbits. Published by Elsevier Ltd.
C1 [Elvis, Martin; McDowell, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hoffman, Jeffrey A.; Binzel, Richard P.] MIT, Cambridge, MA 02139 USA.
RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM elvis@cfa.harvard.edu
FU NASA [NAS8-39073]
FX This paper is based on a talk given at the April 2010 meeting of the
Dynamical Astronomy Division of the American Astronomical Society. We
thank the late Brian Marsden, Alan Harris, Tim Spahr, Slatko Ivezic and
B.C. Crandall for valuable assistance and advice. This work was
supported in part by NASA contract NAS8-39073.
NR 28
TC 8
Z9 8
U1 0
U2 5
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 OCT
PY 2011
VL 59
IS 13
BP 1408
EP 1412
DI 10.1016/j.pss.2011.05.006
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 833OI
UT WOS:000295894400008
ER
PT J
AU Liu, Q
Peterson, PM
Ge, XJ
AF Liu, Qing
Peterson, Paul M.
Ge, Xue-jun
TI Phylogenetic signals in the realized climate niches of Chinese grasses
(Poaceae)
SO PLANT ECOLOGY
LA English
DT Article
DE BEP and PACCMAD clades; C4 node; Niche evolution; Phylogeny; Poaceae;
Species distribution model
ID C-4 GRASSES; GEOGRAPHICAL-DISTRIBUTION; ECOLOGICAL DISTRIBUTION;
HAWAIIAN-ISLANDS; FUNCTIONAL TYPES; TRAIT EVOLUTION; NORTH-AMERICA; C4
GRASSES; PHOTOSYNTHESIS; PATTERNS
AB Explaining relationships between species richness and biogeographical patterns over a broad geographic scale is a central issue of biogeography and macroecology. We document the realized climate niches for grasses in China's nature reserves and discuss its formation mechanism using grass richness data combined with climatic, physiological, and phylogenetic data. Our results suggest that climate niche structure of grasses is phylogenetically conservative for BEP (Bambusoideae, Ehrhartoideae, and Pooideae) and PACMAD (Panicoideae, Arundinoideae, Chloridoideae, Micrairoideae, Aristidoideae, and Danthonioideae) clades along temperature gradients and for Chloridoideae and Panicoideae along precipitation gradients. At the national scale, the divergence patterns of climate niches between two major clades are more distinguishable than between C-3 and C-4 grasses. High rates of climate niche evolution are found in C-4 clades in the subtropical forest region. There appears to be a strong association between elevation gradients and grass diversity: the specific environmental conditions (e.g. energy) and the rapid shifts of climate conditions drive high grass diversification. Evolutionary conservatism of climate niches may be influenced by the specific adaptive ability to changing environmental conditions within NAD-ME/NADP-ME clades. Our results indicate that adaptations to major climate changes may be accomplished by C-4 grass nodes of high climate niche evolutionary rates in China's nature reserves.
C1 [Liu, Qing; Ge, Xue-jun] Chinese Acad Sci, Key Lab Plant Resources Conservat & Sustainable U, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China.
[Peterson, Paul M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
RP Liu, Q (reprint author), Chinese Acad Sci, Key Lab Plant Resources Conservat & Sustainable U, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China.
EM liuqing@scib.ac.cn; xjge@scib.ac.cn
FU National Natural Science Foundation of China [30700043]; Key Laboratory
of Plant Resources Conservation and Sustainable Utilization, Chinese
Academy of Sciences [200922]; Chinese Government [2008491004]; Chinese
Academy of Sciences [KSCX2-EW-J-28]
FX We thank China Meteorological Data Sharing Service System for accessing
the digital climatic data. This study was supported by the National
Natural Science Foundation of China (No. 30700043), the Key Laboratory
of Plant Resources Conservation and Sustainable Utilization, Chinese
Academy of Sciences (No. 200922), the Chinese Government Scholarship to
QL (No. 2008491004), and the Knowledge Innovation Program of the Chinese
Academy of Sciences (KSCX2-EW-J-28). We also thank two anonymous
reviewers for their constructive comments that improved the manuscript.
NR 73
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U1 4
U2 24
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1385-0237
J9 PLANT ECOL
JI Plant Ecol.
PD OCT
PY 2011
VL 212
IS 10
BP 1733
EP 1746
DI 10.1007/s11258-011-9946-7
PG 14
WC Plant Sciences; Ecology; Forestry
SC Plant Sciences; Environmental Sciences & Ecology; Forestry
GA 834SG
UT WOS:000295983700014
ER
PT J
AU Raviele, ME
AF Raviele, Maria E.
TI Experimental assessment of maize phytolith and starch taphonomy in
carbonized cooking residues
SO JOURNAL OF ARCHAEOLOGICAL SCIENCE
LA English
DT Article
DE Zea mays; Maize; Phytoliths; Starch; Residues; Taphonomy; Eastern North
America
ID GRAIN ANALYSIS; NORTH-AMERICA; ZEA-MAYS; NEW-YORK; FREQUENCIES;
ARTIFACTS; EVOLUTION; ISOTOPE; LOCUS
AB Many taphonomic studies of plant microfossils, specifically phytoliths and starch, are concerned with post-depositional movement, contamination, and morphological changes due to environmental fluctuations or plant processing. Additionally, the identification of phytoliths and starches archaeologically are based on their presence or absence. This paper examines whether it is possible to identify maize (Zea mays ssp. mays) phytolith and starch abundance associated with different processing behaviors as replicated through experimentally produced cooking residues. If successful, identification of likely associated processing and taphonomy of these microfossils will allow for a more refined interpretation of plant use as it relates to timing and plant form and processing. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Raviele, Maria E.] Smithsonian Inst, Off Policy & Anal, Washington, DC 20013 USA.
[Raviele, Maria E.] Michigan State Univ, Dept Anthropol, E Lansing, MI 48824 USA.
RP Raviele, ME (reprint author), Smithsonian Inst, Off Policy & Anal, MRC 502,POB 37012, Washington, DC 20013 USA.
EM ravielem@gmail.com
FU National Science Foundation [BCS-0843130]; Wenner-Gren Dissertation
Fieldwork Grant [7811]
FX Funding for this work was provided through a National Science Foundation
Doctoral Dissertation Improvement Grant (Award BCS-0843130) and a
Wenner-Gren Dissertation Fieldwork Grant (Grant #7811). I would like to
thank Jerry Fankhauser for providing the milk stage dent maize used in
these experiments, Drs. William Lovis and John Hart for their extensive
comments on earlier drafts and the comments of two anonymous reviewers.
NR 41
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U1 1
U2 14
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 OCT
PY 2011
VL 38
IS 10
BP 2708
EP 2713
DI 10.1016/j.jas.2011.06.008
PG 6
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 822NP
UT WOS:000295055500022
ER
PT J
AU Meier, DC
Davis, JM
Vicenzi, EP
AF Meier, Douglas C.
Davis, Jeffrey M.
Vicenzi, Edward P.
TI An Examination of Kernite (Na(2)B(4)O(6)(OH)(2)center dot 3H(2)O) Using
X-Ray and Electron Spectroscopies: Quantitative Microanalysis of a
Hydrated Low-Z Mineral
SO MICROSCOPY AND MICROANALYSIS
LA English
DT Article
DE borate; kernite; hydrate; light elements; electron-probe microanalysis
(EPMA); wavelength-dispersive X-ray spectroscopy (WDS); X-ray
diffraction (XRD); X-ray photoelectron spectroscopy (XPS);
variable-pressure scanning electron microscopy (VP-SEM); auger electron
spectroscopy (AES)
ID NA2B4O6(OH)2.3H2O; BORON; GLASS
AB Mineral borates, the primary industrial source of boron, are found in a large variety of compositions. One such source, kernite (Na(2)B(4)O(6)(OH)(2)center dot 3H2O), offers an array of challenges for traditional electron-probe microanalysis (EPMA)-it is hygroscopic, an electrical insulator, composed entirely of light elements, and sensitive to both low pressures and the electron beam. However, the approximate stoichiometric composition of kernite can be analyzed with careful preparation, proper selection of reference materials, and attention to the details of quantification procedures, including correction for the time dependency of the sodium X-ray signal. Moreover, a reasonable estimation of the mineral's water content can also be made by comparing the measured oxygen to the calculated stoichiometric oxygen content. X-ray diffraction, variable-pressure electron imaging, and visual inspection elucidate the structural consequences of high vacuum treatment of kernite, while Auger electron spectroscopy and X-ray photoelectron spectroscopy confirm electron beam-driven migration of sodium and oxygen out of the near-surface region (sampling depth approximate to 2 nm). These surface effects are insufficiently large to significantly affect the EPMA results (sampling depth approximate to 400 nm at 5 keV).
C1 [Meier, Douglas C.; Davis, Jeffrey M.; Vicenzi, Edward P.] NIST, Surface & Microanal Sci Div, Gaithersburg, MD 20899 USA.
[Vicenzi, Edward P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
RP Meier, DC (reprint author), NIST, Surface & Microanal Sci Div, 100 Bur Dr MS8371, Gaithersburg, MD 20899 USA.
EM dmeier@nist.gov
NR 30
TC 1
Z9 1
U1 1
U2 8
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1431-9276
J9 MICROSC MICROANAL
JI Microsc. microanal.
PD OCT
PY 2011
VL 17
IS 5
BP 718
EP 727
DI 10.1017/S1431927611000602
PG 10
WC Materials Science, Multidisciplinary; Microscopy
SC Materials Science; Microscopy
GA 829UF
UT WOS:000295609100011
PM 21892991
ER
PT J
AU Thapa, R
Phillips, JD
Rocco, E
Reasenberg, RD
AF Thapa, Rajesh
Phillips, James D.
Rocco, Emanuele
Reasenberg, Robert D.
TI Subpicometer length measurement using semiconductor laser tracking
frequency gauge
SO OPTICS LETTERS
LA English
DT Article
ID INTERFEROMETRY; ACCURACY
AB We have demonstrated heretofore unattained distance precision of 0.14 pm (2 pm) incremental and 14 nm (2.9 mu m) absolute in a resonant (nonresonant) interferometer at an averaging time of 1 s, using inexpensive telecommunications diode lasers. We have controlled the main source of error, that due to spurious reflection and the resulting amplitude modulation. In the resonant interferometer, absolute distance precision is well under lambda/6. Therefore, after an interruption, an absolute distance measurement can be used to return to the same interferometer order. (C) 2011 Optical Society of America
C1 [Thapa, Rajesh; Phillips, James D.; Rocco, Emanuele; Reasenberg, Robert D.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Phillips, JD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM jphillips@cfa.harvard.edu
FU National Aeronautics and Space Administration (NASA) [NNX07AI11G,
NNX08AO04G]
FX This work was supported by the National Aeronautics and Space
Administration (NASA) through grants NNX07AI11G and NNX08AO04G.
NR 11
TC 10
Z9 10
U1 0
U2 2
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
J9 OPT LETT
JI Opt. Lett.
PD OCT 1
PY 2011
VL 36
IS 19
BP 3759
EP 3761
PG 3
WC Optics
SC Optics
GA 827GD
UT WOS:000295415600015
PM 21964088
ER
PT J
AU Cardoso, P
Borges, PAV
Triantis, KA
Ferrandez, MA
Martin, JL
AF Cardoso, Pedro
Borges, Paulo A. V.
Triantis, Kostas A.
Ferrandez, Miguel A.
Martin, Jose L.
TI Adapting the IUCN Red List criteria for invertebrates
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE Arthropoda; Conservation priority; Extinction; Risk assessment;
Threatened species; World Conservation Union
ID POPULATION VIABILITY ANALYSIS; SPECIES DISTRIBUTIONS; CONSERVATION
STATUS; EXTINCTION DEBT; TAXONOMIC BIAS; CLIMATE-CHANGE; BIODIVERSITY;
AZORES; EUROPE; UNCERTAINTY
AB The IUCN Red List is the most useful list of species that are at risk for extinction worldwide, as it relies on a number of objective criteria. Nevertheless, there is a taxonomic bias that excludes species with small body sizes, narrow distribution ranges and low dispersal abilities, which constitute the vast Majority of the planet's biota, particularly local endemics.
By evaluating each IUCN criterion separately, we (i) identify the shortcomings for invertebrate applications, (ii) explain how risk categories may be wrongly applied due to inapplicable and/or misleading thresholds, (iii) suggest alternative ways of applying the existing criteria in a more realistic way and (iv) suggest possible new criteria that were not considered in the current evaluation framework but that could allow a more comprehensive and effective assessment of invertebrates.
By adapting the criteria to rely more explicitly on the Area of Occupancy and the Extent of Occurrence, their respective trends and by using ecological modelling methods, the criteria's applicability would be increased. The change in some thresholds or, eventually, the creation of sub-categories would further increase their adequacy. Additionally, co-extinction could be introduced as an explicit part of the classification process.
As a case study, we evaluated 48 species of Azorean arthropods and Iberian spiders according to the current criteria. More than one-quarter (27%) of all evaluated species were classified as Critically Endangered, 19% as Endangered, 6% as Vulnerable and 8% as Least Concern. The remaining 40% did not have enough data to reach a classification. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
[Cardoso, Pedro; Borges, Paulo A. V.; Triantis, Kostas A.] Univ Azores, Azorean Biodivers Grp CITA A, Angra Do Heroismo, Portugal.
[Triantis, Kostas A.] Univ Athens, Dept Ecol & Taxon, Fac Biol, Athens 11528, Greece.
[Ferrandez, Miguel A.] Soc El Estudio & Conservac Aranas, Madrid, Spain.
[Martin, Jose L.] Canary Agcy Sustainable Dev & Climate Change, Santa Cruz De Tenerife, Canary Islands, Spain.
RP Cardoso, P (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, Rua Capitao Joao dAvila, P-9700042 Angra Do Heroismo, Portugal.
EM pcardoso@ennor.org
RI Borges, Paulo/B-2780-2008; Triantis, Kostas/A-1018-2009; Cardoso,
Pedro/A-8820-2008
OI Borges, Paulo/0000-0002-8448-7623; Cardoso, Pedro/0000-0001-8119-9960
FU Portuguese Foundation for Science and Technology [SFRH/BPD/40688/2007];
Direccao Regional dos Recursos Florestais [17.01-080203]
FX PC is supported by the Portuguese Foundation for Science and Technology
(SFRH/BPD/40688/2007). The data obtained in the Azores was possible due
to the accumulated effort of many colleagues during BALA Project (funded
by the Direccao Regional dos Recursos Florestais - Proj. 17.01-080203)
and more recently the projects "Consequences of land-use change on
Azorean fauna and flora - the 2010 Target" (Ref: Direccao Regional da
Ciencia e Tecnologia M.2.1.2/I/003/2008) and
FCT-PTDC/BIA-BEC/100182/2008 - "Predicting extinctions on islands: a
multi-scale assessment".
NR 69
TC 51
Z9 55
U1 4
U2 41
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0006-3207
EI 1873-2917
J9 BIOL CONSERV
JI Biol. Conserv.
PD OCT
PY 2011
VL 144
IS 10
BP 2432
EP 2440
DI 10.1016/j.biocon.2011.06.020
PG 9
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 823HE
UT WOS:000295112300006
ER
PT J
AU Mason, VC
Li, G
Helgen, KM
Murphy, WJ
AF Mason, Victor C.
Li, Gang
Helgen, Kristofer M.
Murphy, William J.
TI Efficient cross-species capture hybridization and next-generation
sequencing of mitochondrial genomes from noninvasively sampled museum
specimens
SO GENOME RESEARCH
LA English
DT Article
ID COLUGO
AB The ability to uncover the phylogenetic history of recently extinct species and other species known only from archived museum material has rapidly improved due to the reduced cost and increased sequence capacity of next-generation sequencing technologies. One limitation of these approaches is the difficulty of isolating and sequencing large, orthologous DNA regions across multiple divergent species, which is exacerbated for museum specimens, where DNA quality varies greatly between samples and contamination levels are often high. Here we describe the use of cross-species DNA capture hybridization techniques and next-generation sequencing to selectively isolate and sequence partial to full-length mitochondrial DNA genomes from the degraded DNA of museum specimens, using probes generated from the DNA of a single extant species. We demonstrate our approach on specimens from an enigmatic gliding mammal, the Sunda colugo, which is widely distributed throughout Southeast Asia. We isolated DNA from 13 colugo specimens collected 47-170 years ago, and successfully captured and sequenced mitochondrial DNA from every specimen, frequently recovering fragments with 10%-13% sequence divergence from the capture probe sequence. Phylogenetic results reveal deep genetic divergence among colugos, both within and between the islands of Borneo and Java, as well as between the Malay Peninsula and different Sundaic islands. Our method is based on noninvasive sampling of minute amounts of soft tissue material from museum specimens, leaving the original specimen essentially undamaged. This approach represents a paradigm shift away from standard PCR-based approaches for accessing population genetic and phylogenomic information from poorly known and difficult-to-study species.
C1 [Mason, Victor C.; Li, Gang; Murphy, William J.] Texas A&M Univ, Dept Vet Integrat Biosci, College Stn, TX 77843 USA.
[Mason, Victor C.; Murphy, William J.] Texas A&M Univ, Interdisciplinary Program Genet, College Stn, TX 77843 USA.
[Helgen, Kristofer M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
RP Murphy, WJ (reprint author), Texas A&M Univ, Dept Vet Integrat Biosci, College Stn, TX 77843 USA.
EM wmurphy@cvm.tamu.edu
RI li, gang/E-5640-2014
FU National Science Foundation [EF0629849]; Texas AM University
FX This work was supported in part by the National Science Foundation
(EF0629849 to W.J.M.) and Texas A&M University. We thank Linda Gordon
for assistance in sampling the colugo museum specimens. We thank the
Genome Center at Washington University for providing sequence data and
allowing use of the full mtDNA genome for GVA4.
NR 24
TC 59
Z9 59
U1 0
U2 40
PU COLD SPRING HARBOR LAB PRESS, PUBLICATIONS DEPT
PI COLD SPRING HARBOR
PA 1 BUNGTOWN RD, COLD SPRING HARBOR, NY 11724 USA
SN 1088-9051
J9 GENOME RES
JI Genome Res.
PD OCT
PY 2011
VL 21
IS 10
BP 1695
EP 1704
DI 10.1101/gr.120196.111
PG 10
WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology;
Genetics & Heredity
SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology;
Genetics & Heredity
GA 827DQ
UT WOS:000295407800013
PM 21880778
ER
PT J
AU Forgan, DH
Elvis, M
AF Forgan, Duncan H.
Elvis, Martin
TI Extrasolar asteroid mining as forensic evidence for extraterrestrial
intelligence
SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY
LA English
DT Article
ID BETA-PICTORIS; SOLAR-SYSTEM; DEBRIS DISKS; DUST; EVOLUTION; UNIVERSE;
PLANETS; SEARCH; SPACE; DISCS
AB The development of civilizations such as ours into spacefaring, multi-planet entities requires significant raw materials to construct vehicles and habitats. Interplanetary debris, including asteroids and comets, may provide such a source of raw materials. In this article, we present the hypothesis that extraterrestrial intelligences (ETIs) engaged in asteroid mining may be detectable from Earth. Considering the detected disc of debris around Vega as a template, we explore the observational signatures of targeted asteroid mining (TAM), such as unexplained deficits in chemical species, changes in the size distribution of debris and other thermal signatures that may be detectable in the spectral energy distribution (SED) of a debris disc. We find that individual observational signatures of asteroid mining can be explained by natural phenomena, and as such they cannot provide conclusive detections of ETIs. But, it may be the case that several signatures appearing in the same system will prove harder to model without extraterrestrial involvement. Therefore, signatures of TAM are not detections of ETI in their own right, but as part of 'piggy-back' studies carried out in tandem with conventional debris disc research, they could provide a means of identifying unusual candidate systems for further study using other search for extra terrestrial intelligence (SETI) techniques. Received 26 January 2011, accepted 25 March 2011, first published online 9 May 2011
C1 [Forgan, Duncan H.] Univ Edinburgh, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Forgan, DH (reprint author), Univ Edinburgh, SUPA, Inst Astron, Black Ford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
EM dhf@roe.ac.uk
OI Forgan, Duncan/0000-0003-1175-4388
NR 40
TC 2
Z9 2
U1 3
U2 27
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1473-5504
J9 INT J ASTROBIOL
JI Int. J. Astrobiol.
PD OCT
PY 2011
VL 10
IS 4
BP 307
EP 313
DI 10.1017/S1473550411000127
PG 7
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 825ZT
UT WOS:000295321600001
ER
PT J
AU Selvaraj, V
Wildt, DE
Pukazhenthi, BS
AF Selvaraj, Vimal
Wildt, David E.
Pukazhenthi, Budhan S.
TI Induced pluripotent stem cells for conserving endangered species?
SO NATURE METHODS
LA English
DT Editorial Material
ID TECHNOLOGIES; CONSERVATION; WILDLIFE
C1 [Selvaraj, Vimal] Cornell Univ, Dept Anim Sci, Ithaca, NY 14853 USA.
[Wildt, David E.; Pukazhenthi, Budhan S.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA.
RP Selvaraj, V (reprint author), Cornell Univ, Dept Anim Sci, Ithaca, NY 14853 USA.
EM pukazhenthib@si.edu
NR 12
TC 5
Z9 5
U1 1
U2 11
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1548-7091
J9 NAT METHODS
JI Nat. Methods
PD OCT
PY 2011
VL 8
IS 10
BP 805
EP 807
DI 10.1038/nmeth.1715
PG 3
WC Biochemical Research Methods
SC Biochemistry & Molecular Biology
GA 826MJ
UT WOS:000295358000011
PM 21959133
ER
PT J
AU Budaeva, N
Fauchald, K
AF Budaeva, Nataliya
Fauchald, Kristian
TI Phylogeny of the Diopatra generic complex with a revision of
Paradiopatra Ehlres, 1887 (Polychaeta: Onuphidae)
SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE cladistics; distribution; identification key; morphology; new genus; new
species; paedomorphosis; taxonomy
ID ATLANTIC SEA-URCHINS; CUPREA BOSC; EPIBENTHIC MEIOFAUNA; LARVAL
DEVELOPMENT; TUBE-CAPS; ANNELIDA; GENUS; COAST; EUNICIDA; PACIFIC
AB Analysis of 55 morphological characters yielded a phylogenetic reconstruction of the Diopatra complex, currently including three genera (Diopatra, Epidiopatra, and Paradiopatra). The results reject the monophyletic status of the complex and all three genera analysed. It is suggested that several parallel and independent events of paedomorphic evolution took place within the genera Diopatra and Paradiopatra, which led to the recognition of two artificial genera Epidiopatra and Notonuphis. The following taxonomic revisions are proposed: (1) Epidiopatra as a junior synonym of Diopatra; (2) Notonuphis as a junior synonym of Paradiopatra; (3) the Diopatra complex, consisting of two sister genera Diopatra and Paradiopatra, and two basal genera Paxtonia gen. nov. and Protodiopatra gen. nov., erected for two species previously included in Paradiopatra. Reconstruction of phylogenetic relationships within Paradiopatra yields a few reliable clades comprising well-defined groups of species, but supported by homoplastic synapomorphies representing highly adaptive characters. Twenty-six valid species of Paradiopatra, including a new species, Paradiopatra pyricirra sp. nov., are described or re-described and illustrated based on original descriptions and re-examination of type and non-type material. Identification keys to genera included in the Diopatra complex, and to all accepted Paradiopatra species, are presented. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 163, 319-436. doi: 10.1111/j.1096-3642.2011.00701.x
C1 [Budaeva, Nataliya] Russian Acad Sci, PP Shirshov Oceanol Inst, Moscow 117997, Russia.
[Fauchald, Kristian] NMNH, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA.
RP Budaeva, N (reprint author), Russian Acad Sci, PP Shirshov Oceanol Inst, Nakhimovsky Prospekt 36, Moscow 117997, Russia.
