FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Meech, KJ A'Hearn, MF Adams, JA Bacci, P Bai, J Barrera, L Battelino, M Bauer, JM Becklin, E Bhatt, B Biver, N Bockelee-Morvan, D Bodewits, D Bohnhardt, H Boissier, J Bonev, BP Borghini, W Brucato, JR Bryssinck, E Buie, MW Canovas, H Castellano, D Charnley, SB Chen, WP Chiang, P Choi, YJ Christian, DJ Chuang, YL Cochran, AL Colom, P Combi, MR Coulson, IM Crovisier, J Dello Russo, N Dennerl, K DeWahl, K DiSanti, MA Facchini, M Farnham, TL Fernandez, Y Floren, HG Frisk, U Fujiyoshi, T Furusho, R Fuse, T Galli, G Garcia-Hernandez, DA Gersch, A Getu, Z Gibb, EL Gillon, M Guido, E Guillermo, RA Hadamcik, E Hainaut, O Hammel, HB Harker, DE Harmon, JK Harris, WM Hartogh, P Hashimoto, M Hausler, B Herter, T Hjalmarson, A Holland, ST Honda, M Hosseini, S Howell, ES Howes, N Hsieh, HH Hsiao, HY Hutsemekers, D Immler, SM Jackson, WM Jeffers, SV Jehin, E Jones, TJ Ovelar, MD Kaluna, HM Karlsson, T Kawakita, H Keane, JV Keller, LD Kelley, MS Kinoshita, D Kiselev, NN Kleyna, J Knight, MM Kobayashi, H Kobulnicky, HA Kolokolova, L Kreiny, M Kuan, YJ Kuppers, M Lacruz, JM Landsman, WB Lara, LM Lecacheux, A Levasseur-Regourd, AC Li, B Licandro, J Ligustri, R Lin, ZY Lippi, M Lis, DC Lisse, CM Lovell, AJ Lowry, SC Lu, H Lundin, S Magee-Sauer, K Magain, P Manfroid, J Epifani, EM McKay, A Melita, MD Mikuz, H Milam, SN Milani, G Min, M Moreno, R Mueller, BEA Mumma, MJ Nicolini, M Nolan, MC Nordh, HL Nowajewski, PB Team, O Ootsubo, T Paganini, L Perrella, C Pittichova, J Prosperi, E Radeva, YL Reach, WT Remijan, AJ Rengel, M Riesen, TE Rodenhuis, M Rodriguez, DP Russell, RW Sahu, DK Samarasinha, NH Caso, AS Sandqvist, A Sarid, G Sato, M Schleicher, DG Schwieterman, EW Sen, AK Shenoy, D Shi, JC Shinnaka, Y Skvarc, J Snodgrass, C Sitko, ML Sonnett, S Sosseini, S Sostero, G Sugita, S Swinyard, BM Szutowicz, S Takato, N Tanga, P Taylor, PA Tozzi, GP Trabatti, R Trigo-Rodriguez, JM Tubiana, C de Val-Borro, M Vacca, W Vandenbussche, B Vaubaillion, J Velichko, FP Velichko, SF Vervack, RJ Vidal-Nunez, MJ Villanueva, GL Vinante, C Vincent, JB Wang, M Wasserman, LH Watanabe, J Weaver, HA Weissman, PR Wolk, S Wooden, DH Woodward, CE Yamaguchi, M Yamashita, T Yanamandra-Fischer, PA Yang, B Yao, JS Yeomans, DK Zenn, T Zhao, H Ziffer, JE AF Meech, K. J. A'Hearn, M. F. Adams, J. A. Bacci, P. Bai, J. Barrera, L. Battelino, M. Bauer, J. M. Becklin, E. Bhatt, B. Biver, N. Bockelee-Morvan, D. Bodewits, D. Boehnhardt, H. Boissier, J. Bonev, B. P. Borghini, W. Brucato, J. R. Bryssinck, E. Buie, M. W. Canovas, H. Castellano, D. Charnley, S. B. Chen, W. P. Chiang, P. Choi, Y-J Christian, D. J. Chuang, Y-L Cochran, A. L. Colom, P. Combi, M. R. Coulson, I. M. Crovisier, J. Dello Russo, N. Dennerl, K. DeWahl, K. DiSanti, M. A. Facchini, M. Farnham, T. L. Fernandez, Y. Floren, H. G. Frisk, U. Fujiyoshi, T. Furusho, R. Fuse, T. Galli, G. Garcia-Hernandez, D. A. Gersch, A. Getu, Z. Gibb, E. L. Gillon, M. Guido, E. Guillermo, R. A. Hadamcik, E. Hainaut, O. Hammel, H. B. Harker, D. E. Harmon, J. K. Harris, W. M. Hartogh, P. Hashimoto, M. Haeusler, B. Herter, T. Hjalmarson, A. Holland, S. T. Honda, M. Hosseini, S. Howell, E. S. Howes, N. Hsieh, H. H. Hsiao, H-Y Hutsemekers, D. Immler, S. M. Jackson, W. M. Jeffers, S. V. Jehin, E. Jones, T. J. Ovelar, M. de Juan Kaluna, H. M. Karlsson, T. Kawakita, H. Keane, J. V. Keller, L. D. Kelley, M. S. Kinoshita, D. Kiselev, N. N. Kleyna, J. Knight, M. M. Kobayashi, H. Kobulnicky, H. A. Kolokolova, L. Kreiny, M. Kuan, Y-J Kueppers, M. Lacruz, J. M. Landsman, W. B. Lara, L. M. Lecacheux, A. Levasseur-Regourd, A. C. Li, B. Licandro, J. Ligustri, R. Lin, Z-Y Lippi, M. Lis, D. C. Lisse, C. M. Lovell, A. J. Lowry, S. C. Lu, H. Lundin, S. Magee-Sauer, K. Magain, P. Manfroid, J. Epifani, E. Mazzotta McKay, A. Melita, M. D. Mikuz, H. Milam, S. N. Milani, G. Min, M. Moreno, R. Mueller, B. E. A. Mumma, M. J. Nicolini, M. Nolan, M. C. Nordh, H. L. Nowajewski, P. B. Team, Odin Ootsubo, T. Paganini, L. Perrella, C. Pittichova, J. Prosperi, E. Radeva, Y. L. Reach, W. T. Remijan, A. J. Rengel, M. Riesen, T. E. Rodenhuis, M. Rodriguez, D. P. Russell, R. W. Sahu, D. K. Samarasinha, N. H. Sanchez Caso, A. Sandqvist, A. Sarid, G. Sato, M. Schleicher, D. G. Schwieterman, E. W. Sen, A. K. Shenoy, D. Shi, J-C Shinnaka, Y. Skvarc, J. Snodgrass, C. Sitko, M. L. Sonnett, S. Sosseini, S. Sostero, G. Sugita, S. Swinyard, B. M. Szutowicz, S. Takato, N. Tanga, P. Taylor, P. A. Tozzi, G-P Trabatti, R. Trigo-Rodriguez, J. M. Tubiana, C. de Val-Borro, M. Vacca, W. Vandenbussche, B. Vaubaillion, J. Velichko, F. P. Velichko, S. F. Vervack, R. J., Jr. Vidal-Nunez, M. J. Villanueva, G. L. Vinante, C. Vincent, J-B Wang, M. Wasserman, L. H. Watanabe, J. Weaver, H. A. Weissman, P. R. Wolk, S. Wooden, D. H. Woodward, C. E. Yamaguchi, M. Yamashita, T. Yanamandra-Fischer, P. A. Yang, B. Yao, J-S Yeomans, D. K. Zenn, T. Zhao, H. Ziffer, J. E. TI EPOXI: COMET 103P/HARTLEY 2 OBSERVATIONS FROM A WORLDWIDE CAMPAIGN SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE comets: individual (103P/Hartley 2) ID MIDINFRARED SPECTROMETER; SPACE-TELESCOPE; HERSCHEL; PERFORMANCE; PHOTOMETRY; MISSION; NUCLEUS; IMAGER; MIRSI; DUST AB Earth- and space-based observations provide synergistic information for space mission encounters by providing data over longer timescales, at different wavelengths and using techniques that are impossible with an in situ flyby. We report here such observations in support of the EPOXI spacecraft flyby of comet 103P/Hartley 2. The nucleus is small and dark, and exhibited a very rapidly changing rotation period. Prior to the onset of activity, the period was similar to 16.4 hr. Starting in 2010 August the period changed from 16.6 hr to near 19 hr in December. With respect to dust composition, most volatiles and carbon and nitrogen isotope ratios, the comet is similar to other Jupiter-family comets. 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[Trabatti, R.] Stn Astron Descartes, I-27013 Chignolo Po, Italy. [Vandenbussche, B.] KU, Inst Astron, Louvain, Belgium. [Vaubaillion, J.] IMCCE Observ Paris, F-75014 Paris, France. [Velichko, F. P.] Kharkiv Univ, Astron Inst, UA-61022 Kharkov, Ukraine. [Velichko, S. F.] Int Ctr Astron Med & Ecol Res, UA-03680 Kiev, Ukraine. [Vinante, C.] Univ Padua, Dipartimento Geosci, I-35131 Padua, Italy. [Wolk, S.] Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, Cambridge, MA 02138 USA. [Wooden, D. H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ziffer, J. E.] Univ So Maine, Portland, ME 04104 USA. [Lis, D. C.] CALTECH, Pasadena, CA 91125 USA. RP Meech, KJ (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. RI Vervack, Ronald/C-2702-2016; Weaver, Harold/D-9188-2016; Lisse, Carey/B-7772-2016; Charnley, Steven/C-9538-2012; Milam, Stefanie/D-1092-2012; Combi, Michael/J-1697-2012; de Val-Borro, Miguel/H-1319-2013; mumma, michael/I-2764-2013; Nolan, Michael/H-4980-2012; Magee-Sauer, Karen/K-6061-2015; Dello Russo, Neil/G-2727-2015 OI Kelley, Michael/0000-0002-6702-7676; Fernandez, Yanga/0000-0003-1156-9721; Tanga, Paolo/0000-0002-2718-997X; Bodewits, Dennis/0000-0002-2668-7248; Tozzi, Gian Paolo/0000-0003-4775-5788; Christian, Damian/0000-0003-1746-3020; Reach, William/0000-0001-8362-4094; Snodgrass, Colin/0000-0001-9328-2905; Mazzotta Epifani, Elena/0000-0003-1412-0946; Harker, David/0000-0001-6397-9082; Retamales, Guillermo/0000-0002-3973-3848; Brucato, John Robert/0000-0002-4738-5521; Knight, Matthew/0000-0003-2781-6897; Canovas, Hector/0000-0001-7668-8022; Wolk, Scott/0000-0002-0826-9261; Vervack, Ronald/0000-0002-8227-9564; Lisse, Carey/0000-0002-9548-1526; Milam, Stefanie/0000-0001-7694-4129; Combi, Michael/0000-0002-9805-0078; de Val-Borro, Miguel/0000-0002-0455-9384; Nolan, Michael/0000-0001-8316-0680; Magee-Sauer, Karen/0000-0002-4979-9875; Dello Russo, Neil/0000-0002-8379-7304 FU Swedish National Space Board; Canadian Space Agency; National Technology Agency of Finland; Centre National d'Etudes Spatiales (CNES, France); Belgian Fund for Scientific Research (FNRS); Swiss National Science Foundation; European Community [229517]; Spanish Ministerio de Ciencia e Innovacion [AYA2008-01839/ESP, AyA2009-08011]; Junta de Andalucia [PE2007-TIC 02744]; NASA [NNM07AA99C]; Aerospace Corporation; NASA through NASA Astrobiology Institute [NNA04CC08A] FX Odin is a Swedish-led satellite project funded jointly by the Swedish National Space Board, the Canadian Space Agency, the National Technology Agency of Finland, and the Centre National d'Etudes Spatiales (CNES, France). The Swedish Space Corporation is the prime contractor, also responsible for Odin operations. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. We thank A. Tokunaga, Director of the NASA IRTF, for allocating time for an observing campaign at this telescope. The Faulkes Telescope North contributed to the CARA observing campaign. TRAPPIST is a project driven by the University of Liege, in close collaboration with the Observatory of Geneva, supported by the Belgian Fund for Scientific Research (FNRS) and the Swiss National Science Foundation. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013 under grant agreement no. 229517. Faulkes Telescope North contributed to CARA around the flyby period. The CSIC-IEEC and CSIC-IAA teams acknowledge support from grants AYA2008-01839/ESP and AyA2009-08011 from the Spanish Ministerio de Ciencia e Innovacion and PE2007-TIC 02744 from Junta de Andalucia. This work was supported in part by the NASA Planetary Astronomy Program and was performed in part at the Jet Propulsion Laboratory under contract with NASA. This work is also supported in part at The Aerospace Corporation by the Independent Research and Development Program. This work was supported by NASA's Discovery Program through contract NNM07AA99C to the University of Maryland, and in part through the NASA Astrobiology Institute under cooperative agreement no. NNA04CC08A. NR 48 TC 55 Z9 56 U1 0 U2 27 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2011 VL 734 IS 1 AR L1 DI 10.1088/2041-8205/734/1/L1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797NV UT WOS:000293135500001 ER PT J AU Williams, BF Dalcanton, JJ Johnson, LC Weisz, DR Seth, AC Dolphin, A Gilbert, KM Skillman, E Rosema, K Gogarten, SM Holtzman, J de Jong, RS AF Williams, Benjamin F. Dalcanton, Julianne J. Johnson, L. C. Weisz, Daniel R. Seth, Anil C. Dolphin, Andrew Gilbert, Karoline M. Skillman, Evan Rosema, Keith Gogarten, Stephanie M. Holtzman, Jon de Jong, Roelof S. TI THE HISTORY OF STAR FORMATION IN GALAXY DISKS IN THE LOCAL VOLUME AS MEASURED BY THE ADVANCED CAMERA FOR SURVEYS NEARBY GALAXY SURVEY TREASURY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: stellar content ID ULTRA-DEEP-FIELD; ASYMPTOTIC GIANT BRANCH; LYMAN-BREAK GALAXIES; LUMINOSITY FUNCTIONS; STELLAR POPULATIONS; FORMING GALAXIES; REDSHIFT SURVEY; H-ALPHA; EVOLUTION; UNIVERSE AB We present a measurement of the age distribution of stars residing in spiral disks and dwarf galaxies. We derive a complete star formation history of the similar to 140 Mpc(3) covered by the volume-limited sample of galaxies in the Advanced Camera for Surveys (ACS) Nearby Galaxy Survey Treasury (ANGST). The total star formation rate density history (rho(SFR)(t)) is dominated by the large spirals in the volume, although the sample consists mainly of dwarf galaxies. Our rho(SFR)(t) shows a factor of similar to 3 drop at z similar to 2, in approximate agreement with results from other measurement techniques. While our results show that the overall rho(SFR)(t) has decreased since z similar to 1, the measured rates during this epoch are higher than those obtained from other measurement techniques. This enhanced recent star formation rate appears to be largely due to an increase in the fraction of star formation contained in low-mass disks at recent times. Finally, our results indicate that despite the differences at recent times, the epoch of formation of similar to 50% of the stellar mass in dwarf galaxies was similar to that of similar to 50% of the stellar mass in large spiral galaxies (z greater than or similar to 2), despite the observed galaxy-to-galaxy diversity among the dwarfs. C1 [Williams, Benjamin F.; Dalcanton, Julianne J.; Johnson, L. C.; Weisz, Daniel R.; Gilbert, Karoline M.; Rosema, Keith; Gogarten, Stephanie M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dolphin, Andrew] Raytheon Co, Tucson, AZ 85706 USA. [Skillman, Evan] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [de Jong, Roelof S.] Astrophys Inst Potsdam, Potsdam, Germany. RP Williams, BF (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM ben@astro.washington.edu; jd@astro.washington.edu; lcj@astro.washington.edu; dweisz@astro.washington.edu; aseth@cfa.harvard.edu; adolphin@raytheon.com; kgilbert@astro.washington.edu; skillman@astro.umn.edu; krosema@astro.washington.edu; stephanie@astro.washington.edu; holtz@nmsu.edu; rdejong@aip.de OI Gogarten, Stephanie/0000-0002-7231-9745; Johnson, Lent/0000-0001-6421-0953 FU NASA [GO-10915, GO-11986, NAS5-26555]; Space Telescope Science Institute [HST-HF-51273.01] FX Support for this work was provided by NASA through grants GO-10915, GO-11986, and Hubble Fellowship grant HST-HF-51273.01 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 43 TC 8 Z9 8 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 JUN 10 PY 2011 VL 734 IS 1 AR L22 DI 10.1088/2041-8205/734/1/L22 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797NV UT WOS:000293135500022 ER PT J AU Chatterjee, R Marscher, AP Jorstad, SG Markowitz, A Rivers, E Rothschild, RE McHardy, IM Aller, MF Aller, HD Lahteenmaki, A Tornikoski, M Harrison, B Agudo, I Gomez, JL Taylor, BW Gurwell, M AF Chatterjee, Ritaban Marscher, Alan P. Jorstad, Svetlana G. Markowitz, Alex Rivers, Elizabeth Rothschild, Richard E. McHardy, Ian M. Aller, Margo F. Aller, Hugh D. Lahteenmaki, Anne Tornikoski, Merja Harrison, Brandon Agudo, Ivan Gomez, Jose L. Taylor, Brian W. Gurwell, Mark TI CONNECTION BETWEEN THE ACCRETION DISK AND JET IN THE RADIO GALAXY 3C 111 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; galaxies: individual (3C 120); quasars: general; X-rays: binaries; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; RAY-TIMING-EXPLORER; POWER-DENSITY SPECTRUM; BLACK-HOLE MASSES; X-RAY; SEYFERT-1 GALAXIES; POLARIMETRIC OBSERVATIONS; MOLECULAR CLOUDS; HIGH-FREQUENCIES; SCALE STRUCTURE AB We present the results of extensive multi-frequency monitoring of the radio galaxy 3C 111 between 2004 and 2010 at X-ray (2.4-10 keV), optical (R band), and radio (14.5, 37, and 230 GHz) wave bands, as well as multi-epoch imaging with the Very Long Baseline Array (VLBA) at 43 GHz. Over the six years of observation, significant dips in the X-ray light curve are followed by ejections of bright superluminal knots in the VLBA images. This shows a clear connection between the radiative state near the black hole, where the X-rays are produced, and events in the jet. The X-ray continuum flux and Fe line intensity are strongly correlated, with a time lag shorter than 90 days and consistent with zero. This implies that the Fe line is generated within 90 lt-day of the source of the X-ray continuum. The power spectral density function of X-ray variations contains a break, with a steeper slope at shorter timescales. The break timescale of 13(6)(+12) days is commensurate with scaling according to the mass of the central black hole based on observations of Seyfert galaxies and black hole X-ray binaries (BHXRBs). The data are consistent with the standard paradigm, in which the X-rays are predominantly produced by inverse Compton scattering of thermal optical/UV seed photons from the accretion disk by a distribution of hot electrons-the corona-situated near the disk. Most of the optical emission is generated in the accretion disk due to reprocessing of the X-ray emission. The relationships that we have uncovered between the accretion disk and the jet in 3C 111, as well as in the Fanaroff-Riley class I radio galaxy 3C 120 in a previous paper, support the paradigm that active galactic nuclei and Galactic BHXRBs are fundamentally similar, with characteristic time and size scales proportional to the mass of the central black hole. C1 [Chatterjee, Ritaban] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Marscher, Alan P.; Jorstad, Svetlana G.; Harrison, Brandon; Agudo, Ivan; Taylor, Brian W.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, Svetlana G.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Markowitz, Alex; Rivers, Elizabeth; Rothschild, Richard E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [McHardy, Ian M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Aller, Margo F.; Aller, Hugh D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lahteenmaki, Anne; Tornikoski, Merja] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Agudo, Ivan; Gomez, Jose L.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Taylor, Brian W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chatterjee, R (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA. EM ritaban.chatterjee@yale.edu RI Lahteenmaki, Anne/L-5987-2013; Agudo, Ivan/G-1701-2015; Jorstad, Svetlana/H-6913-2013 OI Agudo, Ivan/0000-0002-3777-6182; Jorstad, Svetlana/0000-0001-9522-5453 FU National Science Foundation (NSF) [AST-0406865, AST-0907893]; NASA [NNX08AJ64G, NNX08AY06G]; BU; Lowell Observatory; University of Michigan; UK Science and Technology Facilities Council; Academy of Finland; Spanish Ministry of Science and Innovation [AYA2007-67627-C03-03, AYA2010-14844]; Regional Government of Andalucia (Spain) [P09-FQM-4784]; MICIIN (Spain) [AYA2007-67627-C03-03, AYA2010-14844]; CEIC (Andalucia) [P09-FQM-4784]; Smithsonian Institution; Academia Sinica FX We thank the anonymous referee for many useful comments which helped to improve the quality of the manuscript and for the suggestion to include the data tables. The research at Boston University (BU) was funded in part by the National Science Foundation (NSF) through grants AST-0406865 and AST-0907893 and by NASA through Astrophysical Data Analysis Program grant NNX08AJ64G and XMM-Newton grant NNX08AY06G. 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. The University of Michigan Radio Astronomy Observatory is supported by funds from the NSF, NASA, and the University of Michigan. The VLBA is an instrument of the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Liverpool Telescope is 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 Metsahovi team acknowledges the support from the Academy of Finland. The research at IAA-CSIC is supported by the Spanish Ministry of Science and Innovation grants AYA2007-67627-C03-03 and AYA2010-14844, and by the Regional Government of Andalucia (Spain) grant P09-FQM-4784. 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) grants AYA2007-67627-C03-03 and AYA2010-14844, and by CEIC (Andalucia) grant P09-FQM-4784. 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 82 TC 43 Z9 43 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 JUN 10 PY 2011 VL 734 IS 1 AR 43 DI 10.1088/0004-637X/734/1/43 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OS UT WOS:000291026900043 ER PT J AU France, K Schindhelm, E Burgh, EB Herczeg, GJ Harper, GM Brown, A Green, JC Linsky, JL Yang, H Abgrall, H Ardila, DR Bergin, E Bethell, T Brown, JM Calvet, N Espaillat, C Gregory, SG Hillenbrand, LA Hussain, G Ingleby, L Johns-Krull, CM Roueff, E Valenti, JA Walter, FM AF France, Kevin Schindhelm, Eric Burgh, Eric B. Herczeg, Gregory J. Harper, Graham M. Brown, Alexander Green, James C. Linsky, Jeffrey L. Yang, Hao Abgrall, Herve Ardila, David R. Bergin, Edwin Bethell, Thomas Brown, Joanna M. Calvet, Nuria Espaillat, Catherine Gregory, Scott G. Hillenbrand, Lynne A. Hussain, Gaitee Ingleby, Laura Johns-Krull, Christopher M. Roueff, Evelyne Valenti, Jeff A. Walter, Frederick M. TI THE FAR-ULTRAVIOLET "CONTINUUM" IN PROTOPLANETARY DISK SYSTEMS. II. CARBON MONOXIDE FOURTH POSITIVE EMISSION AND ABSORPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; stars: individual (HN Tau, RECX-11, V4046 Sgr) ID T-TAURI-STARS; HUBBLE-SPACE-TELESCOPE; MOLECULAR-HYDROGEN EMISSION; ETA-CHAMAELEONTIS CLUSTER; FLUORESCENT H-2 EMISSION; PLANET-FORMING REGION; TWIN YOUNG SUNS; CIRCUMSTELLAR DISKS; BETA-PICTORIS; PHOTODISSOCIATION REGIONS AB We exploit the high sensitivity and moderate spectral resolution of the Hubble Space Telescope Cosmic Origins Spectrograph to detect far-ultraviolet (UV) spectral features of carbon monoxide (CO) present in the inner regions of protoplanetary disks for the first time. We present spectra of the classical T Tauri stars HN Tau, RECX-11, and V4046 Sgr, representative of a range of CO radiative processes. HN Tau shows CO bands in absorption against the accretion continuum. The CO absorption most likely arises in warm inner disk gas. We measure a CO column density and rotational excitation temperature of N(CO) = (2 +/- 1) x 10(17) cm(-2) and T-rot(CO) 500 +/- 200 K for the absorbing gas. We also detect CO A-X band emission in RECX-11 and V4046 Sgr, excited by UV line photons, predominantly H I Ly alpha. All three objects show emission from CO bands at lambda > 1560 angstrom, which may be excited by a combination of UV photons and collisions with non-thermal electrons. In previous observations these emission processes were not accounted for due to blending with emission from the accretion shock, collisionally excited H-2, and photo-excited H-2, all of which appeared as a "continuum" whose components could not be separated. The CO emission spectrum is strongly dependent upon the shape of the incident stellar Ly alpha emission profile. We find CO parameters in the range: N(CO) similar to 10(18)-10(19) cm(-2), T-rot(CO) greater than or similar to 300 K for the Ly alpha-pumped emission. We combine these results with recent work on photo-excited and collisionally excited H-2 emission, concluding that the observations of UV-emitting CO and H-2 are consistent with a common spatial origin. We suggest that the CO/H-2 ratio (= N(CO)/N(H-2)) in the inner disk is similar to 1, a transition between the much lower interstellar value and the higher value observed in solar system comets today, a result that will require future observational and theoretical study to confirm. C1 [France, Kevin; Schindhelm, Eric; Burgh, Eric B.; Brown, Alexander; Green, James C.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Herczeg, Gregory J.; Brown, Joanna M.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Harper, Graham M.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. [Linsky, Jeffrey L.; Yang, Hao] Univ Colorado, JILA, Boulder, CO 80309 USA. [Linsky, Jeffrey L.; Yang, Hao] NIST, Boulder, CO 80309 USA. [Abgrall, Herve; Roueff, Evelyne] Observ Paris, Sect Meudon, CNRS, UMR 8102, F-92195 Meudon, France. [Abgrall, Herve; Roueff, Evelyne] Observ Paris, Sect Meudon, LUTH, F-92195 Meudon, France. [Ardila, David R.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Bergin, Edwin; Bethell, Thomas; Calvet, Nuria; Ingleby, Laura] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Espaillat, Catherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gregory, Scott G.; Hillenbrand, Lynne A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Hussain, Gaitee] ESO, D-85748 Garching, Germany. [Johns-Krull, Christopher M.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Valenti, Jeff A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Walter, Frederick M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. RP France, K (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA. EM kevin.france@colorado.edu RI Yang, Hao/F-8396-2014; OI Yang, Hao/0000-0002-9423-2333; Gregory, Scott/0000-0003-3674-5568; Herczeg, Gregory/0000-0002-7154-6065 FU NASA [NAS 5-26555, NNX08AC146, NAS5-98043]; STScI [GO-11616] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.; K.F. thanks Roxana Lupu for enjoyable discussions regarding the far-UV spectrum of CO. This work was support by NASA grants NNX08AC146 and NAS5-98043 to the University of Colorado at Boulder and STScI grants to program GO-11616. NR 98 TC 30 Z9 30 U1 0 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2011 VL 734 IS 1 AR 31 DI 10.1088/0004-637X/734/1/31 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OS UT WOS:000291026900031 ER PT J AU Lee, CW Myers, PC AF Lee, Chang Won Myers, Philip C. TI INTERNAL MOTIONS IN STARLESS DENSE CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: kinematics and dynamics ID LOW-LUMINOSITY OBJECT; SPITZER C2D SURVEY; INFALL MOTIONS; DYNAMICAL STATE; INWARD MOTIONS; CLOUD CORES; CS 2-1; N2H+; IONIZATION; PROTOSTARS AB This paper discusses the statistics of internal motions in starless dense cores and the relation of these motions to core density and evolution. Four spectral lines from three molecular species are analyzed from single-pointing and mapped observations of several tens of starless cores. Blue asymmetric profiles are dominant, indicating that inward motions are prevalent in sufficiently dense starless cores. These blue profiles are found to be more abundant, and their asymmetry is bluer, at core positions with stronger N2H+ line emission or higher column density. Thirty-three starless cores are classified into four different types according to the blueshift and redshift of the lines in their molecular line maps. Among these cores, contracting motions dominate: 19 are classified as contracting, 3 as oscillating, 3 as expanding, and 8 as static. Contracting cores have inward motions all over the core with those motions predominating near the region of peak density. Cores with the bluest asymmetry tend to have greater column density than other cores and all five cores with peak column density > 6 x 10(21) cm(-2) are found to be contracting. This suggests that starless cores are likely to have contracting motions if they are sufficiently condensed. Our classification of the starless cores may indicate a sequence of core evolution in the sense that column density increases from static to contracting cores: the static cores in the earliest stage, the expanding and/or the oscillating cores in the next, and the contracting cores in the latest stage. C1 [Lee, Chang Won] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, CW (reprint author), Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Taejon 305348, South Korea. EM cwl@kasi.re.kr FU Ministry of Education, Science, and Technology [2010-0011605] FX This research was supported by Basic Science Research Program though the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science, and Technology (2010-0011605). NR 32 TC 17 Z9 17 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 JUN 10 PY 2011 VL 734 IS 1 AR 60 DI 10.1088/0004-637X/734/1/60 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OS UT WOS:000291026900060 ER PT J AU Shafter, AW Darnley, MJ Hornoch, K Filippenko, AV Bode, MF Ciardullo, R Misselt, KA Hounsell, RA Chornock, R Matheson, T AF Shafter, A. W. Darnley, M. J. Hornoch, K. Filippenko, A. V. Bode, M. F. Ciardullo, R. Misselt, K. A. Hounsell, R. A. Chornock, R. Matheson, T. TI A SPECTROSCOPIC AND PHOTOMETRIC SURVEY OF NOVAE IN M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M31); novae, cataclysmic variables ID AGAPE MICROLENSING SURVEY; LOCAL GROUP GALAXIES; CLASSICAL NOVAE; SPATIAL-DISTRIBUTION; MAXIMUM MAGNITUDE; POPULATION; TELESCOPE; M-31; FIELD; DISK AB We report the results of a multi-year spectroscopic and photometric survey of novae in M31 that resulted in a total of 53 spectra of 48 individual nova candidates. Two of these, M31N 1995-11e and M31N 2007-11g, were revealed to be long-period Mira variables, not novae. These data double the number of spectra extant for novae in M31 through the end of 2009 and bring to 91 the number of M31 novae with known spectroscopic classifications. We find that 75 novae (82%) are confirmed or likely members of the Fe II spectroscopic class, with the remaining 16 novae (18%) belonging to the He/N (and related) classes. These numbers are consistent with those found for Galactic novae. We find no compelling evidence that spectroscopic class depends sensitively on spatial position or population within M31 (i.e., bulge versus disk), although the distribution for He/N systems appears slightly more extended than that for the Fe II class. We confirm the existence of a correlation between speed class and ejection velocity (based on line width), as in the case of Galactic novae. Follow-up photometry allowed us to determine light-curve parameters for a total of 47 of the 91 novae with known spectroscopic class. We confirm that more luminous novae generally fade the fastest and that He/N novae are typically faster and brighter than their Fe II counterparts. In addition, we find a weak dependence of nova speed class on position in M31, with the spatial distribution of the fastest novae being slightly more extended than that of slower novae. C1 [Shafter, A. W.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Darnley, M. J.; Bode, M. F.; Hounsell, R. A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Hornoch, K.] Acad Sci Czech Republic, Astron Inst, CZ-25165 Ondrejov, Czech Republic. [Filippenko, A. V.; Chornock, R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Ciardullo, R.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Misselt, K. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matheson, T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Shafter, AW (reprint author), San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. FU National Science Foundation [AST-0908886, AST-0607682, AST-1009566]; TABASGO Foundation FX Finally, we thank the following individuals for contributing images of M31: V. L. Afanasiev, Z. Bardon, M. Burleigh, P. Cagas, S. Casewell, S. N. Dodonov, T. Farnham, A. Galad, J. Gallagher, P. Garnavich, J. Gorosabel, T. Henych, M. Jelinek, A. Karska, C. Kennedy, R. Khan, P. Kubanek, P. Kusnirak, D. Mackey, K. Morhig, B. Mueller, O. Pejcha, J. Prieto, N. Samarasinha, L. Sarounova, P. Sedinova, O. N. Sholukhova, K. Thorne, B. Tucker, M. Tukinska, A. Valeev, M. Wolf, and P. Zasche. We are also grateful to the following for assistance with the Lick spectroscopic observations and reductions: A. Coil, R. J. Foley, M. Ganeshalingam, S. Jha, L. C. Ho, J. Hoffman, D. C. Leonard, W. Li, M. Papenkova, F. J. D. Serduke, J. C. Shields, and J. M. Silverman. Photometric reduction software was kindly provided by P. Cagas (SIMS), F. Hroch (Munipack), and M. Velen and P. Pravec (Aphot). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. A.V.F.'s group at UC Berkeley is grateful for the financial support of the National Science Foundation (most recently through grant AST-0908886) and the TABASGO Foundation. A.W.S. is grateful to the University of Victoria for hospitality during a recent sabbatical leave while this work was being completed, and to the NSF for financial support through grants AST-0607682 and AST-1009566. NR 118 TC 37 Z9 37 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2011 VL 734 IS 1 AR 12 DI 10.1088/0004-637X/734/1/12 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OS UT WOS:000291026900012 ER PT J AU Shivvers, I Berger, E AF Shivvers, I. Berger, E. TI A BEAMING-INDEPENDENT ESTIMATE OF THE ENERGY DISTRIBUTION OF LONG GAMMA-RAY BURSTS: INITIAL RESULTS AND FUTURE PROSPECTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; radiation mechanisms: non-thermal ID BROAD-BAND OBSERVATIONS; HOST GALAXY; X-RAY; OPTICAL AFTERGLOW; RADIO AFTERGLOW; CALORIMETRY; ENERGETICS; MODEL; GRB-030329; GRB-980703 AB We present single-epoch radio afterglow observations of 24 long-duration gamma-ray burst (GRB) on a timescale of greater than or similar to 100 days after the burst. These observations trace the afterglow evolution when the blast wave has decelerated to mildly or non-relativistic velocities and has roughly isotropized. We infer beaming-independent kinetic energies using the Sedov-Taylor self-similar solution, and find a median value for the sample of detected bursts of about 7x10(51) erg, with a 90% confidence range of 1.1x10(50)-3.3x10(53) erg. Both the median and 90% confidence range are somewhat larger than the results of multi-wavelength, multi-epoch afterglow modeling (including large beaming corrections), and the distribution of beaming-corrected gamma-ray energies. This is due to bursts in our sample with only a single-frequency observation for which we can only determine an upper bound on the peak of the synchrotron spectrum. This limitation leads to a wider range of allowed energies than for bursts with a well-measured spectral peak. Our study indicates that single-epoch centimeter-band observations covering the spectral peak on a timescale of delta t similar to 1 yr can provide a robust estimate of the total kinetic energy distribution with a small investment of telescope time. The substantial increase in bandwidth of the Expanded Very Large Array (up to 8 GHz simultaneously with full coverage at 1-40 GHz) will provide the opportunity to estimate the kinetic energy distribution of GRBs with only a few hours of data per burst. C1 [Shivvers, I.; Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shivvers, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Shivvers, Isaac/0000-0003-3373-8047 NR 42 TC 14 Z9 14 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2011 VL 734 IS 1 AR 58 DI 10.1088/0004-637X/734/1/58 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OS UT WOS:000291026900058 ER PT J AU Su, YN Surges, V van Ballegooijen, A DeLuca, E Golub, L AF Su, Yingna Surges, Vincent van Ballegooijen, Adriaan DeLuca, Edward Golub, Leon TI OBSERVATIONS AND MAGNETIC FIELD MODELING OF THE FLARE/CORONAL MASS EJECTION EVENT ON 2010 APRIL 8 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun: flares; Sun: magnetic topology; Sun: UV radiation; Sun: X-rays, gamma rays ID 3-DIMENSIONAL MHD SIMULATION; ACTIVE-REGION 10953; RAY TELESCOPE XRT; FLUX-ROPE; KINK INSTABILITY; NUMERICAL-SIMULATION; SOLAR PROMINENCES; DRIVEN EVOLUTION; HELMET STREAMER; OCTOBER 28 AB We present a study of the flare/coronal mass ejection event that occurred in Active Region 11060 on 2010 April 8. This event also involves a filament eruption, EIT wave, and coronal dimming. Prior to the flare onset and filament eruption, both SDO/AIA and STEREO/EUVI observe a nearly horizontal filament ejection along the internal polarity inversion line, where flux cancellations frequently occur as observed by SDO/HMI. Using the flux-rope insertion method developed by van Ballegooijen, we construct a grid of magnetic field models using two magneto-frictional relaxation methods. We find that the poloidal flux is significantly reduced during the relaxation process, though one relaxation method preserves the poloidal flux better than the other. The best-fit pre-flare NLFFF model is constrained by matching the coronal loops observed by SDO/AIA and Hinode/XRT. We find that the axial flux in this model is very close to the threshold of instability. For the model that becomes unstable due to an increase of the axial flux, the reconnected field lines below the X-point closely match the observed highly sheared flare loops at the event onset. The footpoints of the erupting flux rope are located around the coronal dimming regions. Both observational and modeling results support the premise that this event may be initiated by catastrophic loss of equilibrium caused by an increase of the axial flux in the flux rope, which is driven by flux cancellations. C1 [Su, Yingna; Surges, Vincent; van Ballegooijen, Adriaan; DeLuca, Edward; Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Surges, Vincent] Coll St Scholastica, Duluth, MN 55811 USA. RP Su, YN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ynsu@head.cfa.harvard.edu RI Su, Yingna/J-1674-2012; DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; van Ballegooijen, Adriaan/0000-0002-5622-3540 FU NASA [NNM07AB07C]; LMSAL [SP02H1701R]; NSF-REU [ATM-0851866] FX We thank Dr. Bernhard Kliem and the anonymous referee for reading the manuscript, and we greatly appreciate their valuable comments that significantly improved this paper. Y.S. is grateful to Drs. Paolo Grigis and Kathy Reeves for help with data processing and thanks Mr. Alexander Engell for a useful conversation. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and the NSC (Norway). We thank the teams of SDO/AIA, SDO/HMI, STEREO/SECCHI, Hinode/XRT, KSO, SOHO/LASCO, GOES, and SOLIS for providing the valuable data. The STEREO and HMI data are downloaded via the Virtual Solar Observatory and the Joint Science Operations Center. This paper uses data from the CACTus CME catalog, generated and maintained by the SIDC at the Royal Observatory of Belgium. This project is partially supported under contract NNM07AB07C from NASA to the Smithsonian Astrophysical Observatory (SAO) and SP02H1701R from LMSAL to SAO. V.S. is supported under the NSF-REU solar physics program at SAO, grant number ATM-0851866. NR 74 TC 48 Z9 48 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2011 VL 734 IS 1 AR 53 DI 10.1088/0004-637X/734/1/53 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OS UT WOS:000291026900053 ER PT J AU Zenteno, A Song, J Desai, S Armstrong, R Mohr, JJ Ngeow, CC Barkhouse, WA Allam, SS Andersson, K Bazin, G Benson, BA Bertin, E Brodwin, M Buckley-Geer, EJ Hansen, SM High, FW Lin, H Lin, YT Liu, J Rest, A Smith, RC Stalder, B Stark, AA Tucker, DL Yang, Y AF Zenteno, A. Song, J. Desai, S. Armstrong, R. Mohr, J. J. Ngeow, C. -C. Barkhouse, W. A. Allam, S. S. Andersson, K. Bazin, G. Benson, B. A. Bertin, E. Brodwin, M. Buckley-Geer, E. J. Hansen, S. M. High, F. W. Lin, H. Lin, Y. -T. Liu, J. Rest, A. Smith, R. C. Stalder, B. Stark, A. A. Tucker, D. L. Yang, Y. TI A MULTIBAND STUDY OF THE GALAXY POPULATIONS OF THE FIRST FOUR SUNYAEV-ZEL'DOVICH EFFECT SELECTED GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: evolution; galaxies: formation ID NEAR-INFRARED PROPERTIES; BAND LUMINOSITY FUNCTION; SOUTH-POLE TELESCOPE; HALO OCCUPATION DISTRIBUTION; X-RAY-PROPERTIES; TO-LIGHT RATIOS; REDSHIFT SURVEY; STAR-FORMATION; RED-SEQUENCE; SKY SURVEY AB We present first results of an examination of the optical properties of the galaxy populations in Sunyaev-Zel'dovich Effect (SZE) selected galaxy clusters. Using clusters selected by the South Pole Telescope survey and deep multiband optical data from the Blanco Cosmology Survey, we measure the radial profile, the luminosity function (LF), the blue fraction, and the halo occupation number (HON) of the galaxy populations of these four clusters with redshifts ranging from 0.3 to 1. Our goal is to understand whether there are differences among the galaxy populations of these SZE-selected clusters and previously studied clusters selected in the optical and the X-ray. The radial distributions of galaxies in the four systems are consistent with Navarro-Frenk-White profiles with a galaxy concentration of 3 to 6. We show that the characteristic luminosities in griz bands are consistent with passively evolving populations emerging from a single burst at redshift z = 3. The faint-end power-law slope of the LF is found to be on average alpha approximate to -1.2 in griz. HONs (to m* + 2) for these systems appear to be consistent with those based on X-ray-selected clusters. The blue fraction estimated to 0.36 L*, for the three lower redshift systems, suggests an increase with redshift, although with the current sample the uncertainties are still large. Overall, this pilot study of the first four clusters provides no evidence that the galaxy populations in these systems differ significantly from those in previously studied cluster populations selected in the X-ray or the optical. C1 [Zenteno, A.; Mohr, J. J.; Andersson, K.; Bazin, G.; Liu, J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Zenteno, A.; Mohr, J. J.; Bazin, G.; Liu, J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Desai, S.; Ngeow, C. -C.; Yang, Y.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Desai, S.; Armstrong, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Ngeow, C. -C.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taiwan. [Barkhouse, W. A.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA. [Allam, S. S.; Buckley-Geer, E. J.; Lin, H.; Tucker, D. L.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Benson, B. A.; High, F. W.; Liu, J.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Bertin, E.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Brodwin, M.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hansen, S. M.] Univ Calif Santa Cruz, Observ & Dept Astron, Santa Cruz, CA 95064 USA. [High, F. W.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Lin, Y. -T.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan. [Lin, Y. -T.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Smith, R. C.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Stalder, B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Zenteno, A (reprint author), Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany. OI Tucker, Douglas/0000-0001-7211-5729; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937, PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; Excellence Cluster Universe in Garching; Smithsonian Astrophysical Observatory [SV4-74018, A31]; W. M. Keck Foundation; Brinson Foundation FX The South Pole Telescope is supported by the National Science Foundation through grant ANT-0638937. 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. A.Z., J.M., G.B., and J.L. acknowledge the support of the Excellence Cluster Universe in Garching. This paper includes data gathered with the Blanco 4 m telescope, located at the Cerro Tololo Inter-American Observatory in Chile, which is part of the U.S. National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), under contract with the National Science Foundation. This work is based in part on observations obtained with the Chandra X-ray Observatory (CXO), under contract SV4-74018, A31 with the Smithsonian Astrophysical Observatory which operates the CXO for NASA. We are very grateful for the efforts of the Chandra, XMM-Newton, and CTIO support staff without whom this paper would not be possible. Support for M.B. was provided by the W. M. Keck Foundation. B.S. acknowledges support from the Brinson Foundation. NR 96 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 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2011 VL 734 IS 1 AR 3 DI 10.1088/0004-637X/734/1/3 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OS UT WOS:000291026900003 ER PT J AU Petit, RE Harasewych, MG AF Petit, Richard E. Harasewych, M. G. TI A new Sveltia (Gastropoda: Cancellariidae) from off Guadeloupe, French West Indies SO NAUTILUS LA English DT Article DE Pliocene; biogeography; paciphile AB Sveltia yoyottei, the first Recent species of Sveltia from the tropical western Atlantic, is described from bathyal depths off Guadeloupe, French West Indies. It is distinguished from its closest relative, Sveltia inquilinus (Jung and Petit, 1990) from the Pliocene of the Dominican Republic, by its shorter, more gradate spire, its narrower pseudoumbilicus, and by having fewer, stronger denticles along the outer lip. It differs from the Panamic S. centrota (Dall,1896) in having a smaller, narrower shell with 1-3 axial ribs between adjacent varices. C1 [Harasewych, M. G.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Petit, RE (reprint author), 806 St Charles Rd, N Myrtle Beach, SC 29582 USA. EM r.e.petit@att.net FU Guadeloupe, French West Indies FX We are pleased to acknowledge the assistance of Mr. Dominique Lamy of Guadeloupe, French West Indies, who recognized this specimen to be an unkown species and permitted us to publish this description. NR 5 TC 1 Z9 1 U1 0 U2 0 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 JUN 10 PY 2011 VL 125 IS 2 BP 72 EP 74 PG 3 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 780HI UT WOS:000291844700004 ER PT J AU Zavala, J Vogelsberger, M Slatyer, TR Loeb, A Springel, V AF Zavala, Jesus Vogelsberger, Mark Slatyer, Tracy R. Loeb, Abraham Springel, Volker TI Cosmic X-ray and gamma-ray background from dark matter annihilation SO PHYSICAL REVIEW D LA English DT Article ID HALOES; CANDIDATES; SIMULATION; CLUMPINESS; DENSITY; CLUSTER; CHANDRA; ORIGIN; FIELDS; EARTH AB The extragalactic background light (EBL) observed at multiple wavelengths is a promising tool to probe the nature of dark matter. This radiation might contain a significant contribution from gamma-rays produced promptly by dark matter particle annihilation in the many halos and subhalos within our past-light cone. Additionally, the electrons and positrons produced in the annihilation give energy to the cosmic microwave photons to populate the EBL with X-rays and gamma-rays. To study these signals, we create full-sky maps of the expected radiation from both of these contributions using the high-resolution Millennium-II simulation of cosmic structure formation. Our method also accounts for a possible enhancement of the annihilation rate by a Sommerfeld mechanism due to a Yukawa interaction between the dark matter particles prior to annihilation. We use upper limits on the contributions of unknown sources to the EBL to constrain the intrinsic properties of dark matter using a model-independent approach that can be employed as a template to test different particle physics models. These upper limits are based on observational measurements spanning 8 orders of magnitude in energy (from soft X-rays measured by the CHANDRA satellite to gamma-rays measured by the Fermi satellite), and on expectations for the contributions from nonblazar active galactic nuclei, blazars and star-forming galaxies. To exemplify this approach, we analyze a set of benchmark Sommerfeld-enhanced models that give the correct abundance of dark matter, satisfy constraints from the cosmic microwave background, and fit the cosmic ray spectra measured by PAMELA and Fermi without any contribution from local substructure. We find that these models are in conflict with the EBL constraints unless the contribution of unresolved substructure is small and the dark matter annihilation signal dominates the EBL. We conclude that provided the collisionless cold dark matter paradigm is accurate, even for conservative estimates of the contribution from unresolved substructure and astrophysical backgrounds, the EBL is at least as sensitive a probe of these types of scenarios as the cosmic microwave background. More generally, our results disfavor an explanation of the positron excess measured by the PAMELA satellite based only on dark matter annihilation in the smooth Galactic dark matter halo. C1 [Zavala, Jesus] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Zavala, Jesus] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Vogelsberger, Mark; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Slatyer, Tracy R.] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, Astron Recheninst, D-69120 Heidelberg, Germany. RP Zavala, J (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM jzavalaf@uwaterloo.ca FU NSF [AST-0907890, AST-0807444]; NASA [NNX08AL43G, NNA09DB30A]; Institute for Advanced Study; DOE [DE-FG0290ER40542] FX We would like to thank Neal Weiner, Simon D. M. White, Niayesh Afshordi and Mattia Fornasa for interesting comments and suggestions. J. Z. acknowledges financial support by the Joint Postdoctoral Program in Astrophysical Cosmology of the Max Planck Institute for Astrophysics and the Shanghai Astronomical Observatory and from the CITA National Fellows program. This work was supported in part by NSF Grant No. AST-0907890 and NASA Grant No. NNX08AL43G and NNA09DB30A (for A. L.). T. S. gratefully acknowledges support from the Institute for Advanced Study. The research of T. S. is supported by the DOE under Grant No. DE-FG0290ER40542 and the NSF under Grant No. AST-0807444. NR 76 TC 28 Z9 28 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUN 9 PY 2011 VL 83 IS 12 AR 123513 DI 10.1103/PhysRevD.83.123513 PG 19 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 775CL UT WOS:000291435000003 ER PT J AU McClintock, JE Narayan, R Davis, SW Gou, LJ Kulkarni, A Orosz, JA Penna, RF Remillard, RA Steiner, JF AF McClintock, Jeffrey E. Narayan, Ramesh Davis, Shane W. Gou, Lijun Kulkarni, Akshay Orosz, Jerome A. Penna, Robert F. Remillard, Ronald A. Steiner, James F. TI Measuring the spins of accreting black holes SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 19th International Conference on General Relativity and Gravitation (GR19) CY JUL 06-09, 2010 CL Mexico City, MEXICO ID X-RAY BINARIES; QUASI-PERIODIC OSCILLATIONS; MICROQUASAR XTE J1550-564; ACTIVE GALACTIC NUCLEI; M33 X-7; RELATIVISTIC ACCRETION; TRANSIENT A0620-00; ENERGY EXTRACTION; DISK MODELS; HIGH-STATE AB A typical galaxy is thought to contain tens of millions of stellar-mass black holes, the collapsed remnants of once massive stars, and a single nuclear supermassive black hole. Both classes of black holes accrete gas from their environments. The accreting gas forms a flattened orbiting structure known as an accretion disk. During the past several years, it has become possible to obtain measurements of the spins of the two classes of black holes by modeling the x-ray emission from their accretion disks. Two methods are employed, both of which depend upon identifying the inner radius of the accretion disk with the innermost stable circular orbit, whose radius depends only on the mass and spin of the black hole. In the Fe K alpha method, which applies to both classes of black holes, one models the profile of the relativistically broadened iron line with a special focus on the gravitationally redshifted red wing of the line. In the continuum-fitting (CF) method, which has so far only been applied to stellar-mass black holes, one models the thermal x-ray continuum spectrum of the accretion disk. We discuss both methods, with a strong emphasis on the CF method and its application to stellar-mass black holes. Spin results for eight stellar-mass black holes are summarized. These data are used to argue that the high spins of at least some of these black holes are natal, and that the presence or absence of relativistic jets in accreting black holes is not entirely determined by the spin of the black hole. C1 [McClintock, Jeffrey E.; Narayan, Ramesh; Gou, Lijun; Kulkarni, Akshay; Penna, Robert F.; Steiner, James F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Davis, Shane W.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H4, Canada. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Remillard, Ronald A.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP McClintock, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jem@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 80 TC 130 Z9 130 U1 0 U2 10 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 JUN 7 PY 2011 VL 28 IS 11 AR 114009 DI 10.1088/0264-9381/28/11/114009 PG 17 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 766NK UT WOS:000290789800010 ER PT J AU Appelquist, T Babich, R Brower, RC Cheng, M Clark, MA Cohen, SD Fleming, GT Kiskis, J Lin, MF Neil, ET Osborn, JC Rebbi, C Schaich, D Vranas, PM AF Appelquist, T. Babich, R. Brower, R. C. Cheng, M. Clark, M. A. Cohen, S. D. Fleming, G. T. Kiskis, J. Lin, M. F. Neil, E. T. Osborn, J. C. Rebbi, C. Schaich, D. Vranas, P. M. CA Lattice Strong Dynamics LSD TI Parity Doubling and the S Parameter below the Conformal Window SO PHYSICAL REVIEW LETTERS LA English DT Article ID PHYSICS; QCD AB We describe a lattice simulation of the masses and decay constants of the lowest-lying vector and axial resonances, and the electroweak S parameter, in an SU(3) gauge theory with N(f) = 2 and 6 fermions in the fundamental representation. The spectrum becomes more parity doubled and the S parameter per electroweak doublet decreases when N(f) is increased from 2 to 6, motivating study of these trends as N(f) is increased further, toward the critical value for transition from confinement to infrared conformality. C1 [Appelquist, T.; Fleming, G. T.; Lin, M. F.; Neil, E. T.] Yale Univ, Dept Phys, Sloane Lab, New Haven, CT 06520 USA. [Babich, R.; Brower, R. C.; Cohen, S. D.; Rebbi, C.; Schaich, D.] Boston Univ, Dept Phys, Boston, MA 02215 USA. [Cheng, M.; Vranas, P. M.] Lawrence Livermore Natl Lab, Phys Sci Directorate, Livermore, CA 94550 USA. [Clark, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kiskis, J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Osborn, J. C.] Argonne Leadership Comp Facil, Argonne, IL 60439 USA. RP Appelquist, T (reprint author), Yale Univ, Dept Phys, Sloane Lab, New Haven, CT 06520 USA. RI Schaich, David/J-6644-2013; Fleming, George/L-6614-2013; OI Schaich, David/0000-0002-9826-2951; Fleming, George/0000-0002-4987-7167; Cohen, Saul/0000-0001-6804-3320 FU NNSA; Office of Science of the U.S. Department of Energy; U.S. National Science Foundation FX We thank the Aspen Center for Physics, and LLNL Multiprogrammatic and Institutional Computing for BlueGene/L resources. This work was supported by the NNSA and Office of Science of the U.S. Department of Energy, and by the U.S. National Science Foundation. NR 17 TC 25 Z9 25 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 JUN 6 PY 2011 VL 106 IS 23 AR 231601 DI 10.1103/PhysRevLett.106.231601 PG 4 WC Physics, Multidisciplinary SC Physics GA 773NF UT WOS:000291313300002 PM 21770495 ER PT J AU Thorwirth, S Muck, LA Gauss, J Tamassia, F Lattanzi, V McCarthy, MC AF Thorwirth, Sven Mueck, Leonie Anna Gauss, Juergen Tamassia, Filippo Lattanzi, Valerio McCarthy, Michael C. TI Silicon Oxysulfide, OSiS: Rotational Spectrum, Quantum-Chemical Calculations, and Equilibrium Structure SO JOURNAL OF PHYSICAL CHEMISTRY LETTERS LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; ELECTRONIC-STRUCTURE; DIPOLE-MOMENTS; DOUBLE-BOND; PERTURBATION; SPECTROSCOPY; HYDROGEN; SULFIDE; BORON AB Silicon oxysulfide, OSiS, and seven of its minor isotopic species have been characterized for the first time in the gas phase at high spectral resolution by means of Fourier transform microwave spectroscopy. The equilibrium structure of OSiS has been determined from the experimental data using calculated vibration-rotation interaction constants. The structural parameters (r(O-Si) = 1.5064 angstrom and r(Si-S) = 1.9133 angstrom) are in very good agreement with values from high-level quantum chemical calculations using coupled-cluster techniques together with sophisticated additivity and extrapolation schemes. The bond distances in OSiS are very short in comparison with those in SiO and SiS. This unexpected finding is explained by the partial charges calculated for OSiS via a natural population analysis. The results suggest that electrostatic effects rather than multiple bonding are the key factors in determining bonding in this triatomic molecule. The data presented provide the spectroscopic information needed for radio astronomical searches for OSiS. C1 [Thorwirth, Sven] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Mueck, Leonie Anna; Gauss, Juergen] Johannes Gutenberg Univ Mainz, Inst Phys Chem, D-55099 Mainz, Germany. [Tamassia, Filippo] Univ Bologna, Dipartimento Chim Fis & Inorgan, I-40136 Bologna, Italy. [Lattanzi, Valerio; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lattanzi, Valerio; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Thorwirth, S (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM sthorwirth@ph1.uni-koeln.de; gauss@uni-mainz.de; mccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008; Mueck, Leonie/0000-0002-9890-5451 FU Deutsche Forschungsgemeinschaft (DFG) [TH 1301/3-1, GA 370/5-1]; Graduate School of Excellence "MAINZ"; NSF [CHE-1058063]; NASA [NNX08AE05G] FX S.T. and J.G. gratefully acknowledge funding by the Deutsche Forschungsgemeinschaft (DFG) through grants TH 1301/3-1 and GA 370/5-1. L.A.M. is supported by a fellowship from the Graduate School of Excellence "MAINZ". The work in Cambridge is supported by NSF grant no. CHE-1058063 and NASA grant no. NNX08AE05G. NR 32 TC 10 Z9 10 U1 1 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1948-7185 J9 J PHYS CHEM LETT JI J. Phys. Chem. Lett. PD JUN 2 PY 2011 VL 2 IS 11 BP 1228 EP 1231 DI 10.1021/jz200368x PG 4 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Atomic, Molecular & Chemical SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 775YW UT WOS:000291500600001 PM 26295414 ER PT J AU Gingerich, O AF Gingerich, Owen TI Galileo, the Impact of the Telescope, and the Birth of Modern Astronomy SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 USA SN 0003-049X J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD JUN PY 2011 VL 155 IS 2 BP 134 EP 141 PG 8 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 825UN UT WOS:000295307700002 ER PT J AU Ferrari, FD Fornshell, J Vagelli, AA Ivanenko, VN Dahms, HU AF Ferrari, Frank D. Fornshell, John Vagelli, Alejandro A. Ivanenko, V. N. Dahms, Hans-Uwe TI EARLY POST-EMBRYONIC DEVELOPMENT OF MARINE CHELICERATES AND CRUSTACEANS WITH A NAUPLIUS SO CRUSTACEANA LA English DT Article ID LARVAL DEVELOPMENT; PYCNOGONIDA; MORPHOLOGY; EVOLUTION; ONTOGENY; CEPHALOCARIDA; BRANCHIOPODA; SPINICAUDATA; AMMOTHEIDAE; BRANCHIURA AB Crustaceans that hatch as a nauplius-like larva, as well as xiphosuran and pantopodan chelicerates, are surveyed for five characters: presence or absence of arthrodial membranes separating somites; ventral configuration of the protopod of the second limb; number of transformed (segmented) limbs and limb buds; addition of segments to transformed limbs; fate of limb buds. An arthrodial membrane separates somites 7 and 8 of xiphosurans, a small knob articulates on the protopod of the second limb, and there are nine pairs of limbs but no limb buds. During early development, no arthrodial membranes are added, nor are segments added to limbs 1-9; limbs 10-14 are added as transformed limbs, not as limb buds, after several molts. On the post-embryonic larva of the presumed ancestral pantopodan, arthrodial membranes did not separate adjacent somites, the proximal segment of limb 2 was simple, there were three transformed limbs and no limbs buds. During subsequent molts, arthrodial membranes separated somites 4-7, buds of limbs 4-7 were added in register with each molt, limb buds were reorganized in register into transformed limbs during the following molt, and two segments were added to each transformed limb in register during the next molt. Somites of most crustacean taxa that hatch as a nauplius-like larva are not separated by arthrodial membranes on early post-embryonic stages; exceptions are posterior somites of branchiurans, mystacocaridans and cephalocaridans. Limb 2 (antenna 2) of branchiopods, copepods, thecostracans, mystacocaridans and cephalocaridans bears a naupliar arthrite on the ventral face of the coxa, on branchiurans there is an attenuation, or spine-like outgrowth, on the ventral face, and on ostracodes, remipedes, euphausiaceans, mysidaceans and dendrobranchiate decapods there is no ventral structure. Most of these crustaceans hatch with three transformed limbs; exceptions include myodocopan ostracodes with six and branchiurans with seven. The number of limb buds varies from none on remipedes to three on branchiurans and cephalocaridans. Limb buds of podocopan ostracodes, branchiurans, mystacocaridans and cephalocaridans are reorganized into transformed limbs after one molt; reorganization of limb buds of branchiopods, copepods, thecostracans, remipedes, euphausiaceans, mysidaceans and dendrobranchiates are delayed several molts. Early post-embryonic development of pantopodan chelicerates is more similar to that of podocopan ostracodes than it is to that of any other crustacean taxon, and no crustacean exhibits an early post-embryonic development similar to that of xiphosurans. Within the crustacean lineage, articulating somites, a naupliar arthrite or ventral attenuation on the coxa of antenna 2, and delayed reorganization of limb buds are apomorphies. Absence of a naupliar arthrite on ostracodes is inherited from the last stem lineage arthropod but its absence on remipedes and malacostracans is derived, and perhaps more than once. C1 [Ferrari, Frank D.; Fornshell, John] Smithsonian Inst, Natl Museum Nat Hist, MRC 534, IZ MSC, Suitland, MD 20746 USA. [Vagelli, Alejandro A.] New Jersey Acad Aquat Sci, Camden, NJ 08103 USA. [Ivanenko, V. N.] Moscow MV Lomonosov State Univ, Fac Biol, Dept Invertebrate Zool, Moscow 119899, Russia. [Dahms, Hans-Uwe] Sangmyung Univ, Coll Convergence, Green Life Sci Dept, Seoul 110743, South Korea. RP Ferrari, FD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 534, IZ MSC, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM ferrarif@si.edu; johnfornshell@hotmail.com; avagelli@njaas.org; ivanenko@mail.bio.msu.ru; hansdahms@smu.ac.kr RI Ivanenko, Viatcheslav/B-8198-2008 OI Ivanenko, Viatcheslav/0000-0003-1255-0491 FU Smithsonian Institution's Office of Fellowships; Ministry of Education and Science of the Russian Federation FX The Smithsonian Institution's Office of Fellowships supported visits of H.-U.D. and V.N.I.; V.N.I. also was supported by The Ministry of Education and Science of the Russian Federation. We extend special thanks to Lana Ong (National Museum of Natural History, Smithsonian Institution) for specimen and figure preparations and to Scott Whittaker (National Museum of Natural History, Smithsonian Institution) for SEM preparations. Mark J. Grygier (Lake Biwa Museum) provided specimens of thecostracans and Rob Smith (Lake Biwa Museum) answered questions about ostracodes. NR 64 TC 9 Z9 11 U1 1 U2 10 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X J9 CRUSTACEANA JI Crustaceana PD JUN PY 2011 VL 84 IS 7 BP 869 EP 893 DI 10.1163/001121611X579745 PG 25 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 808PA UT WOS:000293989700006 ER PT J AU Zhang, GB Mendez, M Jonker, P Hiemstra, B AF Zhang, Guobao Mendez, Mariano Jonker, Peter Hiemstra, Beike TI The distance and internal composition of the neutron star in EXO 0748-676 with XMM-Newton SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dense matter; equation of state; stars: individual: EXO 0748-676; stars: neutron; X-rays: binaries ID X-RAY BURST; EQUATION-OF-STATE; EXO-0748-676; MASS; CONSTRAINTS; ABUNDANCES; DISCOVERY; SPECTRA; MATTER AB Recently, the neutron star X-ray binary EXO 0748-676 underwent a transition to quiescence. We analysed an XMM-Newton observation of this source in quiescence, where we fitted the spectrum with two different neutron star atmosphere models. From the fits we constrained the allowed parameter space in the mass-radius diagram for this source for an assumed range of distances to the system. Comparing the results with different neutron star equations of state, we constrained the distance to EXO 0748-676. We found that strange quark matter equation of state is consistent with the mass and radius from our fits only if EXO 0748-676 is at a distance of less than 5 kpc, whereas the normal neutron star equation of state is consistent with our best-fitting mass and radius if the distance is similar to 7 kpc, as deduced from properties of the X-ray bursts. C1 [Zhang, Guobao; Mendez, Mariano; Hiemstra, Beike] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Jonker, Peter] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, Peter] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. RP Zhang, GB (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM zhang@astro.rug.nl RI Mendez, Mariano/C-8011-2012 OI Mendez, Mariano/0000-0003-2187-2708 FU Netherlands Organisation for Scientific Research FX This work is based on the observations obtained from XMM-Newton. We acknowledge an anonymous referee for useful comments. PJ acknowledges support from a VIDI grant from the Netherlands Organisation for Scientific Research. NR 22 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2011 VL 414 IS 2 BP 1077 EP 1081 DI 10.1111/j.1365-2966.2011.18443.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 792JS UT WOS:000292740500019 ER PT J AU Mullaney, JR Alexander, DM Goulding, AD Hickox, RC AF Mullaney, J. R. Alexander, D. M. Goulding, A. D. Hickox, R. C. TI Defining the intrinsic AGN infrared spectral energy distribution and measuring its contribution to the infrared output of composite galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: general; galaxies: Seyfert; infrared: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY CORRELATION; HIGH-RESOLUTION SPECTROSCOPY; SUPERMASSIVE BLACK-HOLES; DEEP FIELD-SOUTH; SEYFERT-GALAXIES; LUMINOSITY FUNCTION; NEARBY GALAXIES; HOST GALAXIES; COSMOLOGICAL EVOLUTION AB We use infrared spectroscopy and photometry to empirically define the intrinsic mid- to far-infrared spectral energy distribution (i.e. 6-100 mu m SED) of thermal emission produced by typical (i.e. 2-10 keV luminosity, L2-10 keV similar to 10(42)-10(44) erg s(-1)) active galactic nuclei (hereafter AGNs). The average infrared SED of typical AGNs is best described as a broken power law at less than or similar to 40 mu m that falls steeply at greater than or similar to 40 mu m (i.e. at far-infrared wavelengths). Despite this fall-off at long wavelengths, at least three of the 11 AGNs in our sample have demonstrated SEDs that are AGN dominated even at 60 mu m, demonstrating the importance of accounting for any AGN contribution when calculating galaxy infrared luminosities. We find that the average intrinsic AGN 6-100 mu m SED gets bluer with increasing X-ray luminosity - a trend seen both within our sample and also when we compare it with the intrinsic SEDs of more luminous quasars (i.e. L2-10 keV greater than or similar to 10(44) erg s(-1)). The range of intrinsic AGN SEDs is more closely matched by clumpy, rather than continuous, torus models. Using our intrinsic AGN SEDs we define a set of correction factors to convert either monochromatic infrared or X-ray luminosities into total (i.e. 8-1000 mu m) AGN infrared luminosities. We outline a procedure that uses our newly defined intrinsic AGN infrared SEDs, in conjunction with a selection of host-galaxy templates, to measure the AGN contribution to the infrared output of composite galaxies from photometry alone. We verify the accuracy of our SED-fitting procedure by comparing our results to two independent measures of AGN contribution: (1) 12-mu m luminosities obtained from high spatial resolution observations of nearby galaxies and (2) the equivalent width of the 11.25-mu m PAH feature. Our SED-fitting procedure opens up the possibility of measuring the intrinsic AGN luminosities for large numbers of galaxies with well-sampled infrared data (e.g. IRAS, ISO, Spitzer and Herschel). C1 [Mullaney, J. R.; Alexander, D. M.; Goulding, A. D.; Hickox, R. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Mullaney, J. R.] Univ Paris Diderot, CNRS, CEA DSM Irfu, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Goulding, A. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mullaney, JR (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM james.r.mullaney@gmail.com OI Alexander, David/0000-0002-5896-6313 FU Eurotalents Fellowship Program; Leverhulme Trust; Royal Society; STFC; NASA; JPL/Caltech FX We would like to thank D. Elbaz and K. M. Dasyra for their useful comments on the paper. Furthermore, we would like to thank the referee, H. Netzer, for his comments, which significantly improved the quality of the paper. We gratefully acknowledge support from the Eurotalents Fellowship Program (JRM) the Leverhulme Trust (JRM; DMA), the Royal Society (DMA), an STFC Studentship (ADG) and an STFC Postdoctoral Fellowship (RCH). This work is based (in part) on observations made with the Spitzer Space Telescope and has made use of the NASA/IPAC Infrared Science Archive, both of which are 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 73 TC 178 Z9 178 U1 2 U2 4 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 JUN PY 2011 VL 414 IS 2 BP 1082 EP 1110 DI 10.1111/j.1365-2966.2011.18448.x PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 792JS UT WOS:000292740500020 ER PT J AU Kulkarni, AK Penna, RF Shcherbakov, RV Steiner, JF Narayan, R Sadowski, A Zhu, YC McClintock, JE Davis, SW McKinney, JC AF Kulkarni, Akshay K. Penna, Robert F. Shcherbakov, Roman V. Steiner, James F. Narayan, Ramesh Sadowski, Aleksander Zhu, Yucong McClintock, Jeffrey E. Davis, Shane W. McKinney, Jonathan C. TI Measuring black hole spin by the continuum-fitting method: effect of deviations from the Novikov-Thorne disc model SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; MHD; methods: numerical; X-rays: binaries ID THIN ACCRETION DISK; X-RAY CONTINUUM; MAGNETOHYDRODYNAMIC SIMULATIONS; VERTICAL STRUCTURE; IRON LINES; INNER-DISK; SLIM DISKS; SPECTRA; BINARIES; SYSTEMS AB The X-ray spectra of accretion discs of eight stellar mass black holes have been analysed to date using the thermal continuum-fitting method, and the spectral fits have been used to estimate the spin parameters of the black holes. However, the underlying model used in this method of estimating spin is the general relativistic thin-disc model of Novikov & Thorne, which is only valid for razor-thin discs. We therefore expect errors in the measured values of spin due to inadequacies in the theoretical model. We investigate this issue by computing spectra of numerically calculated models of thin accretion discs around black holes, obtained via three-dimensional general relativistic magnetohydrodynamic (GRMHD) simulations. We apply the continuum-fitting method to these computed spectra to estimate the black hole spins and check how closely the values match the actual spin used in the GRMHD simulations. We find that the error in the dimensionless spin parameter is up to about 0.2 for a non-spinning black hole, depending on the inclination. For black holes with spins of 0.7, 0.9 and 0.98, the errors are up to about 0.1, 0.03 and 0.01, respectively. These errors are comparable to or smaller than those arising from current levels of observational uncertainty. Furthermore, we estimate that the GRMHD simulated discs from which these error estimates are obtained correspond to effective disc luminosities of about 0.4-0.7 Eddington, and that the errors will be smaller for discs with luminosities of 0.3 Eddington or less, which are used in the continuum-fitting method. We thus conclude that use of the Novikov-Thorne thin-disc model does not presently limit the accuracy of the continuum-fitting method of measuring black hole spin. C1 [Kulkarni, Akshay K.; Penna, Robert F.; Shcherbakov, Roman V.; Steiner, James F.; Narayan, Ramesh; Zhu, Yucong; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sadowski, Aleksander] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Davis, Shane W.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H4, Canada. [McKinney, Jonathan C.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [McKinney, Jonathan C.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RP Kulkarni, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM akulkarni@cfa.harvard.edu; rpenna@cfa.harvard.edu; rshcherbakov@cfa.harvard.edu; jsteiner@cfa.harvard.edu; rnarayan@cfa.harvard.edu; as@camk.edu.pl; yzhu@cfa.harvard.edu; jem@head.cfa.harvard.edu; swd@cita.utoronto.ca; jmckinne@stanford.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX08AH32G]; NSF [AST-0805832] FX The authors wish to thank Jason Dexter for a critical reading of the manuscript, and the referee for several comments that helped improve the paper. This work was supported by NASA grant NNX08AH32G and NSF grant AST-0805832. The simulations presented in this work were performed using resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, and TeraGrid resources provided by the National Institute for Computational Sciences (NICS). NR 57 TC 47 Z9 47 U1 0 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 JUN PY 2011 VL 414 IS 2 BP 1183 EP 1194 DI 10.1111/j.1365-2966.2011.18446.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 792JS UT WOS:000292740500027 ER PT J AU Pont, F Husnoo, N Mazeh, T Fabrycky, D AF Pont, Frederic Husnoo, Nawal Mazeh, Tsevi Fabrycky, Daniel TI Determining eccentricities of transiting planets: a divide in the mass-period plane SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planetary systems ID OBSERVATIONAL EVIDENCE; EXTRASOLAR PLANETS; HOT JUPITERS; EXOPLANETS; ORBIT; SYSTEMS; BINARIES; WASP-12B; GJ-436 AB The two dominant features in the distribution of orbital parameters for close-in exoplanets are the prevalence of circular orbits for very short periods, and the observation that planets on closer orbits tend to be heavier. The first feature is interpreted as a signature of tidal evolution, while the origin of the second, a 'mass-period relation' for hot Jupiters, is not understood. In this paper we reconsider the ensemble properties of transiting exoplanets with well-measured parameters, focusing on orbital eccentricity and the mass-period relation. We recalculate the constraints on eccentricity in a homogeneous way, using new radial velocity data, with particular attention to statistical biases. We find that planets on circular orbits gather in a well-defined region of the mass-period plane, close to the minimum period for any given mass. Exceptions to this pattern reported in the literature can be attributed to statistical biases. The ensemble data is compatible with classical tide theory with orbital circularization caused by tides raised on the planet, and suggest that tidal circularization and the stopping mechanisms for close-in planets are closely related to each other. The position mass-period relation is compatible with a relation between a planet's Hill radius and its present orbit. C1 [Pont, Frederic; Husnoo, Nawal] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Mazeh, Tsevi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Fabrycky, Daniel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pont, F (reprint author), Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. EM fpont@astro.ex.ac.uk OI Fabrycky, Daniel/0000-0003-3750-0183 FU UK STFC [F011083/1]; Israel Science Foundation [655/07]; NASA FX This research was supported by the UK STFC (FP; grant F011083/1), the Israel Science Foundation (TM; grant 655/07) and by NASA (DF; Michelson fellowship). The authors thank the anonymous referee for useful comments that helped improve the manuscript. NR 42 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 JUN PY 2011 VL 414 IS 2 BP 1278 EP 1284 DI 10.1111/j.1365-2966.2011.18462.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 792JS UT WOS:000292740500034 ER PT J AU Boylan-Kolchin, M Besla, G Hernquist, L AF Boylan-Kolchin, Michael Besla, Gurtina Hernquist, Lars TI Dynamics of the Magellanic Clouds in a Lambda cold dark matter universe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxy: formation; Galaxy: fundamental parameters; galaxies: formation; galaxies: kinematics and dynamics; Magellanic Clouds ID DIGITAL SKY SURVEY; N-BODY SIMULATIONS; MILKY-WAY; PROPER-MOTION; LOCAL GROUP; HALO MASS; VELOCITY DISPERSION; ORBITAL PARAMETERS; ANGULAR-MOMENTUM; DENSITY PROFILE AB We examine Milky Way-Magellanic Cloud systems selected from the Millennium-II Simulation in order to place the orbits of the Magellanic Clouds in a cosmological context. Our analysis shows that satellites massive enough to be LMC analogues are typically accreted at late times. Moreover, those that are accreted at early times and survive to the present have orbital properties that are discrepant with those observed for the LMC. The high velocity of the LMC, coupled with the dearth of unbound orbits seen in the simulation, argues that the mass of the MW's halo is unlikely to be less than 2 x 10(12) M-circle dot. This conclusion is further supported by statistics of haloes hosting satellites with masses, velocities and separations comparable to those of the LMC. We further show that: (1) LMC and SMC-mass objects are not particularly uncommon in MW-mass haloes; (2) the apparently high angular momentum of the LMC is not cosmologically unusual; and (3) it is rare for a MW halo to host a LMC-SMC binary system at z = 0, but high speed binary pairs accreted at late times are possible. Based on these results, we conclude that the LMC was accreted within the past four Gyr and is currently making its first pericentric passage about the MW. C1 [Boylan-Kolchin, Michael] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Boylan-Kolchin, Michael] Univ Calif Irvine, Ctr Galaxy Evolut, Irvine, CA 92697 USA. [Besla, Gurtina; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Boylan-Kolchin, M (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. EM m.bk@uci.edu OI Boylan-Kolchin, Michael/0000-0002-9604-343X NR 67 TC 52 Z9 52 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2011 VL 414 IS 2 BP 1560 EP 1572 DI 10.1111/j.1365-2966.2011.18495.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 792JS UT WOS:000292740500058 ER PT J AU Balberg, S Loeb, A AF Balberg, Shmuel Loeb, Abraham TI Supernova shock breakout through a wind SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; supernovae: general; supernovae: individual: SN 2008D; stars: winds, outflows ID RADIATION MEDIATED SHOCKS; CORE-COLLAPSE SUPERNOVAE; RAY TRANSIENT 080109; 2008D; EVOLUTION; EMISSION; WAVES; GALEX; NOVAE; STAR AB The breakout of a supernova shock wave through the progenitor star's outer envelope is expected to appear as an X-ray flash. However, if the supernova explodes inside an optically thick wind, the breakout flash is delayed. We present a simple model for estimating the conditions at shock breakout in a wind based on the general observable quantities in the X-ray flash light curve; the total energy EX, and the diffusion time after the peak, t(diff). We base the derivation on the self-similar solution for the forward-reverse shock structure expected for an ejecta plowing through a pre-existing wind at large distances from the progenitor's surface. We find simple quantitative relations for the shock radius and velocity at breakout. By relating the ejecta density profile to the pre-explosion structure of the progenitor, the model can also be extended to constrain the combination of explosion energy and ejecta mass. For the observed case of XRO08109/SN2008D, our model provides reasonable constraints on the breakout radius, explosion energy and ejecta mass, and predicts a high shock velocity which naturally accounts for the observed non-thermal spectrum. C1 [Balberg, Shmuel; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Balberg, Shmuel] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. RP Balberg, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM shmblbrg@phys.huji.ac.il FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX We wish to thank Alicia Soderberg for valuable comments and Udi Nakar and Eli Waxman for helpful discussions. We also thank Roger Chevalier for his helpful comments as the referee of this paper. SB thanks the Institute for Theory & Computation (ITC) at Harvard University for its kind hospitality. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 27 TC 39 Z9 39 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2011 VL 414 IS 2 BP 1715 EP 1720 DI 10.1111/j.1365-2966.2011.18505.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 792JS UT WOS:000292740500069 ER PT J AU Mouttham, LL Buhr, M Freeman, EW Widowski, TM Graham, LH Brown, JL AF Mouttham, L. L. Buhr, M. Freeman, E. W. Widowski, T. M. Graham, L. H. Brown, J. L. TI Interrelationship of serum testosterone, dominance and ovarian cyclicity status in female African elephants SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE African elephant; Testosterone; Dominance; Ovarian cyclicity ID LOXODONTA-AFRICANA; NORTH-AMERICA; MAXIMUS; ANDROGEN; BEHAVIOR; RANK; POPULATION; PREGNANCY; URINARY; MUSTH AB The African elephant population in North American zoos is not self-sustaining, in part due to the prevalence of ovarian acyclicity. While little is known about the cause of this condition, earlier research has shown that females without cyclic corpus luteum (CL) function rank higher in the dominance hierarchy than females with cyclic CL function. The goal of this study was to measure longitudinal serum testosterone concentrations in captive female African elephants to determine if there is a relationship among serum testosterone concentrations, social dominance rank and ovarian cyclicity status. Weekly blood samples from 49 female African elephants (24 having and 25 not having cyclic CL function at 22 facilities) were collected over a 12-month period and analyzed for serum testosterone using an enzymeimmunoassay. A progesterone radioimmunoassay was used to quantify serum progestagen concentrations and categorize ovarian cyclicity status. The dominance hierarchy of individual elephants within each herd was assessed by a written temperament survey, which identified 19 dominant, 15 middle and 15 subordinate females. No clear patterns of serum testosterone secretion were observed in females with and without cyclic CL function. Furthermore, no significant relationships were found among serum testosterone concentrations, dominance rank, and ovarian cyclicity status. These data suggest that increased circulating testosterone concentrations are not associated with greater rates of ovarian acyclicity or dominance status in captive female African elephants. Published by Elsevier B.V. C1 [Mouttham, L. L.; Freeman, E. W.; Brown, J. L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Mouttham, L. L.; Buhr, M.; Widowski, T. M.; Graham, L. H.] Univ Guelph, Guelph, ON N1G 2W1, Canada. [Freeman, E. W.] George Mason Univ, New Century Coll, Fairfax, VA 22030 USA. RP Brown, JL (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remt Rd, Front Royal, VA 22630 USA. EM brownjan@si.edu FU Smithsonian National Zoological Park; African Lion Safari; Natural Sciences and Engineering Research Council of Canada; Ontario Ministry of Agriculture, Food and Rural Affairs FX We thank all participating institutions for providing serum samples and completing temperament surveys: African Lion Safari, Caldwell Zoo, Cheyenne Mountain Zoo, Indianapolis Zoo, Jacksonville Zoo, Knoxville Zoological Gardens, Lee Richardson Zoo, Lion Country Safari, Louisville Zoo, Maryland Zoo, Miami MetroZoo, Milwaukee County Zoo, Nashville Zoo, North Carolina Zoo, Pittsburgh Zoo, Riverbanks Zoo and Garden, Sedgwick County Zoo, Seneca Park Zoo, Tampa's Lowry Park Zoo, Toledo Zoo, Utah's Hogle Zoo, Virginia Zoo, and Wildlife Safari. Special thanks to Nicole Presley, Nicole Parker, Natalia Oviedo-Prado and Sarah Putman of the SCBI Endocrine Laboratory and Katie Hickey of the University of Guelph for assistance with sample analyses. This study was supported by the Smithsonian National Zoological Park, African Lion Safari, Natural Sciences and Engineering Research Council of Canada, and Ontario Ministry of Agriculture, Food and Rural Affairs. NR 47 TC 8 Z9 8 U1 2 U2 18 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 JUN PY 2011 VL 126 IS 1-2 BP 115 EP 121 DI 10.1016/j.anireprosci.2011.04.006 PG 7 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA 801FQ UT WOS:000293424200018 PM 21592691 ER PT J AU Kozarev, KA Korreck, KE Lobzin, VV Weber, MA Schwadron, NA AF Kozarev, K. A. Korreck, K. E. Lobzin, V. V. Weber, M. A. Schwadron, N. A. TI OFF-LIMB SOLAR CORONAL WAVEFRONTS FROM SDO/AIA EXTREME-ULTRAVIOLET OBSERVATIONS-IMPLICATIONS FOR PARTICLE PRODUCTION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE shock waves; Sun: coronal mass ejections (CMEs); Sun: particle emission; Sun: radio radiation ID WHITE-LIGHT OBSERVATIONS; MASS EJECTION; ACTIVE REGIONS; RADIO; ACCELERATION; SHOCK AB We derive kinematic properties for two recent solar coronal transient waves observed off the western solar limb with the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) mission. The two waves occurred over similar to 10 minute intervals on consecutive days-2010 June 12 and 13. For the first time, off-limb waves are imaged with a high 12 s cadence, making possible detailed analysis of these transients in the low corona between similar to 1.1 and 2.0 solar radii (R(S)). We use observations in the 193 and 211 angstrom AIA channels to constrain the kinematics of both waves. We obtain initial velocities for the two fronts of similar to 1287 and similar to 736 km s(-1), and accelerations of -1170 and -800 m s(-2), respectively. Additionally, differential emission measure analysis shows the June 13 wave is consistent with a weak shock. Extreme-ultraviolet (EUV) wave positions are correlated with positions from simultaneous type II radio burst observations. We find good temporal and height association between the two, suggesting that the waves may be the EUV signatures of coronal shocks. Furthermore, the events are associated with significant increases in proton fluxes at 1 AU, possibly related to how waves propagate through the coronal magnetic field. Characterizing these coronal transients will be key to connecting their properties with energetic particle production close to the Sun. C1 [Kozarev, K. A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Kozarev, K. A.; Korreck, K. E.; Weber, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lobzin, V. V.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Schwadron, N. A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RP Kozarev, KA (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. EM kamen@bu.edu OI Lobzin, Vasily/0000-0001-5655-9928 FU Lockheed-Martin [SP02H 1701R]; NASA [NNX07AC14G] FX We acknowledge support under AIA subcontract SP02H 1701R from Lockheed-Martin and NASA LWS EMMREM project NNX07AC14G. We thank David Long, Maher Dayeh, Marc De Rosa, Steve Saar, and Suli Ma for help and discussions. NR 28 TC 47 Z9 47 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 JUN 1 PY 2011 VL 733 IS 2 AR L25 DI 10.1088/2041-8205/733/2/L25 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797NQ UT WOS:000293135000009 ER PT J AU Walker, MG Combet, C Hinton, JA Maurin, D Wilkinson, MI AF Walker, M. G. Combet, C. Hinton, J. A. Maurin, D. Wilkinson, M. I. TI DARK MATTER IN THE CLASSICAL DWARF SPHEROIDAL GALAXIES: A ROBUST CONSTRAINT ON THE ASTROPHYSICAL FACTOR FOR gamma-RAY FLUX CALCULATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dark matter; galaxies: kinematics and dynamics; Local Group ID EXPLORING HALO SUBSTRUCTURE; MILKY-WAY; LEO-I; GIANT STARS; LOCAL GROUP; URSA-MINOR; MODELS; ANNIHILATION; PROFILE; DRACO AB We present a new analysis of the relative detectability of dark matter annihilation in the Milky Way's eight "classical" dwarf spheroidal (dSph) satellite galaxies. Ours is similar to previous analyses in that we use Markov-Chain Monte Carlo techniques to fit dark matter halo parameters to empirical velocity dispersion profiles via the spherical Jeans equation, but more general in the sense that we do not adopt priors derived from cosmological simulations. We show that even without strong constraints on the shapes of dSph dark matter density profiles (we require only that the inner profile satisfies - lim(r -> 0) d ln rho/d ln r <= 1), we obtain a robust and accurate constraint on the astrophysical component of a prospective dark matter annihilation signal, provided that the integration angle is approximately twice the projected half-light radius of the dSph divided by distance to the observer, alpha(int) similar to 2r(h)/d. Using this integration angle, which represents a compromise between maximizing prospective flux and minimizing uncertainty in the dSph's dark matter distribution, we calculate the relative detectability of the classical dSphs by ground-and space-based gamma-ray observatories. C1 [Walker, M. G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Walker, M. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Combet, C.; Hinton, J. A.; Maurin, D.; Wilkinson, M. I.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Maurin, D.] Univ Grenoble 1, CNRS, IN2P3, Lab Phys Subatom & Cosmol,INPG, F-38026 Grenoble, France. [Maurin, D.] Univ Paris 06, CNRS, Inst Astrophys Paris, F-75014 Paris, France. RP Walker, MG (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM mwalker@cfa.harvard.edu; dmaurin@lspc.in2p3.fr RI Walker, Matthew/P-1777-2014 OI Walker, Matthew/0000-0003-2496-1925 FU NASA [HST-HF-51283, NAS 5-26555]; STFC; Royal Society FX We thank the referee, Gary Mamon, for providing suggestions that improved the quality of this Letter. We are grateful to Walter Dehnen for providing his code for use in generating artificial dSph data sets. M. G. W. 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. C. C. acknowledges support from an STFC rolling grant at the University of Leicester. J.A.H. acknowledges the support of an STFC Advanced Fellowship. M. I. W. acknowledges the Royal Society for support via a University Research Fellowship. NR 47 TC 31 Z9 31 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 JUN 1 PY 2011 VL 733 IS 2 AR L46 DI 10.1088/2041-8205/733/2/L46 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797NQ UT WOS:000293135000030 ER PT J AU Perez, L Frenzel, P Brenner, M Escobar, J Hoelzmann, P Scharf, B Schwalb, A AF Perez, Liseth Frenzel, Peter Brenner, Mark Escobar, Jaime Hoelzmann, Philipp Scharf, Burkhard Schwalb, Antje TI Late Quaternary (24-10 ka BP) environmental history of the Neotropical lowlands inferred from ostracodes in sediments of Lago Peten Itza, Guatemala SO JOURNAL OF PALEOLIMNOLOGY LA English DT Article DE Non-marine ostracodes; Training set; Transfer function; Late Pleistocene; Lago Peten Itza; Guatemala; Environmental change ID YUCATAN PENINSULA; FRESH-WATER; CLIMATE-CHANGE; CENTRAL-AMERICA; CRUSTACEA; MEXICO; LAKES; RECONSTRUCTION; ASSEMBLAGES; DIVERSITY AB We inferred late Pleistocene and early Holocene (24-10 ka BP) environmental conditions in and around Lago Peten Itza, Guatemala from ostracode remains in the lake sediments. Multivariate statistics were run on autecological information for 29 extant ostracode species collected in 63 aquatic ecosystems on the Yucatan Peninsula along a steep, increasing NW-S precipitation gradient and across a large altitudinal range. Conductivity and water depth are the most important factors that shape ostracode communities. Transfer functions were developed and applied to fossil ostracode assemblages in a similar to 76-m sediment core (PI-6, similar to 85 ka) taken in 71 m of water from Lago Peten Itza, to infer past shifts in conductivity and water level. Results suggest climate was cold and wet during the Last Glacial Maximum (LGM). Alternating dry and wet conditions characterized the deglacial. Early Holocene climate was warmer and wetter. The LGM was characterized by low ostracode species richness (4 spp.) and abundance (<940 valves g(-1)), dominance of benthic over nektobenthic taxa, abundant Physocypria globula, conductivity as low as 190 mu S cm(-1), and clay-rich sediments with relatively high total organic carbon and low C/N ratios (<14), suggesting relatively deeper water at the core site associated with abundant precipitation. Greatest water depth at the core site during the LGM occurred late in the period and was similar to 50 m. The deglacial was characterized by drier conditions, higher ostracode species richness (6 spp.) and abundances up to 18,115 valves g(-1), dominance of nektobenthic species, and presence of shallow-water and littoral-zone indicators such as Heterocypris punctata and Strandesia intrepida, conductivity up to 550 mu S cm(-1), C/N ratios as high as 37, and gypsum deposition. Lowest inferred lake depth at the core site during the deglacial was similar to 20 m. The early Holocene was characterized by high numbers of ostracode remains, up to 25,500 valves g(-1), and the presence of L. opesta and P. globula. Cytheridella ilosvayi was absent from late Pleistocene sediments, suggesting it colonized northern Central America during the Holocene. C1 [Perez, Liseth; Frenzel, Peter; Scharf, Burkhard; Schwalb, Antje] Tech Univ Carolo Wilhelmina Braunschweig, Inst Umweltgeol, D-38106 Braunschweig, Germany. [Frenzel, Peter] Univ Jena, Inst Geowissensch, D-07749 Jena, Germany. [Brenner, Mark; Escobar, Jaime] Univ Florida, Land Use & Environm Change Inst, Gainesville, FL 32611 USA. [Brenner, Mark] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. [Escobar, Jaime] Smithsonian Trop Res Inst STRI, Ctr Trop Paleoecol & Archaeol, Balboa 084303092, Panama. [Hoelzmann, Philipp] Free Univ Berlin, Inst Geog Wissensch, D-12249 Berlin, Germany. [Escobar, Jaime] Univ Florida, Sch Nat Resources & Environm, Gainesville, FL 32611 USA. RP Perez, L (reprint author), Tech Univ Carolo Wilhelmina Braunschweig, Inst Umweltgeol, Langer Kamp 19C, D-38106 Braunschweig, Germany. EM l.perez@tu-bs.de; Peter.Frenzel@uni-jena.de; brenner@ufl.edu; jaimee@ufl.edu; phoe@zedat.fu-berlin.de; Burkhard.W.Scharf@t-online.de; antje.schwalb@tu-bs.de RI Frenzel, Peter/F-5247-2012; OI Hoelzmann, Philipp/0000-0001-8709-8474 FU Deutsche Forschungsgemeinschaft (DFG) [Schw 671/3]; Technische Universitat Braunschweig FX We thank all those who facilitated fieldwork in Mexico, Belize and Guatemala. Special thanks to: Andreas Muller and other participants in the Peten Itza Scientific Drilling Project, Aaron Lewis (University of Belize), the Forestry and Fisheries Departments (Belize), Margarita Palmieri, Margaret Dix, Roberto Moreno, Eleonor de Tott (Universidad del Valle de Guatemala), Rodrigo Morales, Franklin Herrera (CONAP, Guatemala), Ismael Ordonez (AMSCLAE, Guatemala), Julio Morales Cancino (AMPI, Guatemala), Roderico Pineda, Mario Buch (Trifinio, Guatemala), Gerald Islebe (ECOSUR-Chetumal, Mexico), Secretaria de Relaciones Exteriores (SRE, Mexico), Comision Nacional de Acuacultura y Pesca (CONAPESCA, Mexico), Alberto de Jesus Navarrete (ECOSUR-Chetumal, Mexico), the National Lacustrine Core Repository (LacCore, University of Minnesota), Julia Lorenschat, Rita Bugja, Rita Lohr, Benjamin Gilfedder, Yvonne Hermanns, Harald Biester (Institut fur Umweltgeologie, Braunschweig), Dietmar Keyser (Zoologisches Institut und Zoologisches Museum, Hamburg), Steffen Mischke (Freie Universitat Berlin), Douglas Schnurrenberger, Dustin Grzesik, David Klassen, Luciana Mitsue, Jose Harders, Carmen Herold, Bessie Oliva, Alma Quilo, Gabriela Alfaro, Jacobo Blijdenstein, Melisa Orozco, Silja Ramirez, Luis Toruno, Mario Cruz, Javier Perez y Perez, and Carolina Alvarado de Perez. The Deutsche Forschungsgemeinschaft (DFG, grant Schw 671/3) and the Technische Universitat Braunschweig provided financial support. NR 52 TC 10 Z9 12 U1 0 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2728 J9 J PALEOLIMNOL JI J. Paleolimn. PD JUN PY 2011 VL 46 IS 1 BP 59 EP 74 DI 10.1007/s10933-011-9514-0 PG 16 WC Environmental Sciences; Geosciences, Multidisciplinary; Limnology SC Environmental Sciences & Ecology; Geology; Marine & Freshwater Biology GA 797RG UT WOS:000293144700005 ER PT J AU Wendler, I Willems, H Grafe, KU Ding, L Luo, H AF Wendler, Ines Willems, Helmut Graefe, Kai-Uwe Ding, Lin Luo, Hui TI Upper Cretaceous inter-hemispheric correlation between the Southern Tethys and the Boreal: chemo- and biostratigraphy and paleoclimatic reconstructions from a new section in the Tethys Himalaya, S-Tibet SO NEWSLETTERS ON STRATIGRAPHY LA English DT Article DE Upper Cretaceous; carbon isotopes; biostratigraphy; correlation; paleogeography; paleoclimate ID ORBITAL TIME-SCALE; CARBON-ISOTOPE STRATIGRAPHY; CAMPANIAN PLANKTONIC-FORAMINIFERA; SEA-LEVEL CHANGE; PRODUCTIVITY FLUCTUATIONS; BOUNDARY STRATOTYPE; PELAGIC CARBONATES; NORTHERN GERMANY; COASTAL TANZANIA; EXMOUTH PLATEAU AB A new, 430 m long and mostly continuous Upper Cretaceous section from southern hemisphere low paleolatitudes in the Tethys Himalaya (Guru, Tibet) is presented. The lithology, microfacies and fossil contents of the Guru section indicate a continuous shallowing trend from open oceanic conditions at the slope during the Turonian to shallow marine inner shelf environments in the Maastrichtian, interrupted by short periods of stagnation or slight deepening. Strong variations in sedimentation rates and contents of carbonate, quartz, organic carbon and sulfur appear to reflect a combination of regional and global processes. On regional scale, the patterns of varying elastic sediment supply seem to be related to the fast northward drift of the Indian plate from the temperate climate belt in the Turonian and Coniacian, crossing the arid zone during the Santonian and early Campanian, and passing into the tropical humid belt in the late Campanian. On global scale, similar sedimentary changes as in Guru with a transition from clay-rich Turonian sediments to Coniacian carbonates are found in other regions of the world, suggesting an additional influence of global oceanic and climatic factors. Intervals of omission, erosion and reworking in upper Coniacian and lower Campanian sediments of the Guru section appear to coincide with global sea-level lowstands. Well preserved planktic foraminifera occur over most of the Guru section and provide good biostratigraphic control for correlation of stable carbon and oxygen isotopes with data from the reference section for the boreal and Maastrichtian carbon isotope fluctuations can be related to cyclic variations in carbonate showing detailed correlation of bulk sediment carbon isotopes and comparable trends in oxygen isotopes. The real white chalk in northern Germany at Lagerdorf-Kronsmoor and with the English Chalk reference section, content at Lagerdorf-Kronsmoor which are thought to be driven by long eccentricity. This indicates orbital forcing of both carbonate accumulation and carbon isotope signature, most likely mediated by global sea-level changes. The possibility of detailed delta C-13 correlation from boreal sections of the northern hemisphere to a low-latitude section of the southern hemisphere allows for global correlation with an accuracy not achieved by biostratigraphic methods so far. It further enables linking of microfossil and macrofossil biozones, facilitating precise comparison of shallow and deep water sections, which is essential for the improvement of our understanding of timing, causes and effects of climatic and oceanographic processes. C1 [Wendler, Ines; Willems, Helmut; Graefe, Kai-Uwe] Univ Bremen, Dept Geol Sci, D-28334 Bremen, Germany. [Willems, Helmut; Luo, Hui] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Nanjing 210008, Peoples R China. [Ding, Lin] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100085, Peoples R China. RP Wendler, I (reprint author), Smithsonian Museum Nat Hist, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. EM wendleri@si.edu; willems@uni-bremen.de; ugraefe@uni-bremen.de; dinglin@itpcas.ac.cn; huiluo@nigpas.ac.cn FU German Science Foundation [DFG Wi 725/25]; University of Bremen FX Field work in South Tibet has been made possible by the support of our Chinese colleagues from ITP-CAS, Beijing and NIGPAS-CAS, Nanjing. J. Lindtke is greatly acknowledged for his help during field work and subsequent sample preparation. A. Huber is thanked for the preparation of thin-sections. We thank J. Wendler for his comments on an earlier version of the manuscript. We highly appreciate helpful discussion with B. T. Huber on the planktic foraminifera biozonation in the Guru section. We are grateful to M.-R. Petrizzo and S. Voigt for constructive reviews that helped improving the quality of the manuscript. The study has been funded by the German Science Foundation (DFG Wi 725/25) and University of Bremen. NR 59 TC 17 Z9 17 U1 1 U2 18 PU GEBRUDER BORNTRAEGER PI STUTTGART PA JOHANNESSTR 3A, D-70176 STUTTGART, GERMANY SN 0078-0421 J9 NEWSL STRATIGR JI Newsl. Stratigr. PD JUN PY 2011 VL 44 IS 2 BP 137 EP 171 DI 10.1127/0078-0421/2011/0010 PG 35 WC Geology SC Geology GA 793FJ UT WOS:000292805500005 ER PT J AU Robinson, H Skvarla, JJ AF Robinson, Harold Skvarla, John J. TI A New Monotypic Genus, Ananthura, from Tropical Africa (Asteraceae, Vernonieae) SO NOVON LA English DT Article DE Africa; Ananthura; Asteraceae; Gymnantheminae; IUCN Red List; Vernonieae ID POLLEN MORPHOLOGY; COMPOSITAE; WORLD AB A new genus, Ananthura H. Rob. & Skvarla (Asteraceae, Vernonieae), is described for Vernonia pteropoda Oliv. & Hiern in Oliv. of Central Africa. The genus has broad median shields on the involucral bracts and lophate, strongly tricolporate pollen. It is placed in the subtribe Gymnantheminae. The name V. urophylla Muschl. is lectotypified. C1 [Robinson, Harold] Smithsonian Inst, Museum Natl Hist Nat, Dept Bot, Washington, DC 20013 USA. [Skvarla, John J.] Univ Oklahoma, Oklahoma Biol Survey, Norman, OK 73019 USA. [Skvarla, John J.] Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA. RP Robinson, H (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM Robinsoh@si.edu; jskvarla@ou.edu NR 21 TC 2 Z9 2 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 JUN PY 2011 VL 21 IS 2 BP 251 EP 255 DI 10.3417/2010062 PG 5 WC Plant Sciences SC Plant Sciences GA 788KG UT WOS:000292443200018 ER PT J AU Immer, K Brunthaler, A Reid, MJ Bartkiewicz, A Choi, YK Menten, KM Moscadelli, L Sanna, A Wu, YW Xu, Y Zhang, B Zheng, XW AF Immer, K. Brunthaler, A. Reid, M. J. Bartkiewicz, A. Choi, Y. K. Menten, K. M. Moscadelli, L. Sanna, A. Wu, Y. W. Xu, Y. Zhang, B. Zheng, X. W. TI THE VLBA CALIBRATOR SEARCH FOR THE BeSSeL SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrometry; Galaxy: general; H II regions; radio continuum: general; surveys ID CELESTIAL REFERENCE FRAME; H-II REGIONS AB We present the results of a survey of radio continuum sources near the Galactic plane using the Very Long Baseline Array (VLBA). Our observations are designed to identify compact extragalactic sources of milliarcsecond size that can be used for parallax measurements in the Bar and Spiral Structure Legacy Survey. We selected point sources from the NVSS and CORNISH catalogs with flux densities above 30 mJy and within 1 degrees.5 of known maser targets. Of the 1529 sources observed, 199 were detected. For sources detected on three or more baselines, we determined accurate positions and evaluated their quality as potential calibrators. Most of the 1330 sources that were not detected with the VLBA are probably of extragalactic origin. C1 [Immer, K.; Brunthaler, A.; Choi, Y. K.; Menten, K. M.; Sanna, A.; Zhang, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Immer, K.; Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bartkiewicz, A.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Moscadelli, L.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Wu, Y. W.; Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. RP Immer, K (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kimmer@mpifr-bonn.mpg.de RI Bartkiewicz, Anna/D-6212-2014; OI Moscadelli, Luca/0000-0002-8517-8881 FU ERC [247078] FX This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). NR 18 TC 17 Z9 17 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2011 VL 194 IS 2 AR 25 DI 10.1088/0067-0049/194/2/25 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 778CB UT WOS:000291675700009 ER PT J AU Jonker, PG Bassa, CG Nelemans, G Steeghs, D Torres, MAP Maccarone, TJ Hynes, RI Greiss, S Clem, J Dieball, A Mikles, VJ Britt, CT Gossen, L Collazzi, AC Wijnands, R Zand, JJMI Mendez, M Rea, N Kuulkers, E Ratti, EM van Haaften, LM Heinke, C Ozel, F Groot, PJ Verbunt, F AF Jonker, P. G. Bassa, C. G. Nelemans, G. Steeghs, D. Torres, M. A. P. Maccarone, T. J. Hynes, R. I. Greiss, S. Clem, J. Dieball, A. Mikles, V. J. Britt, C. T. Gossen, L. Collazzi, A. C. Wijnands, R. Zand, J. J. M. In't Mendez, M. Rea, N. Kuulkers, E. Ratti, E. M. van Haaften, L. M. Heinke, C. Oezel, F. Groot, P. J. Verbunt, F. TI THE GALACTIC BULGE SURVEY: OUTLINE AND X-RAY OBSERVATIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE accretion, accretion disks; binaries: close; X-rays: binaries ID BLACK-HOLE; CATACLYSMIC VARIABLES; SOURCE CATALOG; PLANE SURVEY; MILKY-WAY; LUMINOSITY FUNCTION; BINARY POPULATION; CHAMPLANE SURVEY; POINT SOURCES; MASS AB We introduce the Galactic Bulge Survey (GBS) and we provide the Chandra source list for the region that has been observed to date. Among the goals of the GBS are constraining the neutron star (NS) equation of state and the black hole (BH) mass distribution via the identification of eclipsing NS and BH low-mass X-ray binaries (LMXBs). The latter goal will, in addition, be obtained by significantly enlarging the number of BH systems for which a BH mass can be derived. Further goals include constraining X-ray binary formation scenarios, in particular the common envelope phase and the occurrence of kicks, via source-type number counts and an investigation of the spatial distribution of X-ray binaries, respectively. The GBS targets two strips of 6 degrees x 1 degrees (12 deg(2) in total), one above (1 degrees < b < 2 degrees) and one below (-2 degrees < b < -1 degrees) the Galactic plane in the direction of the Galactic center at both X-ray and optical wavelengths. By avoiding the Galactic plane (-1 degrees < b < 1 degrees) we limit the influence of extinction on the X-ray and optical emission but still sample relatively large number densities of sources. The survey is designed such that a large fraction of the X-ray sources can be identified from their optical spectra. The X-ray survey, by design, covers a large area on the sky while the depth is shallow using 2 ks per Chandra pointing. In this way we maximize the predicted number ratio of (quiescent) LMXBs to cataclysmic variables. The survey is approximately homogeneous in depth to a 0.5-10 keV flux of 7.7 x 10(-14) erg cm(-2) s(-1). So far, we have covered about two-thirds (8.3 deg(2)) of the projected survey area with Chandra providing over 1200 unique X-ray sources. We discuss the characteristics and the variability of the brightest of these sources. C1 [Jonker, P. G.; Bassa, C. G.; Torres, M. A. P.; Zand, J. J. M. In't; Ratti, E. M.; Verbunt, F.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Bassa, C. G.; Nelemans, G.; van Haaften, L. M.; Groot, P. J.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 AJ Nijmegen, Netherlands. [Jonker, P. G.; Steeghs, D.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bassa, C. G.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Steeghs, D.; Greiss, S.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Maccarone, T. J.; Dieball, A.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hynes, R. I.; Clem, J.; Mikles, V. J.; Britt, C. T.; Gossen, L.; Collazzi, A. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Mendez, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Rea, N.] Inst Ciencias Espai ICE IEEC CSIC, Fac Ciencias, Barcelona 08193, Spain. [Kuulkers, E.] ESA ESAC, ISOC, Madrid 28080, Spain. [Heinke, C.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Oezel, F.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Verbunt, F.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. RP Jonker, PG (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM p.jonker@sron.nl RI Mendez, Mariano/C-8011-2012; Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009; Rea, Nanda/I-2853-2015; Groot, Paul/K-4391-2016; OI Mendez, Mariano/0000-0003-2187-2708; Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746; Rea, Nanda/0000-0003-2177-6388; Groot, Paul/0000-0002-4488-726X; Heinke, Craig/0000-0003-3944-6109 FU Netherlands Organisation for Scientific Research; National Science Foundation [AST-0908789]; NASA/Louisiana Board of Regents [NNX07AT62A/LEQSF(2007-10)]; NSERC; STFC FX P.G.J. and G.N. acknowledge support from the Netherlands Organisation for Scientific Research. R.I.H., C.T.B, V.J.M., and L. G. acknowledge support from National Science Foundation Grant No. AST-0908789 and NASA/Louisiana Board of Regents grant NNX07AT62A/LEQSF(2007-10) Phase3-02. C.O.H. is supported by NSERC. D.S. acknowledges an STFC Advanced Fellowship. T.J.M. and A.D. thank STFC for support via a rolling grant to the University of Southampton. NR 81 TC 40 Z9 40 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2011 VL 194 IS 2 AR 18 DI 10.1088/0067-0049/194/2/18 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 778CB UT WOS:000291675700002 ER PT J AU Peterson, DE Garatti, ACO Bourke, TL Forbrich, J Gutermuth, RA Jorgensen, JK Allen, LE Patten, BM Dunham, MM Harvey, PM Merin, B Chapman, NL Cieza, LA Huard, TL Knez, C Prager, B Evans, NJ AF Peterson, Dawn E. Garatti, Alessio Caratti O. Bourke, Tyler L. Forbrich, Jan Gutermuth, Robert A. Jorgensen, Jes K. Allen, Lori E. Patten, Brian M. Dunham, Michael M. Harvey, Paul M. Merin, Bruno Chapman, Nicholas L. Cieza, Lucas A. Huard, Tracy L. Knez, Claudia Prager, Brian Evans, Neal J., II TI THE SPITZER SURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. III. A MULTI-WAVELENGTH VIEW OF CORONA AUSTRALIS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE infrared: general; ISM: clouds; ISM: individual objects (Corona Australis); ISM: jets and outflows; stars: formation; stars: pre-main sequence ID YOUNG STELLAR OBJECTS; HERBIG-HARO OBJECTS; STAR-FORMATION REGION; X-RAY SOURCES; MOLECULAR-HYDROGEN EMISSION; NEAR-INFRARED OBSERVATIONS; MAIN-SEQUENCE STARS; CRA DARK CLOUD; T-TAURI STARS; R-CRA AB We present Spitzer Space Telescope IRAC and MIPS observations of a 0.85 deg(2) field including the Corona Australis (CrA) star-forming region. At a distance of 130 pc, CrA is one of the closest regions known to be actively forming stars, particularly within its embedded association, the Coronet. Using the Spitzer data, we identify 51 young stellar objects (YS0s) in CrA which include sources in the well-studied Coronet cluster as well as sources distributed throughout the molecular cloud. Twelve of the YSOs discussed are new candidates, one of which is located in the Coronet. Known YSOs retrieved from the literature are also added to the list, and a total of 116 candidate YSOs in CrA are compiled. Based on these YSO candidates, the star formation rate is computed to be 12M(circle dot) Myr(-1), similar to that of the Lupus clouds. A clustering analysis was also performed, finding that the main cluster core, consisting of 68 members, is elongated (having an aspect ratio of 2.36), with a circular radius of 0.59 pc and mean surface density of 150 pc(-2). In addition, we analyze outflows and jets in CrA by means of new CO and H-2 data. We present 1 3 mm interferometric continuum observations made with the Submillimeter Array (SMA) covering R CrA, IRS 5, IRS 7, and IRAS 18595-3712 (IRAS 32). We also present multi-epoch H2 maps and detect jets and outflows, study their proper motions, and identify exciting sources. The Spitzer and ISAAC/VET observations of IRAS 32 show a bipolar precessing jet, which drives a CO(2-1) outflow detected in the SMA observations. There is also clear evidence for a parsec-scale precessing outflow, which is east west oriented and originates in the SMA 2 region and likely driven by SMA 2 or IRS 7A. C1 [Peterson, Dawn E.; Bourke, Tyler L.; Forbrich, Jan; Patten, Brian M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Garatti, Alessio Caratti O.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Gutermuth, Robert A.] Smith Coll, Coll Astron Dept 5, Northampton, MA 01063 USA. [Gutermuth, Robert A.] Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. [Jorgensen, Jes K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Allen, Lori E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Dunham, Michael M.; Harvey, Paul M.; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Merin, Bruno] European Space Astron Ctr ESA, Herschel Sci Ctr, Madrid 28691, Spain. [Chapman, Nicholas L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cieza, Lucas A.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Huard, Tracy L.; Knez, Claudia; Prager, Brian] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Peterson, DE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dpeterson@cfa.harvard.edu RI Caratti o Garatti, Alessio/D-1537-2012; OI Merin, Bruno/0000-0002-8555-3012; Caratti o Garatti, Alessio/0000-0001-8876-6614 FU National Aeronautics and Space Administration, NASA [1288820, 1298236, 1407]; Science Foundation of Ireland [07/RFP/PHYF790]; Danish National Research Foundation; National Science Foundation FX The authors thank Karl Stapelfeldt, Eli Bressert, and the anonymous referee for their helpful comments. In addition, we thank Amanda Heiderman for very helpful discussions of the overall cloud properties and comparison with her work. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contract numbers 1288820 and 1298236 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. A.C.G. was supported by the Science Foundation of Ireland, grant 07/RFP/PHYF790. The research at Centre for Star and Planet Formation (coauthor J.K.J.) is funded by the Danish National Research Foundation and the University of Copenhagen's programme of excellence.; This research is partially based on observations collected at the European Southern Observatory (Paranal and La Silla, Chile, 079.C-00020(A), 075.C-0561(A), 071.B-0274(A), 065.L-0637(A), 63.1-0031(A)). This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. This research has also made use of NASA's Astrophysics Data System Bibliographic Services and the SIMBAD database, operated at the CDS, Strasbourg, France, and the 2MASS data, obtained as part of the Two Micron All Sky Survey, 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 140 TC 41 Z9 41 U1 1 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 JUN PY 2011 VL 194 IS 2 DI 10.1088/0067-0049/194/2/43 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 778CB UT WOS:000291675700027 ER PT J AU Primini, FA Houck, JC Davis, JE Nowak, MA Evans, IN Glotfelty, KJ Anderson, CS Bonaventura, NR Chen, JC Doe, SM Evans, JD Fabbiano, G Galle, EC Gibbs, DG Grier, JD Hain, RM Hall, DM Harbo, PN He, XQ Karovska, M Kashyap, VL Lauer, J McCollough, ML McDowell, JC Miller, JB Mitschang, AW Morgan, DL Mossman, AE Nichols, JS Plummer, DA Refsdal, BL Rots, AH Siemiginowska, A Sundheim, BA Tibbetts, MS Van Stone, DW Winkelman, SL Zografou, P AF Primini, Francis A. Houck, John C. Davis, John E. Nowak, Michael A. Evans, Ian N. Glotfelty, Kenny J. Anderson, Craig S. Bonaventura, Nina R. Chen, Judy C. Doe, Stephen M. Evans, Janet D. Fabbiano, Giuseppina Galle, Elizabeth C. Gibbs, Danny G., II Grier, John D. Hain, Roger M. Hall, Diane M. Harbo, Peter N. He, Xiangqun (Helen) Karovska, Margarita Kashyap, Vinay L. Lauer, Jennifer McCollough, Michael L. McDowell, Jonathan C. Miller, Joseph B. Mitschang, Arik W. Morgan, Douglas L. Mossman, Amy E. Nichols, Joy S. Plummer, David A. Refsdal, Brian L. Rots, Arnold H. Siemiginowska, Aneta Sundheim, Beth A. Tibbetts, Michael S. Van Stone, David W. Winkelman, Sherry L. Zografou, Panagoula TI STATISTICAL CHARACTERIZATION OF THE CHANDRA SOURCE CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; X-rays: general ID MEDIUM-SENSITIVITY SURVEY; MS SOURCE CATALOGS; FIELD NORTH SURVEY; DIGITAL SKY SURVEY; MULTIWAVELENGTH PROJECT; IN-FLIGHT; PERFORMANCE; CALIBRATION; SHERPA; SOUTH AB The first release of the Chandra Source Catalog (CSC) contains similar to 95,000 X-ray sources in a total area of 0.75% of the entire sky, using data from similar to 3900 separate ACTS observations of a multitude of different types of X-ray sources. In order to maximize the scientific benefit of such a large, heterogeneous data set, careful characterization of the statistical properties of the catalog, i.e., completeness, sensitivity, false source rate, and accuracy of source properties, is required. Characterization efforts of other large Chandra catalogs, such as the ChaMP Point Source Catalog or the 2 Mega-second Deep Field Surveys, while informative, cannot serve this purpose, since the CSC analysis procedures are significantly different and the range of allowable data is much less restrictive. We describe here the characterization process for the CSC. This process includes both a comparison of real CSC results with those of other, deeper Chandra catalogs of the same targets and extensive simulations of blank-sky and point-source populations. C1 [Houck, John C.; Davis, John E.; Nowak, Michael A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hall, Diane M.] Northrop Grumman, Cambridge, MA 02138 USA. [Primini, Francis A.; Evans, Ian N.; Glotfelty, Kenny J.; Anderson, Craig S.; Bonaventura, Nina R.; Chen, Judy C.; Doe, Stephen M.; Evans, Janet D.; Fabbiano, Giuseppina; Galle, Elizabeth C.; Gibbs, Danny G., II; Grier, John D.; Hain, Roger M.; Harbo, Peter N.; He, Xiangqun (Helen); Karovska, Margarita; Kashyap, Vinay L.; Lauer, Jennifer; McCollough, Michael L.; McDowell, Jonathan C.; Miller, Joseph B.; Mitschang, Arik W.; Morgan, Douglas L.; Mossman, Amy E.; Nichols, Joy S.; Plummer, David A.; Refsdal, Brian L.; Rots, Arnold H.; Siemiginowska, Aneta; Sundheim, Beth A.; Tibbetts, Michael S.; Van Stone, David W.; Winkelman, Sherry L.; Zografou, Panagoula] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Primini, FA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM fap@head.cfa.harvard.edu OI Rots, Arnold/0000-0003-2377-2356; Houck, John/0000-0002-6761-6796; Primini, Francis/0000-0002-6077-0643 FU National Aeronautics and Space Administration [NAS 8-03060, SV3-73016] FX The authors acknowledge the support of the National Aeronautics and Space Administration via grants NAS 8-03060 and SV3-73016. NR 43 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2011 VL 194 IS 2 AR 37 DI 10.1088/0067-0049/194/2/37 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 778CB UT WOS:000291675700021 ER PT J AU Shen, Y Richards, GT Strauss, MA Hall, PB Schneider, DP Snedden, S Bizyaev, D Brewington, H Malanushenko, V Malanushenko, E Oravetz, D Pan, K Simmons, A AF Shen, Yue Richards, Gordon T. Strauss, Michael A. Hall, Patrick B. Schneider, Donald P. Snedden, Stephanie Bizyaev, Dmitry Brewington, Howard Malanushenko, Viktor Malanushenko, Elena Oravetz, Dan Pan, Kaike Simmons, Audrey TI A CATALOG OF QUASAR PROPERTIES FROM SLOAN DIGITAL SKY SURVEY DATA RELEASE 7 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE black hole physics; galaxies: active; quasars: general; surveys ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; QSO REDSHIFT SURVEY; NARROW-LINE REGION; 7TH DATA RELEASE; EMISSION-LINE; EDDINGTON RATIO; STELLAR OBJECTS; MG II; LUMINOSITY FUNCTION AB We present a compilation of properties of the 105,783 quasars in the Sloan Digital Sky Survey Data Release 7 (DR7) quasar catalog. In this product, we compile continuum and emission line measurements around the H alpha, H beta, Mg II, and C iv regions, as well as other quantities such as radio properties, and flags indicating broad absorption line quasars, disk emitters, etc. We also compile virial black hole mass estimates based on various calibrations. For the fiducial virial mass estimates we use the Vestergaard & Peterson (VP06) calibrations for H beta and C IV, and our own calibration for Mg II which matches the VP06 H beta masses on average. We describe the construction of this catalog and discuss its limitations. The catalog and its future updates will be made publicly available online. C1 [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Strauss, Michael A.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Hall, Patrick B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Snedden, Stephanie; Bizyaev, Dmitry; Brewington, Howard; Malanushenko, Viktor; Malanushenko, Elena; Oravetz, Dan; Pan, Kaike; Simmons, Audrey] Apache Point Observ, Sunspot, NM 88349 USA. RP Shen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. FU Alfred P. Sloan Research Fellowship; National Aeronautics and Space Administration, NASA [07-ADP07-0035]; National Science Foundation, NSF [AST-0707266, AST-0607634]; NSERC; Alfred P. Sloan Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; Smithsonian Astrophysical Observatory (SAO) FX We thank the anonymous referee for constructive comments that improved the manuscript. Y.S. acknowledges support from a Clay Postdoctoral Fellowship through the Smithsonian Astrophysical Observatory (SAO). G.T.R. acknowledges support from an Alfred P. Sloan Research Fellowship and NASA grant 07-ADP07-0035. M.A.S. acknowledges the support of NSF grant AST-0707266. P.B.H. is supported by NSERC. D.P.S. acknowledges the support of NSF grant AST-0607634.; 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 103 TC 405 Z9 407 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2011 VL 194 IS 2 DI 10.1088/0067-0049/194/2/45 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 778CB UT WOS:000291675700029 ER PT J AU Moreno, C Varughese, T Spadafora, C Arnold, AE Coley, PD Kursar, TA Gerwick, WH Cubilla-Rios, L AF Moreno, Cufemio Varughese, Titto Spadafora, Carmenza Arnold, A. Elizabeth Coley, Phyllis D. Kursar, Thomas A. Gerwick, William H. Cubilla-Rios, Luis TI Chemical Constituents of the New Endophytic Fungus Mycosphaerella sp nov and Their Anti-parasitic Activity SO NATURAL PRODUCT COMMUNICATIONS LA English DT Article DE Endophytic fungus; Mycosphaerella sp nov.; Cercosporin. Anti-parasitic activity; cytotoxic activity ID CERCOSPORINA-KIKUCHII MATSUMOTO; PHOTOSENSITIZING TOXIN; SECONDARY METABOLITES; CELL-LINES; CONSERVATION; DIVERSITY; PARASITES; TOMOYASU; PIGMENT; DNA AB Chemical investigation of a new endophytic fungus, Mycosphaerella sp. nov. strain F2140, associated with the foliage of the plant Psychotria horizontalis (Rubiaceae) in Panama, resulted in the isolation of cercosporin (1) and a new cercosporin analog (3) as the major components. The structures of minor compounds in the extract were elucidated by detailed spectroscopic analysis as 2-(2-butyl)-6-ethyl-3-hydroxy-6-methylcyclohex-2-ene-1,5-dione (4), 3-(2-butyl)-6-ethyl-5-hydroxy-2-methoxy-6-methyl-cyclohex-2-enone (5), and an isomer of 5 (6). To study the influence of the hydroxy groups on the anti-parasitic activity of cercosporin, compound 1 was acetylated to obtain derivative 2. The isolated compounds 1 6 were tested in vitro to determine their anti-parasitic activity against the causal agents of malaria (Plasmodium falciparum), leishmaniasis (Leishmania donovani), and Chagas disease (Trypanosoma cruzi). Cytotoxicity and potential anticancer activity of these compounds were evaluated using mammalian Vero cells and MCF7 cancer cell lines, respectively. Compounds 1 and 2 displayed high potency against L. donovani (IC(50) 0.46 and 0.64 mu M), T. cruzi (IC(50) 1.08 and 0.78 mu M), P. falciparum (IC(50) 1.03 and 2.99 mu M), and MCF7 cancer cell lines (IC(50) 4.68 and 3.56 mu M). Compounds 3-6 were not active in these assays at a concentration of 10 mu g/mL. C1 [Moreno, Cufemio; Varughese, Titto; Cubilla-Rios, Luis] Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. [Varughese, Titto; Coley, Phyllis D.; Kursar, Thomas A.; Cubilla-Rios, Luis] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. [Spadafora, Carmenza] Natl Secretariat Sci Technol & Innovat, Inst Adv Sci Invest & High Technol Serv, City Of Knowledge, Panama. [Arnold, A. Elizabeth] Univ Arizona, Sch Plant Sci, Tucson, AZ 85721 USA. [Coley, Phyllis D.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Gerwick, William H.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92093 USA. [Gerwick, William H.] Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92093 USA. RP Cubilla-Rios, L (reprint author), Univ Panama, Fac Nat Exact Sci & Technol, Lab Trop Bioorgan Chem, Panama City, Panama. EM lucr@ancon.up.pa OI Spadafora, Carmenza/0000-0002-3002-9467; Moreno Pineda, Eufemio/0000-0002-9643-0341 FU US NIH grant for the International Cooperative Biodiversity Groups [2 U01 TW006634-06]; College of Agriculture and Life Sciences at the University of Arizona FX This work was supported by US NIH grant for the International Cooperative Biodiversity Groups program (ICBG-Panama; 2 U01 TW006634-06). We thank Malkanthi Gunatilaka and Douglas Mahana for assistance with DNA sequencing, and the College of Agriculture and Life Sciences at the University of Arizona for logistical and financial support. We express our thanks to the personnel of Panama's Autoridad Nacional del Ambiente for facilitating this research. NR 34 TC 1 Z9 1 U1 1 U2 6 PU NATURAL PRODUCTS INC PI WESTERVILLE PA 7963 ANDERSON PARK LN, WESTERVILLE, OH 43081 USA SN 1934-578X J9 NAT PROD COMMUN JI Nat. Prod. Commun. PD JUN PY 2011 VL 6 IS 6 BP 835 EP 840 PG 6 WC Chemistry, Medicinal; Food Science & Technology SC Pharmacology & Pharmacy; Food Science & Technology GA 780EW UT WOS:000291838300020 ER PT J AU Shen, Y Silver, E Hutton, R Zou, YM AF Shen, Yang Silver, Eric Hutton, Roger Zou, Yaming TI The status of the micro-calorimeter at the Shanghai EBIT SO PHYSICA SCRIPTA LA English DT Article; Proceedings Paper CT 15th International Conference on the Physics of Highly Charged Ions, HCI2010 CY AUG 29-SEP 03, 2010 CL Fudan Univ, Shanghai, PEOPLES R CHINA HO Fudan Univ ID BEAM ION-TRAP; LABORATORY ASTROPHYSICS; MICROCALORIMETER AB This paper contains a brief introduction to the main parameters of a micro-calorimeter designed to operate at the Shanghai electron beam ion trap. This is followed by short descriptions of some aspects of the calorimeter. C1 [Shen, Yang; Hutton, Roger; Zou, Yaming] Fudan Univ, Inst Modern Phys, Shanghai EBIT Lab, Shanghai 200433, Peoples R China. [Silver, Eric] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Shen, Y (reprint author), Fudan Univ, Inst Modern Phys, Shanghai EBIT Lab, Shanghai 200433, Peoples R China. EM rhutton@fudan.edu.cn NR 11 TC 0 Z9 0 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0031-8949 J9 PHYS SCRIPTA JI Phys. Scr. PD JUN PY 2011 VL T144 AR 014060 DI 10.1088/0031-8949/2011/T144/014060 PG 3 WC Physics, Multidisciplinary SC Physics GA 779QR UT WOS:000291795900061 ER PT J AU Smith, LF Smith, JK Arcand, KK Smith, RK Bookbinder, J Keach, K AF Smith, Lisa F. Smith, Jeffrey K. Arcand, Kimberly K. Smith, Randall K. Bookbinder, Jay Keach, Kelly TI Aesthetics and Astronomy: Studying the Public's Perception and Understanding of Imagery From Space SO SCIENCE COMMUNICATION LA English DT Article DE Expert/Novice Differences; Deep Space Imagery; Educational Outreach ID PHYSICS PROBLEMS; PAINTINGS AB This study examined the scientific understanding of astronomical pictures by experts and nonexperts. It explored how both groups perceive astronomical images and their understanding of both what they are seeing and the science that underlies the images. Data comprised n = 8,866 responses from a survey linked to the NASA Astronomical Picture of the Day website and four focus groups held at the Harvard-Smithsonian Center for Astrophysics. Results indicated that variations in presentation of color, explanation, and scale affect comprehension of astronomical imagery. With those who are more expert, shorter, more technical explanations are effective; however, scales are still necessary for complete comprehension. Experts tend to look at the images from a more scientific, data-oriented perspective while nonexperts are more likely to focus, especially initially, on the aesthetic or emotional values of the images. Results provide suggestions for educational outreach to the public. C1 [Smith, Lisa F.; Smith, Jeffrey K.; Keach, Kelly] Univ Otago, Dunedin, New Zealand. [Arcand, Kimberly K.; Smith, Randall K.; Bookbinder, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, LF (reprint author), 145 Union St,POB 56, Dunedin 9054, New Zealand. EM professor.lisa.smith@gmail.com NR 35 TC 9 Z9 9 U1 0 U2 4 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 1075-5470 J9 SCI COMMUN JI Sci. Commun. PD JUN PY 2011 VL 33 IS 2 BP 201 EP 238 DI 10.1177/1075547010379579 PG 38 WC Communication SC Communication GA 778CU UT WOS:000291677700003 ER PT J AU Laurance, WF Laurance, SG Useche, DC AF Laurance, William F. Laurance, Susan G. Useche, D. Carolina TI Gender differences in science: no support for the 'Homer Simpson Effect' among tropical researchers SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter ID FEMALE AUTHORS C1 [Laurance, William F.; Laurance, Susan G.] James Cook Univ, Ctr Trop Environm & Sustainabil Sci TESS, Cairns, Qld 4870, Australia. [Laurance, William F.; Laurance, Susan G.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. [Useche, D. Carolina] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Laurance, WF (reprint author), James Cook Univ, Ctr Trop Environm & Sustainabil Sci TESS, Cairns, Qld 4870, Australia. EM bill.laurance@jcu.edu.au RI Laurance, William/B-2709-2012; James Cook University, TESS/B-8171-2012; Research ID, CTBCC /O-3564-2014; Laurance, Susan/G-6021-2011 OI Laurance, Susan/0000-0002-2831-2933 NR 8 TC 4 Z9 5 U1 1 U2 14 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD JUN PY 2011 VL 26 IS 6 BP 262 EP 263 DI 10.1016/j.tree.2011.03.010 PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 780HA UT WOS:000291843900002 PM 21481965 ER PT J AU Bacon, CD Johnson, GP Meimberg, H Puppo, P Simmons, MP Wagner, WL AF Bacon, Christine D. Johnson, Gabriel P. Meimberg, Harald Puppo, Pamela Simmons, Mark P. Wagner, Warren L. TI DEVELOPMENT OF MICROSATELLITES IN THE HAWAIIAN ENDEMIC PALM PRITCHARDIA MARTII (ARECACEAE) AND THEIR UTILITY IN CONGENERS SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Hawaii; microsatellites; Pritchardia; species delimitation AB Premise of the study: Pritchardia (loulu palm) is the seventh largest flowering plant genus in the Hawaiian archipelago, and many species are of high conservation concern. The island radiation has produced many cryptic species complexes across fine ecological gradients. Microsatellite primers were optimized to investigate genetic diversity of Pritchardia martii (Gaudich.) H. Wendl. and species boundaries among the Hawaiian Pritchardia. Methods and Results: Six new loci and three previously described loci for a closely related genus, Phoenix, were optimized and tested. Five loci were polymorphic, and 72 alleles were detected across loci within P. martii. The five loci were also polymorphic across the other 27 currently recognized Pritchardia species. Conclusions: These results indicate the utility of these microsatellite markers for understanding the conservation genetics of P. martii and species delimitation and hybridization across the genus. C1 [Bacon, Christine D.; Simmons, Mark P.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Johnson, Gabriel P.] Museum Support Ctr, Dept Bot, Smithsonian Inst, Suitland, MD 20746 USA. [Meimberg, Harald; Puppo, Pamela] Univ Porto, Ctr Invest Biodiversidade & Recursos Genet, CIBIO, P-4485661 Vairao, Portugal. [Johnson, Gabriel P.] Museum Support Ctr, Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20746 USA. [Wagner, Warren L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Bacon, CD (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. EM cbacon@rams.colostate.edu RI Simmons, Mark/F-7157-2013 OI Simmons, Mark/0000-0003-3896-4633 FU National Science Foundation [DEB-1010731]; National Tropical Botanical Garden; Smithsonian Institution FX This work was supported by a National Science Foundation Grant (DEB-1010731), the National Tropical Botanical Garden McBryde Graduate Fellowship, and a Smithsonian Institution Pre-doctoral Fellowship to C.D.B. NR 11 TC 0 Z9 0 U1 1 U2 8 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 JUN PY 2011 VL 98 IS 6 BP E139 EP E140 DI 10.3732/ajb.1100073 PG 2 WC Plant Sciences SC Plant Sciences GA 774OJ UT WOS:000291395600002 PM 21653501 ER PT J AU Witte, JC Duncan, BN Douglass, AR Kurosu, TP Chance, K Retscher, C AF Witte, J. C. Duncan, B. N. Douglass, A. R. Kurosu, T. P. Chance, K. Retscher, C. TI The unique OMI HCHO/NO2 feature during the 2008 Beijing Olympics: Implications for ozone production sensitivity SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Air quality; OMI; NO2; HCHO; Beijing Olympics ID AIR-QUALITY; MONITORING INSTRUMENT; SOURCE APPORTIONMENT; TROPOSPHERIC OZONE; POLLUTION; CHINA; EMISSIONS; NOX; FORMALDEHYDE; ATMOSPHERE AB In preparation of the Beijing Summer Olympic and Paralympics Games, strict emission control measures (ECMs) were imposed between July and September 2008 on motor vehicle traffic and industrial emissions to improve air quality. We estimated changes in the chemical sensitivity of ozone production to these ECMs using Ozone Monitoring Instrument (OMI) column measurements of formaldehyde (HCHO) and nitrogen dioxide (NO2), where their ratio serves as a proxy for the sensitivity. During the ECMs, OMI NO2 significantly decreased, subsequently increasing the HCHO/NO2. For the first half of the ECM time period, the ratios maintained values greater than two indicating that ozone production became primarily NOx-limited. In contrast, ozone production was predominantly volatile organic compound (VOC)-limited or mixed VOC-NOx-Iimited during the same period in the preceding three years. After the ECMs were lifted, NO2 and HCHO/NO2 returned to their previous values. The 2005-2008 OMI record shows that this transition to a predominantly NO,-limited regime during the ECMs was unique. Meteorological factors likely explain the variability in HCHO/NO2, particularly the transition to a mixed NOx-VOC-limitation in mid-August during the Olympics, where ozone production became sensitive to both NOx and VOCs until the end of the ECMs. The mixed VOC-NOx-limited regime observed during the Paralympics is also unique because previous years show that Beijing in September is predominantly VOC-limited. Beijing's large-scale tree-planting program was expected to increase levels of biogenic VOCs, but this is not supported by OMI HCHO data. However, MODIS vegetation indices show a small increase in vegetation cover from 2003 leading up to the Games in 2008. After the Games, however, there was a downturn in the indices (2009 and 2010) to levels similar to 2006. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Witte, J. C.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Witte, J. C.; Duncan, B. N.; Douglass, A. R.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. [Kurosu, T. P.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Retscher, C.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Witte, JC (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA. EM jacquelyn.Witte@nasa.gov RI Duncan, Bryan/A-5962-2011; Douglass, Anne/D-4655-2012; OI Chance, Kelly/0000-0002-7339-7577 FU NASA's Atmospheric Chemistry, Modeling and Analysis; Applied Sciences Air Quality Programs FX This work is supported by NASA's Atmospheric Chemistry, Modeling and Analysis and Applied Sciences Air Quality Programs. NR 45 TC 9 Z9 11 U1 6 U2 52 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 JUN PY 2011 VL 45 IS 18 BP 3103 EP 3111 DI 10.1016/j.atmosenv.2011.03.015 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 775JB UT WOS:000291454500011 ER PT J AU Wikramanayake, E Dinerstein, E Seidensticker, J Lumpkin, S Pandav, B Shrestha, M Mishra, H Ballou, J Johnsingh, AJT Chestin, I Sunarto, S Thinley, P Thapa, K Jiang, GS Elagupillay, S Kafley, H Pradhan, NMB Jigme, K Teak, S Cutter, P Aziz, MA Than, U AF Wikramanayake, Eric Dinerstein, Eric Seidensticker, John Lumpkin, Susan Pandav, Bivash Shrestha, Mahendra Mishra, Hemanta Ballou, Jonathan Johnsingh, A. J. T. Chestin, Igor Sunarto, Sunarto Thinley, Phuntsho Thapa, Kanchan Jiang, Guangshun Elagupillay, Sivananthan Kafley, Hemanta Pradhan, Narendra Man Babu Jigme, Karma Teak, Seng Cutter, Peter Aziz, Md. Abdul Than, Utin TI A landscape-based conservation strategy to double the wild tiger population SO CONSERVATION LETTERS LA English DT Article DE Connectivity; conservation; corridors; metapopulations; tigers; tiger ecology; tiger landscapes ID DENSITIES; VIABILITY; MAMMALS; PREY AB In an unprecedented response to the rapid decline in wild tiger populations, the Heads of Government of the 13 tiger range countries endorsed the St. Petersburg Declaration in November 2010, pledging to double the wild tiger population. We conducted a landscape analysis of tiger habitat to determine if a recovery of such magnitude is possible. The reserves in 20 priority tiger landscapes can potentially support > 10,000 tigers, almost thrice the current estimate. However, most core reserves where tigers breed are small and land-use change in rapidly developing Asia threatens to increase reserve and population isolation. Maintaining population viability and resilience will depend upon a landscape approach to manage tigers as metapopulations. Thus, both site-level protection and landscape-scale interventions to secure habitat corridors are simultaneous imperatives. Co-benefits, such as payment schemes for carbon and other ecosystem services, should be employed as strategies to mainstream landscape conservation in tiger habitat into development processes. C1 [Wikramanayake, Eric; Dinerstein, Eric] World Wildlife Fund, Washington, DC 20037 USA. [Seidensticker, John; Lumpkin, Susan; Ballou, Jonathan] Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Pandav, Bivash] Nepal Program, World Wildlife Fund, Kathmandu, Nepal. [Shrestha, Mahendra] Natl Fish & Wildlife Fdn, Save Tiger Fund, Washington, DC 20005 USA. [Mishra, Hemanta] Bridge Fund, Vienna, VA 22181 USA. [Johnsingh, A. J. T.] Nat Conservat Fdn, Bangalore, Karnataka, India. [Johnsingh, A. J. T.] WWF India, Delhi, India. [Chestin, Igor] Russian Federat, Moscow 109240, Russia. [Sunarto, Sunarto; Thapa, Kanchan] Virginia Polytech Inst & State Univ, Dept Fisheries & Wildlife Sci, Blacksburg, VA 24061 USA. [Thinley, Phuntsho] Jigme Dorji Natl Pk, Dept Forests & Pk Serv, Thimphu, Bhutan. [Jiang, Guangshun] World Wildlife Fund, China Program, Harbin, Peoples R China. [Jiang, Guangshun] NE Forestry Univ, Coll Wildlife Resources, Harbin, Peoples R China. [Elagupillay, Sivananthan] Dept Wildlife & Natl Pk, Kuala Lumpur, Malaysia. [Kafley, Hemanta] Univ Missouri, Dept Fisheries & Wildlife Sci, Columbia, MO 65211 USA. [Pradhan, Narendra Man Babu] Chitwan Natl Pk, Dept Natl Parks & Wildlife, Bharatpur, Nepal. [Jigme, Karma] Dept Forests & Pk Serv, Thimphu, Bhutan. [Teak, Seng] WWF Cambodia, Chamkarmon Phnom Penh, Cambodia. [Cutter, Peter; Than, Utin] WWF Greater Mekong Programme, Bangkok, Thailand. [Aziz, Md. Abdul] Jahangirnagar Univ, Dhaka, Bangladesh. [Aziz, Md. Abdul] Wildlife Trust Bangladesh, Dhaka, Bangladesh. RP Dinerstein, E (reprint author), World Wildlife Fund, 1250 24th St,NW, Washington, DC 20037 USA. EM eric.dinerstein@wwfus.org RI Kafley, Hemanta/E-1973-2015; OI Thinley, Phuntsho/0000-0002-5062-8010 NR 35 TC 44 Z9 47 U1 6 U2 69 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1755-263X J9 CONSERV LETT JI Conserv. Lett. PD JUN-JUL PY 2011 VL 4 IS 3 BP 219 EP 227 DI 10.1111/j.1755-263X.2010.00162.x PG 9 WC Biodiversity Conservation SC Biodiversity & Conservation GA 774QZ UT WOS:000291402500006 ER PT J AU Lobanov, Y Tong, E Blundell, R Hedden, A Voronov, B Gol'tsman, G AF Lobanov, Y. Tong, E. Blundell, R. Hedden, A. Voronov, B. Gol'tsman, G. TI Large-Signal Frequency Response of an HEB Mixer: From 300 MHz to Terahertz SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Frequency response; hot electron bolometer; waveguide mixers AB We present a study of the large signal frequency response of an HEB mixer over a wide frequency range. In our experiments, we have subjected the HEB mixer to incident electromagnetic radiation from 0.3 GHz to 1 THz. The mixer element is an NbN film deposited on crystalline quartz. The mixer chip is mounted in a waveguide cavity, coupled to free space with a diagonal horn. At microwave frequencies, electromagnetic radiation is applied through the coaxial bias port of the mixer block. At higher frequencies the input signal passes via the diagonal horn feed. At each frequency, the incident power is varied and a family of I-V curves is recorded. From the curves we identify 3 distinct regimes of operation of the mixer separated by the phonon relaxation frequency and the superconducting energy gap frequency observed at about 3 GHz and 660 GHz respectively. In this paper, we will present observed curves and discuss the results of our experiment. C1 [Lobanov, Y.; Tong, E.; Blundell, R.; Hedden, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. [Voronov, B.; Gol'tsman, G.] Moscow State Pedag Univ, Moscow 119992, Russia. RP Lobanov, Y (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. EM ylobanov@cfa.harvard.edu RI Lobanov, Yury/A-3615-2014; OI Lobanov, Yury/0000-0001-7801-0223; Tong, Edward/0000-0002-7736-4203 NR 9 TC 6 Z9 6 U1 0 U2 9 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2011 VL 21 IS 3 BP 628 EP 631 DI 10.1109/TASC.2011.2105851 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 769XB UT WOS:000291050500127 ER PT J AU Lobanov, YV Tong, CYE Hedden, AS Blundell, R Voronov, BM Gol'tsman, GN AF Lobanov, Yury V. Tong, Cheuk-yu E. Hedden, Abigail S. Blundell, Raymond Voronov, Boris M. Gol'tsman, Gregory N. TI Direct Measurement of the Gain and Noise Bandwidths of HEB Mixers SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Gain and noise bandwidth of the HEB mixer; HEB mixer impedance; hot electron bolometer ID ELECTRON BOLOMETER MIXERS; OPERATION; RECEIVER AB The intermediate frequency (IF) bandwidth of a hot electron bolometer (HEB) mixer is an important parameter of the mixer, in that it helps to determine its suitability for a given application. With the availability of wideband low noise amplifiers, it is simple to measure the performance of an HEB mixer over a wide range of IF at a fixed LO frequency using the standard Y-factor method. This in-situ method allows us to measure both the gain and noise bandwidths simultaneously. We have also measured mixer output impedance with a vector network analyser. Intrinsic time constant has been extracted from the impedance data and compared to the mixer's bandwidths determined from receiver Y-factor measurement. C1 [Lobanov, Yury V.; Tong, Cheuk-yu E.; Hedden, Abigail S.; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Voronov, Boris M.; Gol'tsman, Gregory N.] Moscow State Pedag Univ, Moscow 119991, Russia. RP Lobanov, YV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ylobanov@cfa.harvard.edu RI Lobanov, Yury/A-3615-2014; OI Lobanov, Yury/0000-0001-7801-0223; Tong, Edward/0000-0002-7736-4203 NR 20 TC 5 Z9 5 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2011 VL 21 IS 3 BP 645 EP 648 DI 10.1109/TASC.2010.2095403 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 769XB UT WOS:000291050500131 ER PT J AU Tong, CYE Paine, SN Blundell, R AF Tong, Cheuk-Yu E. Paine, Scott N. Blundell, Raymond TI Characterization of SIS Receivers Using a Digital Spectrometer SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article DE Spectrometer; standing wave measurements; superconductor-insulator-superconductor (SIS) mixers AB Fourier transform based digital spectrometers, which offer wide instantaneous bandwidth and high spectral resolution, are widely used in SIS receiver systems. In this paper, we demonstrate that a digital spectrometer connected to the output of an SIS receiver can be used to probe the standing wave structure in the optics between the SIS mixer and a terminating input load. It can be shown that this standing wave induces ripples in the output power spectrum of the mixer, the amplitude of which depends on the product of the voltage reflection coefficients of the load and the mixer. This relation can be exploited to derive the input reflection coefficient of the SIS mixer as well as its sideband ratio. Both the theory and experimental details will be presented. C1 [Tong, Cheuk-Yu E.; Paine, Scott N.; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM etong@cfa.harvard.edu OI Tong, Edward/0000-0002-7736-4203; Paine, Scott/0000-0003-4622-5857 NR 11 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2011 VL 21 IS 3 BP 659 EP 662 DI 10.1109/TASC.2010.2100016 PN 1 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 769XB UT WOS:000291050500134 ER PT J AU Zeininger, A Richmond, BG Hartman, G AF Zeininger, Angel Richmond, Brian G. Hartman, Gideon TI Metacarpal head biomechanics: A comparative backscattered electron image analysis of trabecular bone mineral density in Pan troglodytes, Pongo pygmaeus, and Homo sapiens SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Hands; Primate locomotion; Knuckle-walking ID MICRO-COMPUTED TOMOGRAPHY; KNUCKLE-WALKING; FEMORAL-HEAD; APPARENT DENSITY; SUBCHONDRAL BONE; DISTAL RADIUS; HAND POSTURES; ARCHITECTURE; PRIMATES; JOINT AB Great apes and humans use their hands in fundamentally different ways, but little is known about joint biomechanics and internal bone variation. This study examines the distribution of mineral density in the third metacarpal heads in three hominoid species that differ in their habitual joint postures and loading histories. We test the hypothesis that micro-architectural properties relating to bone mineral density reflect habitual joint use. The third metacarpal heads of Pan troglodytes, Pongo pygmaeus, and Homo sapiens were sectioned in a sagittal plane and imaged using backscattered electron microscopy (BSE-SEM). For each individual, 72 areas of subarticular cortical (subchondral) and trabecular bone were sampled from within 12 consecutive regions of the BSE-SEM images. In each area, gray levels (representing relative mineralization density) were quantified. Results show that chimpanzee, orangutan, and human metacarpal III heads have different gray level distributions. Weighted mean gray levels (WMGLs) in the chimpanzee showed a distinct pattern in which the 'knuckle-walking' regions (dorsal) and 'climbing' regions (palmar) are less mineralized, interpreted to reflect elevated remodeling rates, than the distal regions. Pongo pygmaeus exhibited the lowest WMGLs in the distal region, suggesting elevated remodeling rates in this region, which is loaded during hook grip hand postures associated with suspension and climbing. Differences among regions within metacarpal heads of the chimpanzee and orangutan specimens are significant (Kruskal Wallis, p < 0.001). In humans, whose hands are used for manipulation as opposed to locomotion, mineralization density is much more uniform throughout the metacarpal head. WMGLs were significantly (p < 0.05) lower in subchondral compared to trabecular regions in all samples except humans. This micro-architectural approach offers a means of investigating joint loading patterns in primates and shows significant differences in metacarpal joint biomechanics among great apes and humans. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20051 USA. [Zeininger, Angel] Univ Texas Austin, Dept Anthropol, Austin, TX 78712 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Hartman, Gideon] Univ Connecticut, Dept Anthropol, Storrs, CT 06269 USA. RP Richmond, BG (reprint author), George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, 2110 G St NW, Washington, DC 20051 USA. EM brich@gwu.edu FU NSF-IGERT [DGE-9987590]; NSF [BCS-0521835] FX We thank Scott Whittaker, Amelia Logan, and Ed Vicenzi for assistance in SEM data collection and permission to use the SEM facilities at the Smithsonian Institution's National Museum of Natural History. We are grateful to Tim Gooding of the NMNH's Mineral Sciences Department for aiding in sample preparation. We thank Mary Marzke and Caley Orr of Arizona State University for donating the Pongo specimen. Thanks also to Nicole Griffin and Matt Skinner for helpful discussions and assistance, and to Tim Bromage, the anonymous reviewers, the Associate Editor, Susan Anton, Liza Shapiro, and Shannon McFarlin for constructive comments and suggestions on an earlier version of this manuscript. This research was supported in part by an Undergraduate Research Internship to AZ funded by NSF-IGERT grant DGE-9987590, and NSF BCS-0521835 to BR. NR 49 TC 9 Z9 9 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 JUN PY 2011 VL 60 IS 6 BP 703 EP 710 DI 10.1016/j.jhevol.2011.01.002 PG 8 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 771FX UT WOS:000291143700005 PM 21316735 ER PT J AU Gilmour, CC Elias, DA Kucken, AM Brown, SD Palumbo, AV Schadt, CW Wall, JD AF Gilmour, Cynthia C. Elias, Dwayne A. Kucken, Amy M. Brown, Steven D. Palumbo, Anthony V. Schadt, Christopher W. Wall, Judy D. TI Sulfate-Reducing Bacterium Desulfovibrio desulfuricans ND132 as a Model for Understanding Bacterial Mercury Methylation SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID DESULFOBULBUS-PROPIONICUS 1PR3; ESTUARINE SEDIMENT SLURRIES; MARINE-SEDIMENTS; METHYLMERCURY PRODUCTION; CHESAPEAKE BAY; VULGARIS HILDENBOROUGH; ANAEROBIC-BACTERIA; STABLE-ISOTOPES; CARBON-DIOXIDE; PURE CULTURES AB We propose the use of Desulfovibrio desulfuricans ND132 as a model species for understanding the mechanism of microbial Hg methylation. Strain ND132 is an anaerobic dissimilatory sulfate-reducing bacterium (DSRB), isolated from estuarine mid-Chesapeake Bay sediments. It was chosen for study because of its exceptionally high rates of Hg methylation in culture and its metabolic similarity to the lost strain D. desulfuricans LS, the only organism for which methylation pathways have been partially defined. Strain ND132 is an incomplete oxidizer of short-chain fatty acids. It is capable of respiratory growth using fumarate as an electron acceptor, supporting growth without sulfide production. We used enriched stable Hg isotopes to show that ND132 simultaneously produces and degrades methylmercury (MeHg) during growth but does not produce elemental Hg. MeHg produced by cells is mainly excreted, and no MeHg is produced in spent medium. Mass balances for Hg and MeHg during the growth of cultures, including the distribution between filterable and particulate phases, illustrate how medium chemistry and growth phase dramatically affect Hg solubility and availability for methylation. The available information on Hg methylation among strains in the genus Desulfovibrio is summarized, and we present methylation rates for several previously untested species. About 50% of Desulfovibrio strains tested to date have the ability to produce MeHg. Importantly, the ability to produce MeHg is constitutive and does not confer Hg resistance. A 16S rRNA-based alignment of the genus Desulfovibrio allows the very preliminary assessment that there may be some evolutionary basis for the ability to produce MeHg within this genus. C1 [Gilmour, Cynthia C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Elias, Dwayne A.; Brown, Steven D.; Palumbo, Anthony V.; Schadt, Christopher W.] Oak Ridge Natl Lab, BioSci Div, Oak Ridge, TN USA. [Kucken, Amy M.; Wall, Judy D.] Univ Missouri, Dept Biochem & Mol Microbiol & Immunol, Columbia, MO USA. RP Gilmour, CC (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM gilmourc@si.edu RI Palumbo, Anthony/A-4764-2011; Elias, Dwayne/B-5190-2011; Schadt, Christopher/B-7143-2008; Brown, Steven/A-6792-2011; Gilmour, Cynthia/G-1784-2010 OI Palumbo, Anthony/0000-0002-1102-3975; Elias, Dwayne/0000-0002-4469-6391; Schadt, Christopher/0000-0001-8759-2448; Brown, Steven/0000-0002-9281-3898; Gilmour, Cynthia/0000-0002-1720-9498 FU U.S. Department of Energy; Office of Biological and Environmental Research, Office of Science at Oak Ridge National Laboratory (ORNL) [DE-FG02-07ER64396]; National Science Foundation [DEB0351050]; SERC; Department of Energy [DE-AC05-00OR22725] FX This work was supported by the U.S. Department of Energy under the Subsurface Biogeochemical Research Program (SBR), Office of Biological and Environmental Research, Office of Science, in part through the Mercury Science Focus Area Program at Oak Ridge National Laboratory (ORNL), through DE-FG02-07ER64396 (J.D.W.), by National Science Foundation grant DEB0351050 (C.C.G.), and by the SERC Research Experience for Undergraduates program. ORNL is managed by University of Tennessee UT-Battelle, LLC, for the Department of Energy under contract no. DE-AC05-00OR22725. NR 71 TC 74 Z9 79 U1 7 U2 71 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD JUN PY 2011 VL 77 IS 12 BP 3938 EP 3951 DI 10.1128/AEM.02993-10 PG 14 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 773WI UT WOS:000291341800005 PM 21515733 ER PT J AU Lotfi, E Jamshidi-Ghaleh, K Moslemi, F Masalehdan, H AF Lotfi, E. Jamshidi-Ghaleh, K. Moslemi, F. Masalehdan, H. TI Optical multistability in 1D photonic crystals with nonlinear Thue-Morse structure SO APPLIED PHYSICS A-MATERIALS SCIENCE & PROCESSING LA English DT Article AB A 1D photonic crystal structure contains 16 layers, 8 common dielectric layers and 8 layers with nonlinear medium, with an arrangement similar to the 5th generation, Thue-Morse multilayer is presented. The properties of photonics band gap, field distribution and optical multistability are investigated. On the band gap, 5 resonant modes is observed. On the behavior of output intensity versus input intensity around resonant frequencies, the multistability response observed. When the frequency of incident field is close to the resonant frequency, the threshold intensity of multistability is decreased. C1 [Masalehdan, H.] Bonab Islamic Azad Univ, Phys Engn Opt Laser Dept, Bonab, Iran. [Lotfi, E.] Fac Bonab Engn & Technol, Bonab, Iran. [Jamshidi-Ghaleh, K.] Azarbaijan Univ Tarbiat Moallem, Dept Phys, Tabriz, Iran. [Moslemi, F.] Islamic Azad Univ, Gogan Branch, Dept Phys, Gogan, Iran. [Masalehdan, H.] Smithsonian Inst, Dept Appl Phys, Washington, DC 20013 USA. RP Masalehdan, H (reprint author), Bonab Islamic Azad Univ, Phys Engn Opt Laser Dept, Bonab, Iran. EM H.Masalehdan@Gmail.com NR 11 TC 3 Z9 3 U1 1 U2 9 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0947-8396 J9 APPL PHYS A-MATER JI Appl. Phys. A-Mater. Sci. Process. PD JUN PY 2011 VL 103 IS 3 BP 669 EP 672 DI 10.1007/s00339-010-6200-4 PG 4 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA 771MF UT WOS:000291161700032 ER PT J AU Yavitt, JB Harms, KE Garcia, MN Mirabello, MJ Wright, SJ AF Yavitt, Joseph B. Harms, Kyle E. Garcia, Milton N. Mirabello, Matt J. Wright, S. Joseph TI Soil fertility and fine root dynamics in response to 4 years of nutrient (N, P, K) fertilization in a lowland tropical moist forest, Panama SO AUSTRAL ECOLOGY LA English DT Article DE fine root biomass; fine root turnover; forest nutrient fertilization; minirhizotron; nutrient availability ID NORTHERN HARDWOOD FOREST; RAIN-FORESTS; LIFE-SPAN; PHOSPHORUS FERTILIZATION; TERRESTRIAL ECOSYSTEMS; HEDLEY FRACTIONATION; AVAILABILITY; NITROGEN; LIMITATION; BIOMASS AB The question of how tropical trees cope with infertile soils has been challenging to address, in part, because fine root dynamics must be studied in situ. We used annual fertilization with nitrogen (N as urea, 12.5 g N m-2 year-1), phosphorus (P as superphosphate, 5 g P m-2 year-1) and potassium (K as KCl, 5 g K m-2 year-1) within 38 ha of old-growth lowland tropical moist forest in Panama and examined fine root dynamics with minirhizotron images. We expected that added P, above all, would (i) decrease fine root biomass but, (ii) have no impact on fine root turnover. Soil in the study area was moderately acidic (pH = 5.28), had moderate concentrations of exchangeable base cations (13.4 cmol kg-1), low concentrations of Bray-extractable phosphate (PO(4) = 2.2 mg kg-1), and modest concentrations of KCl-extractable nitrate (NO(3) = 5.0 mg kg-1) and KCl-extractable ammonium (NH(4) = 15.5 mg kg-1). Added N increased concentrations of KCl-extractable NO(3) and acidified the soil by one pH unit. Added P increased concentrations of Bray-extractable PO(4) and P in the labile fraction. Concentrations of exchangeable K were elevated in K addition plots but reduced by N additions. Fine root dynamics responded to added K rather than added P. After 2 years, added K decreased fine root biomass from 330 to 275 g m-2. The turnover coefficient of fine roots < 1 mm diameter ranged from 2.6 to 4.4 per year, and the largest values occurred in plots with added K. This study supported the view that biomass and dynamics of fine roots respond to soil nutrient availability in species-rich, lowland tropical moist forest. However, K rather than P elicited root responses. Fine roots smaller than 1 mm have a short lifetime (< 140 days), and control of fine root production by nutrient availability in tropical forests deserves more study. C1 [Yavitt, Joseph B.; Mirabello, Matt J.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Harms, Kyle E.; Garcia, Milton N.; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Yavitt, JB (reprint author), Cornell Univ, Dept Nat Resources, Fernow Hall, Ithaca, NY 14853 USA. EM jby1@cornell.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Andrew W. Mellon Foundation; Smithsonian Scholarly Studies program; Smithsonian Tropical Research Institute FX Research support provided by grants from the Andrew W. Mellon Foundation and the Smithsonian Scholarly Studies program. The Smithsonian Tropical Research Institute provides support for the ongoing Gigante Fertilization Project. We thank Omar Hernandez and Rufino Gonzalez in Panama and many students at Cornell University for assistance in the field and in the laboratory. NR 69 TC 39 Z9 40 U1 9 U2 74 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1442-9985 J9 AUSTRAL ECOL JI Austral Ecol. PD JUN PY 2011 VL 36 IS 4 BP 433 EP 445 DI 10.1111/j.1442-9993.2010.02157.x PG 13 WC Ecology SC Environmental Sciences & Ecology GA 769YY UT WOS:000291055400009 ER PT J AU Adey, WH Kangas, PC Mulbry, W AF Adey, Walter H. Kangas, Patrick C. Mulbry, Walter TI Algal Turf Scrubbing: Cleaning Surface Waters with Solar Energy while Producing a Biofuel SO BIOSCIENCE LA English DT Article DE algae; biofuel; ecological engineering; nitrogen; phosphorus ID DAIRY MANURE EFFLUENT; LOADING RATES; NUTRIENT REMOVAL; PRODUCTIVITY; BIOMASS; MICROALGAE; RECOVERY; STREAMS; SYSTEM AB As human populations have expanded, Earth's atmosphere and natural waters have become dumps for agricultural and industrial wastes. Remediation methods of the last half century have been largely unsuccessful. In many US watersheds, surface waters are eutrophic, and coastal water bodies, such as the Chesapeake Bay and the Gulf of Mexico, have become increasingly hypoxic. The algal turf scrubber (ATS) is an engineered system for flowing pulsed wastewaters over sloping surfaces with attached, naturally seeded filamentous algae. This treatment has been demonstrated for tertiary sewage, farm wastes, streams, and large aquaculture systems; rates as large as 40 million to 80 million liters per day (lpd) are routine. Whole-river-cleaning systems of 12 billion lpd are in development. The algal biomass, produced at rates 5 to 10 times those of other types of land-based agriculture, can be fermented, and significant research and development efforts to produce ethanol, butanol, and methane are under way. Unlike with algal photobioreactor systems, the cost of producing biofuels from the cleaning of wastewaters by ATS can be quite low. C1 [Adey, Walter H.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kangas, Patrick C.] Univ Maryland, Dept Environm Sci & Technol, College Pk, MD 20742 USA. [Mulbry, Walter] ARS, Environm Management & Byprod Utilizat Lab, USDA, Beltsville, MD USA. RP Adey, WH (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. EM adeyw@si.edu FU Lewis Foundation FX We gratefully acknowledge HydroMentia, Inc., for providing figures 4 and 5 and John Miller (Western Michigan University) for providing information for table 1. Funding was provided by a gift from the Lewis Foundation to the Smithsonian Institution. J. Emmett Duffy and Raleigh Hood provided many constructive comments on the manuscript and submitted supporting letters in an early stage of manuscript development. Their insightful comments were crucial to the development of a cogent manuscript. NR 51 TC 34 Z9 35 U1 6 U2 76 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD JUN PY 2011 VL 61 IS 6 BP 434 EP 441 DI 10.1525/bio.2011.61.6.5 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 773TM UT WOS:000291333700005 ER PT J AU Armitage, SAO Broch, JF Marin, HF Nash, DR Boomsma, JJ AF Armitage, Sophie A. O. Broch, Jens F. Fernandez Marin, Hermogenes Nash, David R. Boomsma, Jacobus J. TI IMMUNE DEFENSE IN LEAF-CUTTING ANTS: A CROSS-FOSTERING APPROACH SO EVOLUTION LA English DT Article DE Acromyrmex echinatior; antibacterial activity; cross-fostering; ecological immunology; metapleural gland; Pseudonocardia ID FUNGUS-GROWING ANTS; METAPLEURAL GLAND SECRETION; ACROMYRMEX-OCTOSPINOSUS; ANTIMICROBIAL DEFENSE; MUTUALISTIC BACTERIUM; TRIPARTITE MUTUALISM; EVOLUTIONARY ECOLOGY; BATEMANS PRINCIPLE; GENETIC DIVERSITY; SOCIAL IMMUNITY AB To ameliorate the impact of disease, social insects combine individual innate immune defenses with collective social defenses. This implies that there are different levels of selection acting on investment in immunity, each with their own trade-offs. We present the results of a cross-fostering experiment designed to address the influences of genotype and social rearing environment upon individual and social immune defenses. We used a multiply mating leaf-cutting ant, enabling us to test for patriline effects within a colony, as well as cross-colony matriline effects. The worker's father influenced both individual innate immunity (constitutive antibacterial activity) and the size of the metapleural gland, which secretes antimicrobial compounds and functions in individual and social defense, indicating multiple mating could have important consequences for both defense types. However, the primarily social defense, a Pseudonocardia bacteria that helps to control pathogens in the ants' fungus garden, showed a significant colony of origin by rearing environment interaction, whereby ants that acquired the bacteria of a foster colony obtained a less abundant cover of bacteria: one explanation for this pattern would be co-adaptation between host colonies and their vertically transmitted mutualist. These results illustrate the complexity of the selection pressures that affect the expression of multilevel immune defenses. C1 [Armitage, Sophie A. O.; Broch, Jens F.; Fernandez Marin, Hermogenes; Nash, David R.; Boomsma, Jacobus J.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. [Fernandez Marin, Hermogenes] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Armitage, SAO (reprint author), Univ Munster, Inst Evolut & Biodivers, Hufferstr 1, D-48149 Munster, Germany. EM sophie.armitage@uni-muenster.de RI Nash, David/B-2916-2009; Armitage, Sophie/A-6961-2012; Nash, David/H-4433-2012; Boomsma, Jacobus/M-2785-2014 OI Nash, David/0000-0002-0462-6794; Armitage, Sophie/0000-0002-5561-9543; Nash, David/0000-0002-0462-6794; Boomsma, Jacobus/0000-0002-3598-1609 FU Danish National Research Foundation; Panamanian government; Intra-European Marie Curie fellowship; Volkswagen Foundation FX We would like to thank the Smithsonian Tropical Research Institute for providing facilities for the collection of ant colonies and the Autoridad Nacional del Ambiente (ANAM) for permission to collect and export the ants from Panama to Denmark. We would also like to thank S. Mathiasen for microsatellite advice, J. Pedersen for paternity assignment advice, A. Ivens for unpublished AFLP data, C. Sick for assistance with the antibacterial assay, and A. Read and two anonymous referees for their constructive comments. Funding was provided by the Danish National Research Foundation for JFB, HFM, DRN, and JJB, a SENACYT post-doctoral fellowship from the Panamanian government for HFM, and an individual Intra-European Marie Curie fellowship and a Volkswagen Foundation postdoctoral fellowship for SAOA. NR 53 TC 11 Z9 11 U1 2 U2 34 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0014-3820 J9 EVOLUTION JI Evolution PD JUN PY 2011 VL 65 IS 6 BP 1791 EP 1799 DI 10.1111/j.1558-5646.2011.01241.x PG 9 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 772XB UT WOS:000291270300020 PM 21644963 ER PT J AU Riley, S AF Riley, Sheila TI Bitter Bitch SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila] Smithsonian Inst Libs, Washington, DC USA. RP Riley, S (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2011 VL 136 IS 10 BP 94 EP 94 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 771YB UT WOS:000291195500057 ER PT J AU Hong, T AF Hong, Terry TI An Empty Room SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2011 VL 136 IS 10 BP 96 EP 96 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 771YB UT WOS:000291195500064 ER PT J AU McCoy, MW Bolker, BM Warkentin, KM Vonesh, JR AF McCoy, Michael W. Bolker, Benjamin M. Warkentin, Karen M. Vonesh, James R. TI Predicting Predation through Prey Ontogeny Using Size-Dependent Functional Response Models SO AMERICAN NATURALIST LA English DT Article DE size structure; consumer-resource; predator-prey; density dependence; Bayesian; amphibian ID RED-EYED TREEFROG; INTRAGUILD PREDATION; BODY-SIZE; STRUCTURED POPULATIONS; ECOLOGICAL COMMUNITIES; HATCHING PLASTICITY; MUTUAL INTERFERENCE; SELECTIVE PREDATION; LARVAL DRAGONFLIES; ALTERNATIVE PREY AB The functional response is a critical link between consumer and resource dynamics, describing how a consumer's feeding rate varies with prey density. Functional response models often assume homogenous prey size and size-independent feeding rates. However, variation in prey size due to ontogeny and competition is ubiquitous, and predation rates are often size dependent. Thus, functional responses that ignore prey size may not effectively predict predation rates through ontogeny or in heterogeneous populations. Here, we use short-term response-surface experiments and statistical modeling to develop and test prey size-dependent functional responses for water bugs and dragonfly larvae feeding on red-eyed treefrog tadpoles. We then extend these models through simulations to predict mortality through time for growing prey. Both conventional and size-dependent functional response models predicted average overall mortality in short-term mixed-cohort experiments, but only the size-dependent models accurately captured how mortality was spread across sizes. As a result, simulations that extrapolated these results through prey ontogeny showed that differences in size-specific mortality are compounded as prey grow, causing predictions from conventional and size-dependent functional response models to diverge dramatically through time. Our results highlight the importance of incorporating prey size when modeling consumer-prey dynamics in size-structured, growing prey populations. C1 [McCoy, Michael W.; Vonesh, James R.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. [McCoy, Michael W.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Bolker, Benjamin M.] McMaster Univ, Dept Math & Stat, Hamilton, ON L8S 4K1, Canada. [Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Warkentin, Karen M.] Smithsonian Trop Res Inst, Balboa, Panama. RP McCoy, MW (reprint author), Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. EM anura@ufl.edu RI Vonesh, James/I-1573-2013; OI Vonesh, James/0000-0003-2481-9988; Bolker, Benjamin/0000-0002-2127-0443 FU National Science Foundation (NSF) [DEB-0716923, DEB-0717220, IGERT-0801544]; Boston University; Virginia Commonwealth University; STRI FX We thank the Autoridad Nacional del Ambiente de Panama for permission to conduct this research in Panama (permiso no. SE/A-41-08) and the Smithsonian Tropical Research Institute (STRI) for use of their facilities and logistical support. This research was conducted under Boston University Institutional Animal Care and Use Committee (IACUC) protocol 08-011 and STRI's IACUC protocol 2008-04-06-24-08. We thank C. Casey, D. Emery, K. Gonyer, J. Hite, M. Hughey, A. Nicolas, S. Summit, and J. Worley for their hours in the field and collecting and processing data. We thank D. Dent, M. Hughey, K. McCoy, and J. Touchon for many insightful discussions about the work and two anonymous reviewers for their suggestions to improve the manuscript. This research was supported by National Science Foundation (NSF) grants DEB-0716923 to K.M.W. and DEB-0717220 to J.R.V., Boston University, Virginia Commonwealth University, STRI, and NSF grant IGERT-0801544 to B.M.B. NR 96 TC 26 Z9 27 U1 6 U2 56 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD JUN PY 2011 VL 177 IS 6 BP 752 EP 766 DI 10.1086/659950 PG 15 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 768QZ UT WOS:000290953000006 PM 21597252 ER PT J AU Westbrook, JW Kitajima, K Burleigh, JG Kress, WJ Erickson, DL Wright, SJ AF Westbrook, Jared W. Kitajima, Kaoru Burleigh, J. Gordon Kress, W. John Erickson, David L. Wright, S. Joseph TI What Makes a Leaf Tough? Patterns of Correlated Evolution between Leaf Toughness Traits and Demographic Rates among 197 Shade-Tolerant Woody Species in a Neotropical Forest SO AMERICAN NATURALIST LA English DT Article DE functional traits; leaf toughness; defense; phylogenetically independent contrasts; shade tolerance; life-history trade-offs ID PHYLOGENETICALLY INDEPENDENT CONTRASTS; LOWLAND RAIN-FORESTS; FRACTURE-TOUGHNESS; TROPICAL FORESTS; HABITAT SPECIALIZATION; MOLECULAR EVOLUTION; RELATIVE IMPORTANCE; AMAZONIAN FORESTS; DIVERGENCE TIMES; PLANT DIVERSITY AB Slow-growing juveniles of shade-tolerant plant species are predicted to have tough leaves because of the high cost of leaf replacement in shade relative to potential carbon gain. We assessed the degree of correlated evolution among eight traits associated with leaf toughness and the relationships of those traits with the growth and mortality rates of 197 tree and shrub species from the understory of the 50-ha forest dynamics plot on Barro Colorado Island, Panama. Path analysis with phylogenetically independent contrasts revealed that leaves attained material toughness (resistance to fracture per unit fracture area) through increases in tissue density, percent cellulose per unit dry mass, and vein fracture toughness. Lamina density and cellulose content evolved independently and thus represent different paths to material toughness. Structural toughness (resistance to fracture per unit fracture length) depended on material toughness and lamina thickness. Mortality rates of individuals 1-10 cm in stem diameter were negatively correlated with material toughness and lamina density but were independent of structural toughness and cell wall fiber contents. Leaf toughness traits were uncorrelated with relative growth rates. Results imply that material toughness enhances resistance to natural enemies, which increases survival and offsets the biomass allocation cost of producing tough leaves in the shaded understory. C1 [Westbrook, Jared W.; Kitajima, Kaoru; Burleigh, J. Gordon] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Kitajima, Kaoru; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama. [Kress, W. John; Erickson, David L.] Smithsonian Natl Museum Nat Hist, Dept Bot MRC 166, Washington, DC 20013 USA. RP Westbrook, JW (reprint author), Univ Florida, Dept Biol, POB 118525, Gainesville, FL 32611 USA. EM jwestbrook@ufl.edu RI Kitajima, Kaoru/E-8877-2012; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU F. H. Levinson Fund; National Science Foundation; MacArthur Foundation FX We thank D. Brassfield for leaf collection, E. Oriel for measuring leaf toughness, and M. Samaniego for preparing the leaf samples. K. Bjorndal generously allowed us to use her ANKOM fiber analyzer, and A. Boulos and K. Williams assisted with the fiber analysis. We also thank N. Swenson and A. Zanne for advice on phylogenetically independent contrast analysis. The F. H. Levinson Fund supported leaf trait measurements. The National Science Foundation and MacArthur Foundation have supported the Barro Colorado Island 50-ha plot censuses. NR 76 TC 36 Z9 36 U1 1 U2 49 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD JUN PY 2011 VL 177 IS 6 BP 800 EP 811 DI 10.1086/659963 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 768QZ UT WOS:000290953000010 PM 21597256 ER PT J AU Gruberbauer, M Huber, D Kuschnig, R Weiss, WW Guenther, DB Matthews, JM Moffat, AFJ Rowe, JF Rucinski, SM Sasselov, D Fischer, M AF Gruberbauer, M. Huber, D. Kuschnig, R. Weiss, W. W. Guenther, D. B. Matthews, J. M. Moffat, A. F. J. Rowe, J. F. Rucinski, S. M. Sasselov, D. Fischer, M. TI MOST observations of the roAp stars HD 9289, HD 99563, and HD 134214 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: oscillations; stars: chemically peculiar; stars: magnetic field; stars: rotation ID OSCILLATING AP STARS; UPPER ATMOSPHERIC VARIABILITY; PHOTOMETRY; SPACE; HD-134214 AB We report on the analysis of high-precision space-based photometry of the roAp (rapidly oscillating Ap) stars HD 9289, HD 99563, and HD 134214. All three stars were observed by the MOST satellite for more than 25 days, allowing unprecedented views of their pulsation. We find previously unknown candidate frequencies in all three stars. We establish the rotation period of HD 9289 (8.5 d) for the first time and show that the star is pulsating in two modes that show different mode geometries. We present a detailed analysis of HD 99563' s mode multiplet and find a new candidate frequency that appears to be independent of the previously known mode. Finally, we report on 11 detected pulsation frequencies in HD 134214, nine of which have never before been detected in photometry, and three of which are completely new detections. Thanks to the unprecedentedly small frequency uncertainties, the p-mode spectrum of HD 134214 can be seen to have a well-defined large frequency spacing similar to the well-studied roAp star HD 24712 (HR 1217). C1 [Gruberbauer, M.; Huber, D.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron IfA, A-1180 Vienna, Austria. [Gruberbauer, M.; Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Huber, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, S. M.] Univ Toronto, Dept Phys & Astron, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fischer, M.] Vienna Univ Technol, Inst Telecommun, A-1040 Vienna, Austria. RP Gruberbauer, M (reprint author), Univ Vienna, Inst Astron IfA, Turkenschanzstr 17, A-1180 Vienna, Austria. EM mgruberbauer@ap.smu.ca; dhuber@physics.usyd.edu.au; rainer.kuschnig@univie.ac.at; werner.weiss@univie.ac.at; guenther@ap.smu.ca; matthews@astro.ubc.ca; moffat@astro.umontreal.ca; jasonfrowe@gmail.com; rucinski@astro.utoronto.ca; sasselov@cfa.harvard.edu; michael.fischer@nt.tuwien.ac.at FU Natural Sciences & Engineering Research Council (NSERC) Canada; Austrian Science Funds [P 22691-N16] FX The authors dedicate this work to the memory of our dear friend and colleague Dr. Piet Reegen, who will be greatly missed by us all. The authors would like to thank Hideyuki Saio (Tohoku University) for contributing his models and valuable discussion. M.G., D.B.G., A.F.J.M., J.M.M., and S.R. acknowledge funding from the Natural Sciences & Engineering Research Council (NSERC) Canada, and W. W. from the Austrian Science Funds (P 22691-N16). NR 33 TC 3 Z9 4 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2011 VL 530 AR A135 DI 10.1051/0004-6361/201116736 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OW UT WOS:000291027400135 ER PT J AU Klaassen, PD Wilson, CD Keto, ER Zhang, Q Galvan-Madrid, R Liu, HYB AF Klaassen, P. D. Wilson, C. D. Keto, E. R. Zhang, Q. Galvan-Madrid, R. Liu, H-Y B. TI High resolution CO observation of massive star forming regions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: massive; stars: protostars; ISM: jets and outflows; ISM: kinematics and dynamics; submillimeter: ISM; HII regions ID ULTRACOMPACT HII REGION; VELOCITY MOLECULAR OUTFLOWS; H-II REGIONS; METHANOL MASERS; ACCRETION FLOW; G10.6-0.4; GAS; CLUSTER; INFALL; CORES AB Context. To further understand the processes involved in the formation of massive stars, we have undertaken a study of the gas dynamics surrounding three massive star forming regions. By observing the large scale structures at high resolution, we are able to determine properties such as driving source, and spatially resolve the bulk dynamical properties of the gas such as infall and outflow. Aims. With high resolution observations, we are able to determine which of the cores in a cluster forming massive stars is responsible for the large scale structures. Methods. We present CO observations of three massive star forming regions with known HII regions and show how the CO traces both infall and outflow. By combining data taken in two SMA configurations with JCMT observations, we are able to see large scale structures at high resolution. Results. We find large (0.26-0.40 pc), massive (2-3 M-circle dot) and energetic (13-17 x 10(44) erg) outflows emanating from the edges of two HII regions suggesting they are being powered by the protostar(s) within. We find infall signatures in two of our sources with mass infall rates of order 10(-4) M-circle dot yr(-1). Conclusions. We suggest that star formation is ongoing in these sources despite the presence of HII regions. We further conclude that the source(s) within a single HII region are responsible for the observed large scale structures; that these large structures are not the net effect of multiple outflows from multiple HII regions and hot cores. C1 [Klaassen, P. D.] European So Observ, D-8046 Garching, Germany. [Wilson, C. D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Keto, E. R.; Zhang, Q.; Galvan-Madrid, R.; Liu, H-Y B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Galvan-Madrid, R.] UNAM, Ctr Radioastron & Astrofis, Morelia, Michoacan, Mexico. [Galvan-Madrid, R.; Liu, H-Y B.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Liu, H-Y B.] Natl Taiwan Univ, Dept Phys, Taipei, Taiwan. RP Klaassen, PD (reprint author), European So Observ, Karl Schwarzschild Str 2, D-8046 Garching, Germany. EM pklaasse@eso.org OI Zhang, Qizhou/0000-0003-2384-6589 NR 59 TC 13 Z9 13 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2011 VL 530 AR A53 DI 10.1051/0004-6361/201016371 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OW UT WOS:000291027400053 ER PT J AU Pillai, T Kauffmann, J Wyrowski, F Hatchell, J Gibb, AG Thompson, MA AF Pillai, T. Kauffmann, J. Wyrowski, F. Hatchell, J. Gibb, A. G. Thompson, M. A. TI Probing the initial conditions of high-mass star formation II. Fragmentation, stability, and chemistry towards high-mass star-forming regions G29.96-0.02 and G35.20-1.74 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; molecular data; turbulence; ISM: clouds; ISM: jets ond outflows; ISM: molecules ID INFRARED DARK CLOUDS; MOLECULAR CLOUDS; COMPETITIVE ACCRETION; PROTOSTELLAR CORES; GALACTIC PLANE; MAIN CLOUD; COLD CORES; CONTINUUM; PROTOSTARS; TURBULENT AB Most work on high-mass star formation has focused on observations of young massive stars in protoclusters. Very little is known about the preceding stage. Here, we present a new high-resolution study of pre-protocluster regions in tracers exclusively probing the coldest and dense gas (NH2D). The two target regions G29.96-0.02 and G35.20-1.74 (W48) are drawn from the SCAMPS project, which searches for pre-protoclusters near known ultracompact HII regions. We used our data to constrain the chemical, thermal, kinematic, and physical conditions (i.e., densities) in G29.96e and G35.20w. NH3, NH2D, HCO+, and continuum emission were mapped using the VLA, PdBI, and BIMA. In particular, NH2D is a unique tracer of cold, precluster gas at high densities, while NH3 traces both the cold and warm gas of modest-to-high densities. In G29.96e, Spitzer images reveal two massive filaments, one of them in extinction (infrared dark cloud). Dust and line observations reveal fragmentation into multiple massive cores strung along filamentary structures. Most of these are cold (<20 K), dense (> 10(5) cm(-3)) and highly deuterated ([NH2D/NH3] > 6%). In particular, we observe very low line widths in NH2D (FWHM less than or similar to 1 km s(-1)). These are very narrow lines that are unexpected towards a region forming massive stars. Only one core in the center of each filament appears to be forming massive stars (identified by the presence of masers and massive outflows); however, it appears that only a few such stars are currently forming (i.e., just a single Spitzer source per region). These multi-wavelength, high-resolution observations of high-mass pre-protocluster regions show that the target regions are characterized by (i) turbulent Jeans fragmentation of massive clumps into cores (from a Jeans analysis); (ii) cores and clumps that are "over-bound/subvirial", i.e. turbulence is too weak to support them against collapse, meaning that (iii) some models of monolithic cloud collapse are quantitatively inconsistent with data; (iv) accretion from the core onto a massive star, which can (for observed core sizes and velocities) be sustained by accretion of envelope material onto the core, suggesting that (similar to competitive accretion scenarios) the mass reservoir for star formation is not necessarily limited to the natal core; (v) high deuteration ratios ([NH2D/NH3] > 6%), which make the above discoveries possible; (vi) and the destruction of NH2D toward embedded stars. C1 [Pillai, T.] CALTECH, Pasadena, CA 91125 USA. [Pillai, T.; Kauffmann, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kauffmann, J.] Harvard Univ, Initiat Innovat Comp IIC, Cambridge, MA 02138 USA. [Kauffmann, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wyrowski, F.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Hatchell, J.] Univ Exeter, Exeter EX4 4QJ, Devon, England. [Gibb, A. G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Thompson, M. A.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. RP Pillai, T (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM tpillai@astro.caltech.edu FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Combined Array for Research in Millimeter-wave Astronomy (CARMA); National Science Foundation [AST 05-40399]; NASA 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).; We thank an anonymous referee for a very thorough review which helped to significantly improve the paper. T.P. acknowledges support from the Combined Array for Research in Millimeter-wave Astronomy (CARMA), which is supported by the National Science Foundation through grant AST 05-40399. J.K. also thanks Di Li, his host at JPL, for making this research possible. This project was supported by an appointment of J.K. to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. J.K.s research was executed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Air and Space Administration. 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. NR 80 TC 38 Z9 38 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2011 VL 530 AR A118 DI 10.1051/0004-6361/201015899 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OW UT WOS:000291027400118 ER PT J AU Qin, SL Schilke, P Rolffs, R Comito, C Lis, DC Zhang, Q AF Qin, S. -L. Schilke, P. Rolffs, R. Comito, C. Lis, D. C. Zhang, Q. TI Submillimeter continuum observations of Sagittarius B2 at subarcsecond spatial resolution SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; radio continuum: ISM; ISM: individual objects: Sgr B2; stars: formation ID MASSIVE STAR-FORMATION; SPECTRAL-LINE SURVEY; THERMAL EMISSION; GHZ; TELESCOPE; REGION; INFALL; CORES; GAS AB We report the first high spatial resolution submillimeter continuum observations of the Sagittarius B2 cloud complex using the Submillimeter Array (SMA). With the subarcsecond resolution provided by the SMA, the two massive star-forming clumps Sgr B2(N) and Sgr B2(M) are resolved into multiple compact sources. In total, twelve submillimeter cores are identified in the Sgr B2(M) region, while only two components are observed in the Sgr B2(N) clump. The gas mass and column density are estimated from the dust continuum emission. We find that most of the cores have gas masses in excess of 100 M(circle dot) and column densities above 10(25) cm(-2). The very fragmented appearance of Sgr B2(M), in contrast to the monolithic structure of Sgr B2 (N), suggests that the former is more evolved. The density profile of the Sgr B2(N)-SMA1 core is well fitted by a Plummer density distribution. This would lead one to believe that in the evolutionary sequence of the Sgr B2 cloud complex, a massive star forms first in an homogeneous core, and the rest of the cluster forms subsequently in the then fragmenting structure. C1 [Qin, S. -L.; Schilke, P.; Rolffs, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Rolffs, R.; Comito, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Qin, SL (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM qin@ph1.uni-koeln.de; schilke@ph1.uni-koeln.de OI Zhang, Qizhou/0000-0003-2384-6589 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 23 TC 20 Z9 20 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 JUN PY 2011 VL 530 AR L9 DI 10.1051/0004-6361/201116928 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OW UT WOS:000291027400162 ER PT J AU Schneider, PC Gunther, HM Schmitt, JHMM AF Schneider, P. C. Guenther, H. M. Schmitt, J. H. M. M. TI The X-ray puzzle of the L1551 IRS 5 jet SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: winds, outflows; X-rays: ISM; Herbig-Haro objects; ISM: jets and outflows; ISM: individual objects: HH 154; ISM: individual objects: L1551 IRS 5 ID ADAPTIVE OPTICS SPECTROSCOPY; T-TAURI STARS; PROTOSTELLAR JET; DG-TAURI; THERMAL CONDUCTION; RADIATIVE KNOTS; ATOMIC DATABASE; EMISSION-LINES; YOUNG STARS; DARK-CLOUD AB Protostars are actively accreting matter and they drive spectacular, dynamic outflows, which evolve on timescales of years. X-ray emission from these jets has been detected only in a few cases and little is known about its time evolution. We present a new Chandra observation of L1551 IRS 5's jet in the context of all available X-ray data of this object. Specifically, we perform a spatially resolved spectral analysis of the X-ray emission and find that (a) the total X-ray luminosity is constant over almost one decade, (b) the majority of the X-rays appear to be always located close to the driving source, (c) there is a clear trend in the photon energy as a function of the distance to the driving source indicating that the plasma is cooler at larger distances and (d) the X-ray emission is located in a small volume which is unresolved perpendicular to the jet axis by Chandra. A comparison of our X-ray data of the L1551 IRS 5 jet both with models as well as X-ray observations of other protostellar jets shows that a base/standing shock is a likely and plausible explanation for the apparent constancy of the observed X-ray emission. Internal shocks are also consistent with the observed morphology if the supply of jet material by the ejection of new blobs is sufficiently constant. We conclude that the study of the X-ray emission of protostellar jet sources allows us to diagnose the innermost regions close to the acceleration region of the outflows. C1 [Schneider, P. C.; Schmitt, J. H. M. M.