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 Seid, MA Niven, JE Eberhard, WG Wcislo, WT AF Quesada, Rosannette Triana, Emilia Vargas, Gloria Douglass, John K. Seid, Marc A. Niven, Jeremy E. Eberhard, William G. Wcislo, William T. TI The allometry of CNS size and consequences of miniaturization in orb-weaving and cleptoparasitic spiders SO ARTHROPOD STRUCTURE & DEVELOPMENT LA English DT Article DE Miniaturization; Allometry; Orb-web spiders; cleptoparasitic spiders; Araneae ID CENTRAL NERVOUS-SYSTEM; PLETHODONTID SALAMANDERS; KLEPTOPARASITIC SPIDER; BRAIN SIZE; INSECTS; ARANEAE; BODY; THERIDIIDAE; INFORMATION; COLEOPTERA AB Allometric studies of the gross neuroanatomy of adults from nine species of spiders from six web-weaving families (Orbicularia), and nymphs from six of these species, show that very small spiders resemble other small animals in having disproportionately larger central nervous systems (CNSs) relative to body mass when compared with large-bodied forms. Small spiderlings and minute adult spiders have similar relative CNS volumes. The relatively large CNS of a very small spider occupies up to 78% of the cephalothorax volume. The CNSs of very small spiders extend into their coxae, occupying as much as 26% of the profile area of the coxae of an Anapisona simoni spiderling (body mass < 0.005 mg). Such modifications occur both in species with minute adults, and in tiny spiderlings of species with large-bodied adults. In at least one such species, Leucauge mariana, the CNS of the spiderling extends into a prominent ventral bulge of the sternum. Tiny spiders also have reduced neuronal cell body diameters. The adults of nearly all orbicularian spiders weave prey capture webs, as do the spiderlings, beginning with second instar nymphs. Comparable allometric relations occur in adults of both orb-weaving and cleptoparasitic species, indicating that this behavioral difference is not reflected in differences in gross CNS allometry. Published by Elsevier Ltd. C1 [Quesada, Rosannette; Triana, Emilia; Vargas, Gloria; Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. [Quesada, Rosannette; Triana, Emilia; Vargas, Gloria; Douglass, John K.; Seid, Marc A.; Niven, Jeremy E.; Eberhard, William G.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama. RP Eberhard, WG (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ Rodrigo Facio, San Pedro, Costa Rica. EM william.eberhard@gmail.com; WcisloW@si.edu RI Quesada, Rosannette/E-7947-2015 FU F. H. Levinson Fund; Smithsonian Institution; Smithsonian Tropical Research Institute's (STRI); Royal Society FX We thank S. Tierney, A. Smith, N. Strausfeld, and two anonymous reviewers for help with discussions and comments on the manuscript. Financial support was provided by the F. H. Levinson Fund, the Smithsonian Institution's Scholarly Studies Program to WTW (PI), the Smithsonian Tropical Research Institute's (STRI) "Adelante" Internship program (to RQ), the Royal Society (to JEN), and general research funds from STRI to WTW and WGE. We are grateful to the STRI staff for logistical support, and to the Autoridad Nacional del Medio Ambiente for collecting and research permits, SE/A-51-10. NR 47 TC 16 Z9 17 U1 1 U2 17 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1467-8039 J9 ARTHROPOD STRUCT DEV JI Arthropod Struct. Dev. PD NOV PY 2011 VL 40 IS 6 BP 521 EP 529 DI 10.1016/j.asd.2011.07.002 PG 9 WC Entomology SC Entomology GA 853KW UT WOS:000297426200004 PM 22036838 ER PT J AU Miller, AW Minton, MS Ruiz, GM AF Miller, A. Whitman Minton, Mark S. Ruiz, Gregory M. TI Geographic Limitations and Regional Differences in Ships' Ballast Water Management to Reduce Marine Invasions in the Contiguous United States SO BIOSCIENCE LA English DT Article DE ballast water; shipping; nonnative species; marine invasions; propagule supply ID ECOSYSTEMS; PATTERNS; ECOLOGY AB Marine species are in constant motion in the ballast water and on the hulls of the ships that ply the world's oceans; ships serve as a major vector for biological invasions. Despite federal and state regulations that require ballast water exchange (BWE), particular trade routes impose geographic and temporal constraints on compliance, limiting whether a ship can conduct BWE at the required distance (>= 200 nautical miles) from shore to minimize transfers of coastal organisms. Ships moving across the Americas are largely unable to conduct open-ocean BWE, but instead often conduct exchanges inside coastal waters. Overall, strong differences exist in volumes, geographic sources, and the use of BWE for ballast water discharge among the three major coasts of the contiguous United States. Such patterns suggest important geographic differences in invasion opportunities and also argue for more effective alternative ballast water treatments that can be applied more evenly. C1 [Miller, A. Whitman; Minton, Mark S.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Miller, AW (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM millerw@si.edu OI Ruiz, Gregory/0000-0003-2499-441X; Minton, Mark/0000-0002-9439-4930; Miller, Whitman/0000-0003-0484-182X FU US Coast Guard FX Support for this work was provided by the US Coast Guard. We thank all members of the National Ballast Information Clearinghouse for their assistance in receiving, processing, and organizing the ballast water data. We thank Richard Everett and three anonymous reviewers for their comments and suggestions on the manuscript. NR 27 TC 15 Z9 15 U1 1 U2 15 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD NOV PY 2011 VL 61 IS 11 BP 880 EP 887 DI 10.1525/bio.2011.61.11.7 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 853AM UT WOS:000297398600007 ER PT J AU Hong, T AF Hong, Terry TI Drifting House SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 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 NOV 1 PY 2011 VL 136 IS 18 BP 75 EP 75 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 853PT UT WOS:000297438900071 ER PT J AU Blomme, J Sarro, LM O'Donovan, FT Debosscher, J Brown, T Lopez, M Dubath, P Rimoldini, L Charbonneau, D Dunham, E Mandushev, G Ciardi, DR De Ridder, J Aerts, C AF Blomme, J. Sarro, L. M. O'Donovan, F. T. Debosscher, J. Brown, T. Lopez, M. Dubath, P. Rimoldini, L. Charbonneau, D. Dunham, E. Mandushev, G. Ciardi, D. R. De Ridder, J. Aerts, C. TI Improved methodology for the automated classification of periodic variable stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; methods: statistical; techniques: photometric ID SUPERVISED CLASSIFICATION AB We present a novel automated methodology to detect and classify periodic variable stars in a large data base of photometric time series. The methods are based on multivariate Bayesian statistics and use a multistage approach. We applied our method to the ground-based data of the Trans-Atlantic Exoplanet Survey (TrES) Lyr1 field, which is also observed by the Kepler satellite, covering similar to 26 000 stars. We found many eclipsing binaries as well as classical non-radial pulsators, such as slowly pulsating B stars, ? Doradus, beta Cephei and d Scuti stars. Also a few classical radial pulsators were found. C1 [Blomme, J.; Debosscher, J.; De Ridder, J.; Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Sarro, L. M.] UNED, Dpt Inteligencia Artificial, Madrid 28040, Spain. [O'Donovan, F. T.] CALTECH, Pasadena, CA 91125 USA. [Brown, T.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Brown, T.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Lopez, M.] CSIC, INTA, Ctr Astrobiol, Dept Astrofis, E-28691 Villanueva De La Canada, Spain. [Dubath, P.; Rimoldini, L.] Observ Geneva, CH-1290 Versoix, Switzerland. [Charbonneau, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunham, E.; Mandushev, G.] Lowell Observ, Flagstaff, AZ 86001 USA. [Ciardi, D. R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Aerts, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegem, Netherlands. RP Blomme, J (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Heverlee, Belgium. EM jonas.blomme@ster.kuleuven.be RI Sarro, Luis/L-8082-2014; O'Donovan, Francis/I-2423-2014; OI O'Donovan, Francis/0000-0002-4858-6106; Ciardi, David/0000-0002-5741-3047 FU European Research Council under the European Community [227224]; Research Council of K. U. Leuven [GOA/2008/04]; Fund for Scientific Research of Flanders [G.0332.06]; Belgian Federal Science Policy Office [C90309, C90291]; Spanish Ministerio de Educacion y Ciencia [AYA2005-04286] FX The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 227224 (PROSPERITY), the Research Council of K. U. Leuven (GOA/2008/04), from the Fund for Scientific Research of Flanders (G.0332.06), the Belgian Federal Science Policy Office (C90309: CoRoT Data Exploitation, C90291 Gaia-DPAC) and the Spanish Ministerio de Educacion y Ciencia through grant AYA2005-04286. Public access to the TrES data was provided to the through the NASA Star and Exoplanet Database (NStED, http://nsted.ipac.caltech.edu). NR 13 TC 19 Z9 19 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 418 IS 1 BP 96 EP 106 DI 10.1111/j.1365-2966.2011.19466.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IR UT WOS:000297045700040 ER PT J AU Wright, NJ Barlow, MJ Ercolano, B Rauch, T AF Wright, N. J. Barlow, M. J. Ercolano, B. Rauch, T. TI A 3D photoionization model of the extreme planetary nebula NGC 6302 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planetary nebulae: individual: NGC 6302; ISM: abundances ID ASYMPTOTIC GIANT BRANCH; INTERMEDIATE-MASS STARS; HUBBLE-TYPE OUTFLOWS; HEAVY ELEMENT LINES; POST-AGB STARS; HIGH-EXCITATION; ISO SPECTRUM; X-RAYS; MU-M; CHEMICAL-COMPOSITION AB We present a 3D photoionization model of the planetary nebula NGC 6302, one of the most complex and enigmatic objects of its kind. Its highly bipolar geometry and dense massive disc, coupled with the very wide range of ions present, from neutral species up to Si8+, make it one of the ultimate challenges to nebular photoionization modelling. Our MOCASSIN model is composed of an extremely dense geometrically thin circumstellar disc and a large pair of diffuse bipolar lobes, a combination which was necessary to reproduce the observed emission-line spectrum. The masses of these components, 2.2 M-circle dot and 2.5 M-circle dot, respectively, give a total nebular mass of 4.7 M-circle dot, of which 1.8 M-circle dot (39 per cent) is ionized. Discrepancies between our model fit and the observations are attributed to complex density inhomogeneities in the nebula. The potential to resolve such discrepancies with more complex models is confirmed by exploring a range of models introducing small-scale structures. Compared to solar abundances helium is enhanced by 50 per cent, carbon is slightly subsolar, oxygen is solar, and nitrogen is enhanced by a factor of 6. These all imply a significant third dredge-up coupled with hot-bottom burning CN-cycle conversion of dredged-up carbon to nitrogen. Aluminium is also depleted by a factor of 100, consistent with depletion by dust grains. The central star of NGC 6302 is partly obscured by the opaque circumstellar disc, which is seen almost edge-on, and as such its properties are not well constrained. However, emission from a number of high-ionization 'coronal' lines provides a strong constraint on the form of the high-energy ionizing flux. We model emission from the central star using a series of stellar model atmospheres, the properties of which are constrained from fits to the high-ionization nebular emission lines. Using a solar abundance stellar atmosphere we are unable to fit all of the observed line fluxes, but a substantially better fit was obtained using a 220 000 K hydrogen-deficient stellar atmosphere with log g = 7.0 and L-star = 14 300 L-circle dot. The H-deficient nature of the central star atmosphere suggests that it has undergone some sort of late thermal pulse, and fits to evolutionary tracks imply a central star mass of 0.73-0.82 M-circle dot. Time-scales for these evolutionary tracks suggest the object left the top of the asymptotic giant branch similar to 2100 years ago, in good agreement with studies of the recent mass-loss event that formed one pair of the bipolar lobes. Based on the modelled nebular mass and central star mass we estimate the initial mass of the central star to be 5.5 M-circle dot, in approximate agreement with that derived from evolutionary tracks. C1 [Wright, N. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wright, N. J.; Barlow, M. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Ercolano, B.] Univ Sternwarte Munchen, D-81679 Munich, Germany. [Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany. RP Wright, NJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nwright@head.cfa.harvard.edu RI Barlow, Michael/A-5638-2009 OI Barlow, Michael/0000-0002-3875-1171 FU STFC; BIS; Miracle Consortium; SAO; German Aerospace Center (DLR) [05 OR 0806] FX The simulations presented in this work were performed in the DiRAC Facility jointly funded by STFC and the Large Facilities Capital Fund of BIS. The authors acknowledge support of the STFC funded Miracle Consortium (part of the DiRAC facility) in providing access to the University College London (UCL) Legion High Performance Computing Facility. The authors additionally acknowledge the support of UCL's Research Computing team with the use of the Legion facility, particularly Jeremy Yates and Dugan Witherick. This work has also made use of the CHIANTI data base, a collaborative project involving researchers at NRL (USA) RAL (UK) and the Universities of: Cambridge (UK), George Mason (USA) and Florence (Italy).; We are grateful to the referee, Albert Zijlstra, for a swift and helpful report that has improved the work presented here. We would also like to thank Pete Storey, Mikako Matsuura, Jonathan Rawlings and Tim Gledhill for interesting discussions on this work. NJW acknowledges support from the STFC and an SAO Pre-doctoral Fellowship. BE acknowledges support from an STFC Advanced Fellowship. TR was supported by the German Aerospace Center (DLR) under grant 05 OR 0806. NR 106 TC 15 Z9 15 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 418 IS 1 BP 370 EP 389 DI 10.1111/j.1365-2966.2011.19490.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IR UT WOS:000297045700060 ER PT J AU Narayanan, D Krumholz, M Ostriker, EC Hernquist, L AF Narayanan, Desika Krumholz, Mark Ostriker, Eve C. Hernquist, Lars TI The CO-H2 conversion factor in disc galaxies and mergers SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: clouds; ISM: molecules; galaxies: interactions; galaxies: ISM; galaxies: starburst; galaxies: star formation ID ULTRALUMINOUS INFRARED GALAXIES; GALACTIC MOLECULAR CLOUDS; SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES; GAMMA-RAY EMISSION; PARTICLE HYDRODYNAMICS SIMULATIONS; REDSHIFT SUBMILLIMETER GALAXIES; MODELING CO EMISSION; AEGIS FIELD GALAXIES; INTERSTELLAR-MEDIUM AB Relating the observed CO emission from giant molecular clouds (GMCs) to the underlying H2 column density is a long-standing problem in astrophysics. While the Galactic COH2 conversion factor (XCO) appears to be reasonably constant, observations indicate that XCO may be depressed in high surface density starburst environments. Using a multiscale approach, we investigate the dependence of XCO on the galactic environment in numerical simulations of disc galaxies and galaxy mergers. XCO is proportional to the GMC surface density divided by the integrated CO intensity, WCO, and WCO is related to the kinetic temperature and velocity dispersion in the cloud. In disc galaxies (except within the central similar to kpc), the galactic environment is largely unimportant in setting the physical properties of GMCs provided they are gravitationally bound. The temperatures are roughly constant at similar to 10 K due to the balance of CO cooling and cosmic ray heating, giving a nearly constant COH2 conversion factor in discs. In mergers, the velocity dispersion of the gas rises dramatically during coalescence. The gas temperature also rises as it couples well to the warm (similar to 50 K) dust at high densities (n > 104 cm-3). The rise in velocity dispersion and temperature combine to offset the rise in surface density in mergers, causing XCO to drop by a factor of similar to 210 compared to the disc simulation. This model predicts that high-resolution Atacama Large Millimeter/submillimeter Array observations of nearby ultraluminous infrared galaxies should show velocity dispersions of 101102 km s-1, and brightness temperatures comparable to the dust temperatures. C1 [Narayanan, Desika] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Krumholz, Mark] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ostriker, Eve C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Narayanan, D (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM dnarayanan@as.arizona.edu FU NSF [AST-1009452, AST-0807739, CAREER-0955300, AST-0908185]; Alfred P. Sloan fellowship; NASA [NNX09AK31G]; Spitzer Space Telescope Theoretical Research Program; Harvard FAS Research Computing Group FX This work benefited from discussions had and coding done at the Aspen Center for Physics. DN would like thank Patrik Jonsson for numerous helpful conversations regarding adaptive mesh techniques in radiative transfer modelling, and Rahul Shetty, Andrew Baker, Emanuele Daddi, Robert Feldmann, Adam Leroy, Padelis Papadopoulos and Erik Rosolowsky for sharing their knowledge on XCO in galaxies. As always, T. J. Cox's wisdom was invaluable in understanding the physics associated with galaxy mergers. The authors thank the referee, Simon Glover, for a constructive report. Finally, DN would like to thank Rob Kennicutt for providing the original motivation to pursue this study following an insightful question at the 2007 Gas Accretion and Star Formation Workshop in Garching. DN acknowledges support from the NSF via grant AST-1009452. MK acknowledges support from an Alfred P. Sloan fellowship, the NSF through grants AST-0807739 and CAREER-0955300 and NASA through Astrophysics Theory and Fundamental Physics grant NNX09AK31G and a Spitzer Space Telescope Theoretical Research Program grant. ECO acknowledges support from the NSF via grant AST-0908185. The simulations in this paper were run on the Odyssey cluster, supported by the Harvard FAS Research Computing Group. NR 159 TC 69 Z9 70 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 418 IS 1 BP 664 EP 679 DI 10.1111/j.1365-2966.2011.19516.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IR UT WOS:000297045700085 ER PT J AU Kilic, M Brown, WR Hermes, JJ Prieto, CA Kenyon, SJ Winget, DE Winget, KI AF Kilic, Mukremin Brown, Warren R. Hermes, J. J. Allende Prieto, Carlos Kenyon, S. J. Winget, D. E. Winget, K. I. TI SDSS J163030.58+423305.8: a 40-min orbital period detached white dwarf binary SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational waves; binaries: close; stars: individual: SDSS J163030.58+423305.8; supernovae: general; white dwarfs ID DIGITAL SKY SURVEY; SPY PROJECT; STARS; EVOLUTION; PROGENITOR; SUPERNOVAE; DISCOVERY; CATALOG; SYSTEMS; I. AB We report the discovery of a new detached, double white dwarf (WD) system with an orbital period of 39.8 min. We targeted SDSS J163030.58+423305.8 (hereafter J1630) as part of our radial velocity programme to search for companions around low-mass WDs using the 6.5-m MMT. We detect peak-to-peak radial velocity variations of 576 km s-1. The mass function and optical photometry rule out main-sequence companions. In addition, no millisecond pulsar companions are detected in radio observations. Thus the invisible companion is most likely another WD. Unlike the other 39-min binary SDSS J010657.39-100003.3, follow-up high-speed photometric observations of J1630 obtained at the McDonald 2.1-m telescope do not show significant ellipsoidal variations, indicating a higher primary mass and smaller radius. The absence of eclipses constrain the inclination angle to i= 82 degrees. J1630 contains a pair of WDs, 0.3 M? primary +=0.3 M? invisible secondary, at a separation of =0.32 R. The two WDs will merge in less than 31 Myr. Depending on the core composition of the companion, the merger will form either a single core He-burning subdwarf star or a rapidly rotating massive WD. The gravitational wave strain from J1630 is detectable by instruments like the Laser Interferometer Space Antenna (LISA) within the first year of operation. C1 [Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Brown, Warren R.; Kenyon, S. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Hermes, J. J.; Winget, D. E.; Winget, K. I.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP Kilic, M (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. EM kilic@ou.edu OI Kenyon, Scott/0000-0003-0214-609X FU NSF [AST-0909107]; Norman Hackerman Advanced Research Programme [003658-0255-2007, 003658-0252-2009] FX We thank D. Koester for kindly providing WD model spectra. DEW and JJH gratefully acknowledge the support of the NSF under grant AST-0909107 and the Norman Hackerman Advanced Research Programme under grants 003658-0255-2007 and 003658-0252-2009. NR 34 TC 16 Z9 16 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 418 IS 1 BP L157 EP L161 DI 10.1111/j.1745-3933.2011.01165.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IR UT WOS:000297045700033 ER PT J AU Tchekhovskoy, A Narayan, R McKinney, JC AF Tchekhovskoy, Alexander Narayan, Ramesh McKinney, Jonathan C. TI Efficient generation of jets from magnetically arrested accretion on a rapidly spinning black hole SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; MHD; methods: numerical; galaxies: jets ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; ACTIVE GALACTIC NUCLEI; RELATIVISTIC MAGNETOHYDRODYNAMICS; ELECTROMAGNETIC EXTRACTION; NUMERICAL SCHEME; COLLAPSING STAR; RADIO-SOURCES; DISKS; ENERGY; FIELD AB We describe global, 3D, time-dependent, non-radiative, general-relativistic, magnetohydrodynamic simulations of accreting black holes (BHs). The simulations are designed to transport a large amount of magnetic flux to the centre, more than the accreting gas can force into the BH. The excess magnetic flux remains outside the BH, impedes accretion, and leads to a magnetically arrested disc. We find powerful outflows. For a BH with spin parameter a = 0.5, the efficiency with which the accretion system generates outflowing energy in jets and winds is eta approximate to 30 per cent. For a = 0.99, we find eta approximate to 140 per cent, which means that more energy flows out of the BH than flows in. The only way this can happen is by extracting spin energy from the BH. Thus the a = 0.99 simulation represents an unambiguous demonstration, within an astrophysically plausible scenario, of the extraction of net energy from a spinning BH via the PenroseBlandfordZnajek mechanism. We suggest that magnetically arrested accretion might explain observations of active galactic nuclei with apparent eta approximate to few x 100 per cent. C1 [Tchekhovskoy, Alexander] Princeton Univ, Ctr Theoret Sci, Princeton, NJ 08544 USA. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [McKinney, Jonathan C.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. RP Tchekhovskoy, A (reprint author), Princeton Ctr Theoret Sci, Princeton, NJ USA. EM atchekho@princeton.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST-1041590]; NASA [NNX11AE16G]; [TG-AST10-0040]; [TG-AST080026N]; [TG-AST080025N] FX We thank S. Balbus, K. Beckwith, A. Benson, V. Beskin, I. Contopoulos, L. Foschini, D. Giannios, J. Goodman, I. Igumenshchev, B. Metzger, R. Penna, R. Rafikov, A. Spitkovsky, J. Stone, F. Tombesi, D. Uzdensky for discussions. We thank the anonymous referee for useful suggestions. AT was supported by a Princeton Center for Theoretical Science Fellowship. AT and RN were supported in part by NSF grant AST-1041590 and NASA grant NNX11AE16G. We acknowledge support by the NSF through TeraGrid resources provided by NICS Kraken, where simulations were carried out, NICS Nautilus, where data were analysed, and NCSA MSS, where data were backed up, under grant numbers TG-AST10-0040 (AT), TG-AST080026N (RN) and TG-AST080025N (JCM). NR 42 TC 208 Z9 212 U1 2 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 418 IS 1 BP L79 EP L83 DI 10.1111/j.1745-3933.2011.01147.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IR UT WOS:000297045700017 ER PT J AU Nardini, E Risaliti, G AF Nardini, E. Risaliti, G. TI The effects of X-ray absorption variability in NGC 4395 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: NGC 4395; X-rays: galaxies ID SEYFERT-1 GALAXY NGC-4395; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; EMISSION-LINE; REFLECTION; MODELS; ORIGIN; SOFT AB We present a new X-ray analysis of the dwarf Seyfert galaxy NGC 4395, based on two archival XMMNewton and Suzaku observations. This source is well known for a series of remarkable properties: one of the smallest estimated black hole masses among active galactic nuclei (AGN) (of the order of similar to 105 M?), intense flux variability on very short time-scales (a few tens of seconds) and an unusually flat X-ray continuum (G similar to 1.4 over the 210 keV energy range). NGC 4395 is also characterized by significant variations of the X-ray spectral shape, and here we show that such behaviour can be explained through the partial occultation by circumnuclear cold absorbers with column densities of similar to 10221023 cm-2. In this scenario, the primary X-ray emission is best reproduced by means of a power law with a standard G similar to 1.8 photon index, consistent with both the spectral slope observed at higher energies and the values typical of local AGN. C1 [Nardini, E.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Nardini, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM enardini@cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009; OI Risaliti, Guido/0000-0002-3556-977X FU NASA [NNX08AN48G] FX This work has been partly supported by NASA grant NNX08AN48G. We thank the anonymous referee for constructive and useful comments which significantly improved the content of this paper. NR 28 TC 14 Z9 14 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 417 IS 4 BP 2571 EP 2576 DI 10.1111/j.1365-2966.2011.19423.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IA UT WOS:000297043900011 ER PT J AU Cohen, O AF Cohen, O. TI The independency of stellar mass-loss rates on stellar X-ray luminosity and activity level based on solar X-ray flux and solar wind observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: magnetic field; stars: mass-loss; stars: solar-type; stars: winds; outflows ID HELIOSPHERIC MAGNETIC-FIELD; ANGULAR-MOMENTUM; STARS; SUN; VLA; EJECTIONS; ULYSSES AB Stellar mass-loss rates are an important input ingredient for stellar evolution models since they determine stellar evolution parameters such as stellar spin-down and increase in stellar luminosity through the lifetime of a star. Due to the lack of direct observations of stellar winds from Sun-like stars stellar X-ray luminosity and stellar level of activity are commonly used as a proxy for estimating stellar mass-loss rates. However, such an intuitive activity mass-loss rate relation is not well defined. In this paper, I study the mass-loss rate of the Sun as a function of its activity level. I compare in situ solar wind measurements with the solar activity level represented by the solar X-ray flux. I find no clear dependency of the solar mass flux on solar X-ray flux. Instead, the solar mass-loss rate is scattered around an average value of 2 x 10(-14) M(circle dot)yr(-1). This independency of the mass-loss rate on level of activity can be explained by the fact that the activity level is governed by the large modulations in the solar close magnetic flux, while the mass-loss rate is governed by the rather constant open magnetic flux. I derive a simple expression for stellar mass-loss rates as a function of the stellar ambient weak magnetic field, the stellar radius, the stellar escape velocity and the average height of the Alfven surface. This expression predicts stellar mass-loss rates of 10(-15) to 10(-12) M-circle dot yr(-1) for Sun-like stars. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ocohen@cfa.harvard.edu OI Cohen, Ofer/0000-0003-3721-0215 FU SHINE through NSF [ATM-0823592]; NASA-LWSTRT [NNG05GM44G] FX I would like to thank an unknown referee for his/her review. I thank Jeremy Drake, Vinay Kashyap, Steve Saar, Steven Cranmer and Justin Kasper for their useful comments and discussion during the preparation of this article. OC is supported by SHINE through NSF ATM-0823592 grant and by NASA-LWSTRT grant NNG05GM44G. NR 50 TC 17 Z9 17 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 417 IS 4 BP 2592 EP 2600 DI 10.1111/j.1365-2966.2011.19428.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IA UT WOS:000297043900013 ER PT J AU Kassin, SA Fogarty, L Goodsall, T Clarke, FJ Houghton, RWC Salter, G Thatte, N Tecza, M Davies, RL Weiner, BJ Willmer, CNA Salim, S Cooper, MC Newman, JA Bundy, K Conselice, CJ Koekemoer, AM Lin, LW Moustakas, LA Wang, T AF Kassin, Susan A. Fogarty, L. Goodsall, T. Clarke, F. J. Houghton, R. W. C. Salter, G. Thatte, N. Tecza, M. Davies, Roger L. Weiner, Benjamin J. Willmer, C. N. A. Salim, Samir Cooper, Michael C. Newman, Jeffrey A. Bundy, Kevin Conselice, C. J. Koekemoer, A. M. Lin, Lihwai Moustakas, Leonidas A. Wang, Tao TI Oxford SWIFT integral field spectrograph and multiwavelength observations of the Eagle galaxy at z=0.77 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high-redshift; galaxies: interactions; galaxies: irregular; galaxies: kinematics and dynamics ID STAR-FORMING GALAXIES; TULLY-FISHER RELATION; SIMILAR-TO 0.6; DATA REDUCTION SOFTWARE; INITIAL MASS FUNCTION; EXTENDED GROTH STRIP; TKRS/GOODS-N FIELD; FORMATION RATES; DYNAMICAL EVOLUTION; LUMINOSITY FUNCTION AB The Eagle galaxy at a redshift of 0.77 is studied with the Oxford Short Wavelength Integral Field Spectrograph (SWIFT) and multiwavelength data from the All-wavelength Extended Groth strip International Survey (AEGIS). It was chosen from AEGIS because of the bright and extended emission in its slit spectrum. 3D kinematic maps of the Eagle reveal a gradient in velocity dispersion which spans 3575 +/- 10 km s-1 and a rotation velocity of 25 +/- 5 km s-1 uncorrected for inclination. Hubble Space Telescope images suggest it is close to face-on. In comparison with galaxies from AEGIS at similar redshifts, the Eagle is extremely bright and blue in the rest-frame optical, highly star forming, dominated by unobscured star formation and has a low metallicity for its size. This is consistent with its selection. The Eagle is likely undergoing a major merger and is caught in the early stage of a starburst when it has not yet experienced metal enrichment or formed the mass of dust typically found in star-forming galaxies. C1 [Kassin, Susan A.; Fogarty, L.; Goodsall, T.; Clarke, F. J.; Houghton, R. W. C.; Salter, G.; Thatte, N.; Tecza, M.; Davies, Roger L.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Fogarty, L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Goodsall, T.; Moustakas, Leonidas A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Salter, G.] Univ New S Wales, Dept Astrophys, Sch Phys, Sydney, NSW 2052, Australia. [Weiner, Benjamin J.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Salim, Samir] Indiana Univ, Dept Astron, Bloomington, IN 47404 USA. [Cooper, Michael C.] Univ Calif Irvine, Ctr Galaxy Evolut, Dept Phys & Astron, Irvine, CA 92697 USA. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA USA. [Bundy, Kevin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94705 USA. [Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Lin, Lihwai] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Wang, Tao] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kassin, SA (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA. EM susan.kassin@nasa.gov RI Salim, Siti Mawarni/B-7940-2010; Conselice, Christopher/B-4348-2013; OI Koekemoer, Anton/0000-0002-6610-2048; Salim, Siti Mawarni/0000-0001-5543-5384; Conselice, Christopher/0000-0003-1949-7638; Weiner, Benjamin/0000-0001-6065-7483; Moustakas, Leonidas/0000-0003-3030-2360 FU European Commission [MEXT-CT-2003-002792]; University of Oxford Physics Department; John Fell OUP Research Fund; Caltech Optical Observatories; Observational Astrophysics Rolling Grant at Oxford; Oxford Astrophysics PATT [ST/G004331/1]; NSF [AST00-71198, AST05-07483, AST08-08133]; Balliol College, Oxford; STFC; NASA; NASA ATFP FX The Oxford SWIFT integral field spectrograph is directly supported by a Marie Curie Excellence Grant from the European Commission (MEXT-CT-2003-002792, Team Leader: N. Thatte). It is also supported by additional funds from the University of Oxford Physics Department and the John Fell OUP Research Fund. Additional funds to host and support SWIFT were provided by Caltech Optical Observatories.; Additional support was provided for by the Observational Astrophysics Rolling Grant at Oxford and the Oxford Astrophysics PATT Linked Grant ST/G004331/1. The following NSF grants to the DEEP2 survey are acknowledged: AST00-71198, AST05-07483 and AST08-08133.; LF would like to acknowledge the generous support of the Foley-Bejar Scholarship through Balliol College, Oxford and the support of the STFC.; This work of LAM was carried out in part at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. LAM acknowledges support from the NASA ATFP programme. NR 70 TC 2 Z9 2 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 417 IS 4 BP 2882 EP 2890 DI 10.1111/j.1365-2966.2011.19449.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IA UT WOS:000297043900033 ER PT J AU Pierini, D Giodini, S Finoguenov, A Bohringer, H D'Onghia, E Pratt, GW Democles, J Pannella, M Zibetti, S Braglia, FG Verdugo, M Ziparo, F Koekemoer, AM Salvato, M AF Pierini, D. Giodini, S. Finoguenov, A. Boehringer, H. D'Onghia, E. Pratt, G. W. Democles, J. Pannella, M. Zibetti, S. Braglia, F. G. Verdugo, M. Ziparo, F. Koekemoer, A. M. Salvato, M. CA COSMOS Collaboration TI Two fossil groups of galaxies at z similar to 0.4 in the Cosmic Evolution Survey: accelerated stellar-mass build-up, different progenitors SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: groups: general; galaxies: luminosity function, mass function; X-rays: galaxies: clusters ID HUBBLE-SPACE-TELESCOPE; STAR-FORMATION RATES; DIGITAL SKY SURVEY; LUMINOSITY FUNCTION; ELLIPTIC GALAXIES; CLUSTER GALAXIES; SHELL GALAXIES; RICH CLUSTERS; DARK-MATTER; MILLENNIUM SIMULATION AB We report on two fossil groups of galaxies at redshifts z= 0.425 and 0.372 discovered in the Cosmic Evolution Survey (COSMOS) area. Selected as X-ray extended sources, they have total masses (M200) equal to 1.9(+/- 0.41) x 1013 and 9.5(+/- 0.42) x 1013 M-circle dot, respectively, as obtained from a recent X-ray luminositymass scaling relation. The lower mass system appears isolated, whereas the other sits in a well-known large-scale structure (LSS) populated by 27 other X-ray emitting groups. The identification as fossil is based on the i-band photometry of all the galaxies with a photometric redshift consistent with that of the group at the 2s confidence level and within a projected groupcentric distance equal to 0.5R200, and iAB= 22.5 mag limited spectroscopy. Both fossil groups exhibit high stellar-to-total mass ratios compared to all the X-ray selected groups of similar mass at 0.3 =z= 0.5 in the COSMOS. At variance with the composite galaxy stellar mass functions (GSMFs) of similarly massive systems, both fossil group GSMFs are dominated by passively evolving galaxies down to Mstars similar to 1010 M-circle dot (according to the galaxy broad-band spectral energy distributions). The relative lack of star-forming galaxies with 1010=Mstars= 1011 M-circle dot is confirmed by the galaxy distribution in the b-r versus i colourmagnitude diagram. Hence, the two fossil groups appear as more mature than the coeval, similarly massive groups. Their overall star formation activity ended rapidly after an accelerated build up of the total stellar mass; no significant infall of galaxies with Mstars= 1010 M-circle dot took place in the last 3 to 6 Gyr. This similarity holds although the two fossil groups are embedded in two very different density environments of the LSS, which suggests that their galaxy populations were shaped by processes that do not depend on the LSS. However, their progenitors may do so. We discuss why the late merging of a compact group is favoured over the early assembly as a formation scenario for the isolated, low-mass fossil group. C1 [Pierini, D.; Finoguenov, A.; Boehringer, H.; Verdugo, M.; Ziparo, F.; Salvato, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Giodini, S.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [D'Onghia, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pratt, G. W.; Democles, J.; Pannella, M.] Univ Paris Diderot, CEA Saclay, CNRS,Lab AIM, DAPNIA Serv Astrophys,CEA DSM, F-91191 Gif Sur Yvette, France. [Zibetti, S.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Braglia, F. G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Salvato, M.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Salvato, M.] CALTECH, Pasadena, CA 91125 USA. RP Pierini, D (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM dpierini@mpe.mpg.de OI Koekemoer, Anton/0000-0002-6610-2048 NR 101 TC 6 Z9 6 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 417 IS 4 BP 2927 EP 2937 DI 10.1111/j.1365-2966.2011.19454.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IA UT WOS:000297043900037 ER PT J AU Sheth, RK Diaferio, A AF Sheth, Ravi K. Diaferio, Antonaldo TI How unusual are the Shapley supercluster and the Sloan Great Wall? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; galaxies: clusters: general; dark matter; large-scale structure of Universe ID DARK-MATTER HALOES; PROBABILITY-DISTRIBUTION FUNCTION; GAUSSIAN RANDOM-FIELDS; LARGE-SCALE STRUCTURE; EXCURSION SET MODEL; X-RAY; PERTURBATION-THEORY; GENERAL MORPHOLOGY; GALAXY CLUSTERS; REDSHIFT SURVEY AB We show that extreme value statistics are useful for studying the largest structures in the Universe by using them to assess the significance of two of the most dramatic structures in the local Universe the Shapley supercluster and the Sloan Great Wall. If we assume that the Shapley concentration (volume approximate to 1.2 x 10(5) h(-3) Mpc(3)) evolved from an overdense region in the initial Gaussian fluctuation field, with currently popular choices for the background cosmological model and the shape and amplitude s8 of the initial power spectrum, we estimate that the total mass of the system is within 20 per cent of 1.8 x 1016 h(-1) M-circle dot. Extreme value statistics show that the existence of this massive concentration is not unexpected if the initial fluctuation field was Gaussian, provided there are no other similar objects within a sphere of radius 200 h(-1) Mpc centred on our Galaxy. However, a similar analysis of the Sloan Great Wall, a more distant (z similar to 0.08) and extended concentration of structures (volume similar to 7.2 x 105 h(-3) Mpc3), suggests that it is more unusual. We estimate its total mass to be within 20 per cent of 1.2 x 1017 h(-1) M-circle dot and we find that even if it is the densest such object of its volume within z= 0.2, its existence is difficult to reconcile with the assumption of Gaussian initial conditions if s8 was less than 0.9. This tension can be alleviated if this structure is the densest within the Hubble volume. Finally, we show how extreme value statistics can be used to address the question of how likely it is that an object like the Shapley supercluster exists in the same volume which contains the Sloan Great Wall, finding, again, that Shapley is not particularly unusual. Since it is straightforward to incorporate other models of the initial fluctuation field into our formalism, we expect our approach will allow observations of the largest structures clusters, superclusters and voids to provide relevant constraints on the nature of the primordial fluctuation field. C1 [Sheth, Ravi K.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Sheth, Ravi K.] Abdus Salam Int Ctr Theoret Phys, I-34151 Trieste, Italy. [Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl INFN, Sez Torino, I-10125 Turin, Italy. [Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sheth, RK (reprint author), Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA. EM shethrk@physics.upenn.edu; diaferio@ph.unito.it FU INFN [PD51]; MIUR; NSF-AST [0908241] FX We thank the INFN exchange program for support, and the Centro di Ciencias de Benasque 'Pedro Pascual' for hospitality during the summer of 2008 when most of this work was completed, Jorg Colberg for encouragement then, Aseem Paranjape for encouragement now, and Stefano Camera for providing the opportunity for us to meet again and complete this work. RKS is supported in part by NSF-AST 0908241. AD acknowledges additional support from the INFN grant PD51 and the PRIN-MIUR-2008 grant 'Matter-antimatter asymmetry, dark matter and dark energy in the LHC era'. This research has made use of NASA's Astrophysics Data System. NR 53 TC 23 Z9 23 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 417 IS 4 BP 2938 EP 2949 DI 10.1111/j.1365-2966.2011.19453.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848IA UT WOS:000297043900038 ER PT J AU Pogue, MG AF Pogue, Michael G. TI Larval Description of Copitarsia incommoda (Lepidoptera: Noctuidae) SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Bolivia; Altiplano; invasive species; pest; quinoa AB The last instar of Copitarsia incommoda (Walker) is described for the first time. Specimens in this study were reared from quinoa (Chenopodium quinoa Willd., Chenopodiaceae), Bolivia, La Paz, 4 km S Viacha, Quipaquipani, 3,880 m. The larva of Copitarsia incommoda is compared with larvae of Copitarsia decolora (Guenee) and Copitarsia corruda Pogue and Simmons. C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, Washington, DC 20013 USA. RP Pogue, MG (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, POB 37012,MRC-168, Washington, DC 20013 USA. EM michael.pogue@ars.usda.gov NR 9 TC 0 Z9 0 U1 1 U2 5 PU ENTOMOLOGICAL SOC AMER PI LANHAM PA 10001 DEREKWOOD LANE, STE 100, LANHAM, MD 20706-4876 USA SN 0013-8746 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD NOV PY 2011 VL 104 IS 6 BP 1292 EP 1296 DI 10.1603/AN10099 PG 5 WC Entomology SC Entomology GA 849ZJ UT WOS:000297163900018 ER PT J AU Morowitz, H Sagan, C AF Morowitz, Harold Sagan, Carl TI Life in the Clouds of Venus? SO ASTROBIOLOGY LA English DT Editorial Material C1 [Morowitz, Harold] Yale Univ, Dept Mol Biophys, New Haven, CT 06520 USA. [Sagan, Carl] Smithsonian Astrophys Observ, Harvard Coll Observ, Cambridge, MA USA. RP Morowitz, H (reprint author), Yale Univ, Dept Mol Biophys, New Haven, CT 06520 USA. NR 0 TC 0 Z9 0 U1 5 U2 21 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD NOV PY 2011 VL 11 IS 9 BP 932 EP 932 PG 1 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 851JK UT WOS:000297264300010 ER PT J AU Zeigler, SL Neel, MC Oliveira, L Raboy, BE Fagan, WF AF Zeigler, Sara L. d Neel, Maile C. Oliveira, Leonardo Raboy, Becky E. Fagan, William F. TI Conspecific and heterospecific attraction in assessments of functional connectivity SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Atlantic forest; Brazil; Circuit theory; Dispersal; Graph theory; Golden-headed lion tamarin; Wied's marmoset ID HEADED LION TAMARIN; SOCIAL-INFORMATION USE; LANDSCAPE CONNECTIVITY; HABITAT PATCHES; LEONTOPITHECUS-CHRYSOMELAS; FRAGMENTED LANDSCAPES; REPRODUCTIVE SUCCESS; PLANT CONSERVATION; PERCEPTUAL RANGE; FOREST AB Functional connectivity is known to have an important, positive influence on species persistence. Measurements of functional connectivity traditionally focus on structural attributes of landscapes such as the distance and matrix type between habitat patches as well as on how species interact with those structural attributes. However, we propose that the social behavior of a species, through conspecific and heterospecific attraction, will also impact connectivity by changing how dispersers move with respect to each other and occupied patches. We analyzed functional connectivity patterns using circuit and graph theory for golden-headed lion tamarins (Leontopithecus chrysomelas) in Brazil under three scenarios. In the first scenario, we looked at connectivity without the effects of attraction under varying maximum dispersal distance and ecological movement cost thresholds. In the second scenario, we allowed dispersers to travel over more hostile matrix than they normally would to reach an occupied patch. In the final scenario, we allowed dispersers to move only to occupied patches. We found that, according to the first scenario, range-wide functional landscape connectivity for golden-headed lion tamarins is low at realistic maximum dispersal distance and movement cost thresholds. Incorporating the effects of conspecific or heterospecific attraction would increase functional connectivity, in the case of scenario two, or decrease functional connectivity, in the case of scenario three. Because conspecific/heterospecific attraction can have an impact on movement for some species, this factor should be incorporated in assessments of functional connectivity patterns for social species and others where patch occupancy is likely to influence the movements of dispersers. C1 [Zeigler, Sara L. d] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. [Zeigler, Sara L. d] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Neel, Maile C.] Univ Maryland, Dept Plant Sci & Landscape Architecture, College Pk, MD 20742 USA. [Oliveira, Leonardo; Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Raboy, Becky E.] Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Raboy, Becky E.] Royal Zool Soc Antwerp, Ctr Res & Conservat, Antwerp, Belgium. RP Zeigler, SL (reprint author), Virginia Tech, Dept Biol Sci, 4095 Derring Hall, Blacksburg, VA 24061 USA. EM szeig23@vt.edu RI Oliveira, Leonardo/G-1290-2012 OI Oliveira, Leonardo/0000-0002-1774-0713 FU University of Maryland FX We thank Brad McRae and Santiago Saura for their quick and enthusiastic help with the use of their modeling software. Michael Lloyd provided technical support. Finally, we thank James Dietz, Jennifer Mickelberg, and Carlos Guidorizzi for sharing their unpublished work and for providing interesting discussions on lion tamarin movement. Funding was provided through the Anne G. Wylie Dissertation Fellowship through the University of Maryland (to S.Z. and L.O.). NR 73 TC 11 Z9 11 U1 5 U2 31 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD NOV PY 2011 VL 20 IS 12 BP 2779 EP 2796 DI 10.1007/s10531-011-0107-z PG 18 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 850MX UT WOS:000297200000014 ER PT J AU Cuk, M Gladman, BJ Stewart, ST AF Cuk, Matija Gladman, Brett J. Stewart, Sarah T. TI Rebuttal to the comment by Malhotra and Strom on "Constraints on the source of lunar cataclysm impactors" SO ICARUS LA English DT Editorial Material DE Moon; Moon, Surface; Cratering; Asteroids, Dynamics; Planets, Migration ID CRATERS; ORIGIN AB Cuk et al. (Cuk, M. Gladman, B.J., Stewart, S.T. [2010]. Icarus 207 590-594) concluded that the the lunar cataclysm (late heavy bombardment) was recorded in lunar Imbrian era craters, and that their size distribution is different from that of main belt asteroids (which may have been the dominant pre-Imbrian impactors). This result would likely preclude the asteroid belt as the direct source of lunar cataclysm impactors. Malhotra and Strom (Malhotra, R., Strom, R.G. [2011]. Icarus) maintain that the lunar impactor population in the Imbrian era was the same as in Nectarian and pre-Nectarian periods, and this population had a size distribution identical to that of main belt asteroids. In support of this claim, they present an Imbrian size distribution made from two data sets published by Wilhelms et al. (Wilhelms, D.E., Oberbeck, V.R., Aggarwal, H.R. [1978]. Proc. Lunar Sci. Conf. 9, 3735-3762). However, these two data sets cannot be simply combined as they represent areas of different ages and therefore crater densities. Malhotra and Strom (Malhotra, R., Strom, R.G. [2011]. Icarus) differ with the main conclusion of Wilhelms et al. (Wilhelms, D.E., Oberbeck, V.R., Aggarwal, H.R. [1978]. Proc. Lunar Sci. Conf. 9,3735-3762) that the Nectarian and Imbrian crater size distributions were different. We conclude that the available data indicate that the lunar Imbrian-era impactors had a different size distribution from the older ones, with the Imbrian impactor distribution being significantly richer in small impactors than that of older lunar impactors or current main-belt asteroids. (C) 2011 Elsevier Inc. All rights reserved. C1 [Cuk, Matija] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cuk, Matija; Stewart, Sarah T.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Gladman, Brett J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Cuk, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cuk@eps.harvard.edu OI Stewart, Sarah/0000-0001-9606-1593 NR 10 TC 5 Z9 5 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD NOV PY 2011 VL 216 IS 1 BP 363 EP 365 DI 10.1016/j.icarus.2011.08.011 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 843FQ UT WOS:000296658100031 ER PT J AU Abazajian, KN Calabrese, E Cooray, A De Bernardis, F Dodelson, S Friedland, A Fuller, GM Hannestad, S Keating, BG Linder, EV Lunardini, C Melchiorri, A Miquel, R Pierpaoli, E Pritchard, J Serra, P Takada, M Wong, YYY AF Abazajian, K. N. Calabrese, E. Cooray, A. De Bernardis, F. Dodelson, S. Friedland, A. Fuller, G. M. Hannestad, S. Keating, B. G. Linder, E. V. Lunardini, C. Melchiorri, A. Miquel, R. Pierpaoli, E. Pritchard, J. Serra, P. Takada, M. Wong, Y. Y. Y. TI Cosmological and astrophysical neutrino mass measurements SO ASTROPARTICLE PHYSICS LA English DT Review DE Neutrinos; Cosmology ID LYMAN-ALPHA FOREST; DIGITAL SKY SURVEY; EQUATION-OF-STATE; POWER SPECTRUM; CONCORDANCE MODEL; PRESSURE SUPPORT; DARK-MATTER; PARAMETERS; REIONIZATION; SIMULATIONS AB Cosmological and astrophysical measurements provide powerful constraints on neutrino masses complementary to those from accelerators and reactors. Here we provide a guide to these different probes, for each explaining its physical basis, underlying assumptions, current and future reach. (C) 2011 Elsevier B.V. All rights reserved. C1 [Dodelson, S.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Abazajian, K. N.] Univ Maryland, Dept Phys, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA. [Calabrese, E.; Melchiorri, A.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Calabrese, E.; Melchiorri, A.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, I-00185 Rome, Italy. [Cooray, A.; De Bernardis, F.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dodelson, S.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Dodelson, S.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Friedland, A.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. [Fuller, G. M.; Keating, B. G.] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Hannestad, S.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Linder, E. V.] Berkeley Lab, Berkeley, CA 94720 USA. [Linder, E. V.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Linder, E. V.] Ewha Womans Univ, Inst Early Universe WCU, Seoul, South Korea. [Lunardini, C.] Arizona State Univ, Tempe, AZ 85287 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Miquel, R.] Inst Fis Altes Energies, E-08193 Bellaterra, Barcelona, Spain. [Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Pritchard, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Serra, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Takada, M.] Univ Tokyo, IPMU, Chiba 2778582, Japan. [Wong, Y. Y. Y.] Rhein Westfal TH Aachen, Inst Theoret Teilchenphys & Kosmol, D-52056 Aachen, Germany. RP Dodelson, S (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM Dodelson@fnal.gov RI Takada, Masahiro/A-4364-2011; Serra, Paolo/G-9678-2014; OI Serra, Paolo/0000-0002-7609-3931; Melchiorri, Alessandro/0000-0001-5326-6003; Pritchard, Jonathan/0000-0003-4127-5353; Miquel, Ramon/0000-0002-6610-4836; Pierpaoli, Elena/0000-0002-7957-8993 NR 81 TC 85 Z9 85 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 J9 ASTROPART PHYS JI Astropart Phys. PD NOV PY 2011 VL 35 IS 4 BP 177 EP 184 DI 10.1016/j.astropartphys.2011.07.002 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 846XU UT WOS:000296937300003 ER PT J AU Buchhave, LA Latham, DW Carter, JA Desert, JM Torres, G Adams, ER Bryson, ST Charbonneau, DB Ciardi, DR Kulesa, C Dupree, AK Fischer, DA Fressin, F Gautier, TN Gilliland, RL Howell, SB Isaacson, H Jenkins, JM Marcy, GW McCarthy, DW Rowe, JF Batalha, NM Borucki, WJ Brown, TM Caldwell, DA Christiansen, JL Cochran, WD Deming, D Dunham, EW Everett, M Ford, EB Fortney, JJ Geary, JC Girouard, FR Haas, MR Holman, MJ Horch, E Klaus, TC Knutson, HA Koch, DG Kolodziejczak, J Lissauer, JJ Machalek, P Mullally, F Still, MD Quinn, SN Seager, S Thompson, SE Van Cleve, J AF Buchhave, Lars A. Latham, David W. Carter, Joshua A. Desert, Jean-Michel Torres, Guillermo Adams, Elisabeth R. Bryson, Stephen T. Charbonneau, David B. Ciardi, David R. Kulesa, Craig Dupree, Andrea K. Fischer, Debra A. Fressin, Francois Gautier, Thomas N., III Gilliland, Ronald L. Howell, Steve B. Isaacson, Howard Jenkins, Jon M. Marcy, Geoffrey W. McCarthy, Donald W. Rowe, Jason F. Batalha, Natalie M. Borucki, William J. Brown, Timothy M. Caldwell, Douglas A. Christiansen, Jessie L. Cochran, William D. Deming, Drake Dunham, Edward W. Everett, Mark Ford, Eric B. Fortney, Jonathan J. Geary, John C. Girouard, Forrest R. Haas, Michael R. Holman, Matthew J. Horch, Elliott Klaus, Todd C. Knutson, Heather A. Koch, David G. Kolodziejczak, Jeffrey Lissauer, Jack J. Machalek, Pavel Mullally, Fergal Still, Martin D. Quinn, Samuel N. Seager, Sara Thompson, Susan E. Van Cleve, Jeffrey TI KEPLER-14b: A MASSIVE HOT JUPITER TRANSITING AN F STAR IN A CLOSE VISUAL BINARY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; stars: individual (Kepler-14b, KIC 10264660, 2MASS J19105011+4719589); techniques: photometric; techniques: spectroscopic ID SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; EXTRASOLAR PLANET; K-DWARF; STELLAR; MISSION; II.; PARAMETERS; ATMOSPHERE; DISCOVERY AB We present the discovery of a hot Jupiter transiting an F star in a close visual (0 ''.3 sky projected angular separation) binary system. The dilution of the host star's light by the nearly equal magnitude stellar companion (similar to 0.5 mag fainter) significantly affects the derived planetary parameters, and if left uncorrected, leads to an underestimate of the radius and mass of the planet by 10% and 60%, respectively. Other published exoplanets, which have not been observed with high-resolution imaging, could similarly have unresolved stellar companions and thus have incorrectly derived planetary parameters. Kepler-14b (KOI-98) has a period of P = 6.790 days and, correcting for the dilution, has a mass of M-p = 8.40(-0.34)(+ 0.35) M-J and a radius of R-p = 1.136(-0.054)(+ 0.073) R-J, yielding a mean density of rho(p) = 7.1 +/- 1.1 g cm(-3). C1 [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Latham, David W.; Carter, Joshua A.; Desert, Jean-Michel; Torres, Guillermo; Adams, Elisabeth R.; Charbonneau, David B.; Dupree, Andrea K.; Fressin, Francois; Geary, John C.; Holman, Matthew J.; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91109 USA. [Kulesa, Craig] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Isaacson, Howard; Marcy, Geoffrey W.; Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jenkins, Jon M.; Rowe, Jason F.; Caldwell, Douglas A.; Christiansen, Jessie L.; Machalek, Pavel; Mullally, Fergal; Thompson, Susan E.; Van Cleve, Jeffrey] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [McCarthy, Donald W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Girouard, Forrest R.; Klaus, Todd C.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Kolodziejczak, Jeffrey] MSFC, Huntsville, AL 35805 USA. [Still, Martin D.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Seager, Sara] MIT, Newton, MA 02159 USA. RP Buchhave, LA (reprint author), Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark. RI Carter, Joshua/A-8280-2013; Caldwell, Douglas/L-7911-2014; OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Caldwell, Douglas/0000-0003-1963-9616; /0000-0001-6545-639X; Fischer, Debra/0000-0003-2221-0861; Fortney, Jonathan/0000-0002-9843-4354 FU Carlsberg Foundation; NASA's Science Mission Directorate; NASA; NASA through JPL/Caltech FX The work of L.A.B. was supported by the Carlsberg Foundation. Funding for this Discovery Mission is provided by NASA's Science Mission Directorate. This paper uses observations obtained with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is also based on observations made with the Spitzer Space Telescope which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was also provided by NASA through an award issued by JPL/Caltech. NR 37 TC 35 Z9 35 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2011 VL 197 IS 1 AR 3 DI 10.1088/0067-0049/197/1/3 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400003 ER PT J AU Cochran, WD Fabrycky, DC Torres, G Fressin, F Desert, JM Ragozzine, D Sasselov, D Fortney, JJ Rowe, JF Brugamyer, EJ Bryson, ST Carter, JA Ciardi, DR Howell, SB Steffen, JH Borucki, WJ Koch, DG Winn, JN Welsh, WF Uddin, K Tenenbaum, P Still, M Seager, S Quinn, SN Mullally, F Miller, N Marcy, GW MacQueen, PJ Lucas, P Lissauer, JJ Latham, DW Knutson, H Kinemuchi, K Johnson, JA Jenkins, JM Isaacson, H Howard, A Horch, E Holman, MJ Henze, CE Haas, MR Gilliland, RL Gautier, TN Ford, EB Fischer, DA Everett, M Endl, M Demory, BO Deming, D Charbonneau, D Caldwell, D Buchhave, L Brown, TM Batalha, N AF Cochran, William D. Fabrycky, Daniel C. Torres, Guillermo Fressin, Francois Desert, Jean-Michel Ragozzine, Darin Sasselov, Dimitar Fortney, Jonathan J. Rowe, Jason F. Brugamyer, Erik J. Bryson, Stephen T. Carter, Joshua A. Ciardi, David R. Howell, Steve B. Steffen, Jason H. Borucki, William. J. Koch, David G. Winn, Joshua N. Welsh, William F. Uddin, Kamal Tenenbaum, Peter Still, M. Seager, Sara Quinn, Samuel N. Mullally, F. Miller, Neil Marcy, Geoffrey W. MacQueen, Phillip J. Lucas, Phillip Lissauer, Jack J. Latham, David W. Knutson, Heather Kinemuchi, K. Johnson, John A. Jenkins, Jon M. Isaacson, Howard Howard, Andrew Horch, Elliott Holman, Matthew J. Henze, Christopher E. Haas, Michael R. Gilliland, Ronald L. Gautier, Thomas N., III Ford, Eric B. Fischer, Debra A. Everett, Mark Endl, Michael Demory, Brice-Oliver Deming, Drake Charbonneau, David Caldwell, Douglas Buchhave, Lars Brown, Timothy M. Batalha, Natalie TI KEPLER-18b, c, AND d: A SYSTEM OF THREE PLANETS CONFIRMED BY TRANSIT TIMING VARIATIONS, LIGHT CURVE VALIDATION, WARM-SPITZER PHOTOMETRY, AND RADIAL VELOCITY MEASUREMENTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; stars: individual (Kepler-18, KIC 8644288, 2MASS J19521906+4444467); techniques: photometric; techniques: spectroscopic ID EXOPLANET HD 189733B; SOLAR-TYPE STARS; LOW-DENSITY; INITIAL CHARACTERISTICS; TERRESTRIAL PLANETS; SECONDARY ECLIPSE; SPACE-TELESCOPE; BLEND SCENARIOS; TARGET STARS; SUPER-EARTHS AB We report the detection of three transiting planets around a Sun-like star, which we designate Kepler-18. The transit signals were detected in photometric data from the Kepler satellite, and were confirmed to arise from planets using a combination of large transit-timing variations (TTVs), radial velocity variations, Warm-Spitzer observations, and statistical analysis of false-positive probabilities. The Kepler-18 star has a mass of 0.97M(circle dot), a radius of 1.1R(circle dot), an effective temperature of 5345 K, and an iron abundance of [Fe/H] = +0.19. The planets have orbital periods of approximately 3.5, 7.6, and 14.9 days. The innermost planet "b" is a "super-Earth" with a mass of 6.9 +/- 3.4M(circle plus), a radius of 2.00 +/- 0.10R(circle plus), and a mean density of 4.9 +/- 2.4 g cm(3). The two outer planets "c" and "d" are both low-density Neptune-mass planets. Kepler-18c has a mass of 17.3 +/- 1.9 M-circle plus, a radius of 5.49 +/- 0.26R(circle plus), and a mean density of 0.59 +/- 0.07 g cm(3), while Kepler-18d has a mass of 16.4 +/- 1.4 M-circle plus, a radius of 6.98 +/- 0.33 R-circle plus and a mean density of 0.27 +/- 0.03 g cm(.)(3) Kepler-18c and Kepler-18d have orbital periods near a 2:1 mean-motion resonance, leading to large and readily detected TTVs. C1 [Cochran, William D.; MacQueen, Phillip J.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Fabrycky, Daniel C.; Fortney, Jonathan J.; Miller, Neil] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Torres, Guillermo; Fressin, Francois; Desert, Jean-Michel; Ragozzine, Darin; Sasselov, Dimitar; Carter, Joshua A.; Quinn, Samuel N.; Latham, David W.; Holman, Matthew J.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brugamyer, Erik J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Winn, Joshua N.; Seager, Sara; Demory, Brice-Oliver] MIT, Dept Phys, Cambridge, MA 02139 USA. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Uddin, Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Tenenbaum, Peter; Mullally, F.; Jenkins, Jon M.; Caldwell, Douglas] ETI Inst, Mountain View, CA 94043 USA. [Still, M.; Kinemuchi, K.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marcy, Geoffrey W.; Knutson, Heather; Isaacson, Howard; Howard, Andrew] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Lucas, Phillip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Johnson, John A.] CALTECH, Dept Astron, Pasadena, CA 91109 USA. [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Buchhave, Lars] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. RP Cochran, WD (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. EM wdc@astro.as.utexas.edu; jdesert@cfa.harvard.edu; jwinn@mit.edu; wfw@kublai.sdsu.edu; kamal.uddin@nasa.gov; Peter.Tenenbaum@nasa.gov; martin.d.still@nasa.gov; seager@mit.edu; fergal.mullally@nasa.gov; Karen.Kinemuchi@nasa.gov; johnjohn@astro.caltech.edu; jjenkins@mail.arc.nasa.gov; horche2@southernct.edu; eford@astro.ufl.edu; debra.fischer@gmail.com; Douglas.A.Caldwell@nasa.gov; natalie.m.batalha@nasa.gov RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015 OI Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Demory, Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X; Fischer, Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183; Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320 FU NASA's Science Mission Directorate; NASA through JPL/Caltech; W. M. Keck Foundation; NASA FX Kepler was competitively selected as the tenth Discovery mission. Funding for the Kepler Mission is provided by NASA's Science Mission Directorate. We are deeply grateful for the very hard work of the entire Kepler team. This research is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 83 TC 95 Z9 95 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2011 VL 197 IS 1 AR 7 DI 10.1088/0067-0049/197/1/7 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400007 ER PT J AU Desert, JM Charbonneau, D Demory, BO Ballard, S Carter, JA Fortney, JJ Cochran, WD Endl, M Quinn, SN Isaacson, HT Fressin, F Buchhave, LA Latham, DW Knutson, HA Bryson, ST Torres, G Rowe, JF Batalha, NM Borucki, WJ Brown, TM Caldwell, DA Christiansen, JL Deming, D Fabrycky, DC Ford, EB Gilliland, RL Gillon, M Haas, MR Jenkins, JM Kinemuchi, K Koch, D Lissauer, JJ Lucas, P Mullally, F MacQueen, PJ Marcy, GW Sasselov, DD Seager, S Still, M Tenenbaum, P Uddin, K Winn, JN AF Desert, Jean-Michel Charbonneau, David Demory, Brice-Olivier Ballard, Sarah Carter, Joshua A. Fortney, Jonathan J. Cochran, William D. Endl, Michael Quinn, Samuel N. Isaacson, Howard T. Fressin, Francois Buchhave, Lars A. Latham, David W. Knutson, Heather A. Bryson, Stephen T. Torres, Guillermo Rowe, Jason F. Batalha, Natalie M. Borucki, William J. Brown, Timothy M. Caldwell, Douglas A. Christiansen, Jessie L. Deming, Drake Fabrycky, Daniel C. Ford, Eric B. Gilliland, Ronald L. Gillon, Michael Haas, Michael R. Jenkins, Jon M. Kinemuchi, Karen Koch, David Lissauer, Jack J. Lucas, Philip Mullally, Fergal MacQueen, Phillip J. Marcy, Geoffrey W. Sasselov, Dimitar D. Seager, Sara Still, Martin Tenenbaum, Peter Uddin, Kamal Winn, Joshua N. TI THE HOT-JUPITER KEPLER-17b: DISCOVERY, OBLIQUITY FROM STROBOSCOPIC STARSPOTS, AND ATMOSPHERIC CHARACTERIZATION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE eclipses; planetary systems; stars: individual (Kepler-17b, KIC 10619192, 2MASS 19533486+4748540); techniques: photometric ID EXTRASOLAR GIANT PLANETS; TRANSIT LIGHT-CURVE; HOBBY-EBERLY TELESCOPE; SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; INITIAL CHARACTERISTICS; SECONDARY ECLIPSE; THERMAL EMISSION; STELLAR ACTIVITY; SPECTRAL MODELS AB This paper reports the discovery and characterization of the transiting hot giant exoplanet Kepler-17b. The planet has an orbital period of 1.486 days, and radial velocity measurements from the Hobby-Eberly Telescope show a Doppler signal of 419.5(-15.6)(+13.3) m s(-1). From a transit-based estimate of the host star's mean density, combined with an estimate of the stellar effective temperature T-eff = 5630 +/- 100 from high-resolution spectra, we infer a stellar host mass of 1.06 +/- 0.07 M-circle dot and a stellar radius of 1.02 +/- 0.03 R-circle dot. We estimate the planet mass and radius to be M-P = 2.45 +/- 0.11 M-J and R-P = 1.31 +/- 0.02 R-J. The host star is active, with dark spots that are frequently occulted by the planet. The continuous monitoring of the star reveals a stellar rotation period of 11.89 days, eight times the planet's orbital period; this period ratio produces stroboscopic effects on the occulted starspots. The temporal pattern of these spot-crossing events shows that the planet's orbit is prograde and the star's obliquity is smaller than 15 degrees. We detected planetary occultations of Kepler-17b with both the Kepler and Spitzer Space Telescopes. We use these observations to constrain the eccentricity, e, and find that it is consistent with a circular orbit (e < 0.011). The brightness temperatures of the planet's infrared bandpasses are T-3.6 mu m = 1880 +/- 100 K and T-4.5 mu m = 1770 +/- 150 K. We measure the optical geometric albedo A(g) in the Kepler bandpass and find A(g) = 0.10 +/- 0.02. The observations are best described by atmospheric models for which most of the incident energy is re-radiated away from the day side. C1 [Desert, Jean-Michel; Charbonneau, David; Ballard, Sarah; Carter, Joshua A.; Quinn, Samuel N.; Fressin, Francois; Latham, David W.; Torres, Guillermo; Lissauer, Jack J.; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Demory, Brice-Olivier; Seager, Sara; Winn, Joshua N.] MIT, Cambridge, MA 02159 USA. [Fortney, Jonathan J.; Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Isaacson, Howard T.; Knutson, Heather A.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Caldwell, Douglas A.; Jenkins, Jon M.; Mullally, Fergal; Tenenbaum, Peter] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Kinemuchi, Karen; Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lucas, Philip] Univ Hertfordshire, Ctr Astrophyiscs Res, Hatfield AL10 9AB, Herts, England. [Uddin, Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Desert, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdesert@cfa.harvard.edu RI Carter, Joshua/A-8280-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Demory, Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA; NASA through JPL/Caltech; W. M. Keck Foundation FX This work is also based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.; Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 80 TC 81 Z9 81 U1 0 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 NOV PY 2011 VL 197 IS 1 AR 14 DI 10.1088/0067-0049/197/1/14 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400014 ER PT J AU Desert, JM Charbonneau, D Fortney, JJ Madhusudhan, N Knutson, HA Fressin, F Deming, D Borucki, WJ Brown, TM Caldwell, D Ford, EB Gilliland, RL Latham, DW Marcy, GW Seager, S AF Desert, Jean-Michel Charbonneau, David Fortney, Jonathan J. Madhusudhan, Nikku Knutson, Heather A. Fressin, Francois Deming, Drake Borucki, William J. Brown, Timothy M. Caldwell, Douglas Ford, Eric B. Gilliland, Ronald L. Latham, David W. Marcy, Geoffrey W. Seager, Sara CA Kepler Sci Team TI THE ATMOSPHERES OF THE HOT-JUPITERS KEPLER-5b AND KEPLER-6b OBSERVED DURING OCCULTATIONS WITH WARM-SPITZER AND KEPLER SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE eclipses; planetary systems; techniques: photometric ID EXTRASOLAR GIANT PLANETS; GROUND-BASED DETECTION; INFRARED ARRAY CAMERA; EXOPLANET HD 189733B; SECONDARY ECLIPSE; THERMAL EMISSION; LIGHT CURVES; INITIAL CHARACTERISTICS; TEMPERATURE INVERSION; THEORETICAL SPECTRA AB This paper reports the detection and the measurements of occultations of the two transiting hot giant exoplanets Kepler-5b and Kepler-6b by their parent stars. The observations are obtained in the near-infrared with Warm-Spitzer Space Telescope and at optical wavelengths by combining more than a year of Kepler photometry. The investigation consists of constraining the eccentricities of these systems and of obtaining broadband emergent photometric data for individual planets. For both targets, the occultations are detected at the 3 sigma level at each wavelength with midoccultation times consistent with circular orbits. The brightness temperatures of these planets are deduced from the infrared observations and reach T-Spitzer = 1930 +/- 100 K and T-Spitzer = 1660 +/- 120 K for Kepler-5b and Kepler-6b, respectively. We measure optical geometric albedos A(g) in the Kepler bandpass and find A(g) = 0.12 +/- 0.04 for Kepler-5b and A(g) = 0.11 +/- 0.04 for Kepler-6b, leading to upper an limit for the Bond albedo of A(B) <= 0.17 in both cases. The observations for both planets are best described by models for which most of the incident energy is redistributed on the dayside, with only less than 10% of the absorbed stellar flux redistributed to the nightside of these planets. C1 [Desert, Jean-Michel; Charbonneau, David; Fressin, Francois; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Madhusudhan, Nikku] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Deming, Drake] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Caldwell, Douglas] SETI Inst, Mountain View, CA 94043 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley Astron Dept, Berkeley, CA 94720 USA. [Seager, Sara] MIT, Newton, MA 02159 USA. RP Desert, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdesert@cfa.harvard.edu RI Kepler, S. O. /H-5901-2012; Caldwell, Douglas/L-7911-2014; OI Kepler, S. O. /0000-0002-7470-5703; Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; Charbonneau, David/0000-0002-9003-484X; /0000-0001-6545-639X FU NASA; NASA through JPL/Caltech; NASA's Science Mission Directorate; W. M. Keck Foundation FX We would like to thank Jessie Christiansen, Brice-Olivier Demory, and Pavel Machaleck for discussions about Kepler photometry, light curves analysis, and interpretation. Thank you to the Spitzer staff at IPAC and in particular to Nancy Silbermann for scheduling the observations of this large program. We would like to thank Jacob Bean for a variety of useful discussions. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is also based on observations made with Kepler which was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors would like to thank the many people who generously gave so much their time to make this Mission a success. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is oper-Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 75 TC 24 Z9 24 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2011 VL 197 IS 1 AR 11 DI 10.1088/0067-0049/197/1/11 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400011 ER PT J AU Endl, M MacQueen, PJ Cochran, WD Brugamyer, EJ Buchhave, LA Rowe, J Lucas, P Isaacson, H Bryson, S Howell, SB Fortney, JJ Hansen, T Borucki, WJ Caldwell, D Christiansen, JL Ciardi, DR Demory, BO Everett, M Ford, EB Haas, MR Holman, MJ Horch, E Jenkins, JM Koch, DJ Lissauer, JJ Machalek, P Still, M Welsh, WF Sanderfer, DT Seader, SE Smith, JC Thompson, SE Twicken, JD AF Endl, Michael MacQueen, Phillip J. Cochran, William D. Brugamyer, Erik J. Buchhave, Lars A. Rowe, Jason Lucas, Phillip Isaacson, Howard Bryson, Steve Howell, Steve B. Fortney, Jonathan J. Hansen, Terese Borucki, William J. Caldwell, Douglas Christiansen, Jessie L. Ciardi, David R. Demory, Brice-Olivier Everett, Mark Ford, Eric B. Haas, Michael R. Holman, Matthew J. Horch, Elliott Jenkins, Jon M. Koch, David J. Lissauer, Jack J. Machalek, Pavel Still, Martin Welsh, William F. Sanderfer, Dwight T. Seader, Shawn E. Smith, Jeffrey C. Thompson, Susan E. Twicken, Joseph D. TI KEPLER-15b: A HOT JUPITER ENRICHED IN HEAVY ELEMENTS AND THE FIRST KEPLER MISSION PLANET CONFIRMED WITH THE HOBBY-EBERLY TELESCOPE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; stars: individual (Kepler-15, KOI-128, KIC 11359879, 2MASS J19444814+4908244); techniques: image processing; techniques: photometric; techniques: radial velocities; techniques: spectroscopic ID TRANSITING-PLANET; LIGHT CURVES; SPACED DATA; STARS; SPECTROMETER; PERFORMANCE; EVOLUTION; DISCOVERY; PROGRAM; SCIENCE AB We report the discovery of Kepler-15b (KOI-128), a new transiting exoplanet detected by NASA's Kepler mission. The transit signal with a period of 4.94 days was detected in the quarter 1 (Q1) Kepler photometry. For the first time, we have used the High Resolution Spectrograph (HRS) at the Hobby-Eberly Telescope (HET) to determine the mass of a Kepler planet via precise radial velocity (RV) measurements. The 24 HET/HRS RVs and 6 additional measurements from the Fibre-fed Echelle Spectrograph spectrograph at the Nordic Optical Telescope reveal a Doppler signal with the same period and phase as the transit ephemeris. We used one HET/HRS spectrum of Kepler-15 taken without the iodine cell to determine accurate stellar parameters. The host star is a metal-rich ([Fe/H] = 0.36 +/- 0.07) G-type main-sequence star with T-eff = 5515 +/- 124 K. The semi-amplitude K of the RV orbit is 78.7(-9.5)(+ 8.5) m s(-1), which yields a planet mass of 0.66 +/- 0.1 M-Jup. The planet has a radius of 0.96 +/- 0.06 R-Jup and a mean bulk density of 0.9 +/- 0.2 g cm(-3). The radius of Kepler-15b is smaller than the majority of transiting planets with similar mass and irradiation level. This suggests that the planet is more enriched in heavy elements than most other transiting giant planets. For Kepler-15b we estimate a heavy element mass of 30-40 M-circle plus. C1 [Endl, Michael; MacQueen, Phillip J.; Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Brugamyer, Erik J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, Denmark Ctr Star & Planet Format, DK-1168 Copenhagen, Denmark. [Lucas, Phillip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Demory, Brice-Olivier] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Jenkins, Jon M.; Sanderfer, Dwight T.; Seader, Shawn E.; Smith, Jeffrey C.; Thompson, Susan E.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Machalek, Pavel] SETI Inst, Mountain View, CA 94043 USA. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Endl, M (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. RI Caldwell, Douglas/L-7911-2014; OI Demory, Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X; Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047 FU NASA's Science Mission Directorate FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We thank the hundreds of people who make this mission successful. The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat at Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. Based in part on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. We also thank the anonymous referee for many helpful suggestions to improve the manuscript. NR 43 TC 20 Z9 20 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2011 VL 197 IS 1 AR 13 DI 10.1088/0067-0049/197/1/13 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400013 ER PT J AU Ford, EB Rowe, JF Fabrycky, DC Carter, JA Holman, MJ Lissauer, JJ Ragozzine, D Steffen, JH Batalha, NM Borucki, WJ Bryson, S Caldwell, DA Dunham, EW Gautier, TN Jenkins, JM Koch, DG Li, J Lucas, P Marcy, GW McCauliff, S Mullally, FR Quintana, E Still, M Tenenbaum, P Thompson, SE Twicken, JD AF Ford, Eric B. Rowe, Jason F. Fabrycky, Daniel C. Carter, Joshua A. Holman, Matthew J. Lissauer, Jack J. Ragozzine, Darin Steffen, Jason H. Batalha, Natalie M. Borucki, William J. Bryson, Steve Caldwell, Douglas A. Dunham, Edward W. Gautier, Thomas N., III Jenkins, Jon M. Koch, David G. Li, Jie Lucas, Philip Marcy, Geoffrey W. McCauliff, Sean Mullally, Fergal R. Quintana, Elisa Still, Martin Tenenbaum, Peter Thompson, Susan E. Twicken, Joseph D. TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. I. STATISTICAL ANALYSIS OF THE FIRST FOUR MONTHS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE methods: statistical; planetary systems; planets and satellites: detection; planets and satellites: dynamical evolution and stability; techniques: miscellaneous ID EXTRASOLAR PLANETS; LIGHT CURVES; LOW-MASS; CANDIDATES; SYSTEM; DETECTABILITY; EXOMOONS; DENSITY; TRIPLE; STARS AB The architectures of multiple planet systems can provide valuable constraints on models of planet formation, including orbital migration, and excitation of orbital eccentricities and inclinations. NASA's Kepler mission has identified 1235 transiting planet candidates. The method of transit timing variations (TTVs) has already confirmed seven planets in two planetary systems. We perform a transit timing analysis of the Kepler planet candidates. We find that at least similar to 11% of planet candidates currently suitable for TTV analysis show evidence suggestive of TTVs, representing at least similar to 65 TTV candidates. In all cases, the time span of observations must increase for TTVs to provide strong constraints on planet masses and/or orbits, as expected based on N-body integrations of multiple transiting planet candidate systems (assuming circular and coplanar orbits). We find the fraction of planet candidates showing TTVs in this data set does not vary significantly with the number of transiting planet candidates per star, suggesting significant mutual inclinations and that many stars with a single transiting planet should host additional non-transiting planets. We anticipate that Kepler could confirm (or reject) at least similar to 12 systems with multiple transiting planet candidates via TTVs. Thus, TTVs will provide a powerful tool for confirming transiting planets and characterizing the orbital dynamics of low-mass planets. If Kepler observations were extended to at least seven years, then TTVs would provide much more precise constraints on the dynamics of systems with multiple transiting planets and would become sensitive to planets with orbital periods extending into the habitable zone of solar-type stars. C1 [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Rowe, Jason F.; Caldwell, Douglas A.; Jenkins, Jon M.; Li, Jie; Mullally, Fergal R.; Quintana, Elisa; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.] SETI Inst, Mountain View, CA 94043 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Carter, Joshua A.; Holman, Matthew J.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [McCauliff, Sean] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ford, EB (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32111 USA. EM eford@astro.ufl.edu RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU National Aeronautics and Space Administration [NNX08AR04G, HF-51272.01-A, HF-51267.01-A, NAS 5-26555]; National Science Foundation [0707203]; Space Telescope Science Institute FX Funding for this mission is provided by NASA's Science Mission Directorate. We thank the entire Kepler team for the many years of work that is proving so successful. We thank David Latham for a careful reading of the manuscript. E.B.F. acknowledges support by the National Aeronautics and Space Administration under grant NNX08AR04G issued through the Kepler Participating Scientist Program. This material is based upon work supported by the National Science Foundation under Grant No. 0707203. D.C.F. and J.A.C. acknowledge support for this work was provided by NASA through Hubble Fellowship grants HF-51272.01-A and HF-51267.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 35 TC 46 Z9 46 U1 0 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 NOV PY 2011 VL 197 IS 1 AR 2 DI 10.1088/0067-0049/197/1/2 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400002 ER PT J AU Fortney, JJ Demory, BO Desert, JM Rowe, J Marcy, GW Isaacson, H Buchhave, LA Ciardi, D Gautier, TN Batalha, NM Caldwell, DA Bryson, ST Nutzman, P Jenkins, JM Howard, A Charbonneau, D Knutson, HA Howell, SB Everett, M Fressin, F Deming, D Borucki, WJ Brown, TM Ford, EB Gilliland, RL Latham, DW Miller, N Seager, S Fischer, DA Koch, D Lissauer, JJ Haas, MR Still, M Lucas, P Gillon, M Christiansen, JL Geary, JC AF Fortney, Jonathan J. Demory, Brice-Olivier Desert, Jean-Michel Rowe, Jason Marcy, Geoffrey W. Isaacson, Howard Buchhave, Lars A. Ciardi, David Gautier, Thomas N. Batalha, Natalie M. Caldwell, Douglas A. Bryson, Stephen T. Nutzman, Philip Jenkins, Jon M. Howard, Andrew Charbonneau, David Knutson, Heather A. Howell, Steve B. Everett, Mark Fressin, Francois Deming, Drake Borucki, William J. Brown, Timothy M. Ford, Eric B. Gilliland, Ronald L. Latham, David W. Miller, Neil Seager, Sara Fischer, Debra A. Koch, David Lissauer, Jack J. Haas, Michael R. Still, Martin Lucas, Philip Gillon, Michael Christiansen, Jessie L. Geary, John C. TI DISCOVERY AND ATMOSPHERIC CHARACTERIZATION OF GIANT PLANET KEPLER-12b: AN INFLATED RADIUS OUTLIER SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planets and satellites: atmospheres; stars: individual (Kepler-12, KOI-20, KIC 11804465); techniques: spectroscopic ID TRANSITING EXTRASOLAR PLANETS; SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; LIGHT-CURVE PROJECT; B-LIKE PLANETS; HOT JUPITERS; LOW-DENSITY; INITIAL CHARACTERISTICS; SECONDARY ECLIPSE; THERMAL STRUCTURE AB We report the discovery of planet Kepler-12b (KOI-20), which at 1.695 +/- 0.030 R-J is among the handful of planets with super-inflated radii above 1.65 R-J. Orbiting its slightly evolved G0 host with a 4.438 day period, this 0.431 +/- 0.041 M-J planet is the least irradiated within this largest-planet-radius group, which has important implications for planetary physics. The planet's inflated radius and low mass lead to a very low density of 0.111 +/- 0.010 g cm(-3). We detect the occultation of the planet at a significance of 3.7 sigma in the Kepler bandpass. This yields a geometric albedo of 0.14 +/- 0.04; the planetary flux is due to a combination of scattered light and emitted thermal flux. We use multiple observations with Warm Spitzer to detect the occultation at 7 sigma and 4 sigma in the 3.6 and 4.5 mu m bandpasses, respectively. The occultation photometry timing is consistent with a circular orbit at e < 0.01 (1s) and e < 0.09 (3 sigma). The occultation detections across the three bands favor an atmospheric model with no dayside temperature inversion. The Kepler occultation detection provides significant leverage, but conclusions regarding temperature structure are preliminary, given our ignorance of opacity sources at optical wavelengths in hot Jupiter atmospheres. If Kepler-12b and HD 209458b, which intercept similar incident stellar fluxes, have the same heavy-element masses, the interior energy source needed to explain the large radius of Kepler-12b is three times larger than that of HD 209458b. This may suggest that more than one radius-inflation mechanism is at work for Kepler-12b or that it is less heavy-element rich than other transiting planets. C1 [Fortney, Jonathan J.; Nutzman, Philip; Miller, Neil] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Demory, Brice-Olivier; Seager, Sara] MIT, Cambridge, MA 02139 USA. [Desert, Jean-Michel; Buchhave, Lars A.; Charbonneau, David; Fressin, Francois; Latham, David W.; Geary, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rowe, Jason; Caldwell, Douglas A.; Jenkins, Jon M.; Christiansen, Jessie L.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marcy, Geoffrey W.; Isaacson, Howard; Howard, Andrew; Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Ciardi, David] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Gautier, Thomas N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Gillon, Michael] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland. RP Fortney, JJ (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. EM jfortney@ucolick.org RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Demory, Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X; Fischer, Debra/0000-0003-2221-0861; Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354 FU NASA [NNX09AC22G]; NASA's Science Mission Directorate; NASA through JPL/Caltech FX J.J.F. acknowledges the support of the Kepler Participating Scientist's program via NASA grant NNX09AC22G. Kepler was competitively selected as the tenth Discovery mission. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. We thank the many people who gave so generously of their time to make the Kepler mission a success. We thank Carly Chubak for cross-correlation analyses of the Keck spectra for companions. This work incorporates observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Finally, the authors extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 103 TC 40 Z9 41 U1 0 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 NOV PY 2011 VL 197 IS 1 AR 9 DI 10.1088/0067-0049/197/1/9 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400009 ER PT J AU Fressin, F Torres, G Desert, JM Charbonneau, D Batalha, NM Fortney, JJ Rowe, JF Allen, C Borucki, WJ Brown, TM Bryson, ST Ciardi, DR Cochran, WD Deming, D Dunham, EW Fabrycky, DC Gautier, TN Gilliland, RL Henze, CE Holman, MJ Howell, SB Jenkins, JM Kinemuchi, K Knutson, H Koch, DG Latham, DW Lissauer, JJ Marcy, GW Ragozzine, D Sasselov, DD Still, M Tenenbaum, P Uddin, K AF Fressin, Francois Torres, Guillermo Desert, Jean-Michel Charbonneau, David Batalha, Natalie M. Fortney, Jonathan J. Rowe, Jason F. Allen, Christopher Borucki, William J. Brown, Timothy M. Bryson, Stephen T. Ciardi, David R. Cochran, William D. Deming, Drake Dunham, Edward W. Fabrycky, Daniel C. Gautier, Thomas N., III Gilliland, Ronald L. Henze, Christopher E. Holman, Matthew J. Howell, Steve B. Jenkins, Jon M. Kinemuchi, Karen Knutson, Heather Koch, David G. Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Ragozzine, Darin Sasselov, Dimitar D. Still, Martin Tenenbaum, Peter Uddin, Kamal TI KEPLER-10 c: A 2.2 EARTH RADIUS TRANSITING PLANET IN A MULTIPLE SYSTEM SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE binaries: eclipsing; planetary systems; stars: individual (Kepler-10, KOI-072, KIC 11904151); stars: statistics ID SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; LOW-MASS; OBSERVATIONAL EVIDENCE; SECONDARY ECLIPSE; BLEND SCENARIOS; LIGHT CURVES; WARM SPITZER; CANDIDATES; ATMOSPHERE AB The Kepler mission has recently announced the discovery of Kepler-10 b, the smallest exoplanet discovered to date and the first rocky planet found by the spacecraft. A second, 45 day period transit-like signal present in the photometry from the first eight months of data could not be confirmed as being caused by a planet at the time of that announcement. Here we apply the light curve modeling technique known as BLENDER to explore the possibility that the signal might be due to an astrophysical false positive (blend). To aid in this analysis we report the observation of two transits with the Spitzer Space Telescope at 4.5 mu m. When combined, they yield a transit depth of 344 +/- 85 ppm that is consistent with the depth in the Kepler passband (376 +/- 9 ppm, ignoring limb darkening), which rules out blends with an eclipsing binary of a significantly different color than the target. Using these observations along with other constraints from high-resolution imaging and spectroscopy, we are able to exclude the vast majority of possible false positives. We assess the likelihood of the remaining blends, and arrive conservatively at a false alarm rate of 1.6 x 10(-5) that is small enough to validate the candidate as a planet (designated Kepler-10 c) with a very high level of confidence. The radius of this object is measured to be R-p = 2.227(-0.057)(+ 0.052) R-circle plus (in which the error includes the uncertainty in the stellar properties), but currently available radial-velocity measurements only place an upper limit on its mass of about 20 M-circle plus. Kepler-10 c represents another example (with Kepler-9 d and Kepler-11 g) of statistical "validation" of a transiting exoplanet, as opposed to the usual "confirmation" that can take place when the Doppler signal is detected or transit timing variations are measured. It is anticipated that many of Kepler's smaller candidates will receive a similar treatment since dynamical confirmation may be difficult or impractical with the sensitivity of current instrumentation. C1 [Fressin, Francois; Torres, Guillermo; Desert, Jean-Michel; Charbonneau, David; Holman, Matthew J.; Latham, David W.; Ragozzine, Darin; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. [Fortney, Jonathan J.; Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Allen, Christopher; Tenenbaum, Peter; Uddin, Kamal] Uddin Orbital Sci Corp, Moffett Field, CA 94035 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Ciardi, David R.; Koch, David G.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Jenkins, Jon M.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kinemuchi, Karen; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Knutson, Heather; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ffressin@cfa.harvard.edu RI Ragozzine, Darin/C-4926-2013; OI Fortney, Jonathan/0000-0002-9843-4354; Ciardi, David/0000-0002-5741-3047; Charbonneau, David/0000-0002-9003-484X; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA through JPL/Caltech; NASA FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. This research has made use of the facilities at the NASA Advanced Supercomputing Division (NASA Ames Research Center), and is based also on observations made with the Spitzer Space Telescope which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We thank Mukremin Kilic and Rosanne Di Stefano for helpful discussions about white dwarfs, and the anonymous referee for constructive comments. NR 49 TC 60 Z9 60 U1 2 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2011 VL 197 IS 1 AR 5 DI 10.1088/0067-0049/197/1/5 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400005 ER PT J AU Lissauer, JJ Ragozzine, D Fabrycky, DC Steffen, JH Ford, EB Jenkins, JM Shporer, A Holman, MJ Rowe, JF Quintana, EV Batalha, NM Borucki, WJ Bryson, ST Caldwell, DA Carter, JA Ciardi, D Dunham, EW Fortney, JJ Gautier, TN Howell, SB Koch, DG Latham, DW Marcy, GW Morehead, RC Sasselov, D AF Lissauer, Jack J. Ragozzine, Darin Fabrycky, Daniel C. Steffen, Jason H. Ford, Eric B. Jenkins, Jon M. Shporer, Avi Holman, Matthew J. Rowe, Jason F. Quintana, Elisa V. Batalha, Natalie M. Borucki, William J. Bryson, Stephen T. Caldwell, Douglas A. Carter, Joshua A. Ciardi, David Dunham, Edward W. Fortney, Jonathan J. Gautier, Thomas N., III Howell, Steve B. Koch, David G. Latham, David W. Marcy, Geoffrey W. Morehead, Robert C. Sasselov, Dimitar TI ARCHITECTURE AND DYNAMICS OF KEPLER'S CANDIDATE MULTIPLE TRANSITING PLANET SYSTEMS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE celestial mechanics; planets and satellites: dynamical evolution and stability; planets and satellites: fundamental parameters; planets and satellites: general; planetary systems ID HOT SUPER-EARTHS; 1ST 4 MONTHS; EXTRASOLAR PLANETS; ORBITAL ECCENTRICITIES; SOLAR-SYSTEM; HARPS SEARCH; LIGHT CURVES; SHORT-PERIOD; LOW-MASS; RESONANCES AB About one-third of the similar to 1200 transiting planet candidates detected in the first four months of Kepler data are members of multiple candidate systems. There are 115 target stars with two candidate transiting planets, 45 with three, 8 with four, and 1 each with five and six. We characterize the dynamical properties of these candidate multi-planet systems. The distribution of observed period ratios shows that the vast majority of candidate pairs are neither in nor near low-order mean-motion resonances. Nonetheless, there are small but statistically significant excesses of candidate pairs both in resonance and spaced slightly too far apart to be in resonance, particularly near the 2:1 resonance. We find that virtually all candidate systems are stable, as tested by numerical integrations that assume a nominal mass-radius relationship. Several considerations strongly suggest that the vast majority of these multi-candidate systems are true planetary systems. Using the observed multiplicity frequencies, we find that a single population of planetary systems that matches the higher multiplicities underpredicts the number of singly transiting systems. We provide constraints on the true multiplicity and mutual inclination distribution of the multi-candidate systems, revealing a population of systems with multiple super-Earth-size and Neptune-size planets with low to moderate mutual inclinations. C1 [Lissauer, Jack J.; Jenkins, Jon M.; Rowe, Jason F.; Quintana, Elisa V.; Caldwell, Douglas A.; Morehead, Robert C.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ragozzine, Darin; Holman, Matthew J.; Carter, Joshua A.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.; Fortney, Jonathan J.; Latham, David W.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Ford, Eric B.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Ciardi, David] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Lissauer, JJ (reprint author), NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Jack.Lissauer@nasa.gov RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [HF-51272.01-A, HF-51267.01-A]; STScI [NAS 5-26555] FX Kepler was competitively selected as NASA's tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. The authors thank the many people who gave so generously of their time to make the Kepler mission a success. D.C.F. and J.A.C. acknowledge NASA support through Hubble Fellowship grants HF-51272.01-A and HF-51267.01-A, respectively, awarded by STScI, operated by AURA under contract NAS 5-26555. We thank Bill Cochran, Avi Loeb, Hanno Rein, Subo Dong, and Bill Welsh for valuable discussions and Kevin Zahnle, Tom Greene, Andrew Youdin, and an anonymous reviewer for constructive comments on the manuscript. Numerical integrations to test the stability of nominal planetary systems were run on the supercomputer Pleiades at University of California, Santa Cruz. NR 83 TC 266 Z9 267 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2011 VL 197 IS 1 AR 8 DI 10.1088/0067-0049/197/1/8 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400008 ER PT J AU Moorhead, AV Ford, EB Morehead, RC Rowe, J Borucki, WJ Batalha, NM Bryson, ST Caldwell, DA Fabrycky, DC Gautier, TN Koch, DG Holman, MJ Jenkins, J Li, J Lissauer, JJ Lucas, P Marcy, GW Quinn, SN Quintana, E Ragozzine, D Shporer, A Still, M Torres, G AF Moorhead, Althea V. Ford, Eric B. Morehead, Robert C. Rowe, Jason Borucki, William J. Batalha, Natalie M. Bryson, Stephen T. Caldwell, Douglas A. Fabrycky, Daniel C. Gautier, Thomas N., III Koch, David G. Holman, Matthew J. Jenkins, Jonm. Li, Jie Lissauer, Jack J. Lucas, Philip Marcy, Geoffrey W. Quinn, Samuel N. Quintana, Elisa Ragozzine, Darin Shporer, Avi Still, Martin Torres, Guillermo TI THE DISTRIBUTION OF TRANSIT DURATIONS FOR KEPLER PLANET CANDIDATES AND IMPLICATIONS FOR THEIR ORBITAL ECCENTRICITIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planets and satellites: fundamental parameters ID 1ST 4 MONTHS; EXTRASOLAR PLANETS; LIGHT CURVES; TIMING VARIATIONS; HOT JUPITERS; SUPER-EARTHS; BINARY; SCATTERING; SYSTEMS; STARS AB Doppler planet searches have discovered that giant planets follow orbits with a wide range of orbital eccentricities, revolutionizing theories of planet formation. The discovery of hundreds of exoplanet candidates by NASA's Kepler mission enables astronomers to characterize the eccentricity distribution of small exoplanets. Measuring the eccentricity of individual planets is only practical in favorable cases that are amenable to complementary techniques (e.g., radial velocities, transit timing variations, occultation photometry). Yet even in the absence of individual eccentricities, it is possible to study the distribution of eccentricities based on the distribution of transit durations (relative to the maximum transit duration for a circular orbit). We analyze the transit duration distribution of Kepler planet candidates. We find that for host stars with T-eff > 5100K we cannot invert this to infer the eccentricity distribution at this time due to uncertainties and possible systematics in the host star densities. With this limitation in mind, we compare the observed transit duration distribution with models to rule out extreme distributions. If we assume a Rayleigh eccentricity distribution for Kepler planet candidates, then we find best fits with a mean eccentricity of 0.1-0.25 for host stars with T-eff <= 5100 K. We compare the transit duration distribution for different subsets of Kepler planet candidates and discuss tentative trends with planetary radius and multiplicity. High-precision spectroscopic follow-up observations for a large sample of host stars will be required to confirm which trends are real and which are the results of systematic errors in stellar radii. Finally, we identify planet candidates that must be eccentric or have a significantly underestimated stellar radius. C1 [Moorhead, Althea V.; Ford, Eric B.; Morehead, Robert C.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA. [Rowe, Jason; Caldwell, Douglas A.; Jenkins, Jonm.; Li, Jie; Quintana, Elisa] SETI Inst, Mountain View, CA 94043 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Holman, Matthew J.; Quinn, Samuel N.; Ragozzine, Darin; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lucas, Philip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Marcy, Geoffrey W.; Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Shporer, Avi] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Moorhead, AV (reprint author), Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA. EM altheam@astro.ufl.edu RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU National Aeronautics and Space Administration [NNX08AR04G]; NASA's Science Mission Directorate FX We thank Bill Cochran, Dave Latham, and Tim Brown for their many helpful suggestions and the latter two for their assistance with the Kepler Input Catalog, on which this work relies. We thank the entire Kepler team for the many years of work that is proving so successful. This material is based on work supported by the National Aeronautics and Space Administration under grant NNX08AR04G issued through the Kepler Participating Scientist Program. Funding for this mission is provided by NASA's Science Mission Directorate. NR 41 TC 63 Z9 63 U1 0 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 NOV PY 2011 VL 197 IS 1 AR 1 DI 10.1088/0067-0049/197/1/1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400001 ER PT J AU Welsh, WF Orosz, JA Aerts, C Brown, TM Brugamyer, E Cochran, WD Gilliland, RL Guzik, JA Kurtz, DW Latham, DW Marcy, GW Quinn, SN Zima, W Allen, C Batalha, NM Bryson, S Buchhave, LA Caldwell, DA Gautier, TN Howell, SB Kinemuchi, K Ibrahim, KA Isaacson, H Jenkins, JM Prsa, A Still, M Street, R Wohler, B Koch, DG Borucki, WJ AF Welsh, William F. Orosz, Jerome A. Aerts, Conny Brown, Timothy M. Brugamyer, Erik Cochran, William D. Gilliland, Ronald L. Guzik, Joyce Ann Kurtz, D. W. Latham, David W. Marcy, Geoffrey W. Quinn, Samuel N. Zima, Wolfgang Allen, Christopher Batalha, Natalie M. Bryson, Steve Buchhave, Lars A. Caldwell, Douglas A. Gautier, Thomas N., III Howell, Steve B. Kinemuchi, K. Ibrahim, Khadeejah A. Isaacson, Howard Jenkins, Jon M. Prsa, Andrej Still, Martin Street, Rachel Wohler, Bill Koch, David G. Borucki, William J. TI KOI-54: THE KEPLER DISCOVERY OF TIDALLY EXCITED PULSATIONS AND BRIGHTENINGS IN A HIGHLY ECCENTRIC BINARY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE binaries: close; binaries: spectroscopic; stars: individual (KID 8112039, HD 187091, 2MASS J19461553+4356513); stars: oscillations; stars: variables: general ID CLOSE BINARIES; INITIAL CHARACTERISTICS; SPECTROSCOPIC BINARIES; ORBITAL PARAMETERS; CADENCE DATA; STELLAR; SYSTEMS; EVOLUTION; OPACITIES; SCIENCE AB Kepler observations of the star HD 187091 (KIC 8112039, hereafter KOI-54) revealed a remarkable light curve exhibiting sharp periodic brightening events every 41.8 days with a superimposed set of oscillations forming a beating pattern in phase with the brightenings. Spectroscopic observations revealed that this is a binary star with a highly eccentric orbit, e = 0.83. We are able to match the Kepler light curve and radial velocities with a nearly face-on (i = 5 degrees.5) binary star model in which the brightening events are caused by tidal distortion and irradiation of nearly identical A stars during their close periastron passage. The two dominant oscillations in the light curve, responsible for the beating pattern, have frequencies that are the 91st and 90th harmonic of the orbital frequency. The power spectrum of the light curve, after removing the binary star brightening component, reveals a large number of pulsations, 30 of which have a signal-to-noise ratio greater than or similar to 7. Nearly all of these pulsations have frequencies that are either integer multiples of the orbital frequency or are tidally split multiples of the orbital frequency. This pattern of frequencies unambiguously establishes the pulsations as resonances between the dynamic tides at periastron and the free oscillation modes of one or both of the stars. KOI-54 is only the fourth star to show such a phenomenon and is by far the richest in terms of excited modes. C1 [Welsh, William F.; Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Aerts, Conny; Zima, Wolfgang] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Aerts, Conny; Zima, Wolfgang] Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Brown, Timothy M.; Street, Rachel] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Brown, Timothy M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Brugamyer, Erik; Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Brugamyer, Erik; Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Guzik, Joyce Ann] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England. [Latham, David W.; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Allen, Christopher; Ibrahim, Khadeejah A.; Wohler, Bill] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Caldwell, Douglas A.; Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kinemuchi, K.; Still, Martin] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. RP Welsh, WF (reprint author), San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. EM wfw@sciences.sdsu.edu RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars A./0000-0003-1605-5666 FU NASA, Science Mission Directorate; NASA [NNX08AR14G]; European Research Council under the European Community [227224]; W.M. Keck Foundation FX Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. The authors acknowledge support from the Kepler Participating Scientists Program via NASA grant NNX08AR14G. C.A. and W.Z. received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 227224 (PROSPERITY). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank Gur Windmiller for general assistance and for a careful reading of this manuscript. We especially thank the many members of the Kepler team whose hard work made these observation possible. Finally, we thank the anonymous referee for a thorough review of this paper. NR 38 TC 69 Z9 69 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 NOV PY 2011 VL 197 IS 1 AR 4 DI 10.1088/0067-0049/197/1/4 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 846BO UT WOS:000296872400004 ER PT J AU Beckman, NG Muller-Landau, HC AF Beckman, Noelle G. Muller-Landau, Helene C. TI Linking fruit traits to variation in predispersal vertebrate seed predation, insect seed predation, and pathogen attack SO ECOLOGY LA English DT Article DE fruit development; fruit morphology; germination; Janzen-Connell effects; natural enemies; Panama; plant traits; predispersal seed mortality; seed survival ID MOIST TROPICAL FOREST; DISPERSAL; PLANT; SIZE; TREE; GERMINATION; DIVERSITY; HERBIVORY; DEFENSE; DISEASE AB The importance of vertebrates, invertebrates, and pathogens for plant communities has long been recognized, but their absolute and relative importance in early recruitment of multiple coexisting tropical plant species has not been quantified. Further, little is known about the relationship of fruit traits to seed mortality due to natural enemies in tropical plants. To investigate the influences of vertebrates, invertebrates, and pathogens on reproduction of seven canopy plant species varying in fruit traits, we quantified reductions in fruit development and seed germination due to vertebrates, invertebrates, and fungal pathogens through experimental removal of these enemies using canopy exclosures, insecticide, and fungicide, respectively. We also measured morphological fruit traits hypothesized to mediate interactions of plants with natural enemies of seeds. Vertebrates, invertebrates, and fungi differentially affected predispersal seed mortality depending on the plant species. Fruit morphology explained some variation among species; species with larger fruit and less physical protection surrounding seeds exhibited greater negative effects of fungi on fruit development and germination and experienced reduced seed survival integrated over fruit development and germination in response to vertebrates. Within species, variation in seed size also contributed to variation in natural enemy effects on seed viability. Further, seedling growth was higher for seeds that developed in vertebrate exclosures for Anacardium excelsum and under the fungicide treatment for Castilla elastica, suggesting that predispersal effects of natural enemies may carry through to the seedling stage. This is the first experimental test of the relative effects of vertebrates, invertebrates, and pathogens on seed survival in the canopy. This study motivates further investigation to determine the generality of our results for plant communities. If there is strong variation in natural enemy attack among species related to differences in fruit morphology, then quantification of fruit traits will aid in predicting the outcomes of interactions between plants and their natural enemies. This is particularly important in tropical forests, where high species diversity makes it logistically impossible to study every plant life history stage of every species. C1 [Beckman, Noelle G.; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Unit 9100, Dpo, AA 34002 USA. [Beckman, Noelle G.] Univ Minnesota Twin Cities, St Paul, MN 55108 USA. RP Beckman, NG (reprint author), Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA. EM nbeckman2@unl.edu RI Beckman, Noelle/E-5554-2011 OI Beckman, Noelle/0000-0001-5822-0610 FU National Science Foundation; University of Minnesota Graduate School; University of Minnesota Department of Ecology, Evolution and Behavior; Smithsonian Tropical Research Institute; Bell Museum of Natural History; HSBC FX We thank Jim Dalling, Linda Kinkel, Claudia Neuhauser, David Tilman, Sunshine Van Bael, Marta Vargas, Sandford Weisberg, and S. J. Wright for invaluable advice. We thank Rebeca Acosta, Matt Certo, Sophia Christoforides, Amy Dickson, Reina Heinz, Bernardo Lopez, Christopher Moore, and Serica Zwack for field and laboratory assistance. The Smithsonian Tropical Research Institute provided logistical support. We are grateful for the financial support of the National Science Foundation (Graduate Research Fellowship to N. G. Beckman), the University of Minnesota Graduate School (Doctoral Dissertation Fellowship and International Research Grant to N. G. Beckman), the University of Minnesota Department of Ecology, Evolution and Behavior (Block Grant to N. G. Beckman), the Smithsonian Tropical Research Institute (Supplementary Award to N. G. Beckman), the Bell Museum of Natural History (Dayton Natural History Fund to N. G. Beckman), and the HSBC Climate Partnership (H. C. Muller-Landau). NR 61 TC 12 Z9 12 U1 3 U2 43 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD NOV PY 2011 VL 92 IS 11 BP 2131 EP 2140 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 840GB UT WOS:000296426000014 PM 22164837 ER PT J AU Wang, XG Wiegand, T Wolf, A Howe, R Davies, SJ Hao, ZQ AF Wang, Xugao Wiegand, Thorsten Wolf, Amy Howe, Robert Davies, Stuart J. Hao, Zhanqing TI Spatial patterns of tree species richness in two temperate forests SO JOURNAL OF ECOLOGY LA English DT Article DE aggregation; Changbaishan; determinants of plant community diversity and structure; habitat heterogeneity; Possion processes; temperate forest; Thomas processes; Wabikon ID AREA RELATIONSHIP; RAIN-FOREST; HABITAT ASSOCIATIONS; NORTHEASTERN CHINA; TROPICAL FORESTS; POINT PATTERNS; BETA-DIVERSITY; SOIL CHEMISTRY; NEUTRAL THEORY; DISTRIBUTIONS AB 1. The relative contribution of external vs. internal clustering mechanisms for determining community structure and its manifestations has been the subject of a continuous debate, but few attempts have been made to examine their single and joint effects in a compound process model. 