EM nataliya.budaeva@gmail.com
FU Invertebrate Zoology Division of the National Museum of Natural History;
Russian Foundation for Basic Research [07-04-08292, 06-04-48764];
CeDAMar, a project under the Census of Marine Life programme
FX We would like to thank Andrey Gebruk and Alexander Mironov (SIO RAS) for
their invaluable comments on the manuscript. We are also grateful to the
following individuals and institutions for the loan and exchange of
specimens: Tor Bakke (ZMO), Angelika Brandt (ZMH), Danny Eibye-Jacobsen
(ZMUC), Igor Jirkov (DHB MSU), Ardis Johnston (MCZ), Hironori Komatsu
(NSMT), Jon Anders Kongsrud (ZMUB), Nikita Kucheruk and Antonina
Rogacheva (SIO RAS), Tarik Meziane (MNHN), Birger Neuhaus (ZMB),
Vladislav Potin, Galina Bushinskaya, and Sergey Gagaev (ZIN), Emma
Sherlock, Alexander Muir, and Gordon Paterson (BMNH), Linda Ward and
Geoff Keel (USNM), Joana Zanol (Federal University of Rio de Janeiro,
Brazil). This work was supported by the Smithsonian Institution
fellowship programme (Invertebrate Zoology Division of the National
Museum of Natural History), the Russian Foundation for Basic Research,
grants 07-04-08292, 06-04-48764, and CeDAMar, a project under the Census
of Marine Life programme. The authors thank Guinea Current Large Marine
Ecosystem (GCLME) and the Norad funded EAF-Nansen program
www.eaf-nansen.org for access to material from the Gulf of Guinea
region.
NR 130
TC 13
Z9 15
U1 2
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-4082
EI 1096-3642
J9 ZOOL J LINN SOC-LOND
JI Zool. J. Linn. Soc.
PD OCT
PY 2011
VL 163
IS 2
BP 319
EP 436
DI 10.1111/j.1096-3642.2011.00701.x
PG 118
WC Zoology
SC Zoology
GA 825JB
UT WOS:000295267400001
ER
PT J
AU Wang, LH
Newchurch, MJ
Biazar, A
Liu, X
Kuang, S
Khan, M
Chance, K
AF Wang, Lihua
Newchurch, M. J.
Biazar, Arastoo
Liu, Xiong
Kuang, Shi
Khan, Maudood
Chance, Kelly
TI Evaluating AURA/OMI ozone profiles using ozonesonde data and EPA surface
measurements for August 2006
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE OMI; IONS06; CMAQ; EPA; Ozone evaluation
ID TROPOSPHERIC OZONE; MONITORING INSTRUMENT; RETRIEVALS
AB We evaluate the Ozone Monitoring Instrument (OMI) ozone profile retrieval against ozonesonde data and the Environmental Protection Agency (EPA) surface measurements for August 2006. Comparison of individual OMI ozone profile with ozonesonde indicates that OMI ozone profile can explain the general vertical variation of ozone but is limited in observing the boundary layer ozone, due to weak sensitivity to boundary layer ozone and thick lowest layer (similar to 2.5 km). We made pair-wise comparison between OMI and ozonesondes on 24 OMI vertical layers, as well as the 39 sigma-P vertical layers of the Community Multi-scale Air Quality (CMAQ) modeling system, respectively. OMI shows reasonable agreement with ozonesonde in the lower- to mid-troposphere. In the upper troposphere, while the bias increases, the normalized bias does not show much variation and remains below 10%. Comparison with EPA's surface-monitoring data indicates that OMI observations at the lowest layer (surface to 2.5 km altitude) represent the mean values. While OMI underestimates elevated ozone concentrations, it explains the larger-scale spatial variation seen in the surface monitors. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Wang, Lihua; Newchurch, M. J.; Kuang, Shi] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA.
[Biazar, Arastoo] Univ Alabama, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
RP Newchurch, MJ (reprint author), Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA.
EM mike@nsstc.uah.edu
RI Liu, Xiong/P-7186-2014;
OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577
NR 10
TC 8
Z9 9
U1 1
U2 9
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 OCT
PY 2011
VL 45
IS 31
BP 5523
EP 5530
DI 10.1016/j.atmosenv.2011.06.012
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 822SQ
UT WOS:000295070300014
ER
PT J
AU Gonzalez-Porter, GP
Hailer, F
Flores-Villela, O
Garcia-Anleu, R
Maldonado, JE
AF Gonzalez-Porter, Gracia P.
Hailer, Frank
Flores-Villela, Oscar
Garcia-Anleu, Rony
Maldonado, Jesus E.
TI Patterns of genetic diversity in the critically endangered Central
American river turtle: human influence since the Mayan age?
SO CONSERVATION GENETICS
LA English
DT Article
DE Population genetic structure; Dermatemys mawii; Dermatemydidae;
Mitochondrial DNA; Freshwater turtles
ID CYTOCHROME-B GENE; DNA-SEQUENCE DATA; MOLECULAR SYSTEMATICS;
POPULATION-STRUCTURE; CLADISTIC-ANALYSIS; POND TURTLE; BOX TURTLE;
CONSERVATION; MITOCHONDRIAL; PHYLOGENY
AB We conducted a phylogeographic analysis of the strictly aquatic and critically endangered Central American river turtle, Dermatemys mawii, as part of a conservation management program for the species. We sampled 238 individuals from 15 different localities throughout the species range. Using sequence fragments from the mtDNA Cyt b and ND4 genes, we identified 16 different haplotypes. Overall, our results reveal a signal of phylogeographic structure throughout the range, which appears to have been secondarily blurred by extensive gene flow. Notably, this also applies to genetic structuring across three major hydrological basins that pose biogeographic breaks in other aquatic taxa. Divergence times of mtDNA haplotypes in D. mawii suggest that the main lineages split in the Pliocene-Pleistocene (3.73-0.227 MA) and demographic tests indicate that the species has undergone drastic demographic size fluctuations since this time period. One ancient haplotype (1D) was found to exhibit sequence divergence of up to 2% from other haplogroups. Divergence of this magnitude is indicative of species level differentiation in other turtle genera. Haplotype 1D was found in only two localities, Sarstun and Salinas, but specimens with other haplotypes were also found in those localities. It is not known whether the individuals with the 1D haplotype interbreed with non-1D individuals. Our results suggest that human activity, such as harvesting and long distance transport of animals, may have influenced the current patterns of genetic diversity. For more than 2000 years, D. mawii has been consumed by people from Middle American cultures, and the archeological record contains strong evidence that the Mayans transported animals between villages and far away from their natural distribution range. Therefore, the large-scale pattern of haplotype sharing even across hydrological barriers, the observed low haplotype diversity in some populations and the contemporary absence of a pronounced phylogeographic pattern is likely due to a combination of population expansions, gene flow, extensive human-mediated-movements and recent bottlenecks resulting from over-harvesting.
C1 [Gonzalez-Porter, Gracia P.; Hailer, Frank; Maldonado, Jesus E.] Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
[Gonzalez-Porter, Gracia P.; Flores-Villela, Oscar] Univ Nacl Autonoma Mexico, Museo Zool, Fac Ciencias, Mexico City 04510, DF, Mexico.
[Garcia-Anleu, Rony] Wildlife Conservat Soc Guatemala Program, Flores, Guatemala.
[Maldonado, Jesus E.] Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA.
RP Gonzalez-Porter, GP (reprint author), Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Natl Zool Pk,3001 Connecticut Ave NW, Washington, DC 20008 USA.
EM syedg@si.edu
RI Hailer, Frank/C-9114-2012;
OI Hailer, Frank/0000-0002-2340-1726; Flores-Villela,
Oscar/0000-0002-2849-6912
FU Consejo Nacional de Ciencia y Tecnologia (CONACYT) [210994]; Turtle
Conservation Fund; Conservation International; Philadelphia Zoo;
Philadelphia Zoo Docent council; Elizabeth A. Schreiber and Seabird
Research, Inc.; SCBI's Center for Conservation and Evolutionary Genetics
FX We thank the Posgrado en Ciencias Biologicas from Universidad Nacional
Autonoma de Mexico UNAM; Drs. Ella Vazquez and Luis Medrano Gonzalez for
their valuable insights into the experimental design and data analysis
which greatly improved the quality of this manuscript. Funding was
provided by Consejo Nacional de Ciencia y Tecnologia (CONACYT)
fellowship No. 210994; the Turtle Conservation Fund grants in 2004, 2006
and 2009; Conservation International grants in 2007, and 2009; the
Philadelphia Zoo Conservation Program Financial Support for 2005, 2006,
2007, 2008, an award from the Philadelphia Zoo Docent council in 2007
and Elizabeth A. Schreiber and Seabird Research, Inc. We are grateful to
Robert C. Fleischer and Nancy Rotzel for funding and laboratory support
at the SCBI's Center for Conservation and Evolutionary Genetics. To
Secretaria de Medio Ambiente y Recursos Naturales (SEMARNAT) for the
collection permits: SGPA/DGVS/11385/04; SGPA/DGVS/01789/06 to CITES for
permits: MX 23732/05; MX 25219/05; MX29137/06; GT175507; MX42603/08; to
the government of Belize for permit No. 3176/08; to the USFWS for
permits #MA095827-0; MA119634-0/06; MA139456-0/07; MA194812-0/08;
EN/FIS/15/04/08(10)Vol1. To SEMARNAT and Procuraduria Federal de
Proteccion al Ambiente (PROFEPA) in Veracruz, and Tabasco. Thanks to all
the people who have helped on different parts of this project; for
ideas: Miriam Tsuchiya Jerep, for her important help on running the
program BEAST, K. Buhlmann and Peter Paul Van Dijk; special thanks to
Richard C. Vogt, who help me consolidate the idea of this project and
sharing his expertise on the species. Dr. John Polisar, Carlina Pena,
Rene Calderon, Humberto Bahena, Matha Vaca, Raul Rodriguez, Lisette
Ramos, Greg Georges, Sam Rivera, Judith Rangel, Erasmo Cazares, Darwin
Jimenez, Samuel Cabrera, Kenia Laparra, Manuel Acevedo, Claudia Zenteno,
and Filiberto Ascencio Jimenez, the staff from WCS in Flores, Guatemala,
all the volunteers, and staff at the turtle farm in Nacajuca, Tabasco,
and Zoologico Yumka, Fishermen Cooperative of La Union in Quintana Roo
for their help in the collection and measuring of the animals. Thanks
also to Basilio Sanchez Luna, Gregorio de la Cruz Lopez, and Sharon
Matola for allowing us to work with the animals at their facilities, and
to Dr. Jonathan Campbell and Carl Franklin from the Amphibian and
Reptile Diversity Research Center of the University of Texas at
Arlington for the donation of turtle samples for this study, to Joseph R
Mendelson, for the information on Phylogeography of the genus Bufo, and
to three anonymous reviewers whose comments greatly enhanced the quality
of this manuscript.
NR 87
TC 8
Z9 8
U1 1
U2 13
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1566-0621
EI 1572-9737
J9 CONSERV GENET
JI Conserv. Genet.
PD OCT
PY 2011
VL 12
IS 5
BP 1229
EP 1242
DI 10.1007/s10592-011-0225-x
PG 14
WC Biodiversity Conservation; Genetics & Heredity
SC Biodiversity & Conservation; Genetics & Heredity
GA 819BE
UT WOS:000294799600009
ER
PT J
AU Cibois, A
Beadell, JS
Graves, GR
Pasquet, E
Slikas, B
Sonsthagen, SA
Thibault, JC
Fleischer, RC
AF Cibois, Alice
Beadell, Jon S.
Graves, Gary R.
Pasquet, Eric
Slikas, Beth
Sonsthagen, Sarah A.
Thibault, Jean-Claude
Fleischer, Robert C.
TI Charting the course of reed-warblers across the Pacific islands
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Article
DE Acrocephalidae; Acrocephalus; back-colonization; colonization patterns;
island biogeography; Micronesia; Pacific Ocean islands; phylogeny;
Polynesia; reed-warblers
ID MITOCHONDRIAL SEQUENCE DATA; K-AR AGES; HAWAIIAN-ISLANDS;
FRENCH-POLYNESIA; SOUTH-PACIFIC; PHYLOGENETIC-RELATIONSHIPS; MOLECULAR
PHYLOGENY; MONARCHS POMAREA; HENDERSON ISLAND; NATURAL-HISTORY
AB Aim Deciphering the complex colonization history of island archipelagos is greatly facilitated by comprehensive phylogenies. In this study we investigate the phylogeny and biogeography of the insular reed-warblers (genus Acrocephalus) of the tropical Pacific Ocean, from Australia to eastern Polynesia.
Location Oceania.
Methods We used sequences of mitochondrial DNA (cytochrome b, ND2 and ATP8 genes) to infer the colonization patterns of reed-warblers endemic to Pacific islands and Australia. We sampled all known taxa of Acrocephalus in the Pacific except A. luscinius nijoi, for which no sample was available. Most taxa were represented by toe-pad samples from museum specimens collected in the 19th and 20th centuries. With a few exceptions, several specimens per taxon were sequenced independently in two institutions (Smithsonian Institution and Natural History Museum of Geneva).
Results Our data indicate that Pacific reed-warblers do not form a monophyletic group, because A. luscinius luscinius from Guam falls outside the main Pacific radiation. The remaining Pacific taxa are divided into two clades: one clade includes all the reed-warblers from Micronesia (except Guam) and Australia, and two Polynesian taxa from the Line Islands and the southern Marquesas; the other clade includes all remaining Polynesian taxa. The taxa endemic to three archipelagos (Mariana, Marquesas and Society islands) are polyphyletic, suggesting several independent colonizations.
Main conclusions Our results provide evidence for a complex pattern of colonization of the Pacific by reed-warblers. Calibration analyses suggest that reed-warbler lineages are much younger than the ages of the islands they occupy. Several remote archipelagos were colonized independently more than once. Consequently, we infer that the colonization of reed-warblers in the Pacific did not follow a regular, stepping-stone-like pattern. The phylogeny also suggests a previously undetected case of reverse colonization (from island to continent) for the Australian lineage and indicates that A. luscinius, as currently defined, is not monophyletic. We discuss the supertramp strategy of reed-warblers in the Pacific and show that, although Pacific reed-warblers meet some of the supertramp criteria in their aptitude for colonizing remote archipelagos, their life history characteristics do not fit the model.
C1 [Cibois, Alice] Nat Hist Museum Geneva, Dept Mammal & Ornithol, CH-1211 Geneva 6, Switzerland.
[Beadell, Jon S.; Sonsthagen, Sarah A.; Fleischer, Robert C.] Smithsonian Inst, Genet Program, Natl Museum Nat Hist, Washington, DC 20008 USA.
[Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116, Washington, DC 20013 USA.
[Pasquet, Eric; Thibault, Jean-Claude] Museum Natl Hist Nat, Dept Systemat & Evolut, Origine Struct & Evolut Biodivers UMR7205, Paris, France.
[Pasquet, Eric; Thibault, Jean-Claude] Museum Natl Hist Nat, Serv Systemat Mol, CNRS, UMS2700, F-75005 Paris, France.
[Slikas, Beth] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA.
RP Cibois, A (reprint author), Nat Hist Museum Geneva, Dept Mammal & Ornithol, CP 6434, CH-1211 Geneva 6, Switzerland.
EM alice.cibois@ville-ge.ch
FU DIREN Tahiti; Ornithological Society of Polynesia [6-0056/mdd]; Frank M.
Chapman Memorial Fund (AMNH); European Commission [GB-TAF-1846/2002];
Swiss Academy of Sciences; G. and A. Claraz Foundation; Basel Foundation
for Biological Research; US NSF [DEB-0643291]; Research Opportunities
Fund
FX We are very grateful to Joel Cracraft and Paul Sweet [American Museum of
Natural History (AMNH), New York], Robert Prys-Jones and Mark Adams
[British Museum (Natural History) (BMNH), Tring, UK], Clemency Fisher
and Tony Parker [National Museums Liverpool (NML), UK], Peter-Rene
Becker and Ulrich Burkhardt [Ubersee-Museum Bremen (UMB)], Alexander
Haas and Cordula Bracker [Zoologisches Museum Hamburg (ZMH)] for access
to the collections in their charge and for the sampling of specimens.
The University of Washington Burke Museum and the University of Kansas
kindly provided additional samples or sequences. We thank Sheila Conant
(University of Hawai'i), Chris Filardi (Center for Biodiversity and
Conservation, New York), Robert Moyle (University of Kansas), Jean-Yves
Meyer (Research Delegation, Tahiti), Claude Serra (DIREN Tahiti),
Philippe Raust (Manu, Ornithological Society of Polynesia), Florence
Marteau [Museum d'Histoire Naturelle de Geneve (MHNG) Geneva], Bernd
Leisler (Max Planck Institute for Ornithology, Munchen), Marshall
Weisler (University of Queensland, St Lucia), the Institut pour la
Recherche et le Developpement (Papeete), and the Service de Systematique
Moleculaire [UMS2700-CNRS, Museum National d'Histoire Naturelle (MNHN),
Paris]. Financial support by the DIREN Tahiti and the Ornithological
Society of Polynesia (Convention no. 6-0056/mdd), the Collection Study
Grant from the Frank M. Chapman Memorial Fund (AMNH), the European
Commission's Research Infrastructure Action via the SYN-THESYS Project
(applications GB-TAF-1846/2002), the Swiss Academy of Sciences
(commission of travel grant), the G. and A. Claraz Foundation, the Basel
Foundation for Biological Research, the US NSF (DEB-0643291 to R. C.
F.), and the Research Opportunities Fund (Smithsonian Institution) is
gratefully acknowledged.
NR 91
TC 18
Z9 20
U1 3
U2 21
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0305-0270
EI 1365-2699
J9 J BIOGEOGR
JI J. Biogeogr.
PD OCT
PY 2011
VL 38
IS 10
BP 1963
EP 1975
DI 10.1111/j.1365-2699.2011.02542.x
PG 13
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 822MP
UT WOS:000295052300010
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI Jefferson's Bible
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 1
PU SMITHSONIAN ASSOC
PI WASHINGTON
PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA
SN 0037-7333
J9 SMITHSONIAN
JI Smithsonian
PD OCT
PY 2011
VL 42
IS 6
BP 38
EP 38
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 824MO
UT WOS:000295206200014
ER
PT J
AU Mengual, X
Thompson, FC
AF Mengual, Ximo
Thompson, F. Christian
TI Carmine cochineal killers: the flower fly genus Eosalpingogaster Hull
(Diptera: Syrphidae) revised
SO SYSTEMATIC ENTOMOLOGY
LA English
DT Article
ID BIOLOGICAL-CONTROL; SOUTH-AFRICA; CACTACEAE; DACTYLOPIIDAE; JMODELTEST;
PHYLOGENY; HOMOPTERA; INFERENCE; SELECTION; ALIGNMENT
AB The flower fly genus Eosalpingogaster Hull, predator of the carminic acid producer cochineal (Dactylopiidae), is revised. Two new species are described (knutsoni sp.n. and umbra sp.n.) and an identification key is provided for all known species. Diagnoses, illustrations, synonymies and distributional and biological data are given. Three new synonyms are proposed [texana Curran as jun.syn. of cochenillivora (Guerin-Meneville); liposeta Fluke and dactylopianus Blanchard as jun.syn. of nigriventris (Bigot)] and two lectotypes are designated for cochenillivora (Guerin-Meneville) and nigriventris (Bigot). Eosalpingogaster is elevated to full generic status based on adult morphological characters, biological data and a new phylogenetic analysis of molecular characters with genes 28S, 18S and cytochrome c oxidase subunit I. All data, images and drawings are available online as an example of the utility of international standards for biodiversity informatics.
C1 [Mengual, Ximo; Thompson, F. Christian] Smithsonian Inst, NMNH, Dept Entomol, Washington, DC 20013 USA.
RP Mengual, X (reprint author), Smithsonian Inst, NMNH, Dept Entomol, POB 37012,MRC 0169, Washington, DC 20013 USA.
EM xmengual@gmail.com
OI Mengual, Ximo/0000-0002-6185-9404
NR 92
TC 6
Z9 6
U1 0
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0307-6970
EI 1365-3113
J9 SYST ENTOMOL
JI Syst. Entomol.
PD OCT
PY 2011
VL 36
IS 4
BP 713
EP 731
DI 10.1111/j.1365-3113.2011.00588.x
PG 19
WC Evolutionary Biology; Entomology
SC Evolutionary Biology; Entomology
GA 822LH
UT WOS:000295047400008
ER
PT J
AU Gutermuth, RA
Pipher, JL
Megeath, ST
Myers, PC
Allen, LE
Allen, TS
AF Gutermuth, R. A.
Pipher, J. L.
Megeath, S. T.
Myers, P. C.
Allen, L. E.
Allen, T. S.
TI A CORRELATION BETWEEN SURFACE DENSITIES OF YOUNG STELLAR OBJECTS AND GAS
IN EIGHT NEARBY MOLECULAR CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: stars; stars: formation
ID SPITZER C2D SURVEY; STAR-FORMING REGIONS; DENSE GAS; INTERSTELLAR
CLOUDS; EMBEDDED CLUSTERS; PRESTELLAR CORES; FORMATION RATES; MASS
FUNCTION; FORMATION LAW; ORION NEBULA
AB We report the discovery and characterization of a power-law correlation between the local surface densities of Spitzer-identified, dusty young stellar objects (YSOs) and the column density of gas (as traced by near-IR extinction) in eight molecular clouds within 1 kpc and with 100 or more known YSOs. This correlation, which appears in data smoothed over size scales of similar to 1 pc, varies in quality from cloud to cloud; those clouds with tight correlations, MonR2 and Ophiuchus, are fit with power laws of slope 2.67 and 1.87, respectively. The spread in the correlation is attributed primarily to local gas disruption by stars that formed there or to the presence of very young subregions at the onset of star formation. We explore the ratio of the number of Class II to Class I sources, a proxy for the star formation age of a region, as a function of gas column density; this analysis reveals a declining Class II to Class I ratio with increasing column density. We show that the observed star-gas correlation is consistent with a star formation law where the star formation rate per area varies with the gas column density squared. We also propose a simple picture of thermal fragmentation of dense gas in an isothermal, self-gravitating layer as an explanation for the power law. Finally, we briefly compare the star-gas correlation and its implied star formation law with other recent proposed of star formation laws at similar and larger size scales from nearby star-forming regions.
C1 [Gutermuth, R. A.] Smith Coll, Dept Astron, Coll 5, Northampton, MA 01063 USA.
[Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Pipher, J. L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Megeath, S. T.; Allen, T. S.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
RP Gutermuth, RA (reprint author), Smith Coll, Dept Astron, Coll 5, Northampton, MA 01063 USA.
FU National Aeronautics and Space Administration [1407, 960541]; National
Science Foundation
FX This publication makes use of data products from the Two Micron All Sky
Survey, which is a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center/California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation. This research has made use of the
SIMBAD database, operated at CDS, Strasbourg, France. This research has
made use of the VizieR catalogue access tool, CDS, Strasbourg, France.
This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract 1407 with NASA.
Support for the IRAC instrument was provided by NASA through contract
960541 issued by JPL.
NR 70
TC 84
Z9 84
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 OCT 1
PY 2011
VL 739
IS 2
AR 84
DI 10.1088/0004-637X/739/2/84
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800029
ER
PT J
AU Jimenez-Serra, I
Martin-Pintado, J
Winters, JM
Rodriguez-Franco, A
Caselli, P
AF Jimenez-Serra, I.
Martin-Pintado, J.
Winters, J. -M.
Rodriguez-Franco, A.
Caselli, P.
TI VARIABILITY OF THE SiO THERMAL LINE EMISSION TOWARD THE YOUNG L1448-mm
OUTFLOW
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (L1448); ISM: jets and outflows; shock waves;
stars: formation
ID C-TYPE SHOCKS; MOLECULAR OUTFLOWS; PROPER MOTIONS; X-RAY; WAVES;
EVOLUTION; CLOUDS; ORION; JET; PROPAGATION
AB The detection of narrow SiO thermal emission toward young outflows has been proposed to be a signature of the magnetic precursor of C-shocks. Recent modeling of the SiO emission across C-shocks predicts variations in the SiO line intensity and line shape at the precursor and intermediate-velocity regimes in only a few years. We present high angular resolution (3.'' 8 x 3.'' 3) images of the thermal SiO J = 2 -> 1 emission toward the L1448-mm outflow in two epochs (2004 November-2005 February, 2009 March-April). Several SiO condensations have appeared at intermediate velocities (20-50 km s(-1)) toward the redshifted lobe of the outflow since 2005. Toward one of the condensations (clump D), systematic differences of the dirty beams between 2005 and 2009 could be responsible for the SiO variability. At higher velocities (50-80 km s(-1)), SiO could also have experienced changes in its intensity. We propose that the SiO variability toward L1448-mm is due to a real SiO enhancement by young C-shocks at the internal working surface between the jet and the ambient gas. For the precursor regime (5.2-9.2 km s(-1)), several narrow and faint SiO components are detected. The narrow SiO components tend to be compact, transient and show elongated (bow-shock) morphologies perpendicular to the jet. We speculate that these features are associated with the precursor of C-shocks appearing at the interface of the new SiO components seen at intermediate velocities.