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Guenther, H. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schneider, PC (reprint author), Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM cschneider@hs.uni-hamburg.de; hguenther@head.cfa.harvard.edu; jschmitt@hs.uni-hamburg.de OI Gunther, Hans Moritz/0000-0003-4243-2840 FU DLR [50OR0703]; Chandra [GO6-7017X] FX This work has made use of data obtained by Chandra, from the Chandra data archive and from the XMM-Newton data archive. P.C.S. acknowledges support from the DLR under grant 50OR0703. H.M.G. acknowledges support from Chandra under grant GO6-7017X This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France NR 64 TC 14 Z9 14 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 JUN PY 2011 VL 530 AR A123 DI 10.1051/0004-6361/201016305 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 769OW UT WOS:000291027400123 ER PT J AU Scholz, A Irwin, J Bouvier, J Sipocz, BM Hodgkin, S Eisloffel, J AF Scholz, Alexander Irwin, Jonathan Bouvier, Jerome Sipocz, Brigitta M. Hodgkin, Simon Eisloeffel, Jochen TI Rotation periods for very low mass stars in Praesepe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: activity; brown dwarfs; stars: evolution; stars: low-mass; stars: rotation ID ANGULAR-MOMENTUM EVOLUTION; TIME-SERIES ANALYSIS; FIELD M-DWARFS; MONITOR PROJECT; OPEN CLUSTER; CHROMOSPHERIC ACTIVITY; COMA BERENICES; TRANSIT SURVEY; DATA RELEASE; MODELS AB We investigate the rotation periods of fully convective very low mass (VLM, M < 0.3 M-circle dot) stars, with the aim to derive empirical constraints for the spin-down due to magnetically driven stellar winds. Our analysis is based on a new sample of rotation periods in the main-sequence cluster Praesepe (age 600 Myr). From photometric light curves obtained with the Isaac Newton Telescope, we measure rotation periods for 49 objects, among them 26 in the VLM domain. This enlarges the period sample in this mass and age regime by a factor of 6. Almost all VLM objects in our sample are fast rotators with periods < 2.5 d, in contrast to the stars with M > 0.6 M-circle dot in this cluster which have periods of 7-14 d. Thus, we confirm that the period-mass distribution in Praesepe exhibits a radical break at M similar to 0.3-0.6 M-circle dot. Our data indicate a positive period-mass trend in the VLM regime, similar to younger clusters. In addition, the scatter of the periods increases with mass. For the M > 0.3 M-circle dot objects in our sample, the period distribution is probably affected by binarity. By comparing the Praesepe periods with literature samples in the cluster NGC 2516 (age similar to 150 Myr) we constrain the spin-down in the VLM regime. An exponential rotational braking law P proportional to exp (t/tau) with a mass-dependent tau is required to reproduce the data. The spin-down time-scale tau increases steeply towards lower masses; we derive tau similar to 0.5 Gyr for 0.3 M-circle dot and > 1 Gyr for 0.1 M-circle dot. These constraints are consistent with the current paradigm of the spin-down due to wind braking. We discuss possible physical origins of this behaviour and prospects for future work. C1 [Scholz, Alexander] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Irwin, Jonathan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bouvier, Jerome] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Sipocz, Brigitta M.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Hodgkin, Simon] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eisloeffel, Jochen] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. RP Scholz, A (reprint author), Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliam Pl, Dublin 2, Ireland. EM aleks@cp.dias.ie OI Scholz, Aleks/0000-0001-8993-5053 FU European Commission; Science Foundation Ireland [10/RFP/AST2780] FX We thank the referee, Joel Hartman, for a constructive report that helped to improve the paper. AS would like to thank Philippe Delorme who made his results available prior to publication. BMS is supported by RoPACS, a Marie Curie Initial Training Network funded by the European Commission's Seventh Framework Programme. Part of this work was funded by the Science Foundation Ireland through grant no. 10/RFP/AST2780 to AS. NR 40 TC 18 Z9 18 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 JUN PY 2011 VL 413 IS 4 BP 2595 EP 2605 DI 10.1111/j.1365-2966.2011.18328.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 766XM UT WOS:000290819900024 ER PT J AU Szabo, R Szabados, L Ngeow, CC Smolec, R Derekas, A Moskalik, P Nuspl, J Lehmann, H Furesz, G Molenda-Zakowicz, J Bryson, ST Henden, AA Kurtz, DW Stello, D Nemec, JM Benko, JM Berdnikov, L Bruntt, H Evans, NR Gorynya, NA Pastukhova, EN Simcoe, RJ Grindlay, JE Los, EJ Doane, A Laycock, SG Mink, DJ Champine, G Sliski, A Handler, G Kiss, LL Kollath, Z Kovacs, J Christensen-Dalsgaard, J Kjeldsen, H Allen, C Thompson, SE Van Cleve, J AF Szabo, R. Szabados, L. Ngeow, C. -C. Smolec, R. Derekas, A. Moskalik, P. Nuspl, J. Lehmann, H. Furesz, G. Molenda-Zakowicz, J. Bryson, S. T. Henden, A. A. Kurtz, D. W. Stello, D. Nemec, J. M. Benko, J. M. Berdnikov, L. Bruntt, H. Evans, N. R. Gorynya, N. A. Pastukhova, E. N. Simcoe, R. J. Grindlay, J. E. Los, E. J. Doane, A. Laycock, S. G. Mink, D. J. Champine, G. Sliski, A. Handler, G. Kiss, L. L. Kollath, Z. Kovacs, J. Christensen-Dalsgaard, J. Kjeldsen, H. Allen, C. Thompson, S. E. Van Cleve, J. TI Cepheid investigations using the Kepler space telescope SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; techniques: spectroscopic; stars: individual: V1154 Cygni, KIC 7548061; stars: individual: V2279 Cygni, KIC 8022670; stars: oscillations; stars: variables: Cepheids ID RR LYRAE STARS; VARIABLE-STARS; CLASSICAL CEPHEIDS; RADIAL-VELOCITIES; LIGHT CURVES; ASTEROSEISMOLOGY PROGRAM; CORRELATION SPECTROMETER; INITIAL CHARACTERISTICS; FOURIER DECOMPOSITION; STRUCTURAL-PROPERTIES AB We report results of initial work done on selected candidate Cepheids to be observed with the Kepler space telescope. Prior to the launch, 40 candidates were selected from previous surveys and data bases. The analysis of the first 322 d of Kepler photometry, and recent ground-based follow-up multicolour photometry and spectroscopy allowed us to confirm that one of these stars, V1154 Cyg (KIC 7548061), is indeed a 4.9-d Cepheid. Using the phase lag method, we show that this star pulsates in the fundamental mode. New radial velocity data are consistent with previous measurements, suggesting that a long-period binary component is unlikely. No evidence is seen in the ultraprecise, nearly uninterrupted Kepler photometry for non-radial or stochastically excited modes at the micromagnitude level. The other candidates are not Cepheids, but an interesting mix of possible spotted stars, eclipsing systems and flare stars. C1 [Szabo, R.; Szabados, L.; Derekas, A.; Nuspl, J.; Benko, J. M.; Kiss, L. L.; Kollath, Z.] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary. [Ngeow, C. -C.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taoyuan County, Taiwan. [Smolec, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Derekas, A.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. [Moskalik, P.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Lehmann, H.] Karl Schwarzschild Observ, Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Furesz, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Bryson, S. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Henden, A. A.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst Astrophys, Preston PR1 2HE, Lancs, England. [Stello, D.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada. [Berdnikov, L.; Simcoe, R. J.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow, Russia. [Berdnikov, L.] Moscow Branch, Isaac Newton Inst Chile, Moscow 119992, Russia. [Bruntt, H.] Observ Paris, LESIA, UMR 8109, F-92195 Meudon, France. [Evans, N. R.; Mink, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gorynya, N. A.; Pastukhova, E. N.] Russian Acad Sci, Inst Astron, Moscow 109017, Russia. [Grindlay, J. E.; Los, E. J.; Doane, A.; Laycock, S. G.; Mink, D. J.; Champine, G.] Harvard Coll Observ, Cambridge, MA 02138 USA. [Kovacs, J.] Gothard Astrophys Observ, H-9707 Szombathely, Hungary. [Christensen-Dalsgaard, J.; Kjeldsen, H.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Allen, C.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Thompson, S. E.; Van Cleve, J.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Szabo, R (reprint author), Hungarian Acad Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary. EM rszabo@konkoly.hu RI Smolec, Radoslaw/F-1435-2013; Derekas, Aliz/G-2091-2016; OI Smolec, Radoslaw/0000-0001-7217-4884; Derekas, Aliz/0000-0002-6526-9444; Mink, Jessica/0000-0003-3594-1823; Benko, Jozsef/0000-0003-3851-6603; Szabo, Robert/0000-0002-3258-1909 FU NASA's Science Mission Directorate; Hungarian Academy of Sciences; Hungarian OTKA [K83790, MB08C 81013]; ESA [C98090]; National Science Council (of Taiwan) [NSC 98-2112-M-008-013-MY3]; Austrian Science Fund (FWF) [AP 2120521] FX Funding for the Kepler mission is provided by the NASA's Science Mission Directorate. This project has been supported by the 'Lendulet' programme of the Hungarian Academy of Sciences and the Hungarian OTKA grants K83790 and MB08C 81013. Financial support from the ESA (PECS programme No. C98090) is gratefully acknowledged. C-CN thanks the funding from the National Science Council (of Taiwan) under the contract NSC 98-2112-M-008-013-MY3. RS is supported by the Austrian Science Fund (FWF project AP 2120521). We acknowledge the assistance of the queue observers, Chi-Sheng Lin and Hsiang-Yao Hsiao, from the Lulin Observatory. Part of this project is based on data from the OMC Archive at LAEFF, pre-processed by ISDC. We acknowledge with thanks the variable star observations from the AAVSO International Data base contributed by observers worldwide and used in this research. The authors gratefully acknowledge the entire Kepler team, whose outstanding efforts have made these results possible. NR 57 TC 11 Z9 11 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2011 VL 413 IS 4 BP 2709 EP 2720 DI 10.1111/j.1365-2966.2011.18342.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 766XM UT WOS:000290819900035 ER PT J AU Davis, M Nusser, A Masters, KL Springob, C Huchra, JP Lemson, G AF Davis, Marc Nusser, Adi Masters, Karen L. Springob, Christopher Huchra, John P. Lemson, Gerard TI Local gravity versus local velocity: solutions for beta and non-linear bias SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; dark matter; large-scale structure of Universe ID TULLY-FISHER RELATION; SFI PECULIAR VELOCITIES; GALAXY REDSHIFT SURVEY; DIGITAL SKY SURVEY; BRIGHTEST CLUSTER GALAXIES; LARGE-SCALE FLOWS; PLUS PLUS SURVEY; 100 H(-1) MPC; 1.2 JY SURVEY; COSMOLOGICAL PARAMETERS AB We perform a reconstruction of the cosmological large-scale flows in the nearby Universe using two complementary observational sets. The first, the SFI++ sample of Tully-Fisher (TF) measurements of galaxies, provides a direct probe of the flows. The second, the whole sky distribution of galaxies in the 2MASS (Two Micron All Sky Survey) redshift survey (2MRS), yields a prediction of the flows given the cosmological density parameter, , and a biasing relation between mass and galaxies. We aim at an unbiased comparison between the peculiar velocity fields extracted from the two data sets and its implication on the cosmological parameters and the biasing relation. We expand the fields in a set of orthonormal basis functions, each representing a plausible realization of a cosmological velocity field smoothed in such a way as to give a nearly constant error on the derived SFI++ velocities. The statistical analysis is done on the coefficients of the modal expansion of the fields by means of the basis functions. Our analysis completely avoids the strong error covariance in the smoothed TF velocities by the use of orthonormal basis functions and employs elaborate mock data sets to extensively calibrate the errors in 2MRS predicted velocities. We relate the 2MRS galaxy distribution to the mass density field by a linear bias factor, b, and include a luminosity-dependent, proportional to L alpha, galaxy weighting. We assess the agreement between the fields as a function of alpha and beta = f()/b, where f is the growth factor of linear perturbations. The agreement is excellent with a reasonable chi 2 per degree of freedom. For alpha = 0, we derive 0.28 < beta < 0.37 and 0.24 < beta < 0.43, respectively, at the 68.3 per cent and 95.4 per cent confidence levels (CLs). For beta = 0.33, we get alpha < 0.25 and alpha < 0.5, respectively, at the 68.3 per cent and 95.4 per cent CLs. We set a constraint on the fluctuation normalization, finding Sigma(8) = 0.66 +/- 0.10, which is only 1.5 Sigma deviant from Wilkinson Microwave Anisotropy Probe (WMAP) results. It is remarkable that Sigma(8) determined from this local cosmological test is close to the value derived from the cosmic microwave background, an indication of the precision of the standard model. C1 [Davis, Marc] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Davis, Marc] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Nusser, Adi] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Nusser, Adi] Technion Israel Inst Technol, Asher Space Sci Inst, IL-32000 Haifa, Israel. [Masters, Karen L.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Springob, Christopher] Anglo Australian Observ, Epping, NSW 1710, Australia. [Huchra, John P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lemson, Gerard] Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Davis, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM mdavis@berkeley.edu FU Israel Science Foundation [203/09]; German-Israeli Foundation for Research and Development; Asher Space Research Institute; Winnipeg Research Fund; Peter and Patricia Gruber Foundation; Leverhulme Trust; University of Portsmouth; SEPnet FX We thank Enzo Branchini for a careful reading of the manuscript. MD acknowledges the support provided by the NSF grant AST-0807630. The majority of this research was carried out at the MPA, Garching, when MD was supported by a Humboldt fellowship. AN thanks the MPA for the hospitality. This work was supported by The Israel Science Foundation (grant No. 203/09), the German-Israeli Foundation for Research and Development, the Asher Space Research Institute and by the Winnipeg Research Fund. KLM acknowledges funding from the Peter and Patricia Gruber Foundation as the 2008 Peter and Patricia Gruber Foundation International Astronomical Union Fellow, from a 2010 Leverhulme Trust Early Career Fellowship and from the University of Portsmouth and SEPnet (www.sepnet.ac.uk). The Millennium Simulation data bases used in this paper and the web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory. NR 91 TC 47 Z9 48 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 JUN PY 2011 VL 413 IS 4 BP 2906 EP 2922 DI 10.1111/j.1365-2966.2011.18362.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 766XM UT WOS:000290819900052 ER PT J AU Forbes, DA Spitler, LR Strader, J Romanowsky, AJ Brodie, JP Foster, C AF Forbes, Duncan A. Spitler, Lee R. Strader, Jay Romanowsky, Aaron J. Brodie, Jean P. Foster, Caroline TI Evidence for two phases of galaxy formation from radial trends in the globular cluster system of NGC 1407 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE globular clusters: general; galaxies: formation; galaxies: individual: NGC 1407; galaxies: star clusters: general ID INFRARED CALCIUM TRIPLET; STAR-FORMATION; MILKY-WAY; ELLIPTIC GALAXIES; STELLAR POPULATIONS; VIRGO ELLIPTICALS; ELEMENT ABUNDANCE; FORMATION HISTORY; MASSIVE GALAXIES; SELF-ENRICHMENT AB Here we present the colours of individual globular clusters (GCs) around the massive elliptical galaxy NGC 1407 out to a projected galactocentric radius of 140 kpc or 17 galaxy effective radii (R-e). Such data are a proxy for the halo metallicity. We find steep, and similar, metallicity gradients of similar to -0.4 dex dex-1 for both the blue (metal poor) and red (metal rich) GC subpopulations within 5-8.5 R-e (40-70 kpc). At larger radii the mean GC colours (metallicity) are constant. A similar behaviour is seen in a wide-field study of M87's GC system, and in our own Galaxy. We interpret these radial metallicity trends to indicate an inner region formed by early in situ dissipative processes and an outer halo formed by the ongoing accretion of low-mass galaxies and their GCs. These results provide observational support for the model of galaxy formation whereby massive galaxies form inside-out in two phases. We have also searched the literature for other massive early-type galaxies with reported GC metallicity gradients in their inner regions. No obvious correlation with galaxy mass or environment is found but the sample is currently small. C1 [Forbes, Duncan A.; Spitler, Lee R.; Foster, Caroline] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Romanowsky, Aaron J.; Brodie, Jean P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Forbes, DA (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM dforbes@swin.edu.au RI Spitler, Lee/A-9867-2013; OI Spitler, Lee/0000-0001-5185-9876; Foster, Caroline/0000-0003-0247-1204 NR 66 TC 49 Z9 49 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2011 VL 413 IS 4 BP 2943 EP 2949 DI 10.1111/j.1365-2966.2011.18373.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 766XM UT WOS:000290819900055 ER PT J AU Acciari, VA Aliu, E Araya, M Arlen, T Aune, T Beilicke, M Benbow, W Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Ciupik, L Collins-Hughes, E Cui, W Dickherber, R Duke, C Falcone, A Finley, JP Fortson, L Furniss, A Galante, N Gall, D Godambe, S Griffin, S Guenette, R Gyuk, G Hanna, D Holder, J Hughes, G Hui, CM Humensky, TB Imran, A Kaaret, P Kertzman, M Krawczynski, H Krennrich, F Madhavan, AS Maier, G Majumdar, P McArthur, S Moriarty, P Ong, RA Otte, AN Pandel, D Park, N Perkins, JS Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Saxon, DB Sembroski, GH Senturk, GD Smith, AW Tesic, G Theiling, M Thibadeau, S Varlotta, A Vincent, S Vivier, M Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Weng, S Williams, DA Wood, M Zitzer, B AF Acciari, V. A. Aliu, E. Araya, M. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Collins-Hughes, E. Cui, W. Dickherber, R. Duke, C. Falcone, A. Finley, J. P. Fortson, L. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Kertzman, M. Krawczynski, H. Krennrich, F. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. Moriarty, P. Ong, R. A. Otte, A. N. Pandel, D. Park, N. Perkins, J. S. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Saxon, D. B. Sembroski, G. H. Sentuerk, G. D. Smith, A. W. Tesic, G. Theiling, M. Thibadeau, S. Varlotta, A. Vincent, S. Vivier, M. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Weng, S. Williams, D. A. Wood, M. Zitzer, B. TI GAMMA-RAY OBSERVATIONS OF THE Be/PULSAR BINARY 1A 0535+262 DURING A GIANT X-RAY OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; binaries: general; gamma rays: general; stars: individual (1A 0535+262) ID LARGE-AREA TELESCOPE; PROPORTIONAL COUNTER ARRAY; HESS J0632+057; EMISSION; A0535+262; CATALOG; PULSAR; PERIOD; CALIBRATION; A-0535+26 AB Giant X-ray outbursts, with luminosities of about 10(37) erg s(-1), are observed roughly every five years from the nearby Be/pulsar binary 1A 0535+262. In this article, we present observations of the source with VERITAS at very high energies (VHEs; E > 100 GeV) triggered by the X-ray outburst in 2009 December. The observations started shortly after the onset of the outburst and provided comprehensive coverage of the episode, as well as the 111 day binary orbit. No VHE emission is evident at any time. We also examined data from the contemporaneous observations of 1A 0535+262 with the Fermi/Large Area Telescope at high-energy photons (E > 0.1 GeV) and failed to detect the source at GeV energies. The X-ray continua measured with the Swift/X-Ray Telescope and the RXTE/PCA can be well described by the combination of blackbody and Comptonized emission from thermal electrons. Therefore, the gamma-ray and X-ray observations suggest the absence of a significant population of non-thermal particles in the system. This distinguishes 1A 0535+262 from those Be X-ray binaries (such as PSR B1259-63 and LS I +61 degrees 303) that have been detected at GeV-TeV energies. We discuss the implications of the results on theoretical models. C1 [Araya, M.; Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Weng, S.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 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.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Arlen, T.; Majumdar, P.; Ong, R. A.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [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. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; 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.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 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. [Godambe, S.; Hui, C. M.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Griffin, S.; Guenette, R.; Hanna, D.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Hughes, G.; Maier, G.; 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. [Imran, A.; Krennrich, F.; Madhavan, A. S.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] 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.] 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 Cui, W (reprint author), Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. EM avarlott@purdue.edu; cui@purdue.edu; gernot.maier@desy.de; avarlott@purdue.edu OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586 FU US Department of Energy; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK; Helmholtz Association; NASA; Purdue University FX This research is supported by grants from the US Department of Energy, the US National Science Foundation, the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, 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. G.M. acknowledges support through the Young Investigators Program of the Helmholtz Association. A.V. and W.C. acknowledge financial support from NASA and Purdue University. NR 50 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 JUN 1 PY 2011 VL 733 IS 2 AR 96 DI 10.1088/0004-637X/733/2/96 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 765AP UT WOS:000290676100023 ER PT J AU Buchhave, LA Bakos, GA Hartman, JD Torres, G Latham, DW Andersen, J Kovacs, G Noyes, RW Shporer, A Esquerdo, GA Fischer, DA Johnson, JA Marcy, GW Howard, AW Beky, B Sasselov, DD Furesz, G Quinn, SN Stefanik, RP Szklenar, T Berlind, P Calkins, ML Lazar, J Papp, I Sari, P AF Buchhave, L. A. Bakos, G. A. Hartman, J. D. Torres, G. Latham, D. W. Andersen, J. Kovacs, G. Noyes, R. W. Shporer, A. Esquerdo, G. A. Fischer, D. A. Johnson, J. A. Marcy, G. W. Howard, A. W. Beky, B. Sasselov, D. D. Furesz, G. Quinn, S. N. Stefanik, R. P. Szklenar, T. Berlind, P. Calkins, M. L. Lazar, J. Papp, I. Sari, P. TI HAT-P-28b AND HAT-P-29b: TWO SUB-JUPITER MASS TRANSITING PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-28, GSC 2284-00503, HAT-P-29, GSC 3293-01539); techniques: photometric; techniques: spectroscopic ID EXTRASOLAR PLANET; ECCENTRIC ORBIT; BRIGHT STAR; STELLAR; EMISSION; SEARCH; 2MASS; FIELD; TOOL; SKY AB We present the discovery of two transiting exoplanets. HAT-P-28b orbits a V = 13.03 G3 dwarf star with a period P = 3.2572 days and has a mass of 0.63 +/- 0.04 M-J and a radius of 1.21(-0.08)(+0.11) R-J yielding a mean density of 0.44 +/- 0.09 g cm(-3). HAT-P-29b orbits a V = 11.90 F8 dwarf star with a period P = 5.7232 days and has a mass of 0.78(-0.04)(+0.08) M-J and a radius of 1.11(-0.08)(+0.14) R-J yielding a mean density of 0.71 +/- 0.18 g cm(-3). We discuss the properties of these planets in the context of other known transiting planets. C1 [Buchhave, L. A.; Bakos, G. A.; Hartman, J. D.; Torres, G.; Latham, D. W.; Noyes, R. W.; Esquerdo, G. A.; Beky, B.; Sasselov, D. D.; Furesz, G.; Quinn, S. N.; Stefanik, R. P.; Szklenar, T.; Berlind, P.; Calkins, M. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, L. A.; Andersen, J.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark. [Andersen, J.] Nord Opt Telescope Sci Assoc, La Palma, Canarias, Spain. [Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary. [Shporer, A.] Global Telescope Network, Las Cumbres Observ, Goleta, CA USA. [Shporer, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 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. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Buchhave, LA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. 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 NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G, NCC2-1390]; NSF [AST-0702843, AST-0702821]; Hungarian Scientific Research Foundation (OTKA) [K-81373] FX HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G and SAO IR&D grants. Work of G.A.B. was 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 (program A201Hr) and NASA (N018Hr, N167Hr). This paper uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope and 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 thank to Johan Fynbo for help on the distance estimate. NR 39 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 JUN 1 PY 2011 VL 733 IS 2 AR 116 DI 10.1088/0004-637X/733/2/116 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 765AP UT WOS:000290676100043 ER PT J AU Dupuy, TJ Liu, MC AF Dupuy, Trent J. Liu, Michael C. TI ON THE DISTRIBUTION OF ORBITAL ECCENTRICITIES FOR VERY LOW-MASS BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: general; binaries: visual; brown dwarfs; infrared: stars; stars: low-mass; techniques: high angular resolution ID STAR ADAPTIVE OPTICS; SOLAR-TYPE STARS; EXTRASOLAR GIANT PLANETS; M TELESCOPE PROGRAM; LATE-M DWARFS; H-ALPHA 8; BROWN DWARF; RADIAL-VELOCITY; DYNAMICAL MASS; SPECTROSCOPIC BINARY AB We have compiled a sample of 16 orbits for very low-mass stellar (<0.1M(circle dot)) and brown dwarf binaries, including updated orbits for HD 130948BC and LP 415-20AB. This sample enables the first comprehensive study of the eccentricity distribution for such objects. We find that very low-mass binaries span a broad range of eccentricities from near-circular to highly eccentric (e approximate to 0.8), with a median eccentricity of 0.34. We have examined potential observational biases in this sample, and for visual binaries we show through Monte Carlo simulations that if we choose appropriate selection criteria then all eccentricities are equally represented (less than or similar to 5% difference between input and output eccentricity distributions). The orbits of this sample of very low-mass binaries show some significant differences from their solar-type counterparts. They lack a correlation between orbital period and eccentricity, and display a much higher fraction of near-circular orbits (e < 0.1) than solar-type stars, which together may suggest a different formation mechanism or dynamical history for these two populations. Very low-mass binaries also do not follow the e(2) distribution of Ambartsumian, which would be expected if their orbits were distributed in phase space according to a function of energy alone (e.g., the Boltzmann distribution). We find that current numerical simulations of very low-mass star formation do not completely reproduce the observed properties of our binary sample. The cluster formation model of Bate agrees very well with the overall e distribution, but the lack of any high-e (>0.6) binaries at orbital periods comparable to our sample suggests that tidal damping due to gas disks may play too large of a role in the simulations. In contrast, the circumstellar disk fragmentation model of Stamatellos & Whitworth predicts only high-e binaries and thus is highly inconsistent with our sample. These discrepancies could be explained if multiple formation processes are responsible for producing the field population. C1 [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Dupuy, TJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU W. M. Keck Foundation; NSF [AST-0507833, AST-0909222]; NASA [HST-HF-51271.01-A, NAS 5-26555] 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.; Our research has employed NASA's Astrophysical Data System; and the SIMBAD database operated at CDS, Strasbourg, France. We are grateful to Matthew Bate for providing us with the orbital elements of the lowest-mass binaries in his simulation. We have benefitted from discussions with Adam Kraus about binary formation, John Johnson about RV selection effects, and Tsevi Mazeh about orbital dynamics. T.J.D. and M.C.L. acknowledge support for this work from NSF grants AST-0507833 and AST-0909222. T.J.D. acknowledges support from Hubble Fellowship grant HST-HF-51271.01-A awarded by the Space Telescope Science Institute, which is operated by AURA 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 73 TC 57 Z9 57 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 JUN 1 PY 2011 VL 733 IS 2 AR 122 DI 10.1088/0004-637X/733/2/122 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 765AP UT WOS:000290676100049 ER PT J AU Hao, H Elvis, M Civano, F Lawrence, A AF Hao, Heng Elvis, Martin Civano, Francesca Lawrence, Andy TI HOT-DUST-POOR QUASARS IN MID-INFRARED AND OPTICALLY SELECTED SAMPLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; quasars: general; surveys ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; SPECTRAL ENERGY-DISTRIBUTIONS; DIGITAL SKY SURVEY; WIDE-FIELD CAMERA; GRAVITATIONAL-WAVE; PHOTOMETRIC SYSTEM; LINE REGION; GALAXIES; COLORS AB We show that the hot-dust-poor (HDP) quasars, originally found in the X-ray-selected XMM-COSMOS type 1 active galactic nucleus (AGN) sample, are just as common in two samples selected at optical/infrared wavelengths: the Richards et al. Spitzer/SDSS sample (8.7% +/- 2.2%) and the Palomar-Green-quasar-dominated sample of Elvis et al. (9.5% +/- 5.0%). The properties of the HDP quasars in these two samples are consistent with the XMM-COSMOS sample, except that, at the 99% (similar to 2.5 sigma) significance, a larger proportion of the HDP quasars in the Spitzer/SDSS sample have weak host galaxy contributions, probably due to the selection criteria used. Either the host dust is destroyed (dynamically or by radiation) or is offset from the central black hole due to recoiling. Alternatively, the universality of HDP quasars in samples with different selection methods and the continuous distribution of dust covering factor in type 1 AGNs suggest that the range of spectral energy distributions could be related to the range of tilts in warped fueling disks, as in the model of Lawrence & Elvis, with HDP quasars having relatively small warps. C1 [Hao, Heng; Elvis, Martin; Civano, Francesca] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lawrence, Andy] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Hao, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hhao@cfa.harvard.edu; elvis@cfa.harvard.edu FU NASA [GO7-8136A] FX We thank Michael Strauss and Brandon Kelly for suggestions that greatly improved the paper. This work was supported by NASA Chandra grant number GO7-8136A ( H.H., M.E., and F.C.). This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey. NR 49 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 JUN 1 PY 2011 VL 733 IS 2 AR 108 DI 10.1088/0004-637X/733/2/108 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 765AP UT WOS:000290676100035 ER PT J AU Lee, KS Dey, A Reddy, N Brown, MJI Gonzalez, AH Jannuzi, BT Cooper, MC Fan, XH Bian, FY Glikman, E Stern, D Brodwin, M Cooray, A AF Lee, Kyoung-Soo Dey, Arjun Reddy, Naveen Brown, Michael J. I. Gonzalez, Anthony H. Jannuzi, Buell T. Cooper, Michael C. Fan, Xiaohui Bian, Fuyan Glikman, Eilat Stern, Daniel Brodwin, Mark Cooray, Asantha TI THE AVERAGE PHYSICAL PROPERTIES AND STAR FORMATION HISTORIES OF THE UV-BRIGHTEST STAR-FORMING GALAXIES AT z similar to 3.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dust, extinction; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: stellar content ID LYMAN-BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; STELLAR MASS FUNCTION; ULTRAVIOLET LUMINOSITY DENSITY; K-SELECTED GALAXIES; WIDE-FIELD SURVEY; DUST OBSCURATION; CONTINUUM SLOPE; LARGE-SCALE; DEEP FIELD AB We investigate the average physical properties and star formation histories (SFHs) of the most UV-luminous star-forming galaxies at z similar to 3.7. Our results are based on the average spectral energy distributions (SEDs), constructed from stacked optical-to-infrared photometry, of a sample of the 1913 most UV-luminous star-forming galaxies found in 5.3 deg(2) of the NOAO Deep Wide-Field Survey. We find that the shape of the average SED in the rest optical and infrared is fairly constant with UV luminosity, i.e., more UV-luminous galaxies are, on average, also more luminous at longer wavelengths. In the rest UV, however, the spectral slope beta (equivalent to dlogF(lambda)/dlog lambda; measured at 0.13 mu m < lambda(rest) < 0.28 mu m) rises steeply with the median UV luminosity from -1.8 at L approximate to L* to -1.2 (L approximate to 4-5L*). We use population synthesis analyses to derive their average physical properties and find that (1) L-UV and thus star formation rates (SFRs) scale closely with stellar mass such that more UV-luminous galaxies are also more massive, (2) the median ages indicate that the stellar populations are relatively young (200-400 Myr) and show little correlation with UV luminosity, and (3) more UV-luminous galaxies are dustier than their less-luminous counterparts, such that L approximate to 4-5L* galaxies are extincted up to A(1600) = 2 mag while L approximate to L* galaxies have A(1600) = 0.7-1.5 mag. We argue that the average SFHs of UV-luminous galaxies are better described by models in which SFR increases with time in order to simultaneously reproduce the tight correlation between the UV-derived SFR and stellar mass and their universally young ages. We demonstrate the potential of measurements of the SFR-M-* relation at multiple redshifts to discriminate between simple models of SFHs. Finally, we discuss the fate of these UV-brightest galaxies in the next 1-2 Gyr and their possible connection to the most massive galaxies at z similar to 2. C1 [Lee, Kyoung-Soo; Glikman, Eilat] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Dey, Arjun; Reddy, Naveen; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Cooper, Michael C.; Fan, Xiaohui; Bian, Fuyan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cooray, Asantha] Univ Calif Irvine, Sch Phys Sci, Irvine, CA 92697 USA. RP Lee, KS (reprint author), Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 FU Yale Center for Astronomy and Astrophysics; National Science Foundation [AST-00708490, AST-0071048]; Yale University; NOAO; W. M. Keck Foundation FX We thank the referee for her/his careful and thorough report, which helped improve our paper. K.S.L. gratefully acknowledges the generous support of Gilbert and Jaylee Mead for their namesake fellowship in the Yale Center for Astronomy and Astrophysics. K.S.L. also thanks Adam Muzzin, C. Meg Urry, and Casey Papovich for useful discussions and suggestions. A.H.G. acknowledges support for this work from the National Science Foundation under grant AST-00708490. The analysis in this paper is made partly with the Keck observations awarded through Yale University. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory at the California Institute of Technology. We are grateful for the expert assistance of the staff of Kitt Peak National Observatory where the optical and near-infrared observations of the NDWFS Bootes field were obtained. The authors thank NOAO for supporting the NDWFS. The research activities of A.D. and B.T.J. are supported by NOAO, which is operated by the Association of Universities for Research in Astronomy under a cooperative agreement with the National Science Foundation. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are the University of Arizona on behalf of the Arizona university system; Instituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University; and The Research Corporation, on behalf of the University of Notre Dame, University of Minnesota, and University of Virginia. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership between 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 the staff of the W. M. Keck Observatory, particularly Gregory Wirth. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. The authors also recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. NR 66 TC 45 Z9 45 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2011 VL 733 IS 2 AR 99 DI 10.1088/0004-637X/733/2/99 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 765AP UT WOS:000290676100026 ER PT J AU Meibom, S Mathieu, RD Stassun, KG Liebesny, P Saar, SH AF Meibom, Soren Mathieu, Robert D. Stassun, Keivan G. Liebesny, Paul Saar, Steven H. TI THE COLOR-PERIOD DIAGRAM AND STELLAR ROTATIONAL EVOLUTION-NEW ROTATION PERIOD MEASUREMENTS IN THE OPEN CLUSTER M34 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (M34); stars: activity; stars: late-type; stars: rotation; starspots ID LOW-MASS STARS; SOLAR-TYPE STARS; ANGULAR-MOMENTUM EVOLUTION; MAIN-SEQUENCE STARS; ORION NEBULA CLUSTER; ALPHA-PERSEI CLUSTER; WIYN OPEN CLUSTER; NGC 1039 M34; MONITOR PROJECT; ACTIVE LONGITUDES AB We present the results of a 5 month photometric time-series survey for stellar rotation periods combined with a 4 year radial-velocity survey for membership and binarity in the 220 Myr open cluster M34. We report surface rotation periods for 120 stars, 83 of which are kinematic and photometric late-type cluster members. A comparison to previous work serves to illustrate the importance of high-cadence long baseline photometric observations and membership information. The new M34 periods are less biased against slow rotation and cleaned for non-members. The rotation periods of the cluster members span over more than an order of magnitude from 0.5 days up to 11.5 days, and trace two distinct rotational sequences-fast (C) and moderate-to-slow (I)-in the color-period diagram. The sequences represent two different states (fast and slow) in the rotational evolution of the late-type cluster members. We use the color-period diagrams for M34 and for younger and older clusters to estimate the timescale for the transition from the C to the I sequence and find less than or similar to 150 Myr, similar to 150-300 Myr, and similar to 300-600 Myr for G, early-mid K, and late K dwarfs, respectively. The small number of stars in the gap between C and I suggests a quick transition. We estimate a lower limit on the maximum spin-down rate (dP/dt) during this transition to be similar to 0.06 days Myr(-1) and similar to 0.08 days Myr(-1) for early and late K dwarfs, respectively. We compare the I sequence rotation periods in M34 and the Hyades for G and K dwarfs and find that K dwarfs spin down slower than the Skumanich root t rate. We determine a gyrochronology age of 240 Myr for M34. The gyro-age has a small formal uncertainty of 2% which reflects the tight I sequence in the M34 color-period diagram. We measure the effect of cluster age uncertainties on the gyrochronology age for M34 and find the resulting error on the gyro-age to be consistent with the similar to 15% error estimate for the technique in general. We use the M34 I sequence to redetermine the coefficients in the expression for rotational dependence on color used in gyrochronology. Finally, we propose that stability in the phase, shape, and amplitude of the photometric variability for the 120 rotators over the similar to 5 month duration of our survey is due to spot generation at active stellar longitudes. C1 [Meibom, Soren; Saar, Steven H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mathieu, Robert D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Liebesny, Paul] Emory Univ, Dept Phys Math & Sci, Atlanta, GA 30322 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smeibom@cfa.harvard.edu FU National Science Foundation; NASA [NNX09AH18A, NCC2-1390]; NSF [AST-0349075, AST-0909365, AST-0406615, AST-0908082] FX Visiting Astronomer, Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation.; We thank NOAO and the University of Wisconsin-Madison, Department of Astronomy, for the time granted on the WIYN 0.9 m and 3.5 m telescopes. We express our deep appreciation to the site managers and support staff at both telescopes for their exceptional and friendly support. We are thankful to all observers in the WIYN 0.9 m consortium who provided us with high-quality data through the queue-scheduled observing program. We thank Imants Platais and Constantine Deliyannis for providing astrometric and photometric data to support in support of this study. This work has been supported by partial support to S.M. from NASA grant NNX09AH18A (The Kepler Cluster Study), from partial support to S.M. from the Kepler mission via NASA Cooperative Agreement NCC2-1390, NSF grants AST-0349075 and AST-0909365 to K.G.S., and NSF grants AST-0406615 and AST-0908082 to R.D.M. Finally, we thank the anonymous referee for valuable comments and suggestions that improved the presentation and analysis of our results. NR 83 TC 50 Z9 50 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 JUN 1 PY 2011 VL 733 IS 2 AR 115 DI 10.1088/0004-637X/733/2/115 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 765AP UT WOS:000290676100042 ER PT J AU Sanchis-Ojeda, R Winn, JN Holman, MJ Carter, JA Osip, DJ Fuentes, CI AF Sanchis-Ojeda, Roberto Winn, Joshua N. Holman, Matthew J. Carter, Joshua A. Osip, David J. Fuentes, Cesar I. TI STARSPOTS AND SPIN-ORBIT ALIGNMENT IN THE WASP-4 EXOPLANETARY SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (WASP-4=USNO-B1.00479-0948995); stars: rotation ID SUPER-NEPTUNE HAT-P-11B; PLANETARY SYSTEM; TRANSITING PLANET; HOT JUPITERS; STAR; PHOTOMETRY; FIELD; CONSTRAINTS; CURVES; TRES-1 AB We present photometry of four transits of the exoplanet WASP-4b, each with a precision of approximately 500 ppm and a time sampling of 40-60 s. We have used the data to refine the estimates of the system parameters and ephemerides. During two of the transits we observed a short-lived, low-amplitude anomaly that we interpret as the occultation of a starspot by the planet. We also found evidence for a pair of similar anomalies in previously published photometry. The recurrence of these anomalies suggests that the stellar rotation axis is nearly aligned with the orbital axis, or else the starspot would not have remained on the transit chord. By analyzing the timings of the anomalies we find the sky-projected stellar obliquity to be. lambda = - 1(-12)(+14) - 12 degrees. This result is consistent with (and more constraining than) a recent observation of the Rossiter-McLaughlin effect. It suggests that the planet migration mechanism preserved the initially low obliquity, or else that tidal evolution has realigned the system. Future applications of this method using data from the CoRoT and Kepler missions will allow spin-orbit alignment to be probed for many other exoplanets. C1 [Sanchis-Ojeda, Roberto; Winn, Joshua N.; Carter, Joshua A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Sanchis-Ojeda, Roberto; Winn, Joshua N.; Carter, Joshua A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Holman, Matthew J.; Carter, Joshua A.; Fuentes, Cesar I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Osip, David J.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Fuentes, Cesar I.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. RP Sanchis-Ojeda, R (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Carter, Joshua/A-8280-2013; Sanchis-Ojeda, Roberto/B-6574-2013; Fuentes, Cesar /G-7506-2016; OI Sanchis-Ojeda, Roberto/0000-0002-6193-972X; Carter, Joshua/0000-0001-8152-2561 FU "la Caixa" Fellowship; NASA [HF-51267.01-A, NAS 5-26555]; Space Telescope Science Institute FX We thank the anonymous referee for a comprehensive and helpful report on the manuscript. We gratefully acknowledge support from the NASA Origins program through awards NNX09AD36G and NNX09AB33G, and the MIT Class of 1942. R. S. received financial support through the "la Caixa" Fellowship Grant for Post-Graduate Studies, Caixa d'Estalvis i Pensions de Barcelona "la Caixa," Barcelona, Spain. J.A.C. acknowledges support for this work by NASA through Hubble Fellowship grant 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 41 TC 85 Z9 85 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2011 VL 733 IS 2 AR 127 DI 10.1088/0004-637X/733/2/127 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 765AP UT WOS:000290676100054 ER PT J AU Servillat, M Webb, NA Lewis, F Knigge, C van den Berg, M Dieball, A Grindlay, J AF Servillat, M. Webb, N. A. Lewis, F. Knigge, C. van den Berg, M. Dieball, A. Grindlay, J. TI A DWARF NOVA IN THE GLOBULAR CLUSTER M13 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: individual (M13, NGC 6205); novae, cataclysmic variables; stars: dwarf novae; X-rays: general ID HUBBLE-SPACE-TELESCOPE; X-RAY OBSERVATIONS; ALL-SKY SURVEY; CATACLYSMIC VARIABLES; XMM-NEWTON; ORBITAL PERIOD; DYNAMICAL FORMATION; IMAGE SUBTRACTION; CLOSE BINARIES; SS-CYGNI AB Dwarf novae (DNe) in globular clusters (GCs) seem to be rare with only 13 detections in the 157 known Galactic GCs. We report the identification of a new DN in M13, the 14th DN identified in a GC to date. Using the 2 m Faulkes Telescope North, we conducted a search for stars in M13 that show variability over a year (2005-2006) on timescales of days and months. This led to the detection of one DN showing several outbursts. A Chandra X-ray source is coincident with this DN and shows both a spectrum and variability consistent with that expected from a DN, thus supporting the identification. We searched for a counterpart in Hubble Space Telescope Advanced Camera for Surveys/Wide Field Camera archived images and found at least 11 candidates, of which we could characterize only the 7 brightest, including one with a 3 sigma H alpha excess and a faint blue star. The detection of one DN when more could have been expected likely indicates that our knowledge of the global Galactic population of cataclysmic variables is too limited. The proportion of DNe may be lower than found in catalogs, or they may have a much smaller mean duty cycle (similar to 1%) as proposed by some population synthesis models and recent observations in the field. C1 [Servillat, M.; van den Berg, M.; Grindlay, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Webb, N. A.] Univ Toulouse 3, Observ Midi Pyrenees, IRAP, F-31062 Toulouse, France. [Webb, N. A.] IRAP, F-31028 Toulouse 4, France. [Webb, N. A.] CNRS, F-31028 Toulouse 4, France. [Webb, N. A.] Univ Toulouse, Toulouse, France. [Lewis, F.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Lewis, F.] Univ Glamorgan, Faulkes Telescope Project, Pontypridd CF37 4BD, M Glam, Wales. [Knigge, C.; Dieball, A.] Univ Southampton, Dept Phys, Southampton SO17 1BJ, Hants, England. [van den Berg, M.] Univ Utrecht, Dept Phys & Astron, NL-3508 TC Utrecht, Netherlands. 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 [AR9-0013X, GO0-11063X]; NSF [AST-0909073] FX We thank the anonymous referee whose careful review helped to clarify this paper. M.S. acknowledges supports from NASA/Chandra grants AR9-0013X and GO0-11063X, and NSF grant AST-0909073. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 56 TC 7 Z9 7 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 JUN 1 PY 2011 VL 733 IS 2 AR 106 DI 10.1088/0004-637X/733/2/106 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 765AP UT WOS:000290676100033 ER PT J AU Kapheim, KM Bernal, SP Smith, AR Nonacs, P Wcislo, WT AF Kapheim, Karen M. Bernal, Sandra P. Smith, Adam R. Nonacs, Peter Wcislo, William T. TI Support for maternal manipulation of developmental nutrition in a facultatively eusocial bee, Megalopta genalis (Halictidae) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Megalopta genalis; Maternal effects; Provisioning behavior; Sex investment ratio; Facultative eusociality ID SEXUAL SIZE DIMORPHISM; LASIOGLOSSUM-ZEPHYRUM HYMENOPTERA; BODY-SIZE; SWEAT BEE; SOLITARY BEE; PARENTAL INVESTMENT; DIGGER WASP; LIGATUS HYMENOPTERA; JUVENILE-HORMONE; LARVAL NUTRITION AB Developmental maternal effects are a potentially important source of phenotypic variation, but they can be difficult to distinguish from other environmental factors. This is an important distinction within the context of social evolution, because if variation in offspring helping behavior is due to maternal manipulation, social selection may act on maternal phenotypes, as well as those of offspring. Factors correlated with social castes have been linked to variation in developmental nutrition, which might provide opportunity for females to manipulate the social behavior of their offspring. Megalopta genalis is a mass-provisioning facultatively eusocial sweat bee for which production of males and females in social and solitary nests is concurrent and asynchronous. Female offspring may become either gynes (reproductive dispersers) or workers (non-reproductive helpers). We predicted that if maternal manipulation plays a role in M. genalis caste determination, investment in daughters should vary more than for sons. The mass and protein content of pollen stores provided to female offspring varied significantly more than those of males, but volume and sugar content did not. Sugar content varied more among female eggs in social nests than in solitary nests. Provisions were larger, with higher nutrient content, for female eggs and in social nests. Adult females and males show different patterns of allometry, and their investment ratio ranged from 1.23 to 1.69. Adult body weight varied more for females than males, possibly reflecting increased variation in maternal investment in female offspring. These differences are consistent with a role for maternal manipulation in the social plasticity observed in M. genalis. C1 [Kapheim, Karen M.; Nonacs, Peter] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Bernal, Sandra P.; Smith, Adam R.; Wcislo, William T.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. RP Kapheim, KM (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr S, Los Angeles, CA 90095 USA. EM kapheimk@ucla.edu FU STRI; Smithsonian Institution; UCLA EEB; American Women in Science; US Department of Education; Center for Society Genetics; NSF [IOS-0642085]; Smithsonian Institution Post-doctoral fellowship FX KMK was supported by a Short Term Fellowship from STRI, a Pre-doctoral fellowship from the Smithsonian Institution, a Holmes O. Miller grant and a George Bartholomew fellowship from UCLA EEB, a Joan Wright Goodman award from American Women in Science, a GAANN fellowship from US Department of Education, a graduate fellowship from the Center for Society & Genetics, and a NSF Doctoral Dissertation Improvement Grant. KMK and PN were also supported by NSF grant IOS-0642085. SPB participated in the STRI Internship Program with general research funds provided to WTW. ARS was supported by a Smithsonian Institution Post-doctoral fellowship. We would like to thank Damien Jose Ramirez Garcia and Timothy Alvey for assistance in the field. Oris Acevedo, Belkys Jimenez, and Orelis Arosemena and the rest of the STRI staff provided valuable logistic support. Rose Medeiros and Xiao Chen of UCLA Academic Technology Services provided statistical advice. Research on BCI was conducted with permission from the Autoridad Nacional del Ambiente under permit # SEX/A-34-09, in accordance with the laws of the Republic of Panama. We are thankful for the suggestions of three anonymous reviewers that led to improvements in the manuscript. NR 84 TC 28 Z9 28 U1 7 U2 37 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD JUN PY 2011 VL 65 IS 6 BP 1179 EP 1190 DI 10.1007/s00265-010-1131-9 PG 12 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 765RK UT WOS:000290726100003 ER PT J AU Terrell, KA Wildt, DE Anthony, NM Bavister, BD Leibo, SP Penfold, LM Marker, LL Crosier, AE AF Terrell, Kimberly A. Wildt, David E. Anthony, Nicola M. Bavister, Barry D. Leibo, S. P. Penfold, Linda M. Marker, Laurie L. Crosier, Adrienne E. TI Glycolytic Enzyme Activity Is Essential for Domestic Cat (Felis catus) and Cheetah (Acinonyx jubatus) Sperm Motility and Viability in a Sugar-Free Medium SO BIOLOGY OF REPRODUCTION LA English DT Article DE alpha-chlorohydrin; assisted reproductive technology; endogenous substrates; gamete biology; glycerol; glycogen; glycolysis; lactate; male sexual function; metabolic inhibition; oxidative metabolism; sodium oxamate; sperm metabolism; sperm motility and transport; spermatozoa ID IN-VITRO FERTILIZATION; ALPHA-CHLOROHYDRIN; ACROSOME REACTION; BOAR SPERMATOZOA; DOG SPERMATOZOA; GLYCERALDEHYDE-3-PHOSPHATE DEHYDROGENASE; HYPERACTIVATED MOTILITY; EPIDIDYMAL SPERMATOZOA; MAMMALIAN SPERMATOZOA; TERATOSPERMIC DONORS AB We have previously reported a lack of glucose uptake in domestic cat and cheetah spermatozoa, despite observing that these cells produce lactate at rates that correlate positively with sperm function. To elucidate the role of glycolysis in felid sperm energy production, we conducted a comparative study in the domestic cat and cheetah, with the hypothesis that sperm motility and viability are maintained in both species in the absence of glycolytic metabolism and are fueled by endogenous substrates. Washed ejaculates were incubated in chemically defined medium in the presence/absence of glucose and pyruvate. A second set of ejaculates was exposed to a chemical inhibitor of either lactate dehydrogenase (sodium oxamate) or glyceraldehyde-3-phosphate dehydrogenase (alpha-chlorohydrin). Sperm function (motility and acrosomal integrity) and lactate production were assessed, and a subset of spermatozoa was assayed for intracellular glycogen. In both the cat and cheetah, sperm function was maintained without exogenous substrates and following lactate dehydrogenase inhibition. Lactate production occurred in the absence of exogenous hexoses, but only if pyruvate was present. Intracellular glycogen was not detected in spermatozoa from either species. Unexpectedly, glycolytic inhibition by alpha-chlorohydrin resulted in an immediate decline in sperm motility, particularly in the domestic cat. Collectively, our findings reveal an essential role of the glycolytic pathway in felid spermatozoa that is unrelated to hexose metabolism or lactate formation. Instead, glycolytic enzyme activity could be required for the metabolism of endogenous lipid-derived glycerol, with fatty acid oxidation providing the primary energy source in felid spermatozoa. C1 [Terrell, Kimberly A.; Wildt, David E.; Crosier, Adrienne E.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Terrell, Kimberly A.; Anthony, Nicola M.; Leibo, S. P.] Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA. [Bavister, Barry D.] Univ Puerto Rico, San Juan, PR 00936 USA. [Penfold, Linda M.] White Oak Conservat Ctr, Yulee, FL USA. [Marker, Laurie L.] Cheetah Conservat Fund, Otjiwarongo, Namibia. RP Crosier, AE (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. EM crosiera@si.edu FU National Science Foundation; Louisiana State University; Audubon Center for Research of Endangered Species; Ohrstrom Family Foundation; William H. Donner Foundation, Inc. FX Supported by the National Science Foundation Graduate Research Fellowship Program, Louisiana State University and Audubon Center for Research of Endangered Species Grant Program, the Ohrstrom Family Foundation, and the William H. Donner Foundation, Inc. NR 65 TC 4 Z9 4 U1 3 U2 28 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD JUN PY 2011 VL 84 IS 6 BP 1198 EP 1206 DI 10.1095/biolreprod.110.090225 PG 9 WC Reproductive Biology SC Reproductive Biology GA 766PL UT WOS:000290797900016 PM 21325689 ER PT J AU Zotz, G Wilhelm, K Becker, A AF Zotz, Gerhard Wilhelm, Kerstin Becker, Annette TI Heteroblasty-A Review SO BOTANICAL REVIEW LA English DT Review DE Bromeliaceae; Carnivorous plants; Divaricate shrubs; Epiphytes; Evolution; Hemiepiphytes; Heterophylly; Plant hormones; Leaf development; Phase change ID TILLANDSIA-DEPPEANA BROMELIACEAE; COMPOUND LEAF DEVELOPMENT; VEGETATIVE PHASE-CHANGE; ACACIA-KOA LEGUMINOSAE; PLANT ORGAN SIZE; NEW-ZEALAND; GENETIC-CONTROL; HEDERA-HELIX; PSEUDOPANAX-CRASSIFOLIUS; FUNCTIONAL-SIGNIFICANCE AB Virtually all plants show a certain degree of variation among individual metamers during ontogeny. In some cases, however, there are abrupt and substantial changes in form and function (e.g. in leaf form, leaf size, phyllotaxy, internode length, anthocyanin pigmentation, rooting ability, or wood structure). These plants were called "heteroblastic" by Karl Goebel more than a century ago, but the functional significance of this type of ontogenetic change, the evolutionary trajectories in different plant groups, even their frequency in the plant kingdom are still unresolved issues. We argue that slow progress is partly due to an on-going terminological confusion and the lack of distinction between other developmental processes such as ontogenetic drift. This review develops a conceptual framework for future scientific work, proposes a quantitative index of heteroblasty, and discusses the evidence for developmental regulation, functional significance, and evolutionary implications of heteroblasty to provide a stimulating basis for further research with this fascinating group of plants. C1 [Zotz, Gerhard; Wilhelm, Kerstin] Carl von Ossietzky Univ Oldenburg, Inst Biol & Umweltwissensch, AG Funktionelle Okol, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. Univ Bremen, AG Evolut Entwicklungsgenet Pflanzen, D-28359 Bremen, Germany. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Inst Biol & Umweltwissensch, AG Funktionelle Okol, Postfach 2503, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de RI Becker, Annette/F-2355-2014 OI Becker, Annette/0000-0002-3229-2162 FU Deutsche Forschungsgemeinschaft [GZ ZO 94/4-1, BE 2547/7-2, BE 2547/8-1] FX Of tremendous help in procuring the literature for this review were Herta Sauerbrey (Oldenburg, Germany) and Angel Aguirre (STRI, Panama). Financial support of the Deutsche Forschungsgemeinschaft (GZ ZO 94/4-1) for our current studies on heteroblasty in bromeliads is acknowledged. The Deutsche Forschungsgemeinschaft also funds ongoing research in AB's laboratory (BE 2547/7-2 and/8-1). Critical comments on an earlier draft by Dirk Albach, Oldenburg, are appreciated. NR 147 TC 52 Z9 53 U1 2 U2 65 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0006-8101 J9 BOT REV JI Bot. Rev. PD JUN PY 2011 VL 77 IS 2 BP 109 EP 151 DI 10.1007/s12229-010-9062-8 PG 43 WC Plant Sciences SC Plant Sciences GA 766SC UT WOS:000290805800002 ER PT J AU Meyer, CFJ Aguiar, LMS Aguirre, LF Baumgarten, J Clarke, FM Cosson, JF Villegas, SE Fahr, J Faria, D Furey, N Henry, M Hodgkison, R Jenkins, RKB Jung, KG Kingston, T Kunz, TH MacSwiney, MC Moya, I Patterson, BD Pons, JM Racey, PA Rex, K Sampaio, EM Solari, S Stoner, KE Voigt, CC von Staden, D Weise, CD Kalko, EKV AF Meyer, Christoph F. J. Aguiar, Ludmilla M. S. Aguirre, Luis F. Baumgarten, Julio Clarke, Frank M. Cosson, Jean-Francois Villegas, Sergio Estrada Fahr, Jakob Faria, Deborah Furey, Neil Henry, Mickael Hodgkison, Robert Jenkins, Richard K. B. Jung, Kirsten G. Kingston, Tigga Kunz, Thomas H. MacSwiney, Maria Cristina Moya, Isabel Patterson, Bruce D. Pons, Jean-Marc Racey, Paul A. Rex, Katja Sampaio, Erica M. Solari, Sergio Stoner, Kathryn E. Voigt, Christian C. von Staden, Dietrich Weise, Christa D. Kalko, Elisabeth K. V. TI Accounting for detectability improves estimates of species richness in tropical bat surveys SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE bats; biodiversity monitoring; Chiroptera; community ecology; detection probability; jackknife estimator; species richness ID OCCUPANCY ESTIMATION; ECHOLOCATION CALLS; LOCAL EXTINCTION; TURNOVER RATES; PROBABILITIES; COMMUNITIES; ASSEMBLAGES; DETECTORS; DETERMINANTS; INVENTORY AB P>1. Species richness is a state variable of some interest in monitoring programmes but raw species counts are often biased due to imperfect species detectability. Therefore, monitoring programmes should quantify detectability for target taxa to assess whether it varies over temporal or spatial scales. We assessed the potential for tropical bat monitoring programmes to reliably estimate trends in species richness. 2. Using data from 25 bat assemblages from the Old and New World tropics, we estimated detectability for all species in an assemblage (mean proportion of species detected per sampling plot) and for individual species (species-specific detectability). We further assessed how these estimates of detectability were affected by external sources of variation relating to time, space, survey effort and biological traits. 3. The mean proportion of species detected across 96 sampling plots was estimated at 0 center dot 76 (range 0 center dot 57-1 center dot 00) and was significantly greater for phytophagous than for animalivorous species. Species-averaged detectability for phytophagous species was influenced by the number of surveys and season, whereas the number of surveys and sampling methods [ground- or canopy-level mist nets, harp traps and acoustic sampling (AS)] most strongly affected estimates of detectability for animalivorous bats. Species-specific detectability averaged 0 center dot 4 and was highly heterogeneous across 232 species, with estimates ranging from 0 center dot 03 to 0 center dot 84. Species-level detectability was influenced by a range of external factors such as location, season, or sampling method, suggesting that raw species counts may sometimes be strongly biased. 4.Synthesis and applications. Due to generally high species-specific detection probabilities, Neotropical aerial insectivorous bats proved to be well suited for monitoring using AS. However, for species with low detectability, such as most gleaning animalivores or nectarivores, count data obtained in bat monitoring surveys must be corrected for detection bias. Our results indicate that species-averaged detection probabilities will rarely approach 1 unless many surveys are conducted. Consequently, long-term bat monitoring programmes need to adopt an estimation scheme that corrects for variation in detectability when comparing species richness over time and when making regional comparisons. Similar corrections will be needed for other species-rich tropical taxa. C1 [Meyer, Christoph F. J.; Fahr, Jakob; Hodgkison, Robert; Jung, Kirsten G.; Sampaio, Erica M.; von Staden, Dietrich; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Meyer, Christoph F. J.] Univ Lisbon, Fac Ciencias, Ctr Biol Ambiental, P-1749016 Lisbon, Portugal. [Aguiar, Ludmilla M. S.] Univ Brasilia, Dept Zool, BR-70910900 Brasilia, DF, Brazil. [Aguirre, Luis F.] Univ Mayor San Simon, Ctr Biodiversidad & Genet, Cochabamba, Bolivia. [Aguirre, Luis F.; Moya, Isabel] Ctr Estudios Biol Teor & Aplicada, Programa Para Conservac Murcielagos Bolivia, La Paz, Bolivia. [Baumgarten, Julio; Faria, Deborah] Univ Estadual Santa Cruz, Dept Ciencias Biol, BR-45650000 Ilheus, Bahia, Brazil. [Clarke, Frank M.; Furey, Neil; Jenkins, Richard K. B.; MacSwiney, Maria Cristina] Univ Aberdeen, Inst Biol & Environm Sci, Aberdeen AB24 2TZ, Scotland. [Cosson, Jean-Francois] INRA, UMR CBGP, F-34988 Montferrier Sur Lez, France. [Villegas, Sergio Estrada] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Henry, Mickael] INRA, UMR 406 Abeilles & Environm, F-84914 Avignon, France. [Jenkins, Richard K. B.] Madagasikara Voakajy, Antananarivo, Madagascar. [Jenkins, Richard K. B.] Univ Kent, Sch Anthropol & Conservat, DICE, Canterbury CT2 7NR, Kent, England. [Jenkins, Richard K. B.] Bangor Univ, Sch Environm Nat Resources & Geog, Bangor LL57 2UW, Gwynedd, Wales. [Kingston, Tigga] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. [Kunz, Thomas H.] Boston Univ, Ctr Ecol & Conservat Biol, Dept Biol, Boston, MA 02215 USA. [MacSwiney, Maria Cristina] Univ Veracruzana, Ctr Invest Trop, Veracruz 91019, Mexico. [Patterson, Bruce D.] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. [Pons, Jean-Marc] Museum Natl Hist Nat, Dept Systemat & Evolut, UMR 7205, F-75005 Paris, France. [Racey, Paul A.] Univ Exeter Cornwall, Ctr Ecol & Conservat, Penryn TR10 9EZ, England. [Rex, Katja; Voigt, Christian C.] Leibniz Inst Zoo & Wildlife Res, D-10315 Berlin, Germany. [Solari, Sergio] Univ Antioquia, Inst Biol, Medellin 1226, Colombia. [Stoner, Kathryn E.] Univ Nacl Autonoma Mexico, Ctr Invest & Ecosistemas, Morelia 58089, Michoacan, Mexico. [Weise, Christa D.] Bat Conservat Int, Austin, TX 78716 USA. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Meyer, CFJ (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM cmeyer@fc.ul.pt RI Meyer, Christoph/A-4363-2012; Jenkins, Richard/A-4567-2012; Faria, Deborah/F-2879-2010; Fahr, Jakob/E-8831-2012; Aguiar, Ludmilla/H-7339-2015; baumgarten, julio/A-5630-2012; Stoner, Kathryn/E-1510-2015; Aguiar, Ludmilla /J-7659-2012; OI Cosson, Jean Francois/0000-0003-0863-5871; Meyer, Christoph/0000-0001-9958-8913; Fahr, Jakob/0000-0002-9174-1204; Aguiar, Ludmilla/0000-0002-9180-5052; baumgarten, julio/0000-0001-9258-7547; Stoner, Kathryn/0000-0002-9964-1697; Aguiar, Ludmilla /0000-0002-9180-5052; Patterson, Bruce D./0000-0002-2249-7260 FU Conservation International (CI) FX We wish to thank Monika Riepl for assistance with data preparation and Conservation International (CI) for funding. See Supporting Information for a complete list of the funding sources for the studies included in this work. This research evolved from a bat monitoring workshop hosted by the TEAM network at CI. Special thanks go to S. Andelman, K. Jones, T. Kunz and M. Willig who were instrumental in pursuing the idea of this meeting. The authors are grateful to Brock Fenton, two anonymous reviewers, and the Associate Editor for helpful comments on previous versions of the manuscript. NR 47 TC 22 Z9 24 U1 1 U2 87 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 JUN PY 2011 VL 48 IS 3 BP 777 EP 787 DI 10.1111/j.1365-2664.2011.01976.x PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 763VF UT WOS:000290587100031 ER PT J AU Rick, TC Culleton, BJ Smith, CB Johnson, JR Kennett, DJ AF Rick, Torben C. Culleton, Brendan J. Smith, Carley B. Johnson, John R. Kennett, Douglas J. TI Stable isotope analysis of dog, fox, and human diets at a Late Holocene Chumash village (CA-SRI-2) on Santa Rosa Island, California SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Stable isotopes; Paleodiet; Canis familiaris; Urocyon littoralis; Island ecology ID CHANNEL-ISLANDS; BONE-COLLAGEN; SOUTHERN-CALIFORNIA; NITROGEN ISOTOPES; CANIS-FAMILIARIS; MESOLITHIC DOGS; STAR-CARR; CARBON; ARCHAEOLOGY; RATIOS AB Stable carbon (delta C-13) and nitrogen (delta N-15) isotope analyses of dog (Canis familiaris), island fox (Urocyon littoralis), and human bone collagen from CA-SRI-2 (AD 130-1830) on Santa Rosa Island, California provide a proxy of diet and the relationships between humans and these animals. Carbon isotopic signatures indicate that Native Americans and their dogs at CA-SRI-2 subsisted almost exclusively on marine resources, while the island fox ate primarily terrestrial foods. Nitrogen isotopes and archaeofaunal remains indicate that humans and dogs also ate higher trophic level foods, including finfishes, marine mammals, and seabirds with smaller amounts of shellfish. The CA-SRI-2 island foxes appear to have eaten higher amounts of terrestrial foods, similar to the diets observed in modern fox populations. These data generally confirm the commensal relationship assumed to exist between domesticated dogs and people, but the carbon isotopic composition of dogs is enriched similar to 2 parts per thousand compared to humans. We hypothesize that the difference in carbon isotopes between dogs and humans may have resulted from a higher consumption of C3 plants with lower delta C-13 values by humans, or less likely from the ingestion by dogs of significant amounts of bone collagen, which is enriched by similar to 4 parts per thousand over associated muscle. Published by Elsevier Ltd. C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Culleton, Brendan J.; Smith, Carley B.; Kennett, Douglas J.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Johnson, John R.] Santa Barbara Museum Nat Hist, Dept Anthropol, Santa Barbara, CA 93105 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 FU Smithsonian Institution, University of Oregon; Channel Islands National Park [1443CA8120-00-007]; Ann Huston and Kelly Minas of Channel Islands National Park FX This paper is dedicated to the late Phil C. Orr who collected most of the human, dog, and fox remains analyzed in this study in the 1940s and 1950s. Funds for this project were provided by the Smithsonian Institution, University of Oregon, and Channel Islands National Park (Cooperative Agreement #1443CA8120-00-007). We thank Ann Huston and Kelly Minas of Channel Islands National Park for supporting our research. Finally we thank Seth Newsome, anonymous reviewers, Richard Klein, and the editorial staff of the Journal of Archaeological Science for help in the revision, editing, and production of this manuscript. NR 57 TC 15 Z9 15 U1 0 U2 29 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 JUN PY 2011 VL 38 IS 6 BP 1385 EP 1393 DI 10.1016/j.jas.2011.02.008 PG 9 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 761SF UT WOS:000290420300023 ER PT J AU Chance, K Orphal, J AF Chance, K. Orphal, J. TI Revised ultraviolet absorption cross sections of H2CO for the HITRAN database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Ultraviolet spectroscopy; Atmospheric spectroscopy; Atmospheric measurements ID FORMALDEHYDE; GOME AB A revised set of temperature-dependent absorption cross sections for ultraviolet (UV) measurements of formaldehyde (H2CO) has been derived from two existing sets of laboratory cross sections, one using a Fourier transform spectrometer (FTS), and one using a grating instrument. This is conducted to satisfy the recommendation of the HITRAN Advisory Committee to provide a dataset with the spectral resolution and wavelength calibration of Fourier transform spectrometer measurements with the better intensity calibration that the grating measurements obtained. The re-scaled cross sections are now in the HITRAN database, and are recommended for use in atmospheric measurements and modeling, including photolysis calculations. Published by Elsevier Ltd. C1 [Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Orphal, J.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-76344 Eggenstein Leopoldshafen, Germany. RP Chance, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM KChance@CfA.Harvard.edu RI Orphal, Johannes/A-8667-2012; OI Orphal, Johannes/0000-0002-1943-4496; Chance, Kelly/0000-0002-7339-7577 FU NASA; Smithsonian Institution FX This work was supported by NASA and the Smithsonian Institution. NR 12 TC 11 Z9 11 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUN PY 2011 VL 112 IS 9 BP 1509 EP 1510 DI 10.1016/j.jqsrt.2011.02.002 PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 765YI UT WOS:000290744900012 ER PT J AU Clough, GW AF Clough, G. Wayne TI Civil Discourse 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 JUN PY 2011 VL 42 IS 3 BP 22 EP 22 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 766VW UT WOS:000290815700009 ER PT J AU Robinson, TD Meadows, VS Crisp, D Deming, D A'Hearn, MF Charbonneau, D Livengood, TA Seager, S Barry, RK Hearty, T Hewagama, T Lisse, CM McFadden, LA Wellnitz, DD AF Robinson, Tyler D. Meadows, Victoria S. Crisp, David Deming, Drake A'Hearn, Michael F. Charbonneau, David Livengood, Timothy A. Seager, Sara Barry, Richard K. Hearty, Thomas Hewagama, Tilak Lisse, Carey M. McFadden, Lucy A. Wellnitz, Dennis D. TI Earth as an Extrasolar Planet: Earth Model Validation Using EPOXI Earth Observations SO ASTROBIOLOGY LA English DT Article DE Astrobiology; Extrasolar terrestrial planets; Habitability; Planetary science; Radiative transfer ID MOLECULAR SPECTROSCOPIC DATABASE; DISK-AVERAGED SPECTRA; LIGHT-CURVES; EMISSION SPECTROMETER; VEGETATION SIGNATURE; TERRESTRIAL PLANETS; AURA SATELLITE; KEPLER-MISSION; WIDE-FIELD; SEARCH AB The EPOXI Discovery Mission of Opportunity reused the Deep Impact flyby spacecraft to obtain spatially and temporally resolved visible photometric and moderate resolution near-infrared (NIR) spectroscopic observations of Earth. These remote observations provide a rigorous validation of whole-disk Earth model simulations used to better understand remotely detectable extrasolar planet characteristics. We have used these data to upgrade, correct, and validate the NASA Astrobiology Institute's Virtual Planetary Laboratory three-dimensional line-by-line, multiple-scattering spectral Earth model. This comprehensive model now includes specular reflectance from the ocean and explicitly includes atmospheric effects such as Rayleigh scattering, gas absorption, and temperature structure. We have used this model to generate spatially and temporally resolved synthetic spectra and images of Earth for the dates of EPOXI observation. Model parameters were varied to yield an optimum fit to the data. We found that a minimum spatial resolution of similar to 100 pixels on the visible disk, and four categories of water clouds, which were defined by using observed cloud positions and optical thicknesses, were needed to yield acceptable fits. The validated model provides a simultaneous fit to Earth's lightcurve, absolute brightness, and spectral data, with a root-mean-square (RMS) error of typically less than 3% for the multiwavelength lightcurves and residuals of similar to 10% for the absolute brightness throughout the visible and NIR spectral range. We have extended our validation into the mid-infrared by comparing the model to high spectral resolution observations of Earth from the Atmospheric Infrared Sounder, obtaining a fit with residuals of similar to 7% and brightness temperature errors of less than 1 K in the atmospheric window. For the purpose of understanding the observable characteristics of the distant Earth at arbitrary viewing geometry and observing cadence, our validated forward model can be used to simulate Earth's time-dependent brightness and spectral properties for wavelengths from the far ultraviolet to the far infrared. C1 [Robinson, Tyler D.; Meadows, Victoria S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Crisp, David] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Deming, Drake; Livengood, Timothy A.; Barry, Richard K.; Hearty, Thomas; Hewagama, Tilak; McFadden, Lucy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [A'Hearn, Michael F.; Wellnitz, Dennis D.] Univ Maryland, College Pk, MD 20742 USA. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Seager, Sara] MIT, Cambridge, MA 02139 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Robinson, TD (reprint author), Univ Washington, Dept Astron, Phys Astron Bldg,Room C319,3910 15th Ave NE, Seattle, WA 98195 USA. EM robinson@astro.washington.edu RI Wellnitz, Dennis/B-4080-2012; Hewagama, T/C-8488-2012; Livengood, Timothy/C-8512-2012; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; McFadden, Lucy/0000-0002-0537-9975; Charbonneau, David/0000-0002-9003-484X FU NASA; EPOXI mission; NASA Astrobiology Institute FX This work is supported by the NASA Discovery Program and the EPOXI mission. The authors gratefully acknowledge the contributions of the Deep Impact/EPOXI operations team at the Jet Propulsion Laboratory/California Institute of Technology, without whom Earth observations could not have been accomplished. T. R and V. M. gratefully acknowledge the support of the NASA Astrobiology Institute, without which the original Earth model would not have been developed. We would like to thank Jeff Pedelty for his work designing the EPOXI Earth observation program as well as Tom Ackerman and Gwyn Fireman for assistance with MODIS data interpretation. Some of the results in this paper have been derived using the HEALPix (Gorski et al., 2005) package. NR 48 TC 45 Z9 45 U1 1 U2 10 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 JUN PY 2011 VL 11 IS 5 BP 393 EP 408 DI 10.1089/ast.2011.0642 PG 16 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 783MI UT WOS:000292086900002 PM 21631250 ER PT J AU Gunther, HM AF Guenther, H. M. TI Accretion, jets and winds: High-energy emission from young stellar objects Doctoral Thesis Award Lecture 2010 SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE accretion, accretion disks; circumstellar matter; ISM: jets and outflows; stars: winds, outflows; T Tauri stars; X-rays: stars ID T-TAURI-STARS; X-RAY-EMISSION; HERBIG-AE/BE STARS; ORION ULTRADEEP PROJECT; ALL-SKY SURVEY; DG-TAURI; XMM-NEWTON; DISK ACCRETION; MAGNETOSPHERIC ACCRETION; PROTOSTELLAR JET AB This article summarizes the processes of high-energy emission in young stellar objects. Stars of spectral type A and B are called Herbig Ae/Be (HAeBe) stars in this stage, all later spectral types are termed classical T Tauri stars (CTTS). Both types are studied by high-resolution X-ray and UV spectroscopy and modeling. Three mechanisms contribute to the high-energy emission from CTTS: 1) CTTS have active coronae similar to main-sequence stars, 2) the accreted material passes through an accretion shock at the stellar surface, which heats it to a few MK, and 3) some CTTS drive powerful outflows. Shocks within these jets can heat the plasma to X-ray emitting temperatures. Coronae are already well characterized in the literature; for the latter two scenarios models are shown. The magnetic field suppresses motion perpendicular to the field lines in the accretion shock, thus justifying a 1D geometry. The radiative loss is calculated as optically thin emission. A mixture of shocked and coronal gas is fitted to X-ray observations of accreting CTTS. Specifically, the model explains the peculiar line-ratios in the He-like triplets of Ne IX and O VII. All stars require only small mass accretion rates to power the X-ray emission. In contrast, the HAeBe HD 163296 has line ratios similar to coronal sources, indicating that neither a high density nor a strong UV-field is present in the region of the X-ray emission. This could be caused by a shock in its jet. Similar emission is found in the deeply absorbed CTTS DG Tau. Shock velocities between 400 and 500 km s(-1) are required to explain the observed spectrum. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gunther, HM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hguenther@cfa.harvard.edu FU Faculty of the European Space Astronomy Centre [GO6-7017X] FX I thank the Astronomische Gesellschaft for awarding me the newly established Promotionspreis in 2010. The work, which is summarized in this article, would not have been possible without the help and advice of my colleagues at the Hamburger Sternwarte and especially my thesis adviser Prof. J. H. M. M. Schmitt. Jan-Uwe Ness helped a lot i nthe CORA fits to the Mg triplet. H. M. G. acknowledges financial support from Chandra grant GO6-7017X and from the Faculty of the European Space Astronomy Centre. This research made use of the Chandra Transmission Grating Catalog and archive (http://tgcat.mit.edu). NR 112 TC 8 Z9 8 U1 0 U2 4 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD JUN PY 2011 VL 332 IS 5 BP 448 EP 460 DI 10.1002/asna.201111559 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 782JK UT WOS:000292004100003 ER PT J AU Brunthaler, A Reid, MJ Menten, KM Zheng, XW Bartkiewicz, A Choi, YK Dame, T Hachisuka, K Immer, K Moellenbrock, G Moscadelli, L Rygl, KLJ Sanna, A Sato, M Wu, Y Xu, Y Zhang, B AF Brunthaler, A. Reid, M. J. Menten, K. M. Zheng, X. -W. Bartkiewicz, A. Choi, Y. K. Dame, T. Hachisuka, K. Immer, K. Moellenbrock, G. Moscadelli, L. Rygl, K. L. J. Sanna, A. Sato, M. Wu, Y. Xu, Y. Zhang, B. TI The Bar and Spiral Structure Legacy (BeSSeL) survey: Mapping the Milky Way with VLBI astrometry SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE astrometry; Galaxy: fundamental parameters; Galaxy: kinematics and dynamics; Galaxy: structure ID LOCAL STELLAR KINEMATICS; STAR-FORMING REGIONS; TRIGONOMETRIC PARALLAXES; PROPER MOTION; GALACTIC PARAMETERS; MAGELLANIC STREAM; METHANOL MASERS; ORION NEBULA; BLACK-HOLE; DISTANCE AB Astrometric Very Long Baseline Interferometry (VLBI) observations of maser sources in the Milky Way are used to map the spiral structure of our galaxy and to determine fundamental parameters such as the rotation velocity (Theta(0)) and curve and the distance to the Galactic center (R-0). Here, we present an update on our first results, implementing a recent change in the knowledge about the Solar motion. It seems unavoidable that the IAU recommended values for R0 and Theta(0) need a substantial revision. In particular the combination of 8.5 kpc and 220 km s(-1) can be ruled out with high confidence. Combining the maser data with the distance to the Galactic center from stellar orbits and the proper motion of Sgr A* gives best values of R-0 = 8.3 +/- 0.23 kpc and Theta(0) = 239 or 246 +/- 7 km s(-1), for Solar motions of V-circle dot = 12.23 and 5.25 km s(-1), respectively. Finally, we give an outlook to future observations in the Bar and Spiral Structure Legacy (BeSSeL) survey. (C) 2011 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Brunthaler, A.; Menten, K. M.; Choi, Y. K.; Immer, K.; Rygl, K. L. J.; Sanna, A.; Zhang, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.; Dame, T.; Immer, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zheng, X. -W.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. [Bartkiewicz, A.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Hachisuka, K.] Shanghai Astron Observ, Shanghai, Peoples R China. [Moellenbrock, G.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Moscadelli, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Rygl, K. L. J.] Ist Fis Spazio Interplanetario IFSI INAF, I-00133 Rome, Italy. [Sato, M.] Univ Tokyo, Dept Astron, Grad Sch Sci, Tokyo 1130033, Japan. [Wu, Y.; Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210093, Peoples R China. RP Brunthaler, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM brunthal@mpifr-bonn.mpg.de RI Bartkiewicz, Anna/D-6212-2014; he, shuyi/K-2082-2014; OI Moscadelli, Luca/0000-0002-8517-8881 FU national research councils; ERC [247078]; ASI [I/005/07/1] FX The Very Long Baseline Array (VLBA) is an instrument built and operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The European VLBI Network is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). K.L.J.R. is funded by an ASI fellowship under contract number I/005/07/1. NR 74 TC 88 Z9 90 U1 2 U2 9 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD JUN PY 2011 VL 332 IS 5 BP 461 EP 466 DI 10.1002/asna.201111560 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 782JK UT WOS:000292004100004 ER PT J AU Riveros, AJ Enquist, BJ AF Riveros, A. J. Enquist, B. J. TI Metabolic scaling in insects supports the predictions of the WBE model SO JOURNAL OF INSECT PHYSIOLOGY LA English DT Article DE Metabolic scaling; Body size; Termites; Metabolic rate; Nutrient supply network model ID GENERAL-MODEL; MAMMALS; SIZE; TEMPERATURE; ALLOMETRY; CELLS; EVOLUTION; BIOLOGY; GROWTH; FORM AB The functional association between body size and metabolic rate (BS-MR) is one of the most intriguing issues in ecological physiology. An average scaling exponent of 3/4 is broadly observed across animal and plant taxa. The numerical value of 3/4 is theoretically predicted under the optimized version of West, Brown, and Enquist's vascular resource supply network model. Insects, however, have recently been proposed to express a numerically different scaling exponent and thus application of the WBE network model to insects has been rejected. Here, we re-analyze whether such variation is indeed supported by a global deviation across all insect taxa at the order and family levels to assess if specific taxa influence insect metabolic scaling. We show that a previous reported deviation is largely due to the effect of a single insect family (Termitidae). We conclude that the BS-MR relationship in insects broadly supports the core predictions of the WBE model. We suggest that the deviation observed within the termites warrants further investigation and may be due to either difficulty in accurately measuring termite metabolism and/or particularities of their life history. Future work on allometric scaling should assess the nature of variation around the central tendencies in scaling exponents in order to test if this variation is consistent with core assumptions and predictions of the WBE model that stem by relaxing its secondary optimizing assumptions that lead to the 3/4 exponent. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Riveros, A. J.] Univ Arizona, Dept Neurosci, Tucson, AZ 85721 USA. [Enquist, B. J.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. RP Riveros, AJ (reprint author), Smithsonian Trop Res Inst, Lab Behav & Evolutionary Neurobiol, Unit 9100,Box 0948, DPO, AA 34002 USA. EM anjosafat@gmail.com OI Enquist, Brian/0000-0002-6124-7096 FU NSF [IOB-0519483] FX We thank Van Savage for comments on earlier versions of this manuscript. This paper was inspired in part by discussions with members of the ECOL586, Biological Scaling Class in 2007. A.J.R. was supported by an NSF (IOB-0519483) grant to W. Gronenberg. B.J.E. was supported by an NSF Advancing Theory Grant. NR 43 TC 15 Z9 15 U1 1 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-1910 J9 J INSECT PHYSIOL JI J. Insect Physiol. PD JUN PY 2011 VL 57 IS 6 BP 688 EP 693 DI 10.1016/j.jinsphys.2011.01.011 PG 6 WC Entomology; Physiology; Zoology SC Entomology; Physiology; Zoology GA 783YM UT WOS:000292120800003 PM 21296084 ER PT J AU Landt, H Elvis, M Ward, MJ Bentz, MC Korista, KT Karovska, M AF Landt, Hermine Elvis, Martin Ward, Martin J. Bentz, Misty C. Korista, Kirk T. Karovska, Margarita TI The near-infrared broad emission line region of active galactic nuclei - II. The 1-mu m continuum SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: nuclei; quasars: general; infrared: galaxies ID RADIUS-LUMINOSITY RELATIONSHIP; TYPE-1 SEYFERT-GALAXIES; BLACK-HOLE; ENERGY-DISTRIBUTIONS; ACCRETION DISKS; HOST GALAXIES; DUST TORUS; ULTRAVIOLET EXCESS; OPTICAL CONTINUUM; K-CORRECTIONS AB We use quasi-simultaneous near-infrared (near-IR) and optical spectroscopy from four observing runs to study the continuum around 1 mu m in 23 well-known broad emission line active galactic nuclei (AGN). We show that, after correcting the optical spectra for host galaxy light, the AGN continuum around this wavelength can be approximated by the sum of mainly two emission components, a hot dust blackbody and an accretion disc. The accretion disc spectrum appears to dominate the flux at similar to 1 mu m, which allows us to derive a relation for estimating AGN black hole masses based on the near-IR virial product. This result also means that a near-IR reverberation programme can determine the AGN state independent of simultaneous optical spectroscopy. On average we derive hot dust blackbody temperatures of similar to 1400 K, a value close to the sublimation temperature of silicate dust grains, and relatively low hot dust covering factors of similar to 7 per cent. Our preliminary variability studies indicate that in most sources, the hot dust emission responds to changes in the accretion disc flux with the expected time lag; however, a few sources show a behaviour that can be attributed to dust destruction. C1 [Landt, Hermine] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Elvis, Martin; Karovska, Margarita] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ward, Martin J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Bentz, Misty C.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Korista, Kirk T.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. RP Landt, H (reprint author), Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. EM hlandt@unimelb.edu.au FU National Science Foundation [AST-0604066]; National Aeronautics Space Administration FX We are indebted to Brad Peterson for stimulating discussions and his help with the general project. We thank Perry Berlind and Mike Calkins for the FAST observations and Susan Tokarz and Nathalie Martimbeau for the reduction of these data. MCB acknowledges financial support by the National Science Foundation (grant AST-0604066). 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 Space Administration. NR 62 TC 37 Z9 37 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2011 VL 414 IS 1 BP 218 EP 240 DI 10.1111/j.1365-2966.2011.18383.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 784FO UT WOS:000292141600036 ER PT J AU Revnivtsev, M Sazonov, S Forman, W Churazov, E Sunyaev, R AF Revnivtsev, M. Sazonov, S. Forman, W. Churazov, E. Sunyaev, R. TI Luminosity function of faint Galactic sources in the Chandra bulge field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: general; stars: luminosity function, mass function; Galaxy: bulge; X-rays: binaries; X-rays: stars ID X-RAY-EMISSION; EARLY-TYPE GALAXIES; ELLIPTIC GALAXIES; POINT SOURCES; INTERSTELLAR EXTINCTION; CATACLYSMIC VARIABLES; STELLAR POPULATION; MILKY-WAY; RIDGE; ORIGIN AB We study the statistical properties of faint X-ray sources detected in the Chandra bulge field. The unprecedented sensitivity of the Chandra observations allows us to probe the population of faint Galactic X-ray sources down to luminosities L2-10 keV similar to 10(30) erg s(-1) at the Galactic Centre distance. We show that the luminosity function of these CBF sources agrees well with the luminosity function of sources in the solar vicinity. The cumulative luminosity density of sources detected in the CBF in the luminosity range 10(30)-10(32) erg s(-1) per unit stellar mass is L2-10 keV/M-* = (1.7 +/- 0.3) x 10(27) erg s(-1) M-circle dot(-1). Taking into account sources in the luminosity range 10(32)-10(34) erg s-1 from Sazonov et al. 2006, the cumulative luminosity density in the broad luminosity range 10(30)-10(34) erg s(-1) becomes L2-10 keV/M-* =(2.4 +/- 0.4) x 10(27) erg s(-1) M-circle dot(-1). The majority of sources with the faintest luminosities should be active binary stars with hot coronae based on the available luminosity function of X-ray sources in the solar environment. C1 [Revnivtsev, M.; Sazonov, S.; Churazov, E.; Sunyaev, R.] Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. [Revnivtsev, M.] Tech Univ Munich, D-85748 Garching, Germany. [Forman, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Churazov, E.; Sunyaev, R.] Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Revnivtsev, M (reprint author), Russian Acad Sci, Inst Space Res, Profsoyuznaya 84-32, Moscow 117997, Russia. EM revnivtsev@iki.rssi.ru RI Churazov, Eugene/A-7783-2013 FU Russian Foundation of Basic Research [10-02-00492-a]; Russian Academy of Sciences [P-19, OFN-16]; Dynasty Foundation; [NSh-5069.2010.2] FX This research made use of data obtained from the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. This work was supported by a grant of Russian Foundation of Basic Research 10-02-00492-a, grant NSh-5069.2010.2 and programmes of the Russian Academy of Sciences P-19 and OFN-16. SS acknowledges the support of the Dynasty Foundation. NR 33 TC 16 Z9 16 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2011 VL 414 IS 1 BP 495 EP 499 DI 10.1111/j.1365-2966.2011.18411.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 784FO UT WOS:000292141600056 ER PT J AU Zahn, O Mesinger, A McQuinn, M Trac, H Cen, RY Hernquist, LE AF Zahn, Oliver Mesinger, Andrei McQuinn, Matthew Trac, Hy Cen, Renyue Hernquist, Lars E. TI Comparison of reionization models: radiative transfer simulations and approximate, seminumeric models SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE intergalactic medium; cosmology: theory; dark ages, reionization, first stars; diffuse radiation; large-scale structure of Universe ID LY-ALPHA EMITTERS; PROBE WMAP OBSERVATIONS; HYDROGEN REIONIZATION; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; BUBBLE-GROWTH; HIGH-REDSHIFT; HII-REGIONS; PATCHY REIONIZATION; COMPARISON PROJECT AB We compare the predictions of four different algorithms for the distribution of ionized gas during the Epoch of Reionization. These algorithms are all used to run a 100 Mpc h(-1) simulation of reionization with the same initial conditions. Two of the algorithms are state-of-the-art ray-tracing radiative transfer codes that use disparate methods to calculate the ionization history. The other two algorithms are fast but more approximate schemes based on iterative applications of a smoothing filter on the underlying source and density fields. We compare these algorithms' resulting ionization and 21-cm fields using several different statistical measures. The two radiative transfer schemes are in excellent agreement judging by the power spectra of both the ionization fields and the 21-cm emission fields ( agreeing to better than 10 per cent) and are in good agreement with the analytic schemes ( better than 50 per cent) over the range of ionized fractions and wavevectors we compare ( 0.2 < <(x)over bar>(i) < 0.7; 0.1 < k < 10 h Mpc(-1)). This agreement suggests that the different approximations involved in the ray-tracing algorithms are sensible and that seminumerical schemes provide a numerically inexpensive, yet fairly accurate, description of the reionization process. C1 [Zahn, Oliver] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94708 USA. [Zahn, Oliver] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94708 USA. [Mesinger, Andrei; Cen, Renyue] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [McQuinn, Matthew; Trac, Hy; Hernquist, Lars E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McQuinn, Matthew] Univ Calif Berkeley, Berkeley Astron Dept, Berkeley, CA 94720 USA. [Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. RP Zahn, O (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94708 USA. EM zahn@berkeley.edu; mesinger@astro.princeton.edu; mmcquinn@berkeley.edu; htrac@cfa.harvard.edu RI Trac, Hy/N-8838-2014 OI Trac, Hy/0000-0001-6778-3861 FU Berkeley Center for Cosmological Physics; NASA [HST-HF-51245.01-A, NNG06GI09G]; Space Telescope Science Institute; Association of Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555]; Institute for Theory and Computation Fellowship FX OZ wishes to express special gratitude to the co-authors for being supportive in completing this work after he was injured in the fall of 2009. The authors wish to thank Adam Lidz, Steven Furlanetto and Matias Zaldarriaga for helpful discussions. OZ is supported by an Inaugural Fellowship by the Berkeley Center for Cosmological Physics. AM is supported by NASA through Hubble Fellowship grant HST-HF-51245.01-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. MM is supported by NASA through an Einstein Fellowship. HT is supported by an Institute for Theory and Computation Fellowship. RC acknowledges support from NASA grant NNG06GI09G. NR 74 TC 73 Z9 73 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 JUN PY 2011 VL 414 IS 1 BP 727 EP 738 DI 10.1111/j.1365-2966.2011.18439.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 784FO UT WOS:000292141600079 ER PT J AU Kolbe, SE Lockwood, R Hunt, G AF Kolbe, Sarah E. Lockwood, Rowan Hunt, Gene TI Does morphological variation buffer against extinction? A test using veneroid bivalves from the Plio-Pleistocene of Florida SO PALEOBIOLOGY LA English DT Article ID TROPICAL AMERICAN MOLLUSKS; PANAMA LAND-BRIDGE; GEOGRAPHIC RANGE; PHENOTYPIC PLASTICITY; MASS EXTINCTIONS; WESTERN ATLANTIC; LEAST RESISTANCE; VARIABILITY; NEOGENE; EVOLUTION AB Although morphological variation is known to influence the evolutionary fates of species, the relationship between morphological variation and survivorship in the face of extinction-inducing perturbations is poorly understood. Here, we investigate this relationship for veneroid bivalves in association with the Plio-Pleistocene extinction in Florida. Fourteen pairs of related species were selected for analysis, with each pair including one species that survived the Plio-Pleistocene extinction and another that became extinct during the interval. Morphological landmark data were acquired for more than 1500 museum specimens, representing 19 localities that encompass four well-known PlioPleistocene units in the study region. Procrustes superimposition was applied to each sample, and overall multivariate variation was calculated as the mean squared partial Procrustes distance between specimens and their mean form. Morphological variation was calculated at three geographic scales for each species, and differences in variation between survivors and victims were examined within each species pair. Results indicate that species surviving the Plio-Pleistocene extinction were significantly more variable morphologically than victims. Greater morphological variation may promote survivorship by directly enhancing species adaptations to changing conditions or by permitting the occupation of a larger geographic range. Alternatively, high morphological variation and survivorship may both be mediated by a third variable, such as large geographic range. C1 [Kolbe, Sarah E.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Lockwood, Rowan] Coll William & Mary, Dept Geol, Williamsburg, VA 23187 USA. [Hunt, Gene] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Kolbe, SE (reprint author), Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. EM kolbesh@mail.uc.edu RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 FU Chappell Research Fellowship; Charles Center of the College of William and Mary; Southeastern Section of the Geological Society of America FX We thank R. Portell and L. Ward for facilitating access to museum collections, and H. Packard, B. Stackhouse, B. Leatherman, and E. Gnass for providing assistance in data collection. M. Webster and an anonymous reviewer provided valuable comments that greatly improved the manuscript. This project was made possible by a Chappell Research Fellowship and Student Travel Grant from the Charles Center of the College of William and Mary, and by a travel grant from the Southeastern Section of the Geological Society of America. Acknowledgment is made to the Donors of the American Chemical Society Petroleum Research Fund for partial support of this research. NR 87 TC 13 Z9 14 U1 0 U2 12 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PD SUM PY 2011 VL 37 IS 3 BP 355 EP 368 PG 14 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 786XW UT WOS:000292342200002 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. II. Evolutionary dynamics associated with periodic fluctuation in marine diversity SO PALEOBIOLOGY LA English DT Article ID MASS EXTINCTIONS; TAXONOMIC DIVERSITY; COSMIC-RAYS; ORIGINATION; RECORD; RADIATION; HISTORY; CYCLES; AREA; LIFE AB We use Fourier analysis to investigate evolutionary dynamics related to periodicities in marine fossil biodiversity. Coherent periodic fluctuation in both origination and extinction of "short-lived" genera (those that survive <45 Myr) is the source of an observed similar to 62 million year periodicity (which we confirmed in an earlier paper and also found to be ubiquitous in global compilations of marine diversity). We also show that the evolutionary dynamics of "long-lived" genera (those that survive >45 Myr) do not participate in the periodic fluctuation in diversity and differ from those of "short-lived" genera. The difference between the evolutionary dynamics of long- and short-lived genera indicates that the periodic pattern is not simply an artifact of variation in quality of the geologic record. Also, the interplay of these two previously undifferentiated systems, together with the secular increase in abundance of "long-lived" genera, is probably the source of observed but heretofore unexplained differences in evolutionary dynamics between the Paleozoic and post-Paleozoic as reported by others. Testing for cycles similar to the 62-Myr cycle in fossil biodiversity superimposed on the long-term trends of the Phanerozoic as described in Paper I, we find a significant (but weaker) signal in sedimentary rock packages, particularly carbonates, which suggests a connection. The presence of a periodic pattern in evolutionary dynamics of the more vulnerable "short-lived" component of the marine fauna demonstrates that a long-term periodic fluctuation in environmental conditions capable of affecting evolution in the marine realm characterizes our planet's history. Coincidence in timing is more consistent with a common cause than with sampling bias. A previously identified set of mass extinctions preferentially occur during the declining phase of the 62-Myr periodicity, supporting the idea that the periodicity relates to variation in biotically important stresses. Further work should focus on finding links to physical phenomena that might reveal the causal system or systems. C1 [Melott, Adrian L.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bambach, Richard K.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, 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 University of Kansas; Exobiology and Evolutionary Biology [NNX09AM85G] FX We thank J. Alroy, P. Flemings, K. Miller, J. Ogg, and S. Peters for providing some of the data that we analyze herein. T. Hallam made helpful comments. 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. A question from M. Foote (at our presentation at the North American Paleontological Convention in 2009) about how origination and extinction behave as marine diversity periodically fluctuates focused us on this topic. Research support at the University of Kansas was provided by NASA Program Astrobiology: Exobiology and Evolutionary Biology under grant number NNX09AM85G. This paper is PBDB Publication Number 127. NR 62 TC 12 Z9 12 U1 0 U2 0 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SUM PY 2011 VL 37 IS 3 BP 383 EP 408 PG 26 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 786XW UT WOS:000292342200004 ER PT J AU Harding, JM Walton, WJ Trapani, CM Frick, MG Mann, R AF Harding, Juliana M. Walton, Wendy J. Trapani, Christina M. Frick, Michael G. Mann, Roger TI Sea Turtles as Potential Dispersal Vectors for Non-indigenous Species: The Veined Rapa Whelk as an Epibiont of Loggerhead Sea Turtles SO SOUTHEASTERN NATURALIST LA English DT Article ID LA-PLATA ESTUARY; VENOSA VALENCIENNES; CARETTA-CARETTA; CHESAPEAKE BAY; FEMALE SIZE; BLACK-SEA; MURICIDAE; PREDATION; GASTROPOD; VIRGINIA AB We present the first record of Rapana venosa (Veined Rapa Whelk) as an epibiont of Caretta caretta (Loggerhead Sea Turtle) and the first observation of rapa whelks in the South Atlantic Bight, USA. Veined Rapa Whelks are invasive shellfish predators. The only known North American population of Veined Rapa Whelks is in the southern Chesapeake Bay. Collections of Veined Rapa Whelks as epibionts on Loggerhead Sea Turtles from Norfolk, VA and Wassaw Island, GA present a previously undescribed vector for whelk range expansion to widely separated coastal habitats. In October 2008, a live juvenile Loggerhead stranded near Norfolk, VA with a Veined Rapa Whelk attached to its carapace. Since May 2005, a total of eight Loggerheads with Veined Rapa Whelks as epibionts have been observed nesting on Wassaw Island, GA. The shell lengths of the two smallest Wassaw Island whelks (1.9 and 2.6 mm) indicate that the whelks settled from the plankton 24-48 hr immediately prior to collection in Georgia. This time frame is not commensurate with turtle migration from Chesapeake Bay to Wassaw Island and indicates a whelk source that is geographically distinct from the Chesapeake Bay. Rapa whelk use of Loggerhead carapaces as settlement and juvenile habitat is of serious concern given the observed potential for coastal and oceanic migrations by turtles to facilitate Veined Rapa Whelk dispersal. C1 [Harding, Juliana M.; Mann, Roger] Virginia Inst Marine Sci, Coll William & Mary, Dept Fisheries Sci, Gloucester Point, VA 23062 USA. [Walton, Wendy J.; Trapani, Christina M.] Virginia Aquarium & Marine Sci Ctr, Virginia Beach, VA 23451 USA. [Frick, Michael G.] Smithsonian Natl Zool Pk, Friends Natl Zoo, Washington, DC 20008 USA. RP Harding, JM (reprint author), Coastal Carolina Univ, Dept Marine Sci, Conway, SC 29528 USA. EM jharding@coastal.edu NR 46 TC 6 Z9 6 U1 4 U2 18 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1528-7092 J9 SOUTHEAST NAT JI Southeast. Nat. PD JUN PY 2011 VL 10 IS 2 BP 233 EP 244 DI 10.1656/058.010.0204 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 976SS UT WOS:000306605700004 ER PT J AU Ren, H Lu, LM Soejima, A Luke, Q Zhang, DX Chen, ZD Wen, J AF Ren, Hui Lu, Li-Min Soejima, Akiko Luke, Quentin Zhang, Dian-Xiang Chen, Zhi-Duan Wen, Jun TI Phylogenetic analysis of the grape family (Vitaceae) based on the noncoding plastid trnC-petN, trnH-psbA, and trnL-F sequences SO TAXON LA English DT Article DE phylogeny; trnC-petN; trnH-psbA; trnL-trnF; Vitaceae ID ANATOMICAL DEVELOPMENT; COMPARATIVE ONTOGENY; MOLECULAR PHYLOGENY; AUSTRALIAN VITACEAE; FLORAL DEVELOPMENT; VITIS VITACEAE; DNA; INFERENCE; SYSTEMATICS; CHARACTERS AB The phylogeny of Vitaceae was reconstructed sampling 114 accessions of Vitaceae and the outgroup Leea of Leeaceae, using three noncoding plastid markers: trnC-petN, trnH-psbA, and trnL-F. Six 5-merous genera including Parthenocissus, Ytta, Ampelocissus, Vitis, Nothocissus, and Pterisanthes form a well-supported clade. Ampelopsis, Rhoicissus, and the Cissus striata complex form a clade sister to the clade containing all the other taxa of Vitaceae. The core Cissus clade is resolved to be sister to the Cayratia-Tetrastigma-Cyphostemma clade, forming a clade of taxa with 4-merous flowers. The Parthenocissus-Yua clade is sister to the Ampelocissus-Vitis-Nothocissus-Pterisanthes clade. The Old World Cissus is paraphyletic, with the New World core Cissus nested within it. The intercontinental disjunction between Africa and Asia may have evolved at least twice in Cissus. Cayratia is paraphyletic with four Asian species sampled grouping with Tetrastigma and the African species forming another clade. C1 [Lu, Li-Min; Chen, Zhi-Duan; Wen, Jun] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. [Ren, Hui; Zhang, Dian-Xiang] Chinese Acad Sci, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. [Ren, Hui; Lu, Li-Min] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China. [Soejima, Akiko] Kumamoto Univ, Grad Sch Sci & Technol, Kumamoto 8608555, Japan. [Luke, Quentin] Natl Museums Kenya, E African Herbarium, Nairobi 00502, Kenya. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Wen, J (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. EM wenj@si.edu FU National Science Foundation [DEB 0743474]; John D. and Catherine T. MacArthur Foundation; Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution; National Museum of Natural History of the Smithsonian Institution; Office of Undersecretary of Sciences of the Smithsonian Institution FX The study was supported by the National Science Foundation (grant DEB 0743474 to S.R. Manchester and J. Wen) and the John D. and Catherine T. MacArthur Foundation to J. Wen. Laboratory work was done at and partially supported by the Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution. Fieldwork in North America and Madagascar was supported by the Small Grants Program of the National Museum of Natural History of the Smithsonian Institution, and an Endowment grant from the Office of Undersecretary of Sciences of the Smithsonian Institution. NR 63 TC 25 Z9 27 U1 1 U2 23 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 JUN PY 2011 VL 60 IS 3 BP 629 EP 637 PG 9 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 783GZ UT WOS:000292070800001 ER PT J AU Luebert, F Brokamp, G Wen, J Weigend, M Hilger, HH AF Luebert, Federico Brokamp, Grischa Wen, Jun Weigend, Maximilian Hilger, Hartmut H. TI Phylogenetic relationships and morphological diversity in Neotropical Heliotropium (Heliotropiaceae) SO TAXON LA English DT Article DE Andes; Boraginaceae; Boraginales; Heliotropiaceae; Heliotropium; morphological diversity ID CHLOROPLAST DNA; SEQUENCE DATA; CENTRARCHID FISHES; EVOLUTIONARY TREES; DIVERSIFICATION; BORAGINACEAE; RATES; INFERENCE; TOURNEFORTIA; PATTERNS AB Little is known about vegetative morphological diversification in Neotropical plant clades in comparison with diversification of reproductive characters. Phylogenetic relationships of the Neotropical Heliotropium (Heliotropiaceae) were studied using sequences of nrITS and four plastid regions (trnL-trnF, trnS-trnG, trnH-psbA, rps16). Vegetative morphological diversity (leaf morphology, habit), measured as amount of morphospace occupied and as variance of individual characters, was compared among the clades resolved and between groups of species inhabiting dry and humid areas. Three well-supported clades were recovered: (1) Heliotropium sect. Heliothamnus from the tropical Andes; (2)Heliotropium sect. Cochranea from the Peruvian and the Atacama Deserts; and (3) the Tournefortia clade, comprising the remaining American sections of Heliotropium and the mainly Neotropical Tournefortia sect. Tournefortia. Phylogenetic discordance detected between the plastid and nuclear partitions may have been due to lineage sorting, hybridization or differences in number of informative sites. Morphological diversity was largest in the Tournefortia clade and tended to be greater in dry than in humid areas, but without statistical support. Heliotropium sect. Cochranea was as diverse as the Tournefortia clade in leaf morphology and may have experienced adaptive radiation in the Atacama Desert. Lowest vegetative diversity was found in Heliotropium sect. Heliothamnus. The infrageneric delimitation in Heliotropium needs reassessment. C1 [Luebert, Federico; Brokamp, Grischa; Weigend, Maximilian; Hilger, Hartmut H.] Free Univ Berlin, Inst Biol Bot, D-14195 Berlin, Germany. [Luebert, Federico] Univ Chile, Fac Ciencias Forestales, Dept Silvicultura, Santiago, Chile. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Luebert, F (reprint author), Free Univ Berlin, Inst Biol Bot, Altensteinstr 6, D-14195 Berlin, Germany. EM f.luebert@fu-berlin.de RI Luebert, Federico/I-3246-2012; Weigend, Maximilian/F-7989-2014 OI Luebert, Federico/0000-0003-2251-4056; Weigend, Maximilian/0000-0003-0813-6650 FU NSF [DEB 0415573253]; CESAF (Chile); Fondecyt [11085016]; Smithsonian Institution, U.S. National Museum of Natural History; German Academic Exchange Service (DAAD); European Community Research Infrastructure Action [GB-TAF-4514, ES-TAF-136] FX The authors thank M. Antonissen, C. Becker, R. Gajardo, N. Garcia, L. Kritzner, M. Nee and R. Torres for field assistance, S. Teillier, M.O. Dillon and M. Ackermann for plant material and comments, T. Henning for help with Figure 1, P. Pliscoff for obtaining the values of aridity for the species in GIS, L. Bennett and B. Proppe for help at the High Performance Computing of the FU Berlin, and the curators of the herbaria A, AAU, B, BM, BSB, CONC, DR, EIF, F, G, OH, K, LL, M, MA, MO, NY, QCA, SGO, TEX, ULS, US, USM for permitting access to their collections. Fieldwork was supported by the NSF grant DEB 0415573253 (to M.O. Dillon and J. Wen), CESAF (Chile) and Fondecyt grant 11085016 to A. Moreira-Munoz. FL acknowledges the support of a Smithsonian Institution Visiting Scholar Award at the U.S. National Museum of Natural History, and the German Academic Exchange Service (DAAD). This research received support from the SYNTHESYS project, which is financed by European Community Research Infrastructure Action under the FP6 "Structuring the European Research Area" (grant GB-TAF-4514) and the FP7 "Capacities" (grant ES-TAF-136) Programmes. The valuable suggestions of Kathleen Kron, Michael Frohlich and two anonymous reviewers are gratefully acknowledged. NR 142 TC 23 Z9 24 U1 1 U2 10 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD JUN PY 2011 VL 60 IS 3 BP 663 EP 680 PG 18 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 783GZ UT WOS:000292070800004 ER PT J AU Bacon, CD Allan, GJ Zimmer, EA Wagner, WL AF Bacon, Christine D. Allan, Gerard J. Zimmer, Elizabeth A. Wagner, Warren L. TI Genome scans reveal high levels of gene flow in Hawaiian Pittosporum SO TAXON LA English DT Article DE AFLP; gene flow; Hawaiian Islands; hybridization; Pittosporum ID MULTILOCUS GENOTYPE DATA; PHYLOGENETIC INFERENCE; SYMPATRIC SPECIATION; DOMINANT MARKERS; ISLAND PLANTS; RADIATION; HYBRIDIZATION; POPULATION; EVOLUTION; DIVERGENCE AB Species radiations in the Hawaiian Islands have resulted in closely related yet morphologically and often ecologically distinct species, many of which have highly restricted distributions. Eleven species of Pittosporum (Pittosporaceae) are recognized in the Hawaiian Islands, yet it remains unclear whether the morphological variation within Hawaiian Pittosporum is due to hybridization, genetic polymorphism, phenotypic plasticity, or some combination of these processes. In this study of Hawaiian Pittosporum we used a genome-wide approach employing 626 Amplified Fragment Length Polymorphisms (AFLPs) to test species boundaries and elucidate gene flow within and among species. Parsimony trees were constructed to identify clades of individuals that correspond to species, island affinity, and/or sexual system. Network analysis was used to identify the number of lineages in the dataset; results showed a lack of resolution due to reticulation. Based on Bayesian assignment tests, Hawaiian Pittosporum exhibited high levels of gene flow. The interspecific allelic exchange and reticulation caused non-hierarchical relationships between species and a lack of reproductive isolation rendered species boundaries permeable. This study highlights the impact of hybridization on species persistence and conservation as well as on general patterns of Hawaiian biota. C1 [Bacon, Christine D.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Allan, Gerard J.] No Arizona Univ, Dept Biol Sci, Environm Genet Genom Lab, Flagstaff, AZ 86011 USA. [Zimmer, Elizabeth A.; Wagner, Warren L.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Bacon, CD (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. EM cbacon@rams.colostate.edu FU Smithsonian Pre-Doctoral Fellowship; National Tropical Botanical Garden McBryde Graduate Fellowship; Smithsonian Post-Doctoral fellowship; Smithsonian Scholarly Studies Program FX The authors thank David Erickson for advice on preparing samples for AFLP profiling, W. Chris Funk, Andrew Kanarak, and Patrick Reeves for analytical assistance, and Angelica Cibrian-Jaramillo, Mark Simmons, P.J. Garnock-Jones and one anonymous reviewer for comments on the manuscript. Funding for this study was provided by a Smithsonian Pre-Doctoral Fellowship and the National Tropical Botanical Garden McBryde Graduate Fellowship to CDB, a Smithsonian Post-Doctoral fellowship to GJA, and a Smithsonian Scholarly Studies Program Grant to EAZ and WLW. NR 73 TC 6 Z9 6 U1 0 U2 32 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 JUN PY 2011 VL 60 IS 3 BP 733 EP 741 PG 9 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 783GZ UT WOS:000292070800009 ER PT J AU Deutsch, J AF Deutsch, James TI Pictures from a Drawer: Prison and the Art of Portraiture SO WESTERN FOLKLORE LA English DT Book Review C1 [Deutsch, James] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, J (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 8 TC 0 Z9 0 U1 0 U2 2 PU CALIFORNIA FOLKLORE SOC PI POMONA PA WESTERN FOLKLORE DEPT OF ENGL/FOREIGN LANGUAGES 3801 W.TEMPLE AVENUE, POMONA, CA 91768-4010 USA SN 0043-373X J9 WESTERN FOLKLORE JI West. Folk. PD SUM-FAL PY 2011 VL 70 IS 3-4 BP 390 EP 392 PG 3 WC Folklore SC Arts & Humanities - Other Topics GA 955VX UT WOS:000305050100016 ER PT J AU Agueros, MA Posselt, B Anderson, SF Rosenfield, P Haberl, F Homer, L Margon, B Newsom, ER Voges, W AF Agueeros, Marcel A. Posselt, Bettina Anderson, Scott F. Rosenfield, Philip Haberl, Frank Homer, Lee Margon, Bruce Newsom, Emily R. Voges, Wolfgang TI NO CONFIRMED NEW ISOLATED NEUTRON STARS IN THE SDSS DATA RELEASE 4 SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: neutron ID DIGITAL SKY SURVEY; ROSAT ALL-SKY; BRIGHT SOURCE CATALOG; MEDIUM-SENSITIVITY SURVEY; ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; X-RAY SOURCES; XMM-NEWTON; OPTICAL IDENTIFICATIONS; 1RXS J141256.0+792204 AB We report on follow-up observations of candidate X-ray-bright, radio-quiet isolated neutron stars (INSs) identified from correlations of the ROSAT All-Sky Survey (RASS) and the Sloan Digital Sky Survey (SDSS) Data Release 4 in Agueros et al. We obtained Chandra X-ray Observatory exposures for 13 candidates in order to pinpoint the source of X-ray emission in optically blank RASS error circles. These observations eliminated 12 targets as good INS candidates. We discuss subsequent observations of the remaining candidate with XMM-Newton, the Gemini North Observatory, and the Apache Point Observatory. We identify this object as a likely extragalactic source with an unusually high log (f(X)/f(opt)) similar to 2.4. We also use an updated version of the population synthesis models of Popov et al. to estimate the number of RASS-detected INSs in the SDSS Data Release 7 footprint. We find that these models predict similar to 3-4 INSs in the 11,000 deg(2) imaged by SDSS, which is consistent with the number of known INSs that fall within the survey footprint. In addition, our analysis of the four new INS candidates identified in the SDSS footprint implies that they are unlikely to be confirmed as INSs; together, these results suggest that new INSs are not likely to be found from further correlations of the RASS and SDSS. C1 [Agueeros, Marcel A.; Newsom, Emily R.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Posselt, Bettina] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Anderson, Scott F.; Rosenfield, Philip; Homer, Lee] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Haberl, Frank; Voges, Wolfgang] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Margon, Bruce] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Agueros, MA (reprint author), Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA. EM marcel@astro.columbia.edu RI Margon, Bruce/B-5913-2012; Agueros, Marcel/K-7998-2014; OI Agueros, Marcel/0000-0001-7077-3664; Haberl, Frank/0000-0002-0107-5237; Rosenfield, Philip/0000-0001-9306-6049; Posselt, Bettina/0000-0003-2317-9747 FU NSF [AST-0602099]; Deutsche Akademie der Naturforscher Leopoldina (Halle, Germany) [BMBF-LPD 9901/8-170]; Chandra [GO6-7058X]; NASA [NNX07AO59A]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX M.A.A. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0602099. B. P. acknowledges the support of the Deutsche Akademie der Naturforscher Leopoldina (Halle, Germany) under grant BMBF-LPD 9901/8-170. We gratefully acknowledge Chandra grant GO6-7058X and NASA award NNX07AO59A for support of portions of our program. We thank Sergei Popov and Pavel Boldin, who helped develop the population synthesis model used in this work, and Jose Pons and his collaborators for providing cooling curves for the population synthesis calculations. We thank Tom Matheson, Dara Norman, and Anil Seth for their help with the Gemini data, Michael Strauss and Chris Beaumont for their help reconstructing the SDSS footprint, and Paul Green for useful discussions about 1RXS J1406. We thank the referee for suggestions that improved the manuscript.; 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 51 TC 3 Z9 3 U1 0 U2 3 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 JUN PY 2011 VL 141 IS 6 AR 176 DI 10.1088/0004-6256/141/6/176 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 762YQ UT WOS:000290518500003 ER PT J AU Bieryla, A Parker, JW Young, EF McFadden, LA Russell, CT Stern, SA Sykes, MV Gladman, B AF Bieryla, A. Parker, J. Wm. Young, E. F. McFadden, L. A. Russell, C. T. Stern, S. A. Sykes, M. V. Gladman, B. TI A SEARCH FOR SATELLITES AROUND CERES SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids: individual (1 Ceres) ID SHAPE; HST AB We conducted a satellite search around the dwarf planet 1 Ceres using Hubble Space Telescope and ground-based Palomar data. No candidate objects were found orbiting Ceres in its entire stability region down to similar to 500 km from the surface of Ceres. Assuming a satellite would have the same albedo as Ceres, which has a visual geometric albedo of 0.07-0.10, our detection limit is sensitive to satellites larger than 1-2 km in diameter. C1 [Bieryla, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bieryla, A.; Parker, J. Wm.; Young, E. F.; Stern, S. A.] SW Res Inst, Boulder, CO 80302 USA. [McFadden, L. A.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Sykes, M. V.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Gladman, B.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Bieryla, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 6, Cambridge, MA 02138 USA. EM abieryla@cfa.harvard.edu RI Russell, Christopher/E-7745-2012; McFadden, Lucy-Ann/I-4902-2013 OI Russell, Christopher/0000-0003-1639-8298; McFadden, Lucy-Ann/0000-0002-0537-9975 FU STScI [HST-GO-09748] FX This work was supported by the HST grant from STScI (HST-GO-09748). We thank Jake Hanson for his help on the occultation analysis. NR 8 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2011 VL 141 IS 6 AR 197 DI 10.1088/0004-6256/141/6/197 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 762YQ UT WOS:000290518500024 ER PT J AU Chan, T Ingemyr, M Winn, JN Holman, MJ Sanchis-Ojeda, R Esquerdo, G Everett, M AF Chan, Tucker Ingemyr, Mikael Winn, Joshua N. Holman, Matthew J. Sanchis-Ojeda, Roberto Esquerdo, Gil Everett, Mark TI THE TRANSIT LIGHT-CURVE PROJECT. XIV. CONFIRMATION OF ANOMALOUS RADII FOR THE EXOPLANETS TrES-4b, HAT-P-3b, AND WASP-12b SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (TrES-4, HAT-P-3, WASP-12) ID OHMIC DISSIPATION; PLANET SYSTEMS; HOT JUPITERS; STELLAR; PARAMETERS; ATMOSPHERE; MODELS AB We present transit photometry of three exoplanets, TrES-4b, HAT-P-3b, and WASP-12b, allowing for refined estimates of the systems' parameters. TrES-4b and WASP-12b were confirmed to be "bloated" planets, with radii of 1.706 +/- 0.056R(Jup) and 1.736 +/- 0.092R(Jup), respectively. These planets are too large to be explained with standard models of gas giant planets. In contrast, HAT-P-3b has a radius of 0.827 +/- 0.055R(Jup), smaller than a pure hydrogen-helium planet and indicative of a highly metal-enriched composition. Analyses of the transit timings revealed no significant departures from strict periodicity. For TrES-4, our relatively recent observations allow for improvement in the orbital ephemerides, which is useful for planning future observations. C1 [Chan, Tucker; Ingemyr, Mikael; Winn, Joshua N.; Sanchis-Ojeda, Roberto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Ingemyr, Mikael] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Ingemyr, Mikael] Ctr Excellence Educ, Res Sci Inst, Mclean, VA 22102 USA. [Holman, Matthew J.; Esquerdo, Gil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Everett, Mark] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Chan, T (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Sanchis-Ojeda, Roberto/B-6574-2013 OI Sanchis-Ojeda, Roberto/0000-0002-6193-972X FU NASA [NNX09AB33G]; Research Science Institute, Center for Excellence in Education FX We gratefully acknowledge support from the NASA Origins program through award NNX09AB33G and from the Research Science Institute, a program of the Center for Excellence in Education. Some of the data presented herein were obtained with the Nordic Optical Telescope (NOT), jointly operated on the island of La Palma by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos Instituto Astrofisica de Canarias, and ALFOSC, which is owned by the Instituto Astrofisica de Andalucia (IAA) and operated at the NOT under agreement between IAA and NBlfAFG of the Astronomical Observatory of Copenhagen. NR 29 TC 37 Z9 37 U1 1 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 JUN PY 2011 VL 141 IS 6 AR 179 DI 10.1088/0004-6256/141/6/179 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 762YQ UT WOS:000290518500006 ER PT J AU McCleary, JE Wolk, SJ AF McCleary, J. E. Wolk, S. J. TI A SURVEY OF HIGH-CONTRAST STELLAR FLARES OBSERVED BY CHANDRA SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: activity; stars: flare; stars: pre-main sequence; stars: protostars; X-rays: stars ID X-RAY FLARES; ORION NEBULA CLUSTER; LOW-MASS STARS; YOUNG STARS; ROTATIONAL MODULATION; SPITZER OBSERVATIONS; EXTREME-ULTRAVIOLET; EMBEDDED-CLUSTER; INFRARED CLUSTER; FLARING LOOPS AB The X-ray light curves of pre-main-sequence (PMS) stars can show variability in the form of flares altering a baseline characteristic activity level; the largest X-ray flares are characterized by a rapid rise to more than 10 times the characteristic count rate, followed by a slower quasi-exponential decay. Analysis of these high-contrast X-ray flares enables the study of the innermost magnetic fields of PMS stars. We have scanned the ANCHORS database of Chandra observations of star-forming regions to extend the study of flare events on PMS stars both in sky coverage and in volume. We developed a sample of 30 high-contrast flares out of the 14,000 stars of various ages and masses available in ANCHORS at the start of our study. Applying methods of time-resolved spectral analysis, we obtain the temperatures, confining magnetic field strengths, and loop lengths of these bright, energetic flares. The results of the flare analysis are compared to the Two Micron All Sky Survey and Spitzer data available for the stars in our sample. We find that the longest flare loop lengths (of order several stellar radii) are only seen on stars whose IR data indicates the presence of disks. This suggests that the longest flares may stretch all the way to the disk. Such long flares tend to be more tenuous than the other large flares studied. A wide range of loop lengths are observed, indicating that different types of flares may occur on disked young stellar objects. C1 [McCleary, J. E.; Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McCleary, JE (reprint author), New Mexico State Univ, Dept Astron, POB 30001,MSC 4500, Las Cruces, NM 88003 USA. EM mccleary@nmsu.edu OI Wolk, Scott/0000-0002-0826-9261 FU National Aeronautics and Space Administration; National Science Foundation; CXC guest investigator program [AR7-8003A]; NASA [NAS8-03060] FX The authors gratefully acknowledge many useful comments from the anonymous referee as well as the assistance of Ettore Flaccomio with X-ray data reduction and the assistance of Robert Gutermuth in sharing IRAC and MIPS data for the sources in our sample. 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, funded by the National Aeronautics and Space Administration and the National Science Foundation. J.E.M. was supported by the CXC guest investigator program through grant AR7-8003A. S.J.W. was supported by NASA contract NAS8-03060. NR 65 TC 5 Z9 5 U1 1 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 JUN PY 2011 VL 141 IS 6 AR 201 DI 10.1088/0004-6256/141/6/201 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 762YQ UT WOS:000290518500028 ER PT J AU Frankham, R Ballou, JD Eldridge, MDB Lacy, RC Ralls, K Dudash, MR Fenster, CB AF Frankham, Richard Ballou, Jonathan D. Eldridge, Mark D. B. Lacy, Robert C. Ralls, Katherine Dudash, Michele R. Fenster, Charles B. TI Predicting the Probability of Outbreeding Depression SO CONSERVATION BIOLOGY LA English DT Article DE adaptive differentiation; chromosomes; effective population size; genetic diversity; genetic rescue; habitat fragmentation; outbreeding depression; polyploid ID DEPENDENT POSTMATING ISOLATION; REPRODUCTIVE ISOLATION; PINK SALMON; CHAMAECRISTA-FASCICULATA; SYMPATRIC STICKLEBACKS; PHENOTYPIC DIVERGENCE; GENETIC CONSEQUENCES; LOCAL ADAPTATION; POPULATIONS; SPECIATION AB Fragmentation of animal and plant populations typically leads to genetic erosion and increased probability of extirpation. Although these effects can usually be reversed by re-establishing gene flow between population fragments, managers sometimes fail to do so due to fears of outbreeding depression (OD). Rapid development of OD is due primarily to adaptive differentiation from selection or fixation of chromosomal variants. Fixed chromosomal variants can be detected empirically. We used an extended form of the breeders' equation to predict the probability of OD due to adaptive differentiation between recently isolated population fragments as a function of intensity of selection, genetic diversity, effective population sizes, and generations of isolation. Empirical data indicated that populations in similar environments had not developed OD even after thousands of generations of isolation. To predict the probability of OD, we developed a decision tree that was based on the four variables from the breeders' equation, taxonomic status, and gene flow within the last 500 years. The predicted probability of OD in crosses between two populations is elevated when the populations have at least one of the following characteristics: are distinct species, have fixed chromosomal differences, exchanged no genes in the last 500 years, or inhabit different environments. Conversely, the predicted probability of OD in crosses between two populations of the same species is low for populations with the same karyotype, isolated for < 500 years, and that occupy similar environments. In the former case, we recommend crossing be avoided or tried on a limited, experimental basis. In the latter case, crossing can be carried out with low probability of OD. We used crosses with known results to test the decision tree and found that it correctly identified cases where OD occurred. Current concerns about OD in recently fragmented populations are almost certainly excessive. C1 [Frankham, Richard] Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. [Frankham, Richard; Eldridge, Mark D. B.] Australian Museum, Sydney, NSW 2010, Australia. [Ballou, Jonathan D.; Ralls, Katherine] Smithsonian Inst, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Lacy, Robert C.] Chicago Zool Soc, Brookfield, IL 60513 USA. [Dudash, Michele R.; Fenster, Charles B.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Frankham, R (reprint author), Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. EM richard.frankham@mq.edu.au NR 89 TC 195 Z9 200 U1 22 U2 210 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD JUN PY 2011 VL 25 IS 3 BP 465 EP 475 DI 10.1111/j.1523-1739.2011.01662.x PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 762PK UT WOS:000290491700009 PM 21486369 ER PT J AU Morrow, KM Paul, VJ Liles, MR Chadwick, NE AF Morrow, K. M. Paul, V. J. Liles, M. R. Chadwick, N. E. TI Allelochemicals produced by Caribbean macroalgae and cyanobacteria have species-specific effects on reef coral microorganisms SO CORAL REEFS LA English DT Article DE Antimicrobial; Bacteria; Competition; Coral-algal interaction; Phase-shift ID PATHOGEN VIBRIO-SHILOI; SECONDARY METABOLITES; ANTIMICROBIAL ACTIVITIES; CHEMICAL DEFENSES; MARINE PATHOGENS; BAND DISEASE; BACTERIA; ALGAE; PLANTS; PSEUDOALTEROMONAS AB Coral populations have precipitously declined on Caribbean reefs while algal abundance has increased, leading to enhanced competitive damage to corals, which likely is mediated by the potent allelochemicals produced by both macroalgae and benthic cyanobacteria. Allelochemicals may affect the composition and abundance of coral-associated microorganisms that control host responses and adaptations to environmental change, including susceptibility to bacterial diseases. Here, we demonstrate that extracts of six Caribbean macroalgae and two benthic cyanobacteria have both inhibitory and stimulatory effects on bacterial taxa cultured from the surfaces of Caribbean corals, macroalgae, and corals exposed to macroalgal extracts. The growth of 54 bacterial isolates was monitored in the presence of lipophilic and hydrophilic crude extracts derived from Caribbean macroalgae and cyanobacteria using 96-well plate bioassays. All 54 bacterial cultures were identified by ribotyping. Lipophilic extracts from two species of Dictyota brown algae inhibited > 50% of the reef coral bacteria assayed, and hydrophilic compounds from Dictyota menstrualis particularly inhibited Vibrio bacteria, a genus associated with several coral diseases. In contrast, both lipo- and hydrophilic extracts from 2 species of Lyngbya cyanobacteria strongly stimulated bacterial growth. The brown alga Lobophora variegata produced hydrophilic compounds with broad-spectrum antibacterial effects, which inhibited 93% of the bacterial cultures. Furthermore, bacteria cultured from different locations (corals vs. macroalgae vs. coral surfaces exposed to macroalgal extracts) responded differently to algal extracts. These results reveal that extracts from macroalgae and cyanobacteria have species-specific effects on the composition of coral-microbial assemblages, which in turn may increase coral host susceptibility to disease and result in coral mortality. C1 [Morrow, K. M.; Liles, M. R.; Chadwick, N. E.] Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. [Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Morrow, KM (reprint author), Auburn Univ, Dept Biol Sci, 101 Rouse Life Sci Bldg, Auburn, AL 36849 USA. EM morrokm@auburn.edu RI Chadwick, Nanette/F-8076-2013 FU National Oceanic and Atmospheric Administration; NOAA [NA05NOS4781194]; Mote Marine Laboratory [POR 2007-30]; Smithsonian Marine Science Network; Puerto Rico Sea Grant [R-101-1-08] FX We thank the Florida Keys National Marine Sanctuary for granting collection and research permits (FKNMS-2008-019) and the Belize Fisheries Department for permits to collect coral mucus samples. The Harbor Branch Oceanographic Institute at Florida Atlantic University Center for Marine Biomedical and Biotechnology Research, Mote Marine Laboratory, University of the Virgin Islands MacLean Marine Science Center, and the Smithsonian Marine Station at Fort Pierce and the Smithsonian's Carrie Bow Cay Field Station all provided invaluable logistical support. E. A. Guzman, A. Moss and R Ritson-Williams provided field and laboratory assistance. This work was supported by a National Oceanic and Atmospheric Administration National Marine Sanctuary Program Nancy Foster Scholarship to KMM, NOAA's ECOHAB program project NA05NOS4781194 (VJP), a Mote Marine Laboratory Protect our Reefs grant award POR 2007-30 (VJP), the Smithsonian Marine Science Network, and a Puerto Rico Sea Grant R-101-1-08 (NEC). This is contribution #846 of the Smithsonian Marine Station at Fort Pierce, contribution #900 of the Caribbean Coral Reef Ecosystems Program, and contribution #80 of the Auburn University Marine Biology Program. NR 71 TC 31 Z9 35 U1 2 U2 53 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD JUN PY 2011 VL 30 IS 2 BP 309 EP 320 DI 10.1007/s00338-011-0747-1 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 760LY UT WOS:000290327000004 ER PT J AU Brenes-Arguedas, T Roddy, AB Coley, PD Kursar, TA AF Brenes-Arguedas, T. Roddy, A. B. Coley, P. D. Kursar, Thomas A. TI Do differences in understory light contribute to species distributions along a tropical rainfall gradient? SO OECOLOGIA LA English DT Article DE Panama; Shade tolerance; Drought tolerance; Tropical dry forest; Tropical wet forest ID DRY FOREST; TRADE-OFFS; SHADE TOLERANCE; TREE SEEDLINGS; NICHE DIFFERENTIATION; CLIMATIC GRADIENT; RANGE LIMITS; GROWTH; PERFORMANCE; DROUGHT AB In tropical forests, regional differences in annual rainfall correlate with differences in plant species composition. Although water availability is clearly one factor determining species distribution, other environmental variables that covary with rainfall may contribute to distributions. One such variable is light availability in the understory, which decreases towards wetter forests due to differences in canopy density and phenology. We established common garden experiments in three sites along a rainfall gradient across the Isthmus of Panama in order to measure the differences in understory light availability, and to evaluate their influence on the performance of 24 shade-tolerant species with contrasting distributions. Within sites, the effect of understory light availability on species performance depended strongly on water availability. When water was not limiting, either naturally in the wetter site or through water supplementation in drier sites, seedling performance improved at higher light. In contrast, when water was limiting at the drier sites, seedling performance was reduced at higher light, presumably due to an increase in water stress that affected mostly wet-distribution species. Although wetter forest understories were on average darker, wet-distribution species were not more shade-tolerant than dry-distribution species. Instead, wet-distribution species had higher absolute growth rates and, when water was not limiting, were better able to take advantage of small increases in light than dry-distribution species. Our results suggest that in wet forests the ability to grow fast during temporary increases in light may be a key trait for successful recruitment. The slower growth rates of the dry-distribution species, possibly due to trade-offs associated with greater drought tolerance, may exclude these species from wetter forests. C1 [Coley, P. D.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Brenes-Arguedas, T.; Roddy, A. B.; Coley, P. D.; Kursar, Thomas A.] Smithsonian Trop Res Inst, Ancon, Panama. RP Kursar, TA (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. EM kursar@biology.utah.edu RI Roddy, Adam/M-4523-2013 OI Roddy, Adam/0000-0002-4423-8729 FU National Science Foundation [DEB-0444590]; The Peregrine Fund FX Funding was provided by the National Science Foundation grant DEB-0444590 to T.A.K. and P.D.C. We thank Cecilia Blundo, Marcos Rios, Gonzalo Rivas, Natalia Anaya, and Lissette Jimenez who conducted the fieldwork; Salomon Aguilar and Rolando Perez helped with species identification. We thank the Smithsonian Tropical Research Institute's Environmental Monitoring Program and the Autoridad del Canal de Panama for making climate data publicly available; similarly the Center for Tropical Forest Science, the Missouri Botanical Gardens and InBio made species information, herbarium and distribution maps available. We thank T. Paine and an anonymous reviewer for valuable comments on the manuscript. The Peregrine Fund kindly allowed us access to Gunn Hill. The Smithsonian Tropical Research Institute provided logistical support and research facilities. All work was done in compliance with the laws of Panama and the Autoridad Nacional del Ambiente. Open access to this article was provided by the Berkeley Research Impact Initiative of the University of California-Berkeley. NR 64 TC 19 Z9 20 U1 2 U2 48 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUN PY 2011 VL 166 IS 2 BP 443 EP 456 DI 10.1007/s00442-010-1832-9 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 763VK UT WOS:000290587600015 PM 21120671 ER PT J AU Salk, CF McMahon, SM AF Salk, Carl F. McMahon, Sean M. TI Ecological and environmental factors constrain sprouting ability in tropical trees SO OECOLOGIA LA English DT Article DE Functional traits; Disturbance; Damage; Panama; Prorena ID RESPROUTING ABILITY; NUTRIENT CONTENT; PUERTO-RICO; FOREST; REGENERATION; TRAITS; WET; HABITATS; GROWTH; PANAMA AB Most theories of forest biodiversity focus on the role of seed dispersal and seedling establishment in forest regeneration. In many ecosystems, however, sprouting by damaged stems determines which species occupies a site. Damaged trees can quickly recover from disturbance and out-compete seedlings. Links among species' traits, environmental conditions and sprouting could offer insight into species' resilience to changes in climate, land use, and disturbance. Using data for 25 Neotropical tree species at two sites with contrasting rainfall and soil, we tested hypotheses on how four functional traits (seed mass, leaf mass per area, wood density and nitrogen fixation) influence species' sprouting responses to disturbance and how these relationships are mediated by a tree's environmental context. Most species sprouted in response to cutting, and many species' sprouting rates differed significantly between sites. Individual traits showed no direct correlation with sprouting. However, interactions among traits and site variables did affect sprouting rates. Many species showed increased sprouting in the higher-quality site. Most nitrogen-fixing species showed the opposite trend, sprouting more frequently where resources are scarce. This study highlights the use of functional traits as a proxy for life histories, and demonstrates the importance of environmental effects on demography. C1 [Salk, Carl F.] Duke Univ, Dept Biol, Durham, NC 27708 USA. [McMahon, Sean M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Salk, CF (reprint author), Duke Univ, Dept Biol, Durham, NC 27708 USA. EM cfs14@duke.edu OI Salk, Carl/0000-0003-2833-8292 FU HSBC Bank's Climate Partnership; Smithsonian Tropical Research Institute's Center for Tropical Forest Science FX We would like to thank Dylan Craven, Jeff Hall and Emilio Mariscal for facilitating field work and access to PRO-RENA plantations. Jessica Metcalf, James Justus, Peter Vesk and several anonymous reviewers provided helpful comments. Funding for SMM was partially provided by HSBC Bank's Climate Partnership and the Smithsonian Tropical Research Institute's Center for Tropical Forest Science. All work described in this paper complies with Panamanian law. NR 28 TC 6 Z9 6 U1 2 U2 17 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUN PY 2011 VL 166 IS 2 BP 485 EP 492 DI 10.1007/s00442-010-1850-7 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 763VK UT WOS:000290587600018 PM 21116651 ER PT J AU Morrison, CL Ross, SW Nizinski, MS Brooke, S Jarnegren, J Waller, RG Johnson, RL King, TL AF Morrison, Cheryl L. Ross, Steve W. Nizinski, Martha S. Brooke, Sandra Jaernegren, Johanna Waller, Rhian G. Johnson, Robin L. King, Tim L. TI Genetic discontinuity among regional populations of Lophelia pertusa in the North Atlantic Ocean SO CONSERVATION GENETICS LA English DT Article DE Cold-water coral; Connectivity; Gene flow; Dispersal barriers; Isolation by distance ID GULF-OF-MEXICO; MULTILOCUS GENOTYPE DATA; DEEP-SEA CORAL; REEF-BUILDING CORALS; MARINE POPULATIONS; LINNAEUS 1758; MICROSATELLITE LOCI; ALLELE FREQUENCIES; LARVAL DISPERSAL; SELF-RECRUITMENT AB Knowledge of the degree to which populations are connected through larval dispersal is imperative to effective management, yet little is known about larval dispersal ability or population connectivity in Lophelia pertusa, the dominant framework-forming coral on the continental slope in the North Atlantic Ocean. Using nine microsatellite DNA markers, we assessed the spatial scale and pattern of genetic connectivity across a large portion of the range of L. pertusa in the North Atlantic Ocean. A Bayesian modeling approach found four distinct genetic groupings corresponding to ocean regions: Gulf of Mexico, coastal southeastern U.S., New England Seamounts, and eastern North Atlantic Ocean. An isolation-by-distance pattern was supported across the study area. Estimates of pairwise population differentiation were greatest with the deepest populations, the New England Seamounts (average F (ST) = 0.156). Differentiation was intermediate with the eastern North Atlantic populations (F (ST) = 0.085), and smallest between southeastern U.S. and Gulf of Mexico populations (F (ST) = 0.019), with evidence of admixture off the southeastern Florida peninsula. Connectivity across larger geographic distances within regions suggests that some larvae are broadly dispersed. Heterozygote deficiencies were detected within the majority of localities suggesting deviation from random mating. Gene flow between ocean regions appears restricted, thus, the most effective management scheme for L. pertusa involves regional reserve networks. C1 [Morrison, Cheryl L.; Johnson, Robin L.; King, Tim L.] US Geol Survey, Leetown Sci Ctr, Aquat Ecol Branch, Biol Resources Div, Kearneysville, WV 25430 USA. [Ross, Steve W.] UNC Wilmington, Ctr Marine Sci, Wilmington, NC 28409 USA. [Nizinski, Martha S.] Smithsonian Inst, NHB, NMFS Natl Systemat Lab, Washington, DC 20013 USA. [Brooke, Sandra] Marine Conservat Biol Inst, Bellevue, WA 98004 USA. [Jaernegren, Johanna] Norwegian Inst Nat Res, N-7485 Trondheim, Norway. [Waller, Rhian G.] Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA. RP Morrison, CL (reprint author), US Geol Survey, Leetown Sci Ctr, Aquat Ecol Branch, Biol Resources Div, 11649 Leetown Rd, Kearneysville, WV 25430 USA. EM cmorrison@usgs.gov FU USGS; Minerals Management Service; SEUS [DASS2005]; Duke/UNC Oceanographic Consortium (to SWR); Statoil Hydro; Norwegian Academy of Science and Letters; USGS-BRD Leetown Science Center, Aquatic Ecology Branch FX This investigation was financially supported by the USGS Outer Continental Shelf Ecosystem Program and was sponsored by the Minerals Management Service. NOAA Office of Ocean Exploration supported field work both in the SEUS via four cruises (grants to S. W. Ross and S. Brooke, lead PIs) and also to the New England and Corner Rise Seamounts (cruise DASS2005, grant to L. Watling, T. Shank, S. France, R. Waller and P. Auster, lead PIs). Thanks to the ROV pilots and crew of the R/V Ronald H. Brown facilitating collection of the NES samples. The two R/V Cape Hatteras missions were sponsored by the Duke/UNC Oceanographic Consortium (to SWR), and we thank that ship's personnel for excellent support. We thank J.M. Roberts and G. Duineveld for facilitating cruise participation of SWR on R/V Pelagia where ENAO samples were collected. Norwegian collections were financially supported by Statoil Hydro and The Norwegian Academy of Science and Letters. Special thanks to USGS Lophelia I research colleagues: G. Brewer, C. Kellogg, K. Sulak and the crew at the USGS Coastal Ecology and Conservation Research. We also thank the Continental Shelf Associates Lophelia I scientists for allowing an author (CLM) to participate on GOM cruises. The USGS-BRD Leetown Science Center, Aquatic Ecology Branch, provided partial funding to CLM. The following individuals kindly donated coral samples: E. Cordes, C. Fisher, W. Schroeder, A. Davies, J. Reed, C. Messing. Thanks are extended to the following individuals for helpful discussions regarding data collection and analyses: M. Eackles, B. Lubinski, C. Young, and J. Switzer. Harbor Branch Oceanographic Institution, the crew members of the R/V Seward Johnson I and II, and the JSL submersible crew helped make this research possible. M. Carlson produced maps and calculated geographic distances. M. Rhode and M. Springmann assisted with Figs 1 and 2, respectively. Comments by J. Switzer, M. Miller and 3 anonymous reviewers improved the manuscript. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U. S. Government. NR 96 TC 28 Z9 28 U1 1 U2 31 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 JUN PY 2011 VL 12 IS 3 BP 713 EP 729 DI 10.1007/s10592-010-0178-5 PG 17 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 760IY UT WOS:000290319200011 ER PT J AU Angelier, F Ballentine, B Holberton, RL Marra, PP Greenberg, R AF Angelier, F. Ballentine, B. Holberton, R. L. Marra, P. P. Greenberg, R. TI What drives variation in the corticosterone stress response between subspecies? A common garden experiment of swamp sparrows (Melospiza georgiana) SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE corticosterone; development; moult; selection; stress response ID BASE-LINE CORTICOSTERONE; ADRENOCORTICAL-RESPONSE; REPRODUCTIVE SUCCESS; CIRCULATING CORTICOSTERONE; MORPHOLOGICAL ADAPTATION; SEASONAL-CHANGES; INDIVIDUAL RISK; MIGRATORY BIRD; ZEBRA FINCH; ZONOTRICHIA AB Although differences in the corticosterone stress response have frequently been reported between populations or closely related subspecies, their origin remains unclear. These differences may appear because individuals adjust their corticosterone stress response to the environmental conditions they are experiencing. However, they may also result from selection that has favoured individuals with specific corticosterone stress response or from environmental factors that have affected the development of the corticosterone stress response during early life. We investigated these hypotheses by studying the corticosterone stress response of two closely related subspecies of swamp sparrows (Melospiza sp.). We showed for the first time that two closely related subspecies can differ in their corticosterone stress response when raised at the laboratory and held in similar conditions for a year. Thus, we demonstrated that selection, developmental processes or a conjunction of both of these processes can account for variation in the stress response between closely related subspecies. C1 [Angelier, F.; Ballentine, B.; Marra, P. P.; Greenberg, R.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Angelier, F.] Univ Calif Davis, Dept Neurobiol Physiol & Behav, Davis, CA 95616 USA. [Ballentine, B.] Univ W Georgia, Dept Biol, Carrollton, GA USA. [Holberton, R. L.] Univ Maine, Lab Avian Biol, Dept Biol Sci, Orono, ME USA. RP Angelier, F (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM frederic_angelier@yahoo.fr FU FONZ; NSF [0649679]; Smithsonian Institution; IOF FX The project was funded by FONZ and a NSF grant (0649679) to P. P. M. and R. L. H. B. B. was supported by a Smithsonian Institution post-doctoral fellowship. F. A. was supported by a IOF Marie-Curie fellowship (Polarclimstress). We thank the Justin Bredlau and David Moore for their help in the field. We thank Sarah Warner for her generous support in Delaware. We thank the volunteers of the Friends of the National Zoo for the enormous help in hand-raising swamp sparrows. We especially thank Dan Rauch, volunteer coordinator, Anne Bissell, Tracy Brown, Glenn Court, Lee Hanley, and Gail Lewin for their dedication to this project. We thank the veterinarian staff at the National Zoo for their support during the course of this project. We thank the laboratory group and the Migratory Bird Center for help in the laboratory, especially J. Dowling and M. Thomas. NR 81 TC 13 Z9 13 U1 2 U2 30 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD JUN PY 2011 VL 24 IS 6 BP 1274 EP 1283 DI 10.1111/j.1420-9101.2011.02260.x PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 760GT UT WOS:000290313500012 PM 21443644 ER PT J AU Huijse, P Estevez, PA Zegers, P Principe, JC Protopapas, P AF Huijse, Pablo Estevez, Pablo A. Zegers, Pablo Principe, Jose C. Protopapas, Pavlos TI Period Estimation in Astronomical Time Series Using Slotted Correntropy SO IEEE SIGNAL PROCESSING LETTERS LA English DT Article DE Correntropy; information theory; spectral analysis; time series analysis; variable stars ID VARIABLE-STARS; SPACED DATA; PROJECT; PHASE AB In this letter, we propose a method for period estimation in light curves from periodic variable stars using correntropy. Light curves are astronomical time series of stellar brightness over time, and are characterized as being noisy and unevenly sampled. We propose to use slotted time lags in order to estimate correntropy directly from irregularly sampled time series. A new information theoretic metric is proposed for discriminating among the peaks of the correntropy spectral density. The slotted correntropy method outperformed slotted correlation, string length, VarTools (Lomb-Scargle periodogram and Analysis of Variance), and SigSpec applications on a set of light curves drawn from the MACHO survey. C1 [Huijse, Pablo; Estevez, Pablo A.] Univ Chile, Dept Elect Engn, Santiago, Chile. [Huijse, Pablo; Estevez, Pablo A.] Univ Chile, Adv Min Technol Ctr, Santiago, Chile. [Zegers, Pablo] Univ Los Andes, Coll Engn & Appl Sci, Santiago, Chile. [Principe, Jose C.] Univ Florida, Computat Neuroengn Lab, Gainesville, FL 32601 USA. [Protopapas, Pavlos] Sch Engn & Appl Sci, IACS, Cambridge, MA 02138 USA. [Protopapas, Pavlos] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Huijse, P (reprint author), Univ Chile, Dept Elect Engn, Santiago, Chile. EM phuijse@ing.uchile.cl; pestevez@cec.uchile.cl; pzegers@miuandes.cl; principe@cnel.ufl.edu; pprotopapas@cfa.harvard.edu RI Estevez, Pablo/A-9377-2008; Huijse, Pablo/J-4700-2015 OI Estevez, Pablo/0000-0001-9164-4722; Huijse, Pablo/0000-0003-3541-1697 FU CONICYT-CHILE [FONDECYT 1080643, 1110701]; Doctorate Scholarship program FX This work was supported by CONICYT-CHILE under Grants FONDECYT 1080643 and 1110701, and its Doctorate Scholarship program. The associate editor coordinating the review of this manuscript and approving it for publication was Dr. Alfred Mertins. NR 16 TC 11 Z9 11 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1070-9908 J9 IEEE SIGNAL PROC LET JI IEEE Signal Process. Lett. PD JUN PY 2011 VL 18 IS 6 BP 371 EP 374 DI 10.1109/LSP.2011.2141987 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA 754GF UT WOS:000289842300008 ER PT J AU Henry, AG Brooks, AS Piperno, DR AF Henry, Amanda G. Brooks, Alison S. Piperno, Dolores R. TI Reply to Collins and Copeland: Spontaneous gelatinization not supported by evidence SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter ID STARCH GRAINS C1 [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Balboa, Panama. [Henry, Amanda G.] Max Planck Inst Evolutionary Anthropol, Plant Foods & Hominin Dietary Ecol Res Grp, D-04103 Leipzig, Germany. [Brooks, Alison S.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. RP Piperno, DR (reprint author), Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. EM pipernod@si.edu OI Henry, Amanda/0000-0002-2923-4199 NR 6 TC 4 Z9 4 U1 0 U2 3 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 31 PY 2011 VL 108 IS 22 BP E146 EP E146 DI 10.1073/pnas.1104199108 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 770RM UT WOS:000291106200002 ER PT J AU Hershler, R Liu, HP AF Hershler, Robert Liu, Hsiu-Ping TI Comments on the paper "Is the track of the Yellowstone hotspot driven by a deep mantle plume? - Review of volcanism, faulting, and uplift in light of new data" by Kenneth Pierce and Lisa Morgan [J. Volcanol. Geotherm. Res. 188 (2009), 1-25] SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Editorial Material ID HYDROBIIDAE; PYRGULOPSIS; ANNELIDA C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Coll, Dept Biol, Denver, CO 80217 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. EM hershlerr@si.edu NR 8 TC 1 Z9 1 U1 2 U2 16 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD MAY 30 PY 2011 VL 202 IS 3-4 BP 262 EP 263 DI 10.1016/j.jvolgeores.2011.01.005 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 772OB UT WOS:000291242100008 ER PT J AU Su, M Yadav, APS Shimon, M Keating, BG AF Su, Meng Yadav, Amit P. S. Shimon, Meir Keating, Brian G. TI Impact of instrumental systematics on the CMB bispectrum SO PHYSICAL REVIEW D LA English DT Article ID PRE-LAUNCH STATUS; PRIMORDIAL NON-GAUSSIANITY; BACKGROUND POLARIZATION MEASUREMENTS; FAST ESTIMATOR; ANISOTROPIES; HFI; TEMPERATURE; CALIBRATION; INFLATION AB We study the effects of instrumental systematics on the estimation of primordial non-Gaussianity using the cosmic microwave background (CMB) bispectrum from both the temperature and the polarization anisotropies. For temperature systematics we consider gain fluctuation and beam distortions. For polarization we consider effects related to known instrumental systematics: calibration, pixel rotation, differential gain, pointing, and ellipticity of the instrument beam. We consider these effects at the next to leading order, which we refer to as nonlinear systematic effects. We find that if the instrumental response is linearly proportional to the received CMB intensity, then only the shape of the primordial CMB bispectrum, if there is any, will be distorted. We show that the nonlinear response of the instrument can in general result in spurious non-Gaussian features on both the CMB temperature and polarization anisotropies, even if the primordial CMB is completely Gaussian. We determine the level for both the linear and nonlinear systematics parameters for which they would cause no significant degradation of our ability to constrain the primordial non-Gaussianity amplitude f(NL). We find that the nonlinear systematics are potentially a bigger worry for extracting the primordial non-Gaussianity than the linear systematics, especially because the current and near future CMB probes are optimized for CMB power-spectrum measurements which are not particularly sensitive to the nonlinear instrument response. We find that if instrumental nonlinearities are not controlled by dedicated calibration, the effective local non-Gaussianity can be as large as f(NL) similar to O(10) before the corresponding nonlinearities show up in the CMB dipole measurements. The higher-order multipoles are even less sensitive to instrumental nonlinearities. C1 [Su, Meng] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Yadav, Amit P. S.] Inst Adv Study, Princeton, NJ 08540 USA. [Shimon, Meir; Keating, Brian G.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Su, M (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-10, Cambridge, MA 02138 USA. EM mengsu@cfa.harvard.edu FU NASA [NNX08AG40G]; NSF [AST-0807444] FX We are particularly thankful to M. Zaldarriaga for useful discussions on the project and providing comments on the paper. We acknowledge helpful conversations with X. Chen. A. P. S. Y. gratefully acknowledges support from IBM Einstein and funding from NASA under Grant No. NNX08AG40G and the NSF under Grant No. AST-0807444. We both acknowledge a CMBPol workshop held at the University of Chicago in July 2009 where this work was started. NR 50 TC 5 Z9 5 U1 0 U2 0 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 MAY 26 PY 2011 VL 83 IS 10 AR 103007 DI 10.1103/PhysRevD.83.103007 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 769IO UT WOS:000291006300001 ER PT J AU Braun, EL Kimball, RT Han, KL Iuhasz-Velez, NR Bonilla, AJ Chojnowski, JL Smith, JV Bowie, RCK Braun, MJ Hackett, SJ Harshman, J Huddleston, CJ Marks, B Miglia, KJ Moore, WS Reddy, S Sheldon, FH Witt, CC Yuri, T AF Braun, Edward L. Kimball, Rebecca T. Han, Kin-Lan Iuhasz-Velez, Naomi R. Bonilla, Amber J. Chojnowski, Jena L. Smith, Jordan V. Bowie, Rauri C. K. Braun, Michael J. Hackett, Shannon J. Harshman, John Huddleston, Christopher J. Marks, Ben D. Miglia, Kathleen J. Moore, William S. Reddy, Sushma Sheldon, Frederick H. Witt, Christopher C. Yuri, Tamaki TI Homoplastic microinversions and the avian tree of life SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID MOLECULAR EVOLUTION; SEQUENCE ALIGNMENT; NEORNITHINE BIRDS; SMALL INVERSIONS; CLATHRIN HEAVY; GENE TREES; PHYLOGENY; GENOMES; DNA; CHARACTERS AB Background: Microinversions are cytologically undetectable inversions of DNA sequences that accumulate slowly in genomes. Like many other rare genomic changes (RGCs), microinversions are thought to be virtually homoplasy-free evolutionary characters, suggesting that they may be very useful for difficult phylogenetic problems such as the avian tree of life. However, few detailed surveys of these genomic rearrangements have been conducted, making it difficult to assess this hypothesis or understand the impact of microinversions upon genome evolution. Results: We surveyed non-coding sequence data from a recent avian phylogenetic study and found substantially more microinversions than expected based upon prior information about vertebrate inversion rates, although this is likely due to underestimation of these rates in previous studies. Most microinversions were lineage-specific or united well-accepted groups. However, some homoplastic microinversions were evident among the informative characters. Hemiplasy, which reflects differences between gene trees and the species tree, did not explain the observed homoplasy. Two specific loci were microinversion hotspots, with high numbers of inversions that included both the homoplastic as well as some overlapping microinversions. Neither stem-loop structures nor detectable sequence motifs were associated with microinversions in the hotspots. Conclusions: Microinversions can provide valuable phylogenetic information, although power analysis indicates that large amounts of sequence data will be necessary to identify enough inversions (and similar RGCs) to resolve short branches in the tree of life. Moreover, microinversions are not perfect characters and should be interpreted with caution, just as with any other character type. Independent of their use for phylogenetic analyses, microinversions are important because they have the potential to complicate alignment of non-coding sequences. Despite their low rate of accumulation, they have clearly contributed to genome evolution, suggesting that active identification of microinversions will prove useful in future phylogenomic studies. C1 [Braun, Edward L.; Kimball, Rebecca T.; Han, Kin-Lan; Bonilla, Amber J.; Chojnowski, Jena L.; Smith, Jordan V.; Yuri, Tamaki] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Iuhasz-Velez, Naomi R.] Univ Florida, Dept Math, Gainesville, FL 32611 USA. [Bowie, Rauri C. K.; Hackett, Shannon J.; Harshman, John; Reddy, Sushma] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. [Bowie, Rauri C. K.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Bowie, Rauri C. K.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Braun, Michael J.; Huddleston, Christopher J.; Yuri, Tamaki] Smithsonian Inst, Dept Vertebrate Zool, Suitland, MD 20746 USA. [Braun, Michael J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. [Marks, Ben D.; Sheldon, Frederick H.; Witt, Christopher C.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Marks, Ben D.; Sheldon, Frederick H.; Witt, Christopher C.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Miglia, Kathleen J.; Moore, William S.] Wayne State Univ, Dept Biol Sci, Detroit, MI 48202 USA. [Reddy, Sushma] Loyola Univ, Dept Biol, Chicago, IL 60626 USA. [Witt, Christopher C.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Witt, Christopher C.] Univ New Mexico, Museum SW Biol, Albuquerque, NM 87131 USA. [Yuri, Tamaki] Univ Oklahoma, Sam Noble Oklahoma Museum Nat Hist, Norman, OK 73072 USA. RP Braun, EL (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM ebraun68@ufl.edu RI Han, Kin-Lan/G-7121-2011; Witt, Christopher/D-8587-2012; Vincelli, Amber/J-4263-2014; Kimball, Rebecca/C-2290-2009; OI Witt, Christopher/0000-0003-2781-1543; Vincelli, Amber/0000-0002-1247-7784; Braun, Edward/0000-0003-1643-5212; Kimball, Rebecca/0000-0001-5449-5481; Bowie, Rauri/0000-0001-8328-6021 FU U.S. National Science Foundation [DEB-0228682, DEB-0228675, DEB-0228688, DEB-0228617]; University of Florida FX We thank Clare Rittschof and members of the Kimball-Braun lab group for helpful comments on this manuscript and we are grateful to the museums and collectors (Additional file 1) for loaning samples. This work was supported by the U.S. National Science Foundation Assembling the Tree of Life program, grants DEB-0228682 (to RTK, ELB, and David W Steadman), DEB-0228675 (to SJH), DEB-0228688 (to FHS), and DEB-0228617 (to WSM). Publication of this article was funded in part by the University of Florida Open-Access Publishing Fund. NR 60 TC 17 Z9 17 U1 1 U2 18 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 MAY 25 PY 2011 VL 11 AR 141 DI 10.1186/1471-2148-11-141 PG 10 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 782ZA UT WOS:000292050100001 PM 21612607 ER PT J AU Crawford, AJ Alonso, R Jaramillo, CA Sucre, S Ibanez, R AF Crawford, Andrew J. Alonso, Roberto Jaramillo A, Cesar A. Sucre, Samuel Ibanez D, Roberto TI DNA barcoding identifies a third invasive species of Eleutherodactylus (Anura: Eleutherodactylidae) in Panama City, Panama SO ZOOTAXA LA English DT Letter ID DIVERSITY; LIFE C1 [Crawford, Andrew J.] Univ Los Andes, Dept Ciencias Biol, Bogota 4976, Colombia. [Crawford, Andrew J.; Jaramillo A, Cesar A.; Ibanez D, Roberto] Circulo Herpetol Panama, Panama City, Panama. [Crawford, Andrew J.; Jaramillo A, Cesar A.; Ibanez D, Roberto] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Alonso, Roberto] Univ La Habana, Fac Biol, Museo Felipe Poey, Havana, Cuba. [Jaramillo A, Cesar A.] Univ Panama, Fac Med, Dept Histol & Neuroanat Humana, Panama City, Panama. [Sucre, Samuel; Ibanez D, Roberto] Univ Panama, Dept Zool, Escuela Biol, Panama City, Panama. RP Crawford, AJ (reprint author), Univ Los Andes, Dept Ciencias Biol, Bogota 4976, Colombia. EM andrew@dna.ac; ralonso@fbio.uh.cu; jaramilc@si.edu; sam@samfrogs.com; ibanezr@si.edu NR 14 TC 8 Z9 8 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 MAY 25 PY 2011 IS 2890 BP 65 EP 67 PG 3 WC Zoology SC Zoology GA 772CM UT WOS:000291208600006 ER PT J AU Hart, LB Rotstein, DS Wells, RS Bassos-Hull, K Schwacke, LH AF Hart, Leslie Burdett Rotstein, Dave S. Wells, Randall S. Bassos-Hull, Kim Schwacke, Lori H. TI Lacaziosis and lacaziosis-like prevalence among wild, common bottlenose dolphins Tursiops truncatus from the west coast of Florida, USA SO DISEASES OF AQUATIC ORGANISMS LA English DT Article DE Lacaziosis; Lobomycosis; Bottlenose dolphin; Tursiops truncatus; Sarasota Bay; Charlotte Harbor ID INDIAN RIVER LAGOON; GULF-OF-MEXICO; LOBOS DISEASE; SARASOTA BAY; ATLANTIC; LOBOMYCOSIS; SKIN; CAROLINA; ESTUARY; HEALTH AB Lacaziosis (lobomycosis; Lacazia loboi) is a fungal skin disease that naturally occurs only in humans and dolphins. The first reported case of lacaziosis in a bottlenose dolphin Tursiops truncatus occurred in 1970 in Sarasota Bay, Florida, USA, and subsequent photo-ID monitoring of the Sarasota Bay dolphin population has revealed persistence of the disease. The objectives of this study were to estimate lacaziosis prevalence (P) in 2 bottlenose dolphin populations on the west coast of Florida (Sarasota Bay and Charlotte Harbor) and compare disease occurrence to other published estimates of lacaziosis in dolphin populations across the globe. Historic photographic records of dolphins captured and released for health assessment purposes (Sarasota Bay) and photo-ID studies (Charlotte Harbor) were screened for evidence of lesions consistent with lacaziosis. Health assessment data revealed a prevalence of lacaziosis in the Sarasota Bay bottlenose dolphin population between 2 and 3%, and analyses of photo-ID data provided a lacaziosis-like prevalence estimate of 2% for Charlotte Harbor dolphins. With the exception of lacaziosis prevalence estimates for dolphins inhabiting the Indian River Lagoon (P = 0.068; P = 0.12), no statistically significant differences were seen among Sarasota Bay, Charlotte Harbor, and other published estimates. Although lacaziosis is a rare disease among these dolphin populations, studies that assess disease burden among different populations can assist with the surveillance of this zoonotic pathogen. C1 [Hart, Leslie Burdett; Schwacke, Lori H.] Med Univ S Carolina, Div Biostat & Epidemiol, Dept Med, Charleston, SC 29425 USA. [Rotstein, Dave S.] Univ Corp Atmospher Res, Smithsonian Museum Support Ctr, Suitland, MD 20746 USA. [Wells, Randall S.; Bassos-Hull, Kim] Mote Marine Lab, Chicago Zool Soc, Sarasota, FL 34236 USA. [Schwacke, Lori H.] NOAA NCCOS Ctr Human Hlth Risk, Charleston, SC 29412 USA. Med Univ S Carolina, Hollings Marine Lab, Charleston, SC 29412 USA. RP Hart, LB (reprint author), Med Univ S Carolina, Div Biostat & Epidemiol, Dept Med, 135 Cannon St,Suite 303, Charleston, SC 29425 USA. EM leslie.burdett@noaa.gov FU NOAA's Center of Excellence for Oceans and Human Health at the Hollings Marine Laboratory FX The authors thank the staff (especially J. Allen), volunteers, and interns of the Chicago Zoological Society's Sarasota Dolphin Research Program for their assistance in photograph acquisition and knowledge of population demographics. We also thank S. Fire, S. Lane, and W. McFee for reviewing this manuscript. Funding for this project was provided by NOAA's Center of Excellence for Oceans and Human Health at the Hollings Marine Laboratory. NR 41 TC 8 Z9 8 U1 1 U2 15 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0177-5103 EI 1616-1580 J9 DIS AQUAT ORGAN JI Dis. Aquat. Org. PD MAY 24 PY 2011 VL 95 IS 1 BP 49 EP 56 DI 10.3354/dao02345 PG 8 WC Fisheries; Veterinary Sciences SC Fisheries; Veterinary Sciences GA 768SE UT WOS:000290957500006 ER PT J AU Meibom, S Barnes, SA Latham, DW Batalha, N Borucki, WJ Koch, DG Basri, G Walkowicz, LM Janes, KA Jenkins, J Van Cleve, J Haas, MR Bryson, ST Dupree, AK Furesz, G Szentgyorgyi, AH Buchhave, LA Clarke, BD Twicken, JD Quintana, EV AF Meibom, Soren Barnes, Sydney A. Latham, David W. Batalha, Natalie Borucki, William J. Koch, David G. Basri, Gibor Walkowicz, Lucianne M. Janes, Kenneth A. Jenkins, Jon Van Cleve, Jeffrey Haas, Michael R. Bryson, Stephen T. Dupree, Andrea K. Furesz, Gabor Szentgyorgyi, Andrew H. Buchhave, Lars A. Clarke, Bruce D. Twicken, Joseph D. Quintana, Elisa V. TI THE KEPLER CLUSTER STUDY: STELLAR ROTATION IN NGC 6811 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE open clusters and associations: individual (NGC 6811); stars: activity; stars: late-type; starspots; stars: rotation ID LOW-MASS STARS; SOLAR-TYPE STARS; ANGULAR-MOMENTUM LOSS; TIME-SERIES ANALYSIS; INITIAL CHARACTERISTICS; CADENCE DATA; GYROCHRONOLOGY; EVOLUTION; PLEIADES; VELOCITIES AB We present rotation periods for 71 single dwarf members of the open cluster NGC6811 determined using photometry from NASA's Kepler mission. The results are the first from The Kepler Cluster Study, which combines Kepler's photometry with ground-based spectroscopy for cluster membership and binarity. The rotation periods delineate a tight sequence in the NGC 6811 color-period diagram from similar to 1 day at mid-F to similar to 11 days at early-K spectral type. This result extends to 1 Gyr similar prior results in the similar to 600 Myr Hyades and Praesepe clusters, suggesting that rotation periods for cool dwarf stars delineate a well-defined surface in the three-dimensional space of color (mass), rotation, and age. It implies that reliable ages can be derived for field dwarf stars with measured colors and rotation periods, and it promises to enable further understanding of various aspects of stellar rotation and activity for cool stars. C1 [Meibom, Soren; Latham, David W.; Dupree, Andrea K.; Furesz, Gabor; Szentgyorgyi, Andrew H.; Buchhave, Lars A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barnes, Sydney A.] Lowell Observ, Flagstaff, AZ 86001 USA. [Batalha, Natalie; Borucki, William J.; Koch, David G.; Jenkins, Jon; Van Cleve, Jeffrey; Haas, Michael R.; Bryson, Stephen T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Basri, Gibor; Walkowicz, Lucianne M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Janes, Kenneth A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Jenkins, Jon; Van Cleve, Jeffrey; Clarke, Bruce D.; Twicken, Joseph D.; Quintana, Elisa V.] SETI Inst, Mountain View, CA 94043 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Buchhave, Lars A./0000-0003-1605-5666 FU NASA's Science Mission Directorate; NASA [NNX09AH18A, NAS5-26555]; Kepler mission via NASA [NCC2-1390]; Smithsonian Astrophysical Observatory; NASA Office of Space Science [NNX09AF08G] FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. We thank the entire Kepler mission team including engineers, managers, and administrative staff, who have all contributed to the success of the mission. This work has been supported by NASA grant NNX09AH18A (The Kepler Cluster Study) to S.M., and by support to S.M. from the Kepler mission via NASA Cooperative Agreement NCC2-1390. This paper uses data products produced by the Optical and Infrared (OIR) Astronomy Division's Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. S.M. expresses deep appreciation for time awarded on MMT/Hectochelle and for the exceptional and friendly support of the MMT staff. The Kepler 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. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 53 TC 75 Z9 75 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 MAY 20 PY 2011 VL 733 IS 1 AR L9 DI 10.1088/2041-8205/733/1/L9 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797NL UT WOS:000293134500009 ER PT J AU Platais, I Cudworth, KM Kozhurina-Platais, V McLaughlin, DE Meibom, S Veillet, C AF Platais, I. Cudworth, K. M. Kozhurina-Platais, V. McLaughlin, D. E. Meibom, S. Veillet, C. TI A NEW LOOK AT THE OLD STAR CLUSTER NGC 6791 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrometry; open clusters and associations: general; open clusters and associations: individual (NGC 6791); proper motions ID RICH OPEN CLUSTER; GIANT BRANCH; NGC-6791; SYSTEM; PHOTOMETRY; ISOCHRONES; ABUNDANCES; TELESCOPE; EVOLUTION; CATALOG AB We present comprehensive cluster membership and g'r' photometry of the prototypical old, metal-rich Galactic star cluster NGC 6791. The proper-motion catalog contains 58,901 objects down to g' similar to 24, limited to a circular area of radius 30'. The highest precision of the proper motions is 0.08 mas yr(-1). Our proper motions confirm cluster membership of all main and also some rare constituents of NGC 6791. The total number of probable cluster members down to g' = 22 (M(V) similar to +8) is similar to 4800, corresponding to M(tot) approximate to 5000 M(circle dot). New findings include an extended horizontal branch in this cluster. The angular radius of NGC 6791 is at least 15' (the effective radius is Rh similar or equal to 4.'4 while the tidal radius is r(t) similar or equal to 23'). The luminosity function of the cluster peaks at M(g') similar to +4.5 and then steadily declines toward fainter magnitudes. Our data provide evidence that differential reddening may not be ignored in NGC 6791. C1 [Platais, I.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Cudworth, K. M.] Univ Chicago, Yerkes Observ, Williams Bay, WI 53191 USA. [Kozhurina-Platais, V.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [McLaughlin, D. E.] Keele Univ, Astrophys Grp, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Meibom, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Veillet, C.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. RP Platais, I (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM imants@pha.jhu.edu FU NSF [AST 09-08114]; NASA [NNX09AH18A]; STFC FX We thank D. Crawford, J. Cummings, E. Hubbard, T. Kinman, B. Lynds, S. Majewski, R. Michie (deceased), K. Mighell, A. Sarajedini, and M. Sosey, whose time and effort at the telescope made this project possible. We thank the referee Barbara Anthony-Twarog for pointing out the limitations of our data. This work has been supported in part by NSF grant AST 09-08114 to JHU (I.P.) and by NASA grant NNX09AH18A (The Kepler Open Cluster Study). Astrophysics at Keele University is supported by an STFC Rolling Grant. This study is based on observations obtained with MegaPrime/MegaCam, a joint project of Canada-France-Hawaii Telescope (CFHT) and CEA/DAPNIA, at the CFHT which is operated by the NRC of Canada, the Institute National des Sciences de l'Universe of the CNRS, and the University of Hawaii. NR 26 TC 28 Z9 29 U1 1 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 MAY 20 PY 2011 VL 733 IS 1 AR L1 DI 10.1088/2041-8205/733/1/L1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797NL UT WOS:000293134500001 ER PT J AU Riechers, DA Cooray, A Omont, A Neri, R Harris, AI Baker, AJ Cox, P Frayer, DT Carpenter, JM Auld, R Aussel, H Beelen, A Blundell, R Bock, J Brisbin, D Burgarella, D Chanial, P Chapman, SC Clements, DL Conley, A Dowell, CD Eales, S Farrah, D Franceschini, A Gavazzi, R Glenn, J Griffin, M Gurwell, M Ivison, RJ Kim, S Krips, M Mortier, AMJ Oliver, SJ Page, MJ Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rawlings, JI Raymond, G Rodighiero, G Roseboom, IG Rowan-Robinson, M Scott, KS Seymour, N Smith, AJ Symeonidis, M Tugwell, KE Vaccari, M Vieira, JD Vigroux, L Wang, L Wardlow, J Wright, G AF Riechers, Dominik A. Cooray, A. Omont, A. Neri, R. Harris, A. I. Baker, A. J. Cox, P. Frayer, D. T. Carpenter, J. M. Auld, R. Aussel, H. Beelen, A. Blundell, R. Bock, J. Brisbin, D. Burgarella, D. Chanial, P. Chapman, S. C. Clements, D. L. Conley, A. Dowell, C. D. Eales, S. Farrah, D. Franceschini, A. Gavazzi, R. Glenn, J. Griffin, M. Gurwell, M. Ivison, R. J. Kim, S. Krips, M. Mortier, A. M. J. Oliver, S. J. Page, M. J. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rawlings, J. I. Raymond, G. Rodighiero, G. Roseboom, I. G. Rowan-Robinson, M. Scott, K. S. Seymour, N. Smith, A. J. Symeonidis, M. Tugwell, K. E. Vaccari, M. Vieira, J. D. Vigroux, L. Wang, L. Wardlow, J. Wright, G. TI DYNAMICAL STRUCTURE OF THE MOLECULAR INTERSTELLAR MEDIUM IN AN EXTREMELY BRIGHT, MULTIPLY LENSED z similar or equal to 3 SUBMILLIMETER GALAXY DISCOVERED WITH HERSCHEL SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; galaxies: active; galaxies: formation; galaxies: high-redshift; galaxies: starburst; radio lines: galaxies ID PROBE WMAP OBSERVATIONS; GREEN-BANK-TELESCOPE; STAR-FORMATION; HIGH-REDSHIFT; ULTRALUMINOUS GALAXIES; MAJOR MERGERS; GAS; CO; Z=2.3; HCN AB We report the detection of CO(J = 5 -> 4), CO(J = 3 -> 2), and CO(J = 1 -> 0) emission in the strongly lensed, Herschel/SPIRE-selected submillimeter galaxy (SMG) HERMES J105751.1+573027 at z = 2.9574 +/- 0.0001, using the Plateau de Bure Interferometer, the Combined Array for Research in Millimeter-wave Astronomy, and the Green Bank Telescope. The observations spatially resolve the molecular gas into four lensed images with a maximum separation of similar to 9 '' and reveal the internal gas dynamics in this system. We derive lensing-corrected CO line luminosities of L'(CO(1-0)) = (4.17 +/- 0.41), L'(CO(3-2)) = (3.96 +/- 0.20), and L'(CO(5-4)) = (3.45 +/- 0.20) x 10(10) (mu(L)/10.9)(-1) K km s(-1) pc(2), corresponding to luminosity ratios of r(31) = 0.95 +/- 0.10, r(53) = 0.87 +/- 0.06, and r(51) = 0.83 +/- 0.09. This suggests a total molecular gas mass of M-gas = 3.3 x 10(10) (alpha(CO)/0.8) (mu(L)/10.9)(-1) M-circle dot. The gas mass, gas mass fraction, gas depletion timescale, star formation efficiency, and specific star formation rate are typical for an SMG. The velocity structure of the gas reservoir suggests that the brightest two lensed images are dynamically resolved projections of the same dust-obscured region in the galaxy that are kinematically offset from the unresolved fainter images. The resolved kinematics appear consistent with the complex velocity structure observed in major, "wet" (i.e., gas-rich) mergers. Major mergers are commonly observed in SMGs and are likely to be responsible for fueling their intense starbursts at high gas consumption rates. This study demonstrates the level of detail to which galaxies in the early universe can be studied by utilizing the increase in effective spatial resolution and sensitivity provided by gravitational lensing. C1 [Riechers, Dominik A.; Cooray, A.; Carpenter, J. M.; Bock, J.; Dowell, C. D.; Vieira, J. D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Cooray, A.; Kim, S.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Omont, A.; Gavazzi, R.; Vigroux, L.] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [Omont, A.; Gavazzi, R.; Vigroux, L.] Univ Paris 06, F-75014 Paris, France. [Neri, R.; Cox, P.; Krips, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Frayer, D. T.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Auld, R.; Eales, S.; Griffin, M.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aussel, H.; Chanial, P.] Univ Paris Diderot, Irfu CNRS, DSM, Lab AIM Paris Saclay,CEA,CE Saclay, F-91191 Gif Sur Yvette, France. [Beelen, A.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Blundell, R.; Gurwell, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J.; Dowell, C. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brisbin, D.] Cornell Univ, Ithaca, NY 14853 USA. [Burgarella, D.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Clements, D. L.; Mortier, A. M. J.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Conley, A.; Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA. [Farrah, D.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Franceschini, A.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pearson, C. P.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Scott, K. S.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Riechers, DA (reprint author), CALTECH, Dept Astron, MC 249-17,1200 E Calif Blvd, Pasadena, CA 91125 USA. EM dr@caltech.edu RI Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; OI Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Seymour, Nicholas/0000-0003-3506-5536 FU NASA [HST-HF-51235.01, NAS 5-26555]; NSF [AST-0708653]; INSU/CNRS(France); MPG (Germany); IGN (Spain); CARMA partner universities; Associated Universities, Inc. FX We thank the referee for a detailed and helpful report. D.R. acknowledges support from NASA through Hubble Fellowship grant HST-HF-51235.01 awarded by STScI, operated by AURA for NASA, under contract NAS 5-26555. A.J.B. acknowledges support from NSF grant AST-0708653 to Rutgers University. IRAM is supported by INSU/CNRS(France), MPG (Germany), and IGN (Spain). Support for CARMA construction was derived from the Moore and Norris Foundations, the Associates of Caltech, the states of California, Illinois, and Maryland, and the NSF. Ongoing CARMA development and operations are supported by the NSF under a cooperative agreement, and by the CARMA partner universities. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 35 TC 34 Z9 34 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 MAY 20 PY 2011 VL 733 IS 1 AR L12 DI 10.1088/2041-8205/733/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797NL UT WOS:000293134500012 ER PT J AU Nahar, SN Pradhan, AK Chen, GX Eissner, W AF Nahar, Sultana N. Pradhan, Anil K. Chen, Guo-Xin Eissner, Werner TI Highly excited core resonances in photoionization of Fe XVII: Implications for plasma opacities SO PHYSICAL REVIEW A LA English DT Article ID ELECTRON-ION RECOMBINATION; R-MATRIX CALCULATIONS; ATOMIC DATA; TRANSITION-PROBABILITIES; CROSS-SECTIONS; IRON PROJECT; ABUNDANCES; ALGORITHM; STATE AB A comprehensive study of high-accuracy photoionization cross sections is carried out using the relativistic Breit-Pauli R-matrix (BPRM) method for (h nu + Fe XVII -> Fe XVIII + e). Owing to its importance in high-temperature plasmas, the calculations cover a large energy range, particularly the myriad photoexcitation-of-core (PEC) resonances including the n = 3 levels not heretofore considered. The calculations employ a close-coupling wave-function expansion of 60 levels of the core ion Fe XVIII ranging over a wide energy range of nearly 900 eV between the n = 2 and n = 3 levels. Strong-coupling effects due to dipole transition arrays 2p(5) -> 2p(4)(3s, 3d) manifest themselves as large PEC resonances throughout this range and enhance the effective photoionization cross sections orders of magnitude above the background. Comparisons with the erstwhile Opacity Project (OP) and other previous calculations show that the currently available cross sections considerably underestimate the bound-free cross sections. A level-identification scheme is used for spectroscopic designation of the 454 bound fine structure levels of Fe XVII, with n <= 10, l <= 9, and 0 <= J <= 8 of even and odd parities, obtained using the ab initio BPRM method (compared to 181 LS bound states in the OP work). The calculated energies are compared with those available from the National Institute for Standards and Technology database, which lists 63 levels with very good agreement. Level-specific photoionization cross sections are computed for all levels. In addition, partial cross sections for leaving the core ion Fe XVII in the ground state are also obtained. These results should be relevant to modeling of astrophysical and laboratory plasma sources requiring (i) photoionization rates, (ii) extensive nonlocal-thermodynamic-equilibrium models, (iii) total unified electron-ion recombination rates including radiative and dielectronic recombination, and (iv) plasma opacities. We particularly examine PEC and non-PEC resonance strengths and emphasize their expanded role to incorporate inner-shell excitations for improved opacities, as shown by the computed monochromatic opacity of Fe XVII. C1 [Nahar, Sultana N.; Pradhan, Anil K.