2. In this study, we tested four a priori hypotheses on the relative importance of habitat heterogeneity (topography and soil) and internal clustering mechanisms such as dispersal limitation on the species- area relationship (SAR) in two fully mapped 25-ha plots of temperate forests in the Changbaishan (CBS) Nature Reserve, China, and the Chequamegon-Nicolet National Forest in Wisconsin, USA. 3. We used the distance decay curve to test the generality of the results obtained for the SAR. To find out if the relative importance of internal and external clustering mechanisms changed with life stage, we conducted separate analyses for small, large and all trees. 4. Model selection favoured the most complex hypothesis that assumed an influence of both habitat heterogeneity and internal clustering on SAR and the distance decay curve. For the CBS plot, which shows weak topographical structuring, models were consistent with data only if soil factors were included into assessment of habitat heterogeneity. At the Wabikon plot, we could not test soil variables, but inclusion of topographical variables substantially improved the fit of the distance decay curve. 5. In general, the results of the SAR agreed with those of the distance decay curve, but the latter was sensitive to positive habitat-mediated species associations. The SAR, but not distance decay, distinguished among competing hypotheses for the community of large trees at CBS, where species exhibited only weak clustering. 6. Contrary to our expectations, we did not find substantial differences in the relative importance of internal and external clustering mechanisms with life stage. 7. Synthesis. Our analysis of spatial community structure for two relatively diverse temperate forests revealed that the factors governing spatial community structure may not substantially differ from those in highly diverse tropical forests. This result adds to our understanding of the ecological processes underlying the spatial diversity structure in natural forest communities. C1 [Wang, Xugao; Hao, Zhanqing] Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110164, Peoples R China. [Wiegand, Thorsten] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04301 Leipzig, Germany. [Wolf, Amy; Howe, Robert] Univ Wisconsin, Dept Nat & Appl Sci, Green Bay, WI 54311 USA. [Davies, Stuart J.] Harvard Univ, Ctr Trop Forest Sci, Boston, MA 02131 USA. [Davies, Stuart J.] Smithsonian Trop Res Inst, Boston, MA 02131 USA. RP Hao, ZQ (reprint author), Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110164, Peoples R China. EM hzq@iae.ac.cn RI wang, xugao/B-1111-2015; Wiegand, Thorsten/H-5877-2016 OI wang, xugao/0000-0003-1207-8852; Wiegand, Thorsten/0000-0002-3721-2248 FU Chinese Academy of Sciences [KZCX2-YW-QN402, KSCX2-EW-Z-5, KZCX2-EW-401]; National Natural Science Foundation of China [40971286]; National Key Technologies R&D Program of China [2008BAC39B02]; ERC [233066]; Center for Tropical Forest Science of the Smithsonian Tropical Research Institute; HSBC; Cofrin Center for Biodiversity FX We thank the CBS and Wabikon plot census and data management teams, the latter including many student assistants from the University of Wisconsin-Green Bay. In particular, we thank Buhang Li, Ji Ye, Fei Lin, Zuoqiang Yuan, Xuejiao Bai, Liwei Wang and Dingliang Xing for their field work and data collection in the CBS plot. At the Wabikon plot, Gary Fewless, Kathryn Corio and Juniper Sundance were instrumental in collecting and managing the data. This study was sponsored by the Knowledge Innovation Program of the Chinese Academy of Sciences (KZCX2-YW-QN402, KSCX2-EW-Z-5 and KZCX2-EW-401), the National Natural Science Foundation of China (40971286) and the National Key Technologies R&D Program of China (2008BAC39B02). The ERC advanced grant 233066 supported travelling of X.W. The Center for Tropical Forest Science of the Smithsonian Tropical Research Institute and the HSBC Climate Partnership provided support for X.W. and for establishment of the Wabikon Plot. Primary funding for the Wabikon Plot was provided by the Cofrin Center for Biodiversity with additional support from the Department of Natural and Applied Sciences at the University of Wisconsin-Green Bay. We are grateful for permission and important logistic contributions by the U.S. Forest Service, particularly Chequamegon-Nicolet National Forest ecologists Linda Parker and Steven Janke. Other significant contributors to the project include Richard Condit, Steve Dhein and Kimberlee McKeefry. NR 55 TC 26 Z9 37 U1 9 U2 69 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD NOV PY 2011 VL 99 IS 6 BP 1382 EP 1393 DI 10.1111/j.1365-2745.2011.01857.x PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 840FR UT WOS:000296425000009 ER PT J AU Kanagaraj, R Wiegand, T Comita, LS Huth, A AF Kanagaraj, Rajapandian Wiegand, Thorsten Comita, Liza S. Huth, Andreas TI Tropical tree species assemblages in topographical habitats change in time and with life stage SO JOURNAL OF ECOLOGY LA English DT Article DE environmental heterogeneity; habitat preference; multivariate regression tree analysis; plant population and community dynamics; regeneration niche; species assemblages; topography; tropical forest diversity ID MULTIVARIATE REGRESSION TREES; BORNEAN RAIN-FOREST; NEOTROPICAL FOREST; DENSITY-DEPENDENCE; SOIL NUTRIENTS; BETA DIVERSITY; ASSOCIATIONS; ABUNDANCE; PATTERNS; NICHE AB 1. Recent studies have documented shifts in habitat associations of single tropical tree species from one life stage to the next. However, the community-level consequences of such shifts have not been investigated, and it is not clear whether they would amplify, neutralize or completely alter habitat structuring during the transitions to the adult community. 2. We compared habitat-driven species assemblages at three life stages (i.e. recruitment, juvenile and reproductive stages) and six censuses for tree and shrub species in a fully censused 50-ha plot of Panamanian lowland forest. Habitat types were determined using multivariate regression trees that group areas with similar species composition (i.e. species assemblages) according to their topographical characteristics. 3. Three topographical variables (a topographical wetness index, slope and elevation) were major determinants of species assemblages. When analysing individuals of all life stages together, we found a distinct and temporally consistent structuring of the plot into four dominant habitat types (low and high plateaus, slope and swamp) which was consistent with previous classifications. Basically, the same habitat structuring emerged for the juvenile communities of individual censuses. However, recruits showed a weak and temporally inconsistent habitat structuring. 4. A notable homogenization in species assemblages occurred during the transition from juvenile to reproductive, through both a reduction in the number of species assemblages (in 3 censuses, one large reproductive assemblage covered 93% of the plot, and in others, an additional slope habitat emerged) and a reduction in the classification error. Overall, habitat structuring became noisier and weaker over the 25 years of the study. 5. Synthesis. Our results suggest that mortality processes during the transition from recruits to juveniles must enhance the signal of habitat structuring. However, during the transition to the reproductive stage, species may have lost the advantage of being in the habitat with which they had become associated, or the quality of habitat changed during their life span because of larger climatic changes. The homogeneous assemblages of the reproductive stage could be interpreted as support for neutral theories, but further research is required to unravel the mechanisms behind these intriguing observations. C1 [Kanagaraj, Rajapandian; Wiegand, Thorsten; Huth, Andreas] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04318 Leipzig, Germany. [Comita, Liza S.] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Kanagaraj, R (reprint author), UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, Permoserst 15, D-04318 Leipzig, Germany. EM rajapandian.kanagaraj@ufz.de RI Kanagaraj, Rajapandian/D-4972-2015; Wiegand, Thorsten/H-5877-2016 OI Wiegand, Thorsten/0000-0002-3721-2248 FU National Science Foundation; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Celera Foundation; ERC [233066]; National Center for Ecological Analysis and Synthesis; U.S. NSF [EF-0553768]; University of California, Santa Barbara; State of California FX The BCI forest dynamics research project was made possible by National Science Foundation grants to Stephen P. Hubbell, support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Celera Foundation, and numerous private individuals, and through the hard work of over 100 people from 10 countries over the past two decades. The plot project is part the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. R.K and A.H were supported by the ERC advanced grant 233066 to T.W. L.S.C acknowledges the support of a postdoctoral fellowship from the National Center for Ecological Analysis and Synthesis, a Center funded by U.S. NSF (Grant #EF-0553768), the University of California, Santa Barbara, and the State of California. Two anonymous reviewers provided helpful suggestions for improving the manuscript. NR 56 TC 33 Z9 34 U1 1 U2 42 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD NOV PY 2011 VL 99 IS 6 BP 1441 EP 1452 DI 10.1111/j.1365-2745.2011.01878.x PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 840FR UT WOS:000296425000015 ER PT J AU Churchill, CKC Strong, EE Foighil, DO AF Churchill, Celia K. C. Strong, Ellen E. Foighil, Diarmaid O. TI HITCHHIKING JUVENILES IN THE RARE NEUSTONIC GASTROPOD RECLUZIA CF. JEHENNEI (JANTHINIDAE) SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID CAENOGASTROPODA MOLLUSCA GASTROPODA; DWARF MALES; HERMAPHRODITISM; MORPHOLOGY; CARPENTER; BIVALVIA C1 [Churchill, Celia K. C.; Foighil, Diarmaid O.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Churchill, Celia K. C.; Foighil, Diarmaid O.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Strong, Ellen E.] Smithsonian Inst, Washington, DC 20013 USA. RP Churchill, CKC (reprint author), Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. EM celia.churchill@gmail.com FU Smithsonian Predoctoral Fellowship; NSF [OCE 0850625]; National Geographic Society [8601-09] FX We wish to acknowledge Jochen Gerber and Rudiger Bieler of the Field Museum of Natural History for the loaned specimen (FMNH reg. no. 328104), which was collected during the BivATOL Moreton Bay Expedition (2008). SEM was performed at the University of Michigan Electron Microbeam Analysis Laboratory. Denis Riek photographed live specimens and John Megahan provided the illustration in Figure 1B. Supplementary Material is included with the permissions of Phil Colman and Des Beechey (Editor, Australian Shell News). Funding for this research comes from a Smithsonian Predoctoral Fellowship award to C.K.C.C., and NSF award OCE 0850625 and National Geographic Society award 8601-09 to D.OF. NR 31 TC 5 Z9 5 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 J9 J MOLLUS STUD JI J. Molluscan Stud. PD NOV PY 2011 VL 77 BP 441 EP 444 DI 10.1093/mollus/eyr020 PN 4 PG 4 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 842US UT WOS:000296627100013 ER PT J AU Alves-Brito, A Hau, GKT Forbes, DA Spitler, LR Strader, J Brodie, JP Rhode, KL AF Alves-Brito, Alan Hau, George K. T. Forbes, Duncan A. Spitler, Lee R. Strader, Jay Brodie, Jean P. Rhode, Katherine L. TI Spectra of globular clusters in the Sombrero galaxy: evidence for spectroscopic metallicity bimodality SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE globular clusters: general; galaxies: individual: Sombrero (M104, NGC 4594); galaxies: star clusters: general ID COLOR-MAGNITUDE RELATION; STELLAR POPULATIONS; ELLIPTIC GALAXIES; WIDE-FIELD; BLUE TILT; SYSTEMS; PHOTOMETRY; VIRGO; M87; DISTRIBUTIONS AB We present a large sample of over 200 integrated-light spectra of confirmed globular clusters (GCs) associated with the Sombrero (M104) galaxy taken with the Deep Imaging Multi-Object Spectrograph (DEIMOS) instrument on the Keck telescope. A significant fraction of the spectra have signal-to-noise ratio levels high enough to allow measurements of GC metallicities using the method of Brodie & Huchra. We find a distribution of spectroscopic metallicities in the range -2.2 < [Fe/H] < + 0.1 that is bimodal, with peaks at [Fe/H] similar to -1.4 and -0.6. Thus, the GC system of the Sombrero galaxy, like a few other galaxies now studied in detail, reveals a bimodal spectroscopic metallicity distribution supporting the long-held belief that colour bimodality reflects two metallicity subpopulations. This further suggests that the transformation from optical colour to metallicity for old stellar populations, such as GCs, is not strongly non-linear. We also explore the radial and magnitude distribution with metallicity for GC subpopulations but small number statistics prevent any clear trends in these distributions. C1 [Alves-Brito, Alan; Hau, George K. T.; Forbes, Duncan A.; Spitler, Lee R.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Alves-Brito, Alan] Dept Astron & Astrofis, PUC, Santiago 7820436, Chile. [Hau, George K. T.] European So Observ, Santiago 6670191, Chile. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02144 USA. [Brodie, Jean P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Rhode, Katherine L.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Alves-Brito, A (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM abrito@astro.puc.cl RI Spitler, Lee/A-9867-2013; Alves-Brito, Alan/J-2430-2013 OI Spitler, Lee/0000-0001-5185-9876; FU CNPq [200227/2008-4]; FONDE-CYT [3100013]; ARC; NSF [AST-0917706, AST-0909237, AST-0071048, AST-0808099]; JPL/Caltech [1310512] FX AAB acknowledges CNPq (PDE, 200227/2008-4) and FONDE-CYT (3100013) for financial support. GKTH, DAF and LRS thank ARC for financial support. JS acknowledges support from NSF grants AST-0917706 and AST-0909237. We are grateful to Caroline Foster and Bill Harris for useful discussions and suggestions. We thank an anonymous referee for useful comments and suggestions. Support for this work was provided by award 1310512, issued by JPL/Caltech. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. This work was supported by the National Science Foundation through grant AST-0808099. We thank Steve Zepf for his help in supplying an object list of globular candidates, and Arunav Kundu for his help with astrometry. NR 49 TC 26 Z9 27 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 417 IS 3 BP 1823 EP 1838 DI 10.1111/j.1365-2966.2011.19368.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848HX UT WOS:000297043600014 ER PT J AU Rani, B Gupta, AC Bachev, R Strigachev, A Semkov, E D'Ammando, F Wiita, PJ Gurwell, MA Ovcharov, E Mihov, B Boeva, S Peneva, S AF Rani, Bindu Gupta, Alok C. Bachev, R. Strigachev, A. Semkov, E. D'Ammando, F. Wiita, P. J. Gurwell, M. A. Ovcharov, E. Mihov, B. Boeva, S. Peneva, S. TI Spectral energy distribution variation in BL Lacs and flat spectrum radio quasars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; galaxies: active; BL Lacertae objects: general ID OBJECT S5 0716+714; GAMMA-RAY FLARE; OPTICAL INTRADAY VARIABILITY; ACTIVE GALACTIC NUCLEI; LOG-PARABOLIC SPECTRA; LARGE-AREA TELESCOPE; LACERTAE OBJECTS; MULTIWAVELENGTH OBSERVATIONS; WEBT CAMPAIGN; EXTRAGALACTIC SOURCES AB We present the results of our study of spectral energy distributions (SEDs) of a sample of 10 low- to intermediate-synchrotron-peaked blazars. We investigate some of the physical parameters most likely responsible for the observed short-term variations in blazars. To do so, we focus on the study of changes in the SEDs of blazars corresponding to changes in their respective optical fluxes. We model the observed spectra of blazars from radio to optical frequencies using a synchrotron model that entails a log-parabolic distribution of electron energies. A significant correlation among the two fitted spectral parameters (a, b) of log-parabolic curves and a negative trend among the peak frequency and spectral curvature parameter, b, emphasize that the SEDs of blazars are fitted well by log-parabolic curves. On considering each model parameter that could be responsible for changes in the observed SEDs of these blazars, we find that changes in the jet Doppler factors are most important. C1 [Rani, Bindu; Gupta, Alok C.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, India. [Rani, Bindu; Gupta, Alok C.] DDU Gorakhpur Univ, Dept Phys, Gorakhpur 273009, Uttar Pradesh, India. [Rani, Bindu; Bachev, R.; Strigachev, A.; Semkov, E.; Mihov, B.; Boeva, S.; Peneva, S.] Bulgarian Acad Sci, Inst Astron, Sofia 1784, Bulgaria. [Rani, Bindu; Bachev, R.; Strigachev, A.; Semkov, E.; Mihov, B.; Boeva, S.; Peneva, S.] Bulgarian Acad Sci, Natl Astron Observ, Sofia 1784, Bulgaria. [D'Ammando, F.] INAF IASF Palermo, I-90146 Palermo, Italy. [Wiita, P. J.] Coll New Jersey, Dept Phys, Ewing, NJ 08628 USA. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ovcharov, E.] Univ Sofia, Dept Astron, Sofia 1164, Bulgaria. RP Rani, B (reprint author), Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, India. EM bindu@aries.res.in OI Wiita, Paul/0000-0002-1029-3746 FU Bulgarian Ministry of Education and Sciences [BIn - 13/09, DO 02-85, DO02-340/08]; Indo-Bulgaria bilateral scientific exchange project INT/Bulgaria [B-5/08]; DST, India; University of Michigan; National Science Foundation [AST-0607523]; Smithsonian Institution; Academia Sinica FX We thank the referee, Dr Paolo Giommi, for several helpful suggestions. BR is thankful to Professor D. C. Srivastava for his valuable suggestions and encouragements and to Mr Ravi Joshi for help while finalizing the text. This research was partially supported by Scientific Research Fund of the Bulgarian Ministry of Education and Sciences (BIn - 13/09, DO 02-85 and DO02-340/08) and by Indo-Bulgaria bilateral scientific exchange project INT/Bulgaria/B-5/08 funded by DST, India. RB and AS acknowledge the kind hospitality of ARIES, Nainital, India. This research has made use of data from the University of Michigan Radio Astronomy Observatory which has been supported by the University of Michigan and by a series of grants from the National Science Foundation, most recently AST-0607523. BR is very grateful to Margo Aller for providing the data at radio frequencies. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We used these data in our research. The Australia Telescope Compact Array is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The efforts of ATNF staff in maintaining the ATCA calibrator data base (http://www.narrabri.atnf.csiro.au/calibrators/) are gratefully acknowledged. SMARTS data are made available by Yale University at http://www.astro.yale.edu/smarts/fermi through Fermi GI grant 011283. NR 87 TC 10 Z9 10 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 417 IS 3 BP 1881 EP 1890 DI 10.1111/j.1365-2966.2011.19373.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848HX UT WOS:000297043600018 ER PT J AU Margutti, R Chincarini, G Granot, J Guidorzi, C Berger, E Bernardini, MG Gehrels, N Soderberg, AM Stamatikos, M Zaninoni, E AF Margutti, R. Chincarini, G. Granot, J. Guidorzi, C. Berger, E. Bernardini, M. G. Gehrels, N. Soderberg, A. M. Stamatikos, M. Zaninoni, E. TI X-ray flare candidates in short gamma-ray bursts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; gamma-ray burst: general ID LAG-LUMINOSITY RELATION; AFTERGLOW LIGHT CURVES; EXTENDED EMISSION; TELESCOPE OBSERVATIONS; TEMPORAL PROPERTIES; PROMPT EMISSION; PEAK LUMINOSITY; HOST GALAXIES; NEUTRON-STARS; SWIFT AB We present the first systematic study of X-ray flare candidates in short gamma-ray bursts (SGRBs) exploiting the large 6-year Swift data base with the aim to constrain the physical nature of such fluctuations. We find that flare candidates appear in different types of SGRB host galaxy environments and show no clear correlation with the X-ray afterglow lifetime; flare candidates are detected both in SGRBs with a bright extended emission in the soft gamma-rays and in SGRBs which do not show such component. We furthermore show that SGRB X-ray flare candidates only partially share the set of observational properties of long GRB (LGRB) flares. In particular, the main parameter driving the duration evolution of X-ray variability episodes in both classes is found to be the elapsed time from the explosion, with very limited dependence on the different progenitors, environments, central engine lifetimes, prompt variability time-scales and energy budgets. On the contrary, SGRB flare candidates significantly differ from LGRB flares in terms of peak luminosity, isotropic energy, flare-to-prompt luminosity ratio and relative variability flux. However, these differences disappear when the central engine time-scales and energy budget are accounted for, suggesting that (i) flare candidates and prompt pulses in SGRBs likely have a common origin; (ii) similar dissipation and/or emission mechanisms are responsible for the prompt and flare emission in LGRBs and SGRBs, with SGRBs being less energetic albeit faster evolving versions of the long class. Finally, we show that in strict analogy to the SGRB prompt emission, flares candidates fall off the lag-luminosity relation defined by LGRBs, thus strengthening the SGRB flare-prompt pulse connection. C1 [Margutti, R.; Chincarini, G.; Bernardini, M. G.; Zaninoni, E.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Margutti, R.; Berger, E.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chincarini, G.] Univ Milano Bicocca, Dip Fis G Occhialini, I-20126 Milan, Italy. [Granot, J.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Granot, J.] Tel Aviv Univ, Raymond & Beverly Sackler Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Granot, J.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Guidorzi, C.] Univ Ferrara, Dept Phys, I-44122 Ferarra, Italy. [Gehrels, N.; Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Zaninoni, E.] Univ Padua, Dip Astron, I-35122 Padua, Italy. RP Margutti, R (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Italy. EM raffaella.margutti@brera.inaf.it RI Gehrels, Neil/D-2971-2012 FU ASI [SWIFT I/011/07/0]; Ministry of University and Research of Italy [PRIN MIUR 2007TNYZXL]; MAE (Ministry of Exterior); University of Milano Bicocca, Italy; ERC FX We thank the anonymous referee for helpful suggestions that improved the quality of this work. RM thanks Lorenzo Amati for sharing his data before publication. This work is supported by ASI grant SWIFT I/011/07/0, by the Ministry of University and Research of Italy (PRIN MIUR 2007TNYZXL), by MAE (Ministry of Exterior), by the University of Milano Bicocca, Italy and by the ERC advanced research grant 'GRBs'. NR 77 TC 27 Z9 28 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV PY 2011 VL 417 IS 3 BP 2144 EP 2160 DI 10.1111/j.1365-2966.2011.19397.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848HX UT WOS:000297043600035 ER PT J AU Perkins, SL Martinsen, ES Falk, BG AF Perkins, S. L. Martinsen, E. S. Falk, B. G. TI Do molecules matter more than morphology? Promises and pitfalls in parasites SO PARASITOLOGY LA English DT Article DE Integrated taxonomy; molecular systematics; cryptic species ID INTERNAL TRANSCRIBED SPACER-1; ANIMAL MITOCHONDRIAL-DNA; CHAIN-REACTION PRIMERS; AVIAN BLOOD PARASITES; RNA GENE-SEQUENCES; MALARIA PARASITES; HOST-SPECIFICITY; CYTOCHROME-B; PLASMODIUM-FALCIPARUM; CRYPTIC DIVERSITY AB Systematics involves resolving both the taxonomy and phylogenetic placement of organisms. We review the advantages and disadvantages of the two kinds of information commonly used for such inferences - morphological and molecular data - as applied to the systematics of metazoan parasites generally, with special attention to the malaria parasites. The problems that potentially confound the use of morphology in parasites include challenges to consistent specimen preservation, plasticity of features depending on hosts or other environmental factors, and morphological convergence. Molecular characters such as DNA sequences present an alternative data source and are particularly useful when not all the parasite's life stages are present or when parasitaemia is low. Nonetheless, molecular data can bring challenges that include troublesome DNA isolation, paralogous gene copies, difficulty in developing molecular markers, and preferential amplification in mixed species infections. Given the differential benefits and shortcomings of both molecular and morphological characters, both should be implemented in parasite taxonomy and phylogenetics. C1 [Perkins, S. L.; Falk, B. G.] Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA. [Martinsen, E. S.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Falk, B. G.] Amer Museum Nat Hist, Richard Gilder Grad Sch, New York, NY 10024 USA. RP Perkins, SL (reprint author), Amer Museum Nat Hist, Sackler Inst Comparat Genom, Cent Pk W & 79th St, New York, NY 10024 USA. EM perkins@amnh.org OI Perkins, Susan/0000-0002-5400-5662 NR 103 TC 32 Z9 33 U1 2 U2 36 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0031-1820 EI 1469-8161 J9 PARASITOLOGY JI Parasitology PD NOV PY 2011 VL 138 IS 13 BP 1664 EP 1674 DI 10.1017/S0031182011000679 PG 11 WC Parasitology SC Parasitology GA 847JY UT WOS:000296970400003 PM 21729351 ER PT J AU Zarowiecki, M Loaiza, JR Conn, JE AF Zarowiecki, Magdalena Loaiza, Jose R. Conn, Jan E. TI Towards a new role for vector systematics in parasite control SO PARASITOLOGY LA English DT Article DE Species complex; speciation; biogeography; vector systematics ID ALBITARSIS COMPLEX DIPTERA; MULTILOCUS GENOTYPE DATA; ANOPHELES-GAMBIAE; SPECIES DELIMITATION; GENE-FLOW; MALARIA VECTOR; POPULATION-STRUCTURE; SOUTHEAST-ASIA; COMPARATIVE SUSCEPTIBILITY; LEUCOSPHYRUS GROUP AB Vector systematics research is being transformed by the recent development of theoretical, experimental and analytical methods, as well as conceptual insights into speciation and reconstruction of evolutionary history. We review this progress using examples from the mosquito genus Anopheles. The conclusion is that recent progress, particularly in the development of better tools for understanding evolutionary history, makes systematics much more informative for vector control purposes, and has increasing potential to inform and improve targeted vector control programmes. C1 [Zarowiecki, Magdalena] Nat Hist Museum, Dept Zool, London SW7 5BD, England. [Loaiza, Jose R.] Univ Panama, Programa Ctr Amer Maestria Entomol Vicerrectoria, Panama City, Panama. [Loaiza, Jose R.] Smithsonian Trop Res Inst, Unit 0948, Balboa Ancon, Panama. [Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Griffin Lab, Slingerlands, NY USA. [Conn, Jan E.] SUNY Albany, Sch Publ Hlth, Dept Biomed Sci, Albany, NY 12222 USA. RP Zarowiecki, M (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England. EM mz3@sanger.ac.uk OI Zarowiecki, Magdalena/0000-0001-6102-7731; Conn, Jan/0000-0002-5301-7020 FU Natural History Museum FX This work was supported by the Natural History Museum (M.Z., Prize Studentship). NR 93 TC 4 Z9 5 U1 1 U2 9 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0031-1820 EI 1469-8161 J9 PARASITOLOGY JI Parasitology PD NOV PY 2011 VL 138 IS 13 BP 1723 EP 1729 DI 10.1017/S003118201100062X PG 7 WC Parasitology SC Parasitology GA 847JY UT WOS:000296970400007 PM 21679487 ER PT J AU Ibanez-Mejia, M Ruiz, J Valencia, VA Cardona, A Gehrels, GE Mora, AR AF Ibanez-Mejia, Mauricio Ruiz, Joaquin Valencia, Victor A. Cardona, Agustin Gehrels, George E. Mora, Andres R. TI The Putumayo Orogen of Amazonia and its implications for Rodinia reconstructions: New U-Pb geochronological insights into the Proterozoic tectonic evolution of northwestern South America SO PRECAMBRIAN RESEARCH LA English DT Article DE South America; Amazonia; Putumayo Orogen; Rodinia; Grenville; U-Pb geochronology ID NEOPROTEROZOIC ACTIVE MARGIN; EASTERN GRENVILLE PROVINCE; NORTHERN OAXACAN COMPLEX; LARGE OCEAN BASINS; COLOMBIAN ANDES; LLANO UPLIFT; ZIRCON GEOCHRONOLOGY; SVECONORWEGIAN PROVINCE; GUICHICOVI COMPLEX; U/PB GEOCHRONOLOGY AB Outcrops of late Meso- to early Neoproterozoic crust in northwestern South America are restricted to isolated exposures of basement inliers within the northern Andes of Colombia, Peru and Venezuela. However, evidence for the existence of an autochthonous Stenian-Tonian belt in northern Amazonia that is undisturbed by Andean orogenesis has not been recognized so far. Here we report similar to 1200 new single-zircon U-Pb geochronological analyses from 19 Proterozoic rock samples of northwestern South America collected from the Garzon and Las Minas Andean cordilleran inliers, drill-core samples from the foreland basin basement, and outcrops of cratonic Amazonia in eastern Colombia (western Guyana shield). Our new geochronological results document the existence of a previously unrecognized Meso- to Neoproterozoic orogenic belt buried under the north Andean foreland basins, herein termed the Putumayo Orogen, which has implications for Proterozoic tectonic reconstructions of Amazonia during the assembly of the supercontinent Rodinia. Based on the interpretations of new and pre-existing data, we propose a three-stage tectonometamorphic evolution for this orogenic segment characterized by: (1) development of a pericratonic fringing-arc system outboard of Amazonia's leading margin during Mesoproterozoic time from similar to 1.3 to 1.1 Ga, where the protoliths for metaigneous and metavolcanosedimentary units of the Colombian and Mexican inliers would have originated in a commonly evolving Colombian-Oaxaquian fringing-arc system; (2) amphibolite-grade metamorphism and migmatization between ca. 1.05 and 1.01 Ga by inferred amalgamation of these parautochtonous arc terranes onto the continental margin, and (3) granulite-grade metamorphism at similar to 0.99 Ga during continent-continent collision related to Rodinia final assembly. Along with additional paleogeographic constraints, this new geochronological framework suggests that the final metamorphic phase of the Putumayo Orogen was likely the result of collisional interactions with the Sveconorwegian province of Baltica, in contrast to previously proposed models that place this margin of Amazonia as the conjugate of the Grenville province of Laurentia. (C) 2011 Elsevier B.V. All rights reserved. C1 [Ibanez-Mejia, Mauricio; Ruiz, Joaquin; Gehrels, George E.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Valencia, Victor A.] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. [Cardona, Agustin] Smithsonian Trop Res Inst, Balboa, Panama. [Mora, Andres R.] ECOPETROL, Inst Colombiano Petr ICP, Santander, Spain. RP Ibanez-Mejia, M (reprint author), Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. EM ibanezm@email.arizona.edu OI Ibanez-Mejia, Mauricio/0000-0002-7839-2425 FU Ecopetrol-ICP; GSA [9184-09]; Chevron-Texaco through University of Arizona; NSF-EAR [0443387, 0732436] FX This research benefited from funding provided to M.I. by Ecopetrol-ICP, the GSA student Grant #9184-09 and a Chevron-Texaco summer Grant through the University of Arizona. The Laserchron center is partially funded by NSF-EAR Grants #0443387 and #0732436. The authors would like to thank the Colombian Instituto Nacional del Petroleo (ICP-ECOPETROL) and the Litoteca Nacional de Colombia for allowing access to the core samples. M.I. would specially like to thank Monica Carvalho for help with figure elaboration, Camilo Bustamante for assistance during fieldwork, Kendra Murray for editorial improvements and Ana Milena Rangel for assistance during core sampling at the Litoteca Nacional. Insightful comments from reviewers Alan Collins and David Chew as well as the editorial assistance of Peter Cawood are greatly appreciated as they helped improve the final version of this manuscript. This paper is specially dedicated to the memory of Prof. Dr. Thomas Van der Hammen for his pioneering contributions on the geology of Colombia and the Amazonas region. NR 118 TC 37 Z9 38 U1 0 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0301-9268 J9 PRECAMBRIAN RES JI Precambrian Res. PD NOV PY 2011 VL 191 IS 1-2 BP 58 EP 77 DI 10.1016/j.precamres.2011.09.005 PG 20 WC Geosciences, Multidisciplinary SC Geology GA 848VM UT WOS:000297083200004 ER PT J AU Unghire, JM Sutton-Grier, AE Flanagan, NE Richardson, CJ AF Unghire, Joshua M. Sutton-Grier, Ariana E. Flanagan, Neal E. Richardson, Curtis J. TI Spatial Impacts of Stream and Wetland Restoration on Riparian Soil Properties in the North Carolina Piedmont SO RESTORATION ECOLOGY LA English DT Article DE floodplain; geostatistics; kriging; soil organic matter; spatial variability ID PAIRED NATURAL WETLANDS; ECOSYSTEM DEVELOPMENT; VARIABILITY; ECOLOGY; DENITRIFICATION; BIODIVERSITY; SCALE; MARSH AB Hydric soil development of riparian wetlands is primarily influenced by the hydrologic connection between the floodplains and the stream channel. Often, the goal of riparian restoration is to revitalize this connectivity through a restructuring of the stream channel and the floodplain; however, the effects of this restructuring on the physical and spatial characteristics of soil properties are rarely considered. The objective of this study was to quantify the impacts of restoration efforts on the spatial characteristics of soil properties by means of a pre- and post-restoration comparison. We determined that the spatial patterns of soil organic matter (SOM) and exchangeable phosphorus (P(ex)) appeared less variable in the years following restoration than in the years before restoration. Mean SOM significantly decreased after restoration, whereas mean P(ex) significantly increased. The spatial characteristics and mean concentrations of NO(2)-NO(3) did not differ much between sampling dates. The loss of this spatial patterning in SOM and P(ex) and the decrease in SOM pools may represent negative impacts of restoration on important ecosystem characteristics. This study demonstrates that soil properties and spatial patterns can be negatively affected by restoration activities potentially hindering ecosystem development and function. C1 [Unghire, Joshua M.; Flanagan, Neal E.; Richardson, Curtis J.] Duke Univ, Nicholas Sch Environm, Wetland Ctr, Durham, NC 27708 USA. [Sutton-Grier, Ariana E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Unghire, JM (reprint author), 806 Parkwood Ave,Floor 2, Annapolis, MD 21403 USA. EM JMUnghire@alumni.duke.edu OI Sutton-Grier, Ariana/0000-0002-1242-7728 FU Duke University Wetlands Center (DUWC) FX This research was supported by the Duke University Wetlands Center (DUWC) endowment fund, Curtis J. Richardson, Director. Invaluable laboratory support was provided by Wes Willis of the DUWC. In addition, we want to thank Song Qian for his guidance with statistical analysis. Also, a special thanks to Jean Still, Joe Williams, Mengchi Ho, Brian Roberts, and Wyatt Hartman for laboratory and field assistance. NR 44 TC 9 Z9 9 U1 3 U2 32 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1061-2971 J9 RESTOR ECOL JI Restor. Ecol. PD NOV PY 2011 VL 19 IS 6 BP 738 EP 746 DI 10.1111/j.1526-100X.2010.00726.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 848TS UT WOS:000297078600010 ER PT J AU Baresch, A Smith, JAC Winter, K Valerio, AL Jaramillo, C AF Baresch, Andres Smith, J. Andrew C. Winter, Klaus Lucia Valerio, Ana Jaramillo, Carlos TI KARATOPHYLLUM BROMELIOIDES LD GOMEZ REVISITED: A PROBABLE FOSSIL CAM BROMELIAD SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Aechmea magdalenae; Bromeliaceae; CAM photosynthesis; Karatophyllum bromelioides; leaf morphology; travertine ID HISTORICAL BIOGEOGRAPHY; ADAPTIVE RADIATION; AECHMEA-MAGDALENAE; GROWTH; PHOTOSYNTHESIS; PHYLOGENY; PANAMA; ZONE AB Premise of the study: The fossil leaf Karatophyllum bromelioides L. D. Gomez found in Costa Rica was proposed by Gomez (1972) to belong to the Bromeliaceae and to date from the middle Tertiary. If the age and affinity of this specimen were proven to be correct, it would constitute the oldest record of this large and ecologically diverse monocotyledonous family. Key results: Morphological features of the fossil (leaf dimensions, marginal spines, cuticular traces) indicate a close affinity with the extant bromeliad Aechmea magdalenae (Andre) Andre ex Baker. Leaf thickness (1.6 mm at maximum) suggests that K. bromelioides L. D. Gomez performed CAM photosynthesis. The geological information does not corroborate the estimated age and location of the specimen; the fossil is suggested to be of more recent origin. Conclusions: The affinity of this fossil to Bromeliaceae was confirmed, but the uncertainties surrounding its age and collection locality mitigate against its use in inferences concerning the evolutionary history of the family. C1 [Baresch, Andres; Winter, Klaus; Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Smith, J. Andrew C.] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. [Lucia Valerio, Ana] Museo Nacl Costa Rica, Dept Hist Nat, San Jose, Costa Rica. RP Baresch, A (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA. EM ba.andres@gmail.com FU U.S. National Science Foundation [0966884, EAR 0824299, EAR 0418042]; Mark Tupper Fellowship; Ricardo Perez SA; Smithsonian Tropical Research Institute FX Financial support for this investigation was provided by the U.S. National Science Foundation Partnerships in International Research and Education grant 0966884 (OISE, EAR, DRL), EAR 0824299, and EAR 0418042, the Mark Tupper Fellowship, Ricardo Perez SA, and the Smithsonian Tropical Research Institute. The authors thank Jorge Aranda and Aurelio Virgo for assistance and Camilla Crifo, Judy Jernstedt, John G. Conran, and an anonymous reviewer for useful comments and reviews of the manuscript. NR 25 TC 2 Z9 2 U1 0 U2 4 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD NOV PY 2011 VL 98 IS 11 BP 1905 EP 1908 DI 10.3732/ajb.1100261 PG 4 WC Plant Sciences SC Plant Sciences GA 844PU UT WOS:000296760500026 PM 22034484 ER PT J AU Bedell, M Villaume, A Weiss, L Sliski, D Strelnitski, V Walker, G Williams, J Henden, A Krajci, T AF Bedell, Megan Villaume, Alexa Weiss, Lauren Sliski, David Strelnitski, Vladimir Walker, Gary Williams, Jedediyah Henden, Arne Krajci, Tom TI MONITORING H alpha EMISSION AND CONTINUUM OF UXORs: RR Tauri SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; methods: observational; stars: individual (RR Tauri); stars: pre-main sequence; stars: variables: general ID HERBIG AE/BE STARS; YOUNG STARS; VARIABILITY; PHOTOMETRY; CATALOG; DISKS AB The Maria Mitchell Observatory, in collaboration with the Astrokolkhoz Observatory, started a program of photometric monitoring of UX Ori-type stars (UXORs) with narrowband interference filters (IFs; augmented with the traditional broadband filters) aimed at separating the H alpha emission variations from those of the continuum. We present the method of separation and the first results for RR Tau obtained in two seasons, each roughly 100 days long (2010 Winter-Spring and 2010 Fall-2011 Spring). We confirm the conclusion from previous studies that the H alpha emission in this star is less variable than the continuum. Although some correlation between the two is not excluded, the amplitude of H alpha variations is much smaller (factors of 3-5) than that of the continuum. These results are compatible with Grinin's model of UXORs, which postulates the presence of small obscuring circumstellar clouds as the cause of the continuum fading, as well as the presence of a circumstellar reflection/emission nebula, larger than the star and the obscuring clouds, which is responsible for H alpha emission and the effect of the "color reversal" in deep minima. However, the results of both our broadband and narrowband photometry indicate that the obscuration model may be insufficient to explain all of the observations. Disk accretion, the presence of stellar or (proto) planetary companion(s), as well as the intrinsic variations of the star, may contribute to the observed light variations. We argue, in particular, that the H alpha emission may be more closely correlated with the intrinsic variations of the star than with the much stronger observed variations caused by the cloud obscuration. If this hypothesis is correct, the close monitoring of H alpha emission with IFs, accessible to small-size telescopes, may become an important tool in studying the physical nature of the UXORs' central stars. C1 [Bedell, Megan; Villaume, Alexa; Weiss, Lauren; Sliski, David; Strelnitski, Vladimir; Walker, Gary; Williams, Jedediyah] Maria Mitchell Observ, Nantucket, MA 02554 USA. [Bedell, Megan] Haverford Coll, Haverford, PA 19041 USA. [Villaume, Alexa] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Weiss, Lauren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Weiss, Lauren] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Henden, Arne] AAVSO, Cambridge, MA 02138 USA. [Krajci, Tom] Astrokolkhoz Observ, Cloudcroft, NM 88317 USA. RP Bedell, M (reprint author), Maria Mitchell Observ, 4 Vestal St, Nantucket, MA 02554 USA. FU NSF REU [AST-0851892]; Maria Mitchell Association; MMA; NSF; Keenan Foundation FX The major part of this project was accomplished by the MMO REU interns M.B., A.V., and L.W., who thank the support from the NSF REU grant AST-0851892 and from the Maria Mitchell Association. D.S. thanks the support by the MMA and its Presidential Award for Excellence in Science, Mathematics and Engineering Mentoring. The MMO observations were performed on its new 24 inch telescope; the authors thank the NSF PREST program, the Keenan Foundation, and numerous individual donors whose financial support made the purchasing and running of this instrument possible. Authors also thank the referee for a valuable suggestion about possible parallels in physics of UXORs and T Tau stars. NR 15 TC 0 Z9 0 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 NOV PY 2011 VL 142 IS 5 AR 164 DI 10.1088/0004-6256/142/5/164 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844VH UT WOS:000296777000021 ER PT J AU Drake, JJ Ball, B Eldridge, JJ Ness, JU Stancliffe, RJ AF Drake, Jeremy J. Ball, B. Eldridge, John J. Ness, J. -U. Stancliffe, Richard J. TI CLOSE TO THE DREDGE: PRECISE X-RAY C AND N ABUNDANCES IN lambda ANDROMEDA AND ITS PRECOCIOUS RED GIANT BRANCH MIXING PROBLEM SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: abundances; stars: activity; stars: coronae; stars: evolution; stars: late-type; X-rays: stars ID LOW-MASS STARS; CARBON-ISOTOPE RATIOS; METAL-POOR STARS; OLD DISK GIANTS; CHEMICAL-COMPOSITION; STELLAR MODELS; RGB-STARS; THERMOHALINE CONVECTION; EVOLUTIONARY SEQUENCE; NITROGEN ABUNDANCES AB Chandra LETG+HRC-S and XMM-Newton RGS spectra of H-like C and N lines formed in the corona of the primary star of the RS CVn-type binary lambda And, a mildly metal-poor G8 III-IV first ascent giant that completed dredge-up similar to 50 Myr ago, have been used to make a precise measurement of its surface C/N ratio. We obtain the formal result [C/N] = 0.03 +/- 0.07, which is typical of old disk giants and in agreement with standard dredge-up theory for stars less than or similar to 1 M-circle dot. In contrast, these stars as a group, including lambda And, have C-12/C-13 less than or similar to 20, which is much lower than standard model predictions. We show that the abundances of the old disk giants are consistent with models including thermohaline mixing that begins at the red giant branch luminosity function "bump." Instead, lambda And indicates that the C-12/C-13 anomaly can be present immediately following dredge-up, contrary to current models of extra mixing on the red giant branch. In the context of other recent C and N abundance results for RS CVn-type binaries it seems likely that the anomaly is associated with either strong magnetic activity, fast rotation, or both, rather than close binarity itself. C1 [Drake, Jeremy J.; Ball, B.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Eldridge, John J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ness, J. -U.] SRE OAX, XMM Newton Observ SOC, European Space Agcy, Madrid 28691, Spain. [Stancliffe, Richard J.] Monash Univ, Ctr Stellar & Planetary Astrophys, Sch Math Sci, Melbourne, Vic 3800, Australia. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS-3,60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu; jje@ast.cam.ac.uk; Jan-Uwe.Ness@sciops.esa.int; richard.stancliffe@monash.edu FU NASA AISRP; NASA [NAS8-39073]; Chandra X-ray Center [AR4-5002X]; CXC science team FX We thank the NASA AISRP for providing financial assistance for the development of the PINTofALE package. J.J.D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center during the course of this research. B. B. was supported by Chandra award number AR4-5002X issued by the Chandra X-ray Center. J.J.D. thanks H. Tananbaum and the CXC science team for advice and support. NR 80 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2011 VL 142 IS 5 AR 144 DI 10.1088/0004-6256/142/5/144 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844VH UT WOS:000296777000001 ER PT J AU Lyo, AR Ohashi, N Qi, CH Wilner, DJ Su, YN AF Lyo, A-Ran Ohashi, Nagayoshi Qi, Chunhua Wilner, David J. Su, Yu-Nung TI MILLIMETER OBSERVATIONS OF THE TRANSITION DISK AROUND HD 135344B (SAO 206462) SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; protoplanetary disks; stars: pre-main sequence ID MAIN-SEQUENCE STARS; VEGA-EXCESS STARS; HERBIG AE STARS; PROTOPLANETARY DISK; CIRCUMSTELLAR DISKS; MOLECULAR DISK; YOUNG STARS; CO EMISSION; DUST; SUBMILLIMETER AB We present similar to 1 '' resolution 1.3 mm dust continuum and spectral line ((CO)-C-12 and (CO)-C-13 J = 2-1) observations of the transitional disk system HD 135344B obtained with the Submillimeter Array. The disk shows a Keplerian rotation pattern with an inclination of similar to 11 degrees, based on the spatially and spectrally resolved (CO)-C-12 and (CO)-C-13 emission. The data show clear evidence for both dust and gas surface density reductions in the inner region of the disk (radius less than or similar to 50 AU) from the continuum and (CO)-C-13 J = 2-1 data, respectively. The presence of this inner cavity in both the dust and gas is more consistent with clearing by giant planet formation than by photoevaporation or by grain growth. There is also an indication of global CO gas depletion in the disk, as the mass estimated from (CO)-C-13 emission (similar to 3.8 x 10(-4) M-circle dot) is about two orders of magnitude lower than that derived from the 1.3mm continuum (similar to 2.8 x 10(-2) M-circle dot). C1 [Lyo, A-Ran] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Ohashi, Nagayoshi; Su, Yu-Nung] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Qi, Chunhua; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Lyo, AR (reprint author), Korea Astron & Space Sci Inst, 61-1 Hwaam Dong, Taejon 305348, South Korea. EM arl@kasi.re.kr FU Smithsonian Institution; Academia Sinica FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 35 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD NOV PY 2011 VL 142 IS 5 AR 151 DI 10.1088/0004-6256/142/5/151 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844VH UT WOS:000296777000008 ER PT J AU Stencel, RE Kloppenborg, BK Wall, RE Hopkins, JL Howell, SB Hoard, DW Rayner, J Bus, S Tokunaga, A Sitko, ML Bradford, S Russell, RW Lynch, DK Hammel, H Whitney, B Orton, G Yanamandra-Fisher, P Hora, JL Hinz, P Hoffmann, W Skemer, A AF Stencel, Robert E. Kloppenborg, Brian K. Wall, Randall E., Jr. Hopkins, Jeffrey L. Howell, Steve B. Hoard, D. W. Rayner, John Bus, Schelte Tokunaga, Alan Sitko, Michael L. Bradford, Suellen Russell, Ray W. Lynch, David K. Hammel, Heidi Whitney, Barbara Orton, Glenn Yanamandra-Fisher, Padma Hora, Joseph L. Hinz, Philip Hoffmann, William Skemer, Andrew TI INFRARED STUDIES OF EPSILON AURIGAE IN ECLIPSE SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; protoplanetary disks; stars: individual (epsilon Aurigae) ID SPITZER-SPACE-TELESCOPE; ABSORPTION-LINES; ARRAY CAMERA; SECONDARY; SYSTEM; STARS; DISK; SPECTROGRAPH; ULTRAVIOLET; PHOTOMETRY AB We report here on a series of medium resolution spectro-photometric observations of the enigmatic long period eclipsing binary epsilon Aurigae, during its eclipse interval of 2009-2011, using near-infrared spectra obtained with SpeX on tHe Infrared Telescope Facility (IRTF), mid-infrared spectra obtained with BASS on AOES and IRTF, MIRSI on IRTF, and MIRAC4 on the MMT, along with mid-infrared photometry using MIRSI on IRTF and MIRAC4 on the MMT, plus 1995-2000 timeframe published photometry and data obtained with Denver's TNTCAM2 at WIRO. The goals of these observations included: (1) comparing eclipse depths with prior eclipse data, (2) confirming the re-appearance of CO absorption bands at and after mid-eclipse, associated with sublimation in the disk, (3) seeking evidence for any mid-infrared solid state spectral features from particles in the disk, and (4) providing evidence that the externally irradiated disk has azimuthal temperature differences. IR eclipse depths appear similar to those observed during the most recent (1983) eclipse, although evidence for post-mid-eclipse disk temperature increase is present, due to F star heated portions of the disk coming into view. Molecular CO absorption returned 57 days after nominal mid-eclipse, but was not detected at mid-eclipse plus 34 days, narrowing the association with differentially heated sub-regions in the disk. Transient He I 10830A absorption was detected at mid-eclipse, persisting for at least 90 days thereafter, providing a diagnostic for the hot central region. The lack of solid-state features in Spitzer Infrared Spectrograph, BASS, and MIRAC spectra to date suggests the dominance of large particles (micron-sized) in the disk. Based on these observations, mid-infrared studies out of eclipse can directly monitor and map the disk thermal changes, and better constrain disk opacity and thermal conductivity. C1 [Stencel, Robert E.; Kloppenborg, Brian K.; Wall, Randall E., Jr.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Hopkins, Jeffrey L.] Hopkins Phoenix Observ, Phoenix, AZ 85033 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Rayner, John; Bus, Schelte; Tokunaga, Alan] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Sitko, Michael L.; Bradford, Suellen] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Sitko, Michael L.; Bradford, Suellen; Hammel, Heidi; Whitney, Barbara] Space Sci Inst, Boulder, CO 80301 USA. [Russell, Ray W.; Lynch, David K.] Aerosp Corp, Los Angeles, CA 90009 USA. [Orton, Glenn; Yanamandra-Fisher, Padma] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hinz, Philip; Hoffmann, William; Skemer, Andrew] Univ Arizona, Steward Observ, Dept Astron, Tucson, AZ 85721 USA. RP Stencel, RE (reprint author), Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. EM rstencel@du.edu OI Skemer, Andrew/0000-0001-6098-3924; Hora, Joseph/0000-0002-5599-4650 FU bequest of William Herschel Womble; astronomy at the University of Denver; NSF [AST 97-24506, AST 10-16678, JPL RSA 1414715]; NASA ADP [NNX09AC73G]; The Aerospace Corporation; National Aeronautics and Space Administration, Science Mission Directorate [NNX-08AE38A] FX This work was supported in part by the bequest of William Herschel Womble in support of astronomy at the University of Denver, by NSF grants AST 97-24506 and AST 10-16678, and JPL RSA 1414715 to the University of Denver, by NASA ADP grant NNX09AC73G to the University of Cincinnati, and by The Aerospace Corporation's Independent Research and Development Program. Observations reported here were obtained in part as Visiting Astronomers at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. Observations reported here were obtained in part at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Observations were also obtained in part at the University of Wyoming's Infrared Observatory (WIRO), involving access for which we are grateful. The first author thanks Dana Backman for the encouragement to obtain mid-IR data during the mid-1990s, and the many observers involved in those and all the data reported here. We also thank Jeff Hopkins, Brian McCandless, Thomas Rutherford, and the AAVSO for access to their visual observation records. NR 37 TC 11 Z9 11 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2011 VL 142 IS 5 AR 174 DI 10.1088/0004-6256/142/5/174 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844VH UT WOS:000296777000031 ER PT J AU Beaumont, CN Williams, JP Goodman, AA AF Beaumont, Christopher N. Williams, Jonathan P. Goodman, Alyssa A. TI CLASSIFYING STRUCTURES IN THE INTERSTELLAR MEDIUM WITH SUPPORT VECTOR MACHINES: THE G16.05-0.57 SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G16.05-0.57, M17); ISM: supernova remnants; techniques: image processing ID PRINCIPAL COMPONENT ANALYSIS; CLASSIFICATION; EXTRACTION; ALGORITHM; EMISSION; OUTFLOWS; PERSEUS; CLOUDS; CO AB We apply Support Vector Machines (SVMs)-a machine learning algorithm-to the task of classifying structures in the interstellar medium (ISM). As a case study, we present a position-position-velocity (PPV) data cube of (12)CO J = 3-2 emission toward G16.05-0.57, a supernova remnant that lies behind the M17 molecular cloud. Despite the fact that these two objects partially overlap in PPV space, the two structures can easily be distinguished by eye based on their distinct morphologies. The SVM algorithm is able to infer these morphological distinctions, and associate individual pixels with each object at >90% accuracy. This case study suggests that similar techniques may be applicable to classifying other structures in the ISM-a task that has thus far proven difficult to automate. C1 [Beaumont, Christopher N.; Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Beaumont, Christopher N.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beaumont, CN (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM beaumont@ifa.hawaii.edu RI Goodman, Alyssa/A-6007-2010; OI Goodman, Alyssa/0000-0003-1312-0477; Williams, Jonathan/0000-0001-5058-695X FU NSF [AST-0908159] FX We are grateful to C. Brogan for sharing her 20 cm data of G16.05-0.57, and to K. Binsted for discussions regarding this manuscript. We also thank the anonymous referee for his or her careful feedback. J.P.W. acknowledges support from NSF. This material is based upon work supported by the National Science Foundation under Grant No. AST-0908159. NR 32 TC 8 Z9 8 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2011 VL 741 IS 1 AR 14 DI 10.1088/0004-637X/741/1/14 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844TA UT WOS:000296769000014 ER PT J AU Cranmer, SR Saar, SH AF Cranmer, Steven R. Saar, Steven H. TI TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: coronae; stars: late-type; stars: magnetic field; stars: mass-loss; stars: winds, outflows; turbulence ID MAIN-SEQUENCE STARS; HORIZONTAL-BRANCH STARS; ANGULAR-MOMENTUM LOSS; SOLAR-LIKE STARS; FUNDAMENTAL STELLAR PARAMETERS; ROTATION-ACTIVITY CORRELATION; PHOTOSPHERIC MAGNETIC-FIELD; HERTZSPRUNG-RUSSELL DIAGRAM; WAVE ENERGY-SPECTRA; LOW-GRAVITY STARS AB The basic mechanisms responsible for producing winds from cool, late-type stars are still largely unknown. We take inspiration from recent progress in understanding solar wind acceleration to develop a physically motivated model of the time-steady mass loss rates of cool main-sequence stars and evolved giants. This model follows the energy flux of magnetohydrodynamic turbulence from a subsurface convection zone to its eventual dissipation and escape through open magnetic flux tubes. We show how Alfven waves and turbulence can produce winds in either a hot corona or a cool extended chromosphere, and we specify the conditions that determine whether or not coronal heating occurs. These models do not utilize arbitrary normalization factors, but instead predict the mass loss rate directly from a star's fundamental properties. We take account of stellar magnetic activity by extending standard age-activity-rotation indicators to include the evolution of the filling factor of strong photospheric magnetic fields. We compared the predicted mass loss rates with observed values for 47 stars and found significantly better agreement than was obtained from the popular scaling laws of Reimers, Schroder, and Cuntz. The algorithm used to compute cool-star mass loss rates is provided as a self-contained and efficient computer code. We anticipate that the results from this kind of model can be incorporated straightforwardly into stellar evolution calculations and population synthesis techniques. C1 [Cranmer, Steven R.; Saar, Steven H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu; ssaar@cfa.harvard.edu FU Smithsonian Institution Research Endowment; National Aeronautics and Space Administration (NASA) [NNX09AB27G, NNX10AC11G] FX The authors gratefully acknowledge Nancy Brickhouse, Andrea Dupree, Adriaan van Ballegooijen, Stan Owocki, Ofer Cohen, and the anonymous referee for many valuable discussions. This work was supported by the Sprague Fund of the Smithsonian Institution Research Endowment, and by the National Aeronautics and Space Administration (NASA) under grants NNX09AB27G and NNX10AC11G to the Smithsonian Astrophysical Observatory. This research made extensive use of NASA's Astrophysics Data System and the SIMBAD database operated at CDS, Strasbourg, France. This research has also made use of the NASA/IPAC/NExScI Star and Exoplanet Database (NStED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 242 TC 81 Z9 81 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 1 PY 2011 VL 741 IS 1 AR 54 DI 10.1088/0004-637X/741/1/54 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844TA UT WOS:000296769000054 ER PT J AU Fox, OD Chevalier, RA Skrutskie, MF Soderberg, AM Filippenko, AV Ganeshalingam, M Silverman, JM Smith, N Steele, TN AF Fox, Ori D. Chevalier, Roger A. Skrutskie, Michael F. Soderberg, Alicia M. Filippenko, Alexei V. Ganeshalingam, Mohan Silverman, Jeffrey M. Smith, Nathan Steele, Thea N. TI A SPITZER SURVEY FOR DUST IN TYPE IIn SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; infrared: stars; stars: mass-loss; stars: winds, outflows; supernovae: general ID CORE-COLLAPSE SUPERNOVAE; LUMINOUS BLUE VARIABLES; WOLF-RAYET STARS; MASSIVE STARS; INFRARED ECHO; CIRCUMSTELLAR INTERACTION; SPACE-TELESCOPE; SN 2005IP; PRESUPERNOVA EVOLUTION; RADIO-EMISSION AB Recent observations suggest that Type IIn supernovae (SNe IIn) may exhibit late-time (>100 days) infrared (IR) emission from warm dust more than other types of core-collapse SNe. Mid-IR observations, which span the peak of the thermal spectral energy distribution, provide useful constraints on the properties of the dust and, ultimately, the circumstellar environment, explosion mechanism, and progenitor system. Due to the low SN IIn rate (<10% of all core-collapse SNe), few IR observations exist for this subclass. The handful of isolated studies, however, show late-time IR emission from warm dust that, in some cases, extends for five or six years post-discovery. While previous Spitzer/IRAC surveys have searched for dust in SNe, none have targeted the Type IIn subclass. This paper presents results from a warm Spitzer/IRAC survey of the positions of all 68 known SNe IIn within a distance of 250 Mpc between 1999 and 2008 that have remained unobserved by Spitzer more than 100 days post-discovery. The detection of late-time emission from 10 targets (similar to 15%) nearly doubles the database of existing mid-IR observations of SNe IIn. Although optical spectra show evidence for new dust formation in some cases, the data show that in most cases the likely origin of the mid-IR emission is pre-existing dust, which is continuously heated by optical emission generated by ongoing circumstellar interaction between the forward shock and circumstellar medium. Furthermore, an emerging trend suggests that these SNe decline at similar to 1000-2000 days post-discovery once the forward shock overruns the dust shell. The mass-loss rates associated with these dust shells are consistent with luminous blue variable progenitors. C1 [Fox, Ori D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Chevalier, Roger A.; Skrutskie, Michael F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Filippenko, Alexei V.; Ganeshalingam, Mohan; Silverman, Jeffrey M.; Smith, Nathan; Steele, Thea N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Smith, Nathan] Steward Observ, Dept Astron, Tucson, AZ 85721 USA. RP Fox, OD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM ori.d.fox@nasa.gov FU NASA; NSF [AST-0807727, AST-0908886]; TABASGO Foundation; W. M. Keck Foundation; Bill and Marina Kast FX This work is based on observations made with the Spitzer Space Telescope (PID 60122), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. O.D.F. is grateful for support from the NASA Postdoctoral Program (NPP). R.A.C. was supported by NSF grant AST-0807727. A.V.F. is grateful for the support of NSF grant AST-0908886 and the TABASGO Foundation. J.M.S. thanks Marc J. Staley for a graduate fellowship. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The Kast spectrograph on the Lick 3 m Shane telescope was funded by a gift from Bill and Marina Kast. We thank the staffs of the Lick and Keck Observatories for their assistance with the observations. We are also grateful to many students and postdocs who helped take and reduce the optical spectra. NR 141 TC 51 Z9 52 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 1 PY 2011 VL 741 IS 1 AR 7 DI 10.1088/0004-637X/741/1/7 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844TA UT WOS:000296769000007 ER PT J AU MacLachlan, JM Matthews, LD Wood, K Gallagher, JS AF MacLachlan, J. M. Matthews, L. D. Wood, K. Gallagher, J. S. TI THE STABILITY OF LOW SURFACE BRIGHTNESS DISKS BASED ON MULTI-WAVELENGTH MODELING SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; galaxies: spiral; radiative transfer ID EDGE-ON GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; TELESCOPE ADVANCED CAMERA; CARLO RADIATION TRANSFER; INFRARED EXTINCTION LAW; HI IMAGING OBSERVATIONS; DIFFUSE IONIZED-GAS; SPIRAL GALAXIES; STAR-FORMATION; NGC 4244 AB To investigate the structure and composition of the dusty interstellar medium (ISM) of low surface brightness (LSB) disk galaxies, we have used multi-wavelength photometry to construct spectral energy distributions for three low-mass, edge-on LSB galaxies (V-rot = 88-105 km s(-1)). We use Monte Carlo radiation transfer codes that include the effects of transiently heated small grains and polycyclic aromatic hydrocarbon molecules to model and interpret the data. We find that, unlike the high surface brightness galaxies previously modeled, the dust disks appear to have scale heights equal to or exceeding their stellar scale heights. This result supports the findings of previous studies that low-mass disk galaxies have dust scale heights comparable to their stellar scale heights and suggests that the cold ISM of low-mass, LSB disk galaxies may be stable against fragmentation and gravitational collapse. This may help to explain the lack of observed dust lanes in edge-on LSB galaxies and their low current star formation rates. Dust masses are found in the range (1.16-2.38) x 10(6) M-circle dot, corresponding to face-on (edge-on), V-band, optical depths 0.034 less than or similar to tau(face) less than or similar to 0.106 (0.69 less than or similar to tau(eq) less than or similar to 1.99). C1 [MacLachlan, J. M.; Wood, K.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Matthews, L. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gallagher, J. S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP MacLachlan, JM (reprint author), Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM jmm55@st-andrews.ac.uk FU Jet Propulsion Laboratory (JPL) [1279242]; National Aeronautic and Space Administration (NASA) [1407]; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX Financial support for this work was provided to L.D.M. through contract 1279242 from the Jet Propulsion Laboratory (JPL). This work is based in part on observations from the Spitzer Space Telescope, operated by JPL, California Institute of Technology, under contract 1407 with the National Aeronautic and Space Administration (NASA).; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 77 TC 23 Z9 23 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2011 VL 741 IS 1 AR 6 DI 10.1088/0004-637X/741/1/6 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844TA UT WOS:000296769000006 ER PT J AU McLean, M Berger, E Irwin, J Forbrich, J Reiners, A AF McLean, M. Berger, E. Irwin, J. Forbrich, J. Reiners, A. TI PERIODIC RADIO EMISSION FROM THE M7 DWARF 2MASS J13142039+1320011: IMPLICATIONS FOR THE MAGNETIC FIELD TOPOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum: stars; stars: activity; stars: low-mass; stars: magnetic field ID LOW-MASS STARS; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; ELECTRON-CYCLOTRON MASER; FULLY CONVECTIVE STARS; LSPM-NORTH CATALOG; LARGE-SCALE; ULTRACOOL DWARF; BROWN DWARFS; DUST CLOUDS; X-RAY AB We present multi-epoch radio and optical observations of the M7 dwarf 2MASS J13142039+1320011. We detect a similar to 1 mJy source at 1.43, 4.86, 8.46, and 22.5 GHz, making it the most luminous radio emission over the widest frequency range detected from an ultracool dwarf to date. A 10 hr Very Large Array observation reveals that the radio emission varies sinusoidally with a period of 3.89 +/- 0.05 hr, and an amplitude of approximate to 30% at 4.86 GHz and approximate to 20% at 8.46 GHz. The periodicity is also seen in circular polarization, where at 4.86 GHz the polarization reverses helicity from left-to right-handed in phase with the total intensity. An archival detection in the Faint Images of the Radio Sky at Twenty Centimeters survey indicates that the radio emission has been stable for at least a decade. We also detect periodic photometric variability in several optical filters with a period of 3.79 hr and measure a rotation velocity of v sin i = 45 +/- 5 km s(-1), in good agreement with the radio and optical periods. The subtle difference in radio and optical periods may be due to differential rotation, with Delta Omega approximate to 1 rad day(-1) between the equation and poles. The period and rotation velocity allow us to place a lower limit on the radius of the source of greater than or similar to 0.13 R-circle dot, about 30% larger than theoretical expectations. The properties of the radio emission can be explained with a simple model of a magnetic dipole misaligned relative to the stellar rotation axis, with the sinusoidal variations and helicity reversal due to the rotation of the magnetic poles relative to our line of sight. The long-term stability of the radio emission indicates that the magnetic field (and hence the dynamo) is stable on a much longer timescale than the convective turnover time of similar to 0.2 yr. If the radio emission is due to gyrosynchrotron emission the inferred magnetic field strength is similar to 0.1 kG, while the electron cyclotron maser process requires a field of at least 8 kG. C1 [McLean, M.; Berger, E.; Irwin, J.; Forbrich, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reiners, A.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. RP McLean, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [AST-1008361, AST-0807690]; David and Lucile Packard Fellowship for Science and Engineering; DFG [RE 1664/4-1] FX The authors acknowledge assistance from Philip Nutzman, Zachory Berta, and Peter Challis. E. B. acknowledges support for this work from the National Science Foundation under grant AST-1008361. J.I. gratefully acknowledges funding for the MEarth project from the David and Lucile Packard Fellowship for Science and Engineering (awarded to David Charbonneau), and support from the National Science Foundation under grant number AST-0807690. A. R. received research funding from the DFG as an Emmy Noether fellow (RE 1664/4-1). This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. NR 50 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2011 VL 741 IS 1 AR 27 DI 10.1088/0004-637X/741/1/27 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844TA UT WOS:000296769000027 ER PT J AU Starikova, S Cool, R Eisenstein, D Forman, W Jones, C Hickox, R Kenter, A Kochanek, C Kravtsov, A Murray, SS Vikhlinin, A AF Starikova, S. Cool, R. Eisenstein, D. Forman, W. Jones, C. Hickox, R. Kenter, A. Kochanek, C. Kravtsov, A. Murray, S. S. Vikhlinin, A. TI CONSTRAINING HALO OCCUPATION PROPERTIES OF X-RAY ACTIVE GALACTIC NUCLEI USING CLUSTERING OF CHANDRA SOURCES IN THE BOOTES SURVEY REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: statistics; large-scale structure of universe; X-rays: galaxies ID CROSS-CORRELATION FUNCTION; SUPERMASSIVE BLACK-HOLES; LUMINOUS RED GALAXIES; DIGITAL SKY SURVEY; SPATIAL CORRELATION-FUNCTION; REDSHIFT-SPACE DISTORTIONS; DARK-MATTER HALOES; ANALYTIC MODEL; NUMERICAL SIMULATIONS; ANGULAR-CORRELATION AB We present one of the most precise measurements to date of the spatial clustering of X-ray-selected active galactic nuclei (AGNs) using a sample derived from the Chandra X-ray Observatory survey in the Bootes field. The real-space two-point correlation function over a redshift interval from z = 0.17 to z similar to 3 is well described by the power law,. xi(r) = (r/r(0))-(gamma), for comoving separations r less than or similar to 20 h(-1) Mpc. We find gamma = 1.84 +/- 0.12 and gamma(0) consistent with no redshift trend within the sample (varying between r(0) = 5.5 +/- 0.6 h(-1) Mpc for < z > = 0.37 and r(0) = 6.9 +/- 1.0 h(-1) Mpc for < z > = 1.28). Furthermore, we are able to measure the projections of the two-point correlation function both on the sky plane and in the line of sight. We use these measurements to show that the Chandra/Bootes AGNs are predominantly located at the centers of dark matter halos with circular velocity v(max) > 320 km s(-1) or M(180) > 4.1 x 10(12) h(-1) M(circle dot), and tend to avoid satellite galaxies in halos of this or higher mass. The halo occupation properties inferred from the clustering properties of Chandra/Bootes AGNs-the mass scale of the parent dark matter halos, the lack of significant redshift evolution of the clustering length, and the low satellite fraction-are broadly consistent with the Hopkins et al. scenario of quasar activity triggered by mergers of similarly sized galaxies. C1 [Starikova, S.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Starikova, S.; Eisenstein, D.; Forman, W.; Jones, C.; Kenter, A.; Murray, S. S.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cool, R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hickox, R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Kochanek, C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kravtsov, A.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, E Fermi Inst, Chicago, IL 60637 USA. [Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Vikhlinin, A.] Space Res Inst IKI, Moscow, Russia. RP Starikova, S (reprint author), Univ Padua, Dipartimento Astron, Vicolo Osservatorio 2, I-35122 Padua, Italy. OI Forman, William/0000-0002-9478-1682 FU Smithsonian Institution and NASA [NAS8-39073, NAS8-03060]; NSF [AST-0708154]; NASA [NAG5-13274]; Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-0551142] FX This work was supported by the Smithsonian Institution and NASA through contracts NAS8-39073 and NAS8-03060 (CXC). A.K. is supported by NSF grant AST-0708154, by NASA grant NAG5-13274, and by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-0551142 and an endowment from the Kavli Foundation. We thank O. Gnedin and A. Franceschini for useful discussions and comments. Facilities: CXO, MMT NR 73 TC 27 Z9 27 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 1 PY 2011 VL 741 IS 1 AR 15 DI 10.1088/0004-637X/741/1/15 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844TA UT WOS:000296769000015 ER PT J AU Evans, DA Summers, AC Hardcastle, MJ Kraft, RP Gandhi, P Croston, JH Lee, JC AF Evans, D. A. Summers, A. C. Hardcastle, M. J. Kraft, R. P. Gandhi, P. Croston, J. H. Lee, J. C. TI THE SUZAKU VIEW OF THE DISK-JET CONNECTION IN THE LOW-EXCITATION RADIO GALAXY NGC 6251 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (NGC 6251); galaxies: jets; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATIONS; X-RAY; FR-I; NGC-6251; CHANDRA; ENVIRONMENT; DICHOTOMY; ACCRETION; SAMPLE AB We present results from an 87 ks Suzaku observation of the canonical low-excitation radio galaxy (LERG) NGC6251. We have previously suggested that LERGs violate conventional active galactic nucleus unification schemes: they may lack an obscuring torus and are likely to accrete in a radiatively inefficient manner, with almost all of the energy released by the accretion process being channeled into powerful jets. We model the 0.5-20 keV Suzaku spectrum with a single power law of photon index Gamma = 1.82(-0.05)(+0.04) , together with two collisionally ionized plasma models whose parameters are consistent with the known galaxy- and group-scale thermal emission. Our observations confirm that there are no signatures of obscured, accretion-related X-ray emission in NGC 6251, and we show that the luminosity of any such component must be substantially sub-Eddington in nature. C1 [Evans, D. A.; Kraft, R. P.; Lee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Evans, D. A.; Summers, A. C.] Elon Univ, Dept Phys, Elon, NC 27244 USA. [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Gandhi, P.] Japan Aerosp Explorat Agcy, ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Evans, DA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012; XRAY, SUZAKU/A-1808-2009 OI Hardcastle, Martin/0000-0003-4223-1117; FU NASA [NNX11AD34G]; Jet Propulsion Laboratory, California Institute of Technology, under NASA FX We thank the anonymous referee for providing constructive comments. D.A.E. gratefully acknowledges financial support for this work from NASA under grant number NNX11AD34G. This research has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). This research has also used the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 24 TC 3 Z9 3 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2011 VL 741 IS 1 AR L4 DI 10.1088/2041-8205/741/1/L4 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844NC UT WOS:000296753000004 ER PT J AU Long, DM DeLuca, EE Gallagher, PT AF Long, David M. DeLuca, Edward E. Gallagher, Peter T. TI THE WAVE PROPERTIES OF CORONAL BRIGHT FRONTS OBSERVED USING SDO/AIA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: magnetic topology; waves ID EXTREME-ULTRAVIOLET WAVE; EIT WAVES; MASS EJECTION; SOLAR CORONA; QUIET SUN; PROPAGATING DISTURBANCE; QUADRATURE OBSERVATIONS; SOHO/EIT OBSERVATIONS; MORETON WAVES; MHD WAVES AB Coronal bright fronts (CBFs) are large-scale wavefronts that propagate through the solar corona at hundreds of kilometers per second. While their kinematics have been studied in detail, many questions remain regarding the temporal evolution of their amplitude and pulse width. Here, contemporaneous high cadence, multi-thermal observations of the solar corona from the Solar Dynamic Observatory (SDO) and Solar TErrestrial RElations Observatory (STEREO) spacecraft are used to determine the kinematics and expansion rate of a CBF wavefront observed on 2010 August 14. The CBF was found to have a lower initial velocity with weaker deceleration in STEREO observations compared to SDO observations (similar to 340 km s(-1) and -72 m s(-2) as opposed to similar to 410 km s(-1) and -279 m s(-2)). The CBF kinematics from SDO were found to be highly passband-dependent, with an initial velocity ranging from 379 +/- 12 km s(-1) to 460 +/- 28 km s(-1) and acceleration ranging from -128 +/- 28 m s(-2) to -431 +/- 86 m s(-2) in the 335 angstrom and 304 angstrom passbands, respectively. These kinematics were used to estimate a quiet coronal magnetic field strength range of similar to 1-2 G. Significant pulse broadening was also observed, with expansion rates of similar to 130 km s(-1) (STEREO) and similar to 220 km s(-1) (SDO). By treating the CBF as a linear superposition of sinusoidal waves within a Gaussian envelope, the resulting dispersion rate of the pulse was found to be similar to 8-13 Mm(2) s(-1). These results are indicative of a fast-mode magnetoacoustic wave pulse propagating through an inhomogeneous medium. C1 [Long, David M.; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Long, David M.; Gallagher, Peter T.] Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland. RP Long, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM longda@tcd.ie RI Long, David/J-3227-2013; DeLuca, Edward/L-7534-2013; Gallagher, Peter/C-7717-2011 OI Long, David/0000-0003-3137-0277; DeLuca, Edward/0000-0001-7416-2895; Gallagher, Peter/0000-0001-9745-0400 FU Irish Research Council for Science, Engineering and Technology (IRCSET) FX D.M.L. is a 2010-2011 Pre-Doctoral Fellow at the Harvard-Smithsonian Center for Astrophysics, and carried out some of this work while a Government of Ireland Scholar supported by the Irish Research Council for Science, Engineering and Technology (IRCSET). We thank S. Patsourakos, R. T. J. McAteer, D. S. Bloomfield, and J. Raymond for useful discussions, and the anonymous referee whose comments helped to improve this Letter. NR 41 TC 22 Z9 23 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2011 VL 741 IS 1 AR L21 DI 10.1088/2041-8205/741/1/L21 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844NC UT WOS:000296753000021 ER PT J AU Pillitteri, I Gunther, HM Wolk, SJ Kashyap, VL Cohen, O AF Pillitteri, I. Guenther, H. M. Wolk, S. J. Kashyap, V. L. Cohen, O. TI X-RAY ACTIVITY PHASED WITH PLANET MOTION IN HD 189733? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: activity; stars: coronae; stars: individual (HD189733); X-rays: stars ID STELLAR ACTIVITY ENHANCEMENT; EXTRASOLAR GIANT PLANETS; PROXIMA-CENTAURI; ATOMIC DATABASE; EMISSION-LINES; HOT JUPITERS; XMM-NEWTON; STARS; SPECTROSCOPY; ACCRETION AB We report on the follow-up XMM-Newton observation of the planet-hosting star HD 189733 we obtained in 2011 April. We observe a flare just after the secondary transit of the hot Jupiter. This event shares the same phase and many of the characteristics of the flare we observed in 2009. We suggest that a systematic interaction between planet and stellar magnetic fields when the planet passes close to active regions on the star can lead to periodic variability phased with planetary motion. By means of high-resolution X-ray spectroscopy with the Reflection Grating Spectrometer on board XMM-Newton, we determine that the corona of this star is unusually dense. C1 [Pillitteri, I.; Guenther, H. M.; Wolk, S. J.; Kashyap, V. L.; Cohen, O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pillitteri, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Pillitteri, Ignazio/L-1549-2016; OI Pillitteri, Ignazio/0000-0003-4948-6550; Gunther, Hans Moritz/0000-0003-4243-2840; Wolk, Scott/0000-0002-0826-9261; Cohen, Ofer/0000-0003-3721-0215 FU XMM [NNX09AP46G]; NASA [NAS8-03060, NAS8-39073]; NASA LWSTRT [NNG05GM44G] FX The XMM-Newton guest investigator program supported I.P. and H.M.G. through grant NNX09AP46G. S.J.W. was supported by NASA Contract NAS8-03060 to the Chandra Science Center. V.K. acknowledges CXC NASA Contract NAS8-39073 and O.C. acknowledges NASA LWSTRT Grant NNG05GM44G. NR 28 TC 18 Z9 18 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2011 VL 741 IS 1 AR L18 DI 10.1088/2041-8205/741/1/L18 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844NC UT WOS:000296753000018 ER PT J AU Winn, JN Albrecht, S Johnson, JA Torres, G Cochran, WD Marcy, GW Howard, AW Isaacson, H Fischer, D Doyle, L Welsh, W Carter, JA Fabrycky, DC Ragozzine, D Quinn, SN Shporer, A Howell, SB Latham, DW Orosz, J Prsa, A Slawson, RW Borucki, WJ Koch, D Barclay, T Boss, AP Christensen-Dalsgaard, J Girouard, FR Jenkins, J Klaus, TC Meibom, S Morris, RL Sasselov, D Still, M Van Cleve, J AF Winn, Joshua N. Albrecht, Simon Johnson, John Asher Torres, Guillermo Cochran, William D. Marcy, Geoffrey W. Howard, Andrew W. Isaacson, Howard Fischer, Debra Doyle, Laurance Welsh, William Carter, Joshua A. Fabrycky, Daniel C. Ragozzine, Darin Quinn, Samuel N. Shporer, Avi Howell, Steve B. Latham, David W. Orosz, Jerome Prsa, Andrej Slawson, Robert W. Borucki, William J. Koch, David Barclay, Thomas Boss, Alan P. Christensen-Dalsgaard, Jorgen Girouard, Forrest R. Jenkins, Jon Klaus, Todd C. Meibom, Soren Morris, Robert L. Sasselov, Dimitar Still, Martin Van Cleve, Jeffrey TI SPIN-ORBIT ALIGNMENT FOR THE CIRCUMBINARY PLANET HOST KEPLER-16 A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: general; planets and satellites: formation; stars: individual (Kepler-16 A, KIC 12644769); stars: low-mass; stars: rotation ID LOWER MAIN-SEQUENCE; CLOSE BINARY-SYSTEMS; LOW-MASS STARS; ECLIPSING BINARY; ABSOLUTE DIMENSIONS; EVOLUTIONARY MODELS; HIERARCHICAL TRIPLE; BROWN DWARF; ROTATION; STELLAR AB Kepler-16 is an eccentric low-mass eclipsing binary with a circumbinary transiting planet. Here, we investigate the angular momentum of the primary star, based on Kepler photometry and Keck spectroscopy. The primary star's rotation period is 35.1 +/- 1.0 days, and its projected obliquity with respect to the stellar binary orbit is 1.degrees 6 +/- 2.degrees 4. Therefore, the three largest sources of angular momentum-the stellar orbit, the planetary orbit, and the primary's rotation-are all closely aligned. This finding supports a formation scenario involving accretion from a single disk. Alternatively, tides may have realigned the stars despite their relatively wide separation (0.2 AU), a hypothesis that is supported by the agreement between the measured rotation period and the "pseudosynchronous" period of tidal evolution theory. The rotation period, chromospheric activity level, and fractional light variations suggest a main-sequence age of 2-4 Gyr. Evolutionary models of low-mass stars can match the observed masses and radii of the primary and secondary stars to within about 3%. C1 [Winn, Joshua N.; Albrecht, Simon] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.; Albrecht, Simon] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Johnson, John Asher] NASA Exoplanet Sci Inst NExScI, Pasadena, CA USA. [Torres, Guillermo; Carter, Joshua A.; Ragozzine, Darin; Quinn, Samuel N.; Latham, David W.; Meibom, Soren; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Doyle, Laurance; Slawson, Robert W.; Jenkins, Jon; Morris, Robert L.; Van Cleve, Jeffrey] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA. [Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Welsh, William; Orosz, Jerome] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Boss, Alan P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Christensen-Dalsgaard, Jorgen] Aarhus Univ, Danish AsteroSeismol Ctr, DK-8000 Aarhus C, Denmark. [Christensen-Dalsgaard, Jorgen] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Girouard, Forrest R.; Klaus, Todd C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Barclay, Thomas/0000-0001-7139-2724; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA [NNX09AB33G]; NSF [AST-1007992]; W. M. Keck Foundation FX We thank Brice-Olivier Demory, Nevin Weinberg, and Jamie Lloyd for helpful discussions. Work by J.N.W. and S.A. was supported by NASA Origins award NNX09AB33G. G.T. acknowledges partial support from the NSF through grant AST-1007992. Funding for the Kepler Discovery mission is provided by NASA's Science Mission Directorate. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration, and was made possible by the generous financial support of the W. M. Keck Foundation. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. NR 47 TC 34 Z9 34 U1 1 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2011 VL 741 IS 1 AR L1 DI 10.1088/2041-8205/741/1/L1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844NC UT WOS:000296753000001 ER PT J AU Brickhouse, NS AF Brickhouse, Nancy S. TI Magnetic accretion onto young stars SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE Accretion; Atomic physics; Magnetic fields; Stars: individual (TW Hydrae); Techniques: spectroscopic; X-rays: stars ID CLASSICAL T-TAURI; EMISSION-LINE DIAGNOSTICS; MAGNETOSPHERIC ACCRETION; DISK ACCRETION; HYDRAE; CHANDRA; PLASMA AB Young T Tauri stars exhibit strong solar-type magnetic activity, with extremely high temperature coronae and energetic flares. In a few systems discovered with Chandra and XMM-Newton there is also evidence for X-ray emission produced by shocks associated with magnetically channeled accretion. A recent 489 ksec Chandra HETG/ACIS-S observation of the classical T Tauri star TW Hydrae has provided a wealth of spectroscopic diagnostics not available in lower signal-to-noise ratio observations. Using line ratios for electron temperature, electron density, and column density we have found that the shock produced by the accelerating material in the accretion stream behaves as predicted by standard theory. However, the properties of the post-shock plasma differ substantially from the predictions of standard 1D shock models (Brickhouse et al. in Astrophys. J. 710:1835, 2010). The accretion process apparently heats the stellar atmosphere up to soft X-ray emitting temperatures, providing hot ions to populate the magnetic corona, in loops, stellar wind, and/or jets. This gas is highly turbulent, as evidenced by non-thermal line broadening. The observed properties of the accretion-fed corona should constrain theoretical models of an accretion-driven dynamo. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brickhouse, NS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nbrickhouse@cfa.harvard.edu OI Brickhouse, Nancy/0000-0002-8704-4473 FU NASA [Chandra GO7-8018X, NAS8-03060] FX The author acknowledges collaborators S. R. Cranmer, A. K. Dupree, G.J.M. Luna, and S.J. Wolk. This work was supported by Chandra GO7-8018X from NASA to the Smithsonian Astrophysical Observatory (SAO) and by NASA contract NAS8-03060 to SAO for the Chandra X-ray Center. NR 23 TC 0 Z9 0 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD NOV PY 2011 VL 336 IS 1 BP 75 EP 79 DI 10.1007/s10509-010-0562-0 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844EZ UT WOS:000296731800013 ER PT J AU Simpson, C Kiessling, W Mewis, H Baron-Szabo, RC Muller, J AF Simpson, Carl Kiessling, Wolfgang Mewis, Heike Baron-Szabo, Rosemarie C. Mueller, Johannes TI EVOLUTIONARY DIVERSIFICATION OF REEF CORALS: A COMPARISON OF THE MOLECULAR AND FOSSIL RECORDS SO EVOLUTION LA English DT Article DE Diversification; extinction; fossils; molecular phylogenies; reef corals; speciation ID MARINE DIVERSITY; EXTINCTION RISK; RATES; PHYLOGENIES; ORIGINATION; SPECIATION; SCLERACTINIA; MITOCHONDRIAL; RADIATIONS; MODELS AB Understanding historical patterns of diversity dynamics is of paramount importance for many evolutionary questions. The fossil record has long been the only source of information on patterns of diversification, but the molecular record, derived from time-calibrated phylogenies, is becoming an important additional resource. Both fossil and molecular approaches have shortcomings and biases. These have been well studied for fossil data but much less so for molecular data and empirical comparisons between approaches are lacking. Here, we compare the patterns of diversification derived from fossil and molecular data in scleractinian reef coral species. We also assess the robustness of molecular diversification rates to poor taxon sampling. We find that the temporal pattern of molecular diversification rates is robust to incomplete sampling when rates are calculated per interval. The major obstacle of molecular methods is that rate estimates are distorted because diversification rates can never be negative, whereas the fossil record suffers from incomplete preservation and inconsistent taxonomy. Nevertheless, the molecular pattern of diversification is comparable to the pattern we observe in the fossil record, with the timing of major diversification pulses coinciding in each dataset. For example, both agree that the end-Triassic coral extinction was a catastrophic bottleneck in scleractinian evolution. C1 [Simpson, Carl; Kiessling, Wolfgang; Mewis, Heike; Mueller, Johannes] Humboldt Univ, Museum Nat Kunde, Leibniz Inst, D-10115 Berlin, Germany. [Baron-Szabo, Rosemarie C.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Simpson, C (reprint author), Humboldt Univ, Museum Nat Kunde, Leibniz Inst, D-10115 Berlin, Germany. EM carl.simpson@mfn-berlin.de; wolfgang.kiessling@mfn-berlin.de; heike.mewis@mfn-berlin.de; actinacis@hotmail.com; Johannes.mueller@mfn-berlin.de RI Kiessling, Wolfgang/E-2259-2015; Muller, Johannes/A-6293-2017 OI Muller, Johannes/0000-0001-5801-856X FU VolkswagenStiftung; DFG [KI 806/7-1] FX We thank U. Merkel for contributing substantially to the coral occurrence data and P. Harnik for comments. We also thank G. Hunt, A. Miller, and two anonymous referees for constructive reviews. This work was supported by the VolkswagenStiftung and DFG project # KI 806/7-1. This is Paleobiology Database publication #135. NR 56 TC 20 Z9 20 U1 2 U2 35 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 J9 EVOLUTION JI Evolution PD NOV PY 2011 VL 65 IS 11 BP 3274 EP 3284 DI 10.1111/j.1558-5646.2011.01365.x PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 843VK UT WOS:000296702800020 PM 22023591 ER PT J AU Higgins, L Coddington, J Goodnight, C Kuntner, M AF Higgins, Linden Coddington, Jonathan Goodnight, Charles Kuntner, Matjaz TI Testing ecological and developmental hypotheses of mean and variation in adult size in nephilid orb-weaving spiders SO EVOLUTIONARY ECOLOGY LA English DT Article DE Female gigantism; Sexual size dimorphism; Nephilidae; Nephila; Nephilengys ID DWARF MALE SPIDERS; MALE BODY-SIZE; SEXUAL-DIMORPHISM; PHENOTYPIC PLASTICITY; CONFIDENCE-INTERVALS; DEVELOPMENT TIME; REACTION NORMS; SEASON LENGTH; GIANT FEMALE; CLAVIPES AB Fecundity selection has been hypothesized to drive the evolution of female gigantism in the orb-weaving family Nephilidae. Several species of these spiders also exhibit large amounts of variation in size at maturity in one or both sexes. In this article, we attempt to detect correlations of mean and variation in adult size at a phylogenetic scale between the sexes and with latitude. We tested six predictions derived from three broad developmental, ecological, and age structure hypotheses, using independent contrasts and a recent species-level nephilid phylogeny as well as least squares and other conventional statistics: 1. In both sexes, species with larger mean size will have greater variation in size; 2. Males and females will show correlated changes in mean size and of variation in size; 3. In both sexes, mean size will be negatively correlated with the midpoint of the latitudinal range; 4. In both sexes, tropical species will be more variable; 5. In both sexes, more widespread species will be more variable; 6. Variation in male size will be positively correlated with mean female size. In no cases were male and female development correlated, suggesting that in this lineage male and female body size evolve independently. The only significant trend detected was a positive phylogenetic correlation between variation in female size and latitude, the opposite of prediction 4. Power tests showed that in all tests of the ecological hypothesis, sample sizes were more than adequate to detect significant trends, if present. Our results suggest that evolutionary trends in juvenile development among species are too weak to be detectable in such data sets. C1 [Higgins, Linden; Goodnight, Charles] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Coddington, Jonathan] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Ljubljana, Slovenia. RP Higgins, L (reprint author), Univ Vermont, Dept Biol, Burlington, VT 05405 USA. EM Linden.Higgins@uvm.edu; coddington@si.edu; Charles.Goodnight@uvm.edu; kuntner@gmail.com FU US National Science Foundation [INT-1235778, DEB-9712353, EAR-0228699]; Slovenian Research Agency [Z1-7082-0618, BI-US/06-07-026]; European Commission [MIRG-CT-2005 036536] FX We are grateful to many people for help in the preparation of this manuscript, especially numerous patient curators. Financial support during the collection of data and preparation of the manuscript came from the US National Science Foundation with grants to LEH (INT-1235778) and JC (PEET grant DEB-9712353 and EAR-0228699), from the Slovenian Research Agency to MK and JC (ARRS grants Z1-7082-0618, BI-US/06-07-026) and the European Commission's 6th FP to MK (MIRG-CT-2005 036536). From the Smithsonian NMNH, D. DeRoche helped with the specimen management and K. Darrow prepared all the figures. Specimen measurements and data entry were done in part by M. Gregoric. (Ljubljana) and A. Gallant Bernstein, J. Madden, R. Webber, B. Mulcahey and S. Wanamaker at UVM. Additional data were graciously contributed by J. Schneider, M. Elgar, and H. Japyassu. T. Garland and P. Midford helped us navigate the intricacies of PDAP within Mesquite. Conversations with K. Pickett also aided in our understanding of the statistics employed in these analyses. Comments from several anonymous reviewers were very helpful in preparation of the final manuscript. NR 58 TC 11 Z9 11 U1 2 U2 19 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0269-7653 J9 EVOL ECOL JI Evol. Ecol. PD NOV PY 2011 VL 25 IS 6 BP 1289 EP 1306 DI 10.1007/s10682-011-9475-9 PG 18 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 834RV UT WOS:000295982300008 ER PT J AU Ivanenko, VN Defaye, D Segonzac, M Khripounoff, A Sarrazin, J Ferrari, FD AF Ivanenko, Viatcheslav N. Defaye, Danielle Segonzac, Michel Khripounoff, Alexis Sarrazin, Jozee Ferrari, Frank D. TI A new species of Exrima, synonymy of four species of Aphotopontius, Stygiopontius and Rhogobius, and record of first copepodid stage of Dirivultidae (Copepoda: Siphonostomatoida) from deep-sea hydrothermal vents of the East Pacific Rise (13 degrees N) SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE Copepoda; Siphonostomatoida; Dirivultidae; new species; synonymy; new records; deep-sea; hydrothermal vents; East Pacific Rise; Mid-Atlantic Ridge ID MID-ATLANTIC RIDGE; N-SP COPEPODA; NORTHEASTERN PACIFIC; COLD SEEPS; FAMILY; WATER; ASTEROCHERIDAE; HARPACTICOIDA; SITES; GENUS AB Females of the new species Exrima walteri sp. nov. were found in sediment trap samples deployed over different sites of the East Pacific Rise (13 degrees N) at 2600 m depth. Four traps were deposited during the HOPE99 cruise (1999) and recovered during the AMISTAD (1999) cruise on the research vessel 'L'Atalante'. The new species is distinguished from congeners, E. singula Humes, 1987 and E. dolichopus Humes, 1987, by the following derived characters: first somite of the urosome with 3 (one dorsal and two lateral) stout conical extensions; distal endopodal segment on the swimming leg 4 broad. In addition, many specimens of copepodids I and lecithotrophic nauplii, identified as belonging to Dirivultidae gen. sp., were found in the samples of all sediment traps. This is the first record of copepodids I and of a nauplius of dirivultids from the Pacific Ocean. Study of type and additional material collected during different Ifremer cruises at different vent sites (HERO91, EXOMAR, PHARE and MoMARETO) required synonymy of four species of Aphotopontius Humes, 1987, Stygiopontius Humes, 1987 and Rhogobius Humes, 1987. Aphotopontius rapunculus Humes and Segonzac, 1998 is transferred to the genus Rhogobius because it possesses all presumed derived attributes of this genus: last abdominal somite with lobes at sides of anal operculum; second segment of antennal endopod elongate and slender. A new study of the type material suggests that: Aphotopontius temperatus Humes, 1997 is a synonym of A. atlanteus Humes, 1996; Stygiopontius lumiger Humes, 1989 is a synonym of S. sentifer Humes, 1987 while S. bulbisetiger Humes, 1996 is a synonym of S. pectinatus Humes, 1987. Females of the three synonymized species were found to be sub-adult females at copepodid V. Leg 6 on these specimens is one seta located dorsolaterally on the posterior part of the genital somite. This position for leg 6 is unknown for copepodid V of other siphonostomatoids whose leg 6 is located ventrally at copepodid V; the dorsolateral position is presumed derived and shared by the dirivultid genera Aphotopontius Humes, 1987 and Stygiopontius Humes, 1987. A new key to the Dirivultidae genera is presented. C1 [Ivanenko, Viatcheslav N.] Moscow MV Lomonosov State Univ, Dept Invertebrate Zool, Fac Biol, Moscow 119899, Russia. [Defaye, Danielle; Segonzac, Michel] Museum Natl Hist Nat, Dept Milieux & Peuplements Aquat, UMR 7208, F-75005 Paris, France. [Khripounoff, Alexis; Sarrazin, Jozee] IFREMER, Dept Etude Ecosyst Profonds, Lab Environm Profond, Ctr Brest, F-29280 Plouzane, France. [Ferrari, Frank D.] Smithsonian Inst, IZ MSC, Natl Museum Nat Hist, Suitland, MD 20746 USA. RP Ivanenko, VN (reprint author), Moscow MV Lomonosov State Univ, Dept Invertebrate Zool, Fac Biol, Moscow 119899, Russia. EM ivanenko@mail.bio.msu.ru RI Ivanenko, Viatcheslav/B-8198-2008; MNHN/CNRS/UPMC/IRD, UMR BOREA/B-2312-2012 OI Ivanenko, Viatcheslav/0000-0003-1255-0491; FU Museum National d'Histoire Naturelle and Ifremer (France); Smithsonian Institution (USA); Russian Foundation for Basic Research [09-04-01523-a]; Ministry of Education and Science of the Russian Federation [02.740.11.0280, H1291, 02.740.11.0875]; AMORES [MAST3 CT 95-0040]; EXOCET/D FX The authors are indebted to the chief scientists of the cruises HERO91 (chief scientist Daniel Desbruyeres), AMISTAD (chief scientist Christian Jeanthon), HOPE99 (chief scientist Francois Lallier), PHARE (chief scientist Nadine Le Bris), EXOMAR (chief scientist Anne Godfroy), and MoMARETO (chief scientists Jozee Sarrazin and Pierre-Marie Sarradin); the crews of the research vessels 'Nadir', 'L'Atalante' and 'Pourquoi Pas?' and of the manned submersible 'Nautile', and the remotely operated vehicle 'Victor 6000'. The cruises were supported by European programmes AMORES (MAST3 CT 95-0040) and EXOCET/D. Philippe Crassous (Ifremer DEEP) prepared sampling arrays; Patrick Briand (Ifremer DEEP) provided sorted material and data obtained during colonization experiments. This work was supported by grants from the Museum National d'Histoire Naturelle and Ifremer (France), Smithsonian Institution (USA), the Russian Foundation for Basic Research (09-04-01523-a), and the Ministry of Education and Science of the Russian Federation (02.740.11.0280, H1291, 02.740.11.0875). NR 35 TC 2 Z9 2 U1 0 U2 8 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 EI 1469-7769 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD NOV PY 2011 VL 91 IS 7 BP 1547 EP 1559 DI 10.1017/S0025315411000178 PG 13 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 837VI UT WOS:000296233300016 ER PT J AU Cardoso, NA Le Pendu, Y Lapenta, MJ Raboy, BE AF Cardoso, Nayara A. Le Pendu, Yvonnick Lapenta, Marina J. Raboy, Becky E. TI Frugivory patterns and seed dispersal by golden-headed lion tamarins (Leontopithecus chrysomelas) in Una Biological Reserve, Bahia, Brazil SO MAMMALIA LA English DT Article DE Atlantic forest; frugivory; Leontopithecus chrysomelas; primates; seed dispersal; South America ID SAGUINUS-FUSCICOLLIS; SOUTHEASTERN BRAZIL; SYMPATRIC PRIMATES; ALOUATTA-SENICULUS; ATLANTIC FOREST; SOUTHERN BAHIA; RAIN-FOREST; MONKEYS; BLACK; GERMINATION AB This study identified fruit species eaten by Leontopithecus chrysomelas (golden-headed lion tamarins; GHLTs) and related their consumption to seed dispersal. Two GHLT groups were monitored from September 2006 through August 2007 in Una Biological Reserve, Bahia, Brazil. GHLTs consumed fruit from 71 species, preferred mature fruit and swallowed the seeds of most species (76.8%). Smaller seeds were swallowed and larger seeds were generally discarded. GHLTs defecated in low quantities and more than 50% of the faeces contained seeds from only one species. Most faeces were deposited far from the parental tree (>20m) and only 24.2% under the parental tree. The defecation pattern of L. chrysomelas could reduce competition between seeds and facilitate the establishment of seedlings from the most consumed species. Faeces were deposited widely throughout home ranges and away from a seed's parental tree increasing the chances that seeds reach favourable environments and avoid competition with other seedlings. Additionally, defecations also occurred in the same habitat type as a seed's parental tree, keeping species within their typical habitat. GHLTs in Una Biological Reserve were efficient dispersers and might play an important role in the maintenance of floristic composition and regeneration of habitat. C1 [Cardoso, Nayara A.; Le Pendu, Yvonnick] Univ Estadual Santa Cruz, Dept Biol, BR-45662900 Ilheus, Bahia, Brazil. [Lapenta, Marina J.] Inst Pri Matas Conservcao Biodiversidade, BR-30140970 Belo Horizonte, MG, Brazil. [Raboy, Becky E.] Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. RP Cardoso, NA (reprint author), Univ Estadual Santa Cruz, Dept Biol, Rodovia Ilheus Itabuna,Km 16, BR-45662900 Ilheus, Bahia, Brazil. EM nayara_cardoso@yahoo.com.br RI Le Pendu, Yvonnick/B-3463-2008 FU FAPESB [1629/2006] FX Field work was carried out within the infrastructure of the Golden-Headed Lion Tamarin Project (PIs B.E. Raboy and J.M. Dietz). We thank the Instituto de Estudos Socioambientais do Sul da Bahia (IESB) and Universidade Estadual de Santa Cruz (UESC)-Zoology Postgraduate Program for providing institutional and logistic support. We thank IBAMA for the permission to work in Una Biological Reserve (Licence number 12279-1) and FAPESB for the scholarship grant to N.A. Cardoso (Term 1629/2006). We are extremely grateful to Gilvan Gomes Mota and Jiomario dos Santos Souza for their field assistance and to James Dietz, Lilian Catenacci, Kristel De Vleeschouwer, Leonardo Neves and Carlos Guidorizzi for their assistance with GHLT captures and/or processing during the study period. NR 63 TC 3 Z9 3 U1 4 U2 33 PU WALTER DE GRUYTER & CO PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0025-1461 J9 MAMMALIA JI Mammalia PD NOV PY 2011 VL 75 IS 4 BP 327 EP 337 DI 10.1515/MAMM.2011.042 PG 11 WC Zoology SC Zoology GA 844RQ UT WOS:000296765400003 ER PT J AU Pre, CG Culver, SJ Mallinson, DJ Farrell, KM Corbett, DR Horton, BP Hillier, C Riggs, SR Snyder, SW Buzas, MA AF Pre, Candace Grand Culver, Stephen J. Mallinson, David J. Farrell, Kathleen M. Corbett, D. Reide Horton, Benjamin P. Hillier, Caroline Riggs, Stanley R. Snyder, Scott W. Buzas, Martin A. TI Rapid Holocene coastal change revealed by high-resolution micropaleontological analysis, Pamlico Sound, North Carolina, USA SO QUATERNARY RESEARCH LA English DT Article DE Foraminifera; Diatoms; Holocene; Paleoenvironments ID RADIOCARBON AGE CALIBRATION; RECENT ENVIRONMENTAL-CHANGE; CAL KYR BP; OUTER BANKS; BENTHIC FORAMINIFERA; ALBEMARLE EMBAYMENT; UNITED-STATES; CLIMATE; RECORD; ISLAND AB Foraminiferal analyses of 404 contiguous samples, supported by diatom, lithologic, geochronologic and seismic data, reveal both rapid and gradual Holocene paleoenvironmental changes in an 8.21-m vibracore taken from southern Pamlico Sound, North Carolina. Data record initial flooding of a latest Pleistocene river drainage and the formation of an estuary 9000 yr ago. Estuarine conditions were punctuated by two intervals of marine influence from approximately 4100 to 3700 and 1150 to 500 cal yr BP. Foraminiferal assemblages in the muddy sand facies that accumulated during these intervals contain many well-preserved benthic foraminiferal species, which occur today in open marine settings as deep as the mid shelf, and significant numbers of well-preserved planktonic foraminifera, some typical of Gulf Stream waters. We postulate that these marine-influenced units resulted from temporary destruction of the southern Outer Banks barrier islands by hurricanes. The second increase in marine influence is coeval with increased rate of sea-level rise and a peak in Atlantic tropical cyclone activity during the Medieval Climate Anomaly. This high-resolution analysis demonstrates the range of environmental variability and the rapidity of coastal change that can result from the interplay of changing climate, sea level and geomorphology in an estuarine setting. (C) 2011 University of Washington. Published by Elsevier Inc. All rights reserved. C1 [Pre, Candace Grand; Culver, Stephen J.; Mallinson, David J.; Corbett, D. Reide; Riggs, Stanley R.; Snyder, Scott W.] E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. [Pre, Candace Grand; Horton, Benjamin P.] Univ Penn, Sea Level Res Lab, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. [Farrell, Kathleen M.] N Carolina Geol Survey, Raleigh Field Off & Core Repository, Raleigh, NC 27699 USA. [Corbett, D. Reide] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA. [Hillier, Caroline] Argos Ecol Ltd, Annfield Plain, Durham DH9 7XN, England. [Buzas, Martin A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Culver, SJ (reprint author), E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. EM culvers@ecu.edu FU Cushman Foundation; U.S. Geological Survey [02ERAG0044]; American Chemical Society FX We thank I. Abbene, D. Ames, J. Foley, J. Jett, M. Hale, K. McDowell, L Metger, J. Ricardo, J. Rosenberger, C. Smith, D. Twamley, D. Vance, J. Watson and J. Woods for their assistance. The efforts of Stephen Gallagher and an anonymous reviewer are greatly appreciated. The Cushman Foundation and the U.S. Geological Survey (cooperative agreement 02ERAG0044) provided funding for this project. Acknowledgement is also made to the donors of The American Chemical Society Petroleum Research Fund for partial support of this research. NR 68 TC 7 Z9 7 U1 2 U2 30 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0033-5894 J9 QUATERNARY RES JI Quat. Res. PD NOV PY 2011 VL 76 IS 3 BP 319 EP 334 DI 10.1016/j.yqres.2011.06.012 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 843LA UT WOS:000296672100004 ER PT J AU Gowaty, PA AF Gowaty, Patricia Adair TI What is sexual selection and the short herstory of female trait variation SO BEHAVIORAL ECOLOGY LA English DT Editorial Material DE sexual selection ID BLUEBIRDS SIALIA-SIALIS; DECREASE OFFSPRING VIABILITY; EASTERN BLUEBIRDS; MATE PREFERENCES; REPRODUCTIVE COMPENSATION; ANAS-PLATYRHYNCHOS; CONSTRAINTS; AGGRESSION; HYPOTHESIS; MALLARDS C1 [Gowaty, Patricia Adair] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Gowaty, Patricia Adair] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA 90095 USA. [Gowaty, Patricia Adair] Smithsonian Trop Res Inst, Unit 9100, DPO, AA 34002 USA. RP Gowaty, PA (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr S, Los Angeles, CA 90095 USA. EM gowaty@eeb.ucla.edu NR 16 TC 1 Z9 1 U1 9 U2 37 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 J9 BEHAV ECOL JI Behav. Ecol. PD NOV-DEC PY 2011 VL 22 IS 6 BP 1146 EP 1147 DI 10.1093/beheco/arr113 PG 2 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 838MB UT WOS:000296295000007 ER PT J AU Knudsen, E Linden, A Both, C Jonzen, N Pulido, F Saino, N Sutherland, WJ Bach, LA Coppack, T Ergon, T Gienapp, P Gill, JA Gordo, O Hedenstroom, A Lehikoinen, E Marra, PP Moller, AP Nilsson, ALK Peron, G Ranta, E Rubolini, D Sparks, TH Spina, F Studds, CE Saether, SA Tryjanowski, P Stenseth, NC AF Knudsen, Endre Linden, Andreas Both, Christiaan Jonzen, Niclas Pulido, Francisco Saino, Nicola Sutherland, William J. Bach, Lars A. Coppack, Timothy Ergon, Torbjorn Gienapp, Phillip Gill, Jennifer A. Gordo, Oscar Hedenstrom, Anders Lehikoinen, Esa Marra, Peter P. Moller, Anders P. Nilsson, Anna L. K. Peron, Guillaume Ranta, Esa Rubolini, Diego Sparks, Tim H. Spina, Fernando Studds, Colin E. Saether, Stein A. Tryjanowski, Piotr Stenseth, Nils Chr. TI Challenging claims in the study of migratory birds and climate change SO BIOLOGICAL REVIEWS LA English DT Article DE bird migration; climate change; phenology; annual life cycle; match-mismatch; endogenous control; phenotypic plasticity; microevolutionary change; population trends; integrative biology ID NORTH-ATLANTIC OSCILLATION; LONG-DISTANCE MIGRANTS; SPRING ARRIVAL DATES; TERM POPULATION DECLINES; STORKS CICONIA-CICONIA; WEST-AFRICAN RAINFALL; AVIAN MIGRATION; NATURAL-SELECTION; AMERICAN BIRDS; BARN SWALLOW AB Recent shifts in phenology in response to climate change are well established but often poorly understood. Many animals integrate climate change across a spatially and temporally dispersed annual life cycle, and effects are modulated by ecological interactions, evolutionary change and endogenous control mechanisms. Here we assess and discuss key statements emerging from the rapidly developing study of changing spring phenology in migratory birds. These well-studied organisms have been instrumental for understanding climate-change effects, but research is developing rapidly and there is a need to attack the big issues rather than risking affirmative science. Although we agree poorly on the support for most claims, agreement regarding the knowledge basis enables consensus regarding broad patterns and likely causes. Empirical data needed for disentangling mechanisms are still scarce, and consequences at a population level and on community composition remain unclear. With increasing knowledge, the overall support ('consensus view') for a claim increased and between-researcher variability in support ('expert opinions') decreased, indicating the importance of assessing and communicating the knowledge basis. A proper integration across biological disciplines seems essential for the field's transition from affirming patterns to understanding mechanisms and making robust predictions regarding future consequences of shifting phenologies. C1 [Knudsen, Endre; Ergon, Torbjorn; Nilsson, Anna L. K.; Saether, Stein A.; Stenseth, Nils Chr.] Univ Oslo, CEES, Dept Biol, NO-0316 Oslo, Norway. [Linden, Andreas; Ranta, Esa] Univ Helsinki, Dept Biol & Environm Sci, Integrat Ecol Unit, FIN-00014 Helsinki, Finland. [Both, Christiaan] Univ Groningen, Ctr Ecol & Evolutionary Studies, Anim Ecol Grp, NL-9750 AA Haren, Netherlands. [Jonzen, Niclas; Hedenstrom, Anders] Lund Univ, Dept Biol, SE-22362 Lund, Sweden. [Pulido, Francisco; Gordo, Oscar] Univ Complutense Madrid, Dept Zool & Phys Anthropol, Fac Biol, E-28040 Madrid, Spain. [Saino, Nicola; Rubolini, Diego] Univ Milan, Dipartimento Biol, I-20133 Milan, Italy. [Sutherland, William J.] Univ Cambridge, Dept Zool, Conservat Sci Grp, Cambridge CB2 3EJ, England. [Bach, Lars A.] Lund Univ, Dept Theoret Ecol, SE-22362 Lund, Sweden. [Coppack, Timothy] Univ Zurich, Zool Museum, CH-8057 Zurich, Switzerland. [Gienapp, Phillip] Univ Helsinki, Dept Biol & Environm Sci, Ecol Genet Res Unit, FIN-00014 Helsinki, Finland. [Gill, Jennifer A.] Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England. [Lehikoinen, Esa] Univ Turku, Sect Ecol, Turku 20014, Finland. [Marra, Peter P.; Studds, Colin E.] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [Moller, Anders P.] Univ Paris 11, Lab Ecol Syst & Evolut, F-91405 Orsay, France. [Peron, Guillaume] CNRS, Ctr Ecol Fonct & Evolut, Equipe Biometrie & Biol Populat, UMR 5175, F-34293 Montpellier, France. [Sparks, Tim H.; Tryjanowski, Piotr] Poznan Univ Life Sci, Inst Zool, PL-60625 Poznan, Poland. [Spina, Fernando] Ist Super Protez Ric Ambientale, I-40064 Ozzano Dell Emilia, Italy. RP Stenseth, NC (reprint author), Univ Oslo, CEES, Dept Biol, POB 1066 Blindern, NO-0316 Oslo, Norway. EM n.c.stenseth@bio.uio.no RI Both, Christiaan/E-6459-2011; Studds, Colin/C-3701-2012; Pulido, Francisco/C-6697-2012; Coppack, Timothy/D-1204-2010; Gordo, Oscar/A-4701-2013; Sutherland, William/B-1291-2013; PERON, Guillaume/C-5379-2013; Gienapp, Phillip/A-2261-2014; Gill, Jennifer/A-7759-2008; Hedenstrom, Anders/F-5377-2010; Evolution and Conservation Biology, UCM Group /K-9382-2014; Rubolini, Diego/F-2851-2011; Lehikoinen, Esa /I-6128-2013; Stenseth, Nils Chr./G-5212-2016; Linden, Andreas/D-9315-2017; OI Pulido, Francisco/0000-0002-2430-8080; Gordo, Oscar/0000-0003-3766-0566; Gienapp, Phillip/0000-0002-9368-8769; Hedenstrom, Anders/0000-0002-1757-0945; Rubolini, Diego/0000-0003-2703-5783; Lehikoinen, Esa /0000-0002-6932-3604; Stenseth, Nils Chr./0000-0002-1591-5399; Linden, Andreas/0000-0002-5548-2671; Linden, Anthony/0000-0002-9343-9180; Bach, Lars A./0000-0001-8610-7834; Sutherland, William/0000-0002-6498-0437; Sparks, Tim/0000-0003-4382-7051; Nilsson, Anna/0000-0002-5609-4988; Saino, Nicola/0000-0002-0230-3967 FU NordForsk through the Nordic Centre of Excellence EcoClim FX E.K., A.L., N.J., L.B., T.E., N.C.S. and two meetings were partially funded by NordForsk through the Nordic Centre of Excellence EcoClim. We thank collaborators and field workers inside and outside academia for thought-provoking long-term data and discussions, and the reviewers for comments and suggestions that helped improve the manuscript. NR 237 TC 124 Z9 125 U1 20 U2 256 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1464-7931 EI 1469-185X J9 BIOL REV JI Biol. Rev. PD NOV PY 2011 VL 86 IS 4 BP 928 EP 946 DI 10.1111/j.1469-185X.2011.00179.x PG 19 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 840XL UT WOS:000296475300010 PM 21489123 ER PT J AU Mascaro, J Litton, CM Hughes, RF Uowolo, A Schnitzer, SA AF Mascaro, Joseph Litton, Creighton M. Hughes, R. Flint Uowolo, Amanda Schnitzer, Stefan A. TI Minimizing Bias in Biomass Allometry: Model Selection and Log-transformation of Data SO BIOTROPICA LA English DT Article DE allometry; Hawai'i; heteroscedasticity; linear regression; nonlinear regression analysis; Psidium cattleianum ID LOGARITHMIC TRANSFORMATION; FORESTS; HAWAII; INVASION; PLANTS AB Nonlinear regression is increasingly used to develop allometric equations for forest biomass estimation (i.e., as opposed to the traditional approach of log-transformation followed by linear regression). Most statistical software packages, however, assume additive errors by default, violating a key assumption of allometric theory and possibly producing spurious models. Here, we show that such models may bias stand-level biomass estimates by up to 100 percent in young forests, and we present an alternative nonlinear fitting approach that conforms with allometric theory. C1 [Mascaro, Joseph] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 96025 USA. [Mascaro, Joseph; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama. [Mascaro, Joseph; Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53211 USA. [Litton, Creighton M.] Univ Hawaii Manoa, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA. [Hughes, R. Flint; Uowolo, Amanda] US Forest Serv, Inst Pacific Isl Forestry, USDA, Hilo, HI 96720 USA. RP Mascaro, J (reprint author), Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 96025 USA. EM jmascaro@stanford.edu OI Schnitzer, Stefan/0000-0002-2715-9455 FU Applied Ecological Services Inc.; NSF; UWM; National Science Foundation [DEB-0816486] FX Jim Baldwin (USFS-PSW) provided assistance fitting models. J. Mascaro was supported by a grant from Applied Ecological Services Inc., an NSF Graduate Research Fellowship, and a UWM Golda Meir Library Scholar Award. Additional support was provided by a grant from the National Science Foundation to C. M. Litton (DEB-0816486). Comments from four anonymous reviewers improved this manuscript. NR 17 TC 27 Z9 29 U1 8 U2 37 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD NOV PY 2011 VL 43 IS 6 BP 649 EP 653 DI 10.1111/j.1744-7429.2011.00798.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 846NF UT WOS:000296909800001 ER PT J AU Yanoviak, SP Berghoff, SM Linsenmair, KE Zotz, G AF Yanoviak, Stephen P. Berghoff, Stefanie M. Linsenmair, K. Eduard Zotz, Gerhard TI Effects of an Epiphytic Orchid on Arboreal Ant Community Structure in Panama SO BIOTROPICA LA English DT Article DE Annona glabra; Caularthron bilamellatum; myrmecophyte; tropical forest ID TROPICAL RAIN-FOREST; SPECIES-DIVERSITY; ANNONA-GLABRA; CANOPY; ABUNDANCE; NECTAR; INVERTEBRATES; ASSEMBLAGES; HYMENOPTERA; FORMICIDAE AB Epiphytes are conspicuous structural elements of tropical forest canopies. Individual tree crowns in lowland forests may support more than 30 ant species, yet we know little about the effects of epiphytes on ant diversity. We examined the composition of arboreal ant communities on Annona glabra trees and their interactions with the epiphytic orchid Caularthron bilamellatum in Panama. We surveyed the ants on 73 trees (45 with C. bilamellatum and 28 lacking epiphytes) and recorded their nest sites and behavioral dominance at baits. We found a total of 49 ant species (in 20 genera), ranging 1-9 species per tree. Trees with C. bilamellatum had higher average (+SD) ant species richness (4.2 + 2.28) than trees without epiphytes (2.7 + 1.21). Hollow pseudobulbs (PBs) of C. bilamellatum were used as nest sites by 32 ant species, but only 43 percent of suitable PBs were occupied. Ant species richness increased with PB abundance in trees, but nest sites did not appear to be a limiting resource on A. glabra. We detected no close association between ants and the orchid. We conclude that higher ant species richness in the presence of the orchid is due to bottom-up effects, especially the year-round supply of extrafloral nectar. The structure of ant communities on A. glabra partly reflects interference competition among behaviorally dominant species and stochastic factors, as observed in other forests. C1 [Yanoviak, Stephen P.] Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA. [Berghoff, Stefanie M.; Linsenmair, K. Eduard] Univ Wurzburg, Theodor Boveri Inst, Dept Anim Ecol & Trop Biol, D-97074 Wurzburg, Germany. [Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Balboa, Panama. RP Yanoviak, SP (reprint author), Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA. EM spyanoviak@ualr.edu FU University of Wurzburg (HSPIII); National Science Foundation [IOS-0843120] FX Critical input from Jack Longino and two anonymous reviewers improved this paper. Comments from Ulrich Simon provided the inspiration for this project and Jack Longino assisted with ant identifications. Oris Acevedo, Hans Peter Heckrodt, Sabine Armsen, and the staff of the Smithsonian Tropical Research Institute provided logistical support. This work was supported by grants from the University of Wurzburg (HSPIII) to SMB and the National Science Foundation (IOS-0843120) to SPY. NR 58 TC 9 Z9 9 U1 2 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD NOV PY 2011 VL 43 IS 6 BP 731 EP 737 DI 10.1111/j.1744-7429.2011.00764.x PG 7 WC Ecology SC Environmental Sciences & Ecology GA 846NF UT WOS:000296909800011 ER PT J AU Farris, DW Jaramillo, C Bayona, G Restrepo-Moreno, SA Montes, C Cardona, A Mora, A Speakman, RJ Glascock, MD Valencia, V AF Farris, David W. Jaramillo, Carlos Bayona, German Restrepo-Moreno, Sergio A. Montes, Camilo Cardona, Agustin Mora, Andres Speakman, Robert J. Glascock, Michael D. Valencia, Victor TI Fracturing of the Panamanian Isthmus during initial collision with South America SO GEOLOGY LA English DT Article ID NORTHERN ANDES; GEOCHEMICAL EVOLUTION; EASTERN CORDILLERA; WESTERN PANAMA; LAND-BRIDGE; ARC; DEFORMATION; COLOMBIA; PLATE; STRATIGRAPHY AB Tectonic collision between South America and Panama began at 23-25 Ma. The collision is significant because it ultimately led to development of the Panamanian Isthmus, which in turn had wide-ranging oceanic, climatic, biologic, and tectonic implications. Within the Panama Canal Zone, volcanic activity transitioned from hydrous mantle-wedge-derived arc magmatism to localized extensional arc magmatism at 24 Ma, and overall marks a permanent change in arc evolution. We interpret the arc geochemical change to result from fracturing of the Panama block during initial collision with South America. Fracturing of the Panama block led to localized crustal extension, normal faulting, sedimentary basin formation, and extensional magmatism in the Canal Basin and Bocas del Toro. Synchronous with this change, both Panama and inboard South America experienced a broad episode of exhumation indicated by ( U-Th)/He and fission-track thermochronology coupled with changing geographic patterns of sedimentary deposition in the Colombian Eastern Cordillera and Llanos Basin. Such observations allow for construction of a new tectonic model of the South America-Panama collision, northern Andes uplift and Panama orocline formation. Finally, synchroneity of Panama arc chemical changes and linked uplift indicates that onset of collision and Isthmus formation began earlier than commonly assumed. C1 [Farris, David W.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. [Jaramillo, Carlos; Bayona, German; Restrepo-Moreno, Sergio A.; Montes, Camilo; Cardona, Agustin] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. [Bayona, German; Montes, Camilo; Cardona, Agustin] Corp Geol ARES, Bogota, Colombia. [Restrepo-Moreno, Sergio A.] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. [Mora, Andres] Ecopetrol, Inst Colombiano Petr, Bucaramanga, Colombia. [Speakman, Robert J.] Museum Conservat Inst, Smithsonian Inst, Washington, DC 20012 USA. [Glascock, Michael D.] Univ Missouri, Archaeometry Lab, Columbia, MO 65211 USA. [Valencia, Victor] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. RP Farris, DW (reprint author), Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. OI Glascock, Michael D./0000-0003-0686-7556; Speakman, Robert/0000-0003-2063-154X; Montes, Camilo/0000-0002-3553-0787 FU National Science Foundation (NSF) [0966884, DEB-0733725]; Smithsonian Institution; Panama Canal Authority; National Geographic; SENACYT; Ricardo Perez SA FX This contribution to the Panama Canal Project (PCP) was supported by National Science Foundation (NSF) PIRE grant 0966884 (OISE, EAR, DRL). Funding also came from NSF grant DEB-0733725, the Smithsonian Institution, the Panama Canal Authority, Mr. Mark Tupper, the National Geographic, SENACYT, and Ricardo Perez SA. Thanks go to the Panama Canal Authority, Ministerio de Industria y Comercio, Odebretch, and to the Kuna Congress and Nation for access and logistical help. NR 34 TC 110 Z9 112 U1 8 U2 52 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD NOV PY 2011 VL 39 IS 11 BP 1007 EP 1010 DI 10.1130/G32237.1 PG 4 WC Geology SC Geology GA 842OA UT WOS:000296607600006 ER PT J AU Lucking, R Schulz, K Crespo, A Nash, TH Lumbsch, HT AF Luecking, Robert Schulz, Katja Crespo, Ana Nash, Thomas H. Lumbsch, H. Thorsten TI The Encyclopedia of Life (EOL) as a scientific resource and outreach medium applied to the lichen family Parmeliaceae (Ascomycota: Lecanorales) SO LICHENOLOGIST LA English DT Article DE BioSync; Index Fungorum; Hypogymnia; Menegazzia; Parmotrema ID COMMUNICATION; FUTURE AB A brief discussion of the Encyclopedia of Life and the LifeDesks websites as a means to assemble and publish species pages and taxonomic information on the internet, for both the scientific community and the public, is provided. The lichen family Parmeliaceae is the first large group of lichenized fungi for which a concerted effort is currently being undertaken to produce substantial content for the EOL. C1 [Luecking, Robert; Lumbsch, H. Thorsten] Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA. [Schulz, Katja] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Crespo, Ana] Univ Complutense Madrid, Fac Farm, Dept Biol Vegetal 2, E-28040 Madrid, Spain. [Nash, Thomas H.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. RP Lucking, R (reprint author), Field Museum Nat Hist, Dept Bot, 1400 S Lake Shore Dr, Chicago, IL 60605 USA. EM rlucking@fieldmuseum.org RI Lumbsch, Thorsten/K-3573-2012; Crespo, Ana/N-6236-2014; OI Lumbsch, Thorsten/0000-0003-1512-835X; Crespo, Ana/0000-0002-5271-0157; Schulz, Katja/0000-0001-7134-3324 NR 31 TC 1 Z9 1 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0024-2829 J9 LICHENOLOGIST JI Lichenologist PD NOV PY 2011 VL 43 BP 503 EP 510 DI 10.1017/S0024282911000168 PN 6 PG 8 WC Plant Sciences; Mycology SC Plant Sciences; Mycology GA 841IL UT WOS:000296505900002 ER PT J AU Kerr, KCR AF Kerr, Kevin C. R. TI Searching for evidence of selection in avian DNA barcodes SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE birds; cytochrome c oxidase; DNA barcode; mitochondrial DNA; purifying selection; selective sweep ID ANIMAL MITOCHONDRIAL-DNA; CYTOCHROME-C-OXIDASE; NONNEUTRAL EVOLUTION; NATURAL-SELECTION; POPULATION-SIZE; BIRDS; POLYMORPHISM; NEUTRALITY; GENE; INTROGRESSION AB The barcode of life project has assembled a tremendous number of mitochondrial cytochrome c oxidase I (COI) sequences. Although these sequences were gathered to develop a DNA-based system for species identification, it has been suggested that further biological inferences may also be derived from this wealth of data. Recurrent selective sweeps have been invoked as an evolutionary mechanism to explain limited intraspecific COI diversity, particularly in birds, but this hypothesis has not been formally tested. In this study, I collated COI sequences from previous barcoding studies on birds and tested them for evidence of selection. Using this expanded data set, I re-examined the relationships between intraspecific diversity and interspecific divergence and sampling effort, respectively. I employed the McDonald-Kreitman test to test for neutrality in sequence evolution between closely related pairs of species. Because amino acid sequences were generally constrained between closely related pairs, I also included broader intra-order comparisons to quantify patterns of protein variation in avian COI sequences. Lastly, using 22 published whole mitochondrial genomes, I compared the evolutionary rate of COI against the other 12 protein-coding mitochondrial genes to assess intragenomic variability. I found no conclusive evidence of selective sweeps. Most evidence pointed to an overall trend of strong purifying selection and functional constraint. The COI protein did vary across the class Aves, but to a very limited extent. COI was the least variable gene in the mitochondrial genome, suggesting that other genes might be more informative for probing factors constraining mitochondrial variation within species. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. RP Kerr, KCR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. EM kerrkc@si.edu RI Kerr, Kevin/B-8510-2013 OI Kerr, Kevin/0000-0002-6784-3884 FU Ontario Graduate Scholarship; University of Guelph; NSERC; Genome Canada FX This work was funded by an Ontario Graduate Scholarship and through the author's thesis advisor at the University of Guelph, Paul Hebert, by grants from NSERC and Genome Canada. I thank Justin Schonfeld for the computational support necessary to produce the secondary structure predictions. I thank Teresa Crease, Steve Lougheed and Paul Hebert for helpful input and discussion. I thank Beren Robinson and Lee-Ann Hayek for providing assistance with statistical methods. I also thank three anonymous reviewers for comments on an earlier version of this manuscript. NR 58 TC 14 Z9 14 U1 0 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-098X J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD NOV PY 2011 VL 11 IS 6 BP 1045 EP 1055 DI 10.1111/j.1755-0998.2011.03049.x PG 11 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 840EN UT WOS:000296421200013 PM 21777399 ER PT J AU Richter, DD Bacon, AR Mobley, ML Richardson, CJ Andrews, SS West, L Wills, S Billings, S Cambardella, CA Cavallaro, N DeMeester, JE Franzluebbers, AJ Grandy, AS Grunwald, S Gruver, J Hartshorn, AS Janzen, H Kramer, MG Ladha, JK Lajtha, K Liles, GC Markewitz, D Megonigal, PJ Mermut, AR Rasmussen, C Robinson, DA Smith, P Stiles, CA Tate, RL Thompson, A Tugel, AJ van Es, H Yaalon, D Zobeck, TM AF Richter, Daniel deB Bacon, Allan R. Mobley, Megan L. Richardson, Curtis J. Andrews, Susan S. West, Larry Wills, Skye Billings, Sharon Cambardella, Cynthia A. Cavallaro, Nancy DeMeester, Julie E. Franzluebbers, Alan J. Grandy, A. Stuart Grunwald, Sabine Gruver, Joel Hartshorn, Anthony S. Janzen, Henry Kramer, Marc G. Ladha, Jagdish K. Lajtha, Kate Liles, Garrett C. Markewitz, Daniel Megonigal, Patrick J. Mermut, Ahmet R. Rasmussen, Craig Robinson, David A. Smith, Pete Stiles, Cynthia A. Tate, Robert L., III Thompson, Aaron Tugel, Arlene J. van Es, Harold Yaalon, Dan Zobeck, Ted M. TI Human-Soil Relations are Changing Rapidly: Proposals from SSSA's Cross-Divisional Soil Change Working Group SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID ECOSYSTEM SERVICES; FRAMEWORK; SCIENCE; AGRICULTURE; MANAGEMENT; TRANSFORMATION; PERSPECTIVE; MITIGATION; DIVERSITY; AMERICA AB A number of scientists have named our age the Anthropocene because humanity is globally affecting Earth systems, including the soil. Global soil change raises important questions about the future of soil, the environment, and human society. Although many soil scientists strive to understand human forcings as integral to soil genesis, there remains an explicit need for a science of anthropedology to detail how humanity is a fully fledged soil-forming factor and to understand how soil change affects human well being. The development and maturation of anthropedology is critical to achieving land-use sustainability and needs to be nurtured by all soil disciplines, with inputs from allied sciences and the humanities,. The Soil Science Society of America (SSSA) has recently approved a cross-divisional Working Group on Soil Change, which aims to advance the basic and applied science of anthropedology, to facilitate networks of scientists, long-term soil field studies, and regional databases and modeling, and to engage in new modes of communications about human-soil relations. We challenge all interested parties, especially young scientists and students, to contribute to these activities and help grow soil science in the Anthropocene. C1 [Richter, Daniel deB; Bacon, Allan R.; Mobley, Megan L.; Richardson, Curtis J.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Andrews, Susan S.; West, Larry; Wills, Skye] USDA NRCS, Natl Soil Survey Ctr, Lincoln, NE 68508 USA. [Billings, Sharon] Univ Kansas, Kansas Biol Survey, Dep Ecol & Evolutionary Biol, Lawrence, KS 66047 USA. [Cambardella, Cynthia A.] USDA ARS, Natl Lab Agr & Environm, Ames, IA 50011 USA. [Cavallaro, Nancy] Natl Inst Food & Agr, USDA, Washington, DC 20024 USA. [Franzluebbers, Alan J.] USDA ARS, J Phil Campbell Sr Nat Resource Conservat Ctr, Watkinsville, GA 30677 USA. [Grandy, A. Stuart] Univ New Hampshire, Dep Nat Resources & Environm, Durham, NH 03824 USA. [Grunwald, Sabine] Univ Florida, Soil & Water Sci Dep, Gainesville, FL 32611 USA. [Gruver, Joel] Western Illinois Univ, Sch Agr, Macomb, IL 61455 USA. [Hartshorn, Anthony S.] James Madison Univ, Dep Geol & Environm Sci, Harrisonburg, VA 22807 USA. [Janzen, Henry] Agr & Agri Food Canada, Lethbridge Res Ctr, Lethbridge, AB T1J 4B1, Canada. [Kramer, Marc G.] USDA Forest Serv, Portland, OR 97204 USA. [Ladha, Jagdish K.] IRRI, New Delhi 110012, India. [Lajtha, Kate] Oregon State Univ, Dep Crop & Soil Sci, Corvallis, OR 97331 USA. [Liles, Garrett C.] Univ Calif Davis, Dep Land Air & Water Resources, Davis, CA 95616 USA. [Markewitz, Daniel] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. [Megonigal, Patrick J.] Smithsonian Inst, Smithsonian Environm Res Ctr, Washington, DC 20013 USA. [Mermut, Ahmet R.] Univ Saskatchewan, Dep Soil Sci, Saskatoon, SK S7N 5A2, Canada. [Rasmussen, Craig] Univ Arizona, Dep Soil Water & Environm Sci, Tucson, AZ 85721 USA. [Robinson, David A.] Environm Ctr Wales, Ctr Ecol & Hydrol, Bangor LL57 2UW, Gwynedd, Wales. [Smith, Pete] Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland. [Stiles, Cynthia A.] USDA NRCS, Pacific Isl Area State Off, Honolulu, HI 96850 USA. [Tate, Robert L., III] Rutgers State Univ, Dep Environm Sci, New Brunswick, NJ 08901 USA. [Thompson, Aaron] Univ Georgia, Dep Crop & Soil Sci, Athens, GA 30602 USA. [Tugel, Arlene J.] USDA NRCS, Las Cruces, NM 88003 USA. [van Es, Harold] Cornell Univ, Dep Crop & Soil Sci, Ithaca, NY 14853 USA. [Yaalon, Dan] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel. [Zobeck, Ted M.] USDA ARS, Cropping Syst Res Lab, Lubbock, TX 79415 USA. RP Richter, DD (reprint author), Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. EM drichter@duke.edu RI Robinson, David/A-6287-2010; Zobeck, Ted/A-6126-2012; Billings, Sharon/I-5115-2013; Smith, Pete/G-1041-2010; OI Robinson, David/0000-0001-7290-4867; Billings, Sharon/0000-0003-1611-526X; Smith, Pete/0000-0002-3784-1124; Hartshorn, Anthony/0000-0002-0004-5749 NR 85 TC 27 Z9 27 U1 4 U2 40 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD NOV PY 2011 VL 75 IS 6 BP 2079 EP 2084 DI 10.2136/sssaj2011.0124 PG 6 WC Soil Science SC Agriculture GA 841ZK UT WOS:000296553600005 ER PT J AU de Rivera, CE Steves, BP Fofonoff, PW Hines, AH Ruiz, GM AF de Rivera, Catherine E. Steves, Brian P. Fofonoff, Paul W. Hines, Anson H. Ruiz, Gregory M. TI Potential for high-latitude marine invasions along western North America SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Abiotic resistance; Amphibalanus improvisus; biological invasions; Carcinus maenas; environmental niche model; Littorina saxatilis; Styela clava ID SPECIES GEOGRAPHIC DISTRIBUTIONS; GLOBAL CLIMATE-CHANGE; CRAB CARCINUS-MAENAS; LITTORINA-SAXATILIS; DISTRIBUTION MODELS; NICHE SHIFT; PROPAGULE PRESSURE; INTRODUCED CRAB; PLANT INVASIONS; RANGE SHIFTS AB Aim High-latitude regions host many fewer non-native species than temperate ones. The low invasion loads of these colder regions may change with increases in human-mediated propagule supply. We test the hypothesis that colonization by non-native species that have already invaded temperate shorelines would be precluded by environmental conditions if they were introduced to Alaska and other high-latitude regions by shipping or other vectors. Location Pacific coast of North America as well as coastal oceans world-wide. Methods Using 16 habitat descriptors in ecological niche models, we characterized the conditions throughout the native and introduced distributions of four marine species (Amphibalanus improvisus, Carcinus maenas, Littorina saxatilis and Styela clava) that have invaded multiple global regions to test the extent to which suitable conditions for these species exist in Alaska and other high-latitude regions under current and predicted future climate scenarios. Results Models projected environmental match for all four species in many areas beyond their present range limits, suggesting that Alaska and other high-latitude shorelines are currently vulnerable to invasion by non-native species that occur in lower latitudes. Main conclusions Given current and possibly increasing human-mediated species transfers and suitable environmental conditions that exist now and with projected warming, policy and management efforts are urgently needed to minimize invasion opportunities at high latitudes. C1 [de Rivera, Catherine E.; Steves, Brian P.; Fofonoff, Paul W.; Hines, Anson H.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [de Rivera, Catherine E.; Steves, Brian P.; Ruiz, Gregory M.] Portland State Univ, Aquat Bioinvas Res & Policy Inst, Portland, OR 97207 USA. RP de Rivera, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM derivera@pdx.edu OI Ruiz, Gregory/0000-0003-2499-441X FU Prince William Sound Regional Citizen's Advisory Council; U.S. Fish and Wildlife Service FX We thank Lisa Ka'aihue, Denny Lassuy, Bob Piorkowski and Linda Shaw for comments. We also benefited from discussions with Chad Hewitt and Whitman Miller. This project was funded by a grant to GMR, AHH and CED from the Prince William Sound Regional Citizen's Advisory Council and by U.S. Fish and Wildlife Service. NR 75 TC 27 Z9 27 U1 3 U2 46 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD NOV PY 2011 VL 17 IS 6 BP 1198 EP 1209 DI 10.1111/j.1472-4642.2011.00790.x PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 836TG UT WOS:000296134800012 ER PT J AU Visser, MD Muller-Landau, HC Wright, SJ Rutten, G Jansen, PA AF Visser, Marco D. Muller-Landau, Helene C. Wright, S. Joseph Rutten, Gemma Jansen, Patrick A. TI Tri-trophic interactions affect density dependence of seed fate in a tropical forest palm SO ECOLOGY LETTERS LA English DT Article DE Attalea butyracea; Barro Colorado Island; enemies hypothesis; negative density dependence; seed predation; specialization; species coexistence; species diversity; trophic cascade; tropical forest ID BARRO-COLORADO ISLAND; JANZEN-CONNELL MODEL; RAIN-FOREST; SPECIES-DIVERSITY; NEOTROPICAL TREE; BRUCHID BEETLES; PLANT DIVERSITY; PARENT PALM; DISPERSAL; PREDATION AB Natural enemies, especially host-specific enemies, are hypothesised to facilitate the coexistence of plant species by disproportionately inflicting more damage at increasing host abundance. However, few studies have assessed such Janzen-Connell mechanisms on a scale relevant for coexistence and no study has evaluated potential top-down influences on the specialized pests. We quantified seed predation by specialist invertebrates and generalist vertebrates, as well as larval predation on these invertebrates, for the Neotropical palm Attalea butyracea across ten 4-ha plots spanning 20-fold variation in palm density. As palm density increased, seed attack by bruchid beetles increased, whereas seed predation by rodents held constant. But because rodent predation on bruchid larvae increased disproportionately with increasing palm density, bruchid emergence rates and total seed predation by rodents and bruchids combined were both density-independent. Our results demonstrate that top-down effects can limit the potential of host-specific insects to induce negative-density dependence in plant populations. C1 [Visser, Marco D.; Muller-Landau, Helene C.; Wright, S. Joseph; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Visser, Marco D.; Jansen, Patrick A.] Univ Wageningen & Res Ctr, Forest Ecol & Forest Management Grp, Wageningen, Netherlands. [Visser, Marco D.] Radboud Univ Nijmegen, Inst Water & Wetland Res, Dept Expt Plant Ecol, NL-6525 AJ Nijmegen, Netherlands. [Rutten, Gemma] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. [Rutten, Gemma; Jansen, Patrick A.] Univ Groningen, Community & Conservat Ecol Grp, NL-9700 CC Groningen, Netherlands. RP Visser, MD (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama. EM m.visser@science.ru.nl RI Wright, Stuart/M-3311-2013; Jansen, Patrick/G-2545-2015 OI Wright, Stuart/0000-0003-4260-5676; Jansen, Patrick/0000-0002-4660-0314 FU Smithsonian Tropical Research Institute; HSBC; David and Lucile Packard Foundation; Netherlands Organization for Scientific Research FX We thank Eric Oriel Vasquez, Christoph Gahr and Femke Maes for their help in the field and laboratory, Carol Garzon-Lopez and Stephanie Bohlman for providing the BCI crown maps, and Robert Holt, Rob Klinger and two anonymous reviewers for helpful comments. We gratefully acknowledge the financial support of the Smithsonian Tropical Research Institute (MDV), the HSBC Climate Partnership (HCM), the David and Lucile Packard Foundation (HCM) and the Netherlands Organization for Scientific Research (PAJ). NR 49 TC 19 Z9 19 U1 2 U2 40 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD NOV PY 2011 VL 14 IS 11 BP 1093 EP 1100 DI 10.1111/j.1461-0248.2011.01677.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 838CB UT WOS:000296263200003 PM 21899693 ER PT J AU Hosaka, T Yumoto, T Chen, YY Sun, IF Wright, SJ Noor, NSM AF Hosaka, Tetsuro Yumoto, Takakazu Chen, Yu-Yun Sun, I-Fang Wright, S. Joseph Noor, Nur Supardi Md TI Abundance of insect seed predators and intensity of seed predation on Shorea (Dipterocarpaceae) in two consecutive masting events in Peninsular Malaysia SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Alcidodes; Andrioplecta; Dipterocarpaceae; general flowering; Nanophyidae; population dynamics; predator satiation; pre-dispersal seed predator; Shorea ID RAIN-FOREST; BEETLES; PATTERNS; SARAWAK; BORNEO C1 [Hosaka, Tetsuro] Kyoto Univ, Grad Sch Agr, Kyoto 6068502, Japan. [Yumoto, Takakazu] Res Inst Humanity & Nat, Kyoto 6038047, Japan. [Chen, Yu-Yun] Natl Tsing Hua Univ, Hsinchu 300, Taiwan. [Sun, I-Fang] Tunghai Univ, Ctr Trop Ecol & Biodivers, Taichung 40704, Taiwan. [Wright, S. Joseph] Smithsonian Trop Res Inst, Ancon, Panama. [Noor, Nur Supardi Md] Forest Res Inst Malaysia, Kepong 52109, Selangor, Malaysia. RP Hosaka, T (reprint author), Hiroshima Univ, Grad Sch Integrated Arts & Sci, Kagamiyama 1-7-1, Higashihiroshima 7398521, Japan. EM hosaka@hiroshima-u.ac.jp RI Yumoto, Takakazu/B-6215-2013; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU FRIM; National Institute for Environmental Studies, Japan [E-4]; Ministry of Education, Culture, Sports, Science and Technology of Japan; US NSF [DEB-0108388] FX We are grateful to Dr Laurence G. Kirton of the Forest Research Institute of Malaysia (FRIM) for permission to conduct the research in Pasoh. Special thanks are due to Dr Mamoru Kanzaki, Dr Naoya Osawa (Kyoto University) and Dr Toshinori Okuda (Hiroshima University) for their kind support. Dr Hiroaki Kojima and Mr Junnosuke Kanto (Tokyo University of Agriculture) identified weevils and Dr Furumi Komai (Osaka University of Arts) identified moths. This study was partly supported by a joint research project of FRIM and the National Institute for Environmental Studies, Japan: Grant No. E-4, Global Environmental Research Program, Ministry of Education, Culture, Sports, Science and Technology of Japan. Flower and seed rain data collection was supported by the US NSF grant DEB-0108388 awarded to S. P. Hubbell and S. J. Wright. NR 23 TC 4 Z9 4 U1 2 U2 29 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD NOV PY 2011 VL 27 BP 651 EP 655 DI 10.1017/S0266467411000393 PN 6 PG 5 WC Ecology SC Environmental Sciences & Ecology GA 837MS UT WOS:000296208500011 ER PT J AU Fleischer, RC AF Fleischer, Robert C. TI Ladies and gentes: Maternally inherited DNA and ancient honeyguide host races SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material ID MOLOTHRUS-BONARIENSIS; CUCKOO C1 Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. RP Fleischer, RC (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20013 USA. EM fleischerr@si.edu NR 13 TC 1 Z9 1 U1 1 U2 24 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD NOV 1 PY 2011 VL 108 IS 44 BP 17859 EP 17860 DI 10.1073/pnas.1115041108 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 839NH UT WOS:000296373400007 PM 22006330 ER PT J AU Clough, GW AF Clough, G. Wayne TI Simple Pleasures SO SMITHSONIAN LA English DT Article C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD NOV PY 2011 VL 42 IS 7 BP 28 EP + PG 3 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 837FS UT WOS:000296177100013 ER PT J AU Osborn, KJ Haddock, SHD Rouse, GW AF Osborn, Karen J. Haddock, Steven H. D. Rouse, Greg W. TI Swima (Annelida, Acrocirridae), holopelagic worms from the deep Pacific SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Celebes Sea; Cirratuliformia; deep-sea; gelata; midwater; pelagic; Swima bombiviridis; Swima fulgida sp nov.; Swima tawitawiensis sp nov. ID FLABELLIGERIDAE ANNELIDA; POLYCHAETA; SUBSTITUTION; SEDENTARIA; MODEL AB Two new species of Swima, a recently established genus of annelid worms, are introduced, one from deep water off the North American West Coast and the other from the Philippines. The acrocirrid genus now contains three named species, Swima bombiviridis, Swima fulgida sp. nov., and Swima tawitawiensis sp. nov. Swima are holopelagic, occurring only in the water column, and thus far have only been observed below 2700 m. The worms are relatively large, sometimes reaching over 30 mm in length and 5 mm in width. They have gelatinous bodies and fans of long swimming chaetae, which are flattened into paddles in S. tawitawiensis sp. nov. Members of Swima are distinguished from other swimming acrocirrids by their transparent bodies, single medial subulate branchiae, and simple nuchal organs that do not skirt the bases of lateral subulate branchiae. Swima fulgida sp. nov. is distinguished from other members of the genus by its darkly pigmented anterior gut, whereas S. tawitawiensis sp. nov. is distinguished by possessing three subulate head appendages instead of just one and by the shape of its noto- and neurochaetae. Swima species possess four pairs of elliptical, transformed segmental branchiae that produce green bioluminescence when autotomized. These 'bombs' were observed in various states of regeneration on a single individual. Swima are neutrally buoyant, often observed hanging immobile in the water column, and are active, agile swimmers. Although not previously documented in the literature, these worms are not rare in the deep water column. Since the worms were first noticed in 2001, they have been observed on more than half of the Monterey Bay Aquarium Research Institute's midwater remotely operated vehicle dives that went to sufficient depth. The discovery of Swima underscores our lack of knowledge of deep pelagic fauna. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 163, 663-678. doi: 10.1111/j.1096-3642.2011.00727.x C1 [Osborn, Karen J.; Rouse, Greg W.] Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Haddock, Steven H. D.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. RP Osborn, KJ (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20052 USA. EM osbornk@si.edu RI Rouse, Greg/F-2611-2010; OI Rouse, Greg/0000-0001-9036-9263; Osborn, Karen/0000-0002-4226-9257 FU Scripps Institution of Oceanography; University of California; David and Lucile Packard Foundation; National Geographic Society; National Oceanic and Atmospheric Administration; Woods Hole Oceanographic Institution FX We would like to thank Bruce Robison of the Monterey Bay Aquarium Research Institute for ship time made available for observation and collection of several specimens. Thanks go to Larry Madin of Woods Hole Oceanographic Institution, the science party, and crew aboard the R/V Hydrographer Presbitero for their work in the Celebes Sea, for the foresight to collect, photograph, and preserve for morphology and molecular work the single specimen of S. tawitawiensis considered here. Thanks go to the crew of the R/V Western Flyer, the pilots of the ROVs Tiburon and Doc Ricketts, and the MBARI video lab staff for their dedication to deep-sea exploration. We also thank Cynthia Claxton (UC Irvine) for advice regarding Latin usage and form, although any errors are the sole responsibility of the authors. Evelyn York's expertise on the SEM was much appreciated. Scripps Institution of Oceanography funded K. J. O. and G. W. R. and the University of California President's Postdoctoral Fellowship supported K. J. O. The David and Lucile Packard Foundation provided funding to the Monterey Bay Aquarium Research Institute. The National Geographic Society, National Oceanic and Atmospheric Administration, and Woods Hole Oceanographic Institution provided funding for the Celebes Sea Expedition. NR 34 TC 5 Z9 5 U1 1 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD NOV PY 2011 VL 163 IS 3 BP 663 EP 678 DI 10.1111/j.1096-3642.2011.00727.x PG 16 WC Zoology SC Zoology GA 838BK UT WOS:000296261300001 ER PT J AU Liu, Q Triplett, JK Wen, J Peterson, PM AF Liu, Qing Triplett, Jimmy K. Wen, Jun Peterson, Paul M. TI Allotetraploid origin and divergence in Eleusine (Chloridoideae, Poaceae): evidence from low-copy nuclear gene phylogenies and a plastid gene chronogram SO ANNALS OF BOTANY LA English DT Article DE Allotetraploid origin; chloroplast markers; East Africa; Eleusine; low-copy nuclear markers; phylogeny; Poaceae ID IN-SITU HYBRIDIZATION; FINGER MILLET; TRITICEAE GRAMINEAE; C-4 PHOTOSYNTHESIS; GENOME; DNA; EVOLUTIONARY; SEQUENCE; WILD; GRASSLANDS AB Background and Aims Eleusine (Poaceae) is a small genus of the subfamily Chloridoideae exhibiting considerable morphological and ecological diversity in East Africa and the Americas. The interspecific phylogenetic relationships of Eleusine are investigated in order to identify its allotetraploid origin, and a chronogram is estimated to infer temporal relationships between palaeoenvironment changes and divergence of Eleusine in East Africa. Methods Two low-copy nuclear (LCN) markers, Pepc4 and EF-1 alpha, were analysed using parsimony, likelihood and Bayesian approaches. A chronogram of Eleusine was inferred from a combined data set of six plastid DNA markers (ndhA intron, ndhF, rps16-trnK, rps16 intron, rps3, and rpl32-trnL) using the Bayesian dating method. Key Results The monophyly of Eleusine is strongly supported by sequence data from two LCN markers. In the cpDNA phylogeny, three tetraploid species (E. africana, E. coracana and E. kigeziensis) share a common ancestor with the E. indica-E. tristachya clade, which is considered a source of maternal parents for allotetraploids. Two homoeologous loci are isolated from three tetraploid species in the Pepc4 phylogeny, and the maternal parents receive further support. The A-type EF-1 alpha sequences possess three characters, i.e. a large number of variations of intron 2; clade E-A distantly diverged from clade E-B and other diploid species; and seven deletions in intron 2, implying a possible derivation through a gene duplication event. The crown age of Eleusine and the allotetraploid lineage are 3.89 million years ago (mya) and 1.40 mya, respectively. Conclusions The molecular data support independent allotetraploid origins for E. kigeziensis and the E. africana-E. coracana clade. Both events may have involved diploids E. indica and E. tristachya as the maternal parents, but the paternal parents remain unidentified. The habitat-specific hypothesis is proposed to explain the divergence of Eleusine and its allotetraploid lineage. C1 [Liu, Qing] Chinese Acad Sci, Key Lab Plant Resources Conservat & Sustainable U, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. [Triplett, Jimmy K.] Jacksonville State Univ, Dept Biol, Jacksonville, AL 36265 USA. [Wen, Jun; Peterson, Paul M.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Liu, Q (reprint author), Chinese Acad Sci, Key Lab Plant Resources Conservat & Sustainable U, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. EM liuqing@scib.ac.cn; peterson@si.edu FU National Geographic Society Committee for Research and Exploration [8087-06]; Smithsonian Institution, National Natural Science Foundation of China [30700043]; China Scholarship Council [2008491004]; Key Laboratory of Plant Resources Conservation and Sustainable Utilization of Chinese Academy of Sciences [200922]; Chinese Academy of Sciences [KSCX2-EW-J-28] FX We thank USDA-Beltsville National Germplasm System, ILRI-Addis Ababa and J. Travis Columbus for help with caryopsis and leaf collection; Lee Weigt, Jeffery Hunt, Rong Li and Xinwei Xu for help in the laboratory; Robert J. Soreng, Dianxiang Zhang, Gabriel Johnson and Tieyao Tu for helpful discussions; and six anonymous reviewers for their constructive comments that improved the manuscript. This work was supported by the National Geographic Society Committee for Research and Exploration (grant no. 8087-06), the Smithsonian Institution's Small Grants Program, National Natural Science Foundation of China (no. 30700043), the China Scholarship Council Awards (no. 2008491004), the Key Laboratory of Plant Resources Conservation and Sustainable Utilization of Chinese Academy of Sciences (no. 200922) and the Knowledge Innovation Program of the Chinese Academy of Sciences (no. KSCX2-EW-J-28). NR 77 TC 12 Z9 13 U1 3 U2 26 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD NOV PY 2011 VL 108 IS 7 BP 1287 EP 1298 DI 10.1093/aob/mcr231 PG 12 WC Plant Sciences SC Plant Sciences GA 836GN UT WOS:000296098900007 PM 21880659 ER PT J AU O'Meara, C Baez, GP AF O'Meara, Carolyn Perez Baez, Gabriela TI Spatial frames of reference in Mesoamerican languages SO LANGUAGE SCIENCES LA English DT Article DE Mesoamerican languages; Frames of reference; Spatial semantics; Semantic typology; Spatial reference; Language and cognition ID LINGUISTIC RELATIVITY; SPACE ORIENTATION; SEMANTIC TYPOLOGY; BODY; COGNITION; TABLES; PARTS; SHAPE AB This article presents the conceptual and methodological framework for the special issue Frames of reference in Mesoamerican languages, which reports on the use of frames of reference (FoRs) in eight Mesoamerican languages and two non-Mesoamerican control languages. The papers included here are a result of the ongoing collaborative project Spatial language and cognition in Mesoamerica. This article provides a background to the study of FoRs, the research methodology used cross-linguistically, the classification that serves as the basis for the coding of cross-linguistic data, and a preview of the articles in the special issue. Published by Elsevier Ltd. C1 [Perez Baez, Gabriela] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. [O'Meara, Carolyn] Univ Nacl Autonoma Mexico, Inst Invest Filol, Seminario Lenguas Indigenas, Mexico City 04510, DF, Mexico. RP Baez, GP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012, Washington, DC 20013 USA. EM perezbaezg@si.edu NR 70 TC 17 Z9 17 U1 0 U2 8 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0388-0001 J9 LANG SCI JI Lang. Sci. PD NOV PY 2011 VL 33 IS 6 SI SI BP 837 EP 852 DI 10.1016/j.langsci.2011.06.013 PG 16 WC Linguistics; Language & Linguistics SC Linguistics GA 836LK UT WOS:000296113000001 ER PT J AU Baez, GP AF Perez Baez, Gabriela TI Spatial frames of reference preferences in Juchitan Zapotec SO LANGUAGE SCIENCES LA English DT Article DE Zapotec languages; Mesoamerican languages; Spatial frames of reference; Semantic typology; Linguistic relativity ID COGNITION; TYPOLOGY; LANGUAGE; SHAPE AB This article reports on spatial frames of reference (FoRs) preferences in Juchiteco (Zapotec, Otomanguean). The data show that speakers exhibit a strong preference for the absolute and object-centered FoRs, both observer-independent, and overall disfavor most other FoR types. Of particular interest is the limited use of the relative (observer-dependent) FoR. This is relevant in a language such as Juchiteco, which has a productive meronymic (part-naming) system, as it supports the hypothesis put forth by the Spatial Language and Cognition in Mesoamerica project that productive meronymy correlates with a bias against the use of the relative FoR. Published by Elsevier Ltd. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Baez, GP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012, Washington, DC 20013 USA. EM perezbaezg@si.edu NR 47 TC 2 Z9 2 U1 0 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0388-0001 J9 LANG SCI JI Lang. Sci. PD NOV PY 2011 VL 33 IS 6 SI SI BP 943 EP 960 DI 10.1016/j.langsci.2011.06.012 PG 18 WC Linguistics; Language & Linguistics SC Linguistics GA 836LK UT WOS:000296113000006 ER PT J AU Montaser, R Paul, VJ Luesch, H AF Montaser, Rana Paul, Valerie J. Luesch, Hendrik TI Pitipeptolides C-F, antimycobacterial cyclodepsipeptides from the marine cyanobacterium Lyngbya majuscula from Guam SO PHYTOCHEMISTRY LA English DT Article DE Marine cyanobacteria; Lyngbya majuscula; Pitipeptolides; Cytotoxin; Antimycobacterial activity ID NATURAL-PRODUCTS AB Pitipeptolides A (1) and B (2) are cyclic depsipeptides isolated from the marine cyanobacterium Lyngbya majuscula from Piti Bomb Holes, Guam. Additional analogues have now been isolated by revisiting larger collections of the same cyanobacterium. The four identified analogues, pitipeptolides C-F (3-6), are the tetrahydro analogue (3), an analogue with a lower degree of methylation (4) as well as two homologues (5 and 6) of pitipeptolide A. Their structures were elucidated using 20 NMR experiments, chiral HPLC analysis and comparison with pitipeptolide A. The identified analogues showed weaker cytotoxic activities compared to the two major parent compounds, pitipeptolides A (1) and B (2), against HT-29 colon adenocarcinoma and MCF7 breast cancer cells. On the other hand, pitipeptolide F (6) was the most potent pitipeptolide in a disc diffusion assay against Mycobacterium tuberculosis. The latter finding suggests that the structure of pitipeptolides could be optimized for selective antibacterial activity. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Montaser, Rana; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU National Institutes of Health, NIGMS [P41GM086210] FX This research was supported by the National Institutes of Health, NIGMS Grant P41GM086210. We thank J. R. Rocca for technical assistance with NMR data acquisition. This is contribution 852 from the Smithsonian Marine Station. NR 16 TC 15 Z9 15 U1 3 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0031-9422 J9 PHYTOCHEMISTRY JI Phytochemistry PD NOV PY 2011 VL 72 IS 16 BP 2068 EP 2074 DI 10.1016/j.phytochem.2011.07.014 PG 7 WC Biochemistry & Molecular Biology; Plant Sciences SC Biochemistry & Molecular Biology; Plant Sciences GA 834HJ UT WOS:000295950100017 PM 21843895 ER PT J AU Zotz, G Schmidt, G Mikona, C AF Zotz, G. Schmidt, G. Mikona, C. TI What is the proximate cause for size-dependent ecophysiological differences in vascular epiphytes? SO PLANT BIOLOGY LA English DT Article DE Bromeliaceae; nutrient limitation; ontogenetic drift; Orchidaceae; photosynthesis; rain forest; size dependency; specific leaf area ID PLANT SIZE; WATER RELATIONS; TREE HEIGHT; CARBON GAIN; GROWTH; PHOTOSYNTHESIS; BROMELIADS; CONSEQUENCES; NITROGEN; ORCHID AB Size-related variation in physiological parameters as diverse as photosynthetic capacity, abscisic acid relationships or the relative water deficit at stomatal closure have been reported for a large number of vascular epiphytes, but the proximate mechanism behind these observations has not been identified. We test four possible reasons for size-related changes in photosynthetic capacity, leaf-N content and specific leaf area: (i) plant size itself, (ii) plant age or developmental stage, (iii) previous nutrition, or (iv) previous water regime. A suite of study species and approaches were used: a 'natural experiment' with the orchid Polystachya foliosa; an experimental field study with another orchid, Dimerandra emarginata; and a study under controlled conditions with the tank bromeliad, Vriesea sanguinolenta. Neither size, age nor differences in water supply caused differences in leaf N and photosynthetic capacity, while low supply of nutrients yielded, and high supply with nutrients completely removed, size-related trends. The observed size-related trends are thus a consequence of in situ differences in nutrient acquisition. Arguably, the improved nutrient status of larger plants under natural conditions results from larger tanks, holding moisture for increasingly longer intervals, which allows longer periods of decomposition of detritus and of nutrient uptake. C1 [Zotz, G.] Carl von Ossietzky Univ Oldenburg, Inst Biol Umweltwissensch, AG Funkt Okol, D-26111 Oldenburg, Germany. [Zotz, G.] Smithsonian Trop Res Inst, Balboa, Panama. [Schmidt, G.; Mikona, C.] Univ Wurzburg, Lehrstuhl Bot 2, D-8700 Wurzburg, Germany. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Inst Biol Umweltwissensch, AG Funkt Okol, Postfach 2503, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de FU Deutsche Forschungsgemeinschaft [Sonderforschungsbereich 251] FX This research was supported by a grant from the Deutsche Forschungsgemeinschaft (Sonderforschungsbereich 251). Cord Mikona received generous support from the Wilhelm-v. Gwinner Foundation, Munich, Germany. Thanks also to Edgardo Garrido and Vera Thomas for assistance in the field and to Frida Reisberg, Wurzburg, for CHN analysis. Sabine Armsen, Wurzburg, supplied data from her unpublished Master's thesis. Comments by three anonymous reviewers and Diane Byers, Normal, USA, on earlier versions helped to improve the manuscript. Finally, we thank the Republic of Panama for making its natural resources available for study. NR 39 TC 3 Z9 3 U1 1 U2 21 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1435-8603 J9 PLANT BIOLOGY JI Plant Biol. PD NOV PY 2011 VL 13 IS 6 BP 902 EP 908 DI 10.1111/j.1438-8677.2011.00460.x PG 7 WC Plant Sciences SC Plant Sciences GA 835JD UT WOS:000296031800011 PM 21973121 ER PT J AU Kleiman, DG AF Kleiman, Devra G. TI Canid Mating Systems, Social Behavior, Parental Care and Ontogeny: Are they Flexible? SO BEHAVIOR GENETICS LA English DT Article DE Monogamy; Behavioral plasticity; Canids; Sociality; Reproductive behavior ID DOG SPEOTHOS-VENATICUS; CRAB-EATING FOX; WOLF CHRYSOCYON-BRACHYURUS; BUSH DOG; MANED WOLF AB Benson Ginsburg's early studies of canid socialization and wolf social and reproductive behavior were focused, in part, on the degree to which there was flexibility in social development and specifically whether there was a critical period during development after which wolf pups could not be socialized to humans. My focus was the degree to which differences in canid ecology and social structure were correlated with differences in the plasticity of social and reproductive behavior, including development. Canid species are unusual among the Mammalia in being primarily monogamous. Males may play an indirect or direct role in parental care, depending on a species degree of sociality. Canid species also differ in developmental parameters, and reproductive suppression is common in the group-living pack hunters. I review comparative studies of the social and reproductive behavior of three South American canids which vary in their degree of sociality and explore the degree to which the species are ecologically and socially flexible. C1 Smithsonian Natl Zool Pk, Div Conservat & Sci, Washington, DC 20008 USA. RP Kleiman, DG (reprint author), Smithsonian Natl Zool Pk, Div Conservat & Sci, Washington, DC 20008 USA. FU Smithsonian Research Foundation; NIMH [27241-03] FX I would like to thank Benson Ginsburg for giving me a start in canid research and supporting my interests so completely. Without the opportunities he provided, my career would have gone in a very different direction. I also wish to thank George and Mary Rabb for introducing me to the complexities of life within a wolf pack. I would also like to thank those colleagues that contributed so much to the canid studies, especially: Maxeen Biben, Chuck Brady, James Dietz, John Eisenberg, Ingrid Porton, and Melissa Rodden. These studies were supported by grants from the Smithsonian Research Foundation and NIMH 27241-03. NR 34 TC 9 Z9 9 U1 8 U2 126 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0001-8244 EI 1573-3297 J9 BEHAV GENET JI Behav. Genet. PD NOV PY 2011 VL 41 IS 6 SI SI BP 803 EP 809 DI 10.1007/s10519-011-9459-0 PG 7 WC Behavioral Sciences; Genetics & Heredity; Psychology, Multidisciplinary SC Behavioral Sciences; Genetics & Heredity; Psychology GA 826BO UT WOS:000295326600004 PM 21487689 ER PT J AU Purdy, BA Jones, KS Mecholsky, JJ Bourne, G Hulbert, RC MacFadden, BJ Church, KL Warren, MW Jorstad, TF Stanford, DJ Wachowiak, MJ Speakman, RJ AF Purdy, Barbara A. Jones, Kevin S. Mecholsky, John J. Bourne, Gerald Hulbert, Richard C., Jr. MacFadden, Bruce J. Church, Krista L. Warren, Michael W. Jorstad, Thomas F. Stanford, Dennis J. Wachowiak, Melvin J. Speakman, Robert J. TI Earliest art in the Americas: incised image of a proboscidean on a mineralized extinct animal bone from Vero Beach, Florida SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Old Vero site; Incised art; Terminal Pleistocene; Mammoth; Mastodon ID NORTH-AMERICA; BUTCHERY AB A fragmented fossil bone incised with the figure of a proboscidean was recently found at Vero Beach, Florida near the location where Late Pleistocene fauna and human bones were recovered from 1913 to 1916. This engraving may represent the oldest and only existing example of Terminal Pleistocene art depicting a proboscidean in the Americas. Because of the uniqueness, rarity, and potential antiquity of this specimen, caution demanded that a variety of tests be used in an attempt to verify its authenticity. The mineralized bone was identified as mammoth, mastodon, or giant sloth. Rare earth element analysis was consistent with the fossil bone being ancient and originating at or near the Old Vero site (8-IR-9). Forensic analysis suggests the markings on the bone are not recent. Optical microscopy results show no discontinuity in coloration between the carved grooves and the surrounding material indicating that both surfaces aged simultaneously. Scanning electron microscopy (SEM) revealed that the edges of the inscription are worn and show no signs of being incised recently or that the grooves were made with metal tools. In addition, the backscattered SEM images suggest there is no discontinuity in the distribution of light and heavy elements between the scribed region and the surrounding bone indicating that both surfaces aged in the same environment. This is very different from an intentional mark made on the bone for comparison. Energy dispersive x-ray spectroscopy (EDXS) shows that the surface contains significant amounts of calcium, phosphorus, oxygen, and carbon typical of a mineralized bone surface. Examination of a cast and mold of the incised bone by Reflectance Transformation Imaging (RTI) also provided no evidence that the engraving was made recently. All of these results are consistent with the mammoth engraving being authentic. Published by Elsevier Ltd. C1 [Wachowiak, Melvin J.; Speakman, Robert J.] Museum Support Ctr, Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Purdy, Barbara A.; Warren, Michael W.] Univ Florida, Dept Anthropol, Gainesville, FL 32611 USA. [Jones, Kevin S.; Mecholsky, John J.; Bourne, Gerald] Univ Florida, Dept Mat Sci & Engn, Gainesville, FL 32611 USA. [Hulbert, Richard C., Jr.; MacFadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Church, Krista L.] Univ Texas Austin, Dept Anthropol, Austin, TX 78712 USA. [Jorstad, Thomas F.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Stanford, Dennis J.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Speakman, RJ (reprint author), Museum Support Ctr, Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM speakmanj@si.edu RI Bourne, Gerald/B-7219-2008; OI Bourne, Gerald/0000-0001-6977-2138; Hulbert, Richard/0000-0002-2242-4256; Speakman, Robert/0000-0003-2063-154X NR 33 TC 14 Z9 14 U1 2 U2 7 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD NOV PY 2011 VL 38 IS 11 BP 2908 EP 2913 DI 10.1016/j.jas.2011.05.022 PG 6 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 829CI UT WOS:000295552600005 ER PT J AU McRae, SB AF McRae, Susan B. TI Conspecific brood parasitism in the tropics: an experimental investigation of host responses in common moorhens and American purple gallinules SO ECOLOGY AND EVOLUTION LA English DT Article DE Breeding synchrony; egg rejection; Gallinula chloropus; intraspecific brood parasitism; Porphyrula martinica; Rallidae; seasonality; neotropics; wetlands ID INTRASPECIFIC NEST PARASITISM; COOTS FULICA-AMERICANA; EGG DISCRIMINATION; SEXUAL SELECTION; REED WARBLERS; WOOD DUCKS; OWN EGGS; BIRDS; RECOGNITION; EVOLUTION AB Species occupying a broad latitudinal range may show greater phenotypic plasticity in behavior than species with smaller ranges or more specific habitat requirements. This study investigates for the first time the occurrence of conspecific brood parasitism (CBP) in sympatric tropical populations of the common moorhen (Gallinula chloropus pauxilla Bangs) and the American purple gallinule (Porphyrula martinica L.). CBP occurred in at least 20% (N = 76) of common moorhen nests on the Rio Chagres in Panama. Half (N = 20) of the parasitic eggs were accepted, but 10 were destroyed or ejected from host nests. Introductions of experimental eggs into nests revealed hosts were more likely to accept parasitism later in the host's laying period and during incubation, consistent with expectation of an adaptive response. CBP was not detected in a small sympatric population of American purple gallinules. Members of this population did not eject experimental eggs, suggesting a lack of experience with costly CBP. Contrasting ecological factors help explain why these two species of rail (Family Rallidae) differ in regard to CBP. Purple gallinule territories were sparse, owing to the distribution of preferred habitat. Moorhens flocked outside of the breeding season. They nested more synchronously, at higher densities, and primarily in ephemeral floating vegetation. Further, moorhens suffered a rate of nest loss nearly double that of American purple gallinules, and this increased over the course of the breeding season. Moorhen clutches were larger on average, and more variable in size than those of purple gallinules. Reproductive effort and rate (seasonality) constitute important life history differences between these species that may constrain the evolution of reproductive tactics. Comparing these sympatric populations, and others differing in life-history traits and ecological constraints, highlights the role of risk management in the evolution of CBP. C1 [McRae, Susan B.] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. [McRae, Susan B.] Smithsonian Trop Res Inst, Panama City, Panama. RP McRae, SB (reprint author), E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. EM mcraes@ecu.edu FU Smithsonian Postdoctoral Research Fellowship FX Funded by Smithsonian Postdoctoral Research Fellowship. NR 51 TC 5 Z9 6 U1 2 U2 24 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD NOV PY 2011 VL 1 IS 3 BP 317 EP 329 DI 10.1002/ece3.26 PG 13 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 055TQ UT WOS:000312441000005 PM 22393503 ER PT J AU Megill, ND Pavicic, M AF Megill, Norman D. Pavicic, Mladen TI Kochen-Specker Sets and Generalized Orthoarguesian Equations SO ANNALES HENRI POINCARE LA English DT Article ID LATTICES AB We prove that the 7oa class (equational variety) of generalized orthoarguesian lattices is properly included in all noa classes for n < 7. This result strengthens the conjecture that any generalized orthoarguesian equation is strictly stronger than those of lower orders. The result emerged from our recent analysis of whether three-dimensional Kochen-Specker sets can be represented by Greechie lattices, which are a kind of orthomodular lattice. C1 [Megill, Norman D.] Boston Informat Grp, Lexington, MA 02420 USA. [Pavicic, Mladen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pavicic, Mladen] Harvard Univ, Inst Theoret Atom Mol & Optic Phys, Dept Phys, Cambridge, MA 02138 USA. [Pavicic, Mladen] Univ Zagreb, Fac Civil Engn, Phys Chair, Zagreb 41000, Croatia. RP Megill, ND (reprint author), Boston Informat Grp, 19 Locke Ln, Lexington, MA 02420 USA. EM nm@alum.mit.edu; pavicic@grad.hr FU US National Science Foundation through Institute for Theoretical Atomic, Molecular, and Optical Physics (ITAMP) at Harvard University; Smithsonian Astrophysical Observatory; Ministry of Science, Education, and Sport of Croatia [082-0982562-3160] FX One of us (M. P.) would like to thank his host Hossein Sadeghpour for support during his stay at ITAMP. His stay was supported by the US National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics (ITAMP) at Harvard University and Smithsonian Astrophysical Observatory and the Ministry of Science, Education, and Sport of Croatia through the project No. 082-0982562-3160. His part of computation was supported the University Computing Centre (at cluster Isabella) of the University of Zagreb and by the Croatian National Grid Infrastructure. NR 20 TC 1 Z9 1 U1 1 U2 3 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 1424-0637 EI 1424-0661 J9 ANN HENRI POINCARE JI Ann. Henri Poincare PD NOV PY 2011 VL 12 IS 7 BP 1417 EP 1429 DI 10.1007/s00023-011-0109-0 PG 13 WC Physics, Multidisciplinary; Physics, Particles & Fields; Physics, Mathematical SC Physics GA 828RE UT WOS:000295519300005 ER PT J AU van Donkelaar, A Martin, RV Levy, RC da Silva, AM Krzyzanowski, M Chubarova, NE Semutnikova, E Cohen, AJ AF van Donkelaar, Aaron Martin, Randall V. Levy, Robert C. da Silva, Arlindo M. Krzyzanowski, Michal Chubarova, Natalia E. Semutnikova, Eugenia Cohen, Aaron J. TI Satellite-based estimates of ground-level fine particulate matter during extreme events: A case study of the Moscow fires in 2010 SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE MODIS; PM(2.5); Moscow wildfires; Aerosol optical depth ID AEROSOL OPTICAL-THICKNESS; UNITED-STATES; CHEMISTRY; MORTALITY; TRANSPORT; POLLUTION; HEALTH; DEPTH; CHINA; LAND AB We estimate fine particulate matter (PM(2.5)) concentrations daily using MODIS satellite observations of aerosol optical depth (AOD) for a major biomass burning event around Moscow during summer 2010. Evaluation of MODIS AOD with the Moscow AERONET site supports a MODIS-AOD error estimate of +/-(0.05 + 0.2 x AOD) for this event. However, since the smoke was often thick (AOD > 4.0) and spatially variable, the standard MODIS algorithm incorrectly identifies some aerosol as cloud. We test relaxed cloud screening criteria that increase MODIS coverage by 21% and find excellent agreement with coincident operational retrievals (r(2) = 0.994, slope = 1.01) with no evidence of false aerosol detection. We relate the resultant MODIS AOD to PM(2.5) using aerosol vertical profiles from the GEOS-Chem chemical transport model. Our estimates are in good agreement with PM(2.5) values estimated from in-situ PM(10) (r(2) = 0.85, slope = 1.06), and we find that the relationship between AOD and PM2.5 is insensitive to uncertainties in biomass burning emissions. The satellite-derived and in-situ values both indicate that peak daily mean concentrations of approximately 600 mu g m(-3) occurred on August 7, 2010 in the Moscow region of the Russian Federation. We estimate that exposure to air pollution from the Moscow wildfires may have caused hundreds of excess deaths. (C) 2011 Elsevier Ltd. All rights reserved. C1 [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Krzyzanowski, Michal] WHO, European Ctr Environm & Hlth, Reg Off Europe, Bonn, Germany. [Chubarova, Natalia E.] Moscow MV Lomonosov State Univ, Dept Geog, Moscow, Russia. [Semutnikova, Eugenia] Mosecomonitoring, State Environm Org, Moscow, Russia. [Cohen, Aaron J.] Hlth Effects Inst, Boston, MA USA. RP van Donkelaar, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, 6300 Coburg Rd, Halifax, NS B3H 3J5, Canada. EM aaron.van.Donkelaar@dal.ca; randall.martin@dal.ca; robert.c.levy@nasa.gov; arlindo.m.dasilva@nasa.gov; mkr@ecehbonn.euro.who.int; chubarova@imp.kiae.ru; info@mosecom.ru; acohen@healtheffects.org RI da Silva, Arlindo/D-6301-2012; Levy, Robert/M-7764-2013; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI da Silva, Arlindo/0000-0002-3381-4030; Levy, Robert/0000-0002-8933-5303; Martin, Randall/0000-0003-2632-8402; FU Natural Science and Engineering Research Council of Canada (NSERC); Killam Trust FX This work was supported by the Natural Science and Engineering Research Council of Canada (NSERC) and the Killam Trust. NR 48 TC 48 Z9 50 U1 1 U2 32 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD NOV PY 2011 VL 45 IS 34 BP 6225 EP 6232 DI 10.1016/j.atmosenv.2011.07.068 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 831UU UT WOS:000295757400016 ER PT J AU Whattam, SA Stern, RJ AF Whattam, Scott A. Stern, Robert J. TI The 'subduction initiation rule': a key for linking ophiolites, intra-oceanic forearcs, and subduction initiation SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY LA English DT Article DE Ophiolites; Forearcs; Intra-oceanic arcs; Subduction initiation; Tethys; Izu-Bonin-Marianas arc ID VOLCANIC-ROCKS; TETHYAN OPHIOLITES; TRENCH ROLLBACK; OMAN OPHIOLITE; OCEANIC-CRUST; ACCRETION; EVOLUTION; ZONE; ALBANIA; GEOCHEMISTRY AB We establish the 'subduction initiation rule' (SIR) which predicts that most ophiolites form during subduction initiation (SI) and that the diagnostic magmatic chemostratigraphic progression for SIR ophiolites is from less to more HFSE-depleted and LILE-enriched compositions. This chemostratigraphic evolution reflects formation of what ultimately becomes forearc lithosphere as a result of mantle melting that is progressively influenced by subduction zone enrichment during SI. The magmatic chemostratigraphic progression for the Izu-Bonin-Mariana (IBM) forearc and most Tethyan ophiolites is specifically from MORB-like to arc-like (volcanic arc basalts or VAB +/- A boninites or BON) because SI progressed until establishment of a mature subduction zone. MORB-like lavas result from decompression melting of upwelling asthenosphere and are the first magmatic expression of SI. The contribution of fluids from dehydrating oceanic crust and sediments on the sinking slab is negligible in early SI, but continued melting results in a depleted, harzburgitic residue that is progressively metasomatized by fluids from the sinking slab; subsequent partial melting of this residue yields 'typical' SSZ-like lavas in the latter stages of SI. If SI is arrested early, e.g., as a result of collision, 'MORB-only' ophiolites might be expected. Consequently, MORB- and SSZ-only ophiolites may represent end-members of the SI ophiolite spectrum. The chemostratigraphic similarity of the Mariana forearc with that of ophiolites that follow the SIR intimates that a model linking such ophiolites, oceanic forearcs, and SI is globally applicable. C1 [Whattam, Scott A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Stern, Robert J.] Univ Texas Dallas, Geosci Dept, Dallas, TX 75083 USA. RP Whattam, SA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM whattams@si.edu OI Whattam, Scott/0000-0001-9193-9002 FU National Science Foundation FX RJS thanks many of his colleagues who helped him over the years understand what happens during subduction initiation, including Sherm Bloomer, Yildirim Dilek, Mike Gurnis, Osamu Ishizuka, Yas Ohara, Hadi Shafaii Moghadem, Julian Pearce, Mark Reagan, and John Shervais. These insights would not have been possible without support from the National Science Foundation. NR 70 TC 71 Z9 73 U1 10 U2 55 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0010-7999 J9 CONTRIB MINERAL PETR JI Contrib. Mineral. Petrol. PD NOV PY 2011 VL 162 IS 5 BP 1031 EP 1045 DI 10.1007/s00410-011-0638-z PG 15 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 830SN UT WOS:000295677500009 ER PT J AU Rick, TC DeLong, RL Erlandson, JM Braje, TJ Jones, TL Arnold, JE Des Lauriers, MR Hildebrandt, WR Kennett, DJ Vellanoweth, RL Wake, TA AF Rick, Torben C. DeLong, Robert L. Erlandson, Jon M. Braje, Todd J. Jones, Terry L. Arnold, Jeanne E. Des Lauriers, Matthew R. Hildebrandt, William R. Kennett, Douglas J. Vellanoweth, Rene L. Wake, Thomas A. TI Where were the northern elephant seals? Holocene archaeology and biogeography of Mirounga angustirostris SO HOLOCENE LA English DT Article DE historical ecology; human-environmental interactions; marine conservation; Pacific Coast; pinniped; Phocidae ID SOUTHERN NORTHWEST COAST; SAN-MIGUEL ISLAND; POPULATION BOTTLENECK; CALIFORNIA; PACIFIC; AMERICA; OREGON; EXTINCTION; RESPONSES; EXAMPLES AB Driven to the brink of extinction during the nineteenth century commercial fur and oil trade, northern elephant seal (NES, Mirounga angustirostris) populations now exceed 100 000 animals in the northeast Pacific from Alaska to Baja California. Because little is known about the biogeography and ecology of NES prior to the mid-nineteenth century, we synthesize and analyze the occurrence of NES remains in North American archaeological sites. Comparing these archaeological data with modern biogeographical, genetic, and behavioral data, we provide a trans-Holocene perspective on NES distribution and abundance. Compared with other pinnipeds, NES bones are relatively rare throughout the Holocene, even in California where they currently breed in large numbers. Low numbers of NES north of California match contemporary NES distribution, but extremely low occurrences in California suggest their abundance in this area was very different during the Holocene than today. We propose four hypotheses to explain this discrepancy, concluding that ancient human settlement and other activities may have displaced NES from many of their preferred modern habitats during much of the Holocene. C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Erlandson, Jon M.; Kennett, Douglas J.] Univ Oregon, Eugene, OR 97403 USA. [Braje, Todd J.] San Diego State Univ, San Diego, CA 92182 USA. [Jones, Terry L.] California Polytech State Univ, San Luis Obispo, CA USA. [Arnold, Jeanne E.; Wake, Thomas A.] Univ Calif Los Angeles, Los Angeles, CA USA. [Des Lauriers, Matthew R.] Calif State Univ Northridge, Northridge, CA 91330 USA. [Vellanoweth, Rene L.] Calif State Univ Los Angeles, Los Angeles, CA USA. RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. EM rickt@si.edu RI Kennett, Douglas/I-7613-2015; OI Kennett, Douglas/0000-0001-5133-9010; Erlandson, Jon/0000-0002-4705-4319 FU Channel Islands National Park; Western National Parks Association; National Science Foundation; our home institutions FX This paper is dedicated to the late Phillip L. Walker, friend, mentor, and colleague, who helped shape our thinking on numerous topics, including ancient interactions between humans and pinnipeds. Our work on the Channel Islands has been supported by Channel Islands National Park, the Western National Parks Association, the National Science Foundation, and our home institutions. Finally, we thank Arlene Rosen and two anonymous reviewers for constructive comments that greatly improved this manuscript. NR 67 TC 6 Z9 6 U1 1 U2 23 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0959-6836 J9 HOLOCENE JI Holocene PD NOV PY 2011 VL 21 IS 7 BP 1159 EP 1166 DI 10.1177/0959683611400463 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 825ZF UT WOS:000295320200013 ER PT J AU Cardoso, P Erwin, TL Borges, PAV New, TR AF Cardoso, Pedro Erwin, Terry L. Borges, Paulo A. V. New, Tim R. TI The seven impediments in invertebrate conservation and how to overcome them SO BIOLOGICAL CONSERVATION LA English DT Article DE Conservation priorities; Ecosystem services; Extinction; Information shortfalls; Science funding; Species diversity ID WILLINGNESS-TO-PAY; BIODIVERSITY CONSERVATION; ECOSYSTEM SERVICES; RED LIST; AGRICULTURAL LANDSCAPES; SPECIES CONSERVATION; INSECT CONSERVATION; TROPICAL FORESTS; CITIZEN SCIENCE; EXTINCTION AB Despite their high diversity and importance for humankind, invertebrates are often neglected in biodiversity conservation policies. We identify seven impediments to their effective protection: (1) invertebrates and their ecological services are mostly unknown to the general public (the public dilemma); (2) policy-makers and stakeholders are mostly unaware of invertebrate conservation problems (the political dilemma); (3) basic science on invertebrates is scarce and underfunded (the scientific dilemma); (4) most species are undescribed (the Linnean shortfall); (5) the distribution of described species is mostly unknown (the Wallacean shortfall); (6) the abundance of species and their changes in space and time are unknown (the Prestonian shortfall); (7) species ways of life and sensitivities to habitat change are largely unknown (the Hutchinsonian shortfall). Numerous recent developments in taxonomy, inventorying, monitoring, data compilation, statistical analysis and science communication facilitate overcoming these impediments in both policy and practice. We suggest as possible solutions for the public dilemma: better public information and marketing. For the political dilemma: red-listing, legal priority listing and inclusion in environmental impact assessment studies. For the scientific dilemma: parataxonomy, citizen science programs and biodiversity informatics. For the Linnean shortfall: biodiversity surrogacy, increased support for taxonomy and advances in taxonomic publications. For the Wallacean shortfall: funding of inventories, compilation of data in public repositories and species distribution modeling. For the Prestonian shortfall: standardized protocols for inventorying and monitoring, widespread use of analogous protocols and increased support for natural history collections. For the Hutchinsonian shortfall: identifying good indicator taxa and studying extinction rates by indirect evidence. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Cardoso, Pedro; Borges, Paulo A. V.] Univ Acores, Azorean Biodivers Grp CITA A, Dept Ciencias Agr, P-9700042 Angra Do Heroismo, Portugal. [Cardoso, Pedro; Erwin, Terry L.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [New, Tim R.] La Trobe Univ, Dept Zool, Bundoora, Vic 3086, Australia. RP Cardoso, P (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, Dept Ciencias Agr, Rua Capitao Joao Avila, P-9700042 Angra Do Heroismo, Portugal. EM pcardoso@ennor.org RI Borges, Paulo/B-2780-2008; Cardoso, Pedro/A-8820-2008 OI Borges, Paulo/0000-0002-8448-7623; Cardoso, Pedro/0000-0001-8119-9960 FU Portuguese Foundation for Science and Technology [SFRH/BPD/40688/2007, FCT - PTDC/BIA-BEC/104571/2008, FCT - PTDC/BIA-BEC/100182/2008] FX We thank J. Hortal, S. Ribeiro and A.S. Pullin for suggestions and fruitful discussions around the subject. P.C. and P.A.V.B. are supported by the Portuguese Foundation for Science and Technology (SFRH/BPD/40688/2007; FCT - PTDC/BIA-BEC/104571/2008; FCT - PTDC/BIA-BEC/100182/2008). NR 125 TC 143 Z9 150 U1 18 U2 171 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD NOV PY 2011 VL 144 IS 11 BP 2647 EP 2655 DI 10.1016/j.biocon.2011.07.024 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 827QL UT WOS:000295442900013 ER PT J AU Greco, MK Welz, PM Siegrist, M Ferguson, SJ Gallmann, P Roubik, DW Engel, MS AF Greco, M. K. Welz, P. M. Siegrist, M. Ferguson, S. J. Gallmann, P. Roubik, D. W. Engel, M. S. TI Description of an ancient social bee trapped in amber using diagnostic radioentomology SO INSECTES SOCIAUX LA English DT Article DE Proplebeia; Stingless bees; Diagnostic radioentomology; Miocene; Burdigalian; MicroCT; Amber ID TRIGONA-HYPOGEA HYMENOPTERA; RAY SYNCHROTRON MICROTOMOGRAPHY; XYLOCOPA-PUBESCENS SPINOLA; DOMINICAN AMBER; PROVENTRICULAR STRUCTURE; COMPUTERIZED-TOMOGRAPHY; PHYLOGENETIC ANALYSIS; HIGH-RESOLUTION; STINGLESS BEE; CARPENTER BEE AB The application of non-invasive imaging technologies using X-radiation (diagnostic radioentomology, 'DR') is demonstrated for the study of amber-entombed social bees. Here, we examine the external and internal morphology of an Early Miocene (Burdigalian) stingless bee (Apinae: Meliponini) from the Dominican Republic using non-destructive X-ray microtomography analysis. The study permits the accurate reconstruction of features otherwise obscured or impossible to visualize without destroying the sample and allows diagnosis of the specimen as a new species, Proplebeia adbita Greco and Engel. C1 [Greco, M. K.] Univ Bath, Dept Elect & Elect Engn, INVERT Grp, Bath BA2 7AY, Avon, England. [Greco, M. K.] Univ Bern, Dept Klin Vet Med, Vetsuisse Fak, CH-3001 Bern, Switzerland. [Gallmann, P.] Swiss Bee Res Ctr, Agroscope Liebefeld Posieux Res Stn ALP, CH-3033 Bern, Switzerland. [Welz, P. M.; Ferguson, S. J.] Univ Bern, Inst Surg Technol & Biomech, CH-3014 Bern, Switzerland. [Siegrist, M.] Univ Bern, Dept Clin Res, Bone Biol Grp, CH-3010 Bern, Switzerland. [Roubik, D. W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Engel, M. S.] Univ Kansas, Div Entomol Paleoentomol, Dept Ecol & Evolutionary Biol, Nat Hist Museum, Lawrence, KS 66049 USA. [Engel, M. S.] Amer Museum Nat Hist, Div Invertebrate Zool Entomol, New York, NY 10024 USA. RP Greco, MK (reprint author), Univ Bern, Dept Klin Vet Med, Vetsuisse Fak, CH-3001 Bern, Switzerland. EM M.K.Greco@bath.ac.uk RI Ferguson, Stephen/A-4118-2012; Engel, Michael/C-5461-2012; OI Engel, Michael/0000-0003-3067-077X; Greco, Mark/0000-0002-2136-5127 NR 65 TC 5 Z9 7 U1 0 U2 13 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD NOV PY 2011 VL 58 IS 4 BP 487 EP 494 DI 10.1007/s00040-011-0168-8 PG 8 WC Entomology SC Entomology GA 819JK UT WOS:000294821000008 ER PT J AU Stolarski, J Kitahara, MV Miller, DJ Cairns, SD Mazur, M Meibom, A AF Stolarski, Jaroslaw Kitahara, Marcelo V. Miller, David J. Cairns, Stephen D. Mazur, Maciej Meibom, Anders TI The ancient evolutionary origins of Scleractinia revealed by azooxanthellate corals SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID WATER CORALS; MITOCHONDRIAL; PHYLOGENY; SKELETON; AMPLIFICATION; ORDOVICIAN; ANTHOZOA; SCOTLAND; SUGGEST; PRIMERS AB Background: Scleractinian corals are currently a focus of major interest because of their ecological importance and the uncertain fate of coral reefs in the face of increasing anthropogenic pressure. Despite this, remarkably little is known about the evolutionary origins of corals. The Scleractinia suddenly appear in the fossil record about 240 Ma, but the range of morphological variation seen in these Middle Triassic fossils is comparable to that of modern scleractinians, implying much earlier origins that have so far remained elusive. A significant weakness in reconstruction(s) of early coral evolution is that deep-sea corals have been poorly represented in molecular phylogenetic analyses. Results: By adding new data from a large and representative range of deep-water species to existing molecular datasets and applying a relaxed molecular clock, we show that two exclusively deep-sea families, the Gardineriidae and Micrabaciidae, diverged prior to the Complexa/Robusta coral split around 425 Ma, thereby pushing the evolutionary origin of scleractinian corals deep into the Paleozoic. Conclusions: The early divergence and distinctive morphologies of the extant gardineriid and micrabaciid corals suggest a link with Ordovician "scleractiniamorph" fossils that were previously assumed to represent extinct anthozoan skeletonized lineages. Therefore, scleractinian corals most likely evolved from Paleozoic soft-bodied ancestors. Modern shallow-water Scleractinia, which are dependent on symbionts, appear to have had several independent origins from solitary, non-symbiotic precursors. The Scleractinia have survived periods of massive climate change in the past, suggesting that as a lineage they may be less vulnerable to future changes than often assumed. C1 [Stolarski, Jaroslaw] Polish Acad Sci, Inst Paleobiol, PL-00818 Warsaw, Poland. [Kitahara, Marcelo V.; Miller, David J.] James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia. [Kitahara, Marcelo V.; Miller, David J.] James Cook Univ, Coral Genom Grp, Townsville, Qld 4811, Australia. [Cairns, Stephen D.] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. [Mazur, Maciej] Univ Warsaw, Dept Chem, Lab Electrochem, PL-02093 Warsaw, Poland. [Meibom, Anders] LMCM, Museum Natl Hist Nat, UMR 7202, F-75005 Paris, France. RP Stolarski, J (reprint author), Polish Acad Sci, Inst Paleobiol, Twarda 51-55, PL-00818 Warsaw, Poland. EM stolacy@twarda.pan.pl RI Kitahara, Marcelo/D-5560-2011; Manager, MEEL/C-4732-2015 FU Polish Ministry of Science and Higher Education [N307-015733]; European Research Council [246749]; Australian Research Council (ARC) via the ARC Centre of Excellence for Coral Reef Studies (ARC CoE); Coordination for the Improvement of Higher Level Personnel (CAPES); Fisheries Research and Development Corporation (FRDC); Australian Government Department of Environment, Water, Heritage and the Arts; Australian CSIRO (Commonwealth Scientific and Industrial Research Organization) FX This work was supported in part by the Polish Ministry of Science and Higher Education (project N307-015733) to JS, the European Research Council through Advanced Grant 246749 (BIOCARB) to AM, the Australian Research Council (ARC) via the ARC Centre of Excellence for Coral Reef Studies (ARC CoE) to DJM, and PhD scholarship support for MVK via Coordination for the Improvement of Higher Level Personnel (CAPES). The authors also thank Nancy Knowlton, Eldon Ball and Sylvain Foret for their valuable comments on drafts of the manuscript. We would also like to acknowledge all the Smithsonian Institution invertebrate collection staff (NMNH) for sending the New Caledonian material to Australia, especially Paul Greenhall. Special thanks are due to all Museum of Tropical Queensland staff (MTQ-Queensland), especially Carden Wallace, Barbara Done for use of facilities at the Museum of Tropical Queensland. We also thank Philippe Bouchet (MNHN) who generously loaned the New Caledonian material from the Paris Museum to the Smithsonian Institution, and Bertrand Richer de Forges and IRD-Noumea staff and collaborators for their great effort in collecting and preserving the New Caledonian specimens examined in the present study. We extend our gratitude to Felicity McEnnulty (CSIRO) for the loan the Australian specimens examined in the present study, which were collected with funding from the Fisheries Research and Development Corporation (FRDC), Environment Australia (now the Australian Government Department of Environment, Water, Heritage and the Arts), and by the Australian CSIRO (Commonwealth Scientific and Industrial Research Organization) Wealth from Oceans Flagship with the assistance of the Australian Government Department of the Environment, Water, Heritage and the Arts. NR 53 TC 67 Z9 67 U1 4 U2 53 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD OCT 28 PY 2011 VL 11 AR 316 DI 10.1186/1471-2148-11-316 PG 10 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 852LD UT WOS:000297358500001 PM 22034946 ER PT J AU Loos, M Elsenbeer, H AF Loos, Martin Elsenbeer, Helmut TI Topographic controls on overland flow generation in a forest - An ensemble tree approach SO JOURNAL OF HYDROLOGY LA English DT Article DE Overland Bow; Tropical rainforest; Random Forest; Spatial scale; Digital Elevation Model; Topography ID TROPICAL RAIN-FOREST; DIGITAL TERRAIN MODELS; SOIL-MOISTURE; HYDRAULIC CONDUCTIVITY; HYDROLOGICAL PROCESSES; STORMFLOW GENERATION; DEPRESSION-STORAGE; EROSION PROCESSES; CATCHMENT; WATER AB Overland flow is an important hydrological pathway in many forests of the humid tropics. Its generation is subject to topographic controls at differing spatial scales. Our objective was to identify such controls on the occurrence of overland flow in a lowland tropical rainforest. To this end, we installed 95 overland flow detectors (OFDs) in four nested subcatchments of the Lutzito catchment on Barro Colorado Island, Panama, and monitored the frequency of overland flow occurrence during 18 rainfall events at each OFD location temporal frequency. For each such location, we derived three non-digital terrain attributes and 17 digital ones, of which 15 were based on Digital Elevation Models (DEMs) of three different resolutions. These attributes then served as input into a Random Forest ensemble tree model to elucidate the importance and partial and joint dependencies of topographic controls for overland flow occurrence. Lutzito features a high median temporal frequency in overland flow occurrence of 0.421 among OFD locations. However, spatial temporal frequencies of overland flow occurrence vary strongly among these locations and the subcatchments of Lutzito catchment. This variability is best explained by (1) microtopography, (2) coarse terrain sloping and (3) various measures of distance-to-channel, with the contribution of all other terrain attributes being small. Microtopographic features such as concentrated flowlines and wash areas produce highest temporal frequencies, whereas the occurrence of overland flow drops sharply for flow distances and terrain sloping beyond certain threshold values. Our study contributes to understanding both the spatial controls on overland flow generation and the limitations of terrain attributes for the spatially explicit prediction of overland flow frequencies. (C) 2011 Elsevier B.V. All rights reserved. C1 [Loos, Martin; Elsenbeer, Helmut] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany. [Elsenbeer, Helmut] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Loos, M (reprint author), Dr Gebauer Str 40, D-55411 Bingen, Germany. EM martin.loos@alumni.uni-potsdam.de FU German Academic Exchange Service (DAAD) FX This study was funded by the German Academic Exchange Service (DAAD). The Smithsonian Tropical Research Institute kindly provided rainfall data and research facilities. Further financial and logistical support was provided by Ursula and Jurgen Loos. We appreciate the thoughtful and constructive comments by an anonymous reviewer. NR 84 TC 15 Z9 16 U1 4 U2 24 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 J9 J HYDROL JI J. Hydrol. PD OCT 28 PY 2011 VL 409 IS 1-2 BP 94 EP 103 DI 10.1016/j.jhydrol.2011.08.002 PG 10 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 842LT UT WOS:000296601600008 ER PT J AU Tscherbul, TV Klos, J Buchachenko, AA AF Tscherbul, T. V. Klos, J. Buchachenko, A. A. TI Ultracold spin-polarized mixtures of (2)Sigma molecules with S-state atoms: Collisional stability and implications for sympathetic cooling SO PHYSICAL REVIEW A LA English DT Article AB The prospects of sympathetic cooling of polar molecules with magnetically cotrapped alkali-metal atoms are generally considered poor due to strongly anisotropic atom-molecule interactions leading to large spin relaxation rates. Using rigorous quantum scattering calculations based on ab initio interaction potentials, we show that inelastic spin relaxation in low-temperature collisions of CaH((2)Sigma) molecules with Li and Mg atoms occurs at a slow rate despite the strongly anisotropic interactions. This unexpected result, which we rationalize using multichannel quantum-defect theory, opens up the possibility of sympathetic cooling of polar (2)Sigma molecules with alkali-metal atoms in a magnetic trap and with alkaline-earth-metal atoms in an optical dipole trap. C1 [Tscherbul, T. V.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, T. V.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Klos, J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Buchachenko, A. A.] Moscow MV Lomonosov State Univ, Dept Chem, RU-119991 Moscow, Russia. RP Tscherbul, TV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. EM tshcherb@cfa.harvard.edu RI Buchachenko, Alexei/C-8452-2012; Klos, Jacek/A-6457-2008; Tscherbul, Timur/K-3286-2014 OI Buchachenko, Alexei/0000-0003-0701-5531; Klos, Jacek/0000-0002-7407-303X; Tscherbul, Timur/0000-0001-5689-040X FU NSF [CHE-0848110]; RFBR [03-11-00081] FX We thank H.-I Lu, M. J. Wright, and J. M. Doyle for discussions and A. Dalgarno and J. F. E. Croft for helpful comments on the manuscript. This work was supported by NSF grants to the Harvard-MIT CUA and ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. A. A. B. and J. K. acknowledge support from RFBR (project No. 03-11-00081) and the NSF (Grant No. CHE-0848110 to M. H. Alexander). NR 40 TC 15 Z9 15 U1 0 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD OCT 28 PY 2011 VL 84 IS 4 AR 040701 DI 10.1103/PhysRevA.84.040701 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 838JJ UT WOS:000296284300001 ER PT J AU Helgen, KM AF Helgen, Kristofer M. TI The Mammal Family Tree SO SCIENCE LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. RP Helgen, KM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, MRC 108,POB 37012, Washington, DC 20013 USA. EM helgenk@si.edu NR 11 TC 6 Z9 7 U1 3 U2 30 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 28 PY 2011 VL 334 IS 6055 BP 458 EP 459 DI 10.1126/science.1214544 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 837UR UT WOS:000296230500027 PM 22034419 ER PT J AU Benjamin, SP AF Benjamin, Suresh P. TI Phylogenetics and comparative morphology of crab spiders (Araneae: Dionycha, Thomisidae) SO ZOOTAXA LA English DT Article DE Arachnida; Biodiversity; Character weighting; Cladistics; Color change behavior; implied weights; sampling bias ID MISUMENA-VATIA; CHEMICAL ATTRACTION; CLADISTIC-ANALYSIS; REVISION; GENUS; PHILODROMIDAE; SALTICIDAE; ARANEOIDEA; ARACHNIDA; PARSIMONY AB The higher-level phylogenetic relationships of crab spiders (Thomisidae) are studied from morphological data. 33 taxa are coded for 74 characters (53 binary and 21 multistate). Several analyses using equal, successive and implied weights were carried out. The most parsimonious tree obtained by analysis with successive and implied weights is put forward as the preferred hypothesis of thomisid relationships (length 222 steps, CI 0.74, RI 0.83). Thomisidae emerge monophyletic in all analyses, supported by four unambiguous synapomorphies. It is now apparent that thomisid taxa have been mostly defined on the basis of plesiomorphic character states. A number of taxonomic changes, including the description of new taxa are proposed and the evolution of diverse behaviors of thomisids is studied in light of the new phylogenetic result. Color change behavior evolved once within the family, but eye arrangement patterns of the median ocular quadrangle, thought to be diagnostic for many genera, evolved as much as 10 times independently. The following new species are described: Borboropactus nyerere sp. nov., Cebrenninus srivijaya sp. nov., Geraesta lehtineni sp. nov. and Geraesta mkwawa sp. nov. The following new generic synonymies are proposed: Bucranium O. P.-Cambridge, 1881 = Aphantochilus O. P.-Cambridge, 1870; Sanmenia Song and Kim, 1992 = Pharta Thorell, 1891 and Cupa Strand, 1906 = Epidius Thorell, 1877. The following species are synonymized: Regillus divergens Hogg, 1914 and Borboropactus hainanus Song, 1993 = Borboropactus bituberculatus Simon, 1884 syn. nov., Epidius ganxiensis (Yin, Peng & Kim, 1999) = Epidius rubropictus Simon, 1909 syn. nov., Geraesta bilobata Simon, 1897 = Geraesta hirta Simon, 1889 syn. nov., Sanmenia kohi Ono, 1995 = Pharta bimaculata Thorell, 1891 syn. nov. and Sanmenia zhengi (Ono & Song, 1986) = Pharta brevipalpus (Simon, 1903) syn. nov. The following new combinations are proposed: Aphantochilus taurifrons (O. P.-Cambridge, 1881) comb. nov., Epidius typicus (Bosenberg & Strand, 1906) comb. nov., Pharta brevipalpus (Simon, 1903) comb. nov., Pharta gongshan (Yang, Zhu and Song, 2006) comb. nov., Pharta nigra (Tang, Griswold & Peng, 2009) comb. nov. and Pharta tengchong (Tang, Griswold & Yin, 2009) comb. nov. C1 [Benjamin, Suresh P.] Inst Fundamental Studies, Kandy, Sri Lanka. [Benjamin, Suresh P.] Smithsonian Inst, Natl Museum Nat Hist MRC 105, Dept Entomol, Washington, DC 20013 USA. RP Benjamin, SP (reprint author), Inst Fundamental Studies, Hantana Rd, Kandy, Sri Lanka. EM suresh.benjamin@gmail.com FU Smithsonian Institution; Institute of Fundamental Studies FX This study was mainly funded by a Smithsonian Institution postdoctoral fellowship. Additional funding came from Institute of Fundamental Studies. Thanks to the following individuals for spider specimens: Fernando Alvarez, David Court, Gustavo Hormiga, Cristian Grismado, Charles Haddad, Stephen Lew, Lara Lopardo and Tang Guo. Thanks to the following curators for granting access to collections under their care: Jonathan Coddington and Dana M. De Roche (USNM), Jason Dunlop (MNHU), Charles Griswold (CAS), Peter Jager (SMF), Rudy Jocque (MRAC), Torbjorn Kronestedt (SMNH), Christine Rollard and Elise-Anne Leguin (MNHN), Peter Schwendinger (MHNG). David Court and Martin Ramirez improved earlier drafts of this manuscript. Thanks to two anonymous reviewers and Christoph Muster for providing critical comments. The SEMs were taken at the Smithsonian's National Museum of Natural History Scanning Electron Microscope Facility with assistance from Scott Whittaker. NR 117 TC 19 Z9 21 U1 2 U2 6 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 28 PY 2011 IS 3080 BP 1 EP 108 PG 108 WC Zoology SC Zoology GA 846CR UT WOS:000296875300001 ER PT J AU Gallegos, CL Werdell, PJ McClain, CR AF Gallegos, Charles L. Werdell, P. Jeremy McClain, Charles R. TI Long-term changes in light scattering in Chesapeake Bay inferred from Secchi depth, light attenuation, and remote sensing measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID EXOPOLYMER PARTICLES TEP; INHERENT OPTICAL-PROPERTIES; DISSOLVED ORGANIC-MATTER; INFRARED SPECTRAL REGION; OCEANIC WATERS; MARINE PARTICLES; COASTAL WATERS; ABSORPTION-COEFFICIENTS; NATURAL PHYTOPLANKTON; BACKSCATTERING RATIO AB The relationship between the Secchi depth (Z(SD)) and the diffuse attenuation coefficient for photosynthetically active radiation (K-d(PAR)), and in particular the product of the two, Z(SD)center dot K-d(PAR), is governed primarily by the ratio of light scattering to absorption. We analyzed measurements of Z(SD) and K-d(PAR) at main stem stations in Chesapeake Bay and found that the Z(SD)center dot K-d(PAR) product has declined at rates varying from 0.020 to 0.033 yr(-1) over the 17 to 25 years of measurement, implying that there has been a long-term increase in the scattering-to-absorption ratio. Remote sensing reflectance at the green wavelength most relevant to Z(SD) and K-d(PAR) in these waters, R-rs(555), did not exhibit an increasing trend over the 10 years of available measurements. To reconcile the observations we constructed a bio-optical model to calculate Z(SD), K-d(PAR), Z(SD)center dot K-d(PAR), and R-rs(555) as a function of light attenuating substances and their mass-specific absorption and scattering coefficients. When simulations were based exclusively on changes in concentrations of light attenuating substances, a declining trend in Z(SD)center dot K-d entailed an increasing trend in R-rs(555), contrary to observations. To simulate both decreasing Z(SD center dot)K(d)(PAR) and stationary R-rs(555), it was necessary to allow for a declining trend in the ratio of backscattering to total scattering. Within our simulations, this was accomplished by increasing the relative proportion of organic detritus with high mass-specific scattering and low backscattering ratio. An alternative explanation not explicitly modeled is an increasing tendency for the particulate matter to occur in large aggregates. Data to discriminate between these alternatives are not available. C1 [Gallegos, Charles L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Werdell, P. Jeremy; McClain, Charles R.] NASA, Goddard Space Flight Ctr, Ocean Ecol Branch, Greenbelt, MD 20771 USA. RP Gallegos, CL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gallegosc@si.edu RI Werdell, Jeremy/D-8265-2012; OI Gallegos, Charles/0000-0001-5112-0166 NR 75 TC 20 Z9 20 U1 0 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD OCT 27 PY 2011 VL 116 AR C00H08 DI 10.1029/2011JC007160 PG 19 WC Oceanography SC Oceanography GA 838YH UT WOS:000296329800003 ER PT J AU Gregoric, M Agnarsson, I Blackledge, TA Kuntner, M AF Gregoric, Matjaz Agnarsson, Ingi Blackledge, Todd A. Kuntner, Matjaz TI How Did the Spider Cross the River? Behavioral Adaptations for River-Bridging Webs in Caerostris darwini (Araneae: Araneidae) SO PLOS ONE LA English DT Article ID ORB-WEAVING SPIDERS; PHYLOGENY; EVOLUTION; CONSTRUCTION; ULOBORIDAE; SIZE; DIVERSIFICATION; TETRAGNATHIDAE; THERIDIIDAE; COEVOLUTION AB Background: Interspecific coevolution is well described, but we know significantly less about how multiple traits coevolve within a species, particularly between behavioral traits and biomechanical properties of animals' "extended phenotypes''. In orb weaving spiders, coevolution of spider behavior with ecological and physical traits of their webs is expected. Darwin's bark spider (Caerostris darwini) bridges large water bodies, building the largest known orb webs utilizing the toughest known silk. Here, we examine C. darwini web building behaviors to establish how bridge lines are formed over water. We also test the prediction that this spider's unique web ecology and architecture coevolved with new web building behaviors. Methodology: We observed C. darwini in its natural habitat and filmed web building. We observed 90 web building events, and compared web building behaviors to other species of orb web spiders. Conclusions: Caerostris darwini uses a unique set of behaviors, some unknown in other spiders, to construct its enormous webs. First, the spiders release unusually large amounts of bridging silk into the air, which is then carried downwind, across the water body, establishing bridge lines. Second, the spiders perform almost no web site exploration. Third, they construct the orb capture area below the initial bridge line. In contrast to all known orb-weavers, the web hub is therefore not part of the initial bridge line but is instead built de novo. Fourth, the orb contains two types of radial threads, with those in the upper half of the web doubled. These unique behaviors result in a giant, yet rather simplified web. Our results continue to build evidence for the coevolution of behavioral (web building), ecological (web microhabitat) and biomaterial (silk biomechanics) traits that combined allow C. darwini to occupy a unique niche among spiders. C1 [Gregoric, Matjaz; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Ljubljana, Slovenia. [Agnarsson, Ingi] Univ Puerto Rico, Dept Biol, San Juan, PR 00936 USA. [Blackledge, Todd A.] Univ Akron, Dept Biol, Integrated Biosci Program, Akron, OH 44325 USA. [Agnarsson, Ingi; Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan 430062, Hubei, Peoples R China. RP Gregoric, M (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Ljubljana, Slovenia. EM matjaz.gregoric@gmail.com FU National Geographic [8655-09]; Slovenian Research Agency [P1-0236, J1-2063]; National Science Foundation [IOS-0745379] FX This is the second contribution resulting from the 2010 Madagascar expedition, funded by National Geographic (grant 8655-09 to Dr. Agnarsson, Dr. Kuntner and Dr. Blackledge). Additional funding came from the Slovenian Research Agency (grants P1-0236, J1-2063 to Dr. Kuntner) and National Science Foundation (IOS-0745379 to Dr. Blackledge). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 52 TC 9 Z9 9 U1 3 U2 29 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 26 PY 2011 VL 6 IS 10 AR e26847 DI 10.1371/journal.pone.0026847 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 841NR UT WOS:000296519600065 PM 22046378 ER PT J AU Oka, M Phan, TD Eastwood, JP Angelopoulos, V Murphy, NA Oieroset, M Miyashita, Y Fujimoto, M McFadden, J Larson, D AF Oka, M. Phan, T. -D. Eastwood, J. P. Angelopoulos, V. Murphy, N. A. Oieroset, M. Miyashita, Y. Fujimoto, M. McFadden, J. Larson, D. TI Magnetic reconnection X-line retreat associated with dipolarization of the Earth's magnetosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID NEUTRAL LINE; SUBSTORM EXPANSION; CURRENT DISRUPTION; MAGNETOTAIL; RECOVERY; ONSET; EVENT; FIELD; TAIL AB Magnetic reconnection is the key process of plasma transport in the Earth's magnetotail. The 'X-line' where magnetic field lines reconnect often moves away from the Earth. However, the precise cause of the X-line motion remains unclear. Here we present data from five THEMIS probes positioned along the Sun-Earth line and show that a tailward retreat motion of the X-line (detected by the outermost probe P1) occurred when the dipolarized inner magnetosphere started to return to a more stretched, tail-like configuration (observed by the inner probes P3, P4, and P5). At an intermediate location (P2), the total pressure was increasing. These observations are consistent with the idea that the pressure increase in the inner magnetosphere eventually causes the X-line to retreat tailward. Citation: Oka, M., T.-D. Phan, J. P. Eastwood, V. Angelopoulos, N. A. Murphy, M. Oieroset, Y. Miyashita, M. Fujimoto, J. McFadden, and D. Larson (2011), Magnetic reconnection X-line retreat associated with dipolarization of the Earth's magnetosphere, Geophys. Res. Lett., 38, L20105, doi:10.1029/2011GL049350. C1 [Oka, M.; Phan, T. -D.; Oieroset, M.; McFadden, J.; Larson, D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Eastwood, J. P.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BW, England. [Angelopoulos, V.] Univ Calif Los Angeles, IGPP, ESS, Los Angeles, CA 90095 USA. [Murphy, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miyashita, Y.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Fujimoto, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. RP Oka, M (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM moka@ssl.berkeley.edu RI NASA MMS, Science Team/J-5393-2013; OI NASA MMS, Science Team/0000-0002-9504-5214; Oka, Mitsuo/0000-0003-2191-1025; Murphy, Nicholas/0000-0001-6628-8033 FU NSF [ATM-0503374]; NASA at UC Berkeley [NNX08AO83G]; Imperial College London; NASA [NNX11AB61G] FX The authors acknowledge helpful discussions with M. Cartwright. We also acknowledge K. H. Glassmeier and his group at Technical University of Braunschweig for providing the magnetometer data (FGM). We made extensive use of the software (TDAS) developed by the THEMIS team as well as the Coordinated Data Analysis Web of NASA. This research was funded by NSF grant ATM-0503374 and NASA grant NNX08AO83G at UC Berkeley. JPE holds an STFC Advanced Fellowship at Imperial College London. NAM is supported by NASA grant NNX11AB61G. NR 27 TC 17 Z9 17 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 26 PY 2011 VL 38 AR L20105 DI 10.1029/2011GL049350 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 839CT UT WOS:000296343000005 ER PT J AU Peer, BD Kuehn, MJ Rothstein, SI Fleischer, RC AF Peer, Brian D. Kuehn, Michael J. Rothstein, Stephen I. Fleischer, Robert C. TI Persistence of host defence behaviour in the absence of avian brood parasitism SO BIOLOGY LETTERS LA English DT Article DE brood parasitism; coevolution; egg rejection; molecular clock; relaxed selection ID COWBIRD PARASITISM; COEVOLUTION; CUCKOO; DISCRIMINATION AB The fate of host defensive behaviour in the absence of selection from brood parasitism is critical to long-term host-parasite coevolution. We investigated whether New World Bohemian waxwings Bombycilla garrulus that are allopatric from brown-headed cowbird Molothrus ater and common cuckoo Cuculus canorus parasitism have retained egg rejection behaviour. We found that egg rejection was expressed by 100 per cent of Bohemian waxwings. Our phylogeny revealed that Bohemian and Japanese waxwings Bombycilla japonica were sister taxa, and this clade was sister to the cedar waxwing Bombycilla cedrorum. In addition, there was support for a split between Old and New World Bohemian waxwings. Our molecular clock estimates suggest that egg rejection may have been retained for 2.8-3.0 Myr since NewWorld Bohemian waxwings inherited it from their common ancestor with the rejecter cedar waxwings. These results support the 'single trajectory' model of host-brood parasite coevolution that once hosts evolve defences, they are retained, forcing parasites to become more specialized over time. C1 [Peer, Brian D.; Fleischer, Robert C.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Peer, Brian D.; Kuehn, Michael J.; Rothstein, Stephen I.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Peer, Brian D.] Western Illinois Univ, Dept Sci Biol, Macomb, IL 61455 USA. [Kuehn, Michael J.] Western Fdn Vertebrate Zool, Camarillo, CA 93012 USA. RP Peer, BD (reprint author), Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA. EM bd-peer@wiu.edu FU Western Illinois University; N.S.F. [0078139] FX This research was supported by N.S.F. grant 0078139 awarded to S.I.R., R.C.F. and B.D.P. B.D.P. and R.C.F. were supported by a Faculty Mentoring grant from Western Illinois University while preparing the article. NR 24 TC 18 Z9 20 U1 3 U2 26 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD OCT 23 PY 2011 VL 7 IS 5 BP 670 EP 673 DI 10.1098/rsbl.2011.0268 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 818QE UT WOS:000294768400011 PM 21493623 ER PT J AU Yunes, N Kocsis, B Loeb, A Haiman, Z AF Yunes, Nicolas Kocsis, Bence Loeb, Abraham Haiman, Zoltan TI Imprint of Accretion Disk-Induced Migration on Gravitational Waves from Extreme Mass Ratio Inspirals SO PHYSICAL REVIEW LETTERS LA English DT Article ID ACTIVE GALACTIC NUCLEI; STANDARD SIRENS; BLACK-HOLES; PLANET MIGRATION; MHD TURBULENCE; VISCOSITY; LISA; SATELLITES; BINARIES; STARS AB We study the effects of a thin gaseous accretion disk on the inspiral of a stellar-mass black hole into a supermassive black hole. We construct a phenomenological angular momentum transport equation that reproduces known disk effects. Disk torques modify the gravitational wave phase evolution to detectable levels with LISA for reasonable disk parameters. The Fourier transform of disk-modified waveforms acquires a correction with a different frequency trend than post-Newtonian vacuum terms. Such inspirals could be used to detect accretion disks with LISA and to probe their physical parameters. C1 [Yunes, Nicolas] MIT, Dept Phys, Cambridge, MA 02139 USA. [Yunes, Nicolas] MIT Kavli Inst, Cambridge, MA 02139 USA. [Yunes, Nicolas; Kocsis, Bence; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Haiman, Zoltan] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Yunes, N (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 FU NASA [PF9-00063, PF0-110080, NAS8-03060, NNX08AL43G, NNA09DB30A, NNX08AH35G]; NSF [AST-0907890]; Hungarian National Office for Research and Technology (NKTH); Hungarian Research Fund (OTKA) [68228] FX B. K. and N. Y. acknowledge support from the NASA through Einstein Fellowship PF9-00063 and PF0-110080 issued by the Chandra X-ray Observatory, operated by the SAO, on behalf of NASA under NAS8-03060. A. L. acknowledges support from NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A, Z. H. from the Polanyi Program of the Hungarian National Office for Research and Technology (NKTH) and from NASA grant NNX08AH35G, and B. K. from the Hungarian Research Fund (OTKA) grant 68228. NR 38 TC 28 Z9 28 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD OCT 21 PY 2011 VL 107 IS 17 AR 171103 DI 10.1103/PhysRevLett.107.171103 PG 5 WC Physics, Multidisciplinary SC Physics GA 847PN UT WOS:000296985000001 PM 22107500 ER PT J AU Hong, J Allen, B Grindlay, J Barthelemy, S Baker, R Garson, A Krawczynski, H Apple, J Cleveland, WH AF Hong, J. Allen, B. Grindlay, J. Barthelemy, S. Baker, R. Garson, A. Krawczynski, H. Apple, J. Cleveland, W. H. TI Flight performance of an advanced CZT imaging detector in a balloon-borne wide-field hard X-ray telescope-ProtoEXIST1 SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE Hard X-ray imaging; CdZnTe; Coded-aperture imaging AB We successfully carried out the first high-altitude balloon flight of a wide-field hard X-ray coded-aperture telescope ProtoEXIST1, which was launched from the Columbia Scientific Balloon Facility at Ft. Sumner, New Mexico on October 9, 2009. ProtoEXIST1 is the first implementation of an advanced CdZnTe (CZT) imaging detector in our ongoing program to establish the technology required for next generation wide-field hard X-ray telescopes such as the High Energy Telescope (HET) in the Energetic X-ray Imaging Survey Telescope (EXIST). The CZT detector plane in ProtoEXIST1 consists of an 8 x 8 array of closely tiled 2 cm x 2 cm x 0.5 cm thick pixellated CZT crystals, each with 8 x 8 pixels, mounted on a set of readout electronics boards and covering a 256 cm(2) active area with 2.5 mm pixels. A tungsten mask, mounted at 90 cm above the detector provides shadowgrams of X-ray sources in the 30-600 keV band for imaging, allowing a fully coded field of view of 9 degrees x 9 degrees (and 19 degrees x 19 degrees for 50% coding fraction) with an angular resolution of 20'. In order to reduce the background radiation, the detector is surrounded by semi-graded (Pb/Sn/Cu) passive shields on the four sides all the way to the mask. On the back side, a 26 cm x 26 cm x 2 cm CsI(Na) active shield provides signals to tag charged particle induced events as well as greater than or similar to 100 keV background photons from below. The flight duration was only about 7.5 h due to strong winds (60 knots) at float altitude (38-39 km). Throughout the flight, the CZT detector performed excellently. The telescope observed Cyg X-1, a bright black hole binary system, for similar to 1 h at the end of the flight. Despite a few problems with the pointing and aspect systems that caused the telescope to track about 6.4 degrees off the target, the analysis of the Cyg X-1 data revealed an X-ray source at 7.2 sigma in the 30-100 key energy band at the expected location from the optical images taken by the onboard daytime star camera. The success of this first flight is very encouraging for the future development of the advanced CZT imaging detectors (ProtoEXIST2, with 0.6 mm pixels), which will take advantage of the modularization architecture employed in ProtoEXIST1. (C) 2011 Elsevier B.V. All rights reserved. C1 [Hong, J.; Allen, B.; Grindlay, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barthelemy, S.; Baker, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Garson, A.; Krawczynski, H.] Washington Univ, St Louis, MO 63130 USA. [Garson, A.; Krawczynski, H.] McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Apple, J.; Cleveland, W. H.