C1 [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Martin-Pintado, J.; Rodriguez-Franco, A.] CSIC INTA, Ctr Astrobiol, E-28850 Madrid, Spain.
[Winters, J. -M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Rodriguez-Franco, A.] Univ Complutense Madrid, Escuela Univ Opt, Dept Matemat Aplicada Biomatemat, E-28037 Madrid, Spain.
[Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
RP Jimenez-Serra, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ijimenez-serra@cfa.harvard.edu; jmartin@cab.inta-csic.es;
winters@iram.fr; rodriguezfa@cab.inta-csic.es; P.Caselli@leeds.ac.uk
RI Martin-Pintado, Jesus/H-6107-2015
OI Martin-Pintado, Jesus/0000-0003-4561-3508
FU INSU/CNRS (France); MPG (Germany); IGN (Spain); SMA; MICINN
[ESP2007-65812-C02-C01, AYA2010-21697-C05-01]; AstroMadrid [CAM
S2009/ESP-1496]
FX Based on observations carried out with the IRAM Plateau de Bure
Interferometer (PdBI). IRAM is supported by INSU/CNRS (France), MPG
(Germany), and IGN (Spain).; We thank the IRAM director, P. Cox, for
letting us carry out the second epoch of the PdBI SiO observations,
despite the reticence of the IRAM Programme Committee. We acknowledge an
anonymous referee for his/her critical reading and constructive comments
that helped to largely improve the manuscript. I. J.-S. acknowledges the
Smithsonian Astrophysical Observatory for the support provided through
an SMA fellowship. J. M.-P. and I. J.-S. have been partially funded by
MICINN grants ESP2007-65812-C02-C01 and AYA2010-21697-C05-01 and
AstroMadrid (CAM S2009/ESP-1496).
NR 34
TC 4
Z9 4
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 OCT 1
PY 2011
VL 739
IS 2
AR 80
DI 10.1088/0004-637X/739/2/80
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800025
ER
PT J
AU Lin, L
Kouveliotou, C
Baring, MG
van der Horst, AJ
Guiriec, S
Woods, PM
Gogus, E
Kaneko, Y
Scargle, J
Granot, J
Preece, R
von Kienlin, A
Chaplin, V
Watts, AL
Wijers, RAMJ
Zhang, SN
Bhat, N
Finger, MH
Gehrels, N
Harding, A
Kaper, L
Kaspi, V
Mcenery, J
Meegan, CA
Paciesas, WS
Pe'er, A
Ramirez-Ruiz, E
van der Klis, M
Wachter, S
Wilson-Hodge, C
AF Lin, Lin
Kouveliotou, Chryssa
Baring, Matthew G.
van der Horst, Alexander J.
Guiriec, Sylvain
Woods, Peter M.
Gogus, Ersin
Kaneko, Yuki
Scargle, Jeffrey
Granot, Jonathan
Preece, Robert
von Kienlin, Andreas
Chaplin, Vandiver
Watts, Anna L.
Wijers, Ralph A. M. J.
Zhang, Shuang Nan
Bhat, Narayan
Finger, Mark H.
Gehrels, Neil
Harding, Alice
Kaper, Lex
Kaspi, Victoria
Mcenery, Julie
Meegan, Charles A.
Paciesas, William S.
Pe'er, Asaf
Ramirez-Ruiz, Enrico
van der Klis, Michiel
Wachter, Stefanie
Wilson-Hodge, Colleen
TI Fermi/GAMMA-RAY BURST MONITOR OBSERVATIONS OF SGR J0501+4516 BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (SGR J0501+4516); X-rays: bursts
ID SOFT GAMMA-REPEATERS; RESONANT CYCLOTRON SCATTERING; 1E 1547.0-5408;
MAGNETAR; EMISSION; SGR-1900+14; SPECTRA; TIME;
SOFT-GAMMA-REPEATER-1806-20; SPECTROSCOPY
AB We present our temporal and spectral analyses of 29 bursts from SGR J0501+4516, detected with the gamma-ray burst monitor on board the Fermi Gamma-ray Space Telescope during 13 days of the source's activation in 2008 (August 22-September 3). We find that the T-90 durations of the bursts can be fit with a log-normal distribution with a mean value of similar to 123 ms. We also estimate for the first time event durations of soft gamma repeater (SGR) bursts in photon space (i.e., using their deconvolved spectra) and find that these are very similar to the T-90 values estimated in count space (following a log-normal distribution with a mean value of similar to 124 ms). We fit the time-integrated spectra for each burst and the time-resolved spectra of the five brightest bursts with several models. We find that a single power law with an exponential cutoff model fits all 29 bursts well, while 18 of the events can also be fit with two blackbody functions. We expand on the physical interpretation of these two models and we compare their parameters and discuss their evolution. We show that the time-integrated and time-resolved spectra reveal that E-peak decreases with energy flux (and fluence) to a minimum of similar to 30 keV at F = 8.7 x 10(-6) erg cm(-2) s(-1), increasing steadily afterward. Two more sources exhibit a similar trend: SGRs J1550-5418 and 1806-20. The isotropic luminosity, L-iso, corresponding to these flux values is roughly similar for all sources (0.4-1.5 x 10(40) erg s(-1)).
C1 [Lin, Lin; Zhang, Shuang Nan] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Lin, Lin; Guiriec, Sylvain; Preece, Robert; Chaplin, Vandiver; Bhat, Narayan; Paciesas, William S.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Kouveliotou, Chryssa; Wilson-Hodge, Colleen] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
[van der Horst, Alexander J.; Finger, Mark H.; Meegan, Charles A.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA.
[Woods, Peter M.] Corvid Technol, Huntsville, AL 35806 USA.
[Gogus, Ersin; Kaneko, Yuki] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey.
[Scargle, Jeffrey] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Granot, Jonathan] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[von Kienlin, Andreas] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Watts, Anna L.; Wijers, Ralph A. M. J.; Kaper, Lex; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Zhang, Shuang Nan] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China.
[Gehrels, Neil; Harding, Alice; Mcenery, Julie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kaspi, Victoria] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Wachter, Stefanie] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Lin, L (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
EM lin.lin@uah.edu
RI Gehrels, Neil/D-2971-2012; Harding, Alice/D-3160-2012; McEnery,
Julie/D-6612-2012;
OI Wijers, Ralph/0000-0002-3101-1808; Preece, Robert/0000-0003-1626-7335
FU NASA [NNH07ZDA001-GLAST, NNX10AC59A]; Scientific and Technological
Research Council of Turkey (TUBITAK) [109T755]; Bundesministeriums fur
Wirtschaft und Technologie (BMWi) [50 OG 1101]; Netherlands Organization
for Scientific Research (NWO); European Research Council [247295]
FX This publication is part of the GBM/Magnetar Key Project (NASA grant
NNH07ZDA001-GLAST, PI: C. Kouveliotou). M. G. B. acknowledges support
from NASA through grant NNX10AC59A. E.G. and Y.K. acknowledge the
support from the Scientific and Technological Research Council of Turkey
(TUBITAK) through grant 109T755. A. v. K. was supported by the
Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR
grant 50 OG 1101. A. L. W. acknowledges support from a Netherlands
Organization for Scientific Research (NWO) Vidi Grant. R.A.M.J.W.
acknowledges support from the European Research Council via Advanced
Investigator Grant No. 247295.
NR 48
TC 22
Z9 22
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 OCT 1
PY 2011
VL 739
IS 2
AR 87
DI 10.1088/0004-637X/739/2/87
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800032
ER
PT J
AU Oberst, TE
Parshley, SC
Nikola, T
Stacey, GJ
Lohr, A
Lane, AP
Stark, AA
Kamenetzky, J
AF Oberst, T. E.
Parshley, S. C.
Nikola, T.
Stacey, G. J.
Loehr, A.
Lane, A. P.
Stark, A. A.
Kamenetzky, J.
TI A 205 mu m [N II] MAP OF THE CARINA NEBULA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE H II regions; infrared: ISM; ISM: individual objects (Carina Nebula);
ISM: lines and bands; photon-dominated region (PDR); submillimeter: ISM
ID LASER MAGNETIC-RESONANCE; ANTARCTIC-SUBMILLIMETER-TELESCOPE;
LONG-WAVELENGTH SPECTROMETER; FAR-INFRARED OBSERVATIONS; MOLECULAR CLOUD
COMPLEX; STAR-FORMING REGION; PHOTODISSOCIATION REGIONS; C-II;
INTERSTELLAR-MEDIUM; PHYSICAL CONDITIONS
AB We present the results of a similar to 250 arcmin(2) mapping of the 205 mu m [N II] fine-structure emission over the northern Carina Nebula, including the Car I and Car II H II regions. Spectra were obtained using the South Pole Imaging Fabry-Perot Interferometer (SPIFI) at the Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) at the South Pole. We supplement the 205 mu m data with new reductions of far-IR fine-structure spectra from the Infrared Space Observatory (ISO) Long Wavelength Spectrometer (LWS) in 63 mu m [O I], 122 mu m [N II], 146 mu m [O I], and 158 mu m [C II]; the 146 mu m [O I] data include 90 raster positions which have not been previously published. Morphological comparisons are made with optical, radio continuum, and CO maps. The 122/205 line ratio is used to probe the density of the low-ionization gas, and the 158/205 line ratio is used to probe the fraction of C+ arising from photodissociation regions (PDRs). The [O I] and [C II] lines are used to construct a PDR model of Carina. When the PDR properties are compared with other sources, Carina is found to be more akin to 30 Doradus than galactic star-forming regions such as Orion, M17, or W49; this is consistent with the view of Carina as a more evolved region, where much of the parent molecular cloud has been ionized or swept away. These data constitute the first ground-based detection of the 205 mu m [N II] line, and the third detection overall since those of COBE FIRAS and the Kuiper Airborne Observatory in the early 1990s.
C1 [Oberst, T. E.; Parshley, S. C.; Nikola, T.; Stacey, G. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Loehr, A.; Lane, A. P.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kamenetzky, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA.
RP Oberst, TE (reprint author), Westminster Coll, Dept Phys, New Wilmington, PA 16172 USA.
EM oberstte@westminster.edu
FU NASA [GSRP NNG05GK70H]; NSF [IGERT DGE-9870631, CSIP DGE-0231913,
OPP-0094605, OPP-0338149, OPP0126090]
FX The authors especially thank the following individuals and groups:
Carole E. Tucker, who provided SPIFI's filters; Jacob W. Kooi, for
operating local oscillators at the AST/RO during SPIFI calibration; K.
Sigfrid Yngvesson and the TREND group, for use of the TREND laser at the
AST/RO during SPIFI calibration; and prior members of the SPIFI team,
including C. Matt Bradford, Alberto D. Bolatto, James M. Jackson, Mark
R. Swain, Maureen L. Savage, Jacqueline A. Davidson, and similar to 15
undergraduate student researchers. Finally, we are thankful for the
support of the following grants: NASA GSRP NNG05GK70H; NSF IGERT
DGE-9870631; NSF CSIP DGE-0231913; and NSF OPP-0094605, OPP-0338149, and
OPP0126090.
NR 94
TC 22
Z9 22
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2011
VL 739
IS 2
AR 100
DI 10.1088/0004-637X/739/2/100
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800045
ER
PT J
AU Perlman, ES
Georganopoulos, M
Marshall, HL
Schwartz, DA
Padgett, CA
Gelbord, J
Lovell, JEJ
Worrall, DM
Birkinshaw, M
Murphy, DW
Jauncey, DL
AF Perlman, Eric S.
Georganopoulos, Markos
Marshall, Herman L.
Schwartz, Daniel A.
Padgett, C. A.
Gelbord, Jonathan
Lovell, J. E. J.
Worrall, Diana M.
Birkinshaw, Mark
Murphy, David W.
Jauncey, David L.
TI DEEP MULTIWAVEBAND OBSERVATIONS OF THE JETS OF 0208-512 AND 1202-262
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: jets; quasars: individual (PKS0208-512,
PKS1202-262); radio continuum: galaxies; X-rays: galaxies
ID X-RAY JETS; SPACE-TELESCOPE OBSERVATIONS; SPECTRUM RADIO QUASARS;
INVERSE-COMPTON MODEL; EXTRAGALACTIC JETS; SOUTHERN-HEMISPHERE; PKS
0637-752; CHANDRA; EMISSION; SYNCHROTRON
AB We present deep Hubble Space Telescope, Chandra, Very Large Array, and Australia Telescope Compact Array images of the jets of PKS 0208-512 and PKS 1202-262, which were found in a Chandra survey of a flux-limited sample of flat-spectrum radio quasars with jets. We discuss in detail their X-ray morphologies and spectra. We find optical emission from one knot in the jet of PKS 1202-262 and two regions in the jet of PKS 0208-512. The X-ray emission of both jets is most consistent with external Comptonization of cosmic microwave background photons by particles within the jet, while the optical emission is most consistent with the synchrotron process. We model the emission from the jet in this context and discuss implications for jet emission models, including magnetic field and beaming parameters.
C1 [Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Perlman, Eric S.; Georganopoulos, Markos] Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Georganopoulos, Markos; Padgett, C. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Marshall, Herman L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Schwartz, Daniel A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Gelbord, Jonathan] Univ Durham, Dept Phys, Sci Labs, Durham DH1 3LE, England.
[Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Lovell, J. E. J.; Jauncey, David L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Worrall, Diana M.; Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Murphy, David W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 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; georgano@umbc.edu; hermanm@space.mit.edu;
das@head-cfa.harvard.edu; j.m.gelbord@durham.ac.uk;
Jim.Lovell@utas.edu.au; d.worrall@bristol.ac.uk;
mark.birkinshaw@bristol.ac.uk; dwm@sgra.jpl.nasa.gov;
david.jauncey@csiro.au
OI Perlman, Eric/0000-0002-3099-1664
FU Chandra GO [G02-3151D, G04- 5107X]; HST [STGO-10002.01]; NASA
[NAG5-9997, NNG05-GD63DG, SAO SV1-61010, NAS8-39073, NAS8-03060]; UMBC
[NNX07-AM17G]; CXC [GO2-3151A, G02-3151C]
FX E. S. P., C. A. P., and M. G. acknowledge support from Chandra GO grants
G02-3151D and G04- 5107X), HST (grant STGO-10002.01), and NASA (LTSA
grants NAG5-9997 and NNG05-GD63DG at UMBC and NNX07-AM17G at FIT). H. L.
M. was supported under NASA contract SAO SV1-61010 for the Chandra X-Ray
Center (CXC). J.M.G. was supported under Chandra grant GO2-3151A to MIT
from the CXC. D. A. S. was partially supported by Chandra grant
G02-3151C to SAO from the CXC, and by NASA contracts NAS8-39073 and
NAS8-03060 to the CXC.
NR 53
TC 3
Z9 3
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD OCT 1
PY 2011
VL 739
IS 2
AR 65
DI 10.1088/0004-637X/739/2/65
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821IZ
UT WOS:000294969800010
ER
PT J
AU Binder, B
Williams, BF
Kong, AKH
Gaetz, TJ
Plucinsky, PP
Dalcanton, JJ
Weisz, DR
AF Binder, B.
Williams, B. F.
Kong, A. K. H.
Gaetz, T. J.
Plucinsky, P. P.
Dalcanton, J. J.
Weisz, D. R.
TI CHANDRA DETECTION OF SN 2010da FOUR MONTHS AFTER OUTBURST: EVIDENCE FOR
A HIGH-MASS X-RAY BINARY IN NGC 300
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE stars: massive; supernovae: individual (SN 2010da); X-rays: binaries
ID SMALL-MAGELLANIC-CLOUD; ACIS SURVEY; XMM-NEWTON
AB We present the results of a 63 ks Chandra observation of the "supernova impostor" SN 2010da four months after it was first observed on 2010 May 24. We detect an X-ray source at similar to 7 sigma confidence coincident with the optical location of the outburst. Our imaging analysis has revealed a hard central point source, surrounded by soft diffuse emission extending similar to 8 '' north of the central source. The diffuse emission has a hardness ratio (similar to-0.4), 0.35-2 keV luminosity (similar to 6 x 10(35) erg s(-1)), and size (similar to 70 pc) consistent with that of a supernova remnant, although the low number of counts prohibits detailed spectral modeling. The 0.5-6 keV spectrum of the central point source is well described by both a power law with Gamma similar to 0 and a blackbody with kT similar to 1.8 keV, with no evidence for intrinsic absorption beyond the Galactic column. We estimate the 0.3-10 keV luminosity to be similar to 2 x 10(37) erg s(-1), a factor of similar to 25 decrease since the initial outburst. The high X-ray luminosity and slow fading rate is not consistent with this object being a single massive star undergoing an outburst. When combined with the optical and infrared properties of the outburst and progenitor systems, our X-ray observations suggest the SN 2010da system may be a Be X-ray binary system which experienced an extremely bright optical outburst near simultaneously with a bright, Type II X-ray outburst.
C1 [Binder, B.; Williams, B. F.; Dalcanton, J. J.; Weisz, D. R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan.
[Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan.
[Gaetz, T. J.; Plucinsky, P. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Binder, B (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA.
FU Chandra grant [GO1-12118X]; NASA [NAS8-03060]
FX The authors thank an anonymous referee for the many helpful comments
which significantly improved this manuscript, as well as C. S. Kochanek,
J. L. Prieto, and R. Humphreys for insightful communications on this
source. The authors thank M. Eracleous and E. Skillman for comments on
early drafts of this manuscript. This work made use of data supplied by
the UK Swift Science Data Centre at the University of Leicester and the
NASA/IPAC Extragalactic Database (NED) which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. B.B.
and B.F.W. acknowledge support from Chandra grant GO1-12118X. T.J.G. and
P.P.P. acknowledge support of NASA Contract NAS8-03060.
NR 33
TC 6
Z9 6
U1 0
U2 5
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 OCT 1
PY 2011
VL 739
IS 2
AR L51
DI 10.1088/2041-8205/739/2/L51
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821TP
UT WOS:000294997600017
ER
PT J
AU Fayolle, EC
Bertin, M
Romanzin, C
Michaut, X
Oberg, KI
Linnartz, H
Fillion, JH
AF Fayolle, Edith C.
Bertin, Mathieu
Romanzin, Claire
Michaut, Xavier
Oeberg, Karin I.
Linnartz, Harold
Fillion, Jean-Hugues
TI CO ICE PHOTODESORPTION: A WAVELENGTH-DEPENDENT STUDY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: molecules; molecular data;
molecular processes
ID PROTOPLANETARY DISKS; ELECTRON-IMPACT; WATER ICE; DESORPTION;
INTERSTELLAR; N-2; ADSORPTION; RADIATION; MOLECULES; SURFACES
AB UV-induced photodesorption of ice is a non-thermal evaporation process that can explain the presence of cold molecular gas in a range of interstellar regions. Information on the average UV photodesorption yield of astrophysically important ices exists for broadband UV lamp experiments. UV fields around low-mass pre-main-sequence stars, around shocks and in many other astrophysical environments are however often dominated by discrete atomic and molecular emission lines. It is therefore crucial to consider the wavelength dependence of photodesorption yields and mechanisms. In this work, for the first time, the wavelength-dependent photodesorption of pure CO ice is explored between 90 and 170 nm. The experiments are performed under ultra high vacuum conditions using tunable synchrotron radiation. Ice photodesorption is simultaneously probed by infrared absorption spectroscopy in reflection mode of the ice and by quadrupole mass spectrometry of the gas phase. The experimental results for CO reveal a strong wavelength dependence directly linked to the vibronic transition strengths of CO ice, implying that photodesorption is induced by electronic transition (DIET). The observed dependence on the ice absorption spectra implies relatively low photodesorption yields at 121.6 nm (Ly alpha), where CO barely absorbs, compared to the high yields found at wavelengths coinciding with transitions into the first electronic state of CO (A(1)Pi at 150 nm); the CO photodesorption rates depend strongly on the UV profiles encountered in different star formation environments.
C1 [Fayolle, Edith C.; Linnartz, Harold] Leiden Univ, Leiden Observ, Sackler Lab Astrophys, NL-2300 RA Leiden, Netherlands.
[Bertin, Mathieu; Romanzin, Claire; Michaut, Xavier; Fillion, Jean-Hugues] Univ Paris 06, Lab Phys Mol Atmosphere & Astrophys, CNRS UMR7092, F-75005 Paris, France.
[Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Fayolle, EC (reprint author), Leiden Univ, Leiden Observ, Sackler Lab Astrophys, POB 9513, NL-2300 RA Leiden, Netherlands.
RI Bertin, Mathieu/C-7134-2012;
OI Bertin, Mathieu/0000-0002-9021-2415; Fayolle, Edith/0000-0001-8109-5256
FU French national program PCMI (Physique chimie du milieu interstellaire);
Dutch program NOVA (Nederlandse Onderzoekschool Voor Astronomie); COST
action [CM0805]; Hubert Curien Partenership "Van Gogh"; NASA; Space
Telescope Science Institute [NAS 5-26555]
FX We are grateful to Ewine van Dishoeck and Marc van Hemert for
stimulating discussions. We thank Hsiao-Chi Lu, Roland Gredel, and Edwin
Bergin for providing useful data. We acknowledge SOLEIL for provision of
synchrotron radiation facilities, as well as Laurent Nahon for technical
help on the beamline DESIRS. Financial support from the French national
program PCMI (Physique chimie du milieu interstellaire), the Dutch
program NOVA (Nederlandse Onderzoekschool Voor Astronomie), the COST
action CM0805 "The Chemical Cosmos," and the Hubert Curien Partenership
"Van Gogh," are gratefully acknowledged. 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.
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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 OCT 1
PY 2011
VL 739
IS 2
AR L36
DI 10.1088/2041-8205/739/2/L36
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821TP
UT WOS:000294997600002
ER
PT J
AU Torok, T
Panasenco, O
Titov, VS
Mikic, Z
Reeves, KK
Velli, M
Linker, JA
De Toma, G
AF Toeroek, T.
Panasenco, O.
Titov, V. S.
Mikic, Z.
Reeves, K. K.
Velli, M.
Linker, J. A.
De Toma, G.
TI A MODEL FOR MAGNETICALLY COUPLED SYMPATHETIC ERUPTIONS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE methods: numerical; Sun: corona; Sun: coronal mass ejections (CMEs);
Sun: filaments, prominences; Sun: flares; Sun: magnetic topology
ID CORONAL MASS EJECTIONS; SOLAR CORONA; FLUX ROPES; FLARES; TOPOLOGY;
RECONNECTION; OSCILLATIONS; CONNECTION; FILAMENTS; LINKAGES
AB Sympathetic eruptions on the Sun have been observed for several decades, but the mechanisms by which one eruption can trigger another remain poorly understood. We present a three-dimensional MHD simulation that suggests two possible magnetic trigger mechanisms for sympathetic eruptions. We consider a configuration that contains two coronal flux ropes located within a pseudo-streamer and one rope located next to it. A sequence of eruptions is initiated by triggering the eruption of the flux rope next to the streamer. The expansion of the rope leads to two consecutive reconnection events, each of which triggers the eruption of a flux rope by removing a sufficient amount of overlying flux. The simulation qualitatively reproduces important aspects of the global sympathetic event on 2010 August 1 and provides a scenario for the so-called twin filament eruptions. The suggested mechanisms are also applicable for sympathetic eruptions occurring in other magnetic configurations.
C1 [Toeroek, T.; Titov, V. S.; Mikic, Z.; Linker, J. A.] Predict Sci Inc, San Diego, CA 92121 USA.
[Panasenco, O.] Helio Res, La Crescenta, CA 91214 USA.
[Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[De Toma, G.] HAO NCAR, Boulder, CO 80307 USA.
RP Torok, T (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA 92121 USA.
RI Reeves, Katharine/P-9163-2014
FU NASA [NNX09AG27G]; NASA/SHP [NNH09AK02I]; Lockheed-Martin [SP02H1701R];
International Space Science Institute via International Team 174 on
Solar Prominence Formation and Equilibrium
FX We thank P. Demoulin, B. Kliem, and K. Schrijver for stimulating
discussions. The contribution of T.T, V.S.T., Z.M., and J.A.L. was
supported by NASA's HTP, LWS, and SR&T programs, CISM (an NSF Science
and Technology Center), and a contract from Lockheed-Martin to
Predictive Science, Inc. O.P. was supported by NASA grant NNX09AG27G,
G.D.T. by NASA/SHP grant NNH09AK02I, and K. K. R. by contract SP02H1701R
from Lockheed-Martin to SAO. M.V's. contribution was carried out at JPL
(Caltech) under a contract with NASA. Computational resources were
provided by NSF TACC in Austin and by NASA NAS at the Ames Research
Center. This work was partially supported by the International Space
Science Institute via International Team 174 on Solar Prominence
Formation and Equilibrium.