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Chen, Guo-Xin] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Eissner, Werner] Inst Theoret Phys, D-70550 Stuttgart, Germany. RP Nahar, SN (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. EM nahar@astronomy.ohio-state.edu FU NASA; US Department of Energy FX This work was partially supported by the NASA Astronomy and Physics Research Analysis Program (SNN) and the US Department of Energy (AKP). The computational work was carried out at the Ohio Supercomputer Center in Columbus Ohio. NR 38 TC 18 Z9 18 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAY 20 PY 2011 VL 83 IS 5 AR 053417 DI 10.1103/PhysRevA.83.053417 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 767MF UT WOS:000290860000008 ER PT J AU Pazourek, R Feist, J Nagele, S Persson, E Schneider, BI Collins, LA Burgdorfer, J AF Pazourek, R. Feist, J. Nagele, S. Persson, E. Schneider, B. I. Collins, L. A. Burgdoerfer, J. TI Universal features in sequential and nonsequential two-photon double ionization of helium SO PHYSICAL REVIEW A LA English DT Article ID DEPENDENT SCHRODINGER-EQUATION; HIGH-HARMONIC-GENERATION; THRESHOLD; LASER; COLLISIONS; HE AB We analyze two-photon double ionization of helium in both the nonsequential ((h) over bar omega < I(2) approximate to 54.4 eV) and sequential (<(h)over bar>omega > I(2)) regime. We show that the energy spacing Delta E = E(1) - E(2) between the two emitted electrons provides the key parameter that controls both the energy and the angular distribution and reveals the universal features present in both the nonsequential and sequential regime. This universality, i.e., independence of (h) over bar omega, is a manifestation of the continuity across the threshold for sequential double ionization. For all photon energies considered, the energy distribution can be described by a universal shape function that contains only the spectral and temporal information entering second-order time-dependent perturbation theory. Angular correlations and distributions are found to be more sensitive to the value of (h) over bar omega. In particular, shake-up interferences have a large effect on the angular distribution. Energy spectra, angular distributions parametrized by the anisotropy parameters beta(j), and total cross sections presented in this paper are obtained by fully correlated time-dependent ab initio calculations. C1 [Pazourek, R.; Feist, J.; Nagele, S.; Persson, E.; Burgdoerfer, J.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. [Feist, J.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Schneider, B. I.] Natl Sci Fdn, Div Phys, Off Cyberinfrastruct, Arlington, VA 22230 USA. [Collins, L. A.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. RP Pazourek, R (reprint author), Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. EM renate.pazourek@tuwien.ac.at RI Nagele, Stefan/E-6938-2011; Feist, Johannes/J-7394-2012 OI Nagele, Stefan/0000-0003-1213-0294; Feist, Johannes/0000-0002-7972-0646 FU FWF-Austria [SFB016, P21141-N16]; NSF [TG-PHY090031]; US Department of Energy [DE-AC52-06NA25396] FX We thank I. Ivanov for sending us results in numerical form. R.P., J.F., S.N., E.P., and J.B. acknowledge support by the FWF-Austria, Grants No. SFB016 and No. P21141-N16. J.F. acknowledges support by the NSF through a grant to ITAMP. This research was supported in part by the National Science Foundation through TeraGrid resources provided by NICS and TACC under Grant No. TG-PHY090031. Additional computational time was provided by the Vienna Scientific Cluster (VSC) and under Institutional Computing at Los Alamos National Laboratory. The Los Alamos National Laboratory is operated by Los Alamos National Security, LLC for the National Nuclear Security Administration of the US Department of Energy under Contract No. DE-AC52-06NA25396. NR 54 TC 29 Z9 30 U1 0 U2 22 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAY 20 PY 2011 VL 83 IS 5 AR 053418 DI 10.1103/PhysRevA.83.053418 PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 767MF UT WOS:000290860000009 ER PT J AU Cohen, O Kashyap, VL Drake, JJ Sokolov, IV Garraffo, C Gombosi, TI AF Cohen, O. Kashyap, V. L. Drake, J. J. Sokolov, I. V. Garraffo, C. Gombosi, T. I. TI THE DYNAMICS OF STELLAR CORONAE HARBORING HOT JUPITERS. I. A TIME-DEPENDENT MAGNETOHYDRODYNAMIC SIMULATION OF THE INTERPLANETARY ENVIRONMENT IN THE HD 189733 PLANETARY SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE planet-star interactions; stars: coronae; stars: magnetic field ID EXTRASOLAR GIANT PLANETS; SOLAR-WIND; AB DORADUS; CHROMOSPHERIC ACTIVITY; MAGNETIC-FIELD; STARS; MAGNETOSPHERE; EXOPLANETS; EVOLUTION; PATTERNS AB We carry out the first time-dependent numerical magnetohydrodynamic modeling of an extrasolar planetary system to study the interaction of the stellar magnetic field and wind with the planetary magnetosphere and outflow. We base our model on the parameters of the HD 189733 system, which harbors a close-in giant planet. Our simulation reveals a highly structured stellar corona characterized by sectors with different plasma properties. The star-planet interaction (SPI) varies in magnitude and complexity, depending on the planetary phase, planetary magnetic field strength, and the relative orientation of the stellar and planetary fields. It also reveals a long, comet-like tail which is a result of the wrapping of the planetary magnetospheric tail by its fast orbital motion. A reconnection event occurs at a specific orbital phase, causing mass loss from the planetary magnetosphere that can generate a hot spot on the stellar surface. The simulation also shows that the system has sufficient energy to produce hot spots observed in Ca II lines in giant planet hosting stars. However, the short duration of the reconnection event suggests that such SPI cannot be observed persistently. C1 [Cohen, O.; Kashyap, V. L.; Drake, J. J.; Garraffo, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sokolov, I. V.; Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gombosi, Tamas/G-4238-2011; Sokolov, Igor/H-9860-2013; OI Gombosi, Tamas/0000-0001-9360-4951; Sokolov, Igor/0000-0002-6118-0469; Cohen, Ofer/0000-0003-3721-0215 FU SHINE through NSF [ATM-0823592]; NASA-LWSTRT [NNG05GM44G]; NASA [NAS8-39073]; NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI FX We thank the anonymous referee for his/her comments. We also thank Scott Wolk and Steve Saar for their useful comments. O.C. is supported by SHINE through NSF ATM-0823592 grant, and by NASA-LWSTRT Grant NNG05GM44G. J.J.D. and V.L.K. were funded by NASA contract NAS8-39073 to the Chandra X-ray Center. Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. NR 45 TC 36 Z9 36 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 MAY 20 PY 2011 VL 733 IS 1 AR 67 DI 10.1088/0004-637X/733/1/67 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600067 ER PT J AU Kaltenegger, L Segura, A Mohanty, S AF Kaltenegger, Lisa Segura, Antigona Mohanty, Subhanjoy TI MODEL SPECTRA OF THE FIRST POTENTIALLY HABITABLE SUPER-EARTH-Gl581d SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth; instrumentation: spectrographs; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: detection; planets and satellites: individual (G1581d) ID EARTH-LIKE PLANETS; EXTRA-SOLAR PLANETS; MOLECULAR SPECTROSCOPIC DATABASE; CARBON-DIOXIDE CLOUDS; LOW-MASS STARS; M-CIRCLE-PLUS; SUPER-EARTHS; M-DWARFS; TERRESTRIAL PLANETS; HARPS SEARCH AB Gl581d has a minimum mass of 7 M-Earth and is the first detected potentially habitable rocky Super-Earth. Our models confirm that a habitable atmosphere can exist on Gl581d. We derive spectroscopic features for atmospheres assuming an Earth-like composition for this planet, from high-oxygen atmosphere analogous to Earth's to high-CO2 atmospheres with and without biotic oxygen concentrations. We find that a minimum CO2 partial pressure of about 7 bar, in an atmosphere with a total surface pressure of 7.6 bar, is needed to maintain a mean surface temperature above freezing on Gl581d. We model transmission and emergent synthetic spectra from 0.4 mu m to 40 mu m and show where indicators of biological activities in such a planet's atmosphere could be observed by future ground-and space-based telescopes. The model we present here only represents one possible nature-an Earth-like composition-of a planet like Gl581d in a wide parameter space. Future observations of atmospheric features can be used to examine if our concept of habitability and its dependence on the carbonate-silicate cycle is correct, and assess whether Gl581d is indeed a habitable Super-Earth. C1 [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Segura, Antigona] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Mohanty, Subhanjoy] Univ London Imperial Coll Sci Technol & Med, Blackett Lab 1010, London SW7 2AZ, England. RP Kaltenegger, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lkaltene@cfa.harvard.edu FU NAI; DFG [ENP Ka 3142/1-1]; [PAPIIT-IN119709-3] FX L.K. acknowledges support from NAI and DFG Funding ENP Ka 3142/1-1. A.S. and L.K. thank the support by project PAPIIT-IN119709-3. NR 85 TC 25 Z9 25 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2011 VL 733 IS 1 AR 35 DI 10.1088/0004-637X/733/1/35 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600035 ER PT J AU Kipping, D Bakos, G AF Kipping, David Bakos, Gaspar TI ANALYSIS OF KEPLER'S SHORT-CADENCE PHOTOMETRY FOR TrES-2b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (TrES-2b); techniques: photometric; techniques: spectroscopic ID TRANSIT LIGHT-CURVE; PLANETARY PARAMETERS; TERRESTRIAL PLANETS; EXTRASOLAR PLANETS; EXOPLANET TRES-2; STELLAR; MODELS; STAR; DETECTABILITY; ATMOSPHERE AB We present an analysis of 18 short-cadence (SC) transit light curves of TrES-2b using quarter 0 (Q0) and quarter 1 (Q1) from the Kepler Mission. The photometry is of unprecedented precision, 237 ppm minute(-1), allowing for the most accurate determination of the transit parameters yet obtained for this system. Global fits of the transit photometry, radial velocities, and known transit times are used to obtain a self-consistent set of refined parameters for this system, including updated stellar and planetary parameters. Special attention is paid to fitting for limb darkening and eccentricity. We place an upper limit on the occultation depth to be < 72.9 ppm to 3 sigma confidence, indicating TrES-2b has the lowest determined geometric albedo for an exoplanet, of A(g) < 0.146. We also produce a transit timing analysis using Kepler's SC data and demonstrate exceptional timing precision at the level of a few seconds for each transit event. With 18 fully sampled transits at such high precision, we are able to produce stringent constraints on the presence of perturbing planets, Trojans, and extrasolar moons. We introduce the novel use of control data to identify phasing effects. We also exclude the previously proposed hypotheses of short-period transit time variation and additional transits but find that the hypothesis of long-term inclination change is neither supported nor refuted by our analysis. C1 [Kipping, David; Bakos, Gaspar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kipping, David] UCL, Dept Phys, London WC1E 6BT, England. RP Kipping, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu FU STFC; HATNet; NASA [NNG04GN74G, NNX08AF23G]; NSF [AST-0702843] FX D.M.K. has been supported by STFC studentships, and by the HATNet as an SAO predoctoral fellow. We acknowledge NASA NNG04GN74G, NNX08AF23G grants, and Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 for G. B.). Special thanks to the amateur astronomy community and the ETD. NR 52 TC 36 Z9 36 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 MAY 20 PY 2011 VL 733 IS 1 AR 36 DI 10.1088/0004-637X/733/1/36 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600036 ER PT J AU Marcus, RA Ragozzine, D Murray-Clay, RA Holman, MJ AF Marcus, Robert A. Ragozzine, Darin Murray-Clay, Ruth A. Holman, Matthew J. TI IDENTIFYING COLLISIONAL FAMILIES IN THE KUIPER BELT SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper Belt: general; planets and satellites: formation ID TRANS-NEPTUNIAN BODIES; ASTEROID FAMILIES; SIZE DISTRIBUTION; 2003 EL61; INCLINATION DISTRIBUTION; CANDIDATE MEMBERS; SOLAR-SYSTEM; OBJECTS; SEARCH; ORIGIN AB The identification and characterization of numerous collisional families-clusters of bodies with a common collisional origin-in the asteroid belt has added greatly to the understanding of asteroid belt formation and evolution. More recent study has also led to an appreciation of physical processes that had previously been neglected (e.g., the Yarkovsky effect). Collisions have certainly played an important role in the evolution of the Kuiper Belt as well, though only one collisional family has been identified in that region to date, around the dwarf planet Haumea. In this paper, we combine insights into collisional families from numerical simulations with the current observational constraints on the dynamical structure of the Kuiper Belt to investigate the ideal sizes and locations for identifying collisional families. We find that larger progenitors (r similar to 500 km) result inmore easily identifiable families, given the difficulty in identifying fragments of smaller progenitors in magnitude-limited surveys, despite their larger spread and less frequent occurrence. However, even these families do not stand out well from the background. Identifying families as statistical overdensities ismuch easier than characterizing families by distinguishing individual members from interlopers. Such identification seems promising, provided the background population is well known. In either case, families will also be much easier to study where the background population is small, i.e., at high inclinations. Overall, our results indicate that entirely different techniques for identifying families will be needed for the Kuiper Belt, and we provide some suggestions. C1 [Marcus, Robert A.; Ragozzine, Darin; Murray-Clay, Ruth A.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marcus, RA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rmarcus@cfa.harvard.edu RI Ragozzine, Darin/C-4926-2013 FU Harvard FAS Research Computing Group FX We thank Zoe Leinhardt for helpful discussions on the nature of collisional families and for an early look at work in progress. We are also grateful to Christian Clanton, Sarah Stewart, and Scott Kenyon for valuable feedback and discussion. This paper was significantly improved by a very thoughtful review from the referee David Nesvorny. The numerical calculations in this paper were performed on the Odyssey cluster supported by the Harvard FAS Research Computing Group. NR 62 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 MAY 20 PY 2011 VL 733 IS 1 AR 40 DI 10.1088/0004-637X/733/1/40 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600040 ER PT J AU Morales-Calderon, M Stauffer, JR Hillenbrand, LA Gutermuth, R Song, I Rebull, LM Plavchan, P Carpenter, JM Whitney, BA Covey, K de Oliveira, CA Winston, E McCaughrean, MJ Bouvier, J Guieu, S Vrba, FJ Holtzman, J Marchis, F Hora, JL Wasserman, LH Terebey, S Megeath, T Guinan, E Forbrich, J Huelamo, N Riviere-Marichalar, P Barrado, D Stapelfeldt, K Hernandez, J Allen, LE Ardila, DR Bayo, A Favata, F James, D Werner, M Wood, K AF Morales-Calderon, M. Stauffer, J. R. Hillenbrand, L. A. Gutermuth, R. Song, I. Rebull, L. M. Plavchan, P. Carpenter, J. M. Whitney, B. A. Covey, K. de Oliveira, C. Alves Winston, E. McCaughrean, M. J. Bouvier, J. Guieu, S. Vrba, F. J. Holtzman, J. Marchis, F. Hora, J. L. Wasserman, L. H. Terebey, S. Megeath, T. Guinan, E. Forbrich, J. Huelamo, N. Riviere-Marichalar, P. Barrado, D. Stapelfeldt, K. Hernandez, J. Allen, L. E. Ardila, D. R. Bayo, A. Favata, F. James, D. Werner, M. Wood, K. TI YSOVAR: THE FIRST SENSITIVE, WIDE-AREA, MID-INFRARED PHOTOMETRIC MONITORING OF THE ORION NEBULA CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; open clusters and associations: individual (Orion); stars: pre-main sequence; stars: protostars; stars: variables: general ID SEQUENCE ECLIPSING BINARY; SPITZER-SPACE-TELESCOPE; LOW-MASS STARS; T-TAURI STARS; SPECTROSCOPIC BINARY; CIRCUMSTELLAR DISKS; ROTATION PERIODS; PROPER MOTIONS; VARIABILITY; REGION AB We present initial results from time-series imaging at infrared wavelengths of 0.9 deg(2) in the Orion Nebula Cluster (ONC). During Fall 2009 we obtained 81 epochs of Spitzer 3.6 and 4.5 mu m data over 40 consecutive days. We extracted light curves with similar to 3% photometric accuracy for similar to 2000 ONC members ranging from several solar masses down to well below the hydrogen-burning mass limit. For many of the stars, we also have time-series photometry obtained at optical (I(c)) and/or near-infrared (JK(s)) wavelengths. Our data set can be mined to determine stellar rotation periods, identify new pre-main-sequence eclipsing binaries, search for new substellar Orion members, and help better determine the frequency of circumstellar disks as a function of stellar mass in the ONC. Our primary focus is the unique ability of 3.6 and 4.5 mu m variability information to improve our understanding of inner disk processes and structure in the Class I and II young stellar objects (YSOs). In this paper, we provide a brief overview of the YSOVAR Orion data obtained in Fall 2009 and highlight our light curves for AA-Tau analogs-YSOs with narrow dips in flux, most probably due to disk density structures passing through our line of sight. Detailed follow-up observations are needed in order to better quantify the nature of the obscuring bodies and what this implies for the structure of the inner disks of YSOs. C1 [Morales-Calderon, M.; Stauffer, J. R.; Rebull, L. M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Hillenbrand, L. A.; Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Gutermuth, R.] Smith Coll, Coll Astron Dept 5, Northampton, MA 01063 USA. [Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Song, I.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Plavchan, P.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Whitney, B. A.] Space Sci Inst, Boulder, CO 80301 USA. [Covey, K.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Covey, K.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [de Oliveira, C. Alves] Observ Grenoble, Lab Astrophys Grenoble, F-38041 Grenoble 9, France. [Winston, E.; McCaughrean, M. J.] Univ Exeter, Astrophys Grp, Coll Engn Math & Phys Sci, Exeter EX4 4QJ, Devon, England. [McCaughrean, M. J.; Favata, F.] European Space Agcy, Res & Sci Support Dept, Estec, NL-2200 AG Noordwijk, Netherlands. [Bouvier, J.] Univ Grenoble 1, CNRS, IPAG, INSU,UMR 5274, F-38041 Grenoble, France. [Vrba, F. J.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Guieu, S.; Bayo, A.] European So Observ, Santiago 19, Chile. [Holtzman, J.] New Mexico State Univ, Las Cruces, NM 88003 USA. [Marchis, F.] UC Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Marchis, F.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Hora, J. L.; Forbrich, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wasserman, L. H.] Lowell Observ, Flagstaff, AZ 86001 USA. [Terebey, S.] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA. [Megeath, T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Guinan, E.] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Huelamo, N.; Riviere-Marichalar, P.; Barrado, D.] CSIC, Ctr Astrobiol, INTA, LAEFF, E-28691 Villanueva De La Canada, Spain. [Barrado, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria, Spain. [Stapelfeldt, K.; Werner, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hernandez, J.] Ctr Invest Astron, Merida 5101 A, Venezuela. [Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Ardila, D. R.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [James, D.] Univ Hawaii, Hoku Kea Observ, Dept Phys & Astron, Hilo, HI 96720 USA. [James, D.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Wood, K.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9AD, Fife, Scotland. RP Morales-Calderon, M (reprint author), CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. EM mariamc@ipac.caltech.edu RI Stapelfeldt, Karl/D-2721-2012; Marchis, Franck/H-3971-2012; Barrado Navascues, David/C-1439-2017; Huelamo, Nuria/C-3042-2017; Morales-Calderon, Maria/C-8384-2017; OI Covey, Kevin/0000-0001-6914-7797; Barrado Navascues, David/0000-0002-5971-9242; Huelamo, Nuria/0000-0002-2711-8143; Morales-Calderon, Maria/0000-0001-9526-9499; Rebull, Luisa/0000-0001-6381-515X; Hora, Joseph/0000-0002-5599-4650 NR 47 TC 86 Z9 86 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 MAY 20 PY 2011 VL 733 IS 1 AR 50 DI 10.1088/0004-637X/733/1/50 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600050 ER PT J AU Ness, JU Osborne, JP Dobrotka, A Page, KL Drake, JJ Pinto, C Detmers, RG Schwarz, G Bode, MF Beardmore, AP Starrfield, S Hernanz, M Sala, G Krautter, J Woodward, CE AF Ness, J. -U. Osborne, J. P. Dobrotka, A. Page, K. L. Drake, J. J. Pinto, C. Detmers, R. G. Schwarz, G. Bode, M. F. Beardmore, A. P. Starrfield, S. Hernanz, M. Sala, G. Krautter, J. Woodward, C. E. TI XMM-NEWTON X-RAY AND ULTRAVIOLET OBSERVATIONS OF THE FAST NOVA V2491 Cyg DURING THE SUPERSOFT SOURCE PHASE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; novae, cataclysmic variables; stars: individual (V2491 Cyg, RS Oph, V4743 Sgr) ID RS-OPHIUCHI; CLASSICAL NOVA; 2006 OUTBURST; LIGHT-CURVE; SPECTRAL EVOLUTION; GRATING SPECTROMETER; SWIFT OBSERVATIONS; MODEL ATMOSPHERES; PERIODIC SIGNALS; V1494 AQUILAE AB Two XMM-Newton observations of the fast classical nova V2491 Cyg were carried out in short succession on days 39.93 and 49.62 after discovery, during the supersoft source (SSS) phase, yielding simultaneous X-ray and UV light curves and high-resolution X-ray spectra. The first X-ray light curve is highly variable, showing oscillations with a period of 37.2 minutes after an extended factor of three decline lasting similar to 3 hr, while the second X-ray light curve is less variable. The cause of the dip is currently unexplained and has most likely the same origin as similar events in the early SSS light curves of the novae V4743 Sgr and RS Oph, as it occurred on the same timescale. The oscillations are not present during the dip minimum and also not in the second observation. The UV light curves are variable but contain no dips and no period. High-resolution X-ray spectra are presented for four intervals of differing intensity. All spectra are atmospheric continua with deep absorption lines and absorption edges. Two interstellar lines of OI and NI are clearly seen at their rest wavelengths, while a large number of high-ionization absorption lines are found at blueshifts indicating an expansion velocity of 3000-3400 km s(-1), which does not change significantly during the epochs of observation. Comparisons with the slower nova V4743 Sgr and the symbiotic recurrent nova RS Oph are presented. The SSS spectrum of V4743 Sgr is much softer with broader and more complex photospheric absorption lines. The ejecta are extended, allowing us to view a larger range of the radial velocity profile. Meanwhile, the absorption lines in RS Oph are as narrow as in V2491 Cyg, but they are less blueshifted. A remarkable similarity in the continua of V2491 Cyg and RS Oph is found. The only differences are smaller line shifts and additional emission lines in RS Oph that are related to the presence of a dense stellar wind from the evolved companion. Three unidentified absorption lines are present in the X-ray spectra of all three novae, with projected rest wavelengths 26.05 angstrom, 29.45 angstrom, and 30.0 angstrom. No entirely satisfactory spectral model is currently available for the soft X-ray spectra of novae in outburst, and careful discussion of assumptions is required. C1 [Ness, J. -U.] ESA, XMM Newton Sci Operat Ctr, Madrid, Spain. [Osborne, J. P.; Page, K. L.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Dobrotka, A.] Slovak Univ Technol Bratislava, Fac Mat Sci & Technol, Inst Mat Sci, Dept Phys, Trnava 91724, Slovakia. [Dobrotka, A.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pinto, C.; Detmers, R. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Schwarz, G.] Amer Astron Soc, Washington, DC 20009 USA. [Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hernanz, M.] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, Bellaterra 08193, Barcelona, Spain. [Sala, G.] EUETIB UPC IEEC, Dept Fis & Engn Nucl, Barcelona 08036, Spain. [Krautter, J.] Heidelberg Univ, D-69117 Heidelberg, Germany. [Woodward, C. E.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. RP Ness, JU (reprint author), ESA, XMM Newton Sci Operat Ctr, Madrid, Spain. RI Hernanz, Margarita/K-1770-2014; OI Hernanz, Margarita/0000-0002-8651-7910; Pinto, Ciro/0000-0003-2532-7379 FU NASA [PF5-60039, NAS8-03060, NAS8-39073]; Chandra X-ray Center; Faculty of the European Space Astronomy Centre; MEXT; Slovak Grant Agency [VEGA-1/0520/10]; STFC; NWO, The Netherlands Organization for Scientific Research; NASA+NSF; MICINN [AYA 2008-01839/ESP]; AGAUR [2009 SGR 315]; FEDER; GS MICINN [AYA 2008-04211-C02-01, AYA 2007-66256] FX We thank the XMM-Newton SOC team for their support in scheduling and analyzing these TOO observations. Special thanks to Aitor Ibarra who supported us with the new SAS tool xmmextractor. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. J.-U.N. gratefully acknowledges support provided by NASA through Chandra Postdoctoral Fellowship grant PF5-60039, awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. A.D. and C.P. acknowledge financial support from the Faculty of the European Space Astronomy Centre. A.D. was supported in part by the Grand-in-Aid for the global COE programs on "The Next Generation of Physics, spun from Diversity and Emergence" from MEXT and also by the Slovak Grant Agency, grant VEGA-1/0520/10. K.L.P., A.P.B., and J.P.O. acknowledge support from STFC. J.J.D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center during the course of this research. SRON Netherlands is supported financially by NWO, The Netherlands Organization for Scientific Research. S.S. acknowledges support from NASA+NSF grants to ASU. We thank Rick Rudy and Dave Lynch for the information on the peak at the later NIR spectra. M.H. acknowledges support from MICINN project AYA 2008-01839/ESP, AGAUR project 2009 SGR 315 and FEDER funds, and GS MICINN projects AYA 2008-04211-C02-01 and AYA 2007-66256. NR 80 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2011 VL 733 IS 1 AR 70 DI 10.1088/0004-637X/733/1/70 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600070 ER PT J AU Perets, HB Murray-Clay, RA AF Perets, Hagai B. Murray-Clay, Ruth A. TI WIND-SHEARING IN GASEOUS PROTOPLANETARY DISKS AND THE EVOLUTION OF BINARY PLANETESIMALS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planet-disk interactions; planets and satellites: dynamical evolution and stability; planets and satellites: formation; protoplanetary disks ID KUIPER-BELT BINARIES; MINOR PLANETS; SETTLING VELOCITY; SOLAR NEBULA; BODIES; DRAG; PARTICLES; STABILITY; NEPTUNE; GROWTH AB One of the first stages of planet formation is the growth of small planetesimals and their accumulation into large planetesimals and planetary embryos. This early stage occurs much before the dispersal of most of the gas from the protoplanetary disk. Due to their different aerodynamic properties, planetesimals of different sizes and shapes experience different drag forces from the gas during this time. Such differential forces produce a wind-shearing (WISH) effect between close by, different-sized planetesimals. For any two planetesimals, a WISH radius can be considered at which the differential acceleration due to the wind becomes greater than the mutual gravitational pull between the planetesimals. We find that the WISH radius could be much smaller than the gravitational shearing radius by the star (the Hill radius). In other words, during the gas-phase of the disk, WISH could play a more important role than tidal perturbations by the star. Here, we study the WISH radii for planetesimal pairs of different sizes and compare the effects of wind and gravitational shearing (drag force versus gravitational tidal force). We then discuss the role of WISH for the stability and survival of binary planetesimals. Binaries are sheared apart by the wind if they are wider than their WISH radius. WISH-stable binaries can also inspiral, and possibly coalesce, due to gas drag. Here, we calculate the WISH radius and the gas-drag-induced merger timescale, providing stability and survival criteria for gas-embedded binary planetesimals. Our results suggest that even WISH-stable binaries may merge in times shorter than the lifetime of the gaseous disk. This may constrain currently observed binary planetesimals to have formed far from the star or at a late stage after the dispersal of most of the disk gas. We note that the WISH radius may also be important for other processes such as planetesimal erosion and planetesimal encounters and collisions in a gaseous environment. C1 [Perets, Hagai B.; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02338 USA. RP Perets, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02338 USA. RI Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X NR 25 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 MAY 20 PY 2011 VL 733 IS 1 AR 56 DI 10.1088/0004-637X/733/1/56 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600056 ER PT J AU Trump, JR Impey, CD Kelly, BC Civano, F Gabor, JM Diamond-Stanic, AM Merloni, A Urry, CM Hao, H Jahnke, K Nagao, T Taniguchi, Y Koekemoer, AM Lanzuisi, G Liu, C Mainieri, V Salvato, M Scoville, NZ AF Trump, Jonathan R. Impey, Christopher D. Kelly, Brandon C. Civano, Francesca Gabor, Jared M. Diamond-Stanic, Aleksandar M. Merloni, Andrea Urry, C. Megan Hao, Heng Jahnke, Knud Nagao, Tohru Taniguchi, Yoshi Koekemoer, Anton M. Lanzuisi, Giorgio Liu, Charles Mainieri, Vincenzo Salvato, Mara Scoville, Nick Z. TI ACCRETION RATE AND THE PHYSICAL NATURE OF UNOBSCURED ACTIVE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: nuclei; galaxies: Seyfert; quasars: emission lines; quasars: general ID BLACK-HOLE MASS; SPECTRAL ENERGY-DISTRIBUTIONS; WIDE-FIELD SURVEY; RADIATIVELY INEFFICIENT ACCRETION; EMISSION-LINE REGIONS; DIGITAL SKY SURVEY; I RADIO GALAXIES; X-RAY-EMISSION; GALACTIC NUCLEI; COSMOS FIELD AB We show how accretion rate governs the physical properties of a sample of unobscured broad-line, narrow-line, and lineless active galactic nuclei (AGNs). We avoid the systematic errors plaguing previous studies of AGN accretion rates by using accurate intrinsic accretion luminosities (L-int) from well-sampled multiwavelength spectral energy distributions from the Cosmic Evolution Survey, and accurate black hole masses derived from virial scaling relations (for broad-line AGNs) or host-AGN relations (for narrow-line and lineless AGNs). In general, broad emission lines are present only at the highest accretion rates (L-int/L-Edd > 10(-2)), and these rapidly accreting AGNs are observed as broad-line AGNs or possibly as obscured narrow-line AGNs. Narrow-line and lineless AGNs at lower specific accretion rates (L-int/L-Edd < 10(-2)) are unobscured and yet lack a broad-line region. The disappearance of the broad emission lines is caused by an expanding radiatively inefficient accretion flow (RIAF) at the inner radius of the accretion disk. The presence of the RIAF also drives L-int/L-Edd < 10(-2) narrow-line and lineless AGNs to have ratios of radio-to-optical/UV emission that are 10 times higher than L-int/L-Edd > 10(-2) broad-line AGNs, since the unbound nature of the RIAF means it is easier to form a radio outflow. The IR torus signature also tends to become weaker or disappear from L-int/L-Edd < 10(-2) AGNs, although there may be additional mid-IR synchrotron emission associated with the RIAF. Together, these results suggest that specific accretion rate is an important physical "axis" of AGN unification, as described by a simple model. C1 [Trump, Jonathan R.; Impey, Christopher D.; Gabor, Jared M.; Diamond-Stanic, Aleksandar M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kelly, Brandon C.; Civano, Francesca; Hao, Heng; Lanzuisi, Giorgio] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Merloni, Andrea; Salvato, Mara] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Urry, C. Megan] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Jahnke, Knud] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Nagao, Tohru; Taniguchi, Yoshi] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Liu, Charles] CUNY Coll Staten Isl, Astrophys Observ, Dept Engn Sci & Phys, Staten Isl, NY 10314 USA. [Liu, Charles] Amer Museum Nat Hist, New York, NY 10024 USA. [Mainieri, Vincenzo] European So Observ, D-85748 Garching, Germany. [Scoville, Nick Z.] CALTECH, Pasadena, CA 91125 USA. RP Trump, JR (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. RI Lanzuisi, Giorgio/K-4378-2013; Urry, Claudia/G-7381-2011; OI Lanzuisi, Giorgio/0000-0001-9094-0984; Urry, Claudia/0000-0002-0745-9792; Jahnke, Knud/0000-0003-3804-2137; Koekemoer, Anton/0000-0002-6610-2048 FU NSF/DDEP [0943995]; NSF [AST-0908044]; NASA [HF-51243.01, NAS 5-26555]; Space Telescope Science Institute; ESA member states FX J.R.T. acknowledges support from NSF/DDEP grant 0943995, and with C.D.I. acknowledges support from NSF grant AST-0908044. B.C.K. acknowledges support from NASA through Hubble Fellowship grant HF-51243.01, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Gordon Richards and Pat Hall provided useful comments on the manuscript, and we thank the anonymous referee for thorough suggestions that greatly improved the clarity of this work.; Based on observations with the XMM-Newton satellite, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA; the Magellan telescope, operated by the Carnegie Observatories; the ESO Very Large Telescope; 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. NR 135 TC 72 Z9 72 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 MAY 20 PY 2011 VL 733 IS 1 AR 60 DI 10.1088/0004-637X/733/1/60 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600060 ER PT J AU Xu, Y Moscadelli, L Reid, MJ Menten, KM Zhang, B Zheng, XW Brunthaler, A AF Xu, Y. Moscadelli, L. Reid, M. J. Menten, K. M. Zhang, B. Zheng, X. W. Brunthaler, A. TI TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. VIII. G12.89+0.49, G15.03-0.68 (M17), AND G27.36-0.16 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: fundamental parameters; Galaxy: kinematics and dynamics; masers; stars: formation; techniques: high angular resolution ID GHZ METHANOL MASERS; VLBA CALIBRATOR SURVEY; PROTOSTELLAR CANDIDATES; GALACTIC PLANE; CONTINUUM; KINEMATICS; SAMPLE; W3(OH) AB We report trigonometric parallaxes for three massive star-forming regions, corresponding to distances of 2.34(-0.11)(+0.13) kpc for G12.89+0.49 (also known as IRAS 18089-1732), 1.98(-0.12)(+0.14) kpc for G15.03-0.68 (in the M17 region), and 8.0(-2.0)(+4.0) kpc for G27.36-0.16. Both G12.89+0.49 and G15.03-0.68 are located in the Carina-Sagittarius spiral arm. C1 [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Moscadelli, L.] Osservatorio Arcetri, Florence, Italy. [Reid, M. J.; Brunthaler, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zhang, B.] Chinese Acad Sci, Shanghai Observ, Shanghai 200030, Peoples R China. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 20093, Peoples R China. RP Xu, Y (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. EM xuye@pmo.ac.cn OI Moscadelli, Luca/0000-0002-8517-8881 FU Chinese NSF [NSF 11073054, NSF 10733030, NSF 10703010, NSF 10621303]; NBRPC [2007CB815403] FX This work was supported by the Chinese NSF through grants NSF 11073054, NSF 10733030, NSF 10703010 and NSF 10621303, and NBRPC (973 Program) under grant 2007CB815403. NR 25 TC 51 Z9 51 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 MAY 20 PY 2011 VL 733 IS 1 AR 25 DI 10.1088/0004-637X/733/1/25 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600025 ER PT J AU Zhang, QZ Wang, K AF Zhang, Qizhou Wang, Ke TI IRDC G030.88+00.13: A TALE OF TWO MASSIVE CLUMPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (G030+00.13); ISM: kinematics and dynamics; stars: formation ID INFRARED-DARK CLOUDS; ULTRACOMPACT HII-REGIONS; STAR-FORMATION; MOLECULAR CLOUDS; H2O MASERS; SUBMILLIMETER ARRAY; DENSITY STRUCTURE; DUST CONTINUUM; GALACTIC PLANE; IRAS SOURCES AB Massive stars (M greater than or similar to 10M(circle dot)) form from collapse of parsec-scale molecular clumps. How molecular clumps fragment to give rise to massive stars in a cluster with a distribution of masses is unclear. We search for cold cores that may lead to future formation of massive stars in a massive (> 10(3)M(circle dot)), low luminosity (4.6 x 10(2) L-circle dot) infrared dark cloud (IRDC) G030.88+00.13. The NH3 data from the Very Large Array (VLA) and Green Bank Telescope reveal that the extinction feature seen in the infrared consists of two distinctive clumps along the same line of sight. The C1 clump at 97 km s(-1) coincides with the extinction in the Spitzer 8 and 24 mu m. Therefore, it is responsible for the majority of the IRDC. The C2 clump at 107 km s(-1) is more compact and has a peak temperature of 45 K. Compact dust cores and H2O masers revealed in the Submillimeter Array and VLA observations are mostly associated with C2, and none are within the IRDC in C1. The luminosity indicates that neither the C1 nor C2 clump has yet to form massive protostars. But C1 might be at a precluster forming stage. The simulated observations rule out 0.1 pc cold cores with masses above 8M(circle dot) within the IRDC. The core masses in C1 and C2 and those in high-mass protostellar objects suggest an evolutionary trend that the mass of cold cores increases over time. Based on our findings, we propose an empirical picture of massive star formation that protostellar cores and the embedded protostars undergo simultaneous mass growth during the protostellar evolution. C1 [Zhang, Qizhou; Wang, Ke] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Ke] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. RP Zhang, QZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM qzhang@cfa.harvard.edu OI Wang, Ke/0000-0002-7237-3856; Zhang, Qizhou/0000-0003-2384-6589 FU Smithsonian Institution; SMA; China Scholarship Council FX We thank Jonathan Swift for permission of using the SMA data, and the anonymous referee for comments that improve the clarity of the paper. Q.Z. acknowledges the support from the Smithsonian Institution Endowment Funds. K.W. acknowledges the support from the SMA predoctoral fellowship and the China Scholarship Council. NR 50 TC 17 Z9 17 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 MAY 20 PY 2011 VL 733 IS 1 AR 26 DI 10.1088/0004-637X/733/1/26 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 760HE UT WOS:000290314600026 ER PT J AU Ubelaker, DH Parra, RC AF Ubelaker, Douglas H. Parra, Roberto C. TI Radiocarbon analysis of dental enamel and bone to evaluate date of birth and death: Perspective from the southern hemisphere SO FORENSIC SCIENCE INTERNATIONAL LA English DT Article DE Radiocarbon; Skeletons; Time since death; Peru ID BOMB C-14; ARTIFICIAL RADIOCARBON; AGE; TURNOVER; CARBON-14; SKELETAL; TEETH AB Radiocarbon analysis was conducted on dental enamel, cortical bone and trabecular bone from four human adults from Andean Peru with known birth dates and death dates, the latter all falling within the modern bomb-curve period. Radiocarbon results were compared with known tropospheric values from the southern hemisphere. The results demonstrate that dental enamel can provide useful information regarding birth dates in consideration of known formation times of the specific teeth examined if the radiocarbon values fall within the modern bomb-curve period. Trabecular bone radiocarbon values are closer to the tropospheric values at the date of death than are values from cortical bone reflecting relative differences in the rate of bone remodeling in those tissues. Age at death also represents an important factor. Published by Elsevier Ireland Ltd. C1 [Ubelaker, Douglas H.] Smithsonian Inst, NMNH, Dept Anthropol, MRC 112, Washington, DC 20013 USA. [Parra, Roberto C.] Inst Med Legal & Ciencias Forenses Peru, Lab Biol Mol & Genet, Lima 1, Peru. RP Ubelaker, DH (reprint author), Smithsonian Inst, NMNH, Dept Anthropol, MRC 112, POB 37012, Washington, DC 20013 USA. EM ubelaked@si.edu; rparra@mpfn.gob.pe NR 35 TC 11 Z9 12 U1 1 U2 17 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD MAY 20 PY 2011 VL 208 IS 1-3 BP 103 EP 107 DI 10.1016/j.forsciint.2010.11.013 PG 5 WC Medicine, Legal SC Legal Medicine GA 756OM UT WOS:000290022600023 PM 21167668 ER PT J AU Ubelaker, DH Zarenko, KM AF Ubelaker, Douglas H. Zarenko, Kristina M. TI Adipocere: What is known after over two centuries of research SO FORENSIC SCIENCE INTERNATIONAL LA English DT Article DE Adipocere; Taphonomy; Formation; Chemical composition; Mummification ID FREE FATTY-ACIDS; CHROMATOGRAPHY-MASS SPECTROMETRY; SOFT-TISSUE; HUMAN REMAINS; GRAVE SOILS; HUMAN-BODY; IDENTIFICATION; DECOMPOSITION; MECHANISM; DEATH AB This paper reviews over two centuries of research focusing on various issues relating to adipocere. Adipocere is a crumbly, soap-like postmortem product that forms from soft tissue in a variety of environments. The timing of the formation and degradation of adipocere depends largely on the environmental circumstances. Once formed, adipocere can persist for hundreds of years, acting as a preservative. In this way, some define it as a process of mummification. This type of persistence can be useful in a forensic context as it can preserve evidence. Sustained interest in adipocere prompted many investigations into the composition and conditions of formation. More recent investigations, aided by technological advances, build upon the knowledge gained from prior studies as well as delve into the chemical composition of adipocere. This in turn provides new information on detection and documentation of constituent substances. Published by Elsevier Ireland Ltd. C1 [Ubelaker, Douglas H.; Zarenko, Kristina M.] Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, MRC 112, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, MRC 112, Washington, DC 20560 USA. EM ubelaked@si.edu; zarenkok@si.edu NR 84 TC 32 Z9 36 U1 6 U2 32 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD MAY 20 PY 2011 VL 208 IS 1-3 BP 167 EP 172 DI 10.1016/j.forsciint.2010.11.024 PG 6 WC Medicine, Legal SC Legal Medicine GA 756OM UT WOS:000290022600031 PM 21185137 ER PT J AU He, FL Hubbell, SP AF He, Fangliang Hubbell, Stephen P. TI Species-area relationships always overestimate extinction rates from habitat loss SO NATURE LA English DT Article ID DEFORESTATION; BIODIVERSITY; PATTERNS AB Extinction from habitat loss is the signature conservation problem of the twenty-first century(1). Despite its importance, estimating extinction rates is still highly uncertain because no proven direct methods or reliable data exist for verifying extinctions. The most widely used indirect method is to estimate extinction rates by reversing the species-area accumulation curve, extrapolating backwards to smaller areas to calculate expected species loss. Estimates of extinction rates based on this method are almost always much higher than those actually observed(2-5). This discrepancy gave rise to the concept of an 'extinction debt', referring to species 'committed to extinction' owing to habitat loss and reduced population size but not yet extinct during a non-equilibrium period(6,7). Here we show that the extinction debt as currently defined is largely a sampling artefact due to an unrecognized difference between the underlying sampling problems when constructing a species-area relationship (SAR) and when extrapolating species extinction from habitat loss. The key mathematical result is that the area required to remove the last individual of a species (extinction) is larger, almost always much larger, than the sample area needed to encounter the first individual of a species, irrespective of species distribution and spatial scale. We illustrate these results with data from a global network of large, mapped forest plots and ranges of passerine bird species in the continental USA; and we show that overestimation can be greater than 160%. Although we conclude that extinctions caused by habitat loss require greater loss of habitat than previously thought, our results must not lead to complacency about extinction due to habitat loss, which is a real and growing threat. C1 [He, Fangliang] Sun Yat Sen Univ, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China. [He, Fangliang] Sun Yat Sen Univ, Sch Life Sci, Guangzhou 510275, Guangdong, Peoples R China. [He, Fangliang] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. RP He, FL (reprint author), Sun Yat Sen Univ, State Key Lab Biocontrol, Guangzhou 510275, Guangdong, Peoples R China. EM fhe@mail.sysu.edu.cn; shubbell@eeb.ucla.edu FU Sun Yat-sen University; Natural Sciences and Engineering Research Council (Canada); NASA (National Aeronautics and Space Administration); US National Science Foundation FX We acknowledge the work of the principal investigators and their field assistants for collecting the field data on the large plots of the Center for Tropical Forest Science network. We are grateful to P. Gowaty, K. Gaston and M. Rosenzweig for their comments on the paper. We thank R. Condit, R. Perez and S. Agular for Barro Colorado Island, R. Valencia for Yasuni, N. Supardi Noor and R. Kassim for Pasoh, D. Thomas, D. Kenfack and G. Chuyong for Korup, W.-H. Ye for Dinghushan, I.-F. Sun and C.-F. Hseih for Fushan, X.-H. Wang for Tiantong, Z.-Q. Hao for Changbaishan and X.-L. Wang for processing the passerine data. This work was supported by Sun Yat-sen University, the Natural Sciences and Engineering Research Council (Canada), NASA (National Aeronautics and Space Administration) and the US National Science Foundation. NR 30 TC 160 Z9 174 U1 12 U2 288 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 19 PY 2011 VL 473 IS 7347 BP 368 EP 371 DI 10.1038/nature09985 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 765QA UT WOS:000290722400047 PM 21593870 ER PT J AU Feild, TS Brodribb, TJ Iglesias, A Chatelet, DS Baresch, A Upchurch, GR Gomez, B Mohr, BAR Coiffard, C Kvacek, J Jaramillo, C AF Feild, Taylor S. Brodribb, Timothy J. Iglesias, Ari Chatelet, David S. Baresch, Andres Upchurch, Garland R., Jr. Gomez, Bernard Mohr, Barbara A. R. Coiffard, Clement Kvacek, Jiri Jaramillo, Carlos TI Fossil evidence for Cretaceous escalation in angiosperm leaf vein evolution SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE angiosperm evolution; plant evolution; transpiration; tropical rainforest; venation ID FLOWERING PLANTS; RAIN-FOREST; DIVERSITY; RADIATION; CAPACITY; VENATION; ECOLOGY; RECORD AB The flowering plants that dominate modern vegetation possess leaf gas exchange potentials that far exceed those of all other living or extinct plants. The great divide in maximal ability to exchange CO(2) for water between leaves of nonangiosperms and angiosperms forms the mechanistic foundation for speculation about how angiosperms drove sweeping ecological and biogeo-chemical change during the Cretaceous. However, there is no empirical evidence that angiosperms evolved highly photosynthetically active leaves during the Cretaceous. Using vein density (D(V)) measurements of fossil angiosperm leaves, we show that the leaf hydraulic capacities of angiosperms escalated several-fold during the Cretaceous. During the first 30 million years of angiosperm leaf evolution, angiosperm leaves exhibited uniformly low vein D(V) that overlapped the D(V) range of dominant Early Cretaceous ferns and gymnosperms. Fossil angiosperm vein densities reveal a subsequent biphasic increase in D(V). During the first mid-Cretaceous surge, angiosperm D(V) first surpassed the upper bound of D(V) limits for nonangiosperms. However, the upper limits of D(V) typical of modern megathermal rainforest trees first appear during a second wave of increased D(V) during the Cretaceous-Tertiary transition. Thus, our findings provide fossil evidence for the hypothesis that significant ecosystem change brought about by angiosperms lagged behind the Early Cretaceous taxonomic diversification of angiosperms. C1 [Feild, Taylor S.] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. [Brodribb, Timothy J.] Univ Tasmania, Dept Plant Sci, Hobart, Tas 7001, Australia. [Iglesias, Ari] Univ Nacl La Plata, Fac Ciencias Nat & Museo, RA-1900 La Plata, Argentina. [Chatelet, David S.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Baresch, Andres; Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Panama. [Upchurch, Garland R., Jr.] Texas State Univ, Dept Biol, San Marcos, TX 78666 USA. [Gomez, Bernard] Univ Lyon 1, CNRS, UMR 5125, F-69622 Villeurbanne, France. [Mohr, Barbara A. R.; Coiffard, Clement] Museum Nat Hist, D-10115 Berlin, Germany. [Kvacek, Jiri] Natl Museum, Prague, Czech Republic. RP Feild, TS (reprint author), Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. EM hedyosmum@gmail.com RI Coiffard, Clement/C-8405-2012; Gomez, Bernard/B-1394-2012; Brodribb, Tim/C-6797-2013 OI Gomez, Bernard/0000-0003-1691-0634; Brodribb, Tim/0000-0002-4964-6107 FU National Science Foundation [DEB-0919071, IOB-0714156]; Consejo Nacional de Investigaciones Cientificas y Tecnicas FX We thank Lawong Balun for assistance during field work. Helpful comments were provided by Patrick Baker, Kevin Boyce, David Beerling, Claire Feild, Peter Wilf, and Hubert Feild. We thank Mauro Passalia, Griselda Puebla, Alejandra Gandolfo, and Elizabeth Hermsen for providing fossil leaf photography for DV measurements. This work was supported by National Science Foundation Grant DEB-0919071, Consejo Nacional de Investigaciones Cientificas y Tecnicas (A. I.), and National Science Foundation Grant IOB-0714156 (to T.S.F.). NR 37 TC 76 Z9 79 U1 6 U2 64 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 17 PY 2011 VL 108 IS 20 BP 8363 EP 8366 DI 10.1073/pnas.1014456108 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 765OZ UT WOS:000290719600058 PM 21536892 ER PT J AU Hong, T AF Hong, Terry TI The Paradise Bird Tattoo 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 MAY 15 PY 2011 VL 136 IS 9 BP 75 EP 75 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 767BF UT WOS:000290829600036 ER PT J AU Cottrell, E Kelley, KA AF Cottrell, Elizabeth Kelley, Katherine A. TI The oxidation state of Fe in MORB glasses and the oxygen fugacity of the upper mantle SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE oxygen fugacity; oxidation state; MORB; mantle; iron; XANES ID FERRIC-FERROUS EQUILIBRIA; SILICATE-GLASSES; REDOX STATES; SOURCE REGIONS; KILAUEA VOLCANO; BASALTIC MAGMAS; CARBON-DIOXIDE; IRON; MELTS; PRESSURE AB Micro-analytical determination of Fe3+/Sigma Fe ratios in mid-ocean ridge basalt (MORB) glasses using micro X-ray absorption near edge structure (mu-XANES) spectroscopy reveals a substantially more oxidized upper mantle than determined by previous studies. Here, we show that global MORBs yield average Fe3+/Sigma Fe ratios of 0.16 +/- 0.01 (n=103), which trace back to primary MORB melts equilibrated at the conditions of the quartz-fayalite-magnetite (QFM) buffer. Our results necessitate an upward revision of the Fe3+/Sigma Fe ratios of MORBs, mantle oxygen fugacity, and the ferric iron content of the mantle relative to previous wet chemical determinations. We show that only 0.01 (absolute, or <10%) of the difference between Fe3+/Sigma Fe ratios determined by micro-colorimety and XANES can be attributed to the Mossbauer-based XANES calibration. The difference must instead derive from a bias between micro-colorimetry performed on experimental vs. natural basalts. Co-variations of Fe3+/Sigma Fe ratios in global MORB with indices of low-pressure fractional crystallization are consistent with Fe3+ behaving incompatibly in shallow MORB magma chambers. MORB Fe3+/Sigma Fe ratios do not, however, vary with indices of the extent of mantle melting (e.g., Na2O(8)) or water concentration. We offer two hypotheses to explain these observations: The bulk partition coefficient of Fe3+ may be higher during peridotite melting than previously thought, and may vary with temperature, or redox exchange between sulfide and sulfate species could buffer mantle melting at similar to QFM. Both explanations, in combination with the measured MORB Fe3+/Sigma Fe ratios, point to a fertile MORB source with greater than 0.3 wt.% Fe2O3. Published by Elsevier B.V. C1 [Cottrell, Elizabeth] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, 10th & Constitut Ave, Washington, DC 20560 USA. [Kelley, Katherine A.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. RP Cottrell, E (reprint author), Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, 10th & Constitut Ave, Washington, DC 20560 USA. EM CottrellE@si.edu RI Kelley, Katherine/J-3728-2013 OI Kelley, Katherine/0000-0002-7516-2683 FU NSF [OCE-0644625, EAR-0841108, EAR-0841006]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-98CH10886]; Smithsonian's Scholarly Studies Program; URI ADVANCE fellowship FX This work would not have been possible without the generosity of Becky Lange at the University of Michigan, Bjorn Mysen at the Geophysical Laboratory, and Tony Lanzirotti at the University of Chicago and NSLS. Discussions with Becky Lange, Charlie Langmuir, and Marc Hirschmann were invaluable during preparation of the manuscript and we benefited greatly from reviews by Dante Canil and Claude Herzberg. We gratefully acknowledge the following individuals and institutions that provided samples: The Division of Petrology and Volcanology at the Smithsonian Institution, The Graduate School of Oceanography at URI, Victor Kress, Charlie Langmuir, Peter Michael, Jim Gill, Ian Carmichael, David Christie, and David Clague. NSF Award OCE-0644625 provided curatorial support for marine geological samples at the University of Rhode Island. We thank the students, staff and volunteers at the Smithsonian and URI who contributed to this work. Use of the National Synchrotron Light Source, Brookhaven National Laboratory, was supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, under Contract No. DE-AC02-98CH10886. We acknowledge support from Smithsonian's Scholarly Studies Program (EC), a URI ADVANCE fellowship (KK) and NSF awards EAR-0841108 (KK) and EAR-0841006 (EC). NR 77 TC 107 Z9 110 U1 6 U2 83 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD MAY 15 PY 2011 VL 305 IS 3-4 BP 270 EP 282 DI 10.1016/j.epsl.2011.03.014 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 773AS UT WOS:000291280000002 ER PT J AU Hall, JS Ashton, MS Garen, EJ Jose, S AF Hall, Jefferson S. Ashton, Mark S. Garen, Eva J. Jose, Shibu TI The ecology and ecosystem services of native trees: Implications for reforestation and land restoration in Mesoamerica SO FOREST ECOLOGY AND MANAGEMENT LA English DT Editorial Material DE Agroforestry; Biodiversity; Carbon sequestration; Local knowledge; Soil; Tropical hydrology ID COSTA-RICA; TROPICAL FORESTS; CARBON STORAGE; HUMID TROPICS; PLANTATIONS; GROWTH; PANAMA; DEFORESTATION; BIODIVERSITY; PERFORMANCE AB Tropical forests provide a variety of goods and services to humanity. Although efforts to protect and manage these forests have increased in recent decades, forest loss continues. The last decade and a half has seen considerable research on reforestation with native species in Mesoamerica, including both biophysical and social aspects. Advances in knowledge have led to increasingly sophisticated reforestation treatments as well as novel ways of deriving forest goods and services from human dominated landscapes. This Special Issue includes articles produced as the result of a conference held in Panama City, Panama in January 2010 with the goal to summarize the state of knowledge of native species reforestation and associated ecosystems services in Mesoamerica. The introduction concludes with a call for continued research, including a mechanistic understanding of tree interactions with the biophysical environment in order to advance or knowledge of ecosystem services and their interactions. Results from these and other studies aimed at socioeconomic aspects of reforestation are critical to land use planning. (C) 2010 Elsevier B.V. All rights reserved. C1 [Hall, Jefferson S.] Smithsonian Trop Res Inst, Agua Salud Project, Balboa, Ancon, Panama. [Garen, Eva J.] Yale Univ, Sch Forestry & Environm Studies, Environm Leadership Training Initiat, New Haven, CT 06511 USA. [Jose, Shibu] Univ Missouri, Sch Nat Resources, Columbia, MO 65211 USA. [Jose, Shibu] Univ Missouri, Ctr Agroforestry, Columbia, MO 65211 USA. RP Hall, JS (reprint author), Smithsonian Trop Res Inst, Agua Salud Project, Apartado 0843-03092, Balboa, Ancon, Panama. EM hallje@si.edu NR 82 TC 25 Z9 28 U1 10 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 MAY 15 PY 2011 VL 261 IS 10 SI SI BP 1553 EP 1557 DI 10.1016/j.foreco.2010.12.011 PG 5 WC Forestry SC Forestry GA 768HJ UT WOS:000290924400001 ER PT J AU van Breugel, M Hall, JS Craven, DJ Gregoire, TG Park, A Dent, DH Wishnie, MH Mariscal, E Deago, J Ibarra, D Cedeno, N Ashton, MS AF van Breugel, Michiel Hall, Jefferson S. Craven, Dylan J. Gregoire, Timothy G. Park, Andrew Dent, Daisy H. Wishnie, Mark H. Mariscal, Emilio Deago, Jose Ibarra, Diogenes Cedeno, Norma Ashton, Mark S. TI Early growth and survival of 49 tropical tree species across sites differing in soil fertility and rainfall in Panama SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Reforestation; Soil fertility; Rainfall; Growth; Survival; Species screening trial ID COSTA-RICA; VEGETATION RECRUITMENT; FLORISTIC COMPOSITION; CARBON SEQUESTRATION; FOREST PLANTATIONS; CLIMATIC GRADIENT; EDAPHIC FACTORS; BIODIVERSITY; RESTORATION; PERFORMANCE AB Reforestation in the tropics takes place across a wide variety of edaphic and climatic conditions. Reforestation trials have demonstrated that edaphic conditions may have a strong effect on species growth and survival. However it is unclear how the relative importance of soil conditions influences species survival and growth under varying amounts of rainfall and lengths of dry season. Two-year growth and mortality of 49 tree species were evaluated in four sites across Panama, representing a soil fertility-rainfall matrix. Despite strong contrasts in environmental conditions, 65% of individual species did not show consistent differences in growth between high- and low-fertility sites or between wet and dry sites. However, early growth and survival were more strongly affected by soil fertility than by rainfall patterns for the second-largest group; 30% of the species grew significantly better in both high-fertility sites than in both low-fertility sites, compared to 6% in both wet sites vs. both dry sites. In the two high-fertility sites, growth of 47% and 69% of the species was better than their across-site means. On the other hand, 55% and 73% of the species grew significantly slower than their across-site averages in the two low-fertility sites. Survival did not appear to be associated to either soil fertility or rainfall. In each site, only a few species had a significantly higher or lower within-site survival than across-site survival. Diversifying the choice of tree species increases the options for reforestation strategies that match species characteristics to local site conditions and to the objectives and management possibilities of landholders. Testing the performance of potential species under different site conditions in screening trials is paramount, both to inform selection from among the vast diversity of tree species in the tropics that show good growth and survival under different local site conditions and to filter out unsuitable species and avoid early failure of the reforestation effort. (C) 2010 Elsevier B.V. All rights reserved. C1 [van Breugel, Michiel; Hall, Jefferson S.; Craven, Dylan J.; Dent, Daisy H.; Wishnie, Mark H.; Mariscal, Emilio; Deago, Jose; Ibarra, Diogenes; Cedeno, Norma] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa, Ancon, Panama. [Craven, Dylan J.; Gregoire, Timothy G.; Ashton, Mark S.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Park, Andrew] Univ Winnipeg, Dept Biol, CFIR, Winnipeg, MB R3B 2E9, Canada. 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; Dent, Daisy/L-3549-2016; OI Craven, Dylan/0000-0003-3940-833X; Dent, Daisy/0000-0002-1219-7344; van Breugel, Michiel/0000-0003-2778-7803 FU Frank Levinson Family Foundation; Grantham Family Foundation; Frank Levinson Donor-Advised Fund at the Peninsula Community Foundation; Yale University; STRI FX This article is a scientific contribution of the Native Species Reforestation Project (PRORENA), a collaborative research program led by the Center for Tropical Forest Science at the Smithsonian Tropical Research Institute (STRI) and Yale School of Forestry and Environmental Studies. The species selection trials in Soberania and Rio Hato were at sites managed by PRORENA under agreement with Panama's National Environmental Authority (ANAM), and the Playa Venado and Las Lajas sites were on land made available by Mr. Ovidio Dias and of ForestFinance, respectively. This research was possible through generous financial support of the Frank Levinson Family Foundation, the Grantham Family Foundation, the Frank Levinson Donor-Advised Fund at the Peninsula Community Foundation, Yale University and STRI. MvB and JSH acknowledge the HSBC Climate Partnership for financial support during analysis and write-up. We like to thank the many people that took care of the seedling production in the nursery, maintained the plantations and assisted with field measurements and data entry. NR 89 TC 26 Z9 28 U1 3 U2 45 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2011 VL 261 IS 10 SI SI BP 1580 EP 1589 DI 10.1016/j.foreco.2010.08.019 PG 10 WC Forestry SC Forestry GA 768HJ UT WOS:000290924400004 ER PT J AU Potvin, C Mancilla, L Buchmann, N Monteza, J Moore, T Murphy, M Oelmann, Y Scherer-Lorenzen, M Turner, BL Wilcke, W Zeugin, F Wolf, S AF Potvin, Catherine Mancilla, Lady Buchmann, Nina Monteza, Jose Moore, Tim Murphy, Meaghan Oelmann, Yvonne Scherer-Lorenzen, Michael Turner, Benjamin L. Wilcke, Wolfgang Zeugin, Fabienne Wolf, Sebastian TI An ecosystem approach to biodiversity effects: Carbon pools in a tropical tree plantation SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Tropical tree plantation; Carbon pools and fluxes; Diversity effect; Ecosystem carbon storage ID SPECIES-DIVERSITY; FOREST ECOSYSTEM; SOIL; PRODUCTIVITY; STORAGE; MANAGEMENT; NITROGEN; BALANCE; PANAMA; CO2 AB This paper presents a synthesis of experiments conducted in a tropical tree plantation established in 2001 and consisting of 22 plots of 45 m x 45 m with either one, three or six native tree species. We examined the changes in carbon (C) pools (trees, herbaceous vegetation, litter, coarse woody debris (CWD), and mineral topsoil at 0-10 cm depth) and fluxes (decomposition of CWD and litter, as well as soil respiration) both through time and among diversity levels. Between 2001 and 2009 the aboveground C pools increased, driven by trees. Across diversity levels, the mean observed aboveground C pool was 7.9 +/- 2.5 Mg ha(-1) in 2006 and 20.4 +/- 7.4 Mg ha(-1) in 2009, a 158% increase. There was no significant diversity effect on the observed aboveground C pool, but we found a significant decrease in the topsoil C pool, with a mean value of 34.5 +/- 2.4 Mg ha(-1) in 2001 and of 25.7 +/- 5.7 Mg ha(-1) in 2009 (F(1,36) = 52.12, p <0.001). Assuming that the biomass C pool in 2001 was negligible (<1 Mg ha-1), then the plantation gained in C, on average, 20 and lost 9 Mg ha-1 in biomass and soil respectively, for an overall gain of similar to 11 Mg ha(-1) over 8 years. Across the entire data set, we uncovered significant effects of diversity on CWD decomposition (diversity: F(2,393) = 15.93, p < 0.001) and soil respiration (monocultures vs mixtures: t = 15.35, df =11, p < 0.05) and a marginally significant time x diversity interaction on the loss of total C from the mineral topsoil pool (see above). Monthly CWD decomposition was significantly faster in monocultures (35.0 +/- 24.1%) compared with triplets (31.3 +/- 21.0%) and six-species mixtures (31.9 +/- 26.8%), while soil respiration was higher in monocultures than in mixtures (t = 15.35, df = 11,p <0.001). Path analyses showed that, as diversity increases, the links among the C pools and fluxes strengthen significantly. Our results demonstrate that tree diversity influences the processes governing the changes in C pools and fluxes following establishment of a tree plantation on a former pasture. We conclude that the choice of tree mixtures for afforestation in the tropics can have a marked influence on C pools and dynamics. (C) 2010 Elsevier B.V. All rights reserved. C1 [Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Potvin, Catherine; Mancilla, Lady; Monteza, Jose; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Buchmann, Nina; Zeugin, Fabienne; Wolf, Sebastian] Swiss Fed Inst Technol, Inst Plant Anim & Agroecosyst Sci, CH-8092 Zurich, Switzerland. [Oelmann, Yvonne] Univ Koblenz Landau, Inst Integrated Nat Sci, D-56070 Koblenz, Germany. [Wilcke, Wolfgang] Univ Bern, Inst Geog, CH-3012 Bern, Switzerland. [Scherer-Lorenzen, Michael] Univ Freiburg, Fac Biol, D-79104 Freiburg, Germany. [Moore, Tim; Murphy, Meaghan] McGill Univ, Dept Geog, Montreal, PQ H3A 2K6, Canada. RP Potvin, C (reprint author), McGill Univ, Dept Biol, 1205 Dr Penfield, Montreal, PQ H3A 1B1, Canada. EM catherine.potvin@mcgill.ca RI Turner, Benjamin/E-5940-2011; Buchmann, Nina/E-6095-2011; Wolf, Sebastian/B-4580-2010; Oelmann, Yvonne/J-8730-2016; Wilcke, Wolfgang/P-4620-2016 OI Turner, Benjamin/0000-0002-6585-0722; Wolf, Sebastian/0000-0001-7717-6993; Oelmann, Yvonne/0000-0003-3513-6568; Wilcke, Wolfgang/0000-0002-6031-4613 FU Ministere de la Recherche, de la Science et de la Technologie du Quebec; Natural Sciences and Engineering Council of Canada; German Research Foundation [DFG Wi 1601/6-1]; North-South Centre of ETH Zurich, Switzerland; Swiss National Science Foundation [3100A0-110031/1] FX The Sardinilla plantation was established with the help to a grant from the Ministere de la Recherche, de la Science et de la Technologie du Quebec. Continuous support from the Smithsonian Tropical Research Institute was invaluable in our ability to maintain this site on the long term. C.P. acknowledges the support from a Discovery grant of the Natural Sciences and Engineering Council of Canada. Jose Luis Bonnilla collected litter fall and analyzed the litter decomposition bags in 2005. In 2007 and 2008 litter fall and the herbaceous vegetation were sampled by Simone Tapernon, Timo Mark, and Lisa Werther, while Volker Hahn helped in measuring soil respiration. This research was funded by the German Research Foundation (DFG Wi 1601/6-1) which we gratefully acknowledge. N.B. and S.W. appreciate funding from the North-South Centre (former Swiss Centre for International Agriculture) of ETH Zurich, Switzerland. Financial support was provided to M.S.-L. and Jan Jansa (ETH Zurich) by the Swiss National Science Foundation (3100A0-110031/1). NR 48 TC 27 Z9 29 U1 5 U2 64 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2011 VL 261 IS 10 SI SI BP 1614 EP 1624 DI 10.1016/j.foreco.2010.11.015 PG 11 WC Forestry SC Forestry GA 768HJ UT WOS:000290924400008 ER PT J AU Neumann-Cosel, L Zimmermann, B Hall, JS van Breugel, M Elsenbeer, H AF Neumann-Cosel, Luisa Zimmermann, Beate Hall, Jefferson S. van Breugel, Michiel Elsenbeer, Helmut TI Soil carbon dynamics under young tropical secondary forests on former pastures-A case study from Panama SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Soil carbon; Secondary forest; Pasture; Land-use change; C sequestration; Panama ID NORTHEASTERN COSTA-RICA; LAND-USE CHANGE; ORGANIC-CARBON; BRAZILIAN AMAZONIA; SUBTROPICAL SOILS; NUTRIENT DYNAMICS; SEQUESTRATION; STOCKS; REFORESTATION; CONVERSION AB Secondary forests are gaining increased importance in tropical landscapes and have recently been reported to act as potential belowground carbon sinks. While economic interest in the management of secondary forests to mitigate carbon emissions is rising, the dynamics of soil carbon stocks under these ecosystems remain poorly understood. Recent studies report conflicting results concerning soil carbon trends as well as multiple confounding factors (e.g. soil type, topography and land-use history) affecting these trends. In this study, organic carbon stocks were measured in the mineral soil up to 20 cm depth of at 24 active pastures, 5-8-year-old, and 12-15-year-old secondary forest sites on former pastures. Additionally, we estimated carbon stocks under a 100-year-old secondary forest and compared them to those of nearby mature forests. Abiotic conditions in the study area were homogenous, enabling us to isolate the effect of land-use change on soil organic carbon stocks. Contrary to our expectations, soil carbon stocks in the top 10 cm did not change with young secondary forest development. Pasture soils stored 24.8 +/- 2.9 Mg ha(-1) carbon (mean +/- standard error) in the top 10 cm, and no accumulation of soil carbon was apparent during the first 15 years of secondary succession. Soil carbon stocks under 100-year-old secondary forests, averaging 43.0 +/- 7.9 Mg ha(-1) (mean +/- standard error), were clearly higher than those recorded at younger sites and approached levels of soil carbon stocks under mature forests. These data indicate that soil carbon stocks in this region of Panama are not affected by the land-use transition from pasture to young secondary regrowth. However, an increase of soil carbon storage might be possible over a longer period of time. Our results support trends observed in other tropical areas and highlight the importance of environmental conditions such as soil properties rather than land-use transitions on soil carbon dynamics. While our understanding of organic carbon dynamics in tropical soils remains limited, these results underscore the challenges of undertaking short-term reforestation projects with the expectation of increasing soil carbon sequestration. 2010 Elsevier BM. All rights reserved. C1 [Neumann-Cosel, Luisa; Zimmermann, Beate; Elsenbeer, Helmut] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany. [Zimmermann, Beate; Hall, Jefferson S.; van Breugel, Michiel; Elsenbeer, Helmut] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Neumann-Cosel, L (reprint author), Univ Potsdam, Inst Earth & Environm Sci, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany. EM luneuman@uni-potsdam.de RI Zimmermann, Beate/B-5164-2012; OI van Breugel, Michiel/0000-0003-2778-7803 FU HSBC; German Academic Exchange Service (DAAD) STRI; ACP; Frank Levinson family foundation; Motta family foundation FX The Agua Salud Project (ASP) is a collaboration among the Smithsonian Tropical Research Institute, the Panama Canal Authority (ACP) and the National Environmental Authority of Panama (ANAM). The ASP would not be possible without collaboration with Robert Stallard, USGS, and Fred Ogden, University of Wyoming. The study is financially supported by the HSBC climate partnership, with additional funding from the German Academic Exchange Service (DAAD) STRI, ACP, the Frank Levinson family foundation and the Motta family foundation. L. Neumann-Cosel acknowledges partial support of the Heinrich-Boll foundation, Germany. We thank Daniela Weber and Federico Davies and the staff of the Smithsonian Tropical Research Institute on BCI and at Tupper campus, Ancon for logistical support, as well as Yadira Montilla, Carlos Diaz, Nathaly Guerrero, Kaleem Fernandez and Guillermo Fernandez for their help in field and laboratory. Sibylle Hassler greatly improved this manuscript by providing constructive comments. Thanks to Murray Lark for invaluable support with statistical concerns and to Egbert G. Leigh, as well as many other scientists in the STRI community, for advice and inspiring discussions. We thank two anonymous reviewers for helpful comments on an earlier version of this manuscript. NR 62 TC 18 Z9 22 U1 0 U2 45 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2011 VL 261 IS 10 SI SI BP 1625 EP 1633 DI 10.1016/j.foreco.2010.07.023 PG 9 WC Forestry SC Forestry GA 768HJ UT WOS:000290924400009 ER PT J AU Hassler, SK Zimmermann, B van Breugel, M Hall, JS Elsenbeer, H AF Hassler, Sibylle K. Zimmermann, Beate van Breugel, Michiel Hall, Jefferson S. Elsenbeer, Helmut TI Recovery of saturated hydraulic conductivity under secondary succession on former pasture in the humid tropics SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Land cover change; Forest; Land use; Overland flow; Soil hydrology; Ecosystem services ID SOIL PHYSICAL-PROPERTIES; OVERLAND-FLOW GENERATION; HYDROLOGICAL CONSEQUENCES; LAND MANAGEMENT; NEW-ZEALAND; FOREST; WATER; DYNAMICS; IMPACTS; DISTURBANCE AB Landscapes in the humid tropics are undergoing a continuous change in land use. Deforestation is still taking its toll on forested areas, but at the same time more and more secondary forests emerge where formerly agricultural lands and pastures are being abandoned. Regarding soil hydrology, the extent to which secondary succession can recover soil hydrological properties disturbed by antecedent deforestation and pasture use is yet poorly understood. We investigated the effect of secondary succession on saturated hydraulic conductivity (Ks) at two soil depths (0-6 and 6-12 cm) using a space-for-time approach in a landscape mosaic in central Panama. The following four land-use classes were studied: pasture (P), secondary forest of 5-8 years of age (SF5), secondary forest of 12-15 years of age (SF12) and secondary forest of more than 100 years of age (SF100), each replicated altogether four times in different micro-catchments across the study region. The hydrological implications of differences in Ks in response to land-use change with land use, especially regarding overland flow generation, were assessed via comparisons with rainfall intensities. Recovery of Ks could be detected in the 0-6 cm depth after 12 years of secondary succession: P and SF5 held similar Ks values, but differed significantly (alpha = 0.05) from SF12 and SF100 which in turn were indistinguishable. Variability within the land cover classes was large but, due to sufficient replication in the study, Ks recovery could be detected nonetheless. Ks in the 6-12 cm depth did not show any differences between the land cover classes; only Ks of the uppermost soil layer was affected by land-use changes. Overland flow - as inferred from comparisons of Ks with rainfall intensities - is more likely on P and SF5 sites compared to SF12 and 5E100 for the upper sample depth; however, generally low values at the 6-12 cm depth are likely to impede vertical percolation during high rainfall intensities regardless of land use. We conclude that Ks can recover from pasture use under secondary succession up to pre-pasture levels, but the process may take more than 8 years. In order to gain comprehensive understanding of Ks change with land use and its hydrological implications, more studies with detailed land-use histories and combined measurements of Ks, overland flow, precipitation and throughfall are essential. (C) 2010 Elsevier B.V. All rights reserved. C1 [Hassler, Sibylle K.; Zimmermann, Beate; Elsenbeer, Helmut] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany. [Zimmermann, Beate; van Breugel, Michiel; Hall, Jefferson S.; Elsenbeer, Helmut] 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 Zimmermann, Beate/B-5164-2012; Hassler, Sibylle/N-6342-2013; OI Hassler, Sibylle/0000-0001-5411-8491; van Breugel, Michiel/0000-0003-2778-7803 FU HSBC; STRI; ACP; Frank Levinson family foundation; Motta family foundation FX The Agua Salud Project (ASP), in which this study was partly undertaken, is a collaboration among the Panama Canal Authority (ACP), the National Environmental Authority of Panama (ANAM), and the Smithsonian Tropical Research Institue (STRI). It is financially supported by the HSBC climate partnership (HCP), with additional funding from STRI, ACP, the Frank Levinson family foundation, and the Motta family foundation. The ASP would not be possible without collaboration of Robert Stallard, US. Geological Survey, and Fred Ogden, University of Wyoming. NR 61 TC 37 Z9 39 U1 3 U2 46 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 EI 1872-7042 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2011 VL 261 IS 10 SI SI BP 1634 EP 1642 DI 10.1016/j.foreco.2010.06.031 PG 9 WC Forestry SC Forestry GA 768HJ UT WOS:000290924400010 ER PT J AU Craven, D Dent, D Braden, D Ashton, MS Berlyn, GP Hall, JS AF Craven, D. Dent, D. Braden, D. Ashton, M. S. Berlyn, G. P. Hall, J. S. TI Seasonal variability of photosynthetic characteristics influences growth of eight tropical tree species at two sites with contrasting precipitation in Panama SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Native tree species; Reforestation; Panama; Eco-physiology; Seasonality; Photosynthesis; Relative growth rate (RGR) ID WOOD SPECIFIC-GRAVITY; RAIN-FOREST; ABANDONED PASTURE; WATER RELATIONS; NATIVE TREES; LIFE-HISTORY; LEAF TRAITS; COSTA-RICA; LIGHT; DROUGHT AB Relative to closed-canopy tropical forests, tree seedlings planted in open grown areas are exposed to higher light intensity, air temperatures, vapor pressure deficit, and greater seasonal fluxes of plant available water than mature tropical forests. The species-specific adaptive capacity to respond to variable precipitation and seasonality in open grown conditions, therefore, is likely to affect species performance in large-scale reforestation efforts. In the present study, we compared the photosynthetic characteristics of eight tropical tree species within and between seasons at two study sites with contrasting dry season intensities. All species except Pseudosamanea guachapele reduced leaf physiological function between the wet and dry seasons. The contrasting severity of seasonal drought stress at the study sites constrained growth rates and photosynthetic characteristics differently. Variation of photosynthetic characteristics at the species level was high, particularly in the dry season. Faster growing species at the less seasonal site, Terminalia amazonia, Inga punctata, Colubrina glandulosa, and Acacia mangium, exhibited a greater adaptive capacity than the other species to down-regulate leaf photosynthesis between seasons. As the dry season was more severe at the more seasonal site, most species strongly reduced physiological function regardless of relative growth rates, except two species (Tectona grandis and P. guachapele) with widespread distributions and relatively high drought tolerance. Our results underscore the need to consider seasonal drought tolerance when selecting tree species for specific reforestation sites. (C) 2010 Elsevier B.V. All rights reserved. C1 [Craven, D.; Braden, D.; Ashton, M. S.; Berlyn, G. P.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Craven, D.; Dent, D.; Ashton, M. S.; Hall, J. S.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Native Species Reforestat Project PRORENA, Balboa, Ancon, Panama. RP Craven, D (reprint author), Yale Univ, Sch Forestry & Environm Studies, 370 Prospect St, New Haven, CT 06511 USA. EM dylan.craven@yale.edu RI Craven, Dylan/K-2717-2012 OI Craven, Dylan/0000-0003-3940-833X FU Frank Levinson Donor-Advised Fund at the Peninsula Community Foundation; Grantham Foundation; School of Forestry and Environmental Studies, Yale University FX We are indebted to the researchers, staff, and students of PRORENA, a joint program of the School of Forestry and Environmental Studies, Yale University, and the Smithsonian Tropical Research Institute's Center for Tropical Forest Science, for designing, establishing, and maintaining this experiment since 2003. Funding to establish and maintain PRORENA has been generously provided by the Frank Levinson Donor-Advised Fund at the Peninsula Community Foundation, the Grantham Foundation, and the School of Forestry and Environmental Studies, Yale University. The comments of Michiel van Breugel and two anonymous reviewers considerably improved previous versions of this manuscript. The authors would like to thank the following people, whose hard work, sage advice, and warm friendship made the present study possible: Michiel van Breugel, Christian Salas, Mark H. Wishnie, Klaus Winter, Lucas Cernusak, Emilio Mariscal, Norma Cedeno, Jose Deago, Diogenes Ibarra, Leidy Martinez, Marcos Valdez, Julio Nunez, Rolando Perez, Adriana Sautu, and Marla Diaz. DC received financial support during data collection, analysis, and write up from the Tropical Resources Institute at Yale University, the Environmental Leadership Training Initiative (ELTI), and Sallie Mae. NR 70 TC 16 Z9 18 U1 6 U2 39 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2011 VL 261 IS 10 SI SI BP 1643 EP 1653 DI 10.1016/j.foreco.2010.09.017 PG 11 WC Forestry SC Forestry GA 768HJ UT WOS:000290924400011 ER PT J AU Murgueitio, E Calle, Z Uribe, F Calle, A Solorio, B AF Murgueitio, Enrique Calle, Zoraida Uribe, Fernando Calle, Alicia Solorio, Baldomero TI Native trees and shrubs for the productive rehabilitation of tropical cattle ranching lands SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Silvopastoral systems (SPS); Intensive silvopastoral systems (ISS); Leucaena leucocephala; Conservation corridors; Connectivity; Focal species; Payment for environmental services (PES); Sustainable cattle ranching; Agroforestry for animal production ID AGRICULTURAL LANDSCAPES; BIODIVERSITY CONSERVATION; SILVOPASTORAL SYSTEM; COUNTRYSIDE BIOGEOGRAPHY; COSTA-RICA; COLOMBIA; SERVICES; MATRIX; BRAZIL; SOILS AB Extensive cattle production currently occupies more than 27% of the rural landscapes in Latin America, and continues to expand. This activity, deeply rooted in the culture and rural economy of the region, requires an urgent transformation if it is to become both more efficient and environmentally friendly. Silvopastoral systems that incorporate native trees and shrubs are instrumental for the productive rehabilitation of cattle production and for biodiversity conservation in agricultural landscapes. We discuss research progress and adoption of intensive silvopastoral systems in Colombia and Mexico. Intensive silvopastoral systems (ISS) are a sustainable form of agroforestry for livestock production that combines fodder shrubs planted at high densities (more than 10,000 plants ha(-1)), trees and palms, and improved pastures. High stocking and the natural production of milk and meat in these systems are achieved through rotational grazing with electric fencing and a permanent supply of water for the cattle. While milk and meat production and cattle reproduction are enhanced, production costs decline as external inputs are replaced by natural processes related to fertility and biological control. We also discuss the importance of the ISS with native trees for climate change adaptation and mitigation, the barriers for their adoption, and how these have been successfully addressed using payment for environmental services, special credits and technical assistance. Finally, we highlight the need for enhancing landscape connectivity by integrating SPS to conservation corridors with native species to promote biodiversity conservation and other environmental services demanded by society. (C) 2010 Elsevier B.V. All rights reserved. C1 [Murgueitio, Enrique; Calle, Zoraida; Uribe, Fernando] CIPAV Ctr Invest Sistemas Sostenibles Prod Agr, Cali, Colombia. [Calle, Alicia] Smithsonian Trop Res Inst, New Haven, CT 06511 USA. [Calle, Alicia] Yale Univ, Sch Forestry & Environm Studies, Environm Leadership & Training Initiat, New Haven, CT 06511 USA. [Solorio, Baldomero] Fdn Produce Michoacan, Morelia 58070, Michoacan, Mexico. RP Calle, Z (reprint author), CIPAV Ctr Invest Sistemas Sostenibles Prod Agr, Carrera 25 6-62, Cali, Colombia. EM Zoraida.Calle@cipav.org.co FU World Bank; Global Environmental Facility FX Several researchers from CIPAV have made important contributions to the development of intensive silvopastoral systems: Cesar Cuartas, Juan F. Naranjo, Carlos H. and Enrique J. Molina, Alvaro Zapata, Carolina Giraldo, Julian Chara and Luis Solarte. The World Bank and the Global Environmental Facility supported the two projects mentioned in this paper: Regional Integrated Silvopastoral Approaches to Ecosystem Management (RISAEM Project) and Mainstreaming Biodiversity in Sustainable Cattle Ranching (MBSCR Project). Stefano Pagiola, Juan Pablo Ruiz (The World Bank), Muhammad Ibrahim (CATIE) and Thomas Walschburger (The Nature Conservancy) made important contributions to the design of Payment for Environmental Services schemes for silvopastoral systems. Several institutions have supported the systems and principles mentioned in this article: in Colombia FEDEGAN, Fundalianza, Fondo Accion, Colciencias and FINAGRO; in Mexico, Fundacion Produce Michoacan and Universidad Autonoma de Yucatan; in Panama, MIDA and CONADES. We are deeply grateful to all of the pioneer farmers who are making the necessary changes in their farms; without them we would have made little progress. NR 88 TC 61 Z9 71 U1 11 U2 93 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2011 VL 261 IS 10 SI SI BP 1654 EP 1663 DI 10.1016/j.foreco.2010.09.027 PG 10 WC Forestry SC Forestry GA 768HJ UT WOS:000290924400012 ER PT J AU Hall, JS Love, BE Garen, EJ Slusser, JL Saltonstall, K Mathias, S van Breugel, M Ibarra, D Bork, EW Spaner, D Wishnie, MH Ashton, MS AF Hall, Jefferson S. Love, Brian E. Garen, Eva J. Slusser, Jacob L. Saltonstall, Kristin Mathias, Shane van Breugel, Michiel Ibarra, Diogenes Bork, Edward W. Spaner, Dean Wishnie, Mark H. Ashton, Mark S. TI Tree plantations on farms: Evaluating growth and potential for success SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Panama; Native trees; Farmer; Restoration; Timber; Species selection trials ID TROPICAL FOREST; ECOSYSTEM SERVICES; CEDRELA-ODORATA; DEGRADED LANDS; NATIVE TREES; LEGUME TREES; COSTA-RICA; PANAMA; REFORESTATION; PERFORMANCE AB Interest in native species is growing across the tropics as reforestation of degraded lands becomes more widespread. In this study four tree species native to Panama - Cedrela odorata, Pachira quinata, Samanea saman, and Tabebuia rosea - were grown on rural farms at two dry tropical sites in Panama for up to five years. Survivorship and growth data at these "on-farm" trials are compared to data recorded from nearby experimental or "species selection" trial sites and evaluated in terms of soil fertility and management. Participant farmers were also asked about their interest in planting trees in general as well as their interest in 61 species grown in the species selection trial. Although, on-farm survivorship was variable and generally lower than that found on the species selection trial, one species (S. saman) experienced high and consistent survivorship. High survivorship combined with growth data from farms at both sites for this species suggests it would be a good candidate for extension projects working with rural farmers. Survivorship of other species appears more sensitive to farmer management and/or local site conditions. Generally lower growth on the Los Santos farms as compared to the species-selection trial is attributed to the lower soil fertility (plant available P) at the on-farm sites compared to the species selection trial. In contrast, only one species - P. quinata - had a growth variable found to be significantly lower between the on-farm and species selection trial sites in Rio Hato. C. odorata, P. quinata T. rosea can all be used in on-farm conditions with consideration to specific site and management conditions. By 2009, approximately 80% of the farmers planting trees still wished to participate in tree planting activities. All of the farmers no longer wishing to continue with the project expressed slow growth rates of trees as a principal reason. All but one of these farmers had growth rates for his/her trees markedly below those of the species selection trial nearby. Some farmers wishing to continue had very high mortality rates (>70% for all species), suggesting non-tangible benefits for participating in project activities. Other species that were not tested on-farm but grew well in the species-selection trials and were of interest to local farmers are discussed. As long as specific site and management conditions are carefully considered, data from species selection trials can be useful in informing tree planting projects with rural farmers; however, care should be taken to manage expectations. (C) 2010 Elsevier B.V. All rights reserved. C1 [Hall, Jefferson S.; Love, Brian E.; Saltonstall, Kristin; van Breugel, Michiel; Ibarra, Diogenes; Wishnie, Mark H.] Smithsonian Inst Global Earth Observ, Smithsonian Trop Res Inst, Balboa, Panama. [Love, Brian E.; Bork, Edward W.; Spaner, Dean] Univ Alberta, Dept Agr Food & Nutr Sci, Edmonton, AB, Canada. [Garen, Eva J.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Slusser, Jacob L.; Mathias, Shane; Ashton, Mark S.] Panama Amer Embassy, US Peace Corps, Ciudad del Saber, Clayton, Panama. RP Hall, JS (reprint author), Smithsonian Inst Global Earth Observ, Smithsonian Trop Res Inst, 401 Ave Rosevelt, Balboa, Panama. EM hallje@si.edu OI van Breugel, Michiel/0000-0003-2778-7803 FU Frank Levinson Donor-Advised Fund at the Peninsula Community Foundation; Levinson Family Foundation; Grantham Family Foundation FX This research was undertaken as part of PRORENA, a collaborative native species reforestation research project between the School of Forestry and Environmental Studies of Yale University and the Center for Tropical Forest Sciences at the Smithsonian Tropical Research Institute. This research project could not have been completed without the participation of the 37 land owners who provided support and space for the on-farm trials as well as the US Peace Corps. Financial support for the species selection and on-farm trials has been provided by the Frank Levinson Donor-Advised Fund at the Peninsula Community Foundation, the Levinson Family Foundation, and the Grantham Family Foundation. Mr. O. Diaz provided additional financial support and land for the species selection trials at Los Santos while those at Rio Hato are managed under a collaborative agreement with the National Environmental Authority of Panama (ANAM). We thank the staff of the Turner lab at STRI for soil analysis and B. Turner for discussions regarding data. Salary support for JSH and MvB was provided by the HSBC Climate Partnership. B. Love was supported by Natural Sciences and Engineering Research Council Canada Graduate Student Scholarship, the John G. Bene Fellowship in Community Forestry offered by the International Development Research Centre, and the University of Alberta Dissertation Fellowship. We are grateful to all the technicians who worked on this project over the years and are particularly indebted to the farmers of Los Santos and Rio Hato, who made this project possible. NR 65 TC 11 Z9 11 U1 2 U2 29 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2011 VL 261 IS 10 SI SI BP 1675 EP 1683 DI 10.1016/j.foreco.2010.09.042 PG 9 WC Forestry SC Forestry GA 768HJ UT WOS:000290924400014 ER PT J AU Garen, EJ Saltonstall, K Ashton, MS Slusser, JL Mathias, S Hall, JS AF Garen, Eva J. Saltonstall, Kristin Ashton, Mark S. Slusser, Jacob L. Mathias, Shane Hall, Jefferson S. TI The tree planting and protecting culture of cattle ranchers and small-scale agriculturalists in rural Panama: Opportunities for reforestation and land restoration SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Agroforestry; Fruit trees; Live fences; Multipurpose trees; Native species; Plantations; Tropical dry forest ID BIODIVERSITY CONSERVATION; AREA SYSTEM; DRY ZONE; AGROFORESTRY; LANDSCAPES; DIVERSITY; TROPICS; MANAGEMENT; FORESTS; FARMERS AB To examine the opportunities available for designing diverse tree planting and land restoration initiatives in agricultural landscapes that contain tropical dry forests, the tree planting and protecting practices of cattle ranchers and small-scale agriculturalists were examined in two study sites in rural Panama. Ninety-nine tree species were identified that they utilize, plant, or protect on their land, the majority of which are native to Panama. The farmers had diverse reasons for maintaining trees, including improving the environment, providing food and shade for cattle, and generating a source of wood for construction, furniture, and firewood. Most of the trees mentioned in the study provide multiple uses and values and the majority of farmers wanted to plant additional trees. Some differences in species preferences and motivations for planting and protecting trees were seen between sites, thereby suggesting that land restoration and tree planting projects should be site specific. Our data indicate that there are ample opportunities to increase native tree cover in our study sites and highlight the need to incorporate farmer input into project design, implementation, and evaluation as a necessary and continuous feature throughout projects. (C) 2010 Elsevier B.V. All rights reserved. C1 [Garen, Eva J.; Saltonstall, Kristin; Hall, Jefferson S.] Smithsonian Trop Res Inst, CTFS, Balboa, Ancon, Panama. [Ashton, Mark S.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT USA. [Slusser, Jacob L.; Mathias, Shane] Panama Amer Embassy, US Peace Corps, Ciudad Del Saber, Clayton, Panama. RP Garen, EJ (reprint author), Smithsonian Trop Res Inst, CTFS, Apartado 0843-03092, Balboa, Ancon, Panama. EM eva.garen@yale.edu FU Frank Levinson Family Foundation FX We would like to thank the farmers of Rio Hato and Los Santos for participating in this study and for sharing their experiences. We also are grateful to PRORENA staff-members and affiliates who contributed to different aspects of the design and implementation of this research, including Jairo Batista, Jose Deago, Brian Love, Emilio Mariscal, Anayansi Batista Vera, and Mark Wishnie. We also would like to thank Dr. Michael Dove, Dr. Amity Doolittle, and Bradford Gentry for their input into the design of this research, as well as two anonymous reviewers for their comments on previous versions of this manuscript. A special thank you to Rolando Perez and Jose Deago for providing their botanical expertise for this analysis. Funding for this research was provided by the Frank Levinson Family Foundation. NR 65 TC 16 Z9 16 U1 1 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD MAY 15 PY 2011 VL 261 IS 10 SI SI BP 1684 EP 1695 DI 10.1016/j.foreco.2010.10.011 PG 12 WC Forestry SC Forestry GA 768HJ UT WOS:000290924400015 ER PT J AU Karanth, KU Gopalaswamy, AM Kumar, NS Delampady, M Nichols, JD Seidensticker, J Noon, BR Pimm, SL AF Karanth, K. Ullas Gopalaswamy, Arjun M. Kumar, N. Samba Delampady, Mohan Nichols, James D. Seidensticker, John Noon, Barry R. Pimm, Stuart L. TI Counting India's Wild Tigers Reliably SO SCIENCE LA English DT Letter ID ABUNDANCE C1 [Karanth, K. Ullas; Gopalaswamy, Arjun M.; Kumar, N. Samba] Ctr Wildlife Studies, Bangalore 560042, Karnataka, India. [Karanth, K. Ullas] Wildlife Conservat Soc Global Conservat Program, Bronx, NY 10460 USA. [Gopalaswamy, Arjun M.] Univ Oxford, Dept Zool, Recanati Kaplan Ctr, Wildlife Conservat Res Unit WildCRU, Abingdon OX13 5QL, Oxon, England. [Kumar, N. Samba] Wildlife Conservat Soc India Program, Bangalore 560070, Karnataka, India. [Delampady, Mohan] Indian Stat Inst, Bangalore Ctr, Stat & Math Unit, Bangalore, Karnataka, India. [Nichols, James D.] US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Seidensticker, John] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Noon, Barry R.] Colorado State Univ, Dept Fish Wildlife & Conservat Biol, Ft Collins, CO 80521 USA. [Pimm, Stuart L.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. RP Karanth, KU (reprint author), Ctr Wildlife Studies, Bangalore 560042, Karnataka, India. EM ukaranth@gmail.com NR 11 TC 16 Z9 16 U1 3 U2 23 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAY 13 PY 2011 VL 332 IS 6031 BP 791 EP 791 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 763CD UT WOS:000290529900021 PM 21566176 ER PT J AU Phillips, RJ Davis, BJ Tanaka, KL Byrne, S Mellon, MT Putzig, NE Haberle, RM Kahre, MA Campbell, BA Carter, LM Smith, IB Holt, JW Smrekar, SE Nunes, DC Plaut, JJ Egan, AF Titus, TN Seu, R AF Phillips, Roger J. Davis, Brian J. Tanaka, Kenneth L. Byrne, Shane Mellon, Michael T. Putzig, Nathaniel E. Haberle, Robert M. Kahre, Melinda A. Campbell, Bruce A. Carter, Lynn M. Smith, Isaac B. Holt, John W. Smrekar, Suzanne E. Nunes, Daniel C. Plaut, Jeffrey J. Egan, Anthony F. Titus, Timothy N. Seu, Roberto TI Massive CO2 Ice Deposits Sequestered in the South Polar Layered Deposits of Mars SO SCIENCE LA English DT Article ID SOLID CO2; CIRCULATION; MODEL AB Shallow Radar soundings from the Mars Reconnaissance Orbiter reveal a buried deposit of carbon dioxide (CO2) ice within the south polar layered deposits of Mars with a volume of 9500 to 12,500 cubic kilometers, about 30 times that previously estimated for the south pole residual cap. The deposit occurs within a stratigraphic unit that is uniquely marked by collapse features and other evidence of interior CO2 volatile release. If released into the atmosphere at times of high obliquity, the CO2 reservoir would increase the atmospheric mass by up to 80%, leading to more frequent and intense dust storms and to more regions where liquid water could persist without boiling. C1 [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. [Phillips, Roger J.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Davis, Brian J.; Putzig, Nathaniel E.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Tanaka, Kenneth L.; Titus, Timothy N.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Byrne, Shane] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Mellon, Michael T.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Haberle, Robert M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Kahre, Melinda A.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. [Smith, Isaac B.; Holt, John W.] Univ Texas Austin, Jackson Sch Geosci, Inst Geophys, Austin, TX 78758 USA. [Smrekar, Suzanne E.; Nunes, Daniel C.; Plaut, Jeffrey J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Egan, Anthony F.] SW Res Inst, Dept Space Operat, Boulder, CO 80302 USA. [Seu, Roberto] Univ Roma La Sapienza, Dept Informat Engn Elect & Telecommun, I-00184 Rome, Italy. RP Phillips, RJ (reprint author), SW Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. EM roger@boulder.swri.edu RI Byrne, Shane/B-8104-2012; Carter, Lynn/D-2937-2012; Holt, John/C-4896-2009; Mellon, Michael/C-3456-2016 FU NASA FX K. Herkenhoff and C. Fortezzo provided useful comments on an earlier version of the paper. Remarks by three anonymous referees were exceedingly helpful. Funding for this work was provided by the NASA MRO project. The radar and imaging data are available through NASA's Planetary Data System. NR 19 TC 55 Z9 55 U1 4 U2 27 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAY 13 PY 2011 VL 332 IS 6031 BP 838 EP 841 DI 10.1126/science.1203091 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 763CD UT WOS:000290529900045 PM 21512003 ER PT J AU Conley, A Cooray, A Vieira, JD Solares, EAG Kim, S Aguirre, JE Amblard, A Auld, R Baker, AJ Beelen, A Blain, A Blundell, R Bock, J Bradford, CM Bridge, C Brisbin, D Burgarella, D Carpenter, JM Chanial, P Chapin, E Christopher, N Clements, DL Cox, P Djorgovski, SG Dowell, CD Eales, S Earle, L Ellsworth-Bowers, TP Farrah, D Franceschini, A Frayer, D Fu, H Gavazzi, R Glenn, J Griffin, M Gurwell, MA Halpern, M Ibar, E Ivison, RJ Jarvis, M Kamenetzky, J Krips, M Levenson, L Lupu, R Mahabal, A Maloney, PD Maraston, C Marchetti, L Marsden, G Matsuhara, H Mortier, AMJ Murphy, E Naylor, BJ Neri, R Nguyen, HT Oliver, SJ Omont, A Page, MJ Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rangwala, N Rawlings, JI Raymond, G Riechers, D Rodighiero, G Roseboom, IG Rowan-Robinson, M Schulz, B Scott, D Scott, K Serra, P Seymour, N Shupe, DL Smith, AJ Symeonidis, M Tugwell, KE Vaccari, M Valiante, E Valtchanov, I Verma, A Viero, MP Vigroux, L Wang, L Wiebe, D Wright, G Xu, CK Zeimann, G Zemcov, M Zmuidzinas, J AF Conley, A. Cooray, A. Vieira, J. D. Solares, E. A. Gonzalez Kim, S. Aguirre, J. E. Amblard, A. Auld, R. Baker, A. J. Beelen, A. Blain, A. Blundell, R. Bock, J. Bradford, C. M. Bridge, C. Brisbin, D. Burgarella, D. Carpenter, J. M. Chanial, P. Chapin, E. Christopher, N. Clements, D. L. Cox, P. Djorgovski, S. G. Dowell, C. D. Eales, S. Earle, L. Ellsworth-Bowers, T. P. Farrah, D. Franceschini, A. Frayer, D. Fu, H. Gavazzi, R. Glenn, J. Griffin, M. Gurwell, M. A. Halpern, M. Ibar, E. Ivison, R. J. Jarvis, M. Kamenetzky, J. Krips, M. Levenson, L. Lupu, R. Mahabal, A. Maloney, P. D. Maraston, C. Marchetti, L. Marsden, G. Matsuhara, H. Mortier, A. M. J. Murphy, E. Naylor, B. J. Neri, R. Nguyen, H. T. Oliver, S. J. Omont, A. Page, M. J. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rangwala, N. Rawlings, J. I. Raymond, G. Riechers, D. Rodighiero, G. Roseboom, I. G. Rowan-Robinson, M. Schulz, B. Scott, Douglas Scott, K. Serra, P. Seymour, N. Shupe, D. L. Smith, A. J. Symeonidis, M. Tugwell, K. E. Vaccari, M. Valiante, E. Valtchanov, I. Verma, A. Viero, M. P. Vigroux, L. Wang, L. Wiebe, D. Wright, G. Xu, C. K. Zeimann, G. Zemcov, M. Zmuidzinas, J. TI DISCOVERY OF A MULTIPLY LENSED SUBMILLIMETER GALAXY IN EARLY HerMES HERSCHEL/SPIRE* DATA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: high-redshift; galaxies: starburst; gravitational lensing: strong; submillimeter: galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; PHOTOMETRIC REDSHIFTS; STAR-FORMATION; NUMBER COUNTS; DUST; ULTRAVIOLET; POPULATION; STARBURSTS; CATALOG; MODELS AB We report the discovery of a bright (f (250 mu m) > 400 mJy), multiply lensed submillimeter galaxy HERMES J105751.1+573027 in Herschel/SPIRE Science Demonstration Phase data from the HerMES project. Interferometric 880 mu m Submillimeter Array observations resolve at least four images with a large separation of similar to 9 ''. A high-resolution adaptive optics K-p image with Keck/NIRC2 clearly shows strong lensing arcs. Follow-up spectroscopy gives a redshift of z = 2.9575, and the lensing model gives a total magnification of mu similar to 11 +/-1. The large image separation allows us to study the multi-wavelength spectral energy distribution (SED) of the lensed source unobscured by the central lensing mass. The far-IR/millimeter-wave SED is well described by a modified black-body fit with an unusually warm dust temperature, 88 +/- 3 K. We derive a lensing-corrected total IR luminosity of (1.43 +/- 0.09) x 10(13) L-circle dot, implying a star formation rate of similar to 2500 M-circle dot yr(-1). However, models primarily developed from brighter galaxies selected at longer wavelengths are a poor fit to the full optical-to-millimeter SED. A number of other strongly lensed systems have already been discovered in early Herschel data, and many more are expected as additional data are collected. C1 [Cooray, A.; Kim, S.; Amblard, A.; Serra, P.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Conley, A.; Earle, L.; Glenn, J.; Maloney, P. D.; Rangwala, N.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Cooray, A.; Vieira, J. D.; Blain, A.; Bock, J.; Bradford, C. M.; Bridge, C.; Carpenter, J. M.; Djorgovski, S. G.; Dowell, C. D.; Fu, H.; Levenson, L.; Mahabal, A.; Murphy, E.; Nguyen, H. T.; Riechers, D.; Schulz, B.; Shupe, D. L.; Viero, M. P.; Xu, C. K.; Zemcov, M.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA. [Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Aguirre, J. E.; Lupu, R.; Scott, K.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Auld, R.; Eales, S.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Beelen, A.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Beelen, A.] CNRS, UMR 8617, F-91405 Orsay, France. [Blundell, R.; Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J.; Bradford, C. M.; Dowell, C. D.; Levenson, L.; Naylor, B. J.; Nguyen, H. T.; Zemcov, M.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brisbin, D.] Cornell Univ, Ithaca, NY 14853 USA. [Burgarella, D.] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Chanial, P.] Univ Paris Diderot, CE Saclay, CNRS, CEA DSM Irfu,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Chapin, E.; Halpern, M.; Marsden, G.; Scott, Douglas; Valiante, E.; Wiebe, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Christopher, N.; Verma, A.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Clements, D. L.; Mortier, A. M. J.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Cox, P.; Krips, M.; Neri, R.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Ellsworth-Bowers, T. P.; Glenn, J.; Kamenetzky, J.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA. [Farrah, D.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Franceschini, A.; Marchetti, L.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Frayer, D.; Omont, A.] NRAO, Green Bank, WV 24944 USA. [Gavazzi, R.; Vigroux, L.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Ibar, E.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Jarvis, M.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Maraston, C.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Matsuhara, H.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Murphy, E.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Ctr Infrared Proc & Anal, JPL, Pasadena, CA 91125 USA. [Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pearson, C. P.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Zeimann, G.] Univ Calif Davis, Davis, CA 95616 USA. RP Conley, A (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA. EM alexander.conley@colorado.edu RI Serra, Paolo/G-9678-2014; amblard, alexandre/L-7694-2014; Lupu, Roxana/P-9060-2014; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; OI Serra, Paolo/0000-0002-7609-3931; amblard, alexandre/0000-0002-2212-5395; Lupu, Roxana/0000-0003-3444-5908; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536; Rodighiero, Giulia/0000-0002-9415-2296 FU CSA (Canada); NAOC (China); CEA (France); CNES, (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA); INSU/CNRS (France); MPG (Germany); IGN (Spain); NSF [ATI-0838178] FX SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics. The IRAM Plateau de Bure Interferometer is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated by Associated Universities, Inc. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by NSF grant ATI-0838178 to CARMA, and by the CARMApartner universities. The authors thank Elisabete da Cunha for running her models for us. The Herschel data presented in this Letter will be released through the Herschel Database in Marseille, HeDaM. 39 NR 36 TC 38 Z9 38 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 10 PY 2011 VL 732 IS 2 AR L35 DI 10.1088/2041-8205/732/2/L35 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797MY UT WOS:000293133200017 ER PT J AU Gacesa, M Muller, HR Cote, R Kharchenko, V AF Gacesa, M. Mueller, H. -R. Cote, R. Kharchenko, V. TI POLARIZATION OF THE CHARGE-EXCHANGE X-RAYS INDUCED IN THE HELIOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE atomic processes; polarization; radiation mechanisms: non-thermal; solar wind; Sun: heliosphere; X-rays: diffuse background ID LOCAL INTERSTELLAR-MEDIUM; SOLAR-WIND; EMISSION-SPECTRA; HOT GAS; BUBBLE; IONS; SPECTROSCOPY; HYDROGEN; EUV AB We report results of a theoretical investigation of polarization of the X-ray emissions induced in charge-exchange collisions of fully stripped solar wind (SW) ions C6+ and O8+ with the heliospheric hydrogen atoms. The polarization of X-ray emissions has been computed for line-of-sight observations within the ecliptic plane as a function of SW ion velocities, including a range of velocities corresponding to the slow and fast SW, and coronal mass ejections. To determine the variability of polarization of heliospheric X-ray emissions, the polarization has been computed for solar minimum conditions with self-consistent parameters of the SW plasma and heliospheric gas and compared with the polarization calculated for an averaged solar activity. We predict the polarization of charge-exchange X-rays to be between 3% and 8%, depending on the line-of-sight geometry, SW ion velocity, and the selected emission lines. C1 [Gacesa, M.; Kharchenko, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gacesa, M.; Cote, R.; Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Mueller, H. -R.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Gacesa, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gacesa@phys.uconn.edu RI Gacesa, Marko/F-8027-2011 OI Gacesa, Marko/0000-0001-5145-051X FU NASA [NNX08AH51G]; NSF [AST-0607641] FX V.K. acknowledges support by NASA grant NNX08AH51G and H.-R.M. acknowledges support by NSF grant AST-0607641. NR 27 TC 0 Z9 0 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 10 PY 2011 VL 732 IS 2 AR L21 DI 10.1088/2041-8205/732/2/L21 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797MY UT WOS:000293133200003 ER PT J AU Jimenez-Serra, I Martin-Pintado, J Baez-Rubio, A Patel, N Thum, C AF Jimenez-Serra, I. Martin-Pintado, J. Baez-Rubio, A. Patel, N. Thum, C. TI EXTREMELY BROAD RADIO RECOMBINATION MASER LINES TOWARD THE HIGH-VELOCITY IONIZED JET IN CEPHEUS A HW2 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (Cepheus A); ISM: jets and outflows; masers; stars: formation ID H-II REGIONS; A HW2; MASSIVE STARS; MWC 349; MWC-349; PROTOSTAR; PHOTOEVAPORATION; RESOLUTION; EMISSION; MOTIONS AB We present the first detection of the H40 alpha, H34 alpha, and H31 alpha radio recombination lines (RRLs) at millimeter wavelengths toward the high-velocity ionized jet in the Cepheus A HW2 star-forming region. From our single-dish and interferometric observations, we find that the measured RRLs show extremely broad asymmetric line profiles with zero-intensity line widths of similar to 1100 km s(-1). From the line widths, we estimate a terminal velocity for the ionized gas in the jet of >= 500 km s(-1), consistent with that obtained from the proper motions of the HW2 radio jet. The total integrated line-to-continuum flux ratios of the H40 alpha, H34 alpha, and H31 alpha lines are 43, 229, and 280 km s(-1), clearly deviating from LTE predictions. These ratios are very similar to those observed for the RRL masers toward MWC349A, suggesting that the intensities of the RRLs toward HW2 are affected by maser emission. Our radiative transfer modeling of the RRLs shows that their asymmetric profiles could be explained by maser emission arising from a bi-conical radio jet with a semi-opening angle of 18 degrees, electron density distribution varying as r(-2.11), and turbulent and expanding wind velocities of 60 and 500 km s(-1). C1 [Jimenez-Serra, I.; Patel, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martin-Pintado, J.; Baez-Rubio, A.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain. [Thum, C.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. 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; baezra@cab.inta-csic.es; npatel@cfa.harvard.edu; thum@iram.fr RI Baez Rubio, Alejandro/F-8184-2016; Martin-Pintado, Jesus/H-6107-2015 OI Baez Rubio, Alejandro/0000-0001-8125-5993; Martin-Pintado, Jesus/0000-0003-4561-3508 FU Smithsonian Astrophysical Observatory; MICINN [ESP2007-65812-C02-C01, AYA2010-21697-C05-01, CAM S2009/ESP-1496] FX I.J.S. acknowledges the Smithsonian Astrophysical Observatory for the support provided through an SMA fellowship. We thank an anonymous referee who helped to improve the manuscript. 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 35 TC 6 Z9 6 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 MAY 10 PY 2011 VL 732 IS 2 AR L27 DI 10.1088/2041-8205/732/2/L27 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797MY UT WOS:000293133200009 ER PT J AU Latham, DW Rowe, JF Quinn, SN Batalha, NM Borucki, WJ Brown, TM Bryson, ST Buchhave, LA Caldwell, DA Carter, JA Christiansen, JL Ciardi, DR Cochran, WD Dunham, EW Fabrycky, DC Ford, EB Gautier, TN Gilliland, RL Holman, MJ Howell, SB Ibrahim, KA Isaacson, H Jenkins, JM Koch, DG Lissauer, JJ Marcy, GW Quintana, EV Ragozzine, D Sasselov, D Shporer, A Steffen, JH Welsh, WF Wohler, B AF Latham, David W. Rowe, Jason F. Quinn, Samuel N. Batalha, Natalie M. Borucki, William J. Brown, Timothy M. Bryson, Stephen T. Buchhave, Lars A. Caldwell, Douglas A. Carter, Joshua A. Christiansen, Jessie L. Ciardi, David R. Cochran, William D. Dunham, Edward W. Fabrycky, Daniel C. Ford, Eric B. Gautier, Thomas N., III Gilliland, Ronald L. Holman, Matthew J. Howell, Steve B. Ibrahim, Khadeejah A. Isaacson, Howard Jenkins, Jon M. Koch, David G. Lissauer, Jack J. Marcy, Geoffrey W. Quintana, Elisa V. Ragozzine, Darin Sasselov, Dimitar Shporer, Avi Steffen, Jason H. Welsh, William F. Wohler, Bill TI A FIRST COMPARISON OF KEPLER PLANET CANDIDATES IN SINGLE AND MULTIPLE SYSTEMS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems ID MASS AB In this Letter, we present an overview of the rich population of systems with multiple candidate transiting planets found in the first four months of Kepler data. The census of multiples includes 115 targets that show two candidate planets, 45 with three, eight with four, and one each with five and six, for a total of 170 systems with 408 candidates. When compared to the 827 systems with only one candidate, the multiples account for 17% of the total number of systems, and one-third of all the planet candidates. We compare the characteristics of candidates found in multiples with those found in singles. False positives due to eclipsing binaries are much less common for the multiples, as expected. Singles and multiples are both dominated by planets smaller than Neptune; 69(-3)(+2) % for singles and 86(-5)(+2)% for multiples. This result, that systems with multiple transiting planets are less likely to include a transiting giant planet, suggests that close-in giant planets tend to disrupt the orbital inclinations of small planets in flat systems, or maybe even prevent the formation of such systems in the first place. C1 [Latham, David W.; Quinn, Samuel N.; Carter, Joshua A.; Holman, Matthew J.; Ragozzine, Darin; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Caldwell, Douglas A.; Christiansen, Jessie L.; Jenkins, Jon M.; Quintana, Elisa V.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Ciardi, David R.] NASA, Exoplanet Sci Inst, CALTECH, Pasadena, CA 91125 USA. [Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 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. [Ibrahim, Khadeejah A.; Wohler, Bill] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Shporer, Avi] Univ Calif Santa Cruz, Dept Phys, Santa Barbara, CA 93106 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Carter, Joshua/A-8280-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate FX We thank the entire Kepler team for all the hard work that has made these results possible. Funding for this Discovery Mission is provided by NASA's Science Mission Directorate. We give special thanks to the anonymous referee for insightful and timely feedback. NR 23 TC 81 Z9 81 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 MAY 10 PY 2011 VL 732 IS 2 AR L24 DI 10.1088/2041-8205/732/2/L24 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797MY UT WOS:000293133200006 ER PT J AU Byhring, HS Cranmer, SR Lie-Svendsen, O Habbal, SR Esser, R AF Byhring, H. S. Cranmer, S. R. Lie-Svendsen, O. Habbal, S. R. Esser, R. TI MODELING IRON ABUNDANCE ENHANCEMENTS IN THE SLOW SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: abundances; Sun: corona ID POLAR CORONAL HOLE; ION CHARGE STATES; PHYSICAL-PROPERTIES; TRANSITION REGION; ELECTRON-TEMPERATURE; FE-XI; SPECTROMETER; VELOCITIES; EMISSION; STREAMER AB We have studied the behavior of Fe ions in the slow solar wind, using a fluid model extending from the chromosphere to 1 AU. Emphasis is on elemental "pileup" in the corona, i.e., a region where the Fe density increases and has a local maximum. We study the behavior of individual Fe ions relative to each other in the pileup region, where Fe+10 and Fe+12 have been used as examples. We find that elemental pileups can occur for a variety of densities and temperatures in the corona. We also calculate the ion fractions and obtain estimates for the freezing-in distance of Fe in the slow solar wind. We find that the freezing-in distance for iron is high, between 3 and 11 R-circle dot, and that a high outflow velocity, of order 50-100 km s(-1), in the region above the temperature maximum is needed to obtain ion fractions for Fe+10 and Fe+12 that are consistent with observations. C1 [Byhring, H. S.; Esser, R.] Univ Tromso, Dept Phys & Technol, NO-9037 Tromso, Norway. [Byhring, H. S.; Cranmer, S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lie-Svendsen, O.] Norwegian Def Res Estab, NO-2027 Kjeller, Norway. [Habbal, S. R.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Byhring, HS (reprint author), Univ Tromso, Dept Phys & Technol, NO-9037 Tromso, Norway. EM hanne-sigrun.byhring@uit.no FU Fulbright; Norwegian Research Council [177570/V30]; NASA [NNX09AB27G, NNX10AC11G] FX Hanne Sigrun Byhring thanks the Solar, Stellar and Planetary Division at the Harvard-Smithsonain Center for Astrophysics for their hospitality while she was a visitor there. We also thank H. Morgan for providing the data for Figure 5 from Habbal et al. (2007), Figure 9. This work has been supported by a Fulbright Scholarship and by the Norwegian Research Council, grant no. 177570/V30. S. R. C. acknowledges the support of NASA grants NNX09AB27G and NNX10AC11G. NR 38 TC 4 Z9 4 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 MAY 10 PY 2011 VL 732 IS 2 AR 119 DI 10.1088/0004-637X/732/2/119 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755ML UT WOS:000289935900059 ER PT J AU Cavagnolo, KW McNamara, BR Wise, MW Nulsen, PEJ Bruggen, M Gitti, M Rafferty, DA AF Cavagnolo, K. W. McNamara, B. R. Wise, M. W. Nulsen, P. E. J. Breuggen, M. Gitti, M. Rafferty, D. A. TI A POWERFUL AGN OUTBURST IN RBS 797 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID COOLING FLOW CLUSTERS; ACTIVE GALACTIC NUCLEI; CENTRAL DOMINANT GALAXIES; BLACK-HOLE MASS; ROSAT BRIGHT SURVEY; X-RAY-EMISSION; STAR-FORMATION; JET POWER; H-ALPHA; CHANDRA OBSERVATION AB Utilizing similar to 50 ks of Chandra X-Ray Observatory imaging, we present an analysis of the intracluster medium (ICM) and cavity system in the galaxy cluster RBS 797. In addition to the two previously known cavities in the cluster core, the new and deeper X-ray image has revealed additional structure associated with the active galactic nucleus (AGN). The surface brightness decrements of the two cavities are unusually large and are consistent with elongated cavities lying close to our line of sight. We estimate a total AGN outburst energy and mean jet power of approximate to(3-6) x 10(60) erg and approximate to(3-6) x 10(45) erg s(-1), respectively, depending on the assumed geometrical configuration of the cavities. Thus, RBS 797 is apparently among the most powerful AGN outbursts known in a cluster. The average mass accretion rate needed to power the AGN by accretion alone is similar to 1 M-circle dot yr(-1). We show that accretion of cold gas onto the AGN at this level is plausible, but that Bondi accretion of the hot atmosphere is probably not. The brightest cluster galaxy (BCG) harbors an unresolved, non-thermal nuclear X-ray source with a bolometric luminosity of approximate to 2 x 10(44) erg s(-1). The nuclear emission is probably associated with a rapidly accreting, radiatively inefficient accretion flow. We present tentative evidence that star formation in the BCG is being triggered by the radio jets and suggest that the cavities may be driving weak shocks (M similar to 1.5) into the ICM, similar to the process in the galaxy cluster MS 0735.6+7421. C1 [Cavagnolo, K. W.] Observ Cote Azur, UNS, CNRS, UMR Cassioee 6202, F-06003 Nice, France. [McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [McNamara, B. R.; Nulsen, P. E. J.; Gitti, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Breuggen, M.] Univ Bremen, Bremen, Germany. [Gitti, M.] Astron Observ Bologna INAF, Bologna, Italy. [Rafferty, D. A.] Leiden Univ, Leiden Observ, Leiden, Netherlands. RP Cavagnolo, KW (reprint author), Observ Cote Azur, UNS, CNRS, UMR Cassioee 6202, F-06003 Nice, France. EM cavagnolo@oca.eu OI Gitti, Myriam/0000-0002-0843-3009; Nulsen, Paul/0000-0003-0297-4493 FU L'Agence Nationale de la Recherche [ANR-09-JCJC-0001-01]; Canadian Natural Science and Engineering Research Council; National Aeronautics and Space Administration [G07-8122X]; National Aeronautics Space Administration [NAS8-03060]; ASI-INAF [I/088/06/0, CXO GO0-11003X] FX K.W.C. acknowledges financial support from L'Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01, and thanks David Gilbank, Sabine Schindler, Axel Schwope, and Chris Waters for helpful input. B. R. M. was supported by a generous grant from the Canadian Natural Science and Engineering Research Council, and thanks support provided by the National Aeronautics and Space Administration through Chandra Award Number G07-8122X 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. M. G. acknowledges support from the grants ASI-INAF I/088/06/0 and CXO GO0-11003X. Some results are based on observations made with the NASA/ESA HST, 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 research has made use of NASA's Astrophysics Data System (ADS), Extragalactic Database (NED), High Energy Astrophysics Science Archive Research Center (HEASARC), data obtained from the Chandra Data Archive, and software provided by the Chandra X-ray Center (CXC). NR 71 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 MAY 10 PY 2011 VL 732 IS 2 AR 71 DI 10.1088/0004-637X/732/2/71 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755ML UT WOS:000289935900011 ER PT J AU Giacintucci, S O'Sullivan, E Vrtilek, J David, LP Raychaudhury, S Venturi, T Athreya, RM Clarke, TE Murgia, M Mazzotta, P Gitti, M Ponman, T Ishwara-Chandra, CH Jones, C Forman, WR AF Giacintucci, Simona O'Sullivan, Ewan Vrtilek, Jan David, Laurence P. Raychaudhury, Somak Venturi, Tiziana Athreya, Ramana M. Clarke, Tracy E. Murgia, Matteo Mazzotta, Pasquale Gitti, Myriam Ponman, Trevor Ishwara-Chandra, C. H. Jones, Christine Forman, William R. TI A COMBINED LOW-RADIO FREQUENCY/X-RAY STUDY OF GALAXY GROUPS. I. GIANT METREWAVE RADIO TELESCOPE OBSERVATIONS AT 235 MHz AND 610 MHz SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; intergalactic medium; radio continuum: galaxies; X-rays: galaxies: clusters ID DEEP CHANDRA OBSERVATION; ACTIVE GALACTIC NUCLEI; GROUP EVOLUTION MULTIWAVELENGTH; MULTIFREQUENCY VLA OBSERVATIONS; NEWTON GROUP SURVEY; X-RAY; XMM-NEWTON; INTRACLUSTER MEDIUM; HOT GAS; COLD FRONTS AB We present new Giant Metrewave Radio Telescope observations at 235 MHz and 610 MHz of 18 X-ray bright galaxy groups. These observations are part of an extended project, presented here and in future papers, which combines low-frequency radio and X-ray data to investigate the interaction between central active galactic nuclei (AGNs) and the intra-group medium (IGM). The radio images show a very diverse population of group-central radio sources, varying widely in size, power, morphology, and spectral index. Comparison of the radio images with Chandra and XMM-Newton X-ray images shows that groups with significant substructure in the X-ray band and marginal radio emission at greater than or similar to 1 GHz host low-frequency radio structures that correlate with substructures in IGM. Radio-filled X-ray cavities, the most evident form of AGN/IGM interaction in our sample, are found in half of the systems and are typically associated with small, low-, or mid-power double radio sources. Two systems, NGC5044 and NGC4636, possess multiple cavities, which are isotropically distributed around the group center, possibly due to group weather. In other systems the radio/X-ray correlations are less evident. However, the AGN/IGM interaction can manifest itself through the effects of the high-pressure medium on the morphology, spectral properties, and evolution of the radio-emitting plasma. In particular, the IGM can confine fading radio lobes in old/dying radio galaxies and prevent them from dissipating quickly. Evidence for radio emission produced by former outbursts that co-exist with current activity is found in six groups of the sample. C1 [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, Simona; O'Sullivan, Ewan; Vrtilek, Jan; David, Laurence P.; Mazzotta, Pasquale; Gitti, Myriam; Jones, Christine; Forman, William R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giacintucci, Simona; Venturi, Tiziana] INAF Ist Radioastron, I-40129 Bologna, Italy. [O'Sullivan, Ewan; Raychaudhury, Somak; Ponman, Trevor] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Athreya, Ramana M.] IISER, Pune 411008, Maharashtra, India. [Clarke, Tracy E.] USN, Res Lab, Washington, DC 20375 USA. [Murgia, Matteo] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. [Mazzotta, Pasquale] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Gitti, Myriam] Osservatorio Astron Bologna INAF, I-40127 Bologna, Italy. TIFR, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. RP Giacintucci, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM simona@astro.umd.edu RI Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; Gitti, Myriam/0000-0002-0843-3009; Murgia, Matteo/0000-0002-4800-0806; O'Sullivan, Ewan/0000-0002-5671-6900; Venturi, Tiziana/0000-0002-8476-6307; Forman, William/0000-0002-9478-1682 FU NASA, Chandra X-ray Center (CXC) [PF0-110071]; European Community under the Marie Curie Research Training Network; Smithsonian Institution; CXC; Chandra X-ray Observatory Center [GO8-9127XR, AR0-11017X, GO0-11003X]; [NNX07AE95GR]; [ASI-INAF I/088/06/0] FX We thank the staff of the GMRT for their help during the observations. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology. S.G. acknowledges the support of NASA through Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray Center (CXC), which is operated by SAO. E.O.S. acknowledges the support of the European Community under the Marie Curie Research Training Network. J.M.V., L.P.D., C.J., and W.R.F. acknowledge the support of the Smithsonian Institution and CXC. This work was supported by grants GO8-9127XR, AR0-11017X, and GO0-11003X issued by the Chandra X-ray Observatory Center, XMM-Newton grant NNX07AE95GR, and grant ASI-INAF I/088/06/0. Basic research in astronomy at the Naval Research Laboratory is supported by 6.1 base funding. This research has made use of data obtained from the Chandra and XMM-Newton Data Archives, and software provided by CXC in the application packages CIAO, ChIPS, and Sherpa. NR 137 TC 34 Z9 34 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 MAY 10 PY 2011 VL 732 IS 2 AR 95 DI 10.1088/0004-637X/732/2/95 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755ML UT WOS:000289935900035 ER PT J AU Kelly, BC Bechtold, J Siemiginowska, A AF Kelly, Brandon C. Bechtold, Jill Siemiginowska, Aneta TI ARE THE VARIATIONS IN QUASAR OPTICAL FLUX DRIVEN BY THERMAL FLUCTUATIONS? (vol 698, pg 895, 2009) SO ASTROPHYSICAL JOURNAL LA English DT Correction ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; X-RAY; VARIABILITY; STEPS; SIZE C1 [Kelly, Brandon C.; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bechtold, Jill] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. RP Kelly, BC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bckelly@cfa.harvard.edu NR 11 TC 2 Z9 2 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 MAY 10 PY 2011 VL 732 IS 2 AR 128 DI 10.1088/0004-637X/732/2/128 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755ML UT WOS:000289935900068 ER PT J AU Meikle, WPS Kotak, R Farrah, D Mattila, S Van Dyk, SD Andersen, AC Fesen, R Filippenko, AV Foley, RJ Fransson, C Gerardy, CL Hoflich, PA Lundqvist, P Pozzo, M Sollerman, J Wheeler, JC AF Meikle, W. P. S. Kotak, R. Farrah, D. Mattila, S. Van Dyk, S. D. Andersen, A. C. Fesen, R. Filippenko, A. V. Foley, R. J. Fransson, C. Gerardy, C. L. Hoeflich, P. A. Lundqvist, P. Pozzo, M. Sollerman, J. Wheeler, J. C. TI DUST AND THE TYPE II-PLATEAU SUPERNOVA 2004dj SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; supernovae: general; supernovae: individual (SN 2004dj) ID SPITZER-SPACE-TELESCOPE; CORE-COLLAPSE SUPERNOVAE; SN 1987A; INFRARED-EMISSION; SHOCK BREAKOUT; EARLY UNIVERSE; CIRCUMSTELLAR INTERACTION; SPECTRAL EVOLUTION; NEARBY GALAXIES; RADIO-EMISSION AB We present mid-infrared (MIR) spectroscopy of a Type II-plateau supernova, SN 2004dj, obtained with the Spitzer Space Telescope, spanning 106-1393 days after explosion. MIR photometry plus optical/near-IR observations are also reported. An early-time MIR excess is attributed to emission from non-silicate dust formed within a cool dense shell (CDS). Most of the CDS dust condensed between 50 days and 165 days, reaching a mass of 0.3 x 10(-5) M-circle dot. Throughout the observations, much of the longer wavelength (> 10 mu m) part of the continuum is explained as an IR echo from interstellar dust. The MIR excess strengthened at later times. We show that this was due to thermal emission from warm, non-silicate dust formed in the ejecta. Using optical/near-IR line profiles and the MIR continua, we show that the dust was distributed as a disk whose radius appeared to be shrinking slowly. The disk radius may correspond to a grain destruction zone caused by a reverse shock which also heated the dust. The dust-disk lay nearly face-on, had high opacities in the optical/near-IR regions, but remained optically thin in the MIR over much of the period studied. Assuming a uniform dust density, the ejecta dust mass by 996 days was (0.5 +/- 0.1) x 10(-4) M-circle dot and exceeded 10(-4) M-circle dot by 1393 days. For a dust density rising toward the center the limit is higher. Nevertheless, this study suggests that the amount of freshly synthesized dust in the SN 2004dj ejecta is consistent with that found from previous studies and adds further weight to the claim that such events could not have been major contributors to the cosmic dust budget. C1 [Meikle, W. P. S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Kotak, R.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Farrah, D.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QJ, E Sussex, England. [Mattila, S.] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-21500 Piikkio, Finland. [Mattila, S.; Fransson, C.; Lundqvist, P.; Sollerman, J.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Van Dyk, S. D.] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Andersen, A. C.; Sollerman, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Fesen, R.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Filippenko, A. V.; Foley, R. J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gerardy, C. L.; Hoeflich, P. A.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Pozzo, M.] UCL, Dept Earth Sci, London WC1E 6BT, England. [Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Meikle, WPS (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. EM p.meikle@imperial.ac.uk RI Pozzo, Monica/C-4965-2011; Kotak, Rubina/F-3325-2011; Andersen, Anja Cetti/P-4822-2014; OI Kotak, Rubina/0000-0001-5455-3653; Andersen, Anja Cetti/0000-0001-8169-7273; Sollerman, Jesper/0000-0003-1546-6615; Van Dyk, Schuyler/0000-0001-9038-9950 FU NASA; W. M. Keck Foundation; NASA through an award issued by JPL/Caltech [1322321]; NSF [AST-0908886, AST-1008962, 0708855, AST-0707769]; TABASGO Foundation; Academy of Finland [8120503]; Knut and Alice Wallenberg Foundation; Danish National Research Foundation FX We thank J. Vinko for providing us with digitized versions of his optical spectra. The work presented here is based on observations made with the Spitzer Space Telescope, the W. M. Keck Observatory, the William Herschel Telescope (WHT), and the 2.4 m Hiltner Telescope of the MDM Observatory. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; it was made possible by the generous financial support of the W. M. Keck Foundation. We extend special gratitude to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. The WHT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Financial support for this research was provided by NASA through an award issued by JPL/Caltech (specifically grant number 1322321 in the case of A.V.F.). A.V.F. gratefully acknowledges additional support from NSF grant AST-0908886 and the TABASGO Foundation. P.A.H. was supported by NSF grants AST-1008962 and 0708855. S.M. acknowledges support from the Academy of Finland (project 8120503). J.S. is a Royal Swedish Academy of Sciences Research Fellow supported by a grant from the Knut and Alice Wallenberg Foundation. J.C.W gratefully acknowledges support from NSF grant AST-0707769. The Dark Cosmology Centre is funded by the Danish National Research Foundation. NR 105 TC 21 Z9 21 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2011 VL 732 IS 2 AR 109 DI 10.1088/0004-637X/732/2/109 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755ML UT WOS:000289935900049 ER PT J AU Riess, AG Macri, L Casertano, S Lampeit, H Ferguson, HC Filippenko, AV Jha, SW Li, WD Chornock, R Silverman, JM AF Riess, Adam G. Macri, Lucas Casertano, Stefano Lampeit, Hubert Ferguson, Henry C. Filippenko, Alexei V. Jha, Saurabh W. Li, Weidong Chornock, Ryan Silverman, Jeffrey M. TI A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE AND WIDE FIELD CAMERA 3 (vol 730, pg 119, 2011) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, Adam G.; Casertano, Stefano; Ferguson, Henry C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Macri, Lucas] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Lampeit, Hubert] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Filippenko, Alexei V.; Li, Weidong; Silverman, Jeffrey M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Riess, AG (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NR 1 TC 204 Z9 204 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2011 VL 732 IS 2 AR 129 DI 10.1088/0004-637X/732/2/129 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755ML UT WOS:000289935900069 ER PT J AU Kuntner, M Agnarsson, I AF Kuntner, Matjaz Agnarsson, Ingi TI Phylogeography of a successful aerial disperser: the golden orb spider Nephila on Indian Ocean islands SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID DAY GECKOS PHELSUMA; SEQUENTIAL COLONIZATION; TRANSOCEANIC DISPERSAL; ARANEAE NEPHILIDAE; SPECIATION; DNA; BIOGEOGRAPHY; THERIDIIDAE; MADAGASCAR; ANELOSIMUS AB Background: The origin and diversification patterns of lineages across the Indian Ocean islands are varied due to the interplay of the complex geographic and geologic island histories, the varying dispersal abilities of biotas, and the proximity to major continental landmasses. Our aim was to reconstruct phylogeographic history of the giant orbweaving spider (Nephila) on western Indian Ocean islands (Madagascar, Mayotte, Reunion, Mauritius, Rodrigues), to test its origin and route of dispersal, and to examine the consequences of good dispersal abilities for colonization and diversification, in comparison with related spiders (Nephilengys) inhabiting the same islands, and with other organisms known for over water dispersal. We used mitochondrial (COI) and nuclear (ITS2) markers to examine phylogenetic and population genetic patterns in Nephila populations and species. We employed Bayesian and parsimony methods to reconstruct phylogenies and haplotype networks, respectively, and calculated genetic distances, fixation indices, and estimated clade ages under a relaxed clock model. Results: Our results suggest an African origin of Madagascar Nephila inaurata populations via Cenozoic dispersal, and the colonization of the Mascarene islands from Madagascar. We find evidence of gene flow across Madagascar and Comoros. The Mascarene islands share a common 'ancestral' COI haplotype closely related to those found on Madagascar, but itself absent, or as yet unsampled, from Madagascar. Each island has one or more unique haplotypes related to the ancestral Mascarene haplotype. The Indian Ocean N. inaurata are genetically distinct from the African populations. Conclusions: Nephila spiders colonized Madagascar from Africa about 2.5 (0.6-5.3) Ma. Our results are consistent with subsequent, recent and rapid, colonization of all three Mascarene islands. On each island, however, we detected unique haplotypes, consistent with a limited gene flow among the islands subsequent to colonization, a scenario that might be referred to as speciation in progress. However, due to relatively small sample sizes, we cannot rule out that we simply failed to collect Mascarene haplotypes on Madagascar, a scenario that might imply human mediated dispersal. Nonetheless, the former interpretation better fits the available data and results in a pattern similar to the related Nephilengys. Nephilengys, however, shows higher genetic divergences with diversification on more remote islands. That the better disperser of the two lineages, Nephila, has colonized more islands but failed to diversify, demonstrates how dispersal ability can shape both the patterns of colonization and formation of species across archipelagos. C1 [Kuntner, Matjaz; Agnarsson, Ingi] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, SI-1001 Ljubljana, Slovenia. [Kuntner, Matjaz; Agnarsson, Ingi] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Agnarsson, Ingi] Univ Puerto Rico Rio Piedras, Dept Biol, San Juan, PR 00931 USA. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM kuntner@gmail.com FU Slovenian Research Agency [Z1-9799-0618-07]; National Science Foundation [DEB-0516038]; European Community [MIRG-CT-2005 036536]; National Geographic Society [8655-09] FX This is contribution number 7 resulting from the 2008 Indian Ocean expedition, funded by the Slovenian Research Agency (grant Z1-9799-0618-07 to I. Agnarsson) and the National Science Foundation (grant DEB-0516038 to T. Blackledge). Additional funding came from the European Community 6th Framework Programme (a Marie Curie International Reintegration Grant MIRG-CT-2005 036536 to M. Kuntner), and the National Geographic Society (grant 8655-09 to the authors). We thank Tjasa Lokovsek, Yadira Ortiz-Ruiz, Jason Rauscher, Peter Trontelj, Miquel Arnedo and Tomas Hrbek for help or advice, Heine C. Kiesbuy and Dennis Hansen for field assistance, and Dominique Strasberg, Sonia Ribes-Beaudemoulin, Benoit Lequettefor, and MICET for logistical help. Finally, we thank our wives, Irena and Laura, for their amazing patience and support during all phases of this research. NR 59 TC 19 Z9 19 U1 1 U2 33 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 MAY 9 PY 2011 VL 11 AR 119 DI 10.1186/1471-2148-11-119 PG 9 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 766NQ UT WOS:000290790600001 PM 21554687 ER PT J AU Capogrosso-Sansone, B AF Capogrosso-Sansone, B. TI Solid phases and pairing in a mixture of polar molecules and atoms SO PHYSICAL REVIEW A LA English DT Article ID MANY-BODY PHYSICS; ULTRACOLD; GASES AB We consider amixture of hard-core bosonic polar molecules, interacting via repulsive dipole-dipole interaction, and one atomic bosonic species. The mixture is confined on a two-dimensional square lattice and, at low enough temperatures, can be described by the two-component Bose-Hubbard model. The latter displays an extremely rich phase diagram including solid, superfluid, and supersolid phases. Here, we mainly focus on the checkerboard molecular solid, stabilized by the long-range dipolar interaction, and study how the presence of atoms affects its robustness both at zero and finite temperatures. We find that, due to atom-molecule interactions, solid phases can be stabilized at both (much) lower strengths of dipolar interaction and higher temperatures, than when no atoms are present. As a byproduct, atoms also order in a solid phase with the same melting temperatures as for molecules. Finally, we find that for large enough interaction between atoms and molecules, a paired supersolid phase can be stabilized. C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Capogrosso-Sansone, B (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, 60 Garden St, Cambridge, MA 02138 USA. FU Institute for Atomic, Molecular, and Optical Physics (ITAMP) FX We would like to especially thank E. Kuznetsova for enlightening discussions. We also acknowledge fruitful discussions with N. Prokof'ev, G. Pupillo, S. Rittenhouse, H. Sadeghpour, S. Soyler, and T. Tscherbul. This work was supported by the Institute for Atomic, Molecular, and Optical Physics (ITAMP). NR 27 TC 3 Z9 3 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAY 9 PY 2011 VL 83 IS 5 AR 053611 DI 10.1103/PhysRevA.83.053611 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 761GG UT WOS:000290384600008 ER PT J AU Reasenberg, RD Lorenzini, EC Patla, BR Phillips, JD Popescu, EE Rocco, E Thapa, R AF Reasenberg, Robert D. Lorenzini, Enrico C. Patla, Biju R. Phillips, James D. Popescu, Eugeniu E. Rocco, Emanuele Thapa, Rajesh TI A quick test of the WEP enabled by a sounding rocket SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 8th International Laser Interferometric Space Antenna (LISA) Symposium CY JUN 28-JUL 02, 2010 CL Stanford, CA ID EQUIVALENCE PRINCIPLE; STEP; SATELLITE AB We describe SR-POEM, a Galilean test of the weak equivalence principle (WEP), which is to be conducted during the free fall portion of a sounding rocket flight. This test of a single pair of substances is aimed at a measurement uncertainty of sigma(eta) < 10(-16) after averaging the results of eight separate drops, each of 40 s duration. The WEP measurement is made with a set of four laser gauges that are expected to achieve 0.1 pm Hz(-1/2). We address the two sources of systematic error that are currently of greatest concern: magnetic force and electrostatic (patch effect) force on the test mass assemblies. The discovery of a violation (eta not equal 0) would have profound implications for physics, astrophysics and cosmology. C1 [Reasenberg, Robert D.; Patla, Biju R.; Phillips, James D.; Popescu, Eugeniu E.; Rocco, Emanuele; Thapa, Rajesh] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Lorenzini, Enrico C.] Univ Padua, Fac Engn, I-35122 Padua, Italy. RP Reasenberg, RD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM reasenberg@cfa.harvard.edu RI Popescu, Eugeniu/B-7342-2012 FU NASA [NNC04GB30G, NNX07AI11G, NNX08AO04G]; Smithsonian 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. We thank the staff at the Wallops Flight Facility for their generous contribution to our understanding of the capabilities and constraints of a sounding rocket flight. NR 21 TC 11 Z9 11 U1 1 U2 9 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 MAY 7 PY 2011 VL 28 IS 9 AR 094014 DI 10.1088/0264-9381/28/9/094014 PG 11 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 752FX UT WOS:000289677700015 ER PT J AU Krakauer, DC Collins, JP Erwin, D Flack, JC Fontana, W Laubichler, MD Prohaska, SJ West, GB Stadler, PF AF Krakauer, David C. Collins, James P. Erwin, Douglas Flack, Jessica C. Fontana, Walter Laubichler, Manfred D. Prohaska, Sonja J. West, Geoffrey B. Stadler, Peter F. TI The challenges and scope of theoretical biology SO JOURNAL OF THEORETICAL BIOLOGY LA English DT Review DE Theory; Model; Physics; Parsimony; Computation ID GENE REGULATORY NETWORKS; POPULATION BIOLOGY; SYSTEMS BIOLOGY; EVOLUTION; ECONOMICS; MODEL; CHEMISTRY; SELECTION; SCIENCE AB Scientific theories seek to provide simple explanations for significant empirical regularities based on fundamental physical and mechanistic constraints. Biological theories have rarely reached a level of generality and predictive power comparable to physical theories. This discrepancy is explained through a combination of frozen accidents, environmental heterogeneity, and widespread non-linearities observed in adaptive processes. At the same time, model building has proven to be very successful when it comes to explaining and predicting the behavior of particular biological systems. In this respect biology resembles alternative model-rich frameworks, such as economics and engineering. In this paper we explore the prospects for general theories in biology, and suggest that these take inspiration not only from physics, but also from the information sciences. Future theoretical biology is likely to represent a hybrid of parsimonious reasoning and algorithmic or rule-based explanation. An open question is whether these new frameworks will remain transparent to human reason. In this context, we discuss the role of machine learning in the early stages of scientific discovery. We argue that evolutionary history is not only a source of uncertainty, but also provides the basis, through conserved traits, for very general explanations for biological regularities, and the prospect of unified theories of life. (c) 2011 Published by Elsevier Ltd. C1 [Krakauer, David C.; Erwin, Douglas; Flack, Jessica C.; Fontana, Walter; West, Geoffrey B.; Stadler, Peter F.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Collins, James P.; Laubichler, Manfred D.] Arizona State Univ, Sch Life Sci, Tempe, AZ USA. [Erwin, Douglas] Smithsonian Museum Nat Hist, Washington, DC USA. [Fontana, Walter] Harvard Univ, Sch Med, Boston, MA USA. [Prohaska, Sonja J.] Univ Leipzig, Bioinformat Grp, Dept Comp Sci, Leipzig, Germany. [Stadler, Peter F.] Fraunhofer Inst IZI, Leipzig, Germany. [Stadler, Peter F.] Max Planck Inst Math Sci, Leipzig, Germany. RP Krakauer, DC (reprint author), Santa Fe Inst, Santa Fe, NM 87501 USA. EM krakauer@santafe.edu RI Stadler, Peter F./L-7857-2015 OI Stadler, Peter F./0000-0002-5016-5191 NR 73 TC 22 Z9 28 U1 4 U2 49 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-5193 J9 J THEOR BIOL JI J. Theor. Biol. PD MAY 7 PY 2011 VL 276 IS 1 BP 269 EP 276 DI 10.1016/j.jtbi.2011.01.051 PG 8 WC Biology; Mathematical & Computational Biology SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational Biology GA 750JW UT WOS:000289543400028 PM 21315730 ER PT J AU Deiner, K Lemmon, AR Mack, AL Fleischer, RC Dumbacher, JP AF Deiner, Kristy Lemmon, Alan R. Mack, Andrew L. Fleischer, Robert C. Dumbacher, John P. TI A Passerine Bird's Evolution Corroborates the Geologic History of the Island of New Guinea SO PLOS ONE LA English DT Article ID PAPUA-NEW-GUINEA; NORTH-AMERICAN BIRDS; MITOCHONDRIAL-DNA; RAIN-FOREST; IRIAN-JAYA; AUSTRALIA; PHYLOGEOGRAPHY; SUBSTITUTIONS; BIOGEOGRAPHY; VEGETATION AB New Guinea is a biologically diverse island, with a unique geologic history and topography that has likely played a role in the evolution of species. Few island-wide studies, however, have examined the phylogeographic history of lowland species. The objective of this study was to examine patterns of phylogeographic variation of a common and widespread New Guinean bird species (Colluricincla megarhyncha). Specifically, we test the mechanisms hypothesized to cause geographic and genetic variation (e.g., vicariance, isolation by distance and founder-effect with dispersal). To accomplish this, we surveyed three regions of the mitochondrial genome and a nuclear intron and assessed differences among 23 of the 30 described subspecies from throughout their range. We found support for eight highly divergent lineages within C. megarhyncha. Genetic lineages were found within continuous lowland habitat or on smaller islands, but all individuals within clades were not necessarily structured by predicted biogeographic barriers. There was some evidence of isolation by distance and potential founder-effects. Mitochondrial DNA sequence divergence among lineages was at a level often observed among different species or even genera of birds (5-11%), suggesting lineages within regions have been isolated for long periods of time. When topographical barriers were associated with divergence patterns, the estimated divergence date for the clade coincided with the estimated time of barrier formation. We also found that dispersal distance and range size are positively correlated across lineages. Evidence from this research suggests that different phylogeographic mechanisms concurrently structure lineages of C. megarhyncha and are not mutually exclusive. These lineages are a result of evolutionary forces acting at different temporal and spatial scales concordant with New Guinea's geological history. C1 [Deiner, Kristy; Dumbacher, John P.] Calif Acad Sci, Dept Vertebrate Zool & Anthropol, San Francisco, CA 94118 USA. [Deiner, Kristy; Dumbacher, John P.] Calif Acad Sci, Ctr Comparat Genom, San Francisco, CA 94118 USA. [Deiner, Kristy] Univ Calif Davis, Genom Variat Lab, Davis, CA 95616 USA. [Lemmon, Alan R.] Florida State Univ, Dept Comp Sci, Tallahassee, FL 32306 USA. [Mack, Andrew L.] Carnegie Museum Nat Hist, Pittsburgh, PA USA. [Fleischer, Robert C.; Dumbacher, John P.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20560 USA. RP Deiner, K (reprint author), Calif Acad Sci, Dept Vertebrate Zool & Anthropol, San Francisco, CA 94118 USA. EM kldeiner@ucdavis.edu FU Smithsonian Scholarly Studies Program; National Zoo; Abbott and Sisley Funds; Christensen Fund; NSF [DEB 0108247] FX Funding was provided by the Smithsonian Scholarly Studies Program, Friends of the National Zoo, the Abbott and Sisley Funds, the Christensen Fund, and NSF Grant DEB 0108247 (PIs Dumbacher, Fleischer and Mack). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 76 TC 10 Z9 12 U1 2 U2 16 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 MAY 6 PY 2011 VL 6 IS 5 AR e19479 DI 10.1371/journal.pone.0019479 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 760DZ UT WOS:000290305600027 PM 21573115 ER PT J AU Shockley, FW Vandenberg, NJ AF Shockley, Floyd W. Vandenberg, Natalia J. TI Notes on the taxonomic identity of Bystus hirtulus (Kirsch) and transfer from Endomychidae to Coccinellidae (Coleoptera: Cucujoidea), with designation of a lectotype for Alexia hirtula Kirsch SO ZOOTAXA LA English DT Article DE Coleoptera; Endomychidae; Coccinellidae; Anamorphinae; Microweiseinae; Cryptognathini; new combinations AB During an examination of type material of the New World endomychid genus Bystus Guerin-Meneville (Anamorphinae), the type series of Alexia hirtula Kirsch from Peru was found to contain a mixture of different taxa, none of which belong to the genus Bystus, the subfamily Anamorphinae, or even the family Endomychidae. Alexia hirtula is transferred to Delphastus Casey (Coccinellidae: Microweiseinae: Serangiini), establishing the new combination, Delphastus hirtulus (Kirsch), and a lectotype is designated. Of the three paralectotypes, one appears to be conspecific with the lectotype, one is identified as an undescribed species of Microscymnus Champion (Coccinellidae: Cryptognathini), and one, a partial specimen lacking the head, pronotum, and one elytron, is identified as a species of Leiodidae in the tribe Scotocryptini, probably Aglyptinus Cockerell. A diagnosis and redescription of D. hirtulus is provided, and Gordon's (1994) key to Delphastus is modified to accommodate the newly transferred species. The historical classification of D. hirtulus is discussed along with characters justifying its revised placement. C1 [Shockley, Floyd W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Vandenberg, Natalia J.] ARS, SEL, Plant Sci Inst,USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Shockley, FW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC-165, Washington, DC 20013 USA. EM ShockleyF@si.edu; Natalia.Vandenberg@ars.usda.gov FU National Science Foundation [0329115] FX We thank Drs. Klaus Klass and Olaf Jaeger, Museum fur Tierkunde, Staatliche Naturhistorische Sammlungen Dresden (SMTD), for loaning us Kirsch's syntypes of Alexia hirtula and for allowing us to dissect one of the specimens. We thank Juanita Forrester and Adriano Giorgi, both of the University of Georgia, and Warren Steiner, Smithsonian Research Associate, National Museum of Natural History (NMNH), for their assistance in making the initial family level identifications of the syntype series. Jens Prena (SEL) translated Kirsch's original description from Latin into English and assisted in tracking down literature citations for old catalogues; both he and Chris Thompson, Smithsonian Research Associate (NMNH), provided valuable discussion on the rules governing zoological nomenclature. Lisa Roberts (SEL) created the setal map and assisted with vector outlines for the head drawings. Marie Metz captured digital images of the type series. Joe McHugh, University of Georgia, and John Brown and Al Norrbom (SEL) provided helpful comments on an earlier draft of this manuscript. This work was partially supported by the National Science Foundation under Grant No. 0329115 (to J.V. McHugh, M.F. Whiting, and K.B. Miller). NR 24 TC 1 Z9 1 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 5 PY 2011 IS 2868 BP 62 EP 68 PG 7 WC Zoology SC Zoology GA 758XF UT WOS:000290200100003 ER PT J AU Bar-Oz, G Zeder, M Hole, F AF Bar-Oz, Guy Zeder, Melinda Hole, Frank TI Role of mass-kill hunting strategies in the extirpation of Persian gazelle (Gazella subgutturosa) in the northern Levant SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID BEHAVIOR; ORIGINS; MARKS AB Continuous and intensive exploitation of wildlife resources by early agricultural societies had major ecological consequences in the ancient Near East. In particular, hunting strategies of post-Neolithic societies involving the mass killing of wild ungulates contributed to the eventual extirpation of a number of wild species. A remarkable deposit of bones of Persian gazelle (Gazella subgutarosa) from fourth millennium BCE levels at Tell Kuran in northeastern Syria provides insight into the unsustainable hunting practices that disrupted gazelle migratory patterns and helped set the course for the virtual extinction of this species and possibly other steppe species in the Levant. The social context of mass kills conducted during periods when people relied primarily on domestic livestock for animal resources sets them apart from the more targeted and sustainable practices of earlier periods, when wild animals were the major or sole source of animal protein. C1 [Bar-Oz, Guy] Univ Haifa, Zinman Inst Archaeol, IL-31905 Haifa, Israel. [Zeder, Melinda] Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Hole, Frank] Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. RP Bar-Oz, G (reprint author), Univ Haifa, Zinman Inst Archaeol, IL-31905 Haifa, Israel. EM guybar@research.haifa.ac.il; zederm@si.edu; frank.hole@yale.edu FU Smithsonian Institution FX We thank Bruce D. Smith, Paul-Louis van Berg, and two anonymous reviewers for their constructive comments on an earlier version of the draft; Paul-Louis van Berg for permitting us to reproduce images from Mission of Khisham; and Anat Regev for drafting the figures. This research was conducted while G.B-O. was on sabbatical leave at the National Museum of Natural History, Smithsonian Institute; G.B.-O. is grateful to the Smithsonian Institution for providing a short-term visitor grant. NR 41 TC 29 Z9 32 U1 1 U2 7 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 3 PY 2011 VL 108 IS 18 BP 7345 EP 7350 DI 10.1073/pnas.1017647108 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 758YF UT WOS:000290203100020 PM 21502520 ER PT J AU D'Ammando, F Raiteri, CM Villata, M Romano, P Pucella, G Krimm, HA Covino, S Orienti, M Giovannini, G Vercellone, S Pian, E Donnarumma, I Vittorini, V Tavani, M Argan, A Barbiellini, G Boffelli, F Bulgarelli, A Caraveo, P Cattaneo, PW Chen, AW Cocco, V Costa, E Del Monte, E De Paris, G Di Cocco, G Evangelista, Y Feroci, M Ferrari, A Fiorini, M Froysland, T Frutti, M Fuschino, F Galli, M Gianotti, F Giuliani, A Labanti, C Lapshov, I Lazzarotto, F Lipari, P Longo, F Marisaldi, M Mereghetti, S Morselli, A Pacciani, L Pellizzoni, A Perotti, F Piano, G Picozza, P Pilia, M Porrovecchio, G Prest, M Rapisarda, M Rappoldi, A Rubini, A Sabatini, S Soffitta, P Striani, E Trifoglio, M Trois, A Vallazza, E Zambra, A Zanello, D Agudo, I Aller, HD Aller, MF Arkharov, AA Bach, U Benitez, E Berdyugin, A Blinov, DA Buemi, CS Chen, WP Di Paola, A Dolci, M Forne, E Fuhrmann, L Gomez, JL Gurwell, MA Jordan, B Jorstad, SG Heidt, J Hiriart, D Hovatta, T Hsiao, HY Kimeridze, G Konstantinova, TS Kopatskaya, EN Koptelova, E Kurtanidze, OM Kurtanidze, SO Larionov, VM Lahteenmaki, A Leto, P Lindfors, E Marscher, AP McBreen, B McHardy, IM Morozova, DA Nilsson, K Pasanen, M Roca-Sogorb, M Sillanpaa, A Takalo, LO Tornikoski, M Trigilio, C Troitsky, IS Umana, G Antonelli, LA Colafrancesco, S Pittori, C Santolamazza, P Verrecchia, F Giommi, P Salotti, L AF D'Ammando, F. Raiteri, C. M. Villata, M. Romano, P. Pucella, G. Krimm, H. A. Covino, S. Orienti, M. Giovannini, G. Vercellone, S. Pian, E. Donnarumma, I. Vittorini, V. Tavani, M. Argan, A. Barbiellini, G. Boffelli, F. Bulgarelli, A. Caraveo, P. Cattaneo, P. W. Chen, A. W. Cocco, V. Costa, E. Del Monte, E. De Paris, G. Di Cocco, G. Evangelista, Y. Feroci, M. Ferrari, A. Fiorini, M. Froysland, T. Frutti, M. Fuschino, F. Galli, M. Gianotti, F. Giuliani, A. Labanti, C. Lapshov, I. Lazzarotto, F. Lipari, P. Longo, F. Marisaldi, M. Mereghetti, S. Morselli, A. Pacciani, L. Pellizzoni, A. Perotti, F. Piano, G. Picozza, P. Pilia, M. Porrovecchio, G. Prest, M. Rapisarda, M. Rappoldi, A. Rubini, A. Sabatini, S. Soffitta, P. Striani, E. Trifoglio, M. Trois, A. Vallazza, E. Zambra, A. Zanello, D. Agudo, I. Aller, H. D. Aller, M. F. Arkharov, A. A. Bach, U. Benitez, E. Berdyugin, A. Blinov, D. A. Buemi, C. S. Chen, W. P. Di Paola, A. Dolci, M. Forne, E. Fuhrmann, L. Gomez, J. L. Gurwell, M. A. Jordan, B. Jorstad, S. G. Heidt, J. Hiriart, D. Hovatta, T. Hsiao, H. Y. Kimeridze, G. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kurtanidze, O. M. Kurtanidze, S. O. Larionov, V. M. Lahteenmaki, A. Leto, P. Lindfors, E. Marscher, A. P. McBreen, B. McHardy, I. M. Morozova, D. A. Nilsson, K. Pasanen, M. Roca-Sogorb, M. Sillanpaa, A. Takalo, L. O. Tornikoski, M. Trigilio, C. Troitsky, I. S. Umana, G. Antonelli, L. A. Colafrancesco, S. Pittori, C. Santolamazza, P. Verrecchia, F. Giommi, P. Salotti, L. TI AGILE detection of extreme gamma-ray activity from the blazar PKS 1510-089 during March 2009 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiation mechanisms: non-thermal; galaxies: active; gamma rays: general; quasars: general; quasars: individual: PKS 1510-089 ID XMM-NEWTON OBSERVATIONS; HIGH-REDSHIFT QUASARS; LARGE-AREA TELESCOPE; RADIO-LOUD QUASARS; GALACTIC NUCLEI; 3C 454.3; MULTIWAVELENGTH OBSERVATIONS; PHOTOMETRIC CALIBRATION; SILICON TRACKER; EMISSION AB We report on the extreme gamma-ray activity from the flat spectrum radio quasar (FSRQ) PKS 1510-089 observed by the AGILE satellite in March 2009. In the same period a radio-to-optical monitoring of the source was provided by the GASP-WEBT and REM facilities. In the radio band we made use also of multi-epoch 15-GHz Very Long Baseline Array data from the MOJAVE Program to get information on the parsec-scale structure. Moreover, several Swift target of opportunity observations were triggered, adding important information on the source behaviour from optical/UV to hard X-rays. We paid particular attention to the calibration of the Swift/UVOT data to make it suitable to the blazars spectra. Simultaneous observations from radio to gamma rays allowed us to study in detail the correlation among the emission variability at different frequencies and to investigate the mechanisms at work during this high activity state of the source. In the period 9-30 March 2009, AGILE detected gamma-ray emission from PKS 1510-089 at a significance level of 21.5-sigma with an average flux over the entire period of (311 +/- 21) x 10(-8) photons cm(-2) s(-1) for photon energies above 100 MeV, and a peak level of (702 +/- 131) x 10(-8) photons cm(-2) s(-1) on daily integration. The activity detected in gamma rays occurred during a period of increasing activity from near-infrared to UV, as monitored by GASP-WEBT, REM and Swift/UVOT. A flaring episode on 26-27 March 2009 was detected from near-IR to UV, suggesting that a single mechanism is responsible for the flux enhancement observed at the end of March. By contrast, Swift/XRT observations seem to show no clear correlation of the X-ray fluxes with the optical and gamma-ray ones. However, the X-ray observations show a harder photon index (Gamma(x) similar or equal to 1.3-1.6) with respect to most FSRQs and a hint of harder-when-brighter behaviour, indicating the possible presence of a second emission component at soft X-ray energies. Moreover, the broad band spectrum from radio-to-UV confirmed the evidence of thermal features in the optical/UV spectrum of PKS 1510-089 also during high gamma-ray state. On the other hand, during 25-26 March 2009 a flat spectrum in the optical/UV energy band was observed, suggesting an important contribution of the synchrotron emission in this part of the spectrum during the brightest gamma-ray flare, therefore a significant shift of the synchrotron peak. C1 [D'Ammando, F.; Romano, P.; Vercellone, S.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy. [D'Ammando, F.; Tavani, M.; Froysland, T.; Piano, G.; Sabatini, S.; Striani, E.] Univ Roma Tor Vergata, Dip Fis, I-00133 Rome, Italy. [D'Ammando, F.; Donnarumma, I.; Vittorini, V.; Tavani, M.; Argan, A.; Cocco, V.; Costa, E.; Del Monte, E.; De Paris, G.; Evangelista, Y.; Feroci, M.; Frutti, M.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Piano, G.; Porrovecchio, G.; Rubini, A.; Sabatini, S.; Soffitta, P.; Striani, E.; Trois, A.; Zambra, A.] INAF IASF Roma, I-00133 Rome, Italy. [Raiteri, C. M.; Villata, M.] INAF, I-10025 Turin, Italy. [Pucella, G.; Rapisarda, M.] ENEA Frascati, I-00044 Rome, Italy. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Covino, S.] INAF, I-23807 Merate, LC, Italy. [Covino, S.] INAF TNG Fdn Galileo Galilei, Tenerife 38712, Spain. [Orienti, M.; Giovannini, G.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Pian, E.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Barbiellini, G.; Longo, F.; Vallazza, E.] Dip Fis, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.; Vallazza, E.] INFN Trieste, I-34127 Trieste, Italy. [Boffelli, F.; Cattaneo, P. W.; Rappoldi, A.] INFN Pavia, I-27100 Pavia, Italy. [Boffelli, F.] Univ Pavia, Dip Fis Nucl & Teor, I-27100 Pavia, Italy. [Bulgarelli, A.; Di Cocco, G.; Fuschino, F.; Gianotti, F.; Labanti, C.; Marisaldi, M.; Trifoglio, M.] INAF IASF Bologna, I-40129 Bologna, Italy. [Caraveo, P.; Chen, A. W.; Fiorini, M.; Giuliani, A.; Mereghetti, S.; Perotti, F.] INAF IASF Milano, I-20133 Milan, Italy. [Ferrari, A.] Univ Turin, Dip Fis Gen, I-10125 Turin, Italy. [Galli, M.] ENEA Bologna, I-40129 Bologna, Italy. [Lipari, P.; Zanello, D.] INFN Roma La Sapienza, I-00185 Rome, Italy. [Morselli, A.; Picozza, P.; Striani, E.] INFN Roma Tor Vergata, I-00133 Rome, Italy. [Pellizzoni, A.; Pilia, M.] INAF Oss Astron Cagliari, I-09012 Capoterra, CA, Italy. [Prest, M.] Univ Insubria, Dip Fis, I-22100 Como, Italy. [Agudo, I.; Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Agudo, I.; Gomez, J. L.; Roca-Sogorb, M.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Arkharov, A. A.; Larionov, V. M.] Russian Acad Sci, Pulkovo Observ, St Petersburg 196140, Russia. [Bach, U.; Fuhrmann, L.] MPIfR, D-53121 Bonn, Germany. [Benitez, E.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Berdyugin, A.; Lindfors, E.; Pasanen, M.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Dept Phys & Astron, Tuorla Observ, Piikkio 21500, Finland. [Blinov, D. A.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Chen, W. P.; Hsiao, H. Y.; Koptelova, E.] Natl Cent Univ, Inst Astron, Lulin Observ, Taipei, Taiwan. [Di Paola, A.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Dolci, M.] Osservatorio Astron Collurania, INAF, I-64100 Teramo, Italy. [Forne, E.] Agrupacio Astron Sabadell, Sabadell, Spain. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jordan, B.; McBreen, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin, Ireland. [Heidt, J.] Heidelberg Univ, ZAH, D-69117 Heidelberg, Germany. [Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 2280, Baja California, Mexico. [Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Kymala 02540, Finland. [Hovatta, T.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Kimeridze, G.; Kurtanidze, O. M.; Kurtanidze, S. O.] Abastumani Observ, GE-383762 Abastumani, Rep of Georgia. [Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [McHardy, I. M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21550, Finland. [Antonelli, L. A.; Colafrancesco, S.; Pittori, C.; Santolamazza, P.; Verrecchia, F.; Giommi, P.] ASI ASDC, I-00044 Rome, Italy. [Salotti, L.] ASI, I-00198 Rome, Italy. RP D'Ammando, F (reprint author), Ist Astrofis Spaziale & Fis Cosm, INAF, Via U La Malfa 153, I-90146 Palermo, Italy. EM filippo.dammando@iasf-roma.inaf.it RI Morselli, Aldo/G-6769-2011; Morozova, Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Lazzarotto, Francesco/J-4670-2012; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Blinov, Dmitry/G-9925-2013; Lahteenmaki, Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Trifoglio, Massimo/F-5302-2015; Agudo, Ivan/G-1701-2015; Grishina, Tatiana/H-6873-2013; Pittori, Carlotta/C-7710-2016; OI Morselli, Aldo/0000-0002-7704-9553; Morozova, Daria/0000-0002-9407-7804; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Blinov, Dmitry/0000-0003-0611-5784; Trifoglio, Massimo/0000-0002-2505-3630; Agudo, Ivan/0000-0002-3777-6182; Grishina, Tatiana/0000-0002-3953-6676; Pittori, Carlotta/0000-0001-6661-9779; Buemi, Carla Simona/0000-0002-7288-4613 FU Italian Space Agency (ASI); Smithsonian Institution; Academia Sinica; NSF; NASA; University of Michigan; MICIIN (Spain) [AYA2007-67627-C03-03, AYA2010-14844]; CEIC (Andalucia) [P09-FQM-4784]; Georgian National Science Foundation [GNSF/ST08/4-404]; UK Science and Technology Facilities Council; Academy of Finland [212656, 210338]; Russian RFBR foundation [09-02-00092]; Italian Space Agency [ASI-INAF I/088/06/0, I/009/10/0] FX The AGILE Mission is funded by the Italian Space Agency (ASI) with scientific participation by the Italian Institute of Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN). We thank the Swift Team for making these observations possible, particularly the duty scientists and science planners. 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. UMRAO is funded by a series of grants from the NSF and NASA and by the University of Michigan. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009, AJ, 137, 3718). Acquisition of the MAPCAT data is supported in part by MICIIN (Spain) grants AYA2007-67627-C03-03 and AYA2010-14844, and by CEIC (Andalucia) grant P09-FQM-4784. Abastumani Observatory team acknowledges financial support by the Georgian National Science Foundation through grant GNSF/ST08/4-404. The Liverpool Telescope is 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 funding from the UK Science and Technology Facilities Council. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, and others). St. Petersburg University team acknowledges support from Russian RFBR foundation via grant 09-02-00092. 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. Some of the authors acknowledge financial support by the Italian Space Agency through contract ASI-INAF I/088/06/0 and I/009/10/0 for the Study of High-Energy Astrophysics. NR 92 TC 26 Z9 28 U1 0 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2011 VL 529 AR A145 DI 10.1051/0004-6361/201016128 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811UD UT WOS:000294240700020 ER PT J AU Ehrenreich, D Desert, JM AF Ehrenreich, D. Desert, J. -M. TI Mass-loss rates for transiting exoplanets SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: general; planets and satellites: atmospheres; ultraviolet: planetary systems; ultraviolet: stars; X-rays: stars ID COROT SPACE MISSION; HOT-JUPITER PLANET; LOW-DENSITY PLANET; METAL-POOR STAR; SOLAR-TYPE STAR; BRIGHT K-STAR; SUN-LIKE STAR; EXTRASOLAR PLANET; ECCENTRIC ORBIT; GIANT PLANETS AB Exoplanets at small orbital distances from their host stars are submitted to intense levels of energetic radiations, X-rays, and extreme ultraviolet (EUV). Depending on the masses and densities of the planets and on the atmospheric heating efficiencies, the stellar energetic inputs can lead to atmospheric mass loss. These evaporation processes are observable in the ultraviolet during planetary transits. The aim of the present work is to quantify the mass-loss rates ((m) over dot), heating efficiencies (eta), and lifetimes for the whole sample of transiting exoplanets, now including hot Jupiters, hot Neptunes, and hot super-Earths. The mass-loss rates and lifetimes are estimated from an "energy diagram" for exoplanets, which compares the planet gravitational potential energy to the stellar X/EUV energy deposited in the atmosphere. We estimate the mass-loss rates of all detected transiting planets to be within 10(6) to 10(13) g s(-1) for various conservative assumptions. High heating efficiencies would imply that hot exoplanets such the gas giants WASP-12b and WASP-17b could be completely evaporated within 1 Gyr. We also show that the heating efficiency can be constrained when m. is inferred from observations and the stellar X/EUV luminosity is known. This leads us to suggest that eta approximate to 100% in the atmosphere of the hot Jupiter HD 209458b, while it could be lower for HD 189733b. Simultaneous observations of transits in the ultraviolet and X-rays are necessary to further constrain the exospheric properties of exoplanets. C1 [Ehrenreich, D.] Univ Grenoble 1, CNRS, IPAG, UMR 5274, F-38041 Grenoble 9, France. [Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ehrenreich, D (reprint author), Univ Grenoble 1, CNRS, IPAG, UMR 5274, BP 53, F-38041 Grenoble 9, France. EM david.ehrenreich@obs.ujf-grenoble.fr; jdesert@cfa.harvard.edu OI Ehrenreich, David/0000-0001-9704-5405 FU Centre National d'Etudes Spatiales (CNES) FX We thank the anonymous referee of this work. We are grateful to Alain Lecavelier des Etangs for all the discussions and advice about this work. We also thank Alfred Vidal-Madjar and Peter Wheatley for inspiration, and Jorge Sanz-Forcada for kindly providing us with updated X-ray flux measurements. D.E. is supported by the Centre National d'Etudes Spatiales (CNES). NR 130 TC 49 Z9 49 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2011 VL 529 AR A136 DI 10.1051/0004-6361/201016356 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 811UD UT WOS:000294240700011 ER PT J AU Touwaide, A AF Touwaide, Alain TI A 15th-century treatise on kidney affections and their treatment? A first approach SO JOURNAL OF NEPHROLOGY LA English DT Article DE 15th Century; Byzantium; History of medicine AB Two Greek manuscripts have preserved a short treatise On the Diagnosis of Kidney Pathologies and Their Treatment attributed to Galen. In the present article, I study the content of this work and suggest that it may describe the effect of gout on the kidneys, unless it describes pseudog-out, that is, chondrocalsinosis of kidneys. On this basis, I suggest that the treatise is not by Galen, but by the 15th-century Byzantine physician Demetrios Pepagomenos. C1 [Touwaide, Alain] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Touwaide, Alain] Inst Preservat Med Tradit, Washington, DC USA. RP Touwaide, A (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, POB 37012, Washington, DC 20013 USA. EM atouwaide@hotmail.com NR 34 TC 0 Z9 0 U1 0 U2 2 PU WICHTIG EDITORE PI MILAN PA 72/74 VIA FRIULI, 20135 MILAN, ITALY SN 1121-8428 J9 J NEPHROL JI J. Nephrol. PD MAY-JUN PY 2011 VL 24 SU 17 SI SI BP S108 EP S113 DI 10.5301/JN.2011.7764 PG 6 WC Urology & Nephrology SC Urology & Nephrology GA 816FJ UT WOS:000294583800019 PM 21614791 ER PT J AU Moore, MJ Hassan, N Gitzendanner, MA Bruenn, RA Croley, M Vandeventer, A Horn, JW Dhingra, A Brockington, SF Latvis, M Ramdial, J Alexandre, R Piedrahita, A Xi, ZX Davis, CC Soltis, PS Soltis, DE AF Moore, Michael J. Hassan, Nasr Gitzendanner, Matthew A. Bruenn, Riva A. Croley, Matthew Vandeventer, Alexia Horn, James W. Dhingra, Amit Brockington, Samuel F. Latvis, Maribeth Ramdial, Jeremy Alexandre, Roolse Piedrahita, Ana Xi, Zhenxiang Davis, Charles C. Soltis, Pamela S. Soltis, Douglas E. TI PHYLOGENETIC ANALYSIS OF THE PLASTID INVERTED REPEAT FOR 244 SPECIES: INSIGHTS INTO DEEPER-LEVEL ANGIOSPERM RELATIONSHIPS FROM A LONG, SLOWLY EVOLVING SEQUENCE REGION SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE Angiosperm Tree of Life; plastid inverted repeat; phylogenetics; large data sets ID NONCODING CHLOROPLAST DNA; FLOWERING PLANT PHYLOGENY; BASAL ANGIOSPERM; LEGUMES LEGUMINOSAE; MOLECULAR PHYLOGENY; GENOME SEQUENCES; DATA SETS; 18S RDNA; GENES; EVOLUTION AB Recent plastid phylogenomic studies have helped clarify the backbone phylogeny of angiosperms. However, the relatively limited taxon sampling in these studies has precluded strongly supported resolution of some regions of angiosperm phylogeny. Other recent work has suggested that the 25,000-bp plastid inverted repeat (IR) region may be a valuable source of characters for resolving these remaining problematic nodes. Consequently, we aligned all available angiosperm IR sequences to produce a matrix of 24,702 aligned bases for 246 accessions, including 36 new accessions. Maximum likelihood analyses of the complete data set yielded a generally well-supported topology that is highly congruent with those of recent plastid phylogenomic analyses. However, reducing taxon sampling to match a recent 83-gene plastid analysis resulted in significant changes in bootstrap support at some nodes. Notably, IR analyses resolved Pentapetalae into three well-supported clades: (1) superasterids (comprising Santalales, Caryophyllales, Berberidopsidales, and Asteridae), (2) superrosids (comprising Vitaceae, Saxifragales, and Rosidae), and (3) Dilleniaceae. These results provide important new evidence for a stable, well-supported phylogenetic framework for angiosperms and demonstrate the utility of IR data for resolving the deeper levels of angiosperm phylogeny. They also reiterate the importance of carefully considering taxon sampling in phylogenomic studies. C1 [Moore, Michael J.; Bruenn, Riva A.; Croley, Matthew] Oberlin Coll, Dept Biol, Oberlin, OH 44074 USA. [Hassan, Nasr] Assiut Univ, Dept Bot, Fac Sci, Assiut 71516, Egypt. [Gitzendanner, Matthew A.; Vandeventer, Alexia; Latvis, Maribeth; Ramdial, Jeremy; Alexandre, Roolse; Piedrahita, Ana; Soltis, Douglas E.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Horn, James W.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Dhingra, Amit] Washington State Univ, Dept Hort & Landscape Architecture, Pullman, WA 99164 USA. [Brockington, Samuel F.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Xi, Zhenxiang; Davis, Charles C.] Harvard Univ Hebaria, Cambridge, MA 02138 USA. [Soltis, Pamela S.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. RP Moore, MJ (reprint author), Oberlin Coll, Dept Biol, Oberlin, OH 44074 USA. EM michael.moore@oberlin.edu RI Soltis, Pamela/L-5184-2015; Brockington, Samuel/K-7819-2013; Dhingra, Amit/E-7369-2010; OI Brockington, Samuel/0000-0003-1216-219X; Gitzendanner, Matthew/0000-0002-7078-4336 FU NSF [EF-0431266]; University of Florida (UF) High-Performance Computing Center; UF Genetics Institute FX We thank three anonymous reviewers for helpful comments that improved the manuscript. We also thank Bob Jansen and Jim Leebens-Mack for access to unpublished genome sequences and Tom Givnish for leaf material of Lilium superbum. We acknowledge the University of Florida (UF) High-Performance Computing Center and the UF Genetics Institute for providing computational resources and support that have contributed to the research results reported in this article. We also thank Rob Ferl and Beth Laughner for lab space and general lab assistance and Gordon Burleigh for helpful correspondence. This study was carried out as part of the Angiosperm Tree of Life Project (NSF grant EF-0431266 to D. E. Soltis and P. S. Soltis, among others). NR 75 TC 40 Z9 44 U1 3 U2 32 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 EI 1537-5315 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD MAY PY 2011 VL 172 IS 4 BP 541 EP 558 DI 10.1086/658923 PG 18 WC Plant Sciences SC Plant Sciences GA 791HJ UT WOS:000292655500007 ER PT J AU Bachvaroff, TR Handy, SM Place, AR Delwiche, CF AF Bachvaroff, Tsvetan R. Handy, Sara M. Place, Allen R. Delwiche, Charles F. TI Alveolate Phylogeny Inferred using Concatenated Ribosomal Proteins SO JOURNAL OF EUKARYOTIC MICROBIOLOGY LA English DT Article DE Alveolate; apicomplexa; phylogeny; ribosomal proteins; syndinian ID OXYRRHIS-MARINA; APICOMPLEXAN PARASITES; MITOCHONDRIAL GENOME; MOLECULAR PHYLOGENY; PERKINSUS-MARINUS; GENETIC DIVERSITY; DINOFLAGELLATE; SEQUENCES; AMOEBOPHRYA; CRYPTOSPORIDIUM AB Dinoflagellates and apicomplexans are a strongly supported monophyletic group in rDNA phylogenies, although this phylogeny is not without controversy, particularly between the two groups. Here we use concatenated protein-coding genes from expressed sequence tags or genomic data to construct phylogenies including "typical" dinophycean dinoflagellates, a parasitic syndinian dinoflagellate, Amoebophrya sp., and two related species, Oxyrrhis marina, and Perkinsus marinus. Seventeen genes encoding proteins associated with the ribosome were selected for phylogenetic analysis. The dataset was limited for the most part by data availability from the dinoflagellates. Forty-five taxa from four major lineages were used: the heterokont outgroup, ciliates, dinoflagellates, and apicomplexans. Amoebophrya sp. was included in this phylogeny as a sole representative of the enigmatic marine alveolate or syndinian lineage. The atypical dinoflagellate O. marina, usually excluded from rDNA analyses due to long branches, was also included. The resulting phylogenies were well supported in concatenated analyses with only a few unstable or weakly supported branches; most features were consistent when different lineages were pruned from the tree or different genes were concatenated. The least stable branches involved the placement of Cryptosporidium spp. within the Apicomplexa and the relationships between P. marinus, Amoebophrya sp., and O. marina. Both bootstrap and approximately unbiased test results confirmed that P. marinus, Amoebophrya sp., O. marina, and the remaining dinoflagellates form a monophyletic lineage to the exclusion of Apicomplexa. C1 [Bachvaroff, Tsvetan R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Handy, Sara M.; Delwiche, Charles F.] Univ Maryland, Dept Mol Genet & Cell Biol, College Pk, MD 20742 USA. [Place, Allen R.] Univ Maryland, Ctr Environm Sci, Inst Marine & Environm Sci, Baltimore, MD 21202 USA. [Delwiche, Charles F.] Maryland Agr Expt Stn, College Pk, MD 20742 USA. RP Bachvaroff, TR (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM bachvarofft@si.edu RI Handy, Sara/C-6195-2008; Place, Allen/F-9267-2013; Delwiche, Charles/C-6549-2008 OI Delwiche, Charles/0000-0001-7854-8584 FU National Science Foundation [EF-0629624] FX This project was funded in part by a National Science Foundation grant from the Assembling the Tree of Life project (#EF-0629624). This manuscript is submission 11-4508 from UMCES. The authors would like to thank D. Wayne Coats for mentorship and support. The authors would also like to thank Dr. Ruth Timme for a critical reading of the manuscript. NR 63 TC 28 Z9 28 U1 0 U2 24 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1066-5234 J9 J EUKARYOT MICROBIOL JI J. Eukaryot. Microbiol. PD MAY-JUN PY 2011 VL 58 IS 3 BP 223 EP 233 DI 10.1111/j.1550-7408.2011.00555.x PG 11 WC Microbiology SC Microbiology GA 788CB UT WOS:000292421900006 PM 21518081 ER PT J AU Peer, BD McIntosh, CE Kuehn, MJ Rothstein, SI Fleischer, RC AF Peer, Brian D. McIntosh, Carl E. Kuehn, Michael J. Rothstein, Stephen I. Fleischer, Robert C. TI COMPLEX BIOGEOGRAPHIC HISTORY OF LANIUS SHRIKES AND ITS IMPLICATIONS FOR THE EVOLUTION OF DEFENSES AGAINST AVIAN BROOD PARASITISM SO CONDOR LA English DT Article DE brood parasitism; coevolution; cuckoo; egg rejection; Lanius; phylogeny; shrike ID DNA CONTROL REGION; COMMON GRACKLES; EGG REJECTION; COEVOLUTION; SEQUENCES; MERIDIONALIS; ABSENCE; COWBIRD AB Using portions of three mitochondrial genes to resolve the uncertain systematic relationships, we constructed a phylogeny of the "gray shrikes" in the genus Lanius. We used the tree and estimates of the rate of evolution of passeriform mtDNA genes to project the nodes' ages and to assess the pattern and age of egg-rejection behavior in shrikes. Our results suggest that Lanius excubitor and L. m. meridionalis are sister taxa and that this clade is sister to L. ludovicianus, then L. sphenocercus is sister to this clade. Lanius excubitor from the Old World was considerably diverged from both New World species and part of a clade also containing four other subspecies of L. meridionalis. The paraphyly and sequence divergence between New World and Old World L. excubitor suggest that these populations represent distinct species. Mapping egg rejection onto the phylogeny suggests that rejection is deeply rooted in shrikes, as it is present as deep as two species, L. collurio and L. bucephalus, that are outgroups to the gray shrikes and in the derived L. ludovicianus. Rejection in L. ludovicianus may have been retained as long as 1.1-1.8 million years, since its clade split from the Old World L. sphenocercus, providing more evidence that once hosts evolve rejection they retain it for long periods of time. These results suggest hosts are becoming increasingly resistant to brood parasitism, which will force parasites to specialize on a few host species. C1 [Peer, Brian D.; McIntosh, Carl E.; Fleischer, Robert C.