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. NR 105 TC 67 Z9 67 U1 5 U2 27 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 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. NR 33 TC 7 Z9 7 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 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. NR 40 TC 33 Z9 35 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 204 DI 10.1088/0004-637X/743/2/204 PG 6 WC Astronomy & Astrophysics 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. NR 48 TC 8 Z9 8 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 DEC 20 PY 2011 VL 743 IS 2 AR 141 DI 10.1088/0004-637X/743/2/141 PG 9 WC Astronomy & Astrophysics 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. NR 79 TC 80 Z9 80 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2011 VL 743 IS 2 AR 114 DI 10.1088/0004-637X/743/2/114 PG 19 WC Astronomy & Astrophysics 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 TC 30 Z9 30 U1 0 U2 9 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 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 TC 8 Z9 8 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 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 TC 11 Z9 11 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 81 Z9 81 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 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 TC 31 Z9 31 U1 0 U2 9 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 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 TC 31 Z9 31 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 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 TC 2 Z9 2 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 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 TC 98 Z9 98 U1 0 U2 20 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 TC 15 Z9 15 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 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 TC 25 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 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 TC 56 Z9 56 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 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 TC 40 Z9 40 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 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 TC 13 Z9 13 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 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 TC 16 Z9 16 U1 0 U2 11 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 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 TC 1 Z9 1 U1 0 U2 9 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 TC 6 Z9 6 U1 0 U2 3 PU BAILEY-MATTHEWS SHELL MUSEUM 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. NR 26 TC 6 Z9 6 U1 2 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD 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. NR 25 TC 78 Z9 78 U1 8 U2 42 PU ELSEVIER SCIENCE INC 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 TC 7 Z9 8 U1 0 U2 5 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. NR 63 TC 18 Z9 18 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 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 TC 101 Z9 101 U1 1 U2 12 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 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 TC 9 Z9 9 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 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 TC 18 Z9 18 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 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 TC 22 Z9 22 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 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 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 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 TC 6 Z9 6 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 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. NR 72 TC 354 Z9 354 U1 6 U2 22 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 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. NR 71 TC 23 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 10 PY 2011 VL 743 IS 1 AR 15 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 TC 20 Z9 20 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 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 TC 17 Z9 17 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 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. NR 49 TC 25 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 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 TC 16 Z9 16 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 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. NR 42 TC 38 Z9 39 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 DEC 10 PY 2011 VL 743 IS 1 AR 90 DI 10.1088/0004-637X/743/1/90 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300090 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. NR 80 TC 66 Z9 66 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 6 DI 10.1088/0004-637X/743/1/6 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 853EF UT WOS:000297408300006 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). NR 47 TC 65 Z9 65 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 2 DI 10.1088/0004-637X/743/1/2 PG 10 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 Z9 28 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. 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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. 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[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. 