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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 OCT 1
PY 2011
VL 739
IS 2
AR L63
DI 10.1088/2041-8205/739/2/L63
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821TP
UT WOS:000294997600029
ER
PT J
AU Prasad, AKSK
Nienow, JA
Hargraves, P
AF Prasad, Akshinthala K. S. K.
Nienow, James A.
Hargraves, Paul
TI Plicate species of the diatom genus Thalassiosira (Bacillariophyta) from
the Atlantic and Gulf coasts of southeastern United States, with the
description of T.livingstoniorum sp nov.
SO PROCEEDINGS OF THE ACADEMY OF NATURAL SCIENCES OF PHILADELPHIA
LA English
DT Article
DE Thalassiosira cedarkeyensis; T. livingstoniorum sp nov.; plicate valves;
Indian River Lagoon; Gulf coast of Florida; diatom blooms; Fenholloway
estuary; Econfina estuary
AB Long-term observations of a marine planktonic plicate Tlzalassiosira species, T. cedarkeyensis Prasad, from the Gulf coasts of Florida, Alabama, and Mississippi and the Atlantic coasts of Florida and Georgia demonstrate its wide occurrence in the southeastern United States and its ability to form extensive blooms. We also report for the first time its ability to form typical Thalassiosira chains, linking sibling cells by threads of chitin. A closely related and co-occurring diatom, T. livingstoniorum, is described on the basis of investigations conducted during 2000-2011 as a new species from many localities in Apalachee Bay on the Gulf coast and Indian River Lagoon on the Atlantic coast of Florida. It differs from T. cedarkeyensis in areola density, presence of continuous cribra on loculate areolae, arrangement and distribution of valve processes, and the number of satellite pores surrounding the valve-face fultoportulae. We have not yet found any evidence of chain formation in T. livingstoniorum. Thalassiosira cedarkeyensis and T. livingstoniorum can be easily distinguished in Naphrax-mounted preparations in light microscopy (LM), and they represent two different groups (lineages?) of plicate species with reference to internal cribrum structure of the loculate areolae. Their differences may justify placement in two different genera. Although T. cedarkeyensis (which has individual cribra on the proximal siliceous layer like T. hyperborea) is abundant and widespread on the Gulf and Atlantic coasts of the southeastern United States, T. livingstoniorum (which has continuous cribra like T. lacustris) has been found, thus far, only in Florida coastal waters. Comparisons are made between these two species and the other morphologically similar extant and extinct plicate species. Thalassiosira livingstoniorum and T. cedarkeyensis, although widespread and frequently encountered during warmer months, may be easily overlooked sources of primary production in the nutrient-rich northeastern Gulf of Mexico.
C1 [Prasad, Akshinthala K. S. K.] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA.
[Nienow, James A.] Valdosta State Univ, Dept Biol, Valdosta, GA 31698 USA.
[Hargraves, Paul] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA.
[Hargraves, Paul] Florida Atlantic Univ, Harbor Branch Oceanog Inst, Boca Raton, FL 33431 USA.
[Hargraves, Paul] Smithsonian Marine Stn, Ft Pierce, FL USA.
RP Prasad, AKSK (reprint author), Florida State Univ, Dept Biol Sci, B-157, Tallahassee, FL 32306 USA.
EM prasad@bio.fsu.edu
FU Florida Fish & Wildlife Research Institute [06135]; State of Florida's
Save our Seas license plate program
FX We acknowledge with gratitude all crew members who made collections used
in this work, especially R. J. Livingston, R. L. Howell IV, and W. K.
Karsteter for the monthly phytoplankton samples from the Econfina and
Fenholloway estuaries from 1991 through 2003, and B. A. Vittor &
Associates, Inc., Dr. Carl M. Way, J. O'Neal, and D. Lee for providing
phytoplankton samples from the same sites from 2003 through 2009. P. A.
Fryxell kindly provided the Latin translation of the description for the
new species. AKSKP thanks K A Riddle and T. Fellers of the Florida State
University Biological Science Imaging Resource Facility for their
skillful and expert technical assistance with scanning electron
microscopes, T. Fellers for Figure 27, and Charles Bad land for
preparing the photographic plates. PEH thanks D. Hanisak (Harbor Branch
Oceanographic Institute (HBOI) at Florida Atlantic University) and J.
Piraino (Smithsonian Marine Station (SMS) at Fort Pierce) for logistic
and technical support. This is HBOI contribution #1839 and SMS
contribution #864. Sample collection in the Indian River Lagoon was
supported by Florida Fish & Wildlife Research Institute (FWC Agreement
#06135 and the State of Florida's Save our Seas license plate program).
NR 95
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PU ACAD NATURAL SCIENCES PHILA
PI PHILADELPHIA
PA SCIENTIFIC PUBLICATIONS, 1900 BENJ FRANKLIN PKWY, PHILADELPHIA, PA
19103-1195 USA
SN 0097-3157
J9 P ACAD NAT SCI PHILA
JI Proc. Acad. Nat. Sci. Phila.
PD OCT
PY 2011
VL 161
BP 1
EP 34
PG 34
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA V29TJ
UT WOS:000208770400001
ER
PT J
AU Wisman, JD
Smith, JF
AF Wisman, Jon D.
Smith, James F.
TI Legitimating Inequality: Fooling Most of the People All of the Time
SO AMERICAN JOURNAL OF ECONOMICS AND SOCIOLOGY
LA English
DT Article
ID UNITED-STATES; INCOME INEQUALITY; MOBILITY; HEALTH; CRIME
AB Over the three decades leading up to the crisis of 2008, inequality dramatically increased in the United States and Great Britain. What stands out, but is seldom noted, is that this occurred within democracies where the relative losers-the overwhelming majority-could in principle have used the political system to block or reverse rising inequality. Why did they not do so? A glance at history reveals that peoples have only very infrequently contested inequality because they were led to believe that their inferior status in terms of income, wealth, and privilege was just, that it was not really so bad, or that it was necessary for their future well-being. Ideological systems legitimated a status quo of inequality, or in more modern times even increasing inequality. This article surveys the manner in which inequality has been historically legitimated, first predominantly by religion, then predominately by economic thought. Attention is then focused on the manner in which contemporary economic science and its popular interpretations in the media have served to legitimate inequality in the U.S. since the mid-1970s. The article concludes with a reflection on the unique conditions that enable the legitimation of inequality to be delegitimated.
C1 [Wisman, Jon D.; Smith, James F.] American Univ, Washington, DC 20016 USA.
[Wisman, Jon D.; Smith, James F.] Smithsonian Inst, Washington, DC 20560 USA.
RP Wisman, JD (reprint author), American Univ, Washington, DC 20016 USA.
NR 83
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U1 1
U2 14
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0002-9246
J9 AM J ECON SOCIOL
JI Am. J. Econ. Sociol.
PD OCT
PY 2011
VL 70
IS 4
BP 974
EP 1013
DI 10.1111/j.1536-7150.2011.00795.x
PG 40
WC Economics; Sociology
SC Business & Economics; Sociology
GA 815WZ
UT WOS:000294562000006
ER
PT J
AU Werling, BP
Meehan, TD
Robertson, BA
Gratton, C
Landis, DA
AF Werling, Ben P.
Meehan, Timothy D.
Robertson, Bruce A.
Gratton, Claudio
Landis, Douglas A.
TI Biocontrol potential varies with changes in biofuel-crop plant
communities and landscape perenniality
SO GLOBAL CHANGE BIOLOGY BIOENERGY
LA English
DT Article
DE biodiversity; biofuels; biological control; ecosystem services; land use
change
ID ECOSYSTEM SERVICES; AGRICULTURAL LANDSCAPES; NATURAL ENEMIES; BENEFICIAL
ARTHROPODS; GRASSLAND ECOSYSTEMS; BIOLOGICAL-CONTROL; BIODIVERSITY;
DIVERSITY; HABITATS; FARMLAND
AB We examined the potential local- and landscape-level impacts of different biofuel production systems on biocontrol, an important service provided by arthropod natural enemies. Specifically, we sampled natural enemies with sweep nets and measured predation of sentinel pest eggs in stands of corn, switchgrass and mixed prairie in Michigan and Wisconsin (total n = 40 for natural enemy sampling, n = 60 for egg predation), relating them to crop type, forb cover and diversity, and the composition and heterogeneity of the surrounding landscape. Grasslands with intermediate levels of forb cover and flower diversity supported two-orders of magnitude more natural enemy biomass, fourfold more natural enemy families, and threefold greater rates of egg predation than corn. Data suggest this was in part due to a general increase in biomass, richness and predation in perennial grasslands compared with corn, combined with a positive effect of intermediate levels of forb cover and flower diversity. Specifically, natural enemy biomass and family richness showed hump-shaped relationships to forb cover that peaked in sites with 5-25% forbs, while egg predation increased with floral diversity. At the landscape scale, both natural-enemy biomass and egg predation increased with the area of forest in the landscape, and egg predation almost doubled as the area of herbaceous, perennial habitats within 1.5km of study sites increased. Our results suggest that floristically diverse, perennial grasslands support diverse and abundant predator communities that contribute to natural pest suppression. In addition, large-scale production of biofuel crops could positively or negatively affect biocontrol services in agricultural landscapes through associated changes in the area of perennial habitats. Biofuel landscapes that incorporate perennial grasslands could support a variety of beneficial organisms and ecosystem services in addition to producing biomass.
C1 [Werling, Ben P.; Landis, Douglas A.] Michigan State Univ, Dept Entomol, DOE Great Lakes Bioenergy Res Ctr, E Lansing, MI 48824 USA.
[Meehan, Timothy D.; Gratton, Claudio] Univ Wisconsin, Dept Entomol, DOE Great Lakes Bioenergy Res Ctr, Madison, WI 53706 USA.
[Robertson, Bruce A.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA.
RP Werling, BP (reprint author), Michigan State Univ, Dept Entomol, DOE Great Lakes Bioenergy Res Ctr, E Lansing, MI 48824 USA.
EM werlingb@msu.edu
FU DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science)
[DE-FC02-07ER64494]; U.S. National Science Foundation; MSU
FX Mary Gardiner, Lauren Bailey, and Hannah Gaines established the GLBRC
Extensive site network and initial sampling protocols. Carol Baker and
Pam Mosley identified flower specimens in Michigan. Special thanks to
participating landowners as well as Ermyas Birru, Michael Burdick,
Amanda Falk, Emily Fricke, Adam Higgins, Steve Hong, Andy Jakubowski,
Liz Loomis, Craig Maier, Rachel Mallinger, Jessica Miesel, Emily
Mueller, Collin Schwantes, Cari Sebright, Ruth Smith and Laura Smith for
invaluable field assistance. Kay Gross, Anna Fiedler, Megan Woltz and
three anonymous reviewers provided comments on the manuscript. This work
was funded by the DOE Great Lakes Bioenergy Research Center (DOE BER
Office of Science DE-FC02-07ER64494), with additional support from the
U.S. National Science Foundation LTER Program, DOE Energy Efficiency and
Renewable Energy, and MSU AgBioResearch (formerly the Michigan
Agricultural Experiment Station).
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1757-1693
J9 GCB BIOENERGY
JI GCB Bioenergy
PD OCT
PY 2011
VL 3
IS 5
BP 347
EP 359
DI 10.1111/j.1757-1707.2011.01092.x
PG 13
WC Agronomy; Biotechnology & Applied Microbiology; Energy & Fuels
SC Agriculture; Biotechnology & Applied Microbiology; Energy & Fuels
GA 818BE
UT WOS:000294723100001
ER
PT J
AU Gaspar, C
Gaston, KJ
Borges, PAV
Cardoso, P
AF Gaspar, Clara
Gaston, Kevin J.
Borges, Paulo A. V.
Cardoso, Pedro
TI Selection of priority areas for arthropod conservation in the Azores
archipelago
SO JOURNAL OF INSECT CONSERVATION
LA English
DT Article
DE Arthropods; Azores; Complementarity; Irreplaceability; Optimisation
algorithm; Reserve selection
ID RESERVE SELECTION; PROTECTED AREAS; BIODIVERSITY; IRREPLACEABILITY;
PERFORMANCE; DIVERSITY; NETWORKS; COSTS; GOAL
AB The largest standardised database available to date for arthropods in native forests of the Azores archipelago was used to determine the minimum optimal set of native forest fragments needed to accomplish four different targets of species occurrence (presence-absence) and abundance (20, 50 and 80%) using different groups of arthropods and all data combined. The results showed that occurrence and 20% abundance targets gave similar optimal solutions for most of the groups considered. At least one fragment on each of the seven studied islands was required to accomplish any occurrence and abundance target. To achieve 80% of abundance for all species, all fragments were necessary and to guarantee 50% of the overall abundance of endemics, 17 out of 18 native forests were needed. A suggestion is made to apply a measure of biotic integrity related to disturbance to select, among alternative optimal solutions, the set of areas that will help to guarantee the viability of populations. Some guidelines for the selection of priority areas for conservation in the Azores are presented.
C1 [Gaspar, Clara; Borges, Paulo A. V.; Cardoso, Pedro] Univ Acores, Azorean Biodivers Grp CITA A, Dept Ciencias Agr, P-9701851 Terceira, Azores, Portugal.
[Gaspar, Clara; Gaston, Kevin J.] Univ Sheffield, Dept Anim & Plant Sci, Biodivers & Macroecol Grp, Sheffield S10 2TN, S Yorkshire, England.
[Cardoso, Pedro] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Gaspar, C (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, Dept Ciencias Agr, P-9701851 Terceira, Azores, Portugal.
EM cgaspar@ennor.org
RI Borges, Paulo/B-2780-2008; Cardoso, Pedro/A-8820-2008
OI Borges, Paulo/0000-0002-8448-7623; Cardoso, Pedro/0000-0001-8119-9960
FU Portuguese Fundacao para a Ciencia e a Tecnologia [BD/11049/2002];
Azorean Fundo Regional da Ciencia e Tecnologia [M3.1.7/F/007/2009];
Fundacao para a Ciencia e a Tecnologia [SFRH/BPD/40688/2007]; Azorean
Direccao Regional dos Recursos Florestais [17.01-080203]
FX We are grateful to all of the researchers that collaborated in the field
and laboratory: Alvaro Vitorino, Anabela Arraiol, Ana Rodrigues, Artur
Serrano, Carlos Aguiar, Catarina Melo, Francisco Dinis, Genage Andre,
Emanuel Barcelos, Fernando Pereira, Hugo Mas, Isabel Amorim, Joao
Amaral, Joaquin Hortal, Lara Dinis, Paula Goncalves, Sandra Jarroca,
Servio Ribeiro and Luis Vieira. The Forest Services provided local
support on each island. Acknowledgments are due to all of the
taxonomists who assisted in the identification of the morphotypes:
Andrew Polaszek, Bivar Sousa, Artur Serrano, Arturo Baz, Fernando
Ilharco, Henrik Enghoff, Jordi Ribes, Jose Quartau, Jorg Wunderlich,
Mario Boieiro, Ole Karsholt, Richard Strassen, Volker Manhert and
Virgilio Vieira. We thank Jon Sadler, Owen Petchey, Simone Fattorini and
an anonymous referee for helpful discussions and suggestions. CG was
funded by the Portuguese Fundacao para a Ciencia e a Tecnologia
(BD/11049/2002) during her PhD research project and has currently a
postdoctoral grant from the Azorean Fundo Regional da Ciencia e
Tecnologia (M3.1.7/F/007/2009). PC is supported by Fundacao para a
Ciencia e a Tecnologia (SFRH/BPD/40688/2007). Field work was also funded
by the Azorean Direccao Regional dos Recursos Florestais (Proj.
17.01-080203).
NR 38
TC 13
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U1 1
U2 7
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1366-638X
EI 1572-9753
J9 J INSECT CONSERV
JI J. Insect Conserv.
PD OCT
PY 2011
VL 15
IS 5
BP 671
EP 684
DI 10.1007/s10841-010-9365-4
PG 14
WC Biodiversity Conservation; Entomology
SC Biodiversity & Conservation; Entomology
GA 814MX
UT WOS:000294460700005
ER
PT J
AU Pour-Biazar, A
Khan, M
Wang, LH
Park, YH
Newchurch, M
McNider, RT
Liu, X
Byun, DW
Cameron, R
AF Pour-Biazar, Arastoo
Khan, Maudood
Wang, Lihua
Park, Yun-Hee
Newchurch, Mike
McNider, Richard T.
Liu, Xiong
Byun, Daewon W.
Cameron, Robert
TI Utilization of satellite observation of ozone and aerosols in providing
initial and boundary condition for regional air quality studies
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID MESOSCALE METEOROLOGICAL MODEL; NONLOCAL CLOSURE-MODEL; EMISSIONS;
SYSTEM; LAYER
AB To demonstrate the efficacy of satellite observations in the realization of the background and transboundary transport of pollution in regional air quality modeling practices, satellite observations of ozone and aerosol optical depth were incorporated in the EPA Models-3 Community Multiscale Air Quality (CMAQ) model (http://www.cmascenter.org). Observations from Ozone Monitoring Instrument (OMI) aboard NASA's Aura satellite and AOD products from the Moderate Resolution Imaging Spectroradiometer (MODIS) onboard Terra (EOS AM) and Aqua (EOS PM) satellites were used to specify initial and lateral boundary conditions (IC/BC) for a simulation that spanned over August 2006. The tools and techniques using the satellite data were tested in the context of current regulatory air quality modeling practices. Daily satellite observations were remapped onto the modeling domain and used as IC/BC for daily segments of a month-long simulation and the results were evaluated against surface and ozonesonde observations. Compared to the standard application of CMAQ, OMI O-3 profiles significantly improved model performance in the free troposphere and MODIS aerosol products substantially improved PM2.5 predictions in the boundary layer. The utilization of satellite data for BC helped in the realization of transboundary transport of pollution and was able to explain the recirculation of pollution from Northeast Corridor to the southeastern region. Ozone in the mid- to upper-troposphere was largely dominated by transport and thus benefited most from satellite provided BC. The ozone within the boundary layer was mostly affected by fast production/loss mechanisms that are impacted by surface emissions, chemistry and removal processes and was not impacted as much. A case study for August 18-22 demonstrated that model errors in the placement of a stationary front were the main reason for errors in PM2.5 predictions as the front acted as a boundary between high and low PM2.5 concentrations.
C1 [Pour-Biazar, Arastoo; McNider, Richard T.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA.
[Cameron, Robert] Bur Ocean Energy Management Regulat & Enforcement, Gulf Mexico OCS Reg, New Orleans, LA 70123 USA.
[Khan, Maudood; Wang, Lihua] Univ Space Res Assoc, Natl Space Sci & Technol Ctr, Huntsville, AL 35806 USA.
[Newchurch, Mike] Univ Alabama, Dept Atmospher Sci, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Byun, Daewon W.] NOAA, Air Resources Lab, Silver Spring, MD 20910 USA.
RP Pour-Biazar, A (reprint author), Univ Alabama, Ctr Earth Syst Sci, 320 Sparkman Dr, Huntsville, AL 35899 USA.
EM biazar@nsstc.uah.edu
RI Liu, Xiong/P-7186-2014
OI Liu, Xiong/0000-0003-2939-574X
FU University of Alabama in Huntsville; Bureau of Ocean Energy Management,
Regulation and Enforcement on Gulf of Mexico Issues; NASA
FX This work was accomplished under partial support from Cooperative
Agreement Between the University of Alabama in Huntsville and the Bureau
of Ocean Energy Management, Regulation and Enforcement on Gulf of Mexico
Issues, and the NASA Science Mission Directorate Applied Sciences
Program.
NR 50
TC 7
Z9 7
U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 30
PY 2011
VL 116
AR D18309
DI 10.1029/2010JD015200
PG 32
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 828XG
UT WOS:000295537000001
ER
PT J
AU Nittler, LR
Starr, RD
Weider, SZ
McCoy, TJ
Boynton, WV
Ebel, DS
Ernst, CM
Evans, LG
Goldsten, JO
Hamara, DK
Lawrence, DJ
McNutt, RL
Schlemm, CE
Solomon, SC
Sprague, AL
AF Nittler, Larry R.
Starr, Richard D.
Weider, Shoshana Z.
McCoy, Timothy J.
Boynton, William V.
Ebel, Denton S.
Ernst, Carolyn M.
Evans, Larry G.
Goldsten, John O.
Hamara, David K.
Lawrence, David J.
McNutt, Ralph L., Jr.
Schlemm, Charles E., II
Solomon, Sean C.
Sprague, Ann L.
TI The Major-Element Composition of Mercury's Surface from MESSENGER X-ray
Spectrometry
SO SCIENCE
LA English
DT Article
ID IRON-SILICATE FRACTIONATION; CHEMICAL-COMPOSITION; MARINER-10;
EVOLUTION; METEORITE; REGOLITH; ORIGIN; MANTLE; CRUST
AB X-ray fluorescence spectra obtained by the MESSENGER spacecraft orbiting Mercury indicate that the planet's surface differs in composition from those of other terrestrial planets. Relatively high Mg/Si and low Al/Si and Ca/Si ratios rule out a lunarlike feldspar-rich crust. The sulfur abundance is at least 10 times higher than that of the silicate portion of Earth or the Moon, and this observation, together with a low surface Fe abundance, supports the view that Mercury formed from highly reduced precursor materials, perhaps akin to enstatite chondrite meteorites or anhydrous cometary dust particles. Low Fe and Ti abundances do not support the proposal that opaque oxides of these elements contribute substantially to Mercury's low and variable surface reflectance.
C1 [Nittler, Larry R.; Weider, Shoshana Z.; Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[McCoy, Timothy J.] Smithsonian Inst, Washington, DC 20013 USA.
[Boynton, William V.; Hamara, David K.; Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Ebel, Denton S.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA.
[Ernst, Carolyn M.; Goldsten, John O.; Lawrence, David J.; McNutt, Ralph L., Jr.; Schlemm, Charles E., II] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA.
RP Nittler, LR (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
EM lnittler@ciw.edu
RI Ernst, Carolyn/I-4902-2012; McNutt, Ralph/E-8006-2010; Lawrence,
David/E-7463-2015;
OI McNutt, Ralph/0000-0002-4722-9166; Lawrence, David/0000-0002-7696-6667;
Weider, Shoshana/0000-0003-1034-909X
FU NASA [NAS5-97271, NASW-00002]
FX We thank the MESSENGER team for the development, cruise, orbit
insertion, and Mercury orbital operations of the MESSENGER spacecraft.
The NASA Discovery Program under contract NAS5-97271 to The Johns
Hopkins University Applied Physics Laboratory and NASW-00002 to the
Carnegie Institution of Washington supports the MESSENGER mission to
Mercury. Several of the authors are supported by NASA's MESSENGER
Participating Scientist Program.
NR 35
TC 158
Z9 158
U1 4
U2 47
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 SEP 30
PY 2011
VL 333
IS 6051
BP 1847
EP 1850
DI 10.1126/science.1211567
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 826PJ
UT WOS:000295365800043
PM 21960623
ER
PT J
AU Peplowski, PN
Evans, LG
Hauck, SA
McCoy, TJ
Boynton, WV
Gillis-Davis, JJ
Ebel, DS
Goldsten, JO
Hamara, DK
Lawrence, DJ
McNutt, RL
Nittler, LR
Solomon, SC
Rhodes, EA
Sprague, AL
Starr, RD
Stockstill-Cahill, KR
AF Peplowski, Patrick N.
Evans, Larry G.
Hauck, Steven A., II
McCoy, Timothy J.
Boynton, William V.
Gillis-Davis, Jeffery J.
Ebel, Denton S.
Goldsten, John O.
Hamara, David K.
Lawrence, David J.
McNutt, Ralph L., Jr.
Nittler, Larry R.
Solomon, Sean C.
Rhodes, Edgar A.
Sprague, Ann L.
Starr, Richard D.
Stockstill-Cahill, Karen R.