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, 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 Biol Sci, Macomb, IL 61455 USA. RP Peer, BD (reprint author), Smithsonian Inst, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk,POB 37012 MRC 5503, Washington, DC 20013 USA. EM BD-Peer@wiu.edu FU National Science Foundation [0078139]; Western Illinois University FX We thank the following institutions and individuals for providing tissue samples used in this study: Burke Museum, University of Washington; American Museum of Natural History; University of Minnesota Bell Museum; Field Museum of Natural History; Natural History Museum, University of Kansas; University of Michigan Museum of Zoology, and Lori Eggert and Nick Mundy. Two anonymous reviewers provided comments that improved the manuscript. This research was supported by National Science Foundation grant 0078139 awarded to SIR, RCF, and BDP, and BDP and RCF were supported by a Faculty Mentoring grant from Western Illinois University while preparing the manuscript. NR 36 TC 3 Z9 4 U1 5 U2 18 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 EI 1938-5129 J9 CONDOR JI Condor PD MAY PY 2011 VL 113 IS 2 BP 385 EP 394 DI 10.1525/cond.2011.100066 PG 10 WC Ornithology SC Zoology GA 779CD UT WOS:000291754800014 ER PT J AU Kilic, M Brown, WR Kenyon, SJ Prieto, CA Andrews, J Kleinman, SJ Winget, KI Winget, DE Hermes, JJ AF Kilic, Mukremin Brown, Warren R. Kenyon, S. J. Allende Prieto, Carlos Andrews, J. Kleinman, S. J. Winget, K. I. Winget, D. E. Hermes, J. J. TI The shortest period detached binary white dwarf system SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational waves; binaries: close; stars: individual: SDSS J010657.39-100003.3; subdwarfs; white dwarfs; Galaxy: stellar content ID AM CVN STARS; SUPERNOVAE; CATALOG; ACCRETION; EVOLUTION; I. AB We identify SDSS J010657.39-100003.3 (hereafter J0106-1000) as the shortest period detached binary white dwarf (WD) system currently known. We targeted J0106-1000 as part of our radial velocity programme to search for companions around known extremely low-mass (ELM; similar to 0.2 M-circle dot) WDs using the 6.5-m Multiple Mirror Telescope. We detect peak-to-peak radial velocity variations of 740 km s(-1) with an orbital period of 39.1 min. The mass function and optical photometry rule out a main-sequence star companion. Follow-up high-speed photometric observations obtained at the McDonald 2.1-m telescope reveal ellipsoidal variations from the distorted primary but no eclipses. This is the first example of a tidally distorted WD. Modelling the light curve, we constrain the inclination angle of the system to be 67 degrees +/- 13 degrees. J0106-1000 contains a pair of WDs (0.17M(circle dot) primary + 0.43M(circle dot) invisible secondary) at a separation of 0.32 R-circle dot. The two WDs will merge in 37 Myr and most likely form a core He-burning single subdwarf star. J0106-1000 is the shortest time-scale merger system currently known. The gravitational wave strain from J0106-1000 is at the detection limit of the Laser Interferometer Space Antenna (LISA). However, accurate ephemeris and orbital period measurements may enable LISA to detect J0106-1000 above the Galactic background noise. C1 [Kilic, Mukremin; Brown, Warren R.; Kenyon, S. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Andrews, J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kleinman, S. J.] Gemini Observ, Hilo, HI 96720 USA. [Winget, K. I.; Winget, D. E.; Hermes, J. J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA under Caltech; NSF [AST-0909107]; Norman Hackerman Advanced Research Program [003658-0255-2007, 003658-0252-2009] FX We thank A. Shporer and S. Nissanke for stimulating discussions, D. Koester for kindly providing WD model spectra and an anonymous referee for useful suggestions. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. KIW, DEW and JJH gratefully acknowledge the support of the NSF under grant AST-0909107 and the Norman Hackerman Advanced Research Program under grants 003658-0255-2007 and 003658-0252-2009. NR 32 TC 28 Z9 28 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 MAY PY 2011 VL 413 IS 1 BP L101 EP L105 DI 10.1111/j.1745-3933.2011.01044.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 776SL UT WOS:000291558100022 ER PT J AU Landt, H Bentz, MC Peterson, BM Elvis, M Ward, MJ Korista, KT Karovska, M AF Landt, Hermine Bentz, Misty C. Peterson, Bradley M. Elvis, Martin Ward, Martin J. Korista, Kirk T. Karovska, Margarita TI The near-infrared radius-luminosity relationship for active galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: nuclei; quasars: general; infrared: galaxies ID BLACK-HOLE MASS; HOST-GALAXY STARLIGHT; LINE REGION SIZES; GROWTH; BULGES AB Black hole masses for samples of active galactic nuclei (AGNs) are currently estimated from single-epoch optical spectra. In particular, the size of the broad-line emitting region needed to compute the black hole mass is derived from the optical or ultraviolet continuum luminosity. Here we consider the relationship between the broad-line region size, R, and the near-infrared (near-IR) AGN continuum luminosity, L, as the near-IR continuum suffers less dust extinction than at shorter wavelengths and the prospects for separating the AGN continuum from host-galaxy starlight are better in the near-IR than in the optical. For a relationship of the form R proportional to L alpha, we obtain for a sample of 14 reverberation-mapped AGN a best-fitting slope of alpha = 0.5 +/- 0.1, which is consistent with the slope of the relationship in the optical band and with the value of 0.5 naively expected from photoionization theory. Black hole masses can then be estimated from the near-IR virial product, which is calculated using the strong and unblended Paschen broad emission lines (Pa alpha or Pa beta). C1 [Landt, Hermine] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Bentz, Misty C.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Peterson, Bradley M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Peterson, Bradley M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Elvis, Martin; Karovska, Margarita] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ward, Martin J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Korista, Kirk T.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. RP Landt, H (reprint author), Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. EM hlandt@unimelb.edu.au FU National Science Foundation (NSF) [AST-1008882]; National Aeronautics Space Administration FX We thank the anonymous referee for comments that helped us to improve the Letter. BMP acknowledges support by the National Science Foundation (NSF grant no. AST-1008882). This research has made use of the NASA/IPAC Extragalactic Data base (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics Space Administration. NR 25 TC 6 Z9 6 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2011 VL 413 IS 1 BP L106 EP L109 DI 10.1111/j.1745-3933.2011.01047.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 776SL UT WOS:000291558100023 ER PT J AU Finkbeiner, DP Goodenough, L Slatyer, TR Vogelsberger, M Weiner, N AF Finkbeiner, Douglas P. Goodenough, Lisa Slatyer, Tracy R. Vogelsberger, Mark Weiner, Neal TI Consistent scenarios for cosmic-ray excesses from Sommerfeld-enhanced dark matter annihilation SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE dark matter theory; dark matter experiments ID POSITRON FRACTION; ELECTRONS; SPECTRA; DENSITY; FERMI; CONTRACTION; DAMA/LIBRA; ENERGIES; HELIUM; SEARCH AB Anomalies in direct and indirect detection have motivated models of dark matter consisting of a multiplet of nearly-degenerate states, coupled by a new GeV-scale interaction. We perform a careful analysis of the thermal freezeout of dark matter annihilation in such a scenario. We compute the range of "boost factors" arising from Sommerfeld enhancement in the local halo for models which produce the correct relic density, and show the effect of including constraints on the saturated enhancement, from the cosmic microwave background (CMB). We find that boost factors from Sommerfeld enhancement of up to similar to 800 are possible in the local halo. When the CMB bounds on the saturated enhancement are applied, the maximal boost factor is reduced to similar to 400 for 1-2 TeV dark matter and sub-GeV force carriers, but remains large enough to explain the observed Fermi and PAMELA electronic signals. We describe regions in the DM mass-boost factor plane where the cosmic may data is well fit for a, range of final states, and show that Sommerfeld enhancement alone is enough to provide the large annihilation cross sections required to fit the data, although for light mediator masses (m(phi) less than or similar to 200 MeV) there is tension with the CMB constraints in the absence of astrophysical boost factors from substructure. Additionally, we consider the circumstances under which WIMPonium formation is relevant and find for heavy WIMPs (greater than or similar to 2 TeV) and soft-spectrum annihilation channels it can be an important consideration; we find regions with m(chi) greater than or similar to 2.8 TeV that are consistent with the CMB bounds with O(600-700) present-day boost factors. C1 [Finkbeiner, Douglas P.; Slatyer, Tracy R.; Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Finkbeiner, Douglas P.; Vogelsberger, Mark] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Goodenough, Lisa; Weiner, Neal] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Slatyer, Tracy R.; Weiner, Neal] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. RP Finkbeiner, DP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dfinkbeiner@cfa.harvard.edu; lcg261@nyu.edu; tslatyer@ias.edu; mvogelsb@cfa.harvard.edu; neal.weiner@nyu.edu FU NASA [NNX10AD85G]; American Australian Association; Institute for Advanced Study; NSF [AST-0807444, 0947827]; DOE OJI [DE-FG02-06ER41417]; Amborse Monell Foundation; [DE-FG02-90ER40542] FX We acknowledge helpful conversations with Jolyon Bloomfield, Rouven Essig, Jonathan Feng, Manoj Kaplinghat, Mariangela Lisanti, Maxim Pospelov, Josh Ruderman, Philip Schuster, Natalia Toro, and Tomer Volansky. DF and TS received partial support from NASA Theory grant NNX10AD85G. TS was partially supported by a Sir Keith Murdoch Fellowship from the American Australian Association during the early phases of this work, and gratefully acknowledges the hospitality of the Aspen Center for Physics, and support from the Institute for Advanced Study. In the later phases of this work, the research of TS was supported by grant #DE-FG02-90ER40542 and NSF grant #AST-0807444. NW is supported by DOE OJI grant #DE-FG02-06ER41417 and NSF grant #0947827, as well as support from the Amborse Monell Foundation. NR 132 TC 35 Z9 35 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 MAY PY 2011 IS 5 AR 002 DI 10.1088/1475-7516/2011/05/002 PG 36 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 772UY UT WOS:000291264100002 ER PT J AU Whittier, CA Milligan, LA Nutter, FB Cranfield, MR Power, ML AF Whittier, Christopher A. Milligan, Lauren A. Nutter, Felicia B. Cranfield, Michael R. Power, Michael L. TI Proximate Composition of Milk From Free-Ranging Mountain Gorillas (Gorilla beringei beringei) SO ZOO BIOLOGY LA English DT Article DE lactation; hand-rearing; great ape; old world primate AB Published data on milk composition for nonhuman primates, especially great apes, are lacking. Milk composition data are important for understanding the physiology and evolution of mammalian milk production, as well as the nutritional requirements of infants. For many primate species these data have added relevance because of the need to hand raise infants orphaned by poaching or separated from their mothers in captivity. The proximate composition (dry matter (DM), protein, fat, sugar) of free-ranging mountain gorilla (MG) (Gorilla beringei beringei) milk was characterized from samples (N = 10) collected opportunistically during field procedures. The mean values for mid-lactation (1-50 months) milk samples from healthy MGs (N = 7) were: 10.7% DM, 1.9% fat, 1.4% crude protein, 6.8% sugar, and 0.53 kcal/g. These results are lower in fat and total energy than most other Hominidae, including humans. One early-lactation sample was high in protein content while the composition of two samples from gorillas with poor health and suspected poor milk quality both deviated from the normal, mid-lactation pattern. This survey adds to the data available for primate milk composition and suggests that wild MG infants normally consume milk that is lower in fat and total energy than human milk. Zoo Biol 30:308-317, 2011. (C) 2010 Wiley-Liss, Inc. C1 [Whittier, Christopher A.] N Carolina State Univ, Environm Med Consortium, Raleigh, NC 27695 USA. [Whittier, Christopher A.] N Carolina State Univ, Dept Clin Sci, Raleigh, NC 27695 USA. [Whittier, Christopher A.] Smithsonian Inst, Natl Zool Pk, Dept Anim Hlth, Washington, DC 20008 USA. [Milligan, Lauren A.] Univ Calif Berkeley, Dept Anthropol, Berkeley, CA 94720 USA. [Nutter, Felicia B.] Tufts Univ Cummings, Dept Environm & Populat Hlth, Sch Vet Med, North Grafton, MA USA. [Cranfield, Michael R.] Mt Gorilla Vet Project Inc, Baltimore, MD USA. [Power, Michael L.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Nutr Lab, Washington, DC USA. [Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Res Dept, Washington, DC 20024 USA. RP Whittier, CA (reprint author), Smithsonian NZP DAH, POB 37012,MRC 5502, Washington, DC 20013 USA. EM whittierc@si.edu OI Power, Michael/0000-0002-6120-3528 FU Mountain Gorilla Veterinary Project Inc.; The Maryland Zoo in Baltimore; The Morris Animal Foundation; North Carolina State University College of Veterinary Medicine; Graduate Assistance in Areas of National Need Fellowship; The Nutrition Laboratory; Smithsonian National Zoological Park FX Grant sponsors: Mountain Gorilla Veterinary Project Inc.; The Maryland Zoo in Baltimore; The Morris Animal Foundation; North Carolina State University College of Veterinary Medicine and the Graduate Assistance in Areas of National Need Fellowship; The Nutrition Laboratory; Smithsonian National Zoological Park. NR 25 TC 4 Z9 5 U1 2 U2 15 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 MAY-JUN PY 2011 VL 30 IS 3 BP 308 EP 317 DI 10.1002/zoo.20363 PG 10 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 777EC UT WOS:000291597400007 PM 21061295 ER PT J AU Salvador, LA Biggs, JS Paul, VJ Luesch, H AF Salvador, Lilibeth A. Biggs, Jason S. Paul, Valerie J. Luesch, Hendrik TI Veraguamides A-G, Cyclic Hexadepsipeptides from a Dolastatin 16-Producing Cyanobacterium Symploca cf. hydnoides from Guam SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID CONSTITUENT AMINO-ACIDS; LYNGBYA-MAJUSCULA; ABSOLUTE-CONFIGURATION; MARINE CYANOBACTERIA; MARFEYS METHOD; SYMPLOSTATIN 1; CYCLODEPSIPEPTIDES; DEPSIPEPTIDE; COLLECTION; PEPTIDE AB Cytotoxicity-directed purification of a Symploca cf. hydnoides sample from Cetti Bay, Guam, afforded seven new cyclic depsipeptides, veraguamides A-G (1-7), together with the known compound dolastatin 16. The planar structures of 1-7 were elucidated using NMR and MS experiments, while enantioselective HPLC and Mosher's analysis of acid and base hydrolysates, respectively, were utilized to assign the absolute configurations of the stereocenters. Veraguamides A-G (1-7) are characterized by the presence of an invariant proline residue, multiple N-methylated amino acids, an alpha-hydroxy acid, and a C(8)-polyketide-derived beta-hydroxy acid moiety with a characteristic terminus as either an alkynyl bromide, alkyne, or vinyl group. These compounds and a semisynthetic analogue (8) showed moderate to weak cytotoxic activity against HT29 colorectal adenocarcinoma and HeLa cervical carcinoma cell lines. Preliminary structure-activity relationship analysis identified several sensitive positions in the veraguamide scaffold that affect the cytotoxic activity of this compound class. Dolastatin 16 showed only weak cytotoxic activity on both cell lines tested. The complete stereostructure of dolastatin 16 was proposed for the first time through degradation followed by a combination of advanced Marfey's analysis and modified Mosher's analysis using phenylglycine methyl ester as a chiral anisotropic reagent. C1 [Salvador, Lilibeth A.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Biggs, Jason S.] Univ Guam, Marine Lab, UOG Stn, Mangilao, GU 96923 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, 1600 SW Archer Rd, 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 are grateful to J. Rocca for assistance in obtaining the NMR spectra, R Montaser for providing an authentic standard of pitiprolamide, and J. Quinata of the Cetti Bay Ecostation (Agat, Guam) for providing the UOGML with access for collections. This is a contribution of the University of Guam Marine Laboratory and contribution #843 from the Smithsonian Marine Station at Fort Pierce. NR 27 TC 23 Z9 23 U1 2 U2 23 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD MAY PY 2011 VL 74 IS 5 BP 917 EP 927 DI 10.1021/np200076t PG 11 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 770ZV UT WOS:000291127900001 PM 21446699 ER PT J AU Ott, C AF Ott, Cindy TI A Visual Critique of Ken Burns's The National Parks: America's Best Idea SO PUBLIC HISTORIAN LA English DT Article DE American art; wilderness myths; visual culture; national parks AB This essay analyzes how Burns adapts his well-known documentary style to the subject of national parks and the effects of his visual representations on viewers' understanding of the parks. It offers two main critiques: first, Burns presents an ideal of nature that inhibits viewers from perceiving how they live in the same world as the parks and that undermines the management of actual parks, and second, he misrepresents park development by minimizing the contributions of American Indians and women, who are vital to understanding the history of park landscapes and nature protection. C1 [Ott, Cindy] St Louis Univ, Amer Studies Dept, St Louis, MO 63103 USA. [Ott, Cindy] Smithsonian Inst, Natl Pk Serv, Washington, DC 20560 USA. [Ott, Cindy] Montana State Univ, Museum Rockies, Bozeman, MT USA. RP Ott, C (reprint author), St Louis Univ, Amer Studies Dept, St Louis, MO 63103 USA. NR 33 TC 0 Z9 0 U1 0 U2 1 PU UNIV CALIFORNIA PRESS PI BERKELEY PA C/O JOURNALS & DIGITAL PUBLISHING DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD MAY PY 2011 VL 33 IS 2 BP 30 EP 36 DI 10.1525/tph.2011.33.2.30 PG 7 WC History SC History GA 770XS UT WOS:000291122400006 ER PT J AU Allen, K AF Allen, Kevin TI The Second Battle of Fort Sumter: The Debate over the Politics of Race and Historical Memory at the Opening of America's Civil War Centennial, 1961 SO PUBLIC HISTORIAN LA English DT Article DE centennial; civil rights; South Carolina; commemoration; slavery AB This paper investigates the ways in which contemporary social and political events shaped the commemoration of the Civil War Centennial in 1960s South Carolina. The Centennial dramatically revealed that the issues that had divided the nation in the nineteenth century remained unresolved in the twentieth. The attempt to create a comprehensive and unifying celebration by avoiding slavery as a major topic was simply not possible amidst the national conflict over segregation. The commemoration ironically came to an explosive head in Charleston a hundred years after the first shots at Fort Sumter. C1 [Allen, Kevin] Smithsonian Inst, Washington, DC 20560 USA. [Allen, Kevin] N Carolina State Hist Preservat Off, Raleigh, NC USA. [Allen, Kevin] Councils Ad Hoc Sesquicentennial Comm, Carthage, MO USA. [Allen, Kevin] City Columbia S Carolina, Planning Dept, Columbia, SC USA. RP Allen, K (reprint author), Massachusetts Dept Conservat & Recreat, Hist Curatorship Program, Boston, MA 02114 USA. NR 41 TC 1 Z9 1 U1 0 U2 1 PU UNIV CALIFORNIA PRESS PI OAKLAND PA 155 GRAND AVE, SUITE 400, OAKLAND, CA 94612-3758 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD MAY PY 2011 VL 33 IS 2 BP 94 EP 109 DI 10.1525/tph.2011.33.2.94 PG 16 WC History SC History GA 770XS UT WOS:000291122400009 ER PT J AU Catlos, EJ Baker, CB Sorensen, SS Jacob, L Cemen, I AF Catlos, Elizabeth J. Baker, Courteney B. Sorensen, Sorena S. Jacob, Lauren Cemen, Ibrahim TI Linking microcracks and mineral zoning of detachment-exhumed granites to their tectonomagmatic history: Evidence from the Salihli and Turgutlu plutons in western Turkey (Menderes Massif) SO JOURNAL OF STRUCTURAL GEOLOGY LA English DT Article DE Microcracics; Granite deformation; Menderes massif; Extensional dynamics; Microtectonics; Protomylonite ID METAMORPHIC CORE COMPLEX; HIGH-PRESSURE METAMORPHISM; CRYSTAL SIZE DISTRIBUTION; DRONNING MAUD LAND; GEDIZ GRABEN; SW TURKEY; IN-SITU; EXTENSIONAL TECTONICS; FRACTURE PROPAGATION; SOUTHWESTERN TURKEY AB The Menderes Massif (western Turkey) is a metamorphic core complex that displays linked syntectonic plutonism and detachment faulting. Fabrics in S-type peraluminous granites (Salihli and Turgutlu) in the detachment (Alasehir) footwall change from isotropic to protomylonitic to mylonitic towards the structure. Samples from the isotropic and protomylonitic zones were imaged in transmitted light, cathodoluminescence (CL), backscattered (BSE), and secondary electrons (SE), and show that these rocks contain abundant microcracks, and that plagioclase grains have zoning consistent with magma mixing. The granites contain fluid inclusion planes (FlPs), myrmekite replacing plagioclase, and the removal of blue luminescence in K-feldspar along microcracks and grain boundaries. Calcite and hydrous minerals commonly fill microcracks. The samples record features that formed due to (1) magma crystallization and ductile deformation (FlPs, mineral zoning), (2) changes in P and/or T (impingement and stress-induced microcracks in protomylonitic rocks), and (3) differences in intrinsic mineral properties (radial, cleavage, blunted, and deflected microcracks). Overprinted microcracks indicate exhumation during pulses. The Middle Miocene ages of these granites reported elsewhere are similar to those from large-scale extensional structures in Greece's Cycladic Massif. The Menderes and Cycladic core complexes may have developed simultaneously due to the widespread intrusion of subduction-related granitoids. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Catlos, Elizabeth J.; Jacob, Lauren] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA. [Baker, Courteney B.] SandRidge Energy Inc, Oklahoma City, OK 73102 USA. [Sorensen, Sorena S.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Cemen, Ibrahim] Univ Alabama, Dept Geol Sci, Tuscaloosa, AL 35487 USA. RP Catlos, EJ (reprint author), Univ Texas Austin, Dept Geol Sci, 1 Univ Stn C1100, Austin, TX 78712 USA. EM ejcatlos@gmail.com RI Catlos, Elizabeth/B-7943-2011 FU National Science Foundation [NSF-0440169]; Smithsonian Institution FX This work was supported by an award to Elizabeth J. Catlos, Ibrahim cemen, and Matthew J. Kohn from the National Science Foundation (NSF-0440169). CL images were generated with the support of the Smithsonian Institution's National Museum of Natural History Fellowship Program. CC and EB samples were collected with assistance from Ibrahim cemen, Matthew.). Kohn, M. Cemal Goncuoglu, Mete Hanger, and Emre Diniz. We acknowledge and thank Nesat Konak for providing detailed geologic maps of the granites, which aided us in locating them in the field. We thank Steven Smith, Gary Axen, and an anonymous reviewer for providing constructive comments that greatly improved the original manuscript. We appreciate editorial handling by Robert E. Holdsworth. NR 152 TC 9 Z9 9 U1 1 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0191-8141 J9 J STRUCT GEOL JI J. Struct. Geol. PD MAY PY 2011 VL 33 IS 5 BP 951 EP 969 DI 10.1016/j.jsg.2011.02.005 PG 19 WC Geosciences, Multidisciplinary SC Geology GA 767AP UT WOS:000290828000013 ER PT J AU Carlstrom, JE Ade, PAR Aird, KA Benson, BA Bleem, LE Busetti, S Chang, CL Chauvin, E Cho, HM Crawford, TM Crites, AT Dobbs, MA Halverson, NW Heimsath, S Holzapfel, WL Hrubes, JD Joy, M Keisler, R Lanting, TM Lee, AT Leitch, EM Leong, J Lu, W Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Ruhl, JE Schaffer, KK Schwan, D Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Tucker, C Vanderlinde, K Vieira, JD Williamson, R AF Carlstrom, J. E. Ade, P. A. R. Aird, K. A. Benson, B. A. Bleem, L. E. Busetti, S. Chang, C. L. Chauvin, E. Cho, H. -M. Crawford, T. M. Crites, A. T. Dobbs, M. A. Halverson, N. W. Heimsath, S. Holzapfel, W. L. Hrubes, J. D. Joy, M. Keisler, R. Lanting, T. M. Lee, A. T. Leitch, E. M. Leong, J. Lu, W. 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. Ruhl, J. E. Schaffer, K. K. Schwan, D. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Tucker, C. Vanderlinde, K. Vieira, J. D. Williamson, R. TI The 10 Meter South Pole Telescope SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID MICROWAVE BACKGROUND ANISOTROPIES; STRONG ELECTROTHERMAL FEEDBACK; POLARIZATION; BOLOMETERS; ARRAYS; WAVES; SUBMILLIMETER AB The South Pole Telescope (SPT) is a 10 m diameter, wide-field, offset Gregorian telescope with a 966 pixel, multicolor, millimeter-wave, bolometer camera. It is located at the Amundsen-Scott South Pole station in Antarctica. The design of the SPT emphasizes careful control of spillover and scattering, to minimize noise and false signals due to ground pickup. The key initial project is a large-area survey at wavelengths of 3, 2, and 1.3 mm, to detect clusters of galaxies via the Sunyaev-Zel'dovich effect and to measure the small-scale angular power spectrum of the cosmic microwave background (CMB). The data will be used to characterize the primordial matter power spectrum and to place constraints on the equation of state of dark energy. A second-generation camera will measure the polarization of the CMB, potentially leading to constraints on the neutrino mass and the energy scale of inflation. C1 [Carlstrom, J. E.; Bleem, L. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Keisler, R.; Leitch, E. M.; Luong-Van, D.; McMahon, J. J.; Meyer, S. S.; Padin, S.; Pryke, C.; Schaffer, K. K.; Vanderlinde, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Luong-Van, D.; Meyer, S. S.; Padin, S.; Pryke, C.; Vanderlinde, K.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Bleem, L. E.; Chang, C. L.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Ade, P. A. R.; Tucker, C.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Benson, B. A.; Holzapfel, W. L.; Lee, A. T.; Schwan, D.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Chauvin, E.] Gen Dynam Satcom Technol, San Jose, CA 95131 USA. [Cho, H. -M.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. [Dobbs, M. A.; Lanting, T. M.] 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. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Leong, J.; Lu, W.; Montroy, T. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Mohr, J. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Carlstrom, JE (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM jc@kicp.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; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation (NSF) [ANT-0638937, ANT-0130612]; US Antarctic Program; Raytheon Polar Services Company; NSF Physics Frontier Center at the University of Chicago [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; National Sciences and Engineering Research Council of Canada; Quebec Fonds de Recherche sur la Nature et les Technologies; Canadian Institute for Advanced Research FX We thank R. Hills for many useful discussions on the optical design. We gratefully acknowledge the contributions to the construction of the telescope from T. Hughes, P. Huntley, B. Johnson, E. Nichols, and his team of iron workers. We also thank the National Science Foundation (NSF) Office of Polar Programs, the US Antarctic Program and the Raytheon Polar Services Company for their support of the project. We are grateful for professional support from the staff of the South Pole station. The SPT is supported by the NSF 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 University group acknowledges funding from the National Sciences and Engineering Research Council of Canada, the Quebec Fonds de Recherche sur la Nature et les Technologies, and the Canadian Institute for Advanced Research. The following individuals acknowledge additional support: J. Carlstrom from the James S. McDonnell Foundation, K. Schaffer from a Kavli Institute for Cosmological Physics (KICP) Fellowship, J. McMahon from a Fermi Fellowship, Z. Staniszewski from a Graduate Assistance in Areas of National Need (GAANN) Fellowship, and A. T. Lee from the Miller Institute for Basic Research in Science, University of California, Berkeley. NR 43 TC 195 Z9 197 U1 1 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAY PY 2011 VL 123 IS 903 BP 568 EP 581 DI 10.1086/659879 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 768NY UT WOS:000290943000007 ER PT J AU Farrell, SA Servillat, M Wiersema, K Barret, D Godet, O Heywood, I Maccarone, TJ Oates, SR Plazolles, B Webb, NA AF Farrell, S. A. Servillat, M. Wiersema, K. Barret, D. Godet, O. Heywood, I. Maccarone, T. J. Oates, S. R. Plazolles, B. Webb, N. A. TI Exploring the nature of the brightest hyper-luminous X-ray source SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE accretion, accretion disks; X-rays: binaries; X-rays: individual (ESO 243-49 HLX-1) ID MASS BLACK-HOLE; PHOENIX DEEP SURVEY; GALAXY ESO 243-49; XMM-NEWTON; CATALOG; CHANDRA; HLX-1; STAR AB The small subset of hyper-luminous X-ray sources with luminosities in excess of similar to 10(41) erg s(-1) are hard to explain without the presence of an intermediate mass black hole, as significantly super-Eddington accretion and/or very small beaming angles are required. The recent discovery of HLX-1, the most luminous object in this class with a record breaking luminosity of similar to 10(42) erg s(-1) in the galaxy ESO 243-49, therefore currently provides some of the strongest evidence for the existence of intermediate mass black holes. HLX-1 is almost an order of magnitude brighter than the other hyperluminous sources, and appears to exhibit X-ray spectral and flux variability similar to Galactic stellar mass black hole X-ray binaries. In this paper we review the current state of knowledge on this intriguing source and outline the results of multi-wavelength studies from radio to ultra-violet wavelengths, including imaging and spectroscopy of the recently identified optical counterpart obtained with the Very Large Telescope. These results continue to support an intermediate mass black hole in excess of 500 M-circle dot. (C) 2011 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Farrell, S. A.; Wiersema, K.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barret, D.; Godet, O.; Plazolles, B.; Webb, N. A.] Univ Toulouse, UPS, CESR, F-31028 Toulouse 9, France. [Barret, D.; Godet, O.; Plazolles, B.; Webb, N. A.] CNRS, UMR5187, F-31028 Toulouse, France. [Heywood, I.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Maccarone, T. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Oates, S. R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Farrell, SA (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM sean.farrell@sydney.edu.au FU European Union [215212]; Chandra grants [AR9-0013X, GO9-0102X] FX We thank the anonymous referee for his/her helpful comments. S.A.F., K.W., T.J.M., I.H., and S.R.O. acknowledge STFC funding. T.J.M. thanks the European Union FP7 for support through grant 215212 lack Hole Universe M.S. is supported in part by Chandra grants AR9-0013X and GO9-0102X. NR 33 TC 8 Z9 8 U1 1 U2 4 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD MAY PY 2011 VL 332 IS 4 SI SI BP 392 EP 397 DI 10.1002/asna.201011507 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 764MG UT WOS:000290633000017 ER PT J AU Fernandez, MJ Dudley, R Bozinovic, F AF Fernandez, Maria Jose Dudley, Robert Bozinovic, Francisco TI Comparative Energetics of the Giant Hummingbird (Patagona gigas) SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Article ID FIELD METABOLIC-RATE; PHYLOGENETICALLY INDEPENDENT CONTRASTS; ECOLOGICAL IMPLICATIONS; ENERGY BUDGETS; OXYGEN-CONSUMPTION; ANNA HUMMINGBIRDS; POTENTIAL ERRORS; FOOD-CONSUMPTION; SMALL MAMMALS; CALYPTE-ANNA AB Hummingbirds (family Trochilidae) represent an extreme outcome in vertebrate physiological design and are the only birds capable of sustained hovering. The giant hummingbird (Patagona gigas) is the largest trochilid, with a mass of similar to 20 g, and is found over an altitudinal range from 0 to 4,500 m above sea level. We report here measurements of daily, basal, and hovering rates of oxygen consumption in the giant hummingbird; compare these values with data from smaller hummingbirds; and assess overall metabolic and allometric limits to trochilid body size. The sustained metabolic scope (i.e., the ratio of daily energy expenditure to basal metabolic rate) in the giant hummingbird is higher than that in smaller hummingbirds but lies below a proposed theoretical maximum value for endotherms. Scaling exponents in the allometric relationships for different modes of energetic expenditure were comparable, suggesting that the giant hummingbird, although a clear outlier in terms of body size, does not obviously deviate from metabolic relationships derived from other trochilid taxa. C1 [Fernandez, Maria Jose; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Fernandez, Maria Jose; Dudley, Robert] Univ N Carolina, Museum Vertebrate Zool, Chapel Hill, NC 27599 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. [Bozinovic, Francisco] Pontificia Univ Catolica Chile, Ctr Adv Studies Ecol & Biodivers, Dept Ecol, Fac Ciencias Biol, Santiago 6513677, Chile. RP Fernandez, MJ (reprint author), Univ N Carolina, Dept Biol, CB 3280, Chapel Hill, NC 27599 USA. EM mjfernan@email.unc.edu FU Fondo de Desarrollo de Area Prioritarias (FONDAP) [1501-0001]; University of California, Berkeley FX We thank S. Beissinger, R. Huey, G. Byrnes, G. Oatley, C. Clark, M. Beaulie, and D. Evangelista for helpful comments on the manuscript. We also thank M. V. Lopez-Calleja for helping to capture birds, assistance, and comments on the manuscript. This work would not have been possible without the generous help of Henk Visser with the doubly labeled water technique. In addition, we acknowledge his work analyzing the doubly labeled water measurements. Also, three anonymous reviewers greatly improved the manuscript. This work was funded by Fondo de Desarrollo de Area Prioritarias (FONDAP) grant 1501-0001 to F.B. and the Tinker Summer Field Research Grant (University of California, Berkeley) to M.J.F. All measurement activities reported in this article were conducted according to current Chilean law and under permit SAG-1485 from Servicio Agricola y Ganadero, Chile. NR 52 TC 7 Z9 7 U1 2 U2 25 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 EI 1537-5293 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD MAY-JUN PY 2011 VL 84 IS 3 BP 333 EP 340 DI 10.1086/660084 PG 8 WC Physiology; Zoology SC Physiology; Zoology GA 764WQ UT WOS:000290665700011 PM 21527824 ER PT J AU Givnish, TJ Barfuss, MHJ Van Ee, B Riina, R Schulte, K Horres, R Gonsiska, PA Jabaily, RS Crayn, DM Smith, JAC Winter, K Brown, GK Evans, TM Holst, BK Luther, H Till, W Zizka, G Berry, PE Sytsma, KJ AF Givnish, Thomas J. Barfuss, Michael H. J. Van Ee, Benjamin Riina, Ricarda Schulte, Katharina Horres, Ralf Gonsiska, Philip A. Jabaily, Rachel S. Crayn, Darren M. Smith, J. Andrew C. Winter, Klaus Brown, Gregory K. Evans, Timothy M. Holst, Bruce K. Luther, Harry Till, Walter Zizka, Georg Berry, Paul E. Sytsma, Kenneth J. TI PHYLOGENY, ADAPTIVE RADIATION, AND HISTORICAL BIOGEOGRAPHY IN BROMELIACEAE: INSIGHTS FROM AN EIGHT-LOCUS PLASTID PHYLOGENY SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Andes; Bromeliaceae; bromeliads; epiphytes; Guayana Shield; historical biogeography; neotropics; Poales; Serra do Mar; tank formation ID DISPERSAL-VICARIANCE ANALYSIS; INFERRING COMPLEX PHYLOGENIES; ANCESTRAL CHARACTER STATES; MOLECULAR EVOLUTION; SOUTHEASTERN BRAZIL; CHLOROPLAST GENOME; MAXIMUM-LIKELIHOOD; ANDEAN UPLIFT; SOUTH-AMERICA; BROMELIOIDEAE BROMELIACEAE AB . Premise : Bromeliaceae form a large, ecologically diverse family of angiosperms native to the New World. We use a bromeliad phylogeny based on eight plastid regions to analyze relationships within the family, test a new, eight-subfamily classification, infer the chronology of bromeliad evolution and invasion of different regions, and provide the basis for future analyses of trait evolution and rates of diversification. . Methods : We employed maximum-parsimony, maximum-likelihood, and Bayesian approaches to analyze 9341 aligned bases for four outgroups and 90 bromeliad species representing 46 of 58 described genera. We calibrate the resulting phylogeny against time using penalized likelihood applied to a monocot-wide tree based on plastid ndhF sequences and use it to analyze patterns of geographic spread using parsimony, Bayesian inference, and the program S-DIVA. . Results : Bromeliad subfamilies are related to each other as follows: (Brocchinioideae, (Lindmanioideae, (Tillandsioideae, (Hechtioideae, (Navioideae, (Pitcairnioideae, (Puyoideae, Bromelioideae))))))). Bromeliads arose in the Guayana Shield ca. 100 million years ago (Ma), spread centrifugally in the New World beginning ca. 16-13 Ma, and dispersed to West Africa ca. 9.3 Ma. Modern lineages began to diverge from each other roughly 19 Ma. . Conclusions : Nearly two-thirds of extant bromeliads belong to two large radiations: the core tillandsioids, originating in the Andes ca. 14.2 Ma, and the Brazilian Shield bromelioids, originating in the Serro do Mar and adjacent regions ca. 9.1 Ma. C1 [Givnish, Thomas J.; Van Ee, Benjamin; Riina, Ricarda; Gonsiska, Philip A.; Jabaily, Rachel S.; Sytsma, Kenneth J.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. [Barfuss, Michael H. J.; Till, Walter] Univ Vienna, Fac Life Sci, Dept Systemat & Evolutionary Bot, A-1030 Vienna, Austria. [Van Ee, Benjamin] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02183 USA. [Riina, Ricarda; Berry, Paul E.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Schulte, Katharina; Zizka, Georg] Res Inst Senckenberg, Dept Bot & Mol Evolut, D-60325 Frankfurt, Germany. [Schulte, Katharina; Zizka, Georg] Goethe Univ Frankfurt, D-60325 Frankfurt, Germany. [Schulte, Katharina; Crayn, Darren M.] James Cook Univ, Australian Trop Herbarium, Cairns, Qld 4878, Australia. [Horres, Ralf] GenXPro, D-60438 Frankfurt, Germany. [Jabaily, Rachel S.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Smith, J. Andrew C.] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. [Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Brown, Gregory K.] Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. [Evans, Timothy M.] Grand Valley State Univ, Dept Biol, Allendale, MI 49401 USA. [Holst, Bruce K.; Luther, Harry] Marie Selby Bot Gardens, Sarasota, FL 34236 USA. RP Givnish, TJ (reprint author), Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. EM givnish@wisc.edu RI Jabaily, Rachel/E-7530-2011; James Cook University, TESS/B-8171-2012; Schulte, Katharina/K-1256-2012; Crayn, Darren/A-7386-2011; Research ID, CTBCC /O-3564-2014; Riina, Ricarda/J-1032-2014 OI Crayn, Darren/0000-0001-6614-4216; Riina, Ricarda/0000-0002-7423-899X FU National Science Foundation [DEB-9981587, DEB-0830036, DEB-0431258, DEB-0129446, DEB-0129414]; Hertel Gift Fund; Commission for Interdisciplinary Ecological Studies (KIOS) at the Austrian Academy of Sciences (OAW); Deutsche Forschungsgemeinshaft [ZI 557/7-1, SCHU 2426/1-1]; Hessian initiative for the development of scientific and economic excellence (LOEWE) at the Biodiversity and Climate Research Centre, Frankfurt am Mein FX The authors gratefully acknowledge financial support for this investigation by grants from the National Science Foundation to P. E. B., K.J.S., and T.J.G. (DEB-9981587), T.J.G. (DEB-0830036), K.J.S. (DEB-0431258), and G. L. B. and T. M. E. (DEB-0129446 and DEB-0129414), and from the Hertel Gift Fund to T.J.G., from the Commission for Interdisciplinary Ecological Studies (KIOS) at the Austrian Academy of Sciences (OAW, 2007-02 to W. T. and M.H.J.B., and from the Deutsche Forschungsgemeinshaft (ZI 557/7-1, SCHU 2426/1-1) and the Hessian initiative for the development of scientific and economic excellence (LOEWE) at the Biodiversity and Climate Research Centre, Frankfurt am Mein, to G.Z. and K. S. Plant material was kindly supplied by the Selby Botanical Garden, the Palmengarten Frankfurt am Main, and the Botanical Gardens of Heidelberg. Alejandra Gandalfo provided some useful references on the geological history of the Andes. Many thanks to two anonymous reviewers and D. E. Soltis for several helpful suggestions. NR 164 TC 137 Z9 153 U1 9 U2 90 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 EI 1537-2197 J9 AM J BOT JI Am. J. Bot. PD MAY PY 2011 VL 98 IS 5 BP 872 EP 895 DI 10.3732/ajb.1000059 PG 24 WC Plant Sciences SC Plant Sciences GA 762LT UT WOS:000290480600021 PM 21613186 ER PT J AU Seymour, N Symeonidis, M Page, MJ Amblard, A Arumugam, V Aussel, H Blain, A Bock, J Boselli, A Buat, V Castro-Rodriguez, N Cava, A Chanial, P Clements, DL Conley, A Conversi, L Cooray, A Dowell, CD Dwek, E Eales, S Elbaz, D Franceschini, A Glenn, J Solares, EAG Griffin, M Hatziminaoglou, E Ibar, E Isaak, K Ivison, RJ Lagache, G Levenson, L Lu, N Madden, S Maffei, B Mainetti, G Marchetti, L Nguyen, HT O'Halloran, B Oliver, SJ Omont, A Panuzzo, P Papageorgiou, A Pearson, CP Perez-Fournon, I Pohlen, M Rawlings, JI Rizzo, D Roseboom, IG Rowan-Robinson, M Schulz, B Scott, D Shupe, DL Smith, AJ Stevens, JA Trichas, M Tugwell, KE Vaccari, M Valtchanov, I Vigroux, L Wang, L Wright, G Xu, CK Zemcov, M AF Seymour, N. Symeonidis, M. Page, M. J. Amblard, A. Arumugam, V. Aussel, H. Blain, A. Bock, J. Boselli, A. Buat, V. Castro-Rodriguez, N. Cava, A. Chanial, P. Clements, D. L. Conley, A. Conversi, L. Cooray, A. Dowell, C. D. Dwek, E. Eales, S. Elbaz, D. Franceschini, A. Glenn, J. Solares, E. A. Gonzalez Griffin, M. Hatziminaoglou, E. Ibar, E. Isaak, K. Ivison, R. J. Lagache, G. Levenson, L. Lu, N. Madden, S. Maffei, B. Mainetti, G. Marchetti, L. Nguyen, H. T. O'Halloran, B. Oliver, S. J. Omont, A. Panuzzo, P. Papageorgiou, A. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rawlings, J. I. Rizzo, D. Roseboom, I. G. Rowan-Robinson, M. Schulz, B. Scott, Douglas Shupe, D. L. Smith, A. J. Stevens, J. A. Trichas, M. Tugwell, K. E. Vaccari, M. Valtchanov, I. Vigroux, L. Wang, L. Wright, G. Xu, C. K. Zemcov, M. TI HerMES: SPIRE emission from radio-selected active galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; infrared: galaxies; radio continuum: galaxies ID STAR-FORMATION HISTORY; SPITZER MIDINFRARED SPECTROSCOPY; INFRARED LUMINOSITY FUNCTIONS; TELESCOPE EXTRAGALACTIC 1ST; M-SELECTED GALAXIES; DEEP-FIELD-SOUTH; HIGH-REDSHIFT; ENERGY-DISTRIBUTIONS; FORMING GALAXIES; SOURCE CATALOG AB We examine the rest-frame far-infrared emission from powerful radio sources with 1.4-GHz luminosity densities of 25 < log(L-1.4/W Hz-1) < 26.5 in the extragalactic Spitzer First Look Survey field. We combine Herschel/SPIRE flux densities with Spitzer/Infrared Array Camera and Multiband Imaging Photometer for Spitzer infrared data to obtain total (m) infrared luminosities for these radio sources. We separate our sources into a moderate, 0.4 < z < 0.9, and a high, 1.2 < z < 3.0, redshift sub-sample and we use Spitzer observations of a z < 0.1 3CRR sample as a local comparison. By comparison to numbers from the Square Kilometre Array (SKA) Simulated Skies, we find that our moderate-redshift sample is complete and our high-redshift sample is 14 per cent complete. We constrain the ranges of mean star formation rates (SFRs) to be 3.4-4.2, 18-41 and 80-581 M-circle dot yr-1 for the local, moderate- and high-redshift samples, respectively. Hence, we observe an increase in the mean SFR with increasing redshift which we can parametrize as similar to(1 + z)Q, where Q = 4.2 +/- 0.8. However, we observe no trends of mean SFR with radio luminosity within the moderate- or high-redshift bins. We estimate that radio-loud active galactic nuclei (AGN) in the high-redshift sample contribute 0.1-0.5 per cent to the total SFR density at that epoch. Hence, if all luminous starbursts host radio-loud AGN we infer a radio-loud phase duty cycle of 0.001-0.005. C1 [Seymour, N.; Symeonidis, M.; Page, M. J.; Rawlings, J. I.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Amblard, A.; Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Arumugam, V.; Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Aussel, H.; Chanial, P.; Elbaz, D.; Madden, S.; Panuzzo, P.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA,DSM,Irfu,CNRS, CE Saclay, F-91191 Gif Sur Yvette, France. [Blain, A.; Bock, J.; Cooray, A.; Dowell, C. D.; Levenson, L.; Lu, N.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boselli, A.; Buat, V.] Univ Aix Marseille, Lab Astrophys Marseille, OAMP, CNRS, F-13388 Marseille 13, France. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Inst Astrofis Canarias IAC, E-38200 Tenerife, Spain. [Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Univ La Laguna ULL, Dept Astrofis, E-38205 Tenerife, Spain. [Clements, D. L.; O'Halloran, B.; Rizzo, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.; Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA. [Conversi, L.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Dwek, E.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Eales, S.; Griffin, M.; Isaak, K.; Papageorgiou, A.; Pohlen, M.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Franceschini, A.; Mainetti, G.; Marchetti, L.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany. [Ibar, E.; Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Lagache, G.] Univ Paris Sud 11, Inst Astrophys Spatiale IAS, F-91405 Orsay, France. [Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Omont, A.; Vigroux, L.] Univ Paris 06, UPMC,CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Pearson, C. P.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Seymour, N (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM nps@mssl.ucl.ac.uk RI Dwek, Eli/C-3995-2012; amblard, alexandre/L-7694-2014; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI amblard, alexandre/0000-0002-2212-5395; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621; Seymour, Nicholas/0000-0003-3506-5536 NR 78 TC 21 Z9 21 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2011 VL 413 IS 3 BP 1777 EP 1786 DI 10.1111/j.1365-2966.2011.18253.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 762NW UT WOS:000290487700024 ER PT J AU Roediger, E Bruggen, M Simionescu, A Bohringer, H Churazov, E Forman, WR AF Roediger, E. Brueggen, M. Simionescu, A. Boehringer, H. Churazov, E. Forman, W. R. TI Gas sloshing, cold front formation and metal redistribution: the Virgo cluster as a quantitative test case SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: clusters: individual: A496; galaxies: clusters: individual: Perseus; galaxies: clusters: individual: Virgo; galaxies: individual: M87; galaxies: clusters: intracluster medium ID XMM-NEWTON OBSERVATIONS; EARLY-TYPE GALAXIES; X-RAY; CHANDRA OBSERVATION; CENTAURUS CLUSTER; TEMPERATURE STRUCTURE; INTERGALACTIC MEDIUM; INTRACLUSTER MEDIUM; ABUNDANCE PROFILES; PERSEUS CLUSTER AB We perform hydrodynamical simulations of minor-merger-induced gas sloshing and the subsequent formation of cold fronts in the Virgo cluster. Comparing to observations, we show for the first time that the sloshing scenario can reproduce the radii and the contrasts in X-ray brightness, projected temperature and metallicity across the cold fronts quantitatively. The comparison suggests a third cold front 20 kpc north-west of the Virgo core. We identify several new features typical for sloshing cold fronts: an alternating distribution of cool, metal-enriched X-ray brightness excess regions and warm brightness deficit regions of reduced metallicity; a constant or radially decreasing temperature accompanied by a plateau in metallicity inside the cold fronts; a warm rim outside the cold fronts and a large-scale brightness asymmetry. We can trace these new features not only in Virgo, but also in other clusters exhibiting sloshing cold fronts. By comparing synthetic and real observations, we estimate that the original minor-merger event took place about 1.5 Gyr ago when a subcluster of 1-4 x 1013 M-circle dot passed the Virgo core at 100-400 kpc distance, where a smaller mass corresponds to a smaller pericentre distance, and vice versa. From our inferred merger geometry, we derive the current location of the disturbing subcluster to be about 1-2 Mpc east of the Virgo core. A possible candidate is M60. Additionally, we quantify the metal redistribution by sloshing and discuss its importance. We verify that the subcluster required to produce the observed cold fronts could be completely ram-pressure-stripped before reaching the Virgo centre, and discuss the conditions required for this to be achieved. Finally, we demonstrate that the bow shock of a fast galaxy passing the Virgo cluster at similar to 400 kpc distance also causes sloshing and leads to very similar cold front structures. The responsible galaxy would be located about 2 Mpc north of the Virgo centre. A possible candidate is M85. C1 [Roediger, E.; Brueggen, M.] Jacobs Univ Bremen, D-28725 Bremen, Germany. [Simionescu, A.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Boehringer, H.] MPE, D-85748 Garching, Germany. [Churazov, E.] MPA, D-85748 Garching, Germany. [Churazov, E.] Moscow Space Res Inst, IKI, Moscow 117810, Russia. [Forman, W. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Roediger, E (reprint author), Jacobs Univ Bremen, POB 750 561, D-28725 Bremen, Germany. EM e.roediger@jacobs-university.de RI Churazov, Eugene/A-7783-2013 FU DFG (German Research Foundation); John-Neumann Institut at the Forschungszentrum Julich [NIC 3229, 3711]; Chandra X-ray Center [PF9-00070]; NASA [NAS8-03060]; DOE ASC/Alliances FX We acknowledge the support of the Priority Programme 'Witnesses of Cosmic History' of the DFG (German Research Foundation) and the supercomputing grants NIC 3229 and 3711 at the John-Neumann Institut at the Forschungszentrum Julich. AS acknowledges the support provided by NASA through Einstein Postdoctoral Fellowship grant number PF9-00070 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We thank John ZuHone and Ryan Johnson for helpful discussions and the anonymous referee for the useful suggestions. The results presented were produced using the FLASH code, a product of the DOE ASC/Alliances-funded Center for Astrophysical Thermonuclear Flashes at the University of Chicago. This research has made use of the NASA/IPAC Extragalactic Database which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 61 TC 54 Z9 54 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 MAY PY 2011 VL 413 IS 3 BP 2057 EP 2077 DI 10.1111/j.1365-2966.2011.18279.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 762NW UT WOS:000290487700047 ER PT J AU Sobolewska, MA Siemiginowska, A Gierlinski, M AF Sobolewska, Malgorzata A. Siemiginowska, Aneta Gierlinski, Marek TI Simulated spectral states of active galactic nuclei and observational predictions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; X-rays: galaxies ID X-RAY-EMISSION; RADIO-QUIET QUASARS; BLACK-HOLE MASS; LINE SEYFERT-1 GALAXIES; HIGH-REDSHIFT QUASARS; ENERGY-DISTRIBUTIONS; XMM-NEWTON; TIMING PROPERTIES; ACCRETION MODELS; PARAMETER SPACE AB Active galactic nuclei (AGN) and galactic black hole binaries (GBHs) represent two classes of accreting black holes. They both contain an accretion disc emitting a thermal radiation, and a non-thermal X-ray emitting 'corona'. GBHs exhibit state transitions, and the spectral states are characterized by different luminosity levels and shapes of the spectral energy distribution (SED). If AGN transitioned in a similar way, the characteristic time-scales of such transitions would exceed similar to 105 yr. Thus the probability to observe an individual AGN transiting between different spectral states is very low. In this paper we follow the spectral evolution of the GBH GRO J1655-40 and then apply its SED evolution pattern to a simulated population of AGN under the reasonable assumption that a large sample of AGN should contain a mixture of sources in different spectral states. We model the X-ray spectra of GRO J1655-40 with the eqpair model and then scale the best-fitting models with the black hole mass to simulate the AGN spectra. We compare the simulated and observed AGN SEDs to determine the spectral states of observed Type 1 AGN, LINER and NLS1 populations. We conclude that bright Type 1 AGN and NLS1 galaxies are in a spectral state similar to the soft spectral state of GBHs, while the spectral state of LINERs may correspond to the hard spectral state of GBHs. We find that taking into account the spread of the black hole masses over several orders of magnitude, as they are in the observed AGN samples, leads to a correlation between the X-ray loudness, alpha(ox), and the monochromatic luminosity at 2500 A. We predict that the alpha(ox) correlates positively with the Eddington luminosity ratio down to the critical value of lambda(crit) = L/L-E approximate to 0.01, and that this correlation changes its sign for the accretion rates below lambda(crit). C1 [Sobolewska, Malgorzata A.; Siemiginowska, Aneta] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Gierlinski, Marek] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Sobolewska, MA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM msobolewska@cfa.harvard.edu OI Gierlinski, Marek/0000-0001-9149-3514 FU NASA [NAS8-39073]; Chandra/grants [GO8-9125A, GO0-11133X] FX We would like to thank the referee for useful comments and suggestions. This research was funded in part by the NASA contract NAS8-39073. Partial support for this work was provided by the Chandra/grants GO8-9125A and GO0-11133X. NR 68 TC 15 Z9 15 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2011 VL 413 IS 3 BP 2259 EP 2268 DI 10.1111/j.1365-2966.2011.18302.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 762NW UT WOS:000290487700062 ER PT J AU Evans, NR DeGioia-Eastwood, K Gagne, M Townsley, L Broos, P Wolk, S Naze, Y Corcoran, M Oskinova, L Moffat, AFJ Wang, JF Walborn, NR AF Evans, Nancy Remage DeGioia-Eastwood, Kathleen Gagne, Marc Townsley, Leisa Broos, Patrick Wolk, Scott Naze, Yael Corcoran, Michael Oskinova, Lida Moffat, Anthony F. J. Wang, Junfeng Walborn, Nolan R. TI THE SEARCH FOR LOW-MASS COMPANIONS OF B STARS IN THE CARINA NEBULA CLUSTER TRUMPLER 16 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE open clusters and associations: individual (Trumpler 16); stars: massive ID X-RAY-EMISSION; CHEMICALLY PECULIAR STARS; ETA-CARINAE; COMPLEX PROJECT; CHANDRA; CATALOG; RADIO AB We have developed lists of likely B3-A0 stars (called "late B" stars) in the young cluster Trumpler 16. The following criteria were used: location within 3' of eta Car, an appropriate V and B - V combination, and proper motion (where available). Color and magnitude cuts have been made assuming an E(B - V) = 0.55 mag +/- 0.1, which is a good approximation close to the center of Trumpler 16. These lists have been cross-correlated with X-ray sources found in the Chandra Carina Complex Project. Previous studies have shown that only very rarely (if at all) do late main-sequence B stars produce X-rays. We present evidence that the X-ray-detected sources are binaries with low-mass companions, since stars less massive than 1.4 M-circle dot are strong X-ray sources at the age of the cluster. Both the median X-ray energies and X-ray luminosities of these sources are in good agreement with values for typical low-mass coronal X-ray sources. We find that 39% of the late B stars based on a list with proper motions have low-mass companions. Similarly, 32% of a sample without proper motions have low-mass companions. We discuss the X-ray detection completeness. These results on low-mass companions of intermediate-mass stars are complementary to spectroscopic and interferometric results and probe new parameter space of low-mass companions at all separations. They do not support a steeply rising distribution of mass ratios to low masses for intermediate-mass (5 M-circle dot) primaries, such as would be found by random pairing from the initial mass function. C1 [Evans, Nancy Remage; Wolk, Scott; Wang, Junfeng] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [DeGioia-Eastwood, Kathleen] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Gagne, Marc] W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. [Townsley, Leisa; Broos, Patrick] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Naze, Yael] Univ Liege, GAPHE Dept AGO, B-4000 Liege, Belgium. [Corcoran, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Oskinova, Lida] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Walborn, Nolan R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu RI Gagne, Marc/C-1130-2013; OI Wolk, Scott/0000-0002-0826-9261; Naze, Yael/0000-0003-4071-9346 FU Chandra X-ray Center NASA [NAS8-03060]; Chandra [GO8-9131X]; ACIS Instrument Team [SV4-74018]; NASA [NAS8-03060]; NSERC (Canada); FQRNT (Quebec); Fonds National de la Recherche Scientifique (Belgium); PRODEX XMM; Action de Recherche Concertee (CFWB Academie Wallonie Europe); STScI FX It is a pleasure to acknowledge many interesting conversations from the Chandra Carina Large Project teams, particularly the Penn State group and the massive star group. We also thank the anonymous referee for suggestions which improved the presentation of the paper. Tables 1 and 2 were generated using data from the CDS VizieR interface. N.R.E. and S.J.W. acknowledge support from the Chandra X-ray Center NASA contract NAS8-03060. This work is supported by Chandra X-ray Observatory grant GO8-9131X (PI: L. Townsley) and by the ACIS Instrument Team contract SV4-74018 (PI: G. Garmire), issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. A.F.J.M. is grateful for financial support from NSERC (Canada) and FQRNT (Quebec). Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the PRODEX XMM and Integral contracts, and the Action de Recherche Concertee (CFWB Academie Wallonie Europe). N.R.W. acknowledges support from STScI which is operated by AURA, Inc., under NASA contract NAS5-26555. NR 31 TC 24 Z9 24 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 MAY PY 2011 VL 194 IS 1 DI 10.1088/0067-0049/194/1/13 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757MC UT WOS:000290088300013 ER PT J AU Gagne, M Fehon, G Savoy, MR Cohen, DH Townsley, LK Broos, PS Povich, MS Corcoran, MF Walborn, NR Evans, NR Moffat, AFJ Naze, Y Oskinova, LM AF Gagne, Marc Fehon, Garrett Savoy, Michael R. Cohen, David H. Townsley, Leisa K. Broos, Patrick S. Povich, Matthew S. Corcoran, Michael F. Walborn, Nolan R. Evans, Nancy Remage Moffat, Anthony F. J. Naze, Yael Oskinova, Lida M. TI CARINA OB STARS: X-RAY SIGNATURES OF WIND SHOCKS AND MAGNETIC FIELDS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE open clusters and associations: individual (Cl Bochum 10, Cl Bochum 11, Cl Collinder 228, Cl Trumpler 14, Cl Trumpler 15, Cl Trumpler 16); stars: early-type; stars: individual (HD 93250, HD 93129A, HD 93403, HD 93205, HD 93343, QZ Car, SS73 24, FO 15, Cl Trumpler 16 22, CPD-59 2610, HD 93501); X-rays: stars ID THETA(1) ORIONIS-C; SPECTRAL ENERGY-DISTRIBUTIONS; XMM-NEWTON OBSERVATIONS; YOUNG STELLAR OBJECTS; HERBIG-AE/BE STARS; SUPERGIANT ZETA-ORIONIS; EMISSION-LINE PROFILES; OPEN CLUSTER NGC-6231; HELIUM-STRONG STARS; HOT-STAR AB The Chandra Carina Complex contains 200 known O- and B-type stars. The Chandra survey detected 68 of the 70 O stars and 61 of 127 known B0-B3 stars. We have assembled a publicly available optical/X-ray database to identify OB stars that depart from the canonical L-X/L-bol relation or whose average X-ray temperatures exceed 1 keV. Among the single O stars with high kT we identify two candidate magnetically confined wind shock sources: Tr16-22, O8.5 V, and LS 1865, O8.5 V((f)). The O4 III(fc) star HD 93250 exhibits strong, hard, variable X-rays, suggesting that it may be a massive binary with a period of > 30 days. The visual O2 If* binary HD 93129A shows soft 0.6 keV and hard 1.9 keV emission components, suggesting embedded wind shocks close to the O2 If* Aa primary and colliding wind shocks between Aa and Ab. Of the 11 known O-type spectroscopic binaries, the long orbital-period systems HD 93343, HD 93403, and QZ Car have higher shock temperatures than short-period systems such as HD 93205 and FO 15. Although the X-rays from most B stars may be produced in the coronae of unseen, low-mass pre-main-sequence companions, a dozen B stars with high L-X cannot be explained by a distribution of unseen companions. One of these, SS73 24 in the Treasure Chest cluster, is a new candidate Herbig Be star. C1 [Gagne, Marc; Fehon, Garrett; Savoy, Michael R.] W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. [Cohen, David H.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Townsley, Leisa K.; Povich, Matthew S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Corcoran, Michael F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, Michael F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Walborn, Nolan R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Evans, Nancy Remage] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada. [Naze, Yael] Univ Liege, Dept AGO, GAPHE, B-4000 Liege, Belgium. [Oskinova, Lida M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. RP Gagne, M (reprint author), W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. RI Gagne, Marc/C-1130-2013; OI Naze, Yael/0000-0003-4071-9346 FU SAO/Chandra X-ray Observatory [GO8-9014X, G09-0019A]; Chandra X-ray Observatory [GO8-9131X]; ACIS Instrument Team [SV4-74018]; NSERC (Canada); FQRNT (Quebec); Space Telescope Science Institute; NASA [NAS5-26555]; NSF [AST-0901646] FX This research has made extensive use of the SIMBAD and Vizier databases, operated at CDS, Strasbourg, France. This work was partially supported by SAO/Chandra X-ray Observatory grants GO8-9014X and G09-0019A (PI: Gagne). The CCCP is supported by Chandra X-ray Observatory grant GO8-9131X (PI: Townsley) and by the ACIS Instrument Team contract SV4-74018 (PI: Garmire), issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. A.F.J.M. is grateful to NSERC (Canada) and FQRNT (Quebec) for financial assistance. N.R.W. acknowledges the support of the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. M. S. P. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0901646. The authors wish to thank the anonymous referee for many helpful suggestions. NR 155 TC 48 Z9 48 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 MAY PY 2011 VL 194 IS 1 DI 10.1088/0067-0049/194/1/5 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757MC UT WOS:000290088300005 ER PT J AU Naze, Y Broos, PS Oskinova, L Townsley, LK Cohen, D Corcoran, MF Evans, NR Gagne, M Moffat, AFJ Pittard, JM Rauw, G Ud-Doula, A Walborn, NR AF Naze, Y. Broos, P. S. Oskinova, L. Townsley, L. K. Cohen, D. Corcoran, M. F. Evans, N. R. Gagne, M. Moffat, A. F. J. Pittard, J. M. Rauw, G. Ud-Doula, A. Walborn, N. R. TI GLOBAL X-RAY PROPERTIES OF THE O AND B STARS IN CARINA SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM: individual objects (Carina nebula); stars: massive; X-rays: stars ID DRIVEN STELLAR WINDS; ETA-CARINAE; OPTICAL SPECTROSCOPY; NEBULA-CLUSTER; CHANDRA; EMISSION; POPULATION; COMPLEX; ABSORPTION; ASSOCIATION AB The key empirical property of the X-ray emission from O stars is a strong correlation between the bolometric and X-ray luminosities. In the framework of the Chandra Carina Complex Project, 129 O and B stars have been detected as X-ray sources; 78 of those, all with spectral type earlier than B3, have enough counts for at least a rough X-ray spectral characterization. This leads to an estimate of the L-X-L-BOL ratio for an exceptional number of 60 O stars belonging to the same region and triples the number of Carina massive stars studied spectroscopically in X-rays. The derived log(L-X/L-BOL) is -7.26 for single objects, with a dispersion of only 0.21 dex. Using the properties of hot massive stars listed in the literature, we compare the X-ray luminosities of different types of objects. In the case of O stars, the L-X-L-BOL ratios are similar for bright and faint objects, as well as for stars of different luminosity classes or spectral types. Binaries appear only slightly harder and slightly more luminous in X-rays than single objects; the differences are not formally significant (at the 1% level), except for the L-X-L-BOL ratio in the medium (1.0-2.5 keV) energy band. Weak-wind objects have similar X-ray luminosities but they display slightly softer spectra compared with "normal" O stars with the same bolometric luminosity. Discarding three overluminous objects, we find a very shallow trend of harder emission in brighter objects. The properties of the few B stars bright enough to yield some spectral information appear to be different overall (constant X-ray luminosities, harder spectra), hinting that another mechanism for producing X-rays, besides wind shocks, might be at work. However, it must be stressed that the earliest and X-ray brightest among these few detected objects are similar to the latest O stars, suggesting a possibly smooth transition between the two processes. C1 [Naze, Y.; Rauw, G.] Univ Liege, GAPHE, Dept AGO, B-4000 Liege, Belgium. [Broos, P. S.; Townsley, L. K.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Oskinova, L.; Gagne, M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Cohen, D.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Corcoran, M. F.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Evans, N. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gagne, M.] W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada. [Moffat, A. F. J.] Ctr Rech Astrophys Quebec, Quebec City, PQ, Canada. [Pittard, J. M.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Ud-Doula, A.] Penn State Worthington Scranton, Dunmore, PA 18512 USA. [Walborn, N. R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. EM naze@astro.ulg.ac.be RI Gagne, Marc/C-1130-2013; OI Pittard, Julian/0000-0003-2244-5070; Naze, Yael/0000-0003-4071-9346 FU Fonds National de la Recherche Scientifique (Belgium); PRODEX XMM; DLR [50 OR 0804]; Royal Society; Chandra [G09-0019B]; NASA [NAS5-26555, NAS8-03060]; Chandra X-ray Observatory [GO8-9131X]; ACIS Instrument Team [SV4-74018] FX The authors thank J. McArthur for providing 0th order spectra of some of the piled-up sources, enabling comparison with the reconstructed data. The authors also thank the anonymous referee for his/her help. Y.N. also thanks her daughter Anais Celeste for letting her finish this paper while she was only one week old. Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the PRODEX XMM and Integral contracts, and the "Action de Recherche Concertee" (CFWB-Academie Wallonie Europe). L.O. acknowledges DLR grant 50 OR 0804 (LMO), J. M. P. thanks the Royal Society for funding a University Research Fellowship, and D. C. acknowledges support from the Chandra grant G09-0019B. The Space Telescope Science Institute is operated by AURA, Inc., under NASA contract NAS5-26555. This work is supported by Chandra X-ray Observatory grant GO8-9131X (PI: L. Townsley) and by the ACIS Instrument Team contract SV4-74018 (PI: G. Garmire), issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. NR 55 TC 59 Z9 59 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 MAY PY 2011 VL 194 IS 1 DI 10.1088/0067-0049/194/1/7 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757MC UT WOS:000290088300007 ER PT J AU Povich, MS Townsley, LK Broos, PS Gagne, M Babler, BL Indebetouw, R Majewski, SR Meade, MR Getman, KV Robitaille, TP Townsend, RHD AF Povich, Matthew S. Townsley, Leisa K. Broos, Patrick S. Gagne, Marc Babler, Brian L. Indebetouw, Remy Majewski, Steven R. Meade, Marilyn R. Getman, Konstantin V. Robitaille, Thomas P. Townsend, Richard H. D. TI CANDIDATE X-RAY-EMITTING OB STARS IN THE CARINA NEBULA IDENTIFIED VIA INFRARED SPECTRAL ENERGY DISTRIBUTIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE infrared: stars; ISM: individual objects (NGC 3372); methods: data analysis; stars: early-type; X-rays: stars ID YOUNG STELLAR OBJECTS; SPITZER-SPACE-TELESCOPE; ETA-CARINAE; INTERSTELLAR EXTINCTION; COMPLEX PROJECT; FORMATION HISTORY; PROPER MOTIONS; MASSIVE STARS; B STARS; M17 AB We report the results of a new survey of massive, OB stars throughout the Carina Nebula using the X-ray point source catalog provided by the Chandra Carina Complex Project (CCCP) in conjunction with infrared (IR) photometry from the Two Micron All-Sky Survey and the Spitzer Space Telescope Vela-Carina survey. Mid-IR photometry is relatively unaffected by extinction, hence it provides strong constraints on the luminosities of OB stars, assuming that their association with the Carina Nebula, and hence their distance, is confirmed. We fit model stellar atmospheres to the optical (UBV) and IR spectral energy distributions (SEDs) of 182 OB stars with known spectral types and measure the bolometric luminosity and extinction for each star. We find that the extinction law measured toward the OB stars has two components: A(V) = 1-1.5 mag produced by foreground dust with a ratio of total-to-selective absorption R-V = 3.1 plus a contribution from local dust with R-V > 4.0 in the Carina molecular clouds that increases as A(V) increases. Using X-ray emission as a strong indicator of association with Carina, we identify 94 candidate OB stars with L-bol greater than or similar to 10(4) L-circle dot by fitting their IR SEDs. If the candidate OB stars are eventually confirmed by follow-up spectroscopic observations, the number of cataloged OB stars in the Carina Nebula will increase by similar to 50%. Correcting for incompleteness due to OB stars falling below the L-bol cutoff or the CCCP detection limit, these results potentially double the size of the young massive stellar population. C1 [Povich, Matthew S.; Townsley, Leisa K.; Broos, Patrick S.; Getman, Konstantin V.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Gagne, Marc] W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. [Babler, Brian L.; Meade, Marilyn R.; Townsend, Richard H. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Indebetouw, Remy; Majewski, Steven R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Robitaille, Thomas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Povich, MS (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM povich@astro.psu.edu RI Gagne, Marc/C-1130-2013; OI Babler, Brian/0000-0002-6984-5752; Robitaille, Thomas/0000-0002-8642-1329 FU NSF [AST-0901646]; Chandra X-ray Observatory [GO8-9131X]; ACIS Instrument Team [SV4-74018]; NASA [NAS8-03060]; Spitzer Space Telescope GO program [40791]; NASA FX We thank the anonymous referee for a prompt, insightful review that helped improve this work, in particular the discussion of systematic errors. We also thank N. R. Walborn and L. M. Oskinova for helpful conversations. M. S. P. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0901646. This work is also supported by Chandra X-ray Observatory grant GO8-9131X (PI: L. K. T.) and by the ACIS Instrument Team contract SV4-74018 (PI: G. Garmire), issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. This work is based on observations from the Spitzer Space Telescope GO program 40791 (Vela-Carina; PI: S. R. M.), supported by NASA through an award issued by the Jet Propulsion Laboratory, California Institute of Technology. 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. NR 71 TC 27 Z9 27 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 MAY PY 2011 VL 194 IS 1 DI 10.1088/0067-0049/194/1/6 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757MC UT WOS:000290088300006 ER PT J AU Townsley, LK Broos, PS Corcoran, MF Feigelson, ED Gagne, M Montmerle, T Oey, MS Smith, N Garmire, GP Getman, KV Povich, MS Evans, NR Naze, Y Parkin, ER Preibisch, T Wang, JF Wou, SJ Chu, YH Cohen, DH Gruendl, RA Hamaguchi, K King, RR Mac Low, MM McCaughrean, MJ Moffat, AFJ Oskinova, LM Pittard, JM Stassun, KG Ud-Doula, A Walborn, NR Waldron, WL Churchwell, E Nictiols, JS Owocki, SP Schulz, NS AF Townsley, Leisa K. Broos, Patrick S. Corcoran, Michael F. Feigelson, Eric D. Gagne, Marc Montmerle, Thierry Oey, M. S. Smith, Nathan Garmire, Gordon P. Getman, Konstantin V. Povich, Matthew S. Evans, Nancy Remage Naze, Yael Parkin, E. R. Preibisch, Thomas Wang, Junfeng Wou, Scott J. Chu, You-Hua Cohen, David H. Gruendl, Robert A. Hamaguchi, Kenji King, Robert R. Mac Low, Mordecai-Mark McCaughrean, Mark J. Moffat, Anthony F. J. Oskinova, L. M. Pittard, Julian M. Stassun, Keivan G. Ud-Doula, Asif Walborn, Nolan R. Waldron, Wayne L. Churchwell, Ed Nictiols, J. S. Owocki, Stanley P. Schulz, N. S. TI AN INTRODUCTION TO THE CHANDRA CARINA COMPLEX PROJECT SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE H II regions; stars: massive; stars: pre-main sequence; X-rays: individual (Carina); X-rays: ISM; X-rays: stars ID X-RAY-EMISSION; STAR-FORMING REGIONS; ORION ULTRADEEP PROJECT; YOUNG STELLAR OBJECTS; ETA-CARINAE; COLLIDING WINDS; NEBULA-CLUSTER; MASSIVE STARS; TRUMPLER 16; 30 DORADUS AB The Great Nebula in Carina provides an exceptional view into the violent massive star formation and feedback that typifies giant H II regions and starburst galaxies. We have mapped the Carina star-forming complex in X-rays, using archival Chandra data and a mosaic of 20 new 60 ks pointings using the Chandra X-ray Observatory's Advanced CCD Imaging Spectrometer, as a testbed for understanding recent and ongoing star formation and to probe Carina's regions of bright diffuse X-ray emission. This study has yielded a catalog of properties of > 14,000 X-ray point sources;> 9800 of them have multiwavelength counterparts. Using Chandra's unsurpassed X-ray spatial resolution, we have separated these point sources from the extensive, spatially-complex diffuse emission that pervades the region; X-ray properties of this diffuse emission suggest that it traces feedback from Carina's massive stars. In this introductory paper, we motivate the survey design, describe the Chandra observations, and present some simple results, providing a foundation for the 15 papers that follow in this special issue and that present detailed catalogs, methods, and science results. C1 [Townsley, Leisa K.; Broos, Patrick S.; Feigelson, Eric D.; Garmire, Gordon P.; Getman, Konstantin V.; Povich, Matthew S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Corcoran, Michael F.; Hamaguchi, Kenji] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, Michael F.; Hamaguchi, Kenji] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, Michael F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Gagne, Marc] W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. [Montmerle, Thierry] Inst Astrophys, F-75014 Paris, France. [Oey, M. S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Evans, Nancy Remage; Wang, Junfeng; Nictiols, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Naze, Yael] Univ Liege, Dept AGO, GAPHE, B-4000 Liege, Belgium. [Parkin, E. R.] Univ Liege, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium. [Parkin, E. R.; Pittard, Julian M.] Univ Leeds, Sch Phys & Astron, Leeds L52 9JT, W Yorkshire, England. [Preibisch, Thomas] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany. [Chu, You-Hua; Gruendl, Robert A.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Cohen, David H.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Hamaguchi, Kenji] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [King, Robert R.; McCaughrean, Mark J.] Univ Exeter, Coll Engn Math & Phys Sci, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Mac Low, Mordecai-Mark] Amer Museum Nat Hist, Div Phys Sci, New York, NY 10024 USA. [McCaughrean, Mark J.] European Space Agcy, Res & Sci Support Dept, Estec, NL-2200 AG Noordwijk, Netherlands. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Moffat, Anthony F. J.] Univ Montreal, Ctr Rech Astrophys Quebec, Montreal, PQ H3C 3J7, Canada. [Oskinova, L. M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Ud-Doula, Asif] Penn State Worthington Scranton, Dunmore, PA 18512 USA. [Walborn, Nolan R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Waldron, Wayne L.] Eureka Sci Inc, Oakland, CA 94602 USA. [Churchwell, Ed] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Owocki, Stanley P.] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA. [Schulz, N. S.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Townsley, LK (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM townsley@astro.psu.edu RI Gagne, Marc/C-1130-2013; OI Pittard, Julian/0000-0003-2244-5070; Wolk, Scott/0000-0002-0826-9261; Mac Low, Mordecai-Mark/0000-0003-0064-4060; Naze, Yael/0000-0003-4071-9346 FU Chandra X-ray Observatory [GO8-9131X]; ACIS Instrument Team [SV4-74018]; NASA [NAS8-03060]; NSF Astronomy and Astrophysics [AST-0901646] FX We very much appreciate the time and effort donated by our anonymous referee to improve this paper. This work is supported by Chandra X-ray Observatory grant GO8-9131X (PI: L. Townsley) and by the ACIS Instrument Team contract SV4-74018 (PI: G. Garmire), issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. S.J.W. is also supported by NASA contract NAS8-03060 (Chandra). M. S. P. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0901646. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under US Government grant NAG W-2166. Near-IR observations were collected with the HAWK-I instrument on the VLT at Paranal Observatory, Chile, under ESO program 60.A-9284(K). This research made use of data products from the Midcourse Space Experiment, the NASA/IPAC Infrared Science Archive, NASA's Astrophysics Data System, and the VizieR catalog access tool, operated at CDS, Strasbourg, France. NR 108 TC 63 Z9 63 U1 1 U2 7 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 MAY PY 2011 VL 194 IS 1 DI 10.1088/0067-0049/194/1/1 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757MC UT WOS:000290088300001 ER PT J AU Wang, JF Feigelson, ED Townsley, LK Broos, PS Getman, KV Wolk, SJ Preibisch, T Stassun, KG Moffat, AFJ Garmire, G King, RR McCaughrean, MJ Zinnecker, H AF Wang, Junfeng Feigelson, Eric D. Townsley, Leisa K. Broos, Patrick S. Getman, Konstantin V. Wolk, Scott J. Preibisch, Thomas Stassun, Keivan G. Moffat, Anthony F. J. Garmire, Gordon King, Robert R. McCaughrean, Mark J. Zinnecker, Hans TI A CHANDRA ACIS STUDY OF THE YOUNG STAR CLUSTER TRUMPLER 15 IN CARINA AND CORRELATION WITH NEAR-INFRARED SOURCES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM: individual objects (Great Nebula in Carina); open clusters and associations: individual (Trumpler 15); stars: pre-main sequence; X-rays: stars ID X-RAY-EMISSION; ORION ULTRADEEP PROJECT; INTERMEDIATE-MASS STARS; MAIN-SEQUENCE; ETA-CARINAE; STELLAR POPULATION; FORMING COMPLEX; NEBULA-CLUSTER; CEPHEUS-B; TR 14 AB Using the highest-resolution X-ray observation of the Trumpler 15 star cluster taken by the Chandra X-ray Observatory, we estimate the total size of its stellar population by comparing the X-ray luminosity function (XLF) of the detected sources to a calibrator cluster and identify for the first time a significant fraction (similar to 14%) of its individual members. The highest-resolution near-IR observation of Trumpler 15 (taken by the HAWK-I instrument on the Very Large Telescope) was found to detect most of our X-ray selected sample of cluster members, with a K-excess disk frequency of 3.8% +/- 0.7%. The near-IR data, XLF, and published spectral types of the brightest members support a cluster age estimate (5-10 Myr) that is older than those for the nearby Trumpler 14 and Trumpler 16 clusters, and suggest that high-mass members may have already exploded as supernovae. The morphology of the inner similar to 0.7 pc core of the cluster is found to be spherical. However, the outer regions (beyond similar to 2 pc) are elongated, forming an "envelope" of stars that, in projection, appears to connect Trumpler 15 to Trumpler 14; this morphology supports the view that these clusters are physically associated. Clear evidence of mass segregation is seen. This study appears in this special issue devoted to the Chandra Carina Complex Project, a 1.42 deg(2) Chandra X-ray survey of the Great Nebula in Carina. C1 [Wang, Junfeng; Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Feigelson, Eric D.; Townsley, Leisa K.; Broos, Patrick S.; Getman, Konstantin V.; Garmire, Gordon] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Preibisch, Thomas] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada. [King, Robert R.; McCaughrean, Mark J.] Univ Exeter, Astrophys Grp, Coll Engn Math & Phys Sci, Exeter EX4 4QL, Devon, England. [McCaughrean, Mark J.] European Space Agcy, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Zinnecker, Hans] Astrophy Inst Potsdam, D-14482 Potsdam, Germany. RP Wang, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261 FU Chandra [GO8-9131X]; ACIS Instrument Team [SV4-74018]; NASA [NAS8-03060, NNX08-AW89G, NAS803060]; NSERC (Canada); FQRNT (Quebec); Leverhulme [F/00 144/BJ]; NASA; National Science Foundation FX We thank the anonymous referee for providing constructive comments, M. Povich for helpful discussion, and G. Carraro for information on the optical catalog published in Carraro 2002). This work is supported by Chandra X-ray Observatory grant GO8-9131X (PI: L. Townsley) and by the ACIS Instrument Team contract SV4-74018 (PI: G. Garmire), issued by the Chandra X-ray Center (CXC), which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. J.W. is supported by NASA grant NNX08-AW89G and Chandra grant GO8-9101X (PI: Fabbiano). S. J.W. is supported by NASA contract NAS803060 (CXC). A.F.J.M thanks NSERC (Canada) and FQRNT (Quebec) for financial assistance. R. R. K. is supported by a Leverhulme research project grant (F/00 144/BJ). The near-infrared observations were collected with the HAWK-I instrument on the VLT at Paranal Observatory, Chile, under ESO program 60.A-9284(K). 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. This research has made use of the SIMBAD database and the VizieR catalog access tool, operated at CDS, Strasbourg, France. NR 71 TC 29 Z9 29 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2011 VL 194 IS 1 DI 10.1088/0067-0049/194/1/11 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757MC UT WOS:000290088300011 ER PT J AU Wolk, SJ Broos, PS Getman, KV Feigelson, ED Preibisch, T Townsley, LK Wang, JF Stassun, KG King, RR McCaughrean, MJ Moffat, AFJ Zinnecker, H AF Wolk, Scott J. Broos, Patrick S. Getman, Konstantin V. Feigelson, Eric D. Preibisch, Thomas Townsley, Leisa K. Wang, Junfeng Stassun, Keivan G. King, Robert R. McCaughrean, Mark J. Moffat, Anthony F. J. Zinnecker, Hans TI THE CHANDRA CARINA COMPLEX PROJECT VIEW OF TRUMPLER 16 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM: individual objects (Great Nebula in Carina); open clusters and associations: individual (Trumpler 16); stars: pre-main sequence; X-rays: stars ID X-RAY-EMISSION; ORION ULTRADEEP PROJECT; ETA-CARINAE; STELLAR POPULATION; NEBULA-CLUSTER; SPECTRAL MORPHOLOGY; EXTINCTION LAW; STAR-CLUSTERS; MASS STARS; OB STARS AB Trumpler 16 is a well-known rich star cluster containing the eruptive supergiant eta Carinae and located in the Carina star-forming complex. In the context of the Chandra Carina Complex Project, we study Trumpler 16 using new and archival X-ray data. A revised X-ray source list of the Trumpler 16 region contains 1232 X-ray sources including 1187 likely Carina members. These are matched to 1047 near-infrared counterparts detected by the HAWK-I instrument at the Very Large Telescope allowing for better selection of cluster members. The cluster is irregular in shape. Although it is roughly circular, there is a high degree of sub-clustering, with no noticeable central concentration and an extension to the southeast. The high-mass stars show neither evidence of mass segregation nor evidence of strong differential extinction. The derived power-law slope of the X-ray luminosity function for Trumpler 16 reveals a much steeper function than the Orion Nebula Cluster, implying a different ratio of solarto higher-mass stars. We estimate the total Trumpler 16 pre-main-sequence population to be > 6500 Class II and Class III X-ray sources. An overall K-excess disk frequency of similar to 8.9% is derived using the X-ray-selected sample, although there is some variation among the sub-clusters, especially in the southeastern extension. X-ray emission is detected from 29 high-mass stars with spectral types between B2 and O3. C1 [Wolk, Scott J.; Wang, Junfeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Broos, Patrick S.; Getman, Konstantin V.; Feigelson, Eric D.; Townsley, Leisa K.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Preibisch, Thomas] Univ Munich, Univ Sternwarte, D-81679 Munich, Germany. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [King, Robert R.; McCaughrean, Mark J.] Univ Exeter, Astrophys Grp, Coll Engn Math & Phys Sci, Exeter EX4 4QL, Devon, England. [McCaughrean, Mark J.] European Space Agcy, Estec, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada. [Zinnecker, Hans] Univ Stuttgart, Deutsch SOFIA Inst, D-7000 Stuttgart, Germany. [Zinnecker, Hans] NASA, Ames Res Ctr, Washington, DC USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261 FU NASA [NAS8-03060 (Chandra)]; Chandra [GO8-9131X]; ACIS Instrument Team [SV4-74018]; NSERC (Canada); FQRNT (Quebec) FX We thank the referee for many useful comments. S.J.W. is supported by NASA contract NAS8-03060 (Chandra). This work is supported by Chandra X-ray Observatory grant GO8-9131X (PI: L. Townsley) and by the ACIS Instrument Team contract SV4-74018 (PI: G. Garmire), issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. A.F.J.M. is grateful to NSERC (Canada) and FQRNT (Quebec) for financial aide. The near-infrared observations were collected with the HAWK-I instrument on the VLT at Paranal Observatory, Chile, under ESO program 60.A-9284(K). This research has made use of the SIMBAD database and the VizieR catalog access tool, operated at CDS, Strasbourg, France. NR 59 TC 31 Z9 31 U1 1 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 MAY PY 2011 VL 194 IS 1 DI 10.1088/0067-0049/194/1/12 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757MC UT WOS:000290088300012 ER PT J AU Berman, DC Balme, MR Rafkin, SCR Zimbelman, JR AF Berman, Daniel C. Balme, Matthew R. Rafkin, Scot C. R. Zimbelman, James R. TI Transverse Aeolian Ridges (TARs) on Mars II: Distributions, orientations, and ages SO ICARUS LA English DT Article DE Mars; Mars, Surface; Mars, Climate ID THERMAL-CONDUCTIVITY MEASUREMENTS; PARTICULATE MATERIALS; MERIDIANI PLANUM; DEPOSITS; EXPLORATION; RESOLUTION; EVOLUTION; CRATER; DUNES; MODEL AB Transverse Aeolian Ridges (TARs), 10 m scale, ripple-like aeolian bedforms with simple morphology, are widespread on Mars but it is unknown what role they play in Mars' wider sediment cycle. We present the results of a survey of all Mars Global Surveyor Narrow angle images in a pole-to-pole study area, 45 longitude wide. Following on from the classification scheme and preliminary surveys of Balme et al. (Balme, M.R., Berman, D.C., Bourke, MC., Zimbelman, J.R. [2008a] Geomorphology 101,703-720) and Wilson and Zimbelman (Wilson, S.A., Zimbelman, J.R. [2004].J. Geophys. Res. 109 (E10). doi:10.1029/2004JE002247) we searched more than 10,000 images, and found that over 2000 reveal at least 5% areal cover by TARs. The mean TAR areal cover in the study area is about 7% (3% in the northern hemisphere and 11% in the southern hemisphere) but TARs are not homogenously distributed - they are concentrated in the mid-low latitudes and almost absent pole-ward of 35 degrees N and 55 degrees S. We found no clear correlation between TAR distribution and any of thermal inertia, kilometer-scale roughness, or elevation. We did find that TARS are less common at extremes of elevation. We found that TARs are most common near the equator (especially in the vicinity of Meridiani Planum, in which area they have a distinctive "barchan-like" morphology) and in large southern-hemisphere impact craters. TARs in the equatorial band are usually associated with outcrops of layered terrain or steep slopes, hence their relative absence in the northern hemisphere. TARs in the southern hemisphere are most commonly associated with low albedo, intercrater dune fields. We speculate that the mid-latitude mantling terrain (e.g., Mustard, J.F., Cooper, CD., Rifkin, M.K. [2001]. Nature 412, 411-414; Kreslavsky, MA., Head, J.W. [2002].J Geophys. Res. 29(15). doi:10.1029/2002GL015392) could also play a role in covering TARs or inhibiting saltation. We compared TAR distribution with general circulation model (GCM) climate data for both surface wind shear stress and wind direction. We performed GCM runs at various obliquity values to simulate the effects of changing obliquity on recent Mars climate. We found good general agreement between TAR orientation and GCM wind directions from present day obliquity conditions in many cases, but found no good correlation between wind shear stress and TAR distribution. We performed preliminary high resolution crater count studies of TARs in both equatorial and southern intracrater dunefield settings and compared these to superposition relationships between TARs and large dark dunes. Our results show that TARs near dunefield appear to be younger than TARs in the equatorial regions. We infer that active saltation from the large dunes keeps TARs active, but that TARs are not active under present day condition when distal to large dunes - perhaps supporting the interpretation that TARs are granule ripples. We conclude that local geology, rather than wind strength, controls TAR distribution, but that their orientation matches present-day regional wind patterns in most cases. We suggest that TARs are likely most (perhaps only) active today when they are proximal to large dark dune fields. (C) 2011 Elsevier Inc. All rights reserved. C1 [Berman, Daniel C.; Balme, Matthew R.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Balme, Matthew R.] Open Univ, Dept Earth & Environm Sci, Milton Keynes MK7 6AA, Bucks, England. [Rafkin, Scot C. R.] SW Res Inst, Boulder, CO 80302 USA. [Zimbelman, James R.] Natl Air & Space Museum, Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Berman, DC (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA. EM bermandc@psi.edu OI Balme, Matthew/0000-0001-5871-7475 NR 46 TC 21 Z9 22 U1 1 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2011 VL 213 IS 1 BP 116 EP 130 DI 10.1016/j.icarus.2011.02.014 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TR UT WOS:000290190100009 ER PT J AU Moullet, A Lellouch, E Moreno, R Gurwell, M AF Moullet, Arielle Lellouch, Emmanuel Moreno, Raphael Gurwell, Mark TI Physical studies of Centaurs and Trans-Neptunian Objects with the Atacama Large Millimeter Array SO ICARUS LA English DT Article DE Trans-Neptunian Objects; Centaurs; Instrumentation ID STELLAR OCCULTATION; PLUTOS SURFACE; SOLAR-SYSTEM; LIGHT CURVES; SIZE; REGION; TNOS; COOL; CHARON; ATMOSPHERE AB Once completed, the Atacama Large Millimeter Array (ALMA) will be the most powerful (sub)millimeter interferometer in terms of sensitivity, spatial resolution and imaging. This paper presents the capabilities of ALMA applied to the observation of Centaurs and Trans-Neptunian Objects, and their possible output in terms of physical properties. Realistic simulations were performed to explore the performances of the different frequency bands and array configurations, and several projects are detailed along with their feasibility, their limitations and their possible targets. Determination of diameters and albedos via the radiometric method appears to be possible on similar to 500 objects, while sampling of the thermal lightcurve to derive the bodies' ellipticity could be performed at least 30 bodies that display a significant optical lightcurve. On a limited number of objects, the spatial resolution allows for direct measurement of the size or even surface mapping with a resolution down to 13 milliarcsec. Finally, ALMA could separate members of multiple systems with a separation power comparable to that of the HST. The overall performance of ALMA will make it an invaluable instrument to explore the outer Solar System, complementary to space-based telescopes and spacecrafts. (C) 2011 Elsevier Inc. All rights reserved. C1 [Moullet, Arielle; Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lellouch, Emmanuel; Moreno, Raphael] Observ Paris, LESIA, Meudon, France. RP Moullet, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM amoullet@cfa.harvard.edu NR 55 TC 7 Z9 7 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAY PY 2011 VL 213 IS 1 BP 382 EP 392 DI 10.1016/j.icarus.2011.02.012 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 758TR UT WOS:000290190100023 ER PT J AU Dayrat, B Conrad, M Balayan, S White, TR Albrecht, C Golding, R Gomes, SR Harasewych, MG Martins, AMD AF Dayrat, Benoit Conrad, Michele Balayan, Shaina White, Tracy R. Albrecht, Christian Golding, Rosemary Gomes, Suzete R. Harasewych, M. G. de Frias Martins, Antonio Manuel TI Phylogenetic relationships and evolution of pulmonate gastropods (Mollusca): New insights from increased taxon sampling SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Ellobiidae; Euthyneura; Macro-evolutionary transitions; Onchidiidae; Veronicellidae ID RIBOSOMAL-RNA SEQUENCES; EUTHYNEURAN GASTROPODS; MAXIMUM-LIKELIHOOD; MULTIPLE ALIGNMENTS; MOLECULAR PHYLOGENY; DNA-SEQUENCES; MIXED MODELS; SYSTEMATICS; HETEROBRANCHIA; BASOMMATOPHORA AB Phylogenetic relationships among higher clades of pulmonate gastropods are reconstructed based on a data set including one nuclear marker (complete ribosomal 18S) and two mitochondrial markers (partial ribosomal 16S and Cytochrome oxidase I) for a total of 96 species. Sequences for 66 of these species are new to science, with a special emphasis on sampling the Ellobiidae, Onchidiidae, and Veronicellidae. Important results include the monophyly of Systellommatophora (Onchidiidae and Veronicellidae) as well as the monophyly of Ellobiidae (including Trimusculus, Otina, and Smeagol). Relationships within Ellobiidae, Onchidiidae, and Veronicellidae are evaluated here for the first time using molecular data. Present results are compared with those from the recent literature, and the current knowledge of phylogenetic relationships among pulmonate gastropods is reviewed: despite many efforts, deep nodes are still uncertain. Identification uncertainties about early fossils of pulmonates are reviewed. Impacts of those phylogenetic and fossil record uncertainties on our understanding of the macro-evolutionary history of pulmonates, especially transitions between aquatic and terrestrial habitats, are discussed. (C) 2011 Elsevier Inc. All rights reserved. C1 [Dayrat, Benoit; Conrad, Michele; Balayan, Shaina; White, Tracy R.] Univ Calif, Sch Nat Sci, Merced, CA 95343 USA. [Albrecht, Christian] Univ Giessen, Dept Anim Ecol & Systemat, D-35392 Giessen, Germany. [Golding, Rosemary] Australian Museum, Sydney, NSW 2010, Australia. [Gomes, Suzete R.] Inst Butantan, Lab Parasitol Malacol, BR-05503900 Sao Paulo, Brazil. [Harasewych, M. G.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [de Frias Martins, Antonio Manuel] Univ Azores, Ctr Biodivers & Genet Resources, CIBIO Acores, P-9501801 Sao Miguel, Azores, Portugal. RP Dayrat, B (reprint author), Univ Calif, Sch Nat Sci, 5200 N Lake Rd, Merced, CA 95343 USA. EM bdayrat@ucmerced.edu RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016; Martins, Antonio/L-7932-2013 OI Martins, Antonio/0000-0001-5358-8424 FU US National Science Foundation [DEB-0933276] FX All laboratory work for the present study was performed using funds from a US National Science Foundation Grant (DEB-0933276, to B. Dayrat). We are very grateful to our colleagues who collected some material and all collection managers and curators who let us borrow some material. Two anonymous reviewers and Associate Editor Neil Blackstone provided constructive comments that helped improve the manuscript. NR 83 TC 61 Z9 64 U1 3 U2 39 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAY PY 2011 VL 59 IS 2 BP 425 EP 437 DI 10.1016/j.ympev.2011.02.014 PG 13 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 760XU UT WOS:000290358800017 PM 21352933 ER PT J AU Kuntner, M Agnarsson, I AF Kuntner, Matjaz Agnarsson, Ingi TI Biogeography and diversification of hermit spiders on Indian Ocean islands (Nephilidae: Nephilengys) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Madagascar; Mascarenes; Comoros; Cenozoic dispersal; Vicariance; Phylogeography; Nephila ID DAY GECKOS PHELSUMA; HISTORICAL BIOGEOGRAPHY; TRANSOCEANIC DISPERSAL; FRESH-WATER; MADAGASCAR; ARANEAE; COLONIZATION; PHYLOGENY; DNA; THERIDIIDAE AB The origin of the terrestrial biota of Madagascar and, especially, the smaller island chains of the western Indian Ocean is relatively poorly understood. Madagascar represents a mixture of Gondwanan vicariant lineages and more recent colonizers arriving via Cenozoic dispersal, mostly from Africa. Dispersal must explain the biota of the smaller islands such as the Comoros and the chain of Mascarene islands, but relatively few studies have pinpointed the source of colonizers, which may include mainland Africa, Asia, Australasia, and Madagascar. The pantropical hermit spiders (genus Nephilengys) seem to have colonized the Indian Ocean island arc stretching from Comoros through Madagascar and onto Mascarenes, and thus offer one opportunity to reveal biogeographical patterns in the Indian Ocean. We test alternative hypotheses on the colonization route of Nephilengys spiders in the Indian Ocean and simultaneously test the current taxonomical hypothesis using genetic and morphological data. We used mitochondrial (COI) and nuclear (ITS2) markers to examine Nephilengys phylogenetic structure with samples from Africa, southeast Asia, and the Indian Ocean islands of Madagascar, Mayotte, Reunion and Mauritius. We used Bayesian and parsimony methods to reconstruct phylogenies and haplotype networks, and calculated genetic distances and fixation indices. Our results suggest an African origin of Madagascar Nephilengys via Cenozoic dispersal, and subsequent colonization of the Mascarene islands from Madagascar. We find strong evidence of gene flow across Madagascar and through the neighboring islands north of it, while phylogenetic trees, haplotype networks, and fixation indices all reveal genetically isolated and divergent lineages on Mauritius and Reunion, consistent with female color morphs. These results, and the discovery of the first males from Reunion and Mauritius, in turn falsify the existing taxonomic hypothesis of a single widespread species, Nephilengys borbonica, throughout the archipelago. Instead, we diagnose three Nephilengys species: Nephilengys livida (Vinson, 1863) from Madagascar and Comoros, N. borbonica (Vinson, 1863) from Reunion, and Nephilengys dodo new species from Mauritius. Nephilengys followed a colonization route to Madagascar from Africa, and on through to the Mascarenes, where it speciated on isolated islands. The related golden orb-weaving spiders, genus Nephila, have followed the same colonization route, but Nephila shows shallower divergencies, implying recent colonization, or a moderate level of gene flow across the archipelago preventing speciation. Unlike their synanthropic congeners, N. borbonica and N. dodo are confined to pristine island forests and their discovery calls for evaluation of their conservation status. (C) 2011 Elsevier Inc. All rights reserved. C1 [Kuntner, Matjaz; Agnarsson, Ingi] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, SI-1001 Ljubljana, Slovenia. [Kuntner, Matjaz; Agnarsson, Ingi] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Agnarsson, Ingi] UPR RP, Dept Biol, San Juan, PR 00931 USA. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM kuntner@gmail.com FU Slovenian Research Agency [Z1-9799-0618-07]; National Science Foundation [DEB-0516038]; European Community [MIRG-CT-2005 036536]; National Geographic Society [8655-09] FX This is contribution number 6 resulting from the 2008 Indian Ocean expedition, funded by the Slovenian Research Agency (Grant Z1-9799-0618-07 to I. Agnarsson) and the National Science Foundation (Grant DEB-0516038 to T. Blackledge). Additional funding came from the European Community 6th Framework Programme (a Marie Curie International Reintegration Grant MIRG-CT-2005 036536 to M. Kuntner), and the National Geographic Society (Grant 8655-09 to the authors). We thank Tjasa Lokovsek, Yadira Ortiz-Ruiz, Jason Rauscher, Peter Trontelj and Miguel Arnedo for lab help or advice, Heine C. Kiesbuy and Dennis Hansen for field assistance, and Dominique Strasberg, Sonia Ribes-Beaudemoulin, Benoit Lequettefor, and MICET for logistical help. We specially thank Christine Griffith for collecting the unknown N. dodo males. Mike Rix and an anonymous reviewer provided valuable feedback. NR 65 TC 27 Z9 27 U1 2 U2 22 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAY PY 2011 VL 59 IS 2 BP 477 EP 488 DI 10.1016/j.ympev.2011.02.002 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 760XU UT WOS:000290358800022 PM 21316478 ER PT J AU McMahon, SM Harrison, SP Armbruster, WS Bartlein, PJ Beale, CM Edwards, ME Kattge, J Midgley, G Morin, X Prentice, IC AF McMahon, Sean M. Harrison, Sandy P. Armbruster, W. Scott Bartlein, Patrick J. Beale, Colin M. Edwards, Mary E. Kattge, Jens Midgley, Guy Morin, Xavier Prentice, I. Colin TI Improving assessment and modelling of climate change impacts on global terrestrial biodiversity SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID MILLENNIAL-SCALE VARIABILITY; PLANT FUNCTIONAL TYPES; LAST GLACIAL MAXIMUM; SPECIES RANGE SHIFTS; VEGETATION DYNAMICS; ECOSYSTEM FUNCTION; FIRE REGIMES; FUTURE; DISTRIBUTIONS; NICHE AB Understanding how species and ecosystems respond to climate change has become a major focus of ecology and conservation biology. Modelling approaches provide important tools for making future projections, but current models of the climate-biosphere interface remain overly simplistic, undermining the credibility of projections. We identify five ways in which substantial advances could be made in the next few years: (i) improving the accessibility and efficiency of biodiversity monitoring data, Oil quantifying the main determinants of the sensitivity of species to climate change, (Hi) incorporating community dynamics into projections of biodiversity responses, (iv) accounting for the influence of evolutionary processes on the response of species to climate change, and (v) improving the biophysical rule sets that define functional groupings of species in global models. C1 [McMahon, Sean M.] Smithsonian Environm Res Ctr, Smithsonian Inst Global Earth Observ, Edgewater, MD 21307 USA. [Harrison, Sandy P.; Prentice, I. Colin] Macquarie Univ, Sch Biol Sci, N Ryde, NSW 2109, Australia. [Armbruster, W. Scott] Univ Portsmouth, Sch Biol Sci, Portsmouth PO1 2DY, Hants, England. [Bartlein, Patrick J.] Univ Oregon, Dept Geog, Eugene, OR 97403 USA. [Beale, Colin M.] Univ York, Dept Biol, York YO10 5DD, N Yorkshire, England. [Edwards, Mary E.] Univ Southampton, Sch Geog, Southampton SO17 1BJ, Hants, England. [Kattge, Jens] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Midgley, Guy] S African Natl Biodivers Inst, ZA-0001 Pretoria, South Africa. [Morin, Xavier] CNRS, Ctr Ecol Fonct & Evolut, F-34293 Montpellier 5, France. [Morin, Xavier] ETH, Forest Ecol Grp, Inst Terr Ecosyst, Dept Environm Sci, CH-8092 Zurich, Switzerland. [Prentice, I. Colin] Univ London Imperial Coll Sci Technol & Med, Grantham Inst, Ascot SL5 7PY, Berks, England. [Morin, Xavier] Univ London Imperial Coll Sci Technol & Med, Div Biol, Ascot SL5 7PY, Berks, England. [Armbruster, W. Scott] Univ Alaska, Inst Arctic Biol, Fairbanks, AK 99775 USA. [Armbruster, W. Scott] NTNU, Dept Biol, N-7491 Trondheim, Norway. RP McMahon, SM (reprint author), Smithsonian Environm Res Ctr, Smithsonian Inst Global Earth Observ, Edgewater, MD 21307 USA. EM mcmahons@si.edu RI Bartlein, Patrick/E-4643-2011; Armbruster, William/B-4799-2013; Morin, Xavier/B-2790-2015; Midgley, Guy/H-3585-2014; Kattge, Jens/J-8283-2016; OI Bartlein, Patrick/0000-0001-7657-5685; Midgley, Guy/0000-0001-8264-0869; Kattge, Jens/0000-0002-1022-8469; Harrison, Sandy/0000-0001-5687-1903 FU QUEST; UK Natural Environment Research Council (NERC); Grantham Institute for Climate Change at Imperial College London; Royal Botanic Gardens, Kew; HSBC Bank Climate Partnership FX This paper was conceived at a workshop on Biodiversity and Climate Change held at the Royal Botanic Gardens, Kew and sponsored by QUEST (http://quest.bris.ac.uk/), a flagship programme of the UK Natural Environment Research Council (NERC), the Grantham Institute for Climate Change at Imperial College London, and the Royal Botanic Gardens, Kew. We thank the workshop organizers for providing a workshop structure that allowed us to focus on gaps and practical solutions, and the other participants for stimulating discussions. This manuscript has benefited from comments by Georgina Mace. Partial funding for SMM came from HSBC Bank Climate Partnership. NR 91 TC 120 Z9 124 U1 28 U2 183 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD MAY PY 2011 VL 26 IS 5 BP 249 EP 259 DI 10.1016/j.tree.2011.02.012 PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 761BW UT WOS:000290370800008 PM 21474198 ER PT J AU Strong, EE Colgan, DJ Healy, JM Lydeard, C Ponder, WF Glaubrecht, M AF Strong, Ellen E. Colgan, Donald J. Healy, John M. Lydeard, Charles Ponder, Winston F. Glaubrecht, Matthias TI Phylogeny of the gastropod superfamily Cerithioidea using morphology and molecules SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE anatomy; freshwater; Mollusca; simultaneous analysis ID MULTIPLE SEQUENCE ALIGNMENT; MALILI LAKE SYSTEM; PYRAZUS-EBENINUS MOLLUSCA; VIVIPARUS-VIVIPARUS L; PARTIAL 28S RDNA; FRESH-WATER; EAST-AFRICA; THALASSOID GASTROPODS; CAMPANILE-SYMBOLICUM; ADAPTIVE RADIATION AB The Cerithioidea is an ecologically important superfamily of basal Caenogastropoda with speciose marine, brackish water, and freshwater lineages primarily in tropical, subtropical, and warm temperate regions of the world. They often represent significant components of the communities where they occur and have given rise to several spectacular endemic radiations in rivers and ancient lakes. Earlier attempts to resolve the phylogenetic history of the group have been based on smaller taxon and character subsets with incongruent results. Here the monophyly and phylogeny of the group is evaluated with expanded morphological and molecular (16S, 28S rRNA) data sets. For morphological analyses, 151 characters (shell, operculum, radula, alimentary tract, kidney, nervous system, reproductive anatomy, and sperm ultrastructure) were scored for 47 cerithioideans (representing 17 families) and nine outgroup taxa. To test monophyly of the Cerithioidea, extended molecular data sets of 16S and 28S sequences for 57 and 44 taxa, respectively, were compiled using new and previously published sources. For combined analyses, a pruned molecular data set was combined with the morphological partition. The morphological data were analysed alone using only parsimony; molecular and simultaneous analyses were performed using both parsimony and Bayesian inference. The effect of excluding unconserved regions of the alignments was also explored. All analyses, with the exception of the individual 16S and 28S data sets, support monophyly of the Cerithioidea as currently formulated. Of the 12 families represented by more than one terminal, only two (Planaxidae, Potamididae) are always supported as monophyletic; Batillariidae, Cerithiidae, Pachychilidae, Pleuroceridae, Semisulcospiridae, Thiaridae, and Turritellidae are monophyletic in most but not all topologies. The combination of diverse data sources (morphology, 16S and 28S sequences) and inclusion of unconserved regions of the alignments improved the recovery of monophyletic families. At deeper levels, a consensus is beginning to emerge in the recognition of three main assemblages, but whether these represent clades or grades is still unclear; the resolution of these assemblages and the branching order within them are sensitive to exclusion of unconserved regions and choice of optimality criterion. No clear conclusion is reached with respect to the number of freshwater invasions, with two invasions supported on some topologies and three supported on others. Progress toward a robust and stable resolution of cerithioidean relationships will require (1) strategically coordinated sampling for additional morphological and molecular data; (2) comprehensive anatomical treatments for several poorly documented limnic lineages (e. g. Melanopsidae, Thiaridae) and comparative data for poorly understood organ systems (e. g. renal system); (3) the addition of poorly known, minute, and/or rare marine taxa, to provide novel character combinations, insight into putative homologies, and to help anchor basal nodes and break up long branches. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 162, 43-89. doi: 10.1111/j.1096-3642.2010.00670.x C1 [Strong, Ellen E.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Colgan, Donald J.] Australian Museum, Evolutionary Biol Unit, Sydney, NSW 2010, Australia. [Healy, John M.] Queensland Museum, Biodivers Program, S Bank, Qld 4101, Australia. [Lydeard, Charles] American Univ, Dept Biol, Washington, DC 20016 USA. [Glaubrecht, Matthias] Humboldt Univ, Museum Naturkunde, Leibniz Inst Res Evolut & Biodivers, D-10115 Berlin, Germany. RP Strong, EE (reprint author), Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 163, Washington, DC 20013 USA. EM stronge@si.edu RI Colgan, Donald/A-3779-2008; OI Colgan, Donald/0000-0002-4731-9700; Strong, Ellen/0000-0001-7181-4114 FU Australian Museum Sydney [GL 297/2-1]; Deutsche Forschungsgemeinschaft [2-2]; Australian Research Council; Queensland Museum; University of Queensland; University of Sydney; U.S. National Science Foundation; Deutscher Akademischer Austausch Dienst FX This study is the result of a long-term collaborative effort initiated by W. F. P. with a visiting fellowship to M. G. Financial support to M. G. by the Australian Museum Sydney (Visiting Research Fellowships in 1996, 1998) and through grants GL 297/2-1 and 2-2 by the Deutsche Forschungsgemeinschaft, is gratefully acknowledged. J. M. H. thanks the Australian Research Council, Queensland Museum, University of Queensland, and University of Sydney for financially supporting his work through fellowships (1986-2002) and the Queensland Museum and Field Museum of Natural History (R. Bieler) for institutional support. Aspects of this project were supported in part through grants from the U.S. National Science Foundation to C. L. and W. F. P., and from the Deutscher Akademischer Austausch Dienst to E. E. S. Special thanks to F. Kohler (Australian Museum Sydney) for the 28S sequence of Hua jacqueti. We are grateful to Daniel Graf (University of Alabama, Tuscaloosa) and two anonymous reviewers, whose comments greatly enhanced the quality of the manuscript. NR 258 TC 27 Z9 31 U1 3 U2 29 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 MAY PY 2011 VL 162 IS 1 BP 43 EP 89 DI 10.1111/j.1096-3642.2010.00670.x PG 47 WC Zoology SC Zoology GA 758KZ UT WOS:000290164900003 ER PT J AU Sidlauskas, BL Mol, JH Vari, RP AF Sidlauskas, Brian L. Mol, Jan H. Vari, Richard P. TI Dealing with allometry in linear and geometric morphometrics: a taxonomic case study in the Leporinus cylindriformis group (Characiformes: Anostomidae) with description of a new species from Suriname SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Amazon; morphology; regression; relative warps; South America; taxonomy ID GENUS PYGOCENTRUS TELEOSTEI; RIO ORINOCO SYSTEM; SHAPE; FISH; OSTARIOPHYSI; GROWTH; WATER; RIVER; REDESCRIPTION; REVOLUTION AB To achieve maximum efficacy, taxonomic studies that seek to distinguish amongst species must first account for allometric shape variation within species. Two recently developed software packages (SMATR and MorphoJ) offer regression-based allometric approaches that are notable for their statistical power and ease of use and that may prove highly useful to taxonomists working with linear or geometric morphometric data. We investigate species delimitation of the slender-bodied fishes in the Leporinus cylindriformis group using these programs and demonstrate the utility of the allometric corrections that they provide. Without allometric correction, many pairs of species are difficult to distinguish on the basis of morphometrics, but once regressions are used to account for marked allometric variation within species, most of the recognized species in this group can be readily distinguished with linear or geometric morphometrics, particularly using variation in the depth of the body. Both approaches returned congruent patterns of separation amongst putative species, but the geometric approach in MorphoJ distinguished amongst four more pairs of species than did the linear approach in SMATR and appears to provide slightly more statistical power. Based on distinctive morphometrics, meristics, and coloration, a highly elongate species of Leporinus from the Suriname, Corantijn, and Coppename rivers of Suriname is described herein as a new species, Leporinus apollo sp. nov. The unique L. cylindriformis holotype from Porto de Moz, Brazil differs in morphology, meristics, and pigmentation from specimens commonly referred to that species from the main basin of the Amazon; the latter specimens may represent an additional undescribed species. The L. cylindriformis holotype itself may represent a rare species or a specimen collected at the edge of its native range. Measurements of the holotype and paratype of Leporinus niceforoi, which were collected in the Amazonian slope of Colombia, differ substantially from similarly pigmented and putatively conspecific specimens from Amazonian portions of Ecuador and Peru. Recently collected specimens from Colombia are needed to determine whether the observed morphometric variation encompassed by the current concept of L. niceforoi indicates a morphocline within a single species, suggests the presence of multiple cryptic species, or results from shrinkage of the types. In all these cases, linear or geometric morphometric data can reliably differentiate amongst species, but only after one accounts for allometric shape variation. The new SMATR and MorphoJ software packages both offer easy and effective approaches to such allometrically informed taxonomy, and may prove useful to any systematist working on taxa that change shape as they grow. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 162, 103-130. doi: 10.1111/j.1096-3642.2010.00677.x C1 [Sidlauskas, Brian L.] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Sidlauskas, Brian L.] Natl Evolutionary Synth Ctr, Durham, NC 27705 USA. [Sidlauskas, Brian L.; Vari, Richard P.] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20013 USA. [Mol, Jan H.] Anton Kom Univ Suriname, Dept Biol, Leysweg, Paramaribo, Surinam. [Mol, Jan H.] Anton Kom Univ Suriname, Ctr Agr Res Suriname, Leysweg, Paramaribo, Surinam. RP Sidlauskas, BL (reprint author), Oregon State Univ, Dept Fisheries & Wildlife, 104 Nash Hall, Corvallis, OR 97331 USA. EM brian.sidlauskas@oregonstate.edu OI Sidlauskas, Brian/0000-0003-0597-4085 FU National Evolutionary Synthesis Center [NSF EF-0423641] FX We thank Mary Anne Rogers and Philip Willink (FMNH) and Sonia Fisch-Muller and Raphael Covain (MHNG) for the loan of the material designated herein as the majority of the type series of L. apollo. Without their assistance, this study would have been impossible. We also thank Karsten Hartel, Mark Sabaj Perez, Mary Anne Rogers, Philip Willink, Rob Robins, Larry Page, Lucia Rapp Py-Daniel, Geraldo Santos, Cristiano Moreira, and Julio Cesar Garavello for making various lots of comparative material available for study. Barry Chernoff introduced us to most of the methods employed herein, and Chris Klingenberg provided invaluable advice on implementing morphometric analyses in his MorphoJ program. Megan McPhee commented on an early version of this analysis and Sam Price and Kevin Middleton pointed us to the exceedingly helpful SMATR package. Sandra Raredon and T. Britt Griswold assisted with photography and radiographs. The map is based on a baseline map by Marilyn Weitzman. The lead author was supported during a portion of this work by a postdoctoral fellowship from the National Evolutionary Synthesis Center (NSF EF-0423641). NR 74 TC 22 Z9 25 U1 4 U2 35 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 MAY PY 2011 VL 162 IS 1 BP 103 EP 130 DI 10.1111/j.1096-3642.2010.00677.x PG 28 WC Zoology SC Zoology GA 758KZ UT WOS:000290164900005 ER PT J AU Hirsch, BT Morrell, LJ AF Hirsch, Ben T. Morrell, Lesley J. TI Measuring marginal predation in animal groups SO BEHAVIORAL ECOLOGY LA English DT Article ID BROWN CAPUCHIN MONKEYS; GROUP SPATIAL POSITION; SELFISH HERD; CEBUS-APELLA; FORAGING GROUPS; FEEDING COMPETITION; VIGILANCE BEHAVIOR; HUNTING SUCCESS; GROUP-SIZE; RISK AB Predation is a major pressure that shapes animal sociality, but predation risk is not homogenous within groups. Animals located on the group edge typically face an increased threat of predation, although different patterns have been reported. We created a simulation model to determine how changes in predator attack distance and prey density influence predation in relation to within-group spatial position. At large attack distances, peripheral animals were attacked far more than central animals. At relatively short attack distances, central individuals were attacked almost as often as peripheral animals. We used 6 different methods to classify within-group spatial position in our simulations and tested which methods were the best predictors of predation risk at different parameter values. The minimum convex polygon and angle of vulnerability methods were the best predictors of predation risk at large and medium attack distances, respectively. At relatively short attack distances, the nearest neighbor distance and neighbor density methods were the best predictors of predation risk. These patterns demonstrate that the threat of marginal predation is dependent on the behavior of predators and that for some predator-prey systems, marginal predation is predicted to be insignificant. We predict that social prey animals should change antipredatory behavior, such as vigilance, within-group spacing, and within-group spatial choice based on the relative distances at which their predators attack. These results demonstrate the importance of incorporating the behavior of predators in empirical studies and predator-prey models. Key words: attack distance, marginal predation, predation, predator behavior, vigilance, within-group spatial position. [Behav Ecol 22: 648-656 (2011)] C1 [Hirsch, Ben T.] Smithsonian Trop Res Inst, Dpo Aa 340029898, Panama. [Hirsch, Ben T.] New York State Museum & Sci Serv, Albany, NY 12230 USA. [Hirsch, Ben T.] Univ Leeds, Inst Integrat & Comparat Biol, Leeds LS2 9JT, W Yorkshire, England. [Morrell, Lesley J.] Univ Hull, Dept Biol Sci, Kingston Upon Hull HU6 7RX, N Humberside, England. RP Hirsch, BT (reprint author), Smithsonian Trop Res Inst, Unit 9100 Box 0948, Dpo Aa 340029898, Panama. EM hirschb@si.edu RI Morrell, Lesley/A-4311-2008 OI Morrell, Lesley/0000-0003-0256-7871 FU Natural Environment Research Council [NE/D008921/1]; National Geographic/Waitt; National Science Foundation [DEB 0717071] FX Natural Environment Research Council Postdoctoral Fellowship (NE/D008921/1) to L.J.M.; a National Geographic/Waitt grant to B. T. H.; and a National Science Foundation grant (DEB 0717071). NR 73 TC 16 Z9 16 U1 2 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 MAY-JUN PY 2011 VL 22 IS 3 BP 648 EP 656 DI 10.1093/beheco/arr026 PG 9 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 754FH UT WOS:000289839600029 ER PT J AU Dapper, AL Baugh, AT Ryan, MJ AF Dapper, Amy L. Baugh, Alexander T. Ryan, Michael J. TI The Sounds of Silence as an Alarm Cue in Tungara Frogs, Physalaemus pustulosus SO BIOTROPICA LA English DT Article DE anuran; chorus; communication; Panama; predation; public information; sexual selection ID BAT PREDATION; LOCALIZATION PERFORMANCE; FIELD CRICKETS; MATE CHOICE; CALLS; ADVERTISEMENT; PARASITOIDS; COMPLEXITY; SIGNALS; INFORMATION AB In many species males vocally advertise for mates in choruses and these choruses serve as acoustic beacons to conspecific females as well as to eavesdropping predators and parasites. Chorusing will often cease in response to disturbances, such as the presence of predators. In some cases the cessation is so rapid and over such a large area that it seems improbable that males are all responding directly to the same local disturbance. Here, we demonstrate experimentally in Neotropical tungara frogs, Physalaemus pustulosus, that the cessation of calling by males spreads rapidly through the chorus. The cessation of chorusing in response to the cessation of playbacks of three calling males is more effective in inducing chorus cessation than is the cessation of one male calling. When three males are calling, the cessation of complex calls is more effective in inducing chorus cessation than simple calls. There is no main effect on whether the final call of the male is complete or is interrupted. We thus conclude that the sudden lack of signals-the 'sounds of silence'-becomes an alarm cue that can explain the rapid cessation of choruses that are common in many chorusing species. C1 [Baugh, Alexander T.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Dapper, Amy L.] Coll William & Mary, Dept Biol, Williamsburg, VA 23187 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Ryan, MJ (reprint author), Univ Texas Austin, Sect Integrat Biol, 1 Univ Stn C0930, Austin, TX 78712 USA. EM mryan@mail.utexas.edu RI Baugh, Alexander/E-4777-2010; OI Baugh, Alexander/0000-0003-2032-892X FU National Science Foundation [IBN 0078150] FX We thank the Smithsonian Tropical Research Institute for logistical support, and the government of Panama for permits to conduct these studies. This research was funded by a grant from the National Science Foundation (IBN 0078150). This research was approved by the University of Texas IACUC. MJR is indebted to P. Simon and A. Garfunkel for first making clear the potency of silence, and to M. D. Tuttle for early discussions of this hypothesis and its testing. NR 39 TC 9 Z9 9 U1 2 U2 23 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2011 VL 43 IS 3 BP 380 EP 385 DI 10.1111/j.1744-7429.2010.00707.x PG 6 WC Ecology SC Environmental Sciences & Ecology GA 755BQ UT WOS:000289902000015 ER PT J AU Levitan, DR Fogarty, ND Jara, J Lotterhos, KE Knowlton, N AF Levitan, Don R. Fogarty, Nicole D. Jara, Javier Lotterhos, Katie E. Knowlton, Nancy TI GENETIC, SPATIAL, AND TEMPORAL COMPONENTS OF PRECISE SPAWNING SYNCHRONY IN REEF BUILDING CORALS OF THE MONTASTRAEA ANNULARIS SPECIES COMPLEX SO EVOLUTION LA English DT Article DE Hybridization; reproductive isolation; reproductive success; spawning behavior; speciation ID REPRODUCTIVE ISOLATION; CARIBBEAN CORAL; SCLERACTINIAN CORALS; POPULATION-STRUCTURE; FAVEOLATA ELLIS; FERTILE PERIOD; PATTERNS; FERTILIZATION; ECOLOGY; GAMETOGENESIS AB When organisms release gametes into the sea, synchrony must be precise to increase fertilization and decrease hybridization. We tagged and genotyped over 400 spawning corals from the three species in the Montastraea annularis species complex. We report on the influence of species, individuals, and genotypes on timing of spawning from 2002 through 2009. During their annual spawning event M. franksi spawns on average 2 h after sunset, whereas M. annularis and M. faveolata spawn 3.5 h after sunset. Only M. franksi and M. annularis have compatible gametes. Individual colonies of the same genotype spawn at approximately the same time after sunset within and across years (within minutes), but different genotypes have significantly different spawning times. Neighboring colonies, regardless of genotype, spawn more synchronously than individuals spaced further apart. At a given distance, clone-mates spawn more synchronously than nonclone-mates. A transplant experiment indicates a genetic and environmental influence on spawn time. There is strong, but not absolute, concordance between spawn time, morphology, and genetics. Tight precision in spawning is achieved via a combination of external cues, genetic precision, and perhaps conspecific signaling. These mechanisms are likely to influence reproductive success and reproductive isolation in a density-dependent manner. C1 [Levitan, Don R.; Fogarty, Nicole D.; Lotterhos, Katie E.] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. [Jara, Javier] Smithsonian Trop Res Inst, Balboa, Panama. [Knowlton, Nancy] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. RP Levitan, DR (reprint author), Florida State Univ, Dept Biol Sci, B-157, Tallahassee, FL 32306 USA. EM levitan@bio.fsu.edu FU NSF; National Museum of Natural History of the Smithsonian Institution FX We thank M. Adreani, B. Biggs, D. Ferrell, J. Grayson, D. Kline, P. Munguia, K. Pawluk, A. Strimaitis, and C. terHorst for field assistance during the spawning events and M. Lowenberg, and K. Reuter for laboratory assistance with genotyping corals. We also thank the staff at the Smithsonian Tropical Research Station in Bocas del Toro. This work was supported by an NSF grant to DRL and NK and by the National Museum of Natural History of the Smithsonian Institution. Research permits were generously supplied by the country of Panama. NR 62 TC 23 Z9 24 U1 0 U2 22 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0014-3820 J9 EVOLUTION JI Evolution PD MAY PY 2011 VL 65 IS 5 BP 1254 EP 1270 DI 10.1111/j.1558-5646.2011.01235.x PG 17 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 754YE UT WOS:000289893000004 PM 21521188 ER PT J AU Merrill, RM Gompert, Z Dembeck, LM Kronforst, MR McMillan, WO Jiggins, CD AF Merrill, Richard M. Gompert, Zachariah Dembeck, Lauren M. Kronforst, Marcus R. McMillan, W. Owen Jiggins, Chris D. TI MATE PREFERENCE ACROSS THE SPECIATION CONTINUUM IN A CLADE OF MIMETIC BUTTERFLIES SO EVOLUTION LA English DT Article DE Assortative mating; Heliconius; mate choice; reproductive isolation; speciation ID HYBRIDIZING HELICONIUS BUTTERFLIES; ECOLOGICAL SPECIATION; REPRODUCTIVE ISOLATION; MULLERIAN MIMICRY; SEXUAL ISOLATION; EVOLUTION; PATTERNS; STICKLEBACKS; LEPIDOPTERA; DROSOPHILA AB Premating behavioral isolation is increasingly recognized as an important part of ecological speciation, where divergent natural selection causes the evolution of reproductive barriers. A number of studies have now demonstrated that traits under divergent natural selection also affect mate preferences. However, studies of single species pairs only capture a snapshot of the speciation process, making it difficult to assess the role of mate preferences throughout the entire process. Heliconius butterflies are well known for their brightly colored mimetic warning patterns, and previous studies have shown that these patterns are also used as mate recognition cues. Here, we present mate preference data for four pairs of sister taxa, representing different stages of divergence, which together allow us to compare diverging mate preferences across the continuum of Heliconius speciation. Using a novel Bayesian approach, our results support a model of ecological speciation in which strong premating isolation arises early, but continues to increase throughout the continuum from polymorphic populations through to "good," sympatric ecologically divergent species. C1 [Merrill, Richard M.; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Gompert, Zachariah] Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. [Gompert, Zachariah] Univ Wyoming, Program Ecol, Laramie, WY 82071 USA. [Dembeck, Lauren M.; McMillan, W. Owen] N Carolina State Univ, WM Keck Ctr Behav Biol, Raleigh, NC 27695 USA. [Dembeck, Lauren M.; McMillan, W. Owen] N Carolina State Univ, Dept Genet, Raleigh, NC 27695 USA. [Kronforst, Marcus R.] Harvard Univ, FAS Ctr Syst Biol, Northwest Labs, Cambridge, MA 02138 USA. [McMillan, W. Owen] Smithsonian Trop Res Inst, Miami, FL 34002 USA. RP Merrill, RM (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. EM r.merrill@zoo.cam.ac.uk RI Jiggins, Chris/B-9960-2008; OI Jiggins, Chris/0000-0002-7809-062X; Gompert, Zachariah/0000-0003-2248-2488 FU Smithsonian Tropical Research Institute; BBSRC [011845]; Leverhulme Trust; NIH [GM008443]; NIH NIGMS [P50GM068763]; National Science Foundation [DEB-0844244, DEB-0715096]; Royal Society URF FX We thank the Smithsonian Tropical Research Institute for support and the Ministerio del Ambiente in Panama, the Ministero de Agricultura Insituto National de Recursos Naturale of Peru, the Ministerio del Ambiente y Energia of Costa Rica, and the Ministerio del Ambiente and the Museo Ecuatoriano de Ciencias Naturales of Ecuador for permission to collect butterflies. We are grateful to J. Dessmann and J. Velez for help raising larvae and conducting experiments, and to M. Abanto for help in the insectaries. We are grateful to two anonymous referees whose comments greatly improved the manuscript. RMM was funded by a BBSRC studentship and the project was also supported by grants from the BBSRC (011845) and Leverhulme Trust. LMD is supported by NIH Training Grant GM008443. MRK is supported by NIH NIGMS grant P50GM068763. WOM is support by grants from the National Science Foundation (DEB-0844244 and DEB-0715096). CDJ is funded by a Royal Society URF. NR 55 TC 44 Z9 45 U1 5 U2 55 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD MAY PY 2011 VL 65 IS 5 BP 1489 EP 1500 DI 10.1111/j.1558-5646.2010.01216.x PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 754YE UT WOS:000289893000022 PM 21521198 ER PT J AU Velez, MI Curtis, JH Brenner, M Escobar, J Leyden, BW de Hatch, MP AF Velez, Maria I. Curtis, Jason H. Brenner, Mark Escobar, Jaime Leyden, Barbara W. de Hatch, Marion Popenoe TI Environmental and Cultural Changes in Highland Guatemala Inferred from Lake Amatitlan Sediments SO GEOARCHAEOLOGY-AN INTERNATIONAL JOURNAL LA English DT Article ID ORGANIC-MATTER; MAYA LOWLANDS; TROPICAL LAKE; CALDERA LAKE; CLIMATE; ARCHAEOLOGY; COLLAPSE; DROUGHT; HISTORY; MEXICO AB We inferred the late Holocene environmental history of the Guatemala highlands from multiple lines of evidence in a sediment core from Lake Amatitlan. Inferred environmental changes are generally synchronous with archaeologically documented highland Maya cultural shifts. Population increases in the Middle Preclassic, Early Classic, and Late Postclassic are associated with deforestation and soil erosion. Land abandonment in the Late Preclassic, Late Classic, and Early Postclassic is associated with evidence for reforestation and soil stabilization. Diatoms indicate relatively lower lake level and greater trophic status at times of reduced human impact, from ca. 250 B. C. to A. D. 125 and from ca. A. D. 875 to 1375. Decreased water levels were probably due to drier climate, to reforestation, or both. Lake eutrophication was caused by reduced water volume combined with a legacy of long-term agricultural activity. Our data contribute to the understanding of relations among ancient Maya culture, climate, and environment. (C) 2011 Wiley Periodicals, Inc. C1 [Velez, Maria I.] Univ Regina, Dept Geol, Regina, SK S4S 0A2, Canada. [Curtis, Jason H.; Brenner, Mark; Escobar, Jaime] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. [Curtis, Jason H.; Brenner, Mark; Escobar, Jaime] Univ Florida, Land Use & Environm Change Inst LUECI, Gainesville, FL 32611 USA. [Escobar, Jaime] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. [de Hatch, Marion Popenoe] Univ Valle Guatemala, Dept Arqueol, Guatemala City 01901, Guatemala. RP Velez, MI (reprint author), Univ Regina, Dept Geol, Regina, SK S4S 0A2, Canada. EM maria.velez@uregina.ca NR 45 TC 6 Z9 6 U1 2 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0883-6353 J9 GEOARCHAEOLOGY JI Geoarchaeology PD MAY-JUN PY 2011 VL 26 IS 3 BP 346 EP 364 DI 10.1002/gea.20352 PG 19 WC Archaeology; Geosciences, Multidisciplinary SC Archaeology; Geology GA 751YJ UT WOS:000289653500002 ER PT J AU Hultgren, KM Duffy, JE AF Hultgren, Kristin M. Duffy, J. Emmett TI MULTI-LOCUS PHYLOGENY OF SPONGE-DWELLING SNAPPING SHRIMP (CARIDEA: ALPHEIDAE: SYNALPHEUS) SUPPORTS MORPHOLOGY-BASED SPECIES CONCEPTS SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE Alpheidae; Caridea; phylogeny; snapping shrimp; Synalpheus gambarelloides ID BELIZE BARRIER-REEF; HOST-SPECIFICITY; DECAPODA; CRUSTACEA; EUSOCIALITY; SPECIATION; DIVERGENCE; RADIATIONS; LIKELIHOOD; ANCIENT AB Alpheid snapping shrimp are one of the most diverse groups of coral-reef fauna, and sponge-dwelling shrimp in the genus Synalpheus (gambarelloides species group) have in particular become a model system for studying the evolution of social biology and host use in marine invertebrates. Despite recent advances in understanding the evolution and systematics of Synalpheus, the taxonomy and phylogenetic relationships within this group remain challenging. More than 20 new species in the S. gambarelloides species group have been described over the past two decades, primarily within several cryptic species complexes, which has doubled the known diversity of this group in the West Atlantic. Here we construct a new phylogenetic tree describing relationships between 40 different species from the S. gambarelloides-group (119 individuals from across the Caribbean), using a combined dataset consisting of two mitochondrial loci (16S and COI), one nuclear protein-coding gene (elongation-factor 2), and 33 morphological characters. Putative conspecific specimens of Synalpheus from multiple locations across the Caribbean were always monophyletic (with one exception), providing strong support for the validity of species concepts based on morphology. Our study also provides further evidence for the monophyly of the S. gambarelloides-group in the Caribbean, resolves the molecular relationships within many recently described species complexes, and provides a new phylogenetic framework for future evolutionary studies of this group. C1 [Hultgren, Kristin M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Duffy, J. Emmett] Virginia Inst Marine Sci, Gloucester Pt, VA 23062 USA. RP Hultgren, KM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 163,POB 37012, Washington, DC 20013 USA. EM hultgrenk@si.edu; jeduffy@vims.edu RI Hultgren, Kristin/F-6862-2011 FU Marine Science Network; Smithsonian Institution's Caribbean Coral Reef Ecosystem (CCRE) FX Funding for this project was provided by a Marine Science Network postdoctoral fellowship from the Smithsonian (to KMH), and by funds from the Smithsonian Institution's Caribbean Coral Reef Ecosystem (CCRE) fund. Collection work at the Smithsonian's Carrie Bow Cay research station in Belize was greatly facilitated by Mike Carpenter and the staff at the Pelican Bay resort; we are also grateful to the staff at the Smithsonian Marine Station in Bocas del Toro, Panama for facilitating collection work there. Tripp Macdonald provided invaluable assistance collecting and identifying specimens in the field and laboratory. Finally, we would like to thank the staff at the Smithsonian's Laboratory of Analytical Biology (LAB) and Dr. Carla Hurt (University of Miami) for assistance with genetic work. NR 61 TC 11 Z9 13 U1 1 U2 10 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD MAY PY 2011 VL 31 IS 2 BP 352 EP 360 DI 10.1651/10-3382.1 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 755UI UT WOS:000289963500019 ER PT J AU Riley, S AF Riley, Sheila TI The Craigslist Murders: A Satire SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila] Smithsonian Inst Libs, Washington, DC USA. RP Riley, S (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 1 PY 2011 VL 136 IS 8 BP 72 EP 72 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 755IU UT WOS:000289923500046 ER PT J AU Long, M Romanova, MM Kulkarni, AK Donati, JF AF Long, M. Romanova, M. M. Kulkarni, A. K. Donati, J. -F. TI Global 3D simulations of disc accretion on to the classical T Tauri star BP Tauri SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; magnetic fields; MHD; stars: magnetic field ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; MAGNETIC NEUTRON-STARS; POWERED STELLAR WINDS; MAGNETOSPHERIC ACCRETION; DIFFERENTIAL ROTATION; PROPELLER REGIME; INCLINED DIPOLE; YOUNG STARS; AB DORADUS; MASS STARS AB We performed global three-dimensional magnetohydrodynamic simulations of accretion on to a star with magnetic field and other properties close to those observed in the classical T Tauri star BP Tau. We observed in the simulations that the disc is disrupted by the dipole component and matter flows towards the star in two funnel streams which form two accretion spots below the dipole magnetic poles. The octupolar component becomes dynamically important very close to the star and it redirects the matter flow to higher latitudes. The spots are meridionally elongated and are located at higher latitudes, compared with the pure dipole case. A series of simulation runs were performed at different accretion rates. We found that a 1.2 kG dipole field truncates the disc at a distance comparable to the corotation radius if the accretion rate is (1.4-2) x 10-9 M-circle dot yr-1, which is at the lower end of the observationally derived values. If the accretion rate is somewhat higher, 8.5 x 10-9 M-circle dot yr-1, then the disc is truncated at r approximate to 3.6R(star), which is a less favourable situation for the slowly rotating BP Tau. The magnetic torque acting on the star is also small; however, it is probably sufficient to support rotational equilibrium at the present state of slow rotation. Disc-magnetosphere interaction leads to inflation of the field lines and to the formation of magnetic towers above and below the disc. The magnetic field of BP Tau is close to potential inside the magnetospheric surface, where magnetic stress dominates over the matter stress. However, it strongly deviates from potential at larger distances from the star. C1 [Long, M.] Univ Illinois, Dept Phys, Ctr Theoret Astrophys, Urbana, IL 61801 USA. [Romanova, M. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Kulkarni, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Donati, J. -F.] CNRS, LATT UMR 5572, F-31400 Toulouse, France. [Donati, J. -F.] Univ Toulouse 3, F-31400 Toulouse, France. RP Long, M (reprint author), Univ Illinois, Dept Phys, Ctr Theoret Astrophys, 1110 W Green St, Urbana, IL 61801 USA. EM long@astro.cornell.edu; romanova@astro.cornell.edu FU NASA through NASA Advanced Supercomputing (NAS) Division at Ames Research Center; NASA Center for Computational Sciences (NCCS) at Goddard Space Flight Center; NSF [AST0709015, AST-0807129]; NASA [NNX08AH25G] FX Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center and the NASA Center for Computational Sciences (NCCS) at Goddard Space Flight Center. The authors thank A. V. Koldoba and G. V. Ustyugova for the earlier development of the codes and the referee S. Mohanty for insightful comments. The research was supported by NSF grant AST0709015. The research of MMR was supported by NASA grant NNX08AH25G and NSF grant AST-0807129. NR 54 TC 27 Z9 27 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 MAY PY 2011 VL 413 IS 2 BP 1061 EP 1071 DI 10.1111/j.1365-2966.2010.18193.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755CQ UT WOS:000289904600025 ER PT J AU Wang, J Navarro, JF Frenk, CS White, SDM Springel, V Jenkins, A Helmi, A Ludlow, A Vogelsberger, M AF Wang, J. Navarro, J. F. Frenk, C. S. White, S. D. M. Springel, V. Jenkins, A. Helmi, A. Ludlow, A. Vogelsberger, M. TI Assembly history and structure of galactic cold dark matter haloes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; Galaxy: formation; dark matter ID GALAXY FORMATION; MILKY-WAY; MASS; EVOLUTION; CLUSTERS; SUBSTRUCTURE; ACCRETION; UNIVERSE; MERGER; GROWTH AB We use the Aquarius simulation series to study the imprint of assembly history on the structure of Galaxy-mass cold dark matter haloes. Our results confirm earlier work regarding the influence of mergers on the mass density profile and the inside-out growth of haloes. The inner regions that contain the visible galaxies are stable since early times and are significantly affected only by major mergers. Particles accreted diffusely or in minor mergers are found predominantly in the outskirts of haloes. Our analysis reveals trends that run counter to current perceptions of hierarchical halo assembly. For example, major mergers (i.e. those with progenitor mass ratios greater than 1:10) contribute little to the total mass growth of a halo, on average less than 20 per cent for our six Aquarius haloes. The bulk is contributed roughly equally by minor mergers and by 'diffuse' material which is not resolved into individual objects. This is consistent with modelling based on excursion-set theory which suggests that about half of this diffuse material should not be part of a halo of any scale. The simulations themselves suggest that a significant fraction is not truly diffuse, since it was ejected from earlier haloes by mergers prior to their joining the main system. The Aquarius simulations resolve haloes to much lower mass scales than are expected to retain gas or form stars. Thus, the fraction of diffuse dark matter accreted by haloes represents a lower limit to the fraction of diffuse baryons accreted by galaxies. Our results thus confirm that most of the baryons from which visible galaxies form are accreted diffusely, rather than through mergers, and they suggest that only relatively rare major mergers will affect galaxy structure at later times. C1 [Wang, J.; Frenk, C. S.; Jenkins, A.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Navarro, J. F.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [White, S. D. M.; Springel, V.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Springel, V.] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, V.] Univ Heidelberg, Zentrum Astron, ARI, D-69120 Heidelberg, Germany. [Helmi, A.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Ludlow, A.] Argelander Inst Astron, D-53121 Bonn, Germany. [Vogelsberger, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wang, J (reprint author), Univ Durham, Dept Phys, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England. EM wangjie@mpa-garching.mpg.de OI Jenkins, Adrian/0000-0003-4389-2232 FU Royal Society; Netherlands Organisation for Scientific Research (NWO); European Research Council [240271]; STFC FX The simulations of the Aquarius Project were carried out at the Leibniz Computing Center, Garching, Germany; at the Computing Centre of the Max-Planck-Society in Garching; at the Institute for Computational Cosmology in Durham; and on the 'STELLA' supercomputer of the LOFAR experiment at the University of Groningen. We thank Shaun Cole for providing us the code to produce Monte Carlo merger trees and Mike Boylan-Kolchin for useful comments and careful reading of the manuscript. JW acknowledges a Royal Society Newton International Fellowship, CSF acknowledges a Royal Society Wolfson Research Merit Award and AH acknowledges support from a VIDI grant by Netherlands Organisation for Scientific Research (NWO). AH acknowledges funding from the European Research Council under ERC-StG GALACTICA-240271. This work was supported by an STFC rolling grant to the Institute for Computational Cosmology. NR 41 TC 60 Z9 60 U1 0 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY PY 2011 VL 413 IS 2 BP 1373 EP 1382 DI 10.1111/j.1365-2966.2011.18220.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755CQ UT WOS:000289904600051 ER PT J AU Vogelsberger, M White, SDM AF Vogelsberger, Mark White, Simon D. M. TI Streams and caustics: the fine-grained structure of Lambda cold dark matter haloes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; dark matter ID PHASE-SPACE STRUCTURE; GALACTIC HALO; SIMULATION AB We present the first and so far the only simulations to follow the fine-grained phase-space structure of galaxy haloes formed from generic Lambda cold dark matter initial conditions. We integrate the geodesic deviation equation in tandem with the N-body equations of motion, demonstrating that this can produce numerically converged results for the properties of fine-grained phase-space streams and their associated caustics, even in the inner regions of haloes. Our effective resolution for such structures is many orders of magnitude better than achieved by conventional techniques on even the largest simulations. We apply these methods to the six Milky Way mass haloes of the Aquarius Project. At 8 kpc from the halo centre, a typical point intersects about 1014 streams with a very broad range of individual densities; the similar to 106 most-massive streams contribute about half of the local dark matter density. As a result, the velocity distribution of dark matter particles should be very smooth with the most-massive fine-grained stream contributing about 0.1 per cent of the total signal. Dark matter particles at this radius have typically passed 200 caustics since the big bang, with a 5-95 per cent range of 50-500. Such caustic counts are a measure of the total amount of dynamical mixing and are very robustly determined by our technique. The peak densities on present-day caustics in the inner halo almost all lie well below the mean local dark matter density. As a result caustics provide a negligible boost (< 0.1 per cent) to the predicted local dark matter annihilation rate. The effective boost is larger in the outer halo but never exceeds about 10 per cent. Thus, fine-grained streams and their associated caustics have no effect on the detectability of the dark matter, either directly in Earth-bound laboratories or indirectly through annihilation radiation, with the exception that resonant cavity experiments searching for axions may see the most-massive local fine-grained streams because of their extreme localization in the energy-momentum space. C1 [Vogelsberger, Mark; White, Simon D. M.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vogelsberger, M (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM mvogelsberger@cfa.harvard.edu NR 39 TC 39 Z9 39 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 MAY PY 2011 VL 413 IS 2 BP 1419 EP 1438 DI 10.1111/j.1365-2966.2011.18224.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755CQ UT WOS:000289904600055 ER PT J AU Sani, E Marconi, A Hunt, LK Risaliti, G AF Sani, E. Marconi, A. Hunt, L. K. Risaliti, G. TI The Spitzer/IRAC view of black hole-bulge scaling relations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies: bulges; galaxies: fundamental parameters; galaxies: nuclei; galaxies: photometry; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; INFRARED ARRAY CAMERA; EARLY-TYPE GALAXIES; DIGITAL SKY SURVEY; TO-LIGHT RATIO; FUNDAMENTAL PLANE; ELLIPTIC GALAXIES; CLASSICAL BULGES; SPIRAL GALAXIES; M-BH AB We present a mid-infrared investigation of the scaling relations between supermassive black hole masses (M-BH) and the structural parameters of the host spheroids in local galaxies. This work is based on 2D bulge-disc decompositions of Spitzer/IRAC 3.6 mu m images of 57 galaxies with M-BH estimates. We first verify the accuracy of our decomposition by examining the Fundamental Plane (FP) of spheroids at 3.6 mu m. Our estimates of effective radii (R-e) and average surface brightnesses, combined with velocity dispersions from the literature, define a FP relation consistent with previous determinations but doubling the observed range in R-e. None of our galaxies is an outlier of the FP, demonstrating the accuracy of our bulge-disc decomposition which also allows us to independently identify pseudo-bulges in our sample. We calibrate M/L at 3.6 mu m by using the tight M-dyn-L-bul relation (similar to 0.1 dex intrinsic dispersion) and find that no colour corrections are required to estimate the stellar mass. The 3.6 mu m luminosity is thus the best tracer of stellar mass yet studied. We then explore the connection between M-BH and bulge structural parameters (luminosity, mass, effective radius). We find tight correlations of M-BH with both 3.6 mu m bulge luminosity and dynamical mass (M-BH/M-dyn similar to 1/1000), with intrinsic dispersions of similar to 0.35 dex, similar to the M-BH-Sigma relation. Our results are consistent with previous determinations at shorter wavelengths. By using our calibrated M/L, we rescale M-BH-L-bul to obtain the M-BH-M-star relation, which can be used as the local reference for high-z studies which probe the cosmic evolution of M-BH-galaxy relations and where the stellar mass is inferred directly from luminosity measurements. The analysis of pseudo-bulges shows that four out of nine lie on the scaling relations within the observed scatter, while those with small M-BH are significantly displaced. We explore the different origins for such behaviour while considering the possibility of nuclear morphological components not reproduced by our 2D decomposition. C1 [Sani, E.; Marconi, A.] Univ Florence, Dipartimento Fis & Astron, I-50125 Florence, Italy. [Sani, E.; Hunt, L. K.; Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sani, E (reprint author), Univ Florence, Dipartimento Fis & Astron, I-50125 Florence, Italy. EM sani@arcetri.astro.it RI Marconi, Alessandro/C-5880-2009; OI Marconi, Alessandro/0000-0002-9889-4238; Risaliti, Guido/0000-0002-3556-977X; Hunt, Leslie/0000-0001-9162-2371 FU NASA [Spitzer/1343503, GO-11735.01] FX The authors are grateful to the anonymous referee for the constructive comments and suggestions. We acknowledge B. M. Peterson for discussing the background effects and analysis method. ES thanks R. I. Davies, A. W. Graham and N. Neumayer for precious discussions on the pseudo-bulges and barred-galaxy behaviours. This work has been partially supported by the NASA grants Spitzer/1343503 and GO-11735.01. We acknowledge the usage of the HyperLeda database ( http://leda.univ-lyon1.fr). This research has made use of the NASA/IPAC extragalactic database (NED). NR 66 TC 94 Z9 94 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 MAY PY 2011 VL 413 IS 2 BP 1479 EP 1494 DI 10.1111/j.1365-2966.2011.18229.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 755CQ UT WOS:000289904600059 ER PT J AU Smith, FA Elliott, SM Lyons, SK AF Smith, Felisa A. Elliott, Scott M. Lyons, S. Kathleen TI Methane and megafauna reply SO NATURE GEOSCIENCE LA English DT Letter ID RATES; EMISSIONS; LAKES; TIME C1 [Smith, Felisa A.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Elliott, Scott M.] Los Alamos Natl Lab, Climate Ocean Sea Ice Modeling Team, Los Alamos, NM 87545 USA. [Lyons, S. Kathleen] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Smith, FA (reprint author), Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. EM fasmith@unm.edu NR 12 TC 1 Z9 1 U1 0 U2 7 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD MAY PY 2011 VL 4 IS 5 BP 272 EP 272 DI 10.1038/ngeo1149 PG 1 WC Geosciences, Multidisciplinary SC Geology GA 756MP UT WOS:000290016000003 ER PT J AU Carter, LM Campbell, DB Campbell, BA AF Carter, Lynn M. Campbell, Donald B. Campbell, Bruce A. TI Geologic Studies of Planetary Surfaces Using Radar Polarimetric Imaging SO PROCEEDINGS OF THE IEEE LA English DT Article DE Moon; polarimetry; radar; Venus ID VENUS; DEPOSITS; MOON; WAVELENGTH; MAGELLAN; ARECIBO; CENTIMETERS; EMISSION; BASIN AB Radar is a useful remote sensing tool for studying planetary geology because it is sensitive to the composition, structure, and roughness of the surface and can penetrate some materials to reveal buried terrain. The Arecibo Observatory radar system transmits a single sense of circular polarization, and both senses of circular polarization are received, which allows for the construction of the Stokes polarization vector. From the Stokes vector, daughter products such as the circular polarization ratio, the degree of linear polarization, and linear polarization angle are obtained. Recent polarimetric imaging using Arecibo has included Venus and the Moon. These observations can be compared to radar data for terrestrial surfaces to better understand surface physical properties and regional geologic evolution. For example, polarimetric radar studies of volcanic settings on Venus, the Moon, and Earth display some similarities, but also illustrate a variety of different emplacement and erosion mechanisms. Polarimetric radar data provide important information about surface properties beyond what can be obtained from single-polarization radar. Future observations using polarimetric synthetic aperture radar will provide information on roughness, composition, and stratigraphy that will support a broader interpretation of surface evolution. C1 [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Campbell, Donald B.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Carter, LM (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. EM lynn.m.carter@nasa.gov; campbell@astro.cornell.edu; campbellb@si.edu RI Carter, Lynn/D-2937-2012 NR 36 TC 17 Z9 18 U1 2 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9219 J9 P IEEE JI Proc. IEEE PD MAY PY 2011 VL 99 IS 5 BP 770 EP 782 DI 10.1109/JPROC.2010.2099090 PG 13 WC Engineering, Electrical & Electronic SC Engineering GA 755EK UT WOS:000289909500004 ER PT J AU Chalk, J Richmond, BG Ross, CF Strait, DS Wright, BW Spencer, MA Wang, QA Dechow, PC AF Chalk, Janine Richmond, Brian G. Ross, Callum F. Strait, David S. Wright, Barth W. Spencer, Mark A. Wang, Qian Dechow, Paul C. TI A Finite Element Analysis of Masticatory Stress Hypotheses SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE skull; feeding; biomechanics; bone strain; anthropoids ID IN-VIVO; SUPRAORBITAL REGION; BONE STRAIN; AUSTRALOPITHECUS-AFRICANUS; FEEDING BIOMECHANICS; RELEVANCE; MACAQUES; CRANIUM; MODELS; MORPHOLOGY AB Understanding how the skull transmits and dissipates forces during feeding provides insights into the selective pressures that may have driven the evolution of primate skull morphology. Traditionally, researchers have interpreted masticatory biomechanics in terms of simple global loading regimes applied to simple shapes (i.e., bending in sagittal and frontal planes, dorsoventral shear, and torsion of beams and cylinders). This study uses finite element analysis to examine the extent to which these geometric models provide accurate strain predictions in the face and evaluate whether simple global loading regimes predict strains that approximate the craniofacial deformation pattern observed during mastication. Loading regimes, including those simulating peak loads during molar chewing and those approximating the global loading regimes, were applied to a previously validated finite element model (FEM) of a macaque (Macaca fascicularis) skull, and the resulting strain patterns were compared. When simple global loading regimes are applied to the FEM, the resulting strains do not match those predicted by simple geometric models, suggesting that these models fail to generate accurate predictions of facial strain. Of the four loading regimes tested, bending in the frontal plane most closely approximates strain patterns in the circumorbital region and lateral face, apparently due to masseter muscle forces acting on the zygomatic arches. However, these results indicate that no single simple global loading regime satisfactorily accounts for the strain pattern found in the validated FEM. Instead, we propose that FE models replace simple cranial models when interpreting bone strain data and formulating hypotheses about craniofacial biomechanics. Am J Phys Anthropol 145:1-10, 2011. (C)2010 Wiley-Liss, Inc. C1 [Chalk, Janine] George Washington Univ, Dept Anthropol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Chalk, Janine; Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Amer Hist, Human Origins Program, Washington, DC 20560 USA. [Ross, Callum F.] Univ Chicago, Dept Organismal Biol & Anat, Chicago, IL 60637 USA. [Wright, Barth W.] Kansas City Univ Med & Biosci, Dept Anat, Kansas City, MO 64106 USA. [Spencer, Mark A.] Arizona State Univ, Sch Human Evolut & Social Change, Inst Human Origins, Tempe, AZ 85287 USA. [Wang, Qian] Mercer Univ, Sch Med, Div Basic Med Sci, Macon, GA 31207 USA. [Dechow, Paul C.] Texas A&M Hlth Sci Ctr, Baylor Coll Dent, Dept Biomed Sci, Dallas, TX 75246 USA. RP Chalk, J (reprint author), George Washington Univ, Dept Anthropol, Hominid Paleobiol Doctoral Program, 2110 G St NW, Washington, DC 20052 USA. EM jchalk@gwmail.gwu.edu FU NSF [0240865]; NSF HOMINID [BCS-0725141, BCS-0725122, BCS-0725147, BCS-0725219, BCS-0725126, BCS-0725183, BCS-0725136] FX NSF; Grant number: 0240865; Grant sponsor: NSF HOMINID; Grant numbers: BCS-0725141 (P. C. D.); BCS-0725122 (B. G. R.); BCS-0725147 (C. F. R.); BCS-0725219 (M. A. S.); BCS-0725126 (D. S. S.); BCS-0725183 (Q. W.); BCS-0725136 (B. W. W.). NR 42 TC 26 Z9 26 U1 0 U2 15 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD MAY PY 2011 VL 145 IS 1 BP 1 EP 10 DI 10.1002/ajpa.21416 PG 10 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 747XW UT WOS:000289355600001 PM 21484756 ER PT J AU De Queiroz, K AF De Queiroz, Kevin TI Branches in the lines of descent: Charles Darwin and the evolution of the species concept SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Evolutionary Synthesis; hierarchy of biological organization; incipient species; isolating mechanisms; lineage; phylogenetic systematics; species selection; taxonomic rank ID SPECIATION; INDIVIDUALS; NOTEBOOKS; SELECTION AB Charles Darwin introduced a novel idea into the concept of species, namely that species are branches in the lines of descent (segments of population lineages). In addition to this novel evolutionary component, Darwin's species concept also retained an older taxonomic component, namely the view that the species category is a taxonomic rank; moreover, he adopted amount of difference as a criterion for ranking lineages as species. Subsequent biologists retained both components of Darwin's species concept, although they replaced Darwin's ranking criterion with ranking criteria that either are more objectively defined or relate more directly to the biological bases of lineage separation and divergence. Numerous alternative ranking criteria were proposed, resulting in a proliferation of species definitions and a controversy concerning the concept of species. That controversy can be resolved by distinguishing more explicitly between the theoretical concept of species and the operational criteria that are used to apply the concept in practice. By viewing the various alternative ranking criteria as operational indicators of lineage separation rather than necessary properties of species, the conflicts among competing species concepts are eliminated, resulting in a unified concept of species. A brief examination of the history of biology reveals that an important shift related to the unified species concept has been emerging ever since Darwin reformulated the concept of species with an evolutionary basis. The species category is effectively being decoupled from the hierarchy of taxonomic ranks and transferred to the hierarchy of biological organization. Published 2011. This article is a US Government work and is in the public domain in the USA. (C) 2011 The Linnean Society of London, Biological Journal of the Linnean Society, 2011, 103, 19-35. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP De Queiroz, K (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM dequeirozk@si.edu NR 77 TC 16 Z9 20 U1 9 U2 73 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD MAY PY 2011 VL 103 IS 1 BP 19 EP 35 DI 10.1111/j.1095-8312.2011.01634.x PG 17 WC Evolutionary Biology SC Evolutionary Biology GA 751UG UT WOS:000289642500002 ER PT J AU Scarlata, CD Elias, BA Godwin, JR Powell, RA Shepherdson, D Shipley, LA Brown, JL AF Scarlata, Candace D. Elias, Becky A. Godwin, John R. Powell, Roger A. Shepherdson, David Shipley, Lisa A. Brown, Janine L. TI Characterizing gonadal and adrenal activity by fecal steroid analyses in pygmy rabbits (Brachylagus idahoensis) SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Brachylagus idalioensis; Cortisol; Hormones; Pregnancy; Progesterone; Pygmy rabbit; Reproduction ID HARES LEPUS-EUROPAEUS; FEMALE RABBIT; PROGESTERONE CONCENTRATIONS; PSEUDOPREGNANT RABBITS; ENDOCRINE PROFILES; WILD RABBITS; PREGNANCY; PLASMA; BEHAVIOR; ESTRADIOL-17-BETA AB In 2001, the sudden collapse of the Columbia Basin population of pygmy rabbits prompted the initiation of a captive breeding program to facilitate reintroduction, but reproductive success in captivity has not met expectations. Therefore, the objective of this study was to characterize the reproductive and adrenal endocrinology of this endangered rabbit species so that appropriate management strategies could be developed to monitor animal welfare and increase reproduction. Fecal samples were collected from 27 female pygmy rabbits over three breeding and non-breeding seasons. HPLC analyses verified the presence of progesterone in the excreta of pygmy rabbits, but the majority of progestagen metabolites were unidentified polar compounds. By contrast, > 70% of glucocorticoid immunoactivity was associated with cortisol. Longitudinal fecal hormone profiles during pregnancy were characterized by a large spike in progestagens shortly after mating, a gradual increase in progestagen and glucocorticoid concentrations throughout gestation and a return of hormones to baseline soon after birth (Day 24). The spike in progestagens 1 day after mating was a significant discovery for this species and appears to provide a reliable means of determining if a successful mating has occurred. Seasonal analyses of hormone excretion found that progestagen baselines did not vary between the breeding and non-breeding seasons, but, as expected, were highest during the breeding season in association with pregnancy. Across seasons, the lowest concentrations of glucocorticoids were associated with the highest rates of offspring production and survival, suggesting a possible link between heightened adrenal activity and lowered reproductive fitness in pygmy rabbits. Published by Elsevier Inc. C1 [Brown, Janine L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Shepherdson, David] Oregon Zoo, Portland, OR USA. [Elias, Becky A.; Shipley, Lisa A.] Washington State Univ, Pullman, WA 99164 USA. [Scarlata, Candace D.; Godwin, John R.; Powell, Roger A.] N Carolina State Univ, Raleigh, NC 27695 USA. RP Brown, JL (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. EM brownjan@si.edu FU Morris Animal Foundation; Smithsonian Institution; Friends of the National Zoo; Washington Department of Fish and Wildlife; North Carolina State University; Washington State University FX The authors are grateful to Dr. Heather Patisaul and Dr. Suzanne Kennedy Stoskopf for stimulating conversations throughout the study and helpful comments on drafts of the manuscript. We thank all the pygmy rabbit keepers (Michael, Becky, Jen, Amy, Hailey, Rachel, Kelli and Leanne) for their dedication to the rabbits and for all the hours spent collecting samples and behavioral data. In addition, thank you to Nicole Presley, Nicole Abbondanza and Sarah Putnam for unwavering technical assistance in the laboratory. Funding for this project was provided by a large grant from the Morris Animal Foundation and several supporting grants from the Smithsonian Institution, Friends of the National Zoo, Washington Department of Fish and Wildlife, North Carolina State University, and Washington State University. NR 54 TC 11 Z9 11 U1 2 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 EI 1095-6840 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD MAY 1 PY 2011 VL 171 IS 3 BP 373 EP 380 DI 10.1016/j.ygcen.2011.03.002 PG 8 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 752QY UT WOS:000289708700017 PM 21377469 ER PT J AU Ratcliffe, JM Jakobsen, L Kalko, EKV Surlykke, A AF Ratcliffe, John M. Jakobsen, Lasse Kalko, Elisabeth K. V. Surlykke, Annemarie TI Frequency alternation and an offbeat rhythm indicate foraging behavior in the echolocating bat, Saccopteryx bilineata SO JOURNAL OF COMPARATIVE PHYSIOLOGY A-NEUROETHOLOGY SENSORY NEURAL AND BEHAVIORAL PHYSIOLOGY LA English DT Article DE Sensory ecology; Foraging; Behavioral flexibility; Source level; Detection distance ID BIG BROWN BATS; EMBALLONURID BATS; EPTESICUS-FUSCUS; CALLS; SONGS; CHIROPTERA; DESIGN; FLIGHT; FIELD; PREY AB The greater sac-winged bat, Saccopteryx bilineata (Emballonuridae), uses two distinct echolocation call sequences: a 'monotonous' sequence, where bats emit similar to 48 kHz calls at a relatively stable rate, and a frequency-alternating sequence, where bats emit calls at similar to 45 kHz (low-note call) and similar to 48 kHz (high-note call). The frequencies of these low-high-note pairs remain stable within sequences. In Panama, we recorded echolocation calls from S. bilineata with a multi-microphone array at two sites: one a known roosting site, the other a known foraging site. Our results indicate that this species (1) only produces monotonous sequences in non-foraging contexts and, at times, directly after emitting a feeding buzz and (2) produces frequency-alternating sequences when actively foraging. These latter sequences are also characterized by an unusual, offbeat emission rhythm. We found significant positive relationships between (1) call intensity and call duration and (2) call intensity and distance from clutter. However, these relationships were weaker than those reported for bats from other families. We speculate on how call frequency alternation and an offbeat emission rhythm might reflect a novel strategy for prey detection at the edge of complex habitat in this ancient family of bats. C1 [Ratcliffe, John M.; Jakobsen, Lasse; Surlykke, Annemarie] Univ So Denmark, Inst Biol, DK-5230 Odense M, Denmark. [Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Ratcliffe, JM (reprint author), Univ So Denmark, Inst Biol, Campusvej 55, DK-5230 Odense M, Denmark. EM jmr@biology.sdu.dk OI Jakobsen, Lasse/0000-0002-8496-5576 FU Danish Natural Science Research Foundation; Oticon Foundation; STRI; German Science Foundation FX We thank Signe Brinklov for field assistance. Signe Brinklov, Brock Fenton, Kirsten Jung, Bjorn Siemers, Sub Zawadzki and two anonymous reviewers provided constructive criticism that helped us improve upon previous versions of the manuscript. STRI provided full access to research facilities and excellent logistical support. This study was funded by research grants from the Danish Natural Science Research Foundation (JMR, AS), the Oticon Foundation (LJ), STRI (EKVK) and the German Science Foundation (EKVK). NR 46 TC 14 Z9 16 U1 0 U2 23 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-7594 J9 J COMP PHYSIOL A JI J. Comp. Physiol. A -Neuroethol. Sens. Neural Behav. Physiol. PD MAY PY 2011 VL 197 IS 5 SI SI BP 413 EP 423 DI 10.1007/s00359-011-0630-0 PG 11 WC Behavioral Sciences; Neurosciences; Physiology; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Physiology; Zoology GA 752JR UT WOS:000289687900003 PM 21327333 ER PT J AU Leshchishina, O Kassi, S Gordon, IE Yu, SS Campargue, A AF Leshchishina, Olga Kassi, Samir Gordon, Iouli E. Yu, Shanshan Campargue, Alain TI The a(1)Delta(g)-X-3 Sigma(-)(g) band of (OO)-O-16-O-17, (OO)-O-17-O-18 and O-17(2) by high sensitivity CRDS near 1.27 mu m SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Oxygen; O-2; O-17 isotopologues; Hyperfine structure; Cavity ring down spectroscopy; Cryogenic cell ID CAVITY RINGDOWN SPECTROSCOPY; HYPERFINE-STRUCTURE; RESONANCE-SPECTRUM; ISOTOPOLOGUES; TRANSITIONS; OXYGEN AB The very weak a(1)Delta(g)-X-3 Sigma(-)(g) system of the three O-17 isotopologues of oxygen - O-16-O-17, (OO)-O-17-O-18 and O-17(2) - was studied by high sensitivity CW-Cavity Ring Down Spectroscopy. The spectra of a O-17 highly enriched sample were recorded at room temperature between 7640 and 7917 cm(-1) and at liquid nitrogen temperature in the 7876-7893 cm(-1) region. The magnetic dipole (0-0) band was observed for all three O-17 isotopologues. At liquid nitrogen temperature, some of the transitions were observed with partially resolved hyperfine splitting due to the O-17 nuclear spin. The electric quadrupole (0-0) band and the (1-1) hot band were also observed for the 180170 and O-17(2) species. The rotational and hyperfine spectroscopic parameters of the X-3 Sigma(-)(g) and a(1)Delta(g) states of the three studied isotopologues were derived from a global fit of the measured line positions and microwave and Raman measurements available in the literature. The spectroscopic constants of the a(1)Delta(g) (v=0, 1) states of O-17(2) are reported for the first time. (C) 2011 Elsevier Ltd. All rights reserved. C1 [Leshchishina, Olga; Kassi, Samir; Campargue, Alain] Univ Grenoble 1, CNRS, LIPHY UMR5588, F-38041 Grenoble, France. [Leshchishina, Olga] Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634021, Russia. [Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Yu, Shanshan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Campargue, A (reprint author), Univ Grenoble 1, CNRS, LIPHY UMR5588, F-38041 Grenoble, France. EM Alain.CAMPARGUE@ujf-grenoble.fr RI Yu, Shanshan/D-8733-2016 FU Grenoble University under the ANR [NT09_436466]; Jet Propulsion Laboratory, California Institute of Technology; Harvard-Smithsonian Center for Astrophysics; National Aeronautics and Space Administration FX Part of this work was performed at Grenoble University under the ANR project "IDEO" (NT09_436466). A portion of this research was performed at Jet Propulsion Laboratory, California Institute of Technology and Harvard-Smithsonian Center for Astrophysics, under contract with the National Aeronautics and Space Administration. NR 23 TC 10 Z9 10 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD MAY PY 2011 VL 112 IS 8 BP 1257 EP 1265 DI 10.1016/j.jqsrt.2011.01.014 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 753XB UT WOS:000289812600001 ER PT J AU Kalfountzou, E Trichas, M Rowan-Robinson, M Clements, D Babbedge, T Seiradakis, JH AF Kalfountzou, E. Trichas, M. Rowan-Robinson, M. Clements, D. Babbedge, T. Seiradakis, J. H. TI EFOSC2 spectroscopy of SWIRE-CDFS galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; catalogues; surveys; quasars: emission lines; galaxies: Seyfert; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; HOST GALAXIES; CLASSIFICATION AB We present the optical spectra of a sample of 34 Spitzer Wide-Area Infrared Extragalactic Survey (SWIRE)-Chandra Deep Field South (CDFS) sources observed with the European Southern Observatory (ESO) Faint Object Spectrograph and Camera (EFOSC2) on the ESO 3.6-m telescope. We have used the spectra and spectroscopic redshifts to validate our photometric redshift codes and spectral energy distribution (SED) template fitting methods. 12 of our sources are infrared luminous galaxies. Of these, five belong to the class of ultraluminous infrared galaxies (ULIRGs) and one to the class of hyperluminous infrared galaxies (HLIRGs), with evidence of both an active galactic nucleus and a starburst component contributing to their extreme infrared luminosity for three, a starburst contributing for one and AGN contributing for two of them. C1 [Kalfountzou, E.; Seiradakis, J. H.] Aristotle Univ Thessaloniki, Dept Phys, Sect Astrophys Astron & Mech, GR-54124 Thessaloniki, Greece. [Kalfountzou, E.] Univ Hertfordshire, Ctr Astrophys, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rowan-Robinson, M.; Clements, D.; Babbedge, T.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. RP Kalfountzou, E (reprint author), Aristotle Univ Thessaloniki, Dept Phys, Sect Astrophys Astron & Mech, GR-54124 Thessaloniki, Greece. EM e.kalfountzou@herts.ac.uk NR 17 TC 7 Z9 8 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 MAY PY 2011 VL 413 IS 1 BP 249 EP 261 DI 10.1111/j.1365-2966.2010.18131.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750DN UT WOS:000289525000019 ER PT J AU Bernardi, G Mitchell, DA Ord, SM Greenhill, LJ Pindor, B Wayth, RB Wyithe, JSB AF Bernardi, G. Mitchell, D. A. Ord, S. M. Greenhill, L. J. Pindor, B. Wayth, R. B. Wyithe, J. S. B. TI Subtraction of point sources from interferometric radio images through an algebraic forward modelling scheme SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; methods: numerical; techniques: interferometric; cosmology: observations; dark ages, reionization, first stars; diffuse radiation ID DYNAMIC-RANGE; FOREGROUND SUBTRACTION; PARAMETER-ESTIMATION; 150 MHZ; REIONIZATION; EPOCH; 21-CM; EMISSION; ARRAY; FIELD AB We present a method for subtracting point sources from interferometric radio images via forward modelling of the instrument response and involving an algebraic non-linear minimization. The method is applied to simulated maps of the Murchison Wide-field Array but is generally useful in cases where only image data are available. After source subtraction, the residual maps have no statistical difference to the expected thermal noise distribution at all angular scales, indicating high effectiveness in the subtraction. Simulations indicate that the errors in recovering the source parameters decrease with increasing signal-to-noise ratio, which is consistent with the theoretical measurement errors. In applying the technique to simulated snapshot observations with the Murchison Wide-field Array, we found that all 101 sources present in the simulation were recovered with an average position error of 10 arcsec and an average flux density error of 0.15 per cent. This led to a dynamic range increase of approximately 3 orders of magnitude. Since all the sources were deconvolved jointly, the subtraction was not limited by source sidelobes but by thermal noise. This technique is a promising deconvolution method for upcoming radio arrays with a huge number of elements and a candidate for the difficult task of subtracting foreground sources from observations of the 21-cm neutral hydrogen signal from the epoch of reionization. C1 [Bernardi, G.; Mitchell, D. A.; Ord, S. M.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pindor, B.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Wayth, R. B.] ICRAR Curtin Inst Radioastron, Perth, WA 6845, Australia. RP Bernardi, G (reprint author), Harvard Smithsonian Ctr Astrophys, Garden St 60, Cambridge, MA 02138 USA. EM gbernardi@cfa.harvard.edu RI Wayth, Randall/B-2444-2013; Ord, Stephen/C-6138-2013; OI Wayth, Randall/0000-0002-6995-4131; Wyithe, Stuart/0000-0001-7956-9758 FU US National Science Foundation [AST-0457585, PHY-0835713] FX We thank an anonymous referee for useful comments. This work was supported by the US National Science Foundation under grants AST-0457585 and PHY-0835713. NR 37 TC 9 Z9 9 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 MAY PY 2011 VL 413 IS 1 BP 411 EP 422 DI 10.1111/j.1365-2966.2010.18145.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750DN UT WOS:000289525000032 ER PT J AU Han, KL Braun, EL Kimball, RT Reddy, S Bowie, RCK Braun, MJ Chojnowski, JL Hackett, SJ Harshman, J Huddleston, CJ Marks, BD Miglia, KJ Moore, WS Sheldon, FH Steadman, DW Witt, CC Yuri, T AF Han, Kin-Lan Braun, Edward L. Kimball, Rebecca T. Reddy, Sushma Bowie, Rauri C. K. Braun, Michael J. Chojnowski, Jena L. Hackett, Shannon J. Harshman, John Huddleston, Christopher J. Marks, Ben D. Miglia, Kathleen J. Moore, William S. Sheldon, Frederick H. Steadman, David W. Witt, Christopher C. Yuri, Tamaki TI Are Transposable Element Insertions Homoplasy Free?: An Examination Using the Avian Tree of Life SO SYSTEMATIC BIOLOGY LA English DT Article ID EVOLUTIONARY HISTORY; CHICKEN GENOME; RETROTRANSPOSABLE ELEMENTS; MOLECULAR SYSTEMATICS; PLACENTAL MAMMALS; PERFECT CHARACTER; DIVERGENCE TIMES; SPECIES TREES; CR-1 ELEMENTS; SEQUENCE DATA C1 [Han, Kin-Lan; Braun, Edward L.; Kimball, Rebecca T.; Chojnowski, Jena L.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Han, Kin-Lan; Braun, Michael J.; Huddleston, Christopher J.] Smithsonian Inst, Dept Vertebrate Zool, Suitland, MD 20746 USA. [Han, Kin-Lan; Braun, Michael J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. [Reddy, Sushma] Loyola Univ, Dept Biol, Chicago, IL 60626 USA. [Reddy, Sushma; Hackett, Shannon J.; Harshman, John] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. [Bowie, Rauri C. K.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Bowie, Rauri C. K.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Marks, Ben D.; Sheldon, Frederick H.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Miglia, Kathleen J.; Moore, William S.] Wayne State Univ, Dept Biol Sci, Detroit, MI 48202 USA. [Steadman, David W.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Witt, Christopher C.; Yuri, Tamaki] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Witt, Christopher C.] Univ New Mexico, Museum SW Biol, Albuquerque, NM 87131 USA. [Yuri, Tamaki] Univ Oklahoma, Sam Noble Oklahoma Museum Nat Hist, Norman, OK 73072 USA. RP Han, KL (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM hankin@ufl.edu RI Han, Kin-Lan/G-7121-2011; Witt, Christopher/D-8587-2012; Kimball, Rebecca/C-2290-2009; OI Braun, Edward/0000-0003-1643-5212; Kimball, Rebecca/0000-0001-5449-5481; Witt, Christopher/0000-0003-2781-1543; Bowie, Rauri/0000-0001-8328-6021 FU U.S. National Science Foundation [DEB-0228682, DEB-0228675, DEB-0228688, DEB-0228617] FX This work was supported by the U.S. National Science Foundation Assembling the Tree of Life Program (DEB-0228682 to R.T.K., E.L.B., and D.W.S., DEB-0228675 to S.J.H., DEB-0228688 to F.H.S., and DEB-0228617 to W.S.M.). NR 73 TC 30 Z9 31 U1 1 U2 12 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 MAY PY 2011 VL 60 IS 3 BP 375 EP 386 DI 10.1093/sysbio/syq100 PG 12 WC Evolutionary Biology SC Evolutionary Biology GA 753UQ UT WOS:000289805600011 PM 21303823 ER PT J AU Sofaer, HR Langin, KM Wilson, J Sillett, TS AF Sofaer, H. R. Langin, K. M. Wilson, J. Sillett, T. S. TI Demography of Songbird Populations in a Rapidly Changing World: The Importance of Long-term Studies SO AMERICAN BIOLOGY TEACHER LA English DT Editorial Material DE Population ecology; density dependence; climate change; online module ID MIGRATORY SONGBIRDS; CLIMATE-CHANGE; FECUNDITY; BIRDS AB A major goal of ecological research is to understand how ecological factors, such as food and predator abundance, interact to shape birth and death rates. Case studies describing this research can provide students with an understanding of how ecological conditions affect demographic rates, as well as an opportunity to explore and interpret real data. We have developed a Web-based teaching module based on a long-term study of a migratory songbird, the black-throated blue warbler (Dendroica caerulescens). The website describes this species and the ecological factors that affect its population growth and provides three exercises developed to span a range of student levels. C1 [Sofaer, H. R.; Langin, K. M.] Colorado State Univ, Ft Collins, CO 80523 USA. [Wilson, J.] Hubbard Brook Res Fdn, Hanover, NH 03755 USA. [Sillett, T. S.] Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP Sofaer, HR (reprint author), Colorado State Univ, 1878 Campus Delivery, Ft Collins, CO 80523 USA. EM helen@lamar.colostate.edu; langink@rams.colostate.edu; jwilson@hbresearchfoundation.org; silletts@si.edu NR 11 TC 0 Z9 0 U1 0 U2 13 PU NATL ASSOC BIOLOGY TEACHERS INC PI RESTON PA 12030 SUNRISE VALLEY DR, #110, RESTON, VA 20191 USA SN 0002-7685 J9 AM BIOL TEACH JI Am. Biol. Teach. PD MAY PY 2011 VL 73 IS 5 BP 285 EP 287 DI 10.1525/abt.2011.73.5.8 PG 3 WC Biology; Education, Scientific Disciplines SC Life Sciences & Biomedicine - Other Topics; Education & Educational Research GA 957UC UT WOS:000305188100008 ER PT J AU Kinman, TD Brown, WR AF Kinman, T. D. Brown, Warren R. TI THE BHB STARS IN THE SURVEY FIELDS OF RODGERS ET AL. (1993): NEW OBSERVATIONS AND COMPARISONS WITH OTHER RECENT SURVEYS SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: structure; stars: horizontal-branch ID HORIZONTAL-BRANCH STARS; RR-LYRAE STARS; A-TYPE STARS; ORTHOGONAL HALO FIELDS; SKY VARIABILITY SURVEY; PHOTOMETRIC STANDARD STARS; NORTH GALACTIC POLE; HIGH-VELOCITY STARS; MILKY-WAY; INNER HALO AB We study blue horizontal branch (BHB) and RR Lyrae stars in the Rodgers et al. fields and compare their velocity and density distributions with other surveys in the same part of the sky. Photometric data are given for 176 early-type stars in the northern field. We identify fourteen BHB stars and four possible BHB stars, and determine the selection efficiency of the Century survey, the HK survey, and the SDSS survey for BHB stars. We give light curves and. radial velocities for three type ab RR Lyrae stars in the northern field; comparison with the nearby LONEOS survey shows that there is likely to be an equal number of lower-amplitude type ab RR Lyrae stars that we do not find. There are therefore at least twice as many BHB stars as type ab RR Lyrae stars in the northern field-similar to the ratio in the solar neighborhood. The velocity distribution of the southern field shows no evidence for an anomalous thick disk that was found by Gilmore et al.; the halo velocity peaks at a slightly prograde rotational velocity but there is also a significant retrograde halo component in this field. The velocity distribution in the northern field shows no evidence of Galactic rotation for vertical bar Z vertical bar >= 4 kpc and a slight prograde motion for vertical bar Z vertical bar < 4 kpc. The space densities of BHB stars in the northern field agree with an extrapolation of the power-law distribution recently derived by de Propris et al. For vertical bar Z vertical bar < 4 kpc, however, we observe an excess of BHB stars compared with this power law. We conclude that these BHB stars mostly belong to a spatially flattened, non-rotating inner halo component of the Milky Way in confirmation of the Kinman et al. analysis of Century survey BHB stars. C1 [Kinman, T. D.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kinman, TD (reprint author), Natl Opt Astron Observ, POB 26732, Tucson, AZ 85726 USA. NR 84 TC 1 Z9 1 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2011 VL 141 IS 5 AR 168 DI 10.1088/0004-6256/141/5/168 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 746JB UT WOS:000289240800027 ER PT J AU Feigelson, ED Getman, KV Townsley, LK Broos, PS Povich, MS Garmire, GP King, RR Montmerle, T Preibisch, T Smith, N Stassun, KG Wang, JF Wolk, S Zinnecker, H AF Feigelson, Eric D. Getman, Konstantin V. Townsley, Leisa K. Broos, Patrick S. Povich, Matthew S. Garmire, Gordon P. King, Robert R. Montmerle, Thierry Preibisch, Thomas Smith, Nathan Stassun, Keivan G. Wang, Junfeng Wolk, Scott Zinnecker, Hans TI X-RAY STAR CLUSTERS IN THE CARINA COMPLEX SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM: individual objects (Carina Nebula); open clusters and associations: individual (Trumpler 14, Trumpler 15, Trumpler 16, Collinder 228, C); stars: formation; stars: pre-main sequence; X-rays: stars ID ORION ULTRADEEP PROJECT; YOUNG STELLAR OBJECTS; MOLECULAR CLOUD; ETA-CARINAE; FORMING COMPLEX; CHANDRA-ACIS; TRUMPLER 16; OB STARS; NEBULA; EMISSION AB The distribution of young stars found in the Chandra Carina Complex Project (CCCP) is examined for clustering structure. X-ray surveys are advantageous for identifying young stellar populations compared to optical and infrared surveys in suffering less contamination from nebular emission and Galactic field stars. The analysis is based on smoothed maps of a spatially complete subsample of similar to 3000 brighter X-ray sources classified as Carina members and similar to 10,000 stars from the full CCCP sample. The principal known clusters are recovered, and some additional smaller groups are identified. No rich embedded clusters are present, although a number of sparse groups are found. The CCCP reveals considerable complexity in clustering properties. The Trumpler 14 and 15 clusters have rich stellar populations in unimodal, centrally concentrated structures several parsecs across. Non-spherical internal structure is seen, and large-scale low surface density distributions surround these rich clusters. Trumpler 16, in contrast, is comprised of several smaller clusters within a circular boundary. Collinder 228 is a third type of cluster which extends over tens of parsecs with many sparse compact groups likely arising from triggered star formation processes. A widely dispersed, but highly populous, distribution of X-ray stars across the similar to 50 pc CCCP mosaic supports a model of past generations of star formation in the region. Collinder 234, a group of massive stars without an associated cluster of pre-main-sequence stars, may be part of this dispersed population. C1 [Feigelson, Eric D.; Getman, Konstantin V.; Townsley, Leisa K.; Broos, Patrick S.; Povich, Matthew S.; Garmire, Gordon P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [King, Robert R.] Univ Exeter, Astrophys Grp, Coll Engn Math & Phys Sci, Exeter EX4 4QL, Devon, England. [Montmerle, Thierry] Inst Astrophys, F-75014 Paris, France. [Preibisch, Thomas] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany. [Smith, Nathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Wang, Junfeng; Wolk, Scott] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zinnecker, Hans] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. RP Feigelson, ED (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM edf@astro.psu.edu OI Wolk, Scott/0000-0002-0826-9261 FU Chandra [GO8-9131X]; ACIS Instrument Team [SV4-74018]; NASA [NAS8-03060]; NSF [AST-0849736] FX We thank Cathie Clarke (Cambridge) and Nicolas Grosso (Strasbourg) for discussions, and the anonymous referee for useful suggestions. This work is supported by Chandra X-Ray Observatory grant GO8-9131X (PI: L. Townsley) and by the ACIS Instrument Team contract SV4-74018 (PI: G. Garmire), issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. K. G. S. is supported by NSF grant AST-0849736. NR 67 TC 41 Z9 41 U1 1 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 MAY PY 2011 VL 194 IS 1 DI 10.1088/0067-0049/194/1/9 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757MC UT WOS:000290088300009 ER PT J AU Povich, MS Smith, N Majewski, SR Getman, KV Townsley, LK Babler, BL Broos, PS Indebetouw, R Meade, MR Robitaille, TP Stassun, KG Whitney, BA Yonekura, Y Fukui, Y AF Povich, Matthew S. Smith, Nathan Majewski, Steven R. Getman, Konstantin V. Townsley, Leisa K. Babler, Brian L. Broos, Patrick S. Indebetouw, Remy Meade, Marilyn R. Robitaille, Thomas P. Stassun, Keivan G. Whitney, Barbara A. Yonekura, Yoshinori Fukui, Yasuo TI A PAN-CARINA YOUNG STELLAR OBJECT CATALOG: INTERMEDIATE-MASS YOUNG STELLAR OBJECTS IN THE CARINA NEBULA IDENTIFIED VIA MID-INFRARED EXCESS EMISSION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; ISM: individual objects (NGC 3372); stars: formation; stars: luminosity function, mass function; stars: pre-main sequence; X-rays: stars ID X-RAY-EMISSION; SPECTRAL ENERGY-DISTRIBUTIONS; SPITZER-SPACE-TELESCOPE; TRIGGERED STAR-FORMATION; LARGE-MAGELLANIC-CLOUD; MAIN-SEQUENCE STARS; ETA-CARINAE; ORION-NEBULA; MU-M; INTERSTELLAR EXTINCTION AB We present a catalog of 1439 young stellar objects (YSOs) spanning the 1.42 deg(2) field surveyed by the Chandra Carina Complex Project (CCCP), which includes the major ionizing clusters and the most active sites of ongoing star formation within the Great Nebula in Carina. Candidate YSOs were identified via infrared (IR) excess emission from dusty circumstellar disks and envelopes, using data from the Spitzer Space Telescope (the Vela-Carina survey) and the Two-Micron All Sky Survey. We model the 1-24 mu m IR spectral energy distributions of the YSOs to constrain physical properties. Our Pan-Carina YSO Catalog (PCYC) is dominated by intermediate-mass (2 M-circle dot < m less than or similar to 10 M-circle dot) objects with disks, including Herbig Ae/Be stars and their less evolved progenitors. The PCYC provides a valuable complementary data set to the CCCP X-ray source catalogs, identifying 1029 YSOs in Carina with no X-ray detection. We also catalog 410 YSOs with X-ray counterparts, including 62 candidate protostars. Candidate protostars with X-ray detections tend to be more evolved than those without. In most cases, X-ray emission apparently originating from intermediate-mass, disk-dominated YSOs is consistent with the presence of low-mass companions, but we also find that X-ray emission correlates with cooler stellar photospheres and higher disk masses. We suggest that intermediate-mass YSOs produce X-rays during their early pre-main-sequence evolution, perhaps driven by magnetic dynamo activity during the convective atmosphere phase, but this emission dies off as the stars approach the main sequence. Extrapolating over the stellar initial mass function scaled to the PCYC population, we predict a total population of > 2 x 10(4) YSOs and a present-day star formation rate (SFR) of >0.008 M-circle dot yr(-1). The global SFR in the Carina Nebula, averaged over the past similar to 5 Myr, has been approximately constant. C1 [Povich, Matthew S.; Getman, Konstantin V.; Townsley, Leisa K.; Broos, Patrick S.