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Apple, J.; Cleveland, W. H.] Univ Space Res Assoc, Huntsville, AL 35812 USA. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jaesub@head.cfa.harvard.edu FU NASA [NNG06WC12G, NNXO9AD76G, NNX10AJ56G] FX This work was supported by NASA Grants NNG06WC12G and NNXO9AD76G to Harvard University, and NASA Grant NNX10AJ56G to Washington University in St. Louis. We thank M. Burke (SAO engineering), N. Gehrels (GSFC), K. Dietz, C.M. Benson, B. Ramsey (MSFC), D. Huie (University of Alabama Hunsville), W.R. Cook and F. Harrison (Caltech) for their support in the development and assembly of the ProtoEXIST1 detector, telescope and gondola. We also thank the McDonnell Center for the Space Sciences for their support in the active CsI shield assembly, and the NASA CSBF balloon launching team for their excellent support. NR 18 TC 6 Z9 6 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD OCT 21 PY 2011 VL 654 IS 1 BP 361 EP 372 DI 10.1016/j.nima.2011.07.025 PG 12 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 831XT UT WOS:000295765100051 ER PT J AU Hogerheijde, MR Bergin, EA Brinch, C Cleeves, LI Fogel, JKJ Blake, GA Dominik, C Lis, DC Melnick, G Neufeld, D Panic, O Pearson, JC Kristensen, L Yildiz, UA van Dishoeck, EF AF Hogerheijde, Michiel R. Bergin, Edwin A. Brinch, Christian Cleeves, L. Ilsedore Fogel, Jeffrey K. J. Blake, Geoffrey A. Dominik, Carsten Lis, Dariusz C. Melnick, Gary Neufeld, David Panic, Olja Pearson, John C. Kristensen, Lars Yildiz, Umut A. van Dishoeck, Ewine F. TI Detection of the Water Reservoir in a Forming Planetary System SO SCIENCE LA English DT Article ID T TAURI STARS; PROTOPLANETARY DISKS; HERSCHEL; LINES; ICE; INTERSTELLAR; EMISSION; SURFACE; REGION; GRAINS AB Icy bodies may have delivered the oceans to the early Earth, yet little is known about water in the ice-dominated regions of extrasolar planet-forming disks. The Heterodyne Instrument for the Far-Infrared on board the Herschel Space Observatory has detected emission lines from both spin isomers of cold water vapor from the disk around the young star TW Hydrae. This water vapor likely originates from ice-coated solids near the disk surface, hinting at a water ice reservoir equivalent to several thousand Earth oceans in mass. The water's ortho-to-para ratio falls well below that of solar system comets, suggesting that comets contain heterogeneous ice mixtures collected across the entire solar nebula during the early stages of planetary birth. C1 [Hogerheijde, Michiel R.; Brinch, Christian; Kristensen, Lars; Yildiz, Umut A.; van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bergin, Edwin A.; Cleeves, L. Ilsedore; Fogel, Jeffrey K. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Dominik, Carsten] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Lis, Dariusz C.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Melnick, Gary] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, David] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Panic, Olja] European So Observ, D-85748 Garching, Germany. [Pearson, John C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Hogerheijde, MR (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM michiel@strw.leidenuniv.nl RI Kristensen, Lars/F-4774-2011; Yildiz, Umut/C-5257-2011; Brinch, Christian/G-5157-2015 OI Kristensen, Lars/0000-0003-1159-3721; Yildiz, Umut/0000-0001-6197-2864; Brinch, Christian/0000-0002-5074-7183 FU Nederlandse Organisatie voor Wetenschappelijk Onderzoek [639.042.404]; NSF [0707777]; NASA FX Herschel is a European Space Agency space observatory with science instruments provided by European-led principal investigator consortia and with important participation from NASA. This work was partially supported by Nederlandse Organisatie voor Wetenschappelijk Onderzoek grant 639.042.404, NSF grant 0707777, and, as part of the NASA Herschel HIFI guaranteed time program, NASA. The data presented here are archived at the Herschel Science Archive, http://archives.esac.esa.int/hda/ui, under OBSID 1342198337 and 1342201585. NR 24 TC 106 Z9 107 U1 4 U2 18 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 21 PY 2011 VL 334 IS 6054 BP 338 EP 340 DI 10.1126/science.1208931 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 835RC UT WOS:000296052500042 PM 22021851 ER PT J AU Cox, P Krips, M Neri, R Omont, A Gusten, R Menten, KM Wyrowski, F Weiss, A Beelen, A Gurwell, MA Dannerbauer, H Ivison, RJ Negrello, M Aretxaga, I Hughes, DH Auld, R Baes, M Blundell, R Buttiglione, S Cava, A Cooray, A Dariush, A Dunne, L Dye, S Eales, SA Frayer, D Fritz, J Gavazzi, R Hopwood, R Ibar, E Jarvis, M Maddox, S Michallowski, M Pascale, E Pohlen, M Rigby, E Smith, DJB Swinbank, AM Temi, P Valtchanov, I van der Werf, P de Zotti, G AF Cox, P. Krips, M. Neri, R. Omont, A. Guesten, R. Menten, K. M. Wyrowski, F. Weiss, A. Beelen, A. Gurwell, M. A. Dannerbauer, H. Ivison, R. J. Negrello, M. Aretxaga, I. Hughes, D. H. Auld, R. Baes, M. Blundell, R. Buttiglione, S. Cava, A. Cooray, A. Dariush, A. Dunne, L. Dye, S. Eales, S. A. Frayer, D. Fritz, J. Gavazzi, R. Hopwood, R. Ibar, E. Jarvis, M. Maddox, S. Michallowski, M. Pascale, E. Pohlen, M. Rigby, E. Smith, D. J. B. Swinbank, A. M. Temi, P. Valtchanov, I. van der Werf, P. de Zotti, G. TI GAS AND DUST IN A SUBMILLIMETER GALAXY AT z=4.24 FROM THE HERSCHEL ATLAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: high-redshift; galaxies: individual (ID 141); galaxies: starburst; submillimeter: galaxies ID ULTRALUMINOUS INFRARED GALAXIES; ISO-LWS SPECTROSCOPY; MICRON LINE DEFICIT; STAR-FORMATION; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; ATOMIC CARBON; MU-M; MOLECULAR GAS; PHYSICAL CONDITIONS AB We report ground-based follow-up observations of the exceptional source, ID 141, one of the brightest sources detected so far in the Herschel Astrophysical Terahertz Large Area Survey cosmological survey. ID 141 was observed using the IRAM 30 m telescope and Plateau de Bure interferometer (PdBI), the Submillimeter Array, and the Atacama Pathfinder Experiment submillimeter telescope to measure the dust continuum and emission lines of the main isotope of carbon monoxide and carbon ([C I] and [C II]). The detection of strong CO emission lines with the PdBI confirms that ID 141 is at high redshift (z = 4.243 +/- 0.001). The strength of the continuum and emission lines suggests that ID 141 is gravitationally lensed. The width (Delta V-FWHM similar to 800 km s(-1)) and asymmetric profiles of the CO and carbon lines indicate orbital motion in a disk or a merger. The properties derived for ID 141 are compatible with an ultraluminous (L-FIR similar to (8.5 +/- 0.3) x 10(13) mu(-1)(L) L-circle dot, where mu L is the amplification factor), dense (n approximate to 10(4) cm(-3)), and warm (T-kin approximate to 40 K) starburst galaxy, with an estimated star formation rate of (0.7-1.7) x 10(4) mu(-1)(L) M-circle dot yr(-1). The carbon emission lines indicate a dense (n approximate to 10(4) cm(-3)) photon-dominated region, illuminated by a far-UV radiation field a few thousand times more intense than that in our Galaxy. In conclusion, the physical properties of the high-z galaxy ID 141 are remarkably similar to those of local ultraluminous infrared galaxies. C1 [Cox, P.; Krips, M.; Neri, R.] IRAM, F-38406 St Martin Dheres, France. [Omont, A.; Gavazzi, R.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France. [Omont, A.; Gavazzi, R.] CNRS, UMR7095, F-75014 Paris, France. [Guesten, R.; Menten, K. M.; Wyrowski, F.; Weiss, A.] MPIfR, D-53121 Bonn, Germany. [Beelen, A.] Univ Paris 11, IAS, F-91405 Orsay, France. [Gurwell, M. A.; Blundell, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dannerbauer, H.] CEA DSM CNRS Univ Paris Diderot, DAPNIA Serv Astrophys, CEA Saclay, AIM, F-91191 Gif Sur Yvette, France. [Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Michallowski, M.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Negrello, M.; Hopwood, R.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Aretxaga, I.; Hughes, D. H.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. [Auld, R.; Dariush, A.; Eales, S. A.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Buttiglione, S.; Jarvis, M.; de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Buttiglione, S.; Jarvis, M.; de Zotti, G.] SISSA, I-34136 Trieste, Italy. [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran. [Dunne, L.; Dye, S.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Swinbank, A. M.] Univ Durham, Inst Computat Cosmol, Durham DH1 3EE, England. [Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [Valtchanov, I.] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Cox, P (reprint author), IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France. EM cox@iram.fr RI Baes, Maarten/I-6985-2013; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017; OI Baes, Maarten/0000-0002-3930-2757; Ivison, R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X; Dye, Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X FU NASA through JPL; Centre National de la Recherche Scientifique (France); Max-Planck Gesellschaft (Germany); Instituto Geografico Nacional (Spain); Smithsonian Institution; Academia Sinica; CONACyT [39953-F]; [ASI-INAF I009/10/0] FX The results described in this paper are based on observations obtained with Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. US participants in H-ATLAS acknowledge support from NASA through a contract from JPL. The ground-based follow-up observations were obtained at the following facilities. The 30 m telescope and the PdBI of IRAM that is funded by the Centre National de la Recherche Scientifique (France), the Max-Planck Gesellschaft (Germany), and the Instituto Geografico Nacional (Spain). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. The Submillimeter Array (SMA) is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Part of this study was supported by financial contribution from the agreement ASI-INAF I009/10/0 and by CONACyT grant 39953-F. NR 69 TC 92 Z9 92 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 OCT 20 PY 2011 VL 740 IS 2 AR 63 DI 10.1088/0004-637X/740/2/63 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844QR UT WOS:000296762900013 ER PT J AU Gupta, RR D'Andrea, CB Sako, M Conroy, C Smith, M Bassett, B Frieman, JA Garnavich, PM Jha, SW Kessler, R Lampeitl, H Marriner, J Nichol, RC Schneider, DP AF Gupta, Ravi R. D'Andrea, Chris B. Sako, Masao Conroy, Charlie Smith, Mathew Bassett, Bruce Frieman, Joshua A. Garnavich, Peter M. Jha, Saurabh W. Kessler, Richard Lampeitl, Hubert Marriner, John Nichol, Robert C. Schneider, Donald P. TI IMPROVED CONSTRAINTS ON TYPE Ia SUPERNOVA HOST GALAXY PROPERTIES USING MULTI-WAVELENGTH PHOTOMETRY AND THEIR CORRELATIONS WITH SUPERNOVA PROPERTIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: photometry; supernovae: general ID DIGITAL SKY SURVEY; STELLAR POPULATION SYNTHESIS; INITIAL MASS FUNCTION; LIGHT-CURVE SHAPES; STAR-FORMATION; HUBBLE DIAGRAM; LOCAL UNIVERSE; SN-IA; METALLICITY; LUMINOSITY AB We improve estimates of the stellar mass and mass-weighted average age of Type Ia supernova (SN Ia) host galaxies by combining UV and near-IR photometry with optical photometry in our analysis. Using 206 SNe Ia drawn from the full three-year Sloan Digital Sky Survey (SDSS-II) Supernova Survey (median redshift of z approximate to 0.2) and multi-wavelength host-galaxy photometry from SDSS, the Galaxy Evolution Explorer, and the United Kingdom Infrared Telescope Infrared Deep Sky Survey, we present evidence of a correlation (1.9 sigma confidence level) between the residuals of SNe Ia about the best-fit Hubble relation and the mass-weighted average age of their host galaxies. The trend is such that older galaxies host SNe Ia that are brighter than average after standard light-curve corrections are made. We also confirm, at the 3.0 sigma level, the trend seen by previous studies that more massive galaxies often host brighter SNe Ia after light-curve correction. C1 [Gupta, Ravi R.; D'Andrea, Chris B.; Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, Mathew] Univ Cape Town, Dept Math & Appl Math, ACGC, ZA-7701 Rondebosch, South Africa. [Bassett, Bruce] S African Astron Observ, ZA-7935 Observatory, South Africa. [Bassett, Bruce] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Rondebosch, South Africa. [Bassett, Bruce] African Inst Math Sci, Cape Town, South Africa. [Frieman, Joshua A.; Kessler, Richard] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Frieman, Joshua A.; Marriner, John] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Kessler, Richard] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Lampeitl, Hubert; Nichol, Robert C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Gupta, RR (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. EM ravgupta@physics.upenn.edu OI Bassett, Bruce/0000-0001-7700-1069 FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration [NNX09AC75G]; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; Cambridge University; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPA); Max-Planck-Institute for Astrophysics (MPIA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; W. M. Keck Foundation FX Funding for the creation and distribution of the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, Cambridge University, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPA), the Max-Planck-Institute for Astrophysics (MPIA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.; This work is based in part on observations made at the following telescopes. The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario Low-Resolution Spectrograph is named for Mike Marcario of High Lonesome Optics, who fabricated several optical elements for the instrument but died before its completion; it is a joint project of the Hobby-Eberly Telescope partnership and the Instituto de Astronomia de la Universidad Nacional Autonomade Mexico. The Apache Point Observatory 3.5 m telescope is owned and operated by the Astrophysical Research Consortium. We thank the observatory director, Suzanne Hawley, and site manager, Bruce Gillespie, for their support of this project. The Subaru Telescope is operated by the National Astronomical Observatory of Japan. The William Herschel Telescope is operated by the Isaac Newton Group on the island of La Palma in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration; the observatory was made possible by the generous financial support of the W. M. Keck Foundation.; This work was funded by the NASA ADP Program NNX09AC75G. NR 61 TC 46 Z9 47 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 OCT 20 PY 2011 VL 740 IS 2 AR 92 DI 10.1088/0004-637X/740/2/92 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844QR UT WOS:000296762900042 ER PT J AU Hajian, A Acquaviva, V Ade, PAR Aguirre, P Amiri, M Appel, JW Barrientos, LF Battistelli, ES Bond, JR Brown, B Burger, B Chervenak, J Das, S Devlin, MJ Dicker, SR Doriese, WB Dunkley, J Dunner, R Essinger-Hileman, T Fisher, RP Fowler, JW Halpern, M Hasselfield, M Hernandez-Monteagudo, C Hilton, GC Hilton, M Hincks, AD Hlozek, R Huffenberger, KM Hughes, DH Hughes, JP Infante, L Irwin, KD Juin, JB Kaul, M Klein, J Kosowsky, A Lau, JM Limon, M Lin, YT Lupton, RH Marriage, TA Marsden, D Mauskopf, P Menanteau, F Moodley, K Moseley, H Netterfield, CB Niemack, MD Nolta, MR Page, LA Parker, L Partridge, B Reid, B Sehgal, N Sherwin, BD Sievers, J Spergel, DN Staggs, ST Swetz, DS Switzer, ER Thornton, R Trac, H Tucker, C Warne, R Wollack, E Zhao, Y AF Hajian, Amir Acquaviva, Viviana Ade, Peter A. R. Aguirre, Paula Amiri, Mandana Appel, John William Felipe Barrientos, L. Battistelli, Elia S. Bond, John R. Brown, Ben Burger, Bryce Chervenak, Jay Das, Sudeep Devlin, Mark J. Dicker, Simon R. Doriese, W. Bertrand Dunkley, Joanna Duenner, Rolando Essinger-Hileman, Thomas Fisher, Ryan P. Fowler, Joseph W. Halpern, Mark Hasselfield, Matthew Hernandez-Monteagudo, Carlos Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hlozek, Renee Huffenberger, Kevin M. Hughes, David H. Hughes, John P. Infante, Leopoldo Irwin, Kent D. Baptiste Juin, Jean Kaul, Madhuri Klein, Jeff Kosowsky, Arthur Lau, Judy M. Limon, Michele Lin, Yen-Ting Lupton, Robert H. Marriage, Tobias A. Marsden, Danica Mauskopf, Phil Menanteau, Felipe Moodley, Kavilan Moseley, Harvey Netterfield, Calvin B. Niemack, Michael D. Nolta, Michael R. Page, Lyman A. Parker, Lucas Partridge, Bruce Reid, Beth Sehgal, Neelima Sherwin, Blake D. Sievers, Jon Spergel, David N. Staggs, Suzanne T. Swetz, Daniel S. Switzer, Eric R. Thornton, Robert Trac, Hy Tucker, Carole Warne, Ryan Wollack, Ed Zhao, Yue TI THE ATACAMA COSMOLOGY TELESCOPE: CALIBRATION WITH THE WILKINSON MICROWAVE ANISOTROPY PROBE USING CROSS-CORRELATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; methods: data analysis; methods: statistical ID BACKGROUND POWER SPECTRUM; WMAP OBSERVATIONS; 148 GHZ; GALAXY CLUSTERS; BEAM PROFILES; ARRAY CAMERA; 2003 FLIGHT; TEMPERATURE; MAPS; POLARIZATION AB We present a new calibration method based on cross-correlations with the Wilkinson Microwave Anisotropy Probe (WMAP) and apply it to data from the Atacama Cosmology Telescope (ACT). ACT's observing strategy and map-making procedure allows an unbiased reconstruction of the modes in the maps over a wide range of multipoles. By directly matching the ACT maps to WMAP observations in the multipole range of 400 < l < 1000, we determine the absolute calibration with an uncertainty of 2% in temperature. The precise measurement of the calibration error directly impacts the uncertainties in the cosmological parameters estimated from the ACT power spectra. We also present a combined map based on ACT and WMAP data that has a high signal-to-noise ratio over a wide range of multipoles. C1 [Hajian, Amir; Bond, John R.; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Hajian, Amir; Acquaviva, Viviana; Das, Sudeep; Dunkley, Joanna; Lin, Yen-Ting; Lupton, Robert H.; Marriage, Tobias A.; Spergel, David N.; Trac, Hy] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hajian, Amir; Appel, John William; Das, Sudeep; Dunkley, Joanna; Duenner, Rolando; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hincks, Adam D.; Lau, Judy M.; Limon, Michele; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.; Zhao, Yue] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Acquaviva, Viviana; Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aguirre, Paula; Felipe Barrientos, L.; Infante, Leopoldo; Baptiste Juin, Jean; Lin, Yen-Ting] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Chervenak, Jay; Moseley, Harvey; Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Devlin, Mark J.; Dicker, Simon R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Marsden, Danica; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Doriese, W. Bertrand; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Cape Town, South Africa. [Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Hughes, David H.] INAOE, Puebla, Mexico. [Lau, Judy M.; Sehgal, Neelima] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Limon, Michele] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. [Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Reid, Beth] Univ Barcelona, ICREA, Barcelona 08028, Spain. [Reid, Beth] Univ Barcelona, ICC, Barcelona 08028, Spain. [Switzer, Eric R.] Kavli Inst Cosmol Phys, Lab Astrophys & Space Res, Chicago, IL 60637 USA. [Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. [Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hajian, A (reprint author), Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Huffenberger, Kevin/0000-0001-7109-0099; Sievers, Jonathan/0000-0001-6903-5074; Limon, Michele/0000-0002-5900-2698 FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731, PIRE-0507768]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation under the auspices of Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; NASA [NNX08AH30G]; Natural Science and Engineering Research Council of Canada (NSERC); NSF [AST-0546035, AST-0606975]; FONDAP Centro de Astrofisica; CONICYT; MECESUP; Fundacion Andes; NSF Physics Frontier Center [PHY-0114422]; South African National Research Foundation (NRF); Meraka Institute; South African Square Kilometer Array (SKA) Project; RCUK; Berkeley Center for Cosmological Physics; World Premier International Research Center Initiative, MEXT, Japan; U.S. Department of Energy [DE-AC3-76SF00515]; NASA Office of Space Science FX This work was supported by the U.S. National Science Foundation through awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731, and PIRE-0507768. Funding was also provided by Princeton University and the University of Pennsylvania. The PIRE program made possible exchanges between Chile, South Africa, Spain, and the United States that enabled this research program. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund-Research Excellence; and the University of Toronto.; A. H., V. A., S. D., and T. A. M. were supported through NASA grant NNX08AH30G. A. D. H. received additional support from a Natural Science and Engineering Research Council of Canada (NSERC) PGS-D scholarship. A. K. and B. P. were partially supported through NSF AST-0546035 and AST-0606975, respectively, for work on ACT. L. I. acknowledge partial support from FONDAP Centro de Astrofisica. R. D. was supported by CONICYT, MECESUP, and Fundacion Andes. E. R. S. acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. K.M., M. Hilton, and R. W. received financial support from the South African National Research Foundation (NRF), the Meraka Institute via funding for the South African Centre for High Performance Computing (CHPC), and the South African Square Kilometer Array (SKA) Project. J.D. received support from an RCUK Fellowship. R. H. received funding from the Rhodes Trust. We thank Norm Jarosik for useful discussions and his contributions. S.D. acknowledges support from the Berkeley Center for Cosmological Physics. Y.-T.L. acknowledges support from the World Premier International Research Center Initiative, MEXT, Japan. N.S. is supported by the U.S. Department of Energy contract to SLAC No. DE-AC3-76SF00515. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. The data will be made public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web site (http://www.physics.princeton.edu/act/). Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. NR 55 TC 24 Z9 24 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2011 VL 740 IS 2 AR 86 DI 10.1088/0004-637X/740/2/86 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844QR UT WOS:000296762900036 ER PT J AU Leier, D Ferreras, I Saha, P Falco, EE AF Leier, Dominik Ferreras, Ignacio Saha, Prasenjit Falco, Emilio E. TI RESOLVING THE BARYON-FRACTION PROFILE IN LENSING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: elliptical and lenticular, cD; galaxies: stellar content; gravitational lensing: strong ID INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; DARK-MATTER HALOES; TO-LIGHT RATIOS; LINE-OF-SIGHT; GRAVITATIONAL LENS; ELLIPTIC GALAXIES; STELLAR MASS; BLACK-HOLES; FUNDAMENTAL PLANE AB The study of the distribution of baryonic matter within dark halos enriches our understanding of galaxy formation. We show the radial dependence of stellar baryon-fraction curves derived for 21 lensing galaxies from the CfA-Arizona Space Telescope LEns Survey (CASTLES) by means of stellar population synthesis and pixel-based mass reconstruction. The sample covers a stellar mass range of M-s similar or equal to 2 x 10(9)-3 x 10(11) M-circle dot (solar masses) which corresponds to a total enclosed mass range of M-L similar or equal to 7 x 10(9)-3 x 10(12) M-circle dot on radial scales from 0.25 R-e to 5 R-e (effective radii). By examining the M-s and M-L dependence on radial distance to the center of each galaxy, we find that there are pairs of lenses on small to intermediate mass scales which approach at large radii the same values for their enclosed total mass but exhibit very different stellar masses and stellar baryon fractions. This peculiar behavior subsides for the most massive lensing galaxies. All the baryon-fraction profiles show that the dark matter halo overtakes the stellar content between 1.5 and 2.5R(e). At 3R(e) most of the stellar component is enclosed. We find evidence for a stellar baryon fraction steadily declining over the full mass range. Furthermore, we shed light on the Fundamental Plane puzzle by showing that the slope of the M-L(< R)-to-M-s ( T10) BROWN DWARF IN A BINARY SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: general; brown dwarfs; infrared: stars; techniques: high angular resolution ID STAR ADAPTIVE OPTICS; EXTRASOLAR GIANT PLANETS; EXOPLANET HOST STAR; INFRARED FILTER SET; MID-T DWARFS; DYNAMICAL MASS; EVOLUTIONARY MODELS; SPECTRAL CLASSIFICATION; PHYSICAL-PROPERTIES; L/T TRANSITION AB We have identified CFBDSIR J1458+1013 as a 0 ''.11 (2.6 AU) physical binary using Keck laser guide star adaptive optics imaging and have measured a distance of 23.1 +/- 2.4 pc to the system based on near-IR parallax data from the Canada-France-Hawaii Telescope. The integrated-light near-IR spectrum indicates a spectral type of T9.5, and model atmospheres suggest a slightly higher temperature and surface gravity than the T10 dwarf UGPS J0722-05. Thus, CFBDSIR J1458+1013AB is the coolest brown dwarf binary found to date. Its secondary component has an absolute H-band magnitude that is 1.9 +/- 0.3 mag fainter than UGPS J0722-05, giving an inferred spectral type of >T10. The secondary's bolometric luminosity of similar to 2 x 10(-7) L-circle dot makes it the least luminous known brown dwarf by a factor of 4-5. By comparing to evolutionary models and T9-T10 objects, we estimate a temperature of 370 +/- 40 K and a mass of 6-15 M-Jup for CFBDSIR J1458+1013B. At such extremes, atmospheric models predict the onset of novel photospheric processes, namely, the appearance of water clouds and the removal of strong alkali lines, but their impact on the emergent spectrum is highly uncertain. Our photometry shows that strong CH4 absorption persists in the H band, the J - K color is bluer than the latest known T dwarfs but not as blue as predicted by current models, and the J - H color delineates a possible inflection in the blueward trend for the latest T dwarfs. Given its low luminosity, atypical colors, and cold temperature, CFBDSIR J1458+1013B is a promising candidate for the hypothesized Y spectral class. However, regardless of its ultimate classification, CFBDSIR J1458+1013AB provides a new benchmark for measuring the properties of brown dwarfs and gas-giant planets, testing substellar models, and constraining the low-mass limit for star formation. C1 [Liu, Michael C.; Bowler, Brendan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Delorme, Philippe; Forveille, Thierry; Delfosse, Xavier] UJF Grenoble 1, CNRS, IPAG, UMR 5274,INSU, F-38041 Grenoble, France. [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Albert, Loic] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Artigau, Etienne] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Artigau, Etienne] Univ Montreal, Observ Mt Megant, Montreal, PQ H3C 3J7, Canada. [Reyle, Celine] Univ Franche Comte, Observ Besancon, Inst Utinam, CNRS,UMR 6213, F-25010 Besancon, France. RP Liu, MC (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM mliu@ifa.hawaii.edu FU W. M. Keck Foundation; NSF [AST-0507833, AST-0909222]; NASA [HF-51271.01-A, NAS 5-26555]; Space Telescope Science Institute FX Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.; It is a pleasure to thank Jim Lyke, Gary Punawai, Cynthia Wilburn, and the Keck Observatory staff for assistance with the LGS AO observing and the staffs of CFHT and VLT for carrying out the queue imaging and spectroscopy. We thank Sandy Leggett and Didier Saumon for making published results readily available and thank Kathleen Brandt for assistance while this paper was being written. Our research has employed the 2MASS data products; NASA's Astrophysical Data System; the SIMBAD database operated at CDS, Strasbourg, France; and the SpeX Prism Spectral Libraries maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism. M.C.L., T.J.D., and B.P.B. acknowledge support for this work from NSF grants AST-0507833 and AST-0909222. Support for this work to T.J.D. was partially provided by NASA through Hubble Fellowship grant HF-51271.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Finally, the authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 77 TC 47 Z9 47 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2011 VL 740 IS 2 AR 108 DI 10.1088/0004-637X/740/2/108 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844QR UT WOS:000296762900058 ER PT J AU Lynch, BJ Reinard, AA Mulligan, T Reeves, KK Rakowski, CE Allred, JC Li, Y Laming, JM MacNeice, PJ Linker, JA AF Lynch, B. J. Reinard, A. A. Mulligan, T. Reeves, K. K. Rakowski, C. E. Allred, J. C. Li, Y. Laming, J. M. MacNeice, P. J. Linker, J. A. TI IONIC COMPOSITION STRUCTURE OF CORONAL MASS EJECTIONS IN AXISYMMETRIC MAGNETOHYDRODYNAMIC MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; magnetohydrodynamics (MHD); Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: heliosphere ID INTER-PLANETARY SHOCK; SLOW SOLAR-WIND; CHARGE STATES; ELECTRON-TEMPERATURE; COMPOSITION SPECTROMETER; MAGNETIC-STRUCTURE; FLUX CANCELLATION; SOHO OBSERVATIONS; IONIZATION STATE; 1 AU AB We present the ionic charge state composition structure derived from axisymmetric MHD simulations of coronal mass ejections (CMEs), initiated via the flux-cancellation and magnetic breakout mechanisms. The flux-cancellation CME simulation is run on the Magnetohydrodynamics-on-A-Sphere code developed at Predictive Sciences, Inc., and the magnetic breakout CME simulation is run on ARC7 developed at NASA GSFC. Both MHD codes include field-aligned thermal conduction, radiative losses, and coronal heating terms which make the energy equations sufficient to calculate reasonable temperatures associated with the steady-state solar wind and model the eruptive flare heating during CME formation and eruption. We systematically track a grid of Lagrangian plasma parcels through the simulation data and calculate the coronal density and temperature history of the plasma in and around the CME magnetic flux ropes. The simulation data are then used to integrate the continuity equations for the ionic charge states of several heavy ion species under the assumption that they act as passive tracers in the MHD flow. We construct two-dimensional spatial distributions of commonly measured ionic charge state ratios in carbon, oxygen, silicon, and iron that are typically elevated in interplanetary coronal mass ejection (ICME) plasma. We find that the slower CME eruption has relatively enhanced ionic charge states and the faster CME eruption shows basically no enhancement in charge states-which is the opposite trend to what is seen in the in situ ICME observations. The primary cause of the difference in the ionic charge states in the two simulations is not due to the different CME initiation mechanisms per se. Rather, the difference lies in their respective implementation of the coronal heating which governs the steady-state solar wind, density and temperature profiles, the duration of the connectivity of the CME to the eruptive flare current sheet, and the contribution of the flare-heated plasma associated with the reconnection jet outflow into the ejecta. Despite the limitations inherent in the first attempt at this novel procedure, the simulation results provide strong evidence in support of the conclusion that enhanced heavy ion charge states within CMEs are a direct consequence of flare heating in the low corona. We also discuss future improvements through combining numerical CME modeling with quantitative ionic charge state calculations. C1 [Lynch, B. J.; Li, Y.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Reinard, A. A.] NOAA Space Weather Predict Ctr, Boulder, CO 80505 USA. [Mulligan, T.] Aerosp Corp, Dept Space Sci, Los Angeles, CA 90009 USA. [Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rakowski, C. E.; Laming, J. M.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Allred, J. C.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [MacNeice, P. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Linker, J. A.] Predict Sci Inc, San Diego, CA 92121 USA. RP Lynch, BJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM blynch@ssl.berkeley.edu; alysha.reinard@noaa.gov; tamitha.mulligan@aero.org; kreeves@cfa.harvard.edu; c.rakowski@nrl.navy.mil; jca32@drexel.edu; yanli@ssl.berkeley.edu; j.laming@nrl.navy.mil; peter.j.macneice@nasa.gov; linkerj@presci.com RI Lynch, Benjamin/B-1300-2013; Reinard, Alysha/H-7808-2013; Reeves, Katharine/P-9163-2014; Allred, Joel/C-9550-2012; MacNeice, Peter/F-5587-2012 OI Reinard, Alysha/0000-0003-0304-2989; Lynch, Benjamin/0000-0001-6886-855X; FU NASA [HTP NNX08AI56G NNX11AJ65G, NASA HGI NNX08AJ04G, SRT NNX08AH54G, HGI NNG08EK62I, TRT NNG04GN00G]; Office of Naval Research; NSF [SHINE ATM0752257] FX B.J.L. thanks S. K. Antiochos and G. H. Fisher for helpful discussion during the preparation of the manuscript. This collaborative research was made possible with support from NASA's Heliosphysics Theory, Guest Investigator, Living With a Star, and SR&T programs, as well as the NSF SHINE program, the Office of Naval Research, and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center). B.J.L. and Y.L. acknowledge support from NASA HTP NNX08AI56G NNX11AJ65G, and NASA HGI NNX08AJ04G; A.A.R. and T.L.M. acknowledge NASA SR&T NNX08AH54G; C.E.R. and J.M.L. acknowledge NASA HGI NNG08EK62I and basic research funds of the Office of Naval Research; K.K.R. acknowledges NSF SHINE ATM0752257; and J.C.A. and P.J.M. acknowledge support from NASA TR&T NNG04GN00G. NR 86 TC 11 Z9 11 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2011 VL 740 IS 2 AR 112 DI 10.1088/0004-637X/740/2/112 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844QR UT WOS:000296762900062 ER PT J AU Ma, CJ McNamara, BR Nulsen, PEJ Schaffer, R Vikhlinin, A AF Ma, C-J McNamara, B. R. Nulsen, P. E. J. Schaffer, R. Vikhlinin, A. TI AVERAGE HEATING RATE OF HOT ATMOSPHERES IN DISTANT CLUSTERS BY RADIO ACTIVE GALACTIC NUCLEUS: EVIDENCE FOR CONTINUOUS ACTIVE GALACTIC NUCLEUS HEATING SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium; quasars: general; radio continuum: galaxies; X-rays: galaxies: clusters ID X-RAY CAVITIES; DEEP CHANDRA OBSERVATION; GALAXY CLUSTERS; COOLING FLOWS; INTRACLUSTER MEDIUM; LUMINOSITY FUNCTION; THERMAL CONDUCTION; GASEOUS ATMOSPHERE; REDSHIFT EVOLUTION; NEARBY CLUSTERS AB We examine atmospheric heating by radio active galactic nuclei (AGNs) in distant X-ray clusters by cross correlating clusters selected from the 400 Square Degree (400SD) X-ray Cluster survey with radio sources in the NRAO VLA Sky Survey. Roughly 30% of the clusters show radio emission above a flux threshold of 3 mJy within a projected radius of 250 kpc. The radio emission is presumably associated with the brightest cluster galaxy. The mechanical jet power for each radio source was determined using scaling relations between radio power and cavity (mechanical) power determined for nearby clusters, groups, and galaxies with hot atmospheres containing X-ray cavities. The average jet power of central radio AGNs is approximately 2 x 10(44) erg s(-1). We find no significant correlation between radio power, and hence mechanical jet power, and the X-ray luminosities of clusters in the redshift range 0.1-0.6. This implies that the mechanical heating rate per particle is higher in lower mass, lower X-ray luminosity clusters. The jet power averaged over the sample corresponds to an atmospheric heating of approximately 0.2 keV per particle within R-500. Assuming the current AGN heating rate does not evolve but remains constant to redshifts of 2, the heating rate per particle would rise by a factor of two. We find that the energy injected from radio AGNs contribute substantially to the excess entropy in hot atmospheres needed to break self-similarity in cluster scaling relations. The detection frequency of radio AGNs is inconsistent with the presence of strong cooling flows in 400SD clusters, but does not exclude weak cooling flows. It is unclear whether central AGNs in 400SD clusters are maintained by feedback at the base of a cooling flow. Atmospheric heating by radio AGNs may retard the development of strong cooling flows at early epochs. C1 [Ma, C-J; McNamara, B. R.; Schaffer, R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Ma, C-J; McNamara, B. R.; Nulsen, P. E. J.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Vikhlinin, A.] Space Res Inst IKI, Moscow, Russia. RP Ma, CJ (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada. OI Nulsen, Paul/0000-0003-0297-4493 FU Chandra Large Project [G09-0140X]; NASA [NAS8-03060] FX C.-J.M. and B.R.M. are supported by Chandra Large Project Grant G09-0140X. B.R.M. acknowledges generous support from the Natural Sciences and Engineering Research Council of Canada. P.E.J.N. was supported by NASA grant NAS8-03060. NR 87 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2011 VL 740 IS 2 AR 51 DI 10.1088/0004-637X/740/2/51 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844QR UT WOS:000296762900001 ER PT J AU Oberg, KI Boogert, ACA Pontoppidan, KM van den Broek, S van Dishoeck, EF Bottinelli, S Blake, GA Evans, NJ AF Oeberg, Karin I. Boogert, A. C. Adwin Pontoppidan, Klaus M. van den Broek, Saskia van Dishoeck, Ewine F. Bottinelli, Sandrine Blake, Geoffrey A. Evans, Neal J., II TI THE SPITZER ICE LEGACY: ICE EVOLUTION FROM CORES TO PROTOSTARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; infrared: ISM; ISM: abundances; ISM: lines and bands; ISM: molecules; molecular processes; stars: formation ID YOUNG STELLAR OBJECTS; LOW-MASS STARS; INTERSTELLAR GRAIN MANTLES; VLT SPECTROSCOPIC SURVEY; MU-M; MOLECULAR CLOUDS; DENSE CLOUDS; INFRARED OBSERVATIONS; GALACTIC-CENTER; UPPER LIMITS AB Ices regulate much of the chemistry during star formation and account for up to 80% of the available oxygen and carbon. In this paper, we use the Spitzer c2d Legacy ice survey, complimented with data sets on ices in cloud cores and high-mass protostars, to determine standard ice abundances and to present a coherent picture of the evolution of ices during low-and high-mass star formation. The median ice composition H2O:CO:CO2:CH3OH:NH3:CH4:XCN is 100:29:29:3:5:5:0.3 and 100:13:13:4:5:2:0.6 toward low-and high-mass protostars, respectively, and 100:31:38:4:-:-:- in cloud cores. In the low-mass sample, the ice abundances with respect to H2O of CH4, NH3, and the component of CO2 mixed with H2O typically vary by <25%, indicative of co-formation with H2O. In contrast, some CO and CO2 ice components, XCN, and CH3OH vary by factors 2-10 between the lower and upper quartile. The XCN band correlates with CO, consistent with its OCN- identification. The origin(s) of the different levels of ice abundance variations are constrained by comparing ice inventories toward different types of protostars and background stars, through ice mapping, analysis of cloud-to-cloud variations, and ice (anti-)correlations. Based on the analysis, the first ice formation phase is driven by hydrogenation of atoms, which results in an H2O-dominated ice. At later prestellar times, CO freezes out and variations in CO freezeout levels and the subsequent CO-based chemistry can explain most of the observed ice abundance variations. The last important ice evolution stage is thermal and UV processing around protostars, resulting in CO desorption, ice segregation, and the formation of complex organic molecules. The distribution of cometary ice abundances is consistent with the idea that most cometary ices have a protostellar origin. C1 [Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. [Boogert, A. C. Adwin] CALTECH, IPAC, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Pontoppidan, Klaus M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Oeberg, Karin I.; van den Broek, Saskia; van Dishoeck, Ewine F.; Bottinelli, Sandrine] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bottinelli, Sandrine] CNRS, UMR 5187, CESR, F-31028 Toulouse 4, France. [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. FU NASA [NAS 5-26555, 1224608, 1230779, 1407]; Space Telescope Science Institute; Netherlands Organization for Scientific Research (NWO); W. M. Keck Foundation FX Support for K.I.O. is provided by NASA through a Hubble Fellowship grant awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Astrochemistry in Leiden is supported by SPINOZA grant of the Netherlands Organization for Scientific Research (NWO). Support for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through contracts 1224608 and 1230779 issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration, and was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize the cultural role and reverence that the summit of Mauna Kea has within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We acknowledge helpful comments from an anonymous referee. NR 82 TC 164 Z9 164 U1 3 U2 35 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2011 VL 740 IS 2 AR 109 DI 10.1088/0004-637X/740/2/109 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844QR UT WOS:000296762900059 ER PT J AU Qi, CH D'Alessio, P Oberg, KI Wilner, DJ Hughes, AM Andrews, SM Ayala, S AF Qi, Chunhua D'Alessio, Paola Oeberg, Karin I. Wilner, David J. Hughes, A. Meredith Andrews, Sean M. Ayala, Sandra TI RESOLVING THE CO SNOW LINE IN THE DISK AROUND HD 163296 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: abundances; planetary systems; protoplanetary disks; radio lines: stars; stars: individual (HD 163296); techniques: interferometric ID HERBIG AE/BE STARS; MAIN-SEQUENCE STARS; T TAURI STARS; PROTOPLANETARY DISKS; ACCRETION DISKS; CIRCUMSTELLAR DISKS; YOUNG OBJECTS; AE STARS; DM-TAU; SUBMILLIMETER ARRAY AB We report Submillimeter Array observations of CO (J = 2-1, 3-2, and 6-5) and its isotopologues ((CO)-C-13 J = 2-1, (CO)-O-18 J = 2-1, and (CO)-O-17 J = 3-2) in the disk around the Herbig Ae star HD 163296 at similar to 2 '' (250 AU) resolution, and interpret these data in the framework of a model that constrains the radial and vertical location of the line emission regions. First, we develop a physically self-consistent accretion disk model with an exponentially tapered edge that matches the spectral energy distribution and spatially resolved millimeter dust continuum emission. Then, we refine the vertical structure of the model using wide range of excitation conditions sampled by the CO lines, in particular the rarely observed J = 6-5 transition. By fitting (CO)-C-13 data in this structure, we further constrain the vertical distribution of CO to lie between a lower boundary below which CO freezes out onto dust grains (T less than or similar to 19 K) and an upper boundary above which CO can be photodissociated (the hydrogen column density from the disk surface is less than or similar to 10(21) cm(-2)). The freezeout at 19 K leads to a significant drop in the gas-phase CO column density beyond a radius of similar to 155 AU, a "CO snow line" that we directly resolve. By fitting the abundances of all CO isotopologues, we derive isotopic ratios of C-12/C-13, O-16/O-18, and O-18/O-17 that are consistent with quiescent interstellar gas-phase values. This detailed model of the HD 163296 disk demonstrates the potential of a staged, parametric technique for constructing unified gas and dust structure models and constraining the distribution of molecular abundances using resolved multi-transition, multi-isotope observations. C1 [Qi, Chunhua; Oeberg, Karin I.; Wilner, David J.; Hughes, A. Meredith; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [D'Alessio, Paola; Ayala, Sandra] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Hughes, A. Meredith] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Qi, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. EM cqi@cfa.harvard.edu; p.dalessio@crya.unam.mx; koberg@cfa.harvard.edu; dwilner@cfa.harvard.edu; mhughes@cfa.harvard.edu; sandrews@cfa.harvard.edu; sayala2001@gmail.com FU NASA [NAS 5-26555]; Space Telescope Science Institute; Miller Institute for Basic Research in Science; NASA Origins of Solar Systems [NNX11AK63G] FX We thank Edwin Bergin, Eugene Chiang, and Jeremy Drake for beneficial conversations, and a referee for constructive comments on the paper. Support for K.I.O. is provided by NASA through a Hubble Fellowship grant awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Support for A. M. H. is provided by a fellowship from the Miller Institute for Basic Research in Science. We acknowledge NASA Origins of Solar Systems grant No. NNX11AK63G. NR 77 TC 50 Z9 50 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2011 VL 740 IS 2 AR 84 DI 10.1088/0004-637X/740/2/84 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844QR UT WOS:000296762900034 ER PT J AU Zhu, L Zhao, JH Wright, MCH AF Zhu, Lei Zhao, Jun-Hui Wright, M. C. H. TI OUTFLOW, INFALL, AND PROTOSTARS IN THE STAR-FORMING CORE W3-SE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: jets and outflows; ISM: kinematics and dynamics; ISM: molecules; radio lines: ISM ID NGC-1333 IRAS-4; PROTOSTELLAR INFALL; NGC 1333-IRAS2; CANDIDATES; ENVELOPE; MOTIONS; SYSTEM; MASS; DISK; JET AB We report new results on outflow and infall in the star-forming cores W3-SE SMA-1 and SMA-2 based on analysis of similar to 2 ''.5 resolution observations of the molecular lines HCN(3-2), HCO+(3-2), N2H+(3-2), and CH3OH(5(2,3)-4(1,3)) with the Submillimeter Array (SMA). A high-velocity bipolar outflow originating from the protostellar core SMA-1 was observed in the HCN(3-2) line, with a projected outflow axis at a position angle of 48 degrees. The detection of the outflow is confirmed from other molecular lines. An inverse P-Cygni profile in the HCN(3-2) line toward SMA-1 suggests that at least one of the double cores accretes matter from the molecular core. A filamentary structure in the molecular gas surrounds SMA-1 and SMA-2. Based on the SMA observations, our analysis suggests that the double pre-stellar cores SMA-1 and SMA-2 result from fragmentation in the collapsing massive molecular core W3-SE, and it is likely that they are forming intermediate-to high-mass stars which will be new members of a star cluster in the W3-SE region. C1 [Zhu, Lei] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Zhu, Lei; Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wright, M. C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Zhu, L (reprint author), Peking Univ, Dept Astron, Beijing 100871, Peoples R China. EM lzhu@cfa.harvard.edu; jzhao@cfa.harvard.edu FU SAO; NSFC [10873019]; Smithsonian Institution; Academia Sinica FX We are grateful to the staff of the SMA and CARMA telescopes who make these observations possible. We also thank the anonymous referee for his detailed comments and questions which have significantly improved the presentation of these results. We thank Wu Y. for the suggestions and discussions in forming the idea of this paper, selecting the research targets and providing the single-dish data of the targets, suggesting the suitable molecular probes, as well as the discussions in the analysis of the results. L.Z. is supported by the SAO pre-doctoral program during this research, and he is also supported by Grant 10873019 at NSFC when staying at Peking University.; The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 25 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2011 VL 740 IS 2 AR 114 DI 10.1088/0004-637X/740/2/114 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844QR UT WOS:000296762900064 ER PT J AU Foster, AR Testa, P AF Foster, Adam R. Testa, Paola TI Fe IX CALCULATIONS FOR THE SOLAR DYNAMICS OBSERVATORY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE atomic data; Sun: UV radiation ID ATOMIC DATA; EMISSION-LINES; HYDROGEN; ELEMENTS; RATES; IONS AB New calculations of the energy levels, radiative transition rates, and collisional excitation rates of Fe IX have been carried out using the Flexible Atomic Code, paying close attention to experimentally identified levels and extending existing calculations to higher energy levels. For lower levels, R-matrix collisional excitation rates from earlier work have been used. Significant emission is predicted by these calculations in the 5f-3d transitions, which will impact analysis of Solar Dynamics Observatory Atmospheric Imaging Assembly observations using the 94 angstrom filter. C1 [Foster, Adam R.; Testa, Paola] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Foster, AR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM afoster@cfa.harvard.edu FU NASA ADP [NNX09AC71G]; Lockheed-Martin [SP02H1701R] FX A.R.F. acknowledges funding from NASA ADP grant NNX09AC71G. P. T. has been supported by contract SP02H1701R from Lockheed-Martin to SAO. NR 22 TC 16 Z9 16 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2011 VL 740 IS 2 AR L52 DI 10.1088/2041-8205/740/2/L52 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844MZ UT WOS:000296752600021 ER PT J AU Liu, MC Deacon, NR Magnier, EA Dupuy, TJ Aller, KM Bowler, BP Redstone, J Goldman, B Burgett, WS Chambers, KC Hodapp, KW Kaiser, N Kudritzki, RP Morgan, JS Price, PA Tonry, JL Wainscoat, RJ AF Liu, Michael C. Deacon, Niall R. Magnier, Eugene A. Dupuy, Trent J. Aller, Kimberly M. Bowler, Brendan P. Redstone, Joshua Goldman, Bertrand Burgett, W. S. Chambers, K. C. Hodapp, K. W. Kaiser, N. Kudritzki, R-P Morgan, J. S. Price, P. A. Tonry, J. L. Wainscoat, R. J. TI A SEARCH FOR HIGH PROPER MOTION T DWARFS WITH Pan-STARRS1+2MASS+WISE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE brown dwarfs; proper motions; solar neighborhood; surveys ID INFRARED SURVEY EXPLORER; COOL BROWN DWARF; SKY SURVEY; 2MASS; TRANSITION; BENCHMARK; BINARIES; WISE; MASS; SPECTROGRAPH AB We have searched approximate to 8200 deg(2) for high proper motion (approximate to 0.'' 5-2.'' 7 year(-1)) T dwarfs by combining first-epoch data from the Pan-STARRS1 (PS1) 3 pi Survey, the Two Micron All Sky Survey (2MASS) All-Sky Point Source Catalog, and the WISE Preliminary Data Release. We identified two high proper motion objects with the very red (W1 - W2) colors characteristic of T dwarfs, one being the known T7.5 dwarf GJ 570D. Near-IR spectroscopy of the other object (PSO J043.5395+02.3995 equivalent to WISEP J025409.45+022359.1) reveals a spectral type of T8, leading to a photometric distance of 7.2 +/- 0.7 pc. The 2.'' 56 year(-1) proper motion of PSO J043.5+02 is the second highest among field T dwarfs, corresponding to a tangential velocity of 87 +/- 8 km s(-1). According to the Besan, con galaxy model, this velocity indicates that its galactic membership is probably in the thin disk, with the thick disk an unlikely possibility. Such membership is in accord with the near-IR spectrum, which points to a surface gravity (age) and metallicity typical of the field population. We combine 2MASS, Sloan Digital Sky Survey, WISE, and PS1 astrometry to derive a preliminary parallax of 171 +/- 45 mas (5.8(-1.2)(+2.0) pc), the first such measurement using PS1 data. The proximity and brightness of PSO J043.5+02 will facilitate future characterization of its atmosphere, variability, multiplicity, distance, and kinematics. The modest number of candidates from our search suggests that the immediate (similar to 10 pc) solar neighborhood does not contain a large reservoir of undiscovered T dwarfs earlier than about T8. C1 [Liu, Michael C.; Deacon, Niall R.; Magnier, Eugene A.; Aller, Kimberly M.; Bowler, Brendan P.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kaiser, N.; Kudritzki, R-P; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Redstone, Joshua] Facebook, Palo Alto, CA 94304 USA. [Goldman, Bertrand] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Liu, MC (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. OI Chambers, Kenneth /0000-0001-6965-7789 FU National Aeronautics and Space Administration [NNX-08AE38A]; NSF [AST-0507833, AST09-09222, AST-0709460]; AFRL [FA9451-06-2-0338]; DFG [Sonderforschungsbereich 881] FX Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program.; The Pan-STARRS1 surveys have been made possible by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the institutions of the Pan-STARRS1 Science Consortium (http://www.ps1sc.org), and NASA. Our research has employed the WISE, SDSS-III, and 2MASS data products; NASA's Astrophysical Data System; the SIMBAD database; the M, L, and T dwarf compendium housed at DwarfArchives.org; and the SpeX Prism Spectral Libraries. This research was supported by NSF Grants AST-0507833 and AST09-09222 (awarded to MCL), AST-0709460 (awarded to EAM), AFRL Cooperative Agreement FA9451-06-2-0338, and DFG-Sonderforschungsbereich 881 "The Milky Way." Finally, the authors wish to recognize the very significant cultural role that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to conduct observations from this mountain. NR 46 TC 26 Z9 26 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2011 VL 740 IS 2 AR L32 DI 10.1088/2041-8205/740/2/L32 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 844MZ UT WOS:000296752600001 ER PT J AU Hill, EM Davis, JL Tamisiea, ME Ponte, RM Vinogradova, NT AF Hill, Emma M. Davis, James L. Tamisiea, Mark E. Ponte, Rui M. Vinogradova, Nadya T. TI Using a spatially realistic load model to assess impacts of Alaskan glacier ice loss on sea level SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID GRAVITY-FIELD; MASS CHANGES; OCEAN MASS; AGE EARTH; GRACE; SURFACE; TRENDS; UPLIFT; FLUX AB Ice loss from glaciers results in highly nonuniform patterns of sea level change due to the effects of self-attraction and loading. To quantify these spatial effects, it is necessary to obtain an ice load model that is both spatially realistic and regionally complete. We demonstrate a technique to produce such a model for the Alaskan glaciers by combining mass balance rates from a Gravity Recovery and Climate Experiment (GRACE) mascon solution with realistic glacier geometries. This load model can be used to solve the "sea level equation" to determine gravitationally self-consistent sea level and gravity rates. The model predicts a significant drop in relative sea level in the near field of the glaciers, with coastal rates of around -9 mm/yr (compared to a global average rise of 0.2 mm/yr) and significant differences to those predicted by a coarser model. The magnitude and sensitivity of these near-field rates imply that the near-field tide gauge records could contain significant information about the spatial distribution of ice loss. Comparison of model gravity rates with an independently produced, spherical harmonic, GRACE solution verifies that our technique can successfully capture the mass changes estimated in the mascon solution within our higher-resolution model. Finally, we use our ice load model to examine the possibility of detecting the effects of ice loss in estimates of ocean bottom pressure (OBP) from GRACE. We use the model to simulate the effects of GRACE signal leakage and show that the OBP signal from leakage has a similar pattern to, but larger amplitude than, the sea level "fingerprint" expected from ice loss. C1 [Hill, Emma M.; Davis, James L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hill, Emma M.] Nanyang Technol Univ, Earth Observ Singapore, Singapore 639798, Singapore. [Davis, James L.] Columbia Univ, Lamont Doherty Earth Observ, Earth Inst, Palisades, NY 10964 USA. [Tamisiea, Mark E.] Natl Oceanog Ctr, Liverpool L3 5DA, Merseyside, England. [Ponte, Rui M.; Vinogradova, Nadya T.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. RP Hill, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ehill@ntu.edu.sg; jdavis@ldeo.columbia.edu; mtam@noc.ac.uk; rponte@aer.com; nvinogra@aer.com RI Davis, James/D-8766-2013; Hill, Emma/B-7037-2011; OI Davis, James/0000-0003-3057-477X; Hill, Emma/0000-0003-0231-5818; Ponte, Rui/0000-0001-7206-6461 FU NASA [NNX08AJ79G, NNX07AM77G, NNX11AC14G, NNX11AB97G]; Earth Observatory of Singapore (EOS) [32]; NERC FX This work was supported by NASA grants NNX08AJ79G, NNX07AM77G, NNX11AC14G, and NNX11AB97G. E. M. H. was partially supported by the Earth Observatory of Singapore (EOS number 32). M. E. T. was funded by NERC as part of Oceans 2025. We are grateful to Scott Luthcke for providing the bounding box coordinates for his published mascon results and to Katherine Quinn for useful discussions. Our routine uses the Generic Mapping Tools [Wessel and Smith, 1998]. The manuscript was significantly improved by reviews from Chris Larsen, two anonymous reviewers, and the Associate Editor. NR 37 TC 4 Z9 4 U1 2 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD OCT 20 PY 2011 VL 116 AR B10407 DI 10.1029/2011JB008339 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 836XK UT WOS:000296151500002 ER PT J AU Munroe, TA Tyler, J Tunnicliffe, V AF Munroe, Thomas A. Tyler, Jennifer Tunnicliffe, Verena TI Description and biological observations on a new species of deepwater symphurine tonguefish (Pleuronectiformes: Cynoglossidae: Symphurus) collected at Volcano-19, Tonga Arc, West Pacific Ocean SO ZOOTAXA LA English DT Article DE taxonomy; deep-sea flatfish; tongue sole; hydrothermal vents; volcanic arcs; seamounts; reversed asymmetry; species description; ocelli AB Symphurus maculopinnis n. sp., described on a single specimen (USNM 398820; 84.4 mm SL), was collected by a remotely operated vehicle (ROV) exploring a hydrothermal vent area located at 561 m on Volcano-19, Tonga Arc, West Pacific (24 degrees 48.439' S, 177 degrees 0.009' W). This new species is distinctive and readily diagnosed from congeners by the following combination of characters: 1-2-2-2-1 pattern of interdigitation of dorsal proximal pterygiophores and neural spines (ID pattern), 14 caudal-fin rays, 3+6 abdominal vertebrae, 49 total vertebrae, 89 scales in a longitudinal row, 92 dorsal-fin rays, 77 anal-fin rays, blunt squarish snout, thick blind-side lips with conspicuous plicae, and conspicuous ocellated (sometimes partially) spots on posterior dorsal and anal fins. Among Symphurus, only S. ocellatus von Bonde, collected at deepwater locations off East Africa, features a similar ID pattern, 14 caudal-fin rays and spots on the posterior dorsal and anal fins. Symphurus maculopinnis differs distinctly from S. ocellatus in its lower and non-overlapping meristic features (49 vs. 54-56 total vertebrae; 92 vs. 97-103 dorsal-fin rays; and 77 vs. 85-89 anal-fin rays), its squarish (vs. pointed) snout, and thick, plicated blind-side lower lip (vs. thin, non-plicated blind-side lower lip). Additional specimens (N= 56) of S. maculopinnis observed and filmed in situ near active venting sites located between ca. 433-561 m on Volcano-19 provide the basis for behavioral and ecological information recorded for the species. Videotapes reveal one individual of S. maculopinnis featuring reversed (dextral) asymmetry from that typical (sinistral) for members of the Cynoglossidae. Specimens with reversed asymmetry are relatively rare in this family and this S. maculopinnis represents only the second known reversed individual among the approximately 42 species of deep-sea (> 200 m) Symphurus. C1 [Munroe, Thomas A.] Smithsonian Inst, Natl Systemat Lab, Natl Marine Fisheries Serv, NOAA,Natl Museum Nat Hist, Washington, DC 20013 USA. [Tyler, Jennifer; Tunnicliffe, Verena] Univ Victoria, Dept Biol, Victoria, BC V8W 3N5, Canada. RP Munroe, TA (reprint author), Smithsonian Inst, Natl Systemat Lab, Natl Marine Fisheries Serv, NOAA,Natl Museum Nat Hist, POB 37012,WC-57,MRC-153, Washington, DC 20013 USA. EM munroet@si.edu; jentyler24@gmail.com; verenat@uvic.ca RI Tunnicliffe, Verena/D-1056-2014 FU NSERC Canada FX L. Willis provided radiographs of the holotype and L. Willis and M. Nizinski provided radiographs of specimens used in the comparisons. J. Clayton and D. Smith assisted with accessioning and cataloguing the holotype. J. Rose compiled the videotape of specimens filmed in situ at Volcano-19 and provided field data associated with the holotype; C. Marzec and M. Benson assisted with publishing and archiving the tonguefish video to the Smithsonian Institution's Ocean Portal website; C. Ames assisted with making video grabs from video tapes. S. Raredon provided photographs of the holotype. Appreciation is extended to curators and collection staff who provided assistance locating specimens, providing catalogue information, or who arranged for loan of specimens used in this study. We acknowledge the field team who collected and filmed this species during the SO192-2 MANGO Expedition, particularly S. K. Juniper and C. Stevens; expedition co-chiefs were U. Schwarz-Schampera and M. Hannington with R/V Sonne and ROV ROPOS. Collection of this specimen was made possible by funding provided to V. Tunnicliffe by NSERC Canada. NR 18 TC 7 Z9 7 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 18 PY 2011 IS 3061 BP 53 EP 66 PG 14 WC Zoology SC Zoology GA 833ZY UT WOS:000295926300003 ER PT J AU Osinski, GR Tornabene, LL Grieve, RAF AF Osinski, Gordon R. Tornabene, Livio L. Grieve, Richard A. F. TI Impact ejecta emplacement on terrestrial planets SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE impact cratering; impact ejecta; Mars; Moon ID CRATERING RECORD; OBLIQUE IMPACTS; LAYERED EJECTA; DEVON ISLAND; MELT ROCKS; RIES; MARS; GERMANY; FLOWS; VENUS AB Impact cratering is one of the most fundamental processes responsible for shaping the surfaces of solid planetary bodies. One of the principal characteristics of impact events is the formation and emplacement of ejecta deposits, an understanding of which is critical for planetary exploration. Current models of ejecta emplacement, however, do not account for several important observations of ejecta deposits on the terrestrial planets, in particular, the presence of more than one layer of ejecta. Furthermore, there is also no universal model for the origin and emplacement of ejecta on different planetary bodies. We present a unifying working hypothesis for the origin and emplacement of ejecta on the terrestrial planets, in which the ejecta are emplaced in a multi-stage process. The generation of the continuous ejecta blanket occurs during the excavation stage of cratering, via the conventional ballistic sedimentation and radial flow model. This is followed by the emplacement of more melt-rich, ground-hugging flows - the "surface melt flow" phase during the terminal stages of crater excavation and the modification stage of crater formation. Minor fallback occurs during the final stages of crater formation. Several factors will affect the final morphology and character of ejecta deposits. The volatile content and cohesiveness of the uppermost target rocks will significantly affect the runout distance of the ballistically emplaced continuous ejecta blanket, with impact angle also influencing the overall geometry of the deposits (e.g., the production of the characteristic butterfly pattern seen in very oblique impacts). Ejecta deposited during the surface melt flow stage is influenced by several factors, most importantly planetary gravity, surface temperature, and the physical properties of the target rocks. Topography and angle of impact play important roles in determining the final distribution of surface melt flow ejecta deposits with respect to the source crater. This working hypothesis of ballistic sedimentation and surface melt flow provides a framework in which observations of ejecta at impact craters can be compared and placed in the context of the respective terrestrial planets. (C) 2011 Elsevier B.V. All rights reserved. C1 [Osinski, Gordon R.; Grieve, Richard A. F.] Univ Western Ontario, Dept Earth Sci Phys & Astron, London, ON N6A 5B7, Canada. [Tornabene, Livio L.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Grieve, Richard A. F.] Nat Resources Canada, Earth Sci Sector, Ottawa, ON K1A 0E8, Canada. RP Osinski, GR (reprint author), Univ Western Ontario, Dept Earth Sci Phys & Astron, 1151 Richmond St, London, ON N6A 5B7, Canada. EM gosinski@uwo.ca FU Natural Sciences and Engineering Research Council of Canada (NSERC); MDA Space Missions; Canadian Space Agency (CSA); CSA Canadian Analogue Research Network (CARN) FX G.R.O. is supported by the Natural Sciences and Engineering Research Council of Canada (NSERC) Industrial Research Chair in Planetary Geology sponsored by MDA Space Missions and the Canadian Space Agency (CSA). Funding from the NSERC Discovery Grant and the CSA Canadian Analogue Research Network (CARN) programs is gratefully acknowledged. Sarah Stewart-Mukhopadhyay and an anonymous reviewer are thanked for their detailed and constructive reviews. NR 99 TC 71 Z9 72 U1 2 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD OCT 15 PY 2011 VL 310 IS 3-4 BP 167 EP 181 DI 10.1016/j.epsl.2011.08.012 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 864XJ UT WOS:000298273500001 ER PT J AU Reeder, LA Erlandson, JM Rick, TC AF Reeder, Leslie A. Erlandson, Jon M. Rick, Torben C. TI Younger Dryas environments and human adaptations on the West Coast of the United States and Baja California SO QUATERNARY INTERNATIONAL LA English DT Article ID LATE QUATERNARY VEGETATION; GULF-OF-CALIFORNIA; SANTA-BARBARA BASIN; SOUTHWESTERN COLUMBIA BASIN; LAST GLACIAL MAXIMUM; SCALE CLIMATE-CHANGE; BATTLE GROUND LAKE; SEA-LEVEL RECORD; NORTH-AMERICA; CURRENT SYSTEM AB On the Pacific Coast of the United States and Baja California, the Younger Dryas was one component of dynamic Late Pleistocene and Holocene environmental changes. Changing climate, sea level rise, and shifting shorelines created ecological challenges for ancient coastal peoples and daunting challenges for archaeologists searching for early coastal sites. This paper reviews the evidence for ecological change in this 'West Coast' region, including shoreline changes that may have submerged or destroyed archaeological sites from this time period. Examining the regional record of human occupation dating to the Younger Dryas, well-dated coastal sites are limited to California's Northern Channel Islands and Isla Cedros off Baja California. A small number of fluted points found in coastal areas may also date to the Younger Dryas, but their context and chronology is not well defined. Review of the implications of these two data sets considers whether the early but discontinuous Younger Dryas archaeological record from the West Coast might result from a migration of maritime peoples from Northeast Asia into the Americas. (C) 2011 Elsevier Ltd and INQUA. All rights reserved. C1 [Reeder, Leslie A.] So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. RP Reeder, LA (reprint author), So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA. EM lreeder@smu.edu OI Erlandson, Jon/0000-0002-4705-4319 NR 155 TC 2 Z9 2 U1 2 U2 22 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 J9 QUATERN INT JI Quat. Int. PD OCT 15 PY 2011 VL 242 IS 2 BP 463 EP 478 DI 10.1016/j.quaint.2011.04.016 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 827NZ UT WOS:000295436500017 ER PT J AU van Breugel, M Ransijn, J Craven, D Bongers, F Hall, JS AF van Breugel, Michiel Ransijn, Johannes Craven, Dylan Bongers, Frans Hall, Jefferson S. TI Estimating carbon stock in secondary forests: Decisions and uncertainties associated with allometric biomass models SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Carbon; Tree allometry; Biomass; Secondary succession; Tropical forest ID ABOVEGROUND TREE BIOMASS; TROPICAL RAIN-FOREST; WOOD DENSITY; CLIMATE-CHANGE; FUNCTIONAL-GROUPS; BRAZILIAN AMAZON; LANDSCAPE-SCALE; LAND-USE; DEFORESTATION; EQUATIONS AB Secondary forests are a major terrestrial carbon sink and reliable estimates of their carbon stocks are pivotal for understanding the global carbon balance and initiatives to mitigate CO2 emissions through forest management and reforestation. A common method to quantify carbon stocks in forests is the use of allometric regression models to convert forest inventory data to estimates of aboveground biomass (AGO). The use of allometric models implies decisions on the selection of extant models or the development of a local model, the predictor variables included in the selected model, and the number of trees and species for destructive biomass measurements. We assess uncertainties associated with these decisions using data from 94 secondary forest plots in central Panama and 244 harvested trees belonging to 26 locally abundant species. AGB estimates from species-specific models were used to assess relative errors of estimates from multispecies models. To reduce uncertainty in the estimation of plot AGO, including wood specific gravity (WSG) in the model was more important than the number of trees used for model fitting. However, decreasing the number of trees increased uncertainty of landscape-level AGB estimates substantially, while including WSG had limited effects on the accuracy of the landscape-level estimates. Predictions of stand and landscape AGB varied strongly among models, making model choice an important source of uncertainty. Local models provided more accurate AGB estimates than foreign models, but high variability in carbon stocks across the landscape implies that developing local models is only justified when landscape sampling is sufficiently intensive. (C) 2011 Elsevier B.V. All rights reserved. C1 [van Breugel, Michiel; Ransijn, Johannes; Craven, Dylan; Hall, Jefferson S.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa, Ancon, Panama. [Ransijn, Johannes; Bongers, Frans] Wageningen Univ, Forest Ecol & Forest Management Grp, Ctr Ecosyst Studies, NL-6700 AA Wageningen, Netherlands. [Ransijn, Johannes] Univ Copenhagen, DK-1958 Frederiksberg C, Denmark. [Craven, Dylan] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. RP van Breugel, M (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Av Roosevelt 401, Balboa, Ancon, Panama. EM mvbreugel@gmail.com RI Craven, Dylan/K-2717-2012; Ransijn, Johannes/D-5324-2015; OI Craven, Dylan/0000-0003-3940-833X; Ransijn, Johannes/0000-0003-0416-2210; van Breugel, Michiel/0000-0003-2778-7803 FU HSBC; STRI; ACP; Frank Levinson Family Foundation; Motta Family Foundation; Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) of Panama FX This paper is a scientific contribution to the Agua Salud Project (ASP), collaboration among the Smithsonian Tropical Research Institute, the Panama Canal Authority (ACP) and the National Environmental Authority of Panama (ANAM). The ASP is supported by the HSBC climate partnership, STRI, the ACP, the Frank Levinson Family Foundation and the Motta Family Foundation. This study was supported by an Anonymous Donor and the Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) of Panama. We thank Daniela Weber and Federico Davis for logistical support, Yuriza Guerrero, Johana Balbuena, Miguel Nunez, Guillermo Fernandez, Fernando Garcia, Carlos Diaz, Anabel Rivas, Jenny Calvo, Manuel Valdes and Gregorio Sala for their help in the collection of field data, Christian Salas and two anonymous reviewers for their valuable comments and Joe Wright for providing data on wood specific gravity. Finally, JR thanks Michele Abene, Adriana Cromer and Gillian Paul for their support and companionship during the field work period. NR 60 TC 66 Z9 67 U1 7 U2 87 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD OCT 15 PY 2011 VL 262 IS 8 BP 1648 EP 1657 DI 10.1016/j.foreco.2011.07.018 PG 10 WC Forestry SC Forestry GA 825QN UT WOS:000295297300034 ER PT J AU Baeza, JA Bolanos, JA Hernandez, JE Lira, C Lopez, R AF Antonio Baeza, J. Bolanos, Juan A. Hernandez, Jesus E. Lira, Carlos Lopez, Regulo TI Monogamy does not last long in Pontonia mexicana, a symbiotic shrimp of the amber pen-shell Pinna carnea from the southeastern Caribbean Sea SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Caridea; Monogamy; Promiscuity; Symbiosis; Venezuela ID CRAB INACHUS-PHALANGIUM; SOCIAL MONOGAMY; SNAPPING SHRIMP; EVOLUTIONARY CONSEQUENCES; HOST CHARACTERISTICS; MATING TACTICS; LIFE-HISTORY; DECAPODA; ANEMONE; DIMORPHISM AB Theory suggests that symbiotic species should be monogamous and form long-lasting heterosexual pairs in/on hosts when inhabiting scarce and small hosts in environments where predation risk away from hosts is high (e.g., tropical subtidal). This prediction was tested with Pontonia mexicana which inhabits the relatively small and scarce amber pen-shell Pinna carnea in the tropical Caribbean. In agreement with theory, P. mexicana were found dwelling as heterosexual pairs in the mantle cavity of pen-shell individuals with more frequency than expected by chance alone. However, additional observations suggested that male-female pairing of P. mexicana does not last long. First, males paired with females that were close to molt and become sexually receptive more frequently than expected by chance alone. In monogamous species in which pairing appears to be long lasting, males occur with females in the same host, independent of the reproductive condition of the female. Second, the body size of paired shrimps was poorly correlated and the relationship between host and shrimp body size was weak. If males and females of P. mexicana were staying within host individuals for long periods of time, a tight correlation between host and shrimp size and between males and females in a pair would have been found. Lastly, sexual dimorphism in terms of cheliped size was evident; males invested considerably more resources to this body structure compared to females. In monogamous species in which pairing appears to be long-term, sexual dimorphism is low or absent given that sexual selection is weak in this mating system. Overall, our data suggests that monogamy in P. mexicana does not last long and that males switch among host individuals in search of receptive females. Manipulative experiments are necessary to understand the conditions favoring short- and long-term monogamy in symbiotic crustaceans. (C) 2011 Elsevier B.V. All rights reserved. C1 [Antonio Baeza, J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23435 USA. [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. [Bolanos, Juan A.; Hernandez, Jesus E.; Lira, Carlos; Lopez, Regulo] Univ Oriente, Nucleo Nueva Esparta, Escuela Ciencias Aplicadas Mar, Grp Invest Carcinol, Isla Margarita, Venezuela. RP Baeza, JA (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23435 USA. EM baezaa@si.edu OI Baeza, Juan Antonio/0000-0002-2573-6773 FU Smithsonian Marine Station (SMS); Smithsonian Tropical Research Institute (STRI) FX JAB (SI) is grateful for the support from a Smithsonian Marine Station (SMS) Postdoctoral Fellowship and a Smithsonian Tropical Research Institute (STRI) Postdoctoral Fellowship. We appreciate the help from several students attending the course "Behavior of Marine Invertebrates" held during 2008 at the Escuela de Ciencias Aplicadas del Mar, Nucleo Nueva Esparta, Universidad de Oriente, for their help during the different steps of sampling, measurement, and data analysis. Dr. M. Soledad Fuentes at NOAA, Milford, CT gently provided access to statistical software and support. This is contribution number 859 of the Smithsonian Marine Station at Fort Pierce. [SS] NR 46 TC 16 Z9 18 U1 0 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD OCT 15 PY 2011 VL 407 IS 1 BP 41 EP 47 DI 10.1016/j.jembe.2011.07.011 PG 7 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 825RG UT WOS:000295299200007 ER PT J AU Clark, MA Joo, B Kennedy, AD Silva, PJ AF Clark, M. A. Joo, Balint Kennedy, A. D. Silva, P. J. TI Improving dynamical lattice QCD simulations through integrator tuning using Poisson brackets and a force-gradient integrator SO PHYSICAL REVIEW D LA English DT Article AB We show how the integrators used for the molecular dynamics step of the Hybrid Monte Carlo algorithm can be further improved. These integrators not only approximately conserve some Hamiltonian H but conserve exactly a nearby shadow Hamiltonian (H) over tilde. This property allows for a new tuning method of the molecular dynamics integrator and also allows for a new class of integrators (force-gradient integrators) which is expected to reduce significantly the computational cost of future large-scale gauge field ensemble generation. C1 [Silva, P. J.] Univ Coimbra, Ctr Fis Computac, P-3000 Coimbra, Portugal. [Clark, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Joo, Balint] Jefferson Lab, Newport News, VA 23606 USA. [Kennedy, A. D.] Univ Edinburgh, Tait Inst, Edinburgh EH9 3JZ, Midlothian, Scotland. [Kennedy, A. D.] Univ Edinburgh, SUPA, Sch Phys & Astron, Edinburgh EH9 3JZ, Midlothian, Scotland. RP Silva, PJ (reprint author), Univ Coimbra, Ctr Fis Computac, P-3000 Coimbra, Portugal. EM psilva@teor.fis.uc.pt RI Silva, Paulo/H-8270-2013 OI Silva, Paulo/0000-0002-3658-2319 FU FCT [SFRH/BPD/40998/2007, PTDC/FIS/100968/2008]; U.S. DOE [DE-FC02-06ER41440, DE-FC02-06ER41449, DE-AC05-060R23177]; NSF [PHY-0835713, OCI-1060067] FX P.J.S. acknowledges support from FCT via Grant No. SFRH/BPD/40998/2007 and Project No. PTDC/FIS/100968/2008. B.J. acknowledges funding through U.S. DOE Grants No. DE-FC02-06ER41440, No. DE-FC02-06ER41449 (SciDAC), and No. DE-AC05-060R23177 under which Jefferson Science Associates LLC manages and operates the Jefferson Lab. M.A.C. acknowledges support from the NSF via PHY-0835713 and OCI-1060067. The numerical results have been obtained using the Chroma library [10]. Simulations have been carried out in Iridis (University of Southampton) and Centaurus (University of Coimbra) High Performance Computing facilities. NR 10 TC 3 Z9 3 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD OCT 14 PY 2011 VL 84 IS 7 AR 071502 DI 10.1103/PhysRevD.84.071502 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 841UX UT WOS:000296541500002 ER PT J AU Trefzger, C Menotti, C Capogrosso-Sansone, B Lewenstein, M AF Trefzger, C. Menotti, C. Capogrosso-Sansone, B. Lewenstein, M. TI Ultracold dipolar gases in optical lattices SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID BOSE-EINSTEIN CONDENSATE; MONTE-CARLO; ATOMS; MOLECULES; BOSONS; TRANSITION; SUPERFLUID; COLLAPSE; STATE; MODEL AB This tutorial is a theoretical work, in which we study the physics of ultra-cold dipolar bosonic gases in optical lattices. Such gases consist of bosonic atoms or molecules that interact via dipolar forces, and that are cooled below the quantum degeneracy temperature, typically in the nK range. When such a degenerate quantum gas is loaded into an optical lattice produced by standing waves of laser light, new kinds of physical phenomena occur. Then, these systems realize extended Hubbard-type models, and can be brought to a strongly correlated regime. The physical properties of such gases, dominated by the long-range, anisotropic dipole-dipole interactions, are discussed using the mean-field approximations and exact quantum Monte Carlo techniques (the worm algorithm). C1 [Trefzger, C.; Menotti, C.; Lewenstein, M.] ICFO Inst Ciencies Foton, Barcelona 08860, Spain. [Menotti, C.] Univ Trent, INO CNR BEC Ctr, I-38123 Povo, Italy. [Menotti, C.] Univ Trent, Dipartimento Fis, I-38123 Povo, Italy. [Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Lewenstein, M.] ICREA, Barcelona 08010, Spain. RP Trefzger, C (reprint author), ICFO Inst Ciencies Foton, Mediterranean Technol Pk, Barcelona 08860, Spain. EM christian.trefzger@lkb.ens.fr RI Lewenstein, Maciej/I-1337-2014 OI Lewenstein, Maciej/0000-0002-0210-7800 FU Spanish MEC [FIS2008-00784]; EU; ERC FX This tutorial was supported by Spanish MEC(FIS2008-00784, QOIT), EU projects AQUTE and NAMEQUAM, and ERC grant QUAGATUA. ML acknowledges also Alexander von Humboldt Stiftung and Hamburg Prize for Theoretical Physics. It is a great pleasure for us to thank everybody in the Quantum Optics Theory Group of ICFO for interesting discussions. We are especially grateful to K Rzazewski, who invited us to write this paper. CT thanks C Menotti, and M Lewenstein for their constant support, and patience, they showed him during these years, the result of which is not only in this work. CT thanks B Capogrosso-Sansone and G Pupillo for their guide in the quantum Monte Carlo work, and Peter Zoller for the kind hospitality in Innsbruck. This work was partially written at the Indian Association for the Cultivation of Science, in Calcutta, while CT was visiting K Sengupta. The warm hospitality he showed him is unique, and CT thanks him together with everybody in the Theoretical Physics Department. NR 87 TC 55 Z9 55 U1 2 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD OCT 14 PY 2011 VL 44 IS 19 AR 193001 DI 10.1088/0953-4075/44/19/193001 PG 31 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 824QO UT WOS:000295217300005 ER PT J AU Plaisance, L Caley, MJ Brainard, RE Knowlton, N AF Plaisance, Laetitia Caley, M. Julian Brainard, Russell E. Knowlton, Nancy TI The Diversity of Coral Reefs: What Are We Missing? SO PLOS ONE LA English DT Article ID BIOLOGICAL IDENTIFICATIONS; BIODIVERSITY HOTSPOTS; MARINE BIODIVERSITY; SPECIES RICHNESS; EXTINCTION RISK; CLIMATE-CHANGE; DNA BARCODES; OCEAN; INVERTEBRATES; CONSERVATION AB Tropical reefs shelter one quarter to one third of all marine species but one third of the coral species that construct reefs are now at risk of extinction. Because traditional methods for assessing reef diversity are extremely time consuming, taxonomic expertise for many groups is lacking, and marine organisms are thought to be less vulnerable to extinction, most discussions of reef conservation focus on maintenance of ecosystem services rather than biodiversity loss. In this study involving the three major oceans with reef growth, we provide new biodiversity estimates based on quantitative sampling and DNA barcoding. We focus on crustaceans, which are the second most diverse group of marine metazoans. We show exceptionally high numbers of crustacean species associated with coral reefs relative to sampling effort (525 species from a combined, globally distributed sample area of 6.3 m(2)). The high prevalence of rare species (38% encountered only once), the low level of spatial overlap (81% found in only one locality) and the biogeographic patterns of diversity detected (Indo-West Pacific > Central Pacific > Caribbean) are consistent with results from traditional survey methods, making this approach a reliable and efficient method for assessing and monitoring biodiversity. The finding of such large numbers of species in a small total area suggests that coral reef diversity is seriously under-detected using traditional survey methods, and by implication, underestimated. C1 [Plaisance, Laetitia; Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Plaisance, Laetitia; Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. [Caley, M. Julian] Australian Inst Marine Sci, Townsville, Qld 4810, Australia. [Brainard, Russell E.] Natl Ocean & Atmospher Adm Fisheries, Pacific Islands Fisheries Sci Ctr, Coral Reef Ecosyst Div, Honolulu, HI USA. RP Plaisance, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM plaisancel@si.edu FU Alfred P. Sloan Foundation; Census of Marine Life; Census of Coral Reefs; BHP Billiton (Australia) FX This work was supported by the Alfred P. Sloan Foundation, Census of Marine Life, Census of Coral Reefs, and BHP Billiton (Australia). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 30 TC 34 Z9 35 U1 4 U2 61 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 13 PY 2011 VL 6 IS 10 AR e25026 DI 10.1371/journal.pone.0025026 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 834QT UT WOS:000295978600008 PM 22022371 ER PT J AU Churchill, CKC Foighil, DO Strong, EE Gittenberger, A AF Churchill, Celia K. C. Foighil, Diarmaid O. Strong, Ellen E. Gittenberger, Adriaan TI Females floated first in bubble-rafting snails SO CURRENT BIOLOGY LA English DT Letter C1 [Churchill, Celia K. C.; Foighil, Diarmaid O.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Churchill, Celia K. C.; Foighil, Diarmaid O.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Strong, Ellen E.] Smithsonian Inst, Washington, DC 20013 USA. [Gittenberger, Adriaan] Netherlands Ctr Biodivers Naturalis, NL-2300 RA Leiden, Netherlands. [Gittenberger, Adriaan] Leiden Univ, Inst Biol, NL-2300 RA Leiden, Netherlands. [Gittenberger, Adriaan] Leiden BioSci Pk, GiMaRIS, NL-2333 CA Leiden, Netherlands. RP Churchill, CKC (reprint author), Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. EM celia.churchill@gmail.com NR 10 TC 5 Z9 5 U1 0 U2 11 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 J9 CURR BIOL JI Curr. Biol. PD OCT 11 PY 2011 VL 21 IS 19 BP R802 EP R803 DI 10.1016/j.cub.2011.08.011 PG 2 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 833QI UT WOS:000295899600004 PM 21996498 ER PT J AU Hughes, AM Wilner, DJ Andrews, SM Williams, JP Su, KYL Murray-Clay, RA Qi, CH AF Hughes, A. Meredith Wilner, David J. Andrews, Sean M. Williams, Jonathan P. Su, Kate Y. L. Murray-Clay, Ruth A. Qi, Chunhua TI RESOLVED SUBMILLIMETER OBSERVATIONS OF THE HR 8799 AND HD 107146 DEBRIS DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; planet-disk interactions; stars: individual (HD 107146, HR 8799) ID SOLAR-TYPE STARS; PLANETARY SYSTEM; KUIPER-BELT; VEGA-LIKE; DUST; EVOLUTION; MASS; PHOTOMETRY; MORPHOLOGY; STABILITY AB We present 880 mu m Submillimeter Array observations of the debris disks around the young solar analog HD 107146 and the multiple-planet host star HR 8799, at an angular resolution of 3 '' and 6 '', respectively. We spatially resolve the inner edge of the disk around HR 8799 for the first time. While the data are not sensitive enough (with rms noise of 1 mJy) to constrain the system geometry, we demonstrate that a model by Su et al. based on the spectral energy distribution (SED) with an inner radius of 150 AU predicts the spatially resolved data well. Furthermore, by modeling simultaneously the SED and visibilities, we demonstrate that the dust is distributed in a broad (of order 100 AU) annulus rather than a narrow ring. We also model the observed SED and visibilities for the HD 107146 debris disk and generate a model of the dust emission that extends in a broad band between 50 and 170 AU from the star. We perform an a posteriori comparison with existing 1.3 mm CARMA observations and demonstrate that a smooth, axisymmetric model reproduces all of the available millimeter-wavelength data well. C1 [Hughes, A. Meredith] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wilner, David J.; Andrews, Sean M.; Murray-Clay, Ruth A.; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Su, Kate Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Hughes, AM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM mhughes@astro.berkeley.edu OI Williams, Jonathan/0000-0001-5058-695X; Su, Kate/0000-0002-3532-5580 FU Miller Institute for Basic Research in Science FX The authors are grateful to Stuartt Corder and John Carpenter for sharing their HD 107146 CARMA data. We also thank Eugene Chiang for constructive comments on the paper. A.M.H. is supported by a fellowship from the Miller Institute for Basic Research in Science. NR 56 TC 37 Z9 37 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2011 VL 740 IS 1 AR 38 DI 10.1088/0004-637X/740/1/38 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 825FL UT WOS:000295256500038 ER PT J AU Kratter, KM Murray-Clay, RA AF Kratter, Kaitlin M. Murray-Clay, Ruth A. TI FRAGMENT PRODUCTION AND SURVIVAL IN IRRADIATED DISKS: A COMPREHENSIVE COOLING CRITERION SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; planetary systems; protoplanetary disks ID GRAVITATING ACCRETION DISCS; GIANT PLANET FORMATION; PROTOSTELLAR DISKS; STAR-FORMATION; LOW-MASS; PROTOPLANETARY DISCS; EPISODIC ACCRETION; LAYERED ACCRETION; INSTABILITY; STABILITY AB Accretion disks that become gravitationally unstable can fragment into stellar or substellar companions. The formation and survival of these fragments depends on the precarious balance between self-gravity, internal pressure, tidal shearing, and rotation. Disk fragmentation depends on two key factors: (1) whether the disk can get to the fragmentation boundary of Q = 1 and (2) whether fragments can survive for many orbital periods. Previous work suggests that to reach Q = 1, and have fragments survive, a disk must cool on an orbital timescale. Here we show that disks heated primarily by external irradiation always satisfy the standard cooling time criterion. Thus, even though irradiation heats disks and makes them more stable in general, once they reach the fragmentation boundary, they fragment more easily. We derive a new cooling criterion that determines fragment survival and calculate a pressure-modified Hill radius, which sets the maximum size of pressure-supported objects in a Keplerian disk. We conclude that fragmentation in protostellar disks might occur at slightly smaller radii than previously thought and recommend tests for future simulations that will better predict the outcome of fragmentation in real disks. C1 [Kratter, Kaitlin M.; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kratter, KM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM kkratter@cfa.harvard.edu FU Institute for Theory and Computation through the Harvard College Observatory FX We thank the referee for detailed comments that improved this work. We also acknowledge Phil Armitage, Charles Gammie, Chris Matzner, and Ken Rice for useful conversations and for comments on an early version of this manuscript. K. M. K. is supported by an Institute for Theory and Computation Postdoctoral Fellowship through the Harvard College Observatory. NR 44 TC 33 Z9 33 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2011 VL 740 IS 1 AR 1 DI 10.1088/0004-637X/740/1/1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 825FL UT WOS:000295256500001 ER PT J AU Luo, B Brandt, WN Xue, YQ Alexander, DM Brusa, M Bauer, FE Comastri, A Fabian, AC Gilli, R Lehmer, BD Rafferty, DA Schneider, DP Vignali, C AF Luo, B. Brandt, W. N. Xue, Y. Q. Alexander, D. M. Brusa, M. Bauer, F. E. Comastri, A. Fabian, A. C. Gilli, R. Lehmer, B. D. Rafferty, D. A. Schneider, D. P. Vignali, C. TI REVEALING A POPULATION OF HEAVILY OBSCURED ACTIVE GALACTIC NUCLEI AT z approximate to 0.5-1 IN THE CHANDRA DEEP FIELD-SOUTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; galaxies: active; galaxies: photometry; galaxies: starburst; infrared: galaxies; X-rays: galaxies ID STAR-FORMATION RATE; ULTRALUMINOUS INFRARED GALAXIES; COMPTON-THICK AGN; X-RAY-EMISSION; POINT-SOURCE CATALOGS; MS SOURCE CATALOGS; PHOTOMETRIC REDSHIFTS; FORMING GALAXIES; NEARBY GALAXIES; STELLAR-MASS AB Heavily obscured (NH greater than or similar to 3 x 10(23) cm(-2)) active galactic nuclei (AGNs) not detected even in the deepest X-ray surveys are often considered to be comparably numerous to the unobscured and moderately obscured AGNs. Such sources are required to fit the cosmic X-ray background (XRB) emission in the 10-30 keV band. We identify a numerically significant population of heavily obscured AGNs at z approximate to 0.5-1 in the Chandra Deep Field-South (CDF-S) and Extended Chandra Deep Field-South by selecting 242 X-ray undetected objects with infrared-based star-formation rates (SFRs) substantially higher (a factor of 3.2 or more) than their SFRs determined from the UV after correcting for dust extinction. An X-ray stacking analysis of 23 candidates in the central CDF-S region using the 4 Ms Chandra data reveals a hard X-ray signal with an effective power-law photon index of Gamma = 0.6(-0.4)(+ 0.3), indicating a significant contribution from obscured AGNs. Based on Monte Carlo simulations, we conclude that 74% +/- 25% of the selected galaxies host obscured AGNs, within which approximate to 95% are heavily obscured and approximate to 80% are Compton-thick (CT; N-H > 1.5 x 10(24) cm(-2)). The heavily obscured objects in our sample are of moderate intrinsic X-ray luminosity (approximate to(0.9-4) x 10(42) erg s(-1) in the 2-10 keV band). The space density of the CT AGNs is (1.6 +/- 0.5) x 10(-4) Mpc(-3). The z approximate to 0.5-1 CT objects studied here are expected to contribute approximate to 1% of the total XRB flux in the 10-30 keV band, and they account for approximate to 5%-15% of the emission in this energy band expected from all CT AGNs according to population-synthesis models. In the 6-8 keV band, the stacked signal of the 23 heavily obscured candidates accounts for <5% of the unresolved XRB flux, while the unresolved approximate to 25% of the XRB in this band can probably be explained by a stacking analysis of the X-ray undetected optical galaxies in the CDF-S (a 2.5 sigma stacked signal). We discuss prospects to identify such heavily obscured objects using future hard X-ray observatories. C1 [Luo, B.; Brandt, W. N.; Xue, Y. Q.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Luo, B.; Brandt, W. N.; Xue, Y. Q.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Luo, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Brusa, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Comastri, A.; Gilli, R.] INAF Osservatorio Astron Bologna, Bologna, Italy. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Lehmer, B. D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rafferty, D. A.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Vignali, C.] Univ Bologna, Dipartimento Astron, Bologna, Italy. RP Luo, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RI Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Vignali, Cristian/0000-0002-8853-9611; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Alexander, David/0000-0002-5896-6313 FU CXC [SP1-12007A, G09-0134A]; NASA [NNX10AC99G]; Science and Technology Facilities Council; ASI/INAF [I/009/10/0] FX We acknowledge financial support from CXC grant SP1-12007A (B.L., W.N.B., Y.Q.X.), CXC grant G09-0134A (B. L., W.N.B., Y.Q.X.), NASA ADP grant NNX10AC99G (W.N.B.), the Science and Technology Facilities Council (D.M.A.), and ASI/INAF grant I/009/10/0 (A.C., C.V., R.G.). We are grateful to T. Yaqoob and K. D. Murphy for providing support for the MYTORUS model and making available the data for our desired half-opening angle. We thank A. T. Steffen for helpful discussions. We also thank the referee for carefully reviewing the manuscript and providing helpful comments that improved this work. NR 126 TC 28 Z9 28 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2011 VL 740 IS 1 AR 37 DI 10.1088/0004-637X/740/1/37 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 825FL UT WOS:000295256500037 ER PT J AU Oberg, KI van der Marel, N Kristensen, LE van Dishoeck, EF AF Oeberg, Karin I. van der Marel, Nienke Kristensen, Lars E. van Dishoeck, Ewine F. TI COMPLEX MOLECULES TOWARD LOW-MASS PROTOSTARS: THE SERPENS CORE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; astrochemistry; ISM: abundances; ISM: molecules ID STAR-FORMING REGIONS; ORGANIC-MOLECULES; IRAS 16293-2422; HOT CORINOS; CHEMISTRY; IRAS-16293-2422; ICES; PHOTODESORPTION; OUTFLOW; L1157 AB Gas-phase complex organic molecules are commonly detected toward high-mass protostellar hot cores. Detections toward low-mass protostars and outflows are comparatively rare, and a larger sample is the key to investigate how the chemistry responds to its environment. Guided by the prediction that complex organic molecules form in CH3OH-rich ices and thermally or non-thermally evaporate with CH3OH, we have identified three sight lines in the Serpens core-SMM1, SMM4, and SMM4-W-which are likely to be rich in complex organics. Using the IRAM 30 m telescope, narrow lines (FWHM of 1-2 km s(-1)) of CH3CHO and CH3OCH3 are detected toward all sources, HCOOCH3 toward SMM1 and SMM4-W, and C2H5OH not at all. Beam-averaged abundances of individual complex organics range between 0.6% and 10% with respect to CH3OH when the CH3OH rotational temperature is applied. The summed complex organic abundances also vary by an order of magnitude, with the richest chemistry toward the most luminous protostar SMM1. The range of abundances compare well with other beam-averaged observations of low-mass sources. Complex organic abundances are of the same order of magnitude toward low-mass protostars and high-mass hot cores, but HCOOCH3 is relatively more important toward low-mass protostars. This is consistent with a sequential ice photochemistry, dominated by CHO-containing products at low temperatures and early times. C1 [Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van der Marel, Nienke; Kristensen, Lars E.; van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, MS 42,60 Garden St, Cambridge, MA 02138 USA. RI Kristensen, Lars/F-4774-2011 OI Kristensen, Lars/0000-0003-1159-3721 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA [NAS 5-26555]; European Community [R113CT 2003 5058187]; Netherlands Organization for Scientific Research (NWO) FX Based on observations carried out with the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).; We are grateful to the IRAM staff for their assistance and to an anonymous referee for helpful comments. Support for K.I.O. is provided by NASA through Hubble Fellowship grant awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Astrochemistry in Leiden is supported by a SPINOZA grant of the Netherlands Organization for Scientific Research (NWO). This work has benefited from research funding from the European Community's sixth Framework Programme under RadioNet R113CT 2003 5058187. NR 27 TC 25 Z9 25 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2011 VL 740 IS 1 AR 14 DI 10.1088/0004-637X/740/1/14 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 825FL UT WOS:000295256500014 ER PT J AU Winebarger, AR Schmelz, JT Warren, HP Saar, SH Kashyap, VL AF Winebarger, Amy R. Schmelz, Joan T. Warren, Harry P. Saar, Steve H. Kashyap, Vinay L. TI USING A DIFFERENTIAL EMISSION MEASURE AND DENSITY MEASUREMENTS IN AN ACTIVE REGION CORE TO TEST A STEADY HEATING MODEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona ID X-RAY TELESCOPE; ULTRAVIOLET IMAGING SPECTROMETER; SOLAR-B SATELLITE; CORONAL LOOPS; TEMPERATURE DISTRIBUTION; SOHO EIT; HINODE; MOSS; TRACE; MISSION AB The frequency of heating events in the corona is an important constraint on the coronal heating mechanisms. Observations indicate that the intensities and velocities measured in active region cores are effectively steady, suggesting that heating events occur rapidly enough to keep high-temperature active region loops close to equilibrium. In this paper, we couple observations of active region (AR) 10955 made with the X-Ray Telescope and the EUV Imaging Spectrometer on board Hinode to test a simple steady heating model. First we calculate the differential emission measure (DEM) of the apex region of the loops in the active region core. We find the DEM to be broad and peaked around 3 MK. We then determine the densities in the corresponding footpoint regions. Using potential field extrapolations to approximate the loop lengths and the density-sensitive line ratios to infer the magnitude of the heating, we build a steady heating model for the active region core and find that we can match the general properties of the observed DEM for the temperature range of 6.3 < log T < 6.7. This model, for the first time, accounts for the base pressure, loop length, and distribution of apex temperatures of the core loops. We find that the density-sensitive spectral line intensities and the bulk of the hot emission in the active region core are consistent with steady heating. We also find, however, that the steady heating model cannot address the emission observed at lower temperatures. This emission may be due to foreground or background structures, or may indicate that the heating in the core is more complicated. Different heating scenarios must be tested to determine if they have the same level of agreement. C1 [Winebarger, Amy R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Schmelz, Joan T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Warren, Harry P.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Saar, Steve H.; Kashyap, Vinay L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA. EM amy.r.winebarger@nasa.gov FU NSF; NASA/SAO FX A.R.W. was supported by an NSF Career grant. Solar physics research at the University of Memphis is supported by a Hinode subcontract from NASA/SAO. A. R. W. thanks Mark Weber for many enlightening conversations on differential emission measures. NR 56 TC 67 Z9 67 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2011 VL 740 IS 1 AR 2 DI 10.1088/0004-637X/740/1/2 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 825FL UT WOS:000295256500002 ER PT J AU Mulcahy, DG Beckstead, TH Sites, JW AF Mulcahy, Daniel G. Beckstead, Thomas H. Sites, Jack W., Jr. TI Molecular Systematics of the Leptodeirini (Colubroidea: Dipsadidae) Revisited: Species-tree Analyses and Multi-locus Data SO COPEIA LA English DT Article ID AMERICAN XENODONTINE SNAKES; GENE-TREE; PHYLOGENETIC ANALYSIS; MAXIMUM-LIKELIHOOD; MITOCHONDRIAL-DNA; COLUBRID SNAKE; DIPSAS-INDICA; SEQUENCES; SERPENTES; LIZARDS AB Cat-eyed snakes (Leptodeira) were thought to be closely related to nightsnakes (Hypsiglena and Pseudoleptodeira) based on morphology and immunological data, which allied these genera with blunt-headed vine snakes (Imantodes) and the Cloud Forest Snake (Cryophis hallbergi). We collected sequence data from six protein-encoding nuclear loci (SLC30A1, ZEB2, FSHR, NTF3, DNAH3, and PNN; 4149 bp) and additional mtDNA data (nad5; 955 bp) added to published cob and nad4 (total 2387 bp mtDNA) from these and other rear-fanged, mildly venomous snakes that prey on vertebrates (frogs and lizards) and from several other dipsadine genera (Dipsas, Sibon, and Atractus) that prey on invertebrates (goo-eaters). We analyzed relationships using concatenation and a coalescent species-tree method. When analyzed separately, using either concatenation or coalescent methods, nuclear data support a different overall topology from the mtDNA data. Like the mtDNA data, the nuclear data support the Leptodeira + Imantodes relationship, but instead place this clade more closely to the goo-eaters, with the nightsnakes as the basal divergence in the group. When the data are combined in concatenation analyses, the more variable mtDNA data appear to overwhelm the nuclear data, but not under the coalescent model. C1 [Mulcahy, Daniel G.] Smithsonian Inst, Museum Support Ctr LAB, Suitland, MD 20746 USA. [Mulcahy, Daniel G.; Beckstead, Thomas H.; Sites, Jack W., Jr.] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA. [Mulcahy, Daniel G.; Beckstead, Thomas H.; Sites, Jack W., Jr.] Brigham Young Univ, Bean Life Sci Museum, Provo, UT 84602 USA. RP Mulcahy, DG (reprint author), Smithsonian Inst, Museum Support Ctr LAB, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM MulcahyD@si.edu; tombeckstead@gmail.com; jack_sites@byu.edu FU BYU; BYU Department of Biology; NSF [EF-0334966] FX This work was funded by a BYU Mentoring Environment Grant (MEG; Office of Research and Creative Activities), the BYU Department of Biology, and by NSF Assembling the Tree of Life-Deep Scaly project (sub-award EF-0334966) to JWS, Jr. W. B. Simison at the California Academy of Sciences allowed extended use of their PhyloCluster. K. de Queiroz provided additional computational resources at the Smithsonian Institution. F. Fontanel la and H. Bracken, both at BYU provided useful discussion and comments on the manuscript. The following institutions and individuals provided tissue loans: KU (W. E. Duellman), LSU (D. Dittman), MVZ (J. McGuire), L. Canseco-Marquez, E. Greenbaum, J. Mendelson, III, T. Papenfuss, and O. Robles-Romero. NR 68 TC 5 Z9 6 U1 1 U2 5 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD OCT 10 PY 2011 IS 3 BP 407 EP 417 DI 10.1643/CH-10-058 PG 11 WC Zoology SC Zoology GA 833BD UT WOS:000295855900008 ER PT J AU Csengeri, T Bontemps, S Schneider, N Motte, F Gueth, F Hora, JL AF Csengeri, T. Bontemps, S. Schneider, N. Motte, F. Gueth, F. Hora, J. L. TI CONVERGENT FLOWS AND LOW-VELOCITY SHOCKS IN DR21(OH) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: kinematics and dynamics; stars: formation ID MOLECULAR CLOUD EVOLUTION; STAR-FORMATION; COMPLEX-MOLECULES; MASER EMISSION; CYGNUS-X; CONTINUUM; CLUSTER; CORE; GAS; FRAGMENTATION AB DR21(OH) is a pc-scale massive, similar to 7000 M-circle dot clump hosting three massive dense cores (MDCs) at an early stage of their evolution. We present a high angular resolution mosaic, covering similar to 70 '' x 100 '', with the IRAM Plateau de Bure Interferometer at 3 mm to trace the dust continuum emission and the N2H+ (J = 1-0) and CH3CN (J = 5-4) molecular emission. The cold, dense gas traced by the compact emission in N2H+ is associated with the three MDCs and shows several velocity components toward each MDC. These velocity components reveal local shears in the velocity fields which are best interpreted as convergent flows. Moreover, we report the detection of weak extended emission from CH3CN at the position of the N2H+ velocity shears. We propose that this extended CH3CN emission is tracing warm gas associated with the low-velocity shocks expected at the location of convergence of the flows where velocity shears are observed. This is the first detection of low-velocity shocks associated with small (subparsec) scale convergent flows which are proposed to be at the origin of the densest structures and of the formation of (high-mass) stars. In addition, we propose that MDCs may be active sites of star formation for more than a crossing time as they continuously receive material from larger scale flows as suggested by the global picture of dynamical, gravity-driven evolution of massive clumps which is favored by the present observations. C1 [Csengeri, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Csengeri, T.; Schneider, N.; Motte, F.] Univ Paris Diderot, CNRS, CEA Saclay, Lab AIM Paris Saclay,CEA INSU,IRFU SAp, F-91191 Gif Sur Yvette, France. [Bontemps, S.] Univ Bordeaux 1, CNRS, OASU LAB UMR5804, F-33270 Floirac, France. [Gueth, F.] IRAM, F-38406 St Martin Dheres, France. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Csengeri, T (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM ctimea@mpifr-bonn.mpg.de FU FP6 Marie-Curie Research Training Network Constellation: the origin of stellar masses [MRTN-CT-2006-035890]; ANR (Agence Nationale pour la Recherche) [ANR-08-BLAN-0241]; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX T. Csengeri acknowledges support from the FP6 Marie-Curie Research Training Network Constellation: the origin of stellar masses (MRTN-CT-2006-035890). This work was also supported by the ANR (Agence Nationale pour la Recherche) project PROBeS, number ANR-08-BLAN-0241.; IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). NR 34 TC 34 Z9 34 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 OCT 10 PY 2011 VL 740 IS 1 AR L5 DI 10.1088/2041-8205/740/1/L5 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 824OH UT WOS:000295210900005 ER PT J AU McIntosh, SW Kiefer, KK Leamon, RJ Kasper, JC Stevens, ML AF McIntosh, Scott W. Kiefer, Kandace K. Leamon, Robert J. Kasper, Justin C. Stevens, Michael L. TI SOLAR CYCLE VARIATIONS IN THE ELEMENTAL ABUNDANCE OF HELIUM AND FRACTIONATION OF IRON IN THE FAST SOLAR WIND: INDICATORS OF AN EVOLVING ENERGETIC RELEASE OF MASS FROM THE LOWER SOLAR ATMOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE solar wind; Sun: chromosphere; Sun: corona; Sun: heliosphere; Sun: surface magnetism; Sun: transition region ID ALFVENIC WAVES; CORONA; SPEED; POWER AB We present and discuss the strong correspondence between evolution of the emission length scale in the lower transition region and in situ measurements of the fast solar wind composition during the most recent solar minimum. We combine recent analyses demonstrating the variance in the (supergranular) network emission length scale measured by the Solar and Heliospheric Observatory (and STEREO) with that of the helium abundance (from Wind) and the degree of iron fractionation in the solar wind (from the Advanced Composition Explorer and Ulysses). The net picture developing is one where a decrease in the helium abundance and the degree of iron fractionation (approaching values expected of the photosphere) in the fast wind indicate a significant change in the process loading material into the fast solar wind during the recent solar minimum. This result is compounded by a study of the helium abundance during the space age using the NASA OMNI database, which shows a slowly decaying amount of helium being driven into the heliosphere over the course of several solar cycles. C1 [McIntosh, Scott W.; Kiefer, Kandace K.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Kiefer, Kandace K.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47906 USA. [Leamon, Robert J.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Kasper, Justin C.; Stevens, Michael L.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP McIntosh, SW (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA. RI Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU NSF [ATM-0541567, ATM-0925177]; NASA [NNG06GC89G, NNX08AL22G, NNX08AH45G]; National Science Foundation FX S.W.M. is supported by NSF ATM-0541567 (ATM-0925177), NASA grants NNG06GC89G, NNX08AL22G, and NNX08AH45G. K3 visited HAO in the summer of 2011 supported by the NSF Research Experience for Undergraduates (REU) program-we greatly appreciate the organization and commitment of the CU/LASP REU program administration group. In addition, we thank Joe Gurman for valuable comments, the Ulysses/SWICS and ACE/SWICS instrument teams for the effort taken to distribute and document the ion composition they serve to the community, and likewise to the OMNI database staff for their continued effort to preserve an essential physical record. NCAR is sponsored by the National Science Foundation. NR 26 TC 9 Z9 9 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 10 PY 2011 VL 740 IS 1 AR L23 DI 10.1088/2041-8205/740/1/L23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 824OH UT WOS:000295210900023 ER PT J AU Viti, S Jimenez-Serra, I Yates, JA Codella, C Vasta, M Caselli, P Lefloch, B Ceccarelli, C AF Viti, S. Jimenez-Serra, I. Yates, J. A. Codella, C. Vasta, M. Caselli, P. Lefloch, B. Ceccarelli, C. TI L1157-B1: WATER AND AMMONIA AS DIAGNOSTICS OF SHOCK TEMPERATURE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (L1157); ISM: jets and outflows; ISM: molecules; stars: formation ID C-TYPE SHOCKS; CHESS SPECTRAL SURVEY; MOLECULAR CLOUDS; INTERSTELLAR AMMONIA; TEMPORAL EVOLUTION; RADIATIVE-TRANSFER; OUTFLOW L1157; EMISSION; WAVES; CORES AB We investigate the origin and nature of the profiles of water and ammonia observed toward the L1157-B1 clump as part of the HIFI CHESS survey using a new code coupling a gas-grain chemical model with a parametric shock model. First results from the unbiased survey reveal different molecular components at different excitation conditions coexisting in the B1 bow shock structure, with NH3, H2CO, and CH3OH emitting only at relatively low outflow velocities whereas H2O shows bright emission at high velocities. Our model suggests that these differences are purely chemical and can be explained by the presence of a C-type shock whose maximum temperature must be close to 4000 K along the B1 clump. C1 [Viti, S.; Yates, J. A.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Codella, C.; Vasta, M.; Caselli, P.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Lefloch, B.; Ceccarelli, C.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [Lefloch, B.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain. RP Viti, S (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM sv@star.ucl.ac.uk OI Codella, Claudio/0000-0003-1514-3074 FU Smithsonian Astrophysical Observatory FX I.J.-S. acknowledges the Smithsonian Astrophysical Observatory for the support provided through a SMA fellowship. NR 41 TC 33 Z9 33 U1 1 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 OCT 10 PY 2011 VL 740 IS 1 AR L3 DI 10.1088/2041-8205/740/1/L3 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 824OH UT WOS:000295210900003 ER PT J AU Aliu, E Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Christiansen, JL Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Duke, C Errando, M Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gibbs, K Gillanders, GH Godambe, S Griffin, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Huan, H Hughes, G Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Krawczynski, H Krennrich, F Lang, MJ Lyutikov, M Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A McCutcheon, M Moriarty, P Mukherjee, R Nunez, P Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pizlo, F Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Ruppel, J Saxon, DB Schroedter, M Sembroski, GH Senturk, GD Smith, AW Staszak, D Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Tyler, J Varlotta, A Vassiliev, VV Vincent, S Vivier, M Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Zitzer, B AF Aliu, E. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Christiansen, J. L. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gibbs, K. Gillanders, G. H. Godambe, S. Griffin, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Huan, H. Hughes, G. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Lyutikov, M. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. McCutcheon, M. Moriarty, P. Mukherjee, R. Nunez, P. Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pizlo, F. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Ruppel, J. Saxon, D. B. Schroedter, M. Sembroski, G. H. Sentuerk, G. D. Smith, A. W. Staszak, D. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Tyler, J. Varlotta, A. Vassiliev, V. V. Vincent, S. Vivier, M. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Zitzer, B. CA VERITAS Collaboration TI Detection of Pulsed Gamma Rays Above 100 GeV from the Crab Pulsar SO SCIENCE LA English DT Article ID HIGH-ENERGY EMISSION; AREA TELESCOPE; OUTER MAGNETOSPHERE; MILLISECOND PULSARS; LIGHT CURVES; SLOT GAPS; NEBULA; RADIATION; TEV; CATALOG AB We report the detection of pulsed gamma rays from the Crab pulsar at energies above 100 giga-electron volts (GeV) with the Very Energetic Radiation Imaging Telescope Array System (VERITAS) array of atmospheric Cherenkov telescopes. The detection cannot be explained on the basis of current pulsar models. The photon spectrum of pulsed emission between 100 mega-electron volts and 400 GeV is described by a broken power law that is statistically preferred over a power law with an exponential cutoff. It is unlikely that the observation can be explained by invoking curvature radiation as the origin of the observed gamma rays above 100 GeV. Our findings require that these gamma rays be produced more than 10 stellar radii from the neutron star. C1 [Griffin, S.; Guenette, R.; Hanna, D.; McCann, A.; McCutcheon, M.; Ragan, K.; Staszak, D.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Gibbs, K.; Perkins, J. S.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.; Smith, A. W.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Collins-Hughes, E.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Christiansen, J. L.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Lyutikov, M.; Pizlo, F.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Nunez, P.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Huan, H.; Humensky, T. B.; Park, N.; Reyes, L. C.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.] DESY, D-15738 Zeuthen, Germany. [Imran, A.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Pohl, M.; Ruppel, J.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. RP McCann, A (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM mccann@hep.physics.mcgill.ca; nepomuk.otte@gmail.com; schroedter@veritas.sao.arizona.edu OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Otte, Adam Nepomuk/0000-0002-5955-6383; Lang, Mark/0000-0003-4641-4201 FU U.S. Department of Energy; NSF; Smithsonian Institution; Natural Sciences and Engineering Research Council of Canada; Science Foundation Ireland (SFI) [10/RFP/AST2748]; Science and Technology Facilities Council in the United Kingdom; Alexander von Humboldt Foundation FX This research is supported by grants from the U.S. Department of Energy, NSF, and the Smithsonian Institution; by Natural Sciences and Engineering Research Council of Canada; by Science Foundation Ireland (SFI 10/RFP/AST2748); and by the Science and Technology Facilities Council in the United Kingdom. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. A.N.O. was supported in part by a Feodor-Lynen fellowship of the Alexander von Humboldt Foundation. We are grateful to M. Roberts and A. Lyne for providing us with Crab-pulsar ephemerides before the public ones became available. NR 32 TC 83 Z9 84 U1 1 U2 6 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 7 PY 2011 VL 334 IS 6052 BP 69 EP 72 DI 10.1126/science.1208192 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 829KW UT WOS:000295580300040 ER PT J AU Cassoff, RM Moore, KM McLellan, WA Barco, SG Rotstein, DS Moore, MJ AF Cassoff, Rachel M. Moore, Kathleen M. McLellan, William A. Barco, Susan G. Rotstein, David S. Moore, Michael J. TI Lethal entanglement in baleen whales SO DISEASES OF AQUATIC ORGANISMS LA English DT Article DE Baleen whales; Entanglement; Mortality; Cetacean; Strandings; Fishing gear; Necropsy; Northwestern Atlantic ID ATLANTIC RIGHT WHALES; WESTERN NORTH-ATLANTIC; MEGAPTERA-NOVAEANGLIAE; EUBALAENA-GLACIALIS; HUMPBACK WHALES; BALAENOPTERA-ACUTOROSTRATA; CYAMIDS CRUSTACEA; BOWHEAD WHALE; MINKE WHALE; INJURIES AB Understanding the scenarios whereby fishing gear entanglement of large whales induces mortality is important for the development of mitigation strategies. Here we present a series of 21 cases involving 4 species of baleen whales in the NW Atlantic, describing the available sighting history, necropsy observations, and subsequent data analyses that enabled the compilation of the manners in which entanglement can be lethal. The single acute cause of entanglement mortality identified was drowning from entanglement involving multiple body parts, with the animal's inability to surface. More protracted causes of death included impaired foraging during entanglement, resulting in starvation after many months; systemic infection arising from open, unresolved entanglement wounds; and hemorrhage or debilitation due to severe gear-related damage to tissues. Serious gear-induced injury can include laceration of large vessels, occlusion of the nares, embedding of line in growing bone, and massive periosteal proliferation of new bone in an attempt to wall off constricting, encircling lines. These data show that baleen whale entanglement is not only a major issue for the conservation of some baleen whale populations, but is also a major concern for the welfare of each affected individual. C1 [Moore, Michael J.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Cassoff, Rachel M.] Univ Penn, Sch Vet Med, Philadelphia, PA 19104 USA. [Moore, Kathleen M.] Int Fund Anim Welf, Yarmouth Port, MA 02675 USA. [McLellan, William A.] Univ N Carolina, Wilmington, NC 28403 USA. [Barco, Susan G.] Virginia Aquarium & Marine Sci Ctr, Stranding Response Program, Virginia Beach, VA 23451 USA. [Rotstein, David S.] Smithsonian Museum Support Ctr, Osteoprep Lab, Suitland, MD 20746 USA. [Moore, Michael J.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. RP Moore, MJ (reprint author), Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. EM mmoore@whoi.edu RI Moore, Michael/E-1707-2015 OI Moore, Michael/0000-0003-3074-6631 FU NOAA [NA09OAR4320129] FX The authors thank the many stranding responders on the North American east coast who have contributed hugely to this dataset. Right whale data were accessed with permission from the North Atlantic Right Whale Consortium necropsy and sightings databases. This case report analysis was supported in part by NOAA Cooperative Agreement No. NA09OAR4320129. Stranding response was supported by multiple NOAA Prescott awards to UNC Wilmington, Virginia Aquarium & Marine Science Center, the Cape Cod Stranding Network and Woods Hole Oceanographic Institution (WHOI). NOAA contracts for right whale necropsy were held by WHOI. NR 43 TC 39 Z9 43 U1 10 U2 51 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0177-5103 J9 DIS AQUAT ORGAN JI Dis. Aquat. Org. PD OCT 6 PY 2011 VL 96 IS 3 BP 175 EP 185 DI 10.3354/dao02385 PG 11 WC Fisheries; Veterinary Sciences SC Fisheries; Veterinary Sciences GA 831GF UT WOS:000295716200001 PM 22132496 ER PT J AU Bean, J AF Bean, Jacob TI EXTRASOLAR PLANETS Homing in on another Earth SO NATURE LA English DT Editorial Material C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bean, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jbean@cfa.harvard.edu NR 4 TC 5 Z9 5 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 6 PY 2011 VL 478 IS 7367 BP 41 EP 42 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 829JN UT WOS:000295575400027 PM 21964338 ER PT J AU Grego, L AF Grego, Laura TI Security in Space: What Is at Stake and How Do We Move Forward? SO ASIAN PERSPECTIVE LA English DT Article DE space security; antisatellite capability; space debris; international security ID DEBRIS AB In recent decades, satellites have become increasingly important in the economic, civil, and military spheres. At the same time, space has become more crowded with satellites and the debris from their use, and many more states have become spacefaring. However, the legal and normative regime has not kept pace with these changes. Recent trends and events-including demonstrations of antisatellite (ASAT) capability, a collision between satellites, and a dramatic increase in dangerous space debris-make clear that the space environment needs more protection, that satellites face growing risks, and that space activities may be a potential source of mistrust and tension between countries. While voluntary confidence-building and transparency measures can help solve some of these issues, more substantive engagement is required to keep space safe and secure into the future. C1 [Grego, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. EM lgrego@ucsusa.org NR 13 TC 1 Z9 1 U1 1 U2 1 PU KYUNGNAM UNIV, INST FAR EASTERN STUDIES PI SEOUL PA 28-42 SAMCHUNG-DONG, CHONGRO-KU, SEOUL, 110-230, SOUTH KOREA SN 0258-9184 J9 ASIAN PERSPECT-SEOUL JI Asian Perspec. PD OCT-DEC PY 2011 VL 35 IS 4 SI SI BP 503 EP 520 PG 18 WC International Relations SC International Relations GA 862DA UT WOS:000298068800002 ER PT J AU Wise, MA Brown, CD AF Wise, Michael A. Brown, Cathleen D. TI Chemical composition of coexisting columbite-group minerals and cassiterite from the Black Mountain pegmatite, Maine SO EUROPEAN JOURNAL OF MINERALOGY LA English DT Article DE cassiterite; columbite-group minerals; pegmatite; Black Mountain; Maine ID ELEMENT GRANITIC PEGMATITES; OXIDE MINERALS; NIOBIUM-TANTALUM; SOUTH-DAKOTA; TA-BEARING; NB-BEARING; GEOCHEMISTRY; WODGINITE; TRENDS; FRACTIONATION AB Detailed examination of hand samples and backscatter electron images of Nb-, Ta-, Sn-oxide minerals from the Black Mountain pegmatite has revealed the presence of discrete crystals, as well as cassiterite-hosted micrograins of columbite-group minerals (CGM). Micrograins and discrete grains of CGM show a wide range of Mn/(Mn + Fe) values, but only the micrograins have limited Ta/(Ta + Nb) values. Trace amounts of Ti, Sc, Fe(3+) and Sn are common in both generations of CGM, but their total rarely exceeds 1.0 oxide wt%. The chemistry of the host cassiterite is relatively homogeneous and pure; the total concentration of FeO, MnO, Nb(2)O(5), Ta(2)O(5) and TiO(2) rarely exceeds 2.0 wt%. While discrete CGM grains show weak progressive zonation and minor replacement, micrograins display complex oscillatory zonation, resorption and/or replacement textures. Textural evidence suggests that the micrograins crystallized after the formation of discrete grains of columbite and cassiterite. On the whole, both discrete crystals and micrograins of CGM show increasing Mn/(Mn + Fe) with fractionation as commonly observed in F-enriched granitic pegmatites. Micrograins of CGM typically show higher Ta/(Ta + Nb) values compared to their discrete crystal counterparts. Textural characteristics of CGM micrograins are inconsistent with an origin by exsolution, and instead, indicate primary precipitation. C1 [Wise, Michael A.; Brown, Cathleen D.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Wise, MA (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. EM wisem@si.edu FU Sprague fund; Smithsonian Institution FX This study was made possible by the Sprague fund and laboratory support of the Smithsonian Institution. We gratefully thank Joe Martin of Rumford, Maine for providing access to the Black Mountain pegmatite and T. S. Ercit and T. Martin for their invaluable discussions regarding columbite inclusions in cassiterite. The authors thank W. Simmons, M. Novak, P. Cerny and Y. Thibault for constructive criticisms which led to considerable improvements of this manuscript. NR 41 TC 3 Z9 3 U1 0 U2 11 PU E SCHWEIZERBARTSCHE VERLAGS PI STUTTGART PA NAEGELE U OBERMILLER, SCIENCE PUBLISHERS, JOHANNESSTRASSE 3A, D 70176 STUTTGART, GERMANY SN 0935-1221 J9 EUR J MINERAL JI Eur. J. Mineral. PD OCT PY 2011 VL 23 IS 5 BP 817 EP 828 DI 10.1127/0935-1221/2011/0023-2102 PG 12 WC Mineralogy SC Mineralogy GA 861SB UT WOS:000298038400011 ER PT J AU Santymire, RM Brown, JL Stewart, RA Santymire, RC Wildt, DE Howard, J AF Santymire, Rachel M. Brown, Janine L. Stewart, Rosemary A. Santymire, Robb C. Wildt, David E. Howard, JoGayle TI Reproductive gonadal steroidogenic activity in the fishing cat (Prionailurus viverrinus) assessed by fecal steroid analyses SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE Fe lid reproduction; Seasonality; Estrous cycle; Ovulation ID INTRAUTERINE ARTIFICIAL-INSEMINATION; NORMAL ESTROUS-CYCLE; LEOPARD NEOFELIS-NEBULOSA; PUMA FELIS-CONCOLOR; LION PANTHERA-LEO; OVARIAN ACTIVITY; SEXUAL-BEHAVIOR; EXOGENOUS GONADOTROPINS; SERUM CONCENTRATIONS; CLOUDED LEOPARD AB Non-invasive fecal steroid analyses were used to characterize gonadal activity in the fishing cat (Prionailurus viverrinus). Estrogen, progestagen and androgen metabolites were quantified in fecal samples collected for 12 months from four males and 10 females housed at seven North American zoological institutions. Male reproductive hormone concentrations did not vary (P > 0.05) among season, and estrogen cycles were observed year-round in females and averaged (+/- SEM) 19.9 +/- 1.0 days. Mean peak estrogen concentration during estrus (460.0 +/- 72.6 ng/g feces) was five-fold higher than baseline (87.3 +/- 14.0 ng/g feces). Five of seven females (71.4%) housed alone or with another female demonstrated spontaneous luteal activity (apparent ovulation without copulation), with mean progestagen concentration (20.3 +/- 4.7 mu g/g feces), increasing nearly five-fold above baseline (4.1 +/- 0.8 mu g/g feces). The non-pregnant luteal phase averaged 32.9 +/- 2.5 days (n = 13). One female delivered kittens 70 days after natural mating with fecal progestagen concentrations averaging 51.2 +/- 5.2 mu g/g feces. Two additional females were administered exogenous gonadotropins (150 IU eCG; 100 IU hCG), which caused hyper-elevated concentrations of fecal estrogen and progestagen (plus ovulation). Results indicate that: (1) male and female fishing cats managed in North American zoos are reproductively active year round; (2) 71.4% of females experienced spontaneous ovulation; and (3) females are responsive to exogenous gonadotropins for ovulation induction, but a regimen that produces a normative ovarian steroidogenic response needs to be identified. (C) 2011 Elsevier B.V. All rights reserved. C1 [Santymire, Rachel M.; Brown, Janine L.; Stewart, Rosemary A.; Santymire, Robb C.; Wildt, David E.; Howard, JoGayle] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Ctr Species Survival, Front Royal, VA 22630 USA. RP Santymire, RM (reprint author), Lincoln Pk Zoo,2001 N Clark St, Chicago, IL 60614 USA. EM rsantymire@lpzoo.org FU Morris Animal Foundation FX This study was supported by the Morris Animal Foundation. The authors thank the animal care staff and management of the partner zoological institutions (Minnesota Zoological Garden, Cincinnati Zoo & Botanical Garden, Sacramento Zoo, San Francisco Zoological Gardens, Happy Hollow Zoo, Oklahoma City Zoological Park, and San Antonio Zoological Gardens and Aquarium) for participation in the study and dedication on fecal sample collections. We thank Dr. Bill Swanson and the animal care and veterinary staff at the Cincinnati Zoo & Botanical Garden for administering exogenous gonadotropins (eCG and hCG) to two female fishing cats. We also thank Claudia Sanchez and Nicole Abbondanza at the National Zoo's Endocrine Research Laboratories for excellent technical assistance. Additionally, we thank Dr. Eric Lonsdorf at Lincoln Park Zoo for assistance with statistical analyses. NR 55 TC 9 Z9 9 U1 1 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD OCT PY 2011 VL 128 IS 1-4 BP 60 EP 72 DI 10.1016/j.anireprosci.2011.09.001 PG 13 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA 859RF UT WOS:000297892800008 PM 21975304 ER PT J AU Ryder, TB Fox, JW Marra, PP AF Ryder, Thomas B. Fox, James W. Marra, Peter P. TI ESTIMATING MIGRATORY CONNECTIVITY OF GRAY CATBIRDS (DUMETELLA CAROLINENSIS) USING GEOLOCATOR AND MARK-RECAPTURE DATA (vol 128, pg 448, 2011) SO AUK LA English DT Correction C1 [Ryder, Thomas B.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [Fox, James W.] British Antarctic Survey, Nat Environm Res Council, Cambridge CB3 0ET, England. RP Ryder, TB (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, POB 37012-MRC5503, Washington, DC 20008 USA. EM rydert@si.edu NR 1 TC 0 Z9 0 U1 1 U2 19 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2011 VL 128 IS 4 BP 810 EP 810 DI 10.1525/auk.2011.128.4.810 PG 1 WC Ornithology SC Zoology GA 859JM UT WOS:000297872700026 ER PT J AU Graur, O Poznanski, D Maoz, D Yasuda, N Totani, T Fukugita, M Filippenko, AV Foley, RJ Silverman, JM Gal-Yam, A Horesh, A Jannuzi, BT AF Graur, O. Poznanski, D. Maoz, D. Yasuda, N. Totani, T. Fukugita, M. Filippenko, A. V. Foley, R. J. Silverman, J. M. Gal-Yam, A. Horesh, A. Jannuzi, B. T. TI Supernovae in the Subaru Deep Field: the rate and delay-time distribution of Type Ia supernovae out to redshift 2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: observational; surveys; supernovae: general; galaxies: distances and redshifts ID DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; CORE-COLLAPSE SUPERNOVAE; WHITE-DWARF BINARY; GAMMA-RAY BURSTS; LUMINOSITY FUNCTIONS; LEGACY SURVEY; LIGHT CURVES AB The Type Ia supernova (SN Ia) rate, when compared to the cosmic star formation history (SFH), can be used to derive the delay-time distribution (DTD; the hypothetical SN Ia rate versus time following a brief burst of star formation) of SNe Ia, which can distinguish among progenitor models. We present the results of a supernova (SN) survey in the Subaru Deep Field (SDF). Over a period of 3 years, we have observed the SDF on four independent epochs with Suprime-Cam on the Subaru 8.2-m telescope, with two nights of exposure per epoch, in the R, i'and z' bands. We have discovered 150 SNe out to redshift z 2. Using 11 photometric bands from the observer-frame far-ultraviolet to the near-infrared, we derive photometric redshifts for the SN host galaxies (for 24 we also have spectroscopic redshifts). This information is combined with the SN photometry to determine the type and redshift distribution of the SN sample. Our final sample includes 28 SNe Ia in the range 1.0 < z < 1.5 and 10 in the range 1.5 < z < 2.0. As our survey is largely insensitive to core-collapse SNe (CC SNe) at z > 1, most of the events found in this range are likely SNe Ia. Our SN Ia rate measurements are consistent with those derived from the Hubble Space Telescope (HST) Great Observatories Origins Deep Survey (GOODS) sample, but the overall uncertainty of our 1.5 < z < 2.0 measurement is a factor of 2 smaller, of 3550 per cent. Based on this sample, we find that the SN Ia rate evolution levels off at 1.0 < z < 2.0, but shows no sign of declining. Combining our SN Ia rate measurements and those from the literature, and comparing to a wide range of possible SFHs, the best-fitting DTD (with a reduced ?2= 0.7) is a power law of the form ?(t) ?t beta, with index beta=-1.1 +/- 0.1 (statistical) +/- 0.17 (systematic). This result is consistent with other recent DTD measurements at various redshifts and environments, and is in agreement with a generic prediction of the double-degenerate progenitor scenario for SNe Ia. Most single-degenerate models predict different DTDs. By combining the contribution from CC SNe, based on the wide range of SFHs, with that from SNe Ia, calculated with the best-fitting DTD, we predict that the mean present-day cosmic iron abundance is in the range ZFe= (0.090.37) ZFe, ?. We further predict that the high-z SN searches now beginning with HST will discover 211 SNe Ia at z > 2. C1 [Graur, O.; Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Poznanski, D.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Poznanski, D.; Filippenko, A. V.; Foley, R. J.; Silverman, J. M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Yasuda, N.; Fukugita, M.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Totani, T.] Kyoto Univ, Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gal-Yam, A.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Horesh, A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Graur, O (reprint author), Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. EM orgraur@wise.tau.ac.il RI Yasuda, Naoki/A-4355-2011; Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Graur, Or/0000-0002-4391-6137 FU Israel Science Foundation; Israel Science Foundation (ISF); Einstein Fellowship; US Department of Energy [DE-FG02-06ER06-04]; NSF [AST-0908886]; TABASGO Foundation; Department of Energy [DE-FG0-08ER41563]; Clay fellowship; Marie Curie IRG FX DM acknowledges support by a grant from the Israel Science Foundation (ISF). DP is supported by an Einstein Fellowship, and by the US Department of Energy Scientific Discovery through Advanced Computing (SciDAC) programme under contract DE-FG02-06ER06-04. AVF is grateful for the financial support of NSF grant AST-0908886, the TABASGO Foundation and Department of Energy grant DE-FG0-08ER41563. RJF is supported by a Clay fellowship. AG is supported by an FP7/Marie Curie IRG fellowship and a grant from the ISF. NR 177 TC 61 Z9 61 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 2 BP 916 EP 940 DI 10.1111/j.1365-2966.2011.19287.x PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848HR UT WOS:000297043000008 ER PT J AU Angus, GW Diaferio, A AF Angus, G. W. Diaferio, Antonaldo TI The abundance of galaxy clusters in modified Newtonian dynamics: cosmological simulations with massive neutrinos SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; cosmology: theory; dark matter; large-scale structure of Universe ID MICROWAVE BACKGROUND ANISOTROPIES; POWER-SPECTRUM; BULLET CLUSTER; DARK-MATTER; LAMBDA-CDM; MOND; EXISTENCE; GRAVITY; HALOS; SCALE AB We present a new particle mesh cosmological N-body code for accurately solving the modified Poisson equation of the quasi-linear formulation of modified Newtonian dynamics (MOND). We generate initial conditions for the Angus cosmological model, which is identical to ? cold dark matter (?CDM) except that the CDM is switched for a single species of thermal sterile neutrinos. We set the initial conditions at z= 250 for a (512 Mpc h-1)3 box with 2563 particles, and we evolve them down to z= 0. We clearly demonstrate the ability of MOND to develop the large-scale structure in a hot dark matter cosmology and contradict the naive expectation that MOND cannot form galaxy clusters. We find that the correct order of magnitude of X-ray clusters (with TX > 4.5 keV) can be formed, but that we overpredict the number of very rich clusters and seriously underpredict the number of lower mass clusters. We present evidence that suggests the density profiles of our simulated clusters are compatible with those of the observed X-ray clusters in MOND. As a last test, we computed the relative velocity between pairs of haloes within 10 Mpc and find that pairs with velocities larger than 3000 km s-1, like the bullet cluster, can form without difficulty. C1 [Angus, G. W.] Univ Cape Town, Astrophys Cosmol & Grav Ctr, ZA-7700 Rondebosch, South Africa. [Angus, G. W.; Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. [Angus, G. W.; Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Angus, GW (reprint author), Univ Cape Town, Astrophys Cosmol & Grav Ctr, Private Bag X3, ZA-7700 Rondebosch, South Africa. EM angus.gz@gmail.com FU National Research Foundation of South Africa; NRF; University of Torino; Regione Piemonte; INFN [PD51]; PRIN-MIUR [2008NEBK003] FX GWA's research is supported by the National Research Foundation of South Africa and in particular the NRF special award for Y-rated researchers is gratefully acknowledged. AD's research is supported by the University of Torino and Regione Piemonte. Partial support is acknowledged from the INFN grant PD51 and PRIN-MIUR-2008 grant '2008NEBK003' 'Matter-antimatter asymmetry, dark matter and dark energy in the LHC era'. We appreciate comments from Silvio Bonometto, Tom Zlosnik, Martin Feix, Benoit Famaey, Gianfranco Gentile and Kurt van der Heyden. Finally, we thank the referee for valuable comments that greatly strengthened the paper. NR 51 TC 23 Z9 23 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 2 BP 941 EP 949 DI 10.1111/j.1365-2966.2011.19321.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848HR UT WOS:000297043000009 ER PT J AU Blondin, S Kasen, D Ropke, FK Kirshner, RP Mandel, KS AF Blondin, Stephane Kasen, Daniel Roepke, Friedrich K. Kirshner, Robert P. Mandel, Kaisey S. TI Confronting 2D delayed-detonation models with light curves and spectra of Type Ia supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general ID FAILED DEFLAGRATION MODEL; HIGH-VELOCITY FEATURES; MAXIMUM LIGHT; THERMONUCLEAR SUPERNOVAE; OPTICAL SPECTROSCOPY; IMPROVED DISTANCES; EQUIVALENT WIDTHS; SNE-IA; DIVERSITY; EXPLOSION AB We compare models for Type Ia supernova (SN Ia) light curves and spectra with an extensive set of observations. The models come from a recent survey of 44 two-dimensional delayed-detonation models computed by Kasen et al., each viewed from multiple directions. The data include optical light curves of 251 SNe Ia, some of which have near-infrared observations, and 2231 low-dispersion spectra from the Center for Astrophysics, plus data from the literature. These allow us to compare a wide range of SN Ia models with observations for a wide range of luminosities and decline rates. The analysis uses standard techniques employed by observers, including MLCS2k2, SALT2 and SNooPy for light-curve analysis, and the Supernova Identification (snid) code of Blondin & Tonry for spectroscopic comparisons to assess how well the models match the data. The ability to use the tools developed for observational data directly on the models marks a significant step forward in the realism of the models. We show that the models that match observed spectra best lie systematically on the observed widthluminosity relation. Conversely, we reject six models with highly asymmetric ignition conditions and a large amount (?1 M?) of synthesized 56Ni that yield poor matches to observed SN Ia spectra. More subtle features of the comparison include the general difficulty of the models to match the U-band flux at early times, caused by hot ionized ejecta that affect the subsequent redistribution of flux at longer wavelengths. The models have systematically higher velocities than the observed spectra at maximum light, as inferred from the Si ii ?6355 line. We examine ways in which the asymptotic kinetic energy of the explosion affects both the predicted velocity and velocity gradient in the Si ii and Ca ii lines. Models with an asymmetric distribution of 56Ni are found to result in a larger variation of photometric and spectroscopic properties with viewing angle, regardless of the initial ignition setup. We discuss more generally whether highly anisotropic ignition conditions are ruled out by observations, and how detailed comparisons between models and observations involving both light curves and spectra can lead to a better understanding of SN Ia explosion mechanisms. C1 [Blondin, Stephane] Univ Aix Marseille, CNRS, CPPM, IN2P3, F-13288 Marseille 9, France. [Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Kasen, Daniel] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Nucl Sci, Berkeley, CA 94720 USA. [Roepke, Friedrich K.] Univ Wurzburg, D-97074 Wurzburg, Germany. [Roepke, Friedrich K.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Kirshner, Robert P.; Mandel, Kaisey S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Blondin, S (reprint author), Univ Aix Marseille, CNRS, CPPM, IN2P3, 163 Ave Luminy, F-13288 Marseille 9, France. EM blondin@cppm.in2p3.fr OI Ropke, Friedrich/0000-0002-4460-0097 FU DOE [DE-FC02-06ER41438]; ORNL; NERSC; Deutsche Forschungsgemeinschaft [RO 3676/1-1]; NSF [AST 09-07903] FX SB acknowledges useful discussions with Luc Dessart, Ryan Foley, Alexei Khokhlov and Masaomi Tanaka. This research has been supported by the DOE SciDAC Program (DE-FC02-06ER41438). Computing time was provided by ORNL through an INCITE award and by NERSC. The work of FKR is supported by the Deutsche Forschungsgemeinschaft via the Emmy Noether programme (RO 3676/1-1). Support for supernova research at Harvard University, including the CfA Supernova Archive, is provided in part by NSF grant AST 09-07903. NR 91 TC 30 Z9 30 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 2 BP 1280 EP 1302 DI 10.1111/j.1365-2966.2011.19345.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 848HR UT WOS:000297043000031 ER PT J AU Koch, F Smith, DR AF Koch, Frank Smith, David R. TI A NEW SPECIES OF CALIROA (HYMENOPTERA: TENTHREDINIDAE) FROM SOUTH AFRICA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Symphyta; Heterarthrinae; Caliroini; Afromontane Region; Limpopo Province; Mpumalanga Province AB Caliroa blanki, n. sp., the first native species of Caliroa from the Afrotropical Region, is described from South Africa. Differences in wing venation from usual Caliroa species and provisional placement in Caliroa are discussed. Discussion and records for the invasive Caliroa cerasi (L.) in South Africa are given. A distribution map is provided for both species. C1 [Koch, Frank] Humboldt Univ, Museum Nat Kunde, Inst Systemat Zool, D-10115 Berlin, Germany. [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Koch, F (reprint author), Humboldt Univ, Museum Nat Kunde, Inst Systemat Zool, Invalidenstr 43, D-10115 Berlin, Germany. EM frank.koch@mfn-berlin.de; dave.smith@ars.usda.gov FU German Research Foundation [445 SUA-113/8/1-3]; International Bureau of the Federal Ministry of Education and Research at the Project Management Agency c/o German Aerospace Center (DLR) [SUA 08/058] FX We are most grateful to the following for allowing examination of specimens in their care: C. D. Eardley (PPRI); M. Kruger (TMSA). The German Research Foundation (445 SUA-113/8/1-3) and the International Bureau of the Federal Ministry of Education and Research at the Project Management Agency c/o German Aerospace Center (DLR) (SUA 08/058) are gratefully acknowledged for providing a research grant. Mike Picker (ZUCT) provided information on C. cerasi. Michele Touchet, Systematic Entomology Laboratory, USDA, Washington, DC, helped with images 1-8. We thank the following for review of the manuscript: H. Goulet, Agriculture Canada, Ottawa, and A. S. Konstantinov and T. J. Henry, Systematic Entomology Laboratory, USDA, Washington, DC. USDA is an equal opportunity provider and employer. NR 11 TC 0 Z9 0 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2011 VL 113 IS 4 BP 442 EP 450 DI 10.4289/0013-8797.113.4.442 PG 9 WC Entomology SC Entomology GA 853QA UT WOS:000297439600005 ER PT J AU Kula, RR Marsh, PM AF Kula, Robert R. Marsh, Paul M. TI DORYCTINAE (HYMENOPTERA: BRACONIDAE) OF KONZA PRAIRIE EXCLUDING SPECIES OF HETEROSPILUS HALIDAY SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE biodiversity; conservation; Flint Hills; gallery forest; Great Plains; Kansas; Nearctic; tallgrass prairie ID NEARCTIC DORYCTINAE; COLEOPTERA BUPRESTIDAE; NORTH-AMERICA; SPATHIUS NEES; LELUTHIA AB The results of a survey of Doryctinae (Hymenoptera: Braconidae), excluding species of Heterospilus Haliday, at Konza Prairie near Manhattan, Kansas are reported. Eleven sites representing prairie and woodland/wetland areas, including gallery forest, were sampled in 2001 and 2005 using Malaise and canopy traps. Topographic trap placement included lowland, midslope, and upland areas. Twenty-four species were collected, including 18 in 2001 and 16 in 2005. Twenty-three of the 24 species were collected from the woodland/wetland sites, including 19 from gallery forest sites; five of the 24 species were collected from the prairie sites. Rhaconotus fasciatus (Ashmead) was the most abundant species in 2001 (n = 13); Callihormius bifasciatus (Ashmead) and Coiba jeffersoni Kula were the most abundant species in 2005 (n = 10). The following new species are described: Doryctes xanthogaster Kula and Marsh, Doryctes xanthosoma Kula and Marsh, Doryctinus zolnerowichi Kula and Marsh, and Pambolidea dollari Kula and Marsh. Glyptocolastes caryae (Ashmead), status revised is removed from synonymy with Glyptocolastes rugulosus (Cresson), the type species for Doryctinus Roman. The latter species is transferred to Acrophasmus Enderlein, resulting in Acrophasmus as a new synonym of Doryctinus. Synonymy of the aforementioned genera results in the following nomenclatural changes: Doryctinus amazonicus (Roman), new combination; Doryctinus arizonensis (Marsh), new combination; Doryctinus atriventris (Cresson), new combination; Doryctinus butleri (Marsh), new combination; Doryctinus costaricensis (Marsh), new combination; Doryctinus erugatus (Marsh), new combination; Doryctinus exilis (Enderlein), new combination; Doryctinus ferrugineus (Marsh), new combination; Doryctinus gauldi (Marsh), new combination; Doryctinus immigrans (Beardsley), new combination; Doryctinus maeandrius (Enderlein), new combination; Doryctinus marshi Greenbaum, revised combination; Doryctinus rubronotum (Marsh), new combination; Doryctinus rugulosus (Cresson), revised combination; Doryctinus scobiciae (Marsh), new combination; and Doryctinus secundus (Muesebeck and Walkley), new combination. Doryctes infuscus Marsh is a new synonym of Doryctes rufipes (Provancher), Pioscelus wichitus (Viereck) is a new synonym of Pioscelus borealis (Ashmead), and Rhaconotus graciliformis (Viereck) is a new synonym of R. fasciatus. The following species are first records for Kansas: C. bifasciatus, Dendrosoter sulcatus Muesebeck, D. rufipes, D. ferrugineus, Ecphylus hypothenemi Ashmead, Ecphylus rohweri Muesebeck, Ontsira mellipes (Ashmead), and Rhaconotus canadensis Marsh. C1 [Kula, Robert R.] ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Kula, RR (reprint author), ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM Robert.Kula@ars.usda.gov; swampy@wildblue.net NR 73 TC 6 Z9 6 U1 0 U2 5 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2011 VL 113 IS 4 BP 451 EP 491 DI 10.4289/0013-8797.113.4.451 PG 41 WC Entomology SC Entomology GA 853QA UT WOS:000297439600006 ER PT J AU Pogue, MG AF Pogue, Michael G. TI USING GENITALIA CHARACTERS AND MITOCHONDRIAL COI SEQUENCES TO PLACE "LEUCOCHLAENA" HIPPARIS (DRUCE) IN SPODOPTERA GUENEE (LEPIDOPTERA: NOCTUIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE DNA barcode region; morphology; taxonomy ID DNA BARCODES; SKIPPER BUTTERFLIES; GENUS AB The species "Leucochlaena" hipparis (Druce) belongs in the genus Spodoptera based on morphological characters of the male and female genitalia, as well as maximum parsimony and maximum likelihood analysis of the 658 bp "barcode" region of cytochrome oxidae (COI). Adult and male and female genitalia are illustrated. Cladograms are included to illustrate the placement of "Leucochlaena" hipparis within Spodoptera. C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, Washington, DC 20013 USA. RP Pogue, MG (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,NMNH, POB 37012,MRC 168, Washington, DC 20013 USA. EM michael.pogue@ars.usda.gov NR 25 TC 1 Z9 2 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2011 VL 113 IS 4 BP 497 EP 507 DI 10.4289/0013-8797.113.4.497 PG 11 WC Entomology SC Entomology GA 853QA UT WOS:000297439600008 ER PT J AU Smith, DR Tripotin, P AF Smith, Davto R. Tripotin, Pierre TI AULACIDAE (HYMENOPTERA) OF KOREA, WITH NOTES ON THEIR BIOLOGY SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE parasitic wasps; Asia; Cerambycidae; Buprestidae; Xiphydriidae ID FAMILY AULACIDAE; XIPHYDRIIDAE; EVANIOIDEA AB Five species of Aulacidae are recorded from Korea: Aulacus salicius Sun and Sheng, 2007, Pristaulacus insularis Konishi, 1990, Pristaulacus intermedius Uchida, 1932, Pristaulacus kostylevi Alekseev,1986, and Pristaulacus jirisani Smith and Tripotin, new species. All except P intermedius represent new country records. A key to species and a diagnosis of each species are provided. Collection notes are given for each species, indicating that Xiphydria palaeanarctica Semenov (Hymenoptera: Xiphydriidae) is the host for A. salicius, and Cerambycidae and possibly Buprestidae (Coleoptera) are the hosts for the Pristaulacus species. C1 [Smith, Davto R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov; p_tripotin@hotmail.com NR 12 TC 1 Z9 3 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2011 VL 113 IS 4 BP 519 EP 530 DI 10.4289/0013-8797.113.4.519 PG 12 WC Entomology SC Entomology GA 853QA UT WOS:000297439600010 ER PT J AU Rowcliffe, JM Carbone, C Jansen, PA Kays, R Kranstauber, B AF Rowcliffe, J. Marcus Carbone, Chris Jansen, Patrick A. Kays, Roland Kranstauber, Bart TI Quantifying the sensitivity of camera traps: an adapted distance sampling approach SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE abundance estimation; animal density; camera detection zone; detection probability; passive infrared motion sensor; Random Encounter Model ID NEOTROPICAL FORESTS; PHOTOGRAPHIC RATES; ESTIMATE DENSITIES; CRYPTIC MAMMALS; POPULATION; TIGERS; LANDSCAPE; DESIGN; BIRDS AB 1. Abundance estimation is a pervasive goal in ecology. The rate of detection by motion-sensitive camera traps can, in principle, provide information on the abundance of many species of terrestrial vertebrates that are otherwise difficult to survey. The random encounter model (REM, Rowcliffe 2008) provides a means estimating abundance from camera trap rate but requires camera sensitivity to be quantified. 2. Here, we develop a method to estimate the area effectively monitored by cameras, which is one of the most important codeterminants of detection rate. Our method borrows from distance sampling theory, applying detection function models to data on the position (distance and angle relative to the camera) where the animals are first detected. Testing the reliability of this approach through simulation, we find that bias depends on the effective detection angle assumed but was generally low at less than 5% for realistic angles typical of camera traps. 3. We adapted standard detection functions to allow for the possibility of smaller animals passing beneath the field of view close to the camera, resulting in reduced detection probability within that zone. Using a further simulation to test this approach, we find that detection distance can be estimated with little or no bias if detection probability is certain for at least some distance from the camera. 4. Applying this method to a 1-year camera trapping data set from Barro Colorado Island, Panama, we show that effective detection distance is related strongly positively to species body mass and weakly negatively to species average speed of movement. There was also a strong seasonal effect, with shorter detection distance during the wet season. Effective detection angle is related more weakly to species body mass, and again strongly to season, with a wider angle in the wet season. 5. This method represents an important step towards practical application of the REM, including abundance estimation for relatively small (< 1 kg) species. C1 [Rowcliffe, J. Marcus; Carbone, Chris] ZSL Inst Zool, London NW1 4RY, England. [Jansen, Patrick A.; Kays, Roland] Smithsonian Trop Res Inst, Balboa, Panama. [Jansen, Patrick A.] Wageningen Univ, Ctr Ecosyst Studies, Wageningen, Netherlands. [Kays, Roland] New York State Museum & Sci Serv, Albany, NY USA. [Kranstauber, Bart] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany. RP Rowcliffe, JM (reprint author), ZSL Inst Zool, Regents Pk, London NW1 4RY, England. EM marcus.rowcliffe@ioz.ac.uk RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU NSF [DEB 0717071]; British Ecological Society; Netherlands Foundation of Scientific Research [NWO-ALW863-07-008] FX We thank Nadia Sitas, Anthony Turner, Daniel Rasmussen and Lennart Suselbeek for assistance in the field and the Smithsonian Tropical Research Institute, especially Oris Acevedo, for general logistical support. Required permits for the work described in this paper were obtained from the Autoridad Nacional del Ambiente, Panama, and the Smithsonian Tropical Research Institute. We are indebted to three referees for their insightful and supportive comments, in particular Steve Buckland. The work was funded by NSF (DEB 0717071) and the British Ecological Society. PAJ was funded by the Netherlands Foundation of Scientific Research (NWO-ALW863-07-008). NR 29 TC 33 Z9 39 U1 9 U2 118 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD OCT PY 2011 VL 2 IS 5 BP 464 EP 476 DI 10.1111/j.2041-210X.2011.00094.x PG 13 WC Ecology SC Environmental Sciences & Ecology GA 852CI UT WOS:000297323700005 ER PT J AU Piperno, DR AF Piperno, Dolores R. TI The Origins of Plant Cultivation and Domestication in the New World Tropics Patterns, Process, and New Developments SO CURRENT ANTHROPOLOGY LA English DT Article ID BALSAS RIVER VALLEY; REAL-ALTO SITE; STARCH GRAINS; NORTHERN PERU; AGRICULTURAL ORIGINS; MANIHOT-ESCULENTA; PHYLOGENETIC-RELATIONSHIPS; TERMINAL PLEISTOCENE; BEHAVIORAL ECOLOGY; PHYTOLITH EVIDENCE AB The New World tropical forest is now considered to be an early and independent cradle of agriculture. As in other areas of the world, our understanding of this issue has been significantly advanced by a steady stream of archaeobotanical, paleoecological, and molecular/genetic data. Also importantly, a renewed focus on formulating testable theories and explanations for the transition from foraging to food production has led to applications from subdisciplines of ecology, economy, and evolution not previously applied to agricultural origins. Most recently, the integration of formerly separated disciplines, such as developmental and evolutionary biology, is causing reconsiderations of how novel phenotypes, including domesticated species, originate and the influence of artificial selection on the domestication process. It is becoming clear that the more interesting question may be the origins of plant cultivation rather than the origins of agriculture. This paper reviews this body of evidence and assesses current views about how and why domestication and plant food production arose. C1 Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeol, Washington, DC 20560 USA. RP Piperno, DR (reprint author), Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeol, 10th St & Constitut Ave, Washington, DC 20560 USA. EM pipernod@si.edu NR 121 TC 46 Z9 47 U1 8 U2 62 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0011-3204 J9 CURR ANTHROPOL JI Curr. Anthropol. PD OCT PY 2011 VL 52 SU 4 BP S453 EP S470 DI 10.1086/659998 PG 18 WC Anthropology SC Anthropology GA 842NO UT WOS:000296606400019 ER PT J AU Smith, BD AF Smith, Bruce D. TI The Cultural Context of Plant Domestication in Eastern North America SO CURRENT ANTHROPOLOGY LA English DT Article ID MISSISSIPPI RIVER VALLEY; NICHE CONSTRUCTION; MIDDLE TENNESSEE; DATES; FIBS; SITE; BP AB The timing and sequence of the independent domestication of indigenous eastern North American seed plants (Cucurbita pepo, Helianthus annuus, Iva annua, Chenopodium berlandieri) and the subsequent development of a crop complex are discussed within a broader environmental and cultural context. The settlements that have yielded the earliest record of eastern domesticates are all small and situated in resource-rich lower-order river valley corridors within oak-savannah and oak-hickory forest regions. Well-preserved floral and faunal assemblages indicate continued substantial reliance on a wide range of wild species with no evidence of resource depletion. Similarly, there is no indication of landscape packing in terms of high site density in these resource-rich river valleys, calling into question developmental models of domestication and agricultural origins that rely on population pressure or resource imbalance as causal factors. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012, Washington, DC 20013 USA. EM smithb@si.edu NR 62 TC 15 Z9 15 U1 8 U2 31 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0011-3204 J9 CURR ANTHROPOL JI Curr. Anthropol. PD OCT PY 2011 VL 52 SU 4 BP S471 EP S484 DI 10.1086/659645 PG 14 WC Anthropology SC Anthropology GA 842NO UT WOS:000296606400020 ER PT J AU Zeder, MA AF Zeder, Melinda A. TI The Origins of Agriculture in the Near East SO CURRENT ANTHROPOLOGY LA English DT Article ID MITOCHONDRIAL-DNA ANALYSIS; BARLEY HORDEUM-VULGARE; DOMESTIC GOATS; PHYLOGEOGRAPHIC STRUCTURE; CATTLE DOMESTICATION; ANIMAL DOMESTICATION; WHEAT DOMESTICATION; NICHE CONSTRUCTION; TETRAPLOID WHEATS; PIG DOMESTICATION AB The emerging picture of plant and animal domestication and agricultural origins in the Near East is dramatically different from that drawn 16 years ago in a landmark article by Bar-Yosef and Meadow. While in 1995 there appeared to have been at least a 1,500-year gap between plant and animal domestication, it now seems that both occurred at roughly the same time, with initial management of morphologically wild future plant and animal domesticates reaching back to at least 11,500 cal BP, if not earlier. A focus on the southern Levant as the core area for crop domestication and diffusion has been replaced by a more pluralistic view that sees domestication of various crops and livestock occurring, sometimes multiple times in the same species, across the entire region. Morphological change can no longer be held to be a leading-edge indicator of domestication. Instead, it appears that a long period of increasingly intensive human management preceded the manifestation of archaeologically detectable morphological change in managed crops and livestock. Agriculture in the Near East arose in the context of broad-based systematic human efforts at modifying local environments and biotic communities to encourage plant and animal resources of economic interest. This process took place across the entire Fertile Crescent during a period of dramatic post-Pleistocene climate and environmental change with considerable regional variation in the scope and intensity of these activities as well as in the range of resources being manipulated. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, MRC 112, Washington, DC 20013 USA. EM zederm@si.edu NR 115 TC 82 Z9 82 U1 9 U2 83 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0011-3204 J9 CURR ANTHROPOL JI Curr. Anthropol. PD OCT PY 2011 VL 52 SU 4 BP S221 EP S235 DI 10.1086/659307 PG 15 WC Anthropology SC Anthropology GA 842NO UT WOS:000296606400006 ER PT J AU Soon, W Dutta, K Legates, DR Velasco, V Zhang, WJ AF Soon, Willie Dutta, Koushik Legates, David R. Velasco, Victor Zhang, WeiJia TI Variation in surface air temperature of China during the 20th century SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Total solar irradiance; Sunshine duration; Surface air temperature; Circum-global teleconnection ID ASIAN SUMMER MONSOON; NORTH-ATLANTIC OSCILLATION; SOLAR-RADIATION CHANGES; YANGTZE-RIVER VALLEY; LONG-TERM TREND; ATMOSPHERIC CIRCULATION; SUNSHINE DURATION; UNITED-STATES; TELECONNECTION PATTERNS; CLIMATE VARIABILITY AB The 20th century surface air temperature (SAT) records of China from various sources are analyzed using data which include the recently released Twentieth Century Reanalysis Project dataset. Two key features of the Chinese records are confirmed: (1) significant 1920s and 1940s warming in the temperature records, and (2) evidence for a persistent multidecadal modulation of the Chinese surface temperature records in co-variations with both incoming solar radiation at the top of the atmosphere as well as the modulated solar radiation reaching ground surface. New evidence is presented for this Sun-climate link for the instrumental record from 1880 to 2002. Additionally, two non-local physical aspects of solar radiation-induced modulation of the Chinese SAT record are documented and discussed. Teleconnections that provide a persistent and systematic modulation of the temperature response of the Tibetan Plateau and/or the tropospheric air column above the Eurasian continent (e.g., 30 degrees N-70 degrees N; 0 degrees-120 degrees E) are described. These teleconnections may originate from the solar irradiance-Arctic-North Atlantic overturning circulation mechanism proposed by Soon (2009). Also considered is the modulation of large-scale land-sea thermal contrasts both in terms of meridional and zonal gradients between the subtropical western Pacific and mid-latitude North Pacific and the continental landmass of China. The Circum-global teleconnection (CGT) pattern of summer circulation of Ding and Wang (2005) provides a physical framework for study of the Sun-climate connection over East Asia. Our results highlight the importance of solar radiation reaching the ground and the concomitant importance of changes in atmospheric transparency or cloudiness or both in motivating a true physical explanation of any Sun-climate connection. We conclude that ground surface solar radiation is an important modulating factor for Chinese SAT changes on multidecadal to centennial timescales. Therefore, a comprehensive view of local and remote factors of climate change in China must take account of this as well as other natural and anthropogenic forcings. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dutta, Koushik] Univ Minnesota, Large Lakes Observ, Duluth, MN 55812 USA. [Legates, David R.] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA. [Velasco, Victor] Univ Nacl Autonoma Mexico, Inst Geofis, Dept Invest Solares & Planetarias, Mexico City 04510, DF, Mexico. [Zhang, WeiJia] Peking Univ, Dept Phys, Beijing 100871, Peoples R China. RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wsoon@cfa.harvard.edu RI Dutta, Koushik/F-9371-2010; OI Dutta, Koushik/0000-0002-5976-7965; Velasco, Victor/0000-0002-0100-8878 NR 163 TC 19 Z9 21 U1 3 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD OCT PY 2011 VL 73 IS 16 BP 2331 EP 2344 DI 10.1016/j.jastp.2011.07.007 PG 14 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 849QY UT WOS:000297141400008 ER PT J AU Diaferio, A Ostorero, L Cardone, V AF Diaferio, Antonaldo Ostorero, Luisa Cardone, Vincenzo TI Gamma-ray bursts as cosmological probes: Lambda CDM vs. conformal gravity SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE modified gravity; gamma ray burst experiments; dark energy experiments; supernova type Ia - standard candles ID GALACTIC ROTATION CURVES; BAYES FACTORS; STANDARD CANDLES; MODEL SELECTION; DARK ENERGY; COSMIC ACCELERATION; HUBBLE DIAGRAM; IA SUPERNOVAE; LUMINOSITY; CONSTANT AB Lambda CDM, for the currently preferred cosmological density Omega(0) and cosmological constant Omega(Lambda), predicts that the Universe expansion decelerates from early times to redshift z approximate to 0.9 and accelerates at later times. On the contrary, the cosmological model based on conformal gravity predicts that the cosmic expansion has always been accelerating. To distinguish between these two very different cosmologies, we resort to gamma-ray bursts (GRBs), which have been suggested to probe the Universe expansion history at z > 1, where identified type Ia supernovae (SNe) are rare. We use the full Bayesian approach to infer the cosmological parameters and the additional parameters required to describe the GRB data available in the literature. For the first time, we use GRBs as cosmological probes without any prior information from other data. In addition, when we combine the GRB samples with SNe, our approach neatly avoids all the inconsistencies of most numerous previous methods that are plagued by the so-called circularity problem. In fact, when analyzed properly, current data are consistent with distance moduli of GRBs and SNe that can respectively be, in a variant of conformal gravity, similar to 15 and similar to 3 magnitudes fainter than in Lambda CDM. Our results indicate that the currently available SN and GRB samples are accommodated equally well by both Lambda CDM and conformal gravity and do not exclude a continuous accelerated expansion. We conclude that GRBs are currently far from being effective cosmological probes, as they are unable to distinguish between these two very different expansion histories. C1 [Diaferio, Antonaldo; Ostorero, Luisa] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. [Diaferio, Antonaldo; Ostorero, Luisa] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Diaferio, Antonaldo; Ostorero, Luisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ostorero, Luisa] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Ostorero, Luisa; Cardone, Vincenzo] Osserv Astron Roma, INAF, I-00040 Rome, Italy. RP Diaferio, A (reprint author), Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Via P Giuria 1, I-10125 Turin, Italy. EM diaferio@ph.unito.it; ostorero@ph.unito.it; winnyenodrac@gmail.com FU INFN [PD51]; PRIN-MIUR [2008NR3EBK_003]; L'OREAL-UNESCO; ASI [I/016/07/0 COFIS] FX We sincerely thank Johannes Buchner and Michael Gruberbauer for developing their superb code APEMoST and making it available to the community (apemost.sourceforge.net). We also are particularly grateful to Johannes Buchner and Stefano Andreon for intense and enlightening correspondence on Bayesian statistics. Stefano Andreon is also acknoweldged for a very stimulating seminar, delivered in Torino, on Bayesian statistics applied to astrophysics that inspired this work. We finally thank Margaret Geller, Xiao-Li Meng and the JCAP Editor, Carl Akerlof, for valuable suggestions on the presentation of our results. Support from the INFN grant PD51 and the PRIN-MIUR-2008 grant 2008NR3EBK_003 "Matter-antimatter asymmetry, dark matter and dark energy in the LHC era" is gratefully acknowledged. LO also acknowledges support from a 2009 National Fellowship "L'OREAL Italia Per le Donne e la Scienza" of the L'OREAL-UNESCO program "For Women in Science" and partial support from the ASI Contract No. I/016/07/0 COFIS. This research has made use of NASA's Astrophysics Data System. NR 87 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD OCT PY 2011 IS 10 AR 008 DI 10.1088/1475-7516/2011/10/008 PG 31 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 844SM UT WOS:000296767600008 ER PT J AU Xie, L Wen, J Li, LQ AF Xie, Lei Wen, Jun Li, Liang-Qian TI Phylogenetic Analyses of Clematis (Ranunculaceae) based on Sequences of Nuclear Ribosomal ITS and Three Plastid Regions SO SYSTEMATIC BOTANY LA English DT Article DE Clematis; divergence times; molecular phylogeny; Ranunculaceae; species radiation ID INDIAN-OCEAN BASIN; TIBETAN PLATEAU; POLYSCIAS ARALIACEAE; NORTHERN-HEMISPHERE; VASCULAR ANATOMY; DNA-SEQUENCES; BIOGEOGRAPHY; EVOLUTION; GENUS; CHLOROPLAST AB Clematis, a largely temperate genus of vines and lianas, consists of approximately 300 species. Based on a sampling of about 75 species, sequences of the nrITS, the plastid atpB-rbcL spacer, psbA-trnH-trnQ spacer, and rpoB-trnC spacer regions were analyzed using parsimony, maximum likelihood, and Bayesian inference methods. Analyses of the combined data set by the three methods yielded similar topologies. Previously recognized genera including Archiclematis and Naravelia are nested within Clematis, supporting the merging of these genera within Clematis. Ten major clades with various levels of support were detected in the combined analyses. Our results in general do not support previous infrageneric classifications based on morphological characters and suggest significant convergence in floral and vegetative characters in Clematis. Several clades were resolved as regional geographic groups. Bayesian dating suggests a relatively ancient origin of the genus in the Oligocene, yet a relatively recent species radiation of the crown Clematis in the Miocene. Geologic and climatic changes in the late Tertiary to Quaternary are perhaps important for the speciation of Clematis, especially in eastern Asia. Long-distance dispersal of the fruits by wind, water, and/or animals and strong environmental adaptability, are proposed as the main mechanisms for the current cosmopolitan distribution and high species diversity of Clematis. C1 [Xie, Lei; Wen, Jun; Li, Liang-Qian] Chinese Acad Sci, State Key Lab Systemat & Evolutionary Bot, Inst Bot, Beijing 100093, Peoples R China. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Wen, J (reprint author), Chinese Acad Sci, State Key Lab Systemat & Evolutionary Bot, Inst Bot, Beijing 100093, Peoples R China. EM wenj@si.edu; lqli@ibcas.ac.cn FU John D. and Catherine T. MacArthur Foundation; National Natural Science Foundation of China [30870146]; National Museum of Natural History; Smithsonian Institution FX We are grateful to Prof. Wang Wen-Tsai for identifying specimens and for his invaluable comments on the manuscript. We thank S. Manchester and C. Anderson for discussions of fossil records and calibration methods. This study was supported by the John D. and Catherine T. MacArthur Foundation (to J. Wen, R. Ree, and G. Mueller), the National Natural Science Foundation of China, Grant No. 30870146, the small grants of the National Museum of Natural History, and the endowment grants of the Smithsonian Institution. Laboratory work was conducted in the Laboratory of Analytical Biology of the National Museum of Natural History of the Smithsonian Institution. We are grateful to Elvira Horandl, Lawrence Janeway, and Quentin Luke for their kind assistance collecting tissue samples. NR 117 TC 18 Z9 20 U1 3 U2 25 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 2011 VL 36 IS 4 BP 907 EP 921 DI 10.1600/036364411X604921 PG 15 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 850GK UT WOS:000297182900010 ER PT J AU Smith, BC AF Smith, Barbara Clark TI Beyond the "Economic" SO WILLIAM AND MARY QUARTERLY LA English DT Article C1 Smithsonian Inst, Natl Museum Amer Hist, Div Polit Hist, Washington, DC 20560 USA. RP Smith, BC (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Div Polit Hist, Washington, DC 20560 USA. NR 6 TC 1 Z9 1 U1 0 U2 0 PU INST EARLY AMER HIST CULT PI WILLIAMSBURG PA BOX 220, WILLIAMSBURG, VA 23187 USA SN 0043-5597 J9 WILLIAM MARY QUART JI William Mary Q. PD OCT PY 2011 VL 68 IS 4 BP 639 EP 643 DI 10.5309/willmaryquar.68.4.0639 PG 5 WC History SC History GA 847QN UT WOS:000296987700009 ER PT J AU Wendler, I Huber, BT MacLeod, KG Wendler, JE AF Wendler, Ines Huber, Brian T. MacLeod, Kenneth G. Wendler, Jens E. TI EARLY EVOLUTIONARY HISTORY OF TUBULOGENERINA AND COLOMIA, WITH NEW SPECIES FROM THE TURONIAN OF EAST AFRICA SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID CARBON ISOTOPIC FRACTIONATION; LIVE BENTHIC FORAMINIFERA; SEDIMENTS AB Two new species, Tuhulogeneriaa turonica and Colomia africana, are described from the Turonian of Tanzania, and the genus Colomia is emended. The genus Tubulogenerina was originally thought to have originated in Europe in the early Eocene. Our discovery of T. turorrica indicates that the roots of the genus reach back to the middle Cretaceous, and argues against a previous conclusion that it originated in temperate European regions. A tropical/subtropical site of origination would be consistent with the observation that most Tuba logo:cram species inhabited warm, shallow-water environments. Tubulogenerina turonica has a relatively simple morphology, suitable as a starting point for morphological trends in the genus during the Cenozoic, thus supporting its status as a plausible ancestral species. In clay-rich middle Cretaceous sediments from Tanzania, foraminifera are exceptionally well preserved, and assemblages include a number of aragonitic taxa, including Colomia africana. This new species is distinguished from others of the genus by its aperture and toothplate structure and its dominantly biserial test without a well-developed uniserial growth stage. Morphologic similarities, however, indicate the close evolutionary relationship with other species of Colomia, so the genus is emended accordingly. Sufficient numbers of C. africana were found in multiple samples to characterize its stable carbon and oxygen isotope values relative to another aragonitic species (Epistomina chapmani) and calcitic species (Bertthelina berthelini) from the same material. Results show an expected offset between calcitic and aragonitic tests that is partially explained by differential fractionation factors, but suggests vital or microhabitat effects contribute to values measured on C. africana. C1 [Wendler, Ines; Wendler, Jens E.] Univ Bremen, Dept Geol Sci, D-28334 Bremen, Germany. [Wendler, Ines; Huber, Brian T.; Wendler, Jens E.] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [MacLeod, Kenneth G.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. RP Wendler, I (reprint author), Univ Bremen, Dept Geol Sci, POB 330 440, D-28334 Bremen, Germany. EM flatter@uni-bremen.de RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 FU Smithsonian Natural History Research Experiences Program; National Science Foundation [EAR 0642993]; Smithsonian Walcott Fund and Scholoarly Studies grants FX This paper benefitted from helpful comments and suggestions from Laia Alegret and an anonymous reviewer. We also thank Ken Finger and Mimi Katz for their editorial suggestions. The authors are very grateful for the assistance of Sarah Ehlinger, Carlos Rodriguez-Russo, Shannon Haynes, Carlos Peredo, and Joshua Johnson with foraminifer picking, we thank Erin Jacobs for her help with digital image editing, and we acknowledge the support of summer student internships from the Smithsonian Natural History Research Experiences Program. We also thank Tim Rose and the Smithsonian's Department of Mineral Sciences for access to their cathodoluminescene microscope. Fieldwork, drilling, and laboratory expenses were funded by a National Science Foundation grant to National Science Foundation grant to BTH and KGM (EAR 0642993) and Smithsonian Walcott Fund and Scholoarly Studies grants to BTH. NR 22 TC 10 Z9 11 U1 0 U2 3 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD OCT PY 2011 VL 41 IS 4 BP 384 EP 400 PG 17 WC Paleontology SC Paleontology GA 847AB UT WOS:000296943200007 ER PT J AU Thompson, JR Foster, DR Scheller, R Kittredge, D AF Thompson, Jonathan R. Foster, David R. Scheller, Robert Kittredge, David TI The influence of land use and climate change on forest biomass and composition in Massachusetts, USA SO ECOLOGICAL APPLICATIONS LA English DT Article DE aboveground biomass; climate change; current trends; forest carbon sequestration; future scenarios; Massachusetts; USA; landscape inertia; landscape simulation; land use legacies; old-growth forest ID NORTHEASTERN NORTH-AMERICA; LANDSCAPE SIMULATION-MODEL; EASTERN UNITED-STATES; NEW-ENGLAND; ABOVEGROUND BIOMASS; CANOPY NITROGEN; CARBON STORAGE; WATER YIELD; USE HISTORY; MANAGEMENT AB Land use and climate change have complex and interacting effects on naturally dynamic forest landscapes. To anticipate and adapt to these changes, it is necessary to understand their individual and aggregate impacts on forest growth and composition. We conducted a simulation experiment to evaluate regional forest change in Massachusetts, USA over the next 50 years (2010-2060). Our objective was to estimate, assuming a linear continuation of recent trends, the relative and interactive influence of continued growth and succession, climate change, forest conversion to developed uses, and timber harvest on live aboveground biomass (AGB) and tree species composition. We examined 20 years of land use records in relation to social and biophysical explanatory variables and used regression trees to create "probability-of-conversion" and "probability-of-harvest" zones. We incorporated this information into a spatially interactive forest landscape simulator to examine forest dynamics as they were affected by land use and climate change. We conducted simulations in a full-factorial design and found that continued forest growth and succession had the largest effect on AGB, increasing stores from 181.83 Tg to 309.56 Tg over 50 years. The increase varied from 49% to 112% depending on the ecoregion within the state. Compared to simulations with no climate or land use, forest conversion reduced gains in AGB by 23.18 Tg (or 18%) over 50 years. Timber harvests reduced gains in AGB by 5.23 Tg (4%). Climate change (temperature and precipitation) increased gains in AGB by 17.3 Tg (13.5%). Pinus strobus and Acer rubrum were ranked first and second, respectively, in terms of total AGB throughout all simulations. Climate change reinforced the dominance of those two species. Timber harvest reduced Quercus rubra from 10.8% to 9.4% of total AGB, but otherwise had little effect on composition. Forest conversion was generally indiscriminate in terms of species removal. Under the naive assumption that future land use patterns will resemble the recent past, we conclude that continued forest growth and recovery will be the dominant mechanism driving forest dynamics over the next 50 years, and that while climate change may enhance growth rates, this will be more than offset by land use, primarily forest conversion to developed uses. C1 [Thompson, Jonathan R.] Smithsonian Conservat Biol Inst, Smithsonian Inst, Front Royal, VA 22630 USA. [Thompson, Jonathan R.; Foster, David R.; Kittredge, David] Harvard Univ, Petersham, MA 01366 USA. [Scheller, Robert] Portland State Univ, Portland, OR 97207 USA. [Kittredge, David] Univ Massachusetts, Dept Nat Resource Conservat, Amherst, MA 01003 USA. RP Thompson, JR (reprint author), Smithsonian Conservat Biol Inst, Smithsonian Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM thompsonjr@si.edu RI Scheller, Robert/B-3135-2009 FU NSF [DEB-9411975] FX We thank Dunbar Carpenter for technical help. Funding for this research was provided by NSF Grant DEB-9411975 to the Harvard Forest, Long Term Ecological Research (LTER) program. NR 95 TC 48 Z9 50 U1 9 U2 79 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD OCT PY 2011 VL 21 IS 7 BP 2425 EP 2444 PG 20 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 836UP UT WOS:000296139200007 PM 22073633 ER PT J AU Blakeslee, AMH Canning-Clode, J Lind, EM Quilez-Badia, G AF Blakeslee, April M. H. Canning-Clode, Joao Lind, Eric M. Quilez-Badia, Gemma TI Biological invasions in the 21st century: Ecological impacts, predictions, and management across land and sea Introduction SO ENVIRONMENTAL RESEARCH LA English DT Editorial Material C1 [Blakeslee, April M. H.] Long Isl Univ, Dept Biol, Brookville, NY USA. [Blakeslee, April M. H.; Canning-Clode, Joao; Lind, Eric M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Canning-Clode, Joao] CIMAR CIIMAR Ctr Marine & Environm Res, Oporto, Portugal. [Lind, Eric M.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Quilez-Badia, Gemma] World Wildlife Fund Nat Mediterranean Program Off, Barcelona, Spain. RP Blakeslee, AMH (reprint author), Long Isl Univ, Dept Biol, CW Post Campus, Brookville, NY USA. EM April.Blakeslee@liu.edu RI Canning Clode, Joao/G-5142-2011; Scientific output, CIIMAR/E-5122-2012 OI Canning Clode, Joao/0000-0003-2143-6535; Scientific output, CIIMAR/0000-0001-6270-2153 NR 6 TC 0 Z9 0 U1 0 U2 15 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0013-9351 J9 ENVIRON RES JI Environ. Res. PD OCT PY 2011 VL 111 IS 7 SI SI BP 891 EP 892 DI 10.1016/j.envres.2011.09.005 PG 2 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA 830LY UT WOS:000295659700001 PM 21958957 ER PT J AU McKenzie, LA Brooks, R Johnston, EL AF McKenzie, Louise A. Brooks, Rob Johnston, Emma L. TI Heritable pollution tolerance in a marine invader SO ENVIRONMENTAL RESEARCH LA English DT Article DE Non-indigenous species; Copper; Offspring size; Maternal provisioning; Heavy metal pollution ID POLYCHAETE NEREIS-DIVERSICOLOR; ECOLOGICAL TIME-SCALES; LIFE-HISTORY; HEAVY-METALS; WATERSIPORA-SUBTORQUATA; CONTAMINATED ESTUARIES; DIFFERENTIAL TOLERANCE; PHENOTYPIC PLASTICITY; ANTIFOULING PAINT; RAPID EVOLUTION AB The global spread of fouling invasive species is continuing despite the use of antifouling biocides. Furthermore, previous evidence suggests that non-indigenous species introduced via hull fouling may be capable of adapting to metal-polluted environments. Using a laboratory based toxicity assay, we investigated tolerance to copper in the non-indigenous bryozoan Watersipora subtorquata from four source populations. Individual colonies were collected from four sites within Port Hacking (Sydney, Australia) and their offspring exposed to a range of copper concentrations. This approach, using a fullsib, split-family design, tests for a genotype by environment (G x E) interaction. Settlement and complete metamorphosis (recruitment) were measured as ecologically relevant endpoints. Larval sizes were also measured for each colony. Successful recruitment was significantly reduced by the highest copper concentration of 80 mu g L(-1). While there was no difference in pollution tolerance between sites, there was a significant G x E interaction, with large variation in the response of colony offspring within sites. Larval size differed significantly both between sites and between colonies and was positively correlated with tolerance. The high level of variation in copper tolerance between colonies suggests that there is considerable potential within populations to adapt to elevated copper levels, as tolerance is a heritable trait. Also, colonies that produce large larvae are more tolerant to copper, suggesting that tolerance may be a direct consequence of larger size. (C) 2011 Elsevier Inc. All rights reserved. C1 Univ New S Wales, Evolut & Ecol Res Ctr, Sydney, NSW 2052, Australia. Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. RP McKenzie, LA (reprint author), Smithsonian Environm Res Ctr, Marine Invas Lab, POB 28, Edgewater, MD 21037 USA. EM mckenziel@si.edu.au; rob.brooks@unsw.edu.au; e.johnston@unsw.edu.au RI Brooks, Robert/A-1251-2008; Johnston, Emma/B-7210-2009 OI Brooks, Robert/0000-0001-6926-0781; Johnston, Emma/0000-0002-2117-366X FU Australian Government; Australian Research Council FX We are grateful to Subtidal Ecology and Ecotoxicology laboratory members for assistance in the field. The authors were supported by the Australian Government and Australian Research Council through Research Fellowships, Postgraduate Awards and Grants. We thank Alistair Poore for comments which improved earlier draughts of this article. NR 83 TC 11 Z9 11 U1 1 U2 48 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0013-9351 J9 ENVIRON RES JI Environ. Res. PD OCT PY 2011 VL 111 IS 7 SI SI BP 926 EP 932 DI 10.1016/j.envres.2010.12.007 PG 7 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA 830LY UT WOS:000295659700006 PM 21295292 ER PT J AU Bisson, IA Butler, LK Hayden, TJ Kelley, P Adelman, JS Romero, LM Wikelski, MC AF Bisson, I. -A. Butler, L. K. Hayden, T. J. Kelley, P. Adelman, J. S. Romero, L. M. Wikelski, M. C. TI Energetic response to human disturbance in an endangered songbird SO ANIMAL CONSERVATION LA English DT Article DE human disturbance; heart rate telemetry; energy expenditure; endangered songbirds; fast life histories; vireo ID HEART-RATE; ADRENOCORTICAL RESPONSES; STRESS-RESPONSE; EXPENDITURE; PENGUINS; BEHAVIOR; BIRDS; REPRODUCTION; METABOLISM; TELEMETRY AB Physiological changes in response to environmental stressors can reveal cryptic effects of disturbance that can potentially lead to species decline. However, such responses may vary with life history. We used heart rate telemetry to continuously and instantaneously measure energy expenditure in response to human-mediated disturbance in a free-living breeding population of the endangered [International Union for Conservation of Nature, vulnerable] black-capped vireo Vireo atricapilla (n = 10). Heart rate predicted 84% of energy expenditure as determined by respirometry (n = 3). Each bird mounted with a 0.5 g heart rate transmitter were subjected to standardized disturbance trials for 1 or 4 h during the day, and for 1 h at night. Only 1-h daytime disturbances elicited an increase in heart rate but this was not significant when compared with control no-disturbance periods. Our findings suggest that black-capped vireos quickly acclimate to a limited amount of human disturbance during the breeding season, which may be an adaptive response for any 'fast-living' species with a short life span and a short and synchronized breeding season. Because similar results were reported for another fast-living species, the common white-eyed vireo Vireo griseus, we suggest that life-history traits are stronger predictors of short-term physiological responses to disturbances than population status. C1 [Bisson, I. -A.; Adelman, J. S.; Wikelski, M. C.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Butler, L. K.; Romero, L. M.] Tufts Univ, Dept Biol, Medford, MA 02155 USA. [Hayden, T. J.] Engineer Res & Dev Ctr, Champaign, IL USA. [Kelley, P.] Severn Elect, Annapolis, MD USA. RP Bisson, IA (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, POB 37102,MRC 5503, Washington, DC 20013 USA. EM BissonI@si.edu RI Kelley, Paul/C-9155-2016 FU Department of Defense through the US Army Corps of Engineers, Engineer Research and Development Center [CS-1396, W9132T-05-C-0023] FX We thank J.L. Granger, S. Lovell, A. Whitley, J. Ferrer, C. Pekins, D. Cimprich, The Nature Conservancy (Fort Hood Chapter) and the Fort Hood Natural Resources Management Branch for their assistance in the field. We are also grateful for valuable comments on the paper from two anonymous reviewers. This project was supported by the Department of Defense, Strategic Environmental Research and Development Program, Project CS-1396, through the US Army Corps of Engineers, Engineer Research and Development Center, contract #W9132T-05-C-0023. Research activities were conducted in accordance with all applicable Federal and State of Texas wildlife and endangered species permits. NR 44 TC 5 Z9 5 U1 2 U2 24 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD OCT PY 2011 VL 14 IS 5 BP 484 EP 491 DI 10.1111/j.1469-1795.2011.00447.x PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 846JX UT WOS:000296894900006 ER PT J AU Bel, MC Rodriguez, J D'Avanzo, P Russell, DM Tomsick, J Corbel, S Lewis, FW Rahoui, F Buxton, M Goldoni, P Kuulkers, E AF Bel, M. Cadolle Rodriguez, J. D'Avanzo, P. Russell, D. M. Tomsick, J. Corbel, S. Lewis, F. W. Rahoui, F. Buxton, M. Goldoni, P. Kuulkers, E. TI Overview of an extensive multi-wavelength study of GX 339-4 during the 2010 outburst SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE black hole physics; stars: individual: GX 339-4; gamma rays: general; X-rays: binaries; infrared: general; radio continuum: general ID X-RAY BINARIES; BLACK-HOLE BINARIES; HIGH-ENERGY OBSERVATIONS; LOW/HARD STATE; GAMMA-RAY; ACCRETION DISK; COMPACT JET; LOW-LUMINOSITY; XTE J1550-564; LIGHT CURVES AB Context. The microquasar GX 339-4 experienced a new outburst in 2010: it was observed simultaneously at various wavelengths from radio up to soft gamma-rays. We focus on observations that are quasi-simultaneous with those made with the INTEGRAL and RXTE satellites: these were collected in 2010 March-April during our INTEGRAL target of opportunity programme, and during some of the other INTEGRAL observing programmes with GX 339-4 in the field-of-view. Aims. X-ray transients are extreme systems that often harbour a black hole, and are known to emit throughout the whole electromagnetic spectrum when in outburst. The goals of our programme are to understand the evolution of the physical processes close to the black hole and to study the connections between the accretion and ejection. Methods. We analysed radio, NIR, optical, UV, X-ray and soft gamma-ray observations. We studied the source evolution in detail by producing light curves, hardness-intensity diagrams and spectra. We fitted the broadband data with phenomenological, then physical, models to study the emission coming from the distinct components. Results. Based on the energy spectra, the source evolved from the canonical hard state to the canonical soft state. The source showed X-ray spectral variations that were correlated with changes in radio, NIR and optical emission. The bolometric flux increased from 0.8 to 2.9 x 10(-8) erg cm(-2) s(-1) while the relative flux and contribution of the hot medium decreased on the average. Reprocessing in the disc was likely to be strong at the end of our observations. Conclusions. The source showed a behaviour similar to that of previous outbursts, with some small deviations in the hard X-ray parameter evolution. The radio, NIR and optical emission from jets was detected and observed to fade as the source softened. The results are discussed within the context of disc and jet models. C1 [Bel, M. Cadolle; Kuulkers, E.] ISOC, ESAC, Madrid, Spain. [Rodriguez, J.; Corbel, S.] Univ Paris Diderot, CNRS, UMR 7158, Lab AIM,CEA DSM,IRFU SAp, Gif Sur Yvette, France. [D'Avanzo, P.] Osserv Astron Brera, INAF, Merate, Italy. [Russell, D. M.] Univ Amsterdam, Anton Pannekoek Inst, NL-1012 WX Amsterdam, Netherlands. [Tomsick, J.] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA. [Lewis, F. W.] Univ Glamorgan, Faulkes Telescope Project, Pontypridd CF37 1DL, M Glam, Wales. [Rahoui, F.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Rahoui, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Buxton, M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Goldoni, P.] Univ Paris Diderot, IRFU SAp, CNRS, UMR 7164,Lab APC,CEA DSM, Paris, France. RP Bel, MC (reprint author), ISOC, ESAC, Madrid, Spain. EM Marion.Cadolle@sciops.esa.int OI Rodriguez, Jerome/0000-0002-4151-4468 FU ESA member states; Faculty of the European Space Astronomy Center (ESAC); European Community [ITN 215212]; NASA [NNX08AW35G] FX We thank the referee for his/her helpful comments that improved our manuscript. We thank the INTEGRAL, Swift and RXTE mission planners for programming the ToO observations described in the paper. The present work is partly based on observations with INTEGRAL, and ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), and Poland, and with the participation of Russia and the USA, and on observations with RXTE. The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M.C.B. acknowledges support from the Faculty of the European Space Astronomy Center (ESAC) and L. Prat's comments. JR acknowledges partial funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement number ITN 215212 "Black Hole Universe". JAT acknowledges partial support from NASA under Swift Guest Observer grant NNX08AW35G. The FT North and South are maintained and operated by Las Cumbres Observatory Global Telescope Network. This research has made use of the NASA Astrophysics Data System Abstract Service and of the SIMBAD database, operated at the CDS, Strasbourg, France. NR 92 TC 18 Z9 18 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 OCT PY 2011 VL 534 AR A119 DI 10.1051/0004-6361/201117684 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 841ZS UT WOS:000296554800136 ER PT J AU Ferrari, C Intema, HT Orru, E Govoni, F Murgia, M Mason, B Bourdin, H Asad, KM Mazzotta, P Wise, MW Mroczkowski, T Croston, JH AF Ferrari, C. Intema, H. T. Orru, E. Govoni, F. Murgia, M. Mason, B. Bourdin, H. Asad, K. M. Mazzotta, P. Wise, M. W. Mroczkowski, T. Croston, J. H. TI Discovery of the correspondence between intra-cluster radio emission and a high pressure region detected through the Sunyaev-Zel'dovich effect SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: RX J1347-1145; radio continuum: galaxies; X-rays: galaxies: clusters; cosmic background radiation ID GALAXY CLUSTERS; RX J1347.5-1145; PARTICLE REACCELERATION; SHOCK-WAVES; SKY SURVEY; CORE; PLASMA; HALOS; GAS AB We analyzed new 237 MHz and 614 MHz GMRT data of the most X-ray luminous galaxy cluster, RXJ1347-1145. Our radio results are compared with the MUSTANG 90 GHz Sunyaev-Zel'dovich effect map and with re-processed Chandra and XMM-Newton archival data of this cluster. We point out for the first time in an unambiguous way the correspondence between a radio excess in a diffuse intra-cluster radio source and a hot region detected through both Sunyaev-Zel'dovich effect and X-ray observations. Our result indicates that electron re-acceleration in the excess emission of the radio mini-halo at the center of RXJ1347-1145 is most likely related to a shock front propagating into the intra-cluster medium. C1 [Ferrari, C.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Cassiopee, Nice, France. [Intema, H. T.; Mason, B.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Orru, E.] Radboud Univ Nijmegen, NL-6525 AJ Nijmegen, Netherlands. [Govoni, F.; Murgia, M.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Ca, Italy. [Bourdin, H.; Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Mazzotta, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wise, M. W.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Mroczkowski, T.] Univ Penn, Philadelphia, PA 19104 USA. [Mroczkowski, T.] NASA, Washington, DC USA. [Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Ferrari, C (reprint author), Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Cassiopee, Nice, France. EM chiara.ferrari@oca.eu RI Mazzotta, Pasquale/B-1225-2016; OI Mroczkowski, Tony/0000-0003-3816-5372; Mazzotta, Pasquale/0000-0002-5411-1748; Murgia, Matteo/0000-0002-4800-0806; Govoni, Federica/0000-0003-3644-3084 FU Agence Nationale de la Recherche [ANR-09-JCJC-0001-01]; BQR program of Observatoire de la Cote d'Azur; Laboratoire Cassiopee [UMR 6202] FX We thank the anonymous referee for her/his useful comments. We are grateful to Giulia Macario for helpful suggestions in the radio data reduction phase. We warmly thank Monique Arnaud for very useful discussions. We would like to thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. CF acknowledges financial support by the "Agence Nationale de la Recherche" through grant ANR-09-JCJC-0001-01. This work was supported by the BQR program of Observatoire de la Cote d'Azur and by Laboratoire Cassiopee (UMR 6202). NR 27 TC 8 Z9 8 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 OCT PY 2011 VL 534 AR L12 DI 10.1051/0004-6361/201117788 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 841ZS UT WOS:000296554800146 ER PT J AU Jorgensen, JK Bourke, TL Luong, QN Takakuwa, S AF Jorgensen, J. K. Bourke, T. L. Luong, Q. Nguyen Takakuwa, S. TI Arcsecond resolution images of the chemical structure of the low-mass protostar IRAS 16293-2422 An overview of a large molecular line survey from the Submillimeter Array SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE circumstellar matter; ISM: molecules; stars: formation; ISM: jets and outflows; submillimeter: ISM; ISM: individual objects: IRAS 16293-2422 ID STAR-FORMATION; HOT CORE; COLOGNE DATABASE; IRAS-16293-2422; ENVELOPES; ABUNDANCES; EVOLUTION; SPECTROSCOPY; CHEMISTRY; OUTFLOWS AB It remains a key challenge to establish the molecular content of different components of low-mass protostars, like their envelopes and disks, and how this depends on the evolutionary stage and/or environment of the young stars. Observations at submillimeter wavelengths provide a direct possibility to study the chemical composition of low-mass protostars through transitions probing temperatures up to a few hundred K in the gas surrounding these sources. This paper presents a large molecular line survey of the deeply embedded protostellar binary IRAS 16293-2422 from the Submillimeter Array (SMA) - including images of individual lines down to approximate to 1.5- 3" (190-380 AU) resolution. More than 500 individual transitions are identified related to 54 molecular species (including isotopologues) probing temperatures up to about 550 K. Strong chemical differences are found between the two components in the protostellar system with a separation between, in particular, the sulfur- and nitrogen-bearing species and oxygen-bearing complex organics. The action of protostellar outflow on the ambient envelope material is seen in images of CO and SiO and appear to influence a number of other species, including (deuterated) water, HDO. The effects of cold gas-phase chemistry is directly imaged through maps of CO, N2D+ and DCO+, showing enhancements of first DCO+ and subsequently N2D+ in the outer envelope where CO freezes-out on dust grains. C1 [Jorgensen, J. K.] Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, DK-2100 Copenhagen O, Denmark. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark. [Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Luong, Q. Nguyen] IRFU Serv Astrophys, CEA DSM, Lab AIM, F-91191 Gif Sur Yvette, France. [Luong, Q. Nguyen] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Takakuwa, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. RP Jorgensen, JK (reprint author), Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. EM jeskj@nbi.dk FU Smithsonian Institution; Lundbeck foundation; Danish National Research Foundation; University of Copenhagen; Bonn International Graduate School of Physics and Astronomy (BIGS); Argelander Institut fur Astronomie; Academia Sinica FX We would like to thank the anonymous referee for a number of good suggestions helping to improve the presentation of this survey. This paper is based on data from the Submillimeter Array: the Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. It is a pleasure to thank everybody involved with the Submillimeter Array for the continued development of this observatory. The research of J.K.J. was supported by a Junior Group Leader Fellowship from the Lundbeck foundation. Research at Centre for Star and Planet Formation is funded by the Danish National Research Foundation and the University of Copenhagen's programme of excellence. Quang Nguyen Luong's research at Bonn University was supported by a M.Sc. fellowship from Bonn International Graduate School of Physics and Astronomy (BIGS) and Argelander Institut fur Astronomie. NR 39 TC 28 Z9 28 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 OCT PY 2011 VL 534 AR A100 DI 10.1051/0004-6361/201117139 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 841ZS UT WOS:000296554800060 ER PT J AU Kaastra, JS Petrucci, PO Cappi, M Arav, N Behar, E Bianchi, S Bloom, J Blustin, AJ Branduardi-Raymont, G Costantini, E Dadina, M Detmers, RG Ebrero, J Jonker, PG Klein, C Kriss, GA Lubinski, P Malzac, J Mehdipour, M Paltani, S Pinto, C Ponti, G Ratti, EM Smith, RAN Steenbrugge, KC de Vries, CP AF Kaastra, J. S. Petrucci, P-O. Cappi, M. Arav, N. Behar, E. Bianchi, S. Bloom, J. Blustin, A. J. Branduardi-Raymont, G. Costantini, E. Dadina, M. Detmers, R. G. Ebrero, J. Jonker, P. G. Klein, C. Kriss, G. A. Lubinski, P. Malzac, J. Mehdipour, M. Paltani, S. Pinto, C. Ponti, G. Ratti, E. M. Smith, R. A. N. Steenbrugge, K. C. de Vries, C. P. TI Multiwavelength campaign on Mrk 509 I. Variability and spectral energy distribution SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; quasars: absorption lines; X-rays: general ID ACTIVE GALACTIC NUCLEI; GALAXY MARKARIAN 509; X-RAY SPECTROSCOPY; REFLECTION GRATING SPECTROMETER; QUASAR OUTFLOW CONTRIBUTION; SEYFERT TYPE-1 GALAXIES; EMISSION-LINE SPECTRA; XMM-NEWTON; ABSORPTION-LINES; PHYSICAL CONDITIONS AB Context. Active galactic nuclei (AGN) show a wealth of interesting physical processes, some of which are poorly understood. In a broader context, they play an important role in processes that are far beyond their immediate surroundings, owing to the high emitted power. Aims. We want to address a number of open questions, including the location and physics of the outflow from AGN, the nature of the continuum emission, the geometry and physical state of the X-ray broad emission line region, the Fe-K line complex, the metal abundances of the nucleus, and finally the interstellar medium of our own Galaxy as seen through the signatures it imprints on the X-ray and UV spectra of AGN. Methods. We study one of the best targets for these aims, the Seyfert 1 galaxy Mrk 509 with a multiwavelength campaign using five satellites (XMM-Newton, INTEGRAL, Chandra, HST, and Swift) and two ground-based facilities (WHT and PAIRITEL). Our observations cover more than five decades in frequency, from 2 mu m to 200 keV. The combination of high-resolution spectroscopy and time variability allows us to disentangle and study the different components. Our campaign covers 100 days from September to December 2009, and is centred on a simultaneous set of deep XMM-Newton and INTEGRAL observations with regular time intervals, spanning seven weeks. Results. We obtain a continuous light curve in the X-ray and UV band, showing a strong, up to 60% flux increase in the soft X-ray band during the three weeks in the middle of our deepest monitoring campaign, and which is correlated with an enhancement of the UV flux. This allows us to study the time evolution of the continuum and the outflow. By stacking the observations, we have also obtained one of the best X-ray and UV spectra of a Seyfert galaxy ever obtained. In this paper we also study the effects of the spectral energy distribution (SED) that we obtained on the photo-ionisation equilibrium. Thanks to our broad-band coverage, uncertainties on the SED do not strongly affect the determination of this equilibrium. Conclusions. Here we present our very successful campaign and in a series of subsequent papers we will elaborate on different aspects of our study. C1 [Kaastra, J. S.; Costantini, E.; Detmers, R. G.; Ebrero, J.; Jonker, P. G.; Pinto, C.; Ratti, E. M.; de Vries, C. P.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Kaastra, J. S.; Detmers, R. G.] Univ Utrecht, Sterrenkundig Inst, NL-3508 TA Utrecht, Netherlands. [Petrucci, P-O.] CNRS INSU, UMR 5274, IPAG, UJF Grenoble 1, F-38041 Grenoble, France. [Cappi, M.; Dadina, M.] INAF IASF Bologna, I-40129 Bologna, Italy. [Arav, N.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Behar, E.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Bianchi, S.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Bloom, J.; Klein, C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Blustin, A. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Branduardi-Raymont, G.; Mehdipour, M.; Smith, R. A. N.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Kriss, G. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lubinski, P.] Ctr Astron M Kopernika, PL-87100 Torun, Poland. [Malzac, J.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Malzac, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Paltani, S.] Univ Geneva, Astron Observ, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Ponti, G.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Steenbrugge, K. C.] Univ Catolica Norte, Inst Astron, Antofagasta, Chile. [Steenbrugge, K. C.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Kaastra, JS (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM j.s.kaastra@sron.nl RI Bianchi, Stefano/B-4804-2010; Cappi, Massimo/F-4813-2015; OI Bianchi, Stefano/0000-0002-4622-4240; Cappi, Massimo/0000-0001-6966-8920; Dadina, Mauro/0000-0002-7858-7564 FU ESA Member States; USA (NASA); NWO, the Netherlands Organization for Scientific Research; CNES; French GDR PCHE; ASI-INAF [I/088/06/0]; NASA/XMM [NNX09AR01G]; NASA through Space Telescope Science Institute; ISF; STFC; Polish MNiSW [NN203065933, 362/1/N-INTEGRAL/2008/09/0]; UK Science & Technology Facilities Council (STFC); EU [FP7-PEOPLE-2009-IEF-254279]; Comite Mixto ESO - Gobierno de Chile; NASA [NAS5-26555] FX This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). It is also based on observations with INTEGRAL, an ESA project with instrument and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic, and Poland and with the participation of Russia and the USA. This work made use of data supplied by the UK Swift Science Data Centre at the University if Leicester. SRON is supported financially by NWO, the Netherlands Organization for Scientific Research. J.S. Kaastra thanks the PI of Swift, Neil Gehrels, for approving the TOO observations, and the duty scientists at the William Herschel Telescope for performing the service observations. P.-O. Petrucci acknowledges financial support from CNES and the French GDR PCHE. M. Cappi, M. Dadina, S. Bianchi, and G. Ponti acknowledge financial support from contract ASI-INAF n. I/088/06/0. N. Arav and G. Kriss gratefully acknowledge support from NASA/XMM-Newton Guest Investigator grant NNX09AR01G. Support for HST Program number 12022 was provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. E. Behar was supported by a grant from the ISF. A. Blustin acknowledges the support of a STFC Postdoctoral Fellowship. P. Lubinski has been supported by the Polish MNiSW grants NN203065933 and 362/1/N-INTEGRAL/2008/09/0. M. Mehdipour acknowledges the support of a PhD studentship awarded by the UK Science & Technology Facilities Council (STFC). G. Ponti acknowledges support via an EU Marie Curie Intra-European Fellowship under contract No. FP7-PEOPLE-2009-IEF-254279. K. Steenbrugge acknowledges the support of Comite Mixto ESO - Gobierno de Chile. NR 132 TC 31 Z9 31 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 OCT PY 2011 VL 534 AR A36 DI 10.1051/0004-6361/201116869 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 841ZS UT WOS:000296554800029 ER PT J AU Lusso, E Comastri, A Vignali, C Zamorani, G Treister, E Sanders, D Bolzonella, M Bongiorno, A Brusa, M Civano, F Gilli, R Mainieri, V Nair, P Aller, MC Carollo, M Koekemoer, AM Merloni, A Trump, JR AF Lusso, E. Comastri, A. Vignali, C. Zamorani, G. Treister, E. Sanders, D. Bolzonella, M. Bongiorno, A. Brusa, M. Civano, F. Gilli, R. Mainieri, V. Nair, P. Aller, M. C. Carollo, M. Koekemoer, A. M. Merloni, A. Trump, J. R. TI The bolometric output and host-galaxy properties of obscured AGN in the XMM-COSMOS survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: statistical; quasars: general; galaxies: active; Galaxy: general; X-rays: general ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES; WIDE-FIELD SURVEY; SPECTRAL ENERGY-DISTRIBUTION; HUBBLE-SPACE-TELESCOPE; X-RAY-EMISSION; SIMILAR-TO 1; LUMINOSITY FUNCTION; MAGNITUDE RELATION AB We present a study of the multi-wavelength properties, from the mid-infrared to the hard X-rays, of a sample of 255 spectroscopically identified X-ray selected type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) are computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. We calculate bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using a multi-component modeling to properly disentangle the emission associated to stellar light from that due to black hole accretion. For 90% of the sample we also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). We find that on average type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, we confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10(10) solar masses. C1 [Lusso, E.; Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Lusso, E.; Comastri, A.; Vignali, C.; Zamorani, G.; Bolzonella, M.; Gilli, R.; Nair, P.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Treister, E.; Sanders, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Bongiorno, A.; Brusa, M.; Merloni, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Merloni, A.] TUM, D-85748 Garching, Germany. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mainieri, V.] ESO, D-85748 Garching, Germany. [Aller, M. C.; Carollo, M.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Trump, J. R.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Lusso, E (reprint author), Univ Bologna, Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy. EM elisabeta.lusso2@unibo.it RI Vignali, Cristian/J-4974-2012; Bolzonella, Micol/O-9495-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Zamorani, Giovanni/0000-0002-2318-301X; Koekemoer, Anton/0000-0002-6610-2048; Vignali, Cristian/0000-0002-8853-9611; Bolzonella, Micol/0000-0003-3278-4607; Brusa, Marcella/0000-0002-5059-6848; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Bongiorno, Angela/0000-0002-0101-6624 FU ASI-INAF [I/009/10/0, I/088/06, ASI/COFIS/WP3110I/026/07/0]; Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur Luft und Raumfahrt; Max-Planck society; NASA [PF8-90055, NAS8-03060]; University of Bologna FX We gratefully thank B. Simmons for her useful comments and suggestions. In Italy, the XMM-COSMOS project is supported by ASI-INAF grants I/009/10/0, I/088/06 and ASI/COFIS/WP3110I/026/07/0. Elisabeta Lusso gratefully acknowledges financial support from the Marco Polo program, University of Bologna. In Germany the XMM-Newton project is supported by the Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur Luft und Raumfahrt and the Max-Planck society. Support for the work of E.T. was provided by NASA through Chandra Postdoctoral Fellowship Award grant number PF8-90055, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. The entire COSMOS collaboration is gratefully acknowledged. NR 88 TC 30 Z9 30 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2011 VL 534 AR A110 DI 10.1051/0004-6361/201117175 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 841ZS UT WOS:000296554800064 ER PT J AU Raiteri, CM Villata, M Aller, MF Gurwell, MA Kurtanidze, OM Lahteenmaki, A Larionov, VM Romano, P Vercellone, S Agudo, I Aller, HD Arkharov, AA Bach, U Benitez, E Berdyugin, A Blinov, DA Borisova, EV Bottcher, M Calle, OJAB Buemi, CS Calcidese, P Carosati, D Casas, R Chen, WP Efimova, NV Gomez, JL Gusbar, C Hawkins, K Heidt, J Hiriart, D Hsiao, HY Jordan, B Jorstad, SG Joshi, M Kimeridze, GN Koptelova, E Konstantinova, TS Kopatskaya, EN Kurtanidze, SO Larionova, EG Larionova, LV Leto, P Li, Y Ligustri, R Lindfors, E Lister, M Marscher, AP Molina, SN Morozova, DA Nieppola, E Nikolashvili, MG Nilsson, K Palma, N Pasanen, M Reinthal, R Roberts, V Ros, JA Roustazadeh, P Sadun, AC Sakamoto, T Schwartz, RD Sigua, LA Sillanpaa, A Takalo, LO Tammi, J Taylor, B Tornikoski, M Trigilio, C Troitsky, IS Umana, G Volvach, A Yuldasheva, TA AF Raiteri, C. M. Villata, M. Aller, M. F. Gurwell, M. A. Kurtanidze, O. M. Lahteenmaki, A. Larionov, V. M. Romano, P. Vercellone, S. Agudo, I. Aller, H. D. Arkharov, A. A. Bach, U. Benitez, E. Berdyugin, A. Blinov, D. A. Borisova, E. V. Casas, R. Calle, O. J. A. Bravo Buemi, C. S. Calcidese, P. Carosati, D. Casas, R. Chen, W-P. Efimova, N. V. Gomez, J. L. Gusbar, C. Hawkins, K. Heidt, J. Hiriart, D. Hsiao, H. Y. Jordan, B. Jorstad, S. G. Joshi, M. Kimeridze, G. N. Koptelova, E. Konstantinova, T. S. Kopatskaya, E. N. Kurtanidze, S. O. Larionova, E. G. Larionova, L. V. Leto, P. Li, Y. Ligustri, R. Lindfors, E. Lister, M. Marscher, A. P. Molina, S. N. Morozova, D. A. Nieppola, E. Nikolashvili, M. G. Nilsson, K. Palma, N. Pasanen, M. Reinthal, R. Roberts, V. Ros, J. A. Roustazadeh, P. Sadun, A. C. Sakamoto, T. Schwartz, R. D. Sigua, L. A. Sillanpaa, A. Takalo, L. O. Tammi, J. Taylor, B. Tornikoski, M. Trigilio, C. Troitsky, I. S. Umana, G. Volvach, A. Yuldasheva, T. A. TI The long-lasting activity of 3C 454.3 GASP-WEBT and satellite observations in 2008-2010 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; quasars: general; quasars: individual: 3C 454.3; galaxies: jets ID SPACE-TELESCOPE OBSERVATIONS; GAMMA-RAY FLARE; GALACTIC NUCLEI; BL-LACERTAE; BLAZAR 3C-454.3; MULTIWAVELENGTH OBSERVATIONS; INFRARED OBSERVATIONS; RADIO VARIABILITY; AGILE DETECTION; CRAZY-DIAMOND AB Context. The blazar 3C 454.3 is one of the most active sources from the radio to the gamma-ray frequencies observed in the past few years. Aims. We present multiwavelength observations of this source from April 2008 to March 2010. The radio to optical data are mostly from the GASP-WEBT, UV and X-ray data from Swift, and gamma-ray data from the AGILE and Fermi satellites. The aim is to understand the connection among emissions at different frequencies and to derive information on the emitting jet. Methods. Light curves in 18 bands were carefully assembled to study flux variability correlations. We improved the calibration of optical-UV data from the UVOT and OM instruments and estimated the Ly alpha flux to disentangle the contributions from different components in this spectral region. Results. The observations reveal prominent variability above 8 GHz. In the optical-UV band, the variability amplitude decreases with increasing frequency due to a steadier radiation from both a broad line region and an accretion disc. The optical flux reaches nearly the same levels in the 2008-2009 and 2009-2010 observing seasons; the mm one shows similar behaviour, whereas the gamma and X-ray flux levels rise in the second period. Two prominent gamma-ray flares in mid 2008 and late 2009 show a double-peaked structure, with a variable gamma/optical flux ratio. The X-ray flux variations seem to follow the gamma-ray and optical ones by about 0.5 and 1 d, respectively. Conclusions. We interpret the multifrequency behaviour in terms of an inhomogeneous curved jet, where synchrotron radiation of increasing wavelength is produced in progressively outer and wider jet regions, which can change their orientation in time. In particular, we assume that the long-term variability is due to this geometrical effect. By combining the optical and mm light curves to fit the gamma and X-ray ones, we find that the gamma (X-ray) emission may be explained by inverse-Comptonisation of synchrotron optical (IR) photons by their parent relativistic electrons (SSC process). A slight, variable misalignment between the synchrotron and Comptonisation zones would explain the increased gamma and X-ray flux levels in 2009-2010, as well as the change in the gamma/optical flux ratio during the outbursts peaks. The time delays of the X-ray flux changes after the gamma, and optical ones are consistent with the proposed scenario. C1 [Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, Turin, Italy. [Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kurtanidze, O. M.; Kimeridze, G. N.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, Abastumani, Rep of Georgia. [Lahteenmaki, A.; Nieppola, E.; Tammi, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Kylmala, Finland. [Larionov, V. M.; Blinov, D. A.; Borisova, E. V.; Calle, O. J. A. Bravo; Efimova, N. V.; Jorstad, S. G.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.; Yuldasheva, T. A.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Larionov, V. M.; Arkharov, A. A.; Efimova, N. V.] Pulkovo Observ, St Petersburg, Russia. [Larionov, V. M.; Blinov, D. A.] St Petersburg Branch, Isaac Newton Inst Chile, St Petersburg, Russia. [Romano, P.; Vercellone, S.] INAF IASF Palermo, Palermo, Italy. [Agudo, I.; Gomez, J. L.; Molina, S. N.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [Agudo, I.; Jorstad, S. G.; Joshi, M.; Marscher, A. P.; Taylor, B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Bach, U.