TI Radioactive Elements on Mercury's Surface from MESSENGER: Implications
for the Planet's Formation and Evolution
SO SCIENCE
LA English
DT Article
ID MARINER-10
AB The MESSENGER Gamma-Ray Spectrometer measured the average surface abundances of the radioactive elements potassium (K, 1150 +/- 220 parts per million), thorium (Th, 220 +/- 60 parts per billion), and uranium (U, 90 +/- 20 parts per billion) in Mercury's northern hemisphere. The abundance of the moderately volatile element K, relative to Th and U, is inconsistent with physical models for the formation of Mercury requiring extreme heating of the planet or its precursor materials, and supports formation from volatile-containing material comparable to chondritic meteorites. Abundances of K, Th, and U indicate that internal heat production has declined substantially since Mercury's formation, consistent with widespread volcanism shortly after the end of late heavy bombardment 3.8 billion years ago and limited, isolated volcanic activity since.
C1 [Peplowski, Patrick N.; Goldsten, John O.; Lawrence, David J.; McNutt, Ralph L., Jr.; Rhodes, Edgar A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA.
[Hauck, Steven A., II] Case Western Reserve Univ, Dept Geol Sci, Cleveland, OH 44106 USA.
[McCoy, Timothy J.; Stockstill-Cahill, Karen R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Boynton, William V.; Hamara, David K.; Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Gillis-Davis, Jeffery J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Ebel, Denton S.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA.
[Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Peplowski, PN (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM patrick.peplowski@jhuapl.edu
RI Lawrence, David/E-7463-2015; Hauck, Steven/A-7865-2008; Peplowski,
Patrick/I-7254-2012; McNutt, Ralph/E-8006-2010
OI Lawrence, David/0000-0002-7696-6667; Hauck, Steven/0000-0001-8245-146X;
Peplowski, Patrick/0000-0001-7154-8143; McNutt,
Ralph/0000-0002-4722-9166
FU NASA [NAS5-97271, NASW-00002]
FX We thank the entire MESSENGER team for their invaluable contributions to
the development and operation of the spacecraft. The MESSENGER project
is supported by the NASA Discovery Program under contract NAS5-97271 to
The Johns Hopkins University Applied Physics Laboratory and NASW-00002
to the Carnegie Institution of Washington. Several authors are supported
by NASA's MESSENGER Participating Scientist Program. All original data
reported in this paper are archived by the NASA Planetary Data System.
NR 26
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U1 3
U2 34
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 SEP 30
PY 2011
VL 333
IS 6051
BP 1850
EP 1852
DI 10.1126/science.1211576
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 826PJ
UT WOS:000295365800044
PM 21960624
ER
PT J
AU Head, JW
Chapman, CR
Strom, RG
Fassett, CI
Denevi, BW
Blewett, DT
Ernst, CM
Watters, TR
Solomon, SC
Murchie, SL
Prockter, LM
Chabot, NL
Gillis-Davis, JJ
Whitten, JL
Goudge, TA
Baker, DMH
Hurwitz, DM
Ostrach, LR
Xiao, ZY
Merline, WJ
Kerber, L
Dickson, JL
Oberst, J
Byrne, PK
Klimczak, C
Nittler, LR
AF Head, James W.
Chapman, Clark R.
Strom, Robert G.
Fassett, Caleb I.
Denevi, Brett W.
Blewett, David T.
Ernst, Carolyn M.
Watters, Thomas R.
Solomon, Sean C.
Murchie, Scott L.
Prockter, Louise M.
Chabot, Nancy L.
Gillis-Davis, Jeffrey J.
Whitten, Jennifer L.
Goudge, Timothy A.
Baker, David M. H.
Hurwitz, Debra M.
Ostrach, Lillian R.
Xiao, Zhiyong
Merline, William J.
Kerber, Laura
Dickson, James L.
Oberst, Juergen
Byrne, Paul K.
Klimczak, Christian
Nittler, Larry R.
TI Flood Volcanism in the Northern High Latitudes of Mercury Revealed by
MESSENGER
SO SCIENCE
LA English
DT Article
ID SMOOTH PLAINS; CALORIS BASIN; EMPLACEMENT; SURFACE; STRATIGRAPHY;
EVOLUTION; FLYBY
AB MESSENGER observations from Mercury orbit reveal that a large contiguous expanse of smooth plains covers much of Mercury's high northern latitudes and occupies more than 6% of the planet's surface area. These plains are smooth, embay other landforms, are distinct in color, show several flow features, and partially or completely bury impact craters, the sizes of which indicate plains thicknesses of more than 1 kilometer and multiple phases of emplacement. These characteristics, as well as associated features, interpreted to have formed by thermal erosion, indicate emplacement in a flood-basalt style, consistent with x-ray spectrometric data indicating surface compositions intermediate between those of basalts and komatiites. The plains formed after the Caloris impact basin, confirming that volcanism was a globally extensive process in Mercury's post-heavy bombardment era.
C1 [Head, James W.; Fassett, Caleb I.; Whitten, Jennifer L.; Goudge, Timothy A.; Baker, David M. H.; Hurwitz, Debra M.; Kerber, Laura; Dickson, James L.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Chapman, Clark R.; Merline, William J.] SW Res Inst, Boulder, CO 80302 USA.
[Strom, Robert G.; Xiao, Zhiyong] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Denevi, Brett W.; Blewett, David T.; Ernst, Carolyn M.; Murchie, Scott L.; Prockter, Louise M.; Chabot, Nancy L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Solomon, Sean C.; Byrne, Paul K.; Klimczak, Christian; Nittler, Larry R.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[Gillis-Davis, Jeffrey J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Ostrach, Lillian R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA.
[Xiao, Zhiyong] China Univ Geosci, Fac Earth Sci, Wuhan 430074, Hubei, Peoples R China.
[Oberst, Juergen] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany.
RP Head, JW (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
EM james_head@brown.edu
RI Ernst, Carolyn/I-4902-2012; Blewett, David/I-4904-2012; Denevi,
Brett/I-6502-2012; Murchie, Scott/E-8030-2015; Chabot,
Nancy/F-5384-2015;
OI Blewett, David/0000-0002-9241-6358; Denevi, Brett/0000-0001-7837-6663;
Murchie, Scott/0000-0002-1616-8751; Chabot, Nancy/0000-0001-8628-3176;
Fassett, Caleb/0000-0001-9155-3804
FU NASA [NAS5-97271, NASW-00002]
FX We thank the MESSENGER team for development and flight operations. The
NASA Discovery Program supports the MESSENGER mission through contract
NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory
and NASW-00002 to the Carnegie Institution of Washington.
NR 31
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U1 12
U2 50
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD SEP 30
PY 2011
VL 333
IS 6051
BP 1853
EP 1856
DI 10.1126/science.1211997
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 826PJ
UT WOS:000295365800045
PM 21960625
ER
PT J
AU Blewett, DT
Chabot, NL
Denevi, BW
Ernst, CM
Head, JW
Izenberg, NR
Murchie, SL
Solomon, SC
Nittler, LR
McCoy, TJ
Xiao, ZY
Baker, DMH
Fassett, CI
Braden, SE
Oberst, J
Scholten, F
Preusker, F
Hurwitz, DM
AF Blewett, David T.
Chabot, Nancy L.
Denevi, Brett W.
Ernst, Carolyn M.
Head, James W.
Izenberg, Noam R.
Murchie, Scott L.
Solomon, Sean C.
Nittler, Larry R.
McCoy, Timothy J.
Xiao, Zhiyong
Baker, David M. H.
Fassett, Caleb I.
Braden, Sarah E.
Oberst, Juergen
Scholten, Frank
Preusker, Frank
Hurwitz, Debra M.
TI Hollows on Mercury: MESSENGER Evidence for Geologically Recent
Volatile-Related Activity
SO SCIENCE
LA English
DT Article
ID VOLCANISM; FLYBY; EROS; CRATERS
AB High-resolution images of Mercury's surface from orbit reveal that many bright deposits within impact craters exhibit fresh-appearing, irregular, shallow, rimless depressions. The depressions, or hollows, range from tens of meters to a few kilometers across, and many have high-reflectance interiors and halos. The host rocks, which are associated with crater central peaks, peak rings, floors, and walls, are interpreted to have been excavated from depth by the crater-forming process. The most likely formation mechanisms for the hollows involve recent loss of volatiles through some combination of sublimation, space weathering, outgassing, or pyroclastic volcanism. These features support the inference that Mercury's interior contains higher abundances of volatile materials than predicted by most scenarios for the formation of the solar system's innermost planet.
C1 [Blewett, David T.; Chabot, Nancy L.; Denevi, Brett W.; Ernst, Carolyn M.; Izenberg, Noam R.; Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Head, James W.; Baker, David M. H.; Fassett, Caleb I.; Hurwitz, Debra M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Solomon, Sean C.; Nittler, Larry R.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA.
[McCoy, Timothy J.] Smithsonian Inst, Washington, DC 20013 USA.
[Xiao, Zhiyong] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Xiao, Zhiyong] China Univ Geosci, Fac Earth Sci, Wuhan 430074, Hubei, Peoples R China.
[Braden, Sarah E.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA.
[Oberst, Juergen; Scholten, Frank; Preusker, Frank] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany.
RP Blewett, DT (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
EM david.blewett@jhuapl.edu
RI Ernst, Carolyn/I-4902-2012; Blewett, David/I-4904-2012; Denevi,
Brett/I-6502-2012; Murchie, Scott/E-8030-2015; Izenberg,
Noam/F-3952-2015; Chabot, Nancy/F-5384-2015;
OI Blewett, David/0000-0002-9241-6358; Denevi, Brett/0000-0001-7837-6663;
Murchie, Scott/0000-0002-1616-8751; Izenberg, Noam/0000-0003-1629-6478;
Chabot, Nancy/0000-0001-8628-3176; Fassett, Caleb/0000-0001-9155-3804
FU NASA; Participating Scientist grant
FX This work was supported by NASA through the MESSENGER project and by a
Participating Scientist grant to D. T. B. M. Robinson offered helpful
comments on the manuscript. We thank N. Fontanella, S. Peel, E. Zhong,
P. Pashai, and E. Coman for assistance with data processing and
compilation. MESSENGER data are archived with the NASA Planetary Data
System.
NR 31
TC 40
Z9 40
U1 11
U2 42
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD SEP 30
PY 2011
VL 333
IS 6051
BP 1856
EP 1859
DI 10.1126/science.1211681
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 826PJ
UT WOS:000295365800046
PM 21960626
ER
PT J
AU Punyasena, SW
Dalling, JW
Jaramillo, C
Turner, BL
AF Punyasena, Surangi W.
Dalling, James W.
Jaramillo, Carlos
Turner, Benjamin L.
TI Comment on "The Response of Vegetation on the Andean Flank in Western
Amazonia to Pleistocene Climate Change"
SO SCIENCE
LA English
DT Editorial Material
ID MAXIMUM
C1 [Punyasena, Surangi W.; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.
[Dalling, James W.; Jaramillo, Carlos; Turner, Benjamin L.] Smithsonian Trop Res Inst, Ancon, Panama.
RP Punyasena, SW (reprint author), Univ Illinois, Dept Plant Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA.
EM punyasena@life.illinois.edu
RI Turner, Benjamin/E-5940-2011; Punyasena, Surangi/C-9134-2011
OI Turner, Benjamin/0000-0002-6585-0722;
NR 14
TC 13
Z9 14
U1 0
U2 7
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD SEP 30
PY 2011
VL 333
IS 6051
DI 10.1126/science.1207525
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 826PJ
UT WOS:000295365800030
PM 21960612
ER
PT J
AU Alfoldi, J
Di Palma, F
Grabherr, M
Williams, C
Kong, LS
Mauceli, E
Russell, P
Lowe, CB
Glor, RE
Jaffe, JD
Ray, DA
Boissinot, S
Shedlock, AM
Botka, C
Castoe, TA
Colbourne, JK
Fujita, MK
Moreno, RG
ten Hallers, BF
Haussler, D
Heger, A
Heiman, D
Janes, DE
Johnson, J
de Jong, PJ
Koriabine, MY
Lara, M
Novick, PA
Organ, CL
Peach, SE
Poe, S
Pollock, DD
de Queiroz, K
Sanger, T
Searle, S
Smith, JD
Smith, Z
Swofford, R
Turner-Maier, J
Wade, J
Young, S
Zadissa, A
Edwards, SV
Glenn, TC
Schneider, CJ
Losos, JB
Lander, ES
Breen, M
Ponting, CP
Lindblad-Toh, K
AF Alfoeldi, Jessica
Di Palma, Federica
Grabherr, Manfred
Williams, Christina
Kong, Lesheng
Mauceli, Evan
Russell, Pamela
Lowe, Craig B.
Glor, Richard E.
Jaffe, Jacob D.
Ray, David A.
Boissinot, Stephane
Shedlock, Andrew M.
Botka, Christopher
Castoe, Todd A.
Colbourne, John K.
Fujita, Matthew K.
Moreno, Ricardo Godinez
ten Hallers, Boudewijn F.
Haussler, David
Heger, Andreas
Heiman, David
Janes, Daniel E.
Johnson, Jeremy
de Jong, Pieter J.
Koriabine, Maxim Y.
Lara, Marcia
Novick, Peter A.
Organ, Chris L.
Peach, Sally E.
Poe, Steven
Pollock, David D.
de Queiroz, Kevin
Sanger, Thomas
Searle, Steve
Smith, Jeremy D.
Smith, Zachary
Swofford, Ross
Turner-Maier, Jason
Wade, Juli
Young, Sarah
Zadissa, Amonida
Edwards, Scott V.
Glenn, Travis C.
Schneider, Christopher J.
Losos, Jonathan B.
Lander, Eric S.
Breen, Matthew
Ponting, Chris P.
Lindblad-Toh, Kerstin
TI The genome of the green anole lizard and a comparative analysis with
birds and mammals
SO NATURE
LA English
DT Article
ID EVOLUTION; CHICKEN; MICROCHROMOSOMES; SAUROPSIDA; REPTILES; PROTEOME;
FISH
AB The evolution of the amniotic egg was one of the great evolutionary innovations in the history of life, freeing vertebrates from an obligatory connection to water and thus permitting the conquest of terrestrial environments(1). Among amniotes, genome sequences are available for mammals and birds(2-4), but not for non-avian reptiles. Here we report the genome sequence of the North American green anole lizard, Anolis carolinensis. We find that A. carolinensis microchromosomes are highly syntenic with chicken microchromosomes, yet do not exhibit the high GC and low repeat content that are characteristic of avian microchromosomes(2). Also, A. carolinensis mobile elements are very young and diverse-more so than in any other sequenced amniote genome. The GC content of this lizard genome is also unusual in its homogeneity, unlike the regionally variable GC content found in mammals and birds(5). We describe and assign sequence to the previously unknown A. carolinensis X chromosome. Comparative gene analysis shows that amniote egg proteins have evolved significantly more rapidly than other proteins. An anole phylogeny resolves basal branches to illuminate the history of their repeated adaptive radiations.
C1 [Alfoeldi, Jessica; Di Palma, Federica; Grabherr, Manfred; Mauceli, Evan; Russell, Pamela; Jaffe, Jacob D.; Heiman, David; Johnson, Jeremy; Lara, Marcia; Peach, Sally E.; Swofford, Ross; Turner-Maier, Jason; Young, Sarah; Lander, Eric S.; Lindblad-Toh, Kerstin] Broad Inst MIT & Harvard, Cambridge, MA 02142 USA.
[Williams, Christina; Breen, Matthew] N Carolina State Univ, Dept Mol Biomed Sci, Coll Vet Med, Raleigh, NC 27606 USA.
[Kong, Lesheng; Fujita, Matthew K.; Heger, Andreas; Ponting, Chris P.] Univ Oxford, MRC, Funct Genom Unit, Dept Physiol Anat & Genet, Oxford OX1 3QX, England.
[Lowe, Craig B.] Stanford Univ, Sch Med, Dept Dev Biol, Stanford, CA 94305 USA.
[Glor, Richard E.] Univ Rochester, Rochester, NY 14607 USA.
[Ray, David A.; Smith, Jeremy D.] Mississippi State Univ, Dept Biochem Mol Biol Entomol & Plant Pathol, Mississippi State, MS 39762 USA.
[Boissinot, Stephane] CUNY, Dept Biol, Queens Coll, New York, NY 11367 USA.
[Shedlock, Andrew M.] Coll Charleston, Dept Biol, Charleston, SC 29424 USA.
[Shedlock, Andrew M.] Coll Charleston, Grad Program Marine Genom, Charleston, SC 29424 USA.
[Botka, Christopher] Harvard Univ, Sch Med, Boston, MA 02115 USA.
[Castoe, Todd A.; Pollock, David D.] Univ Colorado, Sch Med, Dept Biochem & Mol Genet, Aurora, CO 80045 USA.
[Colbourne, John K.; Smith, Zachary] Indiana Univ, Ctr Genom & Bioinformat, Bloomington, IN 47405 USA.
[Fujita, Matthew K.; Moreno, Ricardo Godinez; Janes, Daniel E.; Organ, Chris L.; Sanger, Thomas; Edwards, Scott V.; Losos, Jonathan B.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Fujita, Matthew K.; Moreno, Ricardo Godinez; Janes, Daniel E.; Organ, Chris L.; Sanger, Thomas; Edwards, Scott V.; Losos, Jonathan B.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA.
[ten Hallers, Boudewijn F.; de Jong, Pieter J.; Koriabine, Maxim Y.] Childrens Hosp, Oakland Res Inst, Oakland, CA 94609 USA.
[Haussler, David] Univ Calif Santa Cruz, Ctr Biomol Sci & Engn, Santa Cruz, CA 95064 USA.
[Novick, Peter A.] Queensborough Community Coll, Dept Biol Sci & Geol, Bayside, NY 11364 USA.
[Poe, Steven] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
[Pollock, David D.] Univ Colorado, Program Computat Biosci, Sch Med, Aurora, CO 80045 USA.
[de Queiroz, Kevin] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Wade, Juli] Michigan State Univ, Dept Psychol, Program Neurosci, E Lansing, MI 48824 USA.
[Wade, Juli] Michigan State Univ, Dept Zool, Program Neurosci, E Lansing, MI 48824 USA.
[Glenn, Travis C.] Univ Georgia, Dept Environm Hlth Sci, Athens, GA 30602 USA.
[Glenn, Travis C.] Univ Georgia, Georgia Genom Facil, Athens, GA 30602 USA.
[Schneider, Christopher J.] Boston Univ, Dept Biol, Boston, MA 02215 USA.
[Breen, Matthew] N Carolina State Univ, Ctr Comparat Med & Translat Res, Raleigh, NC 27695 USA.
[Breen, Matthew] Univ N Carolina, Lineberger Comprehens Canc Ctr, Chapel Hill, NC 27514 USA.
[Lindblad-Toh, Kerstin] Uppsala Univ, Dept Med Biochem & Microbiol, Sci Life Lab Uppsala, S-75123 Uppsala, Sweden.
RP Alfoldi, J (reprint author), Broad Inst MIT & Harvard, Cambridge, MA 02142 USA.
EM jalfoldi@broadinstitute.org; kersli@broadinstitute.org
RI wade, juli/F-4993-2012; Glor, Richard/N-4656-2013; Colbourne,
John/L-7748-2014; Kong, Lesheng/O-8933-2015; Pollock, David/M-4740-2016;
OI Heger, Andreas/0000-0001-7720-0447; Glor, Richard/0000-0002-3359-1631;
Colbourne, John/0000-0002-6966-2972; Kong, Lesheng/0000-0002-9225-3421;
Pollock, David/0000-0002-7627-4214; Edwards, Scott/0000-0003-2535-6217;
Ponting, Chris/0000-0003-0202-7816
FU National Human Genome Research Institute (NHGRI); NSF [DEB-0844624,
DEB-0920892]; David and Lucile Packard Foundation
FX Generation of the A. carolinensis sequence at the Broad Institute of MIT
and Harvard was supported by grants from the National Human Genome
Research Institute (NHGRI); S. P. and R. E. G. were supported by NSF
grants DEB-0844624 and DEB-0920892. All sequence data was produced by
the Genome Sequencing Platform of the Broad Institute. We would also
like to thank the David and Lucile Packard Foundation for their early
support of anole genomics, R. Andrews for her advice on lizard egg
biology, C. Hickman and B. Temple and the Herpetology group at the
University of Georgia's Savannah River Ecology Lab for assistance with
sample collection, and L. Gaffney and L. Virnoche for assistance with
figure and text preparation.
NR 26
TC 231
Z9 236
U1 14
U2 108
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD SEP 29
PY 2011
VL 477
IS 7366
BP 587
EP 591
DI 10.1038/nature10390
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 825ZM
UT WOS:000295320900039
PM 21881562
ER
PT J
AU Rapple, J
AF Rapple, John
TI DID BIG PHARMA CREATE THE FLU PANIC?
SO NEW YORK REVIEW OF BOOKS
LA English
DT Editorial Material
C1 Smithsonian Conservat Biol Inst, Front Royal, VA USA.
RP Rapple, J (reprint author), Smithsonian Conservat Biol Inst, Front Royal, VA USA.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU NEW YORK REVIEW
PI NEW YORK
PA 1755 BROADWAY, 5TH FLOOR, NEW YORK, NY 10019 USA
SN 0028-7504
J9 NEW YORK REV BOOKS
JI N. Y. Rev. Books
PD SEP 29
PY 2011
VL 58
IS 14
BP 100
EP 100
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 820AT
UT WOS:000294878600043
ER
PT J
AU Pohl, T
Adams, CS
Sadephpour, HR
AF Pohl, T.
Adams, C. S.
Sadephpour, H. R.
TI Cold Rydberg gases and ultra-cold plasmas
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Editorial Material
ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; NEUTRAL PLASMA;
ENERGY-TRANSFER; ATOMS; MOLECULES; BLOCKADE; STATES; STATISTICS;
COLLOQUIUM; EXPANSION
AB We briefly highlight recent developments in the complementary fields of cold Rydberg gases and ultra-cold plasmas and provide a short overview of the articles in this special issue.
C1 [Pohl, T.] Max Planck Inst Complex Syst, D-01099 Dresden, Germany.
[Adams, C. S.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Sadephpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Pohl, T (reprint author), Max Planck Inst Complex Syst, Nothnitzer Str 38, D-01099 Dresden, Germany.
EM tpohl@pks.mpg.de
RI Pohl, Thomas/B-5133-2013; Adams, Charles/C-8808-2015
OI Adams, Charles/0000-0001-5602-2741
NR 195
TC 17
Z9 17
U1 2
U2 21
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD SEP 28
PY 2011
VL 44
IS 18
SI SI
AR 180201
DI 10.1088/0953-4075/44/18/180201
PG 7
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 822HV
UT WOS:000295035700001
ER
PT J
AU Rittenhouse, ST
Mayle, M
Schmelcher, P
Sadeghpour, HR
AF Rittenhouse, Seth T.
Mayle, M.
Schmelcher, P.
Sadeghpour, H. R.
TI Ultralong-range polyatomic Rydberg molecules formed by a polar perturber
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
ID ATOMS; BLOCKADE; DIMERS; STATES
AB The internal electric field of a Rydberg atom electron can bind a polar molecule to form a giant ultralong-range stable polyatomic molecule. Such molecules not only share their properties with Rydberg atoms (such as long lifetimes and large sizes) but they also possess huge permanent electric dipole moments and in addition allow for coherent control of the polar molecule orientation. In this work, we include additional Rydberg manifolds which couple to the nearly degenerate set of Rydberg states employed in the previous work (S T Rittenhouse and H R Sadeghpour 2010 Phys. Rev. Lett. 104 243002). The coupling of a set of (n + 3) s Rydberg states with the n(l > 2) nearly degenerate Rydberg manifolds in alkali metal atoms leads to pronounced avoided crossings in the Born-Oppenheimer potentials. Ultimately, these avoided crossings enable the formation of the giant polyatomic Rydberg molecules with standard two-photon laser photoassociation techniques.
C1 [Rittenhouse, Seth T.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Mayle, M.; Schmelcher, P.] Univ Hamburg, Zentrum Opt Quantentechnologien, D-22761 Hamburg, Germany.
RP Rittenhouse, ST (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA.
EM srittenhouse@cfa.harvard.edu
RI Mayle, Michael/A-2423-2009; Schmelcher, Peter/D-9592-2014
OI Schmelcher, Peter/0000-0002-2637-0937
FU German Academic Exchange Service (DAAD); NSF through ITAMP at Harvard
University; Smithsonian Astrophysical Observatory
FX The authors thank T V Tscherbul for help in calculating the
Lambda-doublet molecule parameters used in this work. MM acknowledges
financial support from the German Academic Exchange Service (DAAD). STR
and HRS acknowledge financial support from the NSF through ITAMP at
Harvard University and the Smithsonian Astrophysical Observatory.