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Majewski, Steven R.; Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Babler, Brian L.; Meade, Marilyn R.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Robitaille, Thomas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Whitney, Barbara A.] Space Sci Inst, Boulder, CO 80303 USA. [Yonekura, Yoshinori] Osaka Prefecture Univ, Dept Phys Sci, Osaka 5998531, Japan. [Yonekura, Yoshinori] Ibaraki Univ, Ctr Astron, Mito, Ibaraki 3108512, Japan. [Fukui, Yasuo] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. RP Povich, MS (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM povich@astro.psu.edu OI Babler, Brian/0000-0002-6984-5752; Robitaille, Thomas/0000-0002-8642-1329 FU NSF [AST-0901646, AST-0849736]; NASA; Chandra [GO-9131X]; ACIS Instrument Team [SV4-74018] FX We thank E. D. Feigelson, T. Preibisch, and T. Montmerle for insightful conversations that helped improve this work. We thank the anonymous referee for a timely and valuable review. M. S. P. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0901646. This work is based on observations from the Spitzer Space Telescope GO programs 30848 (MIPSCAR; PI: N.S.) and 40791 (Vela-Carina; PI: S. R. M.). 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. Support for this work was provided by NASA through awards issued by the Jet Propulsion Laboratory, California Institute of Technology. This work was also supported by Chandra X-ray Observatory grant GO-9131X (PI: L. K. T.) and by the ACIS Instrument Team contract SV4-74018 (PI: G. Garmire), issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. K. G. S. acknowledges support from NSF grant AST-0849736. NR 81 TC 60 Z9 60 U1 1 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 MAY PY 2011 VL 194 IS 1 DI 10.1088/0067-0049/194/1/14 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757MC UT WOS:000290088300014 ER PT J AU Gingerich, O Van Helden, A AF Gingerich, Owen Van Helden, Albert TI HOW GALILEO CONSTRUCTED THE MOONS OF JUPITER SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Article C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Van Helden, Albert] Univ Utrecht, NL-3508 TC Utrecht, Netherlands. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM a.vanhelden@uu.nl NR 6 TC 5 Z9 5 U1 1 U2 5 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD MAY PY 2011 VL 42 BP 259 EP 264 PN 2 PG 6 WC History & Philosophy Of Science SC History & Philosophy of Science GA 932IU UT WOS:000303285400008 ER PT J AU Gingerich, O AF Gingerich, Owen TI Science and Theology in the Reformation: Studies in Theological Interpretation and Astronomical Observation in Sixteenth-Century Germany SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD MAY PY 2011 VL 42 BP 267 EP 267 PN 2 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA 932IU UT WOS:000303285400010 ER PT J AU Kowalewski, M Payne, JL Smith, FA Wang, SC McShea, DW Xiao, SH Novack-Gottshall, PM McClain, CR Krause, RA Boyer, AG Finnegan, S Lyons, SK Stempien, JA Alroy, J Spaeth, PA AF Kowalewski, Michal Payne, Jonathan L. Smith, Felisa A. Wang, Steve C. McShea, Daniel W. Xiao, Shuhai Novack-Gottshall, Philip M. McClain, Craig R. Krause, Richard A., Jr. Boyer, Alison G. Finnegan, Seth Lyons, S. Kathleen Stempien, Jennifer A. Alroy, John Spaeth, Paula A. TI THE GEOZOIC SUPEREON SO PALAIOS LA English DT Editorial Material ID CONFIDENCE-INTERVALS; WESTERN-AUSTRALIA; LIFE; EARTH; ORIGIN; DIVERSITY; GREENLAND; INCREASE; RANGES; ROCKS C1 [Kowalewski, Michal; Xiao, Shuhai] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. [Payne, Jonathan L.; Wang, Steve C.] Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA. [Smith, Felisa A.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Wang, Steve C.] Swarthmore Coll, Dept Math & Stat, Swarthmore, PA 19081 USA. [McShea, Daniel W.] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Novack-Gottshall, Philip M.] Benedictine Univ, Dept Biol Sci, Lisle, IL 60532 USA. [McClain, Craig R.] Natl Evolutionary Synth Ctr, Durham, NC 27705 USA. [Krause, Richard A., Jr.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA. [Boyer, Alison G.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Finnegan, Seth] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Lyons, S. Kathleen] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Stempien, Jennifer A.] Washington & Lee Univ, Dept Geol, Lexington, VA 24450 USA. [Alroy, John] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. [Spaeth, Paula A.] Northland Coll, Ashland, WI 54806 USA. RP Kowalewski, M (reprint author), Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. EM michalk@vt.edu RI Krause, Richard/C-8724-2009; Kowalewski, Michal/B-4263-2008; Payne, Jonathan/A-1240-2007; Alroy, John/B-4585-2009; Payne, Jonathan/B-8088-2012; Xiao, Shuhai/A-2190-2009 OI Wang, Steve/0000-0002-8953-285X; McClain, Craig/0000-0003-0574-428X; Krause, Richard/0000-0001-5619-4551; Kowalewski, Michal/0000-0002-8575-4711; Novack-Gottshall, Philip/0000-0002-2583-2968; Payne, Jonathan/0000-0002-9601-3310; Xiao, Shuhai/0000-0003-4655-2663 NR 43 TC 4 Z9 4 U1 0 U2 6 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 EI 1938-5323 J9 PALAIOS JI Palaios PD MAY-JUN PY 2011 VL 26 IS 5-6 BP 251 EP 255 DI 10.2110/palo.2011.S03 PG 5 WC Geology; Paleontology SC Geology; Paleontology GA 786YC UT WOS:000292342800001 ER PT J AU Goh, KM Chua, YS Rahman, RNZRA Chan, R Illias, RM AF Goh, Kian Mau Chua, Yung Seng Rahman, Raja Noor Zaliha Raja Abdul Chan, Raymund Illias, Rosli Md. TI A comparison of conventional and miniprimer PCR to elucidate bacteria diversity in Malaysia Ulu Slim hot spring using 16S rDNA clone library SO ROMANIAN BIOTECHNOLOGICAL LETTERS LA English DT Article DE prokaryote biodiversity; thermophiles; hot springs; Restriction Fragment Length Polymorphism ID CANDIDATE DIVISION; SOIL DNA; REMOVAL AB The diversity of the bacterial community in Ulu Slim hot spring was examined using a 16S ribosomal DNA culture-independent approach. A total of 144 different 16S rDNA sequences were cloned and analyzed. The majority of sequences were found to be within the Betaproteobacteria and Gammaproteobacteria while the remaining sequences belonged to the Bacteroidetes, Acidobacteria, Cloroflexi, Nitrospira and candidate divisions. Some of the bacteria 16S sequences could be novel and indigenous to this hot spring as their sequences are low in similarity when compared with known sequences. The 16S ribosomal DNA clone library was assembled using conventional PCR amplification with degenerate 27F and 1492R primers specific for bacterial rDNA. A new miniprimer PCR assay was also used to construct a library. When compared, we conclude that the latter approach which using mutagenized Dynamo-II polymerase utilizing 10-mer primers was a better approach than the conventional PCR as the environmental humid acid inhibition effect was less. Ideally, to best understand the overall prokaryote diversity in the hot spring, it is better to use a combined conventional and miniprimer PCR approach. C1 [Goh, Kian Mau; Chua, Yung Seng; Illias, Rosli Md.] Univ Teknol Malaysia, Fac Biosci & Bioengn, Skudai 81310, Johor, Malaysia. [Rahman, Raja Noor Zaliha Raja Abdul] Univ Putra Malaysia, Fac Biotechnol & Biomol Sci, Enzyme & Microbial Technol Res Group, Serdang, Malaysia. [Chan, Raymund] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20560 USA. [Illias, Rosli Md.] Univ Teknol Malaysia, Fac Chem Engn, Dept Bioproc Engn, Skudai 81310, Johor, Malaysia. RP Goh, KM (reprint author), Univ Teknol Malaysia, Fac Biosci & Bioengn, Skudai 81310, Johor, Malaysia. EM gohkianmau@utm.my RI Goh, Kian Mau/C-7221-2011; OI Goh, KianMau/0000-0002-2839-8722 FU Malaysian Ministry of Higher Education [78393] FX This work was supported by the Malaysian Ministry of Higher Education, Fundamental Research Grant Scheme (FRGS) under Grant Number 78393. We thank FINNZYMES OY for the gift of the Dynamoll polymerase kit. NR 20 TC 2 Z9 3 U1 0 U2 6 PU ARS DOCENDI PI BUCHAREST PA SOS PANDURI 90, SECT 5, BUCHAREST, RO-050663, ROMANIA SN 1224-5984 J9 ROM BIOTECH LETT JI Rom. Biotech. Lett. PD MAY-JUN PY 2011 VL 16 IS 3 BP 6247 EP 6255 PG 9 WC Biotechnology & Applied Microbiology SC Biotechnology & Applied Microbiology GA 786CK UT WOS:000292280200014 ER PT J AU Clough, GW AF Clough, G. Wayne TI Synergies SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAY PY 2011 VL 42 IS 2 BP 28 EP 28 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 753YF UT WOS:000289815900010 ER PT J AU Launius, RD AF Launius, Roger D. TI Climate change and spaceflight: an historiographical review SO WILEY INTERDISCIPLINARY REVIEWS-CLIMATE CHANGE LA English DT Review AB This article discusses the broad use of space-based resources to study climate change and the historical efforts to understand this effort. The historiography of this subject is still in its infancy, but there are several benchmark studies that focus on NASA's efforts along these lines. The key work of Erik Conway, Mark Bowen, and other recent researchers inform this study. This article concludes with a discussion of possibilities for future historical studies in climate change and spaceflight. (C) 2011 John Wiley & Sons, Ltd. WIREs Clim Change 2011 2 412-427 DOI:10.1002/wcc.114 C1 Smithsonian Inst, Space Hist Natl Air & Space Museum, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Space Hist Natl Air & Space Museum, Washington, DC 20560 USA. EM launiusr@si.edu OI Launius, Roger/0000-0003-1633-1253 NR 68 TC 0 Z9 0 U1 0 U2 2 PU WILEY PERIODICALS, INC PI SAN FRANCISCO PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA SN 1757-7780 J9 WIRES CLIM CHANGE JI Wiley Interdiscip. Rev.-Clim. Chang. PD MAY-JUN PY 2011 VL 2 IS 3 BP 412 EP 427 DI 10.1002/wcc.114 PG 16 WC Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 778WJ UT WOS:000291739800007 ER PT J AU Kralj-Fiser, S Gregoric, M Zhang, SC Li, DQ Kuntner, M AF Kralj-Fiser, Simona Gregoric, Matjaz Zhang, Shichang Li, Daiqin Kuntner, Matjaz TI Eunuchs are better fighters SO ANIMAL BEHAVIOUR LA English DT Article DE emasculation; genital amputation; Nephilengys malabarensis; Nephilidae; orb web spider; plugging; sexual cannibalism; sexual conflict ID SPIDER FRONTINELLA-PYRAMITELA; ORB-WEAVING SPIDER; SEXUAL CANNIBALISM; SPERM COMPETITION; DOILY SPIDER; EVOLUTIONARY CONSEQUENCES; GENITAL MUTILATION; NEPHILID SPIDERS; MALE SACRIFICE; ARANEAE AB Genital amputation, that is, genital damage or loss, seems maladaptive because it renders the amputee functionally sterile, but is nevertheless common in sexually dimorphic spiders. In these species, male genital amputation correlates with plugging of female genitals and with sexual cannibalism. Genital amputation in male spiders may be partial or full; the latter is known as the eunuch phenomenon. We tested two adaptive hypotheses about eunuch behaviour in an orb web spider, Nephilengys malabarensis: (1) the plugging hypothesis (i.e. broken male genitals (palps) effectively plug the female genitals) and (2) the better fighter hypothesis (i.e. eunuch males are better fighters than their intact rivals). By staging mating trials, we documented genital amputation (occurrence and frequency), sexual cannibalism and genital organ reuse, morphologically examined plugs to infer their effectiveness, and conducted a series of male-male contests to determine whether eunuch males were better fighters. Copulations always resulted in amputation of the palps: 87.5% of males became eunuchs directly during copulation and plugged females, while 12.5% of males first partially damaged the palps and then severed them after copulation. Sexual cannibalism and plugging effectiveness both reached 75%. Eunuchs guarded females, were highly aggressive and active, and initiated and won contests more often, whereas intact males and half-eunuchs showed significantly lower levels of guarding behaviour, aggression and general activity. Thus, both hypotheses are supported and we conclude that the eunuch phenomenon is adaptive. (C) 2011 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Kralj-Fiser, Simona; Gregoric, Matjaz; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, SI-1001 Ljubljana, Slovenia. [Kralj-Fiser, Simona] Univ Hamburg, Biozentrum Grindel, Hamburg, Germany. [Zhang, Shichang; Li, Daiqin] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Li, Daiqin] Hubei Univ, Coll Life Sci, Wuhan, Peoples R China. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM kuntner@gmail.com RI Li, Daiqin/D-6922-2013 OI Li, Daiqin/0000-0001-8269-7734 FU Slovenian Research Agency [J1-2063]; Raffles Museum for Biodiversity; National University of Singapore; Singapore Ministry of Education AcRF [R-154-000-355-112]; Humboldt fellowship for postdoctoral researchers FX We thank Mark Elgar and an anonymous referee for their most helpful reviews, Jutta Schneider and Mariella Herberstein for commenting on our experimental design, and Ingi Agnarsson for commenting on the manuscript. Cene Fiser and Irena Kuntner kindly offered logistic help and Singapore National Parks supplied the research and collection permits. This work was funded by grants to M.K. from the Slovenian Research Agency (J1-2063) and the Raffles Museum for Biodiversity Research Fellowship, National University of Singapore, and a grant (R-154-000-355-112) to D.L. from the Singapore Ministry of Education AcRF. S.K.F. was supported by a Humboldt fellowship for postdoctoral researchers. NR 49 TC 19 Z9 20 U1 1 U2 21 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD MAY PY 2011 VL 81 IS 5 BP 933 EP 939 DI 10.1016/j.anbehav.2011.02.010 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 746AV UT WOS:000289214300006 ER PT J AU Abramson, A Kenney, JDP Crowl, HH Chung, A van Gorkom, JH Vollmer, B Schiminovich, D AF Abramson, Anne Kenney, Jeffrey D. P. Crowl, Hugh H. Chung, Aeree van Gorkom, J. H. Vollmer, Bernd Schiminovich, David TI CAUGHT IN THE ACT: STRONG, ACTIVE RAM PRESSURE STRIPPING IN VIRGO CLUSTER SPIRAL NGC 4330 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: individual (NGC 4330); galaxies: interactions; galaxies: ISM; galaxies: spiral; galaxies: structure ID STELLAR POPULATION SYNTHESIS; MORPHOLOGY-DENSITY RELATION; STAR-FORMATION RATES; H-ALPHA; DISC GALAXIES; STARBURST GALAXIES; S0 GALAXIES; EVOLUTION; GAS; TRANSFORMATION AB We present a multi-wavelength study of NGC 4330, a highly inclined spiral galaxy in the Virgo Cluster which is a clear example of strong, ongoing intracluster medium-interstellar medium (ICM-ISM) ram pressure stripping. The Hi has been removed from well within the undisturbed old stellar disk, to 50%-65% of R-25. Multi-wavelength data (WIYN BVR-H alpha, Very Large Array 21 cm Hi and radio continuum, and Galaxy Evolution Explorer NUV and FUV) reveal several one-sided extraplanar features likely caused by ram pressure at an intermediate disk-wind angle. At the leading edge of the interaction, the H alpha and dust extinction curve sharply out of the disk in a remarkable and distinctive "upturn" feature that may be generally useful as a diagnostic indicator of active ram pressure. On the trailing side, the ISM is stretched out in a long tail which contains 10% of the galaxy's total Hi emission, 6%-9% of its NUV-FUV emission, but only 2% of the H alpha. The centroid of the Hi tail is downwind of the UV/H alpha tail, suggesting that the ICM wind has shifted most of the ISM downwind over the course of the past 10-300 Myr. Along the major axis, the disk is highly asymmetric in the UV, but more symmetric in H alpha and Hi, also implying recent changes in the distributions of gas and star formation. The UV-optical colors indicate very different star formation histories for the leading and trailing sides of the galaxy. On the leading side, a strong gradient in the UV-optical colors of the gas-stripped disk suggests that it has taken 200-400 Myr to strip the gas from a radius of >8 to 5 kpc, but on the trailing side there is no age gradient. All our data suggest a scenario in which NGC 4330 is falling into the cluster center for the first time and has experienced a significant increase in ram pressure over the last 200-400 Myr. Many of the UV-bright stars that form outside the thin disk due to ram pressure will ultimately produce stellar thick disk and halo components with characteristic morphologies and age distributions distinct from those produced by gravitational interactions. C1 [Abramson, Anne; Kenney, Jeffrey D. P.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Crowl, Hugh H.; van Gorkom, J. H.; Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Chung, Aeree] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Chung, Aeree] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Vollmer, Bernd] Observ Astron, F-67000 Strasbourg, France. RP Abramson, A (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM anne.abramson@yale.edu; jeff.kenney@yale.edu; hugh@astro.columbia.edu; achung@yonsei.ac.kr; jvangork@astro.columbia.edu; bvollmer@astro.u-strasbg.fr; ds@astro.columbia.edu RI Abramson, Anne/J-3014-2015 FU National Science Foundation [0607643] FX This work was partially supported by the National Science Foundation under grant no. 0607643 to Columbia University. GALEX is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d' Etudes Spatiales of France and the Korean Ministry of Science and Technology. We warmly thank the referee for a helpful and thorough report. NR 69 TC 54 Z9 54 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 MAY PY 2011 VL 141 IS 5 AR 164 DI 10.1088/0004-6256/141/5/164 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 746JB UT WOS:000289240800023 ER PT J AU Di Stefano, R AF Di Stefano, R. TI TRANSITS AND LENSING BY COMPACT OBJECTS IN THE KEPLER FIELD: DISRUPTED STARS ORBITING BLUE STRAGGLERS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; blue stragglers; gravitational lensing: micro; white dwarfs ID COMMON ENVELOPE EVOLUTION; X-RAY BINARIES; WHITE-DWARF; MASS; PLANETS; PERTURBATIONS; ULTRACOOL; REGULUS; CURVES AB Kepler's first major discoveries are two hot (T > 10,000 K) small-radius objects orbiting stars in its field. A viable hypothesis is that these are the cores of stars that have each been eroded or disrupted by a companion star. The companion, which is the star monitored today, is likely to have gained mass from its now-defunct partner and can be considered to be a blue straggler. KOI-81 is almost certainly the product of stable mass transfer; KOI-74 may be as well, or it may be the first clear example of a blue straggler created through three-body interactions. We show that mass-transfer binaries are common enough that Kepler should discover similar to 1000 white dwarfs orbiting main-sequence stars. Most of these, like KOI-74 and KOI-81, will be discovered through transits, but many will be discovered through a combination of gravitational lensing and transits, while lensing will dominate for a subset. In fact, some events caused by white dwarfs will have the appearance of "anti-transits"-i.e., short-lived enhancements in the amount of light received from the monitored star. Lensing and other mass-measurement methods provide a way to distinguish white dwarf binaries from planetary systems. This is important for the success of Kepler's primary mission, in light of the fact that white dwarf radii are similar to the radii of terrestrial planets, and that some white dwarfs will have orbital periods that place them in the habitable zones of their stellar companions. By identifying transiting and/or lensing white dwarfs, Kepler will conduct pioneering studies of white dwarfs and of the end states of mass transfer. It may also identify orbiting neutron stars or black holes. The calculations inspired by the discovery of KOI-74 and KOI-81 have implications for ground-based wide-field surveys as well as for future space-based surveys. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [AST-0708924, AST-0908878]; CfA FX It is a pleasure to thank Alison J. Farmer, Robert J. Harris, David Latham, Hagai Perets, Darin Ragozzine, Jason Rowe, Kailash Sahu, Guillermo Torres, and participants in CfA's "exoplanet pizza lunch" for useful discussions. This work was supported in part by NSF under AST-0708924 and AST-0908878, and by a research and development grant from the CfA. NR 35 TC 7 Z9 7 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 MAY PY 2011 VL 141 IS 5 AR 142 DI 10.1088/0004-6256/141/5/142 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 746JB UT WOS:000289240800001 ER PT J AU Hartman, JD Bakos, GA Noyes, RW Sipocz, B Kovacs, G Mazeh, T Shporer, A Pal, A AF Hartman, J. D. Bakos, G. A. Noyes, R. W. Sipocz, B. Kovacs, G. Mazeh, T. Shporer, A. Pal, A. TI A PHOTOMETRIC VARIABILITY SURVEY OF FIELD K AND M DWARF STARS WITH HATNet SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; stars: fundamental parameters; stars: late-type; stars: low-mass; stars: rotation; techniques: photometric ID LOW-MASS STARS; LOWER MAIN-SEQUENCE; DIGITAL SKY SURVEY; DETACHED ECLIPSING BINARIES; TREND FILTERING ALGORITHM; STELLAR EVOLUTION MODELS; OPEN-CLUSTER; VARIABLE-STARS; ABSOLUTE DIMENSIONS; MONITOR PROJECT AB Using light curves from the HATNet survey for transiting extrasolar planets we investigate the optical broadband photometric variability of a sample of 27, 560 field K and M dwarfs selected by color and proper motion (V - K greater than or similar to 3.0, mu > 30 mas yr(-1), plus additional cuts in J - H versus H - K-S and on the reduced proper motion). We search the light curves for periodic variations and for large-amplitude, long-duration flare events. A total of 2120 stars exhibit potential variability, including 95 stars with eclipses and 60 stars with flares. Based on a visual inspection of these light curves and an automated blending classification, we select 1568 stars, including 78 eclipsing binaries (EBs), as secure variable star detections that are not obvious blends. We estimate that a further similar to 26% of these stars may be blends with fainter variables, though most of these blends are likely to be among the hotter stars in our sample. We find that only 38 of the 1568 stars, including five of the EBs, have previously been identified as variables or are blended with previously identified variables. One of the newly identified EBs is 1RXS J154727.5+450803, a known P = 3.55 day, late M-dwarf SB2 system, for which we derive preliminary estimates for the component masses and radii of M-1 = M-2 = 0.258+/-0.008 M-circle dot and R-1 = R-2 = 0.289+/-0.007 R-circle dot. The radii of the component stars are larger than theoretical expectations if the system is older than similar to 200 Myr. The majority of the variables are heavily spotted BY Dra-type stars for which we determine rotation periods. Using this sample, we investigate the relations between period, color, age, and activity measures, including optical flaring, for K and M dwarfs, finding that many of the well-established relations for F, G, and K dwarfs continue into the M dwarf regime. We find that the fraction of stars that is variable with peak-to-peak amplitudes greater than 0.01 mag increases exponentially with the V - K-S color such that approximately half of field dwarfs in the solar neighborhood with M less than or similar to 0.2 M-circle dot are variable at this level. Our data hint at a change in the rotation-activity-age connection for stars with M less than or similar to 0.25M(circle dot). C1 [Hartman, J. D.; Bakos, G. A.; Noyes, R. W.; Sipocz, B.; Pal, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sipocz, B.; Pal, A.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. [Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary. [Mazeh, T.; Shporer, A.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. RP Hartman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Hartman, Joel/0000-0001-8732-6166 FU NASA [NNG04GN74G, NNX08AF23G]; SAO IRD grants; NSF [AST-0702843]; Hungarian Scientific Research Foundation [K-81373]; ISRAEL SCIENCE FOUNDATION [655/07]; U.S. Government [NAG W-2166] FX We thank Lev Or-Tal for calculating the upper limit to the eccentricity for the eclipsing binary 1RXS J154727.5+450803. HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR&D grants. G.A.B. acknowledges support from the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843). G. K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. T. M. acknowledges support from the ISRAEL SCIENCE FOUNDATION (grant no. 655/07). 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. This research has made use of data obtained from or software provided by the US National Virtual Observatory, which is sponsored by the National Science Foundation. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 115 TC 62 Z9 63 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 MAY PY 2011 VL 141 IS 5 AR 166 DI 10.1088/0004-6256/141/5/166 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 746JB UT WOS:000289240800025 ER PT J AU Richards, GT Kruczek, NE Gallagher, SC Hall, PB Hewett, PC Leighly, KM Deo, RP Kratzer, RM Shen, Y AF Richards, Gordon T. Kruczek, Nicholas E. Gallagher, S. C. Hall, Patrick B. Hewett, Paul C. Leighly, Karen M. Deo, Rajesh P. Kratzer, Rachael M. Shen, Yue TI UNIFICATION OF LUMINOUS TYPE 1 QUASARS THROUGH CIV EMISSION SO ASTRONOMICAL JOURNAL LA English DT Article DE line: profiles; quasars: absorption lines; quasars: emission lines; quasars: general; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; BROAD-ABSORPTION-LINE; X-RAY-PROPERTIES; RADIO-QUIET QUASARS; BLACK-HOLE MASS; SPECTRAL ENERGY-DISTRIBUTIONS; OPTICALLY SELECTED QUASARS; 7TH DATA RELEASE; EDDINGTON RATIO AB Using a sample of similar to 30,000 quasars from the 7th Data Release of the Sloan Digital Sky Survey, we explore the range of properties exhibited by high-ionization, broad emission lines, such as CIV lambda 1549. Specifically, we investigate the anti-correlation between continuum luminosity and emission-line equivalent width (the Baldwin Effect (BEff)) and the "blueshifting" of the high-ionization emission lines with respect to low-ionization emission lines. Employing improved redshift determinations from Hewett & Wild, the blueshift of the CIV emission line is found to be nearly ubiquitous, with a mean shift of similar to 810 km s(-1) for radio-quiet (RQ) quasars and similar to 360 km s(-1) for radio-loud (RL) quasars. The BEff is present in both RQ and RL samples. We consider these phenomena within the context of an accretion disk-wind model that is modulated by the nonlinear correlation between ultraviolet and X-ray continuum luminosity. Composite spectra are constructed as a function of CIV emission-line properties in an attempt to reveal empirical relationships between different line species and the continuum. Within a two-component disk+wind model of the broad emission-line region (BELR), where the wind filters the continuum seen by the disk component, we find that RL quasars are consistent with being dominated by the disk component, while broad absorption line quasars are consistent with being dominated by the wind component. Some RQ objects have emission-line features similar to RL quasars; they may simply have insufficient black hole (BH) spin to form radio jets. Our results suggest that there could be significant systematic errors in the determination of L-bol and BH mass that make it difficult to place these findings in a more physical context. However, it is possible to classify quasars in a paradigm where the diversity of BELR parameters is due to differences in an accretion disk wind between quasars (and over time); these differences are underlain primarily by the spectral energy distribution, which ultimately must be tied to BH mass and accretion rate. C1 [Richards, Gordon T.; Kruczek, Nicholas E.; Deo, Rajesh P.; Kratzer, Rachael M.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Gallagher, S. C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Hall, Patrick B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Hewett, Paul C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Leighly, Karen M.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Richards, GT (reprint author), Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA. FU Alfred P. Sloan Research Fellowship; NASA [07-ADP07-0035]; STFC; NSERC; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX G.T.R. acknowledges support from an Alfred P. Sloan Research Fellowship and NASA grant 07-ADP07-0035. G.T.R. thanks Daniel Proga and Michael Eracleous for fruitful discussions. P.C.H. acknowledges support from the STFC-funded Galaxy Formation and Evolution programme at the Institute of Astronomy. P.B.H. is supported by NSERC. 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 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 (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 119 TC 125 Z9 125 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2011 VL 141 IS 5 AR 167 DI 10.1088/0004-6256/141/5/167 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 746JB UT WOS:000289240800026 ER PT J AU Stefanik, RP Torres, G Latham, DW Landsman, W Craig, N Murrett, J AF Stefanik, Robert P. Torres, Guillermo Latham, David W. Landsman, Wayne Craig, Nathaniel Murrett, James TI OBSERVATIONS AND ORBITAL ANALYSIS OF THE GIANT WHITE DWARF BINARY SYSTEM HR 5692 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; methods: data analysis; stars: individual (HR 5692); techniques: spectroscopic; white dwarfs ID INTERMEDIATE ASTROMETRIC DATA; RADIAL-VELOCITIES; SPECTROSCOPIC BINARIES; BARIUM STARS; S STARS; MASS; CATALOG; EXTINCTION; ISOCHRONES; SIRIUS AB We report spectroscopic observations of the red giant star HR5692, previously known to be a binary system both from other spectroscopic work and from deviations in the astrometric motion detected by the Hipparcos satellite. Earlier International Ultraviolet Explorer (IUE) observations had shown the presence of a hot white dwarf companion to the giant primary. We have combined our radial velocity observations with other existing measurements and with the Hipparcos intermediate astrometric data to determine a complete astrometric-spectroscopic orbital solution, providing the inclination angle for the first time. We also determine an improved parallax for the system of 10.12 +/- 0.67 mas. We derive the physical properties of the primary, and with an estimate of its mass from stellar evolution models (1.84 +/- 0.40M(circle dot)), we infer the mass of the white dwarf companion to be M-WD = 0.59 +/- 0.12M(circle dot). An analysis of an IUE white dwarf spectrum, using our parallax, yields T-eff = 30,400 +/- 780 K, log g = 8.25 +/- 0.15, and a mass M-WD = 0.79 +/- 0.09M(circle dot), in marginal agreement with the dynamical mass. C1 [Stefanik, Robert P.; Torres, Guillermo; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Landsman, Wayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Craig, Nathaniel; Murrett, James] Harvard Univ, Cambridge, MA 02138 USA. RP Stefanik, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rstefanik@cfa.harvard.edu FU NSF [AST-0708229, AST-1007992]; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We thank Michael Calkins, Joe Caruso, Gil Esquerdo, and Joe Zajac for obtaining many of the spectroscopic observations used here. We also thank I. Hubeny for his assistance with the TLUSTY code. G. T. acknowledges partial support for this work from NSF grants AST-0708229 and AST-1007992. This research has made use of the SIMBAD database and the VizieR catalog access tool, both operated at CDS, Strasbourg, France, of NASA's Astrophysics Data System Abstract Service, and of data products from the Two Micron All Sky Survey (2MASS), 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. 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. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 56 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2011 VL 141 IS 5 AR 144 DI 10.1088/0004-6256/141/5/144 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 746JB UT WOS:000289240800003 ER PT J AU Berger, JP Monnier, JD Millan-Gabet, R Renard, S Pedretti, E Traub, W Bechet, C Benisty, M Carleton, N Haguenauer, P Kern, P Labeye, P Longa, F Lacasse, M Malbet, F Perraut, K Ragland, S Schloerb, P Schuller, PA Thiebaut, E AF Berger, J. -P. Monnier, J. D. Millan-Gabet, R. Renard, S. Pedretti, E. Traub, W. Bechet, C. Benisty, M. Carleton, N. Haguenauer, P. Kern, P. Labeye, P. Longa, F. Lacasse, M. Malbet, F. Perraut, K. Ragland, S. Schloerb, P. Schuller, P. A. Thiebaut, E. TI First astronomical unit scale image of the GW Orionis triple system Direct detection of a new stellar companion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: general; stars: variables: T Tauri; Herbig Ae/Be; accretion, accretion disks; techniques: interferometric ID INTERFEROMETRY; ACCRETION; EVOLUTION; DISTANCE; NEBULA; TRACKS; STARS; IOTA AB Context. Young and close multiple systems are unique laboratories to probe the initial dynamical interactions between forming stellar systems and their dust and gas environment. Their study is a key building block to understanding the high frequency of main-sequence multiple systems. However, the number of detected spectroscopic young multiple systems that allow dynamical studies is limited. GW Orionis is one such system. It is one of the brightest young T Tauri stars and is surrounded by a massive disk. Aims. Our goal is to probe the GW Orionis multiplicity at angular scales at which we can spatially resolve the orbit. Methods. We used the IOTA/IONIC3 interferometer to probe the environment of GW Orionis with an astronomical unit resolution in 2003, 2004, and 2005. By measuring squared visibilities and closure phases with a good UV coverage we carry out the first image reconstruction of GW Ori from infrared long-baseline interferometry. Results. We obtained the first infrared image of a T Tauri multiple system with astronomical unit resolution. We show that GW Orionis is a triple system, resolve for the first time the previously known inner pair (separation rho similar to 1.4 AU) and reveal a new more distant component (GW Ori C) with a projected separation of similar to 8 AU with direct evidence of motion. Furthermore, the nearly equal (2: 1) H-band flux ratio of the inner components suggests that either GW Ori B is undergoing a preferential accretion event that increases its disk luminosity or that the estimate of the masses has to be revisited in favour of a more equal mass-ratio system that is seen at lower inclination. Conclusions. Accretion disk models of GW Ori will need to be completely reconsidered because of this outer companion C and the unexpected brightness of companion B. C1 [Berger, J. -P.; Haguenauer, P.] European So Observ, Santiago 19, Chile. [Berger, J. -P.; Renard, S.; Kern, P.; Longa, F.; Malbet, F.; Perraut, K.] Univ Grenoble 1, IPAG, CNRS UMR 5571, F-38041 Grenoble, France. [Monnier, J. D.] Univ Michigan, Ann Arbor, MI 48109 USA. [Millan-Gabet, R.] CALTECH, Pasadena, CA 91125 USA. [Pedretti, E.] Univ St Andrews, St Andrews KY16 9AJ, Fife, Scotland. [Traub, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Benisty, M.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Carleton, N.; Lacasse, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Labeye, P.] CEA DRT LETI, F-38054 Grenoble, France. [Ragland, S.] WM Keck Observ, Kamuela, HI 96743 USA. [Schloerb, P.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Schuller, P. A.] Univ Paris 11, CNRS UMR 8617, IAS, F-91405 Orsay, France. [Bechet, C.; Thiebaut, E.] CRAL Observ Lyon, F-69561 St Genis Laval, France. RP Berger, JP (reprint author), European So Observ, Alonso de Cordova 3107 Vitacura,Casilla 19001, Santiago 19, Chile. EM jpberger@eso.org RI Bechet, Clementine/A-6828-2017 OI Bechet, Clementine/0000-0002-0885-3644 FU ASHRA; PNPS/INSU; Michelson fellowship program; CNRS; CNES FX This work was supported by ASHRA, PNPS/INSU, and Michelson fellowship program. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France and getCal software from the NASA Exoplanet Science Institute, Caltech. Bibliographic references were provided by the SAO/NASA Astrophysics Data System. IONIC-3 has been developed by LAOG and CEA-LETI, and funded by the CNRS and CNES. We thank Russel White, Lee Hartmann and S. Meimon for useful discussions. NR 18 TC 4 Z9 4 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 MAY PY 2011 VL 529 AR L1 DI 10.1051/0004-6361/201016219 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200002 ER PT J AU Fayolle, EC Oberg, KI Cuppen, HM Visser, R Linnartz, H AF Fayolle, E. C. Oeberg, K. I. Cuppen, H. M. Visser, R. Linnartz, H. TI Laboratory H2O:CO2 ice desorption data: entrapment dependencies and its parameterization with an extended three-phase model SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; methods: laboratory; methods: analytical; ISM: molecules ID AMORPHOUS SOLID WATER; INTERSTELLAR ICES; THERMAL-DESORPTION; SPECTROSCOPIC SURVEY; PROTOSTELLAR CORES; CO; N-2; MORPHOLOGY; SURFACES; STARS AB Context. Ice desorption affects the evolution of the gas-phase chemistry during the protostellar stage, and also determines the chemical composition of comets forming in circumstellar disks. From observations, most volatile species are found in H2O-dominated ices. Aims. The aim of this study is first to experimentally determine how entrapment of volatiles in H2O ice depends on ice thickness, mixture ratio and heating rate, and second, to introduce an extended three-phase model (gas, ice surface and ice mantle) to describe ice mixture desorption with a minimum number of free parameters. Methods. Thermal H2O:CO2 ice desorption is investigated in temperature programmed desorption experiments of thin (10-40 ML) ice mixtures under ultra-high vacuum conditions. Desorption is simultaneously monitored by mass spectrometry and reflection-absorption infrared spectroscopy. The H2O:CO2 experiments are complemented with selected H2O:CO, and H2O:CO2:CO experiments. The results are modeled with rate equations that connect the gas, ice surface and ice mantle phases through surface desorption and mantle-surface diffusion. Results. The fraction of trapped CO2 increases with ice thickness (10-32 ML) and H2O:CO2 mixing ratio (5:1-10:1), but not with one order of magnitude different heating rates. The fraction of trapped CO2 is 44-84% with respect to the initial CO2 content for the investigated experimental conditions. This is reproduced quantitatively by the extended three-phase model that is introduced here. The H2O:CO and H2O:CO2:CO experiments are consistent with the H2O:CO2 desorption trends, suggesting that the model can be used for other ice species found in the interstellar medium to significantly improve the parameterization of ice desorption. C1 [Fayolle, E. C.; Cuppen, H. M.; Linnartz, H.] Leiden Univ, Leiden Observ, Sackler Lab Astrophys, NL-2300 RA Leiden, Netherlands. [Oeberg, K. 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. EM fayolle@strw.leidenuniv.nl RI Visser, Ruud/J-8574-2012; Cuppen, Herma/F-9729-2015; OI Cuppen, Herma/0000-0003-4397-0739; Fayolle, Edith/0000-0001-8109-5256 FU NASA [NAS 5-26555]; NOVA; Netherlands Research School for Astronomy; NASA through Space Telescope Science Institute FX This work has greatly benefitted from discussions with Ewine van Dishoeck and comments from an anonymous referee. Funding is provided by NOVA, the Netherlands Research School for Astronomy. Support for K. I.. 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. NR 29 TC 36 Z9 36 U1 1 U2 14 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2011 VL 529 AR A74 DI 10.1051/0004-6361/201016121 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200082 ER PT J AU Fontani, F Palau, A Caselli, P Sanchez-Monge, A Butler, MJ Tan, JC Jimenez-Serra, I Busquet, G Leurini, S Audard, M AF Fontani, F. Palau, A. Caselli, P. Sanchez-Monge, A. Butler, M. J. Tan, J. C. Jimenez-Serra, I. Busquet, G. Leurini, S. Audard, M. TI Deuteration as an evolutionary tracer in massive-star formation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: clouds; ISM: molecules; radio lines: ISM ID INFRARED DARK CLOUDS; PROTOCLUSTER IRAS 05358+3543; DENSE INTERSTELLAR CLOUDS; DEUTERIUM FRACTIONATION; INITIAL CONDITIONS; FORMING REGIONS; STELLAR OBJECTS; MOLECULAR-IONS; CORES; N2H+ AB Context. Theory predicts, and observations confirm, that the column density ratio of a molecule containing D to its counterpart containing H can be used as an evolutionary tracer in the low-mass star formation process. Aims. Since it remains unclear if the high-mass star formation process is a scaled-up version of the low-mass one, we investigated whether the relation between deuteration and evolution can be applied to the high-mass regime. Methods. With the IRAM-30 m telescope, we observed rotational transitions of N2D+ and N2H+ and derived the deuterated fraction in 27 cores within massive star-forming regions understood to represent different evolutionary stages of the massive-star formation process. Results. The abundance of N2D+ is higher at the pre-stellar/cluster stage, then drops during the formation of the protostellar object(s) as in the low-mass regime, remaining relatively constant during the ultra-compact HII region phase. The objects with the highest fractional abundance of N2D+ are starless cores with properties very similar to typical pre-stellar cores of lower mass. The abundance of N2D+ is lower in objects with higher gas temperatures as in the low-mass case but does not seem to depend on gas turbulence. Conclusions. Our results indicate that the N2D+-to-N2H+ column density ratio can be used as an evolutionary indicator in both low-and high-mass star formation, and that the physical conditions influencing the abundance of deuterated species likely evolve similarly during the processes that lead to the formation of both low-and high-mass stars. C1 [Fontani, F.] ESO, D-85748 Garching, Germany. [Fontani, F.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Palau, A.] Inst Ciencies Espai CSIC IEEC, Bellaterra 08193, Spain. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Sanchez-Monge, A.; Busquet, G.] Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol IEEC UB, E-08028 Barcelona, Spain. [Butler, M. J.; Tan, J. C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Tan, J. C.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Busquet, G.] INAF Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Leurini, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Audard, M.] Univ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Audard, M.] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland. RP Fontani, F (reprint author), ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM fontani@iram.fr OI Fontani, Francesco/0000-0003-0348-3418 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); European Community [FP7/2007-2013, 229517]; Spanish MICINN [AYA2008-06189-C03]; FEDER; European Social Fund; Italian Space Agency (ASI) [ASI-I/005/07/1]; Swiss National Science Foundation [PP002-110504, P00P2-130188] 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-30 m telescope staff for their help during the observations. We thank the anonymous Referee for his/her comments, which significantly improved the work. F. F. has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 229517. A. P., A.S.-M. and G. B. are supported by the Spanish MICINN grant AYA2008-06189-C03 (co-funded with FEDER funds). A. P. is supported by JAEDoc CSIC fellowship co-funded with the European Social Fund. G. B. is funded by the Italian Space Agency (ASI) with contract ASI-I/005/07/1. M. A. acknowledges support from the Swiss National Science Foundation (grants PP002-110504 and PP00P2-130188) NR 46 TC 49 Z9 49 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2011 VL 529 AR L7 DI 10.1051/0004-6361/201116631 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200008 ER PT J AU Iwasawa, K Sanders, DB Teng, SH U, V Armus, L Evans, AS Howell, JH Komossa, S Mazzarella, JM Petric, AO Surace, JA Vavilkin, T Veilleux, S Trentham, N AF Iwasawa, K. Sanders, D. B. Teng, S. H. U, V. Armus, L. Evans, A. S. Howell, J. H. Komossa, S. Mazzarella, J. M. Petric, A. O. Surace, J. A. Vavilkin, T. Veilleux, S. Trentham, N. TI C-GOALS: Chandra observations of a complete sample of luminous infrared galaxies from the IRAS Revised Bright Galaxy Survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared: galaxies; X-rays: galaxies; galaxies: active; galaxies: starburst ID ACTIVE GALACTIC NUCLEUS; X-RAY-EMISSION; MU-M SPECTROSCOPY; SUPERMASSIVE BLACK-HOLES; FORMATION RATE INDICATOR; SPITZER-SPACE-TELESCOPE; SKY LIRG SURVEY; XMM-NEWTON; OPTICAL SPECTROSCOPY; STARBURST GALAXY AB We present X-ray data for a complete sample of 44 luminous infrared galaxies (LIRGs), obtained with the Chandra X-ray Observatory. These are the X-ray observations of the high luminosity portion of the Great Observatory All-sky LIRG Survey (GOALS), which includes the most luminous infrared selected galaxies, log (L-ir/L-circle dot) >= 11.73, in the local universe, z <= 0.088. X-rays were detected from 43 out of 44 objects, and their arcsec-resolution images, spectra, and radial brightness distributions are presented. With a selection by hard X-ray colour and the 6.4 keV iron line, AGN are found in 37% of the objects, with higher luminosity sources more likely to contain an AGN. These AGN also tend to be found in late-stage mergers. The AGN fraction would increase to 48% if objects with [Ne v]lambda 14.3 mu m detection are included. Double AGN are clearly detected only in NGC 6240 among 24 double/triple systems. Other AGN are found either in single nucleus objects or in one of the double nuclei at similar rates. Objects without conventional X-ray signatures of AGN appear to be hard X-ray quiet, relative to the X-ray to far-IR correlation for starburst galaxies, as discussed elsewhere. Most objects also show extended soft X-ray emission, which is likely related to an outflow from the nuclear region, with a metal abundance pattern suggesting enrichment by core collapse supernovae, as expected for a starburst. C1 [Iwasawa, K.] Univ Barcelona IEEC UB, ICREA, Barcelona 08028, Spain. [Iwasawa, K.] Univ Barcelona IEEC UB, ICC, Barcelona 08028, Spain. [Sanders, D. B.; U, V.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Teng, S. H.; Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [U, V.] Harvard Smithsonian Ctr Astrophys, SAO, Cambridge, MA 02138 USA. [Armus, L.; Howell, J. H.; Petric, A. O.; Surace, J. A.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Evans, A. S.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Evans, A. S.] NRAO, Charlottesville, VA 22903 USA. [Komossa, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Mazzarella, J. M.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Vavilkin, T.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Trentham, N.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Iwasawa, K (reprint author), Univ Barcelona IEEC UB, ICREA, Marti & Franques 1, Barcelona 08028, Spain. EM kazushi.iwasawa@icc.ub.edu OI Mazzarella, Joseph/0000-0002-8204-8619 FU National Aeronautics and Space Administration; Chandra [GO6-7098X, GO7-8108A]; SAO FX This research has made use of software packages CIAO provided by the Chandra X-ray Center (CXC) and FTOOLS provided by NASAS's HEASARC. This research has also made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The Chandra data archive is maintained by the Chandra X-ray Center at the Smithsonian Astrophysical Observatory. D. B. S. acknowledges support from Chandra grants GO6-7098X and GO7-8108A. Vivian U also acknowledges support from a NASA Jenkins Predoctoral Fellowship and a SAO Harvard-Smithsonian Predoctoral Fellowship. We thank the referee for helpful comments. NR 103 TC 52 Z9 52 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2011 VL 529 AR A106 DI 10.1051/0004-6361/201015264 PG 50 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200114 ER PT J AU Zhao, W Hong, XY An, T Jiang, DR Zhao, JH Gurvits, LI Yang, J AF Zhao, W. Hong, X. -Y. An, T. Jiang, D. -R. Zhao, J. -H. Gurvits, L. I. Yang, J. TI Radio structure of the blazar 1156+295 with sub-pc resolution SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: jets; galaxies: kinematics and dynamics; quasars: individual: 1156+295; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; GAMMA-RAY SOURCES; GHZ VLBI SURVEY; RELATIVISTIC JETS; EGRET CATALOG; BL-LACERTAE; BLACK-HOLE; MODEL; MULTIFREQUENCY; VARIABILITY AB Aims. 1156+295 is a flat-spectrum quasar that is loud at both radio and gamma-ray wavelengths. Previous observations of the source revealed a radio morphology on pc to kpc scales consistent with a helical jet model. We carried out VLBA observations at centimeter and millimeter wavelengths to study the structure of the innermost jet and understand the relation between the helical structure and astrophysical processes in the central engine. Methods. The source 1156+295 was observed with the VLBA at 86, 43, and 15 GHz at four epochs from 10 May 2003 to 13 March 2005. The observations were carried out in a full polarization mode. The highest resolution of the observations is 0.08 mas (similar to 0.5 pc) at 86 GHz. Results. A core-jet structure with six jet components is identified in 1156+295. Three jet components are detected for the first time. The apparent transverse velocities of the six jet components derived from proper motion measurements range between 3.6 c and 11.6 c, suggesting that highly relativistic jet plasma moves in the direction close to the line of sight. The overall jet has an oscillating morphology with multiple curvatures on pc scales, which might be indicative of a helical pattern. Models of a helical jet are discussed in the context of both Kelvin-Helmholtz (K-H) instability and jet precession. The K-H instability model is in closer agreement with the observed data. Conclusions. The overall radio structure on scales from sub-pc to kpc appears to be fitted with a hydrodynamic model in the fundamental helical mode of Kelvin-Helmholtz (K-H) instability. This helical mode with an initial characteristic wavelength of lambda(0) = 0.2 pc is excited at the base of the jet on the scale of 0.005 pc (or 10(3)R(s), the typical size of the broad line region of a supermassive black hole of 4.3 x 10(8) M-circle dot). A precessing jet model can also fit the observed jet structure on scales of between 10 pc and 300 pc. However, with the precessing jet model, additional astrophysical processes may be required to explain the bendings of the inner jet structure (1 to 10 pc) and re-collimation of the large-scale jet outflow (>300 pc). C1 [Zhao, W.; Hong, X. -Y.; An, T.; Jiang, D. -R.] CAS, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Zhao, W.] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Zhao, J. -H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gurvits, L. I.; Yang, J.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Gurvits, L. I.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan. RP Zhao, W (reprint author), CAS, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China. EM weizhao@shao.ac.cn RI he, shuyi/K-2082-2014 FU National Natural Science Foundation of PR China [NSFC10473018, 10503008]; Ministry of Science and Technology of China [2009CB824900, 2009CB24903]; Chinese Academy of Sciences; University of Michigan; National Science Foundation [AST-0607523, AST99-8154] FX W.Z., X.Y.H., and T. A. are grateful for the support from the National Natural Science Foundation of PR China (NSFC10473018, 10503008), the Ministry of Science and Technology of China (Grant No. 2009CB824900/2009CB24903) and the eScience program "Fast eVLBI Imaging and dUT1 Determination" of the Chinese Academy of Sciences. W.Z. thanks Giuseppe Cimo for the help of calibration for the polarization VLBA data. W.Z. thanks JIVE for the hospitality during her visit to the Netherlands for the data reduction in 2007. The VLBA and VLA are instruments of the National Radio Astronomy Observatory, a facility of the US National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009, AJ, 137, 3718). This research uses the 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. The Owens Valley Radio Observatory Millimeter Array is supported in part of the National Science Foundation NSF Grant AST99-8154. Thanks are given to the anonymous referee for useful comments and suggestions, and Claire Halliday (language editor of A&A) for proof-reading of the text. NR 50 TC 4 Z9 4 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2011 VL 529 AR A113 DI 10.1051/0004-6361/201016192 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 750OG UT WOS:000289557200121 ER PT J AU Andrews, SM Wilner, DJ Espaillat, C Hughes, AM Dullemond, CP McClure, MK Qi, CH Brown, JM AF Andrews, Sean M. Wilner, David J. Espaillat, Catherine Hughes, A. M. Dullemond, C. P. McClure, M. K. Qi, Chunhua Brown, J. M. TI RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planet-disk interactions; planets and satellites: formation; protoplanetary disks; submillimeter: planetary systems ID T-TAURI STARS; GIANT PLANET FORMATION; MAIN-SEQUENCE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; SPITZER C2D SURVEY; HERBIG AE/BE STARS; SUBMILLIMETER CONTINUUM FLUX; YOUNG STELLAR OBJECTS; SELF-SHADOWED DISKS; OPHIUCHI DARK CLOUD AB Circumstellar disks are thought to experience a rapid "transition" phase in their evolution that can have a considerable impact on the formation and early development of planetary systems. We present new and archival high angular resolution (0 ''.3 approximate to 40-75 AU) Submillimeter Array (SMA) observations of the 880 mu m (340 GHz) dust continuum emission from 12 such transition disks in nearby star-forming regions. In each case, we directly resolve a dust-depleted disk cavity around the central star. Using two-dimensional Monte Carlo radiative transfer calculations, we interpret these dust disk structures in a homogeneous, parametric model framework by reproducing their SMA continuum visibilities and spectral energy distributions. The cavities in these disks are large (R-cav = 15-73 AU) and substantially depleted of small (similar to mu m-sized) dust grains, although their mass contents are still uncertain. The structures of the remnant material at larger radii are comparable to normal disks. We demonstrate that these large cavities are relatively common among the millimeter-bright disk population, comprising at least 1 in 5 (20%) of the disks in the bright half (and >= 26% of the upper quartile) of the millimeter luminosity (disk mass) distribution. Utilizing these results, we assess some of the physical mechanisms proposed to account for transition disk structures. As has been shown before, photoevaporation models do not produce the large cavity sizes, accretion rates, and disk masses representative of this sample. A sufficient decrease of the dust optical depths in these cavities by particle growth would be difficult to achieve: substantial growth (to meter sizes or beyond) must occur in large (tens of AU) regions of low turbulence without also producing an abundance of small particles. Given those challenges, we suggest instead that the observations are most commensurate with dynamical clearing due to tidal interactions with low-mass companions-very young (similar to 1 Myr) brown dwarfs or giant planets on long-period orbits. C1 [Andrews, Sean M.; Wilner, David J.; Espaillat, Catherine; Qi, Chunhua; Brown, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, A. M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Dullemond, C. P.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [McClure, M. K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Espaillat, Catherine] NSF Astron & Astrophys, Arlington, VA USA. RP Andrews, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI McClure, Melissa/0000-0003-1878-327X; Dullemond, Cornelis/0000-0002-7078-5910 FU Smithsonian Institution; Academia Sinica FX We thank Karin Oberg, Sijme-Jan Paardekooper, and Aurelien Crida for beneficial conversations, and a referee for a thorough review that helped clarify the text. We are especially grateful to Adam Kraus, who kindly shared his results prior to publication. 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 244 TC 267 Z9 267 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 42 DI 10.1088/0004-637X/732/1/42 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500042 ER PT J AU Ballard, S Christiansen, JL Charbonneau, D Deming, D Holman, MJ A'Hearn, MF Wellnitz, DD Barry, RK Kuchner, MJ Livengood, TA Hewagama, T Sunshine, JM Hampton, DL Lisse, CM Seager, S Veverka, JF AF Ballard, Sarah Christiansen, Jessie L. Charbonneau, David Deming, Drake Holman, Matthew J. A'Hearn, Michael F. Wellnitz, Dennis D. Barry, Richard K. Kuchner, Marc J. Livengood, Timothy A. Hewagama, Tilak Sunshine, Jessica M. Hampton, Don L. Lisse, Carey M. Seager, Sara Veverka, Joseph F. TI A SEARCH FOR ADDITIONAL PLANETS IN FIVE OF THE EXOPLANETARY SYSTEMS STUDIED BY THE NASA EPOXI MISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: image processing; techniques: photometric ID TRANSIT LIGHT-CURVE; DEEP IMPACT MISSION; GIANT PLANET; KEPLER FIELD; HOT JUPITER; TRES-2; PARAMETERS; STAR; DYNAMICS; HAT-P-7B AB We present time series photometry and constraints on additional planets in five of the exoplanetary systems studied by the EPOCh (Extrasolar Planet Observation and Characterization) component of the NASA EPOXI mission: HAT-P-4, TrES-3, TrES-2, WASP-3, and HAT-P-7. We conduct a search of the high-precision time series for photometric transits of additional planets. We find no candidate transits with significance higher than our detection limit. From Monte Carlo tests of the time series using putative periods from 0.5 days to 7 days, we demonstrate the sensitivity to detect Neptune-sized companions around TrES-2, sub-Saturn-sized companions in the HAT-P-4, TrES-3, and WASP-3 systems, and Saturn-sized companions around HAT-P-7. We investigate in particular our sensitivity to additional transits in the dynamically favorable 3: 2 and 2: 1 exterior resonances with the known exoplanets: if we assume coplanar orbits with the known planets, then companions in these resonances with HAT-P-4b, WASP-3b, and HAT-P-7b would be expected to transit, and we can set lower limits on the radii of companions in these systems. In the nearly grazing exoplanetary systems TrES-3 and TrES-2, additional coplanar planets in these resonances are not expected to transit. However, we place lower limits on the radii of companions that would transit if the orbits were misaligned by 2 degrees.0 and 1 degrees.4 for TrES-3 and TrES-2, respectively. C1 [Ballard, Sarah; Charbonneau, David; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Christiansen, Jessie L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Deming, Drake; Barry, Richard K.; Kuchner, Marc J.; Livengood, Timothy A.; Hewagama, Tilak] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [A'Hearn, Michael F.; Wellnitz, Dennis D.; Hewagama, Tilak; Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Hampton, Don L.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Seager, Sara] MIT, Cambridge, MA 02139 USA. [Veverka, Joseph F.] Cornell Univ, Dept Space Sci, Ithaca, NY 14853 USA. RP Ballard, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sballard@cfa.harvard.edu RI Wellnitz, Dennis/B-4080-2012; Hewagama, T/C-8488-2012; Livengood, Timothy/C-8512-2012; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Charbonneau, David/0000-0002-9003-484X FU National Aeronautics and Space Administration [NNX08AB64A, NNX08AD05A] FX Support for this work was provided by the EPOXI Project of the National Aeronautics and Space Administration's Discovery Program via funding to the Goddard Space Flight Center, and to Harvard University via Co-operative Agreement NNX08AB64A, and to the Smithsonian Astrophysical Observatory via Co-operative Agreement NNX08AD05A. NR 33 TC 5 Z9 5 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 41 DI 10.1088/0004-637X/732/1/41 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500041 ER PT J AU Brodwin, M Stern, D Vikhlinin, A Stanford, SA Gonzalez, AH Eisenhardt, PR Ashby, MLN Bautz, M Dey, A Forman, WR Gettings, D Hickox, RC Jannuzi, BT Jones, C Mancone, C Miller, ED Moustakas, LA Ruel, J Snyder, G Zeimann, G AF Brodwin, M. Stern, D. Vikhlinin, A. Stanford, S. A. Gonzalez, A. H. Eisenhardt, P. R. Ashby, M. L. N. Bautz, M. Dey, A. Forman, W. R. Gettings, D. Hickox, R. C. Jannuzi, B. T. Jones, C. Mancone, C. Miller, E. D. Moustakas, L. A. Ruel, J. Snyder, G. Zeimann, G. TI X-RAY EMISSION FROM TWO INFRARED-SELECTED GALAXY CLUSTERS AT z > 1.4 IN THE IRAC SHALLOW CLUSTER SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (ISCS J1432.4+3250, ISCS J1438.1+3414); galaxies: distances and redshifts; galaxies: evolution ID DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; VELOCITY DISPERSION; COMA CLUSTER; MASS; TEMPERATURE; LUMINOSITY; TELESCOPE; COSMOLOGY; ROBUST AB We report the X-ray detection of two z > 1.4 infrared-selected galaxy clusters from the IRAC Shallow Cluster Survey (ISCS). We present new data from the Hubble Space Telescope and the W. M. Keck Observatory that spectroscopically confirm cluster ISCS J1432.4+3250 at z = 1.49, the most distant of 18 confirmed z > 1 clusters in the ISCS to date. We also present new spectroscopy for ISCS J1438.1+3414, previously reported at z = 1.41, and measure its dynamical mass. Clusters ISCS J1432.4+3250 and ISCS J1438.1+3414 are detected in 36 ks and 143 ks Chandra exposures at significances of 5.2 sigma and 9.7 sigma, from which we measure total masses of log (M-200,M-LX/M-circle dot) = 14.4 +/- 0.2 and 14.35(-0.11)(+0.14), respectively. The consistency of the X-ray and dynamical properties of these high-redshift clusters further demonstrates that the ISCS is robustly detecting massive clusters to at least z = 1.5. C1 [Brodwin, M.; Vikhlinin, A.; Ashby, M. L. N.; Forman, W. R.; Jones, C.; Snyder, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, D.; Eisenhardt, P. R.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stanford, S. A.; Zeimann, G.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Gonzalez, A. H.; Gettings, D.; Mancone, C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Bautz, M.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Hickox, R. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Brodwin, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Moustakas, Leonidas/0000-0003-3030-2360 FU Chandra X-Ray Observatory [SV4-74018, A31]; Smithsonian Astrophysical Observatory; NASA [G09-0150A, NAS 5-26555]; JPL/Caltech; NASA through Space Telescope Science Institute [11597, 11663]; W. M. Keck Foundation; U.S. Department of Energy [W-7405-ENG-48] FX This work is based, in part, on observations obtained with the Chandra X-Ray Observatory under contract SV4-74018, A31 with the Smithsonian Astrophysical Observatory which operates Chandra for NASA. Support for this research was provided by NASA grant G09-0150A. This work is also based, in part, on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is based, in part, on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs 11597 and 11663. Support for programs 11597 and 11663 were provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. 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. This work makes use of image data from the NOAO Deep Wide-Field Survey (NDWFS) and the Deep Lens Survey (DLS) as distributed by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation.; This paper would not have been possible without the efforts of the Spitzer, Chandra, HST, and Keck support staff. We thank C. Fedeli for helpful discussions on the evolution of the mass function. Support for M. B. was provided by the W. M. Keck Foundation. The work by S. A. S. at LLNL was performed under the auspices of the U.S. Department of Energy under contract No. W-7405-ENG-48. NR 60 TC 45 Z9 45 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 33 DI 10.1088/0004-637X/732/1/33 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500033 ER PT J AU Cenko, SB Frail, DA Harrison, FA Haislip, JB Reichart, DE Butler, NR Cobb, BE Cucchiara, A Berger, E Bloom, JS Chandra, P Fox, DB Perley, DA Prochaska, JX Filippenko, AV Glazebrook, K Ivarsen, KM Kasliwal, MM Kulkarni, SR LaCluyze, AP Lopez, S Morgan, AN Pettini, M Rana, VR AF Cenko, S. B. Frail, D. A. Harrison, F. A. Haislip, J. B. Reichart, D. E. Butler, N. R. Cobb, B. E. Cucchiara, A. Berger, E. Bloom, J. S. Chandra, P. Fox, D. B. Perley, D. A. Prochaska, J. X. Filippenko, A. V. Glazebrook, K. Ivarsen, K. M. Kasliwal, M. M. Kulkarni, S. R. LaCluyze, A. P. Lopez, S. Morgan, A. N. Pettini, M. Rana, V. R. TI AFTERGLOW OBSERVATIONS OF FERMI LARGE AREA TELESCOPE GAMMA-RAY BURSTS AND THE EMERGING CLASS OF HYPER-ENERGETIC EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; gamma-ray burst: general; radio continuum: general ID 25 APRIL 1998; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; NEUTRINO PAIR ANNIHILATION; FOLLOW-UP OBSERVATIONS; BROAD-BAND AFTERGLOW; X-RAY; LIGHT-CURVES; RADIO AFTERGLOW; BLACK-HOLES; SWIFT-ERA AB We present broadband (radio, optical, and X-ray) light curves and spectra of the afterglows of four long-duration gamma-ray bursts (GRBs; GRBs 090323, 090328, 090902B, and 090926A) detected by the Gamma-Ray Burst Monitor and Large Area Telescope (LAT) instruments on the Fermi satellite. With its wide spectral bandpass, extending to GeV energies, Fermi is sensitive to GRBs with very large isotropic energy releases (10(54) erg). Although rare, these events are particularly important for testing GRB central-engine models. When combined with spectroscopic redshifts, our afterglow data for these four events are able to constrain jet collimation angles, the density structure of the circumburst medium, and both the true radiated energy release and the kinetic energy of the outflows. In agreement with our earlier work, we find that the relativistic energy budget of at least one of these events (GRB 090926A) exceeds the canonical value of 10(51) erg by an order of magnitude. Such energies pose a severe challenge for models in which the GRB is powered by a magnetar or a neutrino-driven collapsar, but remain compatible with theoretical expectations for magnetohydrodynamical collapsar models (e. g., the Blandford-Znajek mechanism). Our jet opening angles (theta) are similar to those found for pre-Fermi GRBs, but the large initial Lorentz factors (Gamma(0)) inferred from the detection of GeV photons imply theta Gamma(0) approximate to 70-90, values which are above those predicted in magnetohydrodynamic models of jet acceleration. Finally, we find that these Fermi-LAT events preferentially occur in a low-density circumburst environment, and we speculate that this might result from the lower mass-loss rates of their lower-metallicity progenitor stars. Future studies of Fermi-LAT afterglows at radio wavelengths with the order-of-magnitude improvement in sensitivity offered by the Extended Very Large Array should definitively establish the relativistic energy budgets of these events. C1 [Cenko, S. B.; Butler, N. R.; Cobb, B. E.; Cucchiara, A.; Bloom, J. S.; Perley, D. A.; Filippenko, A. V.; Morgan, A. N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Frail, D. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Harrison, F. A.; Rana, V. R.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Haislip, J. B.; Reichart, D. E.; Ivarsen, K. M.; LaCluyze, A. P.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Cucchiara, A.; Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandra, P.] Royal Mil Coll Canada, Dept Phys, Kingston, ON, Canada. [Prochaska, J. X.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Glazebrook, K.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Kasliwal, M. M.; Kulkarni, S. R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Lopez, S.] Univ Chile, Dept Astron, Santiago, Chile. [Pettini, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Pettini, M.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. RP Cenko, SB (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Glazebrook, Karl/N-3488-2015; Lopez, Sebastian /I-5657-2016; OI Glazebrook, Karl/0000-0002-3254-9044; Lopez, Sebastian /0000-0003-0389-0902; Rana, Vikram/0000-0003-1703-8796 FU Gary and Cynthia Bengier; Richard and Rhoda Goldman Fund; National Aeronautics and Space Administration (NASA) [NNX09AL08G, NNX10AI21G, NNH07ZDA001N, NNH08ZDA001N, NNG06DO90A, NNX09AQ66G]; National Science Foundation (NSF) [AST-0607485, AST-0908886, AST-0802333]; DOE SciDAC FX S.B.C. and A. V. F. wish to acknowledge generous support from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, National Aeronautics and Space Administration (NASA)/Swift grants NNX09AL08G and NNX10AI21G, and National Science Foundation (NSF) grants AST-0607485 and AST-0908886. D. A. F. and F. A. H. were partially supported by NASA/Fermi Guest Investigator grants NNH07ZDA001N and NNH08ZDA001N. B. E. C. gratefully acknowledges support from an NSF Astronomy & Astrophysics Postdoctoral Fellowship (AST-0802333). N.R.B. is supported through the Einstein Fellowship Program (NASA Cooperative Agreement NNG06DO90A). J.S.B. and his group were partially supported by NASA/Swift Guest Investigator grant NNX09AQ66G and a grant from DOE SciDAC. NR 243 TC 76 Z9 76 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 29 DI 10.1088/0004-637X/732/1/29 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500029 ER PT J AU Donahue, M de Messieres, GE O'Connell, RW Voit, GM Hoffer, A McNamara, BR Nulsen, PEJ AF Donahue, Megan de Messieres, Genevieve E. O'Connell, Robert W. Voit, G. Mark Hoffer, Aaron McNamara, Brian R. Nulsen, Paul E. J. TI POLYCYCLIC AROMATIC HYDROCARBONS, IONIZED GAS, AND MOLECULAR HYDROGEN IN BRIGHTEST CLUSTER GALAXIES OF COOL-CORE CLUSTERS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: clusters: intracluster medium; galaxies: starburst; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; ULTRALUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; RAY-LUMINOUS CLUSTERS; STAR-FORMATION RATES; SPECTRAL ENERGY-DISTRIBUTION; FAR-ULTRAVIOLET OBSERVATIONS; DIFFUSE INTERSTELLAR-MEDIUM; STARBURST GALAXIES; NEARBY GALAXIES AB We present measurements of 5-25 mu m emission features of brightest cluster galaxies (BCGs) with strong optical emission lines in a sample of nine cool-core clusters of galaxies observed with the Infrared Spectrograph on board the Spitzer Space Telescope. These systems provide a view of dusty molecular gas and star formation, surrounded by dense, X-ray-emitting intracluster gas. Past work has shown that BCGs in cool-core clusters may host powerful radio sources, luminous optical emission-line systems, and excess UV, while BCGs in other clusters never show this activity. In this sample, we detect polycyclic aromatic hydrocarbons (PAHs), extremely luminous, rotationally excited molecular hydrogen line emission, forbidden line emission from ionized gas ([Ne II] and [Ne III]), and infrared continuum emission from warm dust and cool stars. We show here that these BCGs exhibit more luminous forbidden neon and H-2 rotational line emission than star-forming galaxies with similar total infrared luminosities, as well as somewhat higher ratios of 70 mu m/24 mu m luminosities. Our analysis suggests that while star formation processes dominate the heating of the dust and PAHs, a heating process consistent with suprathermal electron heating from the hot gas, distinct from star formation, is heating the molecular gas and contributing to the heating of the ionized gas in the galaxies. The survival of PAHs and dust suggests that dusty gas is somehow shielded from significant interaction with the X-ray gas. C1 [Donahue, Megan; Voit, G. Mark; Hoffer, Aaron] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [de Messieres, Genevieve E.; O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [McNamara, Brian R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Nulsen, Paul E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Donahue, M (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM donahue@pa.msu.edu; voit@pa.msu.edu; hofferaa@msu.edu RI Donahue, Megan/B-5361-2012; OI Nulsen, Paul/0000-0003-0297-4493; Voit, Gerard/0000-0002-3514-0383 FU Jet Propulsion Lab [JPL 1353923]; NASA LTSA [NASA NNG-05GD82G]; NSF [AST-0908819, NSF PHY05-51164]; NASA FX The authors are grateful for tabulated plot data from Daniela Calzetti and for discussions with Brent Groves and Michael Dopita. We acknowledge the referee for a careful review of our manuscript. M. D., G. M. V., and A. H. acknowledge support from a Jet Propulsion Lab contract JPL 1353923 and a NASA LTSA grant NASA NNG-05GD82G. G. M. V. acknowledges partial support from NSF grant AST-0908819. M. D. thanks the Aspen Center of Physics where she began this work in the summer of 2008, and the Kavli Institute of Theoretical Physics in Santa Barbara, CA, where she finished the paper in 2011 February. This research was supported in part by the National Science Foundation under grant NSF PHY05-51164. 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 G. D. M., B. R. M., and R.W.O. was provided by NASA through two awards issued by JPL/Caltech. NR 112 TC 46 Z9 46 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 MAY 1 PY 2011 VL 732 IS 1 AR 40 DI 10.1088/0004-637X/732/1/40 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500040 ER PT J AU Foley, RJ Berger, E Fox, O Levesque, EM Challis, PJ Ivans, II Rhoads, JE Soderberg, AM AF Foley, Ryan J. Berger, Edo Fox, Ori Levesque, Emily M. Challis, Peter J. Ivans, Inese I. Rhoads, James E. Soderberg, Alicia M. TI THE DIVERSITY OF MASSIVE STAR OUTBURSTS. I. OBSERVATIONS OF SN2009ip, UGC 2773 OT2009-1, AND THEIR PROGENITORS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; stars: evolution; stars: individual (SN 2009ip, UGC 2773 OT2009-1); stars: massive; stars: mass-loss; stars: variables: general; stars: variables: S Doradus; stars: winds, outflows ID ETA-CARINAE ANALOG; NGC 300; SN 2008S; RADIO-EMISSION; SUPERNOVA; DUST; SPECTROSCOPY; SPECTROGRAPH; TRANSIENT; ERUPTION AB Despite both being outbursts of luminous blue variables (LBVs), SN 2009ip and UGC 2773 OT2009-1 have very different progenitors, spectra, circumstellar environments, and possibly physical mechanisms that generated the outbursts. From pre-eruption Hubble Space Telescope images, we determine that SN 2009ip and UGC 2773 OT2009-1 have initialmasses of greater than or similar to 60 and greater than or similar to 25 M-circle dot, respectively. Optical spectroscopy shows that at peak, SN 2009ip had a 10,000 K photosphere and its spectrum was dominated by narrow H Balmer emission, similar to classical LBV giant outbursts, also known as "supernova impostors." The spectra of UGC 2773 OT2009-1, which also have narrow Ha emission, are dominated by a forest of absorption lines, similar to an F-type supergiant. Blueshifted absorption lines corresponding to ejecta at a velocity of 2000-7000 km s(-1) are present in later spectra of SN 2009ip-an unprecedented observation for LBV outbursts, indicating that the event was the result of a supersonic explosion rather than a subsonic outburst. The velocity of the absorption lines increases between two epochs, suggesting that there were two explosions in rapid succession. A rapid fading and rebrightening event concurrent with the onset of the high-velocity absorption lines is consistent with the double-explosion model. A near-infrared excess is present in the spectra and photometry of UGC 2773 OT2009-1 that is consistent with similar to 2100 K dust emission. We compare the properties of these two events and place them in the context of other known massive star outbursts such as eta Car, NGC 300 OT2008-1, and SN 2008S. This qualitative analysis suggests that massive star outbursts have many physical differences that can manifest as the different observables seen in these two interesting objects. C1 [Foley, Ryan J.; Berger, Edo; Challis, Peter J.; Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fox, Ori] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Levesque, Emily M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Ivans, Inese I.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Rhoads, James E.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Levesque, Emily M.] Smithsonian Astrophys Observ, Cambridge, MA USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu FU NASA GSRP; NASA, ARCS; NASA, VSGC; Ford Foundation; NASA [NAS 5-26555] FX R.J.F. is supported by a Clay Fellowship. O.D.F. is grateful for support from NASA GSRP, ARCS, and VSGC. E. M. L. is supported in part by a Ford Foundation Predoctoral Fellowship.; This study is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. 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 US National Science Foundation on behalf of the Gemini partnership: the NSF(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); the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile; the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona; the Fan Mountain Observatory 0.8 m telescope; and the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. We acknowledge the use of public data from the Swift data archive. NR 71 TC 57 Z9 57 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 MAY 1 PY 2011 VL 732 IS 1 AR 32 DI 10.1088/0004-637X/732/1/32 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500032 ER PT J AU Gitti, M Nulsen, PEJ David, LP McNamara, BR Wise, MW AF Gitti, Myriam Nulsen, Paul E. J. David, Laurence P. McNamara, Brian R. Wise, Michael W. TI A CHANDRA STUDY OF THE LARGE-SCALE SHOCK AND COOL FILAMENTS IN HYDRA A: EVIDENCE FOR SUBSTANTIAL GAS DREDGE-UP BY THE CENTRAL OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: clusters: individual (Hydra A); galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID X-RAY SPECTROSCOPY; GALAXY CLUSTERS; HIGH-RESOLUTION; XMM-NEWTON; A CLUSTER; FEEDBACK; CONSTRAINTS; CAVITIES; OUTFLOW; CORE AB We present the results of a Chandra study of the Hydra A galaxy cluster, where a powerful active galactic nucleus (AGN) outburst created a large-scale cocoon shock. We investigated possible azimuthal variations in shock strength and shape, finding indications for a weak shock with a Mach number in the range similar to 1.2-1.3. We measured the temperature change across the shock front. However, the detection of a temperature rise in the regions immediately inside of the front is complicated by the underlying temperature profile of the cluster atmosphere. We measured the global temperature profile of the cluster up to 700 kpc, which represents the farthest measurement obtained with Chandra for this cluster. A "plateau" in the temperature profile in the range similar to 70-150 kpc indicates the presence of cool gas, which is likely the result of uplift of material by the AGN outburst. After masking the cool filaments visible in the hardness ratio map, the plateau disappears and the temperature profile recovers a typical shape with a peak around 190 kpc, just inside the shock front. However, it is unlikely that such a temperature feature is produced by the shock as it is consistent with the general shape of the temperature profiles observed for relaxed galaxy clusters. We studied the spectral properties of the cool filaments finding evidence that similar to 10(11) M-circle dot of low-entropy material has been dredged up by the rising lobes from the central 30 kpc to the observed current position of 75-150 kpc. The energy required to lift the cool gas is greater than or similar to 2.2 x 10(60) erg, which is comparable to the work required to inflate the cavities and is similar to 25% of the total energy of the large-scale shock. Our results show that the AGN feedback in Hydra A is acting not only by directly heating the gas, but also by removing a substantial amount of potential fuel for the supermassive black hole. C1 [Gitti, Myriam; Nulsen, Paul E. J.; David, Laurence P.; McNamara, Brian R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gitti, Myriam] INAF, Astron Observ Bologna, I-40127 Bologna, Italy. [McNamara, Brian R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. [McNamara, Brian R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [Wise, Michael W.] ASTRON Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. RP Gitti, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Gitti, Myriam/0000-0002-0843-3009; Nulsen, Paul/0000-0003-0297-4493 FU Chandra grants [GO0-11003X, GO0-11136X]; Natural Sciences and Engineering Research Council of Canada; [ASI-INAF I/023/05/0]; [I/088/06/0] FX We thank the referee for constructive comments. We also thank A. Vikhlinin for providing the data used to make the plots in Figure 8. M.G. thanks D. Rafferty for precious advice in data reduction, and F. Brighenti for many insightful discussions. M.G. acknowledges support by grants ASI-INAF I/023/05/0 and I/088/06/0 and by Chandra grants GO0-11003X and GO0-11136X. B.R.M acknowledges support from the Natural Sciences and Engineering Research Council of Canada. NR 31 TC 28 Z9 28 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 MAY 1 PY 2011 VL 732 IS 1 AR 13 DI 10.1088/0004-637X/732/1/13 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500013 ER PT J AU Parrent, JT Thomas, RC Fesen, RA Marion, GH Challis, P Garnavich, PM Milisavljevic, D Vinko, J Wheeler, JC AF Parrent, Jerod T. Thomas, R. C. Fesen, Robert A. Marion, G. H. Challis, Peter Garnavich, Peter M. Milisavljevic, Dan Vinko, Jozsef Wheeler, J. Craig TI A STUDY OF CARBON FEATURES IN TYPE Ia SUPERNOVA SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN 2010Y, 2010ai, PTF10icb) ID DELAYED DETONATION MODELS; HOBBY-EBERLY TELESCOPE; HIGH-VELOCITY EJECTA; MASS WHITE-DWARF; LOW-LUMINOSITY; SN 1999BY; SPECTROSCOPIC OBSERVATIONS; CIRCUMSTELLAR INTERACTION; ABUNDANCE STRATIFICATION; FACTORY OBSERVATIONS AB One of the major differences between various explosion scenarios of Type Ia supernovae (SNe Ia) is the remaining amount of unburned (C+O) material and its velocity distribution within the expanding ejecta. While oxygen absorption features are not uncommon in the spectra of SNe Ia before maximum light, the presence of strong carbon absorption has been reported only in a minority of objects, typically during the pre-maximum phase. The reported low frequency of carbon detections may be due to low signal-to-noise data, low abundance of unburned material, line blending between C II lambda 6580 and Si II lambda 6355, ejecta temperature differences, asymmetrical distribution effects, or a combination of these. However, a survey of published pre-maximum spectra reveals that more SNe Ia than previously thought may exhibit C II lambda 6580 absorption features and relics of line blending near similar to 6300 angstrom. Here we present new SN Ia observations where spectroscopic signatures of C II lambda 6580 are detected and investigate the presence of C II lambda 6580 in the optical spectra of 19 SNe Ia using the parameterized spectrum synthesis code, SYNOW. Most of the objects in our sample that exhibit C II lambda 6580 absorption features are of the low-velocity gradient subtype. Our study indicates that the morphology of carbon-rich regions is consistent with either a spherical distribution or a hemispheric asymmetry, supporting the recent idea that SN Ia diversity may be a result of off-center ignition coupled with observer line-of-sight effects. C1 [Parrent, Jerod T.; Fesen, Robert A.; Milisavljevic, Dan] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Thomas, R. C.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [Marion, G. H.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marion, G. H.; Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. RP Parrent, JT (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. FU NSF [AST-0707669]; Texas Advanced Research Program [ASTRO-ARP-0094]; Hungarian OTKA [K76816] FX We are grateful to Laura Kay for obtaining some of the spectra of SN 2010Y and thank Eddie Baron, David Branch, and Andy Howell for helpful comments on an earlier draft of this paper. J.V. has received support from NSF Grant AST-0707669, Texas Advanced Research Program grant ASTRO-ARP-0094, and Hungarian OTKA Grant K76816. NR 127 TC 60 Z9 60 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 30 DI 10.1088/0004-637X/732/1/30 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500030 ER PT J AU Pe'er, A Ryde, F AF Pe'er, Asaf Ryde, Felix TI A THEORY OF MULTICOLOR BLACKBODY EMISSION FROM RELATIVISTICALLY EXPANDING PLASMAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; plasmas; radiation mechanisms: thermal; radiative transfer; scattering; X-rays: bursts ID GAMMA-RAY-BURSTS; INTERNAL SHOCK MODEL; POWERED GRB OUTFLOWS; PROMPT EMISSION; SPECTRAL PROPERTIES; THERMAL EMISSION; PHOTOSPHERIC EMISSION; MAGNETIC-FIELDS; LORENTZ FACTOR; EFFICIENCY AB We consider the emission of photons from the inner parts of a relativistically expanding plasma outflow, characterized by a constant Lorentz factor, Gamma. Photons that are injected in regions of high optical depth are advected with the flow until they escape at the photosphere. Due to multiple scattering below the photosphere, the locally emerging comoving photon distribution is thermal. However, as an observer simultaneously sees photons emitted from different angles, hence with different Doppler boosting, the observed spectrum is a multicolor blackbody. We calculate here the properties of the observed spectrum at different observed times. Due to the strong dependence of the photospheric radius on the angle to the line of sight, for parameters characterizing gamma-ray bursts (GRBs) thermal photons are seen up to tens of seconds following the termination of the inner engine. At late times, following the inner engine termination, both the number flux and energy flux of the thermal spectrum decay as F proportional to t(-2). At these times, the multicolor blackbody emission results in a power law at low energies (below the thermal peak), with power-law index F-nu proportional to nu(0). We discuss the implications and limitations of this result in the study of GRBs. C1 [Pe'er, Asaf] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Ryde, Felix] Royal Inst Technol, Dept Phys, SE-10691 Stockholm, Sweden. RP Pe'er, A (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM apeer@stsci.edu FU Space Telescope Science Institute FX We would like to thank Mario Livio, Zeljka Bosnjak, Chryssa Kouveliotou, Charles Dermer, Ralph A. M. J. Wijers, Peter Meszaros, Martin Rees, and Bing Zhang for many useful discussions and comments. A. P. is supported by the Riccardo Giacconi Fellowship award of the Space Telescope Science Institute. NR 67 TC 52 Z9 52 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 MAY 1 PY 2011 VL 732 IS 1 AR 49 DI 10.1088/0004-637X/732/1/49 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500049 ER PT J AU Rest, A Foley, RJ Sinnott, B Welch, DL Badenes, C Filippenko, AV Bergmann, M Bhatti, WA Blondin, S Challis, P Damke, G Finley, H Huber, ME Kasen, D Kirshner, RP Matheson, T Mazzali, P Minniti, D Nakajima, R Narayan, G Olsen, K Sauer, D Smith, RC Suntzeff, NB AF Rest, A. Foley, R. J. Sinnott, B. Welch, D. L. Badenes, C. Filippenko, A. V. Bergmann, M. Bhatti, W. A. Blondin, S. Challis, P. Damke, G. Finley, H. Huber, M. E. Kasen, D. Kirshner, R. P. Matheson, T. Mazzali, P. Minniti, D. Nakajima, R. Narayan, G. Olsen, K. Sauer, D. Smith, R. C. Suntzeff, N. B. TI DIRECT CONFIRMATION OF THE ASYMMETRY OF THE CAS A SUPERNOVA WITH LIGHT ECHOES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Cas A); ISM: supernova remnants; supernovae: general ID CASSIOPEIA-A SUPERNOVA; HUBBLE-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; IIB SN 2008AX; X-RAY KNOTS; CORE-COLLAPSE; UBVRI PHOTOMETRY; INFRARED ECHOES; IA SUPERNOVAE; STELLAR WIND AB We report the first detection of asymmetry in a supernova (SN) photosphere based on SN light echo (LE) spectra of Cas A from the different perspectives of dust concentrations on its LE ellipsoid. New LEs are reported based on difference images, and optical spectra of these LEs are analyzed and compared. After properly accounting for the effects of finite dust-filament extent and inclination, we find one field where the He I lambda 5876 and Ha features are blueshifted by an additional similar to 4000 km s(-1) relative to other spectra and to the spectra of the Type IIb SN 1993J. That same direction does not show any shift relative to other Cas A LE spectra in the Ca II near-infrared triplet feature. We compare the perspectives of the Cas A LE dust concentrations with recent three-dimensional modeling of the SN remnant (SNR) and note that the location having the blueshifted He I and Ha features is roughly in the direction of an Fe-rich outflow and in the opposite direction of the motion of the compact object at the center of the SNR. We conclude that Cas A was an intrinsically asymmetric SN. Future LE spectroscopy of this object, and of other historical SNe, will provide additional insight into the connection of the explosion mechanism to SN then to SNR, as well as give crucial observational evidence regarding how stars explode. C1 [Rest, A.; Narayan, G.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Foley, R. J.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sinnott, B.; Welch, D. L.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Badenes, C.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Fac Phys, IL-76100 Rehovot, Israel. [Badenes, C.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bhatti, W. A.; Huber, M. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Blondin, S.] Aix Marseille Univ, CNRS, IN2P3, CPPM, F-13288 Marseille 9, France. [Challis, P.; Damke, G.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Finley, H.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Kasen, D.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Matheson, T.; Olsen, K.; Smith, R. C.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Mazzali, P.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Mazzali, P.] Scuola Normale Super Pisa, I-56127 Pisa, Italy. [Mazzali, P.] INAF Oss Astron Padova, I-35122 Padua, Italy. [Minniti, D.] Vatican Observ, I-00120 Vatican City, Vatican. [Nakajima, R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Sauer, D.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Smith, R. C.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. [Suntzeff, N. B.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. RP Rest, A (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM marcelbergmann@gmail.com RI Sauer, Daniel/A-3033-2012; OI Sauer, Daniel/0000-0002-0317-5063; Bhatti, Waqas/0000-0002-0628-0088; Finley, Hayley/0000-0002-1216-8914; Narayan, Gautham/0000-0001-6022-0484 FU Goldberg Fellowship Program; Natural Sciences and Engineering Research Council of Canada (NSERC); Benoziyo Center for Astrophysics at Weizmann Institute of Science; NSF [AST-0907903]; TABASGO Foundation; NASA, Space Telescope Science Institute [GO-11114]; NASA [NAS 5-26555]; W. M. Keck Foundation; [FONDAP CFA 15010003]; [BASAL CATA PFB-06]; [MIDEPLAN MWM P07-021-F] FX We thank A. Becker, A. Clocchiatti, A. Garg, M. Wood-Vasey, and the referee for useful comments that helped improve the manuscript. We are grateful to B. Jannuzi and H. Schweiker for taking images with the KPNO 4 m telescope prior to the design of the Keck slit masks, to J. M. Silverman for assistance with the Keck observations, and to T. Delaney for giving us access to her manuscript and 3D data for the structure of Cas A before publication. A. R. thanks the Goldberg Fellowship Program for its support. D. W. acknowledges support from the Natural Sciences and Engineering Research Council of Canada (NSERC). C. B. acknowledges the Benoziyo Center for Astrophysics for support at the Weizmann Institute of Science. D. M. is supported by grants from FONDAP CFA 15010003, BASAL CATA PFB-06, and MIDEPLAN MWM P07-021-F. R. P. K. is grateful for the support of NSF grant AST-0907903. A. V. F. is grateful for the support of NSF grant AST-0908886, the TABASGO Foundation, and NASA grant GO-11114 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.; Some of the observations were obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. Part 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 authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. NR 73 TC 43 Z9 43 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 MAY 1 PY 2011 VL 732 IS 1 AR 3 DI 10.1088/0004-637X/732/1/3 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500003 ER PT J AU Rest, A Sinnott, B Welch, DL Foley, RJ Narayan, G Mandel, K Huber, ME Blondin, S AF Rest, A. Sinnott, B. Welch, D. L. Foley, R. J. Narayan, G. Mandel, K. Huber, M. E. Blondin, S. TI ON THE INTERPRETATION OF SUPERNOVA LIGHT ECHO PROFILES AND SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (SN 1987A Cas A); ISM: supernova remnants; supernovae: general ID LARGE-MAGELLANIC-CLOUD; OPTICAL SPECTROPHOTOMETRIC ATLAS; HUBBLE-SPACE-TELESCOPE; CASSIOPEIA-A SUPERNOVA; SHOCK BREAKOUT; SN 1993J; UBVRI PHOTOMETRY; IA SUPERNOVAE; CIRCUMSTELLAR ENVIRONMENT; INFRARED ECHOES AB The light echo (LE) systems of historical supernovae in the Milky Way and local group galaxies provide an unprecedented opportunity to reveal the effects of asymmetry on observables, particularly optical spectra. Scattering dust at different locations on the LE ellipsoid witnesses the supernova from different perspectives, and the light consequently scattered toward Earth preserves the shape of line profile variations introduced by asymmetries in the supernova photosphere. However, the interpretation of supernova LE spectra to date has not involved a detailed consideration of the effects of outburst duration and geometrical scattering modifications due to finite scattering dust filament dimension, inclination, and image point-spread function and spectrograph slit width. In this paper, we explore the implications of these factors and present a framework for future-resolved supernova LE spectra interpretation, and test it against Cas A and SN 1987A LE spectra. We conclude that the full modeling of the dimensions and orientation of the scattering dust using the observed LEs at two or more epochs is critical for the correct interpretation of LE spectra. Indeed, without doing so one might falsely conclude that differences exist when none are actually present. C1 [Rest, A.; Narayan, G.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sinnott, B.; Welch, D. L.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Foley, R. J.; Mandel, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huber, M. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Blondin, S.] Aix Marseille Univ, CNRS, IN2P3, CPPM, F-13288 Marseille 9, France. RP Rest, A (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM arest@stsci.edu OI Narayan, Gautham/0000-0001-6022-0484 FU Goldberg Fellowship Program; NSF [AST-0907903] FX We thank J. Menzies for providing the spectral database of SN 1987A obtained from SAAO. A.R. was partially supported by the Goldberg Fellowship Program. A.R. thanks Jeremiah Murphy for stimulating discussions. Supernova research at Harvard College Observatory is supported in part by NSF grant AST-0907903. Based on observations obtained at the Gemini Observatory (program ID GS-2006B-Q-41), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the US National Science Foundation on behalf of the Gemini partnership: the NSF (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). NOAO is operated by AURA under cooperative agreement with the NSF. NR 79 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 2 DI 10.1088/0004-637X/732/1/2 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500002 ER PT J AU Sehgal, N Trac, H 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 Hajian, A Halpern, M Hasselfield, M Hernandez-Monteagudo, C Hilton, GC Hilton, M Hincks, AD Hlozek, R Holtz, D Huffenberger, KM Hughes, DH Hughes, JP Infante, L Irwin, KD Jones, A Juin, JB Klein, J Kosowsky, A Lau, JM Limon, M Lin, YT Lupton, RH Marriage, TA Marsden, D Martocci, K Mauskopf, P Menanteau, F Moodley, K Moseley, H Netterfield, CB Niemack, MD Nolta, MR Page, LA Parker, L Partridge, B Reid, B Sherwin, BD Sievers, J Spergel, DN Staggs, ST Swetz, DS Switzer, ER Thornton, R Tucker, C Warne, R Wollack, E Zhao, Y AF Sehgal, Neelima Trac, Hy Acquaviva, Viviana Ade, Peter A. R. Aguirre, Paula Amiri, Mandana Appel, John W. Felipe Barrientos, L. Battistelli, Elia S. Bond, J. Richard 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. Hajian, Amir Halpern, Mark Hasselfield, Matthew Hernandez-Monteagudo, Carlos Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hlozek, Renee Holtz, David Huffenberger, Kevin M. Hughes, David H. Hughes, John P. Infante, Leopoldo Irwin, Kent D. Jones, Andrew Baptiste Juin, Jean Klein, Jeff Kosowsky, Arthur Lau, Judy M. Limon, Michele Lin, Yen-Ting Lupton, Robert H. Marriage, Tobias A. Marsden, Danica Martocci, Krista 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 Sherwin, Blake D. Sievers, Jon Spergel, David N. Staggs, Suzanne T. Swetz, Daniel S. Switzer, Eric R. Thornton, Robert Tucker, Carole Warne, Ryan Wollack, Ed Zhao, Yue TI THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV-ZEL'DOVICH EFFECT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general ID SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; BACKGROUND POWER SPECTRUM; TREE PARTICLE-MESH; X-RAY; RADIO-SOURCES; HYDRODYNAMICAL SIMULATIONS; PECULIAR VELOCITIES; SCALING RELATIONS; CATALOG AB We present constraints on cosmological parameters based on a sample of Sunyaev-Zel'dovich-selected (SZ-selected) galaxy clusters detected in a millimeter-wave survey by the Atacama Cosmology Telescope. The cluster sample used in this analysis consists of nine optically confirmed high-mass clusters comprising the high-significance end of the total cluster sample identified in 455 deg(2) of sky surveyed during 2008 at 148 GHz. We focus on the most massive systems to reduce the degeneracy between unknown cluster astrophysics and cosmology derived from SZ surveys. We describe the scaling relation between cluster mass and SZ signal with a four-parameter fit. Marginalizing over the values of the parameters in this fit with conservative priors gives sigma(8) = 0.851 +/- 0.115 and omega = -1.14 +/- 0.35 for a spatially flat wCDM cosmological model with Wilkinson Microwave Anisotropy Probe (WMAP) seven-year priors on cosmological parameters. This gives a modest improvement in statistical uncertainty over WMAP seven-year constraints alone. Fixing the scaling relation between the cluster mass and SZ signal to a fiducial relation obtained from numerical simulations and calibrated by X-ray observations, we find sigma(8) = 0.821 +/- 0.044 and omega = -1.05 +/- 0.20. These results are consistent with constraints from WMAP7 plus baryon acoustic oscillations plus Type Ia supernova which give sigma(8) = 0.802 +/- 0.038 and omega = -0.98 +/- 0.053. A stacking analysis of the clusters in this sample compared to clusters simulated assuming the fiducial model also shows good agreement. These results suggest that, given the sample of clusters used here, both the astrophysics of massive clusters and the cosmological parameters derived from them are broadly consistent with current models. C1 [Sehgal, Neelima; Lau, Judy M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Acquaviva, Viviana; Das, Sudeep; Dunkley, Joanna; Hajian, Amir; Lin, Yen-Ting; Lupton, Robert H.; Marriage, Tobias A.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Acquaviva, Viviana; 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.; Duenner, Rolando; 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. [Appel, John W.; Das, Sudeep; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D.; Holtz, David; Jones, Andrew; Lau, Judy M.; Limon, Michele; Martocci, Krista; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [Bond, J. Richard; Hajian, Amir; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Chervenak, Jay; Moseley, Harvey; Wollack, Ed; Zhao, Yue] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Devlin, Mark J.; Dicker, Simon R.; Klein, Jeff; Limon, Michele; Marriage, Tobias A.; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Doriese, W. Bertrand; Fowler, Joseph W.; 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, Astrophys & Cosmol Res Unit, Sch Math Sci, 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.] 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. [Martocci, Krista; Switzer, Eric R.] Kavli Inst Cosmol Phys, Lab Astrophys & Space Res, Chicago, IL 60637 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, ICC, E-08028 Barcelona, Spain. [Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA. RP Sehgal, N (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. 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; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074; /0000-0002-0896-8628; Limon, Michele/0000-0002-5900-2698 FU US National Science Foundation [AST-0408698, PHY-0355328, AST-0707731, PIRE-0507768]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation; Compute Canada; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; U.S. Department of Energy [DE-AC3-76SF00515]; NASA [NNX08AH30G]; Natural Science and Engineering Research Council of Canada (NSERC); NSF Physics Frontier Center [PHY-0114422]; FONDAP Centro de Astrofisica; RCUK; South African National Research Foundation (NRF); Meraka Institute; South African Square Kilometer Array (SKA) Project; CONICYT; MECESUP; Fundacion Andes; Rhodes Trust; Berkeley Center for Cosmological Physics; World Premier International Research Center Initiative, MEXT, Japan; NASA Office of Space Science; [NSFAST-0546035]; [AST-0606975] FX This work was supported by the US 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. 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.; N.S. is supported by the U.S. Department of Energy contract to SLAC No. DE-AC3-76SF00515. A. H., T. M., S. D., and V. A. were supported through NASA grant NNX08AH30G. A. 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 NSFAST-0546035 and AST-0606975, respectively, for work on ACT. E. S. acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. H. Q. and L. I. acknowledge partial support from FONDAP Centro de Astrofisica. J.D. received support from an RCUK Fellowship. 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. R. D. was supported by CONICYT, MECESUP, and Fundacion Andes. RH acknowledges funding from the Rhodes Trust. 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. Some of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005). 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 87 TC 100 Z9 100 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 MAY 1 PY 2011 VL 732 IS 1 AR 44 DI 10.1088/0004-637X/732/1/44 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500044 ER PT J AU Stacey, WS Heinke, CO Elsner, RF Edmonds, PD Weisskopf, MC Grindlay, JE AF Stacey, W. S. Heinke, C. O. Elsner, R. F. Edmonds, P. D. Weisskopf, M. C. Grindlay, J. E. TI TRANSIENT EXTREMELY SOFT X-RAY EMISSION FROM THE UNUSUALLY BRIGHT CATACLYSMIC VARIABLE IN THE GLOBULAR CLUSTER M3: A NEW CV X-RAY LUMINOSITY RECORD? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; globular clusters: individual (NGC 5272); novae, cataclysmic variables; white dwarfs; X-rays: binaries ID ABSOLUTE MAGNITUDES; SUPERSOFT SOURCES; ACCRETION DISKS; GALACTIC-CENTER; IA SUPERNOVAE; SKY SURVEY; GK-PERSEI; BINARIES; EVOLUTION; NOVAE AB We observed the accreting white dwarf (WD) 1E1339.8+2837 (1E1339) in the globular cluster M3 in 2003 November, 2004 May, and 2005 January, using the Chandra ACIS-S detector. The source was observed in 1992 to possess traits of a supersoft X-ray source (SSS), with a 0.1-2.4 keV luminosity as large as 2 x 10(35) erg s(-1), after which time the source's luminosity fell by roughly two orders of magnitude, adopting a hard X-ray spectrum more typical of cataclysmic variables (CVs). Our observations confirm 1E1339's hard CV-like spectrum, with photon index Gamma = 1.3 +/- 0.2. We found 1E1339 to be highly variable, with a 0.5-10 keV luminosity ranging from (1.4 +/- 0.3) x 10(34) erg s-1 to 8.5(-4.6)(+4.9) x 10(32) erg s(-1), with 1E1339's maximum luminosity being perhaps the highest yet recorded for hard X-ray emission from a WD. In 2005 January, 1E1339 displayed substantial low-energy emission below similar to 0.3 keV. Although current Chandra responses cannot properly model this emission, its bolometric luminosity appears comparable to or greater than that of the hard spectral component. This raises the possibility that the supersoft X-ray emission seen from 1E1339 in 1992 may have shifted to the far-UV. C1 [Stacey, W. S.; Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Elsner, R. F.; Weisskopf, M. C.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Edmonds, P. D.; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stacey, WS (reprint author), Univ Alberta, Dept Phys, 11322-89 Ave, Edmonton, AB T6G 2G7, Canada. EM heinke@ualberta.ca OI Heinke, Craig/0000-0003-3944-6109 NR 44 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2011 VL 732 IS 1 AR 46 DI 10.1088/0004-637X/732/1/46 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500046 ER PT J AU Trump, JR Nagao, T Ikeda, H Murayama, T Impey, CD Stocke, JT Civano, F Elvis, M Jahnke, K Kelly, BC Koekemoer, AM Taniguchi, Y AF Trump, Jonathan R. Nagao, Tohru Ikeda, Hiro Murayama, Takashi Impey, Christopher D. Stocke, John T. Civano, Francesca Elvis, Martin Jahnke, Knud Kelly, Brandon C. Koekemoer, Anton M. Taniguchi, Yoshi TI SPECTROPOLARIMETRIC EVIDENCE FOR RADIATIVELY INEFFICIENT ACCRETION IN AN OPTICALLY DULL ACTIVE GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: nuclei; polarization; quasars: emission lines; radiation mechanisms: general ID X-RAY-BRIGHT; BL LACERTAE OBJECTS; WIDE-FIELD SURVEY; GALACTIC NUCLEI; RADIO-GALAXIES; HELLAS2XMM SURVEY; SEYFERT-GALAXIES; COSMOS FIELD; DEEP SURVEY; BLACK-HOLE AB We present Subaru/FOCAS spectropolarimetry of two active galaxies in the Cosmic Evolution Survey. These objects were selected to be optically dull, with the bright X-ray emission of an active galactic nucleus (AGN) but missing optical emission lines in our previous spectroscopy. Our new observations show that one target has very weak emission lines consistent with an optically dull AGN, while the other object has strong emission lines typical of a host-diluted Type 2 Seyfert galaxy. In neither source do we observe polarized emission lines, with 3 sigma upper limits of P-BLR less than or similar to 2%. This means that the missing broad emission lines (and weaker narrow emission lines) are not due to simple anisotropic obscuration, e. g., by the canonical AGN torus. The weak-lined optically dull AGN exhibits a blue polarized continuum with P = 0.78% +/- 0.07% at 4400 angstrom < lambda(rest) < 7200 angstrom (P = 1.37% +/- 0.16% at 4400 angstrom < lambda(rest) < 5050 angstrom). The wavelength dependence of this polarized flux is similar to that of an unobscured AGN continuum and represents the intrinsic AGN emission, either as synchrotron emission or the outer part of an accretion disk reflected by a clumpy dust scatterer. Because this intrinsic AGN emission lacks emission lines, this source is likely to have a radiatively inefficient accretion flow. C1 [Trump, Jonathan R.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Nagao, Tohru; Ikeda, Hiro] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Murayama, Takashi; Taniguchi, Yoshi] Tohoku Univ, Grad Sch Sci, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Impey, Christopher D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Stocke, John T.] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, UCB 389, Boulder, CO 80309 USA. [Civano, Francesca; Elvis, Martin; Kelly, Brandon C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jahnke, Knud] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Trump, JR (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. OI Jahnke, Knud/0000-0003-3804-2137; Koekemoer, Anton/0000-0002-6610-2048 FU NSF/DDEP [0943995]; NSF [AST-0808133]; Blancheflor Boncompagni Ludovisi foundation; Smithsonian Scholarly Studies; NASA through Space Telescope Science Institute [HF-51243.01]; NASA [NAS 5-26555]; JSPS [17253001, 19340046]; [AST-0908044] FX We thank Takashi Hattori and the staff of Subaru for excellent support during and after observations. We thank Kenta Matsuoka for help in reducing the FOCAS data. Masaomi Tanaka was invaluable in interpreting the spectropolarimetry results. We also thank Hien Tran and Makoto Kishimoto for help in interpreting a polarized continuum in AGNs. We thank the referee for helpful comments which improved the quality of this work. J.R.T. acknowledges support from NSF/DDEP grant 0943995 and NSF grant AST-0808133, and with C.D.I. acknowledges support from AST-0908044. F.C. acknowledges support from the Blancheflor Boncompagni Ludovisi foundation and the Smithsonian Scholarly Studies. B.C.K. acknowledges support from NASA through Hubble Fellowship grant HF-51243.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Y.T. acknowledges support from JSPS grants 17253001 and 19340046. NR 53 TC 6 Z9 6 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 MAY 1 PY 2011 VL 732 IS 1 AR 23 DI 10.1088/0004-637X/732/1/23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 751OD UT WOS:000289626500023 ER PT J AU Szlavecz, K McCormick, M Xia, LJ Saunders, J Morcol, T Whigham, D Filley, T Csuzdi, C AF Szlavecz, Katalin McCormick, Melissa Xia, Lijun Saunders, Jaclyn Morcol, Taylan Whigham, Dennis Filley, Timothy Csuzdi, Csaba TI Ecosystem effects of non-native earthworms in Mid-Atlantic deciduous forests SO BIOLOGICAL INVASIONS LA English DT Article DE Invasive earthworms; Leaf litter decay; Soil respiration; Microbial activity; Seedling growth ID SOIL ORGANIC-MATTER; NORTHERN TEMPERATE FORESTS; LITTER DECOMPOSITION; EXOTIC EARTHWORMS; HARDWOOD FORESTS; OCTET-METHOD; LEAF-LITTER; INVASION; NITROGEN; RESPIRATION AB In many mid-Atlantic forests where both native and non-native earthworms exist, it is the non-native species that are the dominant component of the soil macrofauna. Few earthworm ecology studies, however, focus attention on these forest systems in order to determine the relative ecological roles and potential interactions of the native and non-native earthworms. In a series of field samplings and experimental manipulations we collected data on the effects of earthworms on below-and aboveground ecosystem processes. Earthworm abundance and the ecological processes measured were dynamic in space and time across the range of study sites. Leaf litter decay rates doubled at sites that had abundant non-native earthworms. Earthworms also altered the abundance of soil fungi, the activity of extracellular enzymes, soil respiration, and the growth of tree seedlings but the effects varied among sites depending on differences in land-use history and forest age. Red oak seedling growth was less at sites that had abundant earthworms but tulip poplar and red maple seedlings grew equally well with and without abundant earthworms. These preliminary results suggest that non-native earthworms have significant ecosystem effects, even in forests where native earthworms still occur. Land use history, however, plays an important role in determining what those effects will be, and these effects are likely to be dynamic, depending on the abundance of non-native earthworms. C1 [Szlavecz, Katalin; Xia, Lijun] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21216 USA. [McCormick, Melissa; Saunders, Jaclyn; Morcol, Taylan; Whigham, Dennis] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Filley, Timothy] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. [Filley, Timothy] Purdue Univ, Purdue Climate Change Res Ctr, W Lafayette, IN 47907 USA. [Csuzdi, Csaba] Hungarian Nat Hist Museum, Budapest, Hungary. [Csuzdi, Csaba] HAS, Systemat Zool Res Grp, Budapest, Hungary. RP Szlavecz, K (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, 3400 N Charles St, Baltimore, MD 21216 USA. EM szlavecz@jhu.edu RI Csuzdi, Csaba/A-8619-2010; OI Csuzdi, Csaba/0000-0002-0319-7836; Szlavecz, Katalin/0000-0003-2504-0298; Whigham, Dennis/0000-0003-1488-820X FU United States Department of Agriculture [NRI 2007-35320-18375]; National Science Foundation [EAR-0748442, EEC-0540832 ERC-MIRTHE]; Microsoft Research FX This study was supported by grants from the United States Department of Agriculture (USDA-CSREES NRI 2007-35320-18375, the National Science Foundation (EAR-0748442, EEC-0540832 ERC-MIRTHE), and Microsoft Research. We are most grateful to Scott Pitz and Jay O'Neill, who were instrumental in establishing the field manipulations and subsequent monitoring. Several undergraduates and SERC volunteers provided help in the field: Sarah Frank, Peter Houlihan, Helen Huang, Miriam Johnston, and Kerry Good. Alex Szalay designed and built the shocking equipment. We also thank two anonymous reviewers and Ronaldo Sousa for helpful comments on an earlier version of this manuscript. NR 65 TC 34 Z9 35 U1 11 U2 82 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 EI 1573-1464 J9 BIOL INVASIONS JI Biol. Invasions PD MAY PY 2011 VL 13 IS 5 SI SI BP 1165 EP 1182 DI 10.1007/s10530-011-9959-0 PG 18 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 750PH UT WOS:000289560000009 ER PT J AU Pukazhenthi, BS Della Togna, G Padilla, L Smith, D Sanchez, C Pelican, K Sanjur, OI AF Pukazhenthi, Budhan S. Della Togna, Gina Padilla, Luis Smith, Diorene Sanchez, Carlos Pelican, Katey Sanjur, Oris I. TI Ejaculate Traits and Sperm Cryopreservation in the Endangered Baird's Tapir (Tapirus bairdii) SO JOURNAL OF ANDROLOGY LA English DT Article DE Tapirs; electroejaculation; amides ID CERVUS-ELDI-THAMIN; GAZELLA-DAMA-MHORR; ARTIFICIAL-INSEMINATION; STALLION SEMEN; BOAR SEMEN; REPRODUCTIVE TECHNOLOGY; ASSISTED REPRODUCTION; COLLECTION TECHNIQUES; CYTOPLASMIC DROPLETS; CERATOTHERIUM-SIMUM AB There is little information on the reproductive biology of the male Baird's tapir (Tapirus bairdii). In this study, we characterized the ejaculate traits and evaluated the efficacy of 2 cryodiluents on sperm cryosurvival. Ejaculates were assessed for volume, pH, sperm motility, forward progression, osmolality, sperm concentration, sperm morphology, and acrosomal integrity. For cryopreservation, ejaculates with >50% total sperm motility were washed, and sperm pellets were resuspended in either Botu-Crio (CryoVital, Grandau, Germany) or INRA 96 containing 2% egg yolk and 2.5% each of methyl- and dimethylformamide (INRA 96), and they were cryopreserved over liquid nitrogen vapor. Thawed samples were incubated in vitro (25 degrees C) and evaluated for percent total sperm motility, forward progression, and acrosomal integrity at hourly intervals for 4 hours. Spermic ejaculates were obtained from all males, and the mean seminal volume, sperm concentration per milliliter, percent sperm motility, progressive status, and percent morphologically normal cells were 20.4 +/- 4.3 mL, 101.2 +/- 24.0 x 10(6)/mL, 46.1% +/- 5.0%, 2.9 +/- 0.1, and 6.9% +/- 1.4%, respectively. There was a positive significant correlation between percent normal sperm and animal age (r = 0.66; P < .004). Cryopreservation in either Botu-Crio or INRA 96 resulted in a decline (P < .05) in percent sperm motility and acrosomal integrity. Sperm forward progression remained unaffected immediately after thawing in INRA 96 but continued to decline over time. These results characterize, for the first time, the ejaculate traits of the tapir; demonstrate that tapir spermatozoa can be cryopreserved in diluents containing amides alone or in combination with glycerol; and provide fundamental information critical for development of assisted reproductive technologies for the Baird's tapir. C1 [Pukazhenthi, Budhan S.; Della Togna, Gina; Padilla, Luis] Smithsonians Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Padilla, Luis; Sanchez, Carlos] Smithsonians Natl Zool Pk, Dept Anim Hlth, Front Royal, VA USA. [Smith, Diorene] Summit Pk & Bot Gardens, Summit, Panama. [Pelican, Katey] Univ Minnesota, Dept Vet Populat Med, St Paul, MN 55108 USA. [Sanjur, Oris I.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Pukazhenthi, BS (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM pukazhenthib@si.edu FU National Secretariat of Science, Technology and Innovation, Panama; Morris Animal Foundation FX Supported in part by the National Secretariat of Science, Technology and Innovation, Panama, and by the Morris Animal Foundation. NR 66 TC 12 Z9 12 U1 3 U2 14 PU AMER SOC ANDROLOGY, INC PI LAWRENCE PA C/O ALLEN PRESS, INC PO BOX 368, LAWRENCE, KS 66044 USA SN 0196-3635 EI 1939-4640 J9 J ANDROL JI J. Androl. PD MAY-JUN PY 2011 VL 32 IS 3 BP 260 EP 270 DI 10.2164/jandrol.110.011833 PG 11 WC Andrology SC Endocrinology & Metabolism GA 745AX UT WOS:000289137400007 PM 21051586 ER PT J AU Erlandson, JM Braje, TJ Rick, TC Jew, NP Kennett, DJ Dwyer, N Ainis, AF Vellanoweth, RL Watts, J AF Erlandson, Jon M. Braje, Todd J. Rick, Torben C. Jew, Nicholas P. Kennett, Douglas J. Dwyer, Nicole Ainis, Amira F. Vellanoweth, Rene L. Watts, Jack TI 10,000 years of human predation and size changes in the owl limpet (Lottia gigantea) on San Miguel Island, California SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Archaeology; Historical ecology; Marine fisheries; Shellfish; Channel islands ID NORTHERN CHANNEL-ISLANDS; SOUTH-AFRICA; HUMAN IMPACTS; RESOURCE INTENSIFICATION; HUNTER-GATHERERS; ROCKY SHORES; STONE-AGE; EXPLOITATION; SHELLFISH; MIDDLE AB To investigate potential human impacts on California Channel Island shellfish stocks over the past 10,000 years, we measured 1718 owl limpet shells from 19 archaeological components on San Miguel Island. Inhabiting the middle intertidal zone of Pacific Coast rocky shores, owl limpets are slow-growing mollusks that can live for 30 years and reach lengths of over 100 mm. Recent ecological studies indicate that owl limpets are highly susceptible to heavy human predation, which results in reduced mean shell sizes among Lottia populations along the coasts of Alta and Baja California. On San Miguel Island, we identified a significant trans-Holocene reduction in mean owl limpet size, beginning more than 6500 years ago and accelerating at least 4400 years ago. Fluctuations in limpet size show no clear correlation with changes in sea surface temperature and marine productivity, suggesting that increased predation by growing human populations was primarily responsible for the reduction in Lottia size over time. Our results provide further evidence that prehistoric peoples significantly influenced nearshore fisheries long before the development of the commercial and industrialized fisheries of historic times. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Erlandson, Jon M.; Dwyer, Nicole] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Erlandson, Jon M.; Jew, Nicholas P.; Kennett, Douglas J.] 1218 Univ Oregon, Dept Anthropol, Eugene, OR USA. [Braje, Todd J.] Humboldt State Univ, Dept Anthropol, Arcata, CA 95521 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Ainis, Amira F.; Vellanoweth, Rene L.] Calif State Univ Los Angeles, Dept Anthropol, Los Angeles, CA 90032 USA. [Watts, Jack] Univ Oxford, Dept Archaeol, Oxford, England. RP Erlandson, JM (reprint author), Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. EM jerland@uoregon.edu; tjb50@humboldt.edu; rickt@si.edu; njew@uoregon.edu; dkennett@uoregon.edu; ndwyer@uoregon.edu; ami_banter@hotmail.com; rvellan@exchange.calstatela.edu; jack.watts@gmail.com RI Kennett, Douglas/I-7613-2015; OI Kennett, Douglas/0000-0001-5133-9010; Erlandson, Jon/0000-0002-4705-4319 FU National Science Foundation; Marine Conservation Biology Institute; Channel Islands National Park; Western National Parks Association; Foundation for Exploration and Research on Cultural Origins FX This research was inspired and encouraged by discussions with marine ecologists Paul Dayton, Robert DeLong, Jim Estes, Michael Graham, David Lindberg, Jeremy Jackson, Dan Richards, and Robert Steneck. Funds to support our field and laboratory research were provided by grants from the National Science Foundation, the Marine Conservation Biology Institute, Channel Islands National Park, the Western National Parks Association, the Foundation for Exploration and Research on Cultural Origins, and our home institutions. At Channel Islands National Park, we are indebted to Ann Huston, Kelly Minas, and Ian Williams for their logistical support. Many people have helped us measure Lottia shells in the field and the lab, including Molly Casperson, Robert DeLong, Erik Erlandson, Keith Hamm, Anders Mickelson, and Quntan Shup. Finally, we are grateful to Kent Lightfoot, anonymous reviewers, and the editors for their help in the review, revision, and production of this paper. NR 73 TC 29 Z9 29 U1 1 U2 30 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 MAY PY 2011 VL 38 IS 5 BP 1127 EP 1134 DI 10.1016/j.jas.2010.12.009 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 745PR UT WOS:000289178600019 ER PT J AU Chisholm, RA Pacala, SW AF Chisholm, Ryan A. Pacala, Stephen W. TI Theory predicts a rapid transition from niche-structured to neutral biodiversity patterns across a speciation-rate gradient SO THEORETICAL ECOLOGY LA English DT Article DE Biodiversity; Community ecology; Neutral theory; Niche model; Emergent pattern; Speciation rate ID RELATIVE SPECIES ABUNDANCE; COMMUNITY STRUCTURE; TROPICAL FORESTS; RAIN-FORESTS; CORAL-REEFS; ECOLOGY; DIVERSITY; BIOGEOGRAPHY; MODEL; SCALE AB A central challenge in community ecology is to predict patterns of biodiversity with mechanistic models. The neutral model of biodiversity is a simple model that appears to provide parsimonious and accurate predictions of biodiversity patterns in some ecosystems, even though it ignores processes such as species interactions and niche structure. In a recent paper, we used analytical techniques to reveal why the mean predictions of the neutral model are robust to niche structure in high diversity but not low-diversity ecosystems. In the present paper, we explore this phenomenon further by generating stochastic simulated data from a spatially implicit hybrid niche-neutral model across different speciation rates. We compare the resulting patterns of species richness and abundance with the patterns expected from a pure neutral and a pure niche model. As the speciation rate in the hybrid model increases, we observe a surprisingly rapid transition from an ecosystem in which diversity is almost entirely governed by niche structure to one in which diversity is statistically indistinguishable from that of the neutral model. Because the transition is rapid, one prediction of our abstract model is that high-diversity ecosystems such as tropical forests can be approximated by one simple model-the neutral model-whereas low-diversity ecosystems such as temperate forests can be approximated by another simple model-the niche model. Ecosystems that require the hybrid model are predicted to be rare, occurring only over a narrow range of speciation rates. C1 [Chisholm, Ryan A.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. [Chisholm, Ryan A.; Pacala, Stephen W.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. RP Chisholm, RA (reprint author), Smithsonian Trop Res Inst, MRC0580-12,Unit 9100,Box 0948, Dpo, AA 34002 USA. EM ryan.chis@gmail.com RI Chisholm, Ryan/H-8033-2012 FU STRI; SIGEO/CTFS FX We thank Rampal Etienne for advice on running his code. We thank James Rosindell for helpful discussions. R. A. C. acknowledges STRI and SIGEO/CTFS for financial support. NR 40 TC 8 Z9 9 U1 1 U2 44 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1874-1738 J9 THEOR ECOL-NETH JI Theor. Ecol. PD MAY PY 2011 VL 4 IS 2 SI SI BP 195 EP 200 DI 10.1007/s12080-011-0113-5 PG 6 WC Ecology SC Environmental Sciences & Ecology GA 749OM UT WOS:000289478100007 ER PT J AU Chisholm, RA Muller-Landau, HC AF Chisholm, Ryan A. Muller-Landau, Helene C. TI A theoretical model linking interspecific variation in density dependence to species abundances SO THEORETICAL ECOLOGY LA English DT Article DE Biodiversity; Relative species abundances; Conspecific inhibition; Negative density dependence; Invasion growth rate; Strength of stabilization ID LIMITING NUTRIENTS; TROPICAL TREE; DIVERSITY; COMPETITION; COMMUNITY; MAINTENANCE; BIODIVERSITY; COEXISTENCE; ENVIRONMENT; PATTERNS AB Understanding the factors that govern the commonness and rarity of individual species is a central challenge in community ecology. Empirical studies have often found that abundance is related to traits associated with competitive ability and suitability to the local environment and, more recently, also to negative conspecific density dependence. Here, we construct a theoretical framework to show how a species' abundance is, in general, expected to be dependent on its per-capita growth rate when rare and the rate at which its growth rate declines with increasing abundance (strength of stabilization). We argue that per-capita growth rate when rare can be interpreted as competitive ability and that strength of stabilization largely reflects negative conspecific inhibition. We then analyze a simple spatially implicit model in which each species is defined by three parameters that affect its juvenile survival: its generalized competitive effect on others, its generalized response to competition, and an additional negative effect on conspecifics. This model facilitates the stable coexistence of an arbitrarily large number of species and qualitatively reproduces empirical relationships between abundance, competitive ability, and negative conspecific density dependence. Our results provide theoretical support for the combined roles of competitive ability and negative density dependence in the determination of species abundances in real ecosystems, and suggest new avenues of research for understanding abundance in models and in real communities. C1 [Chisholm, Ryan A.; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. RP Chisholm, RA (reprint author), Smithsonian Trop Res Inst, Dpo, AA 34002 USA. EM ryan.chis@gmail.com RI Chisholm, Ryan/H-8033-2012 FU Smithsonian Institution Global Earth Observatories (SIGEO); HSBC FX We thank Marco Visser for helpful comments on the manuscript. We thank Simon Levin and David Earn for advice on the stability analysis. We gratefully acknowledge the financial support of the Smithsonian Institution Global Earth Observatories (SIGEO) and the HSBC Climate Partnership. NR 33 TC 13 Z9 13 U1 1 U2 33 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1874-1738 J9 THEOR ECOL-NETH JI Theor. Ecol. PD MAY PY 2011 VL 4 IS 2 SI SI BP 241 EP 253 DI 10.1007/s12080-011-0119-z PG 13 WC Ecology SC Environmental Sciences & Ecology GA 749OM UT WOS:000289478100011 ER PT J AU Bonachea, LA Ryan, MJ AF Bonachea, Luis A. Ryan, Michael J. TI Simulated Predation Risk Influences Female Choice in Tungara Frogs, Physalaemus pustulosus SO ETHOLOGY LA English DT Article ID MATE CHOICE; SEARCH COSTS; BEHAVIOR; COMMUNICATION; PARASITOIDS; COURTSHIP; CRICKET; SONG AB While the presence of predators can influence female mate choice, few studies have investigated how females respond to quantitative variation in predation risk. In addition, we know little of how females respond to multiple, independent cues of risk. In this study, we investigated the effects of simulated predation risk on mate choice in tungara frogs, Physalaemus pustulosus, using the advertisement calls of predatory frogs, variation in ambient light, and simulated distance. Females showed aversion to conspecific calls associated with the calls of predators, and females were significantly less likely to travel perceived longer distances while the calls of predatory frogs were broadcast. In both the laboratory and field, females chose among potential mates significantly faster under higher light levels. Female responses to acoustic cues of predation risk were significantly influenced by light level, but decisions about travel distances were not. These results demonstrate that female choice is strongly influenced by perceived predation risk and that females can simultaneously evaluate quantitative variation in different cues of predation risk. The changes in search behavior and mate evaluation we demonstrate indicate that predation plays a strong role in limiting signal evolution and possibly reproductive isolation. C1 [Bonachea, Luis A.] San Jose State Univ, Dept Biol Sci, San Jose, CA 95192 USA. [Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama. RP Bonachea, LA (reprint author), San Jose State Univ, Dept Biol Sci, 1 Washington Sq, San Jose, CA 95192 USA. EM luis.bonachea@sjsu.edu NR 27 TC 14 Z9 14 U1 2 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0179-1613 J9 ETHOLOGY JI Ethology PD MAY PY 2011 VL 117 IS 5 BP 400 EP 407 DI 10.1111/j.1439-0310.2011.01889.x PG 8 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 746NR UT WOS:000289254500005 ER PT J AU Green, DJ Hamrick, MW Richmond, BG AF Green, David J. Hamrick, Mark W. Richmond, Brian G. TI The effects of hypermuscularity on shoulder morphology in myostatin-deficient mice SO JOURNAL OF ANATOMY LA English DT Article DE muscle mass; muscle-bone interactions; myostatin; shoulders ID CROSS-SECTIONAL GEOMETRY; FIBER-TYPE DISTRIBUTION; INCREASED MUSCLE MASS; AUSTRALOPITHECUS-AFARENSIS; BONE MASS; CRANIOFACIAL MORPHOLOGY; CLIMBING EXERCISE; SKELETAL-MUSCLE; SIZE; PROPORTIONS AB Mechanical loads, particularly those generated by skeletal muscle, play a significant role in determining long-bone shape and strength, but it is less clear how these loads influence the morphology of flat bones like the scapula. While scapular morphology has been shown to vary with locomotor mode in mammals, this study seeks to better understand whether genetically modified muscle size can influence scapular shape in the absence of significant locomotor differences. The soft- and hard-tissue morphological characteristics were examined in 11 hypermuscular, mutant (myostatin-deficient), 20 heterozygote, and 15 wild-type mouse shoulders. Body mass did not significantly differ among the genotype groups, but homozygous mutant and heterozygote mice had significantly larger shoulder muscles than wild-type mice. Mutant mice also differed significantly from the wild-type controls in several aspects of scapular size and shape, including glenohumeral joint orientation, total scapular length, superior border length, and supraspinous and infraspinous fossa length. Conversely, several traits describing superoinferior scapular breadth measures (e.g. total breadth and dorsal scapular fossa breadth) did not significantly differ between mutant and wild-type mice. Since the intrinsic musculature of the scapula is oriented in a mediolateral fashion, it follows that mediolaterally configured hard-tissue features like scapular length were most distinct among genotype groups. As had been noted previously with long bones, this study demonstrates that genetically enhanced muscle size has marked effects on the morphological characteristics of the shoulder. C1 [Green, David J.; Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Hamrick, Mark W.] Med Coll Georgia, Dept Cellular Biol & Anat, Augusta, GA 30912 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Green, DJ (reprint author), George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, 2110 G St NW, Washington, DC 20052 USA. EM djgreen6@gmail.com RI Hamrick, Mark/K-1131-2016 FU National Science Foundation (NSF) [9987590, BCS-0824552]; National Institutes of Health [AR049717] FX We wish to thank Drs. Bernard Wood, Robin Bernstein, L. Patricia Hernandez, Stefan Milz, and three anonymous reviewers for critical comments on an earlier draft of this manuscript and the following funding sources: National Science Foundation IGERT grant (9987590), NSF Doctoral Dissertation Improvement Grant (BCS-0824552), and the National Institutes of Health (AR049717). NR 67 TC 4 Z9 4 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8782 EI 1469-7580 J9 J ANAT JI J. Anat. PD MAY PY 2011 VL 218 IS 5 BP 544 EP 557 DI 10.1111/j.1469-7580.2011.01351.x PG 14 WC Anatomy & Morphology SC Anatomy & Morphology GA 745JR UT WOS:000289162200007 PM 21332716 ER PT J AU Fulford, RS Breitburg, DL Luckenbach, M AF Fulford, Richard S. Breitburg, Denise L. Luckenbach, Mark TI Differences in Relative Predation Vulnerability Between Native and Non-native Oyster Larvae and the Influence on Restoration Planning in an Estuarine Ecosystem SO ESTUARIES AND COASTS LA English DT Article DE Oyster; Larvae; Ecosystem management; Estuary ID CTENOPHORE MNEMIOPSIS-LEIDYI; MARINE INVERTEBRATE LARVAE; CHESAPEAKE BAY; CRASSOSTREA-VIRGINICA; CHRYSAORA-QUINQUECIRRHA; GELATINOUS ZOOPLANKTON; CHASMODES-BOSQUIANUS; BIVALVE VELIGERS; EASTERN OYSTERS; GOBIOSOMA-BOSC AB The costs and benefits of non-native introductions as a restoration tool should be estimated prior to any action to prevent both undesirable consequences and waste of restoration resources. The suggested introduction of non-native oyster species, Crassostrea ariakensis, into Chesapeake Bay, USA, provides a good example in which the survival of non-native oysters may differ from that of native oysters, Crassostrea virginica, during the larval stage. Experiments were conducted to compare the predation vulnerability of native and non-native oyster larvae to different predator types (visual vs. non-visual, benthic vs. pelagic). The results suggest that the non-native larvae are more vulnerable to visual and non-visual pelagic predators. Although vulnerability was similar for larvae exposed to benthic non-visual predators, the consumption of one non-native strain was higher than the consumption of native C. virginica larvae. When vulnerability data are combined with predator feeding rates, the predation mortality for non-native larvae in the wild can be much higher than for native larvae. Small changes in larval mortality rates can yield large changes in total larval delivery to the reef for settlement, so these differences among species may contribute to differences in settlement success. These results provide an example of how a comprehensive examination of the perceived benefits of non-native introductions into complex ecosystems can provide important information to inform management decisions. C1 [Fulford, Richard S.] Univ So Mississippi, Gulf Coast Res Lab, Dept Coastal Sci, Ocean Springs, MS 39564 USA. [Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Luckenbach, Mark] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA. RP Fulford, RS (reprint author), Univ So Mississippi, Gulf Coast Res Lab, Dept Coastal Sci, 703 E Beach Dr, Ocean Springs, MS 39564 USA. EM Richard.Fulford@usm.edu; breitburgd@si.edu; luck@vims.edu FU NOAA Chesapeake Bay Office FX This work would not have been possible without the efforts and advice of many people. We particularly wish to thank Rebecca Morris, Eileen Graham, Spencer Bykowski, Genevieve Smith, and Scott Berg for their help in culturing predators and prey and in conducting the experiments. Dr. Roger Newell gave much useful advice on the experimental setup and provided data on his own experiments involving larval vertical distribution. We thank Stephanie Bonniwell for providing oyster larvae for this study. This work was funded by a grant from the NOAA Chesapeake Bay Office. NR 51 TC 4 Z9 4 U1 3 U2 18 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD MAY PY 2011 VL 34 IS 3 BP 618 EP 629 DI 10.1007/s12237-010-9360-8 PG 12 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 741YC UT WOS:000288902400014 ER PT J AU Waegell, M Aravind, PK Megill, N Pavicic, M AF Waegell, Mordecai Aravind, P. K. Megill, Norman D. Pavicic, Mladen TI Parity Proofs of the Bell-Kochen-Specker Theorem Based on the 600-cell SO FOUNDATIONS OF PHYSICS LA English DT Article DE Bell-Kochen-Specker theorem; 600-cell; Quantum noncontextuality; Quantum cryptography ID QUANTUM CRYPTOGRAPHY; 8-DIMENSIONAL SPACE; HIDDEN VARIABLES; VECTORS; MECHANICS AB The set of 60 real rays in four dimensions derived from the vertices of a 600-cell is shown to possess numerous subsets of rays and bases that provide basis-critical parity proofs of the Bell-Kochen-Specker (BKS) theorem (a basis-critical proof is one that fails if even a single basis is deleted from it). The proofs vary considerably in size, with the smallest having 26 rays and 13 bases and the largest 60 rays and 41 bases. There are at least 90 basic types of proofs, with each coming in a number of geometrically distinct varieties. The replicas of all the proofs under the symmetries of the 600-cell yield a total of almost a hundred million parity proofs of the BKS theorem. The proofs are all very transparent and take no more than simple counting to verify. A few of the proofs are exhibited, both in tabular form as well as in the form of MMP hypergraphs that assist in their visualization. A survey of the proofs is given, simple procedures for generating some of them are described and their applications are discussed. It is shown that all four-dimensional parity proofs of the BKS theorem can be turned into experimental disproofs of noncontextuality. C1 [Waegell, Mordecai; Aravind, P. K.] Worcester Polytech Inst, Dept Phys, Worcester, MA 01609 USA. [Megill, Norman D.] Boston Informat Grp, Lexington, MA 02420 USA. [Pavicic, Mladen] Harvard Univ, Inst Theoret Atom Mol & Opt Phys, Dept Phys, Cambridge, MA 02138 USA. [Pavicic, Mladen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Aravind, PK (reprint author), Worcester Polytech Inst, Dept Phys, Worcester, MA 01609 USA. EM caiw@wpi.edu; paravind@wpi.edu; mpavicic@grad.hr FU US National Science Foundation; 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 at ITAMP. M. P.'s stay at ITAMP 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 Ministry of Science, Education, and Sport of Croatia through the project No. 082-0982562-3160. M. P. carried out his part of the computation on the cluster Isabella of the University Computing Centre of the University of Zagreb and on the Croatian National Grid Infrastructure. NR 39 TC 6 Z9 6 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0015-9018 J9 FOUND PHYS JI Found. Phys. PD MAY PY 2011 VL 41 IS 5 BP 883 EP 904 DI 10.1007/s10701-011-9534-7 PG 22 WC Physics, Multidisciplinary SC Physics GA 741YR UT WOS:000288904400006 ER PT J AU Bottger-Schnack, R Machida, RJ AF Boettger-Schnack, Ruth Machida, Ryuji J. TI Comparison of morphological and molecular traits for species identification and taxonomic grouping of oncaeid copepods SO HYDROBIOLOGIA LA English DT Article DE Copepoda; Oncaeidae; Taxonomy; Morphology; DNA barcoding; 12S; COI mt; Mediterranean Sea ID RED-SEA; PHYLOGENETIC POSITION; VERTICAL-DISTRIBUTION; MITOCHONDRIAL-DNA; CALANOID COPEPODS; SP NOV.; POECILOSTOMATOIDA; CYCLOPOIDA; SHMELEVA; GENUS AB The pelagic marine copepod family Oncaeidae is highly diversified (over 100 species worldwide) and includes a great number of sibling species, which are difficult to identify morphologically, because of their very small size (0.18-1.2 mm total length as adults). Global investigations of oncaeid biodiversity are severely hampered by insufficient taxonomic knowledge, in particular for species which have first been described from the European Mediterranean Sea (type locality). Many of these species have been reported as key taxa of small-sized copepod communities in very distant oceanic regions. However, due to the taxonomic uncertainties it cannot be excluded that at least some of these allegedly cosmopolitan species in reality represent a complex of distinct, yet closely related, species. To improve the basis for the identification of Oncaeidae of Mediterranean origin, new diagnostic characters in combination with traditional methods were applied in the present study. Copepods were sampled with fine nets of 0.1 mm mesh size down to a maximum depth of 1,000 m on a west-east-transect in the Mediterranean Sea. Oncaeid species and form variants were predefined morphologically and the genetic identity of the morphospecies was analysed by about 650 and 500 bp region of the mitochondrial COI and 12S srRNA gene sequence, respectively (barcoding). A total of 67 individuals from 24 oncaeid species and forms were successfully analysed, including 12 species and one form of Mediterranean origin. For Oncaeidae, the 12S amplification turned out to be more successful (23 species) than the COI amplification (13 species and 1 form). Together, the morphological and molecular results are discussed with respect to three topics: (1) confirmation of a genetic distinction of three Triconia species, which have been interpreted as sibling species by morphological characters, (2) genetic distance of species within the ovalis-complex of oncaeids and (3) the taxonomic status of two form variants of Oncaea mediterranea (Claus). C1 [Boettger-Schnack, Ruth] Leibniz Inst Marine Sci IFM GEOMAR, Biol Oceanog FB2, D-24105 Kiel, Germany. [Machida, Ryuji J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Bottger-Schnack, R (reprint author), Moorsehdener Weg 8, D-24211 Rastorf Rosenfeld, Germany. EM dschnack@ifm-geomar.de FU German Science Foundation [Schn 455/4-1, Schn 455/5-1]; Alfred P. Sloan Foundation; Ministry of Education, Culture, Sports, Science and Technology of Japan [20241003] FX We wish to thank D. Elvers (University of Bremen) for collecting the fine mesh net plankton samples during RV 'Meteor' cruise 51/2. Thanks are due to Prof. K. Lochte (formerly IFM-GEOMAR, now AWI, Bremerhaven) and Prof. U. Riebesell (IFM-GEOMAR) for providing excellent working conditions to R. B. S. Special thanks are given to Prof. D. Schnack for commenting on the manuscript and to Elisabeth Samusch for personal support to R. B. S. This study was supported by a research grant from the German Science Foundation to R. B. S (Schn 455/4-1). The funding of travel expenses to the 10th ICOC in Thailand by the German Science Foundation (Schn 455/5-1) is gratefully acknowledged. We gratefully acknowledge the support of the Alfred P. Sloan Foundation. Additional support for this project was provided to R. J. M. by a Grant-in-Aid for Scientific Research No. 20241003 from the Ministry of Education, Culture, Sports, Science and Technology of Japan. Data Integration & Analysis System from the Ministry of Education, Culture, Sports, Science and Technology of Japan provided funding to R. J. M. This study is a contribution from the Census of Marine Zooplankton (CMarZ), an ocean realm field project of the Census of Marine Life. NR 61 TC 13 Z9 19 U1 0 U2 23 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD MAY PY 2011 VL 666 IS 1 BP 111 EP 125 DI 10.1007/s10750-010-0094-1 PG 15 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 743FC UT WOS:000289002100010 ER PT J AU LeBrun, EG Moffett, M Holway, DA AF LeBrun, E. G. Moffett, M. Holway, D. A. TI Convergent evolution of levee building behavior among distantly related ant species in a floodplain ant assemblage SO INSECTES SOCIAUX LA English DT Article DE Formicidae; Nest flooding; Levees; Extended phenotype; Convergent evolution ID ECTATOMMA-OPACIVENTRE ROGER; AGE-POLYETHISM; FORMICIDAE; HYMENOPTERA; PONERINAE; NESTS; ORGANIZATION; VENTILATION; FOREST AB Flooding impacts ground nesting ant colonies by destroying the infrastructure housing and organizing societal function. Here, we report the convergent evolution in distantly related ant species of a behavioral trait that minimizes costs of flooding: the construction of earthen levees around nest entrances. In a South American floodplain ecosystem, we observed five ant species constructing prominent earthen berms encircling nest entrances shortly after large rainfall events. In four of these species, experimental flooding of nests demonstrated that earthen berms sufficed to prevent floodwaters from entering the below ground portions of the nest. Additional manipulations revealed that levee breaching caused, pronounced, and extended reductions in food collection for two distantly related species. Foraging was preempted by the allocation of workers to repair the internal structure of the nest. These findings represent convergent evolution of a functionally important nest construction behavior in response to comparable selective forces. C1 [LeBrun, E. G.] Univ Texas Austin, Sect Integrat Biol, Brackenridge Field Lab, Austin, TX 78703 USA. [Moffett, M.] Smithsonian Inst, Dept Entomol, NMNH, Washington, DC 20560 USA. [Holway, D. A.] Univ Calif San Diego, Div Biol Sci, La Jolla, CA 92093 USA. RP LeBrun, EG (reprint author), Univ Texas Austin, Sect Integrat Biol, Brackenridge Field Lab, 2907 Lake Austin Blvd, Austin, TX 78703 USA. EM elebrun@mail.utexas.edu; naturalist@erols.com; dholway@biomail.ucsd.edu FU National Science Foundation [DEB 07-16966] FX We would like to thank Shawn Wilder, Melissa Wells, the owners and staff of the Hotel Ychoalay (Villa Ocampo), and I.C. Quilmes for assisting and supporting fieldwork. We thank Andy Suarez and an anonymous reviewer for helpful comments on the manuscript. We appreciate Oreste Pividori for allowing access to his land, and the Brackenridge Field Laboratory for logisitical support. Christian Rabeling provided assistance with the identification of the Acromyrmex species. The National Science Foundation (DEB 07-16966 to DAH) provided funding. NR 24 TC 6 Z9 6 U1 1 U2 9 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PD MAY PY 2011 VL 58 IS 2 BP 263 EP 269 DI 10.1007/s00040-011-0151-4 PG 7 WC Entomology SC Entomology GA 736SZ UT WOS:000288515700016 ER PT J AU Goldsmith, GR Comita, LS Chua, SC AF Goldsmith, Gregory R. Comita, Liza S. Chua, Siew Chin TI Evidence for arrested succession within a tropical forest fragment in Singapore SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Bukit Timah; forest dynamics plot; forest fragmentation; leaf litter; secondary forest; seedling regeneration ID SECONDARY FORESTS; RAIN-FOREST; TREE SEEDLINGS; LITTER; LIGHT; CONSERVATION; REGENERATION; DYNAMICS; SOIL C1 [Goldsmith, Gregory R.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Comita, Liza S.] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Chua, Siew Chin] Nanyang Technol Univ, Natl Inst Educ, Asia Programme Nat Sci & Sci Educ, Ctr Trop Forest Sci Arnold Arboretum, Singapore 637616, Singapore. RP Goldsmith, GR (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM grgoldsmith@berkeley.edu OI Comita, Liza/0000-0002-9169-1331 FU Freeman Foundation for Asian Studies; NSF; National Center for Ecological Analysis and Synthesis FX S. Letcher and two anonymous reviewers provided valuable comments. K. Shono and S.K.Y. Lum provided field assistance. The National Parks Board, Singapore and the Center for Tropical Forest Science granted permission to work in BTNR and the forest dynamics plot, respectively. This research is supported by a grant from the Freeman Foundation for Asian Studies and an NSF Graduate Research Fellowship to G.R. Goldsmith. L.S. Comita acknowledges fellowship support from the National Center for Ecological Analysis and Synthesis. NR 23 TC 12 Z9 12 U1 3 U2 28 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 MAY PY 2011 VL 27 BP 323 EP 326 DI 10.1017/S0266467411000010 PN 3 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 738DJ UT WOS:000288619200011 ER PT J AU Venegas, RD Hueter, R Cano, JG Tyminski, J Remolina, JG Maslanka, M Ormos, A Weigt, L Carlson, B Dove, A AF de la Parra Venegas, Rafael Hueter, Robert Gonzalez Cano, Jaime Tyminski, John Gregorio Remolina, Jose Maslanka, Mike Ormos, Andrea Weigt, Lee Carlson, Bruce Dove, Alistair TI An Unprecedented Aggregation of Whale Sharks, Rhincodon typus, in Mexican Coastal Waters of the Caribbean Sea SO PLOS ONE LA English DT Article ID GULF-OF-MEXICO; FISH; IDENTIFICATION; POPULATION; BIOLOGY; WESTERN; BELIZE; REEF AB Whale sharks, Rhincodon typus, are often perceived as solitary behemoths that live and feed in the open ocean. To the contrary, evidence is accumulating that they are gregarious and form seasonal aggregations in some coastal waters. One such aggregation occurs annually north of Cabo Catoche, off Isla Holbox on the Yucatan Peninsula of Mexico. Here we report a second, much denser aggregation of whale sharks (dubbed "the Afuera") that occurs east of the tip of the Yucatan Peninsula in the Caribbean Sea. The 2009 Afuera event comprised the largest aggregation of whale sharks ever reported, with up to 420 whale sharks observed in a single aerial survey, all gathered in an elliptical patch of ocean approximately 18 km(2). Plankton studies indicated that the sharks were feeding on dense homogenous patches of fish eggs, which DNA barcoding analysis identified as belonging to little tunny, Euthynnus alletteratus. This contrasts with the annual Cabo Catoche aggregation nearby, where prey consists mostly of copepods and sergestid shrimp. Increased sightings at the Afuera coincide with decreased sightings at Cabo Catoche, and both groups have the same sex ratio, implying that the same animals are likely involved in both aggregations; tagging data support this idea. With two whale shark aggregation areas, high coastal productivity and a previously-unknown scombrid spawning ground, the northeastern Yucatan marine region is a critical habitat that deserves more concerted conservation efforts. C1 [de la Parra Venegas, Rafael; Gonzalez Cano, Jaime; Gregorio Remolina, Jose] Comis Nacl Areas Nat Protegidas, Proyecto Domino, Cancun, Quintana Roo, Mexico. [Tyminski, John] Mote Marine Lab, Ctr Shark Res, Sarasota, FL 34236 USA. [Maslanka, Mike] Smithsonian Conservat Biol Inst, Washington, DC USA. [Ormos, Andrea; Weigt, Lee] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Washington, DC 20560 USA. [Carlson, Bruce; Dove, Alistair] Georgia Aquarium Res Ctr, Atlanta, GA USA. RP Venegas, RD (reprint author), Comis Nacl Areas Nat Protegidas, Proyecto Domino, Cancun, Quintana Roo, Mexico. EM adove@georgiaaquarium.org RI Dove, Alistair/D-1173-2013; OI Dove, Alistair/0000-0003-3239-4772 FU Mote/Project DOMINO [GAI 001]; Project DOMINO [GAI043] FX Authors BC and AD are employees of Georgia Aquarium, which sponsored the research described in the manuscript through co-operative grants GAI#001 (Mote/Project DOMINO) and GAI#043 (Project DOMINO). Both BC and AD participated in study design, field work, data analysis and manuscript preparation. Research and conservation programs of Georgia Aquarium are described at http://www.georgiaaquarium.org/support-us/conservation/. NR 22 TC 24 Z9 25 U1 9 U2 45 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 29 PY 2011 VL 6 IS 4 AR e18994 DI 10.1371/journal.pone.0018994 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 756OZ UT WOS:000290024700048 ER PT J AU Sidlauskas, B Bernard, C Bloom, D Bronaugh, W Clementson, M Vari, RP AF Sidlauskas, Brian Bernard, Calvin Bloom, Devin Bronaugh, Whitcomb Clementson, Michael Vari, Richard P. TI LIFE IN SCIENCE Ichthyologists Hooked on Facebook SO SCIENCE LA English DT Letter C1 [Sidlauskas, Brian; Bronaugh, Whitcomb] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Sidlauskas, Brian; Vari, Richard P.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Bernard, Calvin; Clementson, Michael] Univ Guyana, Ctr Study Biol Diversity, E Coast Demerara, Guyana. [Bloom, Devin] Univ Toronto Scarborough, Dept Ecol & Evolutionary Biol, Toronto, ON M1C 1A4, Canada. [Bloom, Devin] Univ Toronto Scarborough, Dept Biol Sci, Toronto, ON M1C 1A4, Canada. RP Sidlauskas, B (reprint author), Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. EM brian.sidlauskas@oregonstate.edu NR 0 TC 5 Z9 5 U1 1 U2 13 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD APR 29 PY 2011 VL 332 IS 6029 BP 537 EP 537 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 756DE UT WOS:000289991100055 PM 21527698 ER PT J AU Elvis, M AF Elvis, Martin TI 'Plan B' for X-ray astronomy SO NATURE LA English DT Letter C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM martinselvis2@gmail.com NR 1 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 28 PY 2011 VL 472 IS 7344 BP 418 EP 418 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 755QC UT WOS:000289949600016 PM 21525915 ER PT J AU Pham, LM Le Sage, D Stanwix, PL Yeung, TK Glenn, D Trifonov, A Cappellaro, P Hemmer, PR Lukin, MD Park, H Yacoby, A Walsworth, RL AF Pham, L. M. Le Sage, D. Stanwix, P. L. Yeung, T. K. Glenn, D. Trifonov, A. Cappellaro, P. Hemmer, P. R. Lukin, M. D. Park, H. Yacoby, A. Walsworth, R. L. TI Magnetic field imaging with nitrogen-vacancy ensembles SO NEW JOURNAL OF PHYSICS LA English DT Article ID DIAMOND; SPIN; IMPLANTATION; CENTERS AB We demonstrate a method of imaging spatially varying magnetic fields using a thin layer of nitrogen-vacancy (NV) centers at the surface of a diamond chip. Fluorescence emitted by the two-dimensional NV ensemble is detected by a CCD array, from which a vector magnetic field pattern is reconstructed. As a demonstration, ac current is passed through wires placed on the diamond chip surface, and the resulting ac magnetic field patterns are imaged using an echo-based technique with sub-micron resolution over a 140 mu m x 140 mu m field of view, giving single-pixel sensitivity similar to 100 nT/root Hz. We discuss ongoing efforts to further improve the sensitivity, as well as potential bioimaging applications such as real-time imaging of activity in functional, cultured networks of neurons. C1 [Le Sage, D.; Stanwix, P. L.; Glenn, D.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pham, L. M.; Yeung, T. K.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Yeung, T. K.; Trifonov, A.; Lukin, M. D.; Park, H.; Yacoby, A.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Trifonov, A.] Ioffe Phys Tech Inst RAS, St Petersburg, Russia. [Cappellaro, P.] MIT, Nucl Sci & Engn Dept, Cambridge, MA 02139 USA. [Hemmer, P. R.] Texas AM Univ, Dept Elect & Comp Engn, College Stn, TX 77843 USA. [Park, H.] Harvard Univ, Chem & Chem Biol Dept, Cambridge, MA 02138 USA. RP Walsworth, RL (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM rwalsworth@cfa.harvard.edu RI Cappellaro, Paola/B-1413-2010; Stanwix, Paul/A-5280-2009; OI Cappellaro, Paola/0000-0003-3207-594X; Stanwix, Paul/0000-0002-7069-8569; Le Sage, David/0000-0003-1678-9491 FU NIST; NSF; DARPA FX This work was supported by NIST, NSF and DARPA. We gratefully acknowledge the provision of diamond samples by Apollo Diamond, Inc. and technical discussions with Patrick Doering, Jeronimo Maze and Daniyar Nurgaliev. NR 29 TC 80 Z9 81 U1 10 U2 65 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD APR 28 PY 2011 VL 13 AR 045021 DI 10.1088/1367-2630/13/4/045021 PG 13 WC Physics, Multidisciplinary SC Physics GA 756EO UT WOS:000289994700003 ER PT J AU Nagele, S Pazourek, R Feist, J Doblhoff-Dier, K Lemell, C Tokesi, K Burgdorfer, J AF Nagele, S. Pazourek, R. Feist, J. Doblhoff-Dier, K. Lemell, C. Tokesi, K. Burgdoerfer, J. TI Time-resolved photoemission by attosecond streaking: extraction of time information SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID PULSES; SPECTROSCOPY; IONIZATION; COULOMB; FIELDS; DELAY AB Attosecond streaking of atomic photoemission holds the promise to provide unprecedented information on the release time of the photoelectron. We show that attosecond streaking phase shifts indeed contain timing (or spectral phase) information associated with the Eisenbud-Wigner-Smith time delay matrix of quantum scattering. However, this is only accessible if the influence of the streaking infrared (IR) field on the emission process is properly accounted for. The IR probe field can strongly modify the observed streaking phase shift. We show that the part of the phase shift ('time shift') due to the interaction between the outgoing electron and the combined Coulomb and IR laser fields can be described classically. By contrast, the strong initial-state dependence of the streaking phase shift is only revealed through the solution of the time-dependent Schrodinger equation in its full dimensionality. We find a time delay between the hydrogenic 2s and 2p initial states in He+ exceeding 20 as for a wide range of IR intensities and XUV energies. C1 [Nagele, S.; Pazourek, R.; Doblhoff-Dier, K.; Lemell, C.; Burgdoerfer, J.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. [Feist, J.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Tokesi, K.] Hungarian Acad Sci ATOMKI, Inst Nucl Res, H-4001 Debrecen, Hungary. RP Nagele, S (reprint author), Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. EM stefan.nagele@tuwien.ac.at; renate.pazourek@tuwien.ac.at RI Nagele, Stefan/E-6938-2011; Lemell, Christoph/B-5147-2009; Feist, Johannes/J-7394-2012; Doblhoff-Dier, Katharina/R-5880-2016 OI Nagele, Stefan/0000-0003-1213-0294; Lemell, Christoph/0000-0003-2560-4495; Feist, Johannes/0000-0002-7972-0646; FU FWF-Austria [SFB016, P21141-N16]; TeT [AT-2/2009]; European COST Action [CM0702]; National Science Foundation [TG-PHY090031] FX This work was supported by the FWF-Austria, grant nos SFB016 and P21141-N16, the TeT under grant no AT-2/2009, the European COST Action CM0702, and in part by the National Science Foundation through TeraGrid resources provided by NICS and TACC under grant TG-PHY090031. The computational results presented have also been achieved in part using the Vienna Scientific Cluster (VSC). JF acknowledges support by the NSF through a grant to ITAMP. The authors thank K Schafer for introducing them to the restricted ionization model and acknowledge valuable discussions with U Thumm and C H Zhang. NR 29 TC 78 Z9 78 U1 1 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD APR 28 PY 2011 VL 44 IS 8 AR 081001 DI 10.1088/0953-4075/44/8/081001 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 748SM UT WOS:000289411700001 ER PT J AU Norrbom, AL Uchoa, MA AF Norrbom, Allen L. Uchoa, Manoel A. TI New species and records of Anastrepha (Diptera: Tephritidae) from Brazil SO ZOOTAXA LA English DT Article DE fruit flies; taxonomy ID FRUIT-FLIES DIPTERA; TEPHRITOIDEA; TOCANTINS; STATE AB Three new species of Anastrepha from Brazil are described and illustrated: A. matogrossensis Norrbom & Uchoa (from Mato Grosso), A. oiapoquensis Norrbom & Uchoa (from Amapa), and A. siculigera Norrbom & Uchoa (from Amapa). Anastrepha rafaeli Norrbom & Korytkowski also is reported from the state of Tocantins. C1 [Norrbom, Allen L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, Washington, DC 20013 USA. [Uchoa, Manoel A.] UFGD, Dourados, MS, Brazil. RP Norrbom, AL (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM allen.norrbom@ars.usda.gov; uchoa.manoel@gmail.com FU Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES Foundation, Brazil) FX We thank Rose Benedita Rodrigues Trindade and Darcy Alves do Bomfim who collected some of the examined specimens in projects supported by grants from Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES Foundation, Brazil). We also thank Keiko Uramoto, Roberto Zucchi, and Norman Woodley for their review of this manuscript, and Lucrecia Rodriguez, who enhanced the images. NR 13 TC 7 Z9 7 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 APR 28 PY 2011 IS 2835 BP 61 EP 67 PG 7 WC Zoology SC Zoology GA 755LI UT WOS:000289932300005 ER PT J AU Hultgren, KM MacDonald, KS Duffy, E AF Hultgren, Kristin M. MacDonald, Kenneth S., III Duffy, Emmett TI Sponge-dwelling snapping shrimps (Alpheidae: Synalpheus) of Barbados, West Indies, with a description of a new eusocial species SO ZOOTAXA LA English DT Article DE Decapoda; Caridea; Synalpheus; shrimp; symbiotic; coral reef; eusociality; new species; new records ID CRUSTACEA; DECAPODA AB Sampling of eight sites along the west coast of Barbados, West Indies, yielded 14 species of sponge-dwelling shrimps in the gambarelloides group of the genus Synalpheus, including one new species described here as Synalpheus microneptunus n. sp. The new species is a member of the S. paraneptunus Coutiere species complex and is distinguished from other species in that group by the combination of four carpal segments in the second pereopod, uropodal exopod with 2(nd) disto-lateral tooth smaller than the other two teeth and set in line with movable spine, and a small blade on the scaphocerite. Synalpheus microneptunus n. sp. is the smallest species in the complex (2.2-2.9 mm CL) and lives in small colonies, usually with fewer than 10 individuals, often with a single breeding female. Synalpheus thele Macdonald, Hultgren & Duffy is reported for the first time from outside its type locality in Jamaica. Sampling in Barbados produced fewer species than did similar efforts in Jamaica and Curacao, possibly due to the relatively isolated position of the island at the eastern (windward) edge of the Caribbean Sea. C1 [Hultgren, Kristin M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [MacDonald, Kenneth S., III] New Mexico State Univ, Dept Biol, Las Cruces, NM 88003 USA. [Duffy, Emmett] Coll William & Mary, Virginia Inst Marine Sci, Williamsburg, VA 23187 USA. RP Hultgren, KM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, MRC 163,POB 37012, Washington, DC 20013 USA. EM krhultgren@gmail.com; tripp@nmsu.edu; jeduffy@vims.edu RI Hultgren, Kristin/F-6862-2011; Macdonald, Kenneth/F-9822-2011 FU National Geographic Society; Smithsonian Marine Science Network FX We are grateful to Judith Mendes (Director) and the staff of the Bellairs Research Station, as well as Mr. John Anthony Husband of St. Lucy for facilitating our field research, and to the Barbados Coastal Zone Management Unit for permission to collect and export specimens. This manuscript was improved by comments by two anonymous reviewers. The National Geographic Society and the Smithsonian Marine Science Network provided financial support. This is VIMS contribution number 3152. NR 32 TC 7 Z9 8 U1 0 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 27 PY 2011 IS 2834 BP 1 EP 16 PG 16 WC Zoology SC Zoology GA 754UR UT WOS:000289883700001 ER PT J AU Moser, WE Richardson, DJ Hammond, CI Lazo-Wasem, E AF Moser, William E. Richardson, Dennis J. Hammond, Charlotte I. Lazo-Wasem, Eric TI Molecular Characterization of Helobdella modesta (Verrill, 1872) (Hirudinida: Glossiphoniidae) from its type locality, West River and Whitneyville Lake, New Haven County, Connecticut, USA SO ZOOTAXA LA English DT Letter ID MITOCHONDRIAL GENE-SEQUENCES; LEECH FAMILY GLOSSIPHONIIDAE; MORPHOLOGICAL DATA; PHYLOGENY C1 [Moser, William E.] Museum Support Ctr MRC 534, Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Dept Biol Sci, Hamden, CT 06518 USA. [Lazo-Wasem, Eric] Yale Univ, Div Invertebrate Zool, Peabody Museum Nat Hist, New Haven, CT 06520 USA. RP Moser, WE (reprint author), Museum Support Ctr MRC 534, Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu; Dennis.Richardson@quinnipiac.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu NR 18 TC 6 Z9 6 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 APR 27 PY 2011 IS 2834 BP 65 EP 68 PG 4 WC Zoology SC Zoology GA 754UR UT WOS:000289883700006 ER PT J AU Knowlton, N AF Knowlton, Nancy TI Q&A Nancy Knowlton SO CURRENT BIOLOGY LA English DT Editorial Material C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Knowlton, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. EM knowlton@si.edu NR 0 TC 0 Z9 0 U1 0 U2 5 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 APR 26 PY 2011 VL 21 IS 8 BP R270 EP R271 PG 2 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 757DA UT WOS:000290063400002 PM 21667526 ER PT J AU Schwarz, MP Tierney, SM Rehan, SM Chenoweth, LB Cooper, SJB AF Schwarz, Michael P. Tierney, Simon M. Rehan, Sandra M. Chenoweth, Luke B. Cooper, Steven J. B. TI The evolution of eusociality in allodapine bees: workers began by waiting SO BIOLOGY LETTERS LA English DT Article DE forager castes; social evolution; evo-devo ID SOCIAL EVOLUTION; HYMENOPTERA; APIDAE; ANTHOPHORIDAE; XYLOCOPINAE; BEHAVIOR; FITNESS; BIOLOGY AB Understanding how sterile worker castes in social insects first evolved is one of the supreme puzzles in social evolution. Here, we show that in the bee tribe Allodapini, the earliest societies did not entail a foraging worker caste, but instead comprised females sharing a nest with supersedure of dominance. Subordinates delayed foraging until they became reproductively active, whereupon they provided food for their own brood as well as for those of previously dominant females. The earliest allodapine societies are, therefore, not consistent with an 'evo-devo' paradigm, where decoupling of foraging and reproductive tasks is proposed as a key early step in social evolution. Important features of these ancestral societies were insurance benefits for dominants, headstart benefits for subordinates and direct reproduction for both. The two lineages where morphologically distinct foraging worker castes evolved both occur in ecosystems with severe constraints on independent nesting and where brood rearing periods are very seasonally restricted. These conditions would have strongly curtailed dispersal options and increased the likelihood that dominance supersedure occurred after brood rearing opportunities were largely degraded. The origins of foraging castes, therefore, represented a shift towards assured fitness gains by subordinates, mediated by the dual constraints of social hierarchies and environmental harshness. C1 [Schwarz, Michael P.; Rehan, Sandra M.; Chenoweth, Luke B.] Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA 5001, Australia. [Tierney, Simon M.] Smithsonian Trop Res Inst, Balboa, Panama. [Rehan, Sandra M.] Brock Univ, Dept Biol Sci, St Catharines, ON L2S 3A1, Canada. [Cooper, Steven J. B.] Univ Adelaide, Ctr Evolutionary Biol & Biodivers, Adelaide, SA 5005, Australia. RP Schwarz, MP (reprint author), Flinders Univ S Australia, Sch Biol Sci, GPO Box 2100, Adelaide, SA 5001, Australia. EM michael.schwarz@flinders.edu.au RI Cooper, Steven/I-6291-2012; Tierney, Simon/H-2410-2015 OI Tierney, Simon/0000-0002-8812-6753 FU Australian Research Council FX We thank Tom Chapman, William Wcislo and four anonymous reviewers for helpful suggestions, Andrew Meade for advice on BAYESMULTISTATE, and Trevor Lehmeyer for figure production. This research was supported by the Australian Research Council. NR 20 TC 24 Z9 25 U1 11 U2 40 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD APR 23 PY 2011 VL 7 IS 2 BP 277 EP 280 DI 10.1098/rsbl.2010.0757 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 733EE UT WOS:000288244100032 PM 20943679 ER PT J AU Cubaynes, S Doherty, PF Schreiber, EA Gimenez, O AF Cubaynes, Sarah Doherty, Paul F., Jr. Schreiber, E. A. Gimenez, Olivier TI To breed or not to breed: a seabird's response to extreme climatic events SO BIOLOGY LETTERS LA English DT Article DE El Nino; intermittent breeding; age at first breeding attempt; mark-recapture; seabirds; sea surface temperature ID ANTARCTIC SEABIRD; EL-NINO; VARIABILITY; CONSEQUENCES; SURVIVAL; OCEAN AB Intermittent breeding is an important life-history strategy that has rarely been quantified in the wild and for which drivers remain unclear. It may be the result of a trade-off between survival and reproduction, with individuals skipping breeding when breeding conditions are below a certain threshold. Heterogeneity in individual quality can also lead to heterogeneity in intermittent breeding. We modelled survival, recruitment and breeding probability of the red-footed booby (Sula sula), using a 19 year mark-recapture dataset involving more than 11 000 birds. We showed that skipping breeding was more likely in El-Nino years, correlated with an increase in the local sea surface temperature, supporting the hypothesis that it may be partly an adaptive strategy of birds to face the trade-off between survival and reproduction owing to environmental constraints. We also showed that the age-specific probability of first breeding attempt was synchronized among different age-classes and higher in El-Nino years. This result suggested that pre-breeders may benefit from lowered competition with experienced breeders in years of high skipping probabilities. C1 [Cubaynes, Sarah; Gimenez, Olivier] Ctr Ecol Fonct & Evolut, UMR 5175, F-34293 Montpellier 5, France. [Cubaynes, Sarah] Inst Math & Modelisat Montpellier, UMR 5149, F-34095 Montpellier 5, France. [Doherty, Paul F., Jr.] Colorado State Univ, Dept Fish Wildlife & Conservat Biol, Ft Collins, CO 80523 USA. [Schreiber, E. A.] Natl Museum Nat Hist, Div Birds, Smithsonian Inst, Washington, DC 20560 USA. RP Cubaynes, S (reprint author), Ctr Ecol Fonct & Evolut, UMR 5175, Campus CNRS,1919 Route Mende, F-34293 Montpellier 5, France. EM sarah.cubaynes@cefe.cnrs.fr RI Gimenez, Olivier/G-4281-2010 FU French Research National Agency (ANR) [ANR-08-JCJC-0028-01]; Languedoc-Roussillon region; U.S. Department of Defence FX This work was partly supported by a grant from the French Research National Agency (ANR), reference ANR-08-JCJC-0028-01. P. F. D. thanks the Languedoc-Roussillon region for funding during a sabbatical at Universite Montpellier 2. E. A. S. thanks the U.S. Fish and Wildlife Service or permission to conduct this study and the U.S. Department of Defence for funding. NR 18 TC 37 Z9 38 U1 7 U2 52 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD APR 23 PY 2011 VL 7 IS 2 BP 303 EP 306 DI 10.1098/rsbl.2010.0778 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 733EE UT WOS:000288244100039 PM 20943677 ER PT J AU Mathy, CJM Parish, MM Huse, DA AF Mathy, Charles J. M. Parish, Meera M. Huse, David A. TI Trimers, Molecules, and Polarons in Mass-Imbalanced Atomic Fermi Gases SO PHYSICAL REVIEW LETTERS LA English DT Article ID PHASE-DIAGRAM AB We consider the ground state of a single "spin-down" impurity atom interacting attractively with a "spin-up" atomic Fermi gas. By constructing variational wave functions for polarons, molecules, and trimers, we perform a detailed study of the transitions between these dressed bound states as a function of mass ratio r = m(up arrow)/m(down arrow) and interaction strength. Crucially, we find that the presence of a Fermi sea enhances the stability of the p-wave trimer, which can be viewed as a Fulde-Ferrell-Larkin-Ovchinnikov molecule that has bound an additional majority atom. For sufficiently large r, we find that the transitions lie outside the region of phase separation of the imbalanced Fermi gas and should thus be observable in experiment, unlike the well-studied equal-mass case. C1 [Mathy, Charles J. M.; Parish, Meera M.; Huse, David A.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Mathy, Charles J. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Parish, Meera M.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. RP Mathy, CJM (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. RI Parish, Meera/E-5102-2013 FU ARO [W911NF-07-1-0464]; DARPA; EPSRC [EP/H00369X/1] FX This work was supported under ARO Grant No. W911NF-07-1-0464 with funds from the DARPA OLE Program. M. M. P. acknowledges support from the EPSRC under Grant No. EP/H00369X/1. C.J.M.M. acknowledges support from the NSF through ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. NR 20 TC 47 Z9 47 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD APR 22 PY 2011 VL 106 IS 16 AR 166404 DI 10.1103/PhysRevLett.106.166404 PG 4 WC Physics, Multidisciplinary SC Physics GA 757OL UT WOS:000290097500012 PM 21599393 ER PT J AU Butler, RJ Benson, RBJ Carrano, MT Mannion, PD Upchurch, P AF Butler, Richard J. Benson, Roger B. J. Carrano, Matthew T. Mannion, Philip D. Upchurch, Paul TI Sea level, dinosaur diversity and sampling biases: investigating the 'common cause' hypothesis in the terrestrial realm SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE diversity; sea level; sampling; dinosaur; Mesozoic ID FOSSIL RECORD; ROCK-RECORD; TAXONOMIC DIVERSITY; BIODIVERSITY; EXTINCTION; HETEROGENEITY; COMPLETENESS; VERTEBRATES; DYNAMICS; HISTORY AB The fossil record is our primary window onto the diversification of ancient life, but there are widespread concerns that sampling biases may distort observed palaeodiversity counts. Such concerns have been reinforced by numerous studies that found correlations between measures of sampling intensity and observed diversity. However, correlation does not necessarily mean that sampling controls observed diversity: an alternative view is that both sampling and diversity may be driven by some common factor (e. g. variation in continental flooding driven by sea level). The latter is known as the 'common cause' hypothesis. Here, we present quantitative analyses of the relationships between dinosaur diversity, sampling of the dinosaur fossil record, and changes in continental flooding and sea level, providing new insights into terrestrial common cause. Although raw data show significant correlations between continental flooding/sea level and both observed diversity and sampling, these correlations do not survive detrending or removal of short-term autocorrelation. By contrast, the strong correlation between diversity and sampling is robust to various data transformations. Correlations between continental flooding/sea level and taxic diversity/sampling result from a shared upward trend in all data series, and short-term changes in continental flooding/sea level and diversity/sampling do not correlate. The hypothesis that global dinosaur diversity is tied to sea-level fluctuations is poorly supported, and terrestrial common cause is unsubstantiated as currently conceived. Instead, we consider variation in sampling to be the preferred null hypothesis for short-term diversity variation in the Mesozoic terrestrial realm. C1 [Butler, Richard J.] Bayer Staatssammlung Palaontol & Geol, D-80333 Munich, Germany. [Benson, Roger B. J.] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England. [Carrano, Matthew T.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Mannion, Philip D.; Upchurch, Paul] UCL, Dept Earth Sci, London WC1E 6BT, England. RP Butler, RJ (reprint author), Bayer Staatssammlung Palaontol & Geol, Richard Wagner Str 10, D-80333 Munich, Germany. EM r.butler@lrz.uni-muenchen.de RI Mannion, Philip/B-3159-2011; Benson, Roger/A-1252-2011; Upchurch, Paul/C-1654-2008; Butler, Richard/A-5239-2011; Carrano, Matthew/C-7601-2011; OI Butler, Richard/0000-0003-2136-7541; Carrano, Matthew/0000-0003-2129-1612; Benson, Roger/0000-0001-8244-6177 FU Alexander von Humboldt FX This study is Palaeobiology Database official publication 121. We thank Paul Barrett for useful discussion, and Stephen Brusatte, Graeme Lloyd and Alistair McGowan for comments on an earlier version of the manuscript. Shanan Peters and an anonymous referee provided helpful reviews. R.J.B. is supported by an Alexander von Humboldt Research Fellowship. NR 44 TC 58 Z9 58 U1 0 U2 16 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD APR 22 PY 2011 VL 278 IS 1709 BP 1165 EP 1170 DI 10.1098/rspb.2010.1754 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 733DM UT WOS:000288241300006 PM 20880889 ER PT J AU Desert, JM Bean, J Kempton, EMR Berta, ZK Charbonneau, D Irwin, J Fortney, J Burke, CJ Nutzman, P AF Desert, Jean-Michel Bean, Jacob Kempton, Eliza Miller-Ricci Berta, Zachory K. Charbonneau, David Irwin, Jonathan Fortney, Jonathan Burke, Christopher J. Nutzman, Philip TI OBSERVATIONAL EVIDENCE FOR A METAL-RICH ATMOSPHERE ON THE SUPER-EARTH GJ1214b SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: observational; planetary systems; techniques: photometric ID SPITZER-SPACE-TELESCOPE; EXOPLANET HD 189733B; GJ 1214B; EXTRASOLAR PLANET; SOLID EXOPLANETS; MASS; CHEMISTRY; SEARCH; GAS AB We report observations of two consecutive transits of the warm super-Earth exoplanet GJ 1214b at 3.6 and 4.5 mu m with the Infrared Array Camera instrument on board the Spitzer Space Telescope. The two transit light curves allow for the determination of the transit parameters for this system. We find these parameters to be consistent with the previously determined values and no evidence for transit timing variations. The main investigation consists of measuring the transit depths in each bandpass to constrain the planet's transmission spectrum. Fixing the system scale and impact parameters, we measure R-p/R-star = 0.1176(-0.0009)(+0.0008) and 0.1163(-0.0008)(+0.0010) at 3.6 and 4.5 mu m, respectively. Combining these data with the previously reported MEarth Observatory measurements in the red optical allows us to rule out a cloud-free, solar composition (i.e., hydrogen-dominated) atmosphere at 4.5 sigma confidence. This independently confirms a recent finding that was based on a measurement of the planet's transmission spectrum using the Very Large Telescope (VLT). The Spitzer, MEarth, and VLT observations together yield a remarkably flat transmission spectrum over the large wavelength domain spanned by the data. Consequently, cloud-free atmospheric models require more than 30% metals (assumed to be in the form of H2O) by volume to be consistent with all the observations. C1 [Desert, Jean-Michel; Bean, Jacob; Berta, Zachory K.; Charbonneau, David; Irwin, Jonathan; Burke, Christopher J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kempton, Eliza Miller-Ricci; Fortney, Jonathan; Nutzman, Philip] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Desert, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdesert@cfa.harvard.edu OI Berta-Thompson, Zachory/0000-0002-3321-4924; Fortney, Jonathan/0000-0002-9843-4354; Charbonneau, David/0000-0002-9003-484X FU California Institute of Technology under NASA; Sagan Fellowship Program FX We thank Bryce Croll, Heather Knutson, Dimitar Sasselov, and Leslie Rogers for 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. We thank the Sagan Fellowship Program, which provides support for J.B. and E.K. NR 35 TC 83 Z9 84 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 APR 20 PY 2011 VL 731 IS 2 AR L40 DI 10.1088/2041-8205/731/2/L40 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797LB UT WOS:000293128100019 ER PT J AU Kirkpatrick, CC McNamara, BR Cavagnolo, KW AF Kirkpatrick, C. C. McNamara, B. R. Cavagnolo, K. W. TI ANISOTROPIC METAL-ENRICHED OUTFLOWS DRIVEN BY ACTIVE GALACTIC NUCLEI IN CLUSTERS OF GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: abundances; galaxies: active; X-rays: galaxies: clusters ID DEEP CHANDRA OBSERVATION; X-RAY CAVITIES; INTRACLUSTER MEDIUM; METALLICITY GRADIENTS; ABUNDANCE PROFILES; VORONOI TESSELLATIONS; ELEMENTAL ABUNDANCES; BUOYANT BUBBLES; IRON ABUNDANCE; STAR-FORMATION AB We present an analysis of the spatial distribution of metal-rich gas in 10 galaxy clusters using deep observations from the Chandra X-ray Observatory. The brightest cluster galaxies (BCGs) have experienced recent active galactic nucleus activity in the forms of bright radio emission, cavities, and shock fronts embedded in the hot atmospheres. The heavy elements are distributed anisotropically and are aligned with the large-scale radio and cavity axes. They are apparently being transported from the halo of the BCG into the intracluster medium along large-scale outflows driven by the radio jets. The radial ranges of the metal-enriched outflows are found to scale with jet power as R-Fe alpha P-jet(0.42) jet, with a scatter of only 0.5 dex. The heavy elements are transported beyond the extent of the inner cavities in all clusters, suggesting that this is a long-lasting effect sustained over multiple generations of outbursts. Black holes in BCGs will likely have difficulty ejecting metal-enriched gas beyond 1 Mpc unless their masses substantially exceed 10(9) M-circle dot C1 [Kirkpatrick, C. C.; McNamara, B. R.; Cavagnolo, K. W.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cavagnolo, K. W.] Observ Cote Azur, UNS, CNRS, Cassiopee UMR 6202, F-06003 Nice, France. RP Kirkpatrick, CC (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada. FU Chandra grant [G07-8122X]; Natural Science and Engineering Research Council of Canada; L'Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX We thank Paul Nulsen and Mike Wise for helpful comments. This work was funded in part by Chandra grant G07-8122X and a generous grant from the Natural Science and Engineering Research Council of Canada. K.W.C. acknowledges financial support from L'Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. NR 42 TC 35 Z9 35 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2011 VL 731 IS 2 AR L23 DI 10.1088/2041-8205/731/2/L23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797LB UT WOS:000293128100002 ER PT J AU Smolcic, V Capak, P Ilbert, O Blain, AW Salvato, M Aretxaga, I Schinnerer, E Masters, D Moric, I Riechers, DA Sheth, K Aravena, M Aussel, H Aguirre, J Berta, S Carilli, CL Civano, F Fazio, G Huang, J Hughes, D Kartaltepe, J Koekemoer, AM Kneib, JP LeFloc'h, E Lutz, D McCracken, H Mobasher, B Murphy, E Pozzi, F Riguccini, L Sanders, DB Sargent, M Scott, KS Scoville, NZ Taniguchi, Y Thompson, D Willott, C Wilson, G Yun, M AF Smolcic, V. Capak, P. Ilbert, O. Blain, A. W. Salvato, M. Aretxaga, I. Schinnerer, E. Masters, D. Moric, I. Riechers, D. A. Sheth, K. Aravena, M. Aussel, H. Aguirre, J. Berta, S. Carilli, C. L. Civano, F. Fazio, G. Huang, J. Hughes, D. Kartaltepe, J. Koekemoer, A. M. Kneib, J. -P. LeFloc'h, E. Lutz, D. McCracken, H. Mobasher, B. Murphy, E. Pozzi, F. Riguccini, L. Sanders, D. B. Sargent, M. Scott, K. S. Scoville, N. Z. Taniguchi, Y. Thompson, D. Willott, C. Wilson, G. Yun, M. TI THE REDSHIFT AND NATURE OF AzTEC/COSMOS 1: A STARBURST GALAXY AT z=4.6 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: distances and redshifts; galaxies: high-redshift; galaxies: starburst ID STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; VLA-COSMOS SURVEY; SUBMILLIMETER GALAXIES; MOLECULAR GAS; PHOTOMETRIC REDSHIFTS; SOURCE CATALOG; POPULATION SYNTHESIS; MAJOR MERGER; FIELD AB Based on broadband/narrowband photometry and Keck DEIMO spectroscopy, we report a redshift of z = 4.64(-0.08)(+0.06) for AzTEC/COSMOS 1, the brightest submillimeter galaxy (SMG) in the AzTEC/COSMOS field. In addition to the COSMOS-survey X-ray to radio data, we report observations of the source with Herschel/PACS (100, 160 mu m), CSO/SHARC II (350 mu m), and CARMA and PdBI (3 mm). We do not detect CO(5 -> 4) line emission in the covered redshift ranges, 4.56-4.76 (PdBI/CARMA) and 4.94-5.02 (CARMA). If the line is within this bandwidth, this sets 3 sigma upper limits on the gas mass to less than or similar to 8 x 10(9) M-circle dot and less than or similar to 5 x 10(10) M-circle dot, respectively (assuming similar conditions as observed in z similar to 2 SMGs). This could be explained by a low CO-excitation in the source. Our analysis of the UV-IR spectral energy distribution of AzTEC 1 shows that it is an extremely young (less than or similar to 50 Myr), massive (M-* similar to 10(11) M-circle dot), but compact (less than or similar to 2 kpc) galaxy, forming stars at a rate of similar to 1300 M-circle dot yr(-1). Our results imply that AzTEC 1 is forming stars in a "gravitationally bound" regime in which gravity prohibits the formation of a superwind, leading to matter accumulation within the galaxy and further generations of star formation. C1 [Smolcic, V.] European So Observ, D-85748 Garching, Germany. [Smolcic, V.] Argelander Inst Astron, D-53121 Bonn, Germany. [Blain, A. W.; Salvato, M.; Masters, D.; Riechers, D. A.; Scoville, N. Z.] CALTECH, Pasadena, CA 91125 USA. [Capak, P.; Sheth, K.] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Ilbert, O.; Kneib, J. -P.; McCracken, H.] Univ Provence, CNRS, Lab Astrophys Marseille, F-13376 Marseille 12, France. [Salvato, M.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Aretxaga, I.; Hughes, D.] INAOE, Puebla 72000, Mexico. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Masters, D.; Mobasher, B.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Moric, I.] Univ Zagreb, Dept Phys, Zagreb 10000, Croatia. [Aravena, M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Aussel, H.] CEA Saclay, UMR AIM CEA CNRS UP7, F-91191 Gif Sur Yvette, France. [Aguirre, J.; Scott, K. S.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Berta, S.; Lutz, D.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Civano, F.; Fazio, G.; Huang, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kartaltepe, J.; LeFloc'h, E.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Pozzi, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Riguccini, L.] Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, CEA DSM Irfu CNRS, F-91191 Gif Sur Yvette, France. [Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. [Willott, C.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Wilson, G.; Yun, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Smolcic, V (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. RI Aravena, Manuel/O-2361-2014; Kneib, Jean-Paul/A-7919-2015; OI Kneib, Jean-Paul/0000-0002-4616-4989; Koekemoer, Anton/0000-0002-6610-2048; Schinnerer, Eva/0000-0002-3933-7677 FU NASA [HST-GO-09822, 1407, 1278386, SSC]; Blancheflor Boncompagni Ludovisi foundation; French Agene National de la Recheche [ANR-07-BLAN-0228]; CNES; Programme National Cosmologie et Galaxies; UKF; DFG; DFG Leibniz Prize [FKZ HA 1850/28-1]; European Union [229517]; NSU/CNRS (France); MPG (Germany); IGN (Spain); Betty Moore Foundation; Eileen and Kenneth Norris Foundation; Caltech Associates; NSF; state of California; state of Illinois; state of Maryland; [HST-HF-51235.01]; [NAS 5-26555]; [STScI]; [GO7-8136A] FX The authors acknowledge the significant cultural role that the summit of Mauna Kea has within the indigenous Hawaiian community; NASA grants HST-GO-09822 (contracts 1407, 1278386; SSC); HST-HF-51235.01 (contract NAS 5-26555; STScI); GO7-8136A; Blancheflor Boncompagni Ludovisi foundation (F.C.); French Agene National de la Recheche fund ANR-07-BLAN-0228; CNES; Programme National Cosmologie et Galaxies; UKF; DFG; DFG Leibniz Prize (FKZ HA 1850/28-1); European Union's Seventh Framework programme (grant agreement 229517); making use of the NASA/IPAC IRSA, by JPL/Caltech, under contract with the National Aeronautics and Space Administration; IRAM PdBI supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain); CARMA supported by the states of California, Illinois, and Maryland, the Gordon and Betty Moore Foundation, the Eileen and Kenneth Norris Foundation, the Caltech Associates, and NSF. NR 53 TC 24 Z9 24 U1 2 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 APR 20 PY 2011 VL 731 IS 2 AR L27 DI 10.1088/2041-8205/731/2/L27 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797LB UT WOS:000293128100006 ER PT J AU Bromley, BC Kenyon, SJ AF Bromley, Benjamin C. Kenyon, Scott J. TI A NEW HYBRID N-BODY-COAGULATION CODE FOR THE FORMATION OF GAS GIANT PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planet-disk interactions; planetary systems; planets and satellites: formation; protoplanetary disks ID TURBULENT PROTOPLANETARY DISKS; EVOLVING PROTOSTELLAR DISKS; PRIMORDIAL SOLAR NEBULA; EARLY KUIPER-BELT; T TAURI STARS; OLIGARCHIC GROWTH; SIZE DISTRIBUTION; DEBRIS DISKS; SNOW LINE; EXTRASOLAR PLANETS AB We describe an updated version of our hybrid N-body-coagulation code for planet formation. In addition to the features of our 2006-2008 code, our treatment now includes algorithms for the one-dimensional evolution of the viscous disk, the accretion of small particles in planetary atmospheres, gas accretion onto massive cores, and the response of N-bodies to the gravitational potential of the gaseous disk and the swarm of planetesimals. To validate the N-body portion of the algorithm, we use a battery of tests in planetary dynamics. As a first application of the complete code, we consider the evolution of Pluto-mass planetesimals in a swarm of 0.1-1 cm pebbles. In a typical evolution time of 1-3 Myr, our calculations transform 0.01-0.1 M-circle dot disks of gas and dust into planetary systems containing super-Earths, Saturns, and Jupiters. Low-mass planets form more often than massive planets; disks with smaller alpha form more massive planets than disks with larger alpha. For Jupiter-mass planets, masses of solid cores are 10-100 M-circle plus. C1 [Bromley, Benjamin C.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Bromley, BC (reprint author), Univ Utah, Dept Phys, 201 JFB, Salt Lake City, UT 84112 USA. EM bromley@physics.utah.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA [NNX10AF35G]; NASA TPF Foundation [NNG06GH25G]; Spitzer Guest Observer Program [20132] FX We acknowledge generous allotments of computer time on the NASA "discover" cluster (similar to 1000 cpu days) and on the SI cluster "hydra" (similar to 500 cpu days). Advice and comments from A. Burrows, T. Currie, M. Geller, G. Kennedy, G. Marcy, R. Murray-Clay, H. Perets, D. Spiegel, and A. Youdin greatly improved our presentation. We thank an anonymous referee for comments that clarified many parts of our discussion. Portions of this project were supported by the NASA Astrophysics Theory and Origins of Solar Systems programs through grant NNX10AF35G, the NASA TPF Foundation Science Program, through grant NNG06GH25G, and the Spitzer Guest Observer Program, through grant 20132. NR 160 TC 37 Z9 37 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 APR 20 PY 2011 VL 731 IS 2 AR 101 DI 10.1088/0004-637X/731/2/101 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600024 ER PT J AU Dunham, MK Robitaille, TP Evans, NJ Schlingman, WM Cyganowski, CJ Urquhart, J AF Dunham, Miranda K. Robitaille, Thomas P. Evans, Neal J., II Schlingman, Wayne M. Cyganowski, Claudia J. Urquhart, James TI A MID-INFRARED CENSUS OF STAR FORMATION ACTIVITY IN BOLOCAM GALACTIC PLANE SURVEY SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: stars; ISM: clouds; stars: formation ID INFRARED-DARK CLOUDS; CANDIDATE MASSIVE YSOS; YOUNG STELLAR OBJECTS; H II REGIONS; RMS SURVEY; TRIGONOMETRIC PARALLAXES; MOLECULAR CLOUDS; METHANOL MASERS; (CO)-C-13 OBSERVATIONS; SOUTHERN-HEMISPHERE AB We present the results of a search for mid-infrared signs of star formation activity in the 1.1mm sources in the Bolocam Galactic Plane Survey (BGPS). We have correlated the BGPS catalog with available mid-IR Galactic plane catalogs based on the Spitzer Space Telescope GLIMPSE legacy survey and the Midcourse Space Experiment (MSX) Galactic plane survey. We find that 44% (3712 of 8358) of the BGPS sources contain at least one mid-IR source, including 2457 of 5067 (49%) within the area where all surveys overlap (10 degrees < l < 65 degrees). Accounting for chance alignments between the BGPS and mid-IR sources, we conservatively estimate that 20% of the BPGS sources within the area where all surveys overlap show signs of active star formation. We separate the BGPS sources into four groups based on their probability of star formation activity. Extended Green Objects and Red MSX Sources make up the highest probability group, while the lowest probability group is comprised of "starless" BGPS sources which were not matched to any mid-IR sources. The mean 1.1mm flux of each group increases with increasing probability of active star formation. We also find that the "starless" BGPS sources are the most compact, while the sources with the highest probability of star formation activity are on average more extended with large skirts of emission. A subsample of 280 BGPS sources with known distances demonstrates that mass and mean H-2 column density also increase with probability of star formation activity. C1 [Dunham, Miranda K.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Dunham, Miranda K.; Robitaille, Thomas P.; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Robitaille, Thomas P.; Cyganowski, Claudia J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schlingman, Wayne M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cyganowski, Claudia J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Urquhart, James] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Dunham, MK (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM miranda.dunham@yale.edu OI Robitaille, Thomas/0000-0002-8642-1329 FU University of Texas; NASA; Jet Propulsion Laboratory, California Institute of Technology; National Science Foundation [AST-0708403, AST-0607793, AST-0808119, AST-1003134]; National Radio Astronomy Observatory (NRAO) [GSSP09-0004] FX The authors thank the anonymous referee for insightful comments which have improved this work. We also thank C. Battersby for providing detailed comments. T.P.R. was supported through the University of Texas at Austin Tinsley Visiting Scholar Program and also 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. 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. C.J.C. acknowledges support from NSF grant AST-0808119. C.J.C. was partially supported during this work by a NSF Graduate Research Fellowship, and is currently supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1003134. This paper made use of information from the Red MSX Source (RMS) survey database at http://www.ast.leeds.ac.uk/RMS which was constructed with support from the Science and Technology Facilities Council of the UK. This research has made use of NASA Astrophysics Data System (ADS) Abstract Service and of the SIMBAD database, operated at CDS, Strasbourg, France. NR 73 TC 29 Z9 29 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 APR 20 PY 2011 VL 731 IS 2 AR 90 DI 10.1088/0004-637X/731/2/90 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600013 ER PT J AU Foley, RJ Andersson, K Bazin, G de Haan, T Ruel, J Ade, PAR Aird, KA Armstrong, R Ashby, MLN Bautz, M Benson, BA Bleem, LE Bonamente, M Brodwin, M Carlstrom, JE Chang, CL Clocchiatti, A Crawford, TM Crites, AT Desai, S Dobbs, MA Dudley, JP Fazio, GG Forman, WR Garmire, G George, EM Gladders, MD Gonzalez, AH Halverson, NW High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D Marrone, DP McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Murray, SS Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruhl, JE Saliwanchik, BR Saro, A Schaffer, KK Shaw, L Shirokoff, E Song, J Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Story, K Stubbs, CW Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zenteno, A AF Foley, R. J. Andersson, K. Bazin, G. de Haan, T. Ruel, J. Ade, P. A. R. Aird, K. A. Armstrong, R. Ashby, M. L. N. Bautz, M. Benson, B. A. Bleem, L. E. Bonamente, M. Brodwin, M. Carlstrom, J. E. Chang, C. L. Clocchiatti, A. Crawford, T. M. Crites, A. T. Desai, S. Dobbs, M. A. Dudley, J. P. Fazio, G. G. Forman, W. R. Garmire, G. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Mohr, J. J. Montroy, T. E. Murray, S. S. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Schaffer, K. K. Shaw, L. Shirokoff, E. Song, J. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zenteno, A. TI DISCOVERY AND COSMOLOGICAL IMPLICATIONS OF SPT-CL J2106-5844, THE MOST MASSIVE KNOWN CLUSTER AT z > 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; galaxies: clusters: individual (SPT-CL J2106-5844); galaxies: evolution; galaxies: formation; large-scale structure of universe ID SOUTH-POLE TELESCOPE; IRAC SHALLOW SURVEY; GALAXY CLUSTER; X-RAY; SPECTROSCOPIC CONFIRMATION; VELOCITY DISPERSIONS; ENVIRONMENT; EXTRACTION; PRECISION; REDSHIFTS AB Using the South Pole Telescope (SPT), we have discovered the most massive known galaxy cluster at z > 1, SPT-CL J2106-5844. In addition to producing a strong Sunyaev-Zel'dovich (SZ) effect signal, this system is a luminous X-ray source and its numerous constituent galaxies display spatial and color clustering, all indicating the presence of a massive galaxy cluster. Very Large Telescope and Magellan spectroscopy of 18 member galaxies shows that the cluster is at z = 1.132(-0.003)(+0.002). Chandra observations obtained through a combined HRC-ACIS GTO program reveal an X-ray spectrum with an Fe K line redshifted by z = 1.18 +/- 0.03. These redshifts are consistent with the galaxy colors found in optical, near-infrared, and mid-infrared imaging. SPT-CL J2106-5844 displays extreme X-ray properties for a cluster having a core-excluded temperature of T-X = 11.0(-1.9)(+2.6) keV and a luminosity (within r(500)) of L-X(0.5-2.0 keV) = (13.9 +/- 1.0) x 10(44) erg s(-1). The combined mass estimate from measurements of the SZ effect and X-ray data is M-200 = (1.27 +/- 0.21) x 10(15) h(70)(-1) M-circle dot. The discovery of such amassive gravitationally collapsed system at high redshift provides an interesting laboratory for galaxy formation and evolution, and is a probe of extreme perturbations of the primordial matter density field. We discuss the latter, determining that, under the assumption of Lambda CDM cosmology with only Gaussian perturbations, there is only a 7% chance of finding a galaxy cluster similar to SPT-CL J2106-5844 in the 2500 deg(2) SPT survey region and that only one such galaxy cluster is expected in the entire sky. C1 [Foley, R. J.; Ashby, M. L. N.; Brodwin, M.; Fazio, G. G.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Andersson, K.; Bazin, G.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Andersson, K.; Bautz, M.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bazin, G.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Ruel, J.; Rest, A.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Armstrong, R.; Desai, S.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bonamente, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Desai, S.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Garmire, G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, VP62, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.; Stanford, S. A.] 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. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. RP Foley, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rfoley@cfa.harvard.edu RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Stubbs, Christopher/0000-0003-0347-1724; 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, PHY-0114422, AST-1009012, AST-1009649, MRI-0723073]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA [12800071, 12800088, NAS8-03060]; JPL/Caltech; Chandra X-ray Observatory Center; NASA Office of Space Science; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; Excellence Cluster Universe; DFG [TR33]; Clay Fellowship; KICP Fellowship; W.M. Keck Foundation; Pennsylvania State University [2834-MIT-SAO-4018]; Basal CATA PFB [06/09]; FONDAP [15010003]; Alfred P. Sloan Research Fellowship; Smithsonian Institution; Brinson Foundation FX The South Pole Telescope program is supported by the National Science Foundation through grant ANT-0638937. 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. This work is based in part on observations obtained with the Spitzer Space Telescope (PID 60099), 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. Additional data were obtained with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile. Support for X-ray analysis was provided by NASA through Chandra Project Numbers 12800071 and 12800088 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. Observations from VLT programs 086.A-0741 and 286.A-5021 were included in this work. 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. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. 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. X-ray research at the CfA is supported through NASA Contract NAS 8-03060. The Munich group acknowledges support from the Excellence Cluster Universe and the DFG research program TR33. R.J.F. is supported by a Clay Fellowship. B. A. B. is supported by a KICP Fellowship, support for M. Brodwin was provided by the W.M. Keck Foundation, M. Bautz acknowledges support from contract 2834-MIT-SAO-4018 from the Pennsylvania State University to the Massachusetts Institute of Technology. A.C. acknowledges the support of grants Basal CATA PFB 06/09 and FONDAP No. 15010003. M.D. acknowledges support from an Alfred P. Sloan Research Fellowship, W.F. and C.J. acknowledge support from the Smithsonian Institution, and B.S. acknowledges support from the Brinson Foundation. NR 58 TC 81 Z9 82 U1 1 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 APR 20 PY 2011 VL 731 IS 2 AR 86 DI 10.1088/0004-637X/731/2/86 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600009 ER PT J AU Hickox, RC Myers, AD Brodwin, M Alexander, DM Forman, WR Jones, C Murray, SS Brown, MJI Cool, RJ Kochanek, CS Dey, A Jannuzi, BT Eisenstein, D Assef, RJ Eisenhardt, PR Gorjian, V Stern, D Le Floc'h, E Caldwell, N Goulding, AD Mullaney, JR AF Hickox, Ryan C. Myers, Adam D. Brodwin, Mark Alexander, David M. Forman, William R. Jones, Christine Murray, Stephen S. Brown, Michael J. I. Cool, Richard J. Kochanek, Christopher S. Dey, Arjun Jannuzi, Buell T. Eisenstein, Daniel Assef, Roberto J. Eisenhardt, Peter R. Gorjian, Varoujan Stern, Daniel Le Floc'h, Emeric Caldwell, Nelson Goulding, Andrew D. Mullaney, James R. TI CLUSTERING OF OBSCURED AND UNOBSCURED QUASARS IN THE BOOTES FIELD: PLACING RAPIDLY GROWING BLACK HOLES IN THE COSMIC WEB SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; large-scale structure of universe; quasars: general; surveys ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; LUMINOUS RED GALAXIES; DARK-MATTER HALOES; PHOTOMETRICALLY CLASSIFIED QUASARS; SPECTRAL ENERGY-DISTRIBUTIONS; CROSS-CORRELATION FUNCTION; LARGE-SCALE STRUCTURE; IRAC SHALLOW SURVEY; QSO REDSHIFT SURVEY AB We present the first measurement of the spatial clustering of mid-infrared-selected obscured and unobscured quasars, using a sample in the redshift range 0.7 < z < 1.8 selected from the 9 deg(2) Bootes multiwavelength survey. Recently, the Spitzer Space Telescope and X-ray observations have revealed large populations of obscured quasars that have been inferred from models of the X-ray background and supermassive black hole evolution. To date, little is known about obscured quasar clustering, which allows us to measure the masses of their host dark matter halos and explore their role in the cosmic evolution of black holes and galaxies. In this study, we use a sample of 806 mid-infrared-selected quasars and approximate to 250,000 galaxies to calculate the projected quasar-galaxy cross-correlation function w(p) (R). The observed clustering yields characteristic dark matter halo masses of log(M-halo [h(-1) M-circle dot]) = 12.7(-0.6)(+0.4) and 13.3(-0.4)(+0.3) for unobscured quasars (QSO-1s) and obscured quasars (Obs-QSOs), respectively. The results for QSO-1s are in excellent agreement with previous measurements for optically selected quasars, while we conclude that the Obs-QSOs are at least as strongly clustered as the QSO-1s. We test for the effects of photometric redshift errors on the optically faint Obs-QSOs, and find that our method yields a robust lower limit on the clustering; photo-z errors may cause us to underestimate the clustering amplitude of the Obs-QSOs by at most similar to 20%. We compare our results to previous studies, and speculate on physical implications of stronger clustering for obscured quasars. C1 [Hickox, Ryan C.; Alexander, David M.; Goulding, Andrew D.; Mullaney, James R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Hickox, Ryan C.; Brodwin, Mark; Forman, William R.; Jones, Christine; Murray, Stephen S.; Eisenstein, Daniel; Caldwell, Nelson; Goulding, Andrew D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Myers, Adam D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Cool, Richard J.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Eisenstein, Daniel] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Assef, Roberto J.; Eisenhardt, Peter R.; Gorjian, Varoujan; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Le Floc'h, Emeric; Mullaney, James R.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu CNRS, CE Saclay, F-91191 Gif Sur Yvette, France. RP Hickox, RC (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM ryan.hickox@durham.ac.uk RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Alexander, David/0000-0002-5896-6313; Forman, William/0000-0002-9478-1682 FU NOAO; STFC; SAO; NASA [NNX08AJ28G] FX We thank our colleagues on the NDWFS, AGES, SDWFS, and XBootes teams. We thank the anonymous referee for helpful comments that improved the paper, and Philip Hopkins and Peder Norberg for productive discussions. The NOAO Deep Wide-field Survey, and the research of A.D. and B.T.J. are supported by NOAO, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. This paper would not have been possible without the efforts of the Chandra, Spitzer, KPNO, and MMT support staff. Optical spectroscopy discussed in this paper was obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. The first Spitzer MIPS survey of the Bootes region was obtained using GTO time provided by the Spitzer Infrared Spectrograph Team (PI: James Houck) and by M. Rieke. We thank the collaborators in that work for access to the 24 micron catalog generated from those data. R.C.H. was supported by an STFC Postdoctoral Fellowship and an SAO Postdoctoral Fellowship, and A.D.M. was generously funded by the NASA ADAP program under grant NNX08AJ28G. D.M.A. is grateful to the Royal Society and Philip Leverhulme Prize for their generous support. R.J.A. was supported by the NASA Postdoctoral Program, administered by Oak Ridge Associated Universities through a contract with NASA. NR 134 TC 52 Z9 52 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 APR 20 PY 2011 VL 731 IS 2 AR 117 DI 10.1088/0004-637X/731/2/117 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600040 ER PT J AU Lee, H Kashyap, VL van Dyk, DA Connors, A Drake, JJ Izem, R Meng, XL Min, SD Park, T Ratzlaff, P Siemiginowska, A Zezas, A AF Lee, Hyunsook Kashyap, Vinay L. van Dyk, David A. Connors, Alanna Drake, Jeremy J. Izem, Rima Meng, Xiao-Li Min, Shandong Park, Taeyoung Ratzlaff, Pete Siemiginowska, Aneta Zezas, Andreas TI ACCOUNTING FOR CALIBRATION UNCERTAINTIES IN X-RAY ANALYSIS: EFFECTIVE AREAS IN SPECTRAL FITTING SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; techniques: miscellaneous; X-rays: general ID MULTIPLE-IMPUTATION; SYSTEMATIC-ERRORS; SHERPA; VALUES AB While considerable advance has been made to account for statistical uncertainties in astronomical analyses, systematic instrumental uncertainties have been generally ignored. This can be crucial to a proper interpretation of analysis results because instrumental calibration uncertainty is a form of systematic uncertainty. Ignoring it can underestimate error bars and introduce bias into the fitted values of model parameters. Accounting for such uncertainties currently requires extensive case-specific simulations if using existing analysis packages. Here, we present general statistical methods that incorporate calibration uncertainties into spectral analysis of high-energy data. We first present a method based on multiple imputation that can be applied with any fitting method, but is necessarily approximate. We then describe a more exact Bayesian approach that works in conjunction with a Markov chain Monte Carlo based fitting. We explore methods for improving computational efficiency, and in particular detail a method of summarizing calibration uncertainties with a principal component analysis of samples of plausible calibration files. This method is implemented using recently codified Chandra effective area uncertainties for low-resolution spectral analysis and is verified using both simulated and actual Chandra data. Our procedure for incorporating effective area uncertainty is easily generalized to other types of calibration uncertainties. C1 [Lee, Hyunsook; Kashyap, Vinay L.; Drake, Jeremy J.; Ratzlaff, Pete; Siemiginowska, Aneta] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [van Dyk, David A.; Min, Shandong] Univ Calif Irvine, Dept Stat, Irvine, CA 92697 USA. [Connors, Alanna] Eureka Sci, Oakland, CA 94602 USA. [Izem, Rima] US FDA, Ctr Drug Evaluat & Res, Div Biometr, Silver Spring, MD 20903 USA. [Meng, Xiao-Li] Harvard Univ, Dept Stat, Cambridge, MA 02138 USA. [Park, Taeyoung] Yonsei Univ, Dept Appl Stat, Seoul 120749, South Korea. [Zezas, Andreas] IESL, Fdn Res & Technol, Iraklion 71110, Crete, Greece. [Zezas, Andreas] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. RP Lee, H (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM hlee@cfa.harvard.edu; vkashyap@cfa.harvard.edu; dvd@ics.uci.edu; aconnors@eurekabayes.com; jdrake@cfa.harvard.edu; rima.izem@fda.hhs.gov; meng@stat.harvard.edu; shandonm@uci.edu; taeyoung.t.park@gmail.com; rpete@head.cfa.harvard.edu; asiemiginowska@cfa.harvard.edu; azezas@physics.uoc.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Van Dyk, David/0000-0002-0816-331X FU NASA AISRP [NNG06GF17G]; CXC NASA [NAS8-39073]; NSF [DMS 04-06085, DMS 09-07522, DMS-0405953, DMS-0907185] FX This work was supported by NASA AISRP grant NNG06GF17G (H.L., A.C., V.L.K.), and CXC NASA contract NAS8-39073 (V.L.K., A.S., J.J.D., P.R.), NSF grants DMS 04-06085 and DMS 09-07522 (D.v.D., A.C., S.M., T.P.), and NSF grants DMS-0405953 and DMS-0907185 (X.L.M.). We acknowledge useful discussions with Herman Marshall, Alex Blocker, Jonathan McDowell, and Arnold Rots. NR 52 TC 12 Z9 12 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 APR 20 PY 2011 VL 731 IS 2 AR 126 DI 10.1088/0004-637X/731/2/126 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600049 ER PT J AU Mandel, KS Narayan, G Kirshner, RP AF Mandel, Kaisey S. Narayan, Gautham Kirshner, Robert P. TI TYPE Ia SUPERNOVA LIGHT CURVE INFERENCE: HIERARCHICAL MODELS IN THE OPTICAL AND NEAR-INFRARED SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; methods: statistical; supernovae: general ID HUBBLE-SPACE-TELESCOPE; 2-PARAMETER LUMINOSITY CORRECTION; EXTRAGALACTIC EXTINCTION LAW; CEPHEID CALIBRATIONS; DISTANCE INDICATORS; STANDARD CANDLES; PRECISE DISTANCE; CROSS-VALIDATION; GIBBS SAMPLER; K-CORRECTIONS AB We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction A(V) and the ratio of total-to-selective dust absorption R-V. For SNe with low dust extinction, A(V) less than or similar to 0.4, we find R-V less than or similar to 2.5-2.9, while at high extinctions, A(V) greater than or similar to 1, low values of R-V < 2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11 mag for SNe with optical and NIR data versus 0.15 mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators. C1 [Mandel, Kaisey S.; Narayan, Gautham; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mandel, KS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kmandel@cfa.harvard.edu OI Narayan, Gautham/0000-0001-6022-0484 FU FAS Sciences Division Research Computing Group at Harvard University; NSF [AST-0907903] FX K.M. thanks Stephane Blondin, Peter Challis, Jonathan Chang, Ryan Foley, Jonathan Foster, Andrew Friedman, Andrew Gelman, Malcolm Hicken, Joseph Koo, Sam Kou, and Michael Wood-Vasey for useful discussions, suggestions, and clarifications. We thank the anonymous referee for a thorough review of the manuscript. Computations in this paper were run on the Odyssey cluster supported by the FAS Sciences Division Research Computing Group at Harvard University. Supernova research at Harvard College Observatory is supported in part by NSF grant AST-0907903. NR 105 TC 73 Z9 75 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 APR 20 PY 2011 VL 731 IS 2 AR 120 DI 10.1088/0004-637X/731/2/120 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600043 ER PT J AU Marriage, TA Juin, JB Lin, YT Marsden, D Nolta, MR Partridge, B 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 Hajian, A 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 Kaul, M Klein, J Kosowsky, A Lau, JM Limon, M Lupton, RH Martocci, K Mauskopf, P Menanteau, F Moodley, K Moseley, H Netterfield, CB Niemack, MD Page, LA Parker, L Quintana, H Reid, B Sehgal, N Sherwin, BD Sievers, J Spergel, DN Staggs, ST Swetz, DS Switzer, ER Thornton, R Trac, H Tucker, C Warne, R Wilson, G Wollack, E Zhao, Y AF Marriage, Tobias A. Baptiste Juin, Jean Lin, Yen-Ting Marsden, Danica Nolta, Michael R. Partridge, Bruce 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. Hajian, Amir Halpern, Mark Hasselfield, Matthew Hernandez-Monteagudo, Carlos Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hlozek, Renee Huffenberger, Kevin M. Handel Hughes, David Hughes, John P. Infante, Leopoldo Irwin, Kent D. Kaul, Madhuri Klein, Jeff Kosowsky, Arthur Lau, Judy M. Limon, Michele Lupton, Robert H. Martocci, Krista Mauskopf, Phil Menanteau, Felipe Moodley, Kavilan Moseley, Harvey Netterfield, Calvin B. Niemack, Michael D. Page, Lyman A. Parker, Lucas Quintana, Hernan 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 Wilson, Grant Wollack, Ed Zhao, Yue TI THE ATACAMA COSMOLOGY TELESCOPE: EXTRAGALACTIC SOURCES AT 148 GHz IN THE 2008 SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; galaxies: active; radio continuum: galaxies; surveys ID SOUTH-POLE TELESCOPE; ZELDOVICH POWER SPECTRUM; GALAXY CLUSTERS; SOURCE CATALOG; RADIO-SOURCES; SOURCE COUNTS; SKY SURVEY; ANISOTROPY; FIELD; SZ AB We report on extragalactic sources detected in a 455 deg(2) map of the southern sky made with data at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. We provide a catalog of 157 sources with flux densities spanning two orders of magnitude: from 15 mJy to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low-redshift X-ray-selected galaxy clusters. Estimates of the radio to millimeter-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (> 50 mJy) 148 GHz selected sample with complete cross-identifications from the Australia Telescope 20 GHz survey, we observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha(5-20) = -0.07 +/- 0.06, alpha(20-148) = -0.39 +/- 0.04, and alpha(5-148) = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148 GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C-Sync = (2.8 +/- 0.3) x 10(-6) mu K-2. C1 [Marriage, Tobias A.; Lin, Yen-Ting; Das, Sudeep; Dunkley, Joanna; Hajian, Amir; Lupton, Robert H.; Spergel, David N.; Trac, Hy] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Baptiste Juin, Jean; Lin, Yen-Ting; Aguirre, Paula; Felipe Barrientos, L.; Duenner, Rolando; Infante, Leopoldo; Quintana, Hernan] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. [Marsden, Danica; Devlin, Mark J.; Dicker, Simon R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Nolta, Michael R.; Bond, John R.; Hajian, Amir; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Appel, John William; Das, Sudeep; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D.; Lau, Judy M.; Limon, Michele; Martocci, Krista; 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. [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, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 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. [Handel Hughes, David] INAOE, Puebla, Mexico. [Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [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 Astrophys Lab, New York, NY 10027 USA. [Martocci, Krista; Switzer, Eric R.] Lab Astrophys & Space Res, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Netterfield, Calvin B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Reid, Beth] Univ Barcelona, ICC, E-08028 Barcelona, Spain. [Reid, Beth] Univ Barcelona, ICREA, E-08028 Barcelona, Spain. [Thornton, Robert] W Chester Univ, Dept Phys, W Chester, PA 19383 USA. [Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wilson, Grant] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Marriage, TA (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. 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 Limon, Michele/0000-0002-5900-2698; Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074 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]; FONDECYT [3085031]; Natural Science and Engineering Research Council of Canada (NSERC); NSF [AST-0546035, AST-0606975]; FONDAP Centro de Astrofisica; U.S. Department of Energy [DE-AC3-76SF00515]; CONICYT; MECESUP; Fundacion Andes; Rhodes Trust; NSF Physics Frontier Center [PHY-0114422]; World Premier International Research Center Initiative, MEXT, Japan 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 US 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.; T.M. was supported through NASA grant NNX08AH30G. J.B.J. was supported by the FONDECYT grant 3085031. 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. H. Q. and L. I. acknowledge partial support from FONDAP Centro de Astrofisica. N.S. is supported by the U.S. Department of Energy contract to SLAC no. DE-AC3-76SF00515. R. D. was supported by CONICYT, MECESUP, and Fundacion Andes. R. H. was supported by the Rhodes Trust. E. S. acknowledges support by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics. Y.T.L. acknowledges support from the World Premier International Research Center Initiative, MEXT, Japan. The ACT data will be made public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web site (http://www.physics.princeton.edu/act/). NR 48 TC 54 Z9 54 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 APR 20 PY 2011 VL 731 IS 2 AR 100 DI 10.1088/0004-637X/731/2/100 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600023 ER PT J AU Youdin, AN AF Youdin, Andrew N. TI ON THE FORMATION OF PLANETESIMALS VIA SECULAR GRAVITATIONAL INSTABILITIES WITH TURBULENT STIRRING SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; instabilities; planets and satellites: formation; protoplanetary disks; turbulence ID SOLAR NEBULA; PROTOPLANETARY DISK; PLANET FORMATION; FORMING PLANETESIMALS; STREAMING INSTABILITY; CIRCUMSTELLAR DISKS; LAYERED ACCRETION; SOLID BODIES; DUST LAYER; GROWTH AB We study the gravitational instability (GI) of small solids in a gas disk as a mechanism to form planetesimals. Dissipation from gas drag introduces secular GI, which proceeds even when standard GI criteria for a critical density or Toomre's Q predict stability. We include the stabilizing effects of turbulent diffusion, which suppresses small-scale GI. The radially wide rings that do collapse contain up to similar to 0.1 Earth masses of solids. Subsequent fragmentation of the ring (not modeled here) would produce a clan of chemically homogenous planetesimals. Particle radial drift time scales (and, to a lesser extent, disk lifetimes and sizes) restrict the viability of secular GI to disks with weak turbulent diffusion, characterized by alpha less than or similar to 10(-4). Thus, midplane dead zones are a preferred environment. Large solids with radii greater than or similar to 10 cm collapse most rapidly because they partially decouple from the gas disk. Smaller solids, even below similar to mm sizes, could collapse if particle-driven turbulence is weakened by either localized pressure maxima or super-solar metallicity. Comparison with simulations that include particle clumping by the streaming instability shows that our linear model underpredicts rapid, small-scale gravitational collapse. Thus, the inclusion of more detailed gas dynamics promotes the formation of planetesimals. We discuss relevant constraints from solar system and accretion disk observations. 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] FX I thank Jeremy Goodman for suggesting Descartes' rule of signs to prove instability and an anonymous referee of a previous submission for suggesting the importance of radial turbulent diffusion. Comments from Kaitlin Kratter, Scott Kenyon, and Xeuning Bai greatly improved the presentation. Portions of this project were supported by the NASA Astrophysics Theory Program and Origins of Solar Systems Program through grant NNX10AF35G. NR 71 TC 41 Z9 42 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 APR 20 PY 2011 VL 731 IS 2 AR 99 DI 10.1088/0004-637X/731/2/99 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753MM UT WOS:000289779600022 ER PT J AU Grant, JA Wilson, SA AF Grant, John A. Wilson, Sharon A. TI Late alluvial fan formation in southern Margaritifer Terra, Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MARTIAN IMPACT CRATERS; CHRONOLOGY; EVOLUTION AB Crater statistics indicate alluvial fans, crater floor, and fill/mantling deposits within impact craters >50 km in diameter in southern Margaritifer Terra were likely emplaced during multiple epochs: fans formed during the Amazonian or near the Amazonian-Hesperian boundary, crater floor deposits are likely Hesperian in age, and most fill/mantling deposits are Amazonian. The regional distribution of fans points to a late period of widespread water-driven degradation. Two of the final candidate landing sites for the 2011 Mars Science Laboratory mission would land on or near some of these fans, which appear younger than previously considered. Citation: Grant, J. A., and S. A. Wilson (2011), Late alluvial fan formation in southern Margaritifer Terra, Mars, Geophys. Res. Lett., 38, L08201, doi:10.1029/2011GL046844. C1 [Grant, John A.; Wilson, Sharon A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20560 USA. RP Grant, JA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, POB 37012, Washington, DC 20560 USA. EM grantj@si.edu FU NASA FX We thank the people at the University of Arizona, Ball Aerospace, Malin Space Science Systems, the Jet Propulsion Laboratory, and Lockheed Martin that built and operate the HiRISE and CTX cameras and Mars Reconnaissance Orbiter spacecraft. Reviews by Cathy Quantin and an anonymous reviewer improved the manuscript. This work was supported by NASA. NR 28 TC 38 Z9 38 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 20 PY 2011 VL 38 AR L08201 DI 10.1029/2011GL046844 PG 6 WC Geosciences, Multidisciplinary SC Geology GA 754KW UT WOS:000289854500006 ER PT J AU Freeman, KH Mueller, KE Diefendorf, AF Wing, SL Koch, PL AF Freeman, Katherine H. Mueller, Kevin E. Diefendorf, Aaron F. Wing, Scott L. Koch, Paul L. TI Clarifying the influence of water availability and plant types on carbon isotope discrimination by C3 plants SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Freeman, Katherine H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Mueller, Kevin E.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Diefendorf, Aaron F.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Wing, Scott L.] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Koch, Paul L.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. RP Freeman, KH (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM khf4@psu.edu RI Freeman, Katherine/H-5140-2011; OI Freeman, Katherine/0000-0002-3350-7671; Mueller, Kevin/0000-0002-0739-7472; Wing, Scott/0000-0002-2954-8905 NR 5 TC 8 Z9 9 U1 3 U2 33 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 APR 19 PY 2011 VL 108 IS 16 BP E59 EP E60 DI 10.1073/pnas.1102556108 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 752GV UT WOS:000289680400001 PM 21474782 ER PT J AU Woodhams, DC Bosch, J Briggs, CJ Cashins, S Davis, LR Lauer, A Muths, E Puschendorf, R Schmidt, BR Sheafor, B Voyles, J AF Woodhams, Douglas C. Bosch, Jaime Briggs, Cheryl J. Cashins, Scott Davis, Leyla R. Lauer, Antje Muths, Erin Puschendorf, Robert Schmidt, Benedikt R. Sheafor, Brandon Voyles, Jamie TI Mitigating amphibian disease: strategies to maintain wild populations and control chytridiomycosis SO FRONTIERS IN ZOOLOGY LA English DT Review ID PATHOGEN BATRACHOCHYTRIUM-DENDROBATIDIS; SKIN PEPTIDE DEFENSES; EMERGING INFECTIOUS-DISEASE; HIGH-ELEVATION LAKES; YELLOW-LEGGED FROG; CHYTRID FUNGUS; CUTANEOUS BACTERIA; ECOLOGICAL ETHICS; MIDWIFE TOAD; RANA-MUSCOSA AB Background: Rescuing amphibian diversity is an achievable conservation challenge. Disease mitigation is one essential component of population management. Here we assess existing disease mitigation strategies, some in early experimental stages, which focus on the globally emerging chytrid fungus Batrachochytrium dendrobatidis. We discuss the precedent for each strategy in systems ranging from agriculture to human medicine, and the outlook for each strategy in terms of research needs and long-term potential. Results: We find that the effects of exposure to Batrachochytrium dendrobatidis occur on a spectrum from transient commensal to lethal pathogen. Management priorities are divided between (1) halting pathogen spread and developing survival assurance colonies, and (2) prophylactic or remedial disease treatment. Epidemiological models of chytridiomycosis suggest that mitigation strategies can control disease without eliminating the pathogen. Ecological ethics guide wildlife disease research, but several ethical questions remain for managing disease in the field. Conclusions: Because sustainable conservation of amphibians in nature is dependent on long-term population persistence and co-evolution with potentially lethal pathogens, we suggest that disease mitigation not focus exclusively on the elimination or containment of the pathogen, or on the captive breeding of amphibian hosts. Rather, successful disease mitigation must be context specific with epidemiologically informed strategies to manage already infected populations by decreasing pathogenicity and host susceptibility. We propose population level treatments based on three steps: first, identify mechanisms of disease suppression; second, parameterize epizootiological models of disease and population dynamics for testing under semi-natural conditions; and third, begin a process of adaptive management in field trials with natural populations. C1 [Woodhams, Douglas C.; Davis, Leyla R.; Schmidt, Benedikt R.] Univ Zurich, Inst Evolutionary Biol & Environm Studies, CH-8057 Zurich, Switzerland. [Woodhams, Douglas C.] Smithsonian Trop Res Inst, DPO, AA 34002 USA. [Bosch, Jaime] CSIC, Dept Biol Evolut & Biodiversidad, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. [Briggs, Cheryl J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Cashins, Scott; Puschendorf, Robert] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Cashins, Scott] James Cook Univ, Sch Publ Hlth Trop Med & Rehabil Sci, Amphibian Dis Ecol Grp, Townsville, Qld 4811, Australia. [Lauer, Antje] Calif State Coll Bakersfield, Dept Biol, Bakersfield, CA 93311 USA. [Muths, Erin] US Geol Survey, Ft Collins Sci Ctr, Ft Collins, CO 80526 USA. [Schmidt, Benedikt R.] KARCH, CH-2000 Neuchatel, Switzerland. [Sheafor, Brandon] Carroll Coll, Dept Nat Sci, Helena, MT 59625 USA. [Voyles, Jamie] Univ Idaho, Dept Biol Sci, Moscow, ID 83844 USA. RP Woodhams, DC (reprint author), Univ Zurich, Inst Evolutionary Biol & Environm Studies, Winterthurerstr 190, CH-8057 Zurich, Switzerland. EM dwoodhams@gmail.com RI Schmidt, Benedikt/B-8491-2008; Bosch, Jaime/H-3042-2011; Woodhams, Douglas/B-1962-2012; Puschendorf, Robert/B-6280-2011; Briggs, Cheryl/F-7456-2013; Research ID, CTBCC /O-3564-2014; OI Schmidt, Benedikt/0000-0002-4023-1001; Puschendorf, Robert/0000-0002-8105-171X; Bosch, Jaime/0000-0002-0099-7934 FU Claraz Foundation; Swiss National Science Foundation [31-125099, IZ32Z0_133187/1]; USGS' Amphibian Research and Monitoring Initiative; University of Zurich FX We thank Dr. H. Brandl and Dr. A. Bannigan for assistance with microscopy, and Dr. R.N. Harris for discussion and unpublished results. DCW was supported by the Claraz Foundation, and the Swiss National Science Foundation (31-125099). EM was partially supported by the USGS' Amphibian Research and Monitoring Initiative. This manuscript is contribution number 372 to the USGS Amphibian Research and Monitoring Initiative and contributed to an International Exploratory Workshop supported by the Swiss National Science Foundation (IZ32Z0_133187/1) and the University of Zurich. NR 242 TC 88 Z9 89 U1 13 U2 146 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1742-9994 J9 FRONT ZOOL JI Front. Zool. PD APR 18 PY 2011 VL 8 AR 8 DI 10.1186/1742-9994-8-8 PG 23 WC Zoology SC Zoology GA 767KV UT WOS:000290856400001 PM 21496358 ER PT J AU Ashley, JW Golombek, MP Christensen, PR Squyres, SW McCoy, TJ Schroder, C Fleischer, I Johnson, JR Herkenhoff, KE Parker, TJ AF Ashley, J. W. Golombek, M. P. Christensen, P. R. Squyres, S. W. McCoy, T. J. Schroeder, C. Fleischer, I. Johnson, J. R. Herkenhoff, K. E. Parker, T. J. TI Evidence for mechanical and chemical alteration of iron-nickel meteorites on Mars: Process insights for Meridiani Planum SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ANTARCTIC METEORITES; ORDINARY CHONDRITES; CARBONACEOUS CHONDRITES; GALACTIC EVOLUTION; BURNS FORMATION; GROUND ICE; ORIGIN; SURFACE; OXIDATION; SILICON AB The weathering of meteorites found on Mars involves chemical and physical processes that can provide clues to climate conditions at the location of their discovery. Beginning on sol 1961, the Opportunity rover encountered three large iron meteorites within a few hundred meters of each other. In order of discovery, these rocks have been assigned the unofficial names Block Island, Shelter Island, and Mackinac Island. Each rock presents a unique but complimentary set of features that increase our understanding of weathering processes at Meridiani Planum. Significant morphologic characteristics interpretable as weathering features include (1) a large pit in Block Island, lined with delicate iron protrusions suggestive of inclusion removal by corrosive interaction; (2) differentially eroded kamacite and taenite lamellae in Block Island and Shelter Island, providing relative timing through crosscutting relationships with deposition of (3) an iron oxide-rich dark coating; (4) regmaglypted surfaces testifying to regions of minimal surface modification, with other regions in the same meteorites exhibiting (5) large-scale, cavernous weathering (in Shelter Island and Mackinac Island). We conclude that the current size of the rocks is approximate to their original postfall contours. Their morphology thus likely results from a combination of atmospheric interaction and postfall weathering effects. Among our specific findings is evidence supporting (1) at least one possible episode of aqueous acidic exposure for Block Island; (2) ripple migration over portions of the meteorites; (3) a minimum of two separate episodes of wind abrasion; alternating with (4) at least one episode of coating-forming chemical alteration, most likely at subzero temperatures. C1 [Ashley, J. W.; Christensen, P. R.] Arizona State Univ, Sch Earth & Space Explorat, Mars Space Flight Facil, Tempe, AZ 85287 USA. [Golombek, M. P.; Parker, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [McCoy, T. J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Schroeder, C.] Univ Tubingen, Ctr Appl Geosci, Tubingen, Germany. [Fleischer, I.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, Mainz, Germany. [Johnson, J. R.; Herkenhoff, K. E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. RP Ashley, JW (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Mars Space Flight Facil, Tempe, AZ 85287 USA. RI Schroder, Christian/B-3870-2009; Johnson, Jeffrey/F-3972-2015 OI Schroder, Christian/0000-0002-7935-6039; FU NASA [NNX06-AD83H] FX We would like to express our sincerest thanks to our two anonymous reviewers. Jonathan Hill and Eliana McCartney were supportive in the acquisition of data products. Marc Fries was helpful in preliminary discussions. Ella Mae Lee and Bonnie Redding from the USGS team are thanked for assembling the MI mosaics for this paper. Laurence Garvie of Arizona State University's Center for Meteorite Studies is acknowledged for access to meteorite collections and discussions. For the MIPL geometric model of Block Island, we thank Nick Ruoff for tiepointing and localization, Oleg Pariser for meshing, Kris Capraro for masking off bad areas, Zareh Gorjian and Mike Stetson for cleaning up the model and determining the volume, and Bob Deen for overseeing the effort. Funding was provided in part through NASA Graduate Student Researchers Program grant NNX06-AD83H. NR 112 TC 10 Z9 10 U1 2 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD APR 16 PY 2011 VL 116 AR E00F20 DI 10.1029/2010JE003672 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 751WA UT WOS:000289647200001 ER PT J AU Bozarth, CA Lance, SL Civitello, DJ Glenn, JL Maldonado, JE AF Bozarth, Christine A. Lance, Stacey L. Civitello, David J. Glenn, Julie L. Maldonado, Jesus E. TI Phylogeography of the gray fox (Urocyon cinereoargenteus) in the eastern United States SO JOURNAL OF MAMMALOGY LA English DT Article DE d-loop; eastern United States; gray fox; phylogeography; Pleistocene; Urocyon ID MITOCHONDRIAL-DNA PHYLOGEOGRAPHY; FLYING SQUIRRELS GLAUCOMYS; CONSERVATION GENETICS; POPULATION HISTORY; RED FOXES; BIOGEOGRAPHY; REFUGIA; CONSEQUENCES; EVOLUTION; CLIMATE AB Molecular data have been used to show northward post-Pleistocene range expansions from a refugium in the southeastern United States for several mammal species. Fossil and historical records indicate that gray foxes (Urocyon cinereoargenteus) were not present in the northeastern United States until well after the Pleistocene (ca. 900). To test the hypothesis that gray foxes experienced a post-Pleistocene range expansion we conducted a phylogeographic analysis of gray foxes from across the eastern United States. We sequenced a variable portion of the mitochondria] control region (411 base pairs) from 229 gray fox tissue samples from 15 states, representing the range of all 3 East Coast subspecies. Phylogeographic analyses indicated no clear pattern of genetic structuring of gray fox haplotypes across most of the eastern United States. However, when haplotype frequencies were subdivided into a northeastern and a southern region, we detected a strong signal of differentiation between the Northeast and the rest of the eastern United States. Indicators of molecular diversity and tests for demographic expansion confirmed this division and suggested a very recent expansion of gray foxes into the northeastern states. Our results support the hypothesis that gray foxes 1st colonized the Northeast during a historical period of hemisphere-wide warming, which coincided with the range expansion of deciduous forest. We present the 1st study that analyzes the phylogeographic patterns of the gray fox in the eastern United States. C1 [Bozarth, Christine A.; Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. George Mason Univ, Dept Environm Sci & Publ Policy, Fairfax, VA 22030 USA. [Lance, Stacey L.; Civitello, David J.] Colby Coll, Dept Biol, Waterville, ME 04901 USA. [Lance, Stacey L.] Univ Georgia, Savannah River Ecol Lab, Aiken, SC 29802 USA. [Civitello, David J.] Indiana Univ, Dept Biol, Bloomington, IN 47401 USA. [Glenn, Julie L.] Univ S Carolina, Dept Biol Sci, Peromyscus Genet Stock Ctr, Columbia, SC 29208 USA. RP Bozarth, CA (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. EM bozarthc@si.edu RI Lance, Stacey/K-9203-2013 OI Lance, Stacey/0000-0003-2686-1733 FU Savannah River Ecology Laboratory from the United States Department of Energy [DE-FC09-07SR22506]; Colby College Department of Biology; Faculty Student Special Projects Award; IDeA Networks of Biomedical Research Excellence [P20 RR-016463] FX Financial and logistical assistance was provided by the Savannah River Ecology Laboratory through contract DE-FC09-07SR22506 from the United States Department of Energy to the University of Georgia Research Foundation and by the Colby College Department of Biology, the Dean of Faculty Student Special Projects Award, and IDeA Networks of Biomedical Research Excellence grant P20 RR-016463. We thank J. G. Germaine for coordination of sample collection and DNA extraction; J. D. Schrecengost, J. C. Kilgo, K. V. Miller, and H. S. Ray for tissue collection; and G. Syed, F. Hailer, C. Hofman, C. W. Edwards, and L. L. Rockwood for assistance and guidance. Thanks are extended to the many state wildlife officials and trappers who helped us obtain specimens and to 2 anonymous reviewers whose comments greatly improved this manuscript. NR 65 TC 5 Z9 6 U1 0 U2 23 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 APR 15 PY 2011 VL 92 IS 2 BP 283 EP 294 DI 10.1644/10-MAMM-A-141.1 PG 12 WC Zoology SC Zoology GA 754PV UT WOS:000289869700003 ER PT J AU Wilson, DE Timm, RM AF Wilson, Don E. Timm, Robert M. TI ROBERT S. HOFFMANN: 1929-2010 OBITUARY SO JOURNAL OF MAMMALOGY LA English DT Biographical-Item C1 [Wilson, Don E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Timm, Robert M.] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Timm, Robert M.] Univ Kansas, Biodivers Inst, Lawrence, KS 66045 USA. RP Wilson, DE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. EM wilsond@si.edu; btimm@ku.edu NR 1 TC 0 Z9 0 U1 0 U2 2 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 APR 15 PY 2011 VL 92 IS 2 BP 460 EP 473 PG 14 WC Zoology SC Zoology GA 754PV UT WOS:000289869700020 ER PT J AU Miller, AW Frazier, M Smith, GE Perry, ES Ruiz, GM Tamburri, MN AF Miller, A. Whitman Frazier, Melanie Smith, George E. Perry, Elgin S. Ruiz, Gregory M. Tamburri, Mario N. TI Enumerating Sparse Organisms in Ships' Ballast Water: Why Counting to 10 Is Not So Easy SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID STATISTICAL POWER; PARTICLE AB To reduce ballast water-borne aquatic invasions worldwide, the International Maritime Organization and United States Coast Guard have each proposed discharge standards specifying maximum concentrations of living biota that may be released in ships' ballast water (BW), but these regulations still lack guidance for standardized type approval and compliance testing of treatment systems. Verifying whether BW meets a discharge standard poses significant challenges. Properly treated BW will contain extremely sparse numbers of live organisms, and robust estimates of rare events require extensive sampling efforts. A balance of analytical rigor and practicality is essential to determine the volume of BIN that can be reasonably sampled and processed, yet yield accurate live counts. We applied statistical modeling to a range of sample volumes, plankton concentrations, and regulatory scenarios (i.e., levels of type I and type II errors), and calculated the statistical power of each combination to detect noncompliant discharge concentrations. The model expressly addresses the roles of sampling error, BW volume, and burden of proof on the detection of noncompliant discharges in order to establish a rigorous lower limit of sampling volume. The potential effects of recovery errors (i.e., incomplete recovery and detection of live biota) in relation to sample volume are also discussed. C1 [Miller, A. Whitman; Smith, George E.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Frazier, Melanie] US EPA, Western Ecol Div, Natl Hlth & Environm Effects Res Lab, Off Res & Dev, Newport, OR 97365 USA. [Tamburri, Mario N.] Univ Maryland, Chesapeake Biol Lab, Maritime Environm Resource Ctr, Ctr Environm Sci, Solomons, MD 20688 USA. RP Miller, AW (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM millerw@si.edu RI Frazier, Melanie/A-2367-2012; Tamburri, Mario/F-7193-2013; OI Ruiz, Gregory/0000-0003-2499-441X; Miller, Whitman/0000-0003-0484-182X FU Maryland Port Administration [508923]; U.S. Maritime Administration [DTMA1H0003]; USCG/National Ballast Information Clearinghouse [HSCG23-06-C-MMS065]; U.S. EPA [EP08D00051] FX Support was provided in part by the Maryland Port Administration (508923) and U.S. Maritime Administration (DTMA1H0003) to the Maritime Environmental Resource Center; USCG/National Ballast Information Clearinghouse for A.W.M. (HSCG23-06-C-MMS065); as well as by a U.S. EPA postdoctoral fellowships to M.F. (AMI/GEOSS EP08D00051 and NHEERL). We thank the International Council for the Exploration of the Sea (ICES), Intergovernmental Oceanographic Commission (IOC) and International Maritime Organization (IMO) Working Group on Ballast and Other Ship Vectors, as well as G. F. Riedel, H. Lee II, D. A. Reusser, R A. Everett, M. S. Minton, and K. J. Klug for their comments and suggestions on our analyses. This document has been reviewed in accordance with U.S. Environmental Protection Agency policy and approved for publication. Mention of trade names or commercial products does not constitute endorsement or recommendation for use. NR 31 TC 20 Z9 20 U1 1 U2 17 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD APR 15 PY 2011 VL 45 IS 8 BP 3539 EP 3546 DI 10.1021/es102790d PG 8 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 747SZ UT WOS:000289341300050 PM 21434685 ER PT J AU West-Eberhard, MJ Smith, JAC Winter, K AF West-Eberhard, Mary Jane Smith, J. Andrew C. Winter, Klaus TI Photosynthesis, Reorganized SO SCIENCE LA English DT Editorial Material ID CRASSULACEAN ACID METABOLISM; C-4 PHOTOSYNTHESIS; EVOLUTIONARY; EXPRESSION; ORIGINS C1 [West-Eberhard, Mary Jane] Univ Costa Rica, Smithsonian Trop Res Inst, Escuela Biol, San Pedro, Costa Rica. [Smith, J. Andrew C.] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. [Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP West-Eberhard, MJ (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Escuela Biol, San Pedro, Costa Rica. EM mjwe@sent.com; andrew.smith@plants.ox.ac.uk; winterk@si.edu NR 15 TC 21 Z9 23 U1 9 U2 52 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 APR 15 PY 2011 VL 332 IS 6027 BP 311 EP 312 DI 10.1126/science.1205336 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 750AT UT WOS:000289516600030 PM 21493847 ER PT J AU Woodley, NE AF Woodley, Norman E. TI Vitilevumyia, an enigmatic new genus of Stratiomyidae from Fiji (Diptera) SO ZOOTAXA LA English DT Article DE Diptera; Stratiomyidae; Vitilevumyia; new genus; new species; Viti Levu; Fiji AB A new genus and species of Stratiomyidae (Diptera), Vitilevumyia bobwoodleyi gen. et sp. nov. is described from the island of Viti Levu, Fiji. It exhibits an unusual combination of character states, but is tentatively placed in the tribe Prosopochrysini of the subfamily Stratiomyinae. C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst NHB 168, Washington, DC 20013 USA. RP Woodley, NE (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst NHB 168, POB 37012, Washington, DC 20013 USA. EM norman.woodley@ars.usda.gov FU National Science Foundation [DEB-0425970]; Schlinger Foundation FX I am grateful to Evert Schlinger and Neal Evenhuis (Bishop Museum) for making material available to me from the Terrestrial Arthropod Survey of Fiji project, funded in part by the National Science Foundation (DEB-0425970) and the Schlinger Foundation. I thank Taina Litwak (Systematic Entomology Laboratory) for creating the excellent habitus illustration used as Fig. 1. Gary Ouellette took the image for Fig. 2 and prepared it for publication. Tristan Vanta provided the illustrations used in Figs. 3-6, and Charyn Micheli (Systematic Entomology Laboratory) digitally "inked" the final Figs. 7 and 8 and prepared the final plates; I am grateful for their help. Wayne Mathis (Smithsonian Institution) as well as Steven Lingafelter and Allen Norrbom (both of the Systematic Entomology Laboratory) critically reviewed the manuscript. NR 5 TC 0 Z9 0 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 APR 15 PY 2011 IS 2821 BP 62 EP 68 PG 7 WC Zoology SC Zoology GA 749XD UT WOS:000289504300006 ER PT J AU Tscherbul, TV Sayfutyarova, ER Buchachenko, AA Dalgarno, A AF Tscherbul, T. V. Sayfutyarova, E. R. Buchachenko, A. A. Dalgarno, A. TI He-ThO((1)Sigma(+)) interactions at low temperatures: Elastic and inelastic collisions, transport properties, and complex formation in cold He-4 gas SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; RELAXATION CROSS-SECTIONS; GAUSSIAN-BASIS SETS; POTENTIAL-ENERGY; COUPLED-CLUSTER; SCATTERING; ATOMS; HYDROGEN; QUANTUM; APPROXIMATION AB We present an ab initio study of cold He-4 + ThO((1)Sigma(+)) collisions based on an accurate potential energy surface (PES) evaluated by the coupled cluster method with single, double, and noniterative triple excitations using an extended basis set augmented by bond functions. Variational calculations of rovibrational energy levels show that the He-4-ThO van der Waals complex has a binding energy of 10.9 cm(-1) in its ground J = 0 rotational state. The calculated energy levels are used to obtain the temperature dependence of the chemical equilibrium constant for the formation of the He-ThO complex. We find that complex formation is thermodynamically favored at temperatures below 1 K and predict the maximum abundance of free ground-state ThO(v = 0, j = 0) molecules between 2 and 3 K. The calculated cross sections for momentum transfer in elastic He + ThO collisions display a rich resonance structure below 5 cm(-1) and decline monotonically above this collision energy. The cross sections for rotational relaxation accompanied by momentum transfer decline abruptly to zero at low collision energies (<0.1 cm(-1)). We find that Stark relaxation in He + ThO collisions can be enhanced by applying an external dc electric field of less than 100 kV/cm. Finally, we present calculations of thermally averaged diffusion cross sections for ThO in He gas, and find these to be insensitive to small variations of the PES at temperatures above 1 K. (C) 2011 American Institute of Physics. [doi:10.1063/1.3575399] C1 [Tscherbul, T. V.; Dalgarno, A.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, T. V.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Sayfutyarova, E. R.; Buchachenko, A. A.] Moscow MV Lomonosov State Univ, Dept Chem, Moscow 119991, 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; Tscherbul, Timur/K-3286-2014 OI Buchachenko, Alexei/0000-0003-0701-5531; Tscherbul, Timur/0000-0001-5689-040X FU Chemical Science, Geoscience, and Bioscience Division of the Office of Basic Energy Science, Office of Science, U.S. Department of Energy; NSF; Russian Basic Research Fund [08-03-00414]; Moscow State University FX This work was supported by the Chemical Science, Geoscience, and Bioscience Division of the Office of Basic Energy Science, Office of Science, U.S. Department of Energy and NSF grants to the Harvard-MIT Center for Ultracold Atoms and the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and the Smithsonian Astrophysical Observatory. A. A. B. and E. R. S. acknowledge support from the Russian Basic Research Fund (project 08-03-00414) and from Moscow State University. NR 57 TC 4 Z9 4 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD APR 14 PY 2011 VL 134 IS 14 AR 144301 DI 10.1063/1.3575399 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 750XU UT WOS:000289582300015 PM 21495749 ER PT J AU Berger, T Testa, P Hillier, A Boerner, P Low, BC Shibata, K Schrijver, C Tarbell, T Title, A AF Berger, Thomas Testa, Paola Hillier, Andrew Boerner, Paul Low, Boon Chye Shibata, Kazunari Schrijver, Carolus Tarbell, Ted Title, Alan TI Magneto-thermal convection in solar prominences SO NATURE LA English DT Article ID CORONAL MASS EJECTIONS; QUIESCENT PROMINENCE; HELICAL FLUX; HINODE; EMERGENCE; CONFINEMENT; INSTABILITY; TELESCOPE; DYNAMICS; MISSION AB Coronal cavities are large low-density regions formed by hemispheric-scale magnetic flux ropes suspended in the Sun's outer atmosphere(1). They evolve over time, eventually erupting as the dark cores of coronal mass ejections(2,3). Although coronal mass ejections are common and can significantly affect planetary magnetospheres, the mechanisms by which cavities evolve to an eruptive state remain poorly understood. Recent optical observations(4) of high-latitude 'polar crown' prominences within coronal cavities reveal dark, low-density(5) 'bubbles' that undergo Rayleigh-Taylor instabilities(6,7) to form dark plumes rising into overlying coronal cavities. These observations offered a possible mechanism for coronal cavity evolution, although the nature of the bubbles, particularly their buoyancy, was hitherto unclear. Here we report simultaneous optical and extreme-ultraviolet observations of polar crown prominences that show that these bubbles contain plasma at temperatures in the range (2.5-12) x 10(5) kelvin, which is 25-120 times hotter than the overlying prominence. This identifies a source of the buoyancy, and suggests that the coronal cavity-prominence system supports a novel form of magneto-thermal convection in the solar atmosphere, challenging current hydromagnetic concepts of prominences and their relation to coronal cavities. C1 [Berger, Thomas; Boerner, Paul; Schrijver, Carolus; Tarbell, Ted; Title, Alan] Lockheed Martin Adv Technol Ctr, Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Testa, Paola] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hillier, Andrew; Shibata, Kazunari] Kyoto Univ, Grad Sch Sci, Kwasan Observ, Kyoto 6078471, Japan. [Hillier, Andrew; Shibata, Kazunari] Kyoto Univ, Grad Sch Sci, Hida Observ, Kyoto 6078471, Japan. [Low, Boon Chye] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Berger, T (reprint author), Lockheed Martin Adv Technol Ctr, Solar & Astrophys Lab, O ADBS B 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM berger@lmsal.com FU JAXA and NAOJ (Japan); STFC (UK); NASA; ESA; NSC (Norway); Universality and Emergence FX Hinode is a Japanese mission developed and launched by ISAS/JAXA, in collaboration with NAOJ as a domestic partner, and with NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA, ESA and NSC (Norway). The Solar Dynamics Observatory is part of NASA's Living with a Star programme. K.S. and A.H. are supported by the Grant-in-Aid for the Global COE Program 'The Next Generation of Physics, Spun from Universality and Emergence'. We thank J. Martinez-Sykora for discovering the 2 July 2010 prominence bubble event in the AIA database. NR 27 TC 68 Z9 68 U1 1 U2 7 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD APR 14 PY 2011 VL 472 IS 7342 BP 197 EP 200 DI 10.1038/nature09925 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 749LR UT WOS:000289469100037 PM 21490669 ER PT J AU Lin, TY Finkbeiner, DP AF Lin, Tongyan Finkbeiner, Douglas P. TI Magnetic inelastic dark matter: Directional signals without a directional detector SO PHYSICAL REVIEW D LA English DT Article ID CDMS II EXPERIMENT; SEARCH; DAMA/LIBRA; SIGNATURE; LIMITS AB The magnetic inelastic dark matter (MiDM) model, in which dark matter inelastically scatters off nuclei through a magnetic dipole interaction, has previously been shown to reconcile the DAMA/LIBRA annual modulation signal with null results from other experiments. In this work, we explore the unique directional detection signature of MiDM. After the dark matter scatters into its excited state, it decays with a lifetime of order 1 mu s and emits a photon with energy similar to 100 keV. Both the nuclear recoil and the corresponding emitted photon can be detected by studying delayed coincidence events. The recoil track and velocity of the excited state can be reconstructed from the nuclear interaction vertex and the photon event vertex. The angular distribution of the WIMP recoil tracks is sharply peaked and modulates daily. It is therefore possible to observe the directional modulation of WIMP-nucleon scattering without a large-volume gaseous directional detection experiment. Furthermore, current experiments such as XENON100 can immediately measure this directional modulation and constrain the MiDM parameter space with an exposure of a few thousand kg . day. C1 [Lin, Tongyan; Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lin, TY (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. FU NASA [NNX10AD85G] FX We thank Peter Sorensen, Neal Weiner, and Itay Yavin for useful discussion. We are partially supported by NASA Theory Grant No. NNX10AD85G. This research made use of the NASA Astrophysics Data System (ADS) and the IDL Astronomy User's Library at Goddard [61]. NR 59 TC 7 Z9 7 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD APR 13 PY 2011 VL 83 IS 8 AR 083510 DI 10.1103/PhysRevD.83.083510 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 750BW UT WOS:000289520300002 ER PT J AU Pekar, S Cardoso, P Barriga, JC Carvalho, JC AF Pekar, Stano Cardoso, Pedro Barriga, Javier C. Carvalho, Jose C. TI Update to the zodariid spider fauna of the Iberian Peninsula and Madeira (Araneae: Zodariidae) SO ZOOTAXA LA English DT Article DE Amphiledorus; Selamia; Zodarion; description; distribution; Madeira; Portugal; Spain ID DISTRIBUTIONS; CHECKLIST; PORTUGAL AB This paper describes three new species of the genus Zodarion from the Iberian Peninsula: Z. alentejanum, Z. cesari, and Z. costapratae. One species, Z. lusitanicum, is newly recorded for Spain. In total 46 zodariid species are known from the Iberian Peninsula to date, of which 22 species are recorded from Portugal and 35 species from Spain. New faunistic records and distribution maps are given for another 18 zodariid taxa, either in the Iberian Peninsula or Madeira: Amphiledorus balnearius, Selamia reticulata, Zodarion alacre, Z. algarvense, Z. atlanticum, Z. costablancae, Z. duriense, Z. fuscum, Z. gregua, Z. jozefienae, Z. machadoi, Z. maculatum, Z. marginiceps, Z. merlijni, Z. pseudoelegans, Z. styliferum styliferum, Z. styliferum extraneum, and Z. viduum. C1 [Pekar, Stano] Masaryk Univ, Fac Sci, Dept Bot & Zool, CS-61137 Brno, Czech Republic. [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Cardoso, Pedro] Univ Acores, Azorean Biodivers Grp CITA A, Angra Do Heroismo, Portugal. [Barriga, Javier C.] Univ Complutense Madrid, Fac Biol, Dept Zool & Antropol Fis, E-28040 Madrid, Spain. [Carvalho, Jose C.] Univ Minho, Dept Biol, CBMA Mol & Environm Biol Ctr, BioESER Res Grp, P-4710057 Braga, Portugal. RP Pekar, S (reprint author), Masaryk Univ, Fac Sci, Dept Bot & Zool, Kotlarska 2, CS-61137 Brno, Czech Republic. EM pekar@sci.muni.cz RI Cardoso, Pedro/A-8820-2008; CBMA, CBMA/J-1937-2016; OI Cardoso, Pedro/0000-0001-8119-9960; CBMA, CBMA/0000-0002-2841-2678; Pekar, Stano/0000-0002-0197-5040 FU Ministry of Education, Youth and Sports of the Czech republic [MSM0021622416]; Fundacao para a Ciencia e Tecnologia [SFRH/BPD/40688/2007] FX We would like to thank N.I. Platnick (New York), C. Rollard (Paris), J.S. Almazan (Madrid), and A. de Castro (San Sebastian) for the loan of comparative material. I. Sanchez-Garcia, C. Monzo, L. Crespo, S. Henriques and W. Nentwig are thanked for some material of Zodarion spiders. We are also grateful to M. Jarab, S. Korenko, M. Rezac, M. Hruskova, L. Sentenska, and E. Liznarova for a help to collect some specimens. Staff at the Parque Natural do Vale do Guadiana have helped with fieldwork logistics. SP was supported by the grant no. MSM0021622416 from the Ministry of Education, Youth and Sports of the Czech republic. PC was supported by Fundacao para a Ciencia e Tecnologia (SFRH/BPD/40688/2007). NR 26 TC 2 Z9 3 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 APR 11 PY 2011 IS 2814 BP 19 EP 32 PG 14 WC Zoology SC Zoology GA 746VN UT WOS:000289275900002 ER PT J AU Lee, JJ Park, S Hughes, JP Slane, PO Burrows, DN AF Lee, Jae-Joon Park, Sangwook Hughes, John P. Slane, Patrick O. Burrows, David N. TI SNR 0104-72.3: A REMNANT OF A TYPE Ia SUPERNOVA IN A STAR-FORMING REGION? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (SNR 0104-72.3); ISM: supernova remnants; X-rays: ISM ID SMALL-MAGELLANIC-CLOUD; X-RAY-EMISSION; SOUTHERN SKY; RICH EJECTA; XMM-NEWTON; H I; PROGENITORS; MODELS AB We report our 110 ks Chandra observations of the supernova remnant (SNR) 0104-72.3 in the Small Magellanic Cloud (SMC). The X-ray morphology shows two prominent lobes along the northwest-southeast direction and a soft faint arc in the east. Previous low-resolution X-ray images attributed the unresolved emission from the southeastern lobe to a Be/X-ray star. Our high-resolution Chandra data clearly show that this emission is diffuse, shock-heated plasma, with negligible X-ray emission from the Be star. The eastern arc is positionally coincident with a filament seen in optical and infrared observations. Its X-ray spectrum is well fit by plasma of normal SMC abundances, suggesting that it is from shocked ambient gas. The X-ray spectra of the lobes show overabundant Fe, which is interpreted as emission from the reverse-shocked Fe-rich ejecta. The overall spectral characteristics of the lobes and the arc are similar to those of Type Ia SNRs, and we propose that SNR 0104-72.3 is the first case for a robust candidate Type Ia SNR in the SMC. On the other hand, the remnant appears to be interacting with dense clouds toward the east and to be associated with a nearby star-forming region. These features are unusual for a standard Type Ia SNR. Our results suggest an intriguing possibility that the progenitor of SNR 0104-72.3 might have been a white dwarf of a relatively young population. C1 [Lee, Jae-Joon] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Park, Sangwook] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Lee, JJ (reprint author), Korea Astron & Space Sci Inst, Taejon 305348, South Korea. EM leejjoon@kasi.re.kr FU NASA [NAS8-03060]; Smithsonian Astrophysical Observatory [GO8-9509A] FX We thank the anonymous referee for valuable comments. This work was supported in part by the Smithsonian Astrophysical Observatory under Chandra grant GO8-9509A. P.O.S. acknowledges partial support from NASA contract NAS8-03060. NR 24 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2011 VL 731 IS 1 AR L8 DI 10.1088/2041-8205/731/1/L8 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KQ UT WOS:000293126600008 ER PT J AU Narayan, G Foley, RJ Berger, E Botticella, MT Chornock, R Huber, ME Rest, A Scolnic, D Smartt, S Valenti, S Soderberg, AM Burgett, WS Chambers, KC Flewelling, HA Gates, G Grav, T Kaiser, N Kirshner, RP Magnier, EA Morgan, JS Price, PA Riess, AG Stubbs, CW Sweeney, WE Tonry, JL Wainscoat, RJ Waters, C Wood-Vasey, WM AF Narayan, G. Foley, R. J. Berger, E. Botticella, M. T. Chornock, R. Huber, M. E. Rest, A. Scolnic, D. Smartt, S. Valenti, S. Soderberg, A. M. Burgett, W. S. Chambers, K. C. Flewelling, H. A. Gates, G. Grav, T. Kaiser, N. Kirshner, R. P. Magnier, E. A. Morgan, J. S. Price, P. A. Riess, A. G. Stubbs, C. W. Sweeney, W. E. Tonry, J. L. Wainscoat, R. J. Waters, C. Wood-Vasey, W. M. TI DISPLAYING THE HETEROGENEITY OF THE SN 2002cx-LIKE SUBCLASS OF TYPE Ia SUPERNOVAE WITH OBSERVATIONS OF THE Pan-STARRS-1 DISCOVERED SN 2009ku SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: general; supernovae: individual (SN 2009ku) ID LOW-LUMINOSITY; LIGHT-CURVE; SPECTROSCOPY; EXPLOSION; PROGENITOR; PHOTOMETRY; 2005HK; 2008HA AB SN 2009ku, discovered by Pan-STARRS-1, is a Type Ia supernova (SN Ia), and a member of the distinct SN 2002cx-like class of SNe Ia. Its light curves are similar to the prototypical SN 2002cx, but are slightly broader and have a later rise to maximum in g. SN 2009ku is brighter (similar to 0.6 mag) than other SN 2002cx-like objects, peaking at M-V = -18.4 mag, which is still significantly fainter than typical SNe Ia. SN 2009ku, which had an ejecta velocity of similar to 2000 km s(-1) at 18 days after maximum brightness, is spectroscopically most similar to SN 2008ha, which also had extremely low-velocity ejecta. However, SN 2008ha had an exceedingly low luminosity, peaking at M-V = -14.2 mag, similar to 4 mag fainter than SN 2009ku. The contrast of high luminosity and low ejecta velocity for SN 2009ku is contrary to an emerging trend seen for the SN 2002cx class. SN 2009ku is a counterexample of a previously held belief that the class was more homogeneous than typical SNe Ia, indicating that the class has a diverse progenitor population and/or complicated explosion physics. As the first example of a member of this class of objects from the new generation of transient surveys, SN 2009ku is an indication of the potential for these surveys to find rare and interesting objects. C1 [Narayan, G.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Foley, R. J.; Berger, E.; Chornock, R.; Rest, A.; Soderberg, A. M.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Botticella, M. T.; Smartt, S.; Valenti, S.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Huber, M. E.; Scolnic, D.; Grav, T.; Riess, A. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Rest, A.; Riess, A. G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Burgett, W. S.; Chambers, K. C.; Flewelling, H. A.; Gates, G.; Kaiser, N.; Magnier, E. A.; Morgan, J. S.; Price, P. A.; Sweeney, W. E.; Tonry, J. L.; Wainscoat, R. J.; Waters, C.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. RP Narayan, G (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM gnarayan@cfa.harvard.edu; rfoley@cfa.harvard.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Narayan, Gautham/0000-0001-6022-0484; Chambers, Kenneth /0000-0001-6965-7789; Flewelling, Heather/0000-0002-1050-4056 FU UK Science and Technology Facilities Council on the island of La Palma in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias; Gemini Observatory; National Science Foundation [AST-0507475, AST-0907903]; Clay Fellowship FX This Letter includes data gathered with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile; the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the Nordic Optical Telescope, operated by Denmark, Finland, Iceland, Norway, and Sweden; the Liverpool Telescope operated by the Liverpool John Moores University with financial support from the UK Science and Technology Facilities Council on the island of La Palma in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias; and the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation.; G.N. is supported by NSF award AST-0507475. R.J.F. is supported by a Clay Fellowship. Supernova research at Harvard is supported by NSF grant AST-0907903. NR 32 TC 26 Z9 26 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2011 VL 731 IS 1 AR L11 DI 10.1088/2041-8205/731/1/L11 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KQ UT WOS:000293126600011 ER PT J AU Raymond, JC Vink, J Helder, EA de Laat, A AF Raymond, John C. Vink, J. Helder, E. A. de Laat, A. TI EFFECTS OF NEUTRAL HYDROGEN ON COSMIC-RAY PRECURSORS IN SUPERNOVA REMNANT SHOCK WAVES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; ISM: supernova remnants; shock waves ID BALMER-DOMINATED SHOCKS; SOLAR-WIND; NONRADIATIVE SHOCKS; CYGNUS LOOP; TEMPERATURE EQUILIBRATION; ACCELERATION EFFICIENCY; SN 1006; SN-1006; INSTABILITIES; TURBULENCE AB Many fast supernova remnant shocks show spectra dominated by Balmer lines. The Ha profiles have a narrow component explained by direct excitations and a thermally Doppler broadened component due to atoms that undergo charge exchange in the post-shock region. However, the standard model does not take into account the cosmic-ray shock precursor, which compresses and accelerates plasma ahead of the shock. In strong precursors with sufficiently high densities, the processes of charge exchange, excitation, and ionization will affect the widths of both narrow and broad line components. Moreover, the difference in velocity between the neutrals and the precursor plasma gives rise to frictional heating due to charge exchange and ionization in the precursor. In extreme cases, all neutrals can be ionized by the precursor. In this Letter we compute the ion and electron heating for a wide range of shock parameters, along with the velocity distribution of the neutrals that reach the shock. Our calculations predict very large narrow component widths for some shocks with efficient acceleration, along with changes in the broad-to-narrow intensity ratio used as a diagnostic for the electron-ion temperature ratio. Balmer lines may therefore provide a unique diagnostic of precursor properties. We show that heating by neutrals in the precursor can account for the observed Ha narrow component widths and that the acceleration efficiency is modest in most Balmer line shocks observed thus far. C1 [Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vink, J.; Helder, E. A.; de Laat, A.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu OI Raymond, John/0000-0002-7868-1622 FU NASA [GO-11184.01-A-R]; Netherlands Science Foundation (NWO) FX This work was carried out while J.C.R. was visiting the Astronomical Institute Utrecht as Minnaert Professor. It was supported by NASA grant GO-11184.01-A-R to the Smithsonian Astrophysical Observatory. J.V. and EH are supported by the VIDI grant awarded to J.V. by the Netherlands Science Foundation (NWO). NR 49 TC 22 Z9 22 U1 1 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 APR 10 PY 2011 VL 731 IS 1 AR L14 DI 10.1088/2041-8205/731/1/L14 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KQ UT WOS:000293126600014 ER PT J AU Abdo, AA Ackermann, M Ajello, M Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Carrigan, S Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Costamante, L Cutini, S Davis, DS Dermer, CD de Palma, F Digel, SW Silva, EDE Drell, PS Dubois, R Dumora, D Favuzzi, C Fegan, SJ Fortin, P Frailis, M Fuhrmann, L Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guillemot, L Guiriec, S Hadasch, D Hayashida, M Hays, E Horan, D Hughes, RE Itoh, R Johannesson, G Johnson, AS Johnson, TJ Johnson, WN Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Latronico, L Lee, SH Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Makeev, A Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Naumann-Godo, M Nestoras, I Nolan, PL Norris, JP Nuss, E Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reyes, LC Ripken, J Ritz, S Romani, RW Roth, M Sadrozinski, HFW Sanchez, D Sander, A Scargle, JD Sgro, C Shaw, MS Smith, PD Spandre, G Spinelli, P Strickman, MS Suson, DJ Takahashi, H Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Usher, TL Vandenbroucke, J Vasileiou, V Vilchez, N Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yang, Z Ylinen, T Ziegler, M Acciari, VA Aliu, E Arlen, T Aune, T Beilicke, M Benbow, W Bottcher, M Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Christiansen, JL Ciupik, L Cui, W Perez, ID Dickherber, R Errando, M Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McArthur, S McCann, A McCutcheon, M Moriarty, P Mukherjee, R Ong, RA Otte, AN Pandel, D Perkins, JS Pichel, A Pohl, M Quinn, J Ragan, K Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Senturk, GD Smith, AW Steele, D Swordy, SP Tesic, G Theiling, M Thibadeau, S Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Wood, M Villata, M Raiteri, CM Gurwell, MA Larionov, VM Kurtanidze, OM Aller, MF Lahteenmaki, A Chen, WP Berduygin, A Agudo, I Aller, HD Arkharov, AA Bach, U Bachev, R Beltrame, P Benitez, E Buemi, CS Dashti, J Calcidese, P Capezzali, D Carosati, D Da Rio, D Di Paola, A Diltz, C Dolci, M Dultzin, D Forne, E Gomez, JL Hagen-Thorn, VA Halkola, A Heidt, J Hiriart, D Hovatta, T Hsiao, HY Jorstad, SG Kimeridze, GN Konstantinova, TS Kopatskaya, EN Koptelova, E Leto, P Ligustri, R Lindfors, E Lopez, JM Marscher, AP Mommert, M Mujica, R Nikolashvili, MG Nilsson, K Palma, N Pasanen, M Roca-Sogorb, M Ros, JA Roustazadeh, P Sadun, AC Saino, J Sigua, LA Sillanaa, A Sorcia, M Takalo, LO Tornikoski, M Trigilio, C Turchetti, R Umana, G Belloni, T Blake, CH Bloom, JS Angelakis, E Fumagalli, M Hauser, M Prochaska, JX Riquelme, D Sievers, A Starr, DL Tagliaferri, G Ungerechts, H Wagner, S Zensus, JA AF Abdo, A. A. Ackermann, M. Ajello, M. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carrigan, S. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, Oe. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Costamante, L. Cutini, S. Davis, D. S. Dermer, C. D. de Palma, F. Digel, S. W. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Favuzzi, C. Fegan, S. J. Fortin, P. Frailis, M. Fuhrmann, L. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guillemot, L. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Horan, D. Hughes, R. E. Itoh, R. Johannesson, G. Johnson, A. S. Johnson, T. J. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lee, S. -H. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Makeev, A. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Naumann-Godo, M. Nestoras, I. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Panetta, J. H. Parent, D. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reyes, L. C. Ripken, J. Ritz, S. Romani, R. W. Roth, M. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Scargle, J. D. Sgro, C. Shaw, M. S. Smith, P. D. Spandre, G. Spinelli, P. Strickman, M. S. Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yang, Z. Ylinen, T. Ziegler, M. Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boettcher, M. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Christiansen, J. L. Ciupik, L. Cui, W. de la Calle Perez, I. Dickherber, R. Errando, M. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Moriarty, P. Mukherjee, R. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Senturk, G. Demet Smith, A. W. Steele, D. Swordy, S. P. Tesic, G. Theiling, M. Thibadeau, S. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Wood, M. Villata, M. Raiteri, C. M. Gurwell, M. A. Larionov, V. M. Kurtanidze, O. M. Aller, M. F. Laehteenmaeki, A. Chen, W. P. Berduygin, A. Agudo, I. Aller, H. D. Arkharov, A. A. Bach, U. Bachev, R. Beltrame, P. Benitez, E. Buemi, C. S. Dashti, J. Calcidese, P. Capezzali, D. Carosati, D. Da Rio, D. Di Paola, A. Diltz, C. Dolci, M. Dultzin, D. Forne, E. Gomez, J. L. Hagen-Thorn, V. A. Halkola, A. Heidt, J. Hiriart, D. Hovatta, T. Hsiao, H. -Y. Jorstad, S. G. Kimeridze, G. N. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Leto, P. Ligustri, R. Lindfors, E. Lopez, J. M. Marscher, A. P. Mommert, M. Mujica, R. Nikolashvili, M. G. Nilsson, K. Palma, N. Pasanen, M. Roca-Sogorb, M. Ros, J. A. Roustazadeh, P. Sadun, A. C. Saino, J. Sigua, L. A. Sillanaa, A. Sorcia, M. Takalo, L. O. Tornikoski, M. Trigilio, C. Turchetti, R. Umana, G. Belloni, T. Blake, C. H. Bloom, J. S. Angelakis, E. Fumagalli, M. Hauser, M. Prochaska, J. X. Riquelme, D. Sievers, A. Starr, D. L. Tagliaferri, G. Ungerechts, H. Wagner, S. Zensus, J. A. CA Fermi-LAT Collaboration VERITAS Collaboration GASP-WEBT Consortium TI MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING GAMMA-RAY BLAZAR 3C 66A IN 2008 OCTOBER (vol 726, pg 43, 2011) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. 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EM lreyes@kicp.uchicago.edu RI Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Agudo, Ivan/G-1701-2015; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Johannesson, Gudlaugur/O-8741-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Morselli, Aldo/G-6769-2011; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Funk, Stefan/B-7629-2015 OI Agudo, Ivan/0000-0002-3777-6182; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Johannesson, Gudlaugur/0000-0003-1458-7036; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; giglietto, nicola/0000-0002-9021-2888; Morselli, Aldo/0000-0002-7704-9553; Reimer, Olaf/0000-0001-6953-1385; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Torres, Diego/0000-0002-1522-9065; Funk, Stefan/0000-0002-2012-0080 NR 2 TC 3 Z9 3 U1 0 U2 13 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 APR 10 PY 2011 VL 731 IS 1 AR 77 DI 10.1088/0004-637X/731/1/77 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800077 ER PT J AU Chiar, JE Pendleton, YJ Allamandola, LJ Boogert, ACA Ennico, K Greene, TP Geballe, TR Keane, JV Lada, CJ Mason, RE Roellig, TL Sandford, SA Tielens, AGGM Werner, MW Whittet, DCB Decin, L Eriksson, K AF Chiar, J. E. Pendleton, Y. J. Allamandola, L. J. Boogert, A. C. A. Ennico, K. Greene, T. P. Geballe, T. R. Keane, J. V. Lada, C. J. Mason, R. E. Roellig, T. L. Sandford, S. A. Tielens, A. G. G. M. Werner, M. W. Whittet, D. C. B. Decin, L. Eriksson, K. TI ICES IN THE QUIESCENT IC 5146 DENSE CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; dust, extinction; infrared: ISM; ISM: individual objects (IC 5146); ISM: molecules ID TAURUS DARK CLOUDS; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; DIFFUSE INTERSTELLAR-MEDIUM; SOLID CARBON-MONOXIDE; 3 MICRON SPECTRA; INFRARED-SPECTROSCOPY; MOLECULAR-CLOUD; ABSORPTION FEATURES; ABSOLUTE CALIBRATION AB This paper presents spectra in the 2 to 20 mu m range of quiescent cloud material located in the IC 5146 cloud complex. The spectra were obtained with NASA's Infrared Telescope Facility SpeX instrument and the Spitzer Space Telescope's Infrared Spectrometer. We use these spectra to investigate dust and ice absorption features in pristine regions of the cloud that are unaltered by embedded stars. We find that the H2O-ice threshold extinction is 4.03 +/- 0.05 mag. Once foreground extinction is taken into account, however, the threshold drops to 3.2 mag, equivalent to that found for the Taurus dark cloud, generally assumed to be the touchstone quiescent cloud against which all other dense cloud and embedded young stellar object observations are compared. Substructure in the trough of the silicate band for two sources is attributed to CH3OH and NH3 in the ices, present at the similar to 2% and similar to 5% levels, respectively, relative to H2O-ice. The correlation of the silicate feature with the E(J-K) color excess is found to follow a much shallower slope relative to lines of sight that probe diffuse clouds, supporting the previous results by Chiar et al. C1 [Chiar, J. E.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94035 USA. [Pendleton, Y. J.; Allamandola, L. J.; Ennico, K.; Greene, T. P.; Roellig, T. L.; Sandford, S. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Boogert, A. C. A.] CALTECH, IPAC, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Geballe, T. R.; Mason, R. E.] No Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Keane, J. V.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tielens, A. G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Whittet, D. C. B.] Rensselaer Polytech Inst, New York Ctr Astrobiol, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. [Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Eriksson, K.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. RP Chiar, JE (reprint author), Carl Sagan Ctr, SETI Inst, 189 Bernardo Ave, Mountain View, CA 94035 USA. EM jchiar@seti.org RI Ennico, Kimberly/L-9606-2014; OI Whittet, Douglas/0000-0001-8539-3891 FU NASA [NNX07AK38G]; NASA's Astrobiology [811073.02.12.03]; Laboratory Astrophysics [09-APRA09-0019]; NASA Astrobiology Institute [NNA09DA80A]; Gemini Observatory; National Science Foundation FX This work is based (in part) on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided to J.E.C. by NASA through an award issued by JPL/Caltech and to Y.J.P., L.J.A., K. E., T. P. G., T. L. R., and S. A. S. by NASA. L.J.A. gratefully acknowledges support from NASA's Astrobiology (grant 811073.02.12.03) and Laboratory Astrophysics (grant 09-APRA09-0019) programs. D. C. B. W. is grateful to the NASA Exobiology and Evolutionary Biology Program (grant NNX07AK38G) and the NASA Astrobiology Institute (grant NNA09DA80A) for financial support. R. E. M. and T. R. G. are supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, the United Kingdom, and the United States of America. The work is also based in part on observations made at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NCC 5-538 with the National Aeronautics and Space Administration, Science Mission Directorate, and Planetary Astronomy Program. 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 79 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 APR 10 PY 2011 VL 731 IS 1 AR 9 DI 10.1088/0004-637X/731/1/9 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800009 ER PT J AU Cowan, NB Robinson, T Livengood, TA Deming, D Agol, E A'Hearn, MF Charbonneau, D Lisse, CM Meadows, VS Seager, S Shields, AL Wellnitz, DD AF Cowan, Nicolas B. Robinson, Tyler Livengood, Timothy A. Deming, Drake Agol, Eric A'Hearn, Michael F. Charbonneau, David Lisse, Carey M. Meadows, Victoria S. Seager, Sara Shields, Aomawa L. Wellnitz, Dennis D. TI ROTATIONAL VARIABILITY OF EARTH'S POLAR REGIONS: IMPLICATIONS FOR DETECTING SNOWBALL PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: analytical; methods: numerical; methods: observational; planets and satellites: individual (Earth); techniques: photometric ID GENERAL-CIRCULATION MODEL; EXTRASOLAR PLANETS; LIGHT-CURVES; PHOTOMETRIC VARIABILITY; EXOPLANETS; ALBEDO; OCEAN; SPECTRUM; CLIMATE; SURFACE AB We have obtained the first time-resolved, disk-integrated observations of Earth's poles with the Deep Impact spacecraft as part of the EPOXI mission of opportunity. These data mimic what we will see when we point next-generation space telescopes at nearby exoplanets. We use principal component analysis (PCA) and rotational light curve inversion to characterize color inhomogeneities and map their spatial distribution from these unusual vantage points, as a complement to the equatorial views presented by Cowan et al. in 2009. We also perform the same PCA on a suite of simulated rotational multi-band light curves from NASA's Virtual Planetary Laboratory three-dimensional spectral Earth model. This numerical experiment allows us to understand what sorts of surface features PCA can robustly identify. We find that the EPOXI polar observations have similar broadband colors as the equatorial Earth, but with 20%-30% greater apparent albedo. This is because the polar observations are most sensitive to mid-latitudes, which tend to be more cloudy than the equatorial latitudes emphasized by the original EPOXI Earth observations. The cloudiness of the mid-latitudes also manifests itself in the form of increased variability at short wavelengths in the polar observations and as a dominant gray eigencolor in the south polar observation. We construct a simple reflectance model for a snowball Earth. By construction, our model has a higher Bond albedo than the modern Earth; its surface albedo is so high that Rayleigh scattering does not noticeably affect its spectrum. The rotational color variations occur at short wavelengths due to the large contrast between glacier ice and bare land in those wavebands. Thus, we find that both the broadband colors and diurnal color variations of such a planet would be easily distinguishable from the modern-day Earth, regardless of viewing angle. C1 [Cowan, Nicolas B.] Northwestern Univ, Evanston, IL 60208 USA. [Robinson, Tyler; Agol, Eric; Meadows, Victoria S.; Shields, Aomawa L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Robinson, Tyler; Agol, Eric; Meadows, Victoria S.; Shields, Aomawa L.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA. [Livengood, Timothy A.; Deming, Drake] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [A'Hearn, Michael F.; Wellnitz, Dennis D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Dept Phys, Cambridge, MA 02139 USA. RP Cowan, NB (reprint author), Northwestern Univ, 2131 Tech Dr, Evanston, IL 60208 USA. EM n-cowan@northwestern.edu RI Wellnitz, Dennis/B-4080-2012; Livengood, Timothy/C-8512-2012; Agol, Eric/B-8775-2013; Lisse, Carey/B-7772-2016; OI Agol, Eric/0000-0002-0802-9145; Lisse, Carey/0000-0002-9548-1526; Charbonneau, David/0000-0002-9003-484X FU NASA; National Science Foundation FX This work was supported by the NASA Discovery Program. We thank D. S. Abbot and R. T. Pierrehumbert for providing us with cloud maps of snowball Earth. N.B.C. acknowledges many useful discussions with S. G. Warren about snowball Earth, and thanks W. Sullivan for encouraging him to complete his astrobiology research rotation. E.A. is supported by a National Science Foundation Career Grant. NR 53 TC 22 Z9 22 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2011 VL 731 IS 1 AR 76 DI 10.1088/0004-637X/731/1/76 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800076 ER PT J AU Lal, DV Shastri, P Gabuzda, DC AF Lal, Dharam V. Shastri, Prajval Gabuzda, Denise C. TI SEYFERT GALAXIES: NUCLEAR RADIO STRUCTURE AND UNIFICATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: Seyfert; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; JET-INDUCED VELOCITIES; NARROW-LINE REGION; SPECTRAL ENERGY-DISTRIBUTIONS; STARBURST-AGN CONNECTION; STAR-FORMATION HISTORY; BRIGHT QUASAR SURVEY; H-ALPHA-EMISSION; NGC 4151 AB A radio study of a carefully selected sample of 20 Seyfert galaxies that are matched in orientation-independent parameters, which are measures of intrinsic active galactic nucleus power and host galaxy properties, is presented to test the predictions of the unified scheme hypothesis. Our sample sources have core flux densities greater than 8 mJy at 5 GHz on arcsec scales due to the feasibility requirements. These simultaneous parsec-scale and kiloparsec-scale radio observations reveal (1) that Seyfert 1 and Seyfert 2 galaxies have an equal tendency to show compact radio structures on milliarcsecond scales, (2) the distributions of parsec-scale and kiloparsec-scale radio luminosities are similar for both Seyfert 1 and Seyfert 2 galaxies, (3) there is no evidence for relativistic beaming in Seyfert galaxies, (4) similar distributions of source spectral indices in spite of the fact that Seyferts show nuclear radio flux density variations, and (5) the distributions of the projected linear size for Seyfert 1 and Seyfert 2 galaxies are not significantly different as would be expected in the unified scheme. The latter could be mainly due to a relatively large spread in the intrinsic sizes. We also find that a starburst alone cannot power these radio sources. Finally, an analysis of the kiloparsec-scale radio properties of the CfA Seyfert galaxy sample shows results consistent with the predictions of the unified scheme. C1 [Lal, Dharam V.; Shastri, Prajval] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Lal, Dharam V.] Indian Inst Sci, Dept Phys, Joint Astron Programme, Bangalore 560012, Karnataka, India. [Lal, Dharam V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gabuzda, Denise C.] Univ Coll Cork, Dept Phys, Cork, Ireland. RP Lal, DV (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India. FU Department of Science and Technology, Government of India; Russian Academy of Sciences; Indian National Science Academy; European Commission [ECBFMGECT950012]; national research councils; Indo-Russian; NASA FX We thank the anonymous referee for her/his prompt review of the manuscript and for useful and detailed comments that lead to significant improvement of the paper. D. V. L. is grateful to L. Lanz for her grammatical corrections. This project was done with the financial support from the Indo-Russian International Long Term Programme of the Department of Science and Technology, Government of India and the Russian Academy of Sciences. Financial support in the initial phase from the Indian National Science Academy exchange programme is also acknowledged. D. V. L. acknowledges support from the Joint Institute for VLBI in Europe for a visit there. D. G. acknowledges support from the European Commission under TMR contract No. ECBFMGECT950012. The VLA and VLBA are operated by the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The European VLBI Network is a joint facility of European, Chinese, and other radio astronomy institutes funded by their national research councils. This research has made use of NASA's Astrophysics Data System bibliographic services, the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA, and the SIMBAD database, operated by CDS, Strasbourg, France. Part of this work was supported by the Indo-Russian, ILTP programme. NR 135 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2011 VL 731 IS 1 AR 68 DI 10.1088/0004-637X/731/1/68 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800068 ER PT J AU Lanz, L Bliss, A Kraft, RP Birkinshaw, M Lal, DV Forman, WR Jones, C Worrall, DM AF Lanz, Lauranne Bliss, Amelia Kraft, Ralph P. Birkinshaw, Mark Lal, Dharam V. Forman, William R. Jones, Christine Worrall, Diana M. TI THE INFRARED JET IN 3C 31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual ( NGC 383); galaxies: jets; infrared: galaxies ID RADIO GALAXY 3C-31; SPITZER-SPACE-TELESCOPE; X-RAY JET; CENTAURUS-A; MAGNETIC-FIELD; CHANDRA OBSERVATIONS; RELATIVISTIC MODELS; ELLIPTIC GALAXIES; EMISSION; ARRAY AB We report the detection of infrared emission from the jet of the nearby Fanaroff-Riley type I radio galaxy 3C 31. The jet was detected with the IRAC instrument on Spitzer at 4.5 mu m, 5.8 mu m, and 8.0 mu m out to 30 '' (13 kpc) from the nucleus. We measure radio, infrared, optical, and X-ray fluxes in three regions along the jet determined by the infrared and X-ray morphology. Radio through X-ray spectra in these regions demonstrate that the emission can be interpreted as synchrotron emission from a broken power-law distribution of electron energies. We find significant differences in the high-energy spectra with increasing distance from the nucleus. Specifically, the high-energy slope increases from 0.86 to 1.72 from 1 kpc to 12 kpc along the jet, and the spectral break likewise increases in frequency along the jet from tens to hundreds of GHz to similar to 20 THz. Thus, the ratio of IR-to-X-ray flux in the jet increases by at least an order of magnitude with increasing distance from the nucleus. We argue that these changes cannot simply be the result of spectral aging and that there is ongoing particle acceleration through this region of the jet. The effects of mass loading, turbulence, and jet deceleration, however these processes modify the jet flow in detail, must be causing a change in the electron energy distribution and the efficiency of particle acceleration. C1 [Lanz, Lauranne; Kraft, Ralph P.; Lal, Dharam V.; Forman, William R.; Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bliss, Amelia; Birkinshaw, Mark; Worrall, Diana M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. RP Lanz, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM llanz@head.cfa.harvard.edu OI Lanz, Lauranne/0000-0002-3249-8224 FU Smithsonian Institution; Chandra X-ray Center; NASA [NNX07AQ18G]; Harvard College Observatory FX This work was based on archival data obtained from the Spitzer Science Archive, the Chandra Data Archive, and the Multimission Archive at STScI. This work was supported in part by the Smithsonian Institution, the Chandra X-ray Center, NASA contract NNX07AQ18G, and the Harvard College Observatory. NR 42 TC 3 Z9 3 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 APR 10 PY 2011 VL 731 IS 1 AR 52 DI 10.1088/0004-637X/731/1/52 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800052 ER PT J AU Lovchinsky, I Slane, P Gaensler, BM Hughes, JP Ng, CY Lazendic, JS Gelfand, JD Brogan, CL AF Lovchinsky, I. Slane, P. Gaensler, B. M. Hughes, J. P. Ng, C-Y. Lazendic, J. S. Gelfand, J. D. Brogan, C. L. TI A CHANDRA OBSERVATION OF SUPERNOVA REMNANT G350.1-0.3 AND ITS CENTRAL COMPACT OBJECT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G350.1-0.3); ISM: supernova remnants; stars: individual (XMMU J172054.5-372652); stars: neutron ID GALACTIC PLANE SURVEY; X-RAY-EMISSION; NEUTRON-STAR; PUPPIS-A; CATALOG; EVOLUTION; MIPSGAL AB We present a new Chandra observation of supernova remnant (SNR) G350.1-0.3. The high-resolution X-ray data reveal previously unresolved filamentary structures and allow us to perform detailed spectroscopy in the diffuse regions of this SNR. Spectral analysis demonstrates that the region of brightest emission is dominated by hot, metal-rich ejecta while the ambient material along the perimeter of the ejecta region and throughout the remnant's western half is mostly low-temperature, shocked interstellar/circumstellar medium with solar-type composition. The data reveal that the emission extends far to the west of the ejecta region and imply a lower limit of 6.6 pc on the diameter of the source (at a distance of 4.5 kpc). We show that G350.1-0.3 is likely in the free expansion (ejecta-dominated) stage and calculate an age of 600-1200 years. The derived relationship between the shock velocity and the electron/proton temperature ratio is found to be entirely consistent with that of other SNRs. We perform spectral fits on the X-ray source XMMU J172054.5-372652, a candidate central compact object (CCO), and find that its spectral properties fall within the typical range of other CCOs. We also present archival 24 mu m data of G350.1-0.3 taken with the Spitzer Space Telescope during the MIPSGAL galactic survey and find that the infrared and X-ray morphologies are well correlated. These results help to explain this remnant's peculiar asymmetries and shed new light on its dynamics and evolution. C1 [Lovchinsky, I.; Slane, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaensler, B. M.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Hughes, J. P.] Rutgers State Univ, Piscataway, NJ USA. [Ng, C-Y.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Lazendic, J. S.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Gelfand, J. D.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Brogan, C. L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Lovchinsky, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ilovchin@fas.harvard.edu; slane@cfa.harvard.edu; bryan.gaensler@sydney.edu.au; jph@physics.rutgers.edu; ncy@hep.physics.mcgill.ca; Jasmina.Lazendic-Galloway@monash.edu; jg168@astro.physics.nyu.edu; cbrogan@cv.nrao.edu RI Gaensler, Bryan/F-8655-2010; Ng, Chi Yung/A-7639-2013; Gelfand, Joseph/F-1110-2015; OI Ng, Chi Yung/0000-0002-5847-2612; Gelfand, Joseph/0000-0003-4679-1058; Gaensler, Bryan/0000-0002-3382-9558 FU Chandra grant [GO9-0059X]; NASA [NAS8-03060]; NSF [AST-0702957]; Australian Research Council [FF0561298] FX The authors thank Tea Temim and Daniel Castro for their input and several helpful discussions. I. L. acknowledges support from Chandra grant GO9-0059X. P.O.S. acknowledges partial support from NASA contract NAS8-03060. J.D.G is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0702957. B. M. G. acknowledges the support of the Australian Research Council through grant FF0561298. NR 25 TC 7 Z9 7 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2011 VL 731 IS 1 AR 70 DI 10.1088/0004-637X/731/1/70 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800070 ER PT J AU Mainzer, A Bauer, J Grav, T Masiero, J Cutri, RM Dailey, J Eisenhardt, P McMillan, RS Wright, E Walker, R Jedicke, R Spahr, T Tholen, D Alles, R Beck, R Brandenburg, H Conrow, T Evans, T Fowler, J Jarrett, T Marsh, K Masci, F McCallon, H Wheelock, S Wittman, M Wyatt, P DeBaun, E Elliott, G Elsbury, D Gautier, T Gomillion, S Leisawitz, D Maleszewski, C Micheli, M Wilkins, A AF Mainzer, A. Bauer, J. Grav, T. Masiero, J. Cutri, R. M. Dailey, J. Eisenhardt, P. McMillan, R. S. Wright, E. Walker, R. Jedicke, R. Spahr, T. Tholen, D. Alles, R. Beck, R. Brandenburg, H. Conrow, T. Evans, T. Fowler, J. Jarrett, T. Marsh, K. Masci, F. McCallon, H. Wheelock, S. Wittman, M. Wyatt, P. DeBaun, E. Elliott, G. Elsbury, D. Gautier, T. Gomillion, S. Leisawitz, D. Maleszewski, C. Micheli, M. Wilkins, A. TI PRELIMINARY RESULTS FROM NEOWISE: AN ENHANCEMENT TO THE WIDE-FIELD INFRARED SURVEY EXPLORER FOR SOLAR SYSTEM SCIENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; comets: general; minor planets, asteroids: general; surveys ID NEAR-EARTH ASTEROIDS; JOVIAN TROJAN ASTEROIDS; DUST TRAILS; SIZE DISTRIBUTIONS; PERIOD COMETS; OORT CLOUD; ORIGIN; MISSION; OBJECTS; IRAS AB The Wide-field Infrared Survey Explorer (WISE) has surveyed the entire sky at four infrared wavelengths with greatly improved sensitivity and spatial resolution compared to its predecessors, the Infrared Astronomical Satellite and the Cosmic Background Explorer. NASA's Planetary Science Division has funded an enhancement to the WISE data processing system called "NEOWISE" that allows detection and archiving of moving objects found in the WISE data. NEOWISE has mined the WISE images for a wide array of small bodies in our solar system, including near-Earth objects (NEOs), Main Belt asteroids, comets, Trojans, and Centaurs. By the end of survey operations in 2011 February, NEOWISE identified over 157,000 asteroids, including more than 500 NEOs and similar to 120 comets. The NEOWISE data set will enable a panoply of new scientific investigations. C1 [Mainzer, A.; Bauer, J.; Masiero, J.; Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bauer, J.; Cutri, R. M.; Dailey, J.; Alles, R.; Beck, R.; Brandenburg, H.; Conrow, T.; Evans, T.; Fowler, J.; Jarrett, T.; Marsh, K.; Masci, F.; McCallon, H.; Wheelock, S.; Wittman, M.; Wyatt, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Grav, T.] Johns Hopkins Univ, Dept Astron, Baltimore, MD USA. [McMillan, R. S.; Maleszewski, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Wright, E.] UCLA Astron, Los Angeles, CA 90095 USA. [Walker, R.] Monterey Inst Res Astron, Monterey, CA USA. [Jedicke, R.; Tholen, D.; Elliott, G.; Micheli, M.] 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, 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. [Leisawitz, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM amainzer@jpl.nasa.gov OI Masiero, Joseph/0000-0003-2638-720X; Micheli, Marco/0000-0001-7895-8209 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 WISE, 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 appreciate the contributions of the referee, J. Emery, which greatly improved the manuscript. 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. We thank the Auton Lab of Carnegie Mellon University for use of their libraries, and the PanSTARRS project for MOPS. NR 80 TC 138 Z9 138 U1 1 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 APR 10 PY 2011 VL 731 IS 1 AR 53 DI 10.1088/0004-637X/731/1/53 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800053 ER PT J AU Mingo, B Hardcastle, MJ Croston, JH Evans, DA Hota, A Kharb, P Kraft, RP AF Mingo, B. Hardcastle, M. J. Croston, J. H. Evans, D. A. Hota, A. Kharb, P. Kraft, R. P. TI MARKARIAN 6: SHOCKING THE ENVIRONMENT OF AN INTERMEDIATE SEYFERT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Markarian 6); galaxies: jets; shock waves; X-rays: galaxies ID EARLY-TYPE GALAXIES; ACTIVE GALACTIC NUCLEI; X-RAY-ABSORPTION; XMM-NEWTON OBSERVATIONS; RADIO GALAXIES; LOW-LUMINOSITY; EMISSION-LINE; CENTAURUS-A; NGC 6764; HOT GAS AB Markarian 6 is a nearby (D similar to 78 Mpc) Seyfert 1.5, early-type galaxy, with a double set of radio bubbles. The outer set spans similar to 7.5 kpc and is expanding into the halo regions of the host galaxy. We present an analysis of our new Chandra observation, together with archival XMM-Newton data, to look for evidence of emission from shocked gas around the external radio bubbles, both from spatially resolved regions in Chandra and from spectral analysis of the XMM-Newton data. We also look for evidence of a variable absorbing column along our line of sight to Mrk 6, to explain the evident differences seen in the active galactic nucleus (AGN) spectra from the various, non-contemporaneous, observations. We find that the variable absorption hypothesis explains the differences between the Chandra and XMM-Newton spectra, with the Chandra spectrum being heavily absorbed. The intrinsic N(H) varies from similar to 8 x 10(21) atoms cm(-2) to similar to 3 x 10(23) atoms cm(-2) on short timescales (2-6 years). The past evolution of the source suggests this is probably caused by a clump of gas close to the central AGN, passing in front of us at the moment of the observation. Shells of thermal X-ray emission are detected around the radio bubbles, with a temperature of similar to 0.9 keV. We estimate a temperature of similar to 0.2 keV for the external medium using luminosity constraints from our Chandra image. We analyze these results using the Rankine-Hugoniot shock jump conditions, and obtain a Mach number of similar to 3.9, compatible with a scenario in which the gas in the shells is inducing a strong shock in the surrounding interstellar medium (ISM). This could be the third clear detection of strong shocks produced by a radio-powerful Seyfert galaxy. These results are compatible with previous findings on Centaurus A and NGC 3801, supporting a picture in which these AGN-driven outflows play an important role in the environment and evolution of the host galaxy. C1 [Mingo, B.; Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1SJ, Hants, England. [Evans, D. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hota, A.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Kharb, P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Kraft, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mingo, B (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 FU University of Hertfordshire; Royal Society; South-East Physics Network (SEPNet); NASA [GO9-0117X]; ESA Member States FX B.M. thanks the University of Hertfordshire for a PhD studentship. M.J.H. thanks the Royal Society for a research fellowship. J.H.C acknowledges support from the South-East Physics Network (SEPNet). This work was partially supported by NASA grant GO9-0117X. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. It has also made use of new data from Chandra and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. We thank the anonymous referee for the useful comments. NR 55 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2011 VL 731 IS 1 AR 21 DI 10.1088/0004-637X/731/1/21 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800021 ER PT J AU Samuele, R McNamara, BR Vikhlinin, A Mullis, CR AF Samuele, R. McNamara, B. R. Vikhlinin, A. Mullis, C. R. TI EVIDENCE FOR RAPID REDSHIFT EVOLUTION OF STRONG CLUSTER COOLING FLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: jets; X-rays: galaxies: clusters ID X-RAY-CLUSTERS; STAR-FORMATION; GALAXY CLUSTERS; MOLECULAR GAS; EMISSION; CATALOG; SAMPLE; CORES; SPECTROSCOPY; THRESHOLD AB We present equivalent widths of the [OII]lambda 3727 and H alpha nebular emission lines for 77 brightest cluster galaxies (BCGs) selected from the 160 Square Degree ROSAT X-ray survey. We find no [OII]lambda 3727 or H alpha emission stronger than -15 angstrom or -5 angstrom, respectively, in any BCG. The corresponding emission-line luminosities lie below L similar to 6 x 10(40) erg s(-1), which is a factor of 30 below that of NGC 1275 in the Perseus Cluster. A comparison to the detection frequency of nebular emission in BCGs at z less than or similar to 0.35 drawn from the Brightest Cluster Survey indicates that we should have detected roughly one dozen emission-line galaxies, assuming that the two surveys are selecting similar clusters in the X-ray luminosity range 10(42) erg s(-1) to 5 x 10(44) erg s(-1). The absence of luminous nebular emission (i.e., Perseus-like systems) in our sample is consistent with an increase in the number density of strong cooling flow (cooling core) clusters between z = 0.5 and today. The decline in their numbers at higher redshift could be due to cluster mergers and heating by active galactic nuclei. C1 [Samuele, R.] Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA. [McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [McNamara, B. R.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mullis, C. R.] European So Observ, D-85748 Garching, Germany. RP Samuele, R (reprint author), Northrop Grumman Aerosp Syst, 1 Space Pk, Redondo Beach, CA 90278 USA. EM mcnamara@uwaterloo.ca FU Canada's Natural Sciences and Engineering Research Council FX B.R.M. and R. S. acknowledge Ohio University's Astrophysical Institute for its hospitality while much of the data analysis was performed in pursuit of R.S.'s master's thesis. B. R. M. acknowledges conversations with Alastair Edge, Megan Donahue, Paul Nulsen, Andy Fabian, and a generous grant from Canada's Natural Sciences and Engineering Research Council. NR 31 TC 19 Z9 19 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 APR 10 PY 2011 VL 731 IS 1 AR 31 DI 10.1088/0004-637X/731/1/31 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800031 ER PT J AU Schmelz, JT Jenkins, BS Worley, BT Anderson, DJ Pathak, S Kimble, JA AF Schmelz, J. T. Jenkins, B. S. Worley, B. T. Anderson, D. J. Pathak, S. Kimble, J. A. TI ISOTHERMAL AND MULTITHERMAL ANALYSIS OF CORONAL LOOPS OBSERVED WITH AIA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: fundamental parameters; Sun: UV radiation ID X-RAY TELESCOPE; EUV IMAGING SPECTROMETER; ACTIVE-REGION LOOPS; SOLAR CORONA; TEMPERATURE; EMISSION; HINODE; ANGSTROM; FILTER; EIT AB The coronal filters in the Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory peak at different temperatures; the series covers the entire active region temperature range, making AIA ideal for multithermal analysis. Here, we analyze coronal loops from several active regions that have been observed by AIA. We have specifically targeted cool loops (or at least loops with a cool component) that were chosen in the 171 angstrom channel of AIA, which has a peak response temperature of log T = 5.8. We wanted to determine if the loops could be described as isothermal or multithermal. We find that several of our 12 loops have narrow temperature distributions, which may be consistent with isothermal plasma; these can be modeled with a single flux tube. Other loops have intermediate-width temperature distributions, appear well-constrained, and should be multi-stranded. The remaining loops, however, have unrealistically broad differential emission measures. We find that this problem is the result of missing low-temperature lines in the AIA 131 angstrom channel. If we repeat the analysis without the 131 angstrom data, these loops also appear to be well-constrained and multi-stranded. C1 [Schmelz, J. T.; Jenkins, B. S.; Worley, B. T.; Anderson, D. J.; Pathak, S.; Kimble, J. A.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Schmelz, J. T.] 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 FX We thank Nancy Brickhouse, Steve Saar, and Mark Weber of SAO for help with the AIA data, and University of Memphis undergraduate physics major, Brinkley Mathews, for assistance. 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. We also benefitted from discussions at the Coronal Loops Workshops held in Paris (2002 November), Palermo (2004 September), Santorini (2007 June), and Florence (2009 June). NR 24 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2011 VL 731 IS 1 AR 49 DI 10.1088/0004-637X/731/1/49 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800049 ER PT J AU Sesar, B Juric, M Ivezic, Z AF Sesar, Branimir Juric, Mario Ivezic, Zeljko TI THE SHAPE AND PROFILE OF THE MILKY WAY HALO AS SEEN BY THE CANADA-FRANCE-HAWAII TELESCOPE LEGACY SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: stellar content; Galaxy: structure; stars: statistics ID DIGITAL SKY SURVEY; SAGITTARIUS DWARF GALAXY; STELLAR HALOS; SDSS; CALIBRATION; TOMOGRAPHY; METALLICITY; KINEMATICS; MEGACAM; SYSTEM AB We use Canada-France-Hawaii Telescope Legacy Survey data for 170 deg(2), recalibrated and transformed to the Sloan Digital Sky Survey ugri photometric system, to study the distribution of near-turnoff main-sequence stars in the Galactic halo along four lines of sight to heliocentric distances of similar to 35 kpc. We find that the halo stellar number density profile becomes steeper at Galactocentric distances greater than R-gal similar to 28 kpc, with the power-law index changing from n(inner) = -2.62 +/- 0.04 to n(outer) = -3.8 +/- 0.1. In particular, we test a series of single power-law models and find them to be strongly disfavored by the data. The parameters for the best-fit Einasto profile are n = 2.2 +/- 0.2 and R-e = 22.2 +/- 0.4 kpc. We measure the oblateness of the halo to be q equivalent to c/a = 0.70 +/- 0.01 and detect no evidence of it changing across the range of probed distances. The Sagittarius stream is detected in the l = 173 degrees and b = -62 degrees direction as an overdensity of [Fe/H] similar to -1.5 dex stars at R-gal similar to 32 kpc, providing a new constraint for the Sagittarius stream and dark matter halo models. We also detect the Monoceros stream as an overdensity of [Fe/H] > -1.5 dex stars in the l = 232 degrees and b = 26 degrees direction at R-gal less than or similar to 25 kpc. In the two sight lines where we do not detect significant substructure, the median metallicity is found to be independent of distance within systematic uncertainties ([Fe/H] similar to -1.5 +/- 0.1 dex). C1 [Sesar, Branimir; Ivezic, Zeljko] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Sesar, Branimir] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Juric, Mario] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ivezic, Zeljko] Univ Zagreb, Dept Phys, Zagreb 41000, Croatia. RP Sesar, B (reprint author), Univ Washington, Dept Astron, POB 351580, Seattle, WA 98195 USA. EM bsesar@astro.caltech.edu FU NSF [AST-0908139, AST-1009987, AST-0707901, AST-1008784, AST-0551161]; Croatian National Science Foundation [O-1548-2009]; NASA through Space Telescope Science Institute [HF-51255.01-A, NAS 5-26555]; NASA FX B. S. thanks NSF grant AST-0908139 to J. G. Cohen and NSF grant AST-1009987 to S. R. Kulkarni for partial support.. Z.I. acknowledges support by NSF grants AST-0707901 and AST-1008784 to the University of Washington, by NSF grant AST-0551161 to LSST for design and development activity, and by the Croatian National Science Foundation grant O-1548-2009. M. J. acknowledges support by NASA through Hubble Fellowship grant HF-51255.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Partial support for this work was provided by NASA through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. NR 41 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 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2011 VL 731 IS 1 AR 4 DI 10.1088/0004-637X/731/1/4 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800004 ER PT J AU Smith, BD Hallman, EJ Shull, JM O'Shea, BW AF Smith, Britton D. Hallman, Eric J. Shull, J. Michael O'Shea, Brian W. TI THE NATURE OF THE WARM/HOT INTERGALACTIC MEDIUM. I. NUMERICAL METHODS, CONVERGENCE, AND O VI ABSORPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; intergalactic medium; quasars: absorption lines ID STAR-FORMATION HISTORY; COLD DARK-MATTER; INITIAL MASS FUNCTION; N-BODY SIMULATIONS; LY-ALPHA FOREST; LOW-REDSHIFT; COSMOLOGICAL SIMULATIONS; PHYSICAL CONDITIONS; PRIMORDIAL NUCLEOSYNTHESIS; NONEQUILIBRIUM IONIZATION AB We perform a series of cosmological simulations using Enzo, an Eulerian adaptive-mesh refinement, N-body + hydrodynamical code, applied to study the warm/hot intergalactic medium (WHIM). The WHIM may be an important component of the baryons missing observationally at low redshift. We investigate the dependence of the global star formation rate and mass fraction in various baryonic phases on spatial resolution and methods of incorporating stellar feedback. Although both resolution and feedback significantly affect the total mass in the WHIM, all of our simulations find that the WHIM fraction peaks at z similar to 0.5, declining to 35%-40% at z = 0. We construct samples of synthetic O (VI) absorption lines from our highest-resolution simulations, using several models of oxygen ionization balance. Models that include both collisional ionization and photoionization provide excellent fits to the observed number density of absorbers per unit redshift over the full range of column densities (10(13) cm(-2) less than or similar to N-O (VI) less than or similar to 10(15) cm(-2)). Models that include only collisional ionization provide better fits for high column density absorbers (N-O (VI) less than or similar to 10(14) cm(-2)). The distribution of O (VI) in density and temperature exhibits two populations: one at T similar to 10(5.5) K (collisionally ionized, 55% of total O (VI)) and one at T similar to 10(4.5) K (photoionized, 37%) with the remainder located in dense gas near galaxies. While not a perfect tracer of hot gas, O (VI) provides an important tool for a WHIM baryon census. C1 [Smith, Britton D.; Hallman, Eric J.; Shull, J. Michael] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [O'Shea, Brian W.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Hallman, Eric J.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Smith, BD (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, 389 UCB, Boulder, CO 80309 USA. EM britton.smith@colorado.edu; michael.shull@colorado.edu FU University of Colorado (NASA) [NNZ07-AG77G]; University of Colorado (NSF) [AST-0707474]; NSF [AST-0702923, AR-12131]; NASA ATFP [NNX09-AD80G] FX We are grateful to the anonymous referee for comments that considerably strengthened the paper. We thank Charles Danforth, Brian Keeney, Devin Silvia, Sam Skillman, and Matthew Turk for helpful discussions, Andrew Hopkins for kindly providing the data from Hopkins & Beacom (2006), and Stephen Wilkins for assisting us with data from Wilkins et al. (2008). This work was supported by the Astrophysics Theory Program at the University of Colorado (NASA grant NNZ07-AG77G and NSF grant AST-0707474). E.J.H. was supported by NSF AAPF grant AST-0702923 and HST grant AR-12131. B.W.O. was supported in part by NASA ATFP grant NNX09-AD80G. 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. The simulations were performed on NICS Kraken and TACC Ranger, with computing time from Teragrid allocations TG-AST090040 and TG-AST100004. NR 78 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 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2011 VL 731 IS 1 AR 6 DI 10.1088/0004-637X/731/1/6 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800006 ER PT J AU Stute, M Luna, GJM Sokoloski, JL AF Stute, Matthias Luna, Gerardo J. M. Sokoloski, Jennifer L. TI DETECTION OF X-RAYS FROM THE SYMBIOTIC STAR V1329 Cyg SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: symbiotic; ISM: jets and outflows; stars: individual (V1329 Cyg=HBV 475); white dwarfs; X-rays: stars ID RED GIANTS; R-AQUARII; CH-CYGNI; HYDRODYNAMICAL SIMULATIONS; CHEMICAL-COMPOSITION; JET ACTIVITY; HBV 475; EMISSION; NOVAE; HBV-475 AB We report the detection of X-ray emission from the symbiotic star V1329 Cyg with XMM-Newton. The spectrum from the EPIC pn, MOS1, and MOS2 instruments consists of a two-temperature plasma with k T-1 = 0.11(-0.02)(+0.02) keV and k T-2 = 0.93(-0.14)(+0.12) keV. Unlike the vast majority of symbiotic stars detected in X-rays, the soft component of the spectrum seems to be absorbed only by interstellar material. The shock velocities corresponding to the observed temperatures are about 300 km s(-1) and about 900 km s(-1). We did not find either periodic or aperiodic X-ray variability, with upper limits on the amplitudes of such variations being 46% and 16% (rms), respectively. We also did not find any ultraviolet variability with an rms amplitude of more than approximately 1%. The derived velocities and the unabsorbed nature of the soft component of the X-ray spectrum suggest that some portion of the high energy emission could originate in shocks within a jet and beyond the symbiotic nebula. The lower velocity is consistent with the expansion velocity of the extended structure present in Hubble Space Telescope observations. The higher velocity could be associated with an internal shock at the base of the jet or with shocks in the accretion region. C1 [Stute, Matthias] Univ Tubingen, Inst Astron & Astrophys, Sect Computat Phys, D-72076 Tubingen, Germany. [Stute, Matthias] Univ Turin, Dipartimento Fis Gen A Avogadro, I-10125 Turin, Italy. [Luna, Gerardo J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sokoloski, Jennifer L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Stute, M (reprint author), Univ Tubingen, Inst Astron & Astrophys, Sect Computat Phys, Morgenstelle 10, D-72076 Tubingen, Germany. EM matthias.stute@tat.physik.uni-tuebingen.de FU ESA Member States; USA (NASA); NASA [NNX09AP88G, NNX10AK31G] FX M.S. wishes to thank Hans Martin Schmid for fruitful discussions. 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). We thank NASA for funding this work through XMM-Newton AO-8 awards NNX09AP88G to G.J.M.L. and J.L.S., and NNX10AK31G to J.L.S. We also acknowledge helpful comments and suggestions by an anonymous referee. 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 APR 10 PY 2011 VL 731 IS 1 AR 12 DI 10.1088/0004-637X/731/1/12 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 753KR UT WOS:000289772800012 ER PT J AU Olson, SL AF Olson, Storrs L. TI The fossil record and history of doves on Bermuda (Ayes: Columbidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Bahamas; extinction; Pleistocene; sea level rise; West Indies ID QUATERNARY DEPOSITS; PLEISTOCENE; AVES; POECILOZONITES; GEOCHRONOLOGY; RALLIDAE; GENUS AB Four bones of a dove from Bermuda are tentatively identified with the West Indian Zenaida Dove as cf. Zenaida aurita. These occur in deposits dating to about 55,000 to 28,000 years ago that formed during the last glacial period when the land area of Bermuda was much larger. At that time, the West Indies would have been a much more likely source area than eastern North America for dove as a potential colonist of Bermuda. The Bermuda dove appears to have been a resident and perhaps became extinct as a result of flooding of the Bermuda platform and reduction in land area during the present interglacial. The two doves found on Bermuda today (Mourning Dove Zenaida macroura and Common Ground Dove Columbina passerina) are absent in the fossil record and apparently did not become established on the island until after human settlement in the seventeenth century. C1 Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. RP Olson, SL (reprint author), Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, NHB MRC 116,POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 27 TC 2 Z9 2 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 8 PY 2011 VL 124 IS 1 BP 1 EP 6 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 753GH UT WOS:000289759800001 ER PT J AU Halfen, DT Clouthier, DJ Ziurys, LM Lattanzi, V McCarthy, MC Thaddeus, P Thorwirth, S AF Halfen, D. T. Clouthier, D. J. Ziurys, L. M. Lattanzi, V. McCarthy, M. C. Thaddeus, P. Thorwirth, S. TI The pure rotational spectrum of HPS ((X)over-tilde(1)A '): Chemical bonding in second-row elements SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; MATRIX IR INVESTIGATIONS; AB-INITIO CALCULATIONS; GAUSSIAN-BASIS SETS; MAIN-GROUP ELEMENTS; CIRCUMSTELLAR ENVELOPES; 2ND DERIVATIVES; EQUILIBRIUM STRUCTURE; PHOSPHORUS CHEMISTRY; MICROWAVE-SPECTRA AB The pure rotational spectrum of HPS, as well as its S-34 and D isotopologues, has been recorded at microwave, millimeter, and submillimeter wavelengths, the first observation of this molecule in the gas phase. The data were obtained using a combination of millimeter direct absorption, Fourier transform microwave (FTMW), and microwave-microwave double-resonance techniques, which cover the total frequency range from 15 to 419 GHz. Quantum chemical calculations at the B3LYP and CCSD(T) levels were also performed to aid in spectral identification. HPS was created in the direct absorption experiment from a mixture of elemental phosphorus, H2S, and Ar carrier gas; DPS was produced by adding D-2. In the FTMW study, these species were generated in a pulsed discharge nozzle from PH3 and H2S or D2S, diluted in neon. The spectra recorded for HPS and its isotopologues exhibit clear asymmetric top patterns indicating bent structures; phosphorus hyperfine splittings were also observed in HPS, but not DPS. Analysis of the data yielded rotation, centrifugal distortion, and phosphorus nuclear spin-rotation parameters for the individual species. The r(m)((1)) structure for HPS, calculated from the rotational constants, is r(H-P) = 1.438(1) angstrom, r(P-S) = 1.9320(1) angstrom, and theta(H-P-S) = 101.85(9)degrees. Empirically correcting for zero-point vibrational effects yields the geometry r(e)(H-P) = 1.4321(2) angstrom, r(e)(P-S) = 1.9287(1) angstrom, and theta(e)(H-P-S) = 101.78(1)degrees, in close agreement with the r(m)((1)) structure. A small inertial defect was found for HPS indicating a relatively rigid molecule. Based on these data, the bonding in this species is best represented as H-P=S, similar to the first-row analog HNO, as well as HNS and HPO. Therefore, substitution of phosphorus and sulfur for nitrogen and oxygen does not result in a dramatic structural change. (C) 2011 American Institute of Physics. [doi: 10.1063/1.3562374] C1 [Halfen, D. T.; Ziurys, L. M.] Univ Arizona, Dept Chem, Arizona Radio Observ, Tucson, AZ 85721 USA. [Halfen, D. T.; Ziurys, L. M.] Univ Arizona, Dept Astron, Arizona Radio Observ, Tucson, AZ 85721 USA. [Halfen, D. T.; Ziurys, L. M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Clouthier, D. J.] Univ Kentucky, Dept Chem, Lexington, KY 40506 USA. [Lattanzi, V.; McCarthy, M. C.; Thaddeus, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02318 USA. [Lattanzi, V.; McCarthy, M. C.; Thaddeus, P.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02318 USA. [Thorwirth, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Thorwirth, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Halfen, DT (reprint author), Univ Arizona, Dept Chem, Arizona Radio Observ, Tucson, AZ 85721 USA. RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; Halfen, DeWayne/0000-0003-2483-3616 FU NSF [AST 09-06534, CHE 07-01204]; NASA [NNX10AR83G, NNX08AE05G]; Deutsche Forschungsgemeinschaft [TH 1301/3-1] FX The work here was supported by the NSF Grant No. AST 09-06534 and NASA Exobiology Grant No. NNX10AR83G. D.J.C. also acknowledges NSF support. The work in Cambridge was supported by NSF Grant No. CHE 07-01204 and NASA Grant No. NNX08AE05G. S.T. is grateful to the Deutsche Forschungsgemeinschaft for a research Grant No. (TH 1301/3-1). NR 66 TC 13 Z9 13 U1 0 U2 8 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 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD APR 7 PY 2011 VL 134 IS 13 AR 134302 DI 10.1063/1.3562374 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 746OH UT WOS:000289256100014 PM 21476750 ER PT J AU Strobel, TA Goncharov, AF Seagle, CT Liu, ZX Somayazulu, M Struzhkin, VV Hemley, RJ AF Strobel, Timothy A. Goncharov, Alexander F. Seagle, Christopher T. Liu, Zhenxian Somayazulu, Maddury Struzhkin, Viktor V. Hemley, Russell J. TI High-pressure study of silane to 150 GPa SO PHYSICAL REVIEW B LA English DT Article ID SOLID HYDROGEN-SULFIDE; METALLIC HYDROGEN; INDUCED AMORPHIZATION; MOLECULAR-CRYSTALS; PHASE-TRANSITIONS; RAMAN-SPECTRA; SUPERCONDUCTIVITY; SI; EQUATION; SILICON AB We present an extensive study of the optical, electronic, and structural properties of silane (SiH(4)) to 150 GPa through the use of Raman spectroscopy, optical microscopy, synchrotron infrared reflectivity, optical absorption, and synchrotron x-ray diffraction measurements. To mitigate possible contamination from previously reported metal hydride formation, we performed experiments using gold-lined sample gaskets, finding molecular silane remains in the transparent and insulating P2(1)/c structure until similar to 40 GPa. Silane shows a partial loss of crystallinity above similar to 50 GPa and appears to visibly darken. The darkening is plausibly the result of a loss of molecular character with many enthalpically competitive pathways available, including decomposition, combined with the absorptive nature of the sample. Above 100 GPa we observed crystallization into structures partially consistent with the previously reported nonmolecular I (4) over bar 2d and I4(1)/a types. In the absence of decomposition, silane remains partially transparent and nonmetallic to at least 150 GPa with a band gap constrained between 0.6 and 1.8 eV. Under pressure, silane is sensitive to irradiation from x-rays and lasers, and may easily decompose into metallic silicon. We suggest that previous reports of metallization starting from molecular SiH(4) arise from decomposition, and superconductivity may originate from hydrogen-doped silicon. While silane may readily decompose, the inherent metastability provides access to a wide range of path-and sample-history-dependent states and suggests a unique range of physical properties for hydrogen-rich silicon alloys. C1 [Strobel, Timothy A.; Goncharov, Alexander F.; Seagle, Christopher T.; Liu, Zhenxian; Somayazulu, Maddury; Struzhkin, Viktor V.; Hemley, Russell J.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Seagle, Christopher T.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Strobel, TA (reprint author), Carnegie Inst Washington, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA. EM tstrobel@ciw.edu RI Struzhkin, Viktor/J-9847-2013 OI Struzhkin, Viktor/0000-0002-3468-0548 FU NSF-DMR [DMR-085056]; DOE/BES; DOE/NNSA (CDAC); U.S. Army Research Office [56122-CH-H]; National Science Foundation-Earth Sciences [EAR-0622171]; Department of Energy-Geosciences [DE-FG02-94ER14466]; DOE-NNSA; DOE-BES [DE-AC02-06CH11357]; COMPRES, the Consortium for Materials Properties Research in Earth Sciences, under NSF [EAR06-49658]; US DOE (CDAC) [DE-AC02-98CH10886] FX We acknowledge support from NSF-DMR (Grant No. DMR-085056), DOE/BES, DOE/NNSA (CDAC) and U.S. Army Research Office Grant No. 56122-CH-H. Portions of this work were performed at GeoSoilEnviroCARS (Sector 13), Advanced Photon Source (APS), Argonne National Laboratory. GeoSoilEnviroCARS is supported by the National Science Foundation-Earth Sciences (Grant No. EAR-0622171) and Department of Energy-Geosciences (Grant No. DE-FG02-94ER14466). Portions of this work were performed at HPCAT (Sector 16), Advanced Photon Source (APS), Argonne National Laboratory. HPCAT is supported by CIW, UNLV and LLNL through funding from DOE-NNSA, DOE-BES, and NSF. APS is supported by DOE-BES, under Contract No. DE-AC02-06CH11357. The U2A beamline is supported by COMPRES, the Consortium for Materials Properties Research in Earth Sciences, under NSF Cooperative Agreement Grant No. EAR06-49658 and the US DOE (CDAC, Contract No. DE-AC02-98CH10886). NR 83 TC 25 Z9 27 U1 6 U2 53 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD APR 7 PY 2011 VL 83 IS 14 AR 144102 DI 10.1103/PhysRevB.83.144102 PG 14 WC Physics, Condensed Matter SC Physics GA 746FT UT WOS:000289229200002 ER PT J AU Rowe, TB Sues, HD Reisz, RR AF Rowe, Timothy B. Sues, Hans-Dieter Reisz, Robert R. TI Dispersal and diversity in the earliest North American sauropodomorph dinosaurs, with a description of a new taxon SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Dinosauria; Sauropodomorpha; extinction; vicariance; dispersal; phylogeny ID ORNITHISCHIAN DINOSAURS; KAYENTA FORMATION; EARLY EVOLUTION; BIOGEOGRAPHY; PHYLOGENY; ORIGIN; CROCODYLIFORM; COMPETITION; VICARIANCE; RADIATION AB Sauropodomorph dinosaurs originated in the Southern Hemisphere in the Middle or Late Triassic and are commonly portrayed as spreading rapidly to all corners of Pangaea as part of a uniform Late Triassic to Early Jurassic cosmopolitan dinosaur fauna. Under this model, dispersal allegedly inhibited dinosaurian diversification, while vicariance and local extinction enhanced it. However, apomorphy-based analyses of the known fossil record indicate that sauropodomorphs were absent in North America until the Early Jurassic, reframing the temporal context of their arrival. We describe a new taxon from the Kayenta Formation of Arizona that comprises the third diagnosable sauropodomorph from the Early Jurassic of North America. We analysed its relationships to test whether sauropodomorphs reached North America in a single sweepstakes event or in separate dispersals. Our finding of separate arrivals by all three taxa suggests dispersal as a chief factor in dinosaurian diversification during at least the early Mesozoic. It questions whether a 'cosmopolitan' dinosaur fauna ever existed, and corroborates that vicariance, extinction and dispersal did not operate uniformly in time or under uniform conditions during the Mesozoic. Their relative importance is best measured in narrow time slices and circumscribed geographical regions. C1 [Rowe, Timothy B.] Univ Texas Austin, Jackson Sch Geosci, Austin, TX 78712 USA. [Rowe, Timothy B.] Univ Texas Austin, Vertebrate Paleontol Lab, Austin, TX 78712 USA. [Sues, Hans-Dieter] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Reisz, Robert R.] Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. RP Rowe, TB (reprint author), Univ Texas Austin, Jackson Sch Geosci, C1100, Austin, TX 78712 USA. EM rowe@mail.utexas.edu FU Jackson School of Geosciences; NSF [AToL 0531767] FX This research was funded by the Jackson School of Geosciences and NSF AToL 0531767. Nicola Wong Ken and Ken Dupuis prepared the specimen drawings in figures 3 and 4, respectively. We thank Paul Barrett, Sterling Nesbitt and several anonymous reviewers for improving the manuscript. We thank the Navajo Nation Minerals Division for granting collecting permits. Above all, we thank Elizabeth Gordon, who found the site, and the dozens of members of the vertebrate palaeontology communities at the University of Texas and at Harvard who helped in the arduous fieldwork, preparation and curation of this material. NR 49 TC 9 Z9 9 U1 0 U2 12 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD APR 7 PY 2011 VL 278 IS 1708 BP 1044 EP 1053 DI 10.1098/rspb.2010.1867 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 726BT UT WOS:000287694000012 PM 20926438 ER PT J AU Wurm, Y Wang, J Riba-Grognuz, O Corona, M Nygaard, S Hunt, BG Ingram, KK Falquet, L Nipitwattanaphon, M Gotzek, D Dijkstra, MB Oettler, J Comtesse, F Shih, CJ Wu, WJ Yang, CC Thomas, J Beaudoing, E Pradervand, S Flegel, V Cook, ED Fabbretti, R Stockinger, H Long, L Farmerie, WG Oakey, J Boomsma, JJ Pamilo, P Yi, SV Heinze, J Goodisman, MAD Farinelli, L Harshman, K Hulo, N Cerutti, L Xenarios, I Shoemaker, D Keller, L AF Wurm, Yannick Wang, John Riba-Grognuz, Oksana Corona, Miguel Nygaard, Sanne Hunt, Brendan G. Ingram, Krista K. Falquet, Laurent Nipitwattanaphon, Mingkwan Gotzek, Dietrich Dijkstra, Michiel B. Oettler, Jan Comtesse, Fabien Shih, Cheng-Jen Wu, Wen-Jer Yang, Chin-Cheng Thomas, Jerome Beaudoing, Emmanuel Pradervand, Sylvain Flegel, Volker Cook, Erin D. Fabbretti, Roberto Stockinger, Heinz Long, Li Farmerie, William G. Oakey, Jane Boomsma, Jacobus J. Pamilo, Pekka Yi, Soojin V. Heinze, Juergen Goodisman, Michael A. D. Farinelli, Laurent Harshman, Keith Hulo, Nicolas Cerutti, Lorenzo Xenarios, Ioannis Shoemaker, DeWayne Keller, Laurent TI The genome of the fire ant Solenopsis invicta SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE social insect; caste differences; nonmodel organism; de novo genome assembly ID DIFFERENTIAL GENE-EXPRESSION; HONEY-BEE; JUVENILE-HORMONE; APIS-MELLIFERA; DNA METHYLATION; CHEMORECEPTOR SUPERFAMILY; POPULATION-GENETICS; SEX DETERMINATION; WASP NASONIA; HYMENOPTERA AB Ants have evolved very complex societies and are key ecosystem members. Some ants, such as the fire ant Solenopsis invicta, are also major pests. Here, we present a draft genome of S. invicta, assembled from Roche 454 and Illumina sequencing reads obtained from a focal haploid male and his brothers. We used comparative genomic methods to obtain insight into the unique features of the S. invicta genome. For example, we found that this genome harbors four adjacent copies of vitellogenin. A phylogenetic analysis revealed that an ancestral vitellogenin gene first underwent a duplication that was followed by possibly independent duplications of each of the daughter vitellogenins. The vitellogenin genes have undergone subfunctionalization with queen-and worker-specific expression, possibly reflecting differential selection acting on the queen and worker castes. Additionally, we identified more than 400 putative olfactory receptors of which at least 297 are intact. This represents the largest repertoire reported so far in insects. S. invicta also harbors an expansion of a specific family of lipid-processing genes, two putative orthologs to the transformer/feminizer sex differentiation gene, a functional DNA methylation system, and a single putative telomerase ortholog. EST data indicate that this S. invicta telomerase ortholog has at least four spliceforms that differ in their use of two sets of mutually exclusive exons. Some of these and other unique aspects of the fire ant genome are likely linked to the complex social behavior of this species. C1 [Wurm, Yannick; Wang, John; Riba-Grognuz, Oksana; Corona, Miguel; Nipitwattanaphon, Mingkwan; Dijkstra, Michiel B.; Comtesse, Fabien; Keller, Laurent] Univ Lausanne, Dept Ecol & Evolut, CH-1015 Lausanne, Switzerland. [Wurm, Yannick; Riba-Grognuz, Oksana; Falquet, Laurent; Flegel, Volker; Fabbretti, Roberto; Stockinger, Heinz; Long, Li; Xenarios, Ioannis] Swiss Inst Bioinformat, Vital IT Grp, CH-1015 Lausanne, Switzerland. [Wang, John] Acad Sinica, Biodivers Res Ctr, Taipei 115, Taiwan. [Nygaard, Sanne; Boomsma, Jacobus J.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. [Hunt, Brendan G.; Cook, Erin D.; Yi, Soojin V.; Goodisman, Michael A. D.] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. [Ingram, Krista K.] Colgate Univ, Dept Biol, Hamilton, NY 13346 USA. [Gotzek, Dietrich] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Oettler, Jan; Heinze, Juergen] Univ Regensburg, D-93040 Regensburg, Germany. [Shih, Cheng-Jen; Wu, Wen-Jer; Yang, Chin-Cheng] Natl Taiwan Univ, Dept Entomol, Taipei 10617, Taiwan. [Thomas, Jerome; Beaudoing, Emmanuel; Pradervand, Sylvain; Harshman, Keith] Univ Lausanne, Lausanne Genom Technol Facil, CH-1015 Lausanne, Switzerland. [Farmerie, William G.] Univ Florida, Interdisciplinary Ctr Biotechnol Res, Gainesville, FL 32610 USA. [Oakey, Jane] Biosecur Queensland, Brisbane, Qld 4108, Australia. [Pamilo, Pekka] Univ Helsinki, Dept Biosci, FIN-00014 Helsinki, Finland. [Farinelli, Laurent] Fasteris SA, CH-1228 Plan Les Ouates, Switzerland. [Hulo, Nicolas; Cerutti, Lorenzo; Xenarios, Ioannis] Swiss Inst Bioinformat, CH-1211 Geneva, Switzerland. [Shoemaker, DeWayne] ARS, USDA, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA. RP Wurm, Y (reprint author), Univ Lausanne, Dept Ecol & Evolut, CH-1015 Lausanne, Switzerland. EM yannick.wurm@unil.ch RI Pamilo, Pekka/C-6907-2011; Hunt, Brendan/B-9816-2009; Falquet, Laurent/C-2541-2013; Nygaard, Sanne/M-2569-2014; Boomsma, Jacobus/M-2785-2014; Wurm, Yannick/A-9525-2009; OI Hunt, Brendan/0000-0002-0030-9302; Falquet, Laurent/0000-0001-8102-7579; Nygaard, Sanne/0000-0002-3002-6047; Boomsma, Jacobus/0000-0002-3598-1609; Xenarios, Ioannis/0000-0002-3413-6841; Wurm, Yannick/0000-0002-3140-2809; keller, laurent/0000-0002-5046-9953; Stockinger, Heinz/0000-0003-4666-7719 FU European Union [FP6 036894]; University of Lausanne; Rectorate of the University of Lausanne; ERC; Herbette Foundation; US Department of Agriculture Agriculture and Food Research Initiative Award [2009-35302-05301]; Infectigen grant; Academy of Finland [122210]; National Science Foundation [DEB-0640690, MCB-0950896, DEB-1011349]; Danish National Research Foundation; Bureau of Animal and Plant Health Inspection and Quarantine, Council of Agriculture, Executive Yuan, Taiwan [98AS-9.1.2BQ-B1(1)]; Swiss National Science Foundation [315230B-131083]; Picker Interdisciplinary Science Institute, Colgate University FX We thank Christophe Lucas and members of the Marc Robinson-Rechavi laboratory for advice and discussion; Catherine Berney and Christine La Mendola for help in the laboratory; Kenneth G. Ross (Department of Entomology, University of Georgia, Athens, GA), for providing the ants; Jerome Notari, Laelia Maumary, and Jezaelle Rufener for help rearing the ants; and Hugh M. Robertson for Pogonomyrmex olfactory receptor sequences. We thank Timothy Harkins, Pascal Bouffard, Linda Burton and 454 Life Sciences, a Roche Company (Branford, CT) for sequencer access, construction of 454 sequencing libraries and access to Newbler software, the Interdisciplinary Center for Biotechnology Research at the University of Florida for Roche 454 sequencing, and the Lausanne Genomic Technologies Facility and Fasteris SA for Illumina sequencing. This work was supported by grants from the European Union-funded Network of Excellence Lifespan FP6 036894, the Swiss National Science Foundation, the University of Lausanne, the Rectorate of the University of Lausanne, an ERC Advanced grant and the Herbette Foundation (to L. K.); US Department of Agriculture Agriculture and Food Research Initiative Award 2009-35302-05301 (to D. S. and J.W.); by an Infectigen grant (to L. K., D. S., and Y.W.); the Academy of Finland Grant 122210 (to P. P.); grants from the European Union-funded Network of Excellence Lifespan FP6 036894, the Swiss National Science Foundation, the University of Lausanne, and the Rectorate of the University of Lausanne (to L. K.); by National Science Foundation Grants DEB-0640690 (to M. A. D. G. and S.V.Y.), MCB-0950896 (to S.V.Y. and M. A. D. G.), and DEB-1011349 (to B. G. H., S.V.Y., and M. A. D. G.); by grants from the Danish National Research Foundation (to S.N. and J.J.B.); by Grant 98AS-9.1.2BQ-B1(1) from the Bureau of Animal and Plant Health Inspection and Quarantine, Council of Agriculture, Executive Yuan, Taiwan (to W.-J.W.); by the Swiss National Science Foundation project Grant 315230B-131083 (to L. C. and N.H.); and by the Picker Interdisciplinary Science Institute, Colgate University (K.K.I.). NR 71 TC 163 Z9 171 U1 4 U2 92 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 APR 5 PY 2011 VL 108 IS 14 BP 5679 EP 5684 DI 10.1073/pnas.1009690108 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 746RT UT WOS:000289265300039 PM 21282665 ER PT J AU Wiegmann, BM Trautwein, MD Winkler, IS Barr, NB Kim, JW Lambkin, C Bertone, MA Cassel, BK Bayless, KM Heimberg, AM Wheeler, BM Peterson, KJ Pape, T Sinclair, BJ Skevington, JH Blagoderov, V Caravas, J Kutty, SN Schmidt-Ott, U Kampmeier, GE Thompson, FC Grimaldi, DA Beckenbach, AT Courtney, GW Friedrich, M Meier, R Yeates, DK AF Wiegmann, Brian M. Trautwein, Michelle D. Winkler, Isaac S. Barr, Norman B. Kim, Jung-Wook Lambkin, Christine Bertone, Matthew A. Cassel, Brian K. Bayless, Keith M. Heimberg, Alysha M. Wheeler, Benjamin M. Peterson, Kevin J. Pape, Thomas Sinclair, Bradley J. Skevington, Jeffrey H. Blagoderov, Vladimir Caravas, Jason Kutty, Sujatha Narayanan Schmidt-Ott, Urs Kampmeier, Gail E. Thompson, F. Christian Grimaldi, David A. Beckenbach, Andrew T. Courtney, Gregory W. Friedrich, Markus Meier, Rudolf Yeates, David K. TI Episodic radiations in the fly tree of life SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE molecular systematics; phylogenetics; Insecta; adaptive radiation ID HIGHER-LEVEL PHYLOGENY; DIPTERA INSECTA; MIXED MODELS; EVOLUTION; FLIES; DIVERSIFICATION; CYCLORRHAPHA; MICRORNAS; EXPLAIN; ORIGIN AB Flies are one of four superradiations of insects (along with beetles, wasps, and moths) that account for the majority of animal life on Earth. Diptera includes species known for their ubiquity (Musca domestica house fly), their role as pests (Anopheles gambiae malaria mosquito), and their value as model organisms across the biological sciences (Drosophila melanogaster). A resolved phylogeny for flies provides a framework for genomic, developmental, and evolutionary studies by facilitating comparisons across model organisms, yet recent research has suggested that fly relationships have been obscured by multiple episodes of rapid diversification. We provide a phylogenomic estimate of fly relationships based on molecules and morphology from 149 of 157 families, including 30 kb from 14 nuclear loci and complete mitochondrial genomes combined with 371 morphological characters. Multiple analyses show support for traditional groups (Brachycera, Cyclorrhapha, and Schizophora) and corroborate contentious findings, such as the anomalous Deuterophlebiidae as the sister group to all remaining Diptera. Our findings reveal that the closest relatives of the Drosophilidae are highly modified parasites (including the wingless Braulidae) of bees and other insects. Furthermore, we use micro-RNAs to resolve a node with implications for the evolution of embryonic development in Diptera. We demonstrate that flies experienced three episodes of rapid radiation-lower Diptera (220 Ma), lower Brachycera (180 Ma), and Schizophora (65 Ma)-and a number of life history transitions to hematophagy, phytophagy, and parasitism in the history of fly evolution over 260 million y. C1 [Wiegmann, Brian M.; Trautwein, Michelle D.; Winkler, Isaac S.; Barr, Norman B.; Kim, Jung-Wook; Bertone, Matthew A.; Cassel, Brian K.; Bayless, Keith M.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Wheeler, Benjamin M.] N Carolina State Univ, Dept Comp Sci, Raleigh, NC 27695 USA. [Barr, Norman B.] Anim & Plant Hlth Inspect Serv, Ctr Plant Hlth Sci & Technol, Mission Lab, USDA,Moore Air Base, Edinburg, TX 78541 USA. [Lambkin, Christine] Queensland Museum, Brisbane, Qld 4101, Australia. [Heimberg, Alysha M.; Peterson, Kevin J.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. [Pape, Thomas] Univ Copenhagen, Nat Hist Museum Denmark, DK-2100 Copenhagen O, Denmark. [Sinclair, Bradley J.] Canadian Food Inspect Agcy, Ottawa Plant Lab Entomol, Ottawa, ON K1A 0C6, Canada. [Skevington, Jeffrey H.] Agr & Agri Food Canada, Ottawa, ON K1A 0C6, Canada. [Blagoderov, Vladimir] Nat Hist Museum, Dept Entomol, London SW7 5BD, England. [Caravas, Jason; Friedrich, Markus] Wayne State Univ, Dept Biol Sci, Detroit, MI 48202 USA. [Kutty, Sujatha Narayanan; Meier, Rudolf] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Meier, Rudolf] Natl Univ Singapore, Univ Scholars Programme, Singapore 117543, Singapore. [Schmidt-Ott, Urs] Univ Chicago, Dept Organismal Biol & Anat, Chicago, IL 60637 USA. [Kampmeier, Gail E.] Univ Illinois, Inst Nat Resource Sustainabil, Illinois Nat Hist Survey, Champaign, IL 61820 USA. [Thompson, F. Christian] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Grimaldi, David A.] Amer Museum Nat Hist, New York, NY 10024 USA. [Beckenbach, Andrew T.] Simon Fraser Univ, Dept Biol Sci, Burnaby, BC V5A 1S6, Canada. [Courtney, Gregory W.] Iowa State Univ, Dept Entomol, Ames, IA 50011 USA. [Lambkin, Christine; Yeates, David K.] Commonwealth Sci & Ind Res Org Entomol, Canberra, ACT 2601, Australia. RP Wiegmann, BM (reprint author), N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. EM bwiegman@unity.ncsu.edu RI Pape, Thomas/E-7520-2011; Meier, Rudolf/A-7099-2011; Yeates, David/A-9917-2008; OI Pape, Thomas/0000-0001-6609-0609; Meier, Rudolf/0000-0002-4452-2885; Yeates, David/0000-0001-7729-6143; Blagoderov, Vladimir/0000-0001-8684-8421; Winkler, Isaac/0000-0003-2453-021X FU US National Science Foundation [EF-0334948]; North Carolina State University Genomic Sciences Laboratory, North Carolina State University High Performance Computing; Duke University Scalable Computing Support Center; Duke Shared Cluster Resource FX We thank the many researchers who contributed specimens and scientific collaboration to the FLYTREE Assembling the Tree of Life project, especially M. Foldvari, M. E. Irwin, B. Merz, L. Papp, and S. L. Winterton for access to fly collections and material. We are grateful to A. R. Deans, J. M. Logsdon, Jr., B. C. O'Meara, C. Mitter, J. C. Regier, and especially R. Dunn for review and edits of the manuscript. We also acknowledge the support and technical expertise provided by J. Schaff and the North Carolina State University Genomic Sciences Laboratory, North Carolina State University High Performance Computing, the informatics help staff of the National Evolutionary Synthesis Center, and the Duke University Scalable Computing Support Center and Duke Shared Cluster Resource. This project was supported by US National Science Foundation Assembling the Tree of Life Grant EF-0334948 (to B. M. W., G. E. K., G. W. C., M. F., R. M., and D.K.Y.). NR 40 TC 297 Z9 313 U1 10 U2 93 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 APR 5 PY 2011 VL 108 IS 14 BP 5690 EP 5695 DI 10.1073/pnas.1012675108 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 746RT UT WOS:000289265300041 PM 21402926 ER PT J AU Bohm, SM Wells, K Kalko, EKV AF Boehm, Stefan M. Wells, Konstans Kalko, Elisabeth K. V. TI Top-Down Control of Herbivory by Birds and Bats in the Canopy of Temperate Broad-Leaved Oaks (Quercus robur) SO PLOS ONE LA English DT Article ID WHITE OAK; SPECIES RICHNESS; LEAF TANNINS; FOREST; ARTHROPODS; PREDATION; INSECTS; DEFENSE; DAMAGE; PLANT AB The intensive foraging of insectivorous birds and bats is well known to reduce the density of arboreal herbivorous arthropods but quantification of collateral leaf damage remains limited for temperate forest canopies. We conducted exclusion experiments with nets in the crowns of young and mature oaks, Quercus robur, in south and central Germany to investigate the extent to which aerial vertebrates reduce herbivory through predation. We repeatedly estimated leaf damage throughout the vegetation period. Exclusion of birds and bats led to a distinct increase in arthropod herbivory, emphasizing the prominent role of vertebrate predators in controlling arthropods. Leaf damage (e. g., number of holes) differed strongly between sites and was 59% higher in south Germany, where species richness of vertebrate predators and relative oak density were lower compared with our other study site in central Germany. The effects of bird and bat exclusion on herbivory were 19% greater on young than on mature trees in south Germany. Our results support previous studies that have demonstrated clear effects of insectivorous vertebrates on leaf damage through the control of herbivorous arthropods. Moreover, our comparative approach on quantification of leaf damage highlights the importance of local attributes such as tree age, forest composition and species richness of vertebrate predators for control of arthropod herbivory. C1 [Boehm, Stefan M.; Wells, Konstans] Univ Ulm, Inst Expt Ecol, Ulm, Germany. [Wells, Konstans] Biodivers & Climate Res Ctr BiK F, Frankfurt, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Bohm, SM (reprint author), Univ Ulm, Inst Expt Ecol, Ulm, Germany. EM stefan.boehm@uni-ulm.de RI Biodiversity & Climate Res Ctr, BiK-F/C-4266-2012; Wells, Konstans/A-7232-2010 OI Wells, Konstans/0000-0003-0377-2463 FU German Research Foundation [1374, KA 1241/151] FX This work was funded by the German Research Foundation (www.dfg.de) Priority Program 1374 "Infrastructure-Biodiversity-Exploratories" (KA 1241/151). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 19 Z9 20 U1 4 U2 43 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 APR 4 PY 2011 VL 6 IS 4 AR e17857 DI 10.1371/journal.pone.0017857 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 743ZC UT WOS:000289058700003 PM 21483739 ER PT J AU Freestone, AL Osman, RW Ruiz, GM Torchin, ME AF Freestone, Amy L. Osman, Richard W. Ruiz, Gregory M. Torchin, Mark E. TI Stronger predation in the tropics shapes species richness patterns in marine communities SO ECOLOGY LA English DT Article DE biotic interactions; coexistence; diversity; latitude; local; marine invertebrates; predation; regional; scale; species richness; temperate; tropic ID LATITUDINAL DIVERSITY GRADIENT; RELATIVE IMPORTANCE; TEMPERATE; BIOGEOGRAPHY; RECRUITMENT; COMPETITION; PRESSURE; DEFENSES; PERSPECTIVE; COEXISTENCE AB Species interactions are widely assumed to be stronger at lower latitudes, but surprisingly few experimental studies test this hypothesis, and none ties these processes to observed patterns of species richness across latitude. We report here the first experimental field test that predation is both stronger and has a disproportionate effect on species richness in the tropics relative to the temperate zone. We conducted predator-exclusion experiments on communities of sessile marine invertebrates in four regions, which span 32 degrees latitude, in the western Atlantic Ocean and Caribbean Sea. Over a three-month timescale, predation had no effect on species richness in the temperate zone. In the tropics, however, communities were from two to over ten times more species-rich in the absence of predators than when predators were present. While micro-and macro-predators likely compete for the limited prey resource in the tropics, micropredators alone were able to exert as much pressure on the invertebrate communities as the full predator community. This result highlights the extent to which exposure to even a subset of the predator guild can significantly impact species richness in the tropics. Patterns were consistent in analyses that included relative and total species abundances. Higher species richness in the absence of predators in the tropics was also observed when species occurrences were pooled across two larger spatial scales, site and region, demonstrating a consistent scaling relationship. These experimental results show that predation can both limit local species abundances and shape patterns of regional coexistence in the tropics. When preestablished diverse tropical communities were then exposed to predation for different durations, ranging from one to several days, species richness was always reduced. These findings confirmed that impacts of predation in the tropics are strong and consistent, even in more established communities. Our results offer empirical support for the long-held prediction that predation pressure is stronger at lower latitudes. Furthermore, we demonstrate the magnitude to which variation in predation pressure can contribute to the maintenance of tropical species diversity. C1 [Freestone, Amy L.] Temple Univ, Dept Biol, Philadelphia, PA 19122 USA. [Freestone, Amy L.; Osman, Richard W.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Torchin, Mark E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Freestone, AL (reprint author), Temple Univ, Dept Biol, Philadelphia, PA 19122 USA. EM amy.freestone@temple.edu OI Ruiz, Gregory/0000-0003-2499-441X FU Smithsonian's Marine Science Network FX We are grateful to G. Ashton, K. Larson, S. Reed, C. Schloeder, and B. Sewall for field assistance and helpful discussion, and to S. Harrison and H. Cornell for reviewing an earlier draft of the manuscript. We also greatly appreciate the assistance of the faculty and staff at UCONN Avery Point, particularly R. Whitlatch, Smithsonian Marine Station at Fort Pierce, Caribbean Coral Reef Ecosystems Program, and STRI Bocas del Toro research station. Funding was provided by the Smithsonian's Marine Science Network Postdoctoral Fellowship (A. Freestone) and Scholarly Studies (G. Ruiz and M. Torchin) programs. This is Smithsonian Marine Station at Fort Pierce Contribution No. 834 and Smithsonian Caribbean Coral Reef Ecosystems Program Contribution No. 893. NR 46 TC 37 Z9 38 U1 5 U2 76 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD APR PY 2011 VL 92 IS 4 BP 983 EP 993 DI 10.1890/09-2379.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 763DF UT WOS:000290533700018 PM 21661559 ER PT J AU Pelletier, J Ramankutty, N Potvin, C AF Pelletier, Johanne Ramankutty, Navin Potvin, Catherine TI Diagnosing the uncertainty and detectability of emission reductions for REDD plus under current capabilities: an example for Panama SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE reducing emissions from deforestation and forest degradation in developing countries (REDD plus ); uncertainty analysis; tropical deforestation; emission reductions; developing countries ID LAND-USE CHANGE; GREENHOUSE-GAS EMISSIONS; CARBON BUDGET MODEL; FOREST BIOMASS; TROPICAL FORESTS; BRAZILIAN AMAZON; CANOPY DAMAGE; DEFORESTATION; FLUX; CONSERVATION AB In preparation for the deployment of a new mechanism that could address as much as one fifth of global greenhouse gas emissions by reducing emissions from deforestation and forest degradation (REDD+), important work on methodological issues is still needed to secure the capacity to produce measurable, reportable, and verifiable emissions reductions from REDD+ in developing countries. To contribute to this effort, we have diagnosed the main sources of uncertainty in the quantification of emission from deforestation for Panama, one of the first countries to be supported by the Forest Carbon Partnership Facility of the World Bank and by UN-REDD. Performing sensitivity analyses using a land-cover change emissions model, we identified forest carbon stocks and the quality of land-cover maps as the key parameters influencing model uncertainty. The time interval between two land-cover assessments, carbon density in fallow and secondary forest, and the accuracy of land-cover classifications also affect our ability to produce accurate estimates. Further, we used the model to compare emission reductions from five different deforestation reduction scenarios drawn from governmental input. Only the scenario simulating a reduction in deforestation by half succeeds in crossing outside the confidence bounds surrounding the baseline emission obtained from the uncertainty analysis. These results suggest that with current data, real emission reductions in developing countries could be obscured by their associated uncertainties. Ways of addressing the key sources of error are proposed, for developing countries involved in REDD+, for improving the accuracy of their estimates in the future. These new considerations confirm the importance of current efforts to establish forest monitoring systems and enhance capabilities for REDD+ in developing countries. C1 [Pelletier, Johanne; Potvin, Catherine] McGill Univ, Dept Biol & Global Environm, Montreal, PQ H3A 1B1, Canada. [Pelletier, Johanne; Potvin, Catherine] McGill Univ, Climate Change Ctr, Montreal, PQ H3A 1B1, Canada. [Ramankutty, Navin] McGill Univ, Dept Geog & Global Environm, Montreal, PQ H3A 2K6, Canada. [Ramankutty, Navin] McGill Univ, Climate Change Ctr, Montreal, PQ H3A 2K6, Canada. [Potvin, Catherine] Smithsonian Trop Res Inst, Balboa 2072, Panama. RP Pelletier, J (reprint author), McGill Univ, Dept Biol & Global Environm, 1205 Dr Penfield, Montreal, PQ H3A 1B1, Canada. EM johannepelletier@gmail.com RI Pelletier, Johanne/E-3156-2016; OI Pelletier, Johanne/0000-0001-8161-6410; Ramankutty, Navin/0000-0002-3737-5717 FU FQRNT; Global Environmental and Climate Change Centre (GEC3); NSERC FX We thank E Reyes, R Gutierrez, F Magallon, C Prieto and, C Melgarejo at Autoridad Nacional del Ambiente and the Smithsonian Tropical Research Institute, as well as F Guichard and J Rhemtulla at McGill University, M Desrochers, M Mazerolle and M Papaik at the Centre d'Etudes sur la Foret and F Murchison. We acknowledge funding from the FQRNT and the Global Environmental and Climate Change Centre (GEC3) to JP. CP and NR acknowledge Discovery grants from NSERC. NR 67 TC 32 Z9 32 U1 1 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD APR-JUN PY 2011 VL 6 IS 2 AR 024005 DI 10.1088/1748-9326/6/2/024005 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 826BQ UT WOS:000295326800005 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 Ciupik, L Collins-Hughes, E Cui, W Dickherber, R Duke, C Errando, M Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Griffin, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hughes, JP Hui, CM Humensky, TB Kaaret, P Karlsson, N Kertzman, M Kieda, D Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Ong, RA Orr, M Otte, AN Pandel, D Park, NH Perkins, JS Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Saxon, DB Schroedter, M Sembroski, GH Senturk, GD Slane, P Smith, AW 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 Zitzer, B 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. Ciupik, L. Collins-Hughes, E. Cui, W. Dickherber, R. Duke, C. Errando, M. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Griffin, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hughes, J. P. Hui, C. M. Humensky, T. B. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Ong, R. A. Orr, M. Otte, A. N. Pandel, D. Park, N. H. Perkins, J. S. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Saxon, D. B. Schroedter, M. Sembroski, G. H. Senturk, G. Demet Slane, P. Smith, A. W. 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. Zitzer, B. TI DISCOVERY OF TeV GAMMA-RAY EMISSION FROM TYCHO'S SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: general; ISM: individual objects (G120.1+01.4, Tycho=VER J0025+641) ID GALACTIC PLANE SURVEY; SHOCK ACCELERATION; EXPANSION; ASTRONOMY; SPECTRUM; CATALOG; CHANDRA; HESS; CONSTRAINTS; TURBULENCE AB We report the discovery of TeV gamma-ray emission from the Type Ia supernova remnant (SNR) G120.1+1.4, known as Tycho's SNR. Observations performed in the period 2008-2010 with the VERITAS ground-based gamma-ray observatory reveal weak emission coming from the direction of the remnant, compatible with a point source located at 00(h)25(m)27(s).0, +64 degrees 10'50 '' (J2000). The TeV photon spectrum measured by VERITAS can be described with a power law dN/dE = C(E/3.42 TeV)(-Gamma) with Gamma = 1.95 +/- 0.51(stat) +/- 0.30(sys) and C = (1.55 +/- 0.43(stat) +/- 0.47(sys)) x 10(-14) cm(-2) s(-1) TeV-1. The integral flux above 1 TeV corresponds to similar to 0.9% of the steady Crab Nebula emission above the same energy, making it one of the weakest sources yet detected in TeV gamma rays. We present both leptonic and hadronic models that can describe the data. The lowest magnetic field allowed in these models is similar to 80 mu G, which may be interpreted as evidence for magnetic field amplification. C1 [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.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [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. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; 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.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Grube, J.; Gyuk, G.; Karlsson, N.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Griffin, S.; Guenette, R.; Hanna, D.; McCann, A.; Ragan, K.; 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, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Humensky, T. B.; Park, N. H.; Reyes, L. C.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Kaaret, P.; Pandel, D.; 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. [Maier, G.; Pohl, M.] DESY, D-15738 Zeuthen, Germany. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Pohl, M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Senturk, G. Demet] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Slane, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM dbsaxon@udel.edu; wakely@uchicago.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; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201 FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian Institution; Natural Sciences and Engineering Research Council (NSERC) in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; Science and Technology Facilities Council in the UK; NSERC; NASA [NNX08AZ86G] FX This research is supported by grants from the U.S. Department of Energy, the U.S. National Science Foundation and the Smithsonian Institution, by the Natural Sciences and Engineering Research Council (NSERC) in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by the Science and Technology Facilities Council in the UK. The research presented in this Letter has used data from the Canadian Galactic Plane Survey, a Canadian project with international partners, supported by NSERC. D. B. S. acknowledges the NASA Delaware Space Grant Program for its support of this research. J.P.H. acknowledges support from NASA grant NNX08AZ86G to Rutgers University. NR 50 TC 89 Z9 90 U1 0 U2 7 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 APR 1 PY 2011 VL 730 IS 2 AR L20 DI 10.1088/2041-8205/730/2/L20 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KK UT WOS:000293125600008 ER PT J AU Kurucz, RL AF Kurucz, Robert L. TI Including all the lines SO CANADIAN JOURNAL OF PHYSICS LA English DT Article; Proceedings Paper CT 10th International Colloquium on AtomicSpectroscopy and Oscillator Strengths for Astrophysical andLaboratory Plasmas (ASOS) CY AUG 03-07, 2010 CL Berkeley, CA ID FE-II; TERM ANALYSIS; AB-INITIO; CO I; SPECTRUM; SOLAR; SUPERMULTIPLET; OPACITY; SYSTEM; TIO AB I present a progress report on including all the lines in the line lists, including all the lines in the opacities, and including all the lines in the model atmosphere and spectrum synthesis calculations. The increased opacity will improve stellar atmosphere, pulsation, stellar interior, asteroseismology, nova, supernova, and other radiation-hydrodynamics calculations. I also report on producing high-resolution, high-signal-to-noise atlases for use in verifying the line data and spectrum calculations, and as tools for extending laboratory spectrum analyses to higher energy levels. All the data are available on my web site: kurucz.harvard.edu. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurucz, RL (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM rkurucz@cfa.harvard.edu NR 32 TC 65 Z9 65 U1 2 U2 5 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0008-4204 EI 1208-6045 J9 CAN J PHYS JI Can. J. Phys. PD APR PY 2011 VL 89 IS 4 BP 417 EP 428 DI 10.1139/P10-104 PG 12 WC Physics, Multidisciplinary SC Physics GA 775QA UT WOS:000291475700014 ER PT J AU Penev, L Stoev, P Kress, WJ Knapp, S Erwin, T AF Penev, L. Stoev, P. Kress, W. J. Knapp, S. Erwin, T. TI Cybertaxonomy, semantic markup and semantic enhancements: The PhytoKeys and ZooKeys experience SO SOUTH AFRICAN JOURNAL OF BOTANY LA English DT Meeting Abstract C1 [Penev, L.; Stoev, P.] Pensoft Publishers, Sofia, Bulgaria. [Kress, W. J.; Erwin, T.] Smithsonian Inst, Washington, DC 20560 USA. [Knapp, S.] Nat Hist Museum, London, England. RI Knapp, Sandra/A-4856-2011 OI Knapp, Sandra/0000-0001-7698-3945 NR 0 TC 0 Z9 0 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0254-6299 J9 S AFR J BOT JI S. Afr. J. Bot. PD APR PY 2011 VL 77 IS 2 BP 560 EP 560 PG 1 WC Plant Sciences SC Plant Sciences GA 772MI UT WOS:000291237600181 ER PT J AU Luther, D Greenberg, R AF Luther, David Greenberg, Russell TI THE ISLAND SYNDROME IN COASTAL WETLAND ECOSYSTEMS: CONVERGENT EVOLUTION OF LARGE BILLS IN MANGROVE PASSERINES SO AUK LA English DT Article DE bill morphology; birds; dominance hypothesis; ecological convergence; mangrove; niche variation ID BODY-SIZE; TERRESTRIAL VERTEBRATES; GLOBAL PERSPECTIVE; TIDAL MARSHES; BIRDS; ECOLOGY; CONSERVATION; DIMORPHISM; TRENDS AB Passerine birds on islands tend to have larger bills than their mainland relatives. The morphological shift may be related to reduced interspecific and increased intraspecific competition. Emberizid sparrows in North American salt marshes also show consistently greater bill size. We tested the hypothesis that passerines restricted to mangrove forests, another continental system with low species diversity and high population densities, also have larger bills than their closest nontidal relatives. We found a consistent pantropical pattern of longer and deeper bills in passerine birds restricted to mangroves. These results indicate that disproportionately longer bills in relation to body size in passerines restricted to coastal saline habitats, just like those found on islands, seems to be a general ecological rule. The similar pattern in bill morphology suggests that ecological and evolutionary processes thought to occur only in island systems might also occur in some continental systems. Received 16 November 2010, accepted 31 January 2011. C1 [Luther, David] George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. [Luther, David; Greenberg, Russell] Smithsonian Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Luther, D (reprint author), George Mason Univ, Dept Biol, Fairfax, VA 22030 USA. EM dluther@gmu.edu NR 31 TC 8 Z9 9 U1 7 U2 29 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 APR PY 2011 VL 128 IS 2 BP 201 EP 204 DI 10.1525/auk.2011.10262 PG 4 WC Ornithology SC Zoology GA 767VV UT WOS:000290887600001 ER PT J AU Jehl, JR AF Jehl, Joseph R., Jr. TI IN MEMORIAM: BERTRAM GEORGE MURRAY, JR., 1933-2010 SO AUK LA English DT Biographical-Item C1 Smithsonian Inst, Div Birds, US Natl Museum Nat Hist, Washington, DC 20013 USA. RP Jehl, JR (reprint author), Smithsonian Inst, Div Birds, US Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 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 APR PY 2011 VL 128 IS 2 BP 426 EP 428 DI 10.1525/auk.2011.128.2.426 PG 3 WC Ornithology SC Zoology GA 767VV UT WOS:000290887600024 ER PT J AU Munguia, P Osman, RW Hamilton, J Whitlatch, R Zajac, R AF Munguia, Pablo Osman, Richard W. Hamilton, John Whitlatch, Robert Zajac, Roman TI Changes in habitat heterogeneity alter marine sessile benthic communities SO ECOLOGICAL APPLICATIONS LA English DT Article DE community ecology; diversity; homogeneity; management; metacommunity; model ID PEN SHELL COMMUNITIES; ECOSYSTEM FUNCTION; SPECIES-DIVERSITY; DISTURBANCE; COLONIZATION; BIODIVERSITY; RECRUITMENT; COEXISTENCE; EXTINCTION; PATTERNS AB Habitat heterogeneity is considered an important mechanism influencing diversity patterns in spatially structured habitats. However, spatial heterogeneity is not static and it can change along temporal scales. These changes, whether gradual or rapid, have the potential of forcing species extinctions or facilitating the introduction of nonnative species. Here, we present modeling results that show how changes in spatial heterogeneity over several generations can produce strong changes in benthic species composition residing in eastern Long Island Sound, USA. For many benthic species, hard substrate is a limiting resource which can vary in availability among different coastal areas. We modeled gradual changes from a heterogeneous landscape (mimicking patches of natural hard and soft substrate) to a homogenous one (analogous to a fully developed coast with hard, manmade substrate) and followed the abundance and distribution patterns of species possessing four different life histories. We also modeled changes from homogeneous to heterogeneous landscapes. We found that as regions become more homogeneous, species extinctions become more frequent and poor dispersers dominate locally. In contrast, as habitats become more heterogeneous, species distributing across localities leads to regional species coexistence and fewer extinctions. These results suggest that focusing on changing habitat heterogeneity can be a useful management strategy to prevent poor dispersing species, such as invasive ascidians, from driving communities to monocultures. C1 [Munguia, Pablo; Osman, Richard W.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Hamilton, John; Whitlatch, Robert] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. [Zajac, Roman] Univ New Haven, Dept Biol & Environm Sci, West Haven, CT 06516 USA. [Munguia, Pablo] Univ Texas Austin, Inst Marine Sci, Port Aransas, TX 78373 USA. RP Munguia, P (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM munguia@mail.utexas.edu RI Munguia, Pablo/D-8653-2012; OI Munguia, Pablo/0000-0002-9900-2123 FU Environmental Protection Agency [R832448] FX This research was funded through the Environmental Protection Agency (Grant number: R832448). NR 47 TC 8 Z9 8 U1 5 U2 42 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 APR PY 2011 VL 21 IS 3 BP 925 EP 935 PG 11 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 764VA UT WOS:000290661300023 PM 21639055 ER PT J AU Ram, RS Tereszchuk, K Gordon, IE Walker, KA Bernath, PF AF Ram, R. S. Tereszchuk, K. Gordon, I. E. Walker, K. A. Bernath, P. F. TI Fourier transform emission spectroscopy of the E-2 Pi-X-2 Sigma(+) transition of CaH and CaD SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Stellar atmospheres; Electronic spectra; Rotational analysis; Equilibrium constants ID ELECTRIC-DIPOLE MOMENTS; CALCIUM MONOHYDRIDE; BAND STRENGTHS; SPECTRUM; STATES; MOLECULES; DWARFS; PARAMETERS; X2-SIGMA+; SUBDWARFS AB The emission spectra of CaH and CaD have been recorded at high resolution using a Fourier transform spectrometer and bands belonging to the E-2 Pi-X-2 Sigma(+) transition have been measured in the 20 10020 700 cm(-1) region. A rotational analysis of 0-0 and 1-1 bands of both the isotopologues has been carried out. The present measurements have been combined with the previously available pure rotation and vibration-rotation data to provide improved spectroscopic constants for the E-2 Pi state. The constants Delta G(1/2) = 1199.8867(34) cm(-1), B-e = 4.345032(49) cm(-1), alpha(e) = 0.122115(92) cm(-1), r(e) = 1.986633(11) angstrom for CaH, and Delta G(1/2)=868.7438(46) cm(-1), B-e = 2.212496(51) cm(-1), alpha(e) = 0.036509(97) cm(-1), r(e) = 1.993396(23) angstrom for CaD have been determined. (C) 2011 Elsevier Inc. All rights reserved. C1 [Ram, R. S.; Tereszchuk, K.; Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Ram, R. S.; Bernath, P. F.] Univ Arizona, Dept Chem, Tucson, AZ 85721 USA. [Gordon, I. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Bernath, PF (reprint author), Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. EM pfb500@york.ac.uk RI Bernath, Peter/B-6567-2012 OI Bernath, Peter/0000-0002-1255-396X FU Leverhulme Trust FX We thank the Leverhulme Trust for financial support through a Research Project Grant. The spectra of CaH and CaD were recorded when Tereszchuk, Gordon, Walker and Bernath were at the University of Waterloo. NR 37 TC 9 Z9 9 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD APR PY 2011 VL 266 IS 2 BP 86 EP 91 DI 10.1016/j.jms.2011.03.009 PG 6 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA 768HB UT WOS:000290923500004 ER PT J AU Soltis, DE Smith, SA Cellinese, N Wurdack, KJ Tank, DC Brockington, SF Refulio-Rodriguez, NF Walker, JB Moore, MJ Carlsward, BS Bell, CD Latvis, M Crawley, S Black, C Diouf, D Xi, ZX Rushworth, CA Gitzendanner, MA Sytsma, KJ Qiu, YL Hilu, KW Davis, CC Sanderson, MJ Beaman, RS Olmstead, RG Judd, WS Donoghue, MJ Soltis, PS AF Soltis, Douglas E. Smith, Stephen A. Cellinese, Nico Wurdack, Kenneth J. Tank, David C. Brockington, Samuel F. Refulio-Rodriguez, Nancy F. Walker, Jay B. Moore, Michael J. Carlsward, Barbara S. Bell, Charles D. Latvis, Maribeth Crawley, Sunny Black, Chelsea Diouf, Diaga Xi, Zhenxiang Rushworth, Catherine A. Gitzendanner, Matthew A. Sytsma, Kenneth J. Qiu, Yin-Long Hilu, Khidir W. Davis, Charles C. Sanderson, Michael J. Beaman, Reed S. Olmstead, Richard G. Judd, Walter S. Donoghue, Michael J. Soltis, Pamela S. TI ANGIOSPERM PHYLOGENY: 17 GENES, 640 TAXA SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE angiosperms; bioinformatics; large data sets; molecular systematics; RAxML; Superasteridae; supermatrix; Superrosidae ID RBCL SEQUENCE DATA; SAXIFRAGACEAE SENSU-LATO; CHLOROPLAST TRNL-F; DNA-SEQUENCES; FLOWERING PLANTS; DATA SETS; MOLECULAR PHYLOGENETICS; 18S RDNA; MORPHOLOGICAL EVOLUTION; NUCLEOTIDE-SEQUENCES AB Premise of the study : Recent analyses employing up to five genes have provided numerous insights into angiosperm phylogeny, but many relationships have remained unresolved or poorly supported. In the hope of improving our understanding of angiosperm phylogeny, we expanded sampling of taxa and genes beyond previous analyses. Methods : We conducted two primary analyses based on 640 species representing 330 families. The first included 25 260 aligned base pairs (bp) from 17 genes (representing all three plant genomes, i.e., nucleus, plastid, and mitochondrion). The second included 19 846 aligned bp from 13 genes (representing only the nucleus and plastid). Key results : Many important questions of deep-level relationships in the nonmonocot angiosperms have now been resolved with strong support. Amborellaceae, Nymphaeales, and Austrobaileyales are successive sisters to the remaining angiosperms (Mesangiospermae), which are resolved into Chloranthales + Magnoliidae as sister to Monocotyledoneae + [Ceratophyllaceae + Eudicotyledoneae]. Eudicotyledoneae contains a basal grade subtending Gunneridae. Within Gunneridae, Gunnerales are sister to the remainder (Pentapetalae), which comprises (1) Superrosidae, consisting of Rosidae (including Vitaceae) and Saxifragales; and (2) Superasteridae, comprising Berberidopsidales, Santalales, Caryophyllales, Asteridae, and, based on this study, Dilleniaceae (although other recent analyses disagree with this placement). Within the major subclades of Pentapetalae, most deep-level relationships are resolved with strong support. Conclusions : Our analyses confirm that with large amounts of sequence data, most deep-level relationships within the angiosperms can be resolved. We anticipate that this well-resolved angiosperm tree will be of broad utility for many areas of biology, including physiology, ecology, paleobiology, and genomics. C1 [Soltis, Douglas E.; Latvis, Maribeth; Gitzendanner, Matthew A.; Judd, Walter S.