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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, Emmanuel/B-5959-2017; Cortina, Juan/C-2783-2017; Graciani Diaz, Ricardo/I-5152-2016; Tosti, Gino/E-9976-2013; 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Tjus, Julia/G-8145-2012; Rando, Riccardo/M-7179-2013; Fontaine, Gerard/D-6420-2014; Todero Peixoto, Carlos Jose/G-3873-2012; Rico, Javier/K-8004-2014; Martinez Botella, Gustavo/K-8834-2014; Fernandez, Ester/K-9734-2014; GAug, Markus/L-2340-2014; Marin, Jesus/K-6991-2014; Moralejo Olaizola, Abelardo/M-2916-2014; Tejedor, Luis/N-5494-2014; Berdugo, Javier/A-2858-2015; Ribo, Marc/B-3579-2015; Funk, Stefan/B-7629-2015; Katarzynski, Krzysztof/G-4528-2014; Antoranz, Pedro/H-5095-2015; Delgado, Carlos/K-7587-2014; Miranda, Jose Miguel/F-2913-2013; Stamatescu, Victor/C-9945-2016; Gascon, David/L-8464-2014; Font, Lluis/L-4197-2014; delagnes, eric/G-8782-2011; Sarkar, Subir/G-5978-2011; Takahashi, Keitaro/L-5930-2015; Contreras Gonzalez, Jose Luis/K-7255-2014; de Gouveia Dal Pino, Elisabete/H-9560-2013; Moura Santos, Edivaldo/K-5313-2016; Bissaldi, Elisabetta/K-7911-2016; Temnikov, Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Torres, Diego/O-9422-2016; Sao Carlos Institute of Physics, IFSC/USP/M-2664-2016; Dimitrov, Dinko/J-7682-2013; Drury, Luke/B-1916-2017; Reimer, Olaf/A-3117-2013; Terada, Yukikatsu/A-5879-2013; Botner, Olga/A-9110-2013; Hallgren, Allan/A-8963-2013; Braun, Isabel/C-9373-2012; Hardcastle, Martin/E-2264-2012; Kokkotas, Kostas/B-7878-2010; de souza, Vitor/D-1381-2012; Shellard, Ronald/G-4825-2012; Ghag, Chamkaur/H-2869-2012; Doro, Michele/F-9458-2012; Kowal, Grzegorz/K-5667-2012; van Eldik, Christopher/C-3901-2013 OI Bonanno, Giovanni/0000-0002-4792-3983; Billotta, Sergio/0000-0001-6557-8768; Catalano, Osvaldo/0000-0002-9554-4128; Maccarone, Maria Concetta/0000-0001-8722-0361; GIARRUSSO, SALVATORE/0000-0002-0738-2940; Chadwick, Paula/0000-0002-1468-2685; Molinari, Emilio/0000-0002-1742-7735; Kneiske, Tanja M./0000-0002-3210-6200; La Rosa, Giovanni/0000-0002-3931-2269; Asorey, Hernan/0000-0002-4559-8785; Mineo, Teresa/0000-0002-4931-8445; LA BARBERA, ANTONINO/0000-0002-5880-8913; La Parola, Valentina/0000-0002-8087-6488; Daniel, Michael/0000-0002-8053-7910; Komin, Nukri/0000-0003-3280-0582; De Lotto, Barbara/0000-0003-3624-4480; Bais, Alkiviadis/0000-0003-3899-2001; Di Pierro, Federico/0000-0003-4861-432X; Rando, Riccardo/0000-0001-6992-818X; Vallania, Piero/0000-0001-9089-7875; Balis, Dimitris/0000-0003-1161-7746; Persic, Massimo/0000-0003-1853-4900; Knapp, Johannes/0000-0003-1519-1383; Vercellone, Stefano/0000-0003-1163-1396; Spanier, Felix/0000-0001-6802-4744; Otte, Adam Nepomuk/0000-0002-5955-6383; Bastieri, Denis/0000-0002-6954-8862; Ribo, Marc/0000-0002-9931-4557; Mertsch, Philipp/0000-0002-2197-3421; Punch, Michael/0000-0002-4710-2165; Tavani, Marco/0000-0003-2893-1459; Garrido Beltran, Lluis/0000-0001-8883-6539; Murphy, Alexander/0000-0001-8337-4427; Giubilato, Piero/0000-0003-4358-5355; Covino, Stefano/0000-0001-9078-5507; Paredes, Josep M./0000-0002-1566-9044; Oya, Igor/0000-0002-3881-9324; de Ona Wilhelmi, Emma/0000-0002-5401-0744; Tagliaferri, Gianpiero/0000-0003-0121-0723; Garcia, Beatriz/0000-0003-0919-2734; Testa, Vincenzo/0000-0003-1033-1340; Barrio, Juan/0000-0002-0965-0259; Murase, Kohta/0000-0002-5358-5642; Moulin, Emmanuel/0000-0003-4007-0145; Cortina, Juan/0000-0003-4576-0452; Graciani Diaz, Ricardo/0000-0001-7166-5198; Golev, Valeri/0000-0002-4482-4090; Spiga, Daniele/0000-0003-1163-7843; Pareschi, Giovanni/0000-0003-3967-403X; Arnaldi, Luis Horacio/0000-0002-2370-4014; Kothandan, Divay/0000-0001-9048-7518; Cusumano, Giancarlo/0000-0002-8151-1990; Ghigo, Mauro/0000-0003-2284-9251; Green, Anne/0000-0002-7135-1671; silk, joe/0000-0002-1566-8148; Canestrari, Rodolfo/0000-0003-4591-7763; Lenain, Jean-Philippe/0000-0001-7284-9220; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022; Inoue, Yoshiyuki/0000-0002-7272-1136; Todero Peixoto, Carlos Jose/0000-0003-3669-8212; Rico, Javier/0000-0003-4137-1134; Martinez Botella, Gustavo/0000-0002-1061-8520; GAug, Markus/0000-0001-8442-7877; Marin, Jesus/0000-0002-9049-3667; Moralejo Olaizola, Abelardo/0000-0002-1344-9080; Tejedor, Luis/0000-0003-1525-9085; Berdugo, Javier/0000-0002-7911-8532; Funk, Stefan/0000-0002-2012-0080; Antoranz, Pedro/0000-0002-3015-3601; Delgado, Carlos/0000-0002-7014-4101; Miranda, Jose Miguel/0000-0002-1472-9690; Stamatescu, Victor/0000-0001-9030-7513; Gascon, David/0000-0001-9607-6154; Font, Lluis/0000-0003-2109-5961; Sarkar, Subir/0000-0002-3542-858X; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; de Gouveia Dal Pino, Elisabete/0000-0001-8058-4752; Moura Santos, Edivaldo/0000-0002-2818-8813; Bissaldi, Elisabetta/0000-0001-9935-8106; Temnikov, Petar/0000-0002-9559-3384; Torres, Diego/0000-0002-1522-9065; Drury, Luke/0000-0002-9257-2270; Reimer, Olaf/0000-0001-6953-1385; Terada, Yukikatsu/0000-0002-2359-1857; Braun, Isabel/0000-0002-9389-0502; Hardcastle, Martin/0000-0003-4223-1117; Kokkotas, Kostas/0000-0001-6048-2919; Shellard, Ronald/0000-0002-2983-1815; Doro, Michele/0000-0001-9104-3214; Kowal, Grzegorz/0000-0002-0176-9909; van Eldik, Christopher/0000-0001-9669-645X 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 TC 45 Z9 46 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 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. NR 45 TC 22 Z9 22 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD 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 TC 26 Z9 26 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 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 TC 9 Z9 9 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD 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 TC 38 Z9 38 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD 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. 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EM douglas.marshall@irap.omp.eu RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; 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; 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, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; 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; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; Melchiorri, Alessandro/0000-0001-5326-6003; 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; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; de Gasperis, Giancarlo/0000-0003-2899-2171 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. 