NR 23
TC 12
Z9 12
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD SEP 28
PY 2011
VL 44
IS 18
SI SI
AR 184005
DI 10.1088/0953-4075/44/18/184005
PG 6
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 822HV
UT WOS:000295035700006
ER
PT J
AU Oliveira, C
Avelino, GS
Abe, KT
Mariguela, TC
Benine, RC
Orti, G
Vari, RP
Castro, RMCE
AF Oliveira, Claudio
Avelino, Gleisy S.
Abe, Kelly T.
Mariguela, Tatiane C.
Benine, Ricardo C.
Orti, Guillermo
Vari, Richard P.
Correa e Castro, Ricardo M.
TI Phylogenetic relationships within the speciose family Characidae
(Teleostei: Ostariophysi: Characiformes) based on multilocus analysis
and extensive ingroup sampling
SO BMC EVOLUTIONARY BIOLOGY
LA English
DT Article
ID DNA-SEQUENCES; MIXED MODELS; FISHES; SELECTION; ACTINOPTERYGII;
SUBSTITUTION; INFORMATION; SYSTEMATICS; BOOTSTRAP; INFERENCE
AB Background: With nearly 1,100 species, the fish family Characidae represents more than half of the species of Characiformes, and is a key component of Neotropical freshwater ecosystems. The composition, phylogeny, and classification of Characidae is currently uncertain, despite significant efforts based on analysis of morphological and molecular data. No consensus about the monophyly of this group or its position within the order Characiformes has been reached, challenged by the fact that many key studies to date have non-overlapping taxonomic representation and focus only on subsets of this diversity.
Results: In the present study we propose a new definition of the family Characidae and a hypothesis of relationships for the Characiformes based on phylogenetic analysis of DNA sequences of two mitochondrial and three nuclear genes (4,680 base pairs). The sequences were obtained from 211 samples representing 166 genera distributed among all 18 recognized families in the order Characiformes, all 14 recognized subfamilies in the Characidae, plus 56 of the genera so far considered incertae sedis in the Characidae. The phylogeny obtained is robust, with most lineages significantly supported by posterior probabilities in Bayesian analysis, and high bootstrap values from maximum likelihood and parsimony analyses.
Conclusion: A monophyletic assemblage strongly supported in all our phylogenetic analysis is herein defined as the Characidae and includes the characiform species lacking a supraorbital bone and with a derived position of the emergence of the hyoid artery from the anterior ceratohyal. To recognize this and several other monophyletic groups within characiforms we propose changes in the limits of several families to facilitate future studies in the Characiformes and particularly the Characidae. This work presents a new phylogenetic framework for a speciose and morphologically diverse group of freshwater fishes of significant ecological and evolutionary importance across the Neotropics and portions of Africa.
C1 [Oliveira, Claudio; Avelino, Gleisy S.; Abe, Kelly T.; Mariguela, Tatiane C.; Benine, Ricardo C.] Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Sao Paulo, Brazil.
[Orti, Guillermo] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA.
[Vari, Richard P.] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC USA.
[Correa e Castro, Ricardo M.] Univ Sao Paulo, FFCLRP, Dept Biol, LIRP, Sao Paulo, Brazil.
RP Oliveira, C (reprint author), Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Sao Paulo, Brazil.
EM claudio@ibb.unesp.br
RI Oliveira, Claudio/D-7713-2012; Mariguela, Tatiane/K-2659-2012; Benine,
Ricardo/B-2354-2013
OI Mariguela, Tatiane/0000-0002-9680-5887;
FU FAPESP (Fundacao de Apoio a Pesquisa do Estado de Sao Paulo)
[04/09219-6, 06/05744-4, 06/06749-0, 06/04551-8, 06/00545-3]; CNPq
(Conselho Nacional de Desenvolvimento Cientifico e Tecnologico do
Brasil) [309632/2007-2, 303854/2009-0]; U.S. National Science Foundation
[DEB-0443470]
FX We thank all the individuals and institutions who assisted us in the
collection and identification of the specimens that served as the basis
for this study, with special thanks to Mauro Nirchio, Universidad de
Oriente, for the donation of tissue samples from Venezuela, Oris Sanjur,
Smithsonian Tropical Research Institute, for the donation of tissue
samples from Panama, Martha Valdez-Moreno, El Colegio de la Frontera
Sur, for the donation of tissue samples from Mexico, Hernan Ortega,
Museo de Historia Natural, Universidad Nacional Mayor de San Marcos, for
the donation of tissue samples from Peru, the American Museum of Natural
History for the donation of tissue samples of some Cheirodontinae, and
Osvaldo T. Oyakawa, Janice Cunha, Caroline Doria, Riviane Garcez, and
Gislene Torrente-Vilara for the donation of tissue samples from several
regions within Brazil. We also thank Markus Alexandrou for his help with
the Bayesian analyses. The manuscript was substantially improved with
the help of the Associated Editor of BMC and three anonymous reviewers.
This study is part of the FAPESP (Fundacao de Apoio a Pesquisa do Estado
de Sao Paulo) Thematic Project "Phylogenetic relationships in the
Characidae (Ostariophysi: Characiformes) (FAPESP grant number
04/09219-6, R. M. C. Castro, Principal Investigator). The first and
eighth authors are CNPq (Conselho Nacional de Desenvolvimento Cientifico
e Tecnologico do Brasil) researchers (CNPq grants numbers 309632/2007-2,
303854/2009-0, respectively). The second, third, fourth and fifth
authors were supported by FAPESP (06/05744-4, 06/06749-0, 06/04551-8,
06/00545-3, respectively). A Research Coordination Network (RCN) grant
from the U.S. National Science Foundation (DEB-0443470, PI = G. Orti)
provided funding for a student exchange program supporting the fourth
author.
NR 79
TC 92
Z9 97
U1 0
U2 30
PU BIOMED CENTRAL LTD
PI LONDON
PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND
SN 1471-2148
J9 BMC EVOL BIOL
JI BMC Evol. Biol.
PD SEP 26
PY 2011
VL 11
AR 275
DI 10.1186/1471-2148-11-275
PG 25
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA 831KD
UT WOS:000295728400001
PM 21943181
ER
PT J
AU Kraft, NJB
Comita, LS
Chase, JM
Sanders, NJ
Swenson, NG
Crist, TO
Stegen, JC
Vellend, M
Boyle, B
Anderson, MJ
Cornell, HV
Davies, KF
Freestone, AL
Inouye, BD
Harrison, SP
Myers, JA
AF Kraft, Nathan J. B.
Comita, Liza S.
Chase, Jonathan M.
Sanders, Nathan J.
Swenson, Nathan G.
Crist, Thomas O.
Stegen, James C.
Vellend, Mark
Boyle, Brad
Anderson, Marti J.
Cornell, Howard V.
Davies, Kendi F.
Freestone, Amy L.
Inouye, Brian D.
Harrison, Susan P.
Myers, Jonathan A.
TI Disentangling the Drivers of beta Diversity Along Latitudinal and
Elevational Gradients
SO SCIENCE
LA English
DT Article
ID GAMMA-DIVERSITY; COMMUNITY DIVERSITY; SPECIES-DIVERSITY; AMAZONIAN
FOREST; ALPHA-DIVERSITY; TREE COMMUNITY; SCALE; ENVIRONMENTS;
BIODIVERSITY; RICHNESS
AB Understanding spatial variation in biodiversity along environmental gradients is a central theme in ecology. Differences in species compositional turnover among sites (beta diversity) occurring along gradients are often used to infer variation in the processes structuring communities. Here, we show that sampling alone predicts changes in beta diversity caused simply by changes in the sizes of species pools. For example, forest inventories sampled along latitudinal and elevational gradients show the well-documented pattern that beta diversity is higher in the tropics and at low elevations. However, after correcting for variation in pooled species richness (gamma diversity), these differences in beta diversity disappear. Therefore, there is no need to invoke differences in the mechanisms of community assembly in temperate versus tropical systems to explain these global-scale patterns of beta diversity.
C1 [Kraft, Nathan J. B.; Vellend, Mark] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada.
[Kraft, Nathan J. B.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Comita, Liza S.] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA.
[Comita, Liza S.] Smithsonian Trop Res Inst, Balboa Ancon, Panama.
[Chase, Jonathan M.; Myers, Jonathan A.] Washington Univ, Dept Biol, St Louis, MO 63130 USA.
[Sanders, Nathan J.] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA.
[Sanders, Nathan J.] Univ Copenhagen, Dept Biol, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark.
[Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA.
[Crist, Thomas O.] Miami Univ, Inst Environm & Sustainabil, Oxford, OH 45056 USA.
[Crist, Thomas O.] Miami Univ, Dept Zool, Oxford, OH 45056 USA.
[Stegen, James C.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA.
[Stegen, James C.] Pacific NW Natl Lab, Fundamental & Computat Sci Directorate, Div Biol Sci, Richland, WA 99352 USA.
[Vellend, Mark] Univ Sherbrooke, Dept Biol, Sherbrooke, PQ J1K 2R1, Canada.
[Boyle, Brad] Univ Arizona, Dept Ecol & Evolut, Tucson, AZ 85719 USA.
[Anderson, Marti J.] Massey Univ, New Zealand Inst Adv Study, Auckland 0745, New Zealand.
[Cornell, Howard V.; Harrison, Susan P.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA.
[Davies, Kendi F.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
[Freestone, Amy L.] Temple Univ, Dept Biol, Philadelphia, PA 19122 USA.
[Inouye, Brian D.] Florida State Univ, Tallahassee, FL 32306 USA.
RP Kraft, NJB (reprint author), Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada.
EM nkraft@biodiversity.ubc.ca
RI Swenson, Nathan/A-3514-2012; Kraft, Nathan/A-2817-2012; Sanders,
Nathan/A-6945-2009; Stegen, James/Q-3078-2016; publist,
CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017
OI Swenson, Nathan/0000-0003-3819-9767; Kraft, Nathan/0000-0001-8867-7806;
Sanders, Nathan/0000-0001-6220-6731; Stegen, James/0000-0001-9135-7424;
FU National Center for Ecological Analysis and Synthesis (NCEAS); NSF
[EF-0553768, DBI-0906005]; University of California, Santa Barbara;
state of California; National Science and Engineering Research Council
of Canada; U.S. Department of Energy [DE-FG02-08ER64510]
FX We are grateful to A. H. Gentry, the Missouri Botanical Garden, and
numerous additional collectors who contributed to the latitudinal data
set. The data sets are available in the original publications or
electronically from SALVIAS (www.salvias.net). This work was conducted
as part of the Gradients of beta-diversity Working Group supported by
the National Center for Ecological Analysis and Synthesis (NCEAS), a
center funded by NSF (grant EF-0553768); the University of California,
Santa Barbara; and the state of California. N.J.B.K. was supported by
the National Science and Engineering Research Council of Canada CREATE
Training Program in Biodiversity Research. L. S. C. was supported by an
NCEAS postdoctoral fellowship. N.J.S. was supported by U.S. Department
of Energy Program for Ecosystem Research DE-FG02-08ER64510. J.C.S. was
supported by an NSF Postdoctoral Fellowship in Bioinformatics
(DBI-0906005).
NR 34
TC 180
Z9 191
U1 29
U2 337
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 SEP 23
PY 2011
VL 333
IS 6050
BP 1755
EP 1758
DI 10.1126/science.1208584
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 823KQ
UT WOS:000295121500045
PM 21940897
ER
PT J
AU Ruger, N
Berger, U
Hubbell, SP
Vieilledent, G
Condit, R
AF Rueger, Nadja
Berger, Uta
Hubbell, Stephen P.
Vieilledent, Ghislain
Condit, Richard
TI Growth Strategies of Tropical Tree Species: Disentangling Light and Size
Effects
SO PLOS ONE
LA English
DT Article
ID RAIN-FOREST COMMUNITY; MOIST FOREST; NEIGHBORHOOD ANALYSIS; RELATIVE
IMPORTANCE; SHADE TOLERANCE; SAPLING GROWTH; CANOPY GAPS; MORTALITY;
RESPONSES; RECRUITMENT
AB An understanding of the drivers of tree growth at the species level is required to predict likely changes of carbon stocks and biodiversity when environmental conditions change. Especially in species-rich tropical forests, it is largely unknown how species differ in their response of growth to resource availability and individual size. We use a hierarchical Bayesian approach to quantify the impact of light availability and tree diameter on growth of 274 woody species in a 50-ha long-term forest census plot in Barro Colorado Island, Panama. Light reaching each individual tree was estimated from yearly vertical censuses of canopy density. The hierarchical Bayesian approach allowed accounting for different sources of error, such as negative growth observations, and including rare species correctly weighted by their abundance. All species grew faster at higher light. Exponents of a power function relating growth to light were mostly between 0 and 1. This indicates that nearly all species exhibit a decelerating increase of growth with light. In contrast, estimated growth rates at standardized conditions (5 cm dbh, 5% light) varied over a 9-fold range and reflect strong growth-strategy differentiation between the species. As a consequence, growth rankings of the species at low (2%) and high light (20%) were highly correlated. Rare species tended to grow faster and showed a greater sensitivity to light than abundant species. Overall, tree size was less important for growth than light and about half the species were predicted to grow faster in diameter when bigger or smaller, respectively. Together light availability and tree diameter only explained on average 12% of the variation in growth rates. Thus, other factors such as soil characteristics, herbivory, or pathogens may contribute considerably to shaping tree growth in the tropics.
C1 [Rueger, Nadja] Univ Leipzig, Spezielle Botan & Funktionelle Biodiversitat, Leipzig, Germany.
[Berger, Uta] Tech Univ Dresden, Inst Waldwachstum & Forstliche Informat, Dresden, Tharandt, Germany.
[Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA.
[Hubbell, Stephen P.; Condit, Richard] Ctr Trop Forest Sci, Smithsonian Trop Res Inst, Washington, DE USA.
[Vieilledent, Ghislain] Forest Ecosystem Goods & Serv, UR105, Montpellier, France.
[Vieilledent, Ghislain] DRP Foret & Biodiversite, Antananarivo, Madagascar.
RP Ruger, N (reprint author), Univ Leipzig, Spezielle Botan & Funktionelle Biodiversitat, Leipzig, Germany.
EM nadja.rueger@uni-leipzig.de
RI Vieilledent, Ghislain/D-8323-2011; Ruger, Nadja/J-6393-2015
OI Vieilledent, Ghislain/0000-0002-1685-4997; Ruger,
Nadja/0000-0003-2371-4172
FU Deutsche Forschungsgemeinschaft (DFG) [RU 1536/2-1]; Center for Tropical
Forest Science (CTFS); United States National Science Foundation; John
D. and Catherine T. McArthur Foundation; Smithsonian Tropical Research
Institute
FX NR was partially funded by research grants from Deutsche
Forschungsgemeinschaft (DFG) (RU 1536/2-1) and the Center for Tropical
Forest Science (CTFS). The Barro Colorado Island plot has been made
possible through the support of the United States National Science
Foundation, the John D. and Catherine T. McArthur Foundation and the
Smithsonian Tropical Research Institute. The funders had no role in
study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 74
TC 28
Z9 30
U1 3
U2 55
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD SEP 22
PY 2011
VL 6
IS 9
AR e25330
DI 10.1371/journal.pone.0025330
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 825IJ
UT WOS:000295265100089
PM 21966498
ER
PT J
AU Fabbiano, G
Wang, JF
Elvis, M
Risaliti, G
AF Fabbiano, G.
Wang, Junfeng
Elvis, M.
Risaliti, G.
TI A close nuclear black-hole pair in the spiral galaxy NGC 3393
SO NATURE
LA English
DT Article
ID ACTIVE GALACTIC NUCLEI; X-RAY SOURCE; SYSTEM; REFLECTION; DISCOVERY;
BINARIES; NGC-3393; SUZAKU
AB The current picture of galaxy evolution(1) advocates co-evolution of galaxies and their nuclear massive black holes, through accretion and galactic merging. Pairs of quasars, each with a massive black hole at the centre of its galaxy, have separations of 6,000 to 300,000 light years (refs 2 and 3; 1 parsec = 3.26 light years) and exemplify the first stages of this gravitational interaction. The final stages of the black-hole merging process, through binary black holes and final collapse into a single black hole with gravitational wave emission, are consistent with the sub-light-year separation inferred from the optical spectra(4) and light-variability(5) of two such quasars. The double active nuclei of a few nearby galaxies with disrupted morphology and intense star formation (such as NGC 6240 with a separation(6) of about 2,600 light years and Mrk 463 with a separation(7) of about 13,000 light years between the nuclei) demonstrate the importance of major mergers of equal-mass spiral galaxies in this evolution; such mergers lead to an elliptical galaxy(8), as in the case of the double-radio-nucleus elliptical galaxy 0402+379 (with a separation of about 24 light years between the nuclei)(9). Minor mergers of a spiral galaxy with a smaller companion should be a more common occurrence, evolving into spiral galaxies with active massive black-hole pairs(10), but have hitherto not been seen. Here we report the presence of two active massive black holes, separated by about 490 light years, in the Seyfert(11) galaxy NGC 3393 (50 Mpc, about 160 million light years). The regular spiral morphology and predominantly old circum-nuclear stellar population(12) of this galaxy, and the closeness of the black holes embedded in the bulge, provide a hitherto missing observational point to the study of galaxy/black hole evolution. Comparison of our observations with current theoretical models of mergers suggests that they are the result of minor merger evolution(10).
C1 [Fabbiano, G.; Wang, Junfeng; Elvis, M.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA.
[Risaliti, G.] INAF Arcetri, I-50125 Florence, Italy.
RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA.
EM gfabbiano@cfa.harvard.edu
RI XRAY, SUZAKU/A-1808-2009;
OI Risaliti, Guido/0000-0002-3556-977X
FU NASA
FX This work was supported by a NASA grant (with Principal Investigator
J.W.). We thank P. Gandhi for discussions on the 13 mu m observations.
We used the NASA ADS and NED services. This work includes archival
Chandra and Hubble Space Telescope data. We acknowledge discussions with
T. Di Matteo and L. Mayer at the Aspen Center for Physics 2011 Summer
Program.
NR 30
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U1 1
U2 3
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD SEP 22
PY 2011
VL 477
IS 7365
BP 431
EP 434
DI 10.1038/nature10364
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 822WH
UT WOS:000295080500033
PM 21881560
ER
PT J
AU Guglielmino, M
Penna, V
Capogrosso-Sansone, B
AF Guglielmino, M.
Penna, V.
Capogrosso-Sansone, B.
TI Ising antiferromagnet with ultracold bosonic mixtures confined in a
harmonic trap
SO PHYSICAL REVIEW A
LA English
DT Article
ID ATOMIC MOTT INSULATOR; OPTICAL LATTICE
AB We present accurate results based on quantum Monte Carlo simulations of two-component bosonic systems on a square lattice and in the presence of an external harmonic confinement. Starting from hopping parameters and interaction strengths which stabilize the Ising antiferromagnetic phase in the homogeneous case and at half-integer filling factor, we study how the presence of the harmonic confinement challenges the realization of such a phase. We consider realistic trapping frequencies and number of particles, and we establish under which conditions, i.e., total number of particles and population imbalance, the antiferromagnetic phase can be observed in the trap.
C1 [Guglielmino, M.; Penna, V.] Politecn Torino, Dipartimento Fis, I-10129 Turin, Italy.
[Guglielmino, M.; Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
[Penna, V.] Politecn Torino, CNISM Unita Ric, I-10129 Turin, Italy.
RP Guglielmino, M (reprint author), Politecn Torino, Dipartimento Fis, Corso Duca Abruzzi 24, I-10129 Turin, Italy.
FU Institute for Atomic, Molecular and Optical Physics (ITAMP)
FX We would like to thank F. Minardi, S. Soyler, and S. Kuhr for fruitful
discussions. This work was supported by the Institute for Atomic,
Molecular and Optical Physics (ITAMP). MG wants to thank ITAMP for warm
hospitality and financial support.
NR 26
TC 9
Z9 9
U1 0
U2 2
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 SEP 20
PY 2011
VL 84
IS 3
AR 031603
DI 10.1103/PhysRevA.84.031603
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 822KM
UT WOS:000295044600004
ER
PT J
AU Artigau, E
Lafreniere, D
Doyon, R
Liu, M
Dupuy, TJ
Albert, L
Gagne, J
Malo, L
Gratadour, D
AF Artigau, Etienne
Lafreniere, David
Doyon, Rene
Liu, Michael
Dupuy, Trent J.
Albert, Loic
Gagne, Jonathan
Malo, Lison
Gratadour, Damien
TI DISCOVERY OF TWO L AND T BINARIES WITH WIDE SEPARATIONS AND PECULIAR
PHOTOMETRIC PROPERTIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; stars: individual (SIMP J1619275+031350AB, SIMP
J1501530-013506AB); stars: low-mass
ID STAR ADAPTIVE OPTICS; YOUNG BROWN DWARFS; DIGITAL SKY SURVEY; INFRARED
SPECTRAL CLASSIFICATION; SOLAR-TYPE STARS; LOW-MASS STARS; L/T
TRANSITION; RESOLVED SPECTROSCOPY; TAURI PHASE; FILTER SET
AB We present spatially resolved photometric and spectroscopic observations of two wide brown dwarf binaries uncovered by the Sondage Infrarouge de Mouvement Propre (SIMP) near-infrared proper motion survey. The first pair (SIMP J1619275+031350AB) has a separation of 0.'' 691 (15.2 AU) and components T2.5+T4.0, at the cooler end of the ill-understood J-band brightening. The system is unusual in that the earlier-type primary is bluer in J - K-s than the later-type secondary, whereas the reverse is expected for binaries in the late-L to T dwarf range. This remarkable color reversal can possibly be explained by very different cloud properties between the two components. The second pair (SIMP J1501530-013506AB) consists of an L4.5+ L5.5 (separation 0.'' 96, 30-47 AU) with a surprisingly large flux ratio (Delta J = 1.79 mag) considering the similar spectral types of its components. The large flux ratio could be explained if the primary is itself an equal-luminosity binary, which would make it one of the first known triple brown dwarf systems. Adaptive optics observations could not confirm this hypothesis, but it remains a likely one, which may be verified by high-resolution near-infrared spectroscopy. These two systems add to the handful of known brown dwarf binaries amenable to resolved spectroscopy without the aid of adaptive optics and constitute prime targets to test brown dwarf atmosphere models.
C1 [Artigau, Etienne; Lafreniere, David; Doyon, Rene; Albert, Loic; Gagne, Jonathan; Malo, Lison] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Artigau, Etienne; Lafreniere, David; Doyon, Rene; Albert, Loic; Gagne, Jonathan; Malo, Lison] Univ Montreal, Observ Mt Megant, Montreal, PQ H3C 3J7, Canada.
[Liu, Michael] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Albert, Loic] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA.
[Gratadour, Damien] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92195 Meudon, France.
RP Artigau, E (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada.
EM artigau@astro.umontreal.ca; mliu@ifa.hawaii.edu
OI Gagne, Jonathan/0000-0002-2592-9612; Lafreniere,
David/0000-0002-6780-4252
FU Natural Sciences and Engineering Research Council, Canada; Fonds
Quebecois de la Recherche sur la Nature et les Technologies; Canada
Foundation for Innovation; National Aeronautics and Space
Administration; National Science Foundation; W. M. Keck Foundation
FX The authors thank Marcel Bergman, the Gemini queue observer who took the
SIMP J1501-0135 and SIMP J1619+0313 observations, for notifying them
that two of the SIMP brown dwarf candidates "looked like doubles" in
GNIRS acquisition images. The authors thank Mike Shara for his
leadership and financial support in enabling the CPAPIR observing
campaign on the 1.5 m CTIO telescope. Our special thanks to Alberto
Pasten and Claudio Aguilera for carrying out the SIMP observations and
to Philippe Vallee for managing the SIMP data. This work was supported
in part through grants from the Natural Sciences and Engineering
Research Council, Canada, and from Fonds Quebecois de la Recherche sur
la Nature et les Technologies. CPAPIR was built through a grant from the
Canada Foundation for Innovation. This research has benefited from the
M, L, and T dwarf compendium housed at DwarfArchives.org and maintained
by Chris Gelino, Davy Kirkpatrick, and Adam Burgasser. 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. Based on observations obtained at the
Gemini Observatory (program ID: GS-2007A-Q-28 and GN-2008A-Q-57), 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), CNPq (Brazil), and CONICET (Argentina).