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Smith, Stephen A.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Cellinese, Nico; Latvis, Maribeth; Gitzendanner, Matthew A.; Beaman, Reed S.; Soltis, Pamela S.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Wurdack, Kenneth J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Tank, David C.] Univ Idaho, Dept Forest Ecol & Biogeosci, Moscow, ID 83844 USA. [Tank, David C.] Univ Idaho, Stillinger Herbarium, Moscow, ID 83844 USA. [Brockington, Samuel F.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Refulio-Rodriguez, Nancy F.; Olmstead, Richard G.] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Walker, Jay B.; Sytsma, Kenneth J.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. [Moore, Michael J.] Oberlin Coll, Dept Biol, Oberlin, OH 44074 USA. [Carlsward, Barbara S.] Eastern Illinois Univ, Dept Biol Sci, Charleston, IL 61920 USA. [Bell, Charles D.] Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA. [Crawley, Sunny; Black, Chelsea; Diouf, Diaga; Hilu, Khidir W.] Virginia Polytech Inst & State Univ, Dept Biol Sci, Blacksburg, VA 24061 USA. [Diouf, Diaga] Univ Cheikh AntDeara Diop, Dept Biol Vegetal, Dakar, Senegal. [Xi, Zhenxiang; Rushworth, Catherine A.; Davis, Charles C.] Harvard Univ Herbaria, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Qiu, Yin-Long] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Sanderson, Michael J.] Univ Arizona, Dept Ecol & Evolut Biol, Tucson, AZ 85721 USA. [Donoghue, Michael J.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. RP Soltis, DE (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM dsoltis@botany.ufl.edu RI Soltis, Pamela/L-5184-2015; Brockington, Samuel/K-7819-2013; OI Brockington, Samuel/0000-0003-1216-219X; Cellinese, Nico/0000-0002-7157-9414; Gitzendanner, Matthew/0000-0002-7078-4336; Smith, Stephen/0000-0003-2035-9531 FU NSF [CNS-0821622, DEB-0544039] FX The authors thank the University of Florida High-Performance Computing Center, the UF Genetics Institute, and facilities supported in part by NSF Grant CNS-0821622 for providing computational resources that facilitated the completion of this research. The authors thank E. Mavrodiev for help in preparing some of the figures. This study was carried out as part of the Angiosperm Tree of Life Project (NSF EF-0431266 to D.E.S., P.S.S., W.S.J., and S. R. Manchester, EF-0431242 to C.C.D., DEB-9634231; EF-0431057 to K.H., EF-0431233 to K.J.S., DEB-0431239 to Y.L.Q.) with additional support from NSF grant DEB-0544039 to C.C.D. The authors thank the Royal Botanic Gardens, Kew, and the Missouri Botanical Garden for providing samples used in this study. NR 131 TC 285 Z9 295 U1 14 U2 177 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 APR PY 2011 VL 98 IS 4 BP 704 EP 730 DI 10.3732/ajb.1000404 PG 27 WC Plant Sciences SC Plant Sciences GA 762LL UT WOS:000290479700021 PM 21613169 ER PT J AU Feeley, KJ Davies, SJ Perez, R Hubbell, SP Foster, RB AF Feeley, Kenneth J. Davies, Stuart J. Perez, Rolando Hubbell, Stephen P. Foster, Robin B. TI Directional changes in the species composition of a tropical forest SO ECOLOGY LA English DT Article DE Barro Colorado Island; carbon fertilization; Center for Tropical Forest Science; climate change; drought; El Nino Southern Oscillation; ENSO; Panama; tropical forest ID UNDISTURBED AMAZONIAN FORESTS; GLOBAL ATMOSPHERIC CHANGE; RAIN-FOREST; NEOTROPICAL FOREST; TREE COMMUNITIES; CLIMATE-CHANGE; HABITAT ASSOCIATIONS; PERVASIVE ALTERATION; DROUGHT SENSITIVITY; EL-NINO AB Long-term studies have revealed that the structure and dynamics of many tropical forests are changing, but the causes and consequences of these changes remain debated. To learn more about the forces driving changes within tropical forests, we investigated shifts in tree species composition over the past 25 years within the 50-ha Forest Dynamics Plot on Barro Colorado Island (BCI), Panama, and examined how observed patterns relate to predictions of (1) random population fluctuations, (2) carbon fertilization, (3) succession from past disturbance, (4) recovery from an extreme El Nino drought at the start of the study period, and (5) long-term climate change. We found that there have been consistent and directional changes in the tree species composition. These shifts have led to increased relative representations of drought-tolerant species as determined by the species' occurrence both across a gradient of soil moisture within BCI and across a wider precipitation gradient from a dry forest near the Pacific coast of Panama to a wet forest near its Caribbean coast. These nonrandom changes cannot be explained by stochastic fluctuations or carbon fertilization. They may be the legacy of the El Nino drought, or alternatively, potentially reflect increased aridity due to long-term climate change. By investigating compositional changes, we increased not only our understanding of the ecology of tropical forests and their responses to large-scale disturbances, but also our ability to predict how future global change will impact some of the critical services provided by these important ecosystems. C1 [Feeley, Kenneth J.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Feeley, Kenneth J.] Fairchild Trop Bot Garden, Coral Gables, FL 33156 USA. [Davies, Stuart J.; Perez, Rolando; Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Cambridge, MA 02138 USA. [Davies, Stuart J.; Perez, Rolando; Hubbell, Stephen P.] Harvard Univ, Cambridge, MA 02138 USA. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Foster, Robin B.] Field Museum, Chicago, IL 60605 USA. RP Feeley, KJ (reprint author), Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. EM kjfeeley@gmail.com RI Feeley, Kenneth/A-7631-2009 FU 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; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Celera Foundation FX We thank R. Condit, E. Leigh, D. A. Clark, and M. S. Iman for their comments and insights, and J. Chave for making the wood density values publicly available. The BCI forest dynamics research project was made possible by multiple National Science Foundation grants to Stephen 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; by 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 hundreds of people from many countries over the past three decades. The plot project is part of the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. NR 60 TC 60 Z9 62 U1 9 U2 95 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 APR PY 2011 VL 92 IS 4 BP 871 EP 882 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 763DF UT WOS:000290533700009 PM 21661550 ER PT J AU Uriarte, M Anciaes, M da Silva, MTB Rubim, P Johnson, E Bruna, EM AF Uriarte, Maria Anciaes, Marina da Silva, Mariana T. B. Rubim, Paulo Johnson, Erik Bruna, Emilio M. TI Disentangling the drivers of reduced long-distance seed dispersal by birds in an experimentally fragmented landscape SO ECOLOGY LA English DT Article DE Amazonian rain forest; dispersal kernels; frugivory; habitat fragmentation; Heliconia acuminata; manakins; Manaus, Brazil; patch size; spatially explicit model; thrush; tropical forest; Turdus albicollis ID ENDEMIC AFRICAN TREE; HABITAT FRAGMENTATION; AVIAN FRUGIVORES; FOREST FRAGMENTATION; HELICONIA-ACUMINATA; UNDERSTORY HERB; RECRUITMENT; PATTERNS; PLANT; CONSEQUENCES AB Seed dispersal is a crucial component of plant population dynamics. Human landscape modifications, such as habitat destruction and fragmentation, can alter the abundance of fruiting plants and animal dispersers, foraging rates, vector movement, and the composition of the disperser community, all of which can singly or in concert affect seed dispersal. Here, we quantify and tease apart the effects of landscape configuration, namely, fragmentation of primary forest and the composition of the surrounding forest matrix, on individual components of seed dispersal of Heliconia acuminata, an Amazonian understory herb. First we identified the effects of landscape configuration on the abundance of fruiting plants and six bird disperser species. Although highly variable in space and time, densities of fruiting plants were similar in continuous forest and fragments. However, the two largest-bodied avian dispersers were less common or absent in small fragments. Second, we determined whether fragmentation affected foraging rates. Fruit removal rates were similar and very high across the landscape, suggesting that Heliconia fruits are a key resource for small frugivores in this landscape. Third, we used radiotelemetry and statistical models to quantify how landscape configuration influences vector movement patterns. Bird dispersers flew farther and faster, and perched longer in primary relative to secondary forests. One species also altered its movement direction in response to habitat boundaries between primary and secondary forests. Finally, we parameterized a simulation model linking data on fruit density and disperser abundance and behavior with empirical estimates of seed retention times to generate seed dispersal patterns in two hypothetical landscapes. Despite clear changes in bird movement in response to landscape configuration, our simulations demonstrate that these differences had negligible effects on dispersal distances. However, small fragments had reduced densities of Turdus albicollis, the largest-bodied disperser and the only one to both regurgitate and defecate seeds. This change in Turdus abundance acted together with lower numbers of fruiting plants in small fragments to decrease the probability of long-distance dispersal events from small patches. These findings emphasize the importance of foraging style for seed dispersal and highlight the primacy of habitat size relative to spatial configuration in preserving biotic interactions. C1 [Uriarte, Maria; Anciaes, Marina] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Anciaes, Marina; da Silva, Mariana T. B.; Rubim, Paulo] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Anciaes, Marina; da Silva, Mariana T. B.; Rubim, Paulo] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil. [Johnson, Erik] Louisiana State Univ, Sch Renewable Resources, Baton Rouge, LA 70803 USA. [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. RP Uriarte, M (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, 1200 Amsterdam Ave, New York, NY 10027 USA. EM mu2126@columbia.edu RI Bruna, Emilio/H-2769-2012; Uriarte, Maria/L-8944-2013 OI Bruna, Emilio/0000-0003-3381-8477; FU U.S. National Science Foundation [DEB-0614339, DEB-0614149, INT 98-06351]; NSF [LTREB DEB 0545491] FX We thank B. Bolker for sharing his code, and P. S. Stouffer, C. Yackulic, and two anonymous reviewers for helpful comments on the manuscript. We also thank the technicians and students who helped conduct the censuses, and we are grateful to BDFFP and INPA for their logistical support and to the GIS lab at INPA for providing Landsat images of the study site. Financial support was provided by the U.S. National Science Foundation (award DEB-0614339 to M. Uriarte and DEB-0614149 and INT 98-06351 to E. Bruna). Bird mist-net censuses were supported by award NSF LTREB DEB 0545491 to P. S. Stouffer. This is publication number 565 in the BDFFP Technical Series. NR 53 TC 38 Z9 39 U1 7 U2 85 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 APR PY 2011 VL 92 IS 4 BP 924 EP 937 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 763DF UT WOS:000290533700014 PM 21661555 ER PT J AU Queirolo, D Moreira, JR Soler, L Emmons, LH Rodrigues, FHG Pautasso, AA Cartes, JL Salvatori, V AF Queirolo, Diego Moreira, Jose Roberto Soler, Lucia Emmons, Louise H. Rodrigues, Flavio H. G. Pautasso, Andres A. Luis Cartes, Jose Salvatori, Valeria TI Historical and current range of the Near Threatened maned wolf Chrysocyon brachyurus in South America SO ORYX LA English DT Article DE Biogeography; canid; Chrysocyon brachyurus; historical distribution; maned wolf; range; South America ID BRAZIL; DIET; ARGENTINA AB The Near Threatened maned wolf Chrysocyon brachyurus is a South American endemic canid occurring mainly in grassland-dominated regions. We compiled and mapped recent and historical data to compare the species' present and historical distributions and propose hypotheses for range shifts. There has been recent range expansion in eastern Brazil associated with the deforestation of the Atlantic Forest and conversion of habitat to grasslands for cattle range. The northern, north-eastern and eastern sectors of the species' range have not yet experienced significant modifications, and the species persists in central Brazil, northern and eastern Bolivia, and south-eastern Peru. The largest range contractions have occurred at the species' southern limits but maned wolves are still present in northeastern, central and eastern Argentina, and there are a few records of the species' occurence from Uruguay and northeastern and southern Rio Grande do Sul, southern Brazil. Historically the species occupied nearly all of Rio Grande do Sul, Uruguay and south to at least the 38th parallel in Argentina. The probable causes of the southern range loss are intense anthropogenic pressure combined with limiting abiotic factors such as temperature and humidity. We highlight the need to revise the view of how habitat modifications are influencing the range of C. brachyurus so as to improve and coordinate range-wide conservation strategies. C1 [Queirolo, Diego] Univ Republ, Ctr Univ Rivera, Rivera, Uruguay. [Moreira, Jose Roberto] Empresa Brasileira Pesquisa Agropecuaria, Ctr Nacl Pesquisa Recursos Genet & Biotecnol, Brasilia, DF, Brazil. [Soler, Lucia] Univ Nacl Sur, Catedra Fisiol Anim, DBByF, RA-8000 Bahia Blanca, Buenos Aires, Argentina. [Emmons, Louise H.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Rodrigues, Flavio H. G.] Univ Fed Minas Gerais, Dept Biol Geral, Belo Horizonte, MG, Brazil. [Pautasso, Andres A.] Museo Prov Ciencias Nat Florentino Ameghino, Area Zool Vertebrados, Santa Fe, Argentina. [Luis Cartes, Jose] Asociac Guyra Paraguay, Asuncion, Paraguay. [Salvatori, Valeria] Ist Ecol Applicata, Rome, Italy. RP Queirolo, D (reprint author), Univ Republ, Ctr Univ Rivera, Ituzaingo 667, Rivera, Uruguay. EM diqueirolo@yahoo.com.br RI Rodrigues, Flavio/E-4924-2012 OI Rodrigues, Flavio/0000-0002-4797-0085 NR 59 TC 8 Z9 12 U1 8 U2 40 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0030-6053 J9 ORYX JI Oryx PD APR PY 2011 VL 45 IS 2 BP 296 EP 303 DI 10.1017/S0030605310000372 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 763BJ UT WOS:000290527700024 ER PT J AU Isaac, G AF Isaac, Gwyneira TI Whose Idea Was This? Museums, Replicas, and the Reproduction of Knowledge SO CURRENT ANTHROPOLOGY LA English DT Article ID ART; ARCHAEOLOGY; RESOURCES; MELANESIA; COPYRIGHT; CULTURE; VANUATU; PUEBLO; RETURN; STYLE AB Zuni principles value repetition as an affirmation of the continuity of knowledge, thereby challenging particular Euro-American notions of the "copy" as a devaluation of the "original." Using examples from Zuni philosophy as well as scientific traditions in creating replicas, I examine overlaps and differences between Zuni and Euro-American approaches to the reproduction of knowledge. Contemporary Zuni concerns about controlling the reproduction of esoteric knowledge are explored here through the history of replicas made in the nineteenth century by anthropologists as well as the development of protocols for reproducing knowledge in the newly established Zuni tribal museum. These temporally situated transcultural encounters with and debates over the reproduction of knowledge are used to argue against the cross-cultural applicability of representational theories, as these are characteristically based on Euro-American postmodern notions of the instability of meaning between "copies" and "originals." C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Isaac, G (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012,MRC 112, Washington, DC 20013 USA. EM isaacg@si.edu NR 98 TC 9 Z9 10 U1 0 U2 8 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 APR PY 2011 VL 52 IS 2 BP 211 EP 233 DI 10.1086/659141 PG 23 WC Anthropology SC Anthropology GA 754PJ UT WOS:000289867800004 ER PT J AU Mora, C Aburto-Oropeza, O Bocos, AA Ayotte, PM Banks, S Bauman, AG Beger, M Bessudo, S Booth, DJ Brokovich, E Brooks, A Chabanet, P Cinner, JE Cortes, J Cruz-Motta, JJ Magana, AC DeMartini, EE Edgar, GJ Feary, DA Ferse, SCA Friedlander, AM Gaston, KJ Gough, C Graham, NAJ Green, A Guzman, H Hardt, M Kulbicki, M Letourneur, Y Perez, AL Loreau, M Loya, Y Martinez, C Mascarenas-Osorio, I Morove, T Nadon, MO Nakamura, Y Paredes, G Polunin, NVC Pratchett, MS Bonilla, HR Rivera, F Sala, E Sandin, SA Soler, G Stuart-Smith, R Tessier, E Tittensor, DP Tupper, M Usseglio, P Vigliola, L Wantiez, L Williams, I Wilson, SK Zapata, FA AF Mora, Camilo Aburto-Oropeza, Octavio Ayala Bocos, Arturo Ayotte, Paula M. Banks, Stuart Bauman, Andrew G. Beger, Maria Bessudo, Sandra Booth, David J. Brokovich, Eran Brooks, Andrew Chabanet, Pascale Cinner, Joshua E. Cortes, Jorge Cruz-Motta, Juan J. Cupul Magana, Amilcar DeMartini, Edward E. Edgar, Graham J. Feary, David A. Ferse, Sebastian C. A. Friedlander, Alan M. Gaston, Kevin J. Gough, Charlotte Graham, Nicholas A. J. Green, Alison Guzman, Hector Hardt, Marah Kulbicki, Michel Letourneur, Yves Lopez Perez, Andres Loreau, Michel Loya, Yossi Martinez, Camilo Mascarenas-Osorio, Ismael Morove, Tau Nadon, Marc-Olivier Nakamura, Yohei Paredes, Gustavo Polunin, Nicholas V. C. Pratchett, Morgan S. Bonilla, Hector Reyes Rivera, Fernando Sala, Enric Sandin, Stuart A. Soler, German Stuart-Smith, Rick Tessier, Emmanuel Tittensor, Derek P. Tupper, Mark Usseglio, Paolo Vigliola, Laurent Wantiez, Laurent Williams, Ivor Wilson, Shaun K. Zapata, Fernando A. TI Global Human Footprint on the Linkage between Biodiversity and Ecosystem Functioning in Reef Fishes SO PLOS BIOLOGY LA English DT Article ID CORAL-REEFS; CURRENT KNOWLEDGE; MARINE RESERVES; EASTERN PACIFIC; DEEP-SEA; SERVICES; CONSEQUENCES; PRODUCTIVITY; TEMPERATURES; EXTINCTIONS AB Difficulties in scaling up theoretical and experimental results have raised controversy over the consequences of biodiversity loss for the functioning of natural ecosystems. Using a global survey of reef fish assemblages, we show that in contrast to previous theoretical and experimental studies, ecosystem functioning (as measured by standing biomass) scales in a non-saturating manner with biodiversity (as measured by species and functional richness) in this ecosystem. Our field study also shows a significant and negative interaction between human population density and biodiversity on ecosystem functioning (i.e., for the same human density there were larger reductions in standing biomass at more diverse reefs). Human effects were found to be related to fishing, coastal development, and land use stressors, and currently affect over 75% of the world's coral reefs. Our results indicate that the consequences of biodiversity loss in coral reefs have been considerably underestimated based on existing knowledge and that reef fish assemblages, particularly the most diverse, are greatly vulnerable to the expansion and intensity of anthropogenic stressors in coastal areas. C1 [Mora, Camilo; Tittensor, Derek P.] Dalhousie Univ, Dept Biol, Halifax, NS, Canada. [Aburto-Oropeza, Octavio; Hardt, Marah; Sandin, Stuart A.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. [Ayala Bocos, Arturo] Univ Autonoma Baja California Sur, Dept Biol Marina, La Paz, Mexico. [Ayotte, Paula M.; Nadon, Marc-Olivier; Williams, Ivor] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. [Ayotte, Paula M.; Nadon, Marc-Olivier; Williams, Ivor] NOAA, Coral Reef Ecosyst Div, Pacific Isl Fisheries Sci Ctr, Honolulu, HI USA. [Banks, Stuart] Charles Darwin Univ, Galapagos Isl, Ecuador. [Bauman, Andrew G.; Feary, David A.; Usseglio, Paolo] United Nations Univ, Inst Water Environm & Hlth, Hamilton, ON, Canada. [Bauman, Andrew G.; Cinner, Joshua E.; Graham, Nicholas A. J.; Pratchett, Morgan S.] James Cook Univ, Australian Res Council Ctr Excellence Coral Reef, Townsville, Qld 4811, Australia. [Beger, Maria] Univ Queensland, Sch Biol Sci, Commonwealth Ctr Appl Environm Decis Anal, Brisbane, Qld, Australia. [Bessudo, Sandra; Soler, German] Fdn Malpelo & Otros Ecosistemas Marinos, Bogota, Colombia. [Booth, David J.; Feary, David A.] Univ Technol Sydney, Sch Environm, Sydney, NSW 2007, Australia. [Brokovich, Eran; Loya, Yossi] Tel Aviv Univ, Dept Zool, IL-69978 Tel Aviv, Israel. [Brooks, Andrew] Univ Calif Santa Barbara, Inst Marine Sci, Coastal Res Ctr, Santa Barbara, CA 93106 USA. [Chabanet, Pascale] Inst Rech Dev, Reunion Isl, France. [Cortes, Jorge] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Cruz-Motta, Juan J.] Univ Simon Bolivar, Dept Estudios Ambientales, Caracas, Venezuela. [Cupul Magana, Amilcar] Univ Guadalajara, Ctr Univ Costa, Dept Ciencias Biol, Puerto Vallarta, Mexico. [DeMartini, Edward E.] NOAA, Fisheries Res & Monitoring Div, Pacific Isl Fisheries Sci Ctr, Honolulu, HI USA. [DeMartini, Edward E.] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI USA. [Edgar, Graham J.; Stuart-Smith, Rick] Univ Tasmania, Inst Marine & Antarctic Studies, Hobart, Tas 7001, Australia. [Ferse, Sebastian C. A.] Leibniz Ctr Trop Marine Ecol, Bremen, Germany. [Friedlander, Alan M.; Usseglio, Paolo] Univ Hawaii, Dept Zool, Honolulu, HI 96822 USA. [Gaston, Kevin J.] Univ Sheffield, Dept Anim & Plant Sci, Biodivers & Macroecol Grp, Sheffield S10 2TN, S Yorkshire, England. [Gough, Charlotte] Blue Ventures, London, England. [Green, Alison] Nature Conservancy, Brisbane, Qld, Australia. [Guzman, Hector] Smithsonian Trop Res Inst, Panama City, Panama. [Kulbicki, Michel] Univ Perpignan, Inst Rech Dev, F-66025 Perpignan, France. [Letourneur, Yves; Wantiez, Laurent] Univ Nouvelle Caledonie, Lab Insulaire Vivant & Environm, Noumea, New Caledonia. [Letourneur, Yves] Univ La Reunion, Lab Ecol Marine, St Denis Messageries, France. [Lopez Perez, Andres] Univ Mar, Inst Recursos, Oaxaca, Mexico. [Loreau, Michel] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Martinez, Camilo] Secretaria Nacl Planificac & Desarrollo, Quito, Ecuador. [Mascarenas-Osorio, Ismael] Univ Autonoma Baja California Sur, Ctr Invest Biol Noroeste, La Paz, Mexico. [Morove, Tau] Wildlife Conservat Soc, Papua New Guinea Marine Program, Kavieng, Papua N Guinea. [Nakamura, Yohei] Kochi Univ, Grad Sch Kuroshio Sci, Kochi 780, Japan. [Paredes, Gustavo] Ctr Biodiversidad Marina & Conservac Golfo Calif, San Diego, CA USA. [Polunin, Nicholas V. C.] Newcastle Univ, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Rivera, Fernando] Inst Nazca Invest Marinas, Quito, Ecuador. [Sala, Enric] Ctr Estudis Avancats Blanes, Blanes, Spain. [Sala, Enric] Natl Geog Soc, Washington, DC USA. [Tessier, Emmanuel] Reserve Nat Marine La Reunion, Reunion Isl, France. [Tittensor, Derek P.] World Conservat Monitoring Ctr, United Nations Environm Programme, Cambridge, England. [Tittensor, Derek P.] Microsoft Res Computat Sci Lab, Cambridge, England. [Tupper, Mark] WorldFish Ctr, George Town, Malaysia. [Vigliola, Laurent] Inst Rech Dev, Noumea, New Caledonia. [Wantiez, Laurent] Aquarium Lagons, Noumea, New Caledonia. [Wilson, Shaun K.] Dept Environm & Conservat, Marine Sci Program, Kensington, WA, Australia. [Zapata, Fernando A.] Univ Valle, Dept Biol, Cali, Colombia. RP Mora, C (reprint author), Dalhousie Univ, Dept Biol, Halifax, NS, Canada. EM moracamilo@hotmail.com RI Cinner, Joshua/E-8966-2011; Wantiez, Laurent/L-3343-2013; Vigliola, Laurent/J-7107-2016; Pratchett, Morgan /A-9256-2010; LETOURNEUR, Yves/B-4387-2012; Loya, Yossi/J-3039-2012; Edgar, Graham/C-8341-2013; Beger, Maria/F-9049-2013; Stuart-Smith, Rick/M-1829-2013; Graham, Nicholas/C-8360-2014; OI Wantiez, Laurent/0000-0001-5024-2057; Vigliola, Laurent/0000-0003-4715-7470; Pratchett, Morgan /0000-0002-1862-8459; Cupul-Magana, Amilcar/0000-0002-6455-1253; Lopez-Perez, Andres/0000-0003-1246-7401; LETOURNEUR, Yves/0000-0003-3157-1976; Edgar, Graham/0000-0003-0833-9001; Beger, Maria/0000-0003-1363-3571; Stuart-Smith, Rick/0000-0002-8874-0083; Cinner, Joshua/0000-0003-2675-9317 FU Sloan Foundation; Royal Society; Leverhulme Trust; Nakheel PJSC; Gordon and Betty Moore Foundation; Galapagos National Park Service; Charles Darwin Foundation; Conservation International; Walton Family Foundation; Australian Research Council; National Geographic; Western Indian Ocean Marine Science Association; German National Academic Foundation; National Oceanic and Atmospheric Administration; National Marine Fisheries Service Office of Habitat Conservation; Japan Society for the Promotion of Science; French Institute for Biodiversity; David and Lucile Packard Foundation; Wildlife Conservation Society; United States National Science Foundation; Conservation Leadership Programme; Australian Institute of Marine Sciences; Australian Department of Environment, Water, Heritage and the Arts; Marisla Foundation; World Wildlife Fund; Ocean Conservancy; Natural Sciences and Engineering Council of Canada FX The main funding was provided by the Sloan Foundation through the Census of Marine Life's Future of Marine Animal Populations and Natural Geography in Shore Areas projects. Additional funding and support were provided by the Royal Society; the Leverhulme Trust; Nakheel PJSC; the Gordon and Betty Moore Foundation; Galapagos National Park Service; Charles Darwin Foundation; Conservation International; Walton Family Foundation; the Australian Research Council; National Geographic; the Western Indian Ocean Marine Science Association; the German National Academic Foundation; the Coral Reef Conservation Program of the National Oceanic and Atmospheric Administration; The National Marine Fisheries Service Office of Habitat Conservation; the 21st Century Centers of Excellence Program of the Japan Society for the Promotion of Science; the French Institute for Biodiversity; the David and Lucile Packard Foundation; the Wildlife Conservation Society; the United States National Science Foundation's Long-term Ecological Research Program; The Conservation Leadership Programme; Australian Institute of Marine Sciences; the Australian Department of Environment, Water, Heritage and the Arts; The Marisla Foundation Environment Program; the World Wildlife Fund; The Ocean Conservancy; and the Natural Sciences and Engineering Council of Canada. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 51 TC 339 Z9 351 U1 14 U2 175 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1544-9173 J9 PLOS BIOL JI PLoS. Biol. PD APR PY 2011 VL 9 IS 4 AR e1000606 DI 10.1371/journal.pbio.1000606 PG 9 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA 755NM UT WOS:000289938900001 PM 21483714 ER PT J AU Grav, T Jedicke, R Denneau, L Chesley, S Holman, MJ Spahr, TB AF Grav, Tommy Jedicke, Robert Denneau, Larry Chesley, Steve Holman, Matthew J. Spahr, Timothy B. TI The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID JOVIAN TROJAN ASTEROIDS; JUPITER-FAMILY COMETS; LONG-PERIOD COMETS; NEAR-EARTH OBJECTS; KUIPER-BELT; SIZE DISTRIBUTION; MAGNITUDE DISTRIBUTION; POPULATION; CENTAURS; ORIGIN AB We present here the Pan-STARRS Moving Object Processing System (MOPS) Synthetic Solar System Model (S3M), the first-ever attempt at building a comprehensive flux-limited model of the major small-body populations in the solar system. The goal of the S3M is to provide a valuable tool in the design and testing of the MOPS software, and will be used in the monitoring of the upcoming Pan-STARRS 1 all-sky survey, which started science operations during late spring of 2010. The model is composed of synthetic populations of near-Earth objects (NEOs with a subpopulation of Earth impactors), the main-belt asteroids (MBAs), Jovian Trojans, Centaurs, trans-Neptunian objects (classical, resonant, and scattered trans-Neptunian objects [TNOs]), Jupiter-family comets (JECs), long-period comets (LPCs), and interstellar comets. The model reasonably reproduces the true populations to a minimum of V = 24.5, corresponding to approximately the expected limiting magnitude for Pan-STARRS's ability to detect moving objects. The NEO synthetic population has been extended to H < 25 (corresponding to objects of about 50 m in diameter), allowing for close flybys of the Earth to be modeled. C1 [Grav, Tommy] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Jedicke, Robert; Denneau, Larry] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Chesley, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Holman, Matthew J.; Spahr, Timothy B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Grav, T (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM tgrav@pha.jhu.edu; jedicke@ifa.hawaii.edu; denneau@ifa.hawaii.edu; steve.chesley@jpl.nasa.gov; mholman@cfa.harvard.edu; tspahr@cfa.harvard.cdu FU US Air Force Research Laboratory (Albuquerque, New Mexico) [F29601-02-1-0268] FX The design and construction of the Panoramic Survey Telescope and Rapid Response System by the University of Hawaii Institute for Astronomy is funded by the US Air Force Research Laboratory (Albuquerque, New Mexico) through grant number F29601-02-1-0268. This work was conducted in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 70 TC 24 Z9 24 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD APR PY 2011 VL 123 IS 902 BP 423 EP 447 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 757YM UT WOS:000290124900005 ER PT J AU Rueda, LM Pecor, JE Harrison, BA AF Rueda, L. M. Pecor, J. E. Harrison, B. A. TI Updated distribution records for Anopheles vagus (Diptera: Culicidae) in the Republic of Philippines, and considerations regarding its secondary vector roles in Southeast Asia SO TROPICAL BIOMEDICINE LA English DT Article ID PLASMODIUM-FALCIPARUM; SUBGENUS CELLIA; FLORES-ISLAND; MOSQUITOS; MALARIA; INDONESIA; VIVAX AB Distribution records for Anopheles (Cellia) vagus in the Republic of the Philippines were updated, including recent collection and museum records from Luzon and Visayas Provinces. Larval habitats (e.g. rice paddies, irrigation and drainage ditches), associated species, and the vector potential of this species were also noted. C1 [Rueda, L. M.; Pecor, J. E.] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD 20910 USA. [Harrison, B. A.] N Carolina Dept Environm & Nat Resources, Winston Salem, NC 27107 USA. RP Rueda, LM (reprint author), Smithsonian Inst, Museum Support Ctr MRC 534, Walter Reed Biosystemat Unit, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM ruedapol@si.edu NR 40 TC 7 Z9 7 U1 1 U2 3 PU MALAYSIAN SOC PARASITOLOGY TROPICAL MEDICINE PI KUALA LUMPUR PA C/O INST MEDICAL REEARCH, JALAN PAHANG, KUALA LUMPUR, 50588, MALAYSIA SN 0127-5720 J9 TROP BIOMED JI Trop. Biomed. PD APR PY 2011 VL 28 IS 1 BP 181 EP 187 PG 7 WC Parasitology; Tropical Medicine SC Parasitology; Tropical Medicine GA 754NR UT WOS:000289862500024 PM 21602785 ER PT J AU Merrill, WL AF Merrill, William L. TI The Power of Song: Music and Dance in the Mission Communities of Northern New Spain, 1590-1810 SO CATHOLIC HISTORICAL REVIEW LA English DT Book Review C1 [Merrill, William L.] Smithsonian Inst, Washington, DC 20560 USA. RP Merrill, WL (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CATHOLIC UNIV AMER PRESS PI WASHINGTON PA 620 MICHIGAN AVENUE NE ADMIN BLDG ROOM 303, WASHINGTON, DC 20064 USA SN 0008-8080 J9 CATHOL HIST REV JI Cathol. Hist. Rev. PD APR PY 2011 VL 97 IS 2 BP 400 EP 401 PG 2 WC History SC History GA 749ET UT WOS:000289447100055 ER PT J AU Messner, TC AF Messner, Timothy C. TI White-tailed Deer Management Strategies and Domestication Processes SO HUMAN ECOLOGY LA English DT Article DE Animal domestication; White-tailed deer; Wildlife management; Niche construction; Sport hunting; Archaeology ID ANIMAL DOMESTICATION; KEY DEER; WILD; BEHAVIOR; AGRICULTURE; SELECTION; EVOLUTION; FITNESS; TRAITS AB Today, people in the U.S. commonly engage in mutual relationships with white-tailed deer (WTD) in manners consistent with those that ultimately resulted in the domestication of animals in the past. Using a wide range of media depicting perspectives of sport hunters, biologists, ecologists, and game managers this paper explores: 1) the influence of anthropogenic environments on WTD behavior, 2) 'game' management and the ability to create valued demographics, and 3) the selection for increased antler size in farmed WTD. This study demonstrates that in order to gain a more accurate understanding of domestication, analyses should focus on the evolution of mutualisms between people and animals. Insights gleamed from this analysis also contribute toward our archaeological understanding of prehistoric animal domestication. C1 Smithsonian NMNH, Washington, DC USA. RP Messner, TC (reprint author), Smithsonian NMNH, Washington, DC USA. EM MessnerT@si.edu NR 78 TC 2 Z9 3 U1 4 U2 22 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0300-7839 J9 HUM ECOL JI Hum. Ecol. PD APR PY 2011 VL 39 IS 2 BP 165 EP 178 DI 10.1007/s10745-011-9380-4 PG 14 WC Anthropology; Environmental Studies; Sociology SC Anthropology; Environmental Sciences & Ecology; Sociology GA 750DV UT WOS:000289525900006 ER PT J AU Kemp, AC Buzas, MA Horton, BP Culver, SJ AF Kemp, Andrew C. Buzas, Martin A. Horton, Benjamin P. Culver, Stephen J. TI INFLUENCE OF PATCHINESS ON MODERN SALT-MARSH FORAMINIFERA USED IN SEA-LEVEL STUDIES (NORTH CAROLINA, USA) SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID INTERTIDAL FORAMINIFERA; ATLANTIC-OCEAN; COWPEN MARSH; TEES ESTUARY; OUTER BANKS; ASSEMBLAGES; UK; DISTRIBUTIONS; RISE; ENVIRONMENT AB We collected replicate samples at stations placed systematically along a transect at Oregon Inlet (North Carolina, USA) to investigate spatial homogeneity of dead assemblages of salt-marsh foraminifera. Analysis of variance (ANOVA) was used to investigate the differences in mean proportions for six species (Miliammina fusca, Trochammina inflata, Arenoparrella mexicana, Tiphotrocha comprimata, Haplophragmoides wilherti and Jadammina macrescens) selected because of their importance in distinguishing assemblages across salt marshes in the study region. As expected, ANOVA's on all species indicated significant differences among low-, middle-, and high-marsh zones defined by their flora. No significant differences were found between stations in the low- and high-marsh indicating homogeneity in these zones. In contrast, for all six species in the middle-marsh zone, significant outcomes for ANOVA, cluster analysis and post-hoc comparisons suggested that the middle-marsh should be divided into two zones. In addition, two species exhibited a patchy (inhomogeneous) distribution among all stations in the middle marsh. If confirmed by additional studies, our results indicate that sampling of modern salt-marshes to document the distribution of foraminifera for use in sea-level reconstructions should recognize the spatial variability associated with the middle-marsh floral zone. C1 [Kemp, Andrew C.] Yale Univ, Sch Forestry & Environm Sci, New Haven, CT 06511 USA. [Kemp, Andrew C.] Yale Univ, Yale Climate & Energy Inst, New Haven, CT 06511 USA. [Kemp, Andrew C.; Horton, Benjamin P.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. [Buzas, Martin A.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Culver, Stephen J.] E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. RP Kemp, AC (reprint author), Yale Univ, Sch Forestry & Environm Sci, New Haven, CT 06511 USA. EM andrew.kemp@yale.edu FU United States Geological Survey cooperative agreement award [02ERAG0044]; National Science Foundation [EAR-0717364, EAR-0951686]; NOAA; North Carolina Coastal Geology Cooperative Program; Garry Jones Memorial Award FX We thank United States Geological Survey cooperative agreement award 02ERAG0044 and National Science Foundation awards EAR-0717364 and EAR-0951686. This research is part of NOAA Coastal Ocean Program grant and the North Carolina Coastal Geology Cooperative Program. This paper is a contribution to IGCP Project 588 "Preparing for Coastal Change". A.C. Kemp acknowledges the 2007 Garry Jones Memorial Award (North American Micropaleontology section, SEPM), a University of Pennsylvania summer stipend in Paleontology, and a Geological Society of America graduate student research grant. This manuscript was improved by comments from Katie Szkornik, an anonymous reviewer, and the editorial assistance of Bruce Hayward and Ken Finger. NR 54 TC 9 Z9 10 U1 3 U2 12 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 APR PY 2011 VL 41 IS 2 BP 114 EP 123 PG 10 WC Paleontology SC Paleontology GA 752OF UT WOS:000289701100002 ER PT J AU Buzas, MA Hayek, LAC AF Buzas, Martin A. Hayek, Lee-Ann C. TI COMMUNITY STRUCTURE: GLOBAL EVALUATION AND THE ROLE OF WITHIN COMMUNITY BETA-DIVERSITY SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID SEA BENTHIC FORAMINIFERA; WESTERN ARCTIC-OCEAN; NEW-ZEALAND; SHE ANALYSIS; PLANT-COMMUNITIES; MARINE ECOSYSTEMS; SPECIES-ABUNDANCE; BIODIVERSITY; IDENTIFICATION; PATTERNS AB Community structure is defined as the mathematical statistical distribution of the relative species abundance vector. Consideration of the decomposition equation for species richness, S, evenness, E, and the Shannon estimate of entropy or information, H, plus their respective regressions on the accumulation of the number of individuals, N, in a sample leads to the establishment of three structural types. Each type is defined by the slope, beta(1H), of the regression H versus lnN and depends on the accumulation rate of species between samples (beta-diversity) in a community. These types are designated as 1) Type 0, where H is constant with the accumulation of lnN denoting equilibrium or stability (Log series is a special case); 2) Type 1, where the slope of H is positive with the accumulation of lnN denoting growth or expansion (Log normal is a special case); and 3) Type -1, where the slope of H is negative with the accumulation of lnN denoting decline, instability or stress. In this study, 72 communities were analyzed from environments ranging from marginal marine to the abyss. Only 10 communities are identified as type -1 with the majority of these at lower bathyal and abyssal depths. At abyssal depths the average beta(1H) is -0.057 and data from fossil communities in the Arctic indicate that this unstable, stressed situation has persisted for at least 50 ka. In the Gulf of Mexico at shelf depths, low values for Pui are registered near the Mississippi delta. In contrast, the open-ocean east of New Zealand has an average beta(1H) of 0.227, the highest recorded. Among marginal marine environments an average beta(1H) of -0.030 was recorded in Long Island Sound before the collapse of that community. In contrast, the Indian River Lagoon, Florida had the highest beta(1H) for a marginal marine environment with an average value of 0.195. No simple invariant pattern between type 0 and type 1 communities is prevalent in any environment. Overall 31 communities are type 0 and 31 are type 1. In marginal marine environments (22 communities) the average value of beta(1H) is 0.092. In the open-ocean (50 communities) the average value of beta(1H) is 0.093. Evidently, for any group to remain highly successful on the average a slightly positive value of beta(1H) is required. C1 [Buzas, Martin A.; Hayek, Lee-Ann C.] Smithsonian Inst, MRC 121, Washington, DC 20013 USA. RP Buzas, MA (reprint author), Smithsonian Inst, MRC 121, Washington, DC 20013 USA. EM buzasm@si.edu NR 50 TC 4 Z9 4 U1 1 U2 10 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 APR PY 2011 VL 41 IS 2 BP 138 EP 154 PG 17 WC Paleontology SC Paleontology GA 752OF UT WOS:000289701100004 ER PT J AU Gunasekera, SP Owle, CS Montaser, R Luesch, H Paul, VJ AF Gunasekera, Sarath P. Owle, Chivas S. Montaser, Rana Luesch, Hendrik Paul, Valerie J. TI Malyngamide 3 and Cocosamides A and B from the Marine Cyanobacterium Lyngbya majuscula from Cocos Lagoon, Guam SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID PHILINOPSIS-SPECIOSA; MOLLUSK AB Malyngamide 3 (1) and cocosamides A (2) and B (3) were isolated from the lipophilic extract of a collection of Lyngbya majuscula from Cocos,Lagoon, Guam. The planar structures of compounds 1-3 were determined by spectroscopic methods. The absolute configuration of 1 was determined by modified Mosher's method, NOESY data, and comparison with lyngbic acid (4). The absolute configurations of 2 and 3 were assigned by enantioselective HPLC analysis and comparison with the closely related compound pitipeptolide 4 (5). Compounds 173 showed weak cytotoxicity against MCF7 breast cancer and HT-29 colon cancer cells. C1 [Gunasekera, Sarath P.; Owle, Chivas S.; Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Montaser, Rana; 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 NIH, NIGMS [P41GM806210] FX This research was supported by the NIH, NIGMS Grant P41GM806210. We thank E. Cruz-Rivera for collecting the sample. We also thank the Harbor Branch Oceanographic Institute at Florida Atlantic University spectroscopy facility for 600 MHz NMR spectrometer time and UV measurements and the Florida Atlantic University, Jupiter Campus, for the use of their polarimeter and infrared spectrometer. The high-resolution mass spectrometric analysis was performed by the UCR mass spectrometer facility, Department of Chemistry, University of California at Riverside. This is contribution number 840 from the Smithsonian Marine Station at Fort Pierce. NR 18 TC 13 Z9 13 U1 1 U2 14 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD APR PY 2011 VL 74 IS 4 BP 871 EP 876 DI 10.1021/np1008015 PG 6 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 753CL UT WOS:000289742300052 PM 21341718 ER PT J AU Serra, AL Diaferio, A Murante, G Borgani, S AF Serra, Ana Laura Diaferio, Antonaldo Murante, Giuseppe Borgani, Stefano TI Measuring the escape velocity and mass profiles of galaxy clusters beyond their virial radius SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitation; galaxies: clusters: general; techniques: miscellaneous; cosmology: miscellaneous; cosmology: dark matter; cosmology: large-scale structure of Universe ID X-RAY; SUNYAEV-ZELDOVICH; INFALL REGIONS; COSMOLOGICAL SIMULATIONS; SHAPLEY SUPERCLUSTER; SCALING RELATIONS; REDSHIFT SURVEY; RICH CLUSTERS; COMA CLUSTER; DARK-MATTER AB The caustic technique uses galaxy redshifts alone to measure the escape velocity and mass profiles of galaxy clusters to clustrocentric distances well beyond the virial radius, where dynamical equilibrium does not necessarily hold. We provide a detailed description of this technique and analyse its possible systematic errors. We apply the caustic technique to clusters with mass M(200) >= 10(14)h(-1)M(circle dot) extracted from a cosmological hydrodynamic simulation of Lambda CDM universe. With a few tens of redshifts per squared comoving megaparsec within the cluster, the caustic technique, on average, recovers the profile of the escape velocity from the cluster with better than 10 percent accuracy up to r similar to 4r(200). The caustic technique also recovers the mass profile with better than 10 percent accuracy in the range (0.6 - 4)r(200), but it overestimates the mass up to 70 percent at smaller radii. This overestimate is a consequence of neglecting the radial dependence of the filling function F beta(r). The 1-sigma uncertainty on individual escape velocity profiles increases from similar to 20 to similar to 50 percent when the radius increases from r similar to 0.1r(200) to similar to 4r(200). Individual mass profiles have 1-sigma uncertainty between 40 and 80 percent within the radial range (0.6 - 4) r(200). When the correct virial mass is known, the 1-sigma uncertainty reduces to a constant 50 percent on the same radial range. We show that the amplitude of these uncertainties is completely due to the assumption of spherical symmetry, which is difficult to drop. Other potential refinements of the technique are not crucial. We conclude that, when applied to individual clusters, the caustic technique generally provides accurate escape velocity and mass profiles, although, in some cases, the deviation from the real profile can be substantial. Alternatively, we can apply the technique to synthetic clusters obtained by stacking individual clusters: in this case, the 1-sigma uncertainty on the escape velocity profile is smaller than 20 percent out to 4r(200). The caustic technique thus provides reliable average profiles which extend to regions difficult or impossible to probe with other techniques. C1 [Serra, Ana Laura; Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy. [Serra, Ana Laura; Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, Turin, Italy. [Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murante, Giuseppe] INAF, Osservatorio Astron Torino, Turin, Italy. [Borgani, Stefano] Univ Trieste, Dipartimento Astron, Trieste, Italy. [Borgani, Stefano] INAF, Osservatorio Astron Trieste, Trieste, Italy. [Borgani, Stefano] Ist Nazl Fis Nucl, Sez Trieste, Trieste, Italy. RP Serra, AL (reprint author), Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Via P Giuria 1, I-10125 Turin, Italy. EM serra@ph.unito.it OI Borgani, Stefano/0000-0001-6151-6439; Murante, Giuseppe/0000-0002-5155-130X FU INFN [PD51]; PRIN-MIUR; ASI/COFIS [I/016/07/0] FX AD warmly thanks Margaret Geller and Ken Rines whose contribution to the development and the diffusion of the caustic method has been invaluable over more than a decade now. AD also acknowledges Matthias Bartelmann and the Institut fur Theoretische Astrophysik (ITA) in Heidelberg for their warm hospitality offered during the realization of part of this work. We thank the referee for her/his careful reading of the manuscript that helped to find some inaccuracies in our initial presentation of our results. We acknowledge partial support from the INFN grant PD51, the PRIN-MIUR-2008 grant "Matter-antimatter asymmetry, dark matter and dark energy in the LHC Era", the PRIN-MIUR-2007 grant "The cycle of cosmic baryons" and the contract ASI/COFIS I/016/07/0. NR 72 TC 53 Z9 53 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 APR PY 2011 VL 412 IS 2 BP 800 EP 816 DI 10.1111/j.1365-2966.2010.17946.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900058 ER PT J AU Lovegrove, J Schild, RE Leiter, D AF Lovegrove, Justin Schild, Rudolph E. Leiter, Darryl TI Discovery of universal outflow structures above and below the accretion disc plane in radio-quiet quasars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; quasars: general ID GRAVITATIONALLY LENSED QUASAR; MICROLENSING LIGHT CURVES; ACTIVE GALACTIC NUCLEI; QSO 2237+0305; X-RAY; Q0957+561; REVERBERATION; VARIABILITY AB 59 quasars in the background of the Magellanic Clouds had brightness records monitored by the MACHO project during the years 1992-99. Because the circumpolar fields of these quasars had no seasonal sampling defects, their observation produced data sets well suited to further careful analysis. Following a preliminary report wherein we showed the existence of reverberation in the data for one of the radio-quiet quasars in this group, we now show that similar reverberations have been seen in all of the 55 radio-quiet quasars with adequate data, making possible the determination of the quasar inclination to the observer's line of sight. The reverberation signatures indicate the presence of large-scale elliptical outflow structures similar to that predicted by the Elvis and 'dusty torus' models of quasars, whose characteristic sizes vary within a surprisingly narrow range of scales. More importantly, the observed opening angle relative to the polar axis of the universal elliptical outflow structure present was consistently found to be on the order of 78 degrees. C1 [Lovegrove, Justin; Schild, Rudolph E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lovegrove, Justin] Univ Southampton, Sch Math, Southampton SO17 1BJ, Hants, England. [Lovegrove, Justin] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Lovegrove, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM j.lovegrove@soton.ac.uk FU University of California, Lawrence Livermore National Laboratory [W-7405-Eng-48]; National Science Foundation through the Center for Particle Astrophysics of the University of California [AST-8809616]; Mount Stromlo and Siding Spring Observatory, Australian National University FX We thank Pavlos Protopapas for help with accessing the MACHO programme data files, and we thank the MACHO Consortium for making the brightness records publicly available. We thank Tesvi Mazeh and Victor Vakulik for useful conversations about the properties of the autocorrelation function. We also thank Phil Uttley for discussion of the properties of red noise. DL thanks Alan Bridle of the National Radio Astronomy Observatory (NRAO) for many insightful suggestions and for his hospitality at NRAO during the 2008-09 time period when this research was performed. This paper utilizes public domain data originally obtained by the MACHO Project, whose work was performed under the joint auspices of the US Department of Energy, National Nuclear Security Administration by the University of California, Lawrence Livermore National Laboratory under contract no. W-7405-Eng-48, the National Science Foundation through the Center for Particle Astrophysics of the University of California under cooperative agreement AST-8809616 and the Mount Stromlo and Siding Spring Observatory, part of the Australian National University. NR 28 TC 4 Z9 4 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 APR PY 2011 VL 412 IS 4 BP 2631 EP 2640 DI 10.1111/j.1365-2966.2010.18082.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 747BR UT WOS:000289295800039 ER PT J AU Hamilton, AJ Basset, Y Benke, KK Grimbacher, PS Miller, SE Novotny, V Samuelson, GA Stork, NE Weiblen, GD Yen, JDL AF Hamilton, Andrew J. Basset, Yves Benke, Kurt K. Grimbacher, Peter S. Miller, Scott E. Novotny, Vojtech Samuelson, G. Allan Stork, Nigel E. Weiblen, George D. Yen, Jian D. L. TI Quantifying uncertainty in estimation of tropical arthropod species richness (vol 176, pg 90, 2010) SO AMERICAN NATURALIST LA English DT Correction C1 [Hamilton, Andrew J.; Grimbacher, Peter S.; Stork, Nigel E.; Yen, Jian D. L.] Univ Melbourne, Dept Resource Management & Geog, Richmond, Vic, Australia. [Basset, Yves] Smithsonian Trop Res Inst, Balboa, Panama. [Benke, Kurt K.] Dept Primary Ind, Parkville Ctr, Vic 3052, Australia. [Miller, Scott E.] Natl Museum Nat Hist, Washington, DC 20013 USA. [Miller, Scott E.] Smithsonian Inst, Washington, DC 20013 USA. [Novotny, Vojtech] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice 37005, Czech Republic. [Novotny, Vojtech] Univ S Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Samuelson, G. Allan] Bernice P Bishop Museum, Honolulu, HI USA. [Weiblen, George D.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. RP Hamilton, AJ (reprint author), Univ Melbourne, Dept Resource Management & Geog, Burnley Campus,500 Yarra Blvd, Richmond, Vic, Australia. RI Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014 OI Novotny, Vojtech/0000-0001-7918-8023 NR 1 TC 17 Z9 17 U1 2 U2 28 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD APR PY 2011 VL 177 IS 4 BP 544 EP 545 DI 10.1086/659643 PG 2 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 746IF UT WOS:000289237700014 ER PT J AU Laurance, WF Kakul, T Keenan, RJ Sayer, J Passingan, S Clements, GR Villegas, F Sodhi, NS AF Laurance, William F. Kakul, Titus Keenan, Rodney J. Sayer, Jeffrey Passingan, Simon Clements, Gopalasamy R. Villegas, Felipe Sodhi, Navjot S. TI Predatory corporations, failing governance, and the fate of forests in Papua New Guinea SO CONSERVATION LETTERS LA English DT Article DE Corruption; deforestation; forest management; logging; multinational corporations; REDD; tropical timber ID CONSERVATION AB Papua New Guinea (PNG) sustains some of the world's most biologically and culturally rich forests. Like many tropical nations, PNG is changing rapidly as it attempts to develop economically, but corporate misdealing and weak governance are undermining its capacity to do so sustainably. Overexploitation of forests is rampant, with most accessible forests likely to be logged or disappear in 1-2 decades. The timber industry has long been plagued by endemic corruption, with Rimbunan Hijau, a Malaysian corporation controlling much of the country's timber supplies, considered a chronic offender by many. Most timber is exported as raw logs, mainly to China, providing only limited income and employment for local communities. Because of corruption and weak enforcement capacity, proceeds from logging are often concentrated in the hands of political elites or the wealthy and logging operations often violate mandated standards. Moreover, traditional communal groups in PNG have recently been stripped of their legal rights to impede development projects that are deemed environmentally risky. Human welfare in the country has actually worsened, with mean incomes, adult literacy, and the Human Development Index all falling in recent years. We propose a slate of immediate measures to reduce environmental damage and the exhaustion of timber supplies while increasing societal benefits in PNG. C1 [Laurance, William F.; Kakul, Titus; Clements, Gopalasamy R.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. [Keenan, Rodney J.] Univ Melbourne, Dept Forest & Ecosyst Sci, Creswick, Vic 3363, Australia. [Sayer, Jeffrey] James Cook Univ, Sch Earth & Environm Studies, Cairns, Qld 4870, Australia. [Passingan, Simon] Barefoot Community Serv, Rabaul, Papua N Guinea. [Clements, Gopalasamy R.] Univ Malaya, Ctr Malaysian Indigenous Studies, Kuala Lumpur 50603, Malaysia. [Villegas, Felipe] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Sodhi, Navjot S.] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. RP Laurance, WF (reprint author), James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. EM bill.laurance@jcu.edu.au RI Sayer, Jeffrey/H-5504-2011; Laurance, William/B-2709-2012; James Cook University, TESS/B-8171-2012; Research ID, CTBCC /O-3564-2014; OI Keenan, Rodney/0000-0002-2804-4975 NR 41 TC 17 Z9 18 U1 1 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-263X J9 CONSERV LETT JI Conserv. Lett. PD APR PY 2011 VL 4 IS 2 BP 95 EP 100 DI 10.1111/j.1755-263X.2010.00156.x PG 6 WC Biodiversity Conservation SC Biodiversity & Conservation GA 747EA UT WOS:000289301900003 ER PT J AU Duval, BD Dijkstra, P Natali, SM Megonigal, JP Ketterer, ME Drake, BG Lerdau, MT Gordon, G Anbar, AD Hungate, BA AF Duval, Benjamin D. Dijkstra, Paul Natali, Susan M. Megonigal, J. Patrick Ketterer, Michael E. Drake, Bert G. Lerdau, Manuel T. Gordon, Gwyneth Anbar, Ariel D. Hungate, Bruce A. TI Plant-Soil Distribution of Potentially Toxic Elements in Response to Elevated Atmospheric CO2 SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID SCRUB-OAK ECOSYSTEM; CARBON-DIOXIDE; FOREST; ENRICHMENT; NITROGEN; MERCURY; DECOMPOSITION; MOLYBDENUM; QUALITY; BIOMASS AB The distribution of contaminant elements within ecosystems is an environmental concern because of these elements' potential toxicity to animals and plants and their ability to hinder microbial ecosystem services. As with nutrients, contaminants are cycled within and through ecosystems. Elevated atmospheric CO2 generally increases plant productivity and alters nutrient element cycling, but whether CO2 causes similar effects on the cycling of contaminant elements is unknown. Here we show that 11 years of experimental CO2 enrichment in a sandy soil with low organic matter content causes plants to accumulate contaminants in plant biomass, with declines in the extractable contaminant element pools in surface soils. These results indicate that CO2 alters the distribution of contaminant elements in ecosystems, with plant element accumulation and declining soil availability both likely explained by the CO2 stimulation of plant biomass. Our results highlight the interdependence of element cycles and the importance of taking a broad view of the periodic table when the effects of global environmental change on ecosystem biogeochemistry are considered. C1 [Duval, Benjamin D.; Dijkstra, Paul; Hungate, Bruce A.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA. [Duval, Benjamin D.; Dijkstra, Paul; Hungate, Bruce A.] No Arizona Univ, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA. [Ketterer, Michael E.] No Arizona Univ, Dept Chem & Biochem, Flagstaff, AZ 86011 USA. [Natali, Susan M.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Megonigal, J. Patrick; Drake, Bert G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Lerdau, Manuel T.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Gordon, Gwyneth; Anbar, Ariel D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Duval, BD (reprint author), No Arizona Univ, Dept Biol Sci, Box 5640, Flagstaff, AZ 86011 USA. EM bdduval@illinois.edu RI Hungate, Bruce/F-8991-2011; Lerdau, Manuel/E-7320-2011 OI Hungate, Bruce/0000-0002-7337-1887; Lerdau, Manuel/0000-0003-1864-0834 FU NSF [DEB-0445324]; NSF-IGERT; Science Foundation Arizona FX We thank Hans Anderson, Tom Powell, and David Johnson for maintenance of the Florida experiment. This work was supported by NSF Grant DEB-0445324, a NSF-IGERT fellowship awarded to B.D.D., and funds provided by Science Foundation Arizona to B.D.D. NR 32 TC 13 Z9 14 U1 4 U2 36 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD APR 1 PY 2011 VL 45 IS 7 BP 2570 EP 2574 DI 10.1021/es102250u PG 5 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 741CU UT WOS:000288841500013 PM 21405117 ER PT J AU Altman, I Blakeslee, AMH Osio, GC Rillahan, CB Teck, SJ Meyer, JJ Byers, JE Rosenberg, AA AF Altman, Irit Blakeslee, April M. H. Osio, Giacomo C. Rillahan, Christopher B. Teck, Sarah J. Meyer, John J. Byers, James E. Rosenberg, Andrew A. TI A practical approach to implementation of ecosystem-based management: a case study using the Gulf of Maine marine ecosystem SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Article ID RESILIENCE; SERVICES; IMPACTS; BIODIVERSITY; EXPERIENCES; DEPLETION; SYSTEMS; HISTORY; SHIFTS AB The application of ecosystem-based management (EBM) in marine environments has been widely supported by scientists, managers, and policy makers, yet implementation of this approach is difficult for various scientific, political, and social reasons. A key, but often overlooked, challenge is how to account for multiple and varied human activities and ecosystem services and incorporate ecosystem-level thinking into EBM planning. We developed methods to systematically identify the natural and human components of a specific ecosystem and to qualitatively evaluate the strength of their interactions. Using the Gulf of Maine marine ecosystem as a case study, we show how these methods may be applied, in order to identify and prioritize the most important components to be included in an EBM plan - particularly the human activities that are the strongest drivers of ecosystem change and the ecosystem services most threatened by cumulative and indirect effects of these activities. C1 [Altman, Irit; Byers, James E.] Univ New Hampshire, Dept Biol Sci, Durham, NH 03824 USA. [Blakeslee, April M. H.] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA. [Osio, Giacomo C.; Rosenberg, Andrew A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Rillahan, Christopher B.] War Pacific Natl Hist Pk, Hagatna, GU USA. [Teck, Sarah J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Meyer, John J.] Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA. RP Altman, I (reprint author), Univ New Hampshire, Dept Biol Sci, Durham, NH 03824 USA. EM irit.altman@unh.edu RI Teck, Sarah/C-5179-2009 NR 28 TC 14 Z9 14 U1 1 U2 16 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 EI 1540-9309 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD APR PY 2011 VL 9 IS 3 BP 183 EP 189 DI 10.1890/080186 PG 7 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 748GK UT WOS:000289377800020 ER PT J AU Brown, SD Gilmour, CC Kucken, AM Wall, JD Elias, DA Brandt, CC Podar, M Chertkov, O Held, B Bruce, DC Detter, JC Tapia, R Han, CS Goodwin, LA Cheng, JF Pitluck, S Woyke, T Mikhailova, N Ivanova, NN Han, J Lucas, S Lapidus, AL Land, ML Hauser, LJ Palumbo, AV AF Brown, Steven D. Gilmour, Cynthia C. Kucken, Amy M. Wall, Judy D. Elias, Dwayne A. Brandt, Craig C. Podar, Mircea Chertkov, Olga Held, Brittany Bruce, David C. Detter, John C. Tapia, Roxanne Han, Cliff S. Goodwin, Lynne A. Cheng, Jan-Fang Pitluck, Samuel Woyke, Tanja Mikhailova, Natalia Ivanova, Natalia N. Han, James Lucas, Susan Lapidus, Alla L. Land, Miriam L. Hauser, Loren J. Palumbo, Anthony V. TI Genome Sequence of the Mercury-Methylating Strain Desulfovibrio desulfuricans ND132 SO JOURNAL OF BACTERIOLOGY LA English DT Article ID ESTUARINE SEDIMENT; REDUCING BACTERIA; METHYLMERCURY; HEALTH AB Desulfovibrio desulfuricans strain ND132 is an anaerobic sulfate-reducing bacterium (SRB) capable of producing methylmercury (MeHg), a potent human neurotoxin. The mechanism of methylation by this and other organisms is unknown. We present the 3.8-Mb genome sequence to provide further insight into microbial mercury methylation. C1 [Brown, Steven D.; Elias, Dwayne A.; Brandt, Craig C.; Podar, Mircea; Land, Miriam L.; Hauser, Loren J.; Palumbo, Anthony V.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. [Gilmour, Cynthia C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Kucken, Amy M.; Wall, Judy D.] Univ Missouri, Dept Biochem, Columbia, MO 65211 USA. [Chertkov, Olga; Held, Brittany; Bruce, David C.; Detter, John C.; Tapia, Roxanne; Han, Cliff S.; Goodwin, Lynne A.] Los Alamos Natl Lab, Biosci Div, Los Alamos, NM 87545 USA. [Chertkov, Olga; Held, Brittany; Bruce, David C.; Detter, John C.; Tapia, Roxanne; Han, Cliff S.; Goodwin, Lynne A.; Cheng, Jan-Fang; Pitluck, Samuel; Woyke, Tanja; Mikhailova, Natalia; Ivanova, Natalia N.; Han, James; Lucas, Susan; Lapidus, Alla L.; Land, Miriam L.; Hauser, Loren J.] US DOE, Joint Genome Inst, Walnut Creek, CA 94598 USA. [Cheng, Jan-Fang; Pitluck, Samuel; Woyke, Tanja; Mikhailova, Natalia; Ivanova, Natalia N.; Han, James; Lapidus, Alla L.] Univ Calif Berkeley, Lawrence Berkeley Lab, Genom Div, Berkeley, CA 94720 USA. [Lucas, Susan] Lawrence Livermore Natl Lab, Genom Div, Livermore, CA 94550 USA. RP Brown, SD (reprint author), Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. EM brownsd@ornl.gov RI Palumbo, Anthony/A-4764-2011; Gilmour, Cynthia/G-1784-2010; Elias, Dwayne/B-5190-2011; Hauser, Loren/H-3881-2012; Lapidus, Alla/I-4348-2013; Land, Miriam/A-6200-2011; Brown, Steven/A-6792-2011; OI Palumbo, Anthony/0000-0002-1102-3975; Gilmour, Cynthia/0000-0002-1720-9498; Elias, Dwayne/0000-0002-4469-6391; Lapidus, Alla/0000-0003-0427-8731; Land, Miriam/0000-0001-7102-0031; Brown, Steven/0000-0002-9281-3898; Podar, Mircea/0000-0003-2776-0205 FU Office of Biological and Environmental Research (OBER), Office of Science, U.S. Department of Energy (DOE); Oak Ridge National Laboratory [DE-FG02-073464396]; U.S. Department of Energy [DE-AC05-00OR22725]; Office of Science of the U.S. Department of Energy [AC02-05CH11231] FX This research was supported by the Office of Biological and Environmental Research (OBER), Office of Science, U.S. Department of Energy (DOE), as part of the Mercury Science Focus Area Program at Oak Ridge National Laboratory and grant DE-FG02-073464396 (J.D.W.). Oak Ridge National Laboratory is managed by UT-Battelle, LLC, for the U.S. Department of Energy under contract DE-AC05-00OR22725. The work conducted by the U.S. Department of Energy Joint Genome Institute is supported by the Office of Science of the U.S. Department of Energy under contract no. DE-AC02-05CH11231. NR 15 TC 19 Z9 21 U1 1 U2 17 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0021-9193 EI 1098-5530 J9 J BACTERIOL JI J. Bacteriol. PD APR PY 2011 VL 193 IS 8 BP 2078 EP 2079 DI 10.1128/JB.00170-11 PG 2 WC Microbiology SC Microbiology GA 746GA UT WOS:000289229900040 PM 21357488 ER PT J AU Weldon, PJ Carroll, JF Kramer, M Bedoukian, RH Coleman, RE Bernier, UR AF Weldon, Paul J. Carroll, John F. Kramer, Matthew Bedoukian, Robert H. Coleman, Russell E. Bernier, Ulrich R. TI Anointing Chemicals and Hematophagous Arthropods: Responses by Ticks and Mosquitoes to Citrus (Rutaceae) Peel Exudates and Monoterpene Components SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE Citrus; Ectoparasites; Ticks; Mosquitoes; Monoterpenes; Anointing; Repellent ID FUR-RUBBING BEHAVIOR; ESSENTIAL OIL; IXODES-RICINUS; RHIPICEPHALUS-APPENDICULATUS; REPELLENT ACTIVITY; ATELES-GEOFFROYI; CAPUCHIN MONKEYS; CEBUS-CAPUCINUS; CULICIDAE; DIPTERA AB Some birds and mammals roll on or wipe themselves with the fruits or leaves of Citrus spp. or other Rutaceae. These anointing behaviors, as with anointing in general, are thought to function in the topical acquisition of chemicals that deter consumers, including hematophagous arthropods. We measured avoidance and other responses by nymphal lone star ticks (Amblyomma americanum) and adult female yellow fever mosquitoes (Aedes aegypti) to lemon peel exudate and to 24 volatile monoterpenes (racemates and isomers), including hydrocarbons, alcohols, aldehydes, acetates, ketones, and oxides, present in citrus fruits and leaves in order to examine their potential as arthropod deterrents. Ticks allowed to crawl up vertically suspended paper strips onto a chemically treated zone avoided the peel exudate and geraniol, citronellol, citral, carveol, geranyl acetate, alpha-terpineol, citronellyl acetate, and carvone. Ticks confined in chemically treated paper packets subsequently were impaired in climbing and other behaviors following exposure to the peel exudate and, of the compounds tested, most impaired to carveol. Mosquitoes confined in chambers with chemically treated feeding membranes landed and fed less, and flew more, when exposed to the peel exudate than to controls, and when exposed to aldehydes, oxides, or alcohols versus most hydrocarbons or controls. However, attraction by mosquitoes in an olfactometer was not inhibited by either lemon peel exudate or most of the compounds we tested. Our results support the notion that anointing by vertebrates with citrus-derived chemicals deters ticks. We suggest that some topically applied compounds are converted into more potent arthropod deterrents when oxidized on the integument of anointed animals. C1 [Weldon, Paul J.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Carroll, John F.] ARS, USDA, Invas Insect Biocontrol & Behav Lab, Beltsville Agr Res Ctr, Beltsville, MD 20705 USA. [Kramer, Matthew] ARS, USDA, Biometr Consulting Serv, Beltsville Agr Res Ctr, Beltsville, MD 20705 USA. [Bedoukian, Robert H.] Bedoukian Res Inc, Danbury, CT 06810 USA. [Coleman, Russell E.] Walter Reed Army Inst Res, Dept Entomol, Div Communicable Dis & Immunol, Silver Spring, MD 20910 USA. [Bernier, Ulrich R.] ARS, USDA, Ctr Med Agr & Vet Entomol, Gainesville, FL 32608 USA. RP Weldon, PJ (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM weldonp@si.edu NR 63 TC 26 Z9 26 U1 5 U2 24 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0098-0331 EI 1573-1561 J9 J CHEM ECOL JI J. Chem. Ecol. PD APR PY 2011 VL 37 IS 4 BP 348 EP 359 DI 10.1007/s10886-011-9922-7 PG 12 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 751LD UT WOS:000289618300003 PM 21409496 ER PT J AU Hood, WR Oftedal, OT Kunz, TH AF Hood, Wendy R. Oftedal, Olav T. Kunz, Thomas H. TI Is tissue maturation necessary for flight? Changes in body composition during postnatal development in the big brown bat SO JOURNAL OF COMPARATIVE PHYSIOLOGY B-BIOCHEMICAL SYSTEMIC AND ENVIRONMENTAL PHYSIOLOGY LA English DT Article DE Body composition; Calcium; Chiroptera; Eptesicus fuscus; Flight; Postnatal development ID MYOTIS-LUCIFUGUS; EPTESICUS-FUSCUS; GROWTH-RATES; TADARIDA-BRASILIENSIS; NUTRIENT DEPOSITION; CARCASS COMPOSITION; REPRODUCTIVE-CYCLE; NUTRITIONAL-STATUS; PROTEIN-CONTENT; JAPANESE QUAIL AB Patterns of offspring development reflect the availability of energy and nutrients, limitations on an individual's capacity to use available resources, and tradeoffs between the use of nutrients to support current metabolic demands and tissue growth. To determine if the long period of offspring dependency in bats is associated with the need for an advanced state of tissue maturation prior to flight, we examined body composition during postnatal growth in the big brown bat, Eptesicus fuscus. Despite their large size at birth (22% of maternal mass), newborn bats are relatively immature, containing 82% body water in fat-free mass. However, the total body water content of newborn bat pups decreases to near-adult levels in advance of weaning, while concentrations of total body fat and protein exceed adult values. In contrast to many other mammals, postnatal growth of bat pups was characterized by relatively stable concentrations of calcium and phosphorus, but declining concentrations of magnesium. These levels remained stable or rebounded in late postnatal development. This casts doubt on the hypothesis that low rates of mineral transfer necessitate an extended lactation period in bats. However, our finding of near-adult body composition at weaning is consistent with the hypothesis that extended lactation in bats is necessary for the young to achieve sufficient tissue maturity to undertake the active flight necessary for independent feeding. In this respect, bats differ from most other mammals but resemble birds that must engage in active flight to achieve nutritional independence. C1 [Hood, Wendy R.; Kunz, Thomas H.] Boston Univ, Dept Biol, Ctr Ecol & Conservat Biol, Boston, MA 02215 USA. [Oftedal, Olav T.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Hood, WR (reprint author), Auburn Univ, Dept Biol Sci, 101 Life Sci Bldg, Auburn, AL 36849 USA. EM wrhood@auburn.edu FU National Institutes of Child Health and Development Grant [5-T32HD078387]; Smithsonian Office of Fellowships; Boston University's Center for Ecology and Conservation Biology FX We thank the A. Husk and C. Zahn families for access to their barns for bat collection. K. Jung assisted in the Weld and D. Hellinga, K. Flickinger, L. Nelson and M. Jakubasz assisted in the Nutrition Laboratory. Regina Eisert, Christina Booher, Geoff Hill, participants in the Hill/Hood labs, and three anonymous reviewers made valuable comments contributing to the final form of this manuscript. A National Institutes of Child Health and Development Grant (5-T32HD078387) to I.P. Callard helped support this project in the final year of analysis. W. Hood thanks the Smithsonian Office of Fellowships for a Graduate Student Research Fellowship. Additional support was provided by Boston University's Center for Ecology and Conservation Biology. NR 86 TC 2 Z9 2 U1 1 U2 8 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0174-1578 EI 1432-136X J9 J COMP PHYSIOL B JI J. Comp. Physiol. B-Biochem. Syst. Environ. Physiol. PD APR PY 2011 VL 181 IS 3 BP 423 EP 435 DI 10.1007/s00360-010-0521-7 PG 13 WC Physiology; Zoology SC Physiology; Zoology GA 749ED UT WOS:000289444800011 PM 21046406 ER PT J AU Sanchez-Azofeifa, A Rivard, B Wright, J Feng, JL Li, PJ Chong, MM Bohlman, SA AF Sanchez-Azofeifa, Arturo Rivard, Benoit Wright, Joseph Feng, Ji-Lu Li, Peijun Chong, Mei Mei Bohlman, Stephanie A. TI Estimation of the Distribution of Tabebuia guayacan (Bignoniaceae) Using High-Resolution Remote Sensing Imagery SO SENSORS LA English DT Article DE high-resolution remote sensing; T. guayacan; Spectral Angle Mapping; machine learning ID SUPPORT VECTOR MACHINES; TROPICAL MOIST FOREST; LAND-COVER CHANGE; LEAF-AREA INDEX; HYPERSPECTRAL DISCRIMINATION; SATELLITE DATA; AMAZON FOREST; COSTA-RICA; IN-SITU; CLASSIFICATION AB Species identification and characterization in tropical environments is an emerging field in tropical remote sensing. Significant efforts are currently aimed at the detection of tree species, of levels of forest successional stages, and the extent of liana occurrence at the top of canopies. In this paper we describe our use of high resolution imagery from the Quickbird Satellite to estimate the flowering population of Tabebuia guayacan trees at Barro Colorado Island (BCI), in Panama. The imagery was acquired on 29 April 2002 and 21 March 2004. Spectral Angle Mapping via a One-Class Support Vector machine was used to detect the presence of 422 and 557 flowering tress in the April 2002 and March 2004 imagery. Of these, 273 flowering trees are common to both dates. This study presents a new perspective on the effectiveness of high resolution remote sensing for monitoring a phenological response and its use as a tool for potential conservation and management of natural resources in tropical environments. C1 [Sanchez-Azofeifa, Arturo; Rivard, Benoit; Feng, Ji-Lu; Chong, Mei Mei] Univ Alberta, CEOS, Edmonton, AB T6G 2R3, Canada. [Sanchez-Azofeifa, Arturo; Rivard, Benoit; Feng, Ji-Lu; Chong, Mei Mei] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2R3, Canada. [Sanchez-Azofeifa, Arturo; Wright, Joseph] Smithsonian Trop Res Inst, Panama City, Panama. [Li, Peijun] Peking Univ, Inst Remote Sensing, Beijing 100871, Peoples R China. [Li, Peijun] Peking Univ, GIS, Beijing 100871, Peoples R China. [Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. RP Sanchez-Azofeifa, A (reprint author), Univ Alberta, CEOS, Edmonton, AB T6G 2R3, Canada. EM arturo.sanchez@ualberta.ca; benoit.rivard@ualberta.ca; wrightj@si.edu; jfeng@ualberta.ca; pjli@pku.edu.cn; meimei@ualberta.ca; sbohlman@ufl.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU National Science and Engineering Research Council of Canada (NSERC); Inter American Institute for Global Change Research (IAI) Collaborative Research Network [021]; U.S. National Science Foundation [GEO 0452325] FX This work was supported by the National Science and Engineering Research Council of Canada (NSERC), Discovery Grant Program; and the Inter American Institute for Global Change Research (IAI) Collaborative Research Network program (CRN) II # 021 that is supported by the U.S. National Science Foundation (Grant GEO 0452325). We are also thankful to Donnette Thayer for her help with the English in this manuscript and two anonymous reviewers for their comments. Patrick Jansen and Helene Muller-Landau helped collect the 2005 aerial photographs that were taken by Marcos Guerra of STRI. NR 52 TC 14 Z9 14 U1 1 U2 23 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1424-8220 J9 SENSORS-BASEL JI Sensors PD APR PY 2011 VL 11 IS 4 BP 3831 EP 3851 DI 10.3390/s110403831 PG 21 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA 746GP UT WOS:000289231600023 PM 22163825 ER PT J AU Chen, PT Chen, LQ Wen, J AF Chen, Pingting Chen, Longqing Wen, Jun TI The first phylogenetic analysis of Tetrastigma (Miq.) Planch., the host of Rafflesiaceae SO TAXON LA English DT Article DE phylogeny; plastid DNA; Rafflesia; Rafflesiaceae; Tetrastigma; Vitaceae ID ANATOMICAL DEVELOPMENT; AUSTRALIAN VITACEAE; CHLOROPLAST DNA; SOUTHEAST-ASIA; RPS16 INTRON; FANGED FROGS; SEQUENCE; EVOLUTION; AMPLIFICATION; SYSTEMATICS AB Tetrastigma (Vitaceae) comprises about 95 species widely distributed throughout subtropical and tropical Asia, and extending to Australia. The genus is best known for being the host plants of Rafflesia, with the largest flower in the world, and other members of Rafflesiaceae. The phylogeny of Tetrastigma, however, remains poorly known. Four plastid markers (atpB-rbcL, psbA-trnH, trnL-trnF intergenic spacers, rps16 intron) were employed to infer the first phylogeny of Tetrastigma. Our sampling included eleven reported host species of Rafflesiaceae, being scattered in seven major clades throughout the Tetrastigma tree. A Templeton test rejected the hypothesis cola single origin of the parasite-host relationship between Rafflesiaceae and Tetrastigma. Analysis of 114 accessions representing 53 species and four varieties throughout the distributional range of the genus provided robust support for the monophyly of Tetrastigma, yet Tetrastigma was found to be nested within Cayratia. Tetrastigma subg. Palmicirrata from the Sino-Himalayan region was nested within the large and widely distributed T. subg. Tetrastigma. Two major clades (clades A and F) in our phylogeny correspond to T. sect. Tetrastigma and T. sect. Carinata of subgenus Tetrastigma, respectively. C1 [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC166, Washington, DC 20013 USA. [Chen, Pingting; Chen, Longqing] Cent China Agr Univ, Key Lab Hort Plant Biol, Minist Educ, Coll Hort & Forestry, Wuhan 430070, Peoples R China. RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC166, Washington, DC 20013 USA. EM chenlq0206@163.com; wenj@si.edu FU National Science Foundation; Smithsonian Endowment Grant Program; Small Grant Program of National Museum of Natural History of the Smithsonian Institution; John D. and Catherine T. MacArthur Foundation; College of Horticulture and Forestry of Central China Agricultural University FX We thank W.-H. Chen, J. Gerrath, Z.-L. Nic, Y. Meng, Deden Girmansyah, R. Li, H. Li, Y.-M. Shui, W.-D. Zhu, and Y.-F. Deng for help with collecting leaf material, Z.-L. Nie, H. Sun, S.-L. Zhou, Y.-M. Shui, W.-H. Chen, Nguyen Tiep Hiep, Nguyen Quang Hieu, Leng-Guan Saw, Elizabeth Widjaja, Harry Wiriadinata, Scott Hoover, Abdul Kartonegoro, Deden Girmansyah, Arief Hidayat, and Eko Walujo for facilitating field work and providing field assistance. We thank J. Hunt, R. Li, X.-W. Xu, T.-Y. Tu, Z.-L. Nie, and T.-S. Yi for laboratory assistance, and Todd Barkman, Jimmy Triplett, two anonymous reviewers, and Associate Editor Mary Endress for constructive comments on the manuscript. The study was supported by grants from the National Science Foundation (to S.R. Manchester and J. Wen), the Smithsonian Endowment Grant Program, the Small Grant Program of National Museum of Natural History of the Smithsonian Institution, and the John D. and Catherine T. MacArthur Foundation. Graduate support for P.-T. (Celia) Chen was provided by the College of Horticulture and Forestry of Central China Agricultural University. NR 79 TC 10 Z9 12 U1 3 U2 24 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 APR PY 2011 VL 60 IS 2 BP 499 EP 512 PG 14 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 750ZN UT WOS:000289587100017 ER PT J AU Brooks, RP Brinson, MM Havens, KJ Hershner, CS Rheinhardt, RD Wardrop, DH Whigham, DF Jacobs, AD Rubbo, JM AF Brooks, Robert P. Brinson, Mark M. Havens, Kirk J. Hershner, Carl S. Rheinhardt, Richard D. Wardrop, Denice H. Whigham, Dennis F. Jacobs, Amy D. Rubbo, Jennifer M. TI Proposed Hydrogeomorphic Classification for Wetlands of the Mid-Atlantic Region, USA SO WETLANDS LA English DT Article DE Estuarine wetlands; National Wetlands Inventory ID COASTAL-PLAIN; NORTH-CAROLINA; NUTRIENT DYNAMICS; HYDROLOGY; WATER; INDICATORS; RIVER; HYDROPERIOD; GENERATION; ESTUARIES AB We propose a regional classification for wetlands of the Mid-Atlantic region, USA. It combines functional characteristics recognized by the hydrogeomorphic (HGM) approach with the established classification of the National Wetland Inventory (NWI). The HGM approach supplements the NWI classification by recognizing the importance of geomorphic setting, water sources, and flow dynamics that are key to functioning wetlands. Both NWI and HGM share at their highest levels the Marine, Estuarine, and Lacustrine classes. This classification departs from the NWI system by subdividing the Palustrine system into HGM classes of Slope, Depression, and Flat. Further, the Riverine class expands to include associated Palustrine wetlands, thus recognizing the interdependency between channel and floodplain. Deepwater habitats of NWI are not included because they differ functionally. Mid-Atlantic regional subclasses recognize two subclasses each for Flat, Slope, and Marine Tidal Fringe; three subclasses for Depression; four subclasses for Lacustrine Fringe and Estuarine Tidal Fringe, and five subclasses for Riverine. Taking a similar approach in other geographic regions will better characterize wetlands for assessment and restoration. This approach was applied successfully during a regional wetlands condition assessment. We encourage additional testing by others to confirm its utility in the region. C1 [Brooks, Robert P.; Wardrop, Denice H.; Rubbo, Jennifer M.] Penn State Univ, Dept Geog, University Pk, PA 16802 USA. [Brinson, Mark M.; Rheinhardt, Richard D.] E Carolina Univ, Dept Biol, Greenville, NC USA. [Havens, Kirk J.; Hershner, Carl S.] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Jacobs, Amy D.] Div Water Resources, Delaware Dept Nat Resources & Environm Control, Dover, DE 19904 USA. RP Brooks, RP (reprint author), Penn State Univ, Dept Geog, 302 Walker Bldg, University Pk, PA 16802 USA. EM rpb2@psu.edu OI Whigham, Dennis/0000-0003-1488-820X FU U.S. Environmental Protection Agency's (USEPA) [R-82868401] FX This research has been supported by a grant from the U.S. Environmental Protection Agency's (USEPA) Science to Achieve Results (STAR) Estuarine and Great Lakes (EaGLe) program through funding to the Atlantic Slope Consortium (ASC), a broad multi-institutional group of investigators; USEPA agreement R-82868401. The field trials were supported by a USEPA grant to conduct a regional wetlands assessment, not yet published. Although the research described in this report has been funded wholly or in part by the United States Environmental Protection Agency, it has not been subjected to the Agency's required peer and policy review and, therefore, does not reflect the view of the Agency and no official endorsement should be inferred. The authors appreciate the suggestions of two anonymous reviewers. NR 86 TC 16 Z9 19 U1 2 U2 29 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 EI 1943-6246 J9 WETLANDS JI Wetlands PD APR PY 2011 VL 31 IS 2 BP 207 EP 219 DI 10.1007/s13157-011-0158-7 PG 13 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 746ZC UT WOS:000289288700002 ER PT J AU Post, JE Heaney, PJ Cho, Y AF Post, Jeffrey E. Heaney, Peter J. Cho, Yunchul TI Neutron diffraction study of hydrogen in birnessite structures SO AMERICAN MINERALOGIST LA English DT Article DE Birnessite; Rietveld; neutron; hydrogen ID SYNTHETIC NA-BIRNESSITE; X-RAY-DIFFRACTION; RIETVELD REFINEMENT; THERMAL-DECOMPOSITION; RICH BIRNESSITE; ION-EXCHANGE; MANGANESE; PARAMETERS; KMNO4; WATER AB The positions of hydrogen (deuterium) cations within the interlayer of synthetic Na- and K-bimessite samples have been determined for the first time using Rietveld analysis and Fourier difference syntheses, from time-of-flight powder neutron diffraction data. This study revealed that two symmetry-related D(H) positions are located similar to 1 angstrom above and below the midpoint between the split O interlayer sites in Na-birnessite. This result confirms our earlier interpretation that the split interlayer sites include O atoms from two symmetrically equivalent H(2)O molecules. These molecules are oriented 180 to each other, and they are pivoted about a single set of H(D) atoms positions. The interlayer H(2)O molecules in K-birnessite are oriented such that one of the H(D) atoms is pointed approximately toward the Mn octahedral layer O atoms and the other is directed approximately within the net of interlayer K/O sites. In K-bimessite, six K-O(oct) distances are shorter than 3.35 angstrom, compared with only two Na-O(oct) bond lengths in Na-bimessite, suggesting that K cations are more tightly bonded to the octahedral O atoms than are Na cations. C1 [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Cho, Yunchul] Penn State Univ, Dept Crop & Soil Sci, University Pk, PA 16802 USA. RP Post, JE (reprint author), Smithsonian Inst, Dept Mineral Sci, POB 37012, Washington, DC 20013 USA. EM postj@si.edu FU NSF [EAR07-45374]; Center for Environmental Kinetics Analysis (CEKA); NSF- and DOE-sponsored Environmental Molecular Science Institute (NSF) [CHE-0431328]; DOE FX `Funding for this research was provided by NSF grants EAR07-45374 and the Center for Environmental Kinetics Analysis (CEKA). a NSF- and DOE-sponsored Environmental Molecular Science Institute (NSF CHE-0431328). The IPNS was supported by DOE, and valuable assistance was provided with neutron diffraction experiments by James Richardson and Evan Maxey. NR 30 TC 3 Z9 3 U1 0 U2 16 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD APR PY 2011 VL 96 IS 4 BP 534 EP 540 DI 10.2138/am.2011.3629 PG 7 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 744XR UT WOS:000289129000007 ER PT J AU Kursar, TA AF Kursar, Thomas A. TI What Are the Implications of the Nagoya Protocol for Research on Biodiversity? SO BIOSCIENCE LA English DT Editorial Material ID CONSERVATION C1 [Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Kursar, Thomas A.] Smithsonian Trop Res Inst, Panama City, Panama. RP Kursar, TA (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. EM kursar@biology.utah.edu NR 6 TC 5 Z9 5 U1 0 U2 13 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 APR PY 2011 VL 61 IS 4 BP 256 EP 257 DI 10.1525/bio.2011.61.4.2 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 747KY UT WOS:000289319900007 ER PT J AU Fleishman, E Blockstein, DE Hall, JA Mascia, MB Rudd, MA Scott, JM Sutherland, WJ Bartuska, AM Brown, AG Christen, CA Clement, JP DellaSala, D Duke, CS Eaton, M Fiske, SJ Gosnell, H Haney, JC Hutchins, M Klein, ML Marqusee, J Noon, BR Nordgren, JR Orbuch, PM Powell, J Quarles, SP Saterson, KA Savitt, CC Stein, BA Webster, MS Vedder, A AF Fleishman, Erica Blockstein, David E. Hall, John A. Mascia, Michael B. Rudd, Murray A. Scott, J. Michael Sutherland, William J. Bartuska, Ann M. Brown, A. Gordon Christen, Catherine A. Clement, Joel P. DellaSala, Dominick Duke, Clifford S. Eaton, Marietta Fiske, Shirley J. Gosnell, Hannah Haney, J. Christopher Hutchins, Michael Klein, Mary L. Marqusee, Jeffrey Noon, Barry R. Nordgren, John R. Orbuch, Paul M. Powell, Jimmie Quarles, Steven P. Saterson, Kathryn A. Savitt, Charles C. Stein, Bruce A. Webster, Michael S. Vedder, Amy TI Top 40 Priorities for Science to Inform US Conservation and Management Policy SO BIOSCIENCE LA English DT Article DE conservation; decisionmakers; ecosystems; natural resource management; priority setting ID CLIMATE-CHANGE; UNITED-STATES; ENVIRONMENTAL-MANAGEMENT; ECOLOGICAL QUESTIONS; BIODIVERSITY; IDENTIFICATION; INTEGRATION; DIVERSITY; COLLAPSE; DRIVERS AB To maximize the utility of research to decisionmaking, especially given limited financial resources, scientists must set priorities for their efforts. We present a list of the top 40 high-priority, multidisciplinary research questions directed toward informing some of the most important current and future decisions about management of species, communities, and ecological processes in the United States. The questions were generated by an open, inclusive process that included personal interviews With decisionmakers, broad solicitation of research needs from scientists and policymakers, and an intensive workshop that included scientifically oriented individuals responsible for managing and developing policy related to natural resources. The process differed from previous efforts to set priorities for conservation research in its focus on the engagement of decisionmakers in addition to researchers. The research priorities emphasized the importance of addressing societal context and exploration of trade-offs among alternative policies and actions, as well as more traditional questions related to ecological processes and functions. C1 [Fleishman, Erica] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. [Blockstein, David E.] Natl Council Sci & Environm, Washington, DC USA. [Hall, John A.] US Dept Def, Strateg Environm Res & Dev Program, Environm Secur Technol Certificat Program, Arlington, VA USA. [Mascia, Michael B.] World Wildlife Fund, Conservat Sci Program, Washington, DC 20037 USA. [Rudd, Murray A.] Univ York, Dept Environm, York YO10 5DD, N Yorkshire, England. [Blockstein, David E.] Council Environm Deans & Directors, Washington, DC USA. [Scott, J. Michael] Univ Idaho, US Geol Survey, Moscow, ID 83843 USA. [Scott, J. Michael] Univ Idaho, Cooperat Fish & Wildlife Res Unit, Moscow, ID 83843 USA. [Scott, J. Michael] Univ Idaho, Dept Fish & Wildlife Resources, Moscow, ID 83843 USA. [Sutherland, William J.] Univ Cambridge, Dept Zool, Conservat Sci Grp, Cambridge CB2 1TN, England. [Bartuska, Ann M.] US Dept Agr Forest Serv Res, Washington, DC USA. [Brown, A. Gordon] US Dept Interior, Washington, DC USA. [Brown, A. Gordon] Natl Invas Species Council, Washington, DC USA. [Christen, Catherine A.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Clement, Joel P.] Wilburforce Fdn, Seattle, WA USA. [DellaSala, Dominick] Geos Inst, Ashland, OR USA. [Duke, Clifford S.] Ecol Soc Amer, Sci Programs, Washington, DC USA. [Eaton, Marietta] US Bur Land Management, Washington, DC USA. [Fiske, Shirley J.] Univ Maryland, Dept Anthropol, College Pk, MD 20742 USA. [Gosnell, Hannah] Oregon State Univ, Dept Geosci, Corvallis, OR 97331 USA. [Haney, J. Christopher] Defenders Wildlife, Washington, DC USA. [Hutchins, Michael] Wildlife Soc, Bethesda, MD USA. [Klein, Mary L.] NatureServe, Arlington, VA USA. [Marqusee, Jeffrey] US Dept Def, Environm Secur Technol Certificat, Strateg Environm Res & Dev Program, Arlington, VA USA. [Noon, Barry R.] Colorado State Univ, Dept Fish Wildlife & Conservat Biol, Ft Collins, CO 80523 USA. [Nordgren, John R.] Kresge Fdn, Troy, MI USA. [Orbuch, Paul M.] Orbuch Consulting LLC, Boulder, CO USA. [Powell, Jimmie] Nature Conservancy, Arlington, VA USA. [Quarles, Steven P.] Crowell & Corals Moring LLC, Environm & Nat Resources Grp, Washington, DC USA. [Saterson, Kathryn A.] US EPA, Natl Hlth & Environm Effects Res Lab, Res Triangle Pk, NC 27711 USA. [Savitt, Charles C.] Isl Press, Washington, DC USA. [Stein, Bruce A.] Natl Wildlife Federat, Wildlife Conservat & Global Warming, Washington, DC USA. [Vedder, Amy] Wilderness Soc, Washington, DC USA. [Webster, Michael S.] Gordon & Betty Moore Fdn, Palo Alto, CA USA. RP Fleishman, E (reprint author), Univ Calif Davis, John Muir Inst Environm, Davis, CA 95616 USA. EM efleishman@ucdavis.edu RI Sutherland, William/B-1291-2013; Rudd, Murray/C-1244-2009; OI Rudd, Murray/0000-0001-9533-5070; Mascia, Michael/0000-0002-9874-9778; Sutherland, William/0000-0002-6498-0437 FU Kresge Foundation [239855]; World Wildlife Fund-US FX This work was supported by Kresge Foundation grant 239855 to the University of California, Santa Barbara. Thanks to World Wildlife Fund-US for hosting the workshop. We thank all individuals who contributed questions and three anonymous reviewers for comments that improved the manuscript. Affiliations of authors are provided for ease of identification only. No content in this manuscript implies endorsement by the US government. NR 63 TC 59 Z9 60 U1 9 U2 73 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 APR PY 2011 VL 61 IS 4 BP 290 EP 300 DI 10.1525/bio.2011.61.4.9 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 747KY UT WOS:000289319900014 ER PT J AU Fahr, J Kalko, EKV AF Fahr, Jakob Kalko, Elisabeth K. V. TI Biome transitions as centres of diversity: habitat heterogeneity and diversity patterns of West African bat assemblages across spatial scales SO ECOGRAPHY LA English DT Review ID BIRD SPECIES-DIVERSITY; BETA-DIVERSITY; GAMMA-DIVERSITY; GLOBAL PATTERNS; IVORY-COAST; RAIN-FOREST; LATITUDINAL GRADIENTS; ECHOLOCATION CALLS; INSECTIVOROUS BATS; REGIONAL PROCESSES AB It is widely accepted that species diversity is contingent upon the spatial scale used to analyze patterns and processes. Recent studies using coarse sampling grains over large extents have contributed much to our understanding of factors driving global diversity patterns. This advance is largely unmatched on the level of local to landscape scales despite being critical for our understanding of functional relationships across spatial scales. In our study on West African bat assemblages we employed a spatially explicit and nested design covering local to regional scales. Specifically, we analyzed diversity patterns in two contrasting, largely undisturbed landscapes, comprising a rainforest area and a forest-savanna mosaic in Ivory Coast, West Africa. We employed additive partitioning, rarefaction, and species richness estimation to show that bat diversity increased significantly with habitat heterogeneity on the landscape scale through the effects of beta diversity. Within the extent of our study areas, habitat type rather than geographic distance explained assemblage composition across spatial scales. Null models showed structure of functional groups to be partly filtered on local scales through the effects of vegetation density while on the landscape scale both assemblages represented random draws from regional species pools. We present a mixture model that combines the effects of habitat heterogeneity and complexity on species richness along a biome transect, predicting a unimodal rather than a monotonic relationship with environmental variables related to water. The bat assemblages of our study by far exceed previous figures of species richness in Africa, and refute the notion of low species richness of Afrotropical bat assemblages, which appears to be based largely on sampling biases. Biome transitions should receive increased attention in conservation strategies aiming at the maintenance of ecological and evolutionary processes. C1 [Fahr, Jakob; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, DE-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Fahr, J (reprint author), Univ Ulm, Inst Expt Ecol, DE-89069 Ulm, Germany. EM jakob.fahr@gmail.com RI Fahr, Jakob/E-8831-2012 OI Fahr, Jakob/0000-0002-9174-1204 FU Ministere re de l'Agriculture et des Ressources Animales; Ministere de l'Enseignement Superieur et de la Recherche Scientifique; Republique de Cote d'Ivoire; German Federal Ministry of Education and Research (BMBF) [01LC0017, 01LC0411, 01LC0617E1]; Landesgraduiertenforderung BW; German Academic Exchange Service (DAAD) FX We greatly appreciate the contribution of Stefan Pettersson, Njikoha Ebigbo and Katja Soer to the data set analyzed here. We thank Kouakou Kouame, Koffi Kouadio and Kouadio Kouakou (all CNP) and Georges Gbamlin (TNP) for their dedicated assistance in the field. Vital logistical support was provided by K. Eduard Linsenmair, Frauke Fischer and the employees of the "Projet Biodiversite" at CNP, and by the "Centre de Recherche en Ecologie", the "Projet Autonome pour la Conservation du Parc National de Tai", and the "Tai" Monkey Project" at TNP. Research permits to work in CNP and TNP were kindly granted by the "Ministere re de l'Agriculture et des Ressources Animales" and the "Ministere de l'Enseignement Superieur et de la Recherche Scientifique", Republique de Cote d'Ivoire. Dieter Kock, Senckenberg Museum Frankfurt, offered invaluable help with species identification. Thomas Crist, Lou Jost, Martin Pfeiffer, Erica Sampaio and Joseph Veech helped in various ways with the development and interpretation of our analyses and in shaping our ideas. We appreciate general support by Hans-Ulrich Schnitzler and Mark-Oliver Rodel. This is a contribution of the BIOTA program, funded by the German Federal Ministry of Education and Research (BMBF, project 01LC0017, 01LC0411 and 01LC0617E1). We acknowledge additional funding by the Landesgraduiertenforderung BW and the German Academic Exchange Service (DAAD). Douglas Kelt, Egbert Leigh, Christoph Meyer and three reviewers helped to improve previous versions of the manuscript. NR 102 TC 31 Z9 31 U1 2 U2 68 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0906-7590 J9 ECOGRAPHY JI Ecography PD APR PY 2011 VL 34 IS 2 BP 177 EP 195 DI 10.1111/j.1600-0587.2010.05510.x PG 19 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 745EZ UT WOS:000289150000001 ER PT J AU Maloney, KO Munguia, P AF Maloney, Kelly O. Munguia, Pablo TI Distance decay of similarity in temperate aquatic communities: effects of environmental transition zones, distance measure, and life histories SO ECOGRAPHY LA English DT Article ID REGIONAL SPECIES RICHNESS; STREAM FISH ASSEMBLAGES; UNITED-STATES; HABITAT; ECOREGIONS; PATTERNS; DISPERSAL; ECOLOGY; RIVER; MACROINVERTEBRATES AB The decay of community similarity with distance (distance decay) is reported for many taxa in a variety of geographic settings. However, the importance of scale, distance measure, ecoregions, and ecological transition zones to distance decay has not been thoroughly examined. The goal of our study was to test the effects of these factors on distance decay in two freshwater assemblages (benthic macroinvertebrates and fish) with differing dispersal abilities in small streams within the Patuxent River basin, Maryland, USA. The Patuxent basin contains a geologic Fall Line, an ecological transition zone separating the two main regions of the basin. For both assemblages, we examined distance decay in similarity at several extents: entire Patuxent, Piedmont sub-region, and Plains sub-region using both linear geographic and stream network distances. Decay patterns were observed across all extents and distances. At the Patuxent extent decay rates differed between linear and stream distance only for macroinvertebrates (linear > stream); with both distance measures, similarity in fish decayed faster than similarity in macroinvertebrates. Within the Plains, decay rates for macroinvertebrates were lower than at the Patuxent for both distance measures; no difference in decay rates for this assemblage were detected in the Piedmont. Decay rates of similarity for fish only differed (lower) from rates at the Patuxent when examined at the Piedmont extent with stream distance. Similarity for the subset of sites that were located in separate ecoregions decayed at a slower rate than similarity for the entire data set only for macroinvertebrates with linear distance, suggesting a weak effect of the transition zone on distance decay. Together, these results suggest multiple factors contribute to the distance decay pattern and therefore regional diversity patterns, suggesting conjoint examination of these factors will further our understanding of the mechanisms governing regional diversity patterns. C1 [Maloney, Kelly O.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Munguia, Pablo] Univ Texas Austin, Inst Marine Sci, Port Aransas, TX 78373 USA. RP Maloney, KO (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA. EM maloneyk@si.edu RI Munguia, Pablo/D-8653-2012; OI Munguia, Pablo/0000-0002-9900-2123 FU Smithsonian Post-Doctoral Fellowship; USEPA National Center for Environmental Research (NCER) [R831369] FX We thank the Maryland Dept of Natural Resources and Ryan King, Baylor Univ., for providing data on benthic macroinvertebrates and Stephen Prince, Univ. of Maryland, and Scott Goetz, Woods Hole Research Center, for providing land cover data. We also acknowledge Lori Davias, Eric Lind, Donald Weller and Kathy Bailey-Boomer (SERC), and Helmut Hillebrand and three anonymous reviewers for instructive comments on the manuscript. Funding for this work was provided by the Smithsonian Post-Doctoral Fellowship Program and USEPA National Center for Environmental Research (NCER) Science to Achieve Results (STAR) grant #R831369: A Watershed Classification System for Improved Monitoring and Restoration: Landscape Indicators of Watershed Impairment. Although the research described in this article has been funded by the United States Environmental Protection Agency, it has not been subjected to the Agency's required peer and policy review and therefore does not necessarily reflect the views of the Agency and no official endorsement should be inferred. NR 58 TC 25 Z9 25 U1 1 U2 34 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0906-7590 J9 ECOGRAPHY JI Ecography PD APR PY 2011 VL 34 IS 2 BP 287 EP 295 DI 10.1111/j.1600-0587.2010.06518.x PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 745EZ UT WOS:000289150000011 ER PT J AU Nami, HG AF Nami, Hugo G. TI New detailed paleosecular variation record at Santa Lucia archaeological site (Corrientes province, northeastern Argentina) SO GEOFISICA INTERNACIONAL LA English DT Article DE paleomagnetism; paleosecular variations; Holocene; Archaeology; South America; Argentina ID SOUTH ARGENTINA; SEDIMENTS; EXCURSION AB Paleomagnetic data from a sedimentary section from Santa Lucia archaeological site, Corrientes province (Northeastern Argentina) are reported. Natural remanent magnetization obtained from 74 oriented cores showed normal and intermediate magnetic remanence with negative and positive low inclination values during the Late Holocene. Characteristic remanent magnetization was determined by progressive demagnetization using the AF method. Virtual geomagnetic poles show some agreement with those registered during the terminal Pleistocene and Holocene in other sites from the southern cone of South America. Palaeomagnetic poles for other contemporaneous sites from northeastern Argentina fall some similar to 3-15 degrees away from the Earth's rotation's axis. C1 [Nami, Hugo G.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Nami, Hugo G.] Univ Buenos Aires, Inst Geofis Daniel A Valencio, CONICET, Dept Ciencias Geol,Fac Ciencias Exactas Fis & Nat, Buenos Aires, DF, Argentina. RP Nami, HG (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM hgnami@fulbrightmail.org NR 29 TC 1 Z9 1 U1 0 U2 0 PU INST GEOPHYSICS UNAM PI MEXICO PA APDO POSTAL 22-118, DEL TLALPAN, MEXICO, 14000 D F, MEXICO SN 0016-7169 J9 GEOFIS INT JI Geofis. Int. PD APR-JUN PY 2011 VL 50 IS 2 BP 163 EP 175 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 746BU UT WOS:000289217400003 ER PT J AU Martinez-Alonso, S Mellon, MT Banks, ME Keszthelyi, LP McEwen, AS AF Martinez-Alonso, Sara Mellon, Michael T. Banks, Maria E. Keszthelyi, Laszlo P. McEwen, Alfred S. CA HiRISE Team TI Evidence of volcanic and glacial activity in Chryse and Acidalia Planitiae, Mars SO ICARUS LA English DT Article DE Geological processes; Mars; Mars, Surface ID POLAR LAYERED DEPOSITS; GENERAL-CIRCULATION MODEL; ORBITER LASER ALTIMETER; SUBGLACIAL VOLCANOS; NORTHERN PLAINS; GLOBAL SURVEYOR; GROUND ICE; INTRAGLACIAL VOLCANOES; PALAGONITE-FORMATION; THERMAL INERTIA AB Chryse and Acidalia Planitiae show numerous examples of enigmatic landforms previously interpreted to have been influenced by a water/ice-rich geologic history. These landforms include giant polygons bounded by kilometer-scale arcuate troughs, bright pitted mounds, and mesa-like features. To investigate the significance of the last we have analyzed in detail the region between 60 degrees N, 290 degrees E and 10 degrees N, 360 degrees E utilizing HiRISE (High Resolution Imaging Science Experiment) images as well as regional-scale data for context. The mesas may be analogous to terrestrial tuyas (emergent sub-ice volcanoes), although definitive proof has not been identified. We also report on a blocky unit and associated landforms (drumlins, eskers, inverted valleys, kettle holes) consistent with ice-emplaced volcanic or volcano-sedimentary flows. The spatial association between tuya-like mesas, ice-emplaced flows, and further possible evidence of volcanism (deflated flow fronts, volcanic vents, columnar jointing, rootless cones), and an extensive fluid-rich substratum (giant polygons, bright mounds, rampart craters), allows for the possibility of glaciovolcanic activity in the region. Landforms indicative of glacial activity on Chryse/Acidalia suggest a paleoclimatic environment remarkably different from today's. Climate changes on Mars (driven by orbital/obliquity changes) or giant outflow channel activity could have resulted in ice-sheet-related landforms far from the current polar caps. (C) 2011 Elsevier Inc. All rights reserved. C1 [Martinez-Alonso, Sara] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Mellon, Michael T.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Banks, Maria E.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Keszthelyi, Laszlo P.] US Geol Survey, Flagstaff, AZ 86001 USA. [McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Martinez-Alonso, S (reprint author), Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. EM martinas@colorado.edu RI Martinez-Alonso, Sara/D-8594-2011; Mellon, Michael/C-3456-2016 OI Martinez-Alonso, Sara/0000-0001-5185-8670; FU NASA FX We express our appreciation to the science and operations teams responsible for the success of the MRO mission and in particular to the HiRISE team. We thank Tammy Becker for making available her ISIS script for building HiRISE anaglyphs and Bethany Ehlmann for spectral processing of the CRISM data. Thanks to Moses Milazzo for sharing his expertise on Martian columnar jointing and to Larry Crumpler, Ginny Gulick, and Bruce Kindel for their comments early in the project. This paper benefited greatly from comments by the reviewers (Anonymous, Ernst Hauber, and Thor Thordarson) and the editor (Ken Herkenhoff). SMA recognizes support from NASA's Mars Data Analysis and MRO programs. NR 155 TC 12 Z9 12 U1 3 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD APR PY 2011 VL 212 IS 2 BP 597 EP 621 DI 10.1016/j.icarus.2011.01.004 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745PM UT WOS:000289178100013 ER PT J AU Hong, T AF Hong, Terry TI The Lake 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 APR 1 PY 2011 VL 136 IS 6 BP 86 EP 86 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 746EJ UT WOS:000289225200064 ER PT J AU Balogh, ML Mazzotta, P Bower, RG Eke, V Bourdin, H Lu, T Theuns, T AF Balogh, Michael L. Mazzotta, Pasquale Bower, Richard G. Eke, Vince Bourdin, Herve Lu, Ting Theuns, Tom TI The stellar and hot gas content of low-mass galaxy clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general ID K-BAND PROPERTIES; LUMINOSITY FUNCTION; INTRACLUSTER LIGHT; ABUNDANCE PROFILES; SCALING RELATIONS; REDSHIFT SURVEY; XMM-NEWTON; SAMPLE; TEMPERATURE; CHANDRA AB We analyse the stellar and hot gas content of 18 nearby, low-mass galaxy clusters, detected in redshift space and selected to have a dynamical mass 3 x 1014 < M/M-circle dot < 6 x 1014 (h = 0.7), as measured from the 2dF Galaxy Redshift Survey. We combine X-ray measurements from both Chandra and XMM with ground-based near-infrared observations from CTIO, Anglo-Australian Telescope and Canada-France-Hawaii Telescope to compare the mass in hot gas and stars to the dynamical mass and state of the clusters. Only 13 of the clusters are detected in X-ray emission, and for these systems we find that a range of 7-20 per cent of their baryonic mass, and < 3 per cent of their dynamical mass, is detected in starlight, similar to what is observed in more massive clusters. In contrast, the five undetected clusters are underluminous in X-ray emission, by up to a factor of 10, given their stellar mass. Although the velocity distribution of cluster members in these systems is indistinguishable from a Gaussian, all show subtle signs of being unrelaxed: either they lack a central, dominant galaxy, or the bright galaxy distribution is less concentrated and/or more elongated than the rest of the sample. Thus we conclude that low-mass clusters and groups selected from the velocity distribution of their galaxies exhibit a dichotomy in their hot gas properties. Either they are detected in X-ray, in which case they generally lie on the usual scaling relations, or they are completely undetected in X-ray emission. The non-detections may be partly related to the apparently young dynamical state of the clusters, but it remains a distinct possibility that some of these systems are exceptionally devoid of hot emitting gas as the result of its expulsion or rarefaction. C1 [Balogh, Michael L.; Lu, Ting] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Mazzotta, Pasquale; Bourdin, Herve] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Mazzotta, Pasquale] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bower, Richard G.; Eke, Vince; Theuns, Tom] Univ Durham, Dept Phys, Sci Labs, Durham DH1 3LE, England. [Theuns, Tom] Univ Antwerp, Dept Phys, B-2020 Antwerp, Belgium. RP Balogh, ML (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. EM mbalogh@uwaterloo.ca RI Mazzotta, Pasquale/B-1225-2016 OI Mazzotta, Pasquale/0000-0002-5411-1748 FU National Aeronautics and Space Administration [NNX09AP45G, NNX09AP36G]; NSERC; [ASI-INAF I/023/05/0]; [ASI-INAF I/088/06/0] FX We thank the referee for a thorough and helpful report, and Stefano Andreon for pointing out a few errors in the original text. MLB and TL would like to thank David Gilbank and Sean McGee for many useful discussions about this work and comments on the draft. MLB would like to thank to Patrice Bouchet for carrying out our CTIO observations when we were unable to be present for our run. We thank Terapix, in particular Patrick Hudelot, for their help in reducing CFHT WIRCAM data. MLB would also like to thank Sean McGee for calibrating our AAT data using ASTROMETRY.NET. This research has made use of the NASA/IPAC Extragalactic Data base (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research is supported by an NSERC Discovery grant to MLB. PM and HB acknowledge support by contract ASI-INAF I/023/05/0, ASI-INAF I/088/06/0, NASA grants NNX09AP45G and NNX09AP36G. NR 61 TC 20 Z9 21 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 APR PY 2011 VL 412 IS 2 BP 947 EP 959 DI 10.1111/j.1365-2966.2010.17957.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900017 ER PT J AU Zu, Y Weinberg, DH Dave, R Fardal, M Katz, N Keres, D Oppenheimer, BD AF Zu, Ying Weinberg, David H. Dave, Romeel Fardal, Mark Katz, Neal Keres, Dusan Oppenheimer, Benjamin D. TI Intergalactic dust extinction in hydrodynamic cosmological simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; intergalactic medium ID DIGITAL-SKY-SURVEY; MASS-METALLICITY RELATION; LAMBDA-CDM UNIVERSE; TO-GAS RATIO; GALAXY-MASS; GALACTIC OUTFLOWS; FEEDBACK; HALO; ENRICHMENT; LUMINOSITY AB Recently Menard et al. (hereafter MSFR) detected a subtle but systematic change in the mean colour of quasars as a function of their projected separation from foreground galaxies, extending to comoving separations of similar to 10 h-1 Mpc, which they interpret as a signature of reddening by intergalactic dust. We present theoretical models of this remarkable observation, using smoothed particle hydrodynamic cosmological simulations of a (50 h-1 Mpc)3 volume. Our primary model uses a simulation with galactic winds and assumes that dust traces the intergalactic metals. The predicted galaxy-dust correlation function is similar in form to the galaxy-mass correlation function, and reproducing the MSFR data requires a dust-to-metal mass ratio of 0.24, about half the value in the Galactic interstellar medium (ISM). Roughly half of the reddening arises in dust that is more than 100 h-1 kpc from the nearest massive galaxy. We also examine a simulation with no galactic winds, which predicts a much smaller fraction of intergalactic metals (3 per cent versus 35 per cent) and therefore requires an unphysical dust-to-metal ratio of 2.18 to reproduce the MSFR data. In both models, the signal is dominated by sightlines with E(g - i) = 0.001-0.1. The no-wind simulation can be reconciled with the data if we also allow reddening to arise in galaxies up to several x 1010 M-circle dot. The wind model predicts a mean visual extinction of << A(V)>> approximate to 0.0133 mag out to z = 0.5, with a sightline-to-sightline dispersion similar to the mean, which could be significant for future supernova cosmology studies. Reproducing the MSFR results in these simulations requires that a large fraction of ISM dust survive its expulsion from galaxies and its residence in the intergalactic medium. Future observational studies that provide higher precision and measure the dependence on galaxy type and environment will allow detailed tests for models of enriched galactic outflows and the survival of intergalactic dust. C1 [Zu, Ying; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Weinberg, David H.] Inst Adv Study, Princeton, NJ 08540 USA. [Dave, Romeel] Univ Arizona, Astron Dept, Tucson, AZ 85721 USA. [Fardal, Mark; Katz, Neal] Univ Massachusetts, Dept Phys & Astron, Amherst, MA USA. [Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Oppenheimer, Benjamin D.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Zu, Y (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM yingzu@astronomy.ohio-state.edu OI Zu, Ying/0000-0001-6966-6925 FU NSF [AST-0707985]; Ohio State University; AMIAS membership at the IAS; University of Massachusetts; Harvard University FX We thank Charlie Conroy, Bruce Draine, Brice Menard, Ryan Scranton, Masataka Fukugita and Gordon Richards for helpful discussions. We thank Vimal Simha for investigating the temperature distribution of wind particles as a function of halo mass (see Section 4). This work was supported in part by NSF Grant AST-0707985 and by an Ohio State University Fellowship to YZ. DHW, MF and DK gratefully acknowledge support from, respectively, an AMIAS membership at the IAS, the FCAD Fellows Program at the University of Massachusetts and Harvard University. NR 46 TC 10 Z9 10 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 APR PY 2011 VL 412 IS 2 BP 1059 EP 1069 DI 10.1111/j.1365-2966.2010.17976.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900026 ER PT J AU Mahajan, S Haines, CP Raychaudhury, S AF Mahajan, Smriti Haines, Chris P. Raychaudhury, Somak TI The evolution of dwarf galaxies in the Coma supercluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual: Coma; galaxies: dwarf; galaxies: evolution; galaxies: star formation ID DIGITAL SKY SURVEY; STAR-FORMATION HISTORIES; DISTANT CLUSTERS; STELLAR POPULATIONS; VIRGO CLUSTER; E+A GALAXIES; ORIGIN; GIANT; SPECTROSCOPY; ENVIRONMENT AB We employ spectroscopic and photometric data from the Sloan Digital Sky Survey Data Release 7, in a 500-deg2 region, to understand the evolution of dwarf [similar to(M* + 2) < M-z < M* + 4] galaxies in the Coma supercluster (z = 0.023). We show that in the Coma supercluster, the red dwarf galaxies are mostly concentrated in the dense cores of the Coma and Abell 1367 clusters, and in the galaxy groups embedded in the filament connecting them. The post-starburst (k+A) dwarfs, however, are found in the infall regions of the Coma and Abell 1367 clusters, and occasionally in galaxy groups embedded along the filament, suggesting that strong velocity fields prevalent in the vicinity of deep potential wells may be closely related to the mechanism(s) leading to the post-starburst phase in dwarf galaxies. Moreover, the blue colour of some k+A dwarfs in the Coma cluster, found within its virial radius, suggests that the star formation in these galaxies was quenched very rapidly in the last 500 Myr. More than 60 per cent of all red dwarf galaxies in the supercluster have 0-3 A of H delta in absorption, which suggests that a major episode of star formation occurred in a non-negligible fraction of these galaxies, ending within the last Gyr, allowing them to move to the red sequence. The distribution of the blue dwarf galaxies in the Coma supercluster is bimodal in the EW(H alpha)-EW(H delta) plane, where EW represents equivalent width, with one population having very high emission in H alpha and some emission in H delta. A subpopulation of blue dwarfs is coincident with the red dwarfs in the EW(H alpha)-EW(H delta) plane, showing absorption in H delta and relatively lower emission in H alpha. We suggest that a large fraction of the latter population represents the progenitors of the passive dwarf galaxies that are abundantly found in the cores of low-redshift rich clusters, such as Coma. C1 [Mahajan, Smriti; Haines, Chris P.; Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Mahajan, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sm@star.sr.bham.ac.uk RI Mahajan, Smriti/D-8902-2013; OI Haines, Christopher/0000-0002-8814-8960 FU Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; ORSAS, UK; University of Birmingham FX This research has made use of the SAO/NASA Astrophysics Data System and the NED. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. SM is supported by grants from the ORSAS, UK, and the University of Birmingham. We thank the anonymous referee for constructive comments, which have greatly helped in improving this paper. NR 36 TC 10 Z9 10 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 APR PY 2011 VL 412 IS 2 BP 1098 EP 1104 DI 10.1111/j.1365-2966.2010.17977.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900029 ER PT J AU Molenda-Zakowicz, J Latham, DW Catanzaro, G Frasca, A Quinn, SN AF Molenda-Zakowicz, J. Latham, D. W. Catanzaro, G. Frasca, A. Quinn, S. N. TI Characterizing Kepler asteroseismic targets star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE space vehicles; stars: abundances; binaries: spectroscopic; stars: fundamental parameters ID PROPER-MOTION STARS; SOLAR-TYPE STARS; VELOCITY STANDARD STARS; ELODIE ECHELLE SPECTRA; MAIN-SEQUENCE STARS; METAL-POOR STARS; PARAMETERS T-EFF; ATMOSPHERIC PARAMETERS; SPECTROSCOPIC BINARIES; RADIAL-VELOCITIES AB Stellar structure and evolution can be studied in great detail by asteroseismic methods, provided data of high precision are available. We determine the effective temperature (T-eff), surface gravity (log g), metallicity and the projected rotational velocity (v sin i) of 44 Kepler asteroseismic targets using our high-resolution (R > 20 000) spectroscopic observations; these parameters will then be used to compute asteroseismic models of these stars and to interpret the Kepler light curves. We use the method of cross-correlation to measure the radial velocity (RV) of our targets, while atmospheric parameters are derived using the rotfit code and spectral synthesis method. We discover three double-lined spectroscopic binaries, HIP 94924, HIP 95115 and HIP 97321 - for the last system, we provide the orbital solution, and we report two suspected single-lined spectroscopic binaries, HIP 94112 and HIP 96062. For all stars from our sample we derive RV, v sin i, T-eff, log g and metallicity, and for six stars, we perform a detailed abundance analysis. A spectral classification is done for 33 targets. Finally, we show that the early-type star HIP 94472 is rotating slowly (v sin i = 13 km s-1) and we confirm its classification to the Am spectral type which makes it an interesting and promising target for asteroseismic modelling. The comparison of the results reported in this paper with the information in the Kepler Input Catalogue (KIC) shows an urgent need for verification and refinement of the atmospheric parameters listed in the KIC. That refinement is crucial for making a full use of the data delivered by Kepler and can be achieved only by a detailed ground-based study. C1 [Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Latham, D. W.; Quinn, S. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Catanzaro, G.; Frasca, A.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. RP Molenda-Zakowicz, J (reprint author), Univ Wroclaw, Astron Inst, Ul Kopernika 11, PL-51622 Wroclaw, Poland. EM molenda@astro.uni.wroc.pl OI Catanzaro, Giovanni/0000-0003-4337-8612; Frasca, Antonio/0000-0002-0474-0896 FU Kepler mission [NCC2-1390]; Italian Ministero dell'Istruzione, Universita e Ricerca (MIUR); Polish MNiSW [N203 014 31/2650] FX This work has been partly supported by Kepler mission under cooperation agreement NCC2-1390 (DWL, PI), the Italian Ministero dell'Istruzione, Universita e Ricerca (MIUR) and the Polish MNiSW grant N203 014 31/2650 which are gratefully acknowledged. NR 68 TC 21 Z9 21 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 APR PY 2011 VL 412 IS 2 BP 1210 EP 1220 DI 10.1111/j.1365-2966.2010.17978.x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900039 ER PT J AU Zunckel, C Gott, JR Lunnan, R AF Zunckel, Caroline Gott, J. Richard, III Lunnan, Ragnhild TI Using the topology of large-scale structure to constrain dark energy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dark energy; distance scale; large-scale structure of Universe ID HUBBLE-SPACE-TELESCOPE; MICROWAVE BACKGROUND ANISOTROPIES; DIGITAL SKY SURVEY; ACCELERATING UNIVERSE; GENUS TOPOLOGY; IA SUPERNOVAE; DATA SET; DISCOVERIES; EVOLUTION; CONSTANT AB The use of standard rulers, such as the scale of the baryonic acoustic oscillations (BAOs), has become one of the more powerful techniques employed in Cosmology to probe the entity driving the accelerating expansion of the Universe. In this paper, the topology of large-scale structure (LSS) is used as one such standard ruler to study mysterious 'dark energy'. By following the redshift evolution of the clustering of luminous red galaxies as measured by their 3D topology (counting structures in the cosmic web), we can chart the expansion rate and extract information about the equation of state of dark energy. Using the technique first introduced in Park & Kim, we evaluate the constraints that can be achieved using 3D topology measurements from next-generation LSS surveys, such as the Baryonic Oscillation Spectroscopic Survey. In conjunction with the information that will be available from the Planck satellite, we find a single topology measurement on three different scales is capable of constraining a single dark energy parameter to within 5-10 per cent when dynamics are permitted. This offers an alternative use of the data available from redshift surveys and serves as a cross-check for BAO studies. C1 [Zunckel, Caroline; Gott, J. Richard, III] Princeton Univ, Dept Astrophys, Princeton, NJ 08544 USA. [Zunckel, Caroline] Univ Kwazulu Natal, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Lunnan, Ragnhild] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zunckel, C (reprint author), Princeton Univ, Dept Astrophys, Peyton Hall,4 Ivy Lane, Princeton, NJ 08544 USA. EM caroline.zunckel@gmail.com OI Lunnan, Ragnhild/0000-0001-9454-4639 FU NRF/DST (SA); National Science Foundation (USA) [PIRE-0507768] FX The authors would like to acknowledge Changbom Park for suggesting this collaboration and Young-Rae Kim for providing the theoretical curves in Fig. 1 based on the work in Park & Kim (2009). Thanks are due to Juhan Kim for providing the initial density field of the Horizon Run Simulation. We also acknowledge the Korean Institute for Advanced Study for providing computing resources (KIAS linux cluster system, QUEST) for this work. CZ is funded by an NRF/DST (SA) Innovation Fellowship and a National Science Foundation (USA) fellowship under grant PIRE-0507768. NR 39 TC 9 Z9 9 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 APR PY 2011 VL 412 IS 2 BP 1401 EP 1408 DI 10.1111/j.1365-2966.2010.18015.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737DV UT WOS:000288549900057 ER PT J AU Degenaar, N Wolff, MT Ray, PS Wood, KS Homan, J Lewin, WHG Jonker, PG Cackett, EM Miller, JM Brown, EF Wijnands, R AF Degenaar, N. Wolff, M. T. Ray, P. S. Wood, K. S. Homan, J. Lewin, W. H. G. Jonker, P. G. Cackett, E. M. Miller, J. M. Brown, E. F. Wijnands, R. TI Further X-ray observations of EXO 0748-676 in quiescence: evidence for a cooling neutron star crust SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion,accretion discs; binaries: eclipsing; stars: individual: EXO 0748-676; stars: neutron; X-rays: binaries ID XMM-NEWTON OBSERVATIONS; PHOTON IMAGING CAMERA; LIGHT CURVES; CEN X-4; TRANSIENT KS-1731-260; CHANDRA OBSERVATION; TIMING-EXPLORER; MASS; EMISSION; MXB-1659-29 AB In late 2008, the quasi-persistent neutron star X-ray transient and eclipsing binary EXO 0748-676 started a transition from outburst to quiescence, after it actively accreted for more than 24 yr. In a previous work, we discussed Chandra and Swift observations obtained during the first 5 months of this transition. Here, we report on further X-ray observations of EXO 0748-676, extending the quiescent monitoring to 1.6 yr. Chandra and XMM-Newton data reveal quiescent X-ray spectra composed of a soft, thermal component that is well fitted by a neutron star atmosphere model. An additional hard power-law tail is detected that changes non-monotonically over time, contributing between 4 and 20 per cent to the total unabsorbed 0.5-10 keV flux. The combined set of Chandra, XMM-Newton and Swift data reveals that the thermal bolometric luminosity fades from similar to 1 x 1034 to 6 x 1033 (D/7.4 kpc)2 erg s -1, whereas the inferred neutron star effective temperature decreases from similar to 124 to 109 eV. We interpret the observed decay as cooling of the neutron star crust and show that the fractional quiescent temperature change of EXO 0748-676 is markedly smaller than observed for three other neutron star X-ray binaries that underwent prolonged accretion outbursts. C1 [Degenaar, N.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Wolff, M. T.; Ray, P. S.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Homan, J.; Lewin, W. H. G.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cackett, E. M.; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48105 USA. [Brown, E. F.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Degenaar, N (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM degenaar@uva.nl RI Brown, Edward/F-1721-2011; OI Brown, Edward/0000-0003-3806-5339; Ray, Paul/0000-0002-5297-5278 FU Netherlands Organisation for Scientific Research (NWO); NASA; Chandra grant [GO8-9045X] FX This work was supported by the Netherlands Organisation for Scientific Research (NWO) and made use of the Swift public data archive. We acknowledge Swift PI N. Gehrels and the Swift planning team for their help in carrying out the ToO campaign. EMC was supported by NASA through the Chandra Fellowship Program. MTW, PSR and KSW acknowledge the United States Office of Naval Research. JH and WHGL acknowledge support from Chandra grant GO8-9045X. NR 67 TC 34 Z9 34 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 APR PY 2011 VL 412 IS 3 BP 1409 EP 1418 DI 10.1111/j.1365-2966.2010.17562.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100001 ER PT J AU Leaman, J Li, WD Chornock, R Filippenko, AV AF Leaman, Jesse Li, Weidong Chornock, Ryan Filippenko, Alexei V. TI Nearby supernova rates from the Lick Observatory Supernova Search - I. The methods and data base SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE surveys; supernovae: general; galaxies: evolution ID CORE-COLLAPSE SUPERNOVAE; AUTOMATIC IMAGING TELESCOPE; HUBBLE-SPACE-TELESCOPE; GAMMA-RAY BURSTS; IA SUPERNOVAE; HOST GALAXIES; RELATIVE FREQUENCIES; STAR-FORMATION; HIGH-REDSHIFT; MASSIVE STAR AB This is the first paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search. We have obtained 2.3 million observations of 14 882 sample galaxies over an interval of 11 years (1998 March to 2008 December). We considered 1036 SNe detected in our sample and used an optimal subsample of 726 SNe (274 Type Ia SNe, 116 Type Ibc SNe and Type II 324 SNe) to determine our SN rates. This is the largest and most homogeneous set of nearby SNe ever assembled for this purpose, and ours is the first local SN rate analysis based on CCD imaging and modern image-subtraction techniques. In this paper, we lay the foundation of the study. We derive the recipe for the control-time calculation for SNe with a known luminosity function and provide details on the construction of the galaxy and SN samples used in the calculations. Compared with a complete volume-limited galaxy sample, our sample has a deficit of low-luminosity galaxies but still provides enough statistics for a reliable rate calculation. There is a strong Malmquist bias, so the average size (luminosity or mass) of the galaxies increases monotonically with distance, and this trend is used to showcase a correlation between SN rates and galaxy sizes. Very few core-collapse SNe are found in early-type galaxies, providing strong constraints on the amount of recent star formation within these galaxies. The small average observation interval (similar to 9 d) of our survey ensures that our control-time calculations can tolerate a reasonable amount of uncertainty in the luminosity functions of SNe. We perform Monte Carlo simulations to determine the limiting magnitude of each image and the SN detection efficiency as a function of galaxy Hubble type. The limiting magnitude and the detection efficiency, together with the luminosity function derived from a complete sample of very nearby SNe in Paper II, will be used to calculate the control time and the SN rates in Paper III. C1 [Leaman, Jesse; Li, Weidong; Chornock, Ryan; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Leaman, Jesse] NASA, Ames Res Ctr, Mountain View, CA 94043 USA. [Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Leaman, J (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM jleaman@astro.berkeley.edu; wli@astro.berkeley.edu; rchornock@cfa.harvard.edu; alex@astro.berkeley.edu FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; NSF; University of California; Sylvia & Jim Katzman Foundation; Richard and Rhoda Goldman Fund; NASA FX The LOSS, conducted by AVF's group, has been supported by many grants from the US National Science Foundation (NSF; most recently AST-0607485 and AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC grant DE-FC02-06ER41453 and US Department of Energy grant DE-FG02-08ER41563. The KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, the Richard and Rhoda Goldman Fund and the TABASGO Foundation. We particularly thank Russell M. Genet, who made the KAIT possible with his initial special gift; former Lick Director Joseph S. Miller, who allowed the KAIT to be placed at the Lick Observatory and provided staff support; and the TABASGO Foundation, without which this work would not have been completed. JL is grateful for a fellowship from the NASA Postdoctoral Program. We made use of the NED, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We acknowledge the use of the HyperLeda data base (http://leda.univ-lyon1. fr). NR 123 TC 72 Z9 72 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 APR PY 2011 VL 412 IS 3 BP 1419 EP 1440 DI 10.1111/j.1365-2966.2011.18158.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100002 ER PT J AU Li, WD Leaman, J Chornock, R Filippenko, AV Poznanski, D Ganeshalingam, M Wang, XF Modjaz, M Jha, S Foley, RJ Smith, N AF Li, Weidong Leaman, Jesse Chornock, Ryan Filippenko, Alexei V. Poznanski, Dovi Ganeshalingam, Mohan Wang, Xiaofeng Modjaz, Maryam Jha, Saurabh Foley, Ryan J. Smith, Nathan TI Nearby supernova rates from the Lick Observatory Supernova Search - II. The observed luminosity functions and fractions of supernovae in a complete sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE supernovae: general ID CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY BURST; IA SUPERNOVAE; LIGHT CURVES; HOST GALAXIES; INFRARED OBSERVATIONS; RELATIVE FREQUENCIES; PHYSICAL-PROPERTIES; UBVRI PHOTOMETRY; SHOCK BREAKOUT AB This is the second paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search (LOSS). In this paper, a complete SN sample is constructed, and the observed (uncorrected for host-galaxy extinction) luminosity functions (LFs) of SNe are derived. These LFs solve two issues that have plagued previous rate calculations for nearby SNe: the luminosity distribution of SNe and the host-galaxy extinction. We select a volume-limited sample of 175 SNe, collect photometry for every object and fit a family of light curves to constrain the peak magnitudes and light-curve shapes. The volume-limited LFs show that they are not well represented by a Gaussian distribution. There are notable differences in the LFs for galaxies of different Hubble types (especially for SNe Ia). We derive the observed fractions for the different subclasses in a complete SN sample, and find significant fractions of SNe II-L (10 per cent), IIb (12 per cent) and IIn (9 per cent) in the SN II sample. Furthermore, we derive the LFs and the observed fractions of different SN subclasses in a magnitude-limited survey with different observation intervals, and find that the LFs are enhanced at the high-luminosity end and appear more 'standard' with smaller scatter, and that the LFs and fractions of SNe do not change significantly when the observation interval is shorter than 10 d. We also discuss the LFs in different galaxy sizes and inclinations, and for different SN subclasses. Some notable results are that there is not a strong correlation between the SN LFs and the host-galaxy size, but there might be a preference for SNe IIn to occur in small, late-type spiral galaxies. The LFs in different inclination bins do not provide strong evidence for extreme extinction in highly inclined galaxies, though the sample is still small. The LFs of different SN subclasses show significant differences. We also find that SNe Ibc and IIb come from more luminous galaxies than SNe II-P, while SNe IIn come from less luminous galaxies, suggesting a possible metallicity effect. The limitations and applications of our LFs are also discussed. C1 [Li, Weidong; Leaman, Jesse; Chornock, Ryan; Filippenko, Alexei V.; Poznanski, Dovi; Ganeshalingam, Mohan; Wang, Xiaofeng; Modjaz, Maryam; Jha, Saurabh; Foley, Ryan J.; Smith, Nathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Leaman, Jesse] NASA, Ames Res Ctr, Mountain View, CA 94043 USA. [Chornock, Ryan; Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Poznanski, Dovi] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Wang, Xiaofeng] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. [Modjaz, Maryam] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Jha, Saurabh] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Li, WD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM wli@astro.berkeley.edu RI Wang, Xiaofeng/J-5390-2015 FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; NSF [AST-0205808, AST-0606772]; University of California; Sylvia & Jim Katzman Foundation; Richard and Rhoda Goldman Fund; NASA; Einstein Fellowship; NSFC [10673007, 11073013]; China-973 Program [2009CB824800]; Miller Institute for Basic Research in Science (UC Berkeley) FX We thank the referee, Enrico Cappellaro, for useful comments and suggestions which improved the paper. We are grateful to the many students, postdocs and other collaborators who have contributed to the Katzman Automatic Imaging Telescope and the Lick Observatory Supernova Search over the past two decades, and to discussions concerning the determination of supernova rates - especially Jack Borde, Frank Serduke, Jeffrey Silverman, Thea Steele and Richard R. Treffers. We thank the Lick Observatory staff for their assistance with the operation of KAIT. LOSS, conducted by AVF's group, has been supported by many grants from the US National Science Foundation (NSF; most recently AST-0607485 and AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC grant DE-FC02-06ER41453 and US Department of Energy grant DE-FG02-08ER41563. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, the Richard and Rhoda Goldman Fund and the TABASGO Foundation. We give particular thanks to Russell M. Genet, who made KAIT possible with his initial special gift; former Lick Director Joseph S. Miller, who allowed KAIT to be placed at Lick Observatory and provided staff support; and the TABASGO Foundation, without which this work would not have been completed. JL is grateful for a fellowship from the NASA Postdoctoral Program. DP is supported by an Einstein Fellowship. XW acknowledges NSFC grants (10673007, 11073013) and the China-973 Program 2009CB824800. MM acknowledges NSF grants AST-0205808 and AST-0606772, as well as the Miller Institute for Basic Research in Science (UC Berkeley), for support during the time over which part of this work was conducted. We made use of the NASA/IPAC Extragalactic Data base (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We acknowledge use of the HyperLeda data base (http://leda.univ-lyon1.fr). NR 133 TC 277 Z9 279 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR PY 2011 VL 412 IS 3 BP 1441 EP 1472 DI 10.1111/j.1365-2966.2011.18160.x PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100003 ER PT J AU Li, WD Chornock, R Leaman, J Filippenko, AV Poznanski, D Wang, XF Ganeshalingam, M Mannucci, F AF Li, Weidong Chornock, Ryan Leaman, Jesse Filippenko, Alexei V. Poznanski, Dovi Wang, Xiaofeng Ganeshalingam, Mohan Mannucci, Filippo TI Nearby supernova rates from the Lick Observatory Supernova Search - III. The rate-size relation, and the rates as a function of galaxy Hubble type and colour SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general ID CORE-COLLAPSE SUPERNOVAE; AEGIS FIELD GALAXIES; IA SUPERNOVAE; STAR-FORMATION; MASSIVE STARS; LEGACY SURVEY; HIGH-REDSHIFT; PROGENITORS; POPULATIONS; LUMINOSITY AB This is the third paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search (LOSS). We have considered a sample of similar to 1000 SNe and used an optimal subsample of 726 SNe (274 SNe Ia, 116 SNe Ibc and 324 SNe II) to determine our rates. We study the trend of the rates as a function of a few quantities available for our galaxy sample, such as luminosity in the B and K bands, stellar mass and morphological class. We discuss different choices (SN samples, input SN luminosity functions, inclination correction factors) and their effect on the rates and their uncertainties. A comparison between our SN rates and the published measurements shows that they are consistent with each other to within the uncertainties when the rate calculations are done in the same manner. Nevertheless, our data demonstrate that the rates cannot be adequately described by a single parameter using either galaxy Hubble types or B - K colours. A secondary parameter in galaxy 'size', expressed by luminosity or stellar mass, is needed to adequately describe the rates in the rate-size relation: the galaxies of smaller sizes have higher SN rates per unit mass or per unit luminosity. The trends of the SN rates in galaxies of different Hubble types and colours are discussed. We examine possible causes for the rate-size relation. Physically, such a relation for the core-collapse SNe is probably linked to the correlation between the specific star-formation rate and the galaxy sizes, but it is not clear whether the same link can be established for SNe Ia. We discuss the two-component ('tardy' and 'prompt') model for SN Ia rates, and find that the SN Ia rates in young stellar populations might have a strong correlation with the core-collapse SN rates. We derive volumetric rates for the different SN types [e.g. for SNe Ia, a rate of (0.301 +/- 0.062) x 10-4 SN Mpc-3 yr-1 at redshift 0] and compare them to the measurements at different redshifts. Finally, we estimate the SN rate for the Milky Way Galaxy to be 2.84 +/- 0.60 SNe per century (with a systematic uncertainty of a factor of similar to 2), consistent with published SN rates based on several different techniques. C1 [Li, Weidong; Chornock, Ryan; Leaman, Jesse; Filippenko, Alexei V.; Poznanski, Dovi; Wang, Xiaofeng; Ganeshalingam, Mohan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leaman, Jesse] NASA, Ames Res Ctr, Mountain View, CA 94043 USA. [Poznanski, Dovi] Univ Calif Berkeley, Lawrence Berkeley Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Wang, Xiaofeng] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. [Mannucci, Filippo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Li, WD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM wli@astro.berkeley.edu RI Wang, Xiaofeng/J-5390-2015; OI mannucci, filippo/0000-0002-4803-2381 FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; NSF; University of California; Sylvia & Jim Katzman Foundation; Richard and Rhoda Goldman Fund; NASA; Einstein Fellowship; NSFC [10673007, 11073013]; China-973 Program [2009CB824800] FX The LOSS, conducted by AVF's group, has been supported by many grants from the US National Science Foundation (NSF; most recently AST-0607485 and AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC grant DE-FC02-06ER41453 and US Department of Energy grant DE-FG02-08ER41563. The KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, the Richard and Rhoda Goldman Fund and the TABASGO Foundation. We give particular thanks to Russell M. Genet, who made the KAIT possible with his initial special gift; former Lick Director Joseph S. Miller, who allowed the KAIT to be placed at Lick Observatory and provided staff support; and the TABASGO Foundation, without which this work would not have been completed. JL is grateful for a fellowship from the NASA Postdoctoral Program. DP is supported by an Einstein Fellowship. XW acknowledges NSFC grants (10673007, 11073013) and the China-973 Program 2009CB824800. We made use of the NASA/IPAC Extragalactic Data base (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We acknowledge use of the HyperLeda data base (http://leda.univlyon1.fr). NR 58 TC 199 Z9 202 U1 1 U2 9 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 APR PY 2011 VL 412 IS 3 BP 1473 EP 1507 DI 10.1111/j.1365-2966.2011.18162.x PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100004 ER PT J AU Smith, N Li, WD Filippenko, AV Chornock, R AF Smith, Nathan Li, Weidong Filippenko, Alexei V. Chornock, Ryan TI Observed fractions of core-collapse supernova types and initial masses of their single and binary progenitor stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE binaries: general; stars: evolution; stars: mass-loss; supernovae: general ID WOLF-RAYET STARS; II-P SUPERNOVAE; LUMINOUS BLUE VARIABLES; SPACE-TELESCOPE IMAGES; ELECTRON-CAPTURE SUPERNOVAE; RED SUPERGIANT PROGENITOR; BLACK-HOLE FORMATION; O-TYPE STARS; MASSIVE STARS; CASSIOPEIA-A AB We analyse the observed fractions of core-collapse supernova (SN) types from the Lick Observatory Supernova Search (LOSS), and we discuss the corresponding implications for massive star evolution. For a standard initial mass function, observed fractions of SN types cannot be reconciled with the expectations of single-star evolution. The mass range of Wolf-Rayet (WR) stars that shed their hydrogen envelopes via their own mass-loss accounts for less than half of the observed fraction of Type Ibc supernovae (SNe Ibc). The true progenitors of SNe Ibc must extend to a much lower range of initial masses than classical WR stars, and we argue that most SN Ibc and SN IIb progenitors must arise from binary Roche lobe overflow. In this scenario, SNe Ic would still trace higher initial mass and metallicity, because line-driven winds in the WR stage remove the helium layer and propel the transition from SN Ib to Ic. Less massive progenitors of SNe Ib and IIb may not be classical WR stars; they may be underluminous with weak winds, possibly hidden by overluminous mass-gainer companions that could appear as B[e] supergiants or related objects having aspherical circumstellar material. The remaining SN types (II-P, II-L and IIn) need to be redistributed across the full range of initial masses, so that even some very massive single stars retain H envelopes until explosion. We consider the possibility of direct collapse to black holes without visible SNe, but find this hypothesis difficult to accommodate in most scenarios. Major areas of remaining uncertainty are (1) the detailed influence of binary separation, rotation and metallicity; (2) mass differences in progenitors of SNe IIn compared to SNe II-L and II-P; and (3) the fraction of SNe Ic arising from single stars with the help of eruptive mass-loss, how this depends on metallicity and how it relates to diversity within the SN Ic subclass. Continued studies of progenitor stars and their environments in nearby galaxies, accounting for SN types, may eventually test these ideas. C1 [Smith, Nathan; Li, Weidong; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, N (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM nathans@as.arizona.edu FU US National Science Foundation (NSF) [AST-0607485, AST-0908886]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563]; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; NSF; University of California; Sylvia & Jim Katzman Foundation FX We are grateful to the many students, post-docs and other collaborators who have contributed to the Katzman Automatic Imaging Telescope and the Lick Observatory Supernova Search over the past two decades. We thank the Lick Observatory staff for their assistance with the operation of KAIT. AVF's group has been supported by many grants from the US National Science Foundation (NSF; most recently AST-0607485 and AST-0908886), the TABASGO Foundation, US Department of Energy SciDAC grant DE-FC02-06ER41453 and US Department of Energy grant DE-FG02-08ER41563. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation and the TABASGO Foundation. NR 160 TC 171 Z9 172 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 APR PY 2011 VL 412 IS 3 BP 1522 EP 1538 DI 10.1111/j.1365-2966.2011.17229.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 745IM UT WOS:000289159100006 ER PT J AU Eberhard, WG AF Eberhard, William G. TI Are smaller animals behaviourally limited? Lack of clear constraints in miniature spiders SO ANIMAL BEHAVIOUR LA English DT Article DE miniaturization; orb-weaving behaviour ID ORB-WEAVING SPIDERS; LEUCAUGE-MARIANA; BRAIN SIZE; ARANEAE; CONSTRUCTION; ANTS AB Because of scaling trends in physiology and morphology, very small animals are expected to suffer especially strong selection to reduce the cost of the central nervous system, which may make them more likely to sacrifice behavioural capacities to economize on nervous tissue. This 'size-limitation' hypothesis predicts reduced behavioural capabilities in smaller animals. I tested this hypothesis by comparing web construction behaviour of young nymphs and adults of a very small orb-weaving spider, Anapisona simoni (young nymphs similar to 0.005 mg, adults similar to 0.8 mg), with those of relatives up to 104 times larger. In these comparisons I took advantage of the special opportunities offered by orb webs to study fine behavioural details during web construction, because the webs represent precise records of large numbers of behavioural decisions. Combining these results with those of a previous study, the size-limitation hypothesis was not supported: very small spiders failed to show three predicted trends, and they showed four other trends that were in directions opposite to those predicted by the hypothesis. Two additional intraweb comparisons (at least one of which was probably biased against equal performance by the smallest species) gave a mix of support and lack of support for the predictions, while only one interspecific difference supported the predictions. Other studies have shown that small spiders have relatively large central nervous systems for their body sizes, suggesting that they may maintain behavioural capabilities comparable to those of larger orb weavers by paying the material and metabolic costs of building and maintaining large volumes of nervous tissue. These considerations may have general consequences for the probability of evolving small body sizes and egg sizes in spiders and other animals. The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. C1 [Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. [Eberhard, William G.] Univ Costa Rica, Smithsonian Trop Res Inst, San Pedro, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Pedro, Costa Rica. EM william.eberhard@gmail.com FU Smithsonian Tropical Research Institute; Universidad de Costa Rica FX I thank John Douglass, Mary Jane West Eberhard, Jeremy Niven and William T. Wcislo for useful comments on a previous version, and the Smithsonian Tropical Research Institute and the Universidad de Costa Rica for financial support. NR 57 TC 19 Z9 20 U1 0 U2 14 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 APR PY 2011 VL 81 IS 4 BP 813 EP 823 DI 10.1016/j.anbehav.2011.01.016 PG 11 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 738OT UT WOS:000288651200018 ER PT J AU Barro, G Perez-Gonzalez, PG Gallego, J Ashby, MLN Kajisawa, M Miyazaki, S Villar, V Yamada, T Zamorano, J AF Barro, G. Perez-Gonzalez, P. G. Gallego, J. Ashby, M. L. N. Kajisawa, M. Miyazaki, S. Villar, V. Yamada, T. Zamorano, J. TI UV-TO-FIR ANALYSIS OF SPITZER/IRAC SOURCES IN THE EXTENDED GROTH STRIP. II. PHOTOMETRIC REDSHIFTS, STELLAR MASSES, AND STAR FORMATION RATES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: high-redshift; galaxies: photometry; galaxies: starburst; infrared: galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; LYMAN-BREAK GALAXIES; GOODS-MUSIC SAMPLE; YALE-CHILE MUSYC; ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; INFRARED SPECTROSCOPIC SURVEY; DISTANT RED GALAXIES; K-SELECTED GALAXIES; FORMING GALAXIES AB Based on the ultraviolet to far-infrared photometry already compiled and presented in a companion paper (Paper I), we present a detailed spectral energy distribution (SED) analysis of nearly 80,000 IRAC 3.6 + 4.5 mu m selected galaxies in the Extended Groth Strip. We estimate photometric redshifts, stellar masses, and star formation rates (SFRs) separately for each galaxy in this large sample. The catalog includes 76,936 sources with [3.6] <= 23.75 (85% completeness level of the IRAC survey) over 0.48 deg(2). The typical photometric redshift accuracy is Delta z/(1 + z) = 0.034, with a catastrophic outlier fraction of just 2%. We quantify the systematics introduced by the use of different stellar population synthesis libraries and initial mass functions in the calculation of stellar masses. We find systematic offsets ranging from 0.1 to 0.4 dex, with a typical scatter of 0.3 dex. We also provide UV- and IR-based SFRs for all sample galaxies, based on several sets of dust emission templates and SFR indicators. We evaluate the systematic differences and goodness of the different SFR estimations using the deep FIDEL 70 mu m data available in the Extended Groth Strip. Typical random uncertainties of the IR-bases SFRs are a factor of two, with non-negligible systematic effects at z greater than or similar to 1.5 observed when only MIPS 24 mu m data are available. All data products (SEDs, postage stamps from imaging data, and different estimations of the photometric redshifts, stellar masses, and SFRs of each galaxy) described in this and the companion paper are publicly available, and they can be accessed through our the Web interface utility Rainbow-navigator. C1 [Barro, G.; Perez-Gonzalez, P. G.; Gallego, J.; Villar, V.; Zamorano, J.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kajisawa, M.; Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Miyazaki, S.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Barro, G (reprint author), Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. RI Zamorano, Jaime/K-7706-2014; Perez-Gonzalez, Pablo/J-2871-2016 OI Zamorano, Jaime/0000-0002-8993-5894; Perez-Gonzalez, Pablo/0000-0003-4528-5639 FU Spanish Programa Nacional de Astronomia y Astrofisica [AYA 2006-02358, AYA 2006-15698-C02-02]; Spanish Government; European Union; Spanish MICINN [CSD2006-00070]; NASA [1255094, 1407] FX We thank the referee for providing constructive comments and help in improving the contents of this paper. We thank G. Bruzual and S. Charlot for allowing us to use their models prior to publication. We acknowledge support from the Spanish Programa Nacional de Astronomia y Astrofisica under grants AYA 2006-02358 and AYA 2006-15698-C02-02. P.G.P.-G. acknowledges support from the Ramon y Cajal Program financed by the Spanish Government and the European Union. Partially funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. Support was also provided by NASA through contract no. 1255094 issued by JPL/Caltech. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, Caltech under NASA contract 1407. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. GALEX is a NASA Small Explorer launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and scientific analysis of the GALEX mission. 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. Based in part on data collected at Subaru Telescope and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. NR 133 TC 59 Z9 59 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 APR PY 2011 VL 193 IS 2 AR 30 DI 10.1088/0067-0049/193/2/30 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZG UT WOS:000289059200008 ER PT J AU McDonald, I Boyer, ML van Loon, JT Zijlstra, AA Hora, JL Babler, B Block, M Gordon, K Meade, M Meixner, M Misselt, K Robitaille, T Sewilo, M Shiao, B Whitney, B AF McDonald, I. Boyer, M. L. van Loon, J. Th. Zijlstra, A. A. Hora, J. L. Babler, B. Block, M. Gordon, K. Meade, M. Meixner, M. Misselt, K. Robitaille, T. Sewilo, M. Shiao, B. Whitney, B. TI FUNDAMENTAL PARAMETERS, INTEGRATED RED GIANT BRANCH MASS LOSS, AND DUST PRODUCTION IN THE GALACTIC GLOBULAR CLUSTER 47 TUCANAE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; globular clusters: individual (NGC 104); infrared: stars; stars: AGB and post-AGB; stars: mass-loss; stars: winds, outflows ID SPITZER-SPACE-TELESCOPE; RICH AGB STARS; ALL-SKY SURVEY; HORIZONTAL-BRANCH; MAGELLANIC CLOUDS; OMEGA-CENTAURI; GLOBULAR-CLUSTER-47 TUCANAE; MODEL ATMOSPHERES; STELLAR EVOLUTION; TUC AB Fundamental parameters and time evolution of mass loss are investigated for post-main-sequence stars in the Galactic globular cluster 47 Tucanae (NGC 104). This is accomplished by fitting spectral energy distributions (SEDs) to existing optical and infrared photometry and spectroscopy, to produce a true Hertzsprung-Russell diagram. We confirm the cluster's distance as d = 4611(-200)(+213) pc and age as 12 +/- 1Gyr. Horizontal branch models appear to confirm that no more red giant branch mass loss occurs in 47 Tuc than in the more metal-poor omega Centauri, though difficulties arise due to inconsistencies between the models. Using our SEDs, we identify those stars that exhibit infrared excess, finding excess only among the brightest giants: dusty mass loss begins at a luminosity of similar to 1000 L-circle dot, becoming ubiquitous above L = 2000 L-circle dot. Recent claims of dust production around lower-luminosity giants cannot be reproduced, despite using the same archival Spitzer imagery. C1 [McDonald, I.; Zijlstra, A. A.] Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Boyer, M. L.; Gordon, K.; Meixner, M.; Sewilo, M.; Shiao, B.; Whitney, B.] STScI, Baltimore, MD 21218 USA. [van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Hora, J. L.; Robitaille, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Babler, B.; Meade, M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Block, M.; Misselt, K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP McDonald, I (reprint author), Jodrell Bank Ctr Astrophys, Alan Turing Bldg, Manchester M13 9PL, Lancs, England. EM iain.mcdonald-2@manchester.ac.uk OI Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650; Robitaille, Thomas/0000-0002-8642-1329 FU NASA [1407, 1257184]; NSF FX We are grateful to Livia Origlia for her co-operation in the production of this paper, for her contribution to the analysis and for sharing her original data with us. This paper uses observations made using the Spitzer Space Telescope (operated by JPL, California Institute of Technology under NASA contract 1407 and supported by NASA through JPL (contract number 1257184)); observations using AKARI, a JAXA project with the participation of ESA; and data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and IPAC/CIT, funded by NASA and the NSF. NR 82 TC 33 Z9 33 U1 0 U2 3 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 APR PY 2011 VL 193 IS 2 AR 23 DI 10.1088/0067-0049/193/2/23 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZG UT WOS:000289059200001 ER PT J AU Tullmann, R Gaetz, TJ Plucinsky, PP Kuntz, KD Williams, BF Pietsch, W Haberl, F Long, KS Blair, WP Sasaki, M Winkler, PF Challis, P Pannuti, TG Edgar, RJ Helfand, DJ Hughes, JP Kirshner, RP Mazeh, T Shporer, A AF Tuellmann, R. Gaetz, T. J. Plucinsky, P. P. Kuntz, K. D. Williams, B. F. Pietsch, W. Haberl, F. Long, K. S. Blair, W. P. Sasaki, M. Winkler, P. F. Challis, P. Pannuti, T. G. Edgar, R. J. Helfand, D. J. Hughes, J. P. Kirshner, R. P. Mazeh, T. Shporer, A. TI THE CHANDRA ACIS SURVEY OF M33 (ChASeM33): THE FINAL SOURCE CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE binaries: general; galaxies: individual (M33); ISM: supernova remnants; surveys; X-rays: galaxies ID X-RAY SOURCES; STAR-FORMATION RATE; XMM-NEWTON SURVEY; LUMINOSITY FUNCTION; SPIRAL GALAXIES; MILKY-WAY; SUPERNOVA-REMNANTS; PHOTOMETRIC SURVEY; POINT SOURCES; SOURCE LIST AB This study presents the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers similar to 70% of the D-25 isophote (R approximate to 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of similar to 2.4x10(34) erg s(-1) in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up MMT spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 is presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10(34) erg s(-1) and 1.6 x 10(35) erg s(-1)(for D = 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. C1 [Tuellmann, R.; Gaetz, T. J.; Plucinsky, P. P.; Challis, P.; Edgar, R. J.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kuntz, K. D.; Blair, W. P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kuntz, K. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Williams, B. F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Pietsch, W.; Haberl, F.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Long, K. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sasaki, M.] Univ Tubingen, Inst Astron & Astrophys, Tubingen, Germany. [Winkler, P. F.] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Pannuti, T. G.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. [Helfand, D. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Mazeh, T.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Shporer, A.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Shporer, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Tullmann, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rtuellmann@cfa.harvard.edu RI Sasaki, Manami/P-3045-2016; OI Sasaki, Manami/0000-0001-5302-1866; Haberl, Frank/0000-0002-0107-5237 FU National Aeronautics and Space Administration [G06-7073A]; National Aeronautics Space and Administration [NAS8-03060] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G06-7073A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory and on behalf of the National Aeronautics Space and Administration under contract NAS8-03060. R.T., P.P.P., T.J.G., and R.J.E. acknowledge support under NASA contract NAS8-03060. This work has made use of SAOImage DS9, developed by the Smithsonian Astrophysical Observatory (Joye & Mandel 2003), the XSPEC spectral fitting package (Arnaud 1996), the FUNTOOLS utilities package, the HEASARC FTOOLS package, the CIAO (Chandra Interactive Analysis of Observations) package, and ACIS Extract, the source extraction and characterization tool developed and maintained by Pat Broos. Sincere thanks to Pat Broos for answering our questions regarding AE and for maintaining this important tool and to David Thilker for kindly providing the Hi map of M33. We also acknowledge the heroic effort of the anonymous referee for a careful reading of the manuscript and several comments that helped to improve the paper. NR 68 TC 16 Z9 16 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 APR PY 2011 VL 193 IS 2 AR 31 DI 10.1088/0067-0049/193/2/31 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZG UT WOS:000289059200009 ER PT J AU Liow, LH Simpson, C Bouchard, F Damuth, J Hallgrimsson, B Hunt, G McShea, DW Powell, JR Stenseth, NC Stoller, MK Wagner, G AF Liow, Lee Hsiang Simpson, Carl Bouchard, Frederic Damuth, John Hallgrimsson, Benedikt Hunt, Gene McShea, Dan W. Powell, Jeffrey R. Stenseth, Nils C. Stoller, Melissa K. Wagner, Gunter TI PIONEERING PARADIGMS AND MAGNIFICENT MANIFESTOS-LEIGH VAN VALEN'S PRICELESS CONTRIBUTIONS TO EVOLUTIONARY BIOLOGY SO EVOLUTION LA English DT Biographical-Item ID NATURAL POPULATIONS; TAXONOMIC DIVERSITY; FOSSIL RECORD; SELECTION; EXTINCTION; ORIGINATION; DIVERSIFICATION; EVOLVABILITY; CHARACTERS; MAMMALS C1 [Liow, Lee Hsiang; Stenseth, Nils C.] Univ Oslo, Dept Biol, CEES, Oslo, Norway. [Simpson, Carl] Humboldt Univ, Museum Nat Kunde, Berlin, Germany. [Bouchard, Frederic] Univ Montreal, Dept Philosophie, Montreal, PQ, Canada. [Damuth, John] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Hallgrimsson, Benedikt] Univ Calgary, Dept Cell Biol & Anat, Calgary, AB T2N 1N4, Canada. [Hunt, Gene] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [McShea, Dan W.] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Powell, Jeffrey R.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Stoller, Melissa K.] Univ Chicago, Biol Sci Collegiate Div, Chicago, IL 60637 USA. [Wagner, Gunter] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06405 USA. RP Liow, LH (reprint author), Univ Oslo, Dept Biol, CEES, Oslo, Norway. EM l.h.liow@bio.uio.no RI Simpson, Carl/E-7140-2010; Hunt, Gene/B-3783-2010; Hallgrimsson, Benedikt/A-9616-2008; Liow, Lee Hsiang/E-3481-2010; Stenseth, Nils Chr./G-5212-2016 OI Wagner, Gunter/0000-0002-3097-002X; Hunt, Gene/0000-0001-6430-5020; Hallgrimsson, Benedikt/0000-0002-7192-9103; Liow, Lee Hsiang/0000-0002-3732-6069; Stenseth, Nils Chr./0000-0002-1591-5399 NR 48 TC 1 Z9 1 U1 0 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD APR PY 2011 VL 65 IS 4 BP 917 EP 922 DI 10.1111/j.1558-5646.2011.01242.x PG 6 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 745IE UT WOS:000289158300001 PM 21463292 ER PT J AU Tao, NA Wu, SA Kim, J An, HJ Hinde, K Power, ML Gagneux, P German, JB Lebrilla, CB AF Tao, Nannan Wu, Shuai Kim, Jaehan An, Hyun Joo Hinde, Katie Power, Michael L. Gagneux, Pascal German, J. Bruce Lebrilla, Carlito B. TI Evolutionary Glycomics: Characterization of Milk Oligosaccharides in Primates SO JOURNAL OF PROTEOME RESEARCH LA English DT Article DE primates; milk oligosaccharides; evolution; mass spectrometry; glycomics ID PARASITE SPECIES RICHNESS; DIETARY SIALIC-ACID; CHEMICAL-CHARACTERIZATION; FED INFANTS; SPECTROMETRY; LACTATION; COLOSTRUM; FORMULAS; GLYCANS; SAMPLE AB Free oligosaccharides are abundant components of mammalian milk and have primary roles as prebiotic compounds, in immune defense, and in brain development. A mass spectrometry-based technique is applied to profile milk oligosaccharides from apes (chimpanzee, gorilla, and siamang), new world monkeys (golden lion tamarin and common marmoset), and an old world monkey (rhesus). The purpose of this study is to evaluate the patterns of primate milk oligosaccharide composition from a phylogenetic perspective to assess the extent to which the compositions of HMOs derives from ancestral primate patterns as opposed to more recent evolutionary events. Milk oligosaccharides were quantitated by nanoflow liquid chromatography on chip-based devices. The relative abundances of fucosylated and sialylated milk oligosaccharides in primates were also determined. For a systematic and comprehensive study of evolutionary patterns of milk oligosaccharides, cluster analysis of primate milk was performed using the chromatographic profile. In general, the oligosaccharides in primate milk, including humans, are more complex and exhibit greater diversity compared to the ones in nonprimate milk. A detailed comparison of the oligosaccharides across evolution revealed nonsequential developmental pattern, that is, that primate milk oligosaccharides do not necessarily cluster according to the primate phylogeny. This report represents the first comprehensive and quantitative effort to profile and elucidate the structures of free milk oligosaccharides so that they can be related to glycan function in different primates. C1 [Tao, Nannan; Wu, Shuai; An, Hyun Joo; Lebrilla, Carlito B.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. [Kim, Jaehan] Univ Calif Davis, Dept Viticulture & Enol, Davis, CA 95616 USA. [Hinde, Katie] Univ Calif Davis, Calif Natl Primate Res Ctr, Brain Mind & Behav Unit, Davis, CA 95616 USA. [Power, Michael L.] Smithsonian Natl Zool Pk, Conservat Ecol Ctr, Nutr Lab, Washington, DC 20008 USA. [Gagneux, Pascal] Univ Calif San Diego, Dept Cellular & Mol Med, La Jolla, CA 92093 USA. [Gagneux, Pascal] Univ Calif San Diego, CARTA, La Jolla, CA 92093 USA. [German, J. Bruce] Univ Calif Davis, Dept Food Sci Technol, Davis, CA 95616 USA. [Lebrilla, Carlito B.] Univ Calif Davis, Dept Biochem & Mol Med, Davis, CA 95616 USA. RP Lebrilla, CB (reprint author), Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. EM cblebrilla@ucdavis.edu RI Wu, Shuai/I-8696-2012; Wu, Shuai/N-8552-2014; OI Power, Michael/0000-0002-6120-3528; Hinde, Katie/0000-0002-0528-866X FU California Dairy Research Foundation; Dairy Management Incorporated; University of California Discovery; National Institutes of Health FX Funding is provided by the California Dairy Research Foundation, Dairy Management Incorporated, the University of California Discovery, and the National Institutes of Health. The G. Harold and Leila Y. Mathers Foundation. Dr Frances Gillin, UC San Diego, and Smithsonian National Zoological Park are gratefully acknowledged for providing the milk samples. NR 34 TC 48 Z9 49 U1 6 U2 41 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1535-3893 J9 J PROTEOME RES JI J. Proteome Res. PD APR PY 2011 VL 10 IS 4 BP 1548 EP 1557 DI 10.1021/pr1009367 PG 10 WC Biochemical Research Methods SC Biochemistry & Molecular Biology GA 742EL UT WOS:000288924000011 PM 21214271 ER PT J AU Clough, GW AF Clough, G. Wayne TI Bloom Time 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 APR PY 2011 VL 42 IS 1 BP 26 EP 27 PG 2 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 742DM UT WOS:000288920400011 ER PT J AU Iafolla, V Lucchesi, DM Nozzoli, S Ravenna, M Santoli, F Shapiro, II Lorenzini, EC Cosmo, ML Bombardelli, C Ashenberg, J Cheimets, PN Glashow, S AF Iafolla, V. Lucchesi, D. M. Nozzoli, S. Ravenna, M. Santoli, F. Shapiro, I. I. Lorenzini, E. C. Cosmo, M. L. Bombardelli, C. Ashenberg, J. Cheimets, P. N. Glashow, S. TI General Relativity Accuracy Test (GReAT): New configuration for the differential accelerometer SO ADVANCES IN SPACE RESEARCH LA English DT Article DE General relativity; Equivalence Principle; Differential accelerometer ID WEAK-EQUIVALENCE PRINCIPLE AB We presents the results of an activity concerning the test of the Einstein Weak Equivalence Principle with an accuracy of about 5 x 10(-15). The experiment will be performed in an "Einstein elevator" using a differential accelerometer with a final sensitivity of about 10(-14) g(circle plus)/Hz(1/2). The differential accelerometer is spun about an horizontal axis at a frequency in the range 0.5-1 Hz in order to modulate,, during the free fall, the signal from a possible violation of the Equivalence Principle. In the paper the perturbing effects with the same signature of the possible violation are analyzed and constrained. The experimental results obtained in the laboratory with a first prototype of the differential accelerometer are discussed, comparing this results with those obtained using a new prototype. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Iafolla, V.; Lucchesi, D. M.; Nozzoli, S.; Ravenna, M.; Santoli, F.] Ist Fis Spazio Interplanetario IFSI INAF, I-00133 Rome, Italy. [Shapiro, I. I.; Lorenzini, E. C.; Cosmo, M. L.; Bombardelli, C.; Ashenberg, J.; Cheimets, P. N.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA USA. [Glashow, S.] Boston Univ, Dept Phys, Boston, MA 02215 USA. RP Lucchesi, DM (reprint author), Ist Fis Spazio Interplanetario IFSI INAF, Via Fosso del Cavaliere 100, I-00133 Rome, Italy. EM david.lucchesi@ifsi-roma.inaf.it OI Santoli, Francesco/0000-0003-2493-0109; Iafolla, Valerio Antonio/0000-0001-5297-1157 FU ASI [I/R/098/02]; NASA [NAG8-1780, NAG3-2881] FX This research work was supported by ASI contract I/R/098/02 and NASA grants NAG8-1780 and NAG3-2881 with Don Strayer (NASA/JPL) as Project Scientist. NR 4 TC 5 Z9 5 U1 0 U2 4 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 APR 1 PY 2011 VL 47 IS 7 BP 1225 EP 1231 DI 10.1016/j.asr.2010.11.028 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 741PS UT WOS:000288876600014 ER PT J AU Boselli, A Boissier, S Heinis, S Cortese, L Ilbert, O Hughes, T Cucciati, O Davies, J Ferrarese, L Giovanelli, R Haynes, MP Baes, M Balkowski, C Brosch, N Chapman, SC Charmandaris, V Clemens, MS Dariush, A De Looze, I Alighieri, SD Duc, PA Durrell, PR Emsellem, E Erben, T Fritz, J Garcia-Appadoo, DA Gavazzi, G Grossi, M Jordan, A Hess, KM Huertas-Company, M Hunt, LK Kent, BR Lambas, DG Lancon, A MacArthur, LA Madden, SC Magrini, L Mei, S Momjian, E Olowin, RP Papastergis, E Smith, MWL Solanes, JM Spector, O Spekkens, K Taylor, JE Valotto, C van Driel, W Verstappen, J Vlahakis, C Vollmer, B Xilouris, EM AF Boselli, A. Boissier, S. Heinis, S. Cortese, L. Ilbert, O. Hughes, T. Cucciati, O. Davies, J. Ferrarese, L. Giovanelli, R. Haynes, M. P. Baes, M. Balkowski, C. Brosch, N. Chapman, S. C. Charmandaris, V. Clemens, M. S. Dariush, A. De Looze, I. Alighieri, S. di Serego Duc, P. -A. Durrell, P. R. Emsellem, E. Erben, T. Fritz, J. Garcia-Appadoo, D. A. Gavazzi, G. Grossi, M. Jordan, A. Hess, K. M. Huertas-Company, M. Hunt, L. K. Kent, B. R. Lambas, D. G. Lancon, A. MacArthur, L. A. Madden, S. C. Magrini, L. Mei, S. Momjian, E. Olowin, R. P. Papastergis, E. Smith, M. W. L. Solanes, J. M. Spector, O. Spekkens, K. Taylor, J. E. Valotto, C. van Driel, W. Verstappen, J. Vlahakis, C. Vollmer, B. Xilouris, E. M. TI The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) I. The UV luminosity function of the central 12 sq. deg SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: Virgo; galaxies: evolution; galaxies: fundamental parameters; ultraviolet: galaxies; galaxies: luminosity function, mass function ID DIGITAL SKY SURVEY; EARLY-TYPE GALAXIES; DWARF ELLIPTIC GALAXIES; FAST ALPHA SURVEY; BAND SURFACE PHOTOMETRY; HI SOURCE CATALOG; STAR-FORMATION; COMA CLUSTER; NEARBY CLUSTERS; DATA RELEASE AB The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) is a complete blind survey of the Virgo cluster covering similar to 40 sq. deg in the far UV (FUV, lambda(eff) = 1539 angstrom, Delta lambda = 442 angstrom) and similar to 120 sq. deg in the near UV (NUV, lambda(eff) = 2316 angstrom, Delta lambda = 1060 angstrom). The goal of the survey is to study the ultraviolet (UV) properties of galaxies in a rich cluster environment, spanning a wide luminosity range from giants to dwarfs, and regardless of prior knowledge of their star formation activity. The UV data will be combined with those in other bands (optical: NGVS; far-infrared - submm: HeViCS; HI: ALFALFA) and with our multizone chemo-spectrophotometric models of galaxy evolution to make a complete and exhaustive study of the effects of the environment on the evolution of galaxies in high density regions. We present here the scientific objectives of the survey, describing the observing strategy and briefly discussing different data reduction techniques. Using UV data already in-hand for the central 12 sq. deg we determine the FUV and NUV luminosity functions of the Virgo cluster core for all cluster members and separately for early-and late-type galaxies and compare it to the one obtained in the field and other nearby clusters (Coma, A1367). This analysis shows that the FUV and NUV luminosity functions of the core of the Virgo clusters are flatter (alpha similar to -1.1) than those determined in Coma and A1367. We discuss the possible origin of this difference. C1 [Boselli, A.; Boissier, S.; Heinis, S.; Ilbert, O.] CNRS, Lab Astrophys Marseille, UMR 6110, F-13388 Marseille, France. [Cortese, L.] European So Observ, D-85748 Garching, Germany. [Hughes, T.; Davies, J.; Dariush, A.; Smith, M. W. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Cucciati, O.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Ferrarese, L.; MacArthur, L. A.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V8X 4M6, Canada. [Giovanelli, R.; Haynes, M. P.; Papastergis, E.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Baes, M.; De Looze, I.; Fritz, J.; Verstappen, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Balkowski, C.; Huertas-Company, M.; Mei, S.; van Driel, W.] Univ Paris Diderot, GEPI, Observ Paris, CNRS, F-92195 Meudon, France. [Brosch, N.; Spector, O.] Tel Aviv Univ, Wise Observ, Fac Exact Sci, IL-69978 Tel Aviv, Israel. [Brosch, N.; Spector, O.] Tel Aviv Univ, Florence & Raymoond Sackler Dept Phys & Astron, Fac Exact Sci, IL-69978 Tel Aviv, Israel. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Charmandaris, V.] Inst Theoret & Computat Phys, Iraklion 71003, Greece. [Charmandaris, V.] IESL Fdn Res & Technol Hellas, Iraklion 71110, Greece. [Charmandaris, V.] Observ Paris, F-75014 Paris, France. [Clemens, M. S.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran. [Alighieri, S. di Serego; Hunt, L. K.; Magrini, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Duc, P. -A.; Madden, S. C.] Univ Paris Diderot, Lab AIM Paris Saclay, CNRS, INSU CEA, F-91191 Gif Sur Yvette, France. [Durrell, P. R.] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44512 USA. [Emsellem, E.] Univ Lyon 1, Observ Lyon, Ctr Rech Astrophys Lyon, F-69230 St Genis Laval, France. [Emsellem, E.] Ecole Normale Super Lyon, F-69230 St Genis Laval, France. [Erben, T.] Argelander Inst Astron, D-53121 Bonn, Germany. [Garcia-Appadoo, D. A.] ESO, Santiago, Chile. [Gavazzi, G.] Univ Milano Bicocca, I-20100 Milan, Italy. [Grossi, M.] Univ Lisbon, CAAUL, Observ Astron Lisboa, P-1349018 Lisbon, Portugal. [Jordan, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Jordan, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hess, K. M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Huertas-Company, M.; Mei, S.] Univ Paris Diderot, F-75205 Paris 13, France. [Kent, B. R.] Natl Radio Astron Observ, Charlottesville, VA 22901 USA. [Lambas, D. G.; Valotto, C.] UNC CONICET, Inst Astron Teor & Expt, Cordoba, Argentina. [Lancon, A.; Vollmer, B.] Univ Strasbourg, Observ Astron Strasbourg, CNRS, UMR 7550, F-67000 Strasbourg, France. [MacArthur, L. A.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Momjian, E.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Olowin, R. P.] St Marys Coll, Dept Phys & Astron, Moraga, CA 94575 USA. [Solanes, J. M.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Solanes, J. M.] Univ Barcelona, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Spekkens, K.] Royal Mil Coll Canada, Kingston, ON K7K 7B4, Canada. [Taylor, J. E.] Dept Phys & Astron, Waterloo, ON N2L 1W7, Canada. [Vlahakis, C.] Univ Chile, Dept Astron, Santiago, Chile. [Xilouris, E. M.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. RP Boselli, A (reprint author), CNRS, Lab Astrophys Marseille, UMR 6110, 38 Rue F Joliot Curie, F-13388 Marseille, France. EM Alessandro.Boselli@oamp.fr; Samuel.Boissier@oamp.fr; Sebastien.Heinis@oamp.fr; lcortese@eso.org; Olivier.Ilbert@oamp.fr; Thomas.Hughes@astro.cf.ac.uk; Cucciati@oats.inaf.it; Jonathan.Davies@astro.cf.ac.uk; laura.ferrarese@nrc-cnrc.gc.ca; riccardo@astro.cornell.edu; haynes@astro.cornell.edu; maarten.baes@ugent.be; chantal.balkowski@obspm.fr; moah@wise.tau.ac.il; schapman@ast.cam.ac.uk; vassilis@physics.uoc.gr; marcel.clemens@oapd.inaf.it; Ali.Dariush@astro.cf.ac.uk; ilse.delooze@ugent.be; sperello@arcetri.astro.it; paduc@cea.fr; prdurrell@ysu.edu; emsellem@obs-unic-lyon1.fr; terben@astro.uni-bonn.de; jacopo.fritz@ugent.be; dgarcia@eso.org; giuseppe.gavazzi@mib.infn.it; grossi@oal.ul.pt; ajordan@astro.puc.cl; hess@astro.wisc.edu; marc.huertas@obspm.fr; hunt@arcetri.astro.it; bkent@nrao.edu; dgl@mail.oac.uncor.edu; ariane.lancon@astro.unistra.fr; Lauren.MacArthur@nrc-cnrc.gc.ca; smadden@cea.fr; laura@arcetri.astro.it; simona.mei@obspm.fr; emomjian@nrao.edu; rpolowin@stmarys-ca.edu; papastergis@astro.cornell.edu; Matthew.Smith@astro.cf.ac.uk; jm.solanes@ub.edu; odedspec@wise.tau.ac.il; Kristine.Spekkens@rmc.ca; taylor@uwaterloo.ca; val@mail.oac.uncor.edu; wim.vandriel@obspm.fr; joris.verstappen@ugent.be; vlahakis@das.uchile.cl; Bernd.Vollmer@astro.unistra.fr; xilouris@astro.noa.gr RI Charmandaris, Vassilis/A-7196-2008; di Serego Alighieri, Sperello/E-4067-2010; Baes, Maarten/I-6985-2013; Xilouris, Emmanuel/K-9459-2013; Magrini, Laura/J-2485-2012; OI Cortese, Luca/0000-0002-7422-9823; Charmandaris, Vassilis/0000-0002-2688-1956; di Serego Alighieri, Sperello/0000-0001-8769-2692; Baes, Maarten/0000-0002-3930-2757; Magrini, Laura/0000-0003-4486-6802; Grossi, Marco/0000-0003-4675-3246; Jordan, Andres/0000-0002-5389-3944; Hunt, Leslie/0000-0001-9162-2371 FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; NSF [AST-0607007]; Brinson Foundation FX We wish to thank the GALEX Time Allocation Commetee for the generous allocation of time devoted to this project. We want to thank J. C. Munoz-Mateos for providing us the SDSS data of the SINGS galaxies and M. Seibert for providing us with FUV data manually reduced of fields N. 1, 7 and 11 and M. Balogh and the anonymous referee for useful comments. 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 and of the GOLDMine database (http://goldmine.mib.infn.it/). GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASAs support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National dEtudes Spatiales of France and the Korean Ministry of Science and Technology. 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. R. G. and M. P. H. are supported by NSF grant AST-0607007 and by a grant from the Brinson Foundation. NR 87 TC 37 Z9 37 U1 1 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 APR PY 2011 VL 528 AR A107 DI 10.1051/0004-6361/201016389 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600053 ER PT J AU Mirabel, IF Dijkstra, M Laurent, P Loeb, A Pritchard, JR AF Mirabel, I. F. Dijkstra, M. Laurent, P. Loeb, A. Pritchard, J. R. TI Stellar black holes at the dawn of the universe SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; black hole physics; dark ages, reionization, first stars; cosmology: miscellaneous; intergalactic medium ID GAMMA-RAY BURSTS; STAR-FORMATION RATE; 21-CM FLUCTUATIONS; POPULATION III; GALAXIES; REIONIZATION; REDSHIFT; METALLICITY; ACCRETION; BINARIES AB Context. It is well established that between 380 000 and 1 billion years after the Big Bang the Inter Galactic Medium (IGM) underwent a "phase transformation" from cold and fully neutral to warm (approximate to 10(4) K) and ionized. Whether this phase transformation was fully driven and completed by photoionization by young hot stars is a question of topical interest in cosmology. Aims. We propose here that besides the ultraviolet radiation from massive stars, feedback from accreting black holes in high-mass X-ray binaries (BH-HMXBs) was an additional, important source of heating and reionization of the IGM in regions of low gas density at large distances from star-forming galaxies. Methods. We use current theoretical models on the formation and evolution of primitive massive stars of low metallicity, and the observations of compact stellar remnants in the near and distant universe, to infer that a significant fraction of the first generations of massive stars end up as BH-HMXBs. Results. The total number of energetic ionizing photons from an accreting stellar black hole in an HMXB is comparable to the total number of ionizing photons of its progenitor star. However, the X-ray photons emitted by the accreting black hole are capable of producing several secondary ionizations and the ionizing power of the resulting black hole could be greater than that of its progenitor. Feedback by the large populations of BH-HMXBs heats the IGM to temperatures of approximate to 10(4) K and maintains it ionized on large distance scales. Conclusions. BH-HMXBs determine the early thermal history of the universe and maintain it as ionized over large volumes of space in regions of low density. This has a direct impact on the properties of the faintest galaxies at high redshifts, the smallest dwarf galaxies in the local universe, and on the existing and future surveys at radio wavelengths of atomic hydrogen in the early universe. C1 [Mirabel, I. F.; Laurent, P.] CEA Saclay, IRFU, DSM, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Mirabel, I. F.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Dijkstra, M.; Loeb, A.; Pritchard, J. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Laurent, P.] Lab APC, F-75205 Paris, France. [Dijkstra, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Mirabel, IF (reprint author), CEA Saclay, IRFU, DSM, Serv Astrophys, F-91191 Gif Sur Yvette, France. EM felix.mirabel@cea.fr RI laurent, philippe/E-6211-2013; OI Pritchard, Jonathan/0000-0003-4127-5353 FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX I.F.M. thanks the referee G. Meynet, and A. King, P. Fabbiano, T. Piran, T. Linden and V. Kalogera for useful information and kind comments. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 50 TC 81 Z9 81 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 APR PY 2011 VL 528 AR A149 DI 10.1051/0004-6361/201016357 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737BD UT WOS:000288541600036 ER PT J AU Bogdanov, S van den Berg, M Servillat, M Heinke, CO Grindlay, JE Stairs, IH Ransom, SM Freire, PCC Begin, S Becker, W AF Bogdanov, Slavko van den Berg, Maureen Servillat, Mathieu Heinke, Craig O. Grindlay, Jonathan E. Stairs, Ingrid H. Ransom, Scott M. Freire, Paulo C. C. Begin, Steve Becker, Werner TI CHANDRA X-RAY OBSERVATIONS OF 12 MILLISECOND PULSARS IN THE GLOBULAR CLUSTER M28 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: general; globular clusters: individual (NGC 6626); pulsars: general; pulsars: individual (PSR B1821-24, PSR J1824-2452H); stars: neutron; X-rays: stars ID COUNTING DETECTOR IMAGES; TIMING OBSERVATIONS; WAVELET TRANSFORMS; SAX J1808.4-3658; 47 TUCANAE; EMISSION; RADIO; 47-TUCANAE; CONSTRAINTS; VARIABILITY AB We present a Chandra X-ray Observatory investigation of the millisecond pulsars in the globular cluster M28 (NGC 6626). In what is one of the deepest X-ray observations of a globular cluster, we firmly detect seven and possibly detect two of the 12 known M28 pulsars. With the exception of PSRs B1821-24 and J1824-2452H, the detected pulsars have relatively soft spectra, with X-ray luminosities 10(30)-10(31) erg s(-1) (0.3-8 keV), similar to most "recycled" pulsars in 47 Tucanae and the field of the Galaxy, implying thermal emission from the pulsar magnetic polar caps. We present the most detailed X-ray spectrum to date of the energetic PSR B1821-24. It is well described by a purely non-thermal spectrum with spectral photon index Gamma = 1.23 and luminosity 1.4x10(33)Theta (D/5.5 kpc)(2) erg s(-1) (0.3-8 keV), where Theta is the fraction of the sky covered by the X-ray emission beam(s). We find no evidence for the previously reported line emission feature around 3.3 keV, most likely as a consequence of improvements in instrument calibration. The X-ray spectrum and pulse profile of PSR B1821-24 suggest that the bulk of unpulsed emission from this pulsar is not of thermal origin, and is likely due to low-level non-thermal magnetospheric radiation, an unresolved pulsar wind nebula, and/or small-angle scattering of the pulsed X-rays by interstellar dust grains. The peculiar binary PSR J1824-2452H shows a relatively hard X-ray spectrum and possible variability at the binary period, indicative of an intrabinary shock formed by interaction between the relativistic pulsar wind and matter from its non-degenerate companion star. C1 [van den Berg, Maureen; Servillat, Mathieu; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heinke, Craig O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Stairs, Ingrid H.; Begin, Steve] Univ British Columbia, Dept Phys, Vancouver, BC V6T 1Z1, Canada. [Ransom, Scott M.] Natl Radio Astron Observ, Charlottesville, VA 22901 USA. [Freire, Paulo C. C.