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[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 TC 583 Z9 588 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. NR 92 TC 577 Z9 582 U1 4 U2 48 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 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 TC 14 Z9 14 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD 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 TC 58 Z9 58 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD 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 TC 29 Z9 30 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 TC 12 Z9 12 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 TC 8 Z9 9 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 TC 1 Z9 1 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 TC 30 Z9 30 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 TC 28 Z9 28 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 TC 23 Z9 24 U1 9 U2 176 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 TC 20 Z9 21 U1 3 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 TC 22 Z9 27 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. NR 87 TC 38 Z9 38 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 105 DI 10.1088/0004-637X/742/2/105 PG 30 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. NR 101 TC 65 Z9 65 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2011 VL 742 IS 2 AR 93 DI 10.1088/0004-637X/742/2/93 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 850QM 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. NR 75 TC 54 Z9 55 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 116 DI 10.1088/0004-637X/742/2/116 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 850QM 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. NR 55 TC 5 Z9 5 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 DEC 1 PY 2011 VL 742 IS 2 AR 128 DI 10.1088/0004-637X/742/2/128 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 850QM 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. NR 135 TC 52 Z9 52 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2011 VL 742 IS 2 AR 89 DI 10.1088/0004-637X/742/2/89 PG 20 WC Astronomy & Astrophysics 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. NR 22 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2011 VL 742 IS 2 AR 118 DI 10.1088/0004-637X/742/2/118 PG 7 WC Astronomy & Astrophysics 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 TC 105 Z9 105 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 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. NR 108 TC 54 Z9 55 U1 0 U2 2 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 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. NR 122 TC 150 Z9 150 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD 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. NR 67 TC 19 Z9 19 U1 2 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 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 TC 100 Z9 100 U1 8 U2 14 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 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 TC 80 Z9 81 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 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. NR 73 TC 103 Z9 103 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD 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. NR 64 TC 69 Z9 69 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 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 TC 6 Z9 6 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 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 TC 11 Z9 11 U1 0 U2 9 PU SPRINGER 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 TC 15 Z9 15 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. NR 71 TC 11 Z9 11 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 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. NR 65 TC 34 Z9 34 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 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 TC 30 Z9 30 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 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. NR 48 TC 42 Z9 42 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 65 Z9 65 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2011 VL 742 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 TC 31 Z9 31 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 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 TC 241 Z9 242 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 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 TC 24 Z9 24 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 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 TC 94 Z9 95 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 25 Z9 25 U1 0 U2 8 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 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 TC 12 Z9 12 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. NR 42 TC 217 Z9 220 U1 53 U2 397 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 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. NR 29 TC 110 Z9 118 U1 18 U2 116 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 TC 3 Z9 3 U1 1 U2 10 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 Z9 57 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. NR 57 TC 34 Z9 34 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2011 VL 741 IS 2 AR 111 DI 10.1088/0004-637X/741/2/111 PG 18 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. NR 63 TC 61 Z9 61 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 NOV 10 PY 2011 VL 741 IS 2 AR 91 DI 10.1088/0004-637X/741/2/91 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. NR 47 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 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. NR 137 TC 118 Z9 118 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 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. NR 92 TC 64 Z9 64 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 NOV 10 PY 2011 VL 741 IS 2 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 NR 3 TC 4 Z9 4 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 NOV 10 PY 2011 VL 741 IS 2 AR 127 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. NR 79 TC 44 Z9 44 U1 0 U2 10 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 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. NR 53 TC 39 Z9 39 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 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. NR 37 TC 5 Z9 5 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 114 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. NR 66 TC 146 Z9 146 U1 0 U2 9 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 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 TC 31 Z9 