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 71
TC 10
Z9 10
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 SEP 20
PY 2011
VL 739
IS 1
AR 48
DI 10.1088/0004-637X/739/1/48
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700048
ER
PT J
AU Brammer, GB
Whitaker, KE
van Dokkum, PG
Marchesini, D
Franx, M
Kriek, M
Labbe, I
Lee, KS
Muzzin, A
Quadri, RF
Rudnick, G
Williams, R
AF Brammer, Gabriel B.
Whitaker, K. E.
van Dokkum, P. G.
Marchesini, D.
Franx, M.
Kriek, M.
Labbe, I.
Lee, K. -S.
Muzzin, A.
Quadri, R. F.
Rudnick, G.
Williams, R.
TI THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT
GALAXIES AT 0.4 <= z <= 2.2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift
ID MEDIUM-BAND SURVEY; DEEP-FIELD-SOUTH; STELLAR POPULATION SYNTHESIS;
COLOR-MAGNITUDE DISTRIBUTION; SPECTRAL ENERGY-DISTRIBUTION; K-SELECTED
GALAXIES; YALE-CHILE MUSYC; LUMINOSITY FUNCTION; RED-SEQUENCE;
MULTIWAVELENGTH SURVEY
AB We study the buildup of the bimodal galaxy population using the NEWFIRM Medium-Band Survey, which provides excellent redshifts and well-sampled spectral energy distributions of approximate to 27,000 galaxies with K < 22.8 at 0.4 < z < 2.2. We first show that star-forming galaxies and quiescent galaxies can be robustly separated with a two-color criterion over this entire redshift range. We then study the evolution of the number density and mass density of quiescent and star-forming galaxies, extending the results of the COMBO-17, DEEP2, and other surveys to z = 2.2. The mass density of quiescent galaxies with M greater than or similar to 3 x 10(10) M-circle dot increases by a factor of similar to 10 from z similar to 2 to the present day, whereas the mass density in star-forming galaxies is flat or decreases over the same time period. Modest mass growth by a factor of similar to 2 of individual quiescent galaxies can explain roughly half of the strong density evolution at masses > 10(11) M-circle dot, due to the steepness of the exponential tail of the mass function. The rest of the density evolution of massive, quiescent galaxies is likely due to transformation (e. g., quenching) of the massive star-forming population, a conclusion which is consistent with the density evolution we observe for the star-forming galaxies themselves, which is flat or decreasing with cosmic time. Modest mass growth does not explain the evolution of less massive quiescent galaxies (similar to 10(10.5) M-circle dot), which show a similarly steep increase in their number densities. The less massive quiescent galaxies are therefore continuously formed by transforming galaxies from the star-forming population.
C1 [Brammer, Gabriel B.] European So Observ, Santiago, Chile.
[Brammer, Gabriel B.; Whitaker, K. E.; van Dokkum, P. G.; Lee, K. -S.; Muzzin, A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Marchesini, D.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
[Franx, M.] Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Kriek, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kriek, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Labbe, I.; Quadri, R. F.; Williams, R.] Carnegie Observ, Pasadena, CA 91101 USA.
[Rudnick, G.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
RP Brammer, GB (reprint author), European So Observ, Alonso de Cordova 3107,Casilla 19001, Santiago, Chile.
EM gbrammer@eso.org
FU NSF [AST-0449678, AST-0807974]
FX We thank the anonymous referee for helpful comments and suggestions that
improved the manuscript. Support from NSF grants AST-0449678 and
AST-0807974 is gratefully acknowledged. This research has made extensive
use of the IDL Astronomy Library (http://idlastro.gsfc.nasa.gov/) and
NASA's Astrophysics Data System Bibliographic Services.
NR 93
TC 162
Z9 162
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2011
VL 739
IS 1
AR 24
DI 10.1088/0004-637X/739/1/24
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700024
ER
PT J
AU Chornock, R
Filippenko, AV
Li, W
Marion, GH
Foley, RJ
Modjaz, M
Rafelski, M
Becker, GD
de Vries, WH
Garnavich, P
Jorgenson, RA
Lynch, DK
Malec, AL
Moran, EC
Murphy, MT
Rudy, RJ
Russell, RW
Silverman, JM
Steele, TN
Stockton, A
Wolfe, AM
Woodward, CE
AF Chornock, R.
Filippenko, A. V.
Li, W.
Marion, G. H.
Foley, R. J.
Modjaz, M.
Rafelski, M.
Becker, G. D.
de Vries, W. H.
Garnavich, P.
Jorgenson, R. A.
Lynch, D. K.
Malec, A. L.
Moran, E. C.
Murphy, M. T.
Rudy, R. J.
Russell, R. W.
Silverman, J. M.
Steele, T. N.
Stockton, A.
Wolfe, A. M.
Woodward, C. E.
TI THE TRANSITIONAL STRIPPED-ENVELOPE SN 2008ax: SPECTRAL EVOLUTION AND
EVIDENCE FOR LARGE ASPHERICITY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE polarization; supernovae: general; supernovae: individual (SN 2008ax)
ID CORE-COLLAPSE SUPERNOVAE; DIFFUSE INTERSTELLAR BANDS; NEAR-INFRARED
SPECTRA; REMNANT CASSIOPEIA-A; GAMMA-RAY BURSTS; II-P SUPERNOVA; IB
SUPERNOVAE; X-RAY; OPTICAL SPECTROSCOPY; IA SUPERNOVA
AB Supernova (SN) 2008ax in NGC 4490 was discovered within hours after shock breakout, presenting the rare opportunity to study a core-collapse SN beginning with the initial envelope-cooling phase immediately following shock breakout. We present an extensive sequence of optical and near-infrared spectra, as well as three epochs of optical spectropolarimetry. Our initial spectra, taken two days after shock breakout, are dominated by hydrogen Balmer lines at high velocity. However, by maximum light, He I lines dominated the optical and near-infrared spectra, which closely resembled those of normal Type Ib supernovae (SNe Ib) such as SN 1999ex. This spectroscopic transition defines Type IIb SNe, but the strong similarity of SN 2008ax to normal SNe Ib beginning near maximum light, including an absorption feature near 6270 angstrom due to H alpha at high velocities, suggests that many objects classified as SNe Ib in the literature may have ejected similar amounts of hydrogen as SN 2008ax, roughly a few x 0.01 M-circle dot. Only the unusually early discovery of SN 2008ax allowed us to observe the spectroscopic signatures of the hydrogen-rich outer ejecta. Early-time spectropolarimetry (six and nine days after shock breakout) revealed strong line polarization modulations of 3.4% across H alpha, indicating the presence of large asphericities in the outer ejecta and possibly that the spectrum of SN 2008ax could be dependent on the viewing angle. After removal of interstellar polarization, the continuum shares a common polarization angle with the hydrogen, helium, and oxygen lines, while the calcium and iron absorptions are oriented at different angles. This is clear evidence of deviations from axisymmetry even in the outer ejecta. Intrinsic continuum polarization of 0.64% only nine days after shock breakout shows that the outer layers of the ejecta were quite aspherical. A single epoch of late-time spectropolarimetry as well as the shapes of the nebular line profiles demonstrate that asphericities extended from the outermost layers all the way down to the center of this core-collapse SN. SN 2008ax may in some ways be an extragalactic analog of the explosion giving rise to Cassiopeia A, which has recently been determined to be a remnant of an SN IIb.
C1 [Chornock, R.; Filippenko, A. V.; Li, W.; Modjaz, M.; Silverman, J. M.; Steele, T. N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Chornock, R.; Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Marion, G. H.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA.
[Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Rafelski, M.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Rafelski, M.; Wolfe, A. M.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Becker, G. D.] Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Becker, G. D.; Jorgenson, R. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[de Vries, W. H.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[de Vries, W. H.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Garnavich, P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Lynch, D. K.; Rudy, R. J.; Russell, R. W.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Malec, A. L.; Murphy, M. T.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Moran, E. C.] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA.
[Stockton, A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Woodward, C. E.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
RP Chornock, R (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM rchornock@cfa.harvard.edu
RI Murphy, Michael/B-8832-2008
OI Murphy, Michael/0000-0002-7040-5498
FU W. M. Keck Foundation; National Aeronautics and Space Administration,
Science Mission Directorate [NNX-08AE38A]; NSF [AST-0607485,
AST-0908886]; TABASGO Foundation; Miller Institute for Basic Research in
Science; Aerospace Corporation
FX We acknowledge M. Ganeshalingam, C. V. Griffith, J. Hodge, K. Merriman,
R. Mostardi, D. Poznanski, and X. Wang for assistance with some of the
observations. We would also like to thank the observers of the Lick AGN
Monitoring Project 2008 (LAMP) for obtaining some of these SN 2008ax
spectra during the nightly SN observations, in particular A. J. Barth,
V. N. Bennert, M. C. Bentz, G. Canalizo, K. D. Hiner, C. E. Thornton, J.
L. Walsh, and J.-H. Woo. 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; it
was made possible by the generous financial support of the W. M. Keck
Foundation. The authors wish to recognize and acknowledge the very
significant cultural role and reverence that the summit of Mauna Kea has
always had within the indigenous Hawaiian community; we are most
fortunate to have the opportunity to conduct observations from this
mountain. We also would like to thank the expert assistance of the Keck
and Lick staffs in making these observations possible. Data for this
manuscript were obtained by Visiting Astronomers at the Infrared
Telescope Facility, which is operated by the University of Hawaii under
Cooperative Agreement No. NNX-08AE38A with the National Aeronautics and
Space Administration, Science Mission Directorate, Planetary Astronomy
Program. We thank Alan Tokunaga and the IRTF staff for their help
performing timely observations. A.V.F.'s supernova research group at UC
Berkeley has been supported by NSF grants AST-0607485 and AST-0908886,
as well as by the TABASGO Foundation. M. M. is supported by a fellowship
from the Miller Institute for Basic Research in Science. D. K. L., R. J.
R., and R. W. R. were supported by The Aerospace Corporation's
Independent Research and Development program.
NR 154
TC 35
Z9 35
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2011
VL 739
IS 1
AR 41
DI 10.1088/0004-637X/739/1/41
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700041
ER
PT J
AU Dunkley, J
Hlozek, R
Sievers, J
Acquaviva, V
Ade, PAR
Aguirre, P
Amiri, M
Appel, JW
Barrientos, LF
Battistelli, ES
Bond, JR
Brown, B
Burger, B
Chervenak, J
Das, S
Devlin, MJ
Dicker, SR
Doriese, WB
Dunner, R
Essinger-Hileman, T
Fisher, RP
Fowler, JW
Hajian, A
Halpern, M
Hasselfield, M
Hernandez-Monteagudo, C
Hilton, GC
Hilton, M
Hincks, AD
Huffenberger, KM
Hughes, DH
Hughes, JP
Infante, L
Irwin, KD
Juin, JB
Kaul, M
Klein, J
Kosowsky, A
Lau, JM
Limon, M
Lin, YT
Lupton, RH
Marriage, TA
Marsden, D
Mauskopf, P
Menanteau, F
Moodley, K
Moseley, H
Netterfield, CB
Niemack, MD
Nolta, MR
Page, LA
Parker, L
Partridge, B
Reid, B
Sehgal, N
Sherwin, B
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Thornton, R
Trac, H
Tucker, C
Warne, R
Wollack, E
Zhao, Y
AF Dunkley, J.
Hlozek, R.
Sievers, J.
Acquaviva, V.
Ade, P. A. R.
Aguirre, P.
Amiri, M.
Appel, J. W.
Barrientos, L. F.
Battistelli, E. S.
Bond, J. R.
Brown, B.
Burger, B.
Chervenak, J.
Das, S.
Devlin, M. J.
Dicker, S. R.
Doriese, W. Bertrand
Duenner, R.
Essinger-Hileman, T.
Fisher, R. P.
Fowler, J. W.
Hajian, A.
Halpern, M.
Hasselfield, M.
Hernandez-Monteagudo, C.
Hilton, G. C.
Hilton, M.
Hincks, A. D.
Huffenberger, K. M.
Hughes, D. H.
Hughes, J. P.
Infante, L.
Irwin, K. D.
Juin, J. B.
Kaul, M.
Klein, J.
Kosowsky, A.
Lau, J. M.
Limon, M.
Lin, Y-T.
Lupton, R. H.
Marriage, T. A.
Marsden, D.
Mauskopf, P.
Menanteau, F.
Moodley, K.
Moseley, H.
Netterfield, C. B.
Niemack, M. D.
Nolta, M. R.
Page, L. A.
Parker, L.
Partridge, B.
Reid, B.
Sehgal, N.
Sherwin, B.
Spergel, D. N.
Staggs, S. T.
Swetz, D. S.
Switzer, E. R.
Thornton, R.
Trac, H.
Tucker, C.
Warne, R.
Wollack, E.
Zhao, Y.
TI THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGICAL PARAMETERS FROM THE 2008
POWER SPECTRUM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmological parameters; cosmology:
observations
ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND ANISOTROPIES; PRIMORDIAL
HELIUM ABUNDANCE; BIG-BANG NUCLEOSYNTHESIS; MASSIVE GALAXY CLUSTERS;
STAR-FORMING GALAXIES; SOUTH-POLE TELESCOPE; INFLATIONARY UNIVERSE;
HUBBLE CONSTANT; OBSERVED GROWTH
AB We present cosmological parameters derived from the angular power spectrum of the cosmic microwave background (CMB) radiation observed at 148 GHz and 218 GHz over 296 deg(2) with the Atacama Cosmology Telescope (ACT) during its 2008 season. ACT measures fluctuations at scales 500 < l < 10,000. We fit a model for the lensed CMB, Sunyaev-Zel'dovich (SZ), and foreground contribution to the 148 GHz and 218 GHz power spectra, including thermal and kinetic SZ, Poisson power from radio and infrared point sources, and clustered power from infrared point sources. At l = 3000, about half the power at 148 GHz comes from primary CMB after masking bright radio sources. The power from thermal and kinetic SZ is estimated to be B-3000 = 6.8 +/- 2.9 mu K-2, where B-l = l (l + 1) C-l/2 pi. The IR Poisson power at 148 GHz is B-3000 = 7.8 +/- 0.7 mu K-2 (Cl = 5.5 +/- 0.5 nK(2)), and a clustered IR component is required with B-3000 = 4.6 +/- 0.9 mu K-2, assuming an analytic model for its power spectrum shape. At 218 GHz only about 15% of the power, approximately 27 mu K-2, is CMB anisotropy at l = 3000. The remaining 85% is attributed to IR sources (approximately 50% Poisson and 35% clustered), with spectral index alpha = 3.69 +/- 0.14 for flux scaling as S(v) proportional to v(alpha). We estimate primary cosmological parameters from the less contaminated 148 GHz spectrum, marginalizing over SZ and source power. The Lambda CDM cosmological model is a good fit to the data (chi(2)/dof = 29/46), and Lambda CDM parameters estimated from ACT+Wilkinson Microwave Anisotropy Probe (WMAP) are consistent with the seven-year WMAP limits, with scale invariant ns = 1 excluded at 99.7% confidence level (CL) (3 sigma). A model with no CMB lensing is disfavored at 2.8 sigma. By measuring the third to seventh acoustic peaks, and probing the Silk damping regime, the ACT data improve limits on cosmological parameters that affect the small-scale CMB power. The ACT data combined with WMAP give a 6 sigma detection of primordial helium, with Y-P = 0.313 +/- 0.044, and a 4 sigma detection of relativistic species, assumed to be neutrinos, with N-eff = 5.3 +/- 1.3 (4.6 +/- 0.8 with BAO+H-0 data). From the CMB alone the running of the spectral index is constrained to be dn(s)/d ln k = - 0.034 +/- 0.018, the limit on the tensor-to-scalar ratio is r < 0.25 (95% CL), and the possible contribution of Nambu cosmic strings to the power spectrum is constrained to string tension G mu < 1.6 x 10(-7) ( 95% CL).
C1 [Dunkley, J.; Hlozek, R.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England.
[Dunkley, J.; Appel, J. W.; Das, S.; Essinger-Hileman, T.; Fisher, R. P.; Fowler, J. W.; Hajian, A.; Hincks, A. D.; Lau, J. M.; Limon, M.; Niemack, M. D.; Page, L. A.; Parker, L.; Reid, B.; Sherwin, B.; Staggs, S. T.; Switzer, E. R.; Zhao, Y.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Dunkley, J.; Acquaviva, V.; Das, S.; Hajian, A.; Lin, Y-T.; Lupton, R. H.; Marriage, T. A.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Sievers, J.; Bond, J. R.; Hajian, A.; Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Acquaviva, V.; Hughes, J. P.; Menanteau, F.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Ade, P. A. R.; Mauskopf, P.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aguirre, P.; Barrientos, L. F.; Duenner, R.; Infante, L.; Juin, J. B.; Lin, Y-T.] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Amiri, M.; Battistelli, E. S.; Burger, B.; Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Battistelli, E. S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Brown, B.; Kosowsky, A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Chervenak, J.; Moseley, H.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Das, S.] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Das, S.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Devlin, M. J.; Dicker, S. R.; Kaul, M.; Klein, J.; Limon, M.; Marsden, D.; Swetz, D. S.; Thornton, R.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Doriese, W. Bertrand; Fowler, J. W.; Hilton, G. C.; Irwin, K. D.; Niemack, M. D.; Swetz, D. S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
[Hernandez-Monteagudo, C.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Hilton, M.; Moodley, K.; Warne, R.] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hilton, M.; Moodley, K.] Rosebank, Ctr High Performance Comp, Cape Town, South Africa.
[Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Hughes, D. H.] INAOE, Puebla, Mexico.
[Lau, J. M.; Sehgal, N.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Lau, J. M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Lin, Y-T.] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan.
[Marriage, T. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Partridge, B.] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Reid, B.] Univ Barcelona, ICC, E-08028 Barcelona, Spain.
[Switzer, E. R.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Thornton, R.] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
[Trac, H.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Trac, H.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Dunkley, J (reprint author), Univ Oxford, Subdept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew
James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Huffenberger, Kevin/0000-0001-7109-0099; Sievers,
Jonathan/0000-0001-6903-5074; Limon, Michele/0000-0002-5900-2698
FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
PIRE-0507768]; Princeton University; University of Pennsylvania; RCUK
Fellowship; Rhodes Trust; NASA [NNX08AH30G]; Natural Science and
Engineering Research Council of Canada (NSERC); NSF [AST-0546035,
AST-0606975]; FONDAP Centro de Astrofisica; CONICYT; MECESUP; Fundacion
Andes; NSF Physics Frontier Center [PHY-0114422]; South African National
Research Foundation (NRF); South African Centre for High Performance
Computing (CHPC); South African Square Kilometer Array (SKA); Berkeley
Center for Cosmological Physics; World Premier International Research
Center Initiative, MEXT, Japan; U.S. Department of Energy
[DE-AC3-76SF00515]; Canada Foundation for Innovation under the auspices
of Compute Canada; Government of Toronto; NASA Office of Space Science
FX ACT is on the Chajnantor Science preserve, which was made possible by
the Chilean Comision Nacional de Investigacion Cientifica y Tecnologica.
We are grateful for the assistance we received at various times from the
ALMA, APEX, ASTE, CBI/QUIET, and NANTEN2 groups. The PWV data come from
the public APEX weather Web site. Field operations were based at the Don
Esteban facility run by Astro-Norte. Reed Plimpton and David Jacobson
worked at the telescope during the 2008 season. We thank Norm Jarosik
for support throughout the project. We also thank Adam Moss and Richard
Battye for sharing their cosmic string power spectrum, Laurie Shaw and
Nick Battaglia for providing SZ power spectra, and Bruce Bassett for
suggestions on testing lensing in the power spectrum. We thank Marco
Viero and Graeme Addison for providing useful input on clustered point
sources. This work was supported by the U.S. National Science Foundation
through awards AST-0408698 for the ACT project, and PHY-0355328,
AST-0707731 and PIRE-0507768. Funding was also provided by Princeton
University and the University of Pennsylvania. The PIRE program made
possible exchanges between Chile, South Africa, Spain, and the US that
enabled this research program. J.D. acknowledges support from an RCUK
Fellowship. R. H. received funding from the Rhodes Trust. V. A., S. D.,
A. H., and T. M. were supported through NASA grant NNX08AH30G. A. D. H.
received additional support from a Natural Science and Engineering
Research Council of Canada (NSERC) PGS-D scholarship. A. K. and B. P.
were partially supported through NSF AST-0546035 and AST-0606975,
respectively, for work on ACT. L. I. acknowledges partial support from
FONDAP Centro de Astrofisica. R. D. was supported by CONICYT, MECESUP,
and Fundacion Andes. E. S. acknowledges support by NSF Physics Frontier
Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics.
K. M., M. H., and R. W. received financial support from the South
African National Research Foundation (NRF), the Meraka Institute via
funding for the South African Centre for High Performance Computing
(CHPC), and the South African Square Kilometer Array (SKA) Project. S.
D. acknowledges support from the Berkeley Center for Cosmological
Physics. Y.T.L. acknowledges support from the World Premier
International Research Center Initiative, MEXT, Japan. N.S. is supported
by the U.S. Department of Energy contract to SLAC no. DE-AC3-76SF00515.
Computations were performed on the GPC supercomputer at the SciNet HPC
Consortium. SciNet is funded by the Canada Foundation for Innovation
under the auspices of Compute Canada, the Government of Toronto. 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. The data will be made public through LAMBDA
(http://lambda.gsfc.nasa.gov/) and the ACT Web site
(http://www.physics.princeton.edu/act/).
NR 139
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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 SEP 20
PY 2011
VL 739
IS 1
AR 52
DI 10.1088/0004-637X/739/1/52
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700052
ER
PT J
AU Laskar, T
Berger, E
Chary, RR
AF Laskar, Tanmoy
Berger, Edo
Chary, Ranga-Ram
TI EXPLORING THE GALAXY MASS-METALLICITY RELATION AT z similar to 3-5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: high-redshift; galaxies: ISM; galaxies: luminosity function,
mass function; gamma-ray burst: general; infrared: galaxies
ID GAMMA-RAY BURST; STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; HIGH
COLUMN DENSITY; DIGITAL SKY SURVEY; GRB HOST GALAXY; LY-ALPHA; STELLAR
POPULATIONS; LUMINOSITY FUNCTIONS; SPITZER OBSERVATIONS
AB Long-duration gamma-ray bursts (GRBs) provide a premier tool for studying high-redshift star-forming galaxies thanks to their extreme brightness and association with massive stars. Here we use GRBs to study the galaxy stellar mass-metallicity (M(*)-Z) relation at z similar to 3-5, where conventional direct metallicity measurements are extremely challenging. We use the interstellar medium metallicities of long GRB hosts derived from afterglow absorption spectroscopy, in conjunction with host galaxy stellar masses determined from deep Spitzer 3.6 mu m observations of 20 GRB hosts. We detect about 1/4 of the hosts with M(AB)(I) approximate to -21.5 to -22.5 mag and place a limit of M(AB)(I) greater than or similar to -19 mag on the remaining hosts from a stacking analysis. Using these observations, we present the first rest-frame optical luminosity distribution of long GRB hosts at z greater than or similar to 3 and find that it is similar to the distribution of long GRB hosts at z similar to 1. In comparison to Lyman-break galaxies at the same redshift, GRB hosts are generally fainter, but the sample is too small to rule out an overall similar luminosity function. On the other hand, the GRB hosts appear to be more luminous than the population of Ly alpha emitters at z similar to 3-4. Using a conservative range of mass-to-light ratios for simple stellar populations (with ages of 70 Myr to similar to 2 Gyr), we infer the host stellar masses and present mass-metallicity measurements at z similar to 3-5 (< z > similar to 3.5). We find that the detected GRB hosts, with M(*) approximate to 2 x 10(10) M(circle dot), display a wide range of metallicities, but that the mean metallicity at this mass scale, Z approximate to 0.3 Z(circle dot), is lower than measurements at z less than or similar to 3. Combined with stacking of the non-detected hosts with M(*) less than or similar to 3 x 10(9) M(circle dot) and Z less than or similar to 0.1 Z(circle dot), we find tentative evidence for the existence of an M(*)-Z relation at z similar to 3.5 and continued evolution of this relation to systematically lower metallicities from z similar to 2.
C1 [Laskar, Tanmoy; Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chary, Ranga-Ram] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP Laskar, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NASA; JPL/Caltech
FX We thank the anonymous referee for useful comments, which improved the
quality of the manuscript. 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.
NR 72
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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 SEP 20
PY 2011
VL 739
IS 1
AR 1
DI 10.1088/0004-637X/739/1/1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700001
ER
PT J
AU Levesque, EM
Berger, E
Soderberg, AM
Chornock, R
AF Levesque, Emily M.