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Benitez, E.; Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Berdyugin, A.; Lindfors, E.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Tuorla Observ, Piikkio, Finland. [Casas, R.; Gusbar, C.; Hawkins, K.; Li, Y.; Palma, N.; Roberts, V.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, Catania, Italy. [Calcidese, P.] Osservatorio Astron Reg Autonoma Valle dAosta, St Barthelemy, Italy. [Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain. [Carosati, D.] TNG Fdn Galileo Galilei, INAF, La Palma, Spain. [Casas, R.] Inst Ciencies Espai CSIC IEEC, Barcelona, Spain. [Casas, R.; Ros, J. A.] Agrupacio Astron Sabadell, Sabadell, Spain. [Chen, W-P.; Hsiao, H. Y.; Koptelova, E.] Natl Cent Univ, Grad Inst, Jhongli, Taiwan. [Heidt, J.] Landessternwarte Heidelberg Konigstuhl, ZAH, Heidelberg, Germany. [Hsiao, H. Y.] Natl Cent Univ, Lulin Observ, Jhongli, Taiwan. [Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin, Ireland. [Koptelova, E.] Natl Taiwan Univ, Dept Phys, Taipei, Taiwan. [Ligustri, R.] Circolo Astrofili Talmassons, Talmassons, Italy. [Lister, M.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Nieppola, E.; Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio, Finland. [Palma, N.] Univ Nacl Autonoma Honduras, Fac Ciencias Espaciales, Tegucigalpa Mdc, Honduras. [Sadun, A. C.] Univ Colorado Denver, Dept Phys, Denver, CO USA. [Sakamoto, T.] NASA, Ctr Res & Explorat Space Sci & Technol, GSFC, Greenbelt, MD USA. [Schwartz, R. D.] Galaxy View Observ, Sequim, WA USA. [Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA. [Volvach, A.] Crimean Astrophys Observ, Radio Astron Lab, Crimea, Ukraine. RP Raiteri, CM (reprint author), Osserv Astron Torino, INAF, Turin, Italy. EM raiteri@oato.inaf.it; villata@oato.inaf.it RI Kurtanidze, Omar/J-6237-2014; Molina, Sol Natalia/F-9968-2015; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova, Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Efimova, Natalia/I-2196-2013; Blinov, Dmitry/G-9925-2013; Lahteenmaki, Anne/L-5987-2013; Grishina, Tatiana/H-6873-2013; OI Molina, Sol Natalia/0000-0002-4112-2157; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Larionova, Elena/0000-0002-2471-6500; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Efimova, Natalia/0000-0002-8071-4753; Blinov, Dmitry/0000-0003-0611-5784; Grishina, Tatiana/0000-0002-3953-6676; Villata, Massimo/0000-0003-1743-6946; Larionova, Liudmila/0000-0002-0274-1481; Leto, Paolo/0000-0003-4864-2806; Vercellone, Stefano/0000-0003-1163-1396; Raiteri, Claudia Maria/0000-0003-1784-2784 FU ASI-INAF I/009/10/0; Russian RFBR foundation [09-02-00092]; Georgian National Science Foundation [GNSF/ST08/4-404]; Academy of Finland [212656, 210338, 121148]; NASA [NNX09AU16G, NNX10AP16G, NNX08AV65G, NNX08AV61G, NNX09AT99G]; NSF [AST-0607523, AST-0907893]; University of Michigan; MICIIN (Spain) [AYA2010-14844]; CEIC (Andalucia) [P09-FQM-4784]; Smithsonian Institution; Academia Sinica; BU; Lowell Observatory FX C.M.R. is grateful to Stefania Rasetti from the Torino Observatory Computer Centre for her assistance. We thank the Fermi-LAT team for providing Fermi data. We acknowledge the use of public data from the Swift data archive. We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. St.-Petersburg University team acknowledges support from Russian RFBR foundation via grant 09-02-00092. Abastumani Observatory team acknowledges financial support by the Georgian National Science Foundation through grant GNSF/ST08/4-404. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). The University of Michigan team acknowledges financial support through the NASA Fermi grants NNX09AU16G, NNX10AP16G, and NSF grant AST-0607523. The operation of UMRAO is funded by the University of Michigan. This paper is partly based on observations carried out at the German-Spanish Calar Alto Observatory, which is jointly operated by the MPIA and the IAA-CSIC. Acquisition of the MAPCAT data is supported in part by MICIIN (Spain) grant and AYA2010-14844, and by CEIC (Andalucia) grant P09-FQM-4784. Partly based on observations with the Medicina and Noto telescopes operated by INAF - Istituto di Radioastronomia. This research has made use of NASA's Astrophysics Data System and of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The research at Boston U. was supported by NSF grant AST-0907893 and NASA Fermi GI grants NNX08AV65G, NNX08AV61G, and NNX09AT99G. The PRISM camera at Lowell Observatory was developed by K. Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU, and Lowell Observatory. NR 67 TC 22 Z9 22 U1 2 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2011 VL 534 AR A87 DI 10.1051/0004-6361/201117026 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 841ZS UT WOS:000296554800047 ER PT J AU Stiele, H Pietsch, W Haberl, F Hatzidimitriou, D Barnard, R Williams, BF Kong, AKH Kolb, U AF Stiele, H. Pietsch, W. Haberl, F. Hatzidimitriou, D. Barnard, R. Williams, B. F. Kong, A. K. H. Kolb, U. TI The deep XMM-Newton Survey of M 31 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: individual: M 31; X-rays: galaxies ID X-RAY SOURCES; HUBBLE-SPACE-TELESCOPE; SUPERNOVA REMNANT CANDIDATES; COLOR-MAGNITUDE DIAGRAMS; CURRENTLY FORMING STARS; DISK CLUSTER POPULATION; HIGH-RESOLUTION CAMERA; SMALL-MAGELLANIC-CLOUD; M31 GLOBULAR-CLUSTERS; CHANDRA ACIS SURVEY AB Aims. The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, obtaining a luminosity lower limit similar to 10(35) erg s(-1) in the 0.2-4.5 keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D-25 ellipse. The main goal of the paper is to study the X-ray source population of M 31. Methods. An X-ray catalogue of 1897 sources was created, with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared, and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Results. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as is expected for an HMXB containing a neutron star primary. Conclusions. While our survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help classify these sources. C1 [Stiele, H.; Pietsch, W.; Haberl, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Hatzidimitriou, D.] Univ Athens, Fac Phys, Dept Astrophys Astron & Mech, Athens 15784, Greece. [Hatzidimitriou, D.] Fdn Res & Technol, IESL, Iraklion 71110, Greece. [Barnard, R.; Kolb, U.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Barnard, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Williams, B. F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. RP Stiele, H (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM holger.stiele@brera.inaf.it RI Hatzidimitriou, Despina/A-3732-2015; OI Haberl, Frank/0000-0002-0107-5237 FU ESA Member States; NASA; National Aeronautics and Space Administration; National Science Foundation; Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR) [FKZ 50 OX 0001, FKZ 50 OR 0405]; Max-Planck Society FX Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.; This publication makes use of the USNOFS Image and Catalogue Archive operated by the United States Naval Observatory, Flagstaff Station (http://www.nofs.navy.mil/data/fchpix/), of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation, of the SIMBAD database, operated at CDS, Strasbourg, France, and of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The XMM-Newton project is supported by the Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OX 0001) and the Max-Planck Society. HS acknowledges support by the Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft- und Raumfahrt (BMWI/DLR, FKZ 50 OR 0405). NR 129 TC 32 Z9 32 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 OCT PY 2011 VL 534 AR A55 DI 10.1051/0004-6361/201015270 PG 51 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 841ZS UT WOS:000296554800005 ER PT J AU Poffenbarger, HJ Needelman, BA Megonigal, JP AF Poffenbarger, Hanna J. Needelman, Brian A. Megonigal, J. Patrick TI Salinity Influence on Methane Emissions from Tidal Marshes SO WETLANDS LA English DT Article DE Carbon sequestration; Sulfate reduction; Methane flux; Porewater ID SALT-MARSH; SULFATE REDUCTION; VERTICAL ACCRETION; NATURAL WETLANDS; CARBON-DIOXIDE; RIVER ESTUARY; ELEVATED CO2; PORE-WATER; FLUXES; METHANOGENESIS AB The relationship between methane emissions and salinity is not well understood in tidal marshes, leading to uncertainty about the net effect of marsh conservation and restoration on greenhouse gas balance. We used published and unpublished field data to investigate the relationships between tidal marsh methane emissions, salinity, and porewater concentrations of methane and sulfate, then used these relationships to consider the balance between methane emissions and soil carbon sequestration. Polyhaline tidal marshes (salinity > 18) had significantly lower methane emissions (mean +/- sd = 1 +/- 2 gm(-2) yr(-1)) than other marshes, and can be expected to decrease radiative forcing when created or restored. There was no significant difference in methane emissions from fresh (salinity=0-0.5) and mesohaline (5-18) marshes (42 +/- 76 and 16 +/- 11 gm(-2) yr(-1), respectively), while oligohaline (0.5-5) marshes had the highest and most variable methane emissions (150 +/- 221 gm(-2) yr(-1)). Annual methane emissions were modeled using a linear fit of salinity against log-transformed methane flux (log(CH4) - -0.056 x salinity + 1: 38; r(2) = 0.52; p < 0.0001). Managers interested in using marshes as greenhouse gas sinks can assume negligible methane emissions in polyhaline systems, but need to estimate or monitor methane emissions in lower-salinity marshes. C1 [Poffenbarger, Hanna J.; Needelman, Brian A.] Univ Maryland, Dept Environm Sci & Technol, College Pk, MD 20742 USA. [Megonigal, J. Patrick] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Needelman, BA (reprint author), Univ Maryland, Dept Environm Sci & Technol, 1109 HJ Patterson Hall, College Pk, MD 20742 USA. EM bneed@umd.edu; megonigalp@si.edu FU Maryland Department of Natural Resources FX We thank Andrew Baldwin, Raymond Crew, Emily Hutchins, Miriam Meyers, Nicholas Mudd, Jim Duls, Caitlin Megonigal and U.S. Fish and Wildlife Service staff at the Blackwater Natural Wildlife Refuge. This work was supported by funding from the Maryland Department of Natural Resources Power Plant Research Program. NR 50 TC 89 Z9 100 U1 10 U2 119 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 J9 WETLANDS JI Wetlands PD OCT PY 2011 VL 31 IS 5 BP 831 EP 842 DI 10.1007/s13157-011-0197-0 PG 12 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 843TJ UT WOS:000296695200002 ER PT J AU Lazo-Wasem, EA Pinou, T de Niz, AP Feuerstein, A AF Lazo-Wasem, Eric A. Pinou, Theodora de Niz, Alejandro Pena Feuerstein, Amanda TI Epibionts Associated with the Nesting Marine Turtles Lepidochelys olivacea and Chelonia mydas in Jalisco, Mexico: A Review and Field Guide SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article ID LOGGERHEAD SEA-TURTLES; COPEPODA HARPACTICOIDA; BARNACLES CIRRIPEDIA; CARETTA-CARETTA; COMMENSAL; ATLANTIC; PLANES; STOMATOLEPAS; TESTUDINARIA; CALIFORNIA AB The diversity and frequency of epibiota collected over three years (2001, 2002, 2008) from sea turtles (Lepidochelys olivacea and Chelonia mydas) nesting on Teopa Beach in Jalisco State, Mexico, are described. This diversity is compared to epibiotic assemblages procured from these same turtle species nesting on other Mexican beaches, and the role these turtles play in the conservation and dispersal of these epibiota is discussed. Given the increased awareness of epibionts and the desire of many researchers to make positive identifications, specific diagnoses, photographs and a collecting protocol will serve as a basic aid to the collection and accurate identification of epibionts found on turtles living along the Pacific coast of Mexico. C1 [Lazo-Wasem, Eric A.] Yale Univ, Div Invertebrate Zool, Peabody Museum Nat Hist, New Haven, CT 06520 USA. [Pinou, Theodora; Feuerstein, Amanda] Western Connecticut State Univ, Dept Biol & Environm Sci, Danbury, CT 06810 USA. [de Niz, Alejandro Pena] Ctr Protecc & Conservac Tortugas Marinas Playa Te, Municipio De La Huerta 48894, Jalisco, Mexico. [Feuerstein, Amanda] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Lazo-Wasem, EA (reprint author), Yale Univ, Div Invertebrate Zool, Peabody Museum Nat Hist, New Haven, CT 06520 USA. EM eric.lazo-wasem@yale.edu FU Yale College; Yale Peabody Museum FX We thank Melissa Salgado, Damon Nakamura and Laura Smowle for their help with fieldwork; these students were supported by the Yale College Studies in the Environment Program. Further support for M. Salgado was received from the Yale Class of 1954, and L. Smowle received additional support from the Environmental Engineering Yale Summer Program. Fieldwork by A. Feuerstein was supported by the Yale Peabody Museum Summer Internship Program (2008). Additional support was provided by Connecticut State University-AAUP to T. Pinou. The Brignone family of Costa Careyes, Jalisco, Mexico, generously provided field and logistical support, and access to beaches where the study was conducted, and helped arrange lodging for two of us (E.A. Lazo-Wasem and A. Feuerstein) during the 2008 field season. Also, the family of A. Pena de Niz, especially his wife Dulce, provided considerable general assistance to A. Feuerstein while she lived in Jalisco during the summer of 2008. We thank our colleagues at the University of Guadalajara for their assistant at Campamento La Gloria. Ivan Sazima (Universidade Estadual de Campinas) generously supplied the diagnostic characters to distinguish remoras. Suggestions by reviewers Adam Baldinger (Museum of Comparative Zoology, Harvard University), Christopher Boyko (Dowling College), Michael Frick (Gainesville, Florida) and John Zardus (The Citadel) greatly improved the manuscript. Lourdes Rojas (Yale Peabody Museum) helped with many iterations of the data tables and Daniel Drew (Yale Peabody Museum) pointed out valuable references for historical accounts of remora. NR 55 TC 12 Z9 12 U1 2 U2 13 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD OCT PY 2011 VL 52 IS 2 BP 221 EP 240 PG 20 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 837QM UT WOS:000296218300003 ER PT J AU Corrigan, C AF Corrigan, Cari TI ANTARCTICA: THE BEST PLACE ON EARTH TO COLLECT METEORITES SO ELEMENTS LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Corrigan, C (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 1811-5209 J9 ELEMENTS JI Elements PD OCT PY 2011 VL 7 IS 5 BP 296 EP 296 PG 1 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 838QY UT WOS:000296308500003 ER PT J AU Smith, KM Zaldarriaga, M AF Smith, Kendrick M. Zaldarriaga, Matias TI Algorithms for bispectra: forecasting, optimal analysis and simulation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmic background radiation; early Universe; inflation ID MICROWAVE BACKGROUND MAPS; PROBE WMAP OBSERVATIONS; POWER SPECTRUM; NON-GAUSSIANITY; ANISOTROPIES; REIONIZATION AB We propose a factorizability ansatz for angular bispectra which permits fast algorithms for forecasting, analysis and simulation, yet is general enough to encompass many interesting cosmic microwave background (CMB) bispectra. We describe a suite of general algorithms which apply to any bispectrum which can be represented in factorizable form. First, we present algorithms for Fisher matrix forecasts and the related problem of optimizing the factorizable representation, giving a Fisher forecast for Planck as an example. We show that the CMB can give independent constraints on the amplitude of primordial bispectra of both local and equilateral shape as well as those created by secondary anisotropies. We also show that the integrated Sachs-Wolfe (ISW)-lensing bispectrum should be detected by Planck and could bias estimates of the local type of non-Gaussianity if not properly accounted for. Second, we implement a bispectrum estimator which is fully optimal in the presence of sky cuts and inhomogeneous noise, extends the generality of fast estimators which have been limited to a few specific forms of the bispectrum and improves the running time of existing implementations by several orders of magnitude. Third, we give an algorithm for simulating random, weakly non-Gaussian maps with prescribed power spectrum and factorizable bispectrum. C1 [Smith, Kendrick M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Smith, Kendrick M.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Zaldarriaga, Matias] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Zaldarriaga, Matias] Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP Smith, KM (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM kmsmith@astro.princeton.edu FU Kavli Institure for Cosmological Physics [NSF PHY-0114422]; Packard and Sloan foundations [NSF AST-0506556, NASA NNG05GG84G] FX We would like to thank Wayne Hu, Dragan Huterer, Michele Liguori, Eugene Lim and Bruce Winstein for useful discussions. We acknowledge the use of the FFTW, LAPACK, CAMB and HEALPiX software packages. KMS was supported by the Kavli Institure for Cosmological Physics through the grant NSF PHY-0114422. MZ was supported by the Packard and Sloan foundations, NSF AST-0506556 and NASA NNG05GG84G. NR 50 TC 54 Z9 54 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 1 BP 2 EP 19 DI 10.1111/j.1365-2966.2010.18175.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GV UT WOS:000296276300023 ER PT J AU McDonald, I van Loon, JT Sloan, GC Dupree, AK Zijlstra, AA Boyer, ML Gehrz, RD Evans, A Woodward, CE Johnson, CI AF McDonald, I. van Loon, J. Th. Sloan, G. C. Dupree, A. K. Zijlstra, A. A. Boyer, M. L. Gehrz, R. D. Evans, A. Woodward, C. E. Johnson, C. I. TI Spitzer spectra of evolved stars in omega Centauri and their low-metallicity dust production SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; stars: mass-loss; stars: winds, outflows; globular clusters: general; infrared: stars ID RED-GIANT-BRANCH; GALACTIC GLOBULAR-CLUSTERS; MASS-LOSS; OPTICAL-PROPERTIES; SPACE-TELESCOPE; STELLAR POPULATIONS; INTERSTELLAR-MEDIUM; CIRCUMSTELLAR DUST; MODEL ATMOSPHERES; MAGELLANIC CLOUDS AB Dust production is explored around 14 metal-poor ([Fe/H] = -1.91 to -0.98) giant stars in the Galactic globular cluster omega Centauri using new Spitzer Infrared Spectrograph spectra. This sample includes the cluster's post-asymptotic giant branch (AGB) and carbon stars and is thus the first representative spectral study of dust production in a metal-poor ([Fe/H] < -1) population. Only the more metal-rich stars V6 and V17 ([Fe/H]= -1.08, -1.06) exhibit silicate emission, while the five other stars with mid-infrared excess show only a featureless continuum which we argue is caused by metallic iron dust grains. We examine the metallicity of V42, and find it is likely part of the metal-rich population ([Fe/H] similar to -0.8). Aside from the post-AGB star V1, we find no star from the cluster's bulk, metal-poor ([Fe/H] < -1.5) population - including the carbon stars - to be producing detectable amounts of dust. We compare the dust production to the stars' H alpha line profiles obtained at the Magellan/Clay telescope at Las Campanas Observatory, finding pulsation shocking in the strongest pulsators (V6, V17 and V42), but evidence of outflow in all other stars. We conclude that the onset of dust production does not signify a fundamental change in the material leaving the star. Our data add to a growing body of evidence that metallic iron dominates dust production in metal-poor, oxygen-rich stars, but that dust is probably not the primary accelerant of winds in this mass-metallicity regime. C1 [McDonald, I.; Zijlstra, A. A.] Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [McDonald, I.; van Loon, J. Th.; Evans, A.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Boyer, M. L.] STScI, Baltimore, MD 21218 USA. [Gehrz, R. D.; Woodward, C. E.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Johnson, C. I.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP McDonald, I (reprint author), Jodrell Bank, Ctr Astrophys, Alan Turing Bldg, Manchester M13 9PL, Lancs, England. EM mcdonald@jb.man.ac.uk FU NASA; United States Air Force; National Science Foundation [AST-1003201]; NASA JPL/Spitzer FX RDG was supported by NASA and the United States Air Force. CEW was supported in part by the National Science Foundation and NASA JPL/Spitzer grants awarded to the University of Minnesota. CIJ was supported by the National Science Foundation under award No. AST-1003201. NR 76 TC 20 Z9 20 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 1 BP 20 EP 31 DI 10.1111/j.1365-2966.2011.18963.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GV UT WOS:000296276300024 ER PT J AU Risaliti, G Nardini, E Elvis, M Brenneman, L Salvati, M AF Risaliti, G. Nardini, E. Elvis, M. Brenneman, L. Salvati, M. TI Probing general relativistic effects during active galactic nuclei X-ray eclipses SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE relativistic processes; galaxies: active ID BLACK-HOLE; ACCRETION DISK; NGC 1365; LINE; GALAXIES; SPECTROSCOPY; TRANSITIONS; MCG-6-30-15; ABSORPTION; ABSORBER AB Long X-ray observations of bright active galactic nuclei (AGN) show that X-ray eclipses, with durations from a few hours to a few days, are rather common. This opens up a new window of opportunity in the search for signatures of relativistic effects in AGN: an obscuring cloud covers/uncovers different parts of the accretion disc at different times, allowing a direct check of the expected pattern of disc emission. In particular, the combination of gravitational redshift and relativistic Doppler boosting should imply strong differences between the receding and approaching parts of an inclined thin disc. At present, these effects may be already detectable with a 'lucky' XMM-Newton or Suzaku observation of a complete eclipse by a Compton-thick cloud (a rare, but not impossible-to-see event). In the future, higher sensitivity observatories will be able to perform these tests easily on tens of AGN. This will provide a powerful and direct way to test extreme gravity, and to probe the structure of AGN in the close vicinity of the central black holes. C1 [Risaliti, G.; Salvati, M.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.; Elvis, M.; Brenneman, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nardini, E.] Univ Florence, Dipartimento Fis Astron, I-50125 Florence, Italy. RP Risaliti, G (reprint author), INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. EM grisaliti@cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009; OI Risaliti, Guido/0000-0002-3556-977X FU [NASA NNX08AN48G] FX This work has been partly supported by grants NASA NNX08AN48G. NR 29 TC 12 Z9 12 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 1 BP 178 EP 183 DI 10.1111/j.1365-2966.2011.19055.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GV UT WOS:000296276300031 ER PT J AU Sobolewska, MA Papadakis, IE Done, C Malzac, J AF Sobolewska, M. A. Papadakis, I. E. Done, C. Malzac, J. TI Evidence for a change in the X-ray radiation mechanism in the hard state of Galactic black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; X-rays: binaries ID BROAD-BAND SPECTRUM; ADVECTION-DOMINATED ACCRETION; NOVA-MUSCAE 1991; SGR-A-ASTERISK; GX 339-4; XTE J1550-564; GAMMA-RAY; OUTBURST DECAY; LOW/HARD STATE; NEUTRON-STARS AB We present results on the spectral variability of two Galactic black hole X-ray binaries, GRO J1655-40 and GX 339-4, in the hard state. We confirm a transition in behaviour of the photon index with luminosity, such that the well-known decrease in X-ray photon index with decreasing luminosity only continues down to L-bol similar to 0.01L(E). Below this point, the photon index increases again. For Comptonization models, this implies that the ratio of the Compton luminosity to seed photon luminosity, l(h)/l(s), changes with bolometric luminosity, consistent with a scenario where seed photons change from cyclo-synchrotron at the lowest luminosities to those from a truncated disc. Alternatively, the transition could mark the point below which the non-thermal jet starts to dominate, or where reprocessed photons replace the viscous photons in an outflowing corona model. C1 [Sobolewska, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sobolewska, M. A.; Papadakis, I. E.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Crete, Greece. [Sobolewska, M. A.; Papadakis, I. E.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Sobolewska, M. A.; Papadakis, I. E.] Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece. [Done, C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Malzac, J.] Univ Toulouse, Toulouse, France. [Malzac, J.] UPS OMP, Toulouse, France. [Malzac, J.] IRAP, F-31028 Toulouse 4, France. [Malzac, J.] CNRS, F-31028 Toulouse 4, France. RP Sobolewska, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM msobolewska@cfa.harvard.edu RI Papadakis, Iossif/C-3235-2011; done, chris/D-4605-2016 OI done, chris/0000-0002-1065-7239 FU Chandra grant [GO8-9125A]; Marie-Curie ToK Fellowship [MTKD-CT-2006-039965]; EU FP7-REGPOT [206469]; GdR PCHE in France FX Wewould like to thank the anonymous referee for helpful comments and suggestions. MS acknowledges support from a Chandra grant GO8-9125A and a Marie-Curie ToK Fellowship number MTKD-CT-2006-039965. IEP acknowledges support from the EU FP7-REGPOT 206469 grant. This work was partially supported by the GdR PCHE in France. NR 70 TC 33 Z9 33 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 1 BP 280 EP 288 DI 10.1111/j.1365-2966.2011.19209.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GV UT WOS:000296276300039 ER PT J AU Alsubai, KA Parley, NR Bramich, DM West, RG Sorensen, PM Cameron, AC Latham, DW Horne, K Anderson, DR Bakos, GA Brown, DJA Buchhave, LA Esquerdo, GA Everett, ME Furesz, G Hartman, JD Hellier, C Miller, GM Pollacco, D Quinn, SN Smith, JC Stefanik, RP Szentgyorgyi, A AF Alsubai, K. A. Parley, N. R. Bramich, D. M. West, R. G. Sorensen, P. M. Cameron, A. Collier Latham, D. W. Horne, K. Anderson, D. R. Bakos, G. A. Brown, D. J. A. Buchhave, L. A. Esquerdo, G. A. Everett, M. E. Furesz, G. Hartman, J. D. Hellier, C. Miller, G. M. Pollacco, D. Quinn, S. N. Smith, J. C. Stefanik, R. P. Szentgyorgyi, A. TI Qatar-1b: a hot Jupiter orbiting a metal-rich K dwarf star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; techniques: radial velocities; techniques: spectroscopic; stars: individual: Qatar-1; planetary systems ID M-J PLANET; LIGHT CURVES; SPECTROSCOPIC BINARIES; EXTRASOLAR PLANETS; TRANSIT SEARCHES; ALGORITHM; FIELD; CANDIDATES AB We report the discovery and initial characterization of Qatar-1b, a hot Jupiter-orbiting metal-rich K dwarf star, the first planet discovered by the Qatar Exoplanet Survey. We describe the strategy used to select candidate transiting planets from photometry generated by the Qatar Exoplanet Survey camera array. We examine the rate of astrophysical and other false positives found during the spectroscopic reconnaissance of the initial batch of candidates. A simultaneous fit to the follow-up radial velocities and photometry of Qatar-1b yields a planetary mass of 1.09 +/- 0.08 M-J and a radius of 1.16 +/- 0.05 R-J. The orbital period and separation are 1.420 033 +/- 0.000 016 d and 0.023 43 +/- 0.000 26 au for an orbit assumed to be circular. The stellar density, effective temperature and rotation rate indicate an age greater than 4 Gyr for the system. C1 [Alsubai, K. A.] Qatar Fdn, Doha, Qatar. [Parley, N. R.; Cameron, A. Collier; Horne, K.; Brown, D. J. A.; Miller, G. M.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Bramich, D. M.] European So Observ, D-85748 Garching, Germany. [West, R. G.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Sorensen, P. M.] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Santa Cruz De T, Spain. [Latham, D. W.; Bakos, G. A.; Esquerdo, G. A.; Furesz, G.; Hartman, J. D.; Quinn, S. N.; Stefanik, R. P.; Szentgyorgyi, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Anderson, D. R.; Hellier, C.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Everett, M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Pollacco, D.] Queens Univ, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Smith, J. C.] Hidden Loft Observ, Tucson, AZ 85755 USA. RP Alsubai, KA (reprint author), Qatar Fdn, POB 5825, Doha, Qatar. EM kalsubai@qf.org.qa OI Buchhave, Lars A./0000-0003-1605-5666; Cameron, Andrew/0000-0002-8863-7828; Hartman, Joel/0000-0001-8732-6166 FU Spanoptic Ltd of Glenrothes FX This research has made use of the ESO Data Archive, the NASA Astrophysics Data System and the VizieR catalogue access tool, CDS, Strasbourg, France. The high quality of the JGT photometry reported in this paper owes much to recent telescope upgrades made possible by a generous grant from Spanoptic Ltd of Glenrothes, and carried out with inspired technical effort by Mark Ross, Chris Booth, Roger Stapleton and David Steven. We thank the anonymous referee for several insightful suggestions for improving the clarity of the manuscript and the interpretation of the results. NR 30 TC 26 Z9 26 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 1 BP 709 EP 716 DI 10.1111/j.1365-2966.2011.19316.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GV UT WOS:000296276300078 ER PT J AU Kipping, DM Spiegel, DS AF Kipping, David M. Spiegel, David S. TI Detection of visible light from the darkest world SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: individual: TrES-2 ID IRRADIATED GIANT PLANETS; HOT JUPITER; THERMAL INVERSIONS; KEPLER-FIELD; ATMOSPHERES; ALBEDO; TRES-2; PHOTOMETRY; EMISSION; BINARY AB We present the detection of visible light from the planet TrES-2b, the darkest exoplanet currently known. By analysis of the orbital photometry from publicly available Kepler data (0.4-0.9 mu m), we determine a day-night contrast amplitude of 6.5 +/- 1.9 ppm (parts per million), constituting the lowest amplitude orbital phase variation discovered. The signal is detected to 3.7 sigma confidence and persists in six different methods of modelling the data and thus appears robust. In contrast, we are unable to detect ellipsoidal variations or beaming effects, but we do provide confidence intervals for these terms. If the day-night contrast is interpreted as being due to scattering, it corresponds to a geometric albedo of A(g) = 0.0253 +/- 0.0072. However, our models indicate that there is a significant emission component to dayside brightness, and the true albedo is even lower (<1 per cent). By combining our measurement with Spitzer and ground-based data, we show that a model with moderate redistribution (P-n similar or equal to 0.3) and moderate extra optical opacity (kappa' similar or equal to 0.3-0.4) provide a compatible explanation to the data. C1 [Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spiegel, David S.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu FU Smithsonian Institute FX We thank the Kepler Science Team, especially the DAWG, for making the data used here available. Thanks to A. Burrows, M. Nikku and the anonymous referee for helpful comments, and I. Hubeny and A. Burrows for the development and continued maintenance of COOLTLUSTY and associated opacity data base. DMK is supported by Smithsonian Institute Restricted Endowment Funds. NR 25 TC 34 Z9 34 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 1 BP L88 EP L92 DI 10.1111/j.1745-3933.2011.01127.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GV UT WOS:000296276300019 ER PT J AU McKernan, B Ford, KES Lyra, W Perets, HB Winter, LM Yaqoob, T AF McKernan, B. Ford, K. E. S. Lyra, W. Perets, H. B. Winter, L. M. Yaqoob, T. TI On rapid migration and accretion within discs around supermassive black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accreation, accreation discs; planet-disc interactions; stars: kinematics and dynamics; galaxies: active; galaxies: nuclei; quasars: general ID ACTIVE GALACTIC NUCLEI; III PLANETARY MIGRATION; SOFT-X-RAY; NUMERICAL SIMULATIONS; STELLAR REMNANTS; STAR-FORMATION; MASS; GALAXIES; CLUSTER; EXCESS AB Galactic nuclei should contain a cluster of stars and compact objects in the vicinity of the central supermassive black hole due to stellar evolution, minor mergers and gravitational dynamical friction. By analogy with protoplanetary migration, nuclear cluster objects (NCOs) can migrate in the accretion discs that power active galactic nuclei (AGN) by exchanging angular momentum with disc gas. Here we show that an individual NCO undergoing runaway outward migration comparable to type III protoplanetary migration can generate an accretion rate corresponding to Seyfert AGN or quasar luminosities. Multiple migrating NCOs in an AGN disc can dominate traditional viscous disc accretion, and at large disc radii, ensemble NCO migration and accretion could provide sufficient heating to prevent the gravitational instability from consuming disc gas in star formation. The magnitude and energy of the X-ray soft excess observed at similar to 0.1-1 keV in Seyfert AGN could be explained by a small population of similar to 10(2)-10(3) accreting stellar mass black holes or a few ULXs. NCO migration and accretion in AGN discs are therefore extremely important mechanisms to add to realistic models of AGN discs. C1 [McKernan, B.; Ford, K. E. S.] CUNY, Borough Manhattan Community Coll, Dept Sci, New York, NY 10007 USA. [McKernan, B.; Ford, K. E. S.; Lyra, W.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [McKernan, B.; Ford, K. E. S.] CUNY, Grad Ctr, New York, NY 10016 USA. [Perets, H. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Winter, L. M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA. [Yaqoob, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP McKernan, B (reprint author), CUNY, Borough Manhattan Community Coll, Dept Sci, New York, NY 10007 USA. EM bmckernan@amnh.org RI Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X NR 45 TC 9 Z9 9 U1 4 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 1 BP L103 EP L107 DI 10.1111/j.1745-3933.2011.01132.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GV UT WOS:000296276300022 ER PT J AU Russell, HR van Weeren, RJ Edge, AC McNamara, BR Sanders, JS Fabian, AC Baum, SA Canning, REA Donahue, M O'Dea, CP AF Russell, H. R. van Weeren, R. J. Edge, A. C. McNamara, B. R. Sanders, J. S. Fabian, A. C. Baum, S. A. Canning, R. E. A. Donahue, M. O'Dea, C. P. TI A merger mystery: no extended radio emission in the merging cluster Abell 2146 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE general: clusters: general; galaxies: clusters: individual: A2146; radio continuum: general ID X-RAY-EMISSION; VLA SKY SURVEY; GALAXY CLUSTERS; COMA CLUSTER; COSMIC-RAYS; PARTICLE-ACCELERATION; NONTHERMAL EMISSION; RELIC CANDIDATES; SHOCK-WAVES; DARK-MATTER AB We present a new 400 ks Chandra X-ray observation and a Giant Metrewave Radio Telescope (GMRT) radio observation at 325 MHz of the merging galaxy cluster Abell 2146. The Chandra observation reveals detailed structure associated with the major merger event including the Mach M = 2.1 +/- 0.2 bow shock located ahead of the dense subcluster core and the first known example of an upstream shock (M = 1.6 +/- 0.1). Surprisingly, the deep GMRT observation at 325MHz does not detect any extended radio emission associated with either shock front. All other merging galaxy clusters with X-ray-detected shock fronts, including the Bullet cluster, Abell 520, Abell 754 and Abell 2744, and clusters with candidate shock fronts have detected radio relics or radio halo edges coincident with the shocks. We consider several possible factors which could affect the formation of radio relics, including the shock strength and the presence of a pre-existing electron population, but do not find a favourable explanation for this result. We calculate a 3 sigma upper limit of 13 mJy on extended radio emission, which is significantly below the radio power expected by the observed P-radio-L-X correlation for merging systems. The lack of an extended radio halo in Abell 2146 maybe due to the low cluster mass relative to the majority of merging galaxy clusters with detected radio haloes. C1 [Russell, H. R.; McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [van Weeren, R. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanders, J. S.; Fabian, A. C.; Canning, R. E. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Baum, S. A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. RP Russell, HR (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. EM helen.russell@uwaterloo.ca OI Edge, Alastair/0000-0002-3398-6916; Sanders, Jeremy/0000-0003-2189-4501; van Weeren, Reinout/0000-0002-0587-1660 FU Canadian Space Agency; Royal Society; Royal Netherlands Academy of Arts and Sciences; STFC FX HRR and BRM acknowledge generous financial support from the Canadian Space Agency Space Science Enhancement Program. ACF thanks the Royal Society for support. RJvW and REAC acknowledge funding from the Royal Netherlands Academy of Arts and Sciences and the STFC, respectively. The GMRT is operated by the National Centre for Radio Astrophysics (NCRA). The authors are grateful to the GMRT Director and staff for the award of time and executing the observations. HRR thanks David Green, Julie Hlavacek-Larrondo, Roderick Johnstone and Grant Tremblay for helpful discussions. We also thank the referee and Gianfranco Brunetti for helpful comments that improved this letter. NR 66 TC 42 Z9 42 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 1 BP L1 EP L5 DI 10.1111/j.1745-3933.2011.01098.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GV UT WOS:000296276300001 ER PT J AU Steffen, JH Quinn, SN Borucki, WJ Brugamyer, E Bryson, ST Buchhave, LA Cochran, WD Endl, M Fabrycky, DC Ford, EB Holman, MJ Jenkins, J Koch, D Latham, DW MacQueen, P Mullally, F Prsa, A Ragozzine, D Rowe, JF Sanderfer, DT Seader, SE Short, D Shporer, A Thompson, SE Torres, G Twicken, JD Welsh, WF Windmiller, G AF Steffen, J. H. Quinn, S. N. Borucki, W. J. Brugamyer, E. Bryson, S. T. Buchhave, L. A. Cochran, W. D. Endl, M. Fabrycky, D. C. Ford, E. B. Holman, M. J. Jenkins, J. Koch, D. Latham, D. W. MacQueen, P. Mullally, F. Prsa, A. Ragozzine, D. Rowe, J. F. Sanderfer, D. T. Seader, S. E. Short, D. Shporer, A. Thompson, S. E. Torres, G. Twicken, J. D. Welsh, W. F. Windmiller, G. TI The architecture of the hierarchical triple star KOI 928 from eclipse timing variations seen in Kepler photometry SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: eclipsing ID LIGHT CURVES; LOW-MASS; PLANETS; SYSTEM; GIANT AB We present a hierarchical triple star system (KIC 9140402) where a low-mass eclipsing binary orbits a more massive third star. The orbital period of the binary (4.988 29 d) is determined by the eclipse times seen in photometry from NASA's Kepler spacecraft. The periodically changing tidal field, due to the eccentric orbit of the binary about the tertiary, causes a change in the orbital period of the binary. The resulting eclipse timing variations provide insight into the dynamics and architecture of this system and allow the inference of the total mass of the binary (0.424 +/- 0.017M(circle dot)) and the orbital parameters of the binary about the central star. C1 [Steffen, J. H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Quinn, S. N.; Holman, M. J.; Latham, D. W.; Ragozzine, D.; Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Borucki, W. J.; Bryson, S. T.; Jenkins, J.; Koch, D.; Mullally, F.; Rowe, J. F.; Sanderfer, D. T.; Seader, S. E.; Thompson, S. E.; Twicken, J. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brugamyer, E.; Cochran, W. D.; Endl, M.; MacQueen, P.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Fabrycky, D. C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ford, E. B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Jenkins, J.; Mullally, F.; Seader, S. E.; Thompson, S. E.; Twicken, J. D.] SETI Inst, Mountain View, CA 94043 USA. [Prsa, A.] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Short, D.; Welsh, W. F.; Windmiller, G.] San Diego State Univ, San Diego, CA 92182 USA. [Shporer, A.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. RP Steffen, JH (reprint author), Fermilab Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA. EM jsteffen@fnal.gov RI Steffen, Jason/A-4320-2013; Ragozzine, Darin/C-4926-2013; OI Buchhave, Lars A./0000-0003-1605-5666; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [HF-51272.01-A, HF-51267.01-A]; STScI; AURA [NAS 5-26555] FX Kepler is NASA's 10th Discovery mission with funding provided by NASA's Science Mission Directorate. DCF acknowledges NASA support through Hubble Fellowship grants #HF-51272.01-A and #HF-51267.01-A awarded by STScI and operated by AURA under contract NAS 5-26555. NR 22 TC 15 Z9 15 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 417 IS 1 BP L31 EP L35 DI 10.1111/j.1745-3933.2011.01114.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 838GV UT WOS:000296276300007 ER PT J AU Grindlay, J Hong, J Allen, B Barthelmy, S Baker, R AF Grindlay, J. Hong, J. Allen, B. Barthelmy, S. Baker, R. TI Development of tiled imaging CZT detectors for sensitive wide-field hard X-ray surveys to EXIST SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE CZT detectors; Pixellated CZT; Coded aperture telescopes; Black holes; Wide-field surveys ID BURST AB Motivated by the proposed EXIST mission, a "medium-class" space observatory to survey black holes and the Early Universe proposed to the 2010 NAS/NRC Astronomy and Astrophysics Decadal Survey, we have developed the first "large" area 256 cm(2) close-tiled (0.6 mm gaps) hard X-ray (20-600 key) imaging detector employing pixelated (2.5 mm) CdZnTe (CZT) detectors, each 2 x 2 x 0.5 cm(3). We summarize the design, development and operation of this detector array (8 x 8 CZTs) and its performance as the imager for a coded aperture telescope on a high altitude (40 km) balloon flight in October, 2009, as the ProtoEXIST1 payload. We then outline our current development of a second-generation imager, ProtoEXIST2, with 0.6 mm pixels on a 32 x 32 array on each CZT, and how it will lead to the ultimate imaging system needed for EXIST. Other applications of this technology will also be mentioned. (C) 2010 Elsevier B.V. All rights reserved. C1 [Grindlay, J.; Hong, J.; Allen, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barthelmy, S.; Baker, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Grindlay, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM josh@head.cfa.harvard.edu RI Barthelmy, Scott/D-2943-2012 FU NASA [NNG06WC12G, NN09AD76G] FX This work is supported in part by NASA APRA Grants NNG06WC12G and NN09AD76G. NR 7 TC 6 Z9 6 U1 2 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD OCT 1 PY 2011 VL 652 IS 1 BP 671 EP 673 DI 10.1016/j.nima.2010.09.160 PG 3 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 831XS UT WOS:000295765000162 ER PT J AU Kijbunchoo, N Clayton, GC Vieux, TC Dickerman, N Hillwig, TC Welch, DL Pagnotta, A Tang, SM Grindlay, JE Henden, A AF Kijbunchoo, Nutsinee Clayton, Geoffrey C. Vieux, Timothy C. Dickerman, N. Hillwig, T. C. Welch, D. L. Pagnotta, Ashley Tang, Sumin Grindlay, J. E. Henden, A. TI NSV 11154 Is a New R Coronae Borealis Star SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID CARBON STARS; PHOTOMETRY; DATABASE; EROS-2 AB NSV 11154 has been confirmed as a new member of the rare hydrogen-deficient R Coronae Borealis (RCB) stars based on new photometric and spectroscopic data. Using new photometry, as well as archival plates from the Harvard archive, we have constructed the historical light curve of NSV 11154 from 1896 to the present. The light curve shows the sudden, deep, irregularly spaced declines characteristic of RCB stars. The visible spectrum is typical of a cool (T-eff less than or similar to 5000 K) RCB star, showing no hydrogen lines, strong C-2 Swan bands, and no evidence of C-13. In addition, the star shows small pulsations that are typical of an RCB star and an infrared excess due to circumstellar dust, with a temperature of similar to 800 K. The distance to NSV 11154 is estimated to be similar to 14.5 kpc. RCB stars are very rare in the Galaxy, so each additional star is important to population studies leading to a better understanding the origins of these mysterious stars. Among the known sample of RCB stars, NSV 11154 is unusual in that it lies well above the Galactic plane (5 kpc) and away from the Galactic center, which suggests that its parent population is neither thick disk nor bulge. C1 [Kijbunchoo, Nutsinee; Clayton, Geoffrey C.; Vieux, Timothy C.; Dickerman, N.; Pagnotta, Ashley] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Hillwig, T. C.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA. [Welch, D. L.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Tang, Sumin; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Henden, A.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA. RP Kijbunchoo, N (reprint author), Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. EM nkijbu1@tigers.lsu.edu; gclayton@fenway.phys.lsu.edu; tvieux1@tigers.lsu.edu; todd.hillwig@valpo.edu; welch@physics.mcmaster.ca; pagnotta@phys.lsu.edu; stang@cfa.harvard.edu; josh@head.cfa.harvard.edu; arne@aavso.org FU NSF [AST-0407380, AST-0909073]; Cornel and Cynthia K. Sarosdy Fund FX This article used data from Digital Access to a Sky Century at Harvard (DASCH), supported by NSF grants AST-0407380 and AST-0909073, as well as by the Cornel and Cynthia K. Sarosdy Fund. NR 24 TC 4 Z9 4 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD OCT PY 2011 VL 123 IS 908 BP 1149 EP 1155 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840XK UT WOS:000296475200002 ER PT J AU Szentgyorgyi, A Furesz, G Cheimets, P Conroy, M Eng, R Fabricant, D Fata, R Gauron, T Geary, J McLeod, B Zajac, J Amato, S Bergner, H Caldwell, N Dupree, A Goddard, R Johnston, E Meibom, S Mink, D Pieri, M Roll, J Tokarz, S Wyatt, W Epps, H Hartmann, L Meszaros, S AF Szentgyorgyi, Andrew Furesz, Gabor Cheimets, Peter Conroy, Maureen Eng, Roger Fabricant, Daniel Fata, Robert Gauron, Thomas Geary, John McLeod, Brian Zajac, Joseph Amato, Stephen Bergner, Henry Caldwell, Nelson Dupree, Andrea Goddard, Richard Johnston, Everett Meibom, Soeren Mink, Douglas Pieri, Mario Roll, John Tokarz, Susan Wyatt, William Epps, Harland Hartmann, Lee Meszaros, Szabolcz TI Hectochelle: A Multiobject Optical Echelle Spectrograph for the MMT SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID MOUNTING LARGE LENSES; RED GIANT STARS; CHROMOSPHERIC ACTIVITY; CROSS-DISPERSION; CONVERTED MMT; MASS OUTFLOW; FIBER; SPECTROSCOPY; INSTRUMENTS AB The Hectochelle is an optical band, fiber-fed, multiobject echelle spectrograph deployed at the MMT Observatory on Mount Hopkins, Arizona. The optical fibers that feed the Hectochelle are positioned by the Hectospec robot positioner on the MMT f/5 focal surface, and the Hectochelle shares an optical fiber feed system with the Hectospec, a moderate-dispersion spectrograph that is collocated with the Hectochelle. Hectochelle can record up to 240 spectra simultaneously at a resolution of 38,000. Spectra cover a single diffractive order that is approximately 150 angstrom wide. The total potential operating passband of the Hectochelle extends from 3800 A to 9000 angstrom. Operated in conjunction with the MMT f/5 secondary, the MMT wide-field corrector, and the atmospheric dispersion compensator, the patrol field is 10 in diameter and the individual fiber slits are 1.5 '' in diameter. The throughput of the combined telescope, fiber feed, and spectrograph is measured to be 6.1% at 5275 angstrom, exclusive of atmospheric extinction. A 20 minute observation of a V = 15 F-type star yields a signal-to-noise ratio of 35 per resolution element. Hectochelle had first light 2003 December 4 and continues to be operated at the MMT today. C1 [Szentgyorgyi, Andrew; Furesz, Gabor; Cheimets, Peter; Conroy, Maureen; Eng, Roger; Fabricant, Daniel; Fata, Robert; Gauron, Thomas; Geary, John; McLeod, Brian; Zajac, Joseph; Amato, Stephen; Bergner, Henry; Caldwell, Nelson; Dupree, Andrea; Goddard, Richard; Johnston, Everett; Meibom, Soeren; Mink, Douglas; Pieri, Mario; Roll, John; Tokarz, Susan; Wyatt, William] Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, Cambridge, MA 02138 USA. [Epps, Harland] Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA. [Hartmann, Lee] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Meszaros, Szabolcz] Univ Szeged, Dept Opt & Quantum Elect, Szeged, Hungary. RP Szentgyorgyi, A (reprint author), Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, 60 Garden St, Cambridge, MA 02138 USA. RI Meszaros, Szabolcs/N-2287-2014 OI Meszaros, Szabolcs/0000-0001-8237-5209 FU MMT instrument team; MMT; Whipple FX We are grateful for the contributions and support of the entire MMT instrument team and students and of the MMT and Whipple Observatory staff. We thank Kevin Bennett, David Bosworth, David Boyd, Daniel Blanco, William Brymer, David Caldwell, Shawn Callahan, Florine Collette, Emilio Falco, Craig Foltz, Art Gentile, Charles Hughes, Everett Johnston, Sheila Kannappan, Frank Licata, Steve Nichols, Dale Noll, Ricardo Ortiz, Tim Pickering, Frank Rivera, Phil Ritz, Cory Sassaman, Gary Schmidt, Dennis Smith, Ken Van Horn, David Weaver, Grant Williams and J. T. Williams. We thank the Robot positioner operators Perry Berlind and Mike Calkins and the MMT operators Mike Alegria, Alejandra Milone, and John McAfee. We are grateful to the efforts of the Harvard College Observatory Model Shop led by Larry Knowles. We thank Robert Dew and Diane Nutter of Cleveland Crystals and John Hoose of Richardson Grating Laboratory. NR 35 TC 16 Z9 16 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD OCT PY 2011 VL 123 IS 908 BP 1188 EP 1209 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 840XK UT WOS:000296475200006 ER PT J AU Lu, JM Li, DZ Lutz, S Soejima, A Yi, TS Wen, J AF Lu, Jin-Mei Li, De-Zhu Lutz, Sue Soejima, Akiko Yi, Tingshuang Wen, Jun TI BIOGEOGRAPHIC DISJUNCTION BETWEEN EASTERN ASIA AND NORTH AMERICA IN THE ADIANTUM PEDATUM COMPLEX (PTERIDACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Adiantum pedatum; biogeography; eastern Asia; eastern North America; North America; intercontinental disjunction; phylogeny; Pteridaceae ID BAYESIAN PHYLOGENETIC INFERENCE; HISTORICAL BIOGEOGRAPHY; CHLOROPLAST DNA; POLYSTICHUM DRYOPTERIDACEAE; MOLECULAR DIVERGENCE; FERN BIOGEOGRAPHY; GEOGRAPHIC RANGE; MAIDENHAIR FERN; EVOLUTION; HEMISPHERE AB Premise of the study: Biogeographic analyses of ferns with an eastern Asian-North American disjunction are few. The Adiantum pedatum complex has such a disjunct distribution. The monophyly of the complex needs to be tested and diversification history of the four species needs to be reconstructed. Methods: Plastid (atpA, atpB, rbcL, trnL-F, and rps4-trnS) sequences of 100 accessions representing the biogeographic diversity of Adiantum were analyzed with parsimony and Bayesian inference. Biogeography of the Adiantum pedatum complex was inferred using programs DIVA and LAGRANGE. Divergence times of clades were estimated with the program BEAST. Key results: The A. pedatum complex is monophyletic and sister to the eastern Asian A. edentulum. Accessions of A. pedatum do not form a clade; instead three subgroups are recognizable. The clade of A. aleuticum and A. viridimontanum is nested within A. pedatum. The Asian A. myriosorum is sister to the A. pedatum-A. aleuticum clade. Both DIVA and LAGRANGE analyses suggest an eastern Asian origin of the A. pedatum complex. The age of the crown A. pedatum complex is dated to be at 4.27 (2.24-6.57) million years ago. Conclusions: The currently recognized eastern Asian-North American disjunct species A. pedatum needs to be segregated into three species, corresponding to populations in eastern North America, China, and Japan. The eastern Asian-North American disjunction in the complex is inferred to be the result of two intercontinental migrations, one from eastern Asia into North America in the late Tertiary and the other from North America back to eastern Asia in the Pleistocene. C1 [Lu, Jin-Mei; Lutz, Sue; Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. [Lu, Jin-Mei; Li, De-Zhu] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Lu, Jin-Mei; Li, De-Zhu; Yi, Tingshuang] Germplasm Bank Wild Species, Plant Germplasm & Genom Ctr, Kunming 650204, Yunnan, Peoples R China. [Soejima, Akiko] Kumamoto Univ, Grad Sch Sci & Technol, Kumamoto 8608555, Japan. RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu OI li, de zhu/0000-0002-4990-724X FU John D. and Catherine T. MacArthur Foundation; National Basic Research Program of China (973 Program) [2007CB411601]; National Natural Science Foundation of China [30828001, 31070199, 30800063]; Chinese Academy of Sciences [2010KIBA02, 2009-LSF-GBOWS-01]; SRF for ROCS, SEM FX The study was supported by grants from the John D. and Catherine T. MacArthur Foundation (to J. Wen, R. Ree, and G. Mueller), National Basic Research Program of China (973 Program, grant no. 2007CB411601), the National Natural Science Foundation of China (grant nos. 30828001, 31070199, and 30800063), the Project of Knowledge Innovation Program of the Chinese Academy of Sciences (grant no. 2010KIBA02), the Research Fund for the Large-Scale Scientific Facilities of the Chinese Academy of Sciences (grant no. 2009-LSF-GBOWS-01), and the project sponsored by SRF for ROCS, SEM. NR 93 TC 19 Z9 20 U1 3 U2 21 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD OCT PY 2011 VL 98 IS 10 BP 1680 EP 1693 DI 10.3732/ajb.1100125 PG 14 WC Plant Sciences SC Plant Sciences GA 833ME UT WOS:000295888800023 PM 21965133 ER PT J AU Bruna, EM de Andrade, AS AF Bruna, Emilio M. de Andrade, Ana Segalin TI EDGE EFFECTS ON GROWTH AND BIOMASS PARTITIONING OF AN AMAZONIAN UNDERSTORY HERB (HELICONIA ACUMINATA; HELICONIACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE biomass allocation; common garden; forest fragmentation; Heliconiaceae; Heliconia acuminata; leaf area ratio; relative growth rate; specific leaf area ID TROPICAL RAIN-FOREST; PAST LAND-USE; PHENOTYPIC PLASTICITY; SPATIAL HETEROGENEITY; PLANT-POPULATIONS; HABITAT FRAGMENTATION; CONTRASTING HABITATS; GENOTYPIC VARIATION; LIGHT ENVIRONMENTS; SECONDARY FORESTS AB Premise: After deforestation, environmental changes in the remaining forest fragments are often most intense near the forest edge, but few studies have evaluated plant growth or plasticity of plant growth in response to edge effects. Methods: In a 2-year common garden experiment, we compared biomass allocation and growth of Heliconia acuminata with identical genotypes grown in 50 x 35 m common gardens on a 25-year-old edge and in a forest interior site. Key results: Genetically identical plants transplanted to the forest edge and understory exhibited different patterns of growth and biomass allocation. However, individuals with identical genotypes in the same garden often had very different responses. Plants on forest edges also had higher growth rates and increased biomass at the end of the experiment, almost certainly due to the increased light on the forest edge. Conclusions: With over 70 000 km of forest edge created annually in the Brazilian Amazon, phenotypic plasticity may play an important role in mediating plant responses to these novel environmental conditions. C1 [Bruna, Emilio M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Bruna, Emilio M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA. [Bruna, Emilio M.; de Andrade, Ana Segalin] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, AM, Brazil. [Bruna, Emilio M.; de Andrade, Ana Segalin] Smithsonian Trop Res Inst, BR-69011970 Manaus, AM, Brazil. RP Bruna, EM (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, POB 110430, Gainesville, FL 32611 USA. EM embruna@ufl.edu RI Bruna, Emilio/H-2769-2012 OI Bruna, Emilio/0000-0003-3381-8477 FU NSF [DEB-0309819]; Biological Dynamics of Forest Fragments Project (BDFFP) FX The authors thank J. Ewel, K. Kitajima, and two anonymous reviewers for helpful discussions and comments on the manuscript. A. M dos Reis and O. Ferreira da Silva provided assistance in the field, and financial support was provided by NSF Grant DEB-0309819 and the Biological Dynamics of Forest Fragments Project (BDFFP). This is publication number 584 in the BDFFP Technical Series. The data for the analyses in this article are archived with Data Dryad under record numbers doi:10.5061/dryad.553hc134 NR 62 TC 2 Z9 2 U1 2 U2 34 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD OCT PY 2011 VL 98 IS 10 BP 1727 EP 1734 DI 10.3732/ajb.1000290 PG 8 WC Plant Sciences SC Plant Sciences GA 833ME UT WOS:000295888800026 PM 21965134 ER PT J AU Kuffner, IB Hickey, TD Paul, VJ Morrison, JM Walters, LJ Grablow, KR Turner, T Parish, ER AF Kuffner, Ilsa B. Hickey, T. Don Paul, Valerie J. Morrison, Jennifer M. Walters, Linda J. Grablow, Katie R. Turner, Teresa Parish, Edward R. TI HALF-DEAD COLONIES OF MONTASTRAEA ANNULARIS RELEASE VIABLE GAMETES ON A DEGRADED REEF IN THE US VIRGIN ISLANDS SO BULLETIN OF MARINE SCIENCE LA English DT Editorial Material C1 [Kuffner, Ilsa B.; Hickey, T. Don; Morrison, Jennifer M.] US Geol Survey, St Petersburg, FL 33701 USA. [Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Walters, Linda J.; Grablow, Katie R.] Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. [Turner, Teresa; Parish, Edward R.] Univ Virgin Isl, Div Sci & Math, St Thomas, VI 00802 USA. RP Kuffner, IB (reprint author), US Geol Survey, 600 4th St S, St Petersburg, FL 33701 USA. EM ikuffner@usgs.gov OI Kuffner, Ilsa/0000-0001-8804-7847 NR 1 TC 1 Z9 1 U1 0 U2 4 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD OCT PY 2011 VL 87 IS 4 BP 855 EP 856 DI 10.5343/bms.2010.1103 PG 2 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 835ZA UT WOS:000296074600007 ER PT J AU Weber, CF Zak, DR Hungate, BA Jackson, RB Vilgalys, R Evans, RD Schadt, CW Megonigal, JP Kuske, CR AF Weber, Carolyn F. Zak, Donald R. Hungate, Bruce A. Jackson, Robert B. Vilgalys, Rytas Evans, R. David Schadt, Christopher W. Megonigal, J. Patrick Kuske, Cheryl R. TI Responses of soil cellulolytic fungal communities to elevated atmospheric CO2 are complex and variable across five ecosystems SO ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID SCRUB-OAK ECOSYSTEM; MOJAVE DESERT SOILS; LITTER DECOMPOSITION; CARBON-DIOXIDE; ABOVEGROUND BIOMASS; MICROBIAL BIOMASS; MODEL ECOSYSTEM; NITROGEN; FOREST; O-3 AB Elevated atmospheric CO2 generally increases plant productivity and subsequently increases the availability of cellulose in soil to microbial decomposers. As key cellulose degraders, soil fungi are likely to be one of the most impacted and responsive microbial groups to elevated atmospheric CO2. To investigate the impacts of ecosystem type and elevated atmospheric CO2 on cellulolytic fungal communities, we sequenced 10 677 cbhI gene fragments encoding the catalytic subunit of cellobiohydrolase I, across five distinct terrestrial ecosystem experiments after a decade of exposure to elevated CO2. The cbhI composition of each ecosystem was distinct, as supported by weighted Unifrac analyses (all P-values; < 0.001), with few operational taxonomic units (OTUs) being shared across ecosystems. Using a 114-member cbhI sequence database compiled from known fungi, less than 1% of the environmental sequences could be classified at the family level indicating that cellulolytic fungi in situ are likely dominated by novel fungi or known fungi that are not yet recognized as cellulose degraders. Shifts in fungal cbhI composition and richness that were correlated with elevated CO2 exposure varied across the ecosystems. In aspen plantation and desert creosote bush soils, cbhI gene richness was significantly higher after exposure to elevated CO2 (550 mu mol mol(-1)) than under ambient CO2 (360 mmol mol(-1) CO2). In contrast, while the richness was not altered, the relative abundance of dominant OTUs in desert soil crusts was significantly shifted. This suggests that responses are complex, vary across different ecosystems and, in at least one case, are OTU-specific. Collectively, our results document the complexity of cellulolytic fungal communities in multiple terrestrial ecosystems and the variability of their responses to long-term exposure to elevated atmospheric CO2. C1 [Weber, Carolyn F.; Kuske, Cheryl R.] Los Alamos Natl Lab, Biosci Div, Los Alamos, NM 87545 USA. [Zak, Donald R.] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. [Zak, Donald R.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Hungate, Bruce A.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. [Hungate, Bruce A.] No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. [Jackson, Robert B.; Vilgalys, Rytas] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Jackson, Robert B.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Evans, R. David] Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. [Schadt, Christopher W.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. [Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Washington, DC 20013 USA. RP Kuske, CR (reprint author), Los Alamos Natl Lab, Biosci Div, POB 1663, Los Alamos, NM 87545 USA. EM kuske@lanl.gov RI Zak, Donald/C-6004-2012; Hungate, Bruce/F-8991-2011; Schadt, Christopher/B-7143-2008 OI Hungate, Bruce/0000-0002-7337-1887; Schadt, Christopher/0000-0001-8759-2448 FU US Department of Energy Biological and Environmental Research [2010LANLF260]; DOE [2009LANLE660]; DOE Joint Genome Institute FX This project was funded by the US Department of Energy Biological and Environmental Research Program (SFA#2010LANLF260 to C.R.K.) and the DOE Program for Ecosystem Research (Grant #2009LANLE660 to C. R. K.). Sanger DNA sequencing was conducted at Los Alamos National Laboratory, by the DOE Joint Genome Institute. We wish to thank Kuan-Liang Liu, Gary Xie and John Knepper for providing data analysis advice and writing perl scripts for data analysis and parsing, as well as Lawrence Ticknor for statistical consulting. We also wish to thank Andrea Porras-Alfaro (Western Illinois University), Terri M. Porter (McMaster University), Michael S. Fitzsimons (LANL) and Lynn F. Weber for gifts of fungal cultures or sporocarps as well as Benjamin Wolfe (Harvard University) for providing unpublished cbhI sequence data to add to our database. La Verne Gallegos-Graves (LANL), Jennifer Price (LANL) and Asli Unal (LANL) provided excellent technical support. We also thank multiple people at the different field sites for helping collect field samples. NR 45 TC 22 Z9 22 U1 7 U2 38 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1462-2912 J9 ENVIRON MICROBIOL JI Environ. Microbiol. PD OCT PY 2011 VL 13 IS 10 BP 2778 EP 2793 DI 10.1111/j.1462-2920.2011.02548.x PG 16 WC Microbiology SC Microbiology GA 834OK UT WOS:000295971300014 PM 21883796 ER PT J AU Estrada, C Schulz, S Yildizhan, S Gilbert, LE AF Estrada, Catalina Schulz, Stefan Yildizhan, Selma Gilbert, Lawrence E. TI SEXUAL SELECTION DRIVES THE EVOLUTION OF ANTIAPHRODISIAC PHEROMONES IN BUTTERFLIES SO EVOLUTION LA English DT Article DE Female mating receptivity; Heliconius; male-male competition; male control on female reproduction; sexual conflict; signal evolution ID SEMINAL FLUID PROTEINS; HELICONIUS BUTTERFLIES; DROSOPHILA-MELANOGASTER; CHEMICAL COMMUNICATION; PHYLOGENETIC SIGNAL; SPERM PRECEDENCE; MATING-BEHAVIOR; FEMALE FITNESS; LEPIDOPTERA; CONFLICT AB Competition for mates has resulted in sophisticated mechanisms of male control over female reproduction. Antiaphrodisiacs are pheromones transferred from males to females during mating that reduce attractiveness of females to subsequent courting males. Antiaphrodisiacs generally help unreceptive females reduce male harassment. However, lack of control over pheromone release by females and male control over the amount transferred provides males an opportunity to use antiaphrodisiacs to delay remating by females that have returned to a receptive state. We propose a model for the evolution of antiaphrodisiacs under the influence of intrasexual selection, and determine whether changes in this signal in 11 species of Heliconius butterflies are consistent with two predictions of the model. First, we find that as predicted, male-contributed chemical mixtures are complex and highly variable across species, with limited phylogenetic signal. Second, differences in rates of evolution in pheromone composition between two major clades of Heliconius are as expected: the clade with a greater potential for male-male competition (polyandrous) shows a faster rate of divergence than the one with typically monoandrous mating system. Taken together, our results provide evidence that for females, antiaphrodisiacs can be both honest signals of receptivity (helping reduce harassment) and chastity belts (a male-imposed reduction in remating). C1 [Estrada, Catalina; Gilbert, Lawrence E.] Univ Texas Austin, Brackenridge Field Lab, Austin, TX 78712 USA. [Schulz, Stefan; Yildizhan, Selma] Tech Univ Carolo Wilhelmina Braunschweig, Inst Organ Chem, D-38106 Braunschweig, Germany. [Estrada, Catalina; Gilbert, Lawrence E.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. RP Estrada, C (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092 Balboa, Ancon, Panama. EM estradac@si.edu FU National Science Foundation; Office of International Science and Engineering [0608167]; Animal Behavior Society; Lepidoptera Research Foundation; Section of Integrative Biology of the University of Texas; Fonds der chemischen Industrie; UT Austin FX We thank J. Jamtsho, J. Crutchfield, G. Crutchfield, T. Alexander, S. Marout, A. Wartenberg, K. Busby, C. Strickland, for their help with butterfly rearing and maintenance of greenhouse facilities at Patterson Laboratory and the Brackenridge Field Laboratory. We are also grateful to S. Mikheyev and J. C. Santos for advice in data analysis, S. Pawar, G. Grether, C. Anderson, N. Losin, K. Deere, and three anonymous reviewers for comments on the manuscript, and M. Beltran for providing phylogenetic distances. This work was funded by the National Science Foundation and the Office of International Science and Engineering under grant No 0608167, Animal Behavior Society, Lepidoptera Research Foundation, the Section of Integrative Biology of the University of Texas, and Fonds der chemischen Industrie. The insects were imported to the USA under permits to LEG from USDA APHIS. We thank A. Vega for assistance with Costa Rican research, collecting and exportation permits and staff of P. N. Corcovado for facilitating fieldwork. Austin insectary facilities (LEG) were developed through funding from NSF and UT Austin. NR 80 TC 21 Z9 21 U1 2 U2 61 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0014-3820 J9 EVOLUTION JI Evolution PD OCT PY 2011 VL 65 IS 10 BP 2843 EP 2854 DI 10.1111/j.1558-5646.2011.01352.x PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 828RZ UT WOS:000295521600012 PM 21967426 ER PT J AU Derryberry, EP Claramunt, S Derryberry, G Chesser, RT Cracraft, J Aleixo, A Perez-Eman, J Remsen, JV Brumfield, RT AF Derryberry, Elizabeth P. Claramunt, Santiago Derryberry, Graham Chesser, R. Terry Cracraft, Joel Aleixo, Alexandre Perez-Eman, Jorge Remsen, J. V., Jr. Brumfield, Robb T. TI LINEAGE DIVERSIFICATION AND MORPHOLOGICAL EVOLUTION IN A LARGE-SCALE CONTINENTAL RADIATION: THE NEOTROPICAL OVENBIRDS AND WOODCREEPERS (AVES: FURNARIIDAE) SO EVOLUTION LA English DT Article DE Morphological Evolution; Phylogenetics; Adaptive Radiation ID DENSITY-DEPENDENT DIVERSIFICATION; ADAPTIVE RADIATION; MOLECULAR PHYLOGENIES; ECOLOGICAL OPPORTUNITY; CLADE DIVERSIFICATION; GEOGRAPHIC-VARIATION; SPECIES RICHNESS; EXTINCTION RATES; FOSSIL RECORD; HIGHER TAXA AB Patterns of diversification in species-rich clades provide insight into the processes that generate biological diversity. We tested different models of lineage and phenotypic diversification in an exceptional continental radiation, the ovenbird family Furnariidae, using the most complete species-level phylogenetic hypothesis produced to date for a major avian clade (97% of 293 species). We found that the Furnariidae exhibit nearly constant rates of lineage accumulation but show evidence of constrained morphological evolution. This pattern of sustained high rates of speciation despite limitations on phenotypic evolution contrasts with the results of most previous studies of evolutionary radiations, which have found a pattern of decelerating diversity-dependent lineage accumulation coupled with decelerating or constrained phenotypic evolution. Our results suggest that lineage accumulation in tropical continental radiations may not be as limited by ecological opportunities as in temperate or island radiations. More studies examining patterns of both lineage and phenotypic diversification are needed to understand the often complex tempo and mode of evolutionary radiations on continents. C1 [Derryberry, Elizabeth P.; Claramunt, Santiago; Remsen, J. V., Jr.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Derryberry, Graham] BioComp Asheville, Asheville, NC 28803 USA. [Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. [Cracraft, Joel] Amer Museum Nat Hist, Dept Ornithol, New York, NY 10024 USA. [Aleixo, Alexandre] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [Perez-Eman, Jorge] Cent Univ Venezuela, Inst Zool & Ecol Trop, Caracas 1041A, Venezuela. [Perez-Eman, Jorge] Colecc Ornitol Phelps, Caracas 1010A, Venezuela. RP Derryberry, EP (reprint author), Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. EM brumfld@lsu.edu RI Aleixo, Alexandre/L-3135-2013; OI Brumfield, Robb/0000-0003-2307-0688 FU NSF [DBI-0400797, DEB-0543562, EAR-0228693]; NSF-RTG (Univ. of Arizona); Univ. of Arizona; CNPq (Brazil) [310593/2009-3, 574008/2008-0, 476212/2007-3]; Sigma Xi FX We thank M. E. Alfaro, R. E. Ricklefs, C. D. Cadena, and two anonymous reviewers for helpful comments on earlier drafts of the manuscript. We thank numerous collectors, including C. M. Milensky, and institutions for providing tissue samples (see Table S1) and C. Burney, G. Bravo, C. D. Cadena, A. Cuervo, J. Maley, and L. Naka for sequence data for this project. G. Bravo, J. M. Brown, J. W. Brown, L. Harmon, C. Heibl, W. Pfeiffer, J. McCormack, D. Rabosky, A. Rambaut, and M. Tingley provided code, analysis assistance, and discussion concerning analyses. This research was supported in part by NSF grants DBI-0400797 and DEB-0543562 to RTB, NSF AToL grant EAR-0228693 to JC, Frank M. Chapman (AMNH) and NSF-RTG (Univ. of Arizona) postdoctoral fellowships and a faculty/research small grant (Univ. of Arizona) to RTC, CNPq (Brazil) grants 310593/2009-3, 574008/2008-0, and 476212/2007-3 to AA, and a Sigma Xi Grant-in-Aid of Research to SC. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 90 TC 117 Z9 119 U1 10 U2 77 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0014-3820 J9 EVOLUTION JI Evolution PD OCT PY 2011 VL 65 IS 10 BP 2973 EP 2986 DI 10.1111/j.1558-5646.2011.01374.x PG 14 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 828RZ UT WOS:000295521600022 PM 21967436 ER PT J AU Steppan, SJ Kenagy, GJ Zawadzki, C Robles, R Lyapunova, EA Hoffmann, RS AF Steppan, Scott J. Kenagy, G. J. Zawadzki, Christopher Robles, Rafael Lyapunova, Elena A. Hoffmann, Robert S. TI Molecular data resolve placement of the Olympic marmot and estimate dates of trans-Beringian interchange SO JOURNAL OF MAMMALOGY LA English DT Article DE cytochrome b; historical biogeography; Marmota olympus; phylogeny; RAG1 ID VANCOUVER-ISLAND MARMOT; MORPHOLOGICAL EVOLUTION; GEOMETRIC MORPHOMETRICS; RODENTIA; SCIURIDAE; PHYLOGENY; CRANIUM; DIFFERENTIATION; SPERMOPHILUS; SYSTEMATICS AB We reinvestigated the phylogeny of all 15 species of Marmota to resolve a conflict between 2 published analyses, one by Kruckenhauser et al. and another by Steppan et al., regarding the Olympic marmot (M. olympus) and to improve resolution in the genus. We acquired fresh samples of M. olympus, combined all available data on mitochondrial DNA (cytochrome b [Cytb] and ND3/ND4), new sequences for ND3/ND4, and 2,000 base pairs (bp) of the nuclear RAG1 gene. All analyses indicate that M. olympus is a much older, rather than more recent, offshoot of the widespread hoary marmot (M. caligata) or Vancouver Island marmot (M. vancouverensis). The mitochondrial data and some RAG1 results are largely congruent, but RAG1 differs on several points, including: the subgenus Marmota appears paraphyletic to Petromarmota, with reciprocally monophyletic Palearctic and Nearctic clades; and the long-tailed marmot (M. caudata) and Menzbier's marmot (M. menzbieri) are not sister species, suggesting mitochondrial introgression. Asia was colonized by Marmota from North America at approximately 4.6 million years ago (mya), followed by rapid diversification of several major lineages. M. olympus diverged from the M. caligata-M. vancouverensis lineage at approximately 2.6 mya, whereas M. vancouverensis and M. caligata diverged at only about 0.4-1.2 mya. M. olympus might have survived in isolation on the Olympic Peninsula in a nunatak refugium throughout a series of glacial maxima. C1 [Steppan, Scott J.; Zawadzki, Christopher; Robles, Rafael] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. [Kenagy, G. J.] Univ Washington, Burke Museum, Seattle, WA 98195 USA. [Kenagy, G. J.] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Lyapunova, Elena A.] Russian Acad Sci, Inst Dev Biol, Moscow, Russia. [Hoffmann, Robert S.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Steppan, SJ (reprint author), Florida State Univ, Dept Biol Sci, B-157, Tallahassee, FL 32306 USA. EM steppan@bio.fsu.edu RI Robles, Rafael/F-1967-2010; Lyapunova, Elena/A-4696-2016 FU National Science Foundation [DEB-9221504, DEB-0918982]; Smithsonian Institution; Institute of Developmental Biology, Russian Academy of Sciences, Moscow; Northwest Plateau Institute of Biology, Chinese Academy of Sciences, Xining; Division of Mammals, National Museum of Natural History, Smithsonian Institution, Washington, D.C. FX This paper is dedicated to our friend and colleague Bob Hoffmann, who died before completion of the manuscript. We thank S. Miller in the Florida State University sequencing facility for the DNA sequencing, A. B. Thistle for editorial revisions to this manuscript, and an anonymous reviewer for constructive comments. Field research was supported by the Institute of Developmental Biology, Russian Academy of Sciences, Moscow, the Northwest Plateau Institute of Biology, Chinese Academy of Sciences, Xining, and by the Division of Mammals, National Museum of Natural History, Smithsonian Institution, Washington, D.C. We thank Drs. W. Arnold and T. Ruff of the Research Institute of Wildlife Ecology, University of Veterinary Medicine, Vienna, Austria; J. Cook of the University of Alaska; P. Tongiori of the Department of Animal Biology, University of Modena, Italy; and D. Hafner of the New Mexico Museum of Natural History for loans of frozen tissue. We also thank A. Bryant of the Vancouver Island Marmot recovery team for supplying blood samples. Collecting in Eurasia was funded in part from National Science Foundation grant DEB-9221504 to Drs. R. Harrison and P. Sherman, Cornell University (RSH and E. Yensen, coinvestigators). Laboratory work was supported by a Smithsonian Institution Scholarly Studies Grant to SJS and RSH and National Science Foundation grant DEB-0918982 to SJS. NR 37 TC 7 Z9 7 U1 0 U2 26 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD OCT PY 2011 VL 92 IS 5 BP 1028 EP 1037 DI 10.1644/10-MAMM-A-272.1 PG 10 WC Zoology SC Zoology GA 835FR UT WOS:000296021600012 ER PT J AU Bozarth, CA Hailer, F Rockwood, LL Edwards, CW Maldonado, JE AF Bozarth, Christine A. Hailer, Frank Rockwood, Larry L. Edwards, Cody W. Maldonado, Jesus E. TI Coyote colonization of northern Virginia and admixture with Great Lakes wolves SO JOURNAL OF MAMMALOGY LA English DT Article DE Canis latrans; colonization; control region; coyote; eastern United States; Great Lakes wolf ID MITOCHONDRIAL-DNA PHYLOGEOGRAPHY; BEARS URSUS-AMERICANUS; GRAY WOLF; INTERFERENCE COMPETITION; GENETIC-CHARACTERIZATION; NORTHEASTERN COYOTES; POPULATION HISTORY; EASTERN COYOTES; HABITAT USE; RED WOLVES AB Ecological invasions of generalist species often are facilitated by anthropogenic disturbance. Coyotes (Canis latrans) have benefitted from anthropogenic changes to North American ecosystems and have experienced a dramatic range expansion since the early 19th century. The region east of the Mississippi River has been colonized via 2 routes that have converged in the mid-Atlantic region during the past few decades. Coyotes using the northern route of expansion show molecular evidence of admixture with the Great Lakes wolf (GLW). We used noninvasive molecular techniques to detect the geographic origins of the recent coyote colonization of northern Virginia as a representative of the mid-Atlantic region and to detect signatures of admixture with GLWs. Of 455 individual canid scats screened, we sequenced a variable 282-base pair fragment of the mitochondrial control region from 126 coyote scats, assigned individual identities to samples using 6 microsatellite loci, and conducted phylogeographic analyses by comparing our sequences to previously published haplotypes. In 39 individuals identified in our scat surveys we detected 7 mitochondrial DNA haplotypes, all of which have been previously reported in diverse surrounding geographic localities. Phylogeographic analyses indicate multiple sources of colonization of northern Virginia. One common haplotype detected in northern Virginia is of wolf origin, indicating the presence of admixed coyotes and GLWs from the north. C1 [Bozarth, Christine A.; Hailer, Frank; Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Bozarth, Christine A.; Rockwood, Larry L.; Edwards, Cody W.; Maldonado, Jesus E.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Maldonado, Jesus E.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Bozarth, CA (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. EM bozarthc@si.edu RI Hailer, Frank/C-9114-2012 OI Hailer, Frank/0000-0002-2340-1726 FU Naval Facilities Engineering Command Washington [N40080-08-LTC-0001] FX Financial and logistical assistance was provided by Naval Facilities Engineering Command Washington Cooperative Agreement N40080-08-LTC-0001 for Coyote Population Study at MCBQ, the Smithsonian Conservation Biology Institute Center for Conservation and Evolutionary Genetics, and the Smithsonian Institution National Museum of Natural History. We thank T. Stamps, C. Himmelberger, K. Robinson, N. Rotzel, and L. Lakeman for samples, assistance, and guidance. We also thank S. Lance and J. Leonard for providing haplotype data from their studies. NR 80 TC 17 Z9 18 U1 3 U2 33 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD OCT PY 2011 VL 92 IS 5 BP 1070 EP 1080 DI 10.1644/10-MAMM-A-223.1 PG 11 WC Zoology SC Zoology GA 835FR UT WOS:000296021600016 ER PT J AU Shik, JZ Kaspari, M Yanoviak, SP AF Shik, Jonathan Z. Kaspari, Michael Yanoviak, Stephen P. TI Preliminary Assessment of Metabolic Costs of the Nematode Myrmeconema neotropicum on its Host, the Tropical Ant Cephalotes atratus SO JOURNAL OF PARASITOLOGY LA English DT Article ID ENERGETIC COST; PARASITISM AB The parasitic nematode Myrmeconema neotropicum infects workers of the neotropical arboreal ant Cephalotes atratus. Infected ants exhibit altered behavior, e.g., reduced aggression and slower tempo, as well as physical traits, e.g., gaster changes from shiny black to bright red. These changes are thought to induce fruit mimicry and attract frugivorous birds, which are the presumed paratenic hosts for the nematodes. We used respirometry to measure the energetic costs of nematode infection, testing the prediction of higher metabolic rates for infected workers maintaining both ant and nematode biomass. Contrary to this prediction, infected workers had lower mass-specific metabolic rates than uninfected workers. Parasites are limited to the gasters (abdomens) of adult ants, and infected gasters had 57% more mass, but 37% lower metabolic rates, compared to uninfected glisters. These results use a metabolic currency to measure, in vivo, the energetic costs of parasitism, and they shed light on the complex co-evolutionary relationship between host and parasite. C1 [Shik, Jonathan Z.; Kaspari, Michael] Univ Oklahoma, Dept Zool, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. [Yanoviak, Stephen P.] Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA. RP Shik, JZ (reprint author), N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. EM jonathan.shik@gmail.com OI Kaspari, Michael/0000-0002-9717-5768 FU National Science Foundation [DEB-0842038, IOS 0843120] FX We thank Oris Acevedo, Belkys Jimenez, and the staff of the Smithsonian Tropical Research Institute for logistical support. This project was funded by the National Science Foundation under the grants DEB-0842038 to M.K., and IOS 0843120 to S.P.Y. NR 17 TC 4 Z9 4 U1 5 U2 42 PU AMER SOC PARASITOLOGISTS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-3395 J9 J PARASITOL JI J. Parasitol. PD OCT PY 2011 VL 97 IS 5 BP 958 EP 959 DI 10.1645/GE-2735.1 PG 2 WC Parasitology SC Parasitology GA 834HP UT WOS:000295950700039 PM 21506804 ER PT J AU Fontanella, JE Fish, FE Rybczynski, N Nweeia, MT Ketten, DR AF Fontanella, Janet E. Fish, Frank E. Rybczynski, Natalia Nweeia, Martin T. Ketten, Darlene R. TI Three-dimensional geometry of the narwhal (Monodon monoceros) flukes in relation to hydrodynamics SO MARINE MAMMAL SCIENCE LA English DT Article ID CETACEAN FLUKES; PERFORMANCE; EFFICIENCY; MOVEMENTS; BEHAVIOR C1 [Fontanella, Janet E.; Fish, Frank E.] W Chester Univ, Dept Biol, W Chester, PA 19383 USA. [Rybczynski, Natalia] Canadian Museum Nat, Ottawa, ON K1P 6P4, Canada. [Nweeia, Martin T.] Harvard Univ, Sch Dent Med, Boston, MA 02115 USA. [Nweeia, Martin T.] Smithsonian Inst, Washington, DC 20227 USA. [Ketten, Darlene R.] Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. [Ketten, Darlene R.] Harvard Univ, Sch Med, Dept Otol & Laryngol, Boston, MA 02114 USA. RP Fish, FE (reprint author), W Chester Univ, Dept Biol, W Chester, PA 19383 USA. EM ffish@wcupa.edu FU National Science Foundation [IOS-0640185]; CMN; Office of Naval Research; Harvard University FX We are indebted to Julie Arruda and Scott Cramer of Woods Hole Oceanographic Institution (WHOI) for assistance with transfers and CT scanning of the narwhal flukes and for assistance from James G. Mead and Charles W. Potter of the Marine Mammal Program of the Natural History Museum of the Smithsonian Institution, and Lisa-Marie Leclerc and Jaypootie Kooneeliusie. Sanja Hinic-Frlog assisted NR with transportation of the flukes from the CMN to WHOI. Kamal Khidas and Peter Frank (CMN) provided much help with the paper work and accessioning. The hunters' and trappers' organization of Qikiqtarjuaq are gratefully acknowledged. We are extremely grateful to Kristin Laidre for providing information on narwhals, which aided in the analysis of our data. The transport of all materials was in accordance with CITES permits. This work was funded in part by grants from the National Science Foundation (IOS-0640185) to FEF, by CMN funding to NR, by the Office of Naval Research to DRK, and by Harvard University to MTN. NR 28 TC 5 Z9 5 U1 3 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 EI 1748-7692 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD OCT PY 2011 VL 27 IS 4 BP 889 EP 898 DI 10.1111/j.1748-7692.2010.00439.x PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 834DC UT WOS:000295938200020 ER PT J AU Huang, L Shcherbakov, RV AF Huang, Lei Shcherbakov, Roman V. TI Faraday conversion and rotation in uniformly magnetized relativistic plasmas SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE plasmas; polarization; radiation mechanisms: general; radiative transfer; Galaxy: centre ID SAGITTARIUS-A-ASTERISK; SYNCHROTRON RADIATION; CIRCULAR-POLARIZATION; LINEAR-POLARIZATION; RESPONSE TENSOR; ACCRETION FLOW; THERMAL PLASMA; MODELS AB We provide precise fitting formulae for Faraday conversion and rotation coefficients in uniformly magnetized relativistic plasmas. The formulae are immediately applicable to rotation measure and circular polarization (CP) production in jets and hot accretion flows. We show the recipe and results for arbitrary isotropic particle distributions, in particular thermal and power law. The exact Faraday conversion coefficient is found to approach zero with the increasing particle energy. The non-linear corrections of Faraday conversion and rotation coefficients are found essential for reliable CP interpretation of Sagittarius A*. C1 [Huang, Lei] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Huang, Lei] Chinese Acad Sci, Key Lab Radio Astron, Shanghai 200030, Peoples R China. [Shcherbakov, Roman V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Huang, L (reprint author), Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. EM muduri@shao.ac.cn RI he, shuyi/K-2082-2014 FU National Natural Science Foundation of China [10625314, 10633010, 10821302]; Chinese Academy of Sciences [KJCX2-YW-T03]; National Key Basic Research Development Program of China [2007CB815405]; CAS/SAFEA; China Postdoctoral Science Foundation [20090450822]; Academia Sinica; NASA [NNX08AX04H, NNX11AE16G] FX The authors are grateful to Prof. Makoto Inoue, Dr Rohta Takahashi and Prof. Ramesh Narayan for useful suggestions. The comments of the anonymous referee helped us to improve the presentation of findings. This work was supported in part by the National Natural Science Foundation of China (grants 10625314, 10633010 and 10821302), the Knowledge Innovation Program of the Chinese Academy of Sciences (Grant No. KJCX2-YW-T03), the National Key Basic Research Development Program of China (No. 2007CB815405) and the CAS/SAFEA International Partnership Program for Creative Research Teams. LH acknowledges the support by the China Postdoctoral Science Foundation (grant 20090450822) and Regular Postdoctoral Research Fellowship in Academia Sinica. RVS acknowledges the support by NASA grants NNX08AX04H and NNX11AE16G. NR 25 TC 12 Z9 12 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 416 IS 4 BP 2574 EP 2592 DI 10.1111/j.1365-2966.2011.19207.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 829OJ UT WOS:000295592600015 ER PT J AU O'Sullivan, E Worrall, DM Birkinshaw, M Trinchieri, G Wolter, A Zezas, A Giacintucci, S AF O'Sullivan, E. Worrall, D. M. Birkinshaw, M. Trinchieri, G. Wolter, A. Zezas, A. Giacintucci, S. TI Interaction between the intergalactic medium and central radio source in the NGC 4261 group of galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: 3C 270; galaxies: individual: NGC4261; intergalactic medium; X-rays: galaxies ID DEEP CHANDRA OBSERVATION; X-RAY LUMINOSITY; ACTIVE GALACTIC NUCLEUS; HUBBLE-SPACE-TELESCOPE; XMM-NEWTON OBSERVATION; ELLIPTIC GALAXIES; STAR-FORMATION; HOT GAS; BLACK-HOLE; JET POWER AB Using observations from the Chandra and XMM-Newton X-ray observatories, we examine the interaction between the intragroup medium and central radio source in the nearby NGC 4261 galaxy group. We confirm the presence of cavities associated with the radio lobes and estimate their enthalpy to be similar to 2.4 x 10(58) erg. The mechanical power output of the jets is >= 10(43) erg s(-1), at least a factor of 60 greater than the cooling luminosity in the region the lobes inhabit. We identify rims of compressed gas enclosing the lobes, but find no statistically significant temperature difference between them and their surroundings, suggesting that the lobe expansion velocity is approximately sonic (M <= 1.05). The apparent pressure of the radio lobes, based on the synchrotron minimum energy density argument, is a factor of 5 lower than that of the intragroup medium. Pressure balance could be achieved if the entrainment of thermal gas provided additional non-radiating particles in the lobe plasma, but the energy required to heat these particles would be similar to 20 per cent of the mechanical energy output of the radio source. NGC 4261 has a relatively compact cool core, which should probably be categorized as a galactic corona. The corona is capable of fuelling the active nucleus for considerably longer than the inferred source lifetime, but can be only inefficiently heated by the active galactic nucleus (AGN) or conduction. The expansion of the radio lobes has affected the structure of the gas in the galaxy, compressing and moving the material of the corona without causing significant shock heating, and expelling gas from the immediate neighbourhood of the jets. We discuss the possible implications of this environment for the duration of the AGN outburst and consider mechanisms which might lead to the cessation of nuclear activity. C1 [O'Sullivan, E.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [O'Sullivan, E.; Zezas, A.; Giacintucci, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Worrall, D. M.; Birkinshaw, M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Trinchieri, G.; Wolter, A.] Osserv Astron Brera, I-20121 Milan, Italy. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Zezas, A.] Fdn Res & Technol Hela, IESL, Iraklion 7110, Greece. [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP O'Sullivan, E (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM ejos@star.sr.bham.ac.uk RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Wolter, Anna/0000-0001-5840-9835; O'Sullivan, Ewan/0000-0002-5671-6900; Trinchieri, Ginevra/0000-0002-0227-502X FU National Aeronautics and Space Administration [G08-9094X, NAS8-03060]; ESA Member States; NASA; European Community under the Marie Curie Research Training Network; EU [206469]; Agenzia Spaziale Italiana [ASI-INAF I/009/10/0] FX The authors thank the anonymous referee for several useful suggestions, and P. Bonfini for providing optical data for NGC 4261. EO'S thanks A. Sanderson for useful discussions of the X-ray analysis. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G08-9094X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. This work is partially based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work has used data from the VLA. EO'S acknowledges the support of the European Community under the Marie Curie Research Training Network. Space Astrophysics in Crete is partly supported by EU FP7 Capacities GA No. 206469. GT and AW acknowledge support from the Agenzia Spaziale Italiana through grant ASI-INAF I/009/10/0. We acknowledge the usage of the HyperLeda data base (http://leda.univ-lyon1.fr). NR 98 TC 18 Z9 18 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2011 VL 416 IS 4 BP 2916 EP 2931 DI 10.1111/j.1365-2966.2011.19239.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 829OJ UT WOS:000295592600039 ER PT J AU Toscano, MA Peltier, WR Drummond, R AF Toscano, Marguerite A. Peltier, W. Richard Drummond, Rosemarie TI ICE-5G and ICE-6G models of postglacial relative sea-level history applied to the Holocene coral reef record of northeastern St Croix, U.S.V.I.: investigating the influence of rotational feedback on GIA processes at tropical latitudes SO QUATERNARY SCIENCE REVIEWS LA English DT Article DE Holocene sea-level rise; St. Croix; USVI; Coral reef record; Geophysical sea-level models; Rotational feedback; Latitudinal extent of proglacial forebulge ID GLACIAL-ISOSTATIC-ADJUSTMENT; VIRGIN-ISLANDS; PUERTO-RICO; MANTLE VISCOSITY; VM2 MODEL; EARTH; ATLANTIC; MAXIMUM; BARBADOS; PLATFORM AB Fossil coral reefs along the northeastern coast of St Croix in the Caribbean Sea provide an 8000 year record of dated and interpreted Holocene sea-level change. We herein compare this record with the predictions of models of glacio-hydro-isostatic adjustment for St Croix and for additional sites at similar latitudes in the Greater and Lesser Antilles region. RSL predictions are based upon the model ICE-5G (VM2), and with a modified model ICE-6G (VM5A), both including and excluding the influence of rotational feedback. Misfits between the modeled sea levels and the local geologic data are most apparent for models without rotational feedback, particularly in the prediction of a +2 to +4 m unsupported mid-Holocene misfit at similar to 4 ka, as well as a small-amplitude highstand that extends from 2.5 to 1.5 ka. Incorporation of the influence of rotational feedback provides the best fit to the data, largely eliminating the unsupported mid-Holocene misfit between the data field and the sea-level histories predicted by the models without rotational feedback, and fitting data older than 5 kyr more closely than a previously published latitudinally-averaged sea-level curve for the western Atlantic. The St Croix data therefore demonstrate that rotational influence extends at least 27 degrees further south from its 45 degrees N mid-latitude extremum along the US east coast, and identifies tropical latitudes as influenced by proglacial forebulge collapse. Implications for reef-based sea-level reconstruction include the ability to accurately model sea levels at specific tropical sites with partial Holocene chronologies using the ICE-6G (VM5A) model with rotational feedback. Latitudinally-averaged sea-level curves are therefore of limited use in understanding the relative importance of contributing physical influences on postglacial sea-level history. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Toscano, Marguerite A.] NMNH, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Peltier, W. Richard; Drummond, Rosemarie] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Toscano, MA (reprint author), NMNH, Smithsonian Inst, Dept Paleobiol, POB 37012,MRC-121, Washington, DC 20013 USA. EM toscanom@si.edu; peltier@atmosp.physics.utoronto.ca; rmarie@atmosp.physics.utoronto.ca RI Peltier, William/A-1102-2008 FU NSF [0921879]; Smithsonian Institution, Department of Paleobiology; Canadian Foundation for Climate and Atmospheric Sciences; consortium of Canadian universities; NSERC [A9627] FX NSF grant 0921879 and the Smithsonian Institution, Department of Paleobiology provided support to MAT. This paper is a contribution to the work of the Polar Climate Stability Network which has been sponsored by the Canadian Foundation for Climate and Atmospheric Sciences and by a consortium of Canadian universities as well as NSERC Discovery Grant A9627 to WRP. Computations have been performed on the SciNet facility for High Performance Computation which an element of the Compute Canada HPC platform. Ian Macintyre, Ian Shennan and one anonymous reviewer provided important assistance in improving the manuscript. NR 70 TC 24 Z9 24 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD OCT PY 2011 VL 30 IS 21-22 BP 3032 EP 3042 DI 10.1016/j.quascirev.2011.07.018 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 830NK UT WOS:000295663500012 ER PT J AU Hintz, E AF Hintz, Eric TI Edison's Electric Light: The Art of Invention SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Hintz, Eric] Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA. RP Hintz, E (reprint author), Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 2011 VL 52 IS 4 BP 829 EP 831 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 836MW UT WOS:000296116800022 ER PT J AU Stine, JK AF Stine, Jeffrey K. TI The Nature of New York: An Environmental History of the Empire State SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Stine, Jeffrey K.] Natl Museum Amer Hist, Smithsonian Inst, Div Med & Sci, Washington, DC 20560 USA. RP Stine, JK (reprint author), Natl Museum Amer Hist, Smithsonian Inst, Div Med & Sci, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 2011 VL 52 IS 4 BP 838 EP 840 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 836MW UT WOS:000296116800027 ER PT J AU Moini, M Klauenberg, K Ballard, M AF Moini, Mehdi Klauenberg, Kathryn Ballard, Mary TI Dating Silk By Capillary Electrophoresis Mass Spectrometry SO ANALYTICAL CHEMISTRY LA English DT Article ID ASPARTIC-ACID RACEMIZATION; AMINO-ACIDS; CHROMATOGRAPHY; PRESERVATION AB A new capillary electrophoresis mass spectrometry (CE-MS) technique is introduced for age estimation of silk textiles based on amino acid racemization rates. With an L to D conversion half-life of similar to 2500 years for silk (B. mari) aspartic acid, the technique is capable of dating silk textiles ranging in age from several decades to a few-thousand-years-old. Analysis required only similar to 100 mu g or less of silk fiber. Except for a 2 h acid hydrolysis at 110 degrees C, no other sample preparation is required. The CE-MS analysis takes similar to 20 min, consumes only nanoliters of the amino acid mixture, and provides both amino acid composition profiles and D/L ratios for similar to 11 amino acids. C1 [Moini, Mehdi; Klauenberg, Kathryn; Ballard, Mary] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Moini, M (reprint author), Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM MoiniM@si.edu FU Smithsonian's Museum Conservation Institute FX We wish to thank the Smithsonian's Museum Conservation Institute Director and Deputy Director, Drs. Robert J. Koestler and Paula T. DePriest, for their support of this project. We also wish to thank several curators and conservators who have provided expertise as well as silk samples: Dr. Sumru Kordy and Ms. Esther Methe of the Textile Museum; Dr. James C. Y. Watt and Ms. Joyce Denney of the Metropolitan Museum of Art; Dr. Blythe McCarthy of the Smithsonian's Freer and Sadder Galleries; Ms. Laura Mina of the Smithsonian Museum Conservation Institute; Ms. Phyllis Magidson of the Museum of the City of New York; Ms. Jennifer Jones and Ms. Suzanne Thomassen-Krauss of the National Museum of American History; and Dr. Katja Schmitz-von Ledebur from the Kunsthistoriches Museum, Vienna, Austria. We also wish to thank intern Casey Kohnhorst for her assistance in proteomics analysis of silk acid hydrolysates. NR 31 TC 22 Z9 22 U1 3 U2 22 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0003-2700 J9 ANAL CHEM JI Anal. Chem. PD OCT 1 PY 2011 VL 83 IS 19 BP 7577 EP 7581 DI 10.1021/ac201746u PG 5 WC Chemistry, Analytical SC Chemistry GA 825SY UT WOS:000295303600050 PM 21913691 ER PT J AU Boyer, ML Srinivasan, S van Loon, JT McDonald, I Meixner, M Zaritsky, D Gordon, KD Kemper, F Babler, B Block, M Bracker, S Engelbracht, CW Hora, J Indebetouw, R Meade, M Misselt, K Robitaille, T Sewillo, M Shiao, B Whitney, B AF Boyer, Martha L. Srinivasan, Sundar van Loon, Jacco Th. McDonald, Iain Meixner, Margaret Zaritsky, Dennis Gordon, Karl D. Kemper, F. Babler, Brian Block, Miwa Bracker, Steve Engelbracht, Charles W. Hora, Joe Indebetouw, Remy Meade, Marilyn Misselt, Karl Robitaille, Thomas Sewillo, Marta Shiao, Bernie Whitney, Barbara TI SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). II. COOL EVOLVED STARS SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; Magellanic Clouds; stars: AGB and post-AGB; stars: carbon; stars: mass-loss; supergiants ID ASYMPTOTIC GIANT BRANCH; SPITZER-SPACE-TELESCOPE; MASS-LOSS RATES; RICH AGB-STARS; DWARF IRREGULAR GALAXIES; NEAR-INFRARED PHOTOMETRY; YOUNG STELLAR OBJECTS; CLUSTER 47 TUCANAE; LOCAL GROUP DWARFS; EXTRINSIC S-STARS AB We investigate the infrared (IR) properties of cool, evolved stars in the Small Magellanic Cloud (SMC), including the red giant branch (RGB) stars and the dust-producing red supergiant (RSG) and asymptotic giant branch (AGB) stars using observations from the Spitzer Space Telescope Legacy program entitled "Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity SMC," or SAGE-SMC. The survey includes, for the first time, full spatial coverage of the SMC bar, wing, and tail regions at IR wavelengths (3.6-160 mu m). We identify evolved stars using a combination of near-IR and mid-IR photometry and point out a new feature in the mid-IR color-magnitude diagram that may be due to particularly dusty O-rich AGB stars. We find that the RSG and AGB stars each contribute approximate to 20% of the global SMC flux (extended + point-source) at 3.6 mu m, which emphasizes the importance of both stellar types to the integrated flux of distant metal-poor galaxies. The equivalent SAGE survey of the higher-metallicity Large Magellanic Cloud (SAGE-LMC) allows us to explore the influence of metallicity on dust production. We find that the SMC RSG stars are less likely to produce a large amount of dust (as indicated by the [3.6] - [8] color). There is a higher fraction of carbon-rich stars in the SMC, and these stars appear to reach colors as red as their LMC counterparts, indicating that C-rich dust forms efficiently in both galaxies. A preliminary estimate of the dust production in AGB and RSG stars reveals that the extreme C-rich AGB stars dominate the dust input in both galaxies, and that the O-rich stars may play a larger role in the LMC than in the SMC. C1 [Boyer, Martha L.; Meixner, Margaret; Gordon, Karl D.; Shiao, Bernie] STScI, Baltimore, MD 21218 USA. [Srinivasan, Sundar] CNRS, Inst Astrophys Paris, UPR 341, F-75014 Paris, France. [van Loon, Jacco Th.] Univ Keele, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England. [McDonald, Iain; Kemper, F.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Zaritsky, Dennis; Block, Miwa; Engelbracht, Charles W.; Misselt, Karl] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Babler, Brian; Bracker, Steve; Meade, Marilyn; Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Hora, Joe; Robitaille, Thomas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Sewillo, Marta] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Boyer, ML (reprint author), STScI, Baltimore, MD 21218 USA. EM mboyer@stsci.edu RI Kemper, Francisca/D-8688-2011; OI Kemper, Francisca/0000-0003-2743-8240; Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650; Robitaille, Thomas/0000-0002-8642-1329 FU NASA [1309827, 1340964] FX This work is supported by NASA via JPL contracts 1309827 and 1340964. We thank the anonymous referee for thoughtful remarks. NR 144 TC 64 Z9 64 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2011 VL 142 IS 4 AR 103 DI 10.1088/0004-6256/142/4/103 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822JY UT WOS:000295042500007 ER PT J AU Brown, TM Latham, DW Everett, ME Esquerdo, GA AF Brown, Timothy M. Latham, David W. Everett, Mark E. Esquerdo, Gilbert A. TI KEPLER INPUT CATALOG: PHOTOMETRIC CALIBRATION AND STELLAR CLASSIFICATION SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; methods: data analysis; surveys; techniques: photometric ID DIGITAL SKY SURVEY; DATA RELEASE; STARS; EXTINCTION; SPECTRA; SYSTEM; RADIUS; FIELD; MASS; M67 AB We describe the photometric calibration and stellar classification methods used by the Stellar Classification Project to produce the Kepler Input Catalog (KIC). The KIC is a catalog containing photometric and physical data for sources in the Kepler mission field of view; it is used by the mission to select optimal targets. Four of the visible-light (g, r, i, z) magnitudes used in the KIC are tied to Sloan Digital Sky Survey magnitudes; the fifth (D51) is an AB magnitude calibrated to be consistent with Castelli & Kurucz (CK) model atmosphere fluxes. We derived atmospheric extinction corrections from hourly observations of secondary standard fields within the Kepler field of view. For these filters and extinction estimates, repeatability of absolute photometry for stars brighter than magnitude 15 is typically 2%. We estimated stellar parameters {T(eff), log(g), log(Z), E(B-V)} using Bayesian posterior probability maximization to match observed colors to CK stellar atmosphere models. We applied Bayesian priors describing the distribution of solar-neighborhood stars in the color-magnitude diagram, in log(Z), and in height above the galactic plane. Several comparisons with samples of stars classified by other means indicate that for 4500 K <= T(eff) <= 6500 K, our classifications are reliable within about +/- 200 K and 0.4 dex in log(g) for dwarfs, with somewhat larger log(g) uncertainties for giants. It is difficult to assess the reliability of our log(Z) estimates, but there is reason to suspect that it is poor, particularly at extreme T(eff). Comparisons between the CK models and observed colors are generally satisfactory with some exceptions, notably for stars cooler than 4500 K. Of great importance for the Kepler mission, for T(eff) <= 5400 K, comparison with asteroseismic results shows that the distinction between main-sequence stars and giants is reliable with about 98% confidence. Larger errors in log(g) occur for warmer stars, for which our filter set provides inadequate gravity diagnostics. The KIC is available through the MAST data archive. C1 [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Latham, David W.; Esquerdo, Gilbert A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85721 USA. RP Brown, TM (reprint author), Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. EM tbrown@lcogt.net; latham@cfa.harvard.edu; everett@noao.edu; gesquerd@cfa.harvard.edu FU NASA [NNX10AG02A]; National Science Foundation; NASA with the Smithsonian Astrophysical Observatory [NCC-1390] FX We are grateful to the Mt. Hopkins support and observing staff, especially Carl Hergenrother, for his tireless work obtaining the necessary observations. We also thank Dave Monet, for his indispensable help in implementing the KIC astrometry methods, and for federating the SCP with other catalogs that carry essential information. We thank Steve Howell, for helping to define our photometric approach in the project's early days. We thank Geoff Marcy, Howard Isaacson, Debra Fischer, Bill Cochran, Sam Quinn, Lars Buchhave, Mike Endl, and Phillip MacQueen for the use of their spectra and spectral analysis of Kepler target stars. We also thank Saskia Hekker, Bill Chaplin, Ronald Gilliland, and dozens of members of the Kepler Asteroseismic Consortium for making their seismic data available before publication. We are deeply grateful to the Kepler Science Team and everyone connected with the Kepler mission, for keeping the mission running smoothly, and for providing the amazing Kepler photometric data, the promise of which was the inspiration for the current work. We thank Jeffrey Scargle for a careful reading of an early version of this work, and Don Kolinski for extensive software development help. T.M.B. acknowledges support from NASA Grant Number NNX10AG02A, and thanks HAO/NCAR and Las Cumbres Observatory Global Telescope for patience and support while this work was being done. The National Center for Atmospheric Research is supported by the National Science Foundation. We are grateful to the Kepler mission for partial support of the photometric observations under NASA Cooperative Agreement NCC-1390 with the Smithsonian Astrophysical Observatory. NR 37 TC 390 Z9 390 U1 3 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2011 VL 142 IS 4 AR 112 DI 10.1088/0004-6256/142/4/112 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822JY UT WOS:000295042500016 ER PT J AU Etxaluze, M Smith, HA Tolls, V Stark, AA Gonzalez-Alfonso, E AF Etxaluze, M. Smith, Howard A. Tolls, V. Stark, A. A. Gonzalez-Alfonso, E. TI THE GALACTIC CENTER IN THE FAR-INFRARED SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; Galaxy: center; infrared: ISM; ISM: individual objects (Sgr A*) ID CIRCUMNUCLEAR DISK; MOLECULAR CLOUDS; TEMPERATURE-DEPENDENCE; STELLAR ORBITS; STAR-FORMATION; CENTER REGION; BLACK-HOLE; ISO-LWS; DUST; GALAXY AB We analyze the far-infrared dust emission from the Galactic center region, including the circumnuclear disk (CND) and other structures, using Herschel PACS and SPIRE photometric observations. These Herschel data are complemented by unpublished observations by the Infrared Space Observatory Long Wavelength Spectrometer (ISO-LWS), which used parallel mode scans to obtain photometric images of the region with a larger beam than Herschel but with a complementary wavelength coverage and more frequent sampling with 10 detectors observing at 10 different wavelengths in the range from 46 mu m to 180 mu m, where the emission peaks. We also include data from the Midcourse Space Experiment at 21.3 mu m for completeness. We model the combined ISO-LWS continuum plus Herschel PACS and SPIRE photometric data toward the central 2 pc in Sagittarius A* (Sgr A*), a region that includes the CND. We find that the far-infrared spectral energy distribution is best represented by a continuum that is the sum of three gray body curves from dust at temperatures of 90, 44.5, and 23 K. We obtain temperature and molecular hydrogen column density maps of the region. We estimate the mass of the inner part of the CND to be similar to 5.0 x 10(4) M(circle dot), with luminosities: L(cavity) similar to 2.2 x 10(6) L(circle dot) and LCND similar to 1.5 x 10(6) L(circle dot) in the central 2 pc radius around Sgr A*. We find from the Herschel and ISO data that the cold component of the dust dominates the total dust mass, with a contribution of similar to 3.2 x 10(4) M(circle dot); this important cold material had escaped the notice of earlier studies that relied on shorter wavelength observations. The hotter component disagrees with some earlier estimates, but is consistent with measured gas temperatures and with models that imply shock heating or turbulent effects are at work. We find that the dust grain sizes apparently change widely across the region, perhaps in response to the temperature variations, and we map that distribution. C1 [Etxaluze, M.; Smith, Howard A.; Tolls, V.