31 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 25 Z9 25 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 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 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 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. NR 37 TC 13 Z9 13 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 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. NR 126 TC 50 Z9 51 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 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. NR 81 TC 44 Z9 44 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD 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 TC 16 Z9 17 U1 7 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 TC 4 Z9 5 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD 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 TC 49 Z9 49 U1 0 U2 5 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 TC 52 Z9 52 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 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. NR 53 TC 37 Z9 38 U1 10 U2 81 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 TC 14 Z9 14 U1 2 U2 23 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD NOV PY 2011 VL 113 IS 4 BP 806 EP 816 DI 10.1525/cond.2011.100226 PG 11 WC Ornithology SC Zoology GA 862YJ UT WOS:000298129700011 ER PT J AU Tonra, CM Marra, PP Holberton, RL AF Tonra, Christopher M. Marra, Peter P. Holberton, Rebecca L. TI Migration phenology and winter habitat quality are related to circulating androgen in a long-distance migratory bird SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID WHITE-CROWNED SPARROWS; NON-BREEDING SEASON; EXPERIMENTALLY ELEVATED TESTOSTERONE; STONECHATS SAXICOLA-TORQUATA; RUFOUS-COLLARED SPARROWS; AVIAN LIFE HISTORIES; DARK-EYED JUNCOS; ZONOTRICHIA-CAPENSIS; SETOPHAGA-RUTICILLA; BODY CONDITION AB In migratory birds, the timing of departure from wintering grounds is often dependant on the quality of habitat on an individual's territory and may influence individual fitness, resulting in an interaction of life history stages across large geographical distances. American redstart Setophaga ruticilla males who overwinter in high quality habitats arrive early to breed and subsequently produce more offspring than late arrivers. Since many migratory species overlap vernal migration with the physiological transition to breeding, we examined if breeding preparation plays a role in this seasonal interaction. We tested the hypothesis that early arriving male redstarts from high quality winter habitats are in superior breeding condition by simultaneously measuring winter habitat quality (stable-carbon isotopes) and breeding preparation (circulating androgen, cloacal protuberance (CP) diameter) upon arrival at breeding grounds. Compared with late arrivers, early arriving males were from higher quality winter habitats and had higher androgen, but smaller CPs. Males arriving with higher androgen were in more advanced physiological migratory condition, as measured by haematocrit. Early arrivers were more likely to successfully breed, but there was no significant relationship between androgen upon arrival and breeding success. One possible explanation for these relationships is that androgen measured during arrival is most relevant in a migratory context, such that birds with high androgen may benefit from effects on migratory condition, positively influencing fitness through earlier arrival. C1 [Tonra, Christopher M.; Holberton, Rebecca L.] Univ Maine, Lab Avian Biol, Sch Biol & Ecol, Orono, ME 04469 USA. [Tonra, Christopher M.; Marra, Peter P.; Holberton, Rebecca L.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. RP Tonra, CM (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. EM tonrac@si.edu RI Tonra, Christopher/B-1620-2013 FU National Science Foundation [0649679, 0615701]; American Ornithologist Union; American Museum of Natural History; Cooper Ornithological Society FX This research was funded by grants awarded to PPM (0649679) and RLH (0615701) from the National Science Foundation and to CMT from the American Ornithologist Union Student Research Award, the American Museum of Natural History Frank M. Chapman Award, and the Cooper Ornithological Society Joseph Grinnell Student Research Award. We are grateful to Cord Dorcey, Doug Perez, Stephanie Sult, and especially Mark Thomas for assistance in the field and Nora Diggs, Greg Henkes, and Kayla Porcelli for assistance in the laboratory. For logistical support at our field site and frequent discussions of the phenomena addressed in this study we thank Dick Holmes, Sara Kaiser, Nick Rodenhouse, Scott Sillett, and the Hubbard Brook Research Foundation. We thank Bill Glanz, Matt Reudink, Colin Studds, members of the UMaine Lab of Avian Biology reading group for comments on an earlier draft of this manuscript. Our research was approved by the Univ. of Maine Inst. Animal Care and Use Committee (protocol A2006-07-04) and was in compliance with United States law. NR 69 TC 22 Z9 23 U1 1 U2 43 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD NOV PY 2011 VL 42 IS 5 BP 397 EP 404 DI 10.1111/j.1600-048X.2011.05333.x PG 8 WC Ornithology SC Zoology GA 854PE UT WOS:000297505900003 ER PT J AU Braje, TJ Rick, TC Erlandson, JM Anderson, M DeLong, RL AF Braje, Todd J. Rick, Torben C. Erlandson, Jon M. Anderson, Megan DeLong, Robert L. TI Conflicts in natural and cultural resource management: Archaeological site disturbances by seals and sea lions on California's Northern Channel Islands SO JOURNAL OF FIELD ARCHAEOLOGY LA English DT Article DE seals; sea lions; coastal erosion; archaeological conservation; Channel Islands ID SAN-MIGUEL ISLAND; AQUATIC ADAPTATIONS; SOUTH-AFRICA; EROSION; COAST; SETTLEMENT; PACIFIC; AMERICA AB California's Channel Islands currently have around 150,000 breeding seals and sea lions (pinnipeds). Driven to near extinction by 20th-century exploitation, many pinniped populations have recovered dramatically under federal and state management and continue to expand in number and distribution. Some of these pinniped populations are damaging or destroying coastal archaeological sites as they establish new breeding and haul-out areas-places occupied between periods of foraging activity-on upland landforms. We