Berger, Edo
Soderberg, Alicia M.
Chornock, Ryan
TI METALLICITY IN THE GRB 100316D/SN 2010bh HOST COMPLEX
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: abundances; gamma-ray burst: individual (GRB 100316D)
ID GAMMA-RAY BURST; CORE-COLLAPSE SUPERNOVAE; STARBURST GALAXIES;
STAR-FORMATION; NEARBY LONG; CONNECTION; EMISSION; EXPLOSION; DISCOVERY;
CLASSIFICATION
AB The recent long-duration GRB 100316D, associated with supernova SN 2010bh and detected by Swift, is one of the nearest gamma-ray burst (GRB)-supernovae (SNe) ever observed (z = 0.059). This provides us with a unique opportunity to study the explosion environment on similar to kpc scale in relation to the host galaxy complex. Here we present spatially resolved spectrophotometry of the host galaxy, focusing on both the explosion site and the brightest star-forming regions. Using these data, we extract the spatial profiles of the relevant emission features (H alpha, H beta, [O III]lambda 5007, and [N II]lambda 6584) and use these profiles to examine variations in metallicity and star formation rate (SFR) as a function of position in the host galaxy. We conclude that GRB 100316D/SN2010bh occurred in a low-metallicity host galaxy, and that the GRB-SN explosion site corresponds to the region with the lowest metallicity and highest SFR sampled by our observations.
C1 [Levesque, Emily M.] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Berger, Edo; Soderberg, Alicia M.; Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Levesque, EM (reprint author), Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
EM Emily.Levesque@colorado.edu
FU NASA, Chandra X-ray Center [PF0-110075]; NASA [NAS8-03060]; Swift
[5080010, 6090612]
FX We are grateful for the hospitality and assistance of the support staff
at Las Campanas Observatory in Chile. This paper utilized data from the
Gamma-Ray Burst Coordinates Network (GCN) circulars. E. M. L. is
supported by NASA through Einstein Postdoctoral Fellowship grant number
PF0-110075 awarded by the Chandra X-ray Center, which is operated by the
Smithsonian Astrophysical Observatory for NASA under contract
NAS8-03060. GRB research at Harvard is supported in part by Swift AO5
grant 5080010 and AO6 grant 6090612.
NR 57
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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 SEP 20
PY 2011
VL 739
IS 1
AR 23
DI 10.1088/0004-637X/739/1/23
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700023
ER
PT J
AU Schmelz, JT
Worley, BT
Anderson, DJ
Pathak, S
Kimble, JA
Jenkins, BS
Saar, SH
AF Schmelz, J. T.
Worley, B. T.
Anderson, D. J.
Pathak, S.
Kimble, J. A.
Jenkins, B. S.
Saar, S. H.
TI ISOTHERMAL AND MULTITHERMAL ANALYSIS OF CORONAL LOOPS OBSERVED WITH
ATMOSPHERIC IMAGING ASSEMBLY. II. 211 angstrom SELECTED LOOPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: fundamental parameters; Sun: UV radiation
ID X-RAY TELESCOPE; EMISSION-LINES; ATOMIC DATABASE; REGION; TEMPERATURE;
DISTRIBUTIONS; SPECTROMETER; EXPLORER; CHIANTI
AB An important component of coronal loop analysis involves conflicting results on the cross-field temperature distribution. Are loops isothermal or multithermal? The Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory was designed in part to answer this question. AIA has a series of coronal filters that peak at different temperatures and cover the entire active region temperature range. These properties should make AIA ideal for multithermal analysis, but recent results have shown that the response functions of two of the filters, AIA 94 and 131 angstrom, are missing a significant number of low-temperature emission lines. Here we analyze coronal loops from several active regions that were chosen in the 211 angstrom channel of AIA, which has a peak response temperature of log T = 6.3. The differential emission measure (DEM) analysis of the 12 loops in our sample reveals that using data from the 131 angstrom AIA filter distorts the results, and we have no choice but to do the analysis without these data. The 94 angstrom data do not appear to be as important, simply because the chosen loops are not visible in this channel. If we eliminate the 131 angstrom data, however, we find that our DEM analysis is not well constrained on the cool temperature end of six of our loops. The information revealed by our 211 selected loops indicates that additional atomic data are required in order to pin down the cross-field temperature distribution.
C1 [Schmelz, J. T.; Worley, B. T.; Anderson, D. J.; Pathak, S.; Kimble, J. A.; Jenkins, B. S.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
[Schmelz, J. T.; Saar, S. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
EM jschmelz@memphis.edu
FU NSF [ATM-0402729]; NASA/SAO; [NNM07AB07C]
FX We thank Vinay Kashyap (CfA) for his help with Monte Carlo DEMs. The
Atmospheric Imaging Assembly on the Solar Dynamics Observatory is part
of NASA's Living with a Star program. Solar physics research at the
University of Memphis is supported by NSF ATM-0402729 as well as a
Hinode subcontract from NASA/SAO. S. H. S. is supported by contract
NNM07AB07C to NASA. We also benefited from discussions at theCoronal
Loops Workshops held in Paris (2002 November), Palermo (2004 September),
Santorini (2007 June), and Florence (2009 June).
NR 23
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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 SEP 20
PY 2011
VL 739
IS 1
AR 33
DI 10.1088/0004-637X/739/1/33
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700033
ER
PT J
AU Schwadron, NA
Smith, CW
Spence, HE
Kasper, JC
Korreck, K
Stevens, ML
Maruca, BA
Kiefer, KK
Lepri, ST
McComas, D
AF Schwadron, N. A.
Smith, C. W.
Spence, H. E.
Kasper, J. C.
Korreck, K.
Stevens, M. L.
Maruca, B. A.
Kiefer, K. K.
Lepri, S. T.
McComas, D.
TI CORONAL ELECTRON TEMPERATURE FROM THE SOLAR WIND SCALING LAW THROUGHOUT
THE SPACE AGE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar wind; Sun: corona; Sun: coronal mass ejections (CMEs); Sun:
dynamo; Sun: evolution; sunspots
ID ION COMPOSITION SPECTROMETER; MAGNETIC-FLUX; HELIOSPHERE; ULYSSES;
BALANCE; MINIMA; SWICS; FIELD
AB Recent in situ observations of the solar wind show that charge states (e. g., the O7+/O6+ and C6+/C5+ abundance ratios) and alpha-particle composition evolved through the extended, deep solar minimum between solar cycles 23 and 24 (i.e., from 2006 to 2009). Prior investigations have found that both particle flux and magnetic field strength gradually decreased over this period of time. In this study, we find that (for a given solar wind speed) the coronal electron temperature (as derived from O7+/O6+ and C6+/C5+ measurements from ACE) likewise decreased during this minimum. We use the Schwadron & McComas solar wind scaling law to show that cooler coronal electron temperatures are naturally associated with lower particle fluxes because downward heat conduction must be reduced to keep the average energy loss per particle fixed. The results of the scaling law should apply to all solar wind models and suggest that the evolution of the solar wind is linked to the solar dynamo, which caused the coronal magnetic field strength to decrease in the deep, extended minimum. We utilize the scaling law to project coronal electron temperatures backward in time throughout the space age and find that these temperatures have been decreasing in successive temperature maxima since 1987 but were increasing in successive temperature maxima from 1969 to 1987. Thus, we show how the solar wind scaling law relates solar wind properties observed at 1 AU back to coronal electron temperatures throughout the space age.
C1 [Schwadron, N. A.; Smith, C. W.; Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Kasper, J. C.; Korreck, K.; Stevens, M. L.; Maruca, B. A.; Kiefer, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lepri, S. T.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Schwadron, N. A.; McComas, D.] SW Res Inst, San Antonio, TX 78228 USA.
[McComas, D.] Univ Texas San Antonio, San Antonio, TX 78249 USA.
RP Schwadron, NA (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
RI Lepri, Susan/I-8611-2012; Spence, Harlan/A-1942-2011; Kasper,
Justin/D-1152-2010;
OI Kasper, Justin/0000-0002-7077-930X; Spence, Harlan/0000-0002-2526-2205
FU LRO/CRaTER; Earth Moon Mars Radiation Environment Model (EMMREM);
ACE/SWEPAM; WIND/SWE; NSF
FX N.A.S. was supported by LRO/CRaTER and the Earth Moon Mars Radiation
Environment Model (EMMREM) projects. D.Mc. was supported by ACE/SWEPAM.
J.C.K., M. L. S., K. E. K., and B. A. M. were supported by the WIND/SWE
project. K. K. was supported by the NSF-Solar REU program. We thank the
ACE SWICS and SWIMS instrument team and the Ion Mass Spectrometer
(SWIMS) ACE Science Center for providing the ACE data.
NR 35
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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 SEP 20
PY 2011
VL 739
IS 1
AR 9
DI 10.1088/0004-637X/739/1/9
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700009
ER
PT J
AU Stello, D
Meibom, S
Gilliland, RL
Grundahl, F
Hekker, S
Mosser, B
Kallinger, T
Mathur, S
Garcia, RA
Huber, D
Basu, S
Bedding, TR
Brogaard, K
Chaplin, WJ
Elsworth, YP
Molenda-Zakowicz, J
Szabo, R
Still, M
Jenkins, JM
Christensen-Dalsgaard, J
Kjeldsen, H
Serenelli, AM
Wohler, B
AF Stello, Dennis
Meibom, Soren
Gilliland, Ronald L.
Grundahl, Frank
Hekker, Saskia
Mosser, Benoit
Kallinger, Thomas
Mathur, Savita
Garcia, Rafael A.
Huber, Daniel
Basu, Sarbani
Bedding, Timothy R.
Brogaard, Karsten
Chaplin, William J.
Elsworth, Yvonne P.
Molenda-Zakowicz, Joanna
Szabo, Robert
Still, Martin
Jenkins, Jon M.
Christensen-Dalsgaard, Jorgen
Kjeldsen, Hans
Serenelli, Aldo M.
Wohler, Bill
TI AN ASTEROSEISMIC MEMBERSHIP STUDY OF THE RED GIANTS IN THREE OPEN
CLUSTERS OBSERVED BY KEPLER: NGC 6791, NGC 6819, AND NGC 6811
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE open clusters and associations: individual (NGC 6791, NGC6819, NGC6811);
stars: fundamental parameters; stars: interiors; stars: oscillations;
techniques: photometric
ID SOLAR-LIKE OSCILLATIONS; BOLOMETRIC CORRECTIONS; STELLAR EVOLUTION;
METAL ABUNDANCES; NGC-6791; STARS; OLD; CONSTRAINTS; AMPLITUDES;
ISOCHRONES
AB Studying star clusters offers significant advances in stellar astrophysics due to the combined power of having many stars with essentially the same distance, age, and initial composition. This makes clusters excellent test benches for verification of stellar evolution theory. To fully exploit this potential, it is vital that the star sample is uncontaminated by stars that are not members of the cluster. Techniques for determining cluster membership therefore play a key role in the investigation of clusters. We present results on three clusters in the Kepler field of view based on a newly established technique that uses asteroseismology to identify fore-or background stars in the field, which demonstrates advantages over classical methods such as kinematic and photometry measurements. Four previously identified seismic non-members in NGC6819 are confirmed in this study, and three additional non-members are found-two in NGC6819 and one in NGC6791. We further highlight which stars are, or might be, affected by blending, which needs to be taken into account when analyzing these Kepler data.
C1 [Stello, Dennis; Huber, Daniel; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Grundahl, Frank; Brogaard, Karsten] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hekker, Saskia; Chaplin, William J.; Elsworth, Yvonne P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Mosser, Benoit] Univ Paris 07, LESIA, CNRS, Univ Paris 06,Observ Paris, F-92195 Meudon, France.
[Kallinger, Thomas] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Kallinger, Thomas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Mathur, Savita] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Garcia, Rafael A.] Univ Paris 07, Lab AIM, CEA DSM CNRS, IRFU SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Brogaard, Karsten] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada.
[Molenda-Zakowicz, Joanna] Uniwersytetu Wroclawskiego, Inst Astron, PL-51622 Wroclaw, Poland.
[Szabo, Robert] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Jenkins, Jon M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Serenelli, Aldo M.] Fac Ciencies, Inst Ciencias Espacio CSIC IEEC, Bellaterra 08193, Spain.
[Wohler, Bill] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Stello, D (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
OI Kallinger, Thomas/0000-0003-3627-2561; Brogaard,
Karsten/0000-0003-2001-0276; Bedding, Timothy/0000-0001-5943-1460;
Szabo, Robert/0000-0002-3258-1909; Bedding, Tim/0000-0001-5222-4661;
Basu, Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776;
Serenelli, Aldo/0000-0001-6359-2769
FU NASA's Science Mission Directorate; Australian Research Council;
Hungarian Academy of Sciences; Hungarian OTKA [K83790, MB08C 81013]; UK
Science and Technology Facilities Council (STFC); Carlsberg Foundation;
National Science Foundation; Janos Bolyai Research Scholarship
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors thank the entire Kepler team without whom this
investigation would not have been possible. D. S. acknowledges support
from the Australian Research Council. This project has been supported by
the "Lendulet" program of the Hungarian Academy of Sciences and the
Hungarian OTKA grant K83790 and MB08C 81013. S. H. acknowledges
financial support from the UK Science and Technology Facilities Council
(STFC). K. B. acknowledges financial support from the Carlsberg
Foundation. NCAR is supported by the National Science Foundation. R. S.
thanks the support of the Janos Bolyai Research Scholarship.
NR 45
TC 52
Z9 52
U1 1
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 SEP 20
PY 2011
VL 739
IS 1
AR 13
DI 10.1088/0004-637X/739/1/13
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700013
ER
PT J
AU Weisz, DR
Dalcanton, JJ
Williams, BF
Gilbert, KM
Skillman, ED
Seth, AC
Dolphin, AE
McQuinn, KBW
Gogarten, SM
Holtzman, J
Rosema, K
Cole, A
Karachentsev, ID
Zaritsky, D
AF Weisz, Daniel R.
Dalcanton, Julianne J.
Williams, Benjamin F.
Gilbert, Karoline M.
Skillman, Evan D.
Seth, Anil C.
Dolphin, Andrew E.
McQuinn, Kristen B. W.
Gogarten, Stephanie M.
Holtzman, Jon
Rosema, Keith
Cole, Andrew
Karachentsev, Igor D.
Zaritsky, Dennis
TI THE ACS NEARBY GALAXY SURVEY TREASURY. VIII. THE GLOBAL STAR FORMATION
HISTORIES OF 60 DWARF GALAXIES IN THE LOCAL VOLUME
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: star formation;
galaxies: stellar content; Hertzsprung-Russell and C-M diagrams
ID HUBBLE-SPACE-TELESCOPE; COLOR-MAGNITUDE DIAGRAMS;
LARGE-MAGELLANIC-CLOUD; SPHEROIDAL GALAXIES; IRREGULAR GALAXIES;
H-ALPHA; ADVANCED CAMERA; METALLICITY RELATION; INTERSTELLAR-MEDIUM;
CHEMICAL EVOLUTION
AB We present uniformly measured star formation histories (SFHs) of 60 nearby (D less than or similar to 4 Mpc) dwarf galaxies based on color-magnitude diagrams of resolved stellar populations from images taken with the Hubble Space Telescope and analyzed as part of the ACS Nearby Galaxy Survey Treasury program (ANGST). This volume-limited sample contains 12 dwarf spheroidal (dSph)/dwarf elliptical (dE), 5 dwarf spiral, 28 dwarf irregular (dI), 12 dSph/dI (transition), and 3 tidal dwarf galaxies. The sample spans a range of similar to 10 mag in MB and covers a wide range of environments, from highly interacting to truly isolated. From the best-fit SFHs, we find three significant results for dwarf galaxies in the ANGST volume: (1) the majority of dwarf galaxies formed the bulk of their mass prior to z similar to 1, regardless of current morphological type; (2) the mean SFHs of dIs, transition dwarf galaxies (dTrans), and dSphs are similar over most of cosmic time, and only begin to diverge a few Gyr ago, with the clearest differences between the three appearing during the most recent 1 Gyr; and (3) the SFHs are complex and the mean values are inconsistent with simple SFH models, e. g., single bursts, constant star formation rates (SFRs), or smooth, exponentially declining SFRs. The mean SFHs show clear divergence from the cosmic SFH at z less than or similar to 0.7, which could be evidence that low-mass systems have experienced delayed star formation relative to more massive galaxies. The sample shows a strong density-morphology relationship, such that the dSphs in the sample are less isolated than the dIs. We find that the transition from a gas-rich to gas-poor galaxy cannot be solely due to internal mechanisms such as stellar feedback, and instead is likely the result of external mechanisms, e. g., ram pressure and tidal stripping and tidal forces. In terms of their environments, SFHs, and gas fractions, the majority of the dTrans appear to be low-mass dIs that simply lack Ha emission, similar to Local Group (LG) dTrans DDO 210. However, a handful of dTrans have remarkably low gas fractions, suggesting that they have nearly exhausted their gas supply, analogous to LG dTrans such as Phoenix. Finally, we have also included extensive exploration of uncertainties in the SFH recovery method, including the optimization of time resolution, the effects of photometric depth, and impact of systematic uncertainties due to the limitations in current stellar evolution models.
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.
[Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85756 USA.
[Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 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; jd@astro.washington.edu;
ben@astro.washington.edu; kgilbert@astro.washington.edu;
skillman@astro.umn.edu; aseth@cfa.harvard.edu; adolphin@raytheon.com;
kmcquinn@astro.umn.edu; stephanie@astro.washington.edu; holtz@nmsu.edu;
krosema@astro.washington.edu; andrew.cole@utas.edu.au; ikar@luna.sao.ru;
dzaritsky@as.arizona.edu
OI Cole, Andrew/0000-0003-0303-3855; Gogarten,
Stephanie/0000-0002-7231-9745; Weisz, Daniel/0000-0002-6442-6030
NR 126
TC 155
Z9 155
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2011
VL 739
IS 1
AR 5
DI 10.1088/0004-637X/739/1/5
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700005
ER
PT J
AU Zhu, M
Davis, CJ
Wu, YF
Whitney, BA
Robitaille, T
Peng, R
AF Zhu, Ming
Davis, C. J.
Wu, Yufang
Whitney, B. A.
Robitaille, T.
Peng, R.
TI A MASSIVE PROTOSTAR EMBEDDED IN THE SCUBA CORE JCMT 18354-0649S
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: ISM; infrared: stars; stars: formation
ID YOUNG STELLAR OBJECTS; H-II REGIONS; SPECTRAL ENERGY-DISTRIBUTIONS;
COLLIMATED MOLECULAR JETS; ULTRACOMPACT HII-REGIONS; ARRAY CAMERA IRAC;
STAR-FORMATION; PHYSICAL CONDITIONS; DENSITY STRUCTURE; IMAGING SURVEY
AB We report the discovery of an extremely red object embedded in the massive SCUBA core JCMT 18354-0649S. This object is not associated with any known radio or far-IR source, though it appears in Spitzer IRAC data obtained as part of the GLIMPSE survey. At shorter wavelengths, this embedded source exhibits an extreme color, K - L' = 6.7. At an assumed distance of 5.7 kpc, this source has a near-IR luminosity of similar to 1000 L-circle dot. Its spectral energy distribution (SED) rises sharply from 2.1 mu m to 8 mu m, similar to that of a Class 0 young stellar object. Theoretical modeling of the SED indicates that the central star has a mass of 6-12 M-circle dot, with an optical extinction of more than 30. As both inflow and outflow motions are present in JCMT 18354-0649S, we suggest that this deeply embedded source is (1) a massive protostar in the early stages of accretion, and (2) the driving source of a massive molecular outflow evident in HCN J = 3-2 profiles observed toward this region.
C1 [Zhu, Ming] Natl Astron Observ China, Beijing, Peoples R China.
[Davis, C. J.] Joint Astron Ctr, Hilo, HI 96720 USA.
[Wu, Yufang] Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
[Whitney, B. A.] Space Sci Inst, Boulder, CO 80301 USA.
[Robitaille, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Peng, R.] Caltech Submillimeter Observ, Hilo, HI 96720 USA.
RP Zhu, M (reprint author), Natl Astron Observ China, 20A Datun Rd, Beijing, Peoples R China.
EM mz@nao.cac.cn
OI Robitaille, Thomas/0000-0002-8642-1329
FU NSFC [Y011231001, 10733030, 10873019]; Chinese Academy of Sciences; NSF
[AST-0540882]; NASA
FX M.Z. acknowledges the support from NSFC grant Y011231001 and also from
the "Hundred-talent program" of the Chinese Academy of Sciences. Y. Wu
is grateful for the support of grants 10733030 and 10873019 of NSFC. The
United Kingdom Infrared Telescope is operated by the Joint Astronomy
Centre (JAC) on behalf of the U. K. Science and Technology Facilities
Council (STFC). The H-, K-, and L '-band imaging reported here were
obtained as part of the UKIRT Service Programme. We thank Dr. Watson
Varricatt at the JAC for help with near-IR photometry. The JCMT is also
operated by the Joint Astronomy Centre on behalf of the U. K. STFC, the
National Research Council Canada, and the Netherlands Organisation for
Scientific Research. Caltech Submillimeter Observatory is supported
through NSF grant AST-0540882. This work is based in part on
observations made with the Spitzer Space Telescope, which is operated by
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA. Support for this work was provided by NASA through
an award issued by JPL/Caltech for the GLIMPSE360 project (B. W.). We
thank the GLIMPSE team (PI: E. Churchwell) for making the IRAC images
available on the internet. We also thank the anonymous referee whose
comments helped improve the paper.
NR 69
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
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 20
PY 2011
VL 739
IS 1
AR 53
DI 10.1088/0004-637X/739/1/53
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DS
UT WOS:000294955700053
ER
PT J
AU Brogan, CL
Hunter, TR
Cyganowski, CJ
Friesen, RK
Chandler, CJ
Indebetouw, R
AF Brogan, C. L.
Hunter, T. R.
Cyganowski, C. J.
Friesen, R. K.
Chandler, C. J.
Indebetouw, R.
TI FIRST RESULTS FROM A 1.3 cm EXPANDED VERY LARGE ARRAY SURVEY OF MASSIVE
PROTOSTELLAR OBJECTS: G35.03+0.35
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual objects (G35.03+0.35); stars: formation; stars: massive;
techniques: interferometric
ID H-II REGIONS; GLIMPSE SURVEY; STAR-FORMATION; DENSE CORES; MASERS;
AMMONIA; NH3; THERMOMETER; OUTFLOW; CATALOG
AB We have performed a 1.3 cm survey of 24 massive young stellar objects (MYSOs) using the Expanded Very Large Array. The sources in the sample exhibit a broad range of massive star formation signposts including infrared dark clouds (IRDCs), ultra-compact H II (UC H II) regions, and extended 4.5 mu m emission in the form of extended green objects (EGOs). In this work, we present results for G35.03+0.35 which exhibits all of these phenomena. We simultaneously image the 1.3 cm NH3 (1,1) through (6,6) inversion lines, four CH3OH transitions, two H recombination lines, plus continuum at 0.05 pc resolution. We find three areas of thermal NH3 emission, two within the EGO (designated as the NE and SW cores) and one toward an adjacent IRDC. The NE core contains a UC H II region (CM1) and a candidate hyper-compact H II region (CM2). A region of non-thermal, likely masing NH3 (3,3) and (6,6) emission is coincident with an arc of 44 GHz CH3OH masers. We also detect two new 25 GHz Class-I CH3OH masers. A complementary Submillimeter Array 1.3 mm continuum image shows that the distribution of dust emission is similar to the lower-lying NH3 lines, all peaking to the NW of CM2, indicating the likely presence of an additional MYSO in this protocluster. By modeling the NH3 and 1.3 mm continuum data, we obtain gas temperatures of 20-220 K and masses of 20-130 M-circle dot. The diversity of continuum emission properties and gas temperatures suggests that objects in a range of evolutionary states exist concurrently in this protocluster.
C1 [Brogan, C. L.; Hunter, T. R.; Friesen, R. K.; Indebetouw, R.] NRAO, Charlottesville, VA 22903 USA.
[Cyganowski, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chandler, C. J.] NRAO, Socorro, NM 87801 USA.
[Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
RP Brogan, CL (reprint author), NRAO, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
EM cbrogan@nrao.edu
OI Hunter, Todd/0000-0001-6492-0090
NR 28
TC 15
Z9 15
U1 0
U2 6
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 SEP 20
PY 2011
VL 739
IS 1
AR L16
DI 10.1088/2041-8205/739/1/L16
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900016
ER
EF