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Alcala De Henares 28801, Spain. [Gonzalez-Alfonso, E.] CfA, Alcala De Henares 28801, Spain. RP Etxaluze, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM metxaluz@cfa.harvard.edu OI Stark, Antony/0000-0002-2718-9996 FU NASA [NNX10AD83G] FX We thank the referee for his or her careful reading of the paper, and for the useful comments made. We are very grateful to Tanya Lim for her suggestions on the treatment of the ISO-LWS parallel mode data. This work was supported in part by NASA Grant NNX10AD83G. The ISO-LWS LIA is a joint development of the ISO-LWS Instrument Team at Rutherford Appleton Laboratory and the Infrared Processing and Analysis Center (IPAC/Caltech, USA). HIPE is a joint development by the Herschel Science Ground Segment Consortium consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. NR 47 TC 19 Z9 19 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2011 VL 142 IS 4 AR 134 DI 10.1088/0004-6256/142/4/134 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822JY UT WOS:000295042500038 ER PT J AU Fernandez-Lopez, M Girart, JM Curiel, S Gomez, Y Ho, PTP Patel, N AF Fernandez-Lopez, M. Girart, J. M. Curiel, S. Gomez, Y. Ho, P. T. P. Patel, N. TI A ROTATING MOLECULAR DISK TOWARD IRAS 18162-2048, THE EXCITING SOURCE OF HH 80-81 SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM: individual objects (GGD27, IRAS 18162-2048, HH 80-81); stars: formation; submillimeter: ISM ID HERBIG-HARO OBJECTS; MASSIVE STAR-FORMATION; ULTRACOMPACT HII-REGIONS; LARGE PROPER MOTIONS; THERMAL RADIO JET; HOT CORES; INTERFEROMETRIC OBSERVATIONS; MILLIMETER OBSERVATIONS; COLLISIONAL FORMATION; SUBMILLIMETER ARRAY AB We present several molecular line emission arcsecond and subarcsecond observations obtained with the Submillimeter Array in the direction of the massive protostar IRAS 18162-2048, the exciting source of HH 80-81. The data clearly indicate the presence of a compact (radius approximate to 425-850 AU) SO2 structure, enveloping the more compact (radius less than or similar to 150 AU) 1.4 mm dust emission (reported in a previous paper). The emission spatially coincides with the position of the prominent thermal radio jet which terminates at the HH 80-81 and HH 80N Herbig-Haro objects. Furthermore, the molecular emission is elongated in the direction perpendicular to the axis of the thermal radio jet, suggesting a disk-like structure. We derive a total dynamic mass (disk-like structure and protostar) of 11-15 M-circle dot. The SO2 spectral line data also allow us to constrain the structure temperature between 120 and 160 K and the volume density greater than or similar to 2 x 10(9) cm(-3). We also find that such a rotating flattened system could be unstable due to gravitational disturbances. The data from (CO)-O-17 line emission show a dense core within this star-forming region. Additionally, the H2CO and SO emissions appear clumpy and trace the disk-like structure, a possible interaction between a molecular core and the outflows, and in part, the cavity walls excavated by the thermal radio jet. C1 [Fernandez-Lopez, M.; Curiel, S.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Girart, J. M.] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Bellaterra 08193, Catalunya, Spain. [Gomez, Y.] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, P. T. P.; Patel, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fernandez-Lopez, M (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. EM manferna@gmail.com; girart@ieec.cat; scuriel@astroscu.unam.mx; y.gomez@astrosmo.unam.mx RI Girart, Josep/O-1638-2014 OI Girart, Josep/0000-0002-3829-5591 FU DGAP-UNAM, Mexico; Spanish MICINN [AYA2008-06189-C03]; Catalan AGAUR [2009SGR1172]; CONACyT, Mexico [60581]; CONACyT [80769, 49947-F] FX We thank all members of the SMA staff who made these observations possible. M.F.L. acknowledges financial support from DGAP-UNAM, Mexico. J.M.G. is supported by the Spanish MICINN AYA2008-06189-C03 and the Catalan AGAUR 2009SGR1172 grants. S.C. and M.F.L. acknowledge support from CONACyT grant 60581, Mexico. S.C. and M.F.L. thank the hospitality of the Institut de Ciencies de l'Espai (CSIC-IEEC), Bellaterra, Catalunya, Spain. Y.G. acknowledges support from CONACyT grants 80769 and 49947-F. NR 88 TC 12 Z9 12 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 OCT PY 2011 VL 142 IS 4 AR 97 DI 10.1088/0004-6256/142/4/97 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822JY UT WOS:000295042500001 ER PT J AU Geller, MJ Diaferio, A Kurtz, MJ AF Geller, Margaret J. Diaferio, Antonaldo Kurtz, Michael J. TI MAPPING THE UNIVERSE: THE 2010 RUSSELL LECTURE SO ASTRONOMICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; large-scale structure of universe ID FIBER-FED SPECTROGRAPH; REGION NEARBY SURVEY; DIGITAL SKY SURVEY; GALAXY CLUSTERS; RICH CLUSTERS; MASS PROFILES; REDSHIFT SURVEY; INFALL PATTERNS; HECTOSPEC; EVOLUTION AB Redshift surveys are a powerful tool of modern cosmology. We discuss two aspects of their power to map the distribution of mass and light in the universe: (1) measuring the mass distribution extending into the infall regions of rich clusters and (2) applying deep redshift surveys to the selection of clusters of galaxies and to the identification of very large structures (Great Walls). We preview the HectoMAP project, a redshift survey with median redshift z = 0.34 covering 50 deg(2) to r = 21. We emphasize the importance and power of spectroscopy for exploring and understanding the nature and evolution of structure in the universe. C1 [Geller, Margaret J.; Kurtz, Michael J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mgeller@cfa.harvard.edu; adiaferio@cfa.harvard.edu; mkurtz@cfa.harvard.edu RI KURTZ, Michael /B-3890-2009; OI Kurtz, Michael/0000-0002-6949-0090 FU Smithsonian Institution; Smithsonian Fellowship; INFN [PD51]; [2008NR3EBK] FX The Smithsonian Institution supports the research of Margaret Geller and Michael Kurtz, and during 2010-2011, a Smithsonian Fellowship partially supported Antonaldo Diaferio. INFN grant PD51 and the PRIN-MIUR-2008 grant 2008NR3EBK also support Antonaldo Diaferio. NR 51 TC 7 Z9 7 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 OCT PY 2011 VL 142 IS 4 AR 133 DI 10.1088/0004-6256/142/4/133 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822JY UT WOS:000295042500037 ER PT J AU Gordon, KD Meixner, M Meade, MR Whitney, B Engelbracht, C Bot, C Boyer, ML Lawton, B Sewilo, M Babler, B Bernard, JP Bracker, S Block, M Blum, R Bolatto, A Bonanos, A Harris, J Hora, JL Indebetouw, R Misselt, K Reach, W Shiao, B Tielens, X Carlson, L Churchwell, E Clayton, GC Chen, CHR Cohen, M Fukui, Y Gorjian, V Hony, S Israel, FP Kawamura, A Kemper, F Leroy, A Li, A Madden, S Marble, AR McDonald, I Mizuno, A Mizuno, N Muller, E Oliveira, JM Olsen, K Onishi, T Paladini, R Paradis, D Points, S Robitaille, T Rubin, D Sandstrom, K Sato, S Shibai, H Simon, JD Smith, LJ Srinivasan, S Vijh, U Van Dyk, S van Loon, JT Zaritsky, D AF Gordon, K. D. Meixner, M. Meade, M. R. Whitney, B. Engelbracht, C. Bot, C. Boyer, M. L. Lawton, B. Sewilo, M. Babler, B. Bernard, J. -P. Bracker, S. Block, M. Blum, R. Bolatto, A. Bonanos, A. Harris, J. Hora, J. L. Indebetouw, R. Misselt, K. Reach, W. Shiao, B. Tielens, X. Carlson, L. Churchwell, E. Clayton, G. C. Chen, C. -H. R. Cohen, M. Fukui, Y. Gorjian, V. Hony, S. Israel, F. P. Kawamura, A. Kemper, F. Leroy, A. Li, A. Madden, S. Marble, A. R. McDonald, I. Mizuno, A. Mizuno, N. Muller, E. Oliveira, J. M. Olsen, K. Onishi, T. Paladini, R. Paradis, D. Points, S. Robitaille, T. Rubin, D. Sandstrom, K. Sato, S. Shibai, H. Simon, J. D. Smith, L. J. Srinivasan, S. Vijh, U. Van Dyk, S. van Loon, J. Th Zaritsky, D. TI SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). I. OVERVIEW SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (SMC) ID SPITZER-SPACE-TELESCOPE; MULTIBAND IMAGING PHOTOMETER; INFRARED ARRAY CAMERA; MASS-LOSS RETURN; SPECTRAL IRRADIANCE CALIBRATION; YOUNG STELLAR OBJECTS; GIANT BRANCH STARS; 24 MU-M; ABSOLUTE CALIBRATION; EVOLVED STARS AB The Small Magellanic Cloud (SMC) provides a unique laboratory for the study of the lifecycle of dust given its low metallicity (similar to 1/5 solar) and relative proximity (similar to 60 kpc). This motivated the SAGE-SMC (Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low Metallicity Small Magellanic Cloud) Spitzer Legacy program with the specific goals of studying the amount and type of dust in the present interstellar medium, the sources of dust in the winds of evolved stars, and how much dust is consumed in star formation. This program mapped the full SMC (30 deg(2)) including the body, wing, and tail in seven bands from 3.6 to 160 mu m using IRAC and MIPS on the Spitzer Space Telescope. The data were reduced and mosaicked, and the point sources were measured using customized routines specific for large surveys. We have made the resulting mosaics and point-source catalogs available to the community. The infrared colors of the SMC are compared to those of other nearby galaxies and the 8 mu m/24 mu m ratio is somewhat lower than the average and the 70 mu m/160 mu m ratio is somewhat higher than the average. The global infrared spectral energy distribution (SED) shows that the SMC has approximately 1/3 the aromatic emission/polycyclic aromatic hydrocarbon abundance of most nearby galaxies. Infrared color-magnitude diagrams are given illustrating the distribution of different asymptotic giant branch stars and the locations of young stellar objects. Finally, the average SED of H II/star formation regions is compared to the equivalent Large Magellanic Cloud average H II/star formation region SED. These preliminary results will be expanded in detail in subsequent papers. C1 [Gordon, K. D.; Meixner, M.; Boyer, M. L.; Lawton, B.; Shiao, B.; Smith, L. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Meade, M. R.; Whitney, B.; Babler, B.; Bracker, S.; Churchwell, E.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Whitney, B.] Space Sci Inst, Boulder, CO 80301 USA. [Engelbracht, C.; Block, M.; Misselt, K.; Marble, A. R.; Zaritsky, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bot, C.] Univ Strasbourg, Ctr Donnees Astron Strasbourg CDS, UMR 7550, F-67000 Strasbourg, France. [Sewilo, M.; Carlson, L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bernard, J. -P.] Univ Toulouse, UPS, CESR, F-31028 Toulouse 4, France. [Blum, R.; Harris, J.; Olsen, K.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Bolatto, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bonanos, A.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. [Hora, J. L.; Robitaille, T.] Harvard Smithsonian, CfA, Cambridge, MA 02138 USA. [Indebetouw, R.; Reach, W.; Paladini, R.; Paradis, D.; Van Dyk, S.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Indebetouw, R.; Leroy, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Tielens, X.; Israel, F. P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Clayton, G. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Chen, C. -H. R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Cohen, M.] Monterey Inst Res Astron, Marina, CA 93933 USA. [Fukui, Y.; Kawamura, A.; Mizuno, A.; Mizuno, N.; Muller, E.; Onishi, T.; Sato, S.; Shibai, H.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Gorjian, V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hony, S.; Madden, S.; Rubin, D.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Kawamura, A.; Muller, E.] Natl Astron Observ Japan, ALMA J Project Off, Tokyo 1818588, Japan. [Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Kemper, F.; van Loon, J. Th] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Li, A.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Marble, A. R.] Natl Solar Observ, Tucson, AZ 85719 USA. [McDonald, I.; Oliveira, J. M.] Univ Keele, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Points, S.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, La Serena, Chile. [Sandstrom, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Simon, J. D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Smith, L. J.] European Space Agcy, Res & Sci Support Dept, Baltimore, MD 21218 USA. [Srinivasan, S.] Inst Astrophys, F-75014 Paris, France. [Vijh, U.] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA. RP Gordon, KD (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RI Kemper, Francisca/D-8688-2011; Bonanos, Alceste/K-5392-2013; OI Kemper, Francisca/0000-0003-2743-8240; Bonanos, Alceste/0000-0003-2851-1905; Bot, Caroline/0000-0001-6118-2985; Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650; Reach, William/0000-0001-8362-4094; Robitaille, Thomas/0000-0002-8642-1329; Van Dyk, Schuyler/0000-0001-9038-9950 FU NASA [1340964, 1407] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through Contract Number 1340964 issued by JPL/Caltech. NR 94 TC 85 Z9 85 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2011 VL 142 IS 4 AR 102 DI 10.1088/0004-6256/142/4/102 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822JY UT WOS:000295042500006 ER PT J AU Petit, JM Kavelaars, JJ Gladman, BJ Jones, RL Parker, JW Van Laerhoven, C Nicholson, P Mars, G Rousselot, P Mousis, O Marsden, B Bieryla, A Taylor, M Ashby, MLN Benavidez, P Bagatin, AC Bernabeu, G AF Petit, J-M Kavelaars, J. J. Gladman, B. J. Jones, R. L. Parker, J. Wm Van Laerhoven, C. Nicholson, P. Mars, G. Rousselot, P. Mousis, O. Marsden, B. Bieryla, A. Taylor, M. Ashby, M. L. N. Benavidez, P. Campo Bagatin, A. Bernabeu, G. TI THE CANADA-FRANCE ECLIPTIC PLANE SURVEY-FULL DATA RELEASE: THE ORBITAL STRUCTURE OF THE KUIPER BELT SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper Belt: general; surveys ID TRANS-NEPTUNIAN OBJECTS; TURBULENT PROTOPLANETARY DISKS; EXTENDED SCATTERED DISK; SOLAR-SYSTEM; COLLISIONAL FAMILY; SIZE DISTRIBUTION; DYNAMICAL CLASSIFICATION; LUMINOSITY FUNCTION; GLOBAL EVOLUTION; HAWAII-TELESCOPE AB We report the orbital distribution of the trans-Neptunian objects (TNOs) discovered during the Canada-France Ecliptic Plane Survey (CFEPS), whose discovery phase ran from early 2003 until early 2007. The follow-up observations started just after the first discoveries and extended until late 2009. We obtained characterized observations of 321 deg(2) of sky to depths in the range g similar to 23.5-24.4 AB mag. We provide a database of 169 TNOs with high-precision dynamical classification and known discovery efficiency. Using this database, we find that the classical belt is a complex region with sub-structures that go beyond the usual splitting of inner (interior to 3:2 mean-motion resonance [MMR]), main (between 3: 2 and 2: 1 MMR), and outer (exterior to 2:1 MMR). The main classical belt (a = 40-47 AU) needs to be modeled with at least three components: the "hot" component with a wide inclination distribution and two "cold" components (stirred and kernel) with much narrower inclination distributions. The hot component must have a significantly shallower absolute magnitude (H-g) distribution than the other two components. With 95% confidence, there are 8000(-1600)(+1800) objects in the main belt with H-g <= 8.0, of which 50% are from the hot component, 40% from the stirred component, and 10% from the kernel; the hot component's fraction drops rapidly with increasing Hg. Because of this, the apparent population fractions depend on the depth and ecliptic latitude of a trans-Neptunian survey. The stirred and kernel components are limited to only a portion of the main belt, while we find that the hot component is consistent with a smooth extension throughout the inner, main, and outer regions of the classical belt; in fact, the inner and outer belts are consistent with containing only hot-component objects. The H-g <= 8.0 TNO population estimates are 400 for the inner belt and 10,000 for the outer belt to within a factor of two (95% confidence). We show how the CFEPS Survey Simulator can be used to compare a cosmogonic model for the orbital element distribution to the real Kuiper Belt. C1 [Petit, J-M; Rousselot, P.; Mousis, O.] Observ Besancon, CNRS UMR 6213, Inst UTINAM, F-25010 Besancon, France. [Petit, J-M; Gladman, B. J.; Jones, R. L.; Van Laerhoven, C.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Kavelaars, J. J.; Jones, R. L.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Parker, J. Wm; Bieryla, A.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. [Van Laerhoven, C.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Nicholson, P.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Mars, G.] Observ Cote Azur, F-06304 Nice 4, France. [Marsden, B.; Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Taylor, M.; Bernabeu, G.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada. [Benavidez, P.; Campo Bagatin, A.] Univ Alicante, EPSA, Dept Fis Ingn Sistemas & Teoria Senal, E-03080 Alicante, Spain. RP Petit, JM (reprint author), Observ Besancon, CNRS UMR 6213, Inst UTINAM, BP 1615, F-25010 Besancon, France. RI Bernabeu, Guillermo/L-4703-2014; Campo Bagatin, Adriano/L-2809-2014; OI Bernabeu, Guillermo/0000-0001-5695-0900; Campo Bagatin, Adriano/0000-0001-9840-2216; Taylor, Matthew/0000-0003-3009-4928 FU Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Innovation; National Research Council of Canada; NASA [NNG04GI29G] FX This research was supported by funding from the Natural Sciences and Engineering Research Council of Canada, the Canadian Foundation for Innovation, the National Research Council of Canada, and NASA Planetary Astronomy Program NNG04GI29G. This project could not have been a success without the dedicated staff of the Canada-France-Hawaii telescope as well as the assistance of the skilled telescope operators at KPNO and Mount Palomar. NR 79 TC 59 Z9 59 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2011 VL 142 IS 4 AR 131 DI 10.1088/0004-6256/142/4/131 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 822JY UT WOS:000295042500035 ER PT J AU Kokkin, DL Brunken, S Young, KH Patel, NA Gottlieb, CA Thaddeus, P McCarthy, MC AF Kokkin, D. L. Bruenken, S. Young, K. H. Patel, N. A. Gottlieb, C. A. Thaddeus, P. McCarthy, M. C. TI THE ROTATIONAL SPECTRA OF (SiC2)-Si-29 AND (SiC2)-Si-30 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM: molecules; line: identification; molecular data; radio lines: ISM; submillimeter: ISM ID SILICON DICARBIDE SIC2; LINE SURVEY; MOLECULAR-SPECTROSCOPY; LABORATORY MEASUREMENT; COLOGNE DATABASE; EXCITED-STATE; IRC+10216; ENVELOPE; RESOLUTION; CDMS AB The rotational spectra of (SiC2)-Si-29 and (SiC2)-Si-30, two silicon isotopic species of the abundant astronomical ring (SiC2)-Si-28, have been characterized in the millimeter band between 140 and 360 GHz in a low pressure discharge through SiH4, C2H2, and Ar. Precise rotational and centrifugal distortion constants have been derived for both species by fitting a standard asymmetric top Hamiltonian to 38 a-type transitions of (SiC2)-Si-29 and 35 of (SiC2)-Si-30; the data sets include transitions up to K-a = 8 and at least J = 16. With these new measurements in hand, the most intense radio transitions of both species either have been measured or can now be predicted to better than 1 km s(-1) in equivalent radial velocity up to 500 GHz, more than adequate accuracy for spectral line identifications in circumstellar shells of evolved carbon stars such as IRC+10216 where SiC2 is conspicuous. More than 10 new lines of (SiC2)-Si-29 and (SiC2)-Si-30 have been identified between 295 and 354 GHz in the interferometric spectral line survey of IRC+10216 with the Submillimeter Array. C1 [Kokkin, D. L.] Univ Sydney, Sch Chem, Sydney, NSW 2006, Australia. [Kokkin, D. L.; Bruenken, S.; Young, K. H.; Patel, N. A.; Gottlieb, C. A.; Thaddeus, P.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bruenken, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Kokkin, DL (reprint author), Univ Sydney, Sch Chem, Sydney, NSW 2006, Australia. EM dkokkin@cfa.harvard.edu RI Brunken, Sandra/B-1880-2010; OI Brunken, Sandra/0000-0001-7175-4828; McCarthy, Michael/0000-0001-9142-0008 FU NASA [NNX08AE05G]; University of Sydney; Harvard College Observatory FX This work is supported by NASA grant NNX08AE05G. D.L.K. thanks the University of Sydney for a University Postgraduate Award. S.B. is grateful to the Harvard College Observatory for a Menzel fellowship. NR 22 TC 8 Z9 8 U1 0 U2 12 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 OCT PY 2011 VL 196 IS 2 AR 17 DI 10.1088/0067-0049/196/2/17 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 832XR UT WOS:000295844500003 ER PT J AU Kettenring, KM McCormick, MK Baron, HM Whigham, DF AF Kettenring, Karin M. McCormick, Melissa K. Baron, Heather M. Whigham, Dennis F. TI Mechanisms of Phragmites australis invasion: feedbacks among genetic diversity, nutrients, and sexual reproduction SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE allee effect; anthropogenic development; common reed; cross-pollination; nitrogen; phosphorus; seed viability; superior genotypes ID COMMON REED; CHESAPEAKE BAY; SALT MARSHES; SPARTINA-ALTERNIFLORA; BIOLOGICAL INVASIONS; CRYPTIC INVASION; NORTH-AMERICA; PLANT; NITROGEN; SPREAD AB 1. A fundamental challenge to invasion ecology is to determine what factors cause an exotic species to spread rapidly long after the initial introduction. The increase of a resource (e. g. nitrogen) could trigger an expansion, but in other instances, species have overcome biological limitations (e. g. an Allee effect) like accumulating sufficient genetic diversity for successful reproduction. Understanding the ecological mechanisms governing plant invasions, such as nutrient enrichment or Allee effects, can be used to improve invasive plant management. 2. We used the invasive, introduced grass Phragmites australis as a model to evaluate the role of nutrient enrichment and Allee effects in invasion. Based on recent studies that demonstrated the importance of sexual reproduction in this plant's spread, we chose to focus our efforts on reproductive output. We examined the effects of patch-level genetic diversity on viable seed production across watersheds of the Chesapeake Bay, USA, with differing levels of anthropogenic development (a proxy for nutrient enrichment). In an outdoor mesocosm experiment, we treated Phragmites plants originating from forested and developed watersheds with elevated vs. ambient nutrients and cross vs. self-pollination and determined the effects on viable seed, floret and inflorescence production. 3. The proportion of viable seeds produced at field sites varied widely and was not directly related to watershed development. Instead, seed viability was positively related to patch-level genetic diversity, and patches in more developed watersheds had higher genetic diversity. Also, plants in larger patches produced a higher proportion of viable seeds. In the mesocosm experiment, seed viability was substantially higher for out-crossed plants. Elevated nutrients resulted in greater floret and inflorescence production, particularly for plants originating from developed vs. forested watersheds. 4. These findings have important management implications: small populations should be controlled before they accumulate sufficient genetic variation for prolific viable seed production, and landscape-scale nutrient management could further limit reproductive output. 5. Synthesis and applications. Our research shows how nutrient enrichment and a weak Allee effect can interact across multiple scales to impact invasion success and how understanding the ecological mechanisms governing plant invasions can be used to better inform invasive plant management. C1 [Kettenring, Karin M.] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. [Kettenring, Karin M.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. [Kettenring, Karin M.; McCormick, Melissa K.; Baron, Heather M.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Baron, Heather M.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. RP Kettenring, KM (reprint author), Utah State Univ, Ctr Ecol, 5210 Old Main Hill, Logan, UT 84322 USA. EM karin.kettenring@usu.edu OI Whigham, Dennis/0000-0003-1488-820X FU EPA STAR [692105]; Smithsonian Work-learn internship; Smithsonian Postdoctoral Fellowship FX We thank J. O'Neill, C. Laine, J. Baker for lab assistance; L. Meyerson for pollination advice; S. Durham for statistical advice; and J. Beder, R. Downard, S. Galatowitsch, E. Hazelton, D. Menuz, K. Mercer for manuscript feedback. This research was funded by EPA STAR grant # 692105 to D. Wardrop; a Smithsonian Work-learn internship to H. M. B.; and a Smithsonian Postdoctoral Fellowship to K.M.K. NR 59 TC 44 Z9 47 U1 8 U2 72 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0021-8901 J9 J APPL ECOL JI J. Appl. Ecol. PD OCT PY 2011 VL 48 IS 5 BP 1305 EP 1313 DI 10.1111/j.1365-2664.2011.02024.x PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 823BA UT WOS:000295095100027 ER PT J AU Kibii, JM Clarke, RJ Tocheri, MW AF Kibii, Job M. Clarke, Ron J. Tocheri, Matthew W. TI A hominin scaphoid from Sterkfontein, Member 4: Morphological description and first comparative phenetic 3D analyses SO JOURNAL OF HUMAN EVOLUTION LA English DT Editorial Material DE Australopithecus; Wrist bone; Thumb; Carpal arch ID SOUTH-AFRICA; OLDUVAI GORGE; AUSTRALOPITHECUS-ANAMENSIS; FOOT BONES; HAND; EVOLUTION; PLIOCENE; SHAPE; SIZE; MORPHOMETRICS C1 [Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20013 USA. [Kibii, Job M.; Clarke, Ron J.] Univ Witwatersrand, Sch Anat Sci, Johannesburg, South Africa. [Kibii, Job M.; Clarke, Ron J.] Univ Witwatersrand, Inst Human Evolut, ZA-2050 Johannesburg, South Africa. RP Tocheri, MW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM tocherim@si.edu OI Tocheri, Matthew/0000-0001-7600-8998 NR 48 TC 2 Z9 2 U1 1 U2 8 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD OCT PY 2011 VL 61 IS 4 BP 510 EP 517 DI 10.1016/j.jhevol.2011.06.001 PG 8 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 828LR UT WOS:000295503000013 PM 21788062 ER PT J AU Hanner, R Floyd, R Bernard, A Collette, BB Shivji, M AF Hanner, Robert Floyd, Robin Bernard, Andrea Collette, Bruce B. Shivji, Mahmood TI DNA barcoding of billfishes SO MITOCHONDRIAL DNA LA English DT Article DE COI; rhodopsin; mitochondrial DNA; species delimitation ID MITOCHONDRIAL-DNA; IDENTIFICATION; MARLIN; SPEARFISH; SEQUENCES; NUCLEAR; FISHES; GENE; LIFE; PCR AB DNA barcoding is a method promising fast and accurate identification of animal species based on the sequencing of the mitochondrial c oxidase subunit (COI) gene. In this study, we explore the prospects for DNA barcoding in one particular fish group, the billfishes (suborder Xiphioidei-swordfish, marlins, spearfishes, and sailfish). We sequenced the mitochondrial COI gene from 296 individuals from the 10 currently recognized species of billfishes, and combined these data with a further 57 sequences from previously published projects. We also sequenced the rhodopsin gene from a subset of 72 individuals to allow comparison of mitochondrial results against a nuclear marker. Five of the 10 species are readily distinguishable by COI barcodes. Of the rest, the striped marlin (Kajikia audax) and white marlin (K. albida) show highly similar sequences and are not unambiguously distinguishable by barcodes alone, likewise are the three spearfishes Tetrapturus angustirostris, T. belone, and T. pfluegeri. We discuss the taxonomic status of these species groups in light of our and other data, molecular and morphological. C1 [Hanner, Robert; Floyd, Robin] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Hanner, Robert; Floyd, Robin] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. [Bernard, Andrea; Shivji, Mahmood] Nova SE Univ, Oceanog Ctr, Guy Harvey Res Inst, Dania, FL 33004 USA. [Collette, Bruce B.] Natl Museum Nat Hist, Smithsonian Inst, Natl Marine Fisheries Serv Systemat Lab, MRC 0153, Washington, DC 20560 USA. RP Hanner, R (reprint author), Univ Guelph, Biodivers Inst Ontario, 50 Stone Rd E, Guelph, ON N1G 2W1, Canada. EM rhanner@uoguelph.ca FU Canadian Barcode of Life Network from Genome Canada (through the Ontario Genomics Institute); NSERC FX This work was supported through funding to the Canadian Barcode of Life Network from Genome Canada (through the Ontario Genomics Institute), NSERC, and other sponsors listed at http://www.BOLNET.ca; and additionally by operational funds to the Guy Harvey Research Institute, AFTCO, Inc., and an NSERC postgraduate fellowship (AB). We thank L. Beerkircher, J. Graves, J. McDowell, E. Prince, J. Serafy, and D. Snodgrass for providing tissue samples and Eugene Wong for assistance in the laboratory. We are grateful to Johanne Fischer of the FAO for granting permission to use images from their catalog (Nakamura 1985) for the first figure in our study. The authors report no conflicts of interest. The authors alone are responsible for the content and writing of the paper. NR 46 TC 12 Z9 13 U1 1 U2 12 PU INFORMA HEALTHCARE PI LONDON PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND SN 1940-1736 EI 1940-1744 J9 MITOCHONDR DNA JI Mitochondrial DNA PD OCT PY 2011 VL 22 SU 1 BP 27 EP 36 DI 10.3109/19401736.2011.596833 PG 10 WC Genetics & Heredity SC Genetics & Heredity GA 831JJ UT WOS:000295726100006 PM 21980985 ER PT J AU Moran, JM AF Moran, James M. TI John Peter Huchra Obituary SO PHYSICS TODAY LA English DT Biographical-Item C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moran, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD OCT PY 2011 VL 64 IS 10 BP 66 EP 66 PG 1 WC Physics, Multidisciplinary SC Physics GA 833PS UT WOS:000295898000023 ER PT J AU Elvis, M McDowell, J Hoffman, JA Binzel, RP AF Elvis, Martin McDowell, Jonathan Hoffman, Jeffrey A. Binzel, Richard P. TI Ultra-low delta-v objects and the human exploration of asteroids SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Human exploration; Asteroids; Surveys ID TELESCOPE AB Missions to near-Earth objects (NEOs) are key destinations in NASA's new 'Flexible Path' approach. NEOs are also of interest for science, for the hazards they pose, and for their resources. We emphasize the importance of ultra-low delta-v from LEO to NEO rendezvous as a target selection criterion, as this choice can greatly increase the payload to the NEO. Few such ultra-low delta-v NEOs are currently known; only 65 of the 6699 known NEOs (March 2010) have delta-v < 4.5 km/s, 2/3 of typical LEO-NEO delta-v. Even these are small and hard to recover. Other criteria - short transit times, long launch windows, a robust abort capability, and a safe environment for proximity operations - will further limit the list of accessible objects. Potentially there is at least an order of magnitude more ultra-low delta-v NEOs, but finding them all on a short enough timescale (before 2025) requires a dedicated survey in the optical or mid-IR, optimally from a Venus-like orbit because of the short synodic period for NEOs in that orbit, plus long arc determination of their orbits. Published by Elsevier Ltd. C1 [Elvis, Martin; McDowell, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hoffman, Jeffrey A.; Binzel, Richard P.] MIT, Cambridge, MA 02139 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM elvis@cfa.harvard.edu FU NASA [NAS8-39073] FX This paper is based on a talk given at the April 2010 meeting of the Dynamical Astronomy Division of the American Astronomical Society. We thank the late Brian Marsden, Alan Harris, Tim Spahr, Slatko Ivezic and B.C. Crandall for valuable assistance and advice. This work was supported in part by NASA contract NAS8-39073. NR 28 TC 8 Z9 8 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD OCT PY 2011 VL 59 IS 13 BP 1408 EP 1412 DI 10.1016/j.pss.2011.05.006 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 833OI UT WOS:000295894400008 ER PT J AU Liu, Q Peterson, PM Ge, XJ AF Liu, Qing Peterson, Paul M. Ge, Xue-jun TI Phylogenetic signals in the realized climate niches of Chinese grasses (Poaceae) SO PLANT ECOLOGY LA English DT Article DE BEP and PACCMAD clades; C4 node; Niche evolution; Phylogeny; Poaceae; Species distribution model ID C-4 GRASSES; GEOGRAPHICAL-DISTRIBUTION; ECOLOGICAL DISTRIBUTION; HAWAIIAN-ISLANDS; FUNCTIONAL TYPES; TRAIT EVOLUTION; NORTH-AMERICA; C4 GRASSES; PHOTOSYNTHESIS; PATTERNS AB Explaining relationships between species richness and biogeographical patterns over a broad geographic scale is a central issue of biogeography and macroecology. We document the realized climate niches for grasses in China's nature reserves and discuss its formation mechanism using grass richness data combined with climatic, physiological, and phylogenetic data. Our results suggest that climate niche structure of grasses is phylogenetically conservative for BEP (Bambusoideae, Ehrhartoideae, and Pooideae) and PACMAD (Panicoideae, Arundinoideae, Chloridoideae, Micrairoideae, Aristidoideae, and Danthonioideae) clades along temperature gradients and for Chloridoideae and Panicoideae along precipitation gradients. At the national scale, the divergence patterns of climate niches between two major clades are more distinguishable than between C-3 and C-4 grasses. High rates of climate niche evolution are found in C-4 clades in the subtropical forest region. There appears to be a strong association between elevation gradients and grass diversity: the specific environmental conditions (e.g. energy) and the rapid shifts of climate conditions drive high grass diversification. Evolutionary conservatism of climate niches may be influenced by the specific adaptive ability to changing environmental conditions within NAD-ME/NADP-ME clades. Our results indicate that adaptations to major climate changes may be accomplished by C-4 grass nodes of high climate niche evolutionary rates in China's nature reserves. C1 [Liu, Qing; Ge, Xue-jun] Chinese Acad Sci, Key Lab Plant Resources Conservat & Sustainable U, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. [Peterson, Paul M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Liu, Q (reprint author), Chinese Acad Sci, Key Lab Plant Resources Conservat & Sustainable U, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. EM liuqing@scib.ac.cn; xjge@scib.ac.cn FU National Natural Science Foundation of China [30700043]; Key Laboratory of Plant Resources Conservation and Sustainable Utilization, Chinese Academy of Sciences [200922]; Chinese Government [2008491004]; Chinese Academy of Sciences [KSCX2-EW-J-28] FX We thank China Meteorological Data Sharing Service System for accessing the digital climatic data. This study was supported by the National Natural Science Foundation of China (No. 30700043), the Key Laboratory of Plant Resources Conservation and Sustainable Utilization, Chinese Academy of Sciences (No. 200922), the Chinese Government Scholarship to QL (No. 2008491004), and the Knowledge Innovation Program of the Chinese Academy of Sciences (KSCX2-EW-J-28). We also thank two anonymous reviewers for their constructive comments that improved the manuscript. NR 73 TC 2 Z9 3 U1 4 U2 24 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD OCT PY 2011 VL 212 IS 10 BP 1733 EP 1746 DI 10.1007/s11258-011-9946-7 PG 14 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 834SG UT WOS:000295983700014 ER PT J AU Raviele, ME AF Raviele, Maria E. TI Experimental assessment of maize phytolith and starch taphonomy in carbonized cooking residues SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Zea mays; Maize; Phytoliths; Starch; Residues; Taphonomy; Eastern North America ID GRAIN ANALYSIS; NORTH-AMERICA; ZEA-MAYS; NEW-YORK; FREQUENCIES; ARTIFACTS; EVOLUTION; ISOTOPE; LOCUS AB Many taphonomic studies of plant microfossils, specifically phytoliths and starch, are concerned with post-depositional movement, contamination, and morphological changes due to environmental fluctuations or plant processing. Additionally, the identification of phytoliths and starches archaeologically are based on their presence or absence. This paper examines whether it is possible to identify maize (Zea mays ssp. mays) phytolith and starch abundance associated with different processing behaviors as replicated through experimentally produced cooking residues. If successful, identification of likely associated processing and taphonomy of these microfossils will allow for a more refined interpretation of plant use as it relates to timing and plant form and processing. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Raviele, Maria E.] Smithsonian Inst, Off Policy & Anal, Washington, DC 20013 USA. [Raviele, Maria E.] Michigan State Univ, Dept Anthropol, E Lansing, MI 48824 USA. RP Raviele, ME (reprint author), Smithsonian Inst, Off Policy & Anal, MRC 502,POB 37012, Washington, DC 20013 USA. EM ravielem@gmail.com FU National Science Foundation [BCS-0843130]; Wenner-Gren Dissertation Fieldwork Grant [7811] FX Funding for this work was provided through a National Science Foundation Doctoral Dissertation Improvement Grant (Award BCS-0843130) and a Wenner-Gren Dissertation Fieldwork Grant (Grant #7811). I would like to thank Jerry Fankhauser for providing the milk stage dent maize used in these experiments, Drs. William Lovis and John Hart for their extensive comments on earlier drafts and the comments of two anonymous reviewers. NR 41 TC 12 Z9 13 U1 1 U2 14 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD OCT PY 2011 VL 38 IS 10 BP 2708 EP 2713 DI 10.1016/j.jas.2011.06.008 PG 6 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 822NP UT WOS:000295055500022 ER PT J AU Meier, DC Davis, JM Vicenzi, EP AF Meier, Douglas C. Davis, Jeffrey M. Vicenzi, Edward P. TI An Examination of Kernite (Na(2)B(4)O(6)(OH)(2)center dot 3H(2)O) Using X-Ray and Electron Spectroscopies: Quantitative Microanalysis of a Hydrated Low-Z Mineral SO MICROSCOPY AND MICROANALYSIS LA English DT Article DE borate; kernite; hydrate; light elements; electron-probe microanalysis (EPMA); wavelength-dispersive X-ray spectroscopy (WDS); X-ray diffraction (XRD); X-ray photoelectron spectroscopy (XPS); variable-pressure scanning electron microscopy (VP-SEM); auger electron spectroscopy (AES) ID NA2B4O6(OH)2.3H2O; BORON; GLASS AB Mineral borates, the primary industrial source of boron, are found in a large variety of compositions. One such source, kernite (Na(2)B(4)O(6)(OH)(2)center dot 3H2O), offers an array of challenges for traditional electron-probe microanalysis (EPMA)-it is hygroscopic, an electrical insulator, composed entirely of light elements, and sensitive to both low pressures and the electron beam. However, the approximate stoichiometric composition of kernite can be analyzed with careful preparation, proper selection of reference materials, and attention to the details of quantification procedures, including correction for the time dependency of the sodium X-ray signal. Moreover, a reasonable estimation of the mineral's water content can also be made by comparing the measured oxygen to the calculated stoichiometric oxygen content. X-ray diffraction, variable-pressure electron imaging, and visual inspection elucidate the structural consequences of high vacuum treatment of kernite, while Auger electron spectroscopy and X-ray photoelectron spectroscopy confirm electron beam-driven migration of sodium and oxygen out of the near-surface region (sampling depth approximate to 2 nm). These surface effects are insufficiently large to significantly affect the EPMA results (sampling depth approximate to 400 nm at 5 keV). C1 [Meier, Douglas C.; Davis, Jeffrey M.; Vicenzi, Edward P.] NIST, Surface & Microanal Sci Div, Gaithersburg, MD 20899 USA. [Vicenzi, Edward P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Meier, DC (reprint author), NIST, Surface & Microanal Sci Div, 100 Bur Dr MS8371, Gaithersburg, MD 20899 USA. EM dmeier@nist.gov NR 30 TC 1 Z9 1 U1 1 U2 8 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD OCT PY 2011 VL 17 IS 5 BP 718 EP 727 DI 10.1017/S1431927611000602 PG 10 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA 829UF UT WOS:000295609100011 PM 21892991 ER PT J AU Thapa, R Phillips, JD Rocco, E Reasenberg, RD AF Thapa, Rajesh Phillips, James D. Rocco, Emanuele Reasenberg, Robert D. TI Subpicometer length measurement using semiconductor laser tracking frequency gauge SO OPTICS LETTERS LA English DT Article ID INTERFEROMETRY; ACCURACY AB We have demonstrated heretofore unattained distance precision of 0.14 pm (2 pm) incremental and 14 nm (2.9 mu m) absolute in a resonant (nonresonant) interferometer at an averaging time of 1 s, using inexpensive telecommunications diode lasers. We have controlled the main source of error, that due to spurious reflection and the resulting amplitude modulation. In the resonant interferometer, absolute distance precision is well under lambda/6. Therefore, after an interruption, an absolute distance measurement can be used to return to the same interferometer order. (C) 2011 Optical Society of America C1 [Thapa, Rajesh; Phillips, James D.; Rocco, Emanuele; Reasenberg, Robert D.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Phillips, JD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM jphillips@cfa.harvard.edu FU National Aeronautics and Space Administration (NASA) [NNX07AI11G, NNX08AO04G] FX This work was supported by the National Aeronautics and Space Administration (NASA) through grants NNX07AI11G and NNX08AO04G. NR 11 TC 10 Z9 10 U1 0 U2 2 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD OCT 1 PY 2011 VL 36 IS 19 BP 3759 EP 3761 PG 3 WC Optics SC Optics GA 827GD UT WOS:000295415600015 PM 21964088 ER PT J AU Cardoso, P Borges, PAV Triantis, KA Ferrandez, MA Martin, JL AF Cardoso, Pedro Borges, Paulo A. V. Triantis, Kostas A. Ferrandez, Miguel A. Martin, Jose L. TI Adapting the IUCN Red List criteria for invertebrates SO BIOLOGICAL CONSERVATION LA English DT Article DE Arthropoda; Conservation priority; Extinction; Risk assessment; Threatened species; World Conservation Union ID POPULATION VIABILITY ANALYSIS; SPECIES DISTRIBUTIONS; CONSERVATION STATUS; EXTINCTION DEBT; TAXONOMIC BIAS; CLIMATE-CHANGE; BIODIVERSITY; AZORES; EUROPE; UNCERTAINTY AB The IUCN Red List is the most useful list of species that are at risk for extinction worldwide, as it relies on a number of objective criteria. Nevertheless, there is a taxonomic bias that excludes species with small body sizes, narrow distribution ranges and low dispersal abilities, which constitute the vast Majority of the planet's biota, particularly local endemics. By evaluating each IUCN criterion separately, we (i) identify the shortcomings for invertebrate applications, (ii) explain how risk categories may be wrongly applied due to inapplicable and/or misleading thresholds, (iii) suggest alternative ways of applying the existing criteria in a more realistic way and (iv) suggest possible new criteria that were not considered in the current evaluation framework but that could allow a more comprehensive and effective assessment of invertebrates. By adapting the criteria to rely more explicitly on the Area of Occupancy and the Extent of Occurrence, their respective trends and by using ecological modelling methods, the criteria's applicability would be increased. The change in some thresholds or, eventually, the creation of sub-categories would further increase their adequacy. Additionally, co-extinction could be introduced as an explicit part of the classification process. As a case study, we evaluated 48 species of Azorean arthropods and Iberian spiders according to the current criteria. More than one-quarter (27%) of all evaluated species were classified as Critically Endangered, 19% as Endangered, 6% as Vulnerable and 8% as Least Concern. The remaining 40% did not have enough data to reach a classification. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Cardoso, Pedro; Borges, Paulo A. V.; Triantis, Kostas A.] Univ Azores, Azorean Biodivers Grp CITA A, Angra Do Heroismo, Portugal. [Triantis, Kostas A.] Univ Athens, Dept Ecol & Taxon, Fac Biol, Athens 11528, Greece. [Ferrandez, Miguel A.] Soc El Estudio & Conservac Aranas, Madrid, Spain. [Martin, Jose L.] Canary Agcy Sustainable Dev & Climate Change, Santa Cruz De Tenerife, Canary Islands, Spain. RP Cardoso, P (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, Rua Capitao Joao dAvila, P-9700042 Angra Do Heroismo, Portugal. EM pcardoso@ennor.org RI Borges, Paulo/B-2780-2008; Triantis, Kostas/A-1018-2009; Cardoso, Pedro/A-8820-2008 OI Borges, Paulo/0000-0002-8448-7623; Cardoso, Pedro/0000-0001-8119-9960 FU Portuguese Foundation for Science and Technology [SFRH/BPD/40688/2007]; Direccao Regional dos Recursos Florestais [17.01-080203] FX PC is supported by the Portuguese Foundation for Science and Technology (SFRH/BPD/40688/2007). The data obtained in the Azores was possible due to the accumulated effort of many colleagues during BALA Project (funded by the Direccao Regional dos Recursos Florestais - Proj. 17.01-080203) and more recently the projects "Consequences of land-use change on Azorean fauna and flora - the 2010 Target" (Ref: Direccao Regional da Ciencia e Tecnologia M.2.1.2/I/003/2008) and FCT-PTDC/BIA-BEC/100182/2008 - "Predicting extinctions on islands: a multi-scale assessment". NR 69 TC 51 Z9 55 U1 4 U2 41 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD OCT PY 2011 VL 144 IS 10 BP 2432 EP 2440 DI 10.1016/j.biocon.2011.06.020 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 823HE UT WOS:000295112300006 ER PT J AU Mason, VC Li, G Helgen, KM Murphy, WJ AF Mason, Victor C. Li, Gang Helgen, Kristofer M. Murphy, William J. TI Efficient cross-species capture hybridization and next-generation sequencing of mitochondrial genomes from noninvasively sampled museum specimens SO GENOME RESEARCH LA English DT Article ID COLUGO AB The ability to uncover the phylogenetic history of recently extinct species and other species known only from archived museum material has rapidly improved due to the reduced cost and increased sequence capacity of next-generation sequencing technologies. One limitation of these approaches is the difficulty of isolating and sequencing large, orthologous DNA regions across multiple divergent species, which is exacerbated for museum specimens, where DNA quality varies greatly between samples and contamination levels are often high. Here we describe the use of cross-species DNA capture hybridization techniques and next-generation sequencing to selectively isolate and sequence partial to full-length mitochondrial DNA genomes from the degraded DNA of museum specimens, using probes generated from the DNA of a single extant species. We demonstrate our approach on specimens from an enigmatic gliding mammal, the Sunda colugo, which is widely distributed throughout Southeast Asia. We isolated DNA from 13 colugo specimens collected 47-170 years ago, and successfully captured and sequenced mitochondrial DNA from every specimen, frequently recovering fragments with 10%-13% sequence divergence from the capture probe sequence. Phylogenetic results reveal deep genetic divergence among colugos, both within and between the islands of Borneo and Java, as well as between the Malay Peninsula and different Sundaic islands. Our method is based on noninvasive sampling of minute amounts of soft tissue material from museum specimens, leaving the original specimen essentially undamaged. This approach represents a paradigm shift away from standard PCR-based approaches for accessing population genetic and phylogenomic information from poorly known and difficult-to-study species. C1 [Mason, Victor C.; Li, Gang; Murphy, William J.] Texas A&M Univ, Dept Vet Integrat Biosci, College Stn, TX 77843 USA. [Mason, Victor C.; Murphy, William J.] Texas A&M Univ, Interdisciplinary Program Genet, College Stn, TX 77843 USA. [Helgen, Kristofer M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Murphy, WJ (reprint author), Texas A&M Univ, Dept Vet Integrat Biosci, College Stn, TX 77843 USA. EM wmurphy@cvm.tamu.edu RI li, gang/E-5640-2014 FU National Science Foundation [EF0629849]; Texas AM University FX This work was supported in part by the National Science Foundation (EF0629849 to W.J.M.) and Texas A&M University. We thank Linda Gordon for assistance in sampling the colugo museum specimens. We thank the Genome Center at Washington University for providing sequence data and allowing use of the full mtDNA genome for GVA4. NR 24 TC 59 Z9 59 U1 0 U2 40 PU COLD SPRING HARBOR LAB PRESS, PUBLICATIONS DEPT PI COLD SPRING HARBOR PA 1 BUNGTOWN RD, COLD SPRING HARBOR, NY 11724 USA SN 1088-9051 J9 GENOME RES JI Genome Res. PD OCT PY 2011 VL 21 IS 10 BP 1695 EP 1704 DI 10.1101/gr.120196.111 PG 10 WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity GA 827DQ UT WOS:000295407800013 PM 21880778 ER PT J AU Forgan, DH Elvis, M AF Forgan, Duncan H. Elvis, Martin TI Extrasolar asteroid mining as forensic evidence for extraterrestrial intelligence SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article ID BETA-PICTORIS; SOLAR-SYSTEM; DEBRIS DISKS; DUST; EVOLUTION; UNIVERSE; PLANETS; SEARCH; SPACE; DISCS AB The development of civilizations such as ours into spacefaring, multi-planet entities requires significant raw materials to construct vehicles and habitats. Interplanetary debris, including asteroids and comets, may provide such a source of raw materials. In this article, we present the hypothesis that extraterrestrial intelligences (ETIs) engaged in asteroid mining may be detectable from Earth. Considering the detected disc of debris around Vega as a template, we explore the observational signatures of targeted asteroid mining (TAM), such as unexplained deficits in chemical species, changes in the size distribution of debris and other thermal signatures that may be detectable in the spectral energy distribution (SED) of a debris disc. We find that individual observational signatures of asteroid mining can be explained by natural phenomena, and as such they cannot provide conclusive detections of ETIs. But, it may be the case that several signatures appearing in the same system will prove harder to model without extraterrestrial involvement. Therefore, signatures of TAM are not detections of ETI in their own right, but as part of 'piggy-back' studies carried out in tandem with conventional debris disc research, they could provide a means of identifying unusual candidate systems for further study using other search for extra terrestrial intelligence (SETI) techniques. Received 26 January 2011, accepted 25 March 2011, first published online 9 May 2011 C1 [Forgan, Duncan H.] Univ Edinburgh, SUPA, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Forgan, DH (reprint author), Univ Edinburgh, SUPA, Inst Astron, Black Ford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM dhf@roe.ac.uk OI Forgan, Duncan/0000-0003-1175-4388 NR 40 TC 2 Z9 2 U1 3 U2 27 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD OCT PY 2011 VL 10 IS 4 BP 307 EP 313 DI 10.1017/S1473550411000127 PG 7 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 825ZT UT WOS:000295321600001 ER PT J AU Selvaraj, V Wildt, DE Pukazhenthi, BS AF Selvaraj, Vimal Wildt, David E. Pukazhenthi, Budhan S. TI Induced pluripotent stem cells for conserving endangered species? SO NATURE METHODS LA English DT Editorial Material ID TECHNOLOGIES; CONSERVATION; WILDLIFE C1 [Selvaraj, Vimal] Cornell Univ, Dept Anim Sci, Ithaca, NY 14853 USA. [Wildt, David E.; Pukazhenthi, Budhan S.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Selvaraj, V (reprint author), Cornell Univ, Dept Anim Sci, Ithaca, NY 14853 USA. EM pukazhenthib@si.edu NR 12 TC 5 Z9 5 U1 1 U2 11 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1548-7091 J9 NAT METHODS JI Nat. Methods PD OCT PY 2011 VL 8 IS 10 BP 805 EP 807 DI 10.1038/nmeth.1715 PG 3 WC Biochemical Research Methods SC Biochemistry & Molecular Biology GA 826MJ UT WOS:000295358000011 PM 21959133 ER PT J AU Budaeva, N Fauchald, K AF Budaeva, Nataliya Fauchald, Kristian TI Phylogeny of the Diopatra generic complex with a revision of Paradiopatra Ehlres, 1887 (Polychaeta: Onuphidae) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE cladistics; distribution; identification key; morphology; new genus; new species; paedomorphosis; taxonomy ID ATLANTIC SEA-URCHINS; CUPREA BOSC; EPIBENTHIC MEIOFAUNA; LARVAL DEVELOPMENT; TUBE-CAPS; ANNELIDA; GENUS; COAST; EUNICIDA; PACIFIC AB Analysis of 55 morphological characters yielded a phylogenetic reconstruction of the Diopatra complex, currently including three genera (Diopatra, Epidiopatra, and Paradiopatra). The results reject the monophyletic status of the complex and all three genera analysed. It is suggested that several parallel and independent events of paedomorphic evolution took place within the genera Diopatra and Paradiopatra, which led to the recognition of two artificial genera Epidiopatra and Notonuphis. The following taxonomic revisions are proposed: (1) Epidiopatra as a junior synonym of Diopatra; (2) Notonuphis as a junior synonym of Paradiopatra; (3) the Diopatra complex, consisting of two sister genera Diopatra and Paradiopatra, and two basal genera Paxtonia gen. nov. and Protodiopatra gen. nov., erected for two species previously included in Paradiopatra. Reconstruction of phylogenetic relationships within Paradiopatra yields a few reliable clades comprising well-defined groups of species, but supported by homoplastic synapomorphies representing highly adaptive characters. Twenty-six valid species of Paradiopatra, including a new species, Paradiopatra pyricirra sp. nov., are described or re-described and illustrated based on original descriptions and re-examination of type and non-type material. Identification keys to genera included in the Diopatra complex, and to all accepted Paradiopatra species, are presented. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 163, 319-436. doi: 10.1111/j.1096-3642.2011.00701.x C1 [Budaeva, Nataliya] Russian Acad Sci, PP Shirshov Oceanol Inst, Moscow 117997, Russia. [Fauchald, Kristian] NMNH, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Budaeva, N (reprint author), Russian Acad Sci, PP Shirshov Oceanol Inst, Nakhimovsky Prospekt 36, Moscow 117997, Russia. EM nataliya.budaeva@gmail.com FU Invertebrate Zoology Division of the National Museum of Natural History; Russian Foundation for Basic Research [07-04-08292, 06-04-48764]; CeDAMar, a project under the Census of Marine Life programme FX We would like to thank Andrey Gebruk and Alexander Mironov (SIO RAS) for their invaluable comments on the manuscript. We are also grateful to the following individuals and institutions for the loan and exchange of specimens: Tor Bakke (ZMO), Angelika Brandt (ZMH), Danny Eibye-Jacobsen (ZMUC), Igor Jirkov (DHB MSU), Ardis Johnston (MCZ), Hironori Komatsu (NSMT), Jon Anders Kongsrud (ZMUB), Nikita Kucheruk and Antonina Rogacheva (SIO RAS), Tarik Meziane (MNHN), Birger Neuhaus (ZMB), Vladislav Potin, Galina Bushinskaya, and Sergey Gagaev (ZIN), Emma Sherlock, Alexander Muir, and Gordon Paterson (BMNH), Linda Ward and Geoff Keel (USNM), Joana Zanol (Federal University of Rio de Janeiro, Brazil). This work was supported by the Smithsonian Institution fellowship programme (Invertebrate Zoology Division of the National Museum of Natural History), the Russian Foundation for Basic Research, grants 07-04-08292, 06-04-48764, and CeDAMar, a project under the Census of Marine Life programme. The authors thank Guinea Current Large Marine Ecosystem (GCLME) and the Norad funded EAF-Nansen program www.eaf-nansen.org for access to material from the Gulf of Guinea region. NR 130 TC 13 Z9 15 U1 2 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD OCT PY 2011 VL 163 IS 2 BP 319 EP 436 DI 10.1111/j.1096-3642.2011.00701.x PG 118 WC Zoology SC Zoology GA 825JB UT WOS:000295267400001 ER PT J AU Wang, LH Newchurch, MJ Biazar, A Liu, X Kuang, S Khan, M Chance, K AF Wang, Lihua Newchurch, M. J. Biazar, Arastoo Liu, Xiong Kuang, Shi Khan, Maudood Chance, Kelly TI Evaluating AURA/OMI ozone profiles using ozonesonde data and EPA surface measurements for August 2006 SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE OMI; IONS06; CMAQ; EPA; Ozone evaluation ID TROPOSPHERIC OZONE; MONITORING INSTRUMENT; RETRIEVALS AB We evaluate the Ozone Monitoring Instrument (OMI) ozone profile retrieval against ozonesonde data and the Environmental Protection Agency (EPA) surface measurements for August 2006. Comparison of individual OMI ozone profile with ozonesonde indicates that OMI ozone profile can explain the general vertical variation of ozone but is limited in observing the boundary layer ozone, due to weak sensitivity to boundary layer ozone and thick lowest layer (similar to 2.5 km). We made pair-wise comparison between OMI and ozonesondes on 24 OMI vertical layers, as well as the 39 sigma-P vertical layers of the Community Multi-scale Air Quality (CMAQ) modeling system, respectively. OMI shows reasonable agreement with ozonesonde in the lower- to mid-troposphere. In the upper troposphere, while the bias increases, the normalized bias does not show much variation and remains below 10%. Comparison with EPA's surface-monitoring data indicates that OMI observations at the lowest layer (surface to 2.5 km altitude) represent the mean values. While OMI underestimates elevated ozone concentrations, it explains the larger-scale spatial variation seen in the surface monitors. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Wang, Lihua; Newchurch, M. J.; Kuang, Shi] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. [Biazar, Arastoo] Univ Alabama, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Newchurch, MJ (reprint author), Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. EM mike@nsstc.uah.edu RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 NR 10 TC 8 Z9 9 U1 1 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD OCT PY 2011 VL 45 IS 31 BP 5523 EP 5530 DI 10.1016/j.atmosenv.2011.06.012 PG 8 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 822SQ UT WOS:000295070300014 ER PT J AU Gonzalez-Porter, GP Hailer, F Flores-Villela, O Garcia-Anleu, R Maldonado, JE AF Gonzalez-Porter, Gracia P. Hailer, Frank Flores-Villela, Oscar Garcia-Anleu, Rony Maldonado, Jesus E. TI Patterns of genetic diversity in the critically endangered Central American river turtle: human influence since the Mayan age? SO CONSERVATION GENETICS LA English DT Article DE Population genetic structure; Dermatemys mawii; Dermatemydidae; Mitochondrial DNA; Freshwater turtles ID CYTOCHROME-B GENE; DNA-SEQUENCE DATA; MOLECULAR SYSTEMATICS; POPULATION-STRUCTURE; CLADISTIC-ANALYSIS; POND TURTLE; BOX TURTLE; CONSERVATION; MITOCHONDRIAL; PHYLOGENY AB We conducted a phylogeographic analysis of the strictly aquatic and critically endangered Central American river turtle, Dermatemys mawii, as part of a conservation management program for the species. We sampled 238 individuals from 15 different localities throughout the species range. Using sequence fragments from the mtDNA Cyt b and ND4 genes, we identified 16 different haplotypes. Overall, our results reveal a signal of phylogeographic structure throughout the range, which appears to have been secondarily blurred by extensive gene flow. Notably, this also applies to genetic structuring across three major hydrological basins that pose biogeographic breaks in other aquatic taxa. Divergence times of mtDNA haplotypes in D. mawii suggest that the main lineages split in the Pliocene-Pleistocene (3.73-0.227 MA) and demographic tests indicate that the species has undergone drastic demographic size fluctuations since this time period. One ancient haplotype (1D) was found to exhibit sequence divergence of up to 2% from other haplogroups. Divergence of this magnitude is indicative of species level differentiation in other turtle genera. Haplotype 1D was found in only two localities, Sarstun and Salinas, but specimens with other haplotypes were also found in those localities. It is not known whether the individuals with the 1D haplotype interbreed with non-1D individuals. Our results suggest that human activity, such as harvesting and long distance transport of animals, may have influenced the current patterns of genetic diversity. For more than 2000 years, D. mawii has been consumed by people from Middle American cultures, and the archeological record contains strong evidence that the Mayans transported animals between villages and far away from their natural distribution range. Therefore, the large-scale pattern of haplotype sharing even across hydrological barriers, the observed low haplotype diversity in some populations and the contemporary absence of a pronounced phylogeographic pattern is likely due to a combination of population expansions, gene flow, extensive human-mediated-movements and recent bottlenecks resulting from over-harvesting. C1 [Gonzalez-Porter, Gracia P.; Hailer, Frank; Maldonado, Jesus E.] Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Gonzalez-Porter, Gracia P.; Flores-Villela, Oscar] Univ Nacl Autonoma Mexico, Museo Zool, Fac Ciencias, Mexico City 04510, DF, Mexico. [Garcia-Anleu, Rony] Wildlife Conservat Soc Guatemala Program, Flores, Guatemala. [Maldonado, Jesus E.] Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. RP Gonzalez-Porter, GP (reprint author), Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Natl Zool Pk,3001 Connecticut Ave NW, Washington, DC 20008 USA. EM syedg@si.edu RI Hailer, Frank/C-9114-2012; OI Hailer, Frank/0000-0002-2340-1726; Flores-Villela, Oscar/0000-0002-2849-6912 FU Consejo Nacional de Ciencia y Tecnologia (CONACYT) [210994]; Turtle Conservation Fund; Conservation International; Philadelphia Zoo; Philadelphia Zoo Docent council; Elizabeth A. Schreiber and Seabird Research, Inc.; SCBI's Center for Conservation and Evolutionary Genetics FX We thank the Posgrado en Ciencias Biologicas from Universidad Nacional Autonoma de Mexico UNAM; Drs. Ella Vazquez and Luis Medrano Gonzalez for their valuable insights into the experimental design and data analysis which greatly improved the quality of this manuscript. Funding was provided by Consejo Nacional de Ciencia y Tecnologia (CONACYT) fellowship No. 210994; the Turtle Conservation Fund grants in 2004, 2006 and 2009; Conservation International grants in 2007, and 2009; the Philadelphia Zoo Conservation Program Financial Support for 2005, 2006, 2007, 2008, an award from the Philadelphia Zoo Docent council in 2007 and Elizabeth A. Schreiber and Seabird Research, Inc. We are grateful to Robert C. Fleischer and Nancy Rotzel for funding and laboratory support at the SCBI's Center for Conservation and Evolutionary Genetics. To Secretaria de Medio Ambiente y Recursos Naturales (SEMARNAT) for the collection permits: SGPA/DGVS/11385/04; SGPA/DGVS/01789/06 to CITES for permits: MX 23732/05; MX 25219/05; MX29137/06; GT175507; MX42603/08; to the government of Belize for permit No. 3176/08; to the USFWS for permits #MA095827-0; MA119634-0/06; MA139456-0/07; MA194812-0/08; EN/FIS/15/04/08(10)Vol1. To SEMARNAT and Procuraduria Federal de Proteccion al Ambiente (PROFEPA) in Veracruz, and Tabasco. Thanks to all the people who have helped on different parts of this project; for ideas: Miriam Tsuchiya Jerep, for her important help on running the program BEAST, K. Buhlmann and Peter Paul Van Dijk; special thanks to Richard C. Vogt, who help me consolidate the idea of this project and sharing his expertise on the species. Dr. John Polisar, Carlina Pena, Rene Calderon, Humberto Bahena, Matha Vaca, Raul Rodriguez, Lisette Ramos, Greg Georges, Sam Rivera, Judith Rangel, Erasmo Cazares, Darwin Jimenez, Samuel Cabrera, Kenia Laparra, Manuel Acevedo, Claudia Zenteno, and Filiberto Ascencio Jimenez, the staff from WCS in Flores, Guatemala, all the volunteers, and staff at the turtle farm in Nacajuca, Tabasco, and Zoologico Yumka, Fishermen Cooperative of La Union in Quintana Roo for their help in the collection and measuring of the animals. Thanks also to Basilio Sanchez Luna, Gregorio de la Cruz Lopez, and Sharon Matola for allowing us to work with the animals at their facilities, and to Dr. Jonathan Campbell and Carl Franklin from the Amphibian and Reptile Diversity Research Center of the University of Texas at Arlington for the donation of turtle samples for this study, to Joseph R Mendelson, for the information on Phylogeography of the genus Bufo, and to three anonymous reviewers whose comments greatly enhanced the quality of this manuscript. NR 87 TC 8 Z9 8 U1 1 U2 13 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 EI 1572-9737 J9 CONSERV GENET JI Conserv. Genet. PD OCT PY 2011 VL 12 IS 5 BP 1229 EP 1242 DI 10.1007/s10592-011-0225-x PG 14 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 819BE UT WOS:000294799600009 ER PT J AU Cibois, A Beadell, JS Graves, GR Pasquet, E Slikas, B Sonsthagen, SA Thibault, JC Fleischer, RC AF Cibois, Alice Beadell, Jon S. Graves, Gary R. Pasquet, Eric Slikas, Beth Sonsthagen, Sarah A. Thibault, Jean-Claude Fleischer, Robert C. TI Charting the course of reed-warblers across the Pacific islands SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Acrocephalidae; Acrocephalus; back-colonization; colonization patterns; island biogeography; Micronesia; Pacific Ocean islands; phylogeny; Polynesia; reed-warblers ID MITOCHONDRIAL SEQUENCE DATA; K-AR AGES; HAWAIIAN-ISLANDS; FRENCH-POLYNESIA; SOUTH-PACIFIC; PHYLOGENETIC-RELATIONSHIPS; MOLECULAR PHYLOGENY; MONARCHS POMAREA; HENDERSON ISLAND; NATURAL-HISTORY AB Aim Deciphering the complex colonization history of island archipelagos is greatly facilitated by comprehensive phylogenies. In this study we investigate the phylogeny and biogeography of the insular reed-warblers (genus Acrocephalus) of the tropical Pacific Ocean, from Australia to eastern Polynesia. Location Oceania. Methods We used sequences of mitochondrial DNA (cytochrome b, ND2 and ATP8 genes) to infer the colonization patterns of reed-warblers endemic to Pacific islands and Australia. We sampled all known taxa of Acrocephalus in the Pacific except A. luscinius nijoi, for which no sample was available. Most taxa were represented by toe-pad samples from museum specimens collected in the 19th and 20th centuries. With a few exceptions, several specimens per taxon were sequenced independently in two institutions (Smithsonian Institution and Natural History Museum of Geneva). Results Our data indicate that Pacific reed-warblers do not form a monophyletic group, because A. luscinius luscinius from Guam falls outside the main Pacific radiation. The remaining Pacific taxa are divided into two clades: one clade includes all the reed-warblers from Micronesia (except Guam) and Australia, and two Polynesian taxa from the Line Islands and the southern Marquesas; the other clade includes all remaining Polynesian taxa. The taxa endemic to three archipelagos (Mariana, Marquesas and Society islands) are polyphyletic, suggesting several independent colonizations. Main conclusions Our results provide evidence for a complex pattern of colonization of the Pacific by reed-warblers. Calibration analyses suggest that reed-warbler lineages are much younger than the ages of the islands they occupy. Several remote archipelagos were colonized independently more than once. Consequently, we infer that the colonization of reed-warblers in the Pacific did not follow a regular, stepping-stone-like pattern. The phylogeny also suggests a previously undetected case of reverse colonization (from island to continent) for the Australian lineage and indicates that A. luscinius, as currently defined, is not monophyletic. We discuss the supertramp strategy of reed-warblers in the Pacific and show that, although Pacific reed-warblers meet some of the supertramp criteria in their aptitude for colonizing remote archipelagos, their life history characteristics do not fit the model. C1 [Cibois, Alice] Nat Hist Museum Geneva, Dept Mammal & Ornithol, CH-1211 Geneva 6, Switzerland. [Beadell, Jon S.; Sonsthagen, Sarah A.; Fleischer, Robert C.] Smithsonian Inst, Genet Program, Natl Museum Nat Hist, Washington, DC 20008 USA. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116, Washington, DC 20013 USA. [Pasquet, Eric; Thibault, Jean-Claude] Museum Natl Hist Nat, Dept Systemat & Evolut, Origine Struct & Evolut Biodivers UMR7205, Paris, France. [Pasquet, Eric; Thibault, Jean-Claude] Museum Natl Hist Nat, Serv Systemat Mol, CNRS, UMS2700, F-75005 Paris, France. [Slikas, Beth] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. RP Cibois, A (reprint author), Nat Hist Museum Geneva, Dept Mammal & Ornithol, CP 6434, CH-1211 Geneva 6, Switzerland. EM alice.cibois@ville-ge.ch FU DIREN Tahiti; Ornithological Society of Polynesia [6-0056/mdd]; Frank M. Chapman Memorial Fund (AMNH); European Commission [GB-TAF-1846/2002]; Swiss Academy of Sciences; G. and A. Claraz Foundation; Basel Foundation for Biological Research; US NSF [DEB-0643291]; Research Opportunities Fund FX We are very grateful to Joel Cracraft and Paul Sweet [American Museum of Natural History (AMNH), New York], Robert Prys-Jones and Mark Adams [British Museum (Natural History) (BMNH), Tring, UK], Clemency Fisher and Tony Parker [National Museums Liverpool (NML), UK], Peter-Rene Becker and Ulrich Burkhardt [Ubersee-Museum Bremen (UMB)], Alexander Haas and Cordula Bracker [Zoologisches Museum Hamburg (ZMH)] for access to the collections in their charge and for the sampling of specimens. The University of Washington Burke Museum and the University of Kansas kindly provided additional samples or sequences. We thank Sheila Conant (University of Hawai'i), Chris Filardi (Center for Biodiversity and Conservation, New York), Robert Moyle (University of Kansas), Jean-Yves Meyer (Research Delegation, Tahiti), Claude Serra (DIREN Tahiti), Philippe Raust (Manu, Ornithological Society of Polynesia), Florence Marteau [Museum d'Histoire Naturelle de Geneve (MHNG) Geneva], Bernd Leisler (Max Planck Institute for Ornithology, Munchen), Marshall Weisler (University of Queensland, St Lucia), the Institut pour la Recherche et le Developpement (Papeete), and the Service de Systematique Moleculaire [UMS2700-CNRS, Museum National d'Histoire Naturelle (MNHN), Paris]. Financial support by the DIREN Tahiti and the Ornithological Society of Polynesia (Convention no. 6-0056/mdd), the Collection Study Grant from the Frank M. Chapman Memorial Fund (AMNH), the European Commission's Research Infrastructure Action via the SYN-THESYS Project (applications GB-TAF-1846/2002), the Swiss Academy of Sciences (commission of travel grant), the G. and A. Claraz Foundation, the Basel Foundation for Biological Research, the US NSF (DEB-0643291 to R. C. F.), and the Research Opportunities Fund (Smithsonian Institution) is gratefully acknowledged. NR 91 TC 18 Z9 20 U1 3 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD OCT PY 2011 VL 38 IS 10 BP 1963 EP 1975 DI 10.1111/j.1365-2699.2011.02542.x PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 822MP UT WOS:000295052300010 ER PT J AU Clough, GW AF Clough, G. Wayne TI Jefferson's Bible SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD OCT PY 2011 VL 42 IS 6 BP 38 EP 38 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 824MO UT WOS:000295206200014 ER PT J AU Mengual, X Thompson, FC AF Mengual, Ximo Thompson, F. Christian TI Carmine cochineal killers: the flower fly genus Eosalpingogaster Hull (Diptera: Syrphidae) revised SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID BIOLOGICAL-CONTROL; SOUTH-AFRICA; CACTACEAE; DACTYLOPIIDAE; JMODELTEST; PHYLOGENY; HOMOPTERA; INFERENCE; SELECTION; ALIGNMENT AB The flower fly genus Eosalpingogaster Hull, predator of the carminic acid producer cochineal (Dactylopiidae), is revised. Two new species are described (knutsoni sp.n. and umbra sp.n.) and an identification key is provided for all known species. Diagnoses, illustrations, synonymies and distributional and biological data are given. Three new synonyms are proposed [texana Curran as jun.syn. of cochenillivora (Guerin-Meneville); liposeta Fluke and dactylopianus Blanchard as jun.syn. of nigriventris (Bigot)] and two lectotypes are designated for cochenillivora (Guerin-Meneville) and nigriventris (Bigot). Eosalpingogaster is elevated to full generic status based on adult morphological characters, biological data and a new phylogenetic analysis of molecular characters with genes 28S, 18S and cytochrome c oxidase subunit I. All data, images and drawings are available online as an example of the utility of international standards for biodiversity informatics. C1 [Mengual, Ximo; Thompson, F. Christian] Smithsonian Inst, NMNH, Dept Entomol, Washington, DC 20013 USA. RP Mengual, X (reprint author), Smithsonian Inst, NMNH, Dept Entomol, POB 37012,MRC 0169, Washington, DC 20013 USA. EM xmengual@gmail.com OI Mengual, Ximo/0000-0002-6185-9404 NR 92 TC 6 Z9 6 U1 0 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD OCT PY 2011 VL 36 IS 4 BP 713 EP 731 DI 10.1111/j.1365-3113.2011.00588.x PG 19 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 822LH UT WOS:000295047400008 ER PT J AU Gutermuth, RA Pipher, JL Megeath, ST Myers, PC Allen, LE Allen, TS AF Gutermuth, R. A. Pipher, J. L. Megeath, S. T. Myers, P. C. Allen, L. E. Allen, T. S. TI A CORRELATION BETWEEN SURFACE DENSITIES OF YOUNG STELLAR OBJECTS AND GAS IN EIGHT NEARBY MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: stars; stars: formation ID SPITZER C2D SURVEY; STAR-FORMING REGIONS; DENSE GAS; INTERSTELLAR CLOUDS; EMBEDDED CLUSTERS; PRESTELLAR CORES; FORMATION RATES; MASS FUNCTION; FORMATION LAW; ORION NEBULA AB We report the discovery and characterization of a power-law correlation between the local surface densities of Spitzer-identified, dusty young stellar objects (YSOs) and the column density of gas (as traced by near-IR extinction) in eight molecular clouds within 1 kpc and with 100 or more known YSOs. This correlation, which appears in data smoothed over size scales of similar to 1 pc, varies in quality from cloud to cloud; those clouds with tight correlations, MonR2 and Ophiuchus, are fit with power laws of slope 2.67 and 1.87, respectively. The spread in the correlation is attributed primarily to local gas disruption by stars that formed there or to the presence of very young subregions at the onset of star formation. We explore the ratio of the number of Class II to Class I sources, a proxy for the star formation age of a region, as a function of gas column density; this analysis reveals a declining Class II to Class I ratio with increasing column density. We show that the observed star-gas correlation is consistent with a star formation law where the star formation rate per area varies with the gas column density squared. We also propose a simple picture of thermal fragmentation of dense gas in an isothermal, self-gravitating layer as an explanation for the power law. Finally, we briefly compare the star-gas correlation and its implied star formation law with other recent proposed of star formation laws at similar and larger size scales from nearby star-forming regions. C1 [Gutermuth, R. A.] Smith Coll, Dept Astron, Coll 5, Northampton, MA 01063 USA. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Pipher, J. L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Megeath, S. T.; Allen, T. S.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Gutermuth, RA (reprint author), Smith Coll, Dept Astron, Coll 5, Northampton, MA 01063 USA. FU National Aeronautics and Space Administration [1407, 960541]; National Science Foundation FX This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract 1407 with NASA. Support for the IRAC instrument was provided by NASA through contract 960541 issued by JPL. NR 70 TC 84 Z9 84 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2011 VL 739 IS 2 AR 84 DI 10.1088/0004-637X/739/2/84 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821IZ UT WOS:000294969800029 ER PT J AU Jimenez-Serra, I Martin-Pintado, J Winters, JM Rodriguez-Franco, A Caselli, P AF Jimenez-Serra, I. Martin-Pintado, J. Winters, J. -M. Rodriguez-Franco, A. Caselli, P. TI VARIABILITY OF THE SiO THERMAL LINE EMISSION TOWARD THE YOUNG L1448-mm OUTFLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (L1448); ISM: jets and outflows; shock waves; stars: formation ID C-TYPE SHOCKS; MOLECULAR OUTFLOWS; PROPER MOTIONS; X-RAY; WAVES; EVOLUTION; CLOUDS; ORION; JET; PROPAGATION AB The detection of narrow SiO thermal emission toward young outflows has been proposed to be a signature of the magnetic precursor of C-shocks. Recent modeling of the SiO emission across C-shocks predicts variations in the SiO line intensity and line shape at the precursor and intermediate-velocity regimes in only a few years. We present high angular resolution (3.'' 8 x 3.'' 3) images of the thermal SiO J = 2 -> 1 emission toward the L1448-mm outflow in two epochs (2004 November-2005 February, 2009 March-April). Several SiO condensations have appeared at intermediate velocities (20-50 km s(-1)) toward the redshifted lobe of the outflow since 2005. Toward one of the condensations (clump D), systematic differences of the dirty beams between 2005 and 2009 could be responsible for the SiO variability. At higher velocities (50-80 km s(-1)), SiO could also have experienced changes in its intensity. We propose that the SiO variability toward L1448-mm is due to a real SiO enhancement by young C-shocks at the internal working surface between the jet and the ambient gas. For the precursor regime (5.2-9.2 km s(-1)), several narrow and faint SiO components are detected. The narrow SiO components tend to be compact, transient and show elongated (bow-shock) morphologies perpendicular to the jet. We speculate that these features are associated with the precursor of C-shocks appearing at the interface of the new SiO components seen at intermediate velocities. C1 [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martin-Pintado, J.; Rodriguez-Franco, A.] CSIC INTA, Ctr Astrobiol, E-28850 Madrid, Spain. [Winters, J. -M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Rodriguez-Franco, A.] Univ Complutense Madrid, Escuela Univ Opt, Dept Matemat Aplicada Biomatemat, E-28037 Madrid, Spain. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. RP Jimenez-Serra, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ijimenez-serra@cfa.harvard.edu; jmartin@cab.inta-csic.es; winters@iram.fr; rodriguezfa@cab.inta-csic.es; P.Caselli@leeds.ac.uk RI Martin-Pintado, Jesus/H-6107-2015 OI Martin-Pintado, Jesus/0000-0003-4561-3508 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); SMA; MICINN [ESP2007-65812-C02-C01, AYA2010-21697-C05-01]; AstroMadrid [CAM S2009/ESP-1496] FX Based on observations carried out with the IRAM Plateau de Bure Interferometer (PdBI). IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).; We thank the IRAM director, P. Cox, for letting us carry out the second epoch of the PdBI SiO observations, despite the reticence of the IRAM Programme Committee. We acknowledge an anonymous referee for his/her critical reading and constructive comments that helped to largely improve the manuscript. I. J.-S. acknowledges the Smithsonian Astrophysical Observatory for the support provided through an SMA fellowship. J. M.-P. and I. J.-S. have been partially funded by MICINN grants ESP2007-65812-C02-C01 and AYA2010-21697-C05-01 and AstroMadrid (CAM S2009/ESP-1496). NR 34 TC 4 Z9 4 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2011 VL 739 IS 2 AR 80 DI 10.1088/0004-637X/739/2/80 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821IZ UT WOS:000294969800025 ER PT J AU Lin, L Kouveliotou, C Baring, MG van der Horst, AJ Guiriec, S Woods, PM Gogus, E Kaneko, Y Scargle, J Granot, J Preece, R von Kienlin, A Chaplin, V Watts, AL Wijers, RAMJ Zhang, SN Bhat, N Finger, MH Gehrels, N Harding, A Kaper, L Kaspi, V Mcenery, J Meegan, CA Paciesas, WS Pe'er, A Ramirez-Ruiz, E van der Klis, M Wachter, S Wilson-Hodge, C AF Lin, Lin Kouveliotou, Chryssa Baring, Matthew G. van der Horst, Alexander J. Guiriec, Sylvain Woods, Peter M. Gogus, Ersin Kaneko, Yuki Scargle, Jeffrey Granot, Jonathan Preece, Robert von Kienlin, Andreas Chaplin, Vandiver Watts, Anna L. Wijers, Ralph A. M. J. Zhang, Shuang Nan Bhat, Narayan Finger, Mark H. Gehrels, Neil Harding, Alice Kaper, Lex Kaspi, Victoria Mcenery, Julie Meegan, Charles A. Paciesas, William S. Pe'er, Asaf Ramirez-Ruiz, Enrico van der Klis, Michiel Wachter, Stefanie Wilson-Hodge, Colleen TI Fermi/GAMMA-RAY BURST MONITOR OBSERVATIONS OF SGR J0501+4516 BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (SGR J0501+4516); X-rays: bursts ID SOFT GAMMA-REPEATERS; RESONANT CYCLOTRON SCATTERING; 1E 1547.0-5408; MAGNETAR; EMISSION; SGR-1900+14; SPECTRA; TIME; SOFT-GAMMA-REPEATER-1806-20; SPECTROSCOPY AB We present our temporal and spectral analyses of 29 bursts from SGR J0501+4516, detected with the gamma-ray burst monitor on board the Fermi Gamma-ray Space Telescope during 13 days of the source's activation in 2008 (August 22-September 3). We find that the T-90 durations of the bursts can be fit with a log-normal distribution with a mean value of similar to 123 ms. We also estimate for the first time event durations of soft gamma repeater (SGR) bursts in photon space (i.e., using their deconvolved spectra) and find that these are very similar to the T-90 values estimated in count space (following a log-normal distribution with a mean value of similar to 124 ms). We fit the time-integrated spectra for each burst and the time-resolved spectra of the five brightest bursts with several models. We find that a single power law with an exponential cutoff model fits all 29 bursts well, while 18 of the events can also be fit with two blackbody functions. We expand on the physical interpretation of these two models and we compare their parameters and discuss their evolution. We show that the time-integrated and time-resolved spectra reveal that E-peak decreases with energy flux (and fluence) to a minimum of similar to 30 keV at F = 8.7 x 10(-6) erg cm(-2) s(-1), increasing steadily afterward. Two more sources exhibit a similar trend: SGRs J1550-5418 and 1806-20. The isotropic luminosity, L-iso, corresponding to these flux values is roughly similar for all sources (0.4-1.5 x 10(40) erg s(-1)). C1 [Lin, Lin; Zhang, Shuang Nan] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Lin, Lin; Guiriec, Sylvain; Preece, Robert; Chaplin, Vandiver; Bhat, Narayan; Paciesas, William S.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA. [Kouveliotou, Chryssa; Wilson-Hodge, Colleen] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [van der Horst, Alexander J.; Finger, Mark H.; Meegan, Charles A.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. [Woods, Peter M.] Corvid Technol, Huntsville, AL 35806 USA. [Gogus, Ersin; Kaneko, Yuki] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. [Scargle, Jeffrey] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Granot, Jonathan] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [von Kienlin, Andreas] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Watts, Anna L.; Wijers, Ralph A. M. J.; Kaper, Lex; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Zhang, Shuang Nan] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China. [Gehrels, Neil; Harding, Alice; Mcenery, Julie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kaspi, Victoria] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Wachter, Stefanie] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Lin, L (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. EM lin.lin@uah.edu RI Gehrels, Neil/D-2971-2012; Harding, Alice/D-3160-2012; McEnery, Julie/D-6612-2012; OI Wijers, Ralph/0000-0002-3101-1808; Preece, Robert/0000-0003-1626-7335 FU NASA [NNH07ZDA001-GLAST, NNX10AC59A]; Scientific and Technological Research Council of Turkey (TUBITAK) [109T755]; Bundesministeriums fur Wirtschaft und Technologie (BMWi) [50 OG 1101]; Netherlands Organization for Scientific Research (NWO); European Research Council [247295] FX This publication is part of the GBM/Magnetar Key Project (NASA grant NNH07ZDA001-GLAST, PI: C. Kouveliotou). M. G. B. acknowledges support from NASA through grant NNX10AC59A. E.G. and Y.K. acknowledge the support from the Scientific and Technological Research Council of Turkey (TUBITAK) through grant 109T755. A. v. K. was supported by the Bundesministeriums fur Wirtschaft und Technologie (BMWi) through DLR grant 50 OG 1101. A. L. W. acknowledges support from a Netherlands Organization for Scientific Research (NWO) Vidi Grant. R.A.M.J.W. acknowledges support from the European Research Council via Advanced Investigator Grant No. 247295. NR 48 TC 22 Z9 22 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2011 VL 739 IS 2 AR 87 DI 10.1088/0004-637X/739/2/87 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821IZ UT WOS:000294969800032 ER PT J AU Oberst, TE Parshley, SC Nikola, T Stacey, GJ Lohr, A Lane, AP Stark, AA Kamenetzky, J AF Oberst, T. E. Parshley, S. C. Nikola, T. Stacey, G. J. Loehr, A. Lane, A. P. Stark, A. A. Kamenetzky, J. TI A 205 mu m [N II] MAP OF THE CARINA NEBULA SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; infrared: ISM; ISM: individual objects (Carina Nebula); ISM: lines and bands; photon-dominated region (PDR); submillimeter: ISM ID LASER MAGNETIC-RESONANCE; ANTARCTIC-SUBMILLIMETER-TELESCOPE; LONG-WAVELENGTH SPECTROMETER; FAR-INFRARED OBSERVATIONS; MOLECULAR CLOUD COMPLEX; STAR-FORMING REGION; PHOTODISSOCIATION REGIONS; C-II; INTERSTELLAR-MEDIUM; PHYSICAL CONDITIONS AB We present the results of a similar to 250 arcmin(2) mapping of the 205 mu m [N II] fine-structure emission over the northern Carina Nebula, including the Car I and Car II H II regions. Spectra were obtained using the South Pole Imaging Fabry-Perot Interferometer (SPIFI) at the Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) at the South Pole. We supplement the 205 mu m data with new reductions of far-IR fine-structure spectra from the Infrared Space Observatory (ISO) Long Wavelength Spectrometer (LWS) in 63 mu m [O I], 122 mu m [N II], 146 mu m [O I], and 158 mu m [C II]; the 146 mu m [O I] data include 90 raster positions which have not been previously published. Morphological comparisons are made with optical, radio continuum, and CO maps. The 122/205 line ratio is used to probe the density of the low-ionization gas, and the 158/205 line ratio is used to probe the fraction of C+ arising from photodissociation regions (PDRs). The [O I] and [C II] lines are used to construct a PDR model of Carina. When the PDR properties are compared with other sources, Carina is found to be more akin to 30 Doradus than galactic star-forming regions such as Orion, M17, or W49; this is consistent with the view of Carina as a more evolved region, where much of the parent molecular cloud has been ionized or swept away. These data constitute the first ground-based detection of the 205 mu m [N II] line, and the third detection overall since those of COBE FIRAS and the Kuiper Airborne Observatory in the early 1990s. C1 [Oberst, T. E.; Parshley, S. C.; Nikola, T.; Stacey, G. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Loehr, A.; Lane, A. P.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kamenetzky, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA. RP Oberst, TE (reprint author), Westminster Coll, Dept Phys, New Wilmington, PA 16172 USA. EM oberstte@westminster.edu FU NASA [GSRP NNG05GK70H]; NSF [IGERT DGE-9870631, CSIP DGE-0231913, OPP-0094605, OPP-0338149, OPP0126090] FX The authors especially thank the following individuals and groups: Carole E. Tucker, who provided SPIFI's filters; Jacob W. Kooi, for operating local oscillators at the AST/RO during SPIFI calibration; K. Sigfrid Yngvesson and the TREND group, for use of the TREND laser at the AST/RO during SPIFI calibration; and prior members of the SPIFI team, including C. Matt Bradford, Alberto D. Bolatto, James M. Jackson, Mark R. Swain, Maureen L. Savage, Jacqueline A. Davidson, and similar to 15 undergraduate student researchers. Finally, we are thankful for the support of the following grants: NASA GSRP NNG05GK70H; NSF IGERT DGE-9870631; NSF CSIP DGE-0231913; and NSF OPP-0094605, OPP-0338149, and OPP0126090. NR 94 TC 22 Z9 22 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2011 VL 739 IS 2 AR 100 DI 10.1088/0004-637X/739/2/100 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821IZ UT WOS:000294969800045 ER PT J AU Perlman, ES Georganopoulos, M Marshall, HL Schwartz, DA Padgett, CA Gelbord, J Lovell, JEJ Worrall, DM Birkinshaw, M Murphy, DW Jauncey, DL AF Perlman, Eric S. Georganopoulos, Markos Marshall, Herman L. Schwartz, Daniel A. Padgett, C. A. Gelbord, Jonathan Lovell, J. E. J. Worrall, Diana M. Birkinshaw, Mark Murphy, David W. Jauncey, David L. TI DEEP MULTIWAVEBAND OBSERVATIONS OF THE JETS OF 0208-512 AND 1202-262 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (PKS0208-512, PKS1202-262); radio continuum: galaxies; X-rays: galaxies ID X-RAY JETS; SPACE-TELESCOPE OBSERVATIONS; SPECTRUM RADIO QUASARS; INVERSE-COMPTON MODEL; EXTRAGALACTIC JETS; SOUTHERN-HEMISPHERE; PKS 0637-752; CHANDRA; EMISSION; SYNCHROTRON AB We present deep Hubble Space Telescope, Chandra, Very Large Array, and Australia Telescope Compact Array images of the jets of PKS 0208-512 and PKS 1202-262, which were found in a Chandra survey of a flux-limited sample of flat-spectrum radio quasars with jets. We discuss in detail their X-ray morphologies and spectra. We find optical emission from one knot in the jet of PKS 1202-262 and two regions in the jet of PKS 0208-512. The X-ray emission of both jets is most consistent with external Comptonization of cosmic microwave background photons by particles within the jet, while the optical emission is most consistent with the synchrotron process. We model the emission from the jet in this context and discuss implications for jet emission models, including magnetic field and beaming parameters. C1 [Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Perlman, Eric S.; Georganopoulos, Markos] Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Georganopoulos, Markos; Padgett, C. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marshall, Herman L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Schwartz, Daniel A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Gelbord, Jonathan] Univ Durham, Dept Phys, Sci Labs, Durham DH1 3LE, England. [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Lovell, J. E. J.; Jauncey, David L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Worrall, Diana M.; Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Murphy, David W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Perlman, ES (reprint author), Florida Inst Technol, Dept Phys & Space Sci, 150 W Univ Blvd, Melbourne, FL 32901 USA. EM eperlman@fit.edu; georgano@umbc.edu; hermanm@space.mit.edu; das@head-cfa.harvard.edu; j.m.gelbord@durham.ac.uk; Jim.Lovell@utas.edu.au; d.worrall@bristol.ac.uk; mark.birkinshaw@bristol.ac.uk; dwm@sgra.jpl.nasa.gov; david.jauncey@csiro.au OI Perlman, Eric/0000-0002-3099-1664 FU Chandra GO [G02-3151D, G04- 5107X]; HST [STGO-10002.01]; NASA [NAG5-9997, NNG05-GD63DG, SAO SV1-61010, NAS8-39073, NAS8-03060]; UMBC [NNX07-AM17G]; CXC [GO2-3151A, G02-3151C] FX E. S. P., C. A. P., and M. G. acknowledge support from Chandra GO grants G02-3151D and G04- 5107X), HST (grant STGO-10002.01), and NASA (LTSA grants NAG5-9997 and NNG05-GD63DG at UMBC and NNX07-AM17G at FIT). H. L. M. was supported under NASA contract SAO SV1-61010 for the Chandra X-Ray Center (CXC). J.M.G. was supported under Chandra grant GO2-3151A to MIT from the CXC. D. A. S. was partially supported by Chandra grant G02-3151C to SAO from the CXC, and by NASA contracts NAS8-39073 and NAS8-03060 to the CXC. NR 53 TC 3 Z9 3 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2011 VL 739 IS 2 AR 65 DI 10.1088/0004-637X/739/2/65 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821IZ UT WOS:000294969800010 ER PT J AU Binder, B Williams, BF Kong, AKH Gaetz, TJ Plucinsky, PP Dalcanton, JJ Weisz, DR AF Binder, B. Williams, B. F. Kong, A. K. H. Gaetz, T. J. Plucinsky, P. P. Dalcanton, J. J. Weisz, D. R. TI CHANDRA DETECTION OF SN 2010da FOUR MONTHS AFTER OUTBURST: EVIDENCE FOR A HIGH-MASS X-RAY BINARY IN NGC 300 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: massive; supernovae: individual (SN 2010da); X-rays: binaries ID SMALL-MAGELLANIC-CLOUD; ACIS SURVEY; XMM-NEWTON AB We present the results of a 63 ks Chandra observation of the "supernova impostor" SN 2010da four months after it was first observed on 2010 May 24. We detect an X-ray source at similar to 7 sigma confidence coincident with the optical location of the outburst. Our imaging analysis has revealed a hard central point source, surrounded by soft diffuse emission extending similar to 8 '' north of the central source. The diffuse emission has a hardness ratio (similar to-0.4), 0.35-2 keV luminosity (similar to 6 x 10(35) erg s(-1)), and size (similar to 70 pc) consistent with that of a supernova remnant, although the low number of counts prohibits detailed spectral modeling. The 0.5-6 keV spectrum of the central point source is well described by both a power law with Gamma similar to 0 and a blackbody with kT similar to 1.8 keV, with no evidence for intrinsic absorption beyond the Galactic column. We estimate the 0.3-10 keV luminosity to be similar to 2 x 10(37) erg s(-1), a factor of similar to 25 decrease since the initial outburst. The high X-ray luminosity and slow fading rate is not consistent with this object being a single massive star undergoing an outburst. When combined with the optical and infrared properties of the outburst and progenitor systems, our X-ray observations suggest the SN 2010da system may be a Be X-ray binary system which experienced an extremely bright optical outburst near simultaneously with a bright, Type II X-ray outburst. C1 [Binder, B.; Williams, B. F.; Dalcanton, J. J.; Weisz, D. R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Gaetz, T. J.; Plucinsky, P. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Binder, B (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. FU Chandra grant [GO1-12118X]; NASA [NAS8-03060] FX The authors thank an anonymous referee for the many helpful comments which significantly improved this manuscript, as well as C. S. Kochanek, J. L. Prieto, and R. Humphreys for insightful communications on this source. The authors thank M. Eracleous and E. Skillman for comments on early drafts of this manuscript. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester and the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. B.B. and B.F.W. acknowledge support from Chandra grant GO1-12118X. T.J.G. and P.P.P. acknowledge support of NASA Contract NAS8-03060. NR 33 TC 6 Z9 6 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2011 VL 739 IS 2 AR L51 DI 10.1088/2041-8205/739/2/L51 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821TP UT WOS:000294997600017 ER PT J AU Fayolle, EC Bertin, M Romanzin, C Michaut, X Oberg, KI Linnartz, H Fillion, JH AF Fayolle, Edith C. Bertin, Mathieu Romanzin, Claire Michaut, Xavier Oeberg, Karin I. Linnartz, Harold Fillion, Jean-Hugues TI CO ICE PHOTODESORPTION: A WAVELENGTH-DEPENDENT STUDY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: abundances; ISM: molecules; molecular data; molecular processes ID PROTOPLANETARY DISKS; ELECTRON-IMPACT; WATER ICE; DESORPTION; INTERSTELLAR; N-2; ADSORPTION; RADIATION; MOLECULES; SURFACES AB UV-induced photodesorption of ice is a non-thermal evaporation process that can explain the presence of cold molecular gas in a range of interstellar regions. Information on the average UV photodesorption yield of astrophysically important ices exists for broadband UV lamp experiments. UV fields around low-mass pre-main-sequence stars, around shocks and in many other astrophysical environments are however often dominated by discrete atomic and molecular emission lines. It is therefore crucial to consider the wavelength dependence of photodesorption yields and mechanisms. In this work, for the first time, the wavelength-dependent photodesorption of pure CO ice is explored between 90 and 170 nm. The experiments are performed under ultra high vacuum conditions using tunable synchrotron radiation. Ice photodesorption is simultaneously probed by infrared absorption spectroscopy in reflection mode of the ice and by quadrupole mass spectrometry of the gas phase. The experimental results for CO reveal a strong wavelength dependence directly linked to the vibronic transition strengths of CO ice, implying that photodesorption is induced by electronic transition (DIET). The observed dependence on the ice absorption spectra implies relatively low photodesorption yields at 121.6 nm (Ly alpha), where CO barely absorbs, compared to the high yields found at wavelengths coinciding with transitions into the first electronic state of CO (A(1)Pi at 150 nm); the CO photodesorption rates depend strongly on the UV profiles encountered in different star formation environments. C1 [Fayolle, Edith C.; Linnartz, Harold] Leiden Univ, Leiden Observ, Sackler Lab Astrophys, NL-2300 RA Leiden, Netherlands. [Bertin, Mathieu; Romanzin, Claire; Michaut, Xavier; Fillion, Jean-Hugues] Univ Paris 06, Lab Phys Mol Atmosphere & Astrophys, CNRS UMR7092, F-75005 Paris, France. [Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fayolle, EC (reprint author), Leiden Univ, Leiden Observ, Sackler Lab Astrophys, POB 9513, NL-2300 RA Leiden, Netherlands. RI Bertin, Mathieu/C-7134-2012; OI Bertin, Mathieu/0000-0002-9021-2415; Fayolle, Edith/0000-0001-8109-5256 FU French national program PCMI (Physique chimie du milieu interstellaire); Dutch program NOVA (Nederlandse Onderzoekschool Voor Astronomie); COST action [CM0805]; Hubert Curien Partenership "Van Gogh"; NASA; Space Telescope Science Institute [NAS 5-26555] FX We are grateful to Ewine van Dishoeck and Marc van Hemert for stimulating discussions. We thank Hsiao-Chi Lu, Roland Gredel, and Edwin Bergin for providing useful data. We acknowledge SOLEIL for provision of synchrotron radiation facilities, as well as Laurent Nahon for technical help on the beamline DESIRS. Financial support from the French national program PCMI (Physique chimie du milieu interstellaire), the Dutch program NOVA (Nederlandse Onderzoekschool Voor Astronomie), the COST action CM0805 "The Chemical Cosmos," and the Hubert Curien Partenership "Van Gogh," are gratefully acknowledged. Support for K.I.O is provided by NASA through a Hubble Fellowship grant awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 23 TC 59 Z9 59 U1 1 U2 22 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2011 VL 739 IS 2 AR L36 DI 10.1088/2041-8205/739/2/L36 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821TP UT WOS:000294997600002 ER PT J AU Torok, T Panasenco, O Titov, VS Mikic, Z Reeves, KK Velli, M Linker, JA De Toma, G AF Toeroek, T. Panasenco, O. Titov, V. S. Mikic, Z. Reeves, K. K. Velli, M. Linker, J. A. De Toma, G. TI A MODEL FOR MAGNETICALLY COUPLED SYMPATHETIC ERUPTIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: numerical; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun: flares; Sun: magnetic topology ID CORONAL MASS EJECTIONS; SOLAR CORONA; FLUX ROPES; FLARES; TOPOLOGY; RECONNECTION; OSCILLATIONS; CONNECTION; FILAMENTS; LINKAGES AB Sympathetic eruptions on the Sun have been observed for several decades, but the mechanisms by which one eruption can trigger another remain poorly understood. We present a three-dimensional MHD simulation that suggests two possible magnetic trigger mechanisms for sympathetic eruptions. We consider a configuration that contains two coronal flux ropes located within a pseudo-streamer and one rope located next to it. A sequence of eruptions is initiated by triggering the eruption of the flux rope next to the streamer. The expansion of the rope leads to two consecutive reconnection events, each of which triggers the eruption of a flux rope by removing a sufficient amount of overlying flux. The simulation qualitatively reproduces important aspects of the global sympathetic event on 2010 August 1 and provides a scenario for the so-called twin filament eruptions. The suggested mechanisms are also applicable for sympathetic eruptions occurring in other magnetic configurations. C1 [Toeroek, T.; Titov, V. S.; Mikic, Z.; Linker, J. A.] Predict Sci Inc, San Diego, CA 92121 USA. [Panasenco, O.] Helio Res, La Crescenta, CA 91214 USA. [Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Velli, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [De Toma, G.] HAO NCAR, Boulder, CO 80307 USA. RP Torok, T (reprint author), Predict Sci Inc, 9990 Mesa Rim Rd,Suite 170, San Diego, CA 92121 USA. RI Reeves, Katharine/P-9163-2014 FU NASA [NNX09AG27G]; NASA/SHP [NNH09AK02I]; Lockheed-Martin [SP02H1701R]; International Space Science Institute via International Team 174 on Solar Prominence Formation and Equilibrium FX We thank P. Demoulin, B. Kliem, and K. Schrijver for stimulating discussions. The contribution of T.T, V.S.T., Z.M., and J.A.L. was supported by NASA's HTP, LWS, and SR&T programs, CISM (an NSF Science and Technology Center), and a contract from Lockheed-Martin to Predictive Science, Inc. O.P. was supported by NASA grant NNX09AG27G, G.D.T. by NASA/SHP grant NNH09AK02I, and K. K. R. by contract SP02H1701R from Lockheed-Martin to SAO. M.V's. contribution was carried out at JPL (Caltech) under a contract with NASA. Computational resources were provided by NSF TACC in Austin and by NASA NAS at the Ames Research Center. This work was partially supported by the International Space Science Institute via International Team 174 on Solar Prominence Formation and Equilibrium. NR 50 TC 57 Z9 57 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2011 VL 739 IS 2 AR L63 DI 10.1088/2041-8205/739/2/L63 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821TP UT WOS:000294997600029 ER PT J AU Prasad, AKSK Nienow, JA Hargraves, P AF Prasad, Akshinthala K. S. K. Nienow, James A. Hargraves, Paul TI Plicate species of the diatom genus Thalassiosira (Bacillariophyta) from the Atlantic and Gulf coasts of southeastern United States, with the description of T.livingstoniorum sp nov. SO PROCEEDINGS OF THE ACADEMY OF NATURAL SCIENCES OF PHILADELPHIA LA English DT Article DE Thalassiosira cedarkeyensis; T. livingstoniorum sp nov.; plicate valves; Indian River Lagoon; Gulf coast of Florida; diatom blooms; Fenholloway estuary; Econfina estuary AB Long-term observations of a marine planktonic plicate Tlzalassiosira species, T. cedarkeyensis Prasad, from the Gulf coasts of Florida, Alabama, and Mississippi and the Atlantic coasts of Florida and Georgia demonstrate its wide occurrence in the southeastern United States and its ability to form extensive blooms. We also report for the first time its ability to form typical Thalassiosira chains, linking sibling cells by threads of chitin. A closely related and co-occurring diatom, T. livingstoniorum, is described on the basis of investigations conducted during 2000-2011 as a new species from many localities in Apalachee Bay on the Gulf coast and Indian River Lagoon on the Atlantic coast of Florida. It differs from T. cedarkeyensis in areola density, presence of continuous cribra on loculate areolae, arrangement and distribution of valve processes, and the number of satellite pores surrounding the valve-face fultoportulae. We have not yet found any evidence of chain formation in T. livingstoniorum. Thalassiosira cedarkeyensis and T. livingstoniorum can be easily distinguished in Naphrax-mounted preparations in light microscopy (LM), and they represent two different groups (lineages?) of plicate species with reference to internal cribrum structure of the loculate areolae. Their differences may justify placement in two different genera. Although T. cedarkeyensis (which has individual cribra on the proximal siliceous layer like T. hyperborea) is abundant and widespread on the Gulf and Atlantic coasts of the southeastern United States, T. livingstoniorum (which has continuous cribra like T. lacustris) has been found, thus far, only in Florida coastal waters. Comparisons are made between these two species and the other morphologically similar extant and extinct plicate species. Thalassiosira livingstoniorum and T. cedarkeyensis, although widespread and frequently encountered during warmer months, may be easily overlooked sources of primary production in the nutrient-rich northeastern Gulf of Mexico. C1 [Prasad, Akshinthala K. S. K.] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. [Nienow, James A.] Valdosta State Univ, Dept Biol, Valdosta, GA 31698 USA. [Hargraves, Paul] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. [Hargraves, Paul] Florida Atlantic Univ, Harbor Branch Oceanog Inst, Boca Raton, FL 33431 USA. [Hargraves, Paul] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Prasad, AKSK (reprint author), Florida State Univ, Dept Biol Sci, B-157, Tallahassee, FL 32306 USA. EM prasad@bio.fsu.edu FU Florida Fish & Wildlife Research Institute [06135]; State of Florida's Save our Seas license plate program FX We acknowledge with gratitude all crew members who made collections used in this work, especially R. J. Livingston, R. L. Howell IV, and W. K. Karsteter for the monthly phytoplankton samples from the Econfina and Fenholloway estuaries from 1991 through 2003, and B. A. Vittor & Associates, Inc., Dr. Carl M. Way, J. O'Neal, and D. Lee for providing phytoplankton samples from the same sites from 2003 through 2009. P. A. Fryxell kindly provided the Latin translation of the description for the new species. AKSKP thanks K A Riddle and T. Fellers of the Florida State University Biological Science Imaging Resource Facility for their skillful and expert technical assistance with scanning electron microscopes, T. Fellers for Figure 27, and Charles Bad land for preparing the photographic plates. PEH thanks D. Hanisak (Harbor Branch Oceanographic Institute (HBOI) at Florida Atlantic University) and J. Piraino (Smithsonian Marine Station (SMS) at Fort Pierce) for logistic and technical support. This is HBOI contribution #1839 and SMS contribution #864. Sample collection in the Indian River Lagoon was supported by Florida Fish & Wildlife Research Institute (FWC Agreement #06135 and the State of Florida's Save our Seas license plate program). NR 95 TC 3 Z9 3 U1 0 U2 3 PU ACAD NATURAL SCIENCES PHILA PI PHILADELPHIA PA SCIENTIFIC PUBLICATIONS, 1900 BENJ FRANKLIN PKWY, PHILADELPHIA, PA 19103-1195 USA SN 0097-3157 J9 P ACAD NAT SCI PHILA JI Proc. Acad. Nat. Sci. Phila. PD OCT PY 2011 VL 161 BP 1 EP 34 PG 34 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA V29TJ UT WOS:000208770400001 ER PT J AU Wisman, JD Smith, JF AF Wisman, Jon D. Smith, James F. TI Legitimating Inequality: Fooling Most of the People All of the Time SO AMERICAN JOURNAL OF ECONOMICS AND SOCIOLOGY LA English DT Article ID UNITED-STATES; INCOME INEQUALITY; MOBILITY; HEALTH; CRIME AB Over the three decades leading up to the crisis of 2008, inequality dramatically increased in the United States and Great Britain. What stands out, but is seldom noted, is that this occurred within democracies where the relative losers-the overwhelming majority-could in principle have used the political system to block or reverse rising inequality. Why did they not do so? A glance at history reveals that peoples have only very infrequently contested inequality because they were led to believe that their inferior status in terms of income, wealth, and privilege was just, that it was not really so bad, or that it was necessary for their future well-being. Ideological systems legitimated a status quo of inequality, or in more modern times even increasing inequality. This article surveys the manner in which inequality has been historically legitimated, first predominantly by religion, then predominately by economic thought. Attention is then focused on the manner in which contemporary economic science and its popular interpretations in the media have served to legitimate inequality in the U.S. since the mid-1970s. The article concludes with a reflection on the unique conditions that enable the legitimation of inequality to be delegitimated. C1 [Wisman, Jon D.; Smith, James F.] American Univ, Washington, DC 20016 USA. [Wisman, Jon D.; Smith, James F.] Smithsonian Inst, Washington, DC 20560 USA. RP Wisman, JD (reprint author), American Univ, Washington, DC 20016 USA. NR 83 TC 6 Z9 6 U1 1 U2 14 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9246 J9 AM J ECON SOCIOL JI Am. J. Econ. Sociol. PD OCT PY 2011 VL 70 IS 4 BP 974 EP 1013 DI 10.1111/j.1536-7150.2011.00795.x PG 40 WC Economics; Sociology SC Business & Economics; Sociology GA 815WZ UT WOS:000294562000006 ER PT J AU Werling, BP Meehan, TD Robertson, BA Gratton, C Landis, DA AF Werling, Ben P. Meehan, Timothy D. Robertson, Bruce A. Gratton, Claudio Landis, Douglas A. TI Biocontrol potential varies with changes in biofuel-crop plant communities and landscape perenniality SO GLOBAL CHANGE BIOLOGY BIOENERGY LA English DT Article DE biodiversity; biofuels; biological control; ecosystem services; land use change ID ECOSYSTEM SERVICES; AGRICULTURAL LANDSCAPES; NATURAL ENEMIES; BENEFICIAL ARTHROPODS; GRASSLAND ECOSYSTEMS; BIOLOGICAL-CONTROL; BIODIVERSITY; DIVERSITY; HABITATS; FARMLAND AB We examined the potential local- and landscape-level impacts of different biofuel production systems on biocontrol, an important service provided by arthropod natural enemies. Specifically, we sampled natural enemies with sweep nets and measured predation of sentinel pest eggs in stands of corn, switchgrass and mixed prairie in Michigan and Wisconsin (total n = 40 for natural enemy sampling, n = 60 for egg predation), relating them to crop type, forb cover and diversity, and the composition and heterogeneity of the surrounding landscape. Grasslands with intermediate levels of forb cover and flower diversity supported two-orders of magnitude more natural enemy biomass, fourfold more natural enemy families, and threefold greater rates of egg predation than corn. Data suggest this was in part due to a general increase in biomass, richness and predation in perennial grasslands compared with corn, combined with a positive effect of intermediate levels of forb cover and flower diversity. Specifically, natural enemy biomass and family richness showed hump-shaped relationships to forb cover that peaked in sites with 5-25% forbs, while egg predation increased with floral diversity. At the landscape scale, both natural-enemy biomass and egg predation increased with the area of forest in the landscape, and egg predation almost doubled as the area of herbaceous, perennial habitats within 1.5km of study sites increased. Our results suggest that floristically diverse, perennial grasslands support diverse and abundant predator communities that contribute to natural pest suppression. In addition, large-scale production of biofuel crops could positively or negatively affect biocontrol services in agricultural landscapes through associated changes in the area of perennial habitats. Biofuel landscapes that incorporate perennial grasslands could support a variety of beneficial organisms and ecosystem services in addition to producing biomass. C1 [Werling, Ben P.; Landis, Douglas A.] Michigan State Univ, Dept Entomol, DOE Great Lakes Bioenergy Res Ctr, E Lansing, MI 48824 USA. [Meehan, Timothy D.; Gratton, Claudio] Univ Wisconsin, Dept Entomol, DOE Great Lakes Bioenergy Res Ctr, Madison, WI 53706 USA. [Robertson, Bruce A.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. RP Werling, BP (reprint author), Michigan State Univ, Dept Entomol, DOE Great Lakes Bioenergy Res Ctr, E Lansing, MI 48824 USA. EM werlingb@msu.edu FU DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science) [DE-FC02-07ER64494]; U.S. National Science Foundation; MSU FX Mary Gardiner, Lauren Bailey, and Hannah Gaines established the GLBRC Extensive site network and initial sampling protocols. Carol Baker and Pam Mosley identified flower specimens in Michigan. Special thanks to participating landowners as well as Ermyas Birru, Michael Burdick, Amanda Falk, Emily Fricke, Adam Higgins, Steve Hong, Andy Jakubowski, Liz Loomis, Craig Maier, Rachel Mallinger, Jessica Miesel, Emily Mueller, Collin Schwantes, Cari Sebright, Ruth Smith and Laura Smith for invaluable field assistance. Kay Gross, Anna Fiedler, Megan Woltz and three anonymous reviewers provided comments on the manuscript. This work was funded by the DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science DE-FC02-07ER64494), with additional support from the U.S. National Science Foundation LTER Program, DOE Energy Efficiency and Renewable Energy, and MSU AgBioResearch (formerly the Michigan Agricultural Experiment Station). NR 66 TC 28 Z9 28 U1 6 U2 53 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1757-1693 J9 GCB BIOENERGY JI GCB Bioenergy PD OCT PY 2011 VL 3 IS 5 BP 347 EP 359 DI 10.1111/j.1757-1707.2011.01092.x PG 13 WC Agronomy; Biotechnology & Applied Microbiology; Energy & Fuels SC Agriculture; Biotechnology & Applied Microbiology; Energy & Fuels GA 818BE UT WOS:000294723100001 ER PT J AU Gaspar, C Gaston, KJ Borges, PAV Cardoso, P AF Gaspar, Clara Gaston, Kevin J. Borges, Paulo A. V. Cardoso, Pedro TI Selection of priority areas for arthropod conservation in the Azores archipelago SO JOURNAL OF INSECT CONSERVATION LA English DT Article DE Arthropods; Azores; Complementarity; Irreplaceability; Optimisation algorithm; Reserve selection ID RESERVE SELECTION; PROTECTED AREAS; BIODIVERSITY; IRREPLACEABILITY; PERFORMANCE; DIVERSITY; NETWORKS; COSTS; GOAL AB The largest standardised database available to date for arthropods in native forests of the Azores archipelago was used to determine the minimum optimal set of native forest fragments needed to accomplish four different targets of species occurrence (presence-absence) and abundance (20, 50 and 80%) using different groups of arthropods and all data combined. The results showed that occurrence and 20% abundance targets gave similar optimal solutions for most of the groups considered. At least one fragment on each of the seven studied islands was required to accomplish any occurrence and abundance target. To achieve 80% of abundance for all species, all fragments were necessary and to guarantee 50% of the overall abundance of endemics, 17 out of 18 native forests were needed. A suggestion is made to apply a measure of biotic integrity related to disturbance to select, among alternative optimal solutions, the set of areas that will help to guarantee the viability of populations. Some guidelines for the selection of priority areas for conservation in the Azores are presented. C1 [Gaspar, Clara; Borges, Paulo A. V.; Cardoso, Pedro] Univ Acores, Azorean Biodivers Grp CITA A, Dept Ciencias Agr, P-9701851 Terceira, Azores, Portugal. [Gaspar, Clara; Gaston, Kevin J.] Univ Sheffield, Dept Anim & Plant Sci, Biodivers & Macroecol Grp, Sheffield S10 2TN, S Yorkshire, England. [Cardoso, Pedro] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Gaspar, C (reprint author), Univ Acores, Azorean Biodivers Grp CITA A, Dept Ciencias Agr, P-9701851 Terceira, Azores, Portugal. EM cgaspar@ennor.org RI Borges, Paulo/B-2780-2008; Cardoso, Pedro/A-8820-2008 OI Borges, Paulo/0000-0002-8448-7623; Cardoso, Pedro/0000-0001-8119-9960 FU Portuguese Fundacao para a Ciencia e a Tecnologia [BD/11049/2002]; Azorean Fundo Regional da Ciencia e Tecnologia [M3.1.7/F/007/2009]; Fundacao para a Ciencia e a Tecnologia [SFRH/BPD/40688/2007]; Azorean Direccao Regional dos Recursos Florestais [17.01-080203] FX We are grateful to all of the researchers that collaborated in the field and laboratory: Alvaro Vitorino, Anabela Arraiol, Ana Rodrigues, Artur Serrano, Carlos Aguiar, Catarina Melo, Francisco Dinis, Genage Andre, Emanuel Barcelos, Fernando Pereira, Hugo Mas, Isabel Amorim, Joao Amaral, Joaquin Hortal, Lara Dinis, Paula Goncalves, Sandra Jarroca, Servio Ribeiro and Luis Vieira. The Forest Services provided local support on each island. Acknowledgments are due to all of the taxonomists who assisted in the identification of the morphotypes: Andrew Polaszek, Bivar Sousa, Artur Serrano, Arturo Baz, Fernando Ilharco, Henrik Enghoff, Jordi Ribes, Jose Quartau, Jorg Wunderlich, Mario Boieiro, Ole Karsholt, Richard Strassen, Volker Manhert and Virgilio Vieira. We thank Jon Sadler, Owen Petchey, Simone Fattorini and an anonymous referee for helpful discussions and suggestions. CG was funded by the Portuguese Fundacao para a Ciencia e a Tecnologia (BD/11049/2002) during her PhD research project and has currently a postdoctoral grant from the Azorean Fundo Regional da Ciencia e Tecnologia (M3.1.7/F/007/2009). PC is supported by Fundacao para a Ciencia e a Tecnologia (SFRH/BPD/40688/2007). Field work was also funded by the Azorean Direccao Regional dos Recursos Florestais (Proj. 17.01-080203). NR 38 TC 13 Z9 13 U1 1 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1366-638X EI 1572-9753 J9 J INSECT CONSERV JI J. Insect Conserv. PD OCT PY 2011 VL 15 IS 5 BP 671 EP 684 DI 10.1007/s10841-010-9365-4 PG 14 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 814MX UT WOS:000294460700005 ER PT J AU Pour-Biazar, A Khan, M Wang, LH Park, YH Newchurch, M McNider, RT Liu, X Byun, DW Cameron, R AF Pour-Biazar, Arastoo Khan, Maudood Wang, Lihua Park, Yun-Hee Newchurch, Mike McNider, Richard T. Liu, Xiong Byun, Daewon W. Cameron, Robert TI Utilization of satellite observation of ozone and aerosols in providing initial and boundary condition for regional air quality studies SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MESOSCALE METEOROLOGICAL MODEL; NONLOCAL CLOSURE-MODEL; EMISSIONS; SYSTEM; LAYER AB To demonstrate the efficacy of satellite observations in the realization of the background and transboundary transport of pollution in regional air quality modeling practices, satellite observations of ozone and aerosol optical depth were incorporated in the EPA Models-3 Community Multiscale Air Quality (CMAQ) model (http://www.cmascenter.org). Observations from Ozone Monitoring Instrument (OMI) aboard NASA's Aura satellite and AOD products from the Moderate Resolution Imaging Spectroradiometer (MODIS) onboard Terra (EOS AM) and Aqua (EOS PM) satellites were used to specify initial and lateral boundary conditions (IC/BC) for a simulation that spanned over August 2006. The tools and techniques using the satellite data were tested in the context of current regulatory air quality modeling practices. Daily satellite observations were remapped onto the modeling domain and used as IC/BC for daily segments of a month-long simulation and the results were evaluated against surface and ozonesonde observations. Compared to the standard application of CMAQ, OMI O-3 profiles significantly improved model performance in the free troposphere and MODIS aerosol products substantially improved PM2.5 predictions in the boundary layer. The utilization of satellite data for BC helped in the realization of transboundary transport of pollution and was able to explain the recirculation of pollution from Northeast Corridor to the southeastern region. Ozone in the mid- to upper-troposphere was largely dominated by transport and thus benefited most from satellite provided BC. The ozone within the boundary layer was mostly affected by fast production/loss mechanisms that are impacted by surface emissions, chemistry and removal processes and was not impacted as much. A case study for August 18-22 demonstrated that model errors in the placement of a stationary front were the main reason for errors in PM2.5 predictions as the front acted as a boundary between high and low PM2.5 concentrations. C1 [Pour-Biazar, Arastoo; McNider, Richard T.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35899 USA. [Cameron, Robert] Bur Ocean Energy Management Regulat & Enforcement, Gulf Mexico OCS Reg, New Orleans, LA 70123 USA. [Khan, Maudood; Wang, Lihua] Univ Space Res Assoc, Natl Space Sci & Technol Ctr, Huntsville, AL 35806 USA. [Newchurch, Mike] Univ Alabama, Dept Atmospher Sci, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byun, Daewon W.] NOAA, Air Resources Lab, Silver Spring, MD 20910 USA. RP Pour-Biazar, A (reprint author), Univ Alabama, Ctr Earth Syst Sci, 320 Sparkman Dr, Huntsville, AL 35899 USA. EM biazar@nsstc.uah.edu RI Liu, Xiong/P-7186-2014 OI Liu, Xiong/0000-0003-2939-574X FU University of Alabama in Huntsville; Bureau of Ocean Energy Management, Regulation and Enforcement on Gulf of Mexico Issues; NASA FX This work was accomplished under partial support from Cooperative Agreement Between the University of Alabama in Huntsville and the Bureau of Ocean Energy Management, Regulation and Enforcement on Gulf of Mexico Issues, and the NASA Science Mission Directorate Applied Sciences Program. NR 50 TC 7 Z9 7 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 30 PY 2011 VL 116 AR D18309 DI 10.1029/2010JD015200 PG 32 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 828XG UT WOS:000295537000001 ER PT J AU Nittler, LR Starr, RD Weider, SZ McCoy, TJ Boynton, WV Ebel, DS Ernst, CM Evans, LG Goldsten, JO Hamara, DK Lawrence, DJ McNutt, RL Schlemm, CE Solomon, SC Sprague, AL AF Nittler, Larry R. Starr, Richard D. Weider, Shoshana Z. McCoy, Timothy J. Boynton, William V. Ebel, Denton S. Ernst, Carolyn M. Evans, Larry G. Goldsten, John O. Hamara, David K. Lawrence, David J. McNutt, Ralph L., Jr. Schlemm, Charles E., II Solomon, Sean C. Sprague, Ann L. TI The Major-Element Composition of Mercury's Surface from MESSENGER X-ray Spectrometry SO SCIENCE LA English DT Article ID IRON-SILICATE FRACTIONATION; CHEMICAL-COMPOSITION; MARINER-10; EVOLUTION; METEORITE; REGOLITH; ORIGIN; MANTLE; CRUST AB X-ray fluorescence spectra obtained by the MESSENGER spacecraft orbiting Mercury indicate that the planet's surface differs in composition from those of other terrestrial planets. Relatively high Mg/Si and low Al/Si and Ca/Si ratios rule out a lunarlike feldspar-rich crust. The sulfur abundance is at least 10 times higher than that of the silicate portion of Earth or the Moon, and this observation, together with a low surface Fe abundance, supports the view that Mercury formed from highly reduced precursor materials, perhaps akin to enstatite chondrite meteorites or anhydrous cometary dust particles. Low Fe and Ti abundances do not support the proposal that opaque oxides of these elements contribute substantially to Mercury's low and variable surface reflectance. C1 [Nittler, Larry R.; Weider, Shoshana Z.; Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [McCoy, Timothy J.] Smithsonian Inst, Washington, DC 20013 USA. [Boynton, William V.; Hamara, David K.; Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Ebel, Denton S.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Ernst, Carolyn M.; Goldsten, John O.; Lawrence, David J.; McNutt, Ralph L., Jr.; Schlemm, Charles E., II] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA. RP Nittler, LR (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM lnittler@ciw.edu RI Ernst, Carolyn/I-4902-2012; McNutt, Ralph/E-8006-2010; Lawrence, David/E-7463-2015; OI McNutt, Ralph/0000-0002-4722-9166; Lawrence, David/0000-0002-7696-6667; Weider, Shoshana/0000-0003-1034-909X FU NASA [NAS5-97271, NASW-00002] FX We thank the MESSENGER team for the development, cruise, orbit insertion, and Mercury orbital operations of the MESSENGER spacecraft. The NASA Discovery Program under contract NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington supports the MESSENGER mission to Mercury. Several of the authors are supported by NASA's MESSENGER Participating Scientist Program. NR 35 TC 158 Z9 158 U1 4 U2 47 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 30 PY 2011 VL 333 IS 6051 BP 1847 EP 1850 DI 10.1126/science.1211567 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 826PJ UT WOS:000295365800043 PM 21960623 ER PT J AU Peplowski, PN Evans, LG Hauck, SA McCoy, TJ Boynton, WV Gillis-Davis, JJ Ebel, DS Goldsten, JO Hamara, DK Lawrence, DJ McNutt, RL Nittler, LR Solomon, SC Rhodes, EA Sprague, AL Starr, RD Stockstill-Cahill, KR AF Peplowski, Patrick N. Evans, Larry G. Hauck, Steven A., II McCoy, Timothy J. Boynton, William V. Gillis-Davis, Jeffery J. Ebel, Denton S. Goldsten, John O. Hamara, David K. Lawrence, David J. McNutt, Ralph L., Jr. Nittler, Larry R. Solomon, Sean C. Rhodes, Edgar A. Sprague, Ann L. Starr, Richard D. Stockstill-Cahill, Karen R. TI Radioactive Elements on Mercury's Surface from MESSENGER: Implications for the Planet's Formation and Evolution SO SCIENCE LA English DT Article ID MARINER-10 AB The MESSENGER Gamma-Ray Spectrometer measured the average surface abundances of the radioactive elements potassium (K, 1150 +/- 220 parts per million), thorium (Th, 220 +/- 60 parts per billion), and uranium (U, 90 +/- 20 parts per billion) in Mercury's northern hemisphere. The abundance of the moderately volatile element K, relative to Th and U, is inconsistent with physical models for the formation of Mercury requiring extreme heating of the planet or its precursor materials, and supports formation from volatile-containing material comparable to chondritic meteorites. Abundances of K, Th, and U indicate that internal heat production has declined substantially since Mercury's formation, consistent with widespread volcanism shortly after the end of late heavy bombardment 3.8 billion years ago and limited, isolated volcanic activity since. C1 [Peplowski, Patrick N.; Goldsten, John O.; Lawrence, David J.; McNutt, Ralph L., Jr.; Rhodes, Edgar A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA. [Hauck, Steven A., II] Case Western Reserve Univ, Dept Geol Sci, Cleveland, OH 44106 USA. [McCoy, Timothy J.; Stockstill-Cahill, Karen R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Boynton, William V.; Hamara, David K.; Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Gillis-Davis, Jeffery J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Ebel, Denton S.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Nittler, Larry R.; Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. RP Peplowski, PN (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM patrick.peplowski@jhuapl.edu RI Lawrence, David/E-7463-2015; Hauck, Steven/A-7865-2008; Peplowski, Patrick/I-7254-2012; McNutt, Ralph/E-8006-2010 OI Lawrence, David/0000-0002-7696-6667; Hauck, Steven/0000-0001-8245-146X; Peplowski, Patrick/0000-0001-7154-8143; McNutt, Ralph/0000-0002-4722-9166 FU NASA [NAS5-97271, NASW-00002] FX We thank the entire MESSENGER team for their invaluable contributions to the development and operation of the spacecraft. The MESSENGER project is supported by the NASA Discovery Program under contract NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. Several authors are supported by NASA's MESSENGER Participating Scientist Program. All original data reported in this paper are archived by the NASA Planetary Data System. NR 26 TC 75 Z9 75 U1 3 U2 34 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 30 PY 2011 VL 333 IS 6051 BP 1850 EP 1852 DI 10.1126/science.1211576 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 826PJ UT WOS:000295365800044 PM 21960624 ER PT J AU Head, JW Chapman, CR Strom, RG Fassett, CI Denevi, BW Blewett, DT Ernst, CM Watters, TR Solomon, SC Murchie, SL Prockter, LM Chabot, NL Gillis-Davis, JJ Whitten, JL Goudge, TA Baker, DMH Hurwitz, DM Ostrach, LR Xiao, ZY Merline, WJ Kerber, L Dickson, JL Oberst, J Byrne, PK Klimczak, C Nittler, LR AF Head, James W. Chapman, Clark R. Strom, Robert G. Fassett, Caleb I. Denevi, Brett W. Blewett, David T. Ernst, Carolyn M. Watters, Thomas R. Solomon, Sean C. Murchie, Scott L. Prockter, Louise M. Chabot, Nancy L. Gillis-Davis, Jeffrey J. Whitten, Jennifer L. Goudge, Timothy A. Baker, David M. H. Hurwitz, Debra M. Ostrach, Lillian R. Xiao, Zhiyong Merline, William J. Kerber, Laura Dickson, James L. Oberst, Juergen Byrne, Paul K. Klimczak, Christian Nittler, Larry R. TI Flood Volcanism in the Northern High Latitudes of Mercury Revealed by MESSENGER SO SCIENCE LA English DT Article ID SMOOTH PLAINS; CALORIS BASIN; EMPLACEMENT; SURFACE; STRATIGRAPHY; EVOLUTION; FLYBY AB MESSENGER observations from Mercury orbit reveal that a large contiguous expanse of smooth plains covers much of Mercury's high northern latitudes and occupies more than 6% of the planet's surface area. These plains are smooth, embay other landforms, are distinct in color, show several flow features, and partially or completely bury impact craters, the sizes of which indicate plains thicknesses of more than 1 kilometer and multiple phases of emplacement. These characteristics, as well as associated features, interpreted to have formed by thermal erosion, indicate emplacement in a flood-basalt style, consistent with x-ray spectrometric data indicating surface compositions intermediate between those of basalts and komatiites. The plains formed after the Caloris impact basin, confirming that volcanism was a globally extensive process in Mercury's post-heavy bombardment era. C1 [Head, James W.; Fassett, Caleb I.; Whitten, Jennifer L.; Goudge, Timothy A.; Baker, David M. H.; Hurwitz, Debra M.; Kerber, Laura; Dickson, James L.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Chapman, Clark R.; Merline, William J.] SW Res Inst, Boulder, CO 80302 USA. [Strom, Robert G.; Xiao, Zhiyong] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Denevi, Brett W.; Blewett, David T.; Ernst, Carolyn M.; Murchie, Scott L.; Prockter, Louise M.; Chabot, Nancy L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Solomon, Sean C.; Byrne, Paul K.; Klimczak, Christian; Nittler, Larry R.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Gillis-Davis, Jeffrey J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Ostrach, Lillian R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. [Xiao, Zhiyong] China Univ Geosci, Fac Earth Sci, Wuhan 430074, Hubei, Peoples R China. [Oberst, Juergen] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. RP Head, JW (reprint author), Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. EM james_head@brown.edu RI Ernst, Carolyn/I-4902-2012; Blewett, David/I-4904-2012; Denevi, Brett/I-6502-2012; Murchie, Scott/E-8030-2015; Chabot, Nancy/F-5384-2015; OI Blewett, David/0000-0002-9241-6358; Denevi, Brett/0000-0001-7837-6663; Murchie, Scott/0000-0002-1616-8751; Chabot, Nancy/0000-0001-8628-3176; Fassett, Caleb/0000-0001-9155-3804 FU NASA [NAS5-97271, NASW-00002] FX We thank the MESSENGER team for development and flight operations. The NASA Discovery Program supports the MESSENGER mission through contract NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. NR 31 TC 100 Z9 100 U1 12 U2 50 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 30 PY 2011 VL 333 IS 6051 BP 1853 EP 1856 DI 10.1126/science.1211997 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 826PJ UT WOS:000295365800045 PM 21960625 ER PT J AU Blewett, DT Chabot, NL Denevi, BW Ernst, CM Head, JW Izenberg, NR Murchie, SL Solomon, SC Nittler, LR McCoy, TJ Xiao, ZY Baker, DMH Fassett, CI Braden, SE Oberst, J Scholten, F Preusker, F Hurwitz, DM AF Blewett, David T. Chabot, Nancy L. Denevi, Brett W. Ernst, Carolyn M. Head, James W. Izenberg, Noam R. Murchie, Scott L. Solomon, Sean C. Nittler, Larry R. McCoy, Timothy J. Xiao, Zhiyong Baker, David M. H. Fassett, Caleb I. Braden, Sarah E. Oberst, Juergen Scholten, Frank Preusker, Frank Hurwitz, Debra M. TI Hollows on Mercury: MESSENGER Evidence for Geologically Recent Volatile-Related Activity SO SCIENCE LA English DT Article ID VOLCANISM; FLYBY; EROS; CRATERS AB High-resolution images of Mercury's surface from orbit reveal that many bright deposits within impact craters exhibit fresh-appearing, irregular, shallow, rimless depressions. The depressions, or hollows, range from tens of meters to a few kilometers across, and many have high-reflectance interiors and halos. The host rocks, which are associated with crater central peaks, peak rings, floors, and walls, are interpreted to have been excavated from depth by the crater-forming process. The most likely formation mechanisms for the hollows involve recent loss of volatiles through some combination of sublimation, space weathering, outgassing, or pyroclastic volcanism. These features support the inference that Mercury's interior contains higher abundances of volatile materials than predicted by most scenarios for the formation of the solar system's innermost planet. C1 [Blewett, David T.; Chabot, Nancy L.; Denevi, Brett W.; Ernst, Carolyn M.; Izenberg, Noam R.; Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Head, James W.; Baker, David M. H.; Fassett, Caleb I.; Hurwitz, Debra M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Solomon, Sean C.; Nittler, Larry R.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [McCoy, Timothy J.] Smithsonian Inst, Washington, DC 20013 USA. [Xiao, Zhiyong] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Xiao, Zhiyong] China Univ Geosci, Fac Earth Sci, Wuhan 430074, Hubei, Peoples R China. [Braden, Sarah E.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. [Oberst, Juergen; Scholten, Frank; Preusker, Frank] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. RP Blewett, DT (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM david.blewett@jhuapl.edu RI Ernst, Carolyn/I-4902-2012; Blewett, David/I-4904-2012; Denevi, Brett/I-6502-2012; Murchie, Scott/E-8030-2015; Izenberg, Noam/F-3952-2015; Chabot, Nancy/F-5384-2015; OI Blewett, David/0000-0002-9241-6358; Denevi, Brett/0000-0001-7837-6663; Murchie, Scott/0000-0002-1616-8751; Izenberg, Noam/0000-0003-1629-6478; Chabot, Nancy/0000-0001-8628-3176; Fassett, Caleb/0000-0001-9155-3804 FU NASA; Participating Scientist grant FX This work was supported by NASA through the MESSENGER project and by a Participating Scientist grant to D. T. B. M. Robinson offered helpful comments on the manuscript. We thank N. Fontanella, S. Peel, E. Zhong, P. Pashai, and E. Coman for assistance with data processing and compilation. MESSENGER data are archived with the NASA Planetary Data System. NR 31 TC 40 Z9 40 U1 11 U2 42 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 30 PY 2011 VL 333 IS 6051 BP 1856 EP 1859 DI 10.1126/science.1211681 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 826PJ UT WOS:000295365800046 PM 21960626 ER PT J AU Punyasena, SW Dalling, JW Jaramillo, C Turner, BL AF Punyasena, Surangi W. Dalling, James W. Jaramillo, Carlos Turner, Benjamin L. TI Comment on "The Response of Vegetation on the Andean Flank in Western Amazonia to Pleistocene Climate Change" SO SCIENCE LA English DT Editorial Material ID MAXIMUM C1 [Punyasena, Surangi W.; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Dalling, James W.; Jaramillo, Carlos; Turner, Benjamin L.] Smithsonian Trop Res Inst, Ancon, Panama. RP Punyasena, SW (reprint author), Univ Illinois, Dept Plant Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA. EM punyasena@life.illinois.edu RI Turner, Benjamin/E-5940-2011; Punyasena, Surangi/C-9134-2011 OI Turner, Benjamin/0000-0002-6585-0722; NR 14 TC 13 Z9 14 U1 0 U2 7 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 30 PY 2011 VL 333 IS 6051 DI 10.1126/science.1207525 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 826PJ UT WOS:000295365800030 PM 21960612 ER PT J AU Alfoldi, J Di Palma, F Grabherr, M Williams, C Kong, LS Mauceli, E Russell, P Lowe, CB Glor, RE Jaffe, JD Ray, DA Boissinot, S Shedlock, AM Botka, C Castoe, TA Colbourne, JK Fujita, MK Moreno, RG ten Hallers, BF Haussler, D Heger, A Heiman, D Janes, DE Johnson, J de Jong, PJ Koriabine, MY Lara, M Novick, PA Organ, CL Peach, SE Poe, S Pollock, DD de Queiroz, K Sanger, T Searle, S Smith, JD Smith, Z Swofford, R Turner-Maier, J Wade, J Young, S Zadissa, A Edwards, SV Glenn, TC Schneider, CJ Losos, JB Lander, ES Breen, M Ponting, CP Lindblad-Toh, K AF Alfoeldi, Jessica Di Palma, Federica Grabherr, Manfred Williams, Christina Kong, Lesheng Mauceli, Evan Russell, Pamela Lowe, Craig B. Glor, Richard E. Jaffe, Jacob D. Ray, David A. Boissinot, Stephane Shedlock, Andrew M. Botka, Christopher Castoe, Todd A. Colbourne, John K. Fujita, Matthew K. Moreno, Ricardo Godinez ten Hallers, Boudewijn F. Haussler, David Heger, Andreas Heiman, David Janes, Daniel E. Johnson, Jeremy de Jong, Pieter J. Koriabine, Maxim Y. Lara, Marcia Novick, Peter A. Organ, Chris L. Peach, Sally E. Poe, Steven Pollock, David D. de Queiroz, Kevin Sanger, Thomas Searle, Steve Smith, Jeremy D. Smith, Zachary Swofford, Ross Turner-Maier, Jason Wade, Juli Young, Sarah Zadissa, Amonida Edwards, Scott V. Glenn, Travis C. Schneider, Christopher J. Losos, Jonathan B. Lander, Eric S. Breen, Matthew Ponting, Chris P. Lindblad-Toh, Kerstin TI The genome of the green anole lizard and a comparative analysis with birds and mammals SO NATURE LA English DT Article ID EVOLUTION; CHICKEN; MICROCHROMOSOMES; SAUROPSIDA; REPTILES; PROTEOME; FISH AB The evolution of the amniotic egg was one of the great evolutionary innovations in the history of life, freeing vertebrates from an obligatory connection to water and thus permitting the conquest of terrestrial environments(1). Among amniotes, genome sequences are available for mammals and birds(2-4), but not for non-avian reptiles. Here we report the genome sequence of the North American green anole lizard, Anolis carolinensis. We find that A. carolinensis microchromosomes are highly syntenic with chicken microchromosomes, yet do not exhibit the high GC and low repeat content that are characteristic of avian microchromosomes(2). Also, A. carolinensis mobile elements are very young and diverse-more so than in any other sequenced amniote genome. The GC content of this lizard genome is also unusual in its homogeneity, unlike the regionally variable GC content found in mammals and birds(5). We describe and assign sequence to the previously unknown A. carolinensis X chromosome. Comparative gene analysis shows that amniote egg proteins have evolved significantly more rapidly than other proteins. An anole phylogeny resolves basal branches to illuminate the history of their repeated adaptive radiations. C1 [Alfoeldi, Jessica; Di Palma, Federica; Grabherr, Manfred; Mauceli, Evan; Russell, Pamela; Jaffe, Jacob D.; Heiman, David; Johnson, Jeremy; Lara, Marcia; Peach, Sally E.; Swofford, Ross; Turner-Maier, Jason; Young, Sarah; Lander, Eric S.; Lindblad-Toh, Kerstin] Broad Inst MIT & Harvard, Cambridge, MA 02142 USA. [Williams, Christina; Breen, Matthew] N Carolina State Univ, Dept Mol Biomed Sci, Coll Vet Med, Raleigh, NC 27606 USA. [Kong, Lesheng; Fujita, Matthew K.; Heger, Andreas; Ponting, Chris P.] Univ Oxford, MRC, Funct Genom Unit, Dept Physiol Anat & Genet, Oxford OX1 3QX, England. [Lowe, Craig B.] Stanford Univ, Sch Med, Dept Dev Biol, Stanford, CA 94305 USA. [Glor, Richard E.] Univ Rochester, Rochester, NY 14607 USA. [Ray, David A.; Smith, Jeremy D.] Mississippi State Univ, Dept Biochem Mol Biol Entomol & Plant Pathol, Mississippi State, MS 39762 USA. [Boissinot, Stephane] CUNY, Dept Biol, Queens Coll, New York, NY 11367 USA. [Shedlock, Andrew M.] Coll Charleston, Dept Biol, Charleston, SC 29424 USA. [Shedlock, Andrew M.] Coll Charleston, Grad Program Marine Genom, Charleston, SC 29424 USA. [Botka, Christopher] Harvard Univ, Sch Med, Boston, MA 02115 USA. [Castoe, Todd A.; Pollock, David D.] Univ Colorado, Sch Med, Dept Biochem & Mol Genet, Aurora, CO 80045 USA. [Colbourne, John K.; Smith, Zachary] Indiana Univ, Ctr Genom & Bioinformat, Bloomington, IN 47405 USA. [Fujita, Matthew K.; Moreno, Ricardo Godinez; Janes, Daniel E.; Organ, Chris L.; Sanger, Thomas; Edwards, Scott V.; Losos, Jonathan B.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Fujita, Matthew K.; Moreno, Ricardo Godinez; Janes, Daniel E.; Organ, Chris L.; Sanger, Thomas; Edwards, Scott V.; Losos, Jonathan B.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [ten Hallers, Boudewijn F.; de Jong, Pieter J.; Koriabine, Maxim Y.] Childrens Hosp, Oakland Res Inst, Oakland, CA 94609 USA. [Haussler, David] Univ Calif Santa Cruz, Ctr Biomol Sci & Engn, Santa Cruz, CA 95064 USA. [Novick, Peter A.] Queensborough Community Coll, Dept Biol Sci & Geol, Bayside, NY 11364 USA. [Poe, Steven] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Pollock, David D.] Univ Colorado, Program Computat Biosci, Sch Med, Aurora, CO 80045 USA. [de Queiroz, Kevin] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Wade, Juli] Michigan State Univ, Dept Psychol, Program Neurosci, E Lansing, MI 48824 USA. [Wade, Juli] Michigan State Univ, Dept Zool, Program Neurosci, E Lansing, MI 48824 USA. [Glenn, Travis C.] Univ Georgia, Dept Environm Hlth Sci, Athens, GA 30602 USA. [Glenn, Travis C.] Univ Georgia, Georgia Genom Facil, Athens, GA 30602 USA. [Schneider, Christopher J.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Breen, Matthew] N Carolina State Univ, Ctr Comparat Med & Translat Res, Raleigh, NC 27695 USA. [Breen, Matthew] Univ N Carolina, Lineberger Comprehens Canc Ctr, Chapel Hill, NC 27514 USA. [Lindblad-Toh, Kerstin] Uppsala Univ, Dept Med Biochem & Microbiol, Sci Life Lab Uppsala, S-75123 Uppsala, Sweden. RP Alfoldi, J (reprint author), Broad Inst MIT & Harvard, Cambridge, MA 02142 USA. EM jalfoldi@broadinstitute.org; kersli@broadinstitute.org RI wade, juli/F-4993-2012; Glor, Richard/N-4656-2013; Colbourne, John/L-7748-2014; Kong, Lesheng/O-8933-2015; Pollock, David/M-4740-2016; OI Heger, Andreas/0000-0001-7720-0447; Glor, Richard/0000-0002-3359-1631; Colbourne, John/0000-0002-6966-2972; Kong, Lesheng/0000-0002-9225-3421; Pollock, David/0000-0002-7627-4214; Edwards, Scott/0000-0003-2535-6217; Ponting, Chris/0000-0003-0202-7816 FU National Human Genome Research Institute (NHGRI); NSF [DEB-0844624, DEB-0920892]; David and Lucile Packard Foundation FX Generation of the A. carolinensis sequence at the Broad Institute of MIT and Harvard was supported by grants from the National Human Genome Research Institute (NHGRI); S. P. and R. E. G. were supported by NSF grants DEB-0844624 and DEB-0920892. All sequence data was produced by the Genome Sequencing Platform of the Broad Institute. We would also like to thank the David and Lucile Packard Foundation for their early support of anole genomics, R. Andrews for her advice on lizard egg biology, C. Hickman and B. Temple and the Herpetology group at the University of Georgia's Savannah River Ecology Lab for assistance with sample collection, and L. Gaffney and L. Virnoche for assistance with figure and text preparation. NR 26 TC 231 Z9 236 U1 14 U2 108 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD SEP 29 PY 2011 VL 477 IS 7366 BP 587 EP 591 DI 10.1038/nature10390 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 825ZM UT WOS:000295320900039 PM 21881562 ER PT J AU Rapple, J AF Rapple, John TI DID BIG PHARMA CREATE THE FLU PANIC? SO NEW YORK REVIEW OF BOOKS LA English DT Editorial Material C1 Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Rapple, J (reprint author), Smithsonian Conservat Biol Inst, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU NEW YORK REVIEW PI NEW YORK PA 1755 BROADWAY, 5TH FLOOR, NEW YORK, NY 10019 USA SN 0028-7504 J9 NEW YORK REV BOOKS JI N. Y. Rev. Books PD SEP 29 PY 2011 VL 58 IS 14 BP 100 EP 100 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 820AT UT WOS:000294878600043 ER PT J AU Pohl, T Adams, CS Sadephpour, HR AF Pohl, T. Adams, C. S. Sadephpour, H. R. TI Cold Rydberg gases and ultra-cold plasmas SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Editorial Material ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; NEUTRAL PLASMA; ENERGY-TRANSFER; ATOMS; MOLECULES; BLOCKADE; STATES; STATISTICS; COLLOQUIUM; EXPANSION AB We briefly highlight recent developments in the complementary fields of cold Rydberg gases and ultra-cold plasmas and provide a short overview of the articles in this special issue. C1 [Pohl, T.] Max Planck Inst Complex Syst, D-01099 Dresden, Germany. [Adams, C. S.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Sadephpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Pohl, T (reprint author), Max Planck Inst Complex Syst, Nothnitzer Str 38, D-01099 Dresden, Germany. EM tpohl@pks.mpg.de RI Pohl, Thomas/B-5133-2013; Adams, Charles/C-8808-2015 OI Adams, Charles/0000-0001-5602-2741 NR 195 TC 17 Z9 17 U1 2 U2 21 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD SEP 28 PY 2011 VL 44 IS 18 SI SI AR 180201 DI 10.1088/0953-4075/44/18/180201 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 822HV UT WOS:000295035700001 ER PT J AU Rittenhouse, ST Mayle, M Schmelcher, P Sadeghpour, HR AF Rittenhouse, Seth T. Mayle, M. Schmelcher, P. Sadeghpour, H. R. TI Ultralong-range polyatomic Rydberg molecules formed by a polar perturber SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID ATOMS; BLOCKADE; DIMERS; STATES AB The internal electric field of a Rydberg atom electron can bind a polar molecule to form a giant ultralong-range stable polyatomic molecule. Such molecules not only share their properties with Rydberg atoms (such as long lifetimes and large sizes) but they also possess huge permanent electric dipole moments and in addition allow for coherent control of the polar molecule orientation. In this work, we include additional Rydberg manifolds which couple to the nearly degenerate set of Rydberg states employed in the previous work (S T Rittenhouse and H R Sadeghpour 2010 Phys. Rev. Lett. 104 243002). The coupling of a set of (n + 3) s Rydberg states with the n(l > 2) nearly degenerate Rydberg manifolds in alkali metal atoms leads to pronounced avoided crossings in the Born-Oppenheimer potentials. Ultimately, these avoided crossings enable the formation of the giant polyatomic Rydberg molecules with standard two-photon laser photoassociation techniques. C1 [Rittenhouse, Seth T.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Mayle, M.; Schmelcher, P.] Univ Hamburg, Zentrum Opt Quantentechnologien, D-22761 Hamburg, Germany. RP Rittenhouse, ST (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM srittenhouse@cfa.harvard.edu RI Mayle, Michael/A-2423-2009; Schmelcher, Peter/D-9592-2014 OI Schmelcher, Peter/0000-0002-2637-0937 FU German Academic Exchange Service (DAAD); NSF through ITAMP at Harvard University; Smithsonian Astrophysical Observatory FX The authors thank T V Tscherbul for help in calculating the Lambda-doublet molecule parameters used in this work. MM acknowledges financial support from the German Academic Exchange Service (DAAD). STR and HRS acknowledge financial support from the NSF through ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. NR 23 TC 12 Z9 12 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD SEP 28 PY 2011 VL 44 IS 18 SI SI AR 184005 DI 10.1088/0953-4075/44/18/184005 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 822HV UT WOS:000295035700006 ER PT J AU Oliveira, C Avelino, GS Abe, KT Mariguela, TC Benine, RC Orti, G Vari, RP Castro, RMCE AF Oliveira, Claudio Avelino, Gleisy S. Abe, Kelly T. Mariguela, Tatiane C. Benine, Ricardo C. Orti, Guillermo Vari, Richard P. Correa e Castro, Ricardo M. TI Phylogenetic relationships within the speciose family Characidae (Teleostei: Ostariophysi: Characiformes) based on multilocus analysis and extensive ingroup sampling SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID DNA-SEQUENCES; MIXED MODELS; FISHES; SELECTION; ACTINOPTERYGII; SUBSTITUTION; INFORMATION; SYSTEMATICS; BOOTSTRAP; INFERENCE AB Background: With nearly 1,100 species, the fish family Characidae represents more than half of the species of Characiformes, and is a key component of Neotropical freshwater ecosystems. The composition, phylogeny, and classification of Characidae is currently uncertain, despite significant efforts based on analysis of morphological and molecular data. No consensus about the monophyly of this group or its position within the order Characiformes has been reached, challenged by the fact that many key studies to date have non-overlapping taxonomic representation and focus only on subsets of this diversity. Results: In the present study we propose a new definition of the family Characidae and a hypothesis of relationships for the Characiformes based on phylogenetic analysis of DNA sequences of two mitochondrial and three nuclear genes (4,680 base pairs). The sequences were obtained from 211 samples representing 166 genera distributed among all 18 recognized families in the order Characiformes, all 14 recognized subfamilies in the Characidae, plus 56 of the genera so far considered incertae sedis in the Characidae. The phylogeny obtained is robust, with most lineages significantly supported by posterior probabilities in Bayesian analysis, and high bootstrap values from maximum likelihood and parsimony analyses. Conclusion: A monophyletic assemblage strongly supported in all our phylogenetic analysis is herein defined as the Characidae and includes the characiform species lacking a supraorbital bone and with a derived position of the emergence of the hyoid artery from the anterior ceratohyal. To recognize this and several other monophyletic groups within characiforms we propose changes in the limits of several families to facilitate future studies in the Characiformes and particularly the Characidae. This work presents a new phylogenetic framework for a speciose and morphologically diverse group of freshwater fishes of significant ecological and evolutionary importance across the Neotropics and portions of Africa. C1 [Oliveira, Claudio; Avelino, Gleisy S.; Abe, Kelly T.; Mariguela, Tatiane C.; Benine, Ricardo C.] Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Sao Paulo, Brazil. [Orti, Guillermo] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Vari, Richard P.] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC USA. [Correa e Castro, Ricardo M.] Univ Sao Paulo, FFCLRP, Dept Biol, LIRP, Sao Paulo, Brazil. RP Oliveira, C (reprint author), Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Sao Paulo, Brazil. EM claudio@ibb.unesp.br RI Oliveira, Claudio/D-7713-2012; Mariguela, Tatiane/K-2659-2012; Benine, Ricardo/B-2354-2013 OI Mariguela, Tatiane/0000-0002-9680-5887; FU FAPESP (Fundacao de Apoio a Pesquisa do Estado de Sao Paulo) [04/09219-6, 06/05744-4, 06/06749-0, 06/04551-8, 06/00545-3]; CNPq (Conselho Nacional de Desenvolvimento Cientifico e Tecnologico do Brasil) [309632/2007-2, 303854/2009-0]; U.S. National Science Foundation [DEB-0443470] FX We thank all the individuals and institutions who assisted us in the collection and identification of the specimens that served as the basis for this study, with special thanks to Mauro Nirchio, Universidad de Oriente, for the donation of tissue samples from Venezuela, Oris Sanjur, Smithsonian Tropical Research Institute, for the donation of tissue samples from Panama, Martha Valdez-Moreno, El Colegio de la Frontera Sur, for the donation of tissue samples from Mexico, Hernan Ortega, Museo de Historia Natural, Universidad Nacional Mayor de San Marcos, for the donation of tissue samples from Peru, the American Museum of Natural History for the donation of tissue samples of some Cheirodontinae, and Osvaldo T. Oyakawa, Janice Cunha, Caroline Doria, Riviane Garcez, and Gislene Torrente-Vilara for the donation of tissue samples from several regions within Brazil. We also thank Markus Alexandrou for his help with the Bayesian analyses. The manuscript was substantially improved with the help of the Associated Editor of BMC and three anonymous reviewers. This study is part of the FAPESP (Fundacao de Apoio a Pesquisa do Estado de Sao Paulo) Thematic Project "Phylogenetic relationships in the Characidae (Ostariophysi: Characiformes) (FAPESP grant number 04/09219-6, R. M. C. Castro, Principal Investigator). The first and eighth authors are CNPq (Conselho Nacional de Desenvolvimento Cientifico e Tecnologico do Brasil) researchers (CNPq grants numbers 309632/2007-2, 303854/2009-0, respectively). The second, third, fourth and fifth authors were supported by FAPESP (06/05744-4, 06/06749-0, 06/04551-8, 06/00545-3, respectively). A Research Coordination Network (RCN) grant from the U.S. National Science Foundation (DEB-0443470, PI = G. Orti) provided funding for a student exchange program supporting the fourth author. NR 79 TC 92 Z9 97 U1 0 U2 30 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD SEP 26 PY 2011 VL 11 AR 275 DI 10.1186/1471-2148-11-275 PG 25 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 831KD UT WOS:000295728400001 PM 21943181 ER PT J AU Kraft, NJB Comita, LS Chase, JM Sanders, NJ Swenson, NG Crist, TO Stegen, JC Vellend, M Boyle, B Anderson, MJ Cornell, HV Davies, KF Freestone, AL Inouye, BD Harrison, SP Myers, JA AF Kraft, Nathan J. B. Comita, Liza S. Chase, Jonathan M. Sanders, Nathan J. Swenson, Nathan G. Crist, Thomas O. Stegen, James C. Vellend, Mark Boyle, Brad Anderson, Marti J. Cornell, Howard V. Davies, Kendi F. Freestone, Amy L. Inouye, Brian D. Harrison, Susan P. Myers, Jonathan A. TI Disentangling the Drivers of beta Diversity Along Latitudinal and Elevational Gradients SO SCIENCE LA English DT Article ID GAMMA-DIVERSITY; COMMUNITY DIVERSITY; SPECIES-DIVERSITY; AMAZONIAN FOREST; ALPHA-DIVERSITY; TREE COMMUNITY; SCALE; ENVIRONMENTS; BIODIVERSITY; RICHNESS AB Understanding spatial variation in biodiversity along environmental gradients is a central theme in ecology. Differences in species compositional turnover among sites (beta diversity) occurring along gradients are often used to infer variation in the processes structuring communities. Here, we show that sampling alone predicts changes in beta diversity caused simply by changes in the sizes of species pools. For example, forest inventories sampled along latitudinal and elevational gradients show the well-documented pattern that beta diversity is higher in the tropics and at low elevations. However, after correcting for variation in pooled species richness (gamma diversity), these differences in beta diversity disappear. Therefore, there is no need to invoke differences in the mechanisms of community assembly in temperate versus tropical systems to explain these global-scale patterns of beta diversity. C1 [Kraft, Nathan J. B.; Vellend, Mark] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada. [Kraft, Nathan J. B.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Comita, Liza S.] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Chase, Jonathan M.; Myers, Jonathan A.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Sanders, Nathan J.] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. [Sanders, Nathan J.] Univ Copenhagen, Dept Biol, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. [Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. [Crist, Thomas O.] Miami Univ, Inst Environm & Sustainabil, Oxford, OH 45056 USA. [Crist, Thomas O.] Miami Univ, Dept Zool, Oxford, OH 45056 USA. [Stegen, James C.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. [Stegen, James C.] Pacific NW Natl Lab, Fundamental & Computat Sci Directorate, Div Biol Sci, Richland, WA 99352 USA. [Vellend, Mark] Univ Sherbrooke, Dept Biol, Sherbrooke, PQ J1K 2R1, Canada. [Boyle, Brad] Univ Arizona, Dept Ecol & Evolut, Tucson, AZ 85719 USA. [Anderson, Marti J.] Massey Univ, New Zealand Inst Adv Study, Auckland 0745, New Zealand. [Cornell, Howard V.; Harrison, Susan P.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Davies, Kendi F.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Freestone, Amy L.] Temple Univ, Dept Biol, Philadelphia, PA 19122 USA. [Inouye, Brian D.] Florida State Univ, Tallahassee, FL 32306 USA. RP Kraft, NJB (reprint author), Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada. EM nkraft@biodiversity.ubc.ca RI Swenson, Nathan/A-3514-2012; Kraft, Nathan/A-2817-2012; Sanders, Nathan/A-6945-2009; Stegen, James/Q-3078-2016; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 OI Swenson, Nathan/0000-0003-3819-9767; Kraft, Nathan/0000-0001-8867-7806; Sanders, Nathan/0000-0001-6220-6731; Stegen, James/0000-0001-9135-7424; FU National Center for Ecological Analysis and Synthesis (NCEAS); NSF [EF-0553768, DBI-0906005]; University of California, Santa Barbara; state of California; National Science and Engineering Research Council of Canada; U.S. Department of Energy [DE-FG02-08ER64510] FX We are grateful to A. H. Gentry, the Missouri Botanical Garden, and numerous additional collectors who contributed to the latitudinal data set. The data sets are available in the original publications or electronically from SALVIAS (www.salvias.net). This work was conducted as part of the Gradients of beta-diversity Working Group supported by the National Center for Ecological Analysis and Synthesis (NCEAS), a center funded by NSF (grant EF-0553768); the University of California, Santa Barbara; and the state of California. N.J.B.K. was supported by the National Science and Engineering Research Council of Canada CREATE Training Program in Biodiversity Research. L. S. C. was supported by an NCEAS postdoctoral fellowship. N.J.S. was supported by U.S. Department of Energy Program for Ecosystem Research DE-FG02-08ER64510. J.C.S. was supported by an NSF Postdoctoral Fellowship in Bioinformatics (DBI-0906005). NR 34 TC 180 Z9 191 U1 29 U2 337 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 23 PY 2011 VL 333 IS 6050 BP 1755 EP 1758 DI 10.1126/science.1208584 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 823KQ UT WOS:000295121500045 PM 21940897 ER PT J AU Ruger, N Berger, U Hubbell, SP Vieilledent, G Condit, R AF Rueger, Nadja Berger, Uta Hubbell, Stephen P. Vieilledent, Ghislain Condit, Richard TI Growth Strategies of Tropical Tree Species: Disentangling Light and Size Effects SO PLOS ONE LA English DT Article ID RAIN-FOREST COMMUNITY; MOIST FOREST; NEIGHBORHOOD ANALYSIS; RELATIVE IMPORTANCE; SHADE TOLERANCE; SAPLING GROWTH; CANOPY GAPS; MORTALITY; RESPONSES; RECRUITMENT AB An understanding of the drivers of tree growth at the species level is required to predict likely changes of carbon stocks and biodiversity when environmental conditions change. Especially in species-rich tropical forests, it is largely unknown how species differ in their response of growth to resource availability and individual size. We use a hierarchical Bayesian approach to quantify the impact of light availability and tree diameter on growth of 274 woody species in a 50-ha long-term forest census plot in Barro Colorado Island, Panama. Light reaching each individual tree was estimated from yearly vertical censuses of canopy density. The hierarchical Bayesian approach allowed accounting for different sources of error, such as negative growth observations, and including rare species correctly weighted by their abundance. All species grew faster at higher light. Exponents of a power function relating growth to light were mostly between 0 and 1. This indicates that nearly all species exhibit a decelerating increase of growth with light. In contrast, estimated growth rates at standardized conditions (5 cm dbh, 5% light) varied over a 9-fold range and reflect strong growth-strategy differentiation between the species. As a consequence, growth rankings of the species at low (2%) and high light (20%) were highly correlated. Rare species tended to grow faster and showed a greater sensitivity to light than abundant species. Overall, tree size was less important for growth than light and about half the species were predicted to grow faster in diameter when bigger or smaller, respectively. Together light availability and tree diameter only explained on average 12% of the variation in growth rates. Thus, other factors such as soil characteristics, herbivory, or pathogens may contribute considerably to shaping tree growth in the tropics. C1 [Rueger, Nadja] Univ Leipzig, Spezielle Botan & Funktionelle Biodiversitat, Leipzig, Germany. [Berger, Uta] Tech Univ Dresden, Inst Waldwachstum & Forstliche Informat, Dresden, Tharandt, Germany. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA. [Hubbell, Stephen P.; Condit, Richard] Ctr Trop Forest Sci, Smithsonian Trop Res Inst, Washington, DE USA. [Vieilledent, Ghislain] Forest Ecosystem Goods & Serv, UR105, Montpellier, France. [Vieilledent, Ghislain] DRP Foret & Biodiversite, Antananarivo, Madagascar. RP Ruger, N (reprint author), Univ Leipzig, Spezielle Botan & Funktionelle Biodiversitat, Leipzig, Germany. EM nadja.rueger@uni-leipzig.de RI Vieilledent, Ghislain/D-8323-2011; Ruger, Nadja/J-6393-2015 OI Vieilledent, Ghislain/0000-0002-1685-4997; Ruger, Nadja/0000-0003-2371-4172 FU Deutsche Forschungsgemeinschaft (DFG) [RU 1536/2-1]; Center for Tropical Forest Science (CTFS); United States National Science Foundation; John D. and Catherine T. McArthur Foundation; Smithsonian Tropical Research Institute FX NR was partially funded by research grants from Deutsche Forschungsgemeinschaft (DFG) (RU 1536/2-1) and the Center for Tropical Forest Science (CTFS). The Barro Colorado Island plot has been made possible through the support of the United States National Science Foundation, the John D. and Catherine T. McArthur Foundation and the Smithsonian Tropical Research Institute. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 74 TC 28 Z9 30 U1 3 U2 55 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 22 PY 2011 VL 6 IS 9 AR e25330 DI 10.1371/journal.pone.0025330 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 825IJ UT WOS:000295265100089 PM 21966498 ER PT J AU Fabbiano, G Wang, JF Elvis, M Risaliti, G AF Fabbiano, G. Wang, Junfeng Elvis, M. Risaliti, G. TI A close nuclear black-hole pair in the spiral galaxy NGC 3393 SO NATURE LA English DT Article ID ACTIVE GALACTIC NUCLEI; X-RAY SOURCE; SYSTEM; REFLECTION; DISCOVERY; BINARIES; NGC-3393; SUZAKU AB The current picture of galaxy evolution(1) advocates co-evolution of galaxies and their nuclear massive black holes, through accretion and galactic merging. Pairs of quasars, each with a massive black hole at the centre of its galaxy, have separations of 6,000 to 300,000 light years (refs 2 and 3; 1 parsec = 3.26 light years) and exemplify the first stages of this gravitational interaction. The final stages of the black-hole merging process, through binary black holes and final collapse into a single black hole with gravitational wave emission, are consistent with the sub-light-year separation inferred from the optical spectra(4) and light-variability(5) of two such quasars. The double active nuclei of a few nearby galaxies with disrupted morphology and intense star formation (such as NGC 6240 with a separation(6) of about 2,600 light years and Mrk 463 with a separation(7) of about 13,000 light years between the nuclei) demonstrate the importance of major mergers of equal-mass spiral galaxies in this evolution; such mergers lead to an elliptical galaxy(8), as in the case of the double-radio-nucleus elliptical galaxy 0402+379 (with a separation of about 24 light years between the nuclei)(9). Minor mergers of a spiral galaxy with a smaller companion should be a more common occurrence, evolving into spiral galaxies with active massive black-hole pairs(10), but have hitherto not been seen. Here we report the presence of two active massive black holes, separated by about 490 light years, in the Seyfert(11) galaxy NGC 3393 (50 Mpc, about 160 million light years). The regular spiral morphology and predominantly old circum-nuclear stellar population(12) of this galaxy, and the closeness of the black holes embedded in the bulge, provide a hitherto missing observational point to the study of galaxy/black hole evolution. Comparison of our observations with current theoretical models of mergers suggests that they are the result of minor merger evolution(10). C1 [Fabbiano, G.; Wang, Junfeng; Elvis, M.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Risaliti, G.] INAF Arcetri, I-50125 Florence, Italy. RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA. EM gfabbiano@cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009; OI Risaliti, Guido/0000-0002-3556-977X FU NASA FX This work was supported by a NASA grant (with Principal Investigator J.W.). We thank P. Gandhi for discussions on the 13 mu m observations. We used the NASA ADS and NED services. This work includes archival Chandra and Hubble Space Telescope data. We acknowledge discussions with T. Di Matteo and L. Mayer at the Aspen Center for Physics 2011 Summer Program. NR 30 TC 54 Z9 54 U1 1 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD SEP 22 PY 2011 VL 477 IS 7365 BP 431 EP 434 DI 10.1038/nature10364 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 822WH UT WOS:000295080500033 PM 21881560 ER PT J AU Guglielmino, M Penna, V Capogrosso-Sansone, B AF Guglielmino, M. Penna, V. Capogrosso-Sansone, B. TI Ising antiferromagnet with ultracold bosonic mixtures confined in a harmonic trap SO PHYSICAL REVIEW A LA English DT Article ID ATOMIC MOTT INSULATOR; OPTICAL LATTICE AB We present accurate results based on quantum Monte Carlo simulations of two-component bosonic systems on a square lattice and in the presence of an external harmonic confinement. Starting from hopping parameters and interaction strengths which stabilize the Ising antiferromagnetic phase in the homogeneous case and at half-integer filling factor, we study how the presence of the harmonic confinement challenges the realization of such a phase. We consider realistic trapping frequencies and number of particles, and we establish under which conditions, i.e., total number of particles and population imbalance, the antiferromagnetic phase can be observed in the trap. C1 [Guglielmino, M.; Penna, V.] Politecn Torino, Dipartimento Fis, I-10129 Turin, Italy. [Guglielmino, M.; Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Penna, V.] Politecn Torino, CNISM Unita Ric, I-10129 Turin, Italy. RP Guglielmino, M (reprint author), Politecn Torino, Dipartimento Fis, Corso Duca Abruzzi 24, I-10129 Turin, Italy. FU Institute for Atomic, Molecular and Optical Physics (ITAMP) FX We would like to thank F. Minardi, S. Soyler, and S. Kuhr for fruitful discussions. This work was supported by the Institute for Atomic, Molecular and Optical Physics (ITAMP). MG wants to thank ITAMP for warm hospitality and financial support. NR 26 TC 9 Z9 9 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD SEP 20 PY 2011 VL 84 IS 3 AR 031603 DI 10.1103/PhysRevA.84.031603 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 822KM UT WOS:000295044600004 ER PT J AU Artigau, E Lafreniere, D Doyon, R Liu, M Dupuy, TJ Albert, L Gagne, J Malo, L Gratadour, D AF Artigau, Etienne Lafreniere, David Doyon, Rene Liu, Michael Dupuy, Trent J. Albert, Loic Gagne, Jonathan Malo, Lison Gratadour, Damien TI DISCOVERY OF TWO L AND T BINARIES WITH WIDE SEPARATIONS AND PECULIAR PHOTOMETRIC PROPERTIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; stars: individual (SIMP J1619275+031350AB, SIMP J1501530-013506AB); stars: low-mass ID STAR ADAPTIVE OPTICS; YOUNG BROWN DWARFS; DIGITAL SKY SURVEY; INFRARED SPECTRAL CLASSIFICATION; SOLAR-TYPE STARS; LOW-MASS STARS; L/T TRANSITION; RESOLVED SPECTROSCOPY; TAURI PHASE; FILTER SET AB We present spatially resolved photometric and spectroscopic observations of two wide brown dwarf binaries uncovered by the Sondage Infrarouge de Mouvement Propre (SIMP) near-infrared proper motion survey. The first pair (SIMP J1619275+031350AB) has a separation of 0.'' 691 (15.2 AU) and components T2.5+T4.0, at the cooler end of the ill-understood J-band brightening. The system is unusual in that the earlier-type primary is bluer in J - K-s than the later-type secondary, whereas the reverse is expected for binaries in the late-L to T dwarf range. This remarkable color reversal can possibly be explained by very different cloud properties between the two components. The second pair (SIMP J1501530-013506AB) consists of an L4.5+ L5.5 (separation 0.'' 96, 30-47 AU) with a surprisingly large flux ratio (Delta J = 1.79 mag) considering the similar spectral types of its components. The large flux ratio could be explained if the primary is itself an equal-luminosity binary, which would make it one of the first known triple brown dwarf systems. Adaptive optics observations could not confirm this hypothesis, but it remains a likely one, which may be verified by high-resolution near-infrared spectroscopy. These two systems add to the handful of known brown dwarf binaries amenable to resolved spectroscopy without the aid of adaptive optics and constitute prime targets to test brown dwarf atmosphere models. C1 [Artigau, Etienne; Lafreniere, David; Doyon, Rene; Albert, Loic; Gagne, Jonathan; Malo, Lison] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Artigau, Etienne; Lafreniere, David; Doyon, Rene; Albert, Loic; Gagne, Jonathan; Malo, Lison] Univ Montreal, Observ Mt Megant, Montreal, PQ H3C 3J7, Canada. [Liu, Michael] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Albert, Loic] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Gratadour, Damien] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92195 Meudon, France. RP Artigau, E (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM artigau@astro.umontreal.ca; mliu@ifa.hawaii.edu OI Gagne, Jonathan/0000-0002-2592-9612; Lafreniere, David/0000-0002-6780-4252 FU Natural Sciences and Engineering Research Council, Canada; Fonds Quebecois de la Recherche sur la Nature et les Technologies; Canada Foundation for Innovation; National Aeronautics and Space Administration; National Science Foundation; W. M. Keck Foundation FX The authors thank Marcel Bergman, the Gemini queue observer who took the SIMP J1501-0135 and SIMP J1619+0313 observations, for notifying them that two of the SIMP brown dwarf candidates "looked like doubles" in GNIRS acquisition images. The authors thank Mike Shara for his leadership and financial support in enabling the CPAPIR observing campaign on the 1.5 m CTIO telescope. Our special thanks to Alberto Pasten and Claudio Aguilera for carrying out the SIMP observations and to Philippe Vallee for managing the SIMP data. This work was supported in part through grants from the Natural Sciences and Engineering Research Council, Canada, and from Fonds Quebecois de la Recherche sur la Nature et les Technologies. CPAPIR was built through a grant from the Canada Foundation for Innovation. This research has benefited from the M, L, and T dwarf compendium housed at DwarfArchives.org and maintained by Chris Gelino, Davy Kirkpatrick, and Adam Burgasser. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Based on observations obtained at the Gemini Observatory (program ID: GS-2007A-Q-28 and GN-2008A-Q-57), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 71 TC 10 Z9 10 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 48 DI 10.1088/0004-637X/739/1/48 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700048 ER PT J AU Brammer, GB Whitaker, KE van Dokkum, PG Marchesini, D Franx, M Kriek, M Labbe, I Lee, KS Muzzin, A Quadri, RF Rudnick, G Williams, R AF Brammer, Gabriel B. Whitaker, K. E. van Dokkum, P. G. Marchesini, D. Franx, M. Kriek, M. Labbe, I. Lee, K. -S. Muzzin, A. Quadri, R. F. Rudnick, G. Williams, R. TI THE NUMBER DENSITY AND MASS DENSITY OF STAR-FORMING AND QUIESCENT GALAXIES AT 0.4 <= z <= 2.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID MEDIUM-BAND SURVEY; DEEP-FIELD-SOUTH; STELLAR POPULATION SYNTHESIS; COLOR-MAGNITUDE DISTRIBUTION; SPECTRAL ENERGY-DISTRIBUTION; K-SELECTED GALAXIES; YALE-CHILE MUSYC; LUMINOSITY FUNCTION; RED-SEQUENCE; MULTIWAVELENGTH SURVEY AB We study the buildup of the bimodal galaxy population using the NEWFIRM Medium-Band Survey, which provides excellent redshifts and well-sampled spectral energy distributions of approximate to 27,000 galaxies with K < 22.8 at 0.4 < z < 2.2. We first show that star-forming galaxies and quiescent galaxies can be robustly separated with a two-color criterion over this entire redshift range. We then study the evolution of the number density and mass density of quiescent and star-forming galaxies, extending the results of the COMBO-17, DEEP2, and other surveys to z = 2.2. The mass density of quiescent galaxies with M greater than or similar to 3 x 10(10) M-circle dot increases by a factor of similar to 10 from z similar to 2 to the present day, whereas the mass density in star-forming galaxies is flat or decreases over the same time period. Modest mass growth by a factor of similar to 2 of individual quiescent galaxies can explain roughly half of the strong density evolution at masses > 10(11) M-circle dot, due to the steepness of the exponential tail of the mass function. The rest of the density evolution of massive, quiescent galaxies is likely due to transformation (e. g., quenching) of the massive star-forming population, a conclusion which is consistent with the density evolution we observe for the star-forming galaxies themselves, which is flat or decreasing with cosmic time. Modest mass growth does not explain the evolution of less massive quiescent galaxies (similar to 10(10.5) M-circle dot), which show a similarly steep increase in their number densities. The less massive quiescent galaxies are therefore continuously formed by transforming galaxies from the star-forming population. C1 [Brammer, Gabriel B.] European So Observ, Santiago, Chile. [Brammer, Gabriel B.; Whitaker, K. E.; van Dokkum, P. G.; Lee, K. -S.; Muzzin, A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Marchesini, D.] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Franx, M.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kriek, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kriek, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Labbe, I.; Quadri, R. F.; Williams, R.] Carnegie Observ, Pasadena, CA 91101 USA. [Rudnick, G.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. RP Brammer, GB (reprint author), European So Observ, Alonso de Cordova 3107,Casilla 19001, Santiago, Chile. EM gbrammer@eso.org FU NSF [AST-0449678, AST-0807974] FX We thank the anonymous referee for helpful comments and suggestions that improved the manuscript. Support from NSF grants AST-0449678 and AST-0807974 is gratefully acknowledged. This research has made extensive use of the IDL Astronomy Library (http://idlastro.gsfc.nasa.gov/) and NASA's Astrophysics Data System Bibliographic Services. NR 93 TC 162 Z9 162 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 24 DI 10.1088/0004-637X/739/1/24 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700024 ER PT J AU Chornock, R Filippenko, AV Li, W Marion, GH Foley, RJ Modjaz, M Rafelski, M Becker, GD de Vries, WH Garnavich, P Jorgenson, RA Lynch, DK Malec, AL Moran, EC Murphy, MT Rudy, RJ Russell, RW Silverman, JM Steele, TN Stockton, A Wolfe, AM Woodward, CE AF Chornock, R. Filippenko, A. V. Li, W. Marion, G. H. Foley, R. J. Modjaz, M. Rafelski, M. Becker, G. D. de Vries, W. H. Garnavich, P. Jorgenson, R. A. Lynch, D. K. Malec, A. L. Moran, E. C. Murphy, M. T. Rudy, R. J. Russell, R. W. Silverman, J. M. Steele, T. N. Stockton, A. Wolfe, A. M. Woodward, C. E. TI THE TRANSITIONAL STRIPPED-ENVELOPE SN 2008ax: SPECTRAL EVOLUTION AND EVIDENCE FOR LARGE ASPHERICITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE polarization; supernovae: general; supernovae: individual (SN 2008ax) ID CORE-COLLAPSE SUPERNOVAE; DIFFUSE INTERSTELLAR BANDS; NEAR-INFRARED SPECTRA; REMNANT CASSIOPEIA-A; GAMMA-RAY BURSTS; II-P SUPERNOVA; IB SUPERNOVAE; X-RAY; OPTICAL SPECTROSCOPY; IA SUPERNOVA AB Supernova (SN) 2008ax in NGC 4490 was discovered within hours after shock breakout, presenting the rare opportunity to study a core-collapse SN beginning with the initial envelope-cooling phase immediately following shock breakout. We present an extensive sequence of optical and near-infrared spectra, as well as three epochs of optical spectropolarimetry. Our initial spectra, taken two days after shock breakout, are dominated by hydrogen Balmer lines at high velocity. However, by maximum light, He I lines dominated the optical and near-infrared spectra, which closely resembled those of normal Type Ib supernovae (SNe Ib) such as SN 1999ex. This spectroscopic transition defines Type IIb SNe, but the strong similarity of SN 2008ax to normal SNe Ib beginning near maximum light, including an absorption feature near 6270 angstrom due to H alpha at high velocities, suggests that many objects classified as SNe Ib in the literature may have ejected similar amounts of hydrogen as SN 2008ax, roughly a few x 0.01 M-circle dot. Only the unusually early discovery of SN 2008ax allowed us to observe the spectroscopic signatures of the hydrogen-rich outer ejecta. Early-time spectropolarimetry (six and nine days after shock breakout) revealed strong line polarization modulations of 3.4% across H alpha, indicating the presence of large asphericities in the outer ejecta and possibly that the spectrum of SN 2008ax could be dependent on the viewing angle. After removal of interstellar polarization, the continuum shares a common polarization angle with the hydrogen, helium, and oxygen lines, while the calcium and iron absorptions are oriented at different angles. This is clear evidence of deviations from axisymmetry even in the outer ejecta. Intrinsic continuum polarization of 0.64% only nine days after shock breakout shows that the outer layers of the ejecta were quite aspherical. A single epoch of late-time spectropolarimetry as well as the shapes of the nebular line profiles demonstrate that asphericities extended from the outermost layers all the way down to the center of this core-collapse SN. SN 2008ax may in some ways be an extragalactic analog of the explosion giving rise to Cassiopeia A, which has recently been determined to be a remnant of an SN IIb. C1 [Chornock, R.; Filippenko, A. V.; Li, W.; Modjaz, M.; Silverman, J. M.; Steele, T. N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chornock, R.; Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marion, G. H.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA. [Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Rafelski, M.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Rafelski, M.; Wolfe, A. M.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Becker, G. D.] Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Becker, G. D.; Jorgenson, R. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [de Vries, W. H.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [de Vries, W. H.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Garnavich, P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Lynch, D. K.; Rudy, R. J.; Russell, R. W.] Aerosp Corp, Los Angeles, CA 90009 USA. [Malec, A. L.; Murphy, M. T.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Moran, E. C.] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Stockton, A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Woodward, C. E.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. RP Chornock, R (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM rchornock@cfa.harvard.edu RI Murphy, Michael/B-8832-2008 OI Murphy, Michael/0000-0002-7040-5498 FU W. M. Keck Foundation; National Aeronautics and Space Administration, Science Mission Directorate [NNX-08AE38A]; NSF [AST-0607485, AST-0908886]; TABASGO Foundation; Miller Institute for Basic Research in Science; Aerospace Corporation FX We acknowledge M. Ganeshalingam, C. V. Griffith, J. Hodge, K. Merriman, R. Mostardi, D. Poznanski, and X. Wang for assistance with some of the observations. We would also like to thank the observers of the Lick AGN Monitoring Project 2008 (LAMP) for obtaining some of these SN 2008ax spectra during the nightly SN observations, in particular A. J. Barth, V. N. Bennert, M. C. Bentz, G. Canalizo, K. D. Hiner, C. E. Thornton, J. L. Walsh, and J.-H. Woo. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration; it was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. We also would like to thank the expert assistance of the Keck and Lick staffs in making these observations possible. Data for this manuscript were obtained by Visiting Astronomers at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement No. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. We thank Alan Tokunaga and the IRTF staff for their help performing timely observations. A.V.F.'s supernova research group at UC Berkeley has been supported by NSF grants AST-0607485 and AST-0908886, as well as by the TABASGO Foundation. M. M. is supported by a fellowship from the Miller Institute for Basic Research in Science. D. K. L., R. J. R., and R. W. R. were supported by The Aerospace Corporation's Independent Research and Development program. NR 154 TC 35 Z9 35 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 41 DI 10.1088/0004-637X/739/1/41 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700041 ER PT J AU Dunkley, J Hlozek, R Sievers, J Acquaviva, V Ade, PAR Aguirre, P Amiri, M Appel, JW Barrientos, LF Battistelli, ES Bond, JR Brown, B Burger, B Chervenak, J Das, S Devlin, MJ Dicker, SR Doriese, WB Dunner, R Essinger-Hileman, T Fisher, RP Fowler, JW Hajian, A Halpern, M Hasselfield, M Hernandez-Monteagudo, C Hilton, GC Hilton, M Hincks, AD Huffenberger, KM Hughes, DH Hughes, JP Infante, L Irwin, KD Juin, JB Kaul, M Klein, J Kosowsky, A Lau, JM Limon, M Lin, YT Lupton, RH Marriage, TA Marsden, D Mauskopf, P Menanteau, F Moodley, K Moseley, H Netterfield, CB Niemack, MD Nolta, MR Page, LA Parker, L Partridge, B Reid, B Sehgal, N Sherwin, B Spergel, DN Staggs, ST Swetz, DS Switzer, ER Thornton, R Trac, H Tucker, C Warne, R Wollack, E Zhao, Y AF Dunkley, J. Hlozek, R. Sievers, J. Acquaviva, V. Ade, P. A. R. Aguirre, P. Amiri, M. Appel, J. W. Barrientos, L. F. Battistelli, E. S. Bond, J. R. Brown, B. Burger, B. Chervenak, J. Das, S. Devlin, M. J. Dicker, S. R. Doriese, W. Bertrand Duenner, R. Essinger-Hileman, T. Fisher, R. P. Fowler, J. W. Hajian, A. Halpern, M. Hasselfield, M. Hernandez-Monteagudo, C. Hilton, G. C. Hilton, M. Hincks, A. D. Huffenberger, K. M. Hughes, D. H. Hughes, J. P. Infante, L. Irwin, K. D. Juin, J. B. Kaul, M. Klein, J. Kosowsky, A. Lau, J. M. Limon, M. Lin, Y-T. Lupton, R. H. Marriage, T. A. Marsden, D. Mauskopf, P. Menanteau, F. Moodley, K. Moseley, H. Netterfield, C. B. Niemack, M. D. Nolta, M. R. Page, L. A. Parker, L. Partridge, B. Reid, B. Sehgal, N. Sherwin, B. Spergel, D. N. Staggs, S. T. Swetz, D. S. Switzer, E. R. Thornton, R. Trac, H. Tucker, C. Warne, R. Wollack, E. Zhao, Y. TI THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGICAL PARAMETERS FROM THE 2008 POWER SPECTRUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmological parameters; cosmology: observations ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND ANISOTROPIES; PRIMORDIAL HELIUM ABUNDANCE; BIG-BANG NUCLEOSYNTHESIS; MASSIVE GALAXY CLUSTERS; STAR-FORMING GALAXIES; SOUTH-POLE TELESCOPE; INFLATIONARY UNIVERSE; HUBBLE CONSTANT; OBSERVED GROWTH AB We present cosmological parameters derived from the angular power spectrum of the cosmic microwave background (CMB) radiation observed at 148 GHz and 218 GHz over 296 deg(2) with the Atacama Cosmology Telescope (ACT) during its 2008 season. ACT measures fluctuations at scales 500 < l < 10,000. We fit a model for the lensed CMB, Sunyaev-Zel'dovich (SZ), and foreground contribution to the 148 GHz and 218 GHz power spectra, including thermal and kinetic SZ, Poisson power from radio and infrared point sources, and clustered power from infrared point sources. At l = 3000, about half the power at 148 GHz comes from primary CMB after masking bright radio sources. The power from thermal and kinetic SZ is estimated to be B-3000 = 6.8 +/- 2.9 mu K-2, where B-l = l (l + 1) C-l/2 pi. The IR Poisson power at 148 GHz is B-3000 = 7.8 +/- 0.7 mu K-2 (Cl = 5.5 +/- 0.5 nK(2)), and a clustered IR component is required with B-3000 = 4.6 +/- 0.9 mu K-2, assuming an analytic model for its power spectrum shape. At 218 GHz only about 15% of the power, approximately 27 mu K-2, is CMB anisotropy at l = 3000. The remaining 85% is attributed to IR sources (approximately 50% Poisson and 35% clustered), with spectral index alpha = 3.69 +/- 0.14 for flux scaling as S(v) proportional to v(alpha). We estimate primary cosmological parameters from the less contaminated 148 GHz spectrum, marginalizing over SZ and source power. The Lambda CDM cosmological model is a good fit to the data (chi(2)/dof = 29/46), and Lambda CDM parameters estimated from ACT+Wilkinson Microwave Anisotropy Probe (WMAP) are consistent with the seven-year WMAP limits, with scale invariant ns = 1 excluded at 99.7% confidence level (CL) (3 sigma). A model with no CMB lensing is disfavored at 2.8 sigma. By measuring the third to seventh acoustic peaks, and probing the Silk damping regime, the ACT data improve limits on cosmological parameters that affect the small-scale CMB power. The ACT data combined with WMAP give a 6 sigma detection of primordial helium, with Y-P = 0.313 +/- 0.044, and a 4 sigma detection of relativistic species, assumed to be neutrinos, with N-eff = 5.3 +/- 1.3 (4.6 +/- 0.8 with BAO+H-0 data). From the CMB alone the running of the spectral index is constrained to be dn(s)/d ln k = - 0.034 +/- 0.018, the limit on the tensor-to-scalar ratio is r < 0.25 (95% CL), and the possible contribution of Nambu cosmic strings to the power spectrum is constrained to string tension G mu < 1.6 x 10(-7) ( 95% CL). C1 [Dunkley, J.; Hlozek, R.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Dunkley, J.; Appel, J. W.; Das, S.; Essinger-Hileman, T.; Fisher, R. P.; Fowler, J. W.; Hajian, A.; Hincks, A. D.; Lau, J. M.; Limon, M.; Niemack, M. D.; Page, L. A.; Parker, L.; Reid, B.; Sherwin, B.; Staggs, S. T.; Switzer, E. R.; Zhao, Y.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Dunkley, J.; Acquaviva, V.; Das, S.; Hajian, A.; Lin, Y-T.; Lupton, R. H.; Marriage, T. A.; Spergel, D. N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Sievers, J.; Bond, J. R.; Hajian, A.; Nolta, M. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Acquaviva, V.; Hughes, J. P.; Menanteau, F.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Ade, P. A. R.; Mauskopf, P.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aguirre, P.; Barrientos, L. F.; Duenner, R.; Infante, L.; Juin, J. B.; Lin, Y-T.] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Amiri, M.; Battistelli, E. S.; Burger, B.; Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Battistelli, E. S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Brown, B.; Kosowsky, A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Chervenak, J.; Moseley, H.; Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Das, S.] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Das, S.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Devlin, M. J.; Dicker, S. R.; Kaul, M.; Klein, J.; Limon, M.; Marsden, D.; Swetz, D. S.; Thornton, R.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Doriese, W. Bertrand; Fowler, J. W.; Hilton, G. C.; Irwin, K. D.; Niemack, M. D.; Swetz, D. S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Hernandez-Monteagudo, C.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hilton, M.; Moodley, K.; Warne, R.] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hilton, M.; Moodley, K.] Rosebank, Ctr High Performance Comp, Cape Town, South Africa. [Huffenberger, K. M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Hughes, D. H.] INAOE, Puebla, Mexico. [Lau, J. M.; Sehgal, N.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Lau, J. M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Limon, M.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Lin, Y-T.] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. [Marriage, T. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Partridge, B.] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Reid, B.] Univ Barcelona, ICC, E-08028 Barcelona, Spain. [Switzer, E. R.] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Thornton, R.] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. [Trac, H.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Trac, H.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dunkley, J (reprint author), Univ Oxford, Subdept Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012; OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Huffenberger, Kevin/0000-0001-7109-0099; Sievers, Jonathan/0000-0001-6903-5074; Limon, Michele/0000-0002-5900-2698 FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731, PIRE-0507768]; Princeton University; University of Pennsylvania; RCUK Fellowship; Rhodes Trust; NASA [NNX08AH30G]; Natural Science and Engineering Research Council of Canada (NSERC); NSF [AST-0546035, AST-0606975]; FONDAP Centro de Astrofisica; CONICYT; MECESUP; Fundacion Andes; NSF Physics Frontier Center [PHY-0114422]; South African National Research Foundation (NRF); South African Centre for High Performance Computing (CHPC); South African Square Kilometer Array (SKA); Berkeley Center for Cosmological Physics; World Premier International Research Center Initiative, MEXT, Japan; U.S. Department of Energy [DE-AC3-76SF00515]; Canada Foundation for Innovation under the auspices of Compute Canada; Government of Toronto; NASA Office of Space Science FX ACT is on the Chajnantor Science preserve, which was made possible by the Chilean Comision Nacional de Investigacion Cientifica y Tecnologica. We are grateful for the assistance we received at various times from the ALMA, APEX, ASTE, CBI/QUIET, and NANTEN2 groups. The PWV data come from the public APEX weather Web site. Field operations were based at the Don Esteban facility run by Astro-Norte. Reed Plimpton and David Jacobson worked at the telescope during the 2008 season. We thank Norm Jarosik for support throughout the project. We also thank Adam Moss and Richard Battye for sharing their cosmic string power spectrum, Laurie Shaw and Nick Battaglia for providing SZ power spectra, and Bruce Bassett for suggestions on testing lensing in the power spectrum. We thank Marco Viero and Graeme Addison for providing useful input on clustered point sources. This work was supported by the U.S. National Science Foundation through awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731 and PIRE-0507768. Funding was also provided by Princeton University and the University of Pennsylvania. The PIRE program made possible exchanges between Chile, South Africa, Spain, and the US that enabled this research program. J.D. acknowledges support from an RCUK Fellowship. R. H. received funding from the Rhodes Trust. V. A., S. D., A. H., and T. M. were supported through NASA grant NNX08AH30G. A. D. H. received additional support from a Natural Science and Engineering Research Council of Canada (NSERC) PGS-D scholarship. A. K. and B. P. were partially supported through NSF AST-0546035 and AST-0606975, respectively, for work on ACT. L. I. acknowledges partial support from FONDAP Centro de Astrofisica. R. D. was supported by CONICYT, MECESUP, and Fundacion Andes. E. S. acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. K. M., M. H., and R. W. received financial support from the South African National Research Foundation (NRF), the Meraka Institute via funding for the South African Centre for High Performance Computing (CHPC), and the South African Square Kilometer Array (SKA) Project. S. D. acknowledges support from the Berkeley Center for Cosmological Physics. Y.T.L. acknowledges support from the World Premier International Research Center Initiative, MEXT, Japan. N.S. is supported by the U.S. Department of Energy contract to SLAC no. DE-AC3-76SF00515. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Toronto. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. The data will be made public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web site (http://www.physics.princeton.edu/act/). NR 139 TC 269 Z9 269 U1 4 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 52 DI 10.1088/0004-637X/739/1/52 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700052 ER PT J AU Laskar, T Berger, E Chary, RR AF Laskar, Tanmoy Berger, Edo Chary, Ranga-Ram TI EXPLORING THE GALAXY MASS-METALLICITY RELATION AT z similar to 3-5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: ISM; galaxies: luminosity function, mass function; gamma-ray burst: general; infrared: galaxies ID GAMMA-RAY BURST; STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; HIGH COLUMN DENSITY; DIGITAL SKY SURVEY; GRB HOST GALAXY; LY-ALPHA; STELLAR POPULATIONS; LUMINOSITY FUNCTIONS; SPITZER OBSERVATIONS AB Long-duration gamma-ray bursts (GRBs) provide a premier tool for studying high-redshift star-forming galaxies thanks to their extreme brightness and association with massive stars. Here we use GRBs to study the galaxy stellar mass-metallicity (M(*)-Z) relation at z similar to 3-5, where conventional direct metallicity measurements are extremely challenging. We use the interstellar medium metallicities of long GRB hosts derived from afterglow absorption spectroscopy, in conjunction with host galaxy stellar masses determined from deep Spitzer 3.6 mu m observations of 20 GRB hosts. We detect about 1/4 of the hosts with M(AB)(I) approximate to -21.5 to -22.5 mag and place a limit of M(AB)(I) greater than or similar to -19 mag on the remaining hosts from a stacking analysis. Using these observations, we present the first rest-frame optical luminosity distribution of long GRB hosts at z greater than or similar to 3 and find that it is similar to the distribution of long GRB hosts at z similar to 1. In comparison to Lyman-break galaxies at the same redshift, GRB hosts are generally fainter, but the sample is too small to rule out an overall similar luminosity function. On the other hand, the GRB hosts appear to be more luminous than the population of Ly alpha emitters at z similar to 3-4. Using a conservative range of mass-to-light ratios for simple stellar populations (with ages of 70 Myr to similar to 2 Gyr), we infer the host stellar masses and present mass-metallicity measurements at z similar to 3-5 (< z > similar to 3.5). We find that the detected GRB hosts, with M(*) approximate to 2 x 10(10) M(circle dot), display a wide range of metallicities, but that the mean metallicity at this mass scale, Z approximate to 0.3 Z(circle dot), is lower than measurements at z less than or similar to 3. Combined with stacking of the non-detected hosts with M(*) less than or similar to 3 x 10(9) M(circle dot) and Z less than or similar to 0.1 Z(circle dot), we find tentative evidence for the existence of an M(*)-Z relation at z similar to 3.5 and continued evolution of this relation to systematically lower metallicities from z similar to 2. C1 [Laskar, Tanmoy; Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chary, Ranga-Ram] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Laskar, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA; JPL/Caltech FX We thank the anonymous referee for useful comments, which improved the quality of the manuscript. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 72 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 SEP 20 PY 2011 VL 739 IS 1 AR 1 DI 10.1088/0004-637X/739/1/1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700001 ER PT J AU Levesque, EM Berger, E Soderberg, AM Chornock, R AF Levesque, Emily M. Berger, Edo Soderberg, Alicia M. Chornock, Ryan TI METALLICITY IN THE GRB 100316D/SN 2010bh HOST COMPLEX SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; gamma-ray burst: individual (GRB 100316D) ID GAMMA-RAY BURST; CORE-COLLAPSE SUPERNOVAE; STARBURST GALAXIES; STAR-FORMATION; NEARBY LONG; CONNECTION; EMISSION; EXPLOSION; DISCOVERY; CLASSIFICATION AB The recent long-duration GRB 100316D, associated with supernova SN 2010bh and detected by Swift, is one of the nearest gamma-ray burst (GRB)-supernovae (SNe) ever observed (z = 0.059). This provides us with a unique opportunity to study the explosion environment on similar to kpc scale in relation to the host galaxy complex. Here we present spatially resolved spectrophotometry of the host galaxy, focusing on both the explosion site and the brightest star-forming regions. Using these data, we extract the spatial profiles of the relevant emission features (H alpha, H beta, [O III]lambda 5007, and [N II]lambda 6584) and use these profiles to examine variations in metallicity and star formation rate (SFR) as a function of position in the host galaxy. We conclude that GRB 100316D/SN2010bh occurred in a low-metallicity host galaxy, and that the GRB-SN explosion site corresponds to the region with the lowest metallicity and highest SFR sampled by our observations. C1 [Levesque, Emily M.] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Berger, Edo; Soderberg, Alicia M.; Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Levesque, EM (reprint author), Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. EM Emily.Levesque@colorado.edu FU NASA, Chandra X-ray Center [PF0-110075]; NASA [NAS8-03060]; Swift [5080010, 6090612] FX We are grateful for the hospitality and assistance of the support staff at Las Campanas Observatory in Chile. This paper utilized data from the Gamma-Ray Burst Coordinates Network (GCN) circulars. E. M. L. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF0-110075 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. GRB research at Harvard is supported in part by Swift AO5 grant 5080010 and AO6 grant 6090612. NR 57 TC 29 Z9 29 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 23 DI 10.1088/0004-637X/739/1/23 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700023 ER PT J AU Schmelz, JT Worley, BT Anderson, DJ Pathak, S Kimble, JA Jenkins, BS Saar, SH AF Schmelz, J. T. Worley, B. T. Anderson, D. J. Pathak, S. Kimble, J. A. Jenkins, B. S. Saar, S. H. TI ISOTHERMAL AND MULTITHERMAL ANALYSIS OF CORONAL LOOPS OBSERVED WITH ATMOSPHERIC IMAGING ASSEMBLY. II. 211 angstrom SELECTED LOOPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: fundamental parameters; Sun: UV radiation ID X-RAY TELESCOPE; EMISSION-LINES; ATOMIC DATABASE; REGION; TEMPERATURE; DISTRIBUTIONS; SPECTROMETER; EXPLORER; CHIANTI AB An important component of coronal loop analysis involves conflicting results on the cross-field temperature distribution. Are loops isothermal or multithermal? The Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory was designed in part to answer this question. AIA has a series of coronal filters that peak at different temperatures and cover the entire active region temperature range. These properties should make AIA ideal for multithermal analysis, but recent results have shown that the response functions of two of the filters, AIA 94 and 131 angstrom, are missing a significant number of low-temperature emission lines. Here we analyze coronal loops from several active regions that were chosen in the 211 angstrom channel of AIA, which has a peak response temperature of log T = 6.3. The differential emission measure (DEM) analysis of the 12 loops in our sample reveals that using data from the 131 angstrom AIA filter distorts the results, and we have no choice but to do the analysis without these data. The 94 angstrom data do not appear to be as important, simply because the chosen loops are not visible in this channel. If we eliminate the 131 angstrom data, however, we find that our DEM analysis is not well constrained on the cool temperature end of six of our loops. The information revealed by our 211 selected loops indicates that additional atomic data are required in order to pin down the cross-field temperature distribution. C1 [Schmelz, J. T.; Worley, B. T.; Anderson, D. J.; Pathak, S.; Kimble, J. A.; Jenkins, B. S.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Schmelz, J. T.; Saar, S. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu FU NSF [ATM-0402729]; NASA/SAO; [NNM07AB07C] FX We thank Vinay Kashyap (CfA) for his help with Monte Carlo DEMs. The Atmospheric Imaging Assembly on the Solar Dynamics Observatory is part of NASA's Living with a Star program. Solar physics research at the University of Memphis is supported by NSF ATM-0402729 as well as a Hinode subcontract from NASA/SAO. S. H. S. is supported by contract NNM07AB07C to NASA. We also benefited from discussions at theCoronal Loops Workshops held in Paris (2002 November), Palermo (2004 September), Santorini (2007 June), and Florence (2009 June). NR 23 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 33 DI 10.1088/0004-637X/739/1/33 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700033 ER PT J AU Schwadron, NA Smith, CW Spence, HE Kasper, JC Korreck, K Stevens, ML Maruca, BA Kiefer, KK Lepri, ST McComas, D AF Schwadron, N. A. Smith, C. W. Spence, H. E. Kasper, J. C. Korreck, K. Stevens, M. L. Maruca, B. A. Kiefer, K. K. Lepri, S. T. McComas, D. TI CORONAL ELECTRON TEMPERATURE FROM THE SOLAR WIND SCALING LAW THROUGHOUT THE SPACE AGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: dynamo; Sun: evolution; sunspots ID ION COMPOSITION SPECTROMETER; MAGNETIC-FLUX; HELIOSPHERE; ULYSSES; BALANCE; MINIMA; SWICS; FIELD AB Recent in situ observations of the solar wind show that charge states (e. g., the O7+/O6+ and C6+/C5+ abundance ratios) and alpha-particle composition evolved through the extended, deep solar minimum between solar cycles 23 and 24 (i.e., from 2006 to 2009). Prior investigations have found that both particle flux and magnetic field strength gradually decreased over this period of time. In this study, we find that (for a given solar wind speed) the coronal electron temperature (as derived from O7+/O6+ and C6+/C5+ measurements from ACE) likewise decreased during this minimum. We use the Schwadron & McComas solar wind scaling law to show that cooler coronal electron temperatures are naturally associated with lower particle fluxes because downward heat conduction must be reduced to keep the average energy loss per particle fixed. The results of the scaling law should apply to all solar wind models and suggest that the evolution of the solar wind is linked to the solar dynamo, which caused the coronal magnetic field strength to decrease in the deep, extended minimum. We utilize the scaling law to project coronal electron temperatures backward in time throughout the space age and find that these temperatures have been decreasing in successive temperature maxima since 1987 but were increasing in successive temperature maxima from 1969 to 1987. Thus, we show how the solar wind scaling law relates solar wind properties observed at 1 AU back to coronal electron temperatures throughout the space age. C1 [Schwadron, N. A.; Smith, C. W.; Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Kasper, J. C.; Korreck, K.; Stevens, M. L.; Maruca, B. A.; Kiefer, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lepri, S. T.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Schwadron, N. A.; McComas, D.] SW Res Inst, San Antonio, TX 78228 USA. [McComas, D.] Univ Texas San Antonio, San Antonio, TX 78249 USA. RP Schwadron, NA (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RI Lepri, Susan/I-8611-2012; Spence, Harlan/A-1942-2011; Kasper, Justin/D-1152-2010; OI Kasper, Justin/0000-0002-7077-930X; Spence, Harlan/0000-0002-2526-2205 FU LRO/CRaTER; Earth Moon Mars Radiation Environment Model (EMMREM); ACE/SWEPAM; WIND/SWE; NSF FX N.A.S. was supported by LRO/CRaTER and the Earth Moon Mars Radiation Environment Model (EMMREM) projects. D.Mc. was supported by ACE/SWEPAM. J.C.K., M. L. S., K. E. K., and B. A. M. were supported by the WIND/SWE project. K. K. was supported by the NSF-Solar REU program. We thank the ACE SWICS and SWIMS instrument team and the Ion Mass Spectrometer (SWIMS) ACE Science Center for providing the ACE data. NR 35 TC 23 Z9 23 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 9 DI 10.1088/0004-637X/739/1/9 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700009 ER PT J AU Stello, D Meibom, S Gilliland, RL Grundahl, F Hekker, S Mosser, B Kallinger, T Mathur, S Garcia, RA Huber, D Basu, S Bedding, TR Brogaard, K Chaplin, WJ Elsworth, YP Molenda-Zakowicz, J Szabo, R Still, M Jenkins, JM Christensen-Dalsgaard, J Kjeldsen, H Serenelli, AM Wohler, B AF Stello, Dennis Meibom, Soren Gilliland, Ronald L. Grundahl, Frank Hekker, Saskia Mosser, Benoit Kallinger, Thomas Mathur, Savita Garcia, Rafael A. Huber, Daniel Basu, Sarbani Bedding, Timothy R. Brogaard, Karsten Chaplin, William J. Elsworth, Yvonne P. Molenda-Zakowicz, Joanna Szabo, Robert Still, Martin Jenkins, Jon M. Christensen-Dalsgaard, Jorgen Kjeldsen, Hans Serenelli, Aldo M. Wohler, Bill TI AN ASTEROSEISMIC MEMBERSHIP STUDY OF THE RED GIANTS IN THREE OPEN CLUSTERS OBSERVED BY KEPLER: NGC 6791, NGC 6819, AND NGC 6811 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (NGC 6791, NGC6819, NGC6811); stars: fundamental parameters; stars: interiors; stars: oscillations; techniques: photometric ID SOLAR-LIKE OSCILLATIONS; BOLOMETRIC CORRECTIONS; STELLAR EVOLUTION; METAL ABUNDANCES; NGC-6791; STARS; OLD; CONSTRAINTS; AMPLITUDES; ISOCHRONES AB Studying star clusters offers significant advances in stellar astrophysics due to the combined power of having many stars with essentially the same distance, age, and initial composition. This makes clusters excellent test benches for verification of stellar evolution theory. To fully exploit this potential, it is vital that the star sample is uncontaminated by stars that are not members of the cluster. Techniques for determining cluster membership therefore play a key role in the investigation of clusters. We present results on three clusters in the Kepler field of view based on a newly established technique that uses asteroseismology to identify fore-or background stars in the field, which demonstrates advantages over classical methods such as kinematic and photometry measurements. Four previously identified seismic non-members in NGC6819 are confirmed in this study, and three additional non-members are found-two in NGC6819 and one in NGC6791. We further highlight which stars are, or might be, affected by blending, which needs to be taken into account when analyzing these Kepler data. C1 [Stello, Dennis; Huber, Daniel; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Grundahl, Frank; Brogaard, Karsten] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Hekker, Saskia; Chaplin, William J.; Elsworth, Yvonne P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Mosser, Benoit] Univ Paris 07, LESIA, CNRS, Univ Paris 06,Observ Paris, F-92195 Meudon, France. [Kallinger, Thomas] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kallinger, Thomas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Mathur, Savita] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Garcia, Rafael A.] Univ Paris 07, Lab AIM, CEA DSM CNRS, IRFU SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Brogaard, Karsten] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Molenda-Zakowicz, Joanna] Uniwersytetu Wroclawskiego, Inst Astron, PL-51622 Wroclaw, Poland. [Szabo, Robert] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary. [Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Jenkins, Jon M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Serenelli, Aldo M.] Fac Ciencies, Inst Ciencias Espacio CSIC IEEC, Bellaterra 08193, Spain. [Wohler, Bill] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Stello, D (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. OI Kallinger, Thomas/0000-0003-3627-2561; Brogaard, Karsten/0000-0003-2001-0276; Bedding, Timothy/0000-0001-5943-1460; Szabo, Robert/0000-0002-3258-1909; Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769 FU NASA's Science Mission Directorate; Australian Research Council; Hungarian Academy of Sciences; Hungarian OTKA [K83790, MB08C 81013]; UK Science and Technology Facilities Council (STFC); Carlsberg Foundation; National Science Foundation; Janos Bolyai Research Scholarship FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors thank the entire Kepler team without whom this investigation would not have been possible. D. S. acknowledges support from the Australian Research Council. This project has been supported by the "Lendulet" program of the Hungarian Academy of Sciences and the Hungarian OTKA grant K83790 and MB08C 81013. S. H. acknowledges financial support from the UK Science and Technology Facilities Council (STFC). K. B. acknowledges financial support from the Carlsberg Foundation. NCAR is supported by the National Science Foundation. R. S. thanks the support of the Janos Bolyai Research Scholarship. NR 45 TC 52 Z9 52 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 13 DI 10.1088/0004-637X/739/1/13 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700013 ER PT J AU Weisz, DR Dalcanton, JJ Williams, BF Gilbert, KM Skillman, ED Seth, AC Dolphin, AE McQuinn, KBW Gogarten, SM Holtzman, J Rosema, K Cole, A Karachentsev, ID Zaritsky, D AF Weisz, Daniel R. Dalcanton, Julianne J. Williams, Benjamin F. Gilbert, Karoline M. Skillman, Evan D. Seth, Anil C. Dolphin, Andrew E. McQuinn, Kristen B. W. Gogarten, Stephanie M. Holtzman, Jon Rosema, Keith Cole, Andrew Karachentsev, Igor D. Zaritsky, Dennis TI THE ACS NEARBY GALAXY SURVEY TREASURY. VIII. THE GLOBAL STAR FORMATION HISTORIES OF 60 DWARF GALAXIES IN THE LOCAL VOLUME SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: evolution; galaxies: star formation; galaxies: stellar content; Hertzsprung-Russell and C-M diagrams ID HUBBLE-SPACE-TELESCOPE; COLOR-MAGNITUDE DIAGRAMS; LARGE-MAGELLANIC-CLOUD; SPHEROIDAL GALAXIES; IRREGULAR GALAXIES; H-ALPHA; ADVANCED CAMERA; METALLICITY RELATION; INTERSTELLAR-MEDIUM; CHEMICAL EVOLUTION AB We present uniformly measured star formation histories (SFHs) of 60 nearby (D less than or similar to 4 Mpc) dwarf galaxies based on color-magnitude diagrams of resolved stellar populations from images taken with the Hubble Space Telescope and analyzed as part of the ACS Nearby Galaxy Survey Treasury program (ANGST). This volume-limited sample contains 12 dwarf spheroidal (dSph)/dwarf elliptical (dE), 5 dwarf spiral, 28 dwarf irregular (dI), 12 dSph/dI (transition), and 3 tidal dwarf galaxies. The sample spans a range of similar to 10 mag in MB and covers a wide range of environments, from highly interacting to truly isolated. From the best-fit SFHs, we find three significant results for dwarf galaxies in the ANGST volume: (1) the majority of dwarf galaxies formed the bulk of their mass prior to z similar to 1, regardless of current morphological type; (2) the mean SFHs of dIs, transition dwarf galaxies (dTrans), and dSphs are similar over most of cosmic time, and only begin to diverge a few Gyr ago, with the clearest differences between the three appearing during the most recent 1 Gyr; and (3) the SFHs are complex and the mean values are inconsistent with simple SFH models, e. g., single bursts, constant star formation rates (SFRs), or smooth, exponentially declining SFRs. The mean SFHs show clear divergence from the cosmic SFH at z less than or similar to 0.7, which could be evidence that low-mass systems have experienced delayed star formation relative to more massive galaxies. The sample shows a strong density-morphology relationship, such that the dSphs in the sample are less isolated than the dIs. We find that the transition from a gas-rich to gas-poor galaxy cannot be solely due to internal mechanisms such as stellar feedback, and instead is likely the result of external mechanisms, e. g., ram pressure and tidal stripping and tidal forces. In terms of their environments, SFHs, and gas fractions, the majority of the dTrans appear to be low-mass dIs that simply lack Ha emission, similar to Local Group (LG) dTrans DDO 210. However, a handful of dTrans have remarkably low gas fractions, suggesting that they have nearly exhausted their gas supply, analogous to LG dTrans such as Phoenix. Finally, we have also included extensive exploration of uncertainties in the SFH recovery method, including the optimization of time resolution, the effects of photometric depth, and impact of systematic uncertainties due to the limitations in current stellar evolution models. C1 [Weisz, Daniel R.; Dalcanton, Julianne J.; Williams, Benjamin F.; Gilbert, Karoline M.; Gogarten, Stephanie M.; Rosema, Keith] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Weisz, Daniel R.; Skillman, Evan D.; McQuinn, Kristen B. W.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85756 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Cole, Andrew] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. [Karachentsev, Igor D.] Russian Acad Sci, Special Astrophys Observ, Nizhnji Arkhyz 369167, Karachai Circes, Russia. [Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Weisz, DR (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM dweisz@astro.washington.edu; jd@astro.washington.edu; ben@astro.washington.edu; kgilbert@astro.washington.edu; skillman@astro.umn.edu; aseth@cfa.harvard.edu; adolphin@raytheon.com; kmcquinn@astro.umn.edu; stephanie@astro.washington.edu; holtz@nmsu.edu; krosema@astro.washington.edu; andrew.cole@utas.edu.au; ikar@luna.sao.ru; dzaritsky@as.arizona.edu OI Cole, Andrew/0000-0003-0303-3855; Gogarten, Stephanie/0000-0002-7231-9745; Weisz, Daniel/0000-0002-6442-6030 NR 126 TC 155 Z9 155 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 5 DI 10.1088/0004-637X/739/1/5 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700005 ER PT J AU Zhu, M Davis, CJ Wu, YF Whitney, BA Robitaille, T Peng, R AF Zhu, Ming Davis, C. J. Wu, Yufang Whitney, B. A. Robitaille, T. Peng, R. TI A MASSIVE PROTOSTAR EMBEDDED IN THE SCUBA CORE JCMT 18354-0649S SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; infrared: stars; stars: formation ID YOUNG STELLAR OBJECTS; H-II REGIONS; SPECTRAL ENERGY-DISTRIBUTIONS; COLLIMATED MOLECULAR JETS; ULTRACOMPACT HII-REGIONS; ARRAY CAMERA IRAC; STAR-FORMATION; PHYSICAL CONDITIONS; DENSITY STRUCTURE; IMAGING SURVEY AB We report the discovery of an extremely red object embedded in the massive SCUBA core JCMT 18354-0649S. This object is not associated with any known radio or far-IR source, though it appears in Spitzer IRAC data obtained as part of the GLIMPSE survey. At shorter wavelengths, this embedded source exhibits an extreme color, K - L' = 6.7. At an assumed distance of 5.7 kpc, this source has a near-IR luminosity of similar to 1000 L-circle dot. Its spectral energy distribution (SED) rises sharply from 2.1 mu m to 8 mu m, similar to that of a Class 0 young stellar object. Theoretical modeling of the SED indicates that the central star has a mass of 6-12 M-circle dot, with an optical extinction of more than 30. As both inflow and outflow motions are present in JCMT 18354-0649S, we suggest that this deeply embedded source is (1) a massive protostar in the early stages of accretion, and (2) the driving source of a massive molecular outflow evident in HCN J = 3-2 profiles observed toward this region. C1 [Zhu, Ming] Natl Astron Observ China, Beijing, Peoples R China. [Davis, C. J.] Joint Astron Ctr, Hilo, HI 96720 USA. [Wu, Yufang] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Whitney, B. A.] Space Sci Inst, Boulder, CO 80301 USA. [Robitaille, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peng, R.] Caltech Submillimeter Observ, Hilo, HI 96720 USA. RP Zhu, M (reprint author), Natl Astron Observ China, 20A Datun Rd, Beijing, Peoples R China. EM mz@nao.cac.cn OI Robitaille, Thomas/0000-0002-8642-1329 FU NSFC [Y011231001, 10733030, 10873019]; Chinese Academy of Sciences; NSF [AST-0540882]; NASA FX M.Z. acknowledges the support from NSFC grant Y011231001 and also from the "Hundred-talent program" of the Chinese Academy of Sciences. Y. Wu is grateful for the support of grants 10733030 and 10873019 of NSFC. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre (JAC) on behalf of the U. K. Science and Technology Facilities Council (STFC). The H-, K-, and L '-band imaging reported here were obtained as part of the UKIRT Service Programme. We thank Dr. Watson Varricatt at the JAC for help with near-IR photometry. The JCMT is also operated by the Joint Astronomy Centre on behalf of the U. K. STFC, the National Research Council Canada, and the Netherlands Organisation for Scientific Research. Caltech Submillimeter Observatory is supported through NSF grant AST-0540882. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech for the GLIMPSE360 project (B. W.). We thank the GLIMPSE team (PI: E. Churchwell) for making the IRAC images available on the internet. We also thank the anonymous referee whose comments helped improve the paper. NR 69 TC 1 Z9 1 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2011 VL 739 IS 1 AR 53 DI 10.1088/0004-637X/739/1/53 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 821DS UT WOS:000294955700053 ER PT J AU Brogan, CL Hunter, TR Cyganowski, CJ Friesen, RK Chandler, CJ Indebetouw, R AF Brogan, C. L. Hunter, T. R. Cyganowski, C. J. Friesen, R. K. Chandler, C. J. Indebetouw, R. TI FIRST RESULTS FROM A 1.3 cm EXPANDED VERY LARGE ARRAY SURVEY OF MASSIVE PROTOSTELLAR OBJECTS: G35.03+0.35 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (G35.03+0.35); stars: formation; stars: massive; techniques: interferometric ID H-II REGIONS; GLIMPSE SURVEY; STAR-FORMATION; DENSE CORES; MASERS; AMMONIA; NH3; THERMOMETER; OUTFLOW; CATALOG AB We have performed a 1.3 cm survey of 24 massive young stellar objects (MYSOs) using the Expanded Very Large Array. The sources in the sample exhibit a broad range of massive star formation signposts including infrared dark clouds (IRDCs), ultra-compact H II (UC H II) regions, and extended 4.5 mu m emission in the form of extended green objects (EGOs). In this work, we present results for G35.03+0.35 which exhibits all of these phenomena. We simultaneously image the 1.3 cm NH3 (1,1) through (6,6) inversion lines, four CH3OH transitions, two H recombination lines, plus continuum at 0.05 pc resolution. We find three areas of thermal NH3 emission, two within the EGO (designated as the NE and SW cores) and one toward an adjacent IRDC. The NE core contains a UC H II region (CM1) and a candidate hyper-compact H II region (CM2). A region of non-thermal, likely masing NH3 (3,3) and (6,6) emission is coincident with an arc of 44 GHz CH3OH masers. We also detect two new 25 GHz Class-I CH3OH masers. A complementary Submillimeter Array 1.3 mm continuum image shows that the distribution of dust emission is similar to the lower-lying NH3 lines, all peaking to the NW of CM2, indicating the likely presence of an additional MYSO in this protocluster. By modeling the NH3 and 1.3 mm continuum data, we obtain gas temperatures of 20-220 K and masses of 20-130 M-circle dot. The diversity of continuum emission properties and gas temperatures suggests that objects in a range of evolutionary states exist concurrently in this protocluster. C1 [Brogan, C. L.; Hunter, T. R.; Friesen, R. K.; Indebetouw, R.] NRAO, Charlottesville, VA 22903 USA. [Cyganowski, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandler, C. J.] NRAO, Socorro, NM 87801 USA. [Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. RP Brogan, CL (reprint author), NRAO, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM cbrogan@nrao.edu OI Hunter, Todd/0000-0001-6492-0090 NR 28 TC 15 Z9 15 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2011 VL 739 IS 1 AR L16 DI 10.1088/2041-8205/739/1/L16 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 818OQ UT WOS:000294762900016 ER EF