use archaeological excavations from a prehistoric village on San Miguel Island to illustrate the adverse effects pinnipeds can have on archaeological sites. Estimates based on excavations at Otter Point suggest that in one year nearly 10,000 kg of shellfish remains, 840,000 animal bones, and 1700 formal artifacts were lost to erosion caused by the activities of seals and sea lions. Our study documents potential conflicts between natural and cultural resource management suggesting the need for collaborative efforts between archaeologists and biologists to balance the conservation of both resources. C1 [Braje, Todd J.] San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Anderson, Megan] Humboldt State Univ, Arcata, CA 95521 USA. [DeLong, Robert L.] NOAA, Natl Marine Mammal Lab, Alaska Fisheries Sci Ctr, Calif Current Ecosyst Program, Seattle, WA USA. RP Braje, TJ (reprint author), San Diego State Univ, Dept Anthropol, 5500 Campanile Dr, San Diego, CA 92182 USA. EM tbraje@mail.sdsu.edu OI Erlandson, Jon/0000-0002-4705-4319 NR 55 TC 2 Z9 2 U1 1 U2 12 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0093-4690 J9 J FIELD ARCHAEOL JI J. Field Archaeol. PD NOV PY 2011 VL 36 IS 4 BP 312 EP 321 DI 10.1179/009346911X13200731373863 PG 10 WC Archaeology SC Archaeology GA 863DX UT WOS:000298144100005 ER PT J AU Chambouvet, A Laabir, M Sengco, M Vaquer, A Guillou, L AF Chambouvet, Aurelie Laabir, Mohamed Sengco, Mario Vaquer, Andre Guillou, Laure TI Genetic diversity of Amoebophryidae (Syndiniales) during Alexandrium catenella/tamarense (Dinophyceae) blooms in the Thau lagoon (Mediterranean Sea, France) SO RESEARCH IN MICROBIOLOGY LA English DT Article DE Dinoflagellate; Parasite; Invasive species ID TAMARENSE COMPLEX DINOPHYCEAE; HOST-SPECIFICITY; CHESAPEAKE BAY; CATENELLA; POPULATIONS; PARASITISM; SEQUENCES; PACIFIC AB During toxic spring and fall blooms produced by the dinoflagellate Alexandrium in the Thau lagoon (Mediterranean Sea), we monitored the presence of Amoebophryidae (Syndiniales), a group of parasites virulent toward a wide range of dinoflagellate hosts. A PCR-biased approach unveiled the presence of at least 10 different parasitic groups during Alexandrium proliferation. However, fluorescent in situ hybridization failed to reveal parasitic infection inside Alexandrium cells in field populations. In contrast, several co-occurring, less abundant thecate dinofiagellate species were infected by Amoebophryidae, showing up to 10% of infected cells. We concluded that Alexandrium populations were not infected by these local parasites, at least during our survey. In order to check this resistance capacity on a more global scale, we cross-infected several Alexandrium strains isolated from the Thau lagoon with one strain of the parasite Amoebophrya sp. originating from Salt Pond, MA, USA. All of these hosts were strongly infected by the North American parasite, leading to the conclusion that blooming Alexandrium in the Thau lagoon were not particularly resistant to this kind of parasite. These results provide additional evidence that dinofiagellates may become invasive when they successfully escaped their natural enemies in time and/or space (the "enemy release" hypothesis). (C) 2011 Institut Pasteur. Published by Elsevier Masson SAS. All rights reserved. C1 [Chambouvet, Aurelie; Guillou, Laure] Univ Paris 06, CNRS, UMR 7144, Biol Stn, F-29680 Roscoff, France. [Laabir, Mohamed; Vaquer, Andre] CNRS, UM2 Ecosyst Lagunaires, UMR 5119, F-34095 Montpellier 05, France. [Sengco, Mario] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Guillou, L (reprint author), Univ Paris 06, CNRS, UMR 7144, Biol Stn, Pl G Teissier, F-29680 Roscoff, France. EM a.chambouvet@gmail.com; Mohamed.Laabir@univ-montp2.fr; mario.sengco@gmail.com; Andre.Vaquer@univ-montp2.fr; lguillou@sb-roscoff.fr FU French programs EC2CO; ANR AQUAPARADOX FX We are grateful to Annie Pastoureaud (Ifremer, Sete) for her help during sampling and for use of her cruise facilities. We also thank Anne-Laure Sauvadet for her help in phylogenetic analysis and we are indebted to Morgan Perennou from Ouest-Genopole for sequencing operations. This work was supported by the French programs EC2CO (2006-2008) and the ANR AQUAPARADOX. NR 32 TC 13 Z9 14 U1 1 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0923-2508 J9 RES MICROBIOL JI Res. Microbiol. PD NOV PY 2011 VL 162 IS 9 SI SI BP 959 EP 968 DI 10.1016/j.resmic.2011.03.002 PG 10 WC Microbiology SC Microbiology GA 862VB UT WOS:000298121100017 PM 21392576 ER PT J AU Neufeld, MJ AF Neufeld, Michael J. TI Falling to Earth: An Apollo 15 Astronaut's Journey SO SPACE POLICY LA English DT Book Review C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. EM NeufeldM@si.edu NR 1 TC 0 Z9 0 U1 1 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 J9 SPACE POLICY JI Space Policy PD NOV PY 2011 VL 27 IS 4 BP 253 EP 254 DI 10.1016/j.spacepol.2011.09.003 PG 2 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 867PC UT WOS:000298465300012 ER PT J AU Dow, TL Holaskova, I Brown, JL AF Dow, T. L. Holaskova, I. Brown, J. L. TI Results of the third reproductive assessment survey of north American Asian (Elephas maximus) and African (Loxodonta africana) female elephants SO ZOO BIOLOGY LA English DT Article DE ovarian cyclicity; hormones; reproduction; acyclicity; ultrasound; progestagens ID OVARIAN ACTIVITY; MANAGEMENT; BEHAVIOR; POPULATION; HORMONE; TOOL AB A written survey assessed reproductive status of female Asian and African elephants in AZA/SSP facilities in 2008, and data were compared to surveys conducted in 2002 and 2005. Results showed that ovarian acyclicity rates across the surveys remained unchanged for Asian (13.3, 10.9 and 11.1%) and African (22.1, 31.2 and 30.5%) elephants, respectively (P>0.05), but were higher overall for African compared to Asian elephants (P<0.05). In 2008, the percentages of Asian and African elephants with irregular cycles (14.3 and 15.8%) and irregular + no cycles (25.4 and 46.4%) was similar to 2005 (7.6 and 11.8%; 18.5 and 43.0%), but were increased compared to 2002 (2.6 and 5.2%; 16.0 and 27.3%), respectively (P<0.05). For both species, ovarian acyclicity increased with age (P<0.05). Reproductive tract pathologies did not account for the majority of acyclicity, although rates were higher in noncycling females (P<0.05). Bull presence was associated with increased cyclicity rates (P<0.05) for Asian (92.5 vs. 58.3%) and African (64.9 vs. 57.8%) elephants compared to females at facilities with no male, respectively. Cyclicity rates were higher for Asian (86.8 vs. 65.2%) and African (67.9 vs. 56.7%) elephants managed in free compared to protected contact programs (P<0.05), respectively. Geographical facility location had no effect on cyclicity (P>0.05). In summary, incidence of ovarian cycle problems continues to predominantly affect African elephants. Although percentages of acyclicity did not increase between 2005 and 2008, 42.2% Asian and 30.2% African females were no longer being hormonally monitored; thus, reproductive cycle abnormalities could be worse than current data suggest. Zoo Biol 30:699711, 2011. (c) 2011 Wiley Periodicals, Inc. C1 [Dow, T. L.; Brown, J. L.] Smithsonian Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. [Dow, T. L.; Holaskova, I.] W Virginia Univ, Dept Anim & Nutr Sci, Morgantown, WV 26506 USA. RP Brown, JL (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM brownjan@si.edu NR 34 TC 14 Z9 14 U1 3 U2 16 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD NOV-DEC PY 2011 VL 30 IS 6 BP 699 EP 711 DI 10.1002/zoo.20377 PG 13 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 864PZ UT WOS:000298253500010 PM 21319213 ER PT J AU Forget, PM Jordano, P Lambert, JE Bohning-Gaese, K Traveset, A Wright, SJ AF Forget, Pierre-Michel Jordano, Pedro Lambert, Joanna E. Boehning-Gaese, Katrin Traveset, Anna Joseph Wright, S. TI Frugivores and seed dispersal (1985-2010); the 'seeds' dispersed, established and matured SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY LA English DT Editorial Material ID TROPICAL FORESTS; ECOSYSTEM SERVICES; CONSEQUENCES; REGENERATION; BIRDS; CONSERVATION; RECRUITMENT; MECHANISMS; ANIMALS; AFRICA C1 [Forget, Pierre-Michel] Museum Natl Hist Nat, UMR 7179, F-91800 Brunoy, France. [Jordano, Pedro] Estn Biol Donana EBD CSIC, Integrat Ecol Grp, E-41092 Seville, Spain. [Lambert, Joanna E.] Univ Texas San Antonio, Dept Ecol Anthropol, San Antonio, TX 78249 USA. [Boehning-Gaese, Katrin] Goethe Univ, Dept Biol Sci, D-60323 Frankfurt, Germany. [Boehning-Gaese, Katrin] Biodivers & Climate Res Ctr BiK F, D-60325 Frankfurt, Germany. [Traveset, Anna] Inst Mediterrani Estudis Avancats CSIC UIB, Esporles Mallorca 07190, Illes Balears, Spain. [Joseph Wright, S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Forget, PM (reprint author), Museum Natl Hist Nat, UMR 7179, 1 Ave Petit Chateau, F-91800 Brunoy, France. EM pmf@mnhn.fr RI Biodiversity & Climate Res Ctr, BiK-F/C-4266-2012; Forget, Pierre-Michel/B-4355-2009; Jordano, Pedro/A-5162-2008; Jordano, Pedro/B-6678-2014; Wright, Stuart/M-3311-2013; CSIC, EBD Donana/C-4157-2011 OI Forget, Pierre-Michel/0000-0002-9252-974X; Jordano, Pedro/0000-0003-2142-9116; Jordano, Pedro/0000-0003-2142-9116; Wright, Stuart/0000-0003-4260-5676; CSIC, EBD Donana/0000-0003-4318-6602 NR 74 TC 12 Z9 12 U1 3 U2 34 PU GAUTHIER-VILLARS/EDITIONS ELSEVIER PI PARIS PA 23 RUE LINOIS, 75015 PARIS, FRANCE SN 1146-609X EI 1873-6238 J9 ACTA OECOL JI Acta Oecol.-Int. J. Ecol. PD NOV-DEC PY 2011 VL 37 IS 6 SI SI BP 517 EP 520 DI 10.1016/j.actao.2011.09.008 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 860NU UT WOS:000297955800001 ER PT J AU Fleming, TH Kress, WJ AF Fleming, Theodore H. Kress, W. John TI A brief history of fruits and frugivores SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY LA English DT Article DE Coevolution; Fruits; Frugivores; Phylogenies ID FLOWERING PLANTS; FLESHY FRUITS; SEED SIZE; DISPERSAL; DIVERSITY; EVOLUTION; ANGIOSPERMS; PHYLOGENY; SEQUENCES; BATS AB In this paper we briefly review the evolutionary history of the mutualistic interaction between angiosperms that produce fleshy fruits and their major consumers: frugivorous birds and mammals. Fleshy fruits eaten by these vertebrates are widely distributed throughout angiosperm phylogeny. Similarly, a frugivorous diet has evolved independently many times in birds and mammals. Bird dispersal is more common than mammal-dispersal in all lineages of angiosperms, and we suggest that the evolution of bird fruits may have facilitated the evolution of frugivory in primates. The diets of fruit-eating bats overlap less with those of other kinds of frugivorous vertebrates. With a few exceptions, most families producing vertebrate-dispersed fruit appeared substantially earlier in earth history than families of their vertebrate consumers. It is likely that major radiations of these plants and animals have occurred in the past 30 Ma, in part driven by geological changes and also by the foraging behavior of frugivores in topographically complex landscapes. Overall, this mutualistic interaction has had many evolutionary and ecological consequences for tropical plants and animals for most of the Cenozoic Era. Loss of frugivores and their dispersal services will have a strong negative impact on the ecological and evolutionary dynamics of tropical and subtropical communities. (C) 2011 Elsevier Masson SAS. All rights reserved. C1 [Fleming, Theodore H.] Univ Miami, Tucson, AZ USA. [Fleming, Theodore H.] Univ Arizona, Tucson, AZ USA. [Kress, W. John] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. RP Fleming, TH (reprint author), 6211 N Camino Corozal, Tucson, AZ 85704 USA. EM tedfleming@dakotacom.net NR 53 TC 42 Z9 45 U1 11 U2 103 PU GAUTHIER-VILLARS/EDITIONS ELSEVIER PI PARIS PA 23 RUE LINOIS, 75015 PARIS, FRANCE SN 1146-609X J9 ACTA OECOL JI Acta Oecol.-Int. J. Ecol. PD NOV-DEC PY 2011 VL 37 IS 6 SI SI BP 521 EP 530 DI 10.1016/j.actao.2011.01.016 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 860NU UT WOS:000297955800002 ER PT J AU Kays, R Jansen, PA Knecht, EMH Vohwinkel, R Wikelski, M AF Kays, Roland Jansen, Patrick A. Knecht, Elise M. H. Vohwinkel, Reinhard Wikelski, Martin TI The effect of feeding time on dispersal of Virola seeds by toucans determined from GPS tracking and accelerometers SO ACTA OECOLOGICA-INTERNATIONAL JOURNAL OF ECOLOGY LA English DT Article DE Seed dispersal kernel; Regurgitation time; GPS tracking; Accelerometer; Tropical forests ID SPATIAL-PATTERNS; ANIMAL MOVEMENT; FOREST; ECOLOGY; MODELS; PANAMA; BIRDS; WILD; FRUGIVORE; BEHAVIOR AB Seed dispersal is critical to understanding forest dynamics but is hard to study because tracking seeds is difficult. Even for the best-studied dispersal system of the Neotropics, Virola nobilis, the dispersal kernel remains unknown. We combined high-resolution GPS/3D-acceleration bird tracking, seed-retention experiments, and field observations to quantify dispersal of V. nobilis by their principal dispersers, Ramphastos toucans. We inferred feeding events from movement data, and then estimated spatio-temporally explicit seed-dispersal kernels. Wild toucans moved an average of 1.8 km d(-1) with two distinct activity peaks. Seed retention time in captive toucans averaged 25.5 min (range 4-98 min). Estimated seed dispersal distance averaged 144 +/- 147 m, with a 56% likelihood of dispersal >100 m, two times further than the behaviour-naive estimate from the same data. Dispersal was furthest for seeds ingested in the morning, and increased with seed retention time, but only up to 60 min after feeding. Our study supports the long-standing hypothesis that toucans are excellent dispersers of Virola seeds. To maximize seed dispersal distances trees should ripen fruit in the morning when birds move the most, and produce fruits with gut-processing times around 60 min. Our study demonstrates how new tracking technology can yield nuanced seed dispersal kernels for animals that cannot be directly observed. (C) 2011 Elsevier Masson SAS. All rights reserved. C1 [Kays, Roland] New York State Museum & Sci Serv, Albany, NY USA. [Kays, Roland; Jansen, Patrick A.; Wikelski, Martin] Smithsonian Trop Res Inst, Balboa, Panama. [Jansen, Patrick A.; Knecht, Elise M. H.] Wageningen Univ, Ctr Ecosyst Studies, Wageningen, Netherlands. [Jansen, Patrick A.] Univ Groningen, Ctr Ecol & Evolutionary Studies, Haren, Netherlands. [Vohwinkel, Reinhard] Avifaunist Untersuchungen, D-42553 Velbert, Nordrhein Westf, Germany. [Wikelski, Martin] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell Am Bodensee, Germany. [Wikelski, Martin] Univ Konstanz, Chair Ornithol, D-78457 Constance, Germany. RP Kays, R (reprint author), New York State Museum & Sci Serv, 3140 CEC, Albany, NY USA. EM rkays@mail.nysed.gov RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU Netherlands Organisation for Scientific Research [W84-584, 863-07-008]; National Science Foundation [NSF-DEB 0717071]; Max Planck Institute for Ornithology FX We thank Renee Seidler, Lars Sluiter, Niels Rattenborg, Christian Ziegler, and Bryson Voirin for their assistance in the field, Halit Khoshen from Summit Botanical Gardens and Harald Schmidt and colleagues from Rotterdam Zoo for help with captive toucans, Wolfgang Heidrich, Franz Kuemmeth, Bart Kranstauber Daniel Obando and Alexandro Ortega for technical support, and the Smithsonian Tropical Research Institute and Autoridad Nacional del Ambiente de Panama for administrative support. Thanks to Edgar Perez and the Gamboa resort hotel for allowing us to work on their properties. This study was supported by funding from the Netherlands Organisation for Scientific Research (grants W84-584 and 863-07-008 to P.A.J.), the National Science Foundation (NSF-DEB 0717071 to R.K.), and the Max Planck Institute for Ornithology. NR 47 TC 21 Z9 21 U1 4 U2 55 PU GAUTHIER-VILLARS/EDITIONS ELSEVIER PI PARIS PA 23 RUE LINOIS, 75015 PARIS, FRANCE SN 1146-609X J9 ACTA OECOL JI Acta Oecol.-Int. J. Ecol. PD NOV-DEC PY 2011 VL 37 IS 6 SI SI BP 625 EP 631 DI 10.1016/j.actao.2011.06.007 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 860NU UT WOS:000297955800013 ER PT J AU Keil, K Mccoy, TJ Wilson, L Barrat, JA Rumble, D Meier, MMM Wieler, R Huss, GR AF Keil, Klaus McCoy, Timothy J. Wilson, Lionel Barrat, Jean-Alix Rumble, Doug Meier, Matthias M. M. Wieler, Rainer Huss, Gary R. TI A composite Fe, Ni-FeS and enstatite-forsterite-diopside-glass vitrophyre clast in the Larkman Nunatak 04316 aubrite: Origin by pyroclastic volcanism SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID OXYGEN-ISOTOPE RATIOS; RARE-EARTH-ELEMENT; PARENT BODY; EXPLOSIVE ERUPTIONS; COSMOGENIC NUCLIDES; MELT MIGRATION; CORE FORMATION; SOLAR-SYSTEM; CHONDRITES; METEORITES AB We studied the mineralogy, petrology, and bulk, trace element, oxygen, and noble gas isotopic compositions of a composite clast approximately 20 mm in diameter discovered in the Larkman Nunatak (LAR) 04316 aubrite regolith breccia. The clast consists of two lithologies: One is a quench-textured intergrowth of troilite with spottily zoned metallic Fe, Ni which forms a dendritic or cellular structure. The approximately 30 mu m spacings between the Fe, Ni arms yield an estimated cooling rate of this lithology of approximately 25-30 degrees C s(-1). The other is a quench-textured enstatite-forsterite-diopside-glass vitrophyre lithology. The composition of the clast suggests that it formed at an exceptionally high degree of partial melting, perhaps approaching complete melting, and that the melts from which the composite clast crystallized were quenched from a temperature of approximately 1380-1400 degrees C at a rate of approximately 25-30 degrees C s(-1). The association of the two lithologies in a composite clast allows, for the first time, an estimation of the cooling rate of a silicate vitrophyre in an aubrite of approximately 25-30 degrees C s(-1). While we cannot completely rule out an impact origin of the clast, we present what we consider is very strong evidence that this composite clast is one of the elusive pyroclasts produced during pyroclastic volcanism on the aubrite parent body (Wilson and Keil 1991). We further suggest that this clast was not ejected into space but retained on the aubrite parent body by virtue of the relatively large size of the clast of approximately 20 mm. Our modeling, taking into account the size of the clast, suggests that the aubrite parent body must have been between approximately 40 and 100 km in diameter, and that the melt from which the clast crystallized must have contained an estimated maximum range of allowed volatile mass fractions between approximately 500 and approximately 4500 ppm. C1 [Keil, Klaus; Wilson, Lionel; Huss, Gary R.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Wilson, Lionel] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England. [Barrat, Jean-Alix] UBOIUEM, CNRS UMR Domaines Ocean 6538, F-29280 Plouzane, France. [Rumble, Doug] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Meier, Matthias M. M.; Wieler, Rainer] Swiss Fed Inst Technol, Inst Geochem & Petr, CH-8092 Zurich, Switzerland. RP Keil, K (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. EM keil@hawaii.edu RI Jean-Alix, BARRAT/F-8035-2012; Wieler, Rainer/A-1355-2010; Barrat, Jean-Alix/C-8416-2017; OI Wieler, Rainer/0000-0001-5666-7494; Barrat, Jean-Alix/0000-0003-3158-3109; Meier, Matthias/0000-0002-7179-4173 FU NASA [NNX08AE08G, NNG06GF56G, NNX08AG58G, NNX07AI48G]; Swiss Science Foundation FX We thank Kevin Righter and the staff of the Meteorite Processing Laboratory at NASA's L. B. Johnson Space Center for providing Fig. 1 and the carefully selected and well-documented samples of the various lithologies of LAR 04316. At the University of Hawai'i, we thank Eric Hellebrand for his expert assistance with the electron probe microanalyses, Deon Van Niekerk for the modal analysis of the Fe,Ni-FeS clast, Sasha Krot for his assistance with the X-ray maps, and Ed Scott for insightful discussions of the origin of the zoned metal. We thank Ian Franchi, James Day, and an anonymous reviewer for constructive reviews that helped improve the manuscript considerably. We are grateful to Kees Welten of the University of California, Berkeley for providing his unpublished CRE age of LAR 04316. This work was supported in part by NASA Cosmochemistry grants NNX08AE08G (K. Keil, PI), NNG06GF56G (T. McCoy, PI), NNX08AG58G (G. R. Huss, PI), NNX07AI48G (D. Rumble, PI), and by the Swiss Science Foundation (R. Wieler, PI). This is a Hawai'i Institute of Geophysics and Planetology publication No. 8211 and School of Ocean and Earth Science and Technology Publication no. 8300. NR 73 TC 7 Z9 7 U1 0 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2011 VL 46 IS 11 BP 1719 EP 1741 DI 10.1111/j.1945-5100.2011.01261.x PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 853GQ UT WOS:000297414600009 ER PT J AU Wall, AJ Mathur, R Post, JE Heaney, PJ AF Wall, Andrew J. Mathur, Ryan Post, Jeffrey E. Heaney, Peter J. TI Cu isotope fractionation during bornite dissolution: An in situ X-ray diffraction analysis SO ORE GEOLOGY REVIEWS LA English DT Review DE Copper isotope fractionation; Bornite; Synchrotron XRD ID SOURCE MASS-SPECTROMETRY; UNITED-STATES; SE AUSTRALIA; AU DEPOSIT; COPPER; RATIOS; MINERALIZATION; CHALCOCITE; PORPHYRY; ACID AB Low-temperature ore deposits exhibit a large variation in delta(65)Cu (similar to 12 parts per thousand), and this range has been attributed, in part, to isotope fractionation during weathering reactions of primary minerals such as chalcocite and chalcopyrite. Here, we examine the fractionation of Cu isotopes during dissolution of another important Cu ore mineral, bornite, using a novel approach that combines time-resolved X-ray diffraction (XRD) and isotope analysis of reaction products. During the initial stages of bornite oxidative dissolution by ferric sulfate (<5 mol% of total Cu leached), dissolved Cu was enriched in isotopically heavy Cu ((65)Cu) relative to the solid, with an average apparent isotope fractionation (Delta(aq-min) = delta(65)Cu(aq)-delta(65)Cu(min)(0)) of 2.20 +/- 0.25 parts per thousand. When >20 mol% Cu was leached from the solid, the difference between the Cu isotope composition of the aqueous and mineral phases approached zero, with Delta(0)(aq-min) values ranging from -0.21 +/- 0.61 parts per thousand to 0.92 +/- 0.25 parts per thousand. XRD analysis allowed us to correlate changes in the atomic structure of bornite with the apparent isotope fractionation as the dissolution reaction progressed. These data revealed that the greatest degree of apparent fractionation is accompanied by a steep contraction in the unit-cell volume, which we identified as a transition from stoichiometric to non-stoichiometric bornite. We propose that the initially high A(aq-min) values result from isotopically heavy Cu ((65)Cu) concentrating within Cu(2+) during dissolution. The decrease in the apparent isotope fractionation as the reaction progresses occurs from the distillation of isotopically heavy Cu ((65)Cu) during dissolution or kinetic isotope effects associated with the depletion of Cu from the surfaces of bornite particles. (C) 2011 Elsevier B.V. All rights reserved. C1 [Wall, Andrew J.; Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Mathur, Ryan] Juniata Coll, Dept Geol, Huntingdon, PA 16652 USA. [Post, Jeffrey E.] Smithsonian NMNH, Dept Mineral Sci, Washington, DC 20013 USA. RP Wall, AJ (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM awall@psu.edu FU NSF [EAR07-45374, NSF CHE04-31328]; Center for Environmental Kinetics Analysis (CEKA); DOE; Mineralogical Society of America; Geological Society of America; U.S. Department of Energy, Division of Materials Sciences and Division of Chemical Sciences [DE-AC02-98CH10886]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357] FX Funding for this research was provided by NSF grant EAR07-45374, the Center for Environmental Kinetics Analysis (CEKA), an NSF- and DOE-sponsored Environmental Molecular Science Institute (NSF CHE04-31328), the Edward H. Kraus Crystallographic Research Fund of the Mineralogical Society of America, and by a Geological Society of America Graduate Student Research Grant. This research was carried out at two synchrotron sources: 1) the National Synchrotron Light Source, Brookhaven National Laboratory, which is supported by the U.S. Department of Energy, Division of Materials Sciences and Division of Chemical Sciences, under Contract No. DE-AC02-98CH10886: and 2) the Advanced Photon Source at Argonne National Laboratory, which is supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-06CH11357. We thank the three anonymous reviewers whose comments improved NR 49 TC 18 Z9 21 U1 3 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-1368 J9 ORE GEOL REV JI Ore Geol. Rev. PD NOV PY 2011 VL 42 IS 1 SI SI BP 62 EP 70 DI 10.1016/j.oregeorev.2011.01.001 PG 9 WC Geology; Mineralogy; Mining & Mineral Processing SC Geology; Mineralogy; Mining & Mineral Processing GA 858FS UT WOS:000297781900006 ER PT J AU Quesada, R Triana, E Vargas, G Douglass, JK