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany. [Begin, Steve] Univ Laval, Dept Phys Genie Phys & Opt, Ste Foy, PQ G1K 7P4, Canada. [Becker, Werner] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. [Bogdanov, Slavko] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. EM bogdanov@physics.mcgill.ca OI Bogdanov, Slavko/0000-0002-9870-2742; Begin, Steve/0000-0003-1012-224X; Heinke, Craig/0000-0003-3944-6109; Ransom, Scott/0000-0001-5799-9714 FU NASA [GO8-9072X]; CIFAR Junior Fellowship; NSERC FX We thank Z. Medin, A. Harding, and A. Archibald for useful discussions and the referee F. Camilo for comments. The work presented was funded in part by NASA Chandra grant GO8-9072X awarded through the Harvard College Observatory. S.B. is supported in part by a CIFAR Junior Fellowship. C.O.H. and I.H.S. are supported by NSERC. This research has made use of the NASA Astrophysics Data System (ADS) and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. NR 57 TC 26 Z9 26 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2011 VL 730 IS 2 AR 81 DI 10.1088/0004-637X/730/2/81 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900021 ER PT J AU Brown, JM Kilic, M Brown, WR Kenyon, SJ AF Brown, Justin M. Kilic, Mukremin Brown, Warren R. Kenyon, Scott J. TI THE BINARY FRACTION OF LOW-MASS WHITE DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: evolution; stars: low-mass; white dwarfs ID RED GIANT BRANCH; ECLIPSING BINARY; SOLAR NEIGHBORHOOD; STELLAR EVOLUTION; COMMON-ENVELOPE; CLOSE BINARIES; STARS; POPULATION; NGC-6791; SYSTEMS AB We describe spectroscopic observations of 21 low-mass (<= 0.45M(circle dot)) white dwarfs (WDs) from the Palomar-Green survey obtained over four years. We use both radial velocities and infrared photometry to identify binary systems, and find that the fraction of single, low-mass WDs is <= 30%. We discuss the potential formation channels for these single stars including binary mergers of lower-mass objects. However, binary mergers are not likely to explain the observed number of single low-mass WDs. Thus, additional formation channels, such as enhanced mass loss due to winds or interactions with substellar companions, are likely. C1 [Brown, Justin M.] Franklin & Marshall Coll, Lancaster, PA 17604 USA. [Kilic, Mukremin; Brown, Warren R.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Brown, JM (reprint author), Franklin & Marshall Coll, 415 Harrisburg Ave, Lancaster, PA 17604 USA. EM brown.justin.michael@gmail.com OI Kenyon, Scott/0000-0003-0214-609X FU National Science Foundation Research Experiences for Undergraduates (REU); Department of Defense [0754568]; Smithsonian Institution; NASA under Caltech; National Science Foundation FX We thank G. Nelemans for providing his binary WD population synthesis model results, and Marie Machacek, Jonathan McDowell, Christine Jones, and Kara Tutunjian for their work on the summer REU Program at the Smithsonian Astrophysical Observatory. This work is supported in part by the National Science Foundation Research Experiences for Undergraduates (REU) and Department of Defense Awards to Stimulate and Support Undergraduate Research Experiences (ASSURE) programs under grant No. 0754568, by the Smithsonian Institution, and by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech.; IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. NR 40 TC 20 Z9 20 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 APR 1 PY 2011 VL 730 IS 2 AR 67 DI 10.1088/0004-637X/730/2/67 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900007 ER PT J AU Bulik, T Belczynski, K Prestwich, A AF Bulik, Tomasz Belczynski, Krzysztof Prestwich, Andrea TI IC10 X-1/NGC300 X-1: THE VERY IMMEDIATE PROGENITORS OF BH-BH BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; black hole physics; gravitational waves; stars: evolution ID WOLF-RAYET STARS; BLACK-HOLE; IC-10 X-1; MASS; METALLICITY; GALAXIES; CONSTRAINTS; EVOLUTION; NGC-300; CONSEQUENCES AB We investigate the future evolution of two extragalactic X-ray binaries: IC10 X-1 and NGC300 X-1. Each consists of a high-mass black hole (BH; similar to 20-30 M-circle dot) accreting from a massiveWolf-Rayet (W-R) star companion (greater than or similar to 20 M-circle dot), and both are located in low-metallicity galaxies. We analyze the current state of the systems and demonstrate that both systems will very quickly (less than or similar to 0.3 Myr) form close BH-BH binaries with short coalescence time (similar to 3 Gyr) and large chirp mass (similar to 15 M-circle dot). The formation of a BH-BH system seems unavoidable, as (1) W-R companions are well within their Roche lobes and do not expand, so no Roche lobe overflow is expected; (2) even intense W-R wind mass loss does not remove sufficient mass to prohibit the formation of the second BH; and (3) even if the BH receives a large natal kick, the systems are very closely bound and are almost impossible to disrupt. As there are two such immediate BH-BH progenitor systems within 2 Mpc, and as the current gravitational-wave instruments LIGO/VIRGO (initial stage) can detect such massive BH-BH mergers out to similar to 200 Mpc, the empirically estimated detection rate of such inspirals is R = 3.36(-2.92)(+8.29) at the 99% confidence level. If there is no detection in the current LIGO/VIRGO data (unreleased year of s6 run), the existence of these two massive BH systems poses an interesting challenge. Either the gravitational radiation search is not sensitive to massive inspirals, or there is some fundamental misunderstanding of stellar evolution physics leading directly to the formation of BH-BH binaries. C1 [Bulik, Tomasz; Belczynski, Krzysztof] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Bulik, Tomasz] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Belczynski, Krzysztof] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Prestwich, Andrea] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bulik, T (reprint author), Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. EM tb@astrouw.edu.pl; kbelczyn@nmsu.edu; andreap@head.cfa.harvard.edu FU MSHE [N N203 302835, N N203 404939]; NASA [NNX09AV06A] FX We thank Chris Fryer, Kris Stanek, Aleks Schwarzenberg-Czerny, and Richard O'Shaughnessy for their helpful comments. The authors acknowledge support from MSHE grants N N203 302835 (T. B., K. B.), N N203 404939 (K. B.), and NASA Grant NNX09AV06A to the Center for Gravitational Wave Astronomy, UTB (K.B.). NR 44 TC 36 Z9 36 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 APR 1 PY 2011 VL 730 IS 2 AR 140 DI 10.1088/0004-637X/730/2/140 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900080 ER PT J AU Capak, P Mobasher, B Scoville, NZ McCracken, H Ilbert, O Salvato, M Menendez-Delmestre, K Aussel, H Carilli, C Civano, F Elvis, M Giavalisco, M Jullo, E Kartaltepe, J Leauthaud, A Koekemoer, AM Kneib, JP LeFloch, E Sanders, DB Schinnerer, E Shioya, Y Shopbell, P Tanaguchi, Y Thompson, D Willott, CJ AF Capak, P. Mobasher, B. Scoville, N. Z. McCracken, H. Ilbert, O. Salvato, M. Menendez-Delmestre, K. Aussel, H. Carilli, C. Civano, F. Elvis, M. Giavalisco, M. Jullo, E. Kartaltepe, J. Leauthaud, A. Koekemoer, A. M. Kneib, J. -P. LeFloch, E. Sanders, D. B. Schinnerer, E. Shioya, Y. Shopbell, P. Tanaguchi, Y. Thompson, D. Willott, C. J. TI SPECTROSCOPY OF LUMINOUS z > 7 GALAXY CANDIDATES AND SOURCES OF CONTAMINATION IN z > 7 GALAXY SEARCHES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID LYMAN-BREAK GALAXIES; ULTRA-DEEP-FIELD; STELLAR MASS DENSITY; LY-ALPHA EMITTERS; SIMILAR-TO 7-10; STAR-FORMING GALAXIES; KECK-II-TELESCOPE; HIGH-REDSHIFT; COSMOS FIELD; DARK-MATTER AB We present three bright z(+)-dropout candidates selected from deep near-infrared (NIR) imaging of the COSMOS 2 deg(2) field. All three objects match the 0.8-8 mu m colors of other published z > 7 candidates but are 3 mag brighter, facilitating further study. Deep spectroscopy of two of the candidates covering 0.64-1.02 mu m with Keck-DEIMOS and all three covering 0.94-1.10 mu m and 1.52-1.80 mu m with Keck-NIRSPEC detects weak spectral features tentatively identified as Ly alpha at z = 6.95 and z = 7.69 in two of the objects. The third object is placed at z similar to 1.6 based on a 24 mu m and weak optical detection. A comparison with the spectral energy distributions of known z < 7 galaxies, including objects with strong spectral lines, large extinction, and large systematic uncertainties in the photometry, yields no objects with similar colors. However, the lambda > 1 mu m properties of all three objects can be matched to optically detected sources with photometric redshifts at z similar to 1.8, so the non-detection in the i(+) and z(+) bands is the primary factor which favors a z > 7 solution. If any of these objects are at z similar to 7, the bright end of the luminosity function is significantly higher at z > 7 than suggested by previous studies, but consistent within the statistical uncertainty and the dark matter halo distribution. If these objects are at low redshift, the Lyman break selection must be contaminated by a previously unknown population of low-redshift objects with very strong breaks in their broadband spectral energy distributions and blue NIR colors. The implications of this result on luminosity function evolution at high redshift are discussed. We show that the primary limitation of z > 7 galaxy searches with broad filters is the depth of the available optical data. C1 [Capak, P.; Jullo, E.] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Capak, P.; Scoville, N. Z.; Salvato, M.; Shopbell, P.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Mobasher, B.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [McCracken, H.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Ilbert, O.] Astrophys Lab, F-13376 Marseille 12, France. [Menendez-Delmestre, K.] Carnegie Observ, Pasadena, CA 91101 USA. [Aussel, H.; LeFloch, E.] Univ Paris 07, CNRS, AIM, UMR CEA,UMR 7158, F-91191 Gif Sur Yvette, France. [Carilli, C.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kartaltepe, J.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Leauthaud, A.] Univ Calif Berkeley, LBNL, Berkeley, CA 94720 USA. [Leauthaud, A.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kneib, J. -P.] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Shioya, Y.; Tanaguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. [Willott, C. J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Capak, P (reprint author), Spitzer Sci Ctr, 314-6 Caltech,1201 E Calif Blvd, Pasadena, CA 91125 USA. RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Kneib, Jean-Paul/A-7919-2015 OI Koekemoer, Anton/0000-0002-6610-2048; Schinnerer, Eva/0000-0002-3933-7677; Kneib, Jean-Paul/0000-0002-4616-4989 FU W. M. Keck Foundation; NASA [NAS5-26555, NAS8-03060, 1407, 1278386, HST-GO-09822]; ESA Member States; Associated Universities, Inc.; German Max-Planck-Society; French CNRS; Spanish National Geographical Institute; Spitzer Science Center; French Agene National de la Recheche [ANR-07-BLAN-0228]; CNES; Programme National Cosmologie et Galaxies FX Based on observations with 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 and made possible by the generous financial support of the W. M. Keck Foundation; the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA; the Canada-France-Hawaii Telescope with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii; the United Kingdom Infrared Telescope operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U.K; the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy Data Centre, the Centre National de la Recherche Scientifique de France, TERAPIX and the University of Hawaii; the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS5-26555; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the Chandra X-ray Observatory, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; the 30 m telescope of the Institute for Radioastronomy at Millimeter Wavelengths (IRAM), which is funded by the German Max-Planck-Society, the French CNRS, and the Spanish National Geographical Institute.; 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. Support for this work was provided by the Spitzer Science Center which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under NASA contract 1407, NASA through contract 1278386 issued by the JPL and NASA grant HST-GO-09822. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This research has made use of the NASA/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. H.J.M. and J.P.K. acknowledge support from the French Agene National de la Recheche fund ANR-07-BLAN-0228 as well as from CNES and the Programme National Cosmologie et Galaxies. P.C. acknowledges the Keck remote observing staff who allowed him to simultaneously attend the NIRSPEC observations and the birth of his daughter. NR 102 TC 32 Z9 32 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 APR 1 PY 2011 VL 730 IS 2 AR 68 DI 10.1088/0004-637X/730/2/68 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900008 ER PT J AU Carter, JA Winn, JN Holman, MJ Fabrycky, D Berta, ZK Burke, CJ Nutzman, P AF Carter, Joshua A. Winn, Joshua N. Holman, Matthew J. Fabrycky, Daniel Berta, Zachory K. Burke, Christopher J. Nutzman, Philip TI THE TRANSIT LIGHT CURVE PROJECT. XIII. SIXTEEN TRANSITS OF THE SUPER-EARTH GJ 1214b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: individual (GJ 1214b, GJ 1214); techniques: photometric ID LOW-MASS STARS; EXTRASOLAR PLANETS; EXOPLANET; RADII; STELLAR; SYSTEMS; METALLICITY; PARAMETERS; ATMOSPHERE; SEARCH AB We present optical photometry of 16 transits of the super-Earth GJ 1214b, allowing us to refine the system parameters and search for additional planets via transit timing. Starspot-crossing events are detected in two light curves, and the star is found to be variable by a few percent. Hence, in our analysis, special attention is given to systematic errors that result from starspots. The planet-to-star radius ratio is 0.11610 +/- 0.00048, subject to a possible upward bias by a few percent due to the unknown spot coverage. Even assuming this bias to be negligible, the mean density of the planet can be either 3.03 +/- 0.50 g cm(-3) or 1.89 +/- 0.33 g cm(-3), depending on whether the stellar radius is estimated from evolutionary models, or from an empirical mass-luminosity relation combined with the light curve parameters. One possible resolution is that the orbit is eccentric (e approximate to 0.14), which would favor the higher density, and hence a much thinner atmosphere for the planet. The transit times were found to be periodic within about 15 s, ruling out the existence of any other super-Earths with periods within a factor of two of the known planet. C1 [Carter, Joshua A.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Carter, Joshua A.; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Carter, Joshua A.; Holman, Matthew J.; Fabrycky, Daniel; Berta, Zachory K.; Burke, Christopher J.; Nutzman, Philip] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabrycky, Daniel; Nutzman, Philip] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Carter, JA (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Carter, Joshua/A-8280-2013; OI Berta-Thompson, Zachory/0000-0002-3321-4924; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA [NNX09AB33G, NAS 5-26555, HF-51267.01-A]; Space Telescope Science Institute; MIT FX We thank G. Torres, D. Charbonneau, and J. Irwin for helpful discussions. We gratefully acknowledge support from the NASA Origins program through award NNX09AB33G and from the MIT class of 1942. J.C. acknowledges partial support for this work provided by NASA through Hubble Fellowship grant 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 38 TC 60 Z9 60 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 APR 1 PY 2011 VL 730 IS 2 AR 82 DI 10.1088/0004-637X/730/2/82 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900022 ER PT J AU Li, ZY Jones, C Forman, WR Kraft, RP Lal, DV Di Stefano, R Spitler, LR Tang, SK Wang, QD Gilfanov, M Revnivtsev, M AF Li, Zhiyuan Jones, Christine Forman, William R. Kraft, Ralph P. Lal, Dharam V. Di Stefano, Rosanne Spitler, Lee R. Tang, Shikui Wang, Q. Daniel Gilfanov, Marat Revnivtsev, Mikhail TI X-RAY EMISSION FROM THE SOMBRERO GALAXY: A GALACTIC-SCALE OUTFLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M 104); galaxies: spiral; X-rays: galaxies; X-rays: ISM ID ELLIPTIC GALAXIES; XMM-NEWTON; HOT GAS; STELLAR POPULATION; INTERSTELLAR-MEDIUM; CHANDRA OBSERVATION; EXTRAPLANAR DUST; NEARBY GALAXIES; POINT SOURCES; S0 GALAXIES AB Based on new and archival Chandra observations of the Sombrero galaxy (M 104 = NGC 4594), we study the X-ray emission from its nucleus and the extended X-ray emission in and around its massive stellar bulge. We find that the 0.3-8 keV luminosity of the nucleus appears constant at similar to 2.4x10(40) erg s(-1), or similar to 10(-7) of its Eddington luminosity, on three epochs between 1999 December and 2008 April, but drops by a factor of two in the 2008 November observation. The 2-6 keV unresolved emission from the bulge region closely follows the K-band starlight and most likely arises from unresolved stellar sources. At lower energies, however, the unresolved emission reaches a galactocentric radius of at least 23 kpc, significantly beyond the extent of the starlight, clearly indicating the presence of diffuse hot gas. We isolate the emission of the gas by properly accounting for the emission from unresolved stellar sources, predominantly cataclysmic variables and coronally active binaries, whose quasi-universal X-ray emissivity was recently established. We find a gas temperature of similar to 0.6 keV with little variation across the field of view, except for a lower temperature of similar to 0.3 keV along the stellar disk. The metal abundance is not well constrained due to the limited counting statistics, but is consistent with metal enrichment by Type Ia supernovae (SNe Ia). We measure a total intrinsic 0.3-2 keV luminosity of similar to 2x10(39) erg s(-1), which corresponds to only 1% of the available energy input by SNe Ia in the bulge, but is comparable to the prediction by the latest galaxy formation models for disk galaxies as massive as Sombrero. However, such numerical models do not fully account for internal feedback processes, such as nuclear feedback and stellar feedback, against accretion from the intergalactic medium. On the other hand, we find no evidence for either the nucleus or the very modest star-forming activities in the disk to be a dominant heating source for the diffuse gas. We also show that neither the expected energy released by SNe Ia nor the expected mass returned by evolved stars is recovered by observations. We argue that in Sombrero a galactic-scale subsonic outflow of hot gas continuously removes much of the "missing" energy and mass input from the bulge region. The observed density and temperature distributions of such an outflow, however, continue to pose challenges to theoretical studies. C1 [Li, Zhiyuan; Jones, Christine; Forman, William R.; Kraft, Ralph P.; Lal, Dharam V.; Di Stefano, Rosanne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spitler, Lee R.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Tang, Shikui; Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Gilfanov, Marat] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Revnivtsev, Mikhail] Tech Univ Munich, D-85748 Garching, Germany. [Revnivtsev, Mikhail] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. RP Li, ZY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zyli@cfa.harvard.edu RI Tang, Shikui/D-9798-2012; Spitler, Lee/A-9867-2013; OI Spitler, Lee/0000-0001-5185-9876; Forman, William/0000-0002-9478-1682 FU SAO [G08-9088] FX Z.L. is grateful for the useful comments by and discussions with Robert Crain, Larry David, Hui Dong, and Dan Harris. This work is supported by the SAO grant G08-9088. NR 97 TC 16 Z9 16 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 APR 1 PY 2011 VL 730 IS 2 AR 84 DI 10.1088/0004-637X/730/2/84 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900024 ER PT J AU Murray-Clay, RA Schlichting, HE AF Murray-Clay, Ruth A. Schlichting, Hilke E. TI USING KUIPER BELT BINARIES TO CONSTRAIN NEPTUNE'S MIGRATION HISTORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; Kuiper Belt: general; planet-disk interactions; planets and satellites: formation ID SIZE DISTRIBUTION; PLANET FORMATION; MINOR PLANETS; SOLAR-SYSTEM; INCLINATION DISTRIBUTION; DYNAMICAL EVOLUTION; CANDIDATE MEMBERS; OBJECTS; ORIGIN; BODIES AB Approximately 10%-20% of all Kuiper Belt objects (KBOs) occupy mean-motion resonances with Neptune. This dynamical configuration likely resulted from resonance capture as Neptune migrated outward during the late stages of planet formation. The details of Neptune's planetesimal-driven migration, including its radial extent and the concurrent eccentricity evolution of the planet, are the subject of considerable debate. Two qualitatively different proposals for resonance capture have been proposed-migration-induced capture driven by smooth outward evolution of Neptune's orbit and chaotic capture driven by damping of the planet's eccentricity near its current semi-major axis. We demonstrate that the distribution of comparable-mass, wide-separation binaries occupying resonant orbits can differentiate between these two scenarios. If migration-induced capture occurred, this fraction records information about the formation locations of different populations of KBOs. Chaotic capture, in contrast, randomizes the orbits of bodies as they are placed in resonance. In particular, if KBO binaries are formed by dynamical capture in a protoplanetary disk with a surface mass density typical of observed extrasolar disks, then migration-induced capture produces the following signatures. The 2: 1 resonance should contain a dynamically cold component, with inclinations less than 5 degrees-10 degrees, having a binary fraction comparable to that among cold classical KBOs. If the 3: 2 resonance also hosts a cold component, its binary fraction should be 20%-30% lower than in the cold classical belt. Among cold 2: 1 (and if present 3: 2) KBOs, objects with eccentricities e < 0.2 should have a binary fraction similar to 20% larger than those with e > 0.2. Other binary formation scenarios and disk surface density profiles can generate analogous signatures but produce quantitatively different results. Searches for cold components in the binary fractions of resonant KBOs are currently practical. The additional migration-generated trends described here may be distinguished with objects discovered by LSST. C1 [Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schlichting, Hilke E.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Murray-Clay, RA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM rmurray-clay@cfa.harvard.edu FU Institute for Theory and Computation Fellowship at Harvard University; Space Telescope Science Institute [HST-HF-51281.01-A]; NASA [NAS 5-26555]; FAS Sciences Division Research Computing Group FX We thank Susan Benecchi and Keith Noll for helpful discussions. We thank Eugene Chiang, Renu Malhotra, and an anonymous referee for comments on the manuscript. R.M.-C. acknowledges support by an Institute for Theory and Computation Fellowship at Harvard University. H.S. is supported by NASA through Hubble Fellowship Grant HST-HF-51281.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contact NAS 5-26555. The simulation in Section 3.2 was run on the Odyssey cluster supported by the FAS Sciences Division Research Computing Group. NR 82 TC 15 Z9 15 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2011 VL 730 IS 2 AR 132 DI 10.1088/0004-637X/730/2/132 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900072 ER PT J AU Orosz, JA Steiner, JF McClintock, JE Torres, MAP Remillard, RA Bailyn, CD Miller, JM AF Orosz, Jerome A. Steiner, James F. McClintock, Jeffrey E. Torres, Manuel A. P. Remillard, Ronald A. Bailyn, Charles D. Miller, Jon M. TI AN IMPROVED DYNAMICAL MODEL FOR THE MICROQUASAR XTE J1550-564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; black hole physics; stars: individual (XTE J1550-564); X-rays: binaries ID QUASI-PERIODIC OSCILLATIONS; BLACK-HOLE; EVOLUTIONARY STATUS; 2000 OUTBURST; GRO J1655-40; OPTICAL OBSERVATIONS; INTERSTELLAR-MEDIUM; ACCRETION DISKS; RADIAL-VELOCITY; XTE-J1550-564 AB We present an improved dynamical model of the X-ray binary and microquasar XTE J1550-564 based on new moderate-resolution optical spectroscopy and near-infrared photometry obtained with the 6.5 m Magellan Telescopes at Las Campanas Observatory. Twelve spectra of the source were obtained using the Magellan Echellette Spectrograph between 2008 May 6 and August 4. In addition, several hundred images of the field were obtained between 2006 May and 2009 July in the J and K-S filters using the PANIC camera. The agreement between the 2006/2007 and 2008 J and K-S light curves is not perfect, and the differences can plausibly be attributed to a hot spot on the accretion disk during the 2006/2007 observations. By combining our new radial velocity measurements with previous measurements obtained in 2001 May at the 8.2 m Very Large Telescope and with light curves, we find an orbital period of P = 1.5420333 +/- 0.0000024 days and a radial velocity semiamplitude of K-2 = 363.14 +/- 5.97 km s(-1), which together imply an optical mass function of integral(M) = 7.65 +/- 0.38M(circle dot). We find that the projected rotational velocity of the secondary star is 55 +/- 5 km s(-1), which implies a very extreme mass ratio of Q M/M-2 approximate to 30. Using a model of a Roche lobe-filling star and an azimuthally symmetric accretion disk, we fit simultaneously optical light curves from 2001, near-infrared light curves from 2008, and all of the radial velocity measurements to derive system parameters. We find an inclination of 74 degrees.7 +/- 3 degrees.8 and component masses of M-2 = 0.30 +/- 0.07M(circle dot) and M = 9.10 +/- 0.61M(circle dot) for the secondary star and black hole, respectively. We note that these results depend on the assumption that in 2008, the disk did not have a hot spot, and that the fraction of light contributed by the accretion disk did not change between the spectroscopic and photometric observations. By considering two measured values of the disk fraction and by modeling various combinations of NIR and optical light curves, we show that our adopted black hole mass is probably not seriously in error, where the black hole mass ranges between M = 8.91 +/- 1.10M(circle dot) and M = 13.94 +/- 1.64M(circle dot). The radius of the secondary star for the adopted model is 1.75 +/- 0.12R(circle dot). Using this radius, the average K-S magnitude, and an extinction of A(K) = 0.507 +/- 0.050 mag, we find a distance of 4.38(-0.41)(+0.58) kpc, which is in good agreement with a recent distance estimate based on HI absorption lines. C1 [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Steiner, James F.; McClintock, Jeffrey E.; Torres, Manuel A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bailyn, Charles D.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Orosz, JA (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. EM orosz@sciences.sdsu.edu; jsteiner@cfa.harvard.edu; jem@cfa.harvard.edu; mtorres@cfa.harvard.edu; rr@space.mit.edu; charles.bailyn@yale.edu; jonmm@umich.edu FU National Aeronautics and Space Administration [NNX08AJ55G]; National Science Foundation [AST-0808145, AST-0707627]; Smithsonian Institution FX We thank Danny Steeghs for the use of telescope time at LCO. J.F.S. thanks Paul Martini for his gracious support with the PANIC pipeline. 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 work of J.A.O. was supported in part by the National Science Foundation grant AST-0808145. C.B.D. gratefully acknowledges support from the National Science Foundation grant AST-0707627. The work of J.E.M. was supported in part by NASA grant NNX08AJ55G. J.F.S. was supported by Smithsonian Institution Endowment Funds. R.R. acknowledges support from NASA via the contract for the instrument team of RXTE at MIT. NR 60 TC 56 Z9 56 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 APR 1 PY 2011 VL 730 IS 2 AR 75 DI 10.1088/0004-637X/730/2/75 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900015 ER PT J AU Perets, HB Badenes, C Arcavi, I Simon, JD Gal-Yam, A AF Perets, Hagai B. Badenes, Carles Arcavi, Iair Simon, Joshua D. Gal-Yam, Avishay TI AN EMERGING CLASS OF BRIGHT, FAST-EVOLVING SUPERNOVAE WITH LOW-MASS EJECTA SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (1885A, 1939B, 2002bj); white dwarfs ID X-RAY-EMISSION; SPACE-TELESCOPE IMAGES; IA SUPERNOVAE; S-ANDROMEDAE; SHOCKED EJECTA; LIGHT CURVES; WHITE-DWARFS; HELIUM; REMNANT; EXPLOSION AB A recent analysis of supernova (SN) 2002bj revealed that it was an apparently unique type Ib SN. It showed a high peak luminosity, with absolute magnitude M-R similar to -18.5, but an extremely fast-evolving light curve. It had a rise time of < 7 days followed by a decline of 0.25 mag day(-1) in B band and showed evidence for very low mass of ejecta (< 0.15 M-circle dot). Here we discuss two additional historical events, SN 1885A and SN 1939B, showing similarly fast light curves and low ejected masses. We discuss the low mass of ejecta inferred from our analysis of the SN 1885A remnant in M31 and present for the first time the spectrum of SN 1939B. The old environments of both SN 1885A (in the bulge of M31) and SN 1939B (in an elliptical galaxy with no traces of star formation activity) strongly support old white dwarf (WD) progenitors for these SNe. We find no clear evidence for helium in the spectrum of SN 1939B, as might be expected from a helium-shell detonation on a WD, suggested to be the origin of SN 2002bj. Finally, the discovery of all the observed fast-evolving SNe in nearby galaxies suggests that the rate of these peculiar SNe is at least 1%-2% of all SNe. C1 [Perets, Hagai B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Badenes, Carles; Arcavi, Iair; Gal-Yam, Avishay] Weizmann Inst Sci, Fac Phys, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Badenes, Carles] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Simon, Joshua D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Perets, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hperets@cfa.harvard.edu RI Perets, Hagai/K-9605-2015; OI Perets, Hagai/0000-0002-5004-199X; Badenes, Carles/0000-0003-3494-343X; Gal-Yam, Avishay/0000-0002-3653-5598 FU Israeli Science Foundation; EU; Peter and Patricia Gruber Awards; Weizmann Minerva program; Benoziyo Center for Astrophysics FX We thank Steve Reynolds, Zhiyuan Li, Mike Garcia, and Eduardo Bravo for helpful discussions and data on SNR 1885A. We thank Dovi Poznanski and Ryan Chornock for helpful discussions about fast SNe and data on SN 2002bj. We also thank John Grula, George Carlson, Wal Sargent, Hy Spinrad, Ivan King, Donna Kirkpatrick, Francois Schweizer, George Preston, Andy McWilliam, Doug Mink, and Bob Kirshner for helping with locating, reducing, and analyzing the original spectroscopic plate of SN 1939B. We also thank the anonymous referee, and the second referee, David Branch, for their helpful comments. H.B.P. is a CfA and BIKURA (FIRST) fellow. A.G. is supported by grants from the Israeli Science Foundation, an EU FP7 Marie Curie IRG Fellowship, a research grant from the Peter and Patricia Gruber Awards, the Weizmann Minerva program, and the Benoziyo Center for Astrophysics. NR 57 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 APR 1 PY 2011 VL 730 IS 2 AR 89 DI 10.1088/0004-637X/730/2/89 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900029 ER PT J AU Riess, AG Macri, L Casertano, S Lampeitl, H Ferguson, HC Filippenko, AV Jha, SW Li, WD Chornock, R AF Riess, Adam G. Macri, Lucas Casertano, Stefano Lampeitl, Hubert Ferguson, Henry C. Filippenko, Alexei V. Jha, Saurabh W. Li, Weidong Chornock, Ryan TI A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE AND WIDE FIELD CAMERA 3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmological parameters; dark energy; distance scale; galaxies: distances and redshifts; stars: variables: Cepheids; supernovae: general ID LARGE-MAGELLANIC-CLOUD; PERIOD-LUMINOSITY RELATIONS; EXTRAGALACTIC DISTANCE SCALE; ACTIVE GALAXY NGC-4258; IA SUPERNOVAE; LIGHT CURVES; FUNDAMENTAL PROPERTIES; CEPHEID CALIBRATION; GEOMETRIC DISTANCE; ECLIPSING BINARIES AB We use the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST) to determine the Hubble constant from optical and infrared observations of over 600 Cepheid variables in the host galaxies of eight recent Type Ia supernovae (SNe Ia), providing the calibration for a magnitude-redshift relation based on 253 SNe Ia. Increased precision over past measurements of the Hubble constant comes from five improvements: (1) more than doubling the number of infrared observations of Cepheids in the nearby SN hosts; (2) increasing the sample size of ideal SN Ia calibrators from six to eight; (3) increasing by 20% the number of Cepheids with infrared observations in the megamaser host NGC 4258; (4) reducing the difference in the mean metallicity of the Cepheid comparison samples between NGC 4258 and the SN hosts from Delta log [O/H] = 0.08 to 0.05; and (5) calibrating all optical Cepheid colors with a single camera, WFC3, to remove cross-instrument zero-point errors. The result is a reduction in the uncertainty in H-0 due to steps beyond the first rung of the distance ladder from 3.5% to 2.3%. The measurement of H-0 via the geometric distance to NGC 4258 is 74.8 +/- 3.1 km s(-1) Mpc(-1), a 4.1% measurement including systematic uncertainties. Better precision independent of the distance to NGC 4258 comes from the use of two alternative Cepheid absolute calibrations: (1) 13 Milky Way Cepheids with trigonometric parallaxes measured with HST/fine guidance sensor and Hipparcos and (2) 92 Cepheids in the Large Magellanic Cloud for which multiple accurate and precise eclipsing binary distances are available, yielding 74.4 +/- 2.5 km s(-1) Mpc(-1), a 3.4% uncertainty including systematics. Our best estimate uses all three calibrations but a larger uncertainty afforded from any two: H-0 = 73.8 +/- 2.4 km s(-1) Mpc(-1) including systematic errors, corresponding to a 3.3% uncertainty. The improved measurement of H-0, when combined with the Wilkinson Microwave Anisotropy Probe (WMAP) 7 year data, results in a tighter constraint on the equation-of-state parameter of dark energy of w = -1.08 +/- 0.10. It also rules out the best-fitting gigaparsec-scale void models, posited as an alternative to dark energy. The combined H-0 + WMAP results yield N-eff = 4.2 +/- 0.7 for the number of relativistic particle species in the early universe, a low-significance excess for the value expected from the three known neutrino flavors. C1 [Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, Adam G.; Casertano, Stefano; Ferguson, Henry C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Macri, Lucas] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Lampeitl, Hubert] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Filippenko, Alexei V.; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Riess, AG (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM ariess@stsci.edu OI Macri, Lucas/0000-0002-1775-4859 FU NASA through Space Telescope Science Institute [GO-11570, GO-10802, NAS 5-26555]; NSF [AST-0607485]; TABASGO Foundation; Texas AM University; W. M. Keck Foundation FX We are grateful to William Januszewski for his help in executing this program on HST. We are indebted to Mike Hudson for assisting with the peculiar-velocity calculations from the PSCz survey, to David Larson for contributions to the WMAP MCMC analysis, to Daniel Scolnic for donating some useful routines, and to Mark Huber for an analysis of pre-discovery observations of SN 2007sr. Financial support for this work was provided by NASA through programs GO-11570 and GO-10802 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. A.V.F.'s supernova group at U. C. Berkeley is also supported by NSF grant AST-0607485 and by the TABASGO Foundation. L. M. acknowledges support from a Texas A&M University faculty startup fund. The metallicity measurements for NGC 5584 and NGC 4038/9 presented herein were obtained with 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. We thank Chris Kochanek and Kris Stanek for their support of GO-11570. NR 78 TC 764 Z9 765 U1 4 U2 38 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 APR 1 PY 2011 VL 730 IS 2 AR 119 DI 10.1088/0004-637X/730/2/119 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735TR UT WOS:000288441900059 ER PT J AU Hirsch, BT AF Hirsch, Ben T. TI Spatial position and feeding success in ring-tailed coatis SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Coati; Social foraging; Dominance; Within-group spatial position; Food depletion; Feeding competition; Predation ID MACAQUES MACACA-FASCICULARIS; MONKEYS CEBUS-CAPUCINUS; BROWN CAPUCHIN MONKEYS; ROACH RUTILUS-RUTILUS; NASUA-NASUA; FORAGING GROUPS; GOOSE FLOCKS; HOME-RANGE; ATLANTIC FOREST; FOOD DETECTION AB The location of an animal within a social group has important effects on feeding success. When animals consume quickly eaten food items, individuals located at the front edge of a group typically have greater foraging success. When groups feed at large clumped resources, dominant individuals can often monopolize the resource, leading to higher feeding success in the center of the group. In order to test these predictions, behavioral data relating foraging success to within-group spatial position were recorded from two habituated groups of ring-tailed coatis (Nasua nasua) in Iguazu, Argentina. Foraging success did not fit expected patterns. When feeding on small ground litter invertebrates, coatis had the same foraging success at all spatial positions. This pattern likely resulted from an abundance of invertebrates in the ground litter. When feeding on fruit, individuals in the front of the group had greater feeding success, which was driven by the relatively quick depletion of fruit trees. Dominant juveniles were often located in the front of the group which led to increased access to food. This resulted in higher feeding success on fruits but simultaneously increased their risk of predation. Although groups typically became more elongated and traveled faster when feeding on fruit, it did not appear that the coatis were drastically changing their spacing strategies when switching between the two food types. Paradoxically, spatial position preferences during invertebrate foraging appeared to be driven by fruit trees. Because fruit trees were encountered so frequently, juveniles ranging at the front edge of the group during invertebrate foraging were the first to arrive at fruit trees and thus had higher foraging success. This study demonstrates the importance of how food patch size and depletion rate affect the spatial preferences of individuals. C1 [Hirsch, Ben T.] Smithsonian Trop Res Inst, Unit 9100, Dpo Aa 340029898, Barro Colorado, Panama. [Hirsch, Ben T.] New York State Museum & Sci Serv, Albany, NY 12230 USA. RP Hirsch, BT (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948, Dpo Aa 340029898, Barro Colorado, Panama. EM hirschb@si.edu FU National Science Fund [BCS-0314525] FX I would like to thank Yamil Di Blanco, Santiago Escobar, Carolina Ferrari, Fermino Silva, and Mauro Tammone for help and assistance during the course of the field work. I would also like to thank Viviana Munoz for her veterinary assistance. I am particularly grateful to Charles Janson for the immeasurable amount of advice he gave me during all aspects of this project, and letting me borrow several pieces of much needed field equipment. I am also very thankful for the consistently helpful comments and advice from Mario Di Bitetti. This paper has benefited tremendously thanks to comments by Matt Gompper, Charles Janson, Andreas Koenig, and Diane Doran-Sheehy. I thank the APN for permission to carry out work in Iguazu. This study was funded in part by a National Science Fund grant (BCS-0314525). NR 45 TC 13 Z9 13 U1 5 U2 42 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD APR PY 2011 VL 65 IS 4 BP 581 EP 591 DI 10.1007/s00265-010-1058-1 PG 11 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 735VH UT WOS:000288448000003 ER PT J AU Carvalho, JC Cardoso, P Crespo, LC Henriques, S Carvalho, R Gomes, P AF Carvalho, Jose C. Cardoso, Pedro Crespo, Luis C. Henriques, Sergio Carvalho, Rui Gomes, Pedro TI Biogeographic patterns of spiders in coastal dunes along a gradient of mediterraneity SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Biogeography; Mediterranean; Iberian Peninsula; Coastal dunes; Indicator species; Spiders ID SPECIES RICHNESS; IBERIAN PENINSULA; GREY DUNES; ARANEAE; DIVERSITY; CONSERVATION; BIODIVERSITY; NESTEDNESS; FOREST; BIOINDICATION AB The Iberian Peninsula is recognized for its high levels of species richness, rarity and endemicity. Our main aim was to study biogeographic patterns of spiders in coastal dunes along a gradient of mediterraneity. Distance-decay of similarity, nestedness and co-occurrence metrics were used to explore spider' distribution patterns. A similarity analysis was performed in order to obtain a hierarchical classification of sites. Indicator species analysis was conducted to identify indicator species for the various clustering levels of the site typology. The differentiation among assemblages was further explored by non-metric multidimensional scaling (NMDS) and analysis of similarities (ANOSIM). Assemblages' similarity among sites decreased with climatic/geographic distance. The observed values of nestedness metrics (T and NODF) were not significant, while the co-occurrence metrics (C-score and Checkerboard units) were higher than expected by chance. Cluster analysis showed that spider' assemblages were structured along a gradient from North to South, forming four geographically distinct clusters. ANOSIM tests and NMDS supported the biogeographic patterns identified by cluster analysis. Several indicator species were found for the different levels of the hierarchic site typology. Spider assemblages revealed a high degree of biogeographical structure along the Atlantic coast of the Iberian Peninsula. The coast is a "biogeographic crossroad", encompassing faunistic elements of different origins. The hierarchic typology of sites is generally consistent with the major biogeographic regions and the thermoclimatic belts recognized for the region. Our results indicate that the climatic gradient and historic factors played a key role in the current spiders' biogeographic patterns. C1 [Carvalho, Jose C.; Gomes, Pedro] Univ Minho, Dept Biol, CBMA Mol & Environm Ctr, P-4710057 Braga, Portugal. [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Cardoso, Pedro; Crespo, Luis C.] Univ Azores, Azorean Biodivers Grp CITA A, Angra Do Heroismo, Portugal. [Henriques, Sergio; Carvalho, Rui] Univ Evora, Dept Biol, Evora, Portugal. RP Carvalho, JC (reprint author), Univ Minho, Dept Biol, CBMA Mol & Environm Ctr, Gualtar Campus, P-4710057 Braga, Portugal. EM josecarvalho@bio.uminho.pt RI Cardoso, Pedro/A-8820-2008; Gomes, Pedro/I-8348-2015 OI Cardoso, Pedro/0000-0001-8119-9960; Gomes, Pedro/0000-0002-5595-6988 FU Luso-American Foundation; Fundacao para a Ciencia e Tecnologia [SFRH/BPD/40688/2007] FX We are acknowledged to Jose Antonio Barrientos, Carmen Urones and Stano Pekar for their help with the taxonomic identification of some spider specimens and to Robert Bosmans and Hisham El-Hennawy for their contribution to identify Mediterranean species that occur in Northern Africa. J.C.C. express his gratitude to the Luso-American Foundation for its support (FLAD CandT Links 2010 grant). P.C. is supported by Fundacao para a Ciencia e Tecnologia (SFRH/BPD/40688/2007). NR 60 TC 8 Z9 9 U1 1 U2 31 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 EI 1572-9710 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD APR PY 2011 VL 20 IS 4 BP 873 EP 894 DI 10.1007/s10531-011-0001-8 PG 22 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 737GB UT WOS:000288556000012 ER PT J AU Endara, MJ Coley, PD AF Endara, Maria-Jose Coley, Phyllis D. TI The resource availability hypothesis revisited: a meta-analysis SO FUNCTIONAL ECOLOGY LA English DT Article DE habitat resources; herbivory; meta-analysis; plant apparency; plant defences; plant defence theory; plant growth; resource availability hypothesis ID PLANT DEFENSE; INSECT HERBIVORES; INDUCED RESISTANCE; CHEMICAL DEFENSES; RAIN-FORESTS; PHENOLICS; GROWTH; CHEMISTRY; ECOLOGY; HABITAT AB P>1. Several theories have provided a framework for understanding variation in plant defence against herbivores. Among them, the plant apparency theory and the resource availability hypothesis (RAH) have aimed to explain the patterns of defence investment and the selective pressures that have led to the variety of defensive strategies across species. Here we provide a historical review of both theories, present evidence that shaped their development and contrast their predictions. 2. We present the results of a meta-analysis of the utility of the RAH 25 years after it was proposed and compare it to apparency theory. We performed a meta-analysis of 50 studies that have examined plant growth, defences and herbivory in relation to resource availability across latitude and ontogeny. Specifically, we tested four predictions that follow the RAH: (i) species adapted to resource-rich environments have intrinsically faster growth rates than species adapted to resource-poor environments; (ii) fast-growing species have shorter leaf lifetimes than slow-growing species; (iii) fast-growing species have lower amounts of constitutive defences than slow-growing species; and (iv) fast-growing species support higher herbivory rates than slow-growing species. 3. Our results confirm the predictions that species adapted to resource-poor environments grow inherently more slowly, invest more in constitutive defences and support lower herbivory than species from more productive habitats. Our data also showed that variation in growth rate among species better explains the differences in herbivory than variation in apparency, suggesting that the evolution of different defensive strategies across species is resource, rather than herbivore driven. We also found that the application of this theory appears robust across latitude and ontogeny, as the magnitude of the effect sizes for most of the predictions did not vary significantly between ecosystems or across ontogenic stages. 4. We conclude that the RAH has served as a valid framework for investigating the patterns of plant defences and that its applicability is quite general. C1 [Endara, Maria-Jose; Coley, Phyllis D.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Endara, Maria-Jose] Pontificia Univ Catolica Ecuador, Herbario QCA, Dept Ciencias Biol, Quito, Ecuador. [Coley, Phyllis D.] Smithsonian Trop Res Inst, Balboa, Panama. RP Endara, MJ (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. EM majo.endara@utah.edu NR 73 TC 37 Z9 37 U1 24 U2 192 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD APR PY 2011 VL 25 IS 2 BP 389 EP 398 DI 10.1111/j.1365-2435.2010.01803.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 736NJ UT WOS:000288501100009 ER PT J AU Stinchcomb, GE Messner, TC Driese, SG Nordt, LC Stewart, RM AF Stinchcomb, G. E. Messner, T. C. Driese, S. G. Nordt, L. C. Stewart, R. M. TI Pre-colonial (AD 1100-1600) sedimentation related to prehistoric maize agriculture and climate change in eastern North America SO GEOLOGY LA English DT Article ID NEW-YORK; MULTIPROXY EVIDENCE; LATE-HOLOCENE; RIVER VALLEY; ICE-AGE; USA; VARIABILITY; PHYTOLITHS; LANDSCAPE; ONTARIO AB Despite the importance of understanding the effect of land use on floodplains in eastern North America, few studies have directly addressed the possibility and extent of prehistoric indigenous land use on floodplain development. Here we report geoarchaeological evidence of increasing floodplain sedimentation and prehistoric land-use intensification in the Delaware River Valley (eastern United States) during the Medieval Climate Anomaly-Little Ice Age transition. The evidence of this anthropogenic sedimentation event, documented throughout eastern North America, is designated here as pre-colonial sediment (PCS), ca. A. D. 1100-1600. The data demonstrate that the combined effects of prehistoric land use and climate change affected eastern North American floodplain development several hundred years prior to the onset of major European settlement. C1 [Stinchcomb, G. E.; Driese, S. G.; Nordt, L. C.] Baylor Univ, Terr Paleoclimatol Res Grp, Dept Geol, Waco, TX 76798 USA. [Messner, T. C.] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20560 USA. [Messner, T. C.] Ctr Amer Archaeol, Kampsville, IL 62053 USA. [Stewart, R. M.] Temple Univ, Dept Anthropol, Philadelphia, PA 19122 USA. RP Stinchcomb, GE (reprint author), Baylor Univ, Terr Paleoclimatol Res Grp, Dept Geol, Waco, TX 76798 USA. EM gary_stinchcomb@baylor.edu OI Stinchcomb, Gary/0000-0003-3220-7762 FU U.S. National Park Service; Temple University; Baylor University Geology Department; GSA; National Science Foundation [EAR-0823131] FX This study received support from the U.S. National Park Service, Temple University, Baylor University Geology Department, GSA Student Grants-in-Aid-of-Research, and National Science Foundation grant EAR-0823131 awarded to Driese. We thank Zheng-Hua Li and Sally Horn at the University of Tennessee, Knoxville; the Department of Geography and Geology at the University of Wisconsin Stevens Point; and Peter Allen, Jason Mintz, and Erin Stinchcomb at Baylor University, and Noel Strattan at PHMC for field and lab assistance. Three anonymous reviewers provided helpful comments and suggestions that greatly improved an earlier version of the manuscript. NR 45 TC 19 Z9 19 U1 1 U2 15 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD APR PY 2011 VL 39 IS 4 BP 363 EP 366 DI 10.1130/G31596.1 PG 4 WC Geology SC Geology GA 736PT UT WOS:000288507300019 ER PT J AU Falcon-Lang, HJ Jud, NA Nelson, WJ DiMichele, WA Chaney, DS Lucas, SG AF Falcon-Lang, Howard J. Jud, Nathan A. Nelson, W. John DiMichele, William A. Chaney, Dan S. Lucas, Spencer G. TI Pennsylvanian coniferopsid forests in sabkha facies reveal the nature of seasonal tropical biome SO GEOLOGY LA English DT Article AB Pennsylvanian fossil forests are known from hundreds of sites across tropical Pangea, but nearly all comprise remains of humid Coal Forests. Here we report a unique occurrence of seasonally dry vegetation, preserved in growth position along >5 km of strike, in the Pennsylvanian (early Kasimovian, Missourian) of New Mexico (United States). Analyses of stump anatomy, diameter, and spatial density, coupled with observations of vascular traces and associated megaflora, show that this was a deciduous, mixed-age, coniferopsid woodland (similar to 100 trees per hectare) with an open canopy. The coniferopsids colonized coastal sabkha facies and show tree rings, confirming growth under seasonally dry conditions. Such woodlands probably served as the source of coniferopsids that replaced Coal Forests farther east in central Pangea during drier climate phases. Thus, the newly discovered woodland helps unravel biome-scale vegetation dynamics and allows calibration of climate models. C1 [Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Surrey TW20 0EX, England. [Jud, Nathan A.] Univ Maryland, College Pk, MD 20742 USA. [Nelson, W. John] Illinois State Geol Survey, Champaign, IL 61820 USA. [DiMichele, William A.; Chaney, Dan S.] Natl Museum Nat Hist, Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Lucas, Spencer G.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. RP Falcon-Lang, HJ (reprint author), Univ London, Dept Earth Sci, Surrey TW20 0EX, England. EM h.falcon-lang@es.rhul.ac.uk RI Falcon-Lang, Howard/D-8465-2011; DiMichele, William/K-4301-2012 FU Natural Environment Research Council (UK) [NE/F014120/2]; Smithsonian Institution Endowment program; National Museum of Natural History Small Grants Program FX Falcon-Lang acknowledges a Natural Environment Research Council (UK) Advanced Postdoctoral Fellowship (NE/F014120/2). DiMichele, Chaney, and Nelson acknowledge support from the Smithsonian Institution Endowment program and National Museum of Natural History Small Grants Program. NR 24 TC 32 Z9 32 U1 0 U2 10 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD APR PY 2011 VL 39 IS 4 BP 371 EP 374 DI 10.1130/G31764.1 PG 4 WC Geology SC Geology GA 736PT UT WOS:000288507300021 ER PT J AU Wall, AJ Heaney, PJ Mathur, R Post, JE Hanson, JC Eng, PJ AF Wall, Andrew J. Heaney, Peter J. Mathur, Ryan Post, Jeffrey E. Hanson, Jonathan C. Eng, Peter J. TI A flow-through reaction cell that couples time-resolved X-ray diffraction with stable isotope analysis SO JOURNAL OF APPLIED CRYSTALLOGRAPHY LA English DT Article DE powder X-ray diffraction; synchrotron; time-resolved; Cu isotopes; copper sulfides; chalcocite; covellite; flow-through reaction cells ID NICKEL LATERITE ORES; ION-EXCHANGE; POWDER DIFFRACTION; FRACTIONATION; CU; ENVIRONMENT; MECHANISM; KINETICS; ORIGIN; COPPER AB A non-metallic flow-through reaction cell is described, designed for in situ time-resolved X-ray diffraction coupled with stable isotope analysis. The experimental setup allows the correlation of Cu isotope fractionation with changes in crystal structure during copper sulfide dissolution. This flow-through cell can be applied to many classes of fluid-mineral reactions that involve dissolution or ion exchange. 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. [Hanson, Jonathan C.] Brookhaven Natl Lab, Dept Chem, Upton, NY 11973 USA. [Eng, Peter J.] Univ Chicago, Consortium Adv Radiat Sources, Chicago, IL 60637 USA. RP Wall, AJ (reprint author), Penn State Univ, Dept Geosci, 542 Deike Bldg, University Pk, PA 16802 USA. EM awall@psu.edu RI mathur, ryan/A-5278-2010 FU NSF [EAR07-45374]; Center for Environmental Kinetics Analysis (CEKA); DOE-sponsored Environmental Molecular Science Institute [NSF CHE04-31328]; Mineralogical Society of America; Geological Society of America; US Department of Energy, Division of Materials Sciences and Division of Chemical Sciences [DE-AC02-98CH10886]; US Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357] FX Funding for this research was provided by NSF grant No. 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 a Geological Society of America Graduate Student Research Grant. This research was carried out at two synchrotron sources, the National Synchrotron Light Source, Brookhaven National Laboratory, which is supported by the US Department of Energy, Division of Materials Sciences and Division of Chemical Sciences, under contract No. DE-AC02-98CH10886, and the Advanced Photon Source at Argonne National Laboratory, which is supported by the US Department of Energy, Office of Science, Office of Basic Energy Sciences, under contract No. DE-AC02-06CH11357. NR 23 TC 12 Z9 12 U1 0 U2 17 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0021-8898 J9 J APPL CRYSTALLOGR JI J. Appl. Crystallogr. PD APR PY 2011 VL 44 BP 429 EP 432 DI 10.1107/S0021889811000525 PN 2 PG 4 WC Chemistry, Multidisciplinary; Crystallography SC Chemistry; Crystallography GA 739YQ UT WOS:000288758500023 ER PT J AU Berry, RP Wcislo, WT Warrant, EJ AF Berry, Richard P. Wcislo, William T. Warrant, Eric J. TI Ocellar adaptations for dim light vision in a nocturnal bee SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE ocelli; bee; nocturnal vision; sensitivity; polarisation sensitivity; spectral sensitivity; response dynamics ID DRAGONFLY MEDIAN OCELLUS; LARGE 2ND-ORDER NEURONS; INSECT DORSAL OCELLI; FLYING SWEAT BEES; MEGALOPTA-GENALIS; NEURAL ORGANIZATION; FUNCTIONAL DIVERSITY; GRADED POTENTIALS; OPTICAL ANALYSIS; VISUAL-SYSTEM AB Growing evidence indicates that insect ocelli are strongly adapted to meet the specific functional requirements in the environment in which that insect lives. We investigated how the ocelli of the nocturnal bee Megalopta genalis are adapted to life in the dim understory of a tropical rainforest. Using a combination of light microscopy and three-dimensional reconstruction, we found that the retinae contain bar-shaped rhabdoms loosely arranged in a radial pattern around multi-layered lenses, and that both lenses and retinae form complex non-spherical shapes reminiscent of those described in other ocelli. Intracellular electrophysiology revealed that the photoreceptors have high absolute sensitivity, but that the threshold location varied widely between 109 and 10(11) photons cm(-2) s(-1). Higher sensitivity and greater visual reliability may be obtained at the expense of temporal resolution: the corner frequencies of dark-adapted ocellar photoreceptors were just 4-11 Hz. Spectral sensitivity profiles consistently peaked at 500 nm. Unlike the ocelli of other flying insects, we did not detect UV-sensitive visual pigments in M. genalis, which may be attributable to a scarcity of UV photons under the rainforest canopy at night. In contrast to earlier predictions based on anatomy, the photoreceptors are not sensitive to the e-vector of polarised light. Megalopta genalis ocellar photoreceptors possess a number of unusual properties, including inherently high response variability and the ability to produce spike-like potentials. These properties bear similarities to photoreceptors in the compound eye of the cockroach, and we suggest that the two insects share physiological characteristics optimised for vision in dim light. C1 [Warrant, Eric J.] Lund Univ, Dept Cell & Organism Biol, S-22350 Lund, Sweden. [Berry, Richard P.] Australian Natl Univ, Ctr Visual Sci, Sch Biol, Canberra, ACT 2600, Australia. [Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama. RP Warrant, EJ (reprint author), Lund Univ, Dept Cell & Organism Biol, Solvegatan 35, S-22350 Lund, Sweden. EM eric.warrant@cob.lu.se FU Air Force Office of Scientific Research [FA 4869, FA8655-07-C-4011]; Royal Physiographic Society of Lund; Swedish Research Council FX This work would not have been possible without the help of Drs Rikard Frederiksen, Eva Kreiss and Henrik Malm, who assisted with the collection of bees and various other administrative and technical matters. We would also like to thank the staff of the Smithsonian Tropical Research Institute, in particular Dr Simon Tierney for his extensive help. We are also grateful to the Autoridad Nacional del Ambiente of the Republic of Panama for permission to export bees (permit no. SEX/A-25-09). We would like to thank the Air Force Office of Scientific Research (contracts FA 4869 and FA8655-07-C-4011), the Royal Physiographic Society of Lund and the Swedish Research Council for funding this work. NR 62 TC 13 Z9 13 U1 2 U2 27 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD APR PY 2011 VL 214 IS 8 BP 1283 EP 1293 DI 10.1242/jeb.050427 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 739EO UT WOS:000288696500014 PM 21430205 ER PT J AU Suarez-Rubio, M Leimgruber, P Renner, SC AF Suarez-Rubio, Marcela Leimgruber, Peter Renner, Swen C. TI Influence of exurban development on bird species richness and diversity SO JOURNAL OF ORNITHOLOGY LA English DT Article DE Community response land cover; Land-use change; Rural sprawl; Urban fringe; Eastern deciduous forest ID ESTIMATING SITE OCCUPANCY; LAND-USE; UNITED-STATES; URBAN GRADIENT; RESIDENTIAL DEVELOPMENT; BIOTIC HOMOGENIZATION; HOUSING DEVELOPMENTS; AVIAN ASSEMBLAGES; HUMAN SETTLEMENT; BREEDING BIRDS AB Exurban development is an accelerating land use trend in the United States with new housing units emerging in formerly closed forests. Conservation practitioners and planners suspect exurban development alters ecological processes and biodiversity to a considerable larger extent than suspected by inhabitants of exurban development areas, but empirical support for this assertion is lacking. To examine the consequences of exurban development, we studied forest bird communities in exurban development and forests located in and around Shenandoah National Park and Massanutten Mountain in northern Virginia, USA. We conducted point-count surveys for birds three times at 106 sample locations from April to July 2006. We recorded 44 species in total; 30 species were present in both exurban development and forests, 9 species were only found in exurban development, and 5 species only in forest. Bird species composition differed significantly between land-use types based on analysis in a multi-response permutation procedure (MRPP; P < 0.01). Relative bird abundance for forest specialist species changed significantly in exurban development versus forest (t test, P < 0.05). Three species, American Robin Turdus migratorius, Northern Cardinal Cardinalis cardinalis, and Common Grackle Quiscalus quiscula were indicators of exurban development. Indicators of forest were Carolina Chickadee Poecile carolinensis, Eastern Towhee Pipilo erythrophthalmus, and Wood Thrush Hylocichla mustelina. Our study demonstrates that exurban development alters bird community composition and relative abundance of forest specialist species. C1 [Suarez-Rubio, Marcela] Univ Maryland, Ctr Environm Sci, Appalachian Lab, Frostburg, MD 21532 USA. [Leimgruber, Peter; Renner, Swen C.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Renner, Swen C.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. RP Suarez-Rubio, M (reprint author), Univ Maryland, Ctr Environm Sci, Appalachian Lab, 301 Braddock Rd, Frostburg, MD 21532 USA. EM msuarez@umces.edu; swen.renner@uni-ulm.de RI Renner, Swen/J-3502-2014; Leimgruber, Peter/O-1304-2015; OI Renner, Swen/0000-0002-6893-4219; Leimgruber, Peter/0000-0002-3682-0153; Suarez-Rubio, Marcela/0000-0002-0596-2626 FU Smithsonian's Conservation and Research Center GIS Lab FX We would like to thank Todd Lookingbill and two unknown reviewers for providing critical comments on previous versions of the manuscript. Our special thanks goes to the High Knob Owners Association (especially Kay Clement and Marcy McCann) for organizing access to the facility and contact to the citizens, who always welcomed us and allowed data collection in their community, talked about the regional and High Knob area history, and provided coffee in the 'Bagels-Bunch group' discussions. Jennifer Buff facilitated contacts to Warren County administration for data on exurban development in the county. Gary Somers of The National Park Service, Shenandoah National Park (permit #: SHEN-2006-SCI-0009), and James T Smalls (Forest Ranger of Massanutten Mountain/George Washington and Jefferson National Forests) provided further valuable information and permits to establish the forest point counts for our study. The study was supported with funds from the Smithsonian's Conservation and Research Center GIS Lab. NR 80 TC 14 Z9 15 U1 1 U2 60 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0021-8375 EI 1439-0361 J9 J ORNITHOL JI J. Ornithol. PD APR PY 2011 VL 152 IS 2 BP 461 EP 471 DI 10.1007/s10336-010-0605-x PG 11 WC Ornithology SC Zoology GA 735EI UT WOS:000288395800028 ER PT J AU Kim, S Bachvaroff, TR Handy, SM Delwiche, CF AF Kim, Sunju Bachvaroff, Tsvetan R. Handy, Sara M. Delwiche, Charles F. TI Dynamics of Actin Evolution in Dinoflagellates SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE actin; birth-and-death evolution; dinoflagellate; phylogeny; Dinophysis; dinokaryon ID MULTIGENE FAMILY; CONCERTED EVOLUTION; MAXIMUM-LIKELIHOOD; GENOME SEQUENCE; BINDING-PROTEIN; DEATH EVOLUTION; OXYRRHIS-MARINA; KARENIA-BREVIS; GENES; DINOPHYSIS AB Dinoflagellates have unique nuclei and intriguing genome characteristics with very high DNA content making complete genome sequencing difficult. In dinoflagellates, many genes are found in multicopy gene families, but the processes involved in the establishment and maintenance of these gene families are poorly understood. Understanding the dynamics of gene family evolution in dinoflagellates requires comparisons at different evolutionary scales. Studies of closely related species provide fine-scale information relative to species divergence, whereas comparisons of more distantly related species provides broad context. We selected the actin gene family as a highly expressed conserved gene previously studied in dinoflagellates. Of the 142 sequences determined in this study, 103 were from the two closely related species, Dinophysis acuminata and D. caudata, including full length and partial cDNA sequences as well as partial genomic amplicons. For these two Dinophysis species, at least three types of sequences could be identified. Most copies (79%) were relatively similar and in nucleotide trees, the sequences formed two bushy clades corresponding to the two species. In comparisons within species, only eight to ten nucleotide differences were found between these copies. The two remaining types formed clades containing sequences from both species. One type included the most similar sequences in between-species comparisons with as few as 12 nucleotide differences between species. The second type included the most divergent sequences in comparisons between and within species with up to 93 nucleotide differences between sequences. In all the sequences, most variation occurred in synonymous sites or the 5' UnTranslated Region (UTR), although there was still limited amino acid variation between most sequences. Several potential pseudogenes were found (approximately 10% of all sequences depending on species) with incomplete open reading frames due to frameshifts or early stop codons. Overall, variation in the actin gene family fits best with the "birth and death" model of evolution based on recent duplications, pseudogenes, and incomplete lineage sorting. Divergence between species was similar to variation within species, so that actin may be too conserved to be useful for phylogenetic estimation of closely related species. C1 [Kim, Sunju; Bachvaroff, Tsvetan R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Handy, Sara M.; Delwiche, Charles F.] Univ Maryland, Dept Cell Biol & Mol Genet, College Pk, MD 20742 USA. [Delwiche, Charles F.] Univ Maryland, Maryland Agr Expt Stn, College Pk, MD 20742 USA. RP Bachvaroff, TR (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM bachvarofft@si.edu RI Handy, Sara/C-6195-2008; OI Delwiche, Charles/0000-0001-7854-8584 FU National Science Foundation [EF-0629624]; Smithsonian Postdoctoral Fellowship FX The authors wish to thank Dr D. Wayne Coats of the Smithsonian Environmental Research Center for mentoring and support. The authors thank G. Concepcion, G. Mendez, W. Macturk, and R. Timme of the University of Maryland and two anonymous reviewers for critical reviews of the manuscript. This project was funded in part by a National Science Foundation grant from the Assembling the Tree of Life project (#EF-0629624). This work was supported by a Smithsonian Postdoctoral Fellowship grant to S. K. NR 49 TC 22 Z9 22 U1 2 U2 10 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD APR PY 2011 VL 28 IS 4 BP 1469 EP 1480 DI 10.1093/molbev/msq332 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 737GD UT WOS:000288556200013 PM 21149641 ER PT J AU Welch, AJ Yoshida, AA Fleischer, RC AF Welch, Andreanna J. Yoshida, Allison A. Fleischer, Robert C. TI Mitochondrial and nuclear DNA sequences reveal recent divergence in morphologically indistinguishable petrels SO MOLECULAR ECOLOGY LA English DT Article DE Cytochrome b; gene flow; incomplete lineage sorting; nuclear introns; Procellariiformes ID CHAIN MONTE-CARLO; BAYESIAN PHYLOGENETIC INFERENCE; RUMPED STORM-PETREL; MAXIMUM-LIKELIHOOD; POPULATION-GENETICS; HAPLOTYPE RECONSTRUCTION; MULTIPLE ALIGNMENTS; GALAPAGOS-ISLANDS; SOFTWARE PACKAGE; MIGRATION RATES AB Often during the process of divergence, genetic markers will only gradually obtain the signal of isolation. Studies of recently diverged taxa utilizing both mitochondrial and nuclear data sets may therefore yield gene trees with differing levels of phylogenetic signal as a result of differences in coalescence times. However, several factors can lead to this same pattern, and it is important to distinguish between them to gain a better understanding of the process of divergence and the factors driving it. Here, we employ three nuclear intron loci in addition to the mitochondrial Cytochrome b gene to investigate the magnitude and timing of divergence between two endangered and nearly indistinguishable petrel taxa: the Galapagos (GAPE) and Hawaiian (HAPE) petrels (Pterodroma phaeopygia and P. sandwichensis). Phylogenetic analyses indicated reciprocal monophyly between these two taxa for the mitochondrial data set, but trees derived from the nuclear introns were unresolved. Coalescent analyses revealed effectively no migration between GAPE and HAPE over the last 100 000 generations and that they diverged relatively recently, approximately 550 000 years ago, coincident with a time of intense ecological change in both the Galapagos and Hawaiian archipelagoes. This indicates that recent divergence and incomplete lineage sorting are causing the difference in the strength of the phylogenetic signal of each data set, instead of insufficient variability or ongoing male-biased dispersal. Further coalescent analyses show that gene flow is low even between islands within each archipelago suggesting that divergence may be continuing at a local scale. Accurately identifying recently isolated taxa is becoming increasingly important as many clearly recognizable species are already threatened by extinction. C1 [Welch, Andreanna J.; Yoshida, Allison A.; Fleischer, Robert C.] Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Welch, Andreanna J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. RP Welch, AJ (reprint author), Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA. EM welcha@si.edu FU Smithsonian Office of Fellowships; Smithsonian's Walcott Fund; National Science Foundation [DEB-0745604] FX We thank the following people and organizations for help obtaining samples: Vicki Friesen, Francisco Cruz-Delgado, Jose A. Gonzalez, Nick Holmes, David Anderson, Jay Penniman, Fern Duvall, Josh Adams, Helen James, Peggy Ostrom, Anne Wiley, Megan Spitzer, Christina Gebhard, Galapagos National Park, Hawaii Volcanoes National Park and Bernice P. Bishop Museum. We thank Gary Nunn for early work on this project. We also thank members of the Center for Conservation and Evolutionary Genetics at the Smithsonian Institution's National Zoo, as well as Nancy Rotzel and Adam Bazinet for logistical support. We are grateful to Frank Hailer as well as anonymous reviewers of this manuscript for helpful comments. Funding for this work was provided by the Smithsonian Office of Fellowships, the Smithsonian's Walcott Fund and the National Science Foundation (grant DEB-0745604 to M. Ostrom, H. James, R. Fleischer). NR 96 TC 18 Z9 18 U1 1 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD APR PY 2011 VL 20 IS 7 BP 1364 EP 1377 DI 10.1111/j.1365-294X.2011.05008.x PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 739HK UT WOS:000288705300007 PM 21324012 ER PT J AU Mah, C Foltz, D AF Mah, Christopher Foltz, David TI Molecular phylogeny of the Valvatacea (Asteroidea: Echinodermata) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Antarctica; Asterinidae; biogeography; classification; fossils; Goniasteridae; Ophidiasteridae; Paxillosida; Solasteridae; tropics ID SEA STARS ASTEROIDEA; LARV-AE; PROTOREASTER-NODOSUS; CLASSIFICATION; MITOCHONDRIAL; SYSTEMATICS; GENUS; GONIASTERIDAE; SEQUENCES; BEARING AB The Valvatacea is one the most ecologically important, taxonomically diverse, and widespread groups of post-Palaeozoic (i.e. modern) Asteroidea. Classification within the group has been historically problematic. We present a comprehensively sampled, three-gene (12S, 16S, early-stage histone H3) molecular phylogenetic analysis of the Valvatacea. We include five of the six families within the Paxillosida, the monotypic Notomyotida, and 13 of the 16 families of the living Valvatida. The Solasteridae is removed from the Velatida (Spinulosacea) and joins the Ganeriidae and the Leilasteridae as members of the clade containing the Asterinidae. The Poraniidae is supported as the sister group to the large cluster of Valvatacea. Asteropseids and poraniids are phylogenetically distant, contrary to morphological evidence. Several goniasterid-like ophidiasterids, such as Fromia and Neoferdina are supported as derived goniasterids rather than as Ophidiasteridae. The Benthopectinidae ( Notomyotida) are supported as members of the Paxillosida as are two members of the Pseudarchasterinae that have traditionally been considered members of the Goniasteridae. Our data suggest that Antarctic valvataceans may be derived from sister taxa in adjacent regions. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 161, 769-788. C1 [Mah, Christopher] Natl Museum Nat Hist, Smithsonian Inst Invertebrate Zool, Washington, DC 20560 USA. [Foltz, David] Louisiana State Univ Biol Sci, Baton Rouge, LA 70803 USA. RP Mah, C (reprint author), Natl Museum Nat Hist, Smithsonian Inst Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20560 USA. EM mahch@si.edu FU OPP Antarctic postdoctoral fellowship [0631245]; USARP [ANT-0466308] FX We thank the following for their assistance with specimen assistance and providing tissues for DNA extraction: Kate Neil and Kareen Schnabel at the National Institute of Water and Atmospheric Research (Wellington, New Zealand); Bob VanSyoc and Chrissy Piotrowski at the California Academy of Sciences (San Francisco); Marc Eleaume and Nadia Ameziane at the Museum National D'histoire Naturelle (Paris), Martha Nizinski and Cheryl Ames at the National Marine Fisheries Service (Washington DC), and Dave Pawson, Linda Ward, Jennifer Hammock, and Paul Greenhall at the US National Museum (Washington DC). Some of the 12S and 16S sequences were obtained with the help of Izoduwa O. Abbe, James W. Halk, Caitlyn Blanchard, and Cali Meyer. We thank Lauren VanThiel (US Antarctic Research Program), Loic Villier, Universite de Provence, Marseille, France, Dan Blake, University of Illinois, Urbana-Champaign, and an anonymous reviewer for reading the manuscript and suggesting improvements. A Faculty Research Grant from the LSU Office of Research provided funding to D. Foltz. C. Mah was funded by OPP Antarctic postdoctoral fellowship (0631245) and USARP (ANT-0466308) contracts. NR 88 TC 17 Z9 18 U1 1 U2 18 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 APR PY 2011 VL 161 IS 4 BP 769 EP 788 DI 10.1111/j.1096-3642.2010.00659.x PG 20 WC Zoology SC Zoology GA 738YE UT WOS:000288677700004 ER PT J AU Ahlering, MA Millspaugh, JJ Woods, RJ Western, D Eggert, LS AF Ahlering, M. A. Millspaugh, J. J. Woods, R. J. Western, D. Eggert, L. S. TI Elevated levels of stress hormones in crop-raiding male elephants SO ANIMAL CONSERVATION LA English DT Article DE Loxodonta africana; crop raiding; human-elephant conflict; molecular sexing; fecal glucocorticoids ID LOXODONTA-AFRICANA; SEXUAL SEGREGATION; ASIAN ELEPHANT; NATIONAL-PARK; CONFLICT; PATTERNS; POPULATION; KENYA; CONSERVATION; DNA AB Crop raiding is one of the most common forms of human-elephant conflict. Deterring elephants from raiding crops requires an understanding of the factors influencing the behavior of the individuals involved. We collected fecal samples from five group ranches in southern Kenya where crop-raiding incidents had occurred (n=10) and two protected areas, Amboseli National Park (n=24) and Maasai Mara National Reserve (n=20). We used molecular sexing to sex the individuals and radioimmunoassay kits to determine the level of glucocorticoid metabolites (i.e. stress hormones) in their dung. All crop-raiding individuals were male and had a significantly elevated concentration of glucocorticoid metabolites as compared with the Amboseli elephants (W=12, P=0.0005). We detected no significant difference between Maasai Mara elephants and either Amboseli or the crop-raiding elephants when just males were compared. Our results suggest that crop raiding may be related to stress in elephants. C1 [Ahlering, M. A.; Millspaugh, J. J.; Woods, R. J.; Eggert, L. S.] Univ Missouri, Columbia, MO USA. [Western, D.] African Conservat Ctr, Nairobi, Kenya. RP Ahlering, MA (reprint author), Smithsonian Inst, Natl Zool Pk, 3001 Connecticut Ave, Washington, DC 20008 USA. EM mahlering@gmail.com FU University of Missouri Research Board; Liz Claiborne and Art Ortenburg Foundation FX We would like to thank the staff at the African Conservation Centre and the South Rift Association of Land Owners for their support during the sample collection, especially Ken Mwathe, John Kamanga, Julius Muriuki and Jim Nyamu. We extend a special thanks to Albert Kuseyo and Samantha Russell for all their help in the field and to Alyce Johnson and the Eggert lab for assistance with lab work. This study was supported by the University of Missouri Research Board and the Liz Claiborne and Art Ortenburg Foundation. NR 50 TC 18 Z9 18 U1 13 U2 49 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 APR PY 2011 VL 14 IS 2 BP 124 EP 130 DI 10.1111/j.1469-1795.2010.00400.x PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 735WG UT WOS:000288450700006 ER PT J AU Brown, JL AF Brown, Janine L. TI Female reproductive cycles of wild female felids SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE Gonadal steroids; Noninvasive monitoring; Fecal hormones; Ovarian cycle; Pregnancy ID INTRAUTERINE ARTIFICIAL-INSEMINATION; LEOPARD NEOFELIS-NEBULOSA; PANTHERA-TIGRIS-ALTAICA; LYNX LYNX-PARDINUS; OVARIAN ACTIVITY; DOMESTIC CAT; IBERIAN LYNX; CHORIONIC-GONADOTROPIN; ASSISTED REPRODUCTION; LUTEINIZING-HORMONE AB Many felid species are endangered because of destructive human activities. As a result, zoos are being tasked with sustaining genetically healthy populations in case of catastrophic extinctions. Unfortunately, with the exception of a few species, most felids do not reproduce well in captivity. The ability to track reproductive activity via hormones is key to developing successful ex situ breeding programs. Through the development of noninvasive fecal hormone monitoring techniques, a high degree of variability in estrous cycle characteristics has been found to exist across the taxon, including the type of ovulation. For example, although all felids have induced ovulations, the occurrence of spontaneous ovulations varies across species, and even between individuals within a species. Clouded leopards, fishing cats and margays frequently have spontaneous ovulations, whereas these are rarely observed in the cheetah, tigrina and ocelot. There are marked species differences in the impact of season on reproductive function, with some being exquisitely sensitive to photoperiod (e.g., Pallas' cat), some moderately affected (tiger, clouded leopard, snow leopard), and others that are not influenced at all (e.g., ocelot, tigrina, margay, lion, leopard, fishing cat). One of the greatest challenges remaining is overcoming the problems associated with highly variable ovarian responses to ovulation induction therapies used with assisted reproductive procedures, like artificial insemination (AI). Success is relatively high in the cheetah and ocelot, but few pregnancies have resulted after AI in clouded leopard, fishing cat and tiger. Current knowledge of the reproductive physiology of nondomestic felids, including aspects of the anatomy, behavior and ovarian cycles will be presented, and how the rapidly growing endocrine database is aiding ex situ management efforts. Published by Elsevier B.V. C1 Smithsonian Conservat Biol Inst, Dept Reprod Sci, Ctr Species Survival, Front Royal, VA 22630 USA. RP Brown, JL (reprint author), Smithsonian Conservat Biol Inst, Dept Reprod Sci, Ctr Species Survival, Smithsonians Natl Zool Pk,1500 Remt Rd, Front Royal, VA 22630 USA. EM brownjan@si.edu NR 38 TC 26 Z9 28 U1 16 U2 172 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 APR PY 2011 VL 124 IS 3-4 SI SI BP 155 EP 162 DI 10.1016/j.anireprosci.2010.08.024 PG 8 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA 787DJ UT WOS:000292356500003 PM 20888156 ER PT J AU Spiering, PA Gunther, MS Somers, MJ Wildt, DE Walters, M Wilson, AS Maldonado, JE AF Spiering, Penny A. Gunther, Micaela Szykman Somers, Michael J. Wildt, David E. Walters, Michele Wilson, Amy S. Maldonado, Jesus E. TI Inbreeding, heterozygosity and fitness in a reintroduced population of endangered African wild dogs (Lycaon pictus) SO CONSERVATION GENETICS LA English DT Article DE Endangered; Heterozygosity-fitness correlation; Inbreeding; Lifespan; Lycaon pictus ID CANIS-LUPUS POPULATION; GENETIC DIVERSITY; MULTILOCUS HETEROZYGOSITY; REPRODUCTIVE SUCCESS; MICROSATELLITE LOCI; DOMESTIC DOGS; SOUTH-AFRICA; RED DEER; DEPRESSION; WOLVES AB It is crucial to understand the genetic health and implications of inbreeding in wildlife populations, especially of vulnerable species. Using extensive demographic and genetic data, we investigated the relationships among pedigree inbreeding coefficients, metrics of molecular heterozygosity and fitness for a large population of endangered African wild dogs (Lycaon pictus) in South Africa. Molecular metrics based on 19 microsatellite loci were significantly, but modestly correlated to inbreeding coefficients in this population. Inbred wild dogs with inbreeding coefficients of a parts per thousand yen0.25 and subordinate individuals had shorter lifespans than outbred and dominant contemporaries, suggesting some deleterious effects of inbreeding. However, this trend was confounded by pack-specific effects as many inbred individuals originated from a single large pack. Despite wild dogs being endangered and existing in small populations, findings within our sample population indicated that molecular metrics were not robust predictors in models of fitness based on breeding pack formation, dominance, reproductive success or lifespan of individuals. Nonetheless, our approach has generated a vital database for future comparative studies to examine these relationships over longer periods of time. Such detailed assessments are essential given knowledge that wild canids can be highly vulnerable to inbreeding effects over a few short generations. C1 [Spiering, Penny A.; Wilson, Amy S.; Maldonado, Jesus E.] Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Spiering, Penny A.; Gunther, Micaela Szykman; Wildt, David E.] Ctr Species Survival, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Spiering, Penny A.; Somers, Michael J.; Walters, Michele] Univ Pretoria, Ctr Wildlife Management, ZA-0002 Pretoria, South Africa. [Gunther, Micaela Szykman] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA. [Somers, Michael J.] Univ Pretoria, Ctr Invas Biol, ZA-0002 Pretoria, South Africa. [Walters, Michele] S African Natl Biodivers Inst, Biosystemat Res Biodivers Collect Div, ZA-0001 Pretoria, South Africa. [Walters, Michele] CSIR, ZA-0001 Pretoria, South Africa. RP Spiering, PA (reprint author), Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Natl Zoological Pk, Washington, DC 20008 USA. EM SpieringP@si.edu RI Somers, Michael/A-1523-2008; OI Szykman Gunther, Micaela/0000-0002-7822-8094; /0000-0002-5836-8823 FU Smithsonian Institution Undersecretary; University of Pretoria; Rotterdam Zoo Thandiza Fund; Humboldt State University Sponsored Program Foundation; Association of Zoos and Aquariums; Disney Wildlife Conservation Fund; Knowsley Safari Park; DST-NRF Centre of Excellence for Invasion Biology; Khaki Fever Work Wear; Pittsburgh Zoo; Morris Animal Foundation FX We thank Ezemvelo KwaZulu-Natal Wildlife, especially the management teams at Hluhluwe-iMfolozi Park and the uMkhuze section of iSimangaliso Wetland Park. We also appreciate the assistance of Thanda Private Game Reserve and the wildlife management team. We are grateful to Rob Fleischer, Emily Latch, Sarah Haas, Kalon Armstrong and Nancy Rotzel of the Smithsonian's Conservation Biology Institute for help with laboratory protocols and procedures. Sarah Arnoff, Jan Graf, Gabriella Flacke, Mariana Venter, Carla Naude-Graaff, Sboniso (Zama) Zwane, Brendan Whittington-Jones, Chris Kelly and Warren Becker provided invaluable assistance in the field. We thank Robert Sivinski and Scott Wilson of the Smithsonian's Migratory Bird Center for statistical advice. This research was supported by the Smithsonian Institution Undersecretary for Science Endowment Fund, the University of Pretoria, Rotterdam Zoo Thandiza Fund, Humboldt State University Sponsored Program Foundation, Conservation Endowment Fund of the Association of Zoos and Aquariums, Disney Wildlife Conservation Fund, Knowsley Safari Park, DST-NRF Centre of Excellence for Invasion Biology, Khaki Fever Work Wear, Pittsburgh Zoo Conservation Fund and the Morris Animal Foundation. International travel was generously provided by British Airways. NR 56 TC 11 Z9 11 U1 4 U2 59 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 J9 CONSERV GENET JI Conserv. Genet. PD APR PY 2011 VL 12 IS 2 BP 401 EP 412 DI 10.1007/s10592-010-0147-z PG 12 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 735BX UT WOS:000288389500005 ER PT J AU Miller, JM Hallager, S Monfort, SL Newby, J Bishop, K Tidmus, SA Black, P Houston, B Matthee, CA Fleischer, RC AF Miller, Joshua M. Hallager, Sara Monfort, Steven L. Newby, John Bishop, Kelley Tidmus, Scott A. Black, Peter Houston, Bill Matthee, Conrad A. Fleischer, Robert C. TI Phylogeographic analysis of nuclear and mtDNA supports subspecies designations in the ostrich (Struthio camelus) SO CONSERVATION GENETICS LA English DT Article DE Struthio camelus; Ostrich; Africa; Mitochondrial DNA control region; Phylogeography; Microsatellites ID MITOCHONDRIAL-DNA; POPULATION-STRUCTURE; CONTROL REGION; PANTHERA-LEO; DIVERSITY; EVOLUTION; INFERENCE; HISTORY; LION AB We investigated the phylogeography and subspecies classification of the ostrich (Struthio camelus) by assessing patterns of variation in mitochondrial DNA control region (mtDNA-CR) sequence and across fourteen nuclear microsatellite loci. The current consensus taxonomy of S. camelus names five subspecies based on morphology, geographic range, mtDNA restriction fragment length polymorphism and mtDNA-CR sequence analysis: S. c. camelus, S. c. syriacus, S. c. molybdephanes, S. c. massaicus and S. c. australis. We expanded a previous mtDNA dataset from 18 individual mtDNA-CR sequences to 123 sequences, including sequences from all five subspecies. Importantly, these additional sequences included 43 novel sequences of the red-necked ostrich, S. c. camelus, obtained from birds from Niger. Phylogeographic reconstruction of these sequences matches previous results, with three well-supported clades containing S. c. camelus/syriacus, S. c. molybdophanes, and S. c. massaicus/australis, respectively. The 14 microsatellite loci assessed for 119 individuals of four subspecies (all but S. c. syriacus) showed considerable variation, with an average of 13.4 (+/- 2.0) alleles per locus and a mean observed heterozygosity of 55.7 (+/- 5.3)%. These data revealed high levels of variation within most subspecies, and a structure analysis revealed strong separation between each of the four subspecies. The level of divergence across both marker types suggests the consideration of separate species status for S. c. molybdophanes, and perhaps also for S. c. camelus/syriacus. Both the mtDNA-CR and microsatellite analyzes also suggest that there has been no recent hybridization between the subspecies. These findings are of importance for management of the highly endangered red-necked subspecies (S. c. camelus) and may warrant its placement onto the IUCN red list of threatened animals. C1 [Miller, Joshua M.; Fleischer, Robert C.] Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Hallager, Sara] Anim Care Directorate, Washington, DC 20013 USA. [Monfort, Steven L.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Newby, John; Bishop, Kelley] Sahara Conservat Fund, CH-1148 Lisle, Switzerland. [Tidmus, Scott A.] Anim Programs & Environm Initiat, Lake Buena Vista, FL 32830 USA. [Black, Peter; Houston, Bill] St Louis Zoo, St Louis, MO 63110 USA. [Matthee, Conrad A.] Univ Stellenbosch, Dept Bot & Zool, ZA-7602 Stellenbosch, South Africa. RP Fleischer, RC (reprint author), Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Natl Zoological Pk,POB 37012,MRC 5503, Washington, DC 20013 USA. EM fleischerr@si.edu RI Matthee, Conrad/B-1620-2012; Miller, Joshua/E-3072-2013; Miller, Joshua/J-3393-2014; OI Miller, Joshua/0000-0002-4019-7675; Miller, Joshua/0000-0002-4019-7675; Matthee, Conrad /0000-0002-6836-069X FU Sahara Conservation Fund; Saint Louis Zoo; Smithsonian National Zoological Park; Niger's Ministry of Environment; San Diego Zoo's Wild Animal Park; AZA Conservation Endowment Fund; Disney's Animal Kingdom FX Fieldwork was funded by the Sahara Conservation Fund, Saint Louis Zoo, Smithsonian National Zoological Park, Niger's Ministry of Environment, San Diego Zoo's Wild Animal Park, AZA Conservation Endowment Fund, and Disney's Animal Kingdom; and laboratory analyses by Friends of the National Zoo and the Center for Conservation and Evolutionary Genetics. We thank Niger's Ministry, the Directorate General of Environment, T. J. Robinson, and Dr. Maikano for assistance in the field, and Nancy Rotzel, Laura Morse, Frank Hailer and Emily Latch for help with logistics and/or analysis. NR 38 TC 9 Z9 10 U1 0 U2 16 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 APR PY 2011 VL 12 IS 2 BP 423 EP 431 DI 10.1007/s10592-010-0149-x PG 9 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 735BX UT WOS:000288389500007 ER PT J AU Halofsky, JE Donato, DC Hibbs, DE Campbell, JL Cannon, MD Fontaine, JB Thompson, JR Anthony, RG Bormann, BT Kayes, LJ Law, BE Peterson, DL Spies, TA AF Halofsky, J. E. Donato, D. C. Hibbs, D. E. Campbell, J. L. Cannon, M. Donaghy Fontaine, J. B. Thompson, J. R. Anthony, R. G. Bormann, B. T. Kayes, L. J. Law, B. E. Peterson, D. L. Spies, T. A. TI Mixed-severity fire regimes: lessons and hypotheses from the Klamath-Siskiyou Ecoregion SO ECOSPHERE LA English DT Article DE Biscuit Fire; ecosystem response to fire; fire behavior; fire mosaic; fire regime; fire severity; Klamath-Siskiyou Ecoregion; post-fire ecology AB Although mixed-severity fires are among the most widespread disturbances influencing western North American forests, they remain the least understood. A major question is the degree to which mixed-severity fire regimes are simply an ecological intermediate between low-and high-severity fire regimes, versus a unique disturbance regime with distinct properties. The Klamath-Siskiyou Mountains of southwestern Oregon and northwestern California provide an excellent laboratory for studies of mixed-severity fire effects, as structurally diverse vegetation types in the region foster, and partly arise from, fires of variable severity. In addition, many mixed-severity fires have occurred in the region in the last several decades, including the nationally significant 200,000-ha Biscuit Fire. Since 2002, we have engaged in studies of early ecosystem response to 15 of these fires, ranging from determinants of fire effects to responses of vegetation, wildlife, and biogeochemistry. We present here some of our important early findings regarding mixed-severity fire, thereby updating the state of the science on mixed-severity fire regimes and highlighting questions and hypotheses to be tested in future studies on mixed-severity fire regimes. Our studies in the Klamath-Siskiyou Ecoregion suggest that forests with mixed-severity fire regimes are characterized primarily by their intimately mixed patches of vegetation of varied age, resulting from complex variations in both fire frequency and severity and species responses to this variation. Based on our findings, we hypothesize that the proximity of living and dead forest after mixed-severity fire, and the close mingling of early-and late-seral communities, results in unique vegetation and wildlife responses compared to predominantly low-or high-severity fires. These factors also appear to contribute to high resilience of plant and wildlife species to mixed-severity fire in the Klamath-Siskiyou Ecoregion. More informed management of ecosystems with mixed-severity regimes requires understanding of their wide variability in space and time, and the particular ecological responses that this variability elicits. C1 [Halofsky, J. E.] Univ Washington, Pacific Wildland Fire Sci Lab, Seattle, WA 98103 USA. [Donato, D. C.] Univ Wisconsin, Dept Zool, Madison, WI 53706 USA. [Hibbs, D. E.; Campbell, J. L.; Cannon, M. Donaghy; Kayes, L. J.; Law, B. E.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. [Fontaine, J. B.] Murdoch Univ, Sch Environm Sci, Perth, WA 6150, Australia. [Thompson, J. R.] Smithsonian Conservat Biol Inst, Smithsonian Inst, Front Royal, VA 22630 USA. [Anthony, R. G.] Oregon State Univ, Dept Fisheries & Wildlife, Oregon Cooperat Fish & Wildlife Res Unit, Corvallis, OR 97331 USA. [Bormann, B. T.; Spies, T. A.] US Forest Serv, USDA, Pacific NW Res Stn, Corvallis, OR 97331 USA. [Peterson, D. L.] US Forest Serv, USDA, Pacific NW Res Stn, Pacific Wildland Fire Sci Lab, Seattle, WA 98103 USA. RP Halofsky, JE (reprint author), Univ Washington, Pacific Wildland Fire Sci Lab, Seattle, WA 98103 USA. EM jhalo@uw.edu RI Fontaine, Joseph/M-9186-2013; Law, Beverly/G-3882-2010 OI Fontaine, Joseph/0000-0002-6515-7864; Law, Beverly/0000-0002-1605-1203 FU US Forest Service; US Bureau of Land Management; Oregon Department of Forestry; US Joint Fire Sciences Program; US Geological Survey; Office of Science (BER) US Department of Energy (DOE) [DE-FG02-06ER64318, DE-FG02-04ER63917]; U.S. Environmental Protection Agency NCER-STAR program [R-82830901-0] FX This manuscript was improved with a helpful review by Dave Perry. The authors would also like to thank the US Forest Service and US Bureau of Land Management for support of our research. Funding for the myriad studies that led to this paper was provided by the Oregon Department of Forestry, US Joint Fire Sciences Program, US Bureau of Land Management, US Forest Service, US Geological Survey, Office of Science (BER) US Department of Energy (DOE, Grant no. DE-FG02-06ER64318 and DE-FG02-04ER63917), and the U.S. Environmental Protection Agency NCER-STAR program (Grant #R-82830901-0). NR 87 TC 39 Z9 39 U1 2 U2 34 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD APR PY 2011 VL 2 IS 4 AR UNSP 40 DI 10.1890/ES10-00184.1 PG 19 WC Ecology SC Environmental Sciences & Ecology GA V30IU UT WOS:000208810500002 ER PT J AU Vermeij, GJ Leigh, EG AF Vermeij, Geerat J. Leigh, Egbert G., Jr. TI Natural and human economies compared SO ECOSPHERE LA English DT Article DE economy; ecosystems; monopoly; tragedy of the commons; trends AB Human economies and natural ecosystems (natural economies) share fundamental properties. Both are adaptive, cooperative systems where agents-individuals and groups-compete for locally limiting resources needed to live and reproduce. Successful competitors differentially propagate better knowledge and technology for making a living. Competition has favored innovations, diversification (of species or human occupations), higher productivity, greater interdependence among economic agents, and the emergence of more powerful, interactive individuals and groups, so productivity, diversity, and scales of activity have tended to increase over time. Because economic innovations accumulate, these trends have accelerated over time in both natural and human economies. The shift from mainly genetic origin and transmission of adaptation in natural economies to mainly cultural adaptation among human beings has accelerated these trends dramatically, and made the modern human economy extraordinarily dependent on nonrenewable resources and much more vulnerable to monopolies and tragedies of the commons, internally generated threats less common or less destructive in natural economies. In nature, these internal disruptions are overcome by the advent of new agents, often not involved in causing these disruptions, that compete in new ways. We argue that a comparable shift in societal norms, which govern individual and group status in human society, is needed to keep monopolies and tragedies of the commons from harming both the human economy and the ecosystems on which we depend. C1 [Vermeij, Geerat J.] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. [Leigh, Egbert G., Jr.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Vermeij, GJ (reprint author), Univ Calif Davis, Dept Geol, 1 Shields Ave, Davis, CA 95616 USA. EM gjvermeij@ucdavis.edu FU Smithsonian Tropical Research Institute FX This essay represents a true collaboration in thought and writing to which we have contributed equally. In a paper like this, it is all too easy to ignore very large elephants who happen to be in the room, and we are most grateful to James Brown for calling attention to one of these elephants. We further thank William Frederick for his thoughtful and constructive review. Egbert Leigh is grateful to Samantha Adelberg and to a particularly turbulent seminar audience for helpful remarks, and to the plants and animals of Barro Colorado Island for reminding him what it is his task to explain. We both heartily thank Janice Cooper for technical assistance. Funds for publication were kindly made available by the Smithsonian Tropical Research Institute. NR 146 TC 9 Z9 9 U1 1 U2 13 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD APR PY 2011 VL 2 IS 4 AR UNSP 39 DI 10.1890/ES11-00004.1 PG 16 WC Ecology SC Environmental Sciences & Ecology GA V30IU UT WOS:000208810500001 ER PT J AU Richmond, BG Hatala, K Green, DJ Harris, JWK Braun, DR Kiura, P Mbua, E AF Richmond, Brian G. Hatala, Kevin Green, David J. Harris, John W. K. Braun, David R. Kiura, Purity Mbua, Emma TI Investigating the Evolution of Foot Anatomy & Biomechanics from Fossil Footprints SO FASEB JOURNAL LA English DT Meeting Abstract CT Experimental Biology Meeting 2011 CY APR 09-13, 2011 CL Washington, DC SP Amer Assoc Anatomists (AAA), Amer Physiolog Soc (APS), Amer Soc Biochem & Mol Biol (ASBMB), Amer Soc Investigat Pathol (ASIP), Amer Soc Nutrit (ASN), Amer Soc Pharmacol & Expt Therapeut (ASPET) C1 [Richmond, Brian G.; Hatala, Kevin; Green, David J.] George Washington Univ, Washington, DC USA. [Richmond, Brian G.] Smithsonian Inst, NMNH, Human Origins Program, Washington, DC 20560 USA. [Harris, John W. K.] Rutgers State Univ, New Brunswick, NJ 08903 USA. [Braun, David R.] Univ Cape Town, ZA-7925 Cape Town, South Africa. [Kiura, Purity; Mbua, Emma] Natl Museums Kenya, Nairobi, Kenya. NR 0 TC 0 Z9 0 U1 1 U2 10 PU FEDERATION AMER SOC EXP BIOL PI BETHESDA PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA SN 0892-6638 J9 FASEB J JI Faseb J. PD APR PY 2011 VL 25 PG 1 WC Biochemistry & Molecular Biology; Biology; Cell Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics; Cell Biology GA 032IE UT WOS:000310708401692 ER PT J AU Buffington, ML Nieves-Aldrey, JL AF Buffington, Matthew L. Luis Nieves-Aldrey, Jose TI REVISION OF PLECTOCYNIPINAE (HYMENOPTERA: FIGITIDAE) WITH DESCRIPTIONS OF A NEW GENUS AND THREE NEW SPECIES FROM CHILE SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Araucocynips; Plectocynips; Nothofagus; Aditrochus; galls ID CYNIPOIDEA; EVOLUTION; MORPHOLOGY; CYNIPIDAE; PHYLOGENY; SUBFAMILY AB A revision of Plectocynipinae was initiated following the recent collections of specimens of Plectocynips Diaz and Araucocynips, new genus, from Chile. In addition to a redescription of the subfamily, we provide redescriptions, based on females, of the species of both genera. Descriptions are provided for Araucocynips ariasae, new species, Araucocynips queulensis, new species, and Plectocynips lago, new species, all from Chile. New host records are provided for Plectocynips pilosus Ros-Farre from galls of Aditrochus fagicolus Rubsaamen and Aditrochus coihuensis Ovruski (Hymenoptera: Chalcidoidea) on Nothofagus pumilio (Poepp. & Endl.) Krasser and Nothofagus dombeyi (Mirb.), respectively. In addition, males are described for Araucocynips ariasae, Araucocynips queulensis, and Plectocynips pilosus. C1 [Buffington, Matthew L.] USDA ARS, Systemat Entomol Lab, Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Luis Nieves-Aldrey, Jose] CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolutiva, E-28006 Madrid, Spain. RP Buffington, ML (reprint author), USDA ARS, Systemat Entomol Lab, Smithsonian Inst, Natl Museum Nat Hist, 10th & Constitut Ave,NW POB 37012,MRC 168, Washington, DC 20013 USA. EM matt.buffington@ars.usda.gov; mcnna38@mncn.csic.es RI Nieves-Aldrey, Jose Luis/K-2544-2012 OI Nieves-Aldrey, Jose Luis/0000-0002-4711-7455 FU CSIC - University of Chile [18/05-06]; Ministry of Science and Innovation [CGL2009-10111/BOS, CGL2010-15786/BOS]; National Science Foundation [DEB-0445413] FX Thanks to Audrey Grez, Javier Simonetti, Yuri Zuniga, and Fernando Campos for their assistance and support with logistics and field work carried out during the stay of JLNA in Reserva Nacional Los Queules, and to Corporacion Nacional Forestal (CONAF) for having granted him permission to collect material in national parks and other protected natural areas of Chile. This study was financed with funds of the CSIC - University of Chile cooperation project 18/05-06 and by Projects CGL2009-10111/BOS and CGL2010-15786/BOS of the Ministry of Science and Innovation, conferred to J.L. Nieves-Aldrey. We thank Hector Ibarra (Exp Ediciones al Conocimiento, Concepion, Chile) and Elizabeth Arias (Essig Museum, UC Berkeley) for access to specimens; E. Arias' collecting efforts in Chile were supported by National Science Foundation grant DEB-0445413. Further thanks to Jennifer Read (CNC) and Douglas Yanega (UCRC) for assisting with loans of specimens. Thanks also to Laura Tormo and Marta Furio (CSIC) for technical assistance with SEM images. Jens Prena and Thomas Henry (Systematic Entomology Laboratory, ARS/USDA, NMNH, Washington DC), Johan Liljeblad (Swedish Species Information Centre, Uppsala, Sweden), Juli Pujade-Villar (University of Barcelona, Barcelona, Spain), as well as an anonymous reviewer, helped improve the quality of this manuscript. The USDA is an equal opportunity provider and employer. NR 23 TC 4 Z9 5 U1 0 U2 4 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 APR PY 2011 VL 113 IS 2 BP 91 EP 108 DI 10.4289/0013-8797.113.2.91 PG 18 WC Entomology SC Entomology GA 785NI UT WOS:000292235300001 ER PT J AU Henry, TJ Hoffman, RL Wolski, A AF Henry, Thomas J. Hoffman, Richard L. Wolski, Andrzej TI FIRST NORTH AMERICAN RECORD OF THE OLD WORLD CYLAPINE FULVIUS SUBNITENS POPPIUS (HEMIPTERA: HETEROPTERA: MIRIDAE) FROM VIRGINIA, WITH DESCRIPTIONS AND A KEY TO THE U.S. SPECIES OF FULVIUS SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Plant bugs; new records; United States; diagnoses; distributions; feeding habits ID ANNOTATED LIST AB The first North American record for Fulvius subnitens Poppius is reported based on one specimen collected in southcentral Virginia. Fulvius anthocoroides (Reuter), Fulvius imbecilis (Say), Fulvius slateri Wheeler, and Fulvius subnitens are diagnosed and described, and color images of adults, updated distributions, a review of feeding habits, and an identification key are provided. For each species, the nomenclatural history and most important citations are given. C1 [Henry, Thomas J.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Mus Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Hoffman, Richard L.] Virginia Museum Nat Hist, Martinsville, VA 24112 USA. [Wolski, Andrzej] Opole Univ, Dept Biosystemat, PL-45052 Opole, Poland. RP Henry, TJ (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Mus Nat Hist,Smithsonian Inst, POB 37012,MRC 0168, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov; richard.hoffman@vmnh.virginia.gov; a.wolski@ior.gliwice.pl NR 42 TC 6 Z9 6 U1 0 U2 3 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 APR PY 2011 VL 113 IS 2 BP 127 EP 136 DI 10.4289/0013-8797.113.2.127 PG 10 WC Entomology SC Entomology GA 785NI UT WOS:000292235300004 ER PT J AU Solis, MA AF Solis, M. Alma TI REASSIGNMENT OF FOUR SPECIES CURRENTLY IN HERPETOGRAMMA LEDERER (SPILOMELINAE) TO PYRAUSTINAE (CRAMBIDAE: PYRALOIDEA: LEPIDOPTERA) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Western Hemisphere; Japan; new combination; Pyrausta; Hahncappsia AB During an ongoing study of Herpetogramma Lederer (Spilomelinae), four species, three from the Western Hemisphere and one from Japan, were discovered to be misplaced in the genus and the subfamily. Based on primary type material, the following new and revised combinations and transfers to the Pyraustinae are proposed: the male syntype of Pachyzancla nigripalpis Hampson is designated as the lectotype and is transferred to Pyrausta, and the female syntype of P. nigripalpis is transferred to Hahncappsia as a species of uncertain identity but closest to H. jaliscalis Capps. Pachyzancla straminea Hampson and Pachyzancla holochrysis Hampson are transferred to Pyrausta; Herpetogramma albipennis Inoue is transferred to Aglaops Warren. The adults, genitalia, and labels are illustrated for the first time. C1 ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Solis, MA (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM alma.solis@ars.usda.gov NR 17 TC 0 Z9 1 U1 5 U2 11 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD APR PY 2011 VL 113 IS 2 BP 185 EP 194 DI 10.4289/0013-8797.113.2.185 PG 10 WC Entomology SC Entomology GA 785NI UT WOS:000292235300008 ER PT J AU Bolin, JF Maass, E Musselman, LJ AF Bolin, Jay F. Maass, Erika Musselman, Lytton J. TI A New Species of Hydnora (Hydnoraceae) from Southern Africa SO SYSTEMATIC BOTANY LA English DT Article DE holoparasite; Hydnora africana; Hydnora longicollis; Namibia; parasitic plant; South Africa AB We describe a new species, Hydnora visseri (Hydnoraceae), a holoparasitic perennial species from the Karas Region of Namibia and the Northern Cape Province of South Africa. The new species is a distinct segregate of Hydnora africana and is restricted to transitional and winter rainfall areas of southern Namibia and northwestern South Africa. Hydnora visseri only occurs with H. africana in sympatry in a narrow geographical band where their respective host species occur together. Distinctly longer tepal lobes and the largest flower metrics in the section Euhydnora distinguish H. visseri from H. africana and Hydnora longicollis. At one known site where H. africana and H. visseri occur in sympatry, differences in flowering phenology and host preference appear to reinforce species boundaries. C1 [Bolin, Jay F.] Natl Museum Nat Hist MRC 166, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. [Bolin, Jay F.; Musselman, Lytton J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Maass, Erika] Univ Namibia, Dept Biol Sci, Windhoek, Namibia. RP Bolin, JF (reprint author), Natl Museum Nat Hist MRC 166, Dept Bot, Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM bolinj@si.edu FU U. S. State Department; Mary Payne Hogan Botany Endowment at ODU; University of Namibia Research and Publication Committee FX We would like to thank the Namibian National Botanical Research Institute, in particular E. Kwembeya and G. Maggs-Kolling. Many other experts freely gave their time including R. and D. Brand, O. Von Kaschke, W. Voigt, T. Dold, T. Trinder-Smith, T. Goettert, and K. Wurdack. We thank N. and J. Jacobs, E. Rukoro, V. Libuku, M. Takundwa, and A. Faul for field assistance. Funding was provided by the U. S. State Department Fulbright Program, the Mary Payne Hogan Botany Endowment at ODU, and the University of Namibia Research and Publication Committee. Access to private property and logistical support was provided by the de Bruyn Family and the Gonwana Canon Preserve. Finally this research was conducted under Namibian MET Permits No. 1013/2006 and 1350/2009. NR 22 TC 5 Z9 6 U1 2 U2 6 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD APR-JUN PY 2011 VL 36 IS 2 BP 255 EP 260 DI 10.1600/036364411X569453 PG 6 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 780IH UT WOS:000291847200001 ER PT J AU Burns, JH Faden, RB Steppan, SJ AF Burns, Jean H. Faden, Robert B. Steppan, Scott J. TI Phylogenetic Studies in the Commelinaceae Subfamily Commelinoideae Inferred from Nuclear Ribosomal and Chloroplast DNA Sequences SO SYSTEMATIC BOTANY LA English DT Article DE Callisia; Commelina; cpNA; Murdannia; nrDNA; Tradescantia ID MORPHOLOGICAL DATA; CLADISTIC-ANALYSIS; RBCL SEQUENCES; COMBINING DATA; EVOLUTION; INCONGRUENCE; INFERENCE; ALIGNMENT; MONOCOTS; COMPLEX AB The Commelinaceae are a pantropical family of monocotyledonous herbs. Previous phylogenies in Commelinaceae have emphasized sampling among genera. We extended this previous work by sampling multiple species within some of the largest genera of Commelinaceae (especially Commelina and Tradescantia, and also including Callisia, Cyanotis, Gibasis, and Murdannia), and by sequencing noncoding regions both of the nuclear ribosomal DNA region, 5S NTS, and the chloroplast region, trnL-trnF. We generated a phylogenetic hypothesis for 68 Commelinaceae that partially tests previous morphological, taxonomic classifications. We found little evidence for conflict between nuclear and chloroplast regions for Tradescantia, Murdannia, and Callisia, and some evidence for conflict between the two regions for Commelina, though conflicting regions of the phylogeny were only weakly supported by bootstrap analyses. We found subtribe Tradescantieae to be paraphyletic, consistent with an rbcL study, though with a different topology than that produced by rbcL. In addition, subtribe Commelineae was monophyletic with strong support. We found Callisia to be polyphyletic, consistent with some previous molecular phylogenetic studies, and we found Tradescantia, Gibasis, Cyanotis, Commelina, and Murdannia, to be monophyletic. The molecular phylogenies presented here generally supported previous taxonomic classifications. C1 [Faden, Robert B.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Burns, Jean H.; Steppan, Scott J.] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. RP Burns, JH (reprint author), Case Western Reserve Univ, Dept Biol, 10900 Euclid Ave, Cleveland, OH 44106 USA. EM jbm122@case.edu FU Florida State University; Dissertation Research Grant; Florida Exotic Pest Plant Council; National Science Foundation [DEB 0091776] FX This study was funded by Florida State University's Robert K. Godfrey Endowment Award for the Study of Botany, Dissertation Research Grant, Margaret Menzel Award in the Department of Biological Science, and University Fellowships. Additional support was provided by the Florida Exotic Pest Plant Council Research Grant Award and the National Science Foundation (DEB 0091776 to T. E. Miller). We thank T. E. Miller, F. C. James, D. Houle, W. Parker, K. S. Moriuchi, D. Richardson, M. Rejmanek, and K. Rowe for helpful comments on the writing and idea development. K. Burks provided valuable advice on the choice of Commelinaceae for this study. L. Anderson helped with specimen localities for collection. L. Csiba at the Royal Botanic Gardens, Kew and J. C. Solomon at the Missouri Botanical Gardens provided some of the DNA extractions. T. M. Evans provided sequencing advice and primers for Tradescantia, and S. Bergamo provided sequencing advice and plant materials for Callisia. C. R. Hardy suggested the use of 5S NTS. R. Dhanarajan and M. Asher cloned the 5S NTS region. NR 53 TC 10 Z9 11 U1 0 U2 14 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 APR-JUN PY 2011 VL 36 IS 2 BP 268 EP 276 DI 10.1600/036364411X569471 PG 9 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 780IH UT WOS:000291847200003 ER PT J AU Rota, J AF Rota, Jadranka TI Data partitioning in Bayesian analysis: molecular phylogenetics of metalmark moths (Lepidoptera: Choreutidae) SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID MODEL SELECTION; TREES; GENE; SUBSTITUTION; MORPHOLOGY; INFERENCE; UTILITY AB In this study a multilocus phylogenetic analysis of metalmark moths (Lepidoptera: Choreutidae) focused on resolving the higher-level phylogeny of this group is presented. Through the analysis of this dataset, I explore different data-partitioning strategies in Bayesian phylogenetic inference, and find that a partitioning strategy can have a large influence on the results of phylogenetic analysis. Depending on how the data are partitioned, there can be significant differences in branch support. I also test for the existence of the Bayesian star tree paradox, and its importance in this dataset, and find that it appears to inflate support for the clade including Rhobonda gaurisana, Hemerophila houttuinialis, H. diva and H. felis, but plays no role in other cases where the differences between maximum-likelihood bootstraps and Bayesian posterior probabilities are large. The results of all the phylogenetic analyses strongly suggest that including Millieriinae in Choreutidae renders the family polyphyletic. The monophyly of the other two subfamilies, Brenthiinae and Choreutinae, as well as their sister-group relationship, is strongly supported. Similarly, the monophyly of all the genera examined except Hemerophila is also well supported. To bring the classification of Choreutidae in line with our current understanding of the phylogenetic relationships in the family, I propose to exclude Millieriinae from Choreutidae, elevate it to Millieriidae Heppner, and place it as incertae sedis within Ditrysia. C1 [Rota, Jadranka] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Rota, Jadranka] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Rota, J (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Univ Pk 15, DK-2100 Copenhagen O, Denmark. EM jrota@snm.ku.dk RI Rota, Jadranka/C-6702-2011 OI Rota, Jadranka/0000-0003-0220-3920 FU National Science Foundation [DDIG DEB-0608399, DEB-0072702, DEB 04-22386]; Penner and DeCoursey Endowments; National Geographic Society [7331-02, 7751-04]; Smithsonian Postdoctoral Fellowship FX I thank David Wagner, Elizabeth Jockusch, Paul Lewis and Chris Simon for help with numerous aspects of this project; the Simon lab, especially Kathy Hill, David Marshall and Maxi Polihronakis, for help with lab techniques and data analysis; Terry Harrison and Shen-Horn Yen for sending specimens; Jack Longino, Robert Colwell and the Arthropods of La Selva staff for enabling me to do fieldwork in Costa Rica; Niklas Wahlberg for providing sequences of three additional taxa; Marko Gacesa for help with analyses; John Brown, Charles Mitter, Johan Nylander, Thomas Simonsen, Lars Vilhelmsen and Niklas Wahlberg for helpful comments on an earlier version of the article. Bioinformatics analyses were carried out on the University of Connecticut cluster and computers, as well as the freely available Bioportal cluster (http://www.bioportal.uio.no). This work was supported by: the National Science Foundation (grants DDIG DEB-0608399, DEB-0072702 and DEB 04-22386); the Penner and DeCoursey Endowments to the Department of Ecology and Evolutionary Biology, University of Connecticut, and the Connecticut State Museum of Natural History; National Geographic Society (grants 7331-02 and 7751-04); and a Smithsonian Postdoctoral Fellowship. NR 49 TC 13 Z9 13 U1 0 U2 7 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 APR PY 2011 VL 36 IS 2 BP 317 EP 329 DI 10.1111/j.1365-3113.2010.00563.x PG 13 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 735VS UT WOS:000288449300008 ER PT J AU Huenemoerder, DP Mitschang, A Dewey, D Nowak, MA Schulz, NS Nichols, JS Davis, JE Houck, JC Marshall, HL Noble, MS Morgan, D Canizares, CR AF Huenemoerder, David P. Mitschang, Arik Dewey, Daniel Nowak, Michael A. Schulz, Norbert S. Nichols, Joy S. Davis, John E. Houck, John C. Marshall, Herman L. Noble, Michael S. Morgan, Doug Canizares, Claude R. TI TGCat: THE CHANDRA TRANSMISSION GRATING DATA CATALOG AND ARCHIVE SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; techniques: spectroscopic; X-rays: general ID X-RAY SPECTROSCOPY; SYSTEM AB The Chandra Transmission Grating Data Archive and Catalog (TGCat) provides easy access to analysis-ready products, specifically, high-resolution X-ray count spectra and their corresponding calibrations. The web interface makes it easy to find observations of a particular object, type of object, or type of observation; to quickly assess the quality and potential usefulness of the spectra from pre-computed summary plots; or to customize a view with an interactive plotter, optionally combining spectra over multiple orders or observations. Data and responses can be downloaded as a package or as individual files, and the query results themselves can be retrieved as ASCII or Virtual Observatory tables. Portable reprocessing scripts used to create the archive and which use the Chandra X-ray Center's (CXC's) software and other publicly available software are also available, facilitating standard or customized reprocessing from Level 1 CXC archival data to spectra and responses with minimal user interaction. C1 [Huenemoerder, David P.; Dewey, Daniel; Nowak, Michael A.; Schulz, Norbert S.; Davis, John E.; Houck, John C.; Marshall, Herman L.; Noble, Michael S.; Canizares, Claude R.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Mitschang, Arik; Nichols, Joy S.; Morgan, Doug] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Huenemoerder, DP (reprint author), MIT, Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA. OI Houck, John/0000-0002-6761-6796 FU National Aeronautics and Space Administration [SV3-73016, GO9-0012X]; National Aeronautics Space Administration [NAS8-03060] FX Support for this work was provided by the National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for Support of the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. J.S.N., A.M., and D.M. acknowledge support from the Chandra X-ray Center NASA contract NAS8-03060. Support for the Adara work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO9-0012X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. NR 17 TC 26 Z9 26 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2011 VL 141 IS 4 AR 129 DI 10.1088/0004-6256/141/4/129 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 733IO UT WOS:000288256600025 ER PT J AU Ingleby, L Calvet, N Hernandez, J Briceno, C Espaillat, C Miller, J Bergin, E Hartmann, L AF Ingleby, Laura Calvet, Nuria Hernandez, Jesus Briceno, Cesar Espaillat, Catherine Miller, Jon Bergin, Edwin Hartmann, Lee TI EVOLUTION OF X-RAY AND FAR-ULTRAVIOLET DISK-DISPERSING RADIATION FIELDS SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; protoplanetary disks; stars: pre-main sequence; ultraviolet: stars; X-rays: stars ID T-TAURI STARS; MAIN-SEQUENCE STARS; ALL-SKY SURVEY; ORION OB1 ASSOCIATION; CHAMELEON-I CLOUD; LOW-MASS STARS; SPITZER OBSERVATIONS; FORMING REGION; YOUNG STARS; PLANETARY SYSTEMS AB We present new X-ray and far-ultraviolet (FUV) observations of T Tauri stars covering the age range 1-10 Myr. Our goals are to observationally constrain the intensity of radiation fields responsible for evaporating gas from the circumstellar disk and to assess the feasibility of current photoevaporation models, focusing on X-ray and UV radiation. We greatly increase the number of 7-10 Myr old T Tauri stars observed in X-rays by including observations of the well-populated 25 Ori aggregate in the Orion OB1a subassociation. With these new 7-10 Myr objects, we confirm that X-ray emission remains constant from 1 to 10 Myr. We also show, for the first time, observational evidence for the evolution of FUV radiation fields with a sample of 56 accreting and non-accreting young stars spanning 1 Myr to 1 Gyr. We find that the FUV emission decreases on timescales consistent with the decline of accretion in classical T Tauri stars until reaching the chromospheric level in weak T Tauri stars and debris disks. Overall, we find that the observed strength of high-energy radiation is consistent with that required by photoevaporation models to dissipate the disks in timescales of approximately 10 Myr. Finally, we find that the high-energy fields that affect gas evolution are not similarly affecting dust evolution; in particular, we find that disks with inner clearings, transitional disks, have similar levels of FUV emission as full disks. C1 [Ingleby, Laura; Calvet, Nuria; Miller, Jon; Bergin, Edwin; Hartmann, Lee] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Hernandez, Jesus; Briceno, Cesar] CIDA, Merida 5101A, Venezuela. [Espaillat, Catherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. 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; jesush@cida.ve; briceno@cida.ve; cespaillat@cfa.harvard.edu; jonmm@umich.edu; ebergin@umich.edu; lhartm@umich.edu FU NASA [GO8-9028X, GO8-9029X, NAS8-03060, NAS 5-26555]; NASA from the Space Telescope Science Institute [GO-08317, GO-09081, GO-09374, GO-11145]; National Science Foundation [0901947]; National Aeronautics and Space Administration FX We thank Kevin Luhman for assistance in identifying possible new T Tauri stars in Chamaeleon I. We also thank Jennifer Blum and Jun Ji for their help with X-ray data reduction and analysis techniques. We thank Gregory Herczeg for his assistance with reducing the ACS Chamaeleon data. Support for this work was provided by NASA through Chandra Awards GO8-9028X and GO8-9029X 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. Support for this work was also provided by NASA through grant nos. GO-08317, GO-09081, GO-09374, and GO-11145 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. C. E. was supported by the National Science Foundation under Award No. 0901947. 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 102 TC 29 Z9 29 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 APR PY 2011 VL 141 IS 4 AR 127 DI 10.1088/0004-6256/141/4/127 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 733IO UT WOS:000288256600023 ER PT J AU Mueller, M Delbo', M Hora, JL Trilling, DE Bhattacharya, B Bottke, WF Chesley, S Emery, JP Fazio, G Harris, AW Mainzer, A Mommert, M Penprase, B Smith, HA Spahr, TB Stansberry, JA Thomas, CA AF Mueller, Michael Delbo', M. Hora, J. L. Trilling, D. E. Bhattacharya, B. Bottke, W. F. Chesley, S. Emery, J. P. Fazio, G. Harris, A. W. Mainzer, A. Mommert, M. Penprase, B. Smith, H. A. Spahr, T. B. Stansberry, J. A. Thomas, C. A. TI ExploreNEOs. III. PHYSICAL CHARACTERIZATION OF 65 POTENTIAL SPACECRAFT TARGET ASTEROIDS SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: planetary systems; minor planets, asteroids: general; radiation mechanisms: thermal; space vehicles; surveys ID NEAR-EARTH ASTEROIDS; 10302 1989 ML; SPECTRAL PROPERTIES; OBJECT SURVEY; ALBEDOS; TELESCOPE; DIAMETERS; PHOTOMETRY; MAGNITUDE; MISSION AB Space missions to near-Earth objects (NEOs) are being planned at all major space agencies, and recently a manned mission to an NEO was announced as a NASA goal. Efforts to find and select suitable targets (plus backup targets) are severely hampered by our lack of knowledge of the physical properties of dynamically favorable NEOs. In particular, current mission scenarios tend to favor primitive low-albedo objects. For the vast majority of NEOs, the albedo is unknown. Here we report new constraints on the size and albedo of 65 NEOs with rendezvous Delta nu < 7 km s(-1). Our results are based on thermal-IR flux data obtained in the framework of our ongoing (2009-2011) ExploreNEOs survey using NASA's "Warm-Spitzer" space telescope. As of 2010 July 14, we have results for 293 objects in hand (including the 65 low-Delta nu NEOs presented here); before the end of 2011, we expect to have measured the size and albedo of similar to 700 NEOs (including probably similar to 160 low-Delta nu NEOs). While there are reasons to believe that primitive volatile-rich materials are universally low in albedo, the converse need not be true: the orbital evolution of some dark objects likely has caused them to lose their volatiles by coming too close to the Sun. For all our targets, we give the closest perihelion distance they are likely to have reached (using orbital integrations from Marchi et al. 2009) and corresponding upper limits on the past surface temperature. Low-Delta nu objects for which both albedo and thermal history may suggest a primitive composition include (162998) 2001 SK162, (68372) 2001 PM9, and (100085) 1992 UY4. C1 [Mueller, Michael; Delbo', M.] Observ Cote Azur, CNRS, UNS, Lab Cassiopee, F-06304 Nice 04, France. [Hora, J. L.; Fazio, G.; Smith, H. A.; Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Trilling, D. E.; Thomas, C. A.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA. [Bhattacharya, B.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Bottke, W. F.] SW Res Inst, Boulder, CO 80302 USA. [Chesley, S.; Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Harris, A. W.; Mommert, M.] DLR Inst Planetary Res, D-12489 Berlin, Germany. [Penprase, B.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Stansberry, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Mueller, M (reprint author), Observ Cote Azur, CNRS, UNS, Lab Cassiopee, BP 4229, F-06304 Nice 04, France. EM michael.mueller@oca.eu OI Mueller, Michael/0000-0003-3217-5385; Hora, Joseph/0000-0002-5599-4650; Thomas, Cristina/0000-0003-3091-5757 FU CNRS-INSU; Conseil General des Alpes-Maritimes; ESA [SSA-NEO-ESA-MEM-017/1]; NASA FX Michael Mueller gratefully acknowledges the Henri Poincare Fellowship, which is funded by the CNRS-INSU and the Conseil General des Alpes-Maritimes. The work of M. M. and M. D. is supported by ESA grant SSA-NEO-ESA-MEM-017/1. We thank Patrick Michel for helpful discussions. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by JPL/Caltech under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 50 TC 33 Z9 33 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2011 VL 141 IS 4 AR 109 DI 10.1088/0004-6256/141/4/109 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 733IO UT WOS:000288256600005 ER PT J AU Schnitzer, SA Bongers, F AF Schnitzer, Stefan A. Bongers, Frans TI Increasing liana abundance and biomass in tropical forests: emerging patterns and putative mechanisms SO ECOLOGY LETTERS LA English DT Review DE CO2; disturbance; drought; global change; land use change; liana increases; structural changes; tropical forests ID BELOW-GROUND COMPETITION; BARRO-COLORADO ISLAND; IVY TOXICODENDRON RADICANS; ELEVATED ATMOSPHERIC CO2; FUTURE CLIMATE-CHANGE; RAIN-FOREST; EASTERN AMAZONIA; ABOVEGROUND BIOMASS; TOXICITY RESPONSES; TEMPERATE FORESTS AB P>Tropical forests are experiencing large-scale structural changes, the most apparent of which may be the increase in liana (woody vine) abundance and biomass. Lianas permeate most lowland tropical forests, where they can have a huge effect on tree diversity, recruitment, growth and survival, which, in turn, can alter tree community composition, carbon storage and carbon, nutrient and water fluxes. Consequently, increasing liana abundance and biomass have potentially profound ramifications for tropical forest composition and functioning. Currently, eight studies support the pattern of increasing liana abundance and biomass in American tropical and subtropical forests, whereas two studies, both from Africa, do not. The putative mechanisms to explain increasing lianas include increasing evapotranspirative demand, increasing forest disturbance and turnover, changes in land use and fragmentation and elevated atmospheric CO2. Each of these mechanisms probably contributes to the observed patterns of increasing liana abundance and biomass, and the mechanisms are likely to be interrelated and synergistic. To determine whether liana increases are occurring throughout the tropics and to determine the mechanisms responsible for the observed patterns, a widespread network of large-scale, long-term monitoring plots combined with observational and manipulative studies that more directly investigate the putative mechanisms are essential. C1 [Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama. [Bongers, Frans] Wageningen Univ, Ctr Ecosyst Studies, NL-6700 AA Wageningen, Netherlands. RP Schnitzer, SA (reprint author), Univ Wisconsin, Dept Biol Sci, POB 413, Milwaukee, WI 53201 USA. EM schnitzer@uwm.edu OI Schnitzer, Stefan/0000-0002-2715-9455 FU NSF [DEB-0613666, NSF DEB-0845071, NSF DEB-1019436]; Dutch NWO; Wageningen University; University of Wisconsin - Milwaukee Research Growth Initiative FX We thank R. Burnham, A. Ercoli and two anonymous referees for constructive comments on this manuscript. This work was supported financially by NSF DEB-0613666, NSF DEB-0845071, NSF DEB-1019436, a Dutch NWO Visiting Faculty Fellowship, a Wageningen University Production Ecology & Resource Conservation Fellowship, and the University of Wisconsin - Milwaukee Research Growth Initiative programme. NR 105 TC 178 Z9 189 U1 9 U2 97 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD APR PY 2011 VL 14 IS 4 BP 397 EP 406 DI 10.1111/j.1461-0248.2011.01590.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 732SW UT WOS:000288211000010 PM 21314879 ER PT J AU Buermann, W Chaves, JA Dudley, R McGuire, JA Smith, TB Altshuler, DL AF Buermann, Wolfgang Chaves, Jaime A. Dudley, Robert McGuire, Jimmy A. Smith, Thomas B. Altshuler, Douglas L. TI Projected changes in elevational distribution and flight performance of montane Neotropical hummingbirds in response to climate change SO GLOBAL CHANGE BIOLOGY LA English DT Article DE climate change; elevational shift; hummingbird flight kinematics; wing stroke amplitude; wingbeat frequency ID NICHE CONSERVATISM; BIRD EXTINCTIONS; LAND-USE; IMPACTS; ENERGETICS; ECOLOGY; LIMITS; FRAGMENTATION; ORGANIZATION; COMMUNITIES AB The hovering flight of hummingbirds is one of the most energetically demanding forms of animal locomotion and is influenced by both atmospheric oxygen availability and air density. Montane Neotropical hummingbirds are expected to shift altitudinally upwards in response to climate change to track their ancestral climatic regime, which is predicted to influence their flight performance. In this study, we use the climate envelope approach to estimate upward elevational shifts for five Andean hummingbird species under two climate change scenarios. We then use field-based data on hummingbird flight mechanics to estimate the resulting impact of climate change on aerodynamic performance in hovering flight. Our results show that in addition to significant habitat loss and fragmentation, projected upwards elevational shifts vary between 300 and 700 m, depending on climate change scenario and original mean elevation of the target species. Biomechanical analysis indicates that such upwards elevational shifts would yield a similar to 2-5 degrees increase in wing stroke amplitude with no substantial effect on wingbeat frequency. Overall, the physiological impact of elevational shifts of < 1000 m in response to climate change is likely to be small relative to other factors such as habitat loss, changes in floristic composition, and increased interspecific competition. C1 [Buermann, Wolfgang; Chaves, Jaime A.; Smith, Thomas B.] Univ Calif Los Angeles, Inst Environm, Ctr Trop Res, Los Angeles, CA 90095 USA. [Chaves, Jaime A.; Smith, Thomas B.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Dudley, Robert; McGuire, Jimmy A.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. [McGuire, Jimmy A.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Altshuler, Douglas L.] Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. RP Altshuler, DL (reprint author), Univ Calif Los Angeles, Inst Environm, Ctr Trop Res, Los Angeles, CA 90095 USA. EM douga@ucr.edu OI Altshuler, Douglas/0000-0002-1364-3617 FU National Science Foundation [DEB 0543556, IOS 0923849] FX We thank Chris Barber, Richard Gibbons, Wily Palomino, Marianne van Vlaardingen, Patiacolla Tours, and the many Earthcorps volunteers for assistance and support in the field, and also thank Peter Baik, Jeremy Goldbogen, and Sylvia Heredia for help with data acquisition and analysis. Zac Cheviron provided comments on an earlier version of the manuscript. Our research on the comparative flight performance of hummingbirds has been generously supported by the Earthwatch Institute and the National Science Foundation, most recently through grants DEB 0543556 and IOS 0923849. NR 66 TC 9 Z9 10 U1 4 U2 31 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD APR PY 2011 VL 17 IS 4 BP 1671 EP 1680 DI 10.1111/j.1365-2486.2010.02330.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 728CZ UT WOS:000287853000014 ER PT J AU Turner, BL Engelbrecht, BMJ AF Turner, Benjamin L. Engelbrecht, Bettina M. J. TI Soil organic phosphorus in lowland tropical rain forests SO BIOGEOCHEMISTRY LA English DT Article DE DNA; Inositol phosphate; Lowland tropical forest; Panama; Phosphate diesters; Phosphate monoesters; Soil organic phosphorus; Solution (31)P NMR spectroscopy ID NUCLEAR-MAGNETIC-RESONANCE; P-31 NMR-SPECTROSCOPY; TERRESTRIAL ECOSYSTEMS; HEDLEY FRACTIONATION; EXTRACTION; PEDOGENESIS; FORMS; LIMITATION; DYNAMICS; EDTA AB Phosphorus is widely considered to constrain primary productivity in tropical rain forests, yet the chemistry of soil organic phosphorus in such ecosystems remains poorly understood. We assessed the composition of soil organic phosphorus in 19 contrasting soils under lowland tropical forest in the Republic of Panama using NaOH-EDTA extraction and solution (31)P nuclear magnetic resonance spectroscopy. The soils spanned a strong rainfall gradient (1730-3404 mm y(-1)) and contained a wide range of chemical properties (pH 3.3-7.0; total carbon 2.8-10.4%; total phosphorus 74-1650 mg P kg(-1)). Soil organic phosphorus concentrations ranged between 22 and 494 mg P kg(-1) and were correlated positively with total soil phosphorus, pH, and total carbon, but not with annual rainfall. Organic phosphorus constituted 26 +/- A 1% (mean +/- A STD error, n = 19) of the total phosphorus, suggesting that this represents a broad emergent property of tropical forest soils. Organic phosphorus occurred mainly as phosphate monoesters (68-96% of total organic phosphorus) with smaller concentrations of phosphate diesters in the form of DNA (4-32% of total organic phosphorus). Phosphonates, which contain a direct carbon-phosphorus bond, were detected in only two soils (3% of the organic phosphorus), while pyrophosphate, an inorganic polyphosphate with a chain length of two, was detected in all soils at concentrations up to 13 mg P kg(-1) (3-13% of extracted inorganic phosphorus). Phosphate monoesters were a greater proportion of the total organic phosphorus in neutral soils with high concentrations of phosphorus and organic matter, whereas the proportion of phosphate diesters was greater in very acidic soils low in phosphorus and organic matter. Most soils did not contain detectable concentrations of either myo- or scyllo-inositol hexakisphosphate, which is in marked contrast to many temperate mineral soils that contain abundant inositol phosphates. We conclude that soil properties exert a strong control on the amounts and forms of soil organic phosphorus in tropical rain forests, but that the proportion of the total phosphorus in organic forms is relatively insensitive to variation in climate and soil properties. Further work is now required to assess the contribution of soil organic phosphorus to the nutrition and diversity of plants in these species-rich ecosystems. C1 [Turner, Benjamin L.; Engelbrecht, Bettina M. J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Engelbrecht, Bettina M. J.] Univ Bayreuth, Dept Biol Chem & Geol Sci, D-95440 Bayreuth, Germany. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM turnerbl@si.edu RI Turner, Benjamin/E-5940-2011; Engelbrecht, Bettina/E-9914-2012 OI Turner, Benjamin/0000-0002-6585-0722; FU German Science Foundation (DFG) FX We thank Alex Blumenfeld, Tania Romero, Eric Manzane and Antonio Cueto for technical support, Rick Condit for valuable discussion and calculation of rainfall estimates, Suzanne Lao for assistance with Fig. 1, Nikki Strong for analysis of rock samples from Rio Paja, Sarah Moron and Carlos Jaramillo for assistance in identification of parent materials, and Alex Cheesman for comments on the manuscript. B.M.J.E. was supported by a grant from the German Science Foundation (DFG). The Panama National Environmental Authority (ANAM) granted permission to sample within National Parks. NR 73 TC 67 Z9 73 U1 10 U2 108 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 J9 BIOGEOCHEMISTRY JI Biogeochemistry PD APR PY 2011 VL 103 IS 1-3 BP 297 EP 315 DI 10.1007/s10533-010-9466-x PG 19 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 726TW UT WOS:000287750100019 ER PT J AU Patnaude, DJ Loeb, A Jones, C AF Patnaude, D. J. Loeb, A. Jones, C. TI Evidence for a possible black hole remnant in the Type IIL Supernova 1979C SO NEW ASTRONOMY LA English DT Article DE Supernovae: individual (SN 1979C) - supernova remnants ID X-RAY-EMISSION; SN 1979C; FREE EXPANSION; NEUTRON-STARS; LIGHT CURVES; EVOLUTION; EMERGENCE; FALLBACK; SN1979C; CHANDRA AB We present an analysis of archival X-ray observations of the Type IIL supernova SN 1979C. We find that its X-ray luminosity is remarkably constant at (6.5 +/- 0.1) x 10(38) erg s(-1) over a period of 12 years between 1995 and 2007. The high and steady luminosity is considered as possible evidence for a stellar-mass (similar to 5-10 M-circle dot) black hole accreting material from either a supernova fallback disk or from a binary companion, or possibly from emission from a central pulsar wind nebula. We find that the bright and steady X-ray light curve is not consistent with either a model for a supernova powered by magnetic braking of a rapidly rotating magnetar, or a model where the blast wave is expanding into a dense circumstellar wind. Published by Elsevier B.V. C1 [Patnaude, D. J.; Loeb, A.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Patnaude, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dpatnaude@cfa.harvard.edu FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A, NAS8-03060]; Smithsonian Institution FX We thank Roger Chevalier and Robert Fesen for useful comments on an early draft of this manuscript. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A for A.L, D.J.P and C.J acknowledge support from NASA Contract NAS8-03060 and the Smithsonian Institution. NR 35 TC 11 Z9 11 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1384-1076 J9 NEW ASTRON JI New Astron. PD APR PY 2011 VL 16 IS 3 BP 187 EP 190 DI 10.1016/j.newast.2010.09.004 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 699JT UT WOS:000285660400008 ER PT J AU Moini, M Jiang, LF Bootwala, S AF Moini, Mehdi Jiang, Longfei Bootwala, Samir TI High-throughput analysis using gated multi-inlet mass spectrometry SO RAPID COMMUNICATIONS IN MASS SPECTROMETRY LA English DT Article ID PROTEIN-METAL COMPLEXES; CAPILLARY-ELECTROPHORESIS; AMINO-ACIDS; INTERFACE; MS; PEPTIDES AB Gated multi-inlet mass spectrometry is introduced for high-throughput chemical analysis. In this design, multiple high-pressure liquid chromatography (HPLC) columns or capillary electrophoresis (CE) capillaries are attached to multiple electrosprayers (one for each column or capillary) that spray toward a gated multi-inlet time-of-flight mass spectrometer (TOF-MS). Although all of the sprayers are spraying continuously, only one inlet is exposed at any given time for a specific duration set by the MS data system. The gated multi-sprayer, multi-inlet design significantly enhances the performance of the multi-ESI, multi-inlet TOF-MS with minimal cost and reduces analysis time. The gated multi-sprayer, multi-inlet design was applied to the investigation of column-to-column reproducibility of multiple HPLCs using a peptide mixture and to the simultaneous analysis of four protein digests. In addition, it was applied to the analysis of peptide mixtures using eight CE capillaries. The gated multi-inlet MS has several advantages compared to our previous non-gated multi-inlet MS. For example, because only one inlet is open at one time, the original manufacturer's inlet inner diameter and pumping system can be used, which enhances the sensitivity of detection for each inlet and minimizes the manufacturing cost. In addition, the number of inlets can be increased as desired. The maximum number of liquid streams that can be concurrently analyzed is limited by: (1) the number of inlets, (2) the chromatographic (electrophoretic) peak width, and (3) how fast the gate can move from one position to the next. Copyright (C) 2011 John Wiley & Sons, Ltd. C1 [Moini, Mehdi] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Jiang, Longfei] Univ Texas Austin, Dept Chem & Biochem, Austin, TX 78712 USA. [Bootwala, Samir] Penn Virginia MC Energy, Tulsa, OK 74119 USA. RP Moini, M (reprint author), Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. EM MoiniM@si.edu NR 21 TC 5 Z9 5 U1 1 U2 6 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 MAR 30 PY 2011 VL 25 IS 6 BP 789 EP 794 DI 10.1002/rcm.4924 PG 6 WC Biochemical Research Methods; Chemistry, Analytical; Spectroscopy SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy GA 724SK UT WOS:000287596300014 PM 21337641 ER PT J AU Fleeger, CR Heaney, PJ Post, JE AF Fleeger, Claire R. Heaney, Peter J. Post, Jeffrey E. TI Determining the rate of Cs sequestration by hexagonal H-birnessite and triclinic Na-birnessite as a function of pH SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 241st National Meeting and Exposition of the American-Chemical-Society (ACS) CY MAR 27-31, 2011 CL Anaheim, CA SP Amer Chem Soc C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 27 PY 2011 VL 241 MA 20-GEOC PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 782BO UT WOS:000291982804850 ER PT J AU Keplinger, B Harerimana, IH Desrochers, LP Goodwin, TE Songsasen, N Helsper, JPFG AF Keplinger, Bryan Harerimana, Innocent H. Desrochers, Linda P. Goodwin, Thomas E. Songsasen, Nucharin Helsper, Johannes P. F. G. TI Spde/gc-ms and nmr analysis of volatile organic compounds in maned wolf urine SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 241st National Meeting and Exposition of the American-Chemical-Society (ACS) CY MAR 27-31, 2011 CL Anaheim, CA SP Amer Chem Soc C1 Hendrix Coll, Dept Chem, Conway, AR USA. Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. Plant Res Int, Wageningen, Netherlands. NR 0 TC 0 Z9 0 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 27 PY 2011 VL 241 MA 961-CHED PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 782BO UT WOS:000291982800927 ER PT J AU Shughrue, KM Hark, RR Remus, JJ Harmon, R Wise, MA East, LJ Gonzalez, J Oropeza, DD AF Shughrue, Katrina M. Hark, Richard R. Remus, Jeremiah J. Harmon, Russell Wise, Michael A. East, Lucille J. Gonzalez, Jhanis Oropeza, Dayana D. TI Analysis of the "conflict mineral" columbite-tantalite using laser-induced breakdown spectroscopy (LIBS) and laser ablation inductively coupled plasma mass spectrometry (LA-ICP-MS) SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 241st National Meeting and Exposition of the American-Chemical-Society (ACS) CY MAR 27-31, 2011 CL Anaheim, CA SP Amer Chem Soc C1 Juniata Coll, Dept Chem, Huntingdon, PA 16652 USA. Clarkson Univ, Dept Elect & Comp Engn, Potsdam, NY USA. USA, Res Off, Res Lab, Res Triangle Pk, NC 27709 USA. Smithsonian Inst, Div Mineral, Washington, DC 20560 USA. Appl Spectra Inc, Fremont, CA USA. Univ Calif Berkeley, Lawrence Berkeley Lab, Environm Energy Technol Div, Berkeley, CA 94720 USA. NR 0 TC 0 Z9 0 U1 0 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 27 PY 2011 VL 241 MA 60-ANYL PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 782BO UT WOS:000291982801261 ER PT J AU Smith, BD AF Smith, Bruce D. TI General patterns of niche construction and the management of 'wild' plant and animal resources by small-scale pre-industrial societies SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE human niche construction; resource management; indigenous knowledge small-scale societies; ecosystem engineering; predictive modelling ID FOOD-PRODUCTION; FIRE HISTORY; RAIN-FOREST; NEW-GUINEA; DOMESTICATION; SUBSISTENCE; SETTLEMENT; CHARCOAL; SAVANNA; SITES AB Niche construction efforts by small-scale human societies that involve 'wild' species of plants and animals are organized into a set of six general categories based on the shared characteristics of the target species and similar patterns of human management and manipulation: (i) general modification of vegetation communities, (ii) broadcast sowing of wild annuals, (iii) transplantation of perennial fruit-bearing species, (iv) in-place encouragement of economically important perennials, (v) transplantation and in-place encouragement of perennial root crops, and (vi) landscape modification to increase prey abundance in specific locations. Case study examples, mostly drawn from North America, are presented for each of the six general categories of human niche construction. These empirically documented categories of ecosystem engineering form the basis for a predictive model that outlines potential general principles and commonalities in how small-scale human societies worldwide have modified and manipulated their 'natural' landscapes throughout the Holocene. C1 Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. RP Smith, BD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. EM smithb@si.edu NR 88 TC 71 Z9 74 U1 2 U2 22 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 MAR 27 PY 2011 VL 366 IS 1566 BP 836 EP 848 DI 10.1098/rstb.2010.0253 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 720SX UT WOS:000287302400006 PM 21320898 ER PT J AU Simionescu, A Allen, SW Mantz, A Werner, N Takei, Y Morris, RG Fabian, AC Sanders, JS Nulsen, PEJ George, MR Taylor, GB AF Simionescu, Aurora Allen, Steven W. Mantz, Adam Werner, Norbert Takei, Yoh Morris, R. Glenn Fabian, Andrew C. Sanders, Jeremy S. Nulsen, Paul E. J. George, Matthew R. Taylor, Gregory B. TI Baryons at the Edge of the X-ray-Brightest Galaxy Cluster SO SCIENCE LA English DT Article ID VIRIAL RADIUS; INTRACLUSTER MEDIUM; MASS FRACTION; DARK ENERGY; SUZAKU; CONSTRAINTS; TEMPERATURE; ENTROPY; PROFILE; DENSITY AB Studies of the diffuse x-ray-emitting gas in galaxy clusters have provided powerful constraints on cosmological parameters and insights into plasma astrophysics. However, measurements of the faint cluster outskirts have become possible only recently. Using data from the Suzaku x-ray telescope, we determined an accurate, spatially resolved census of the gas, metals, and dark matter out to the edge of the Perseus Cluster. Contrary to previous results, our measurements of the cluster baryon fraction are consistent with the expected universal value at half of the virial radius. The apparent baryon fraction exceeds the cosmic mean at larger radii, suggesting a clumpy distribution of the gas, which is important for understanding the ongoing growth of clusters from the surrounding cosmic web. C1 [Simionescu, Aurora; Allen, Steven W.; Werner, Norbert; Morris, R. Glenn] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Mantz, Adam] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Takei, Yoh] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Fabian, Andrew C.; Sanders, Jeremy S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Nulsen, Paul E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Taylor, Gregory B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Taylor, Gregory B.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Simionescu, A (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. EM asimi@stanford.edu RI XRAY, SUZAKU/A-1808-2009; OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU NASA [PF9-00070, PF8-90056, NAS8-03060, NNX09AV64G, NNX10AR48G, NNX08AZ88G]; JAXA; U.S. Department of Energy [DE-AC02-76SF00515]; Ministry of Education, Culture, Sports, Science, and Technology of Japan [22111513]; Chandra award [GO0-11138B] FX We thank P. Thomas and O. Young for kindly providing the simulation results shown in Fig. 4. Support for this work was provided by NASA through Einstein Postdoctoral Fellowship grants number PF9-00070 and PF8-90056 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We acknowledge NASA grants NNX09AV64G and NNX10AR48G, issued through the Suzaku Guest Observer program, and grant NNX08AZ88G. The authors thank the Suzaku operation team and Guest Observer Facility, supported by JAXA and NASA. This work was supported in part by the U.S. Department of Energy under contract number DE-AC02-76SF00515. We also acknowledge the Grant-in-Aid for Scientific Research of the Ministry of Education, Culture, Sports, Science, and Technology of Japan (KAKENHI no. 22111513) and Chandra award GO0-11138B. NR 28 TC 150 Z9 150 U1 2 U2 6 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 MAR 25 PY 2011 VL 331 IS 6024 BP 1576 EP 1579 DI 10.1126/science.1200331 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 739XH UT WOS:000288754500047 PM 21436446 ER PT J AU Abbot, P Abe, J Alcock, J Alizon, S Alpedrinha, JAC Andersson, M Andre, JB van Baalen, M Balloux, F Balshine, S Barton, N Beukeboom, LW Biernaskie, JM Bilde, T Borgia, G Breed, M Brown, S Bshary, R Buckling, A Burley, NT Burton-Chellew, MN Cant, MA Chapuisat, M Charnov, EL Clutton-Brock, T Cockburn, A Cole, BJ Colegrave, N Cosmides, L Couzin, ID Coyne, JA Creel, S Crespi, B Curry, RL Dall, SRX Day, T Dickinson, JL Dugatkin, LA El Mouden, C Emlen, ST Evans, J Ferriere, R Field, J Foitzik, S Foster, K Foster, WA Fox, CW Gadau, J Gandon, S Gardner, A Gardner, MG Getty, T Goodisman, MAD Grafen, A Grosberg, R Grozinger, CM Gouyon, PH Gwynne, D Harvey, PH Hatchwell, BJ Heinze, J Helantera, H Helms, KR Hill, K Jiricny, N Johnstone, RA Kacelnik, A Kiers, ET Kokko, H Komdeur, J Korb, J Kronauer, D Kummerli, R Lehmann, L Linksvayer, TA Lion, S Lyon, B Marshall, JAR McElreath, R Michalakis, Y Michod, RE Mock, D Monnin, T Montgomerie, R Moore, AJ Mueller, UG Noe, R Okasha, S Pamilo, P Parker, GA Pedersen, JS Pen, I Pfennig, D Queller, DC Rankin, DJ Reece, SE Reeve, HK Reuter, M Roberts, G Robson, SKA Roze, D Rousset, F Rueppell, O Sachs, JL Santorelli, L Schmid-Hempel, P Schwarz, MP Scott-Phillips, T Shellmann-Sherman, J Sherman, PW Shuker, DM Smith, J Spagna, JC Strassmann, B Suarez, AV Sundstrom, L Taborsky, M Taylor, P Thompson, G Tooby, J Tsutsui, ND Tsuji, K Turillazzi, S Ubeda, F Vargo, EL Voelkl, B Wenseleers, T West, SA West-Eberhard, MJ Westneat, DF Wiernasz, DC Wild, G Wrangham, R Young, AJ Zeh, DW Zeh, JA Zink, A AF Abbot, Patrick Abe, Jun Alcock, John Alizon, Samuel Alpedrinha, Joao A. C. Andersson, Malte Andre, Jean-Baptiste van Baalen, Minus Balloux, Francois Balshine, Sigal Barton, Nick Beukeboom, Leo W. Biernaskie, Jay M. Bilde, Trine Borgia, Gerald Breed, Michael Brown, Sam Bshary, Redouan Buckling, Angus Burley, Nancy T. Burton-Chellew, Max N. Cant, Michael A. Chapuisat, Michel Charnov, Eric L. Clutton-Brock, Tim Cockburn, Andrew Cole, Blaine J. Colegrave, Nick Cosmides, Leda Couzin, Iain D. Coyne, Jerry A. Creel, Scott Crespi, Bernard Curry, Robert L. Dall, Sasha R. X. Day, Troy Dickinson, Janis L. Dugatkin, Lee Alan El Mouden, Claire Emlen, Stephen T. Evans, Jay Ferriere, Regis Field, Jeremy Foitzik, Susanne Foster, Kevin Foster, William A. Fox, Charles W. Gadau, Juergen Gandon, Sylvain Gardner, Andy Gardner, Michael G. Getty, Thomas Goodisman, Michael A. D. Grafen, Alan Grosberg, Rick Grozinger, Christina M. Gouyon, Pierre-Henri Gwynne, Darryl Harvey, Paul H. Hatchwell, Ben J. Heinze, Juergen Helantera, Heikki Helms, Ken R. Hill, Kim Jiricny, Natalie Johnstone, Rufus A. Kacelnik, Alex Kiers, E. Toby Kokko, Hanna Komdeur, Jan Korb, Judith Kronauer, Daniel Kuemmerli, Rolf Lehmann, Laurent Linksvayer, Timothy A. Lion, Sebastien Lyon, Bruce Marshall, James A. R. McElreath, Richard Michalakis, Yannis Michod, Richard E. Mock, Douglas Monnin, Thibaud Montgomerie, Robert Moore, Allen J. Mueller, Ulrich G. Noe, Ronald Okasha, Samir Pamilo, Pekka Parker, Geoff A. Pedersen, Jes S. Pen, Ido Pfennig, David Queller, David C. Rankin, Daniel J. Reece, Sarah E. Reeve, Hudson K. Reuter, Max Roberts, Gilbert Robson, Simon K. A. Roze, Denis Rousset, Francois Rueppell, Olav Sachs, Joel L. Santorelli, Lorenzo Schmid-Hempel, Paul Schwarz, Michael P. Scott-Phillips, Tom Shellmann-Sherman, Janet Sherman, Paul W. Shuker, David M. Smith, Jeff Spagna, Joseph C. Strassmann, Beverly Suarez, Andrew V. Sundstrom, Liselotte Taborsky, Michael Taylor, Peter Thompson, Graham Tooby, John Tsutsui, Neil D. Tsuji, Kazuki Turillazzi, Stefano Ubeda, Francisco Vargo, Edward L. Voelkl, Bernard Wenseleers, Tom West, Stuart A. West-Eberhard, Mary Jane Westneat, David F. Wiernasz, Diane C. Wild, Geoff Wrangham, Richard Young, Andrew J. Zeh, David W. Zeh, Jeanne A. Zink, Andrew TI Inclusive fitness theory and eusociality SO NATURE LA English DT Letter ID KIN SELECTION; EVOLUTION; BEHAVIOUR; MODEL C1 [Abbot, Patrick] Vanderbilt Univ, Nashville, TN 37235 USA. [Abe, Jun] Shizuoka Univ, Fac Agr, Appl Entomol Lab, Shizuoka 4228529, Japan. [Alcock, John] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Alizon, Samuel; Michalakis, Yannis] IRD, UMR CNRS IRD 2724, F-34394 Montpellier 5, France. [Alpedrinha, Joao A. C.; Biernaskie, Jay M.; Brown, Sam; Buckling, Angus; Burton-Chellew, Max N.; El Mouden, Claire; Foster, Kevin; Gardner, Andy; Grafen, Alan; Harvey, Paul H.; Jiricny, Natalie; Kacelnik, Alex; West, Stuart A.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Andersson, Malte] Univ Gothenburg, Dept Zool, SE-40530 Gothenburg, Sweden. [Andre, Jean-Baptiste; van Baalen, Minus; Monnin, Thibaud] Univ Paris 06, CNRS, UMR 7625, Ecole Normale Super, F-75005 Paris, France. [Balloux, Francois] Univ London Imperial Coll Sci Technol & Med, Fac Med, Dept Infect Dis Epidemiol, MRC Ctr Outbreak Anal & Modelling, London W2 1PG, England. [Balshine, Sigal] McMaster Univ, Dept Psychol Neurosci & Behav, Hamilton, ON L8S 4K1, Canada. [Barton, Nick] IST Austria, A-3400 Klosterneuburg, Austria. [Beukeboom, Leo W.] Univ Groningen, Ctr Ecol & Evolutionary Studies, NL-9750 AA Haren, Netherlands. [Bilde, Trine] Aarhus Univ, Dept Biol Sci, DK-8000 Aarhus C, Denmark. [Borgia, Gerald] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Breed, Michael] Univ Colorado, Boulder, CO 80309 USA. [Bshary, Redouan; Lehmann, Laurent] Fac Sci, CH-2000 Neuchatel, Switzerland. [Burley, Nancy T.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. [Cant, Michael A.; Dall, Sasha R. X.; Moore, Allen J.; Young, Andrew J.] Univ Exeter, Ctr Ecol & Conservat, Tremough TR10 9EZ, Penryn, England. [Chapuisat, Michel] Univ Lausanne, Dept Ecol & Evolut, CH-1015 Lausanne, Switzerland. [Charnov, Eric L.] 1 Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Clutton-Brock, Tim; Foster, William A.; Johnstone, Rufus A.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Cockburn, Andrew; Kokko, Hanna] Australian Natl Univ, Res Sch Biol, Canberra, ACT 0200, Australia. [Cole, Blaine J.; Wiernasz, Diane C.] Univ Houston, Dept Biol & Biochem, Houston, TX 77204 USA. [Colegrave, Nick; Reece, Sarah E.] Univ Edinburgh, Ashworth Labs, Sch Biol Sci, Inst Evolut, Edinburgh EH9 3JT, Midlothian, Scotland. [Colegrave, Nick; Reece, Sarah E.] Univ Edinburgh, Ashworth Labs, Sch Biol Sci, Inst Immunol & Infect Res, Edinburgh EH9 3JT, Midlothian, Scotland. [Cosmides, Leda] Univ Calif Santa Barbara, Dept Psychol, Santa Barbara, CA 93106 USA. [Couzin, Iain D.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08540 USA. [Coyne, Jerry A.] Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60637 USA. [Creel, Scott] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA. [Crespi, Bernard] Simon Fraser Univ, Dept Biosci, Burnaby, BC V5A 1S6, Canada. [Curry, Robert L.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Day, Troy; Taylor, Peter] Queens Univ, Dept Math & Stat, Kingston, ON K7L 3N6, Canada. [Dickinson, Janis L.] Cornell Univ, Johnson Ctr, Cornell Lab Ornithol, Ithaca, NY 14850 USA. [Dugatkin, Lee Alan] Univ Louisville, Dept Biol, Louisville, KY 40292 USA. [Emlen, Stephen T.; Shellmann-Sherman, Janet; Sherman, Paul W.] Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA. [Evans, Jay] USDA ARS, Bee Res Lab, Beltsville, MD 20705 USA. [Ferriere, Regis] Ecole Normale Super, CNRS, UMR 7625, Lab Ecol & Evolut, F-75005 Paris, France. [Ferriere, Regis] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Field, Jeremy] Univ Sussex, Sch Life Sci, Brighton BN1 9QG, E Sussex, England. [Foitzik, Susanne] Univ Munich, Dept Biol Behav Ecol Verhaltensokol 2, D-82152 Planegg Martinsried, Germany. [Fox, Charles W.] Univ Kentucky, Dept Entomol, Lexington, KY 40546 USA. [Gadau, Juergen] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Gandon, Sylvain] CEFE UMR 5175, F-34293 Montpellier, France. [Gardner, Michael G.] Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA 5001, Australia. [Getty, Thomas] Michigan State Univ, Kellogg Biol Stn, Hickory Corners, MI 49060 USA. [Getty, Thomas] Michigan State Univ, Dept Zool, Hickory Corners, MI 49060 USA. [Goodisman, Michael A. D.] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. [Goodisman, Michael A. D.] Georgia Inst Technol, Petit Inst Bioengn & Biosci, Atlanta, GA 30332 USA. [Grosberg, Rick] Univ Calif Davis, Coll Biol Sci, Dept Ecol & Evolut, Davis, CA 95616 USA. [Grozinger, Christina M.] Penn State Univ, Huck Inst Life Sci, Ctr Pollinator Res, Chem Ecol Lab 4A, University Pk, PA 16802 USA. [Gouyon, Pierre-Henri] Museum Natl Hist Nat, F-75005 Paris, France. [Gwynne, Darryl] Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. [Hatchwell, Ben J.] Univ Sheffield, Dept Anim & Plant Sci, Western Bank, Sheffield S10 2TN, S Yorkshire, England. [Heinze, Juergen] Univ Regensburg, D-93040 Regensburg, Germany. [Helantera, Heikki; Sundstrom, Liselotte] Univ Helsinki, Dept Biosci, FI-00014 Helsinki, Finland. [Helms, Ken R.] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Hill, Kim] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Kiers, E. Toby] Vrije Univ Amsterdam, Fac Earth & Life Sci, Inst Ecol Sci, Dept Anim Ecol, NL-1081 HV Amsterdam, Netherlands. [Komdeur, Jan] Univ Groningen, Ctr Evolutionary & Ecol Studies, Anim Ecol Grp, NL-9750 AA Haren, Netherlands. [Korb, Judith] Univ Osnabruck, D-49076 Osnabruck, Germany. [Kronauer, Daniel] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Kuemmerli, Rolf] Swiss Fed Inst Aquat Res & Technol, CH-8600 Dubendorf, Switzerland. [Linksvayer, Timothy A.; Pedersen, Jes S.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. [Lion, Sebastien] Univ London, Sch Biol Sci, Egham TW20 0EX, Surrey, England. [Lyon, Bruce] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Marshall, James A. R.] Univ Sheffield, Dept Comp Sci, Sheffield S1 4DP, S Yorkshire, England. [McElreath, Richard] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [McElreath, Richard] Univ Calif Davis, Ctr Populat Biol, Davis, CA 95616 USA. [Michod, Richard E.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Mock, Douglas] Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. [Montgomerie, Robert] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Mueller, Ulrich G.] Univ Texas Austin, Austin, TX 78712 USA. [Noe, Ronald] Psychol Univ Strasbourg, Ethol Primates DEPE IPHC CNRS UMR 7178, F-67087 Strasbourg, France. [Okasha, Samir] Univ Bristol, Dept Philosophy, Bristol BS8 1TB, Avon, England. [Pamilo, Pekka] Univ Helsinki, Bioctr Oulu, Helsinki 00140, Finland. [Pamilo, Pekka] Univ Helsinki, Dept Biosci, Helsinki 00140, Finland. [Parker, Geoff A.] Univ Liverpool, Inst Integrat Biol, Liverpool L69 7ZB, Merseyside, England. [Pen, Ido] Univ Groningen, Theoret Biol Grp, NL-9750 AA Haren, Netherlands. [Pfennig, David] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. [Queller, David C.; Smith, Jeff] Rice Univ, Dept Ecol & Evolutionary Biol, Houston, TX 77005 USA. [Rankin, Daniel J.] Univ Zurich, Dept Biochem, CH-8057 Zurich, Switzerland. [Rankin, Daniel J.] Swiss Inst Bioinformat, CH-1015 Lausanne, Switzerland. [Reuter, Max] UCL, Fac Life Sci, Res Dept Genet Evolut & Environm, London NW1 2HE, England. [Roberts, Gilbert] Newcastle Univ, Fac Med Sci, Inst Neurosci, Ctr Behav & Evolut, Newcastle Upon Tyne NE2 4HH, Tyne & Wear, England. [Robson, Simon K. A.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Roze, Denis] CNRS UPMC UMR 7144, Stn Biol Roscoff, F-29680 Roscoff, France. [Rousset, Francois] Univ Montpellier 2, Inst Sci Evolut, F-34095 Montpellier, France. [Rueppell, Olav] Univ N Carolina, Dept Biol, Greensboro, NC 27403 USA. [Sachs, Joel L.] Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. [Schmid-Hempel, Paul] Swiss Fed Inst Technol, Inst Integrat Biol IBZ, CH-8092 Zurich, Switzerland. [Scott-Phillips, Tom] Univ Edinburgh, Sch Philosophy Psychol & Language Sci, Edinburgh EH8 9AD, Midlothian, Scotland. [Shuker, David M.] Univ St Andrews, Sch Biol, St Andrews KY16 9TH, Fife, Scotland. [Spagna, Joseph C.] William Paterson Univ New Jersey, Wayne, NJ 07470 USA. [Strassmann, Beverly] Univ Michigan, Dept Anthropol, Ann Arbor, MI 48109 USA. [Suarez, Andrew V.] Univ Illinois, Dept Entomol, Urbana, IL 61801 USA. [Suarez, Andrew V.] Univ Illinois, Dept Anim Biol, Urbana, IL 61801 USA. [Taborsky, Michael] Univ Bern, Inst Ecol & Evolut, CH-3032 Hinterkappelen, Switzerland. [Thompson, Graham] Univ Western Ontario, Dept Biol, London, ON N6A 5B7, Canada. [Tooby, John] Univ Calif Santa Barbara, Dept Anthropol, Santa Barbara, CA 93106 USA. [Tsutsui, Neil D.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Tsuji, Kazuki] Univ Ryukyus, Fac Agr, Okinawa 9030213, Japan. [Turillazzi, Stefano] Univ Florence, Dipartimento Biol Evoluzionist, I-50125 Florence, Italy. [Ubeda, Francisco] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37902 USA. [Vargo, Edward L.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Voelkl, Bernard] Humboldt Univ, Inst Theoret Biol, D-10115 Berlin, Germany. [Wenseleers, Tom] Katholieke Univ Leuven, Inst Zool, Dept Biol, B-3000 Louvain, Belgium. [West-Eberhard, Mary Jane] Smithsonian Trop Res Inst, Balboa, Panama. [Westneat, David F.] Univ Kentucky, Dept Biol, Lexington, KY 40506 USA. [Wild, Geoff] Univ Western Ontario, Dept Appl Math, London, ON N6A 5B7, Canada. [Wrangham, Richard] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Zeh, David W.; Zeh, Jeanne A.] Univ Nevada, Dept Biol, Reno, NV 89557 USA. [Zeh, David W.; Zeh, Jeanne A.] Univ Nevada, Program Ecol Evolut & Conservat Biol, Reno, NV 89557 USA. [Zink, Andrew] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. RP Abbot, P (reprint author), Vanderbilt Univ, 221 Kirkland Hall, Nashville, TN 37235 USA. EM Stuart.West@zoo.ox.ac.uk RI Tsuji, Kazuki/D-6607-2014; Gardner, Andy/K-5353-2013; Evans, Jay/C-8408-2012; Brown, Sam/B-5234-2009; Pedersen, Jes Soe/J-6337-2014; West, Stuart/M-3608-2014; Research ID, CTBCC /O-3564-2014; Lion, Sebastien/K-4177-2015; Cockburn, Andrew/A-4864-2008; Taborsky, Michael/F-8420-2013; Hatchwell, Ben/C-5433-2016; Kummerli, Rolf/E-2844-2016; Wenseleers, Tom/J-3960-2013; Thompson, Graham/B-6508-2008; Lyon, Bruce/E-8491-2011; lehmann, laurent/B-6875-2012; Fox, Charles/I-5274-2012; Reuter, Max/B-8987-2008; Parker, Geoff/C-4337-2008; van Baalen, Minus/J-9285-2012; Monnin, Thibaud/J-9409-2012; Gouyon, Pierre-Henri/A-9603-2013; Beukeboom, Leo/D-1808-2012; Rankin, Daniel/E-4178-2013; Shuker, David/E-8827-2013; Bilde, Trine/J-2872-2013; Noe, Ronald/C-4482-2008; Balloux, Francois/D-4783-2009; Cant, Michael/B-1982-2009; Dall, Sasha/B-2642-2010; Reece, Sarah/C-9447-2009; Pamilo, Pekka/C-6907-2011; Kokko, Hanna/C-7861-2009; Helantera, Heikki/C-7568-2011; Robson, Simon/D-1168-2011; Rankin, Daniel/D-7075-2011; Sundstrom, Liselotte/G-5080-2010; Rueppell, Olav/G-2679-2010; Voelkl, Bernhard/D-1390-2009; Montgomerie, Robert/C-6516-2008 OI Sundstrom, Liselotte Bjornsdotter/0000-0002-6176-8940; Westneat, David/0000-0001-5163-8096; Balloux, Francois/0000-0003-1978-7715; Marshall, James/0000-0002-1506-167X; Burton-Chellew, Maxwell/0000-0002-5330-0379; Alpedrinha, Joao/0000-0003-1036-1021; Couzin, Iain/0000-0001-8556-4558; Alizon, Samuel/0000-0002-0779-9543; Wild, Geoff/0000-0001-7821-7304; Tsuji, Kazuki/0000-0002-2027-8582; BREED, MICHAEL/0000-0002-4039-8354; Grafen, Alan/0000-0002-1843-6457; Gardner, Andy/0000-0002-1304-3734; Evans, Jay/0000-0002-0036-4651; Brown, Sam/0000-0003-1892-9275; Pedersen, Jes Soe/0000-0002-4439-2638; West, Stuart/0000-0003-2152-3153; Lion, Sebastien/0000-0002-4081-0038; Taborsky, Michael/0000-0002-1357-4316; Hatchwell, Ben/0000-0002-1039-4782; Kummerli, Rolf/0000-0003-4084-6679; Wenseleers, Tom/0000-0002-1434-861X; Fox, Charles/0000-0002-7545-7967; Reuter, Max/0000-0001-9554-0795; Parker, Geoff/0000-0003-4795-6352; Monnin, Thibaud/0000-0003-3762-942X; Rankin, Daniel/0000-0001-7709-6926; Bilde, Trine/0000-0002-0341-161X; Noe, Ronald/0000-0003-1976-0555; Cant, Michael/0000-0002-1530-3077; Dall, Sasha/0000-0001-9873-6507; Helantera, Heikki/0000-0002-6468-5956; Robson, Simon/0000-0001-8870-1933; Rueppell, Olav/0000-0001-5370-4229; Voelkl, Bernhard/0000-0001-5454-2508; Montgomerie, Robert/0000-0003-4701-4525 FU Biotechnology and Biological Sciences Research Council [BB/H022716/1] NR 16 TC 126 Z9 128 U1 54 U2 457 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD MAR 24 PY 2011 VL 471 IS 7339 BP E1 EP E4 DI 10.1038/nature09831 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 739GJ UT WOS:000288702200001 PM 21430721 ER PT J AU Herre, EA Wcislo, WT AF Herre, Edward Allen Wcislo, William T. TI In defence of inclusive fitness theory SO NATURE LA English DT Letter ID SOCIAL INTERACTIONS; EVOLUTION; EUSOCIALITY; HYMENOPTERA; MONOGAMY; SOLITARY; BEE C1 [Herre, Edward Allen; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama. [Herre, Edward Allen; Wcislo, William T.] Smithsonian Trop Res Inst, MRC 0580 06, Unit 9100, Dpo, AA 34002 USA. RP Herre, EA (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM herrea@si.edu NR 15 TC 21 Z9 22 U1 5 U2 43 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAR 24 PY 2011 VL 471 IS 7339 BP E8 EP E9 DI 10.1038/nature09835 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 739GJ UT WOS:000288702200005 PM 21430725 ER PT J AU Harmelin, JG Ostrovsky, AN Caceres-Chamizo, JP Sanner, J AF Harmelin, Jean-Georges Ostrovsky, Andrew N. Caceres-Chamizo, Julia P. Sanner, Joann TI Bryodiversity in the tropics: taxonomy of Microporella species (Bryozoa, Cheilostomata) with personate maternal zooids from Indian Ocean, Red Sea and southeast Mediterranean SO ZOOTAXA LA English DT Article DE bryozoans; biodiversity; Ascophora; Microporellidae; ovicell; new species; biogeography; alien species ID AEGEAN ISLAND; MARINE; RECORDS; LIST AB The particularly speciose cheilostomate genus Microporella includes taxa whose maternal zooids and associated ovicells present a personate structure, i.e. a particularly developed peristome. Six species of Microporella with personate ovicells are analysed from material sampled in the Indian Ocean, Red Sea and southeast Mediterranean. Consideration of highly diagnostic tiny morphological characters displayed by the primary orifice and the avicularium has made it possible to distinguish three new species, M. browni n. sp., M. maldiviensis n. sp. and M. collaroides n. sp., and to better characterise the other species. Among the latter, two species named by Audouin (1826) from Savigny's drawings (1817), M. coronata and M. genisii, are redescribed and neotypes are selected. Additionally, a new species of the M. coronata species group, Microporella hastingsae n. sp., is proposed following examination of a museum specimen recorded as M. ciliata var. coronata (Hastings 1927). The species dealt with in this study revealed remarkably different patterns of geographic distribution, possibly showing different potential for natural and/or anthropogenic dispersal. The bryozoan assemblages sampled along the coast of Lebanon include four of the six studied species, at least three of them presumably non-indigenous including M. harmeri Hayward, which displays a remarkably wide distribution from the Indian Ocean to the West Pacific and the East Atlantic (Canary Islands). C1 [Harmelin, Jean-Georges] Univ Aix Marseille 2, Ctr Oceanol Marseille, UMR CNRS 6540, Marine Endoume Stn, F-13007 Marseille, France. [Ostrovsky, Andrew N.] St Petersburg State Univ, Dept Invertebrate Zool, Fac Biol & Soil Sci, St Petersburg 199034, Russia. [Ostrovsky, Andrew N.; Caceres-Chamizo, Julia P.] Univ Vienna, Dept Palaeontol, Fac Earth Sci Geog & Astron, Geozentrum, A-1090 Vienna, Austria. [Sanner, Joann] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Harmelin, JG (reprint author), Univ Aix Marseille 2, Ctr Oceanol Marseille, UMR CNRS 6540, Marine Endoume Stn, F-13007 Marseille, France. EM jean-georges.harmelin@univmed.fr; oan_univer@yahoo.com RI Ostrovsky, Andrew/D-6439-2012 OI Ostrovsky, Andrew/0000-0002-3646-9439 FU FWF, Austria [P19337-B17, P22696-B17]; RFBR, Russia [10-04-00085a] FX We are deeply indebted to Dr G. Bitar, Lebanese University, Dr H. Zibrowius, Centre d'Oceanologie de Marseille, A. Azeez A. Hakeem, R. Tomasetti, M. Rifshan, I. Nimad, Marine Laboratory, Banyan Tree Resort, Vabbinfaru Island, Maldives, and Dr M. R. G. Claereboudt, Sultan Qaboos University, Muscat, for their kind assistance and help with collecting material by scuba. Our thanks to Dr P. D. Taylor, Dr K. Tilbrook and M. Spencer Jones, The Natural History Museum, London, Dr J.-L. d'Hondt, Museum National d'Histoire Naturelle, Paris, and Dr J. Scholz, Senckenberg Museum, Frankfurt am Main, for giving access to collections, sending us unpublished photos and checking the type material. Dr K. Kleemann, Department of Palaeontology, University of Vienna, kindly provided additional material, Dr P. J. Hayward, University of Wales, Swansea, sent us photos of the type specimen of M. harmeri and Dr D. P. Gordon provided documents. A. Ostrovsky thanks FWF, Austria (grants P19337-B17 and P22696-B17) and RFBR, Russia (grant 10-04-00085a) for financial support. NR 83 TC 14 Z9 15 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 MAR 23 PY 2011 IS 2798 BP 1 EP 30 PG 30 WC Zoology SC Zoology GA 738NA UT WOS:000288645300001 ER PT J AU Hailer, F Schreiber, EA Miller, JM Levin, II Parker, PG Chesser, RT Fleischer, RC AF Hailer, Frank Schreiber, E. A. Miller, Joshua M. Levin, Iris I. Parker, Patricia G. Chesser, R. Terry Fleischer, Robert C. TI Long-term isolation of a highly mobile seabird on the Galapagos SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Galapagos endemism; microsatellites; morphological differentiation; mtDNA; nuclear introns; philopatry ID POPULATION-STRUCTURE; COMPUTER-PROGRAM; DNA-SEQUENCES; SEA; SOFTWARE; BIRDS; PELECANIFORMES; DIVERGENCE; FREGATIDAE; INFERENCE AB The Galapagos Islands are renowned for their high degree of endemism. Marine taxa inhabiting the archipelago might be expected to be an exception, because of their utilization of pelagic habitats-the dispersal barrier for terrestrial taxa-as foraging grounds. Magnificent frigatebirds (Fregata magnificens) have a highly vagile lifestyle and wide geographical distribution around the South and Central American coasts. Given the potentially high levels of gene flow among populations, the species provides a good test of the effectiveness of the Galapagos ecosystem in isolating populations of highly dispersive marine species. We studied patterns of genetic (mitochondrial DNA, microsatellites and nuclear introns) and morphological variation across the distribution of magnificent frigatebirds. Concordant with predictions from life-history traits, we found signatures of extensive gene flow over most of the range, even across the Isthmus of Panama, which is a major barrier to gene flow in other tropical seabirds. In contrast, individuals from the Galapagos were strongly differentiated from all conspecifics, and have probably been isolated for several hundred thousand years. Our finding is a powerful testimony to the evolutionary uniqueness of the taxa inhabiting the Galapagos archipelago and its associated marine ecosystems. C1 [Hailer, Frank; Schreiber, E. A.; Miller, Joshua M.; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Hailer, Frank; Schreiber, E. A.; Miller, Joshua M.; Fleischer, Robert C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20008 USA. [Levin, Iris I.; Parker, Patricia G.] Univ Missouri, Whitney R Harris World Ecol Ctr, St Louis, MO 63110 USA. [Levin, Iris I.; Parker, Patricia G.] Univ Missouri, Dept Biol, St Louis, MO 63110 USA. [Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20560 USA. RP Hailer, F (reprint author), Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM hailerf@si.edu RI Hailer, Frank/C-9114-2012; Miller, Joshua/E-3072-2013; Miller, Joshua/J-3393-2014 OI Hailer, Frank/0000-0002-2340-1726; Miller, Joshua/0000-0002-4019-7675; Miller, Joshua/0000-0002-4019-7675 FU Microsoft Corporation; Saint Louis Zoo; Zoological Studies at the University of Missouri-St Louis; Smithsonian's James Bond Fund; Marine Science Network; Center for Conservation and Evolutionary Genetics; T. L. Cross and Seabird Research Inc. FX For permits to collect blood samples and facilitation of fieldwork, we thank (i) Bahamas: Department of Agriculture and the Gerace Research Center; (ii) Belize: Ministry of Natural Resources and the Environment, Toledo Institute for Development and Environment, and Belize Audubon Society; (iii) British Virgin Islands: Department of Environment and Fisheries, National Parks Trust, Henry Jarecki and Skip Lazell; (iv) Cayman Islands: Department of the Environment and National Trust; (v) Ecuador: Galapagos National Park, Charles Darwin Foundation; (vi) Jamaica: National Environment and Planning Agency, The Nature Conservancy, Nathalie Zenny, Ann Sutton and Brandon Hay; (vii) Panama: Autoridad Nacional del Ambiente, Smithsonian Tropical Research Institute, George Angehr and Jim Kushlan; and (viii) Dry Tortugas, Florida, US: National Park Service and Sonny Bass. The California Academy of Sciences and National Museum of Natural History are gratefully acknowledged for granting permission to access and sample their collections. We thank Gary Schenk, Jon Beadell, Judy Pierce, Bill Hayes, Mike Favazza, Cheryl McKinley and Anita Carrion for assistance in the field. We thank Thomas Mueller, Don Dearborn, Storrs Olson, Carlos Valle, Peter Beerli, Andreanna Welch, Sharyn Hood, Heather Lerner and Amy Wilson for discussions. Part of this work was carried out by using the resources of Cornell University's Computational Biology Service Unit, which is partially funded by Microsoft Corporation. Galapagos sampling was funded by the Field Research for Conservation programme of the Saint Louis Zoo and the Des Lee Professorship in Zoological Studies at the University of Missouri-St Louis and the Saint Louis Zoo. The Smithsonian's James Bond Fund, Marine Science Network, and the Center for Conservation and Evolutionary Genetics, T. L. Cross and Seabird Research Inc. provided funding. NR 55 TC 24 Z9 24 U1 4 U2 29 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 MAR 22 PY 2011 VL 278 IS 1707 BP 817 EP 825 DI 10.1098/rspb.2010.1342 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 718NJ UT WOS:000287129800005 PM 20861041 ER PT J AU Fong, W Berger, E Chornock, R Tanvir, NR Levan, AJ Fruchter, AS Graham, F Cucchiara, A Fox, DB AF Fong, W. Berger, E. Chornock, R. Tanvir, N. R. Levan, A. J. Fruchter, A. S. Graham, F. Cucchiara, A. Fox, D. B. TI THE OPTICAL AFTERGLOW AND z=0.92 EARLY-TYPE HOST GALAXY OF THE SHORT GRB 100117A SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (100117A) ID GAMMA-RAY BURST; STAR-FORMATION; POPULATION SYNTHESIS; HIGH-REDSHIFT; LIGHT CURVES; GRB-050724; PROGENITOR; ENERGETICS; EMISSION; ENVIRONMENTS AB We present the discovery of the optical afterglow and early-type host galaxy of the short-duration GRB 100117A. The faint afterglow is detected 8.3 hr after the burst with r(AB) = 25.46 +/- 0.20 mag. Follow-up optical and near-infrared observations uncover a coincident compact red galaxy, identified as an early-type galaxy at a spectroscopic redshift of z approximate to 0.915 with a mass of similar to 3 x 10(10) M-circle dot, an age of similar to 1 Gyr, and a luminosity of L-B similar or equal to 0.5 L-*. From a possible weak detection of [O II]lambda 3727 emission at z = 0.915 we infer an upper bound on the star formation rate of similar to 0.1 M-circle dot yr(-1), leading to a specific star formation rate of less than or similar to 0.004 Gyr(-1). Thus, GRB 100117A is only the second short burst to date with a secure early-type host (the other being GRB 050724 at z = 0.257) and it has one of the highest short gamma-ray burst (GRB) redshifts. The offset between the host center and the burst position, 470 +/- 310 pc, is the smallest to date. Combined with the old stellar population age, this indicates that the burst likely originated from a progenitor with no significant kick velocity. However, from the brightness of the optical afterglow we infer a relatively low density of n approximate to 3 x 10(-4) epsilon(-3)(e,-1)epsilon(-1.75)(B,-1) cm(-3). The combination of an optically faint afterglow and host suggests that previous such events may have been missed, thereby potentially biasing the known short GRB host population against z greater than or similar to 1 early-type hosts. C1 [Fong, W.; Berger, E.; Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Fruchter, A. S.; Graham, F.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Cucchiara, A.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. RP Fong, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Swift AO5 grant [5080010]; Swift AO6 grant [6090612] FX We thank Rik Williams and Daniel Kelson for obtaining rapid observations of GRB 100117A with IMACS. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Observations were also 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 Particle Physics and Astronomy Research Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). This work also made use of data supplied by the UK Swift Science Data Center at the University of Leicester. This work was partially supported by Swift AO5 grant 5080010 and AO6 grant 6090612. NR 55 TC 34 Z9 35 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 MAR 20 PY 2011 VL 730 IS 1 AR 26 DI 10.1088/0004-637X/730/1/26 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735XI UT WOS:000288453600026 ER PT J AU Kelly, BC Sobolewska, M Siemiginowska, A AF Kelly, Brandon C. Sobolewska, Malgorzata Siemiginowska, Aneta TI A STOCHASTIC MODEL FOR THE LUMINOSITY FLUCTUATIONS OF ACCRETING BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; methods: data analysis; quasars: general ID ACTIVE GALACTIC NUCLEI; X-RAY VARIABILITY; SEYFERT-1 GALAXY ARAKELIAN-564; POWER-DENSITY SPECTRA; TIME-SERIES ANALYSIS; NARROW-LINE; FUNDAMENTAL PLANE; OPTICAL VARIABILITY; TIMING PROPERTIES; XMM-NEWTON AB In this work, we have developed a new stochastic model for the fluctuations in light curves of accreting black holes. The model is based on a linear combination of stochastic processes and is also the solution to the linear diffusion equation perturbed by a spatially correlated noise field. This allows flexible modeling of the power spectral density (PSD), and we derive the likelihood function for the process, enabling one to estimate the parameters of the process, including break frequencies in the PSD. Our statistical technique is computationally efficient, unbiased by aliasing and red noise leak, and fully accounts for irregular sampling and measurement errors. We show that our stochastic model provides a good approximation to the X-ray light curves of galactic black holes, and the optical and X-ray light curves of active galactic nuclei (AGNs). We use the estimated timescales of our stochastic model to recover the correlation between characteristic timescale of the high-frequency X-ray fluctuations and black hole mass for AGNs, including two new "detections" of the timescale for Fairall 9 and NGC 5548. We find a tight anti-correlation between the black hole mass and the amplitude of the driving noise field, which is proportional to the amplitude of the high-frequency X-ray PSD, and we estimate that this parameter gives black hole mass estimates to within similar to 0.2 dex precision, potentially the most accurate method for AGNs yet. We also find evidence that approximate to 13% of AGN optical PSDs fall off flatter than 1/f(2) and, similar to previous work, find that the optical fluctuations are more suppressed on short timescales compared to the X-rays, but are larger on long timescales, suggesting that the optical fluctuations are not solely due to reprocessing of X-rays. C1 [Kelly, Brandon C.; Sobolewska, Malgorzata; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kelly, BC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bckelly@cfa.harvard.edu FU NASA [HF-01220.01, HF-51243.01, NAS 5-26555, NAS8-39073]; Chandra grant [GO8-9125A] FX We thank Phil Uttley for helpful conversations, and Simon Vaughan, Christopher Kochanek, Chelsea MacLeod, and Eric Feigelson for looking over and commenting on an earlier version of this manuscript. We also thank the anonymous referee for a careful reading and detailed comments which improved the quality of this paper. B.K. acknowledges support by NASA through Hubble Fellowship grants HF-01220.01 and HF-51243.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. This research is funded in part by NASA contract NAS8-39073. Partial support for this work was provided by the Chandra grant GO8-9125A. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. This research has also made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 133 TC 54 Z9 55 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 MAR 20 PY 2011 VL 730 IS 1 AR 52 DI 10.1088/0004-637X/730/1/52 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735XI UT WOS:000288453600051 ER PT J AU Kipping, D Bakos, G AF Kipping, David Bakos, Gaspar TI AN INDEPENDENT ANALYSIS OF KEPLER-4b THROUGH KEPLER-8b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (Kepler-4, Kepler-5, Kepler-6, Kepler-7, Kepler-8); techniques: photometric; techniques: spectroscopic ID EXTRASOLAR GIANT PLANETS; LIGHT-CURVE; TRANSITING PLANETS; MAIN-SEQUENCE; LOW-DENSITY; HOT; STAR; SATELLITES; DISCOVERY; ORBITS AB We present two independent, homogeneous, global analyses of the transit light curves, radial velocities, and spectroscopy of Kepler-4b, Kepler-5b, Kepler-6b, Kepler-7b, and Kepler-8b with numerous differences compared to the previous methods. These include: (1) improved decorrelated parameter fitting set used, (2) new limb-darkening coefficients, (3) time stamps modified to barycentric Julian date for consistency with radial velocity data, (4) two different methods for compensating for the long integration time of Kepler long-cadence data, (5) best-fit secondary eclipse depths and excluded upper limits, and (6) fitted mid-transit times, durations, depths, and baseline fluxes for individual transits. We make several determinations not found in the discovery papers. (1) We detect a secondary eclipse for Kepler-7b of depth (47 +/- 14) ppm and statistical significance 3.5 sigma. We conclude that reflected light is a much more plausible origin than thermal emission and determine a geometric albedo of A(g) = (0.38 +/- 0.12). (2) We find that an eccentric orbit model for the Neptune-mass planet Kepler-4b is detected at the 2 sigma level with e = (0.25 +/- 0.12). If confirmed, this would place Kepler-4b in a similar category as GJ 436b and HAT-P-11b, as an eccentric, Neptune-mass planet. (3) We find weak evidence for a secondary eclipse in Kepler-5b of 2 sigma significance and depth (26 +/- 17) ppm. The most plausible explanation is reflected light caused by a planet of geometric albedo A(g) = (0.15 +/- 0.10). (4) A 2.6 sigma peak in Kepler-6b TTV periodogram is detected and is not easily explained as an aliased frequency. We find that mean-motion resonant (MMR) perturbers, non-resonant perturbers, and a companion extrasolar moon all provide inadequate explanations for this signal and the most likely source is stellar rotation. (5) We find different impact parameters relative to the discovery papers in most cases, but generally self-consistent when compared to the two methods employed here. (6) We constrain the presence of MMR planets for all five planets through an analysis of the mid-transit times. (7) We constrain the presence of extrasolar moons for all five planets. (8) We constrain the presence of Trojans for all five planets. C1 [Kipping, David; Bakos, Gaspar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu FU STFC; HATNet; NASA [NNG04GN74G, NNX08AF23G]; NSF [AST-0702843] FX D.M.K. has been supported by STFC studentships, and by the HATNet as an SAO predoctoral fellow. We acknowledge NASA NNG04GN74G, NNX08AF23G grants, and Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 for G.B.). NR 71 TC 49 Z9 49 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 MAR 20 PY 2011 VL 730 IS 1 AR 50 DI 10.1088/0004-637X/730/1/50 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735XI UT WOS:000288453600049 ER PT J AU Rawls, ML Orosz, JA McClintock, JE Torres, MAP Bailyn, CD Buxton, MM AF Rawls, Meredith L. Orosz, Jerome A. McClintock, Jeffrey E. Torres, Manuel A. P. Bailyn, Charles D. Buxton, Michelle M. TI REFINED NEUTRON STAR MASS DETERMINATIONS FOR SIX ECLIPSING X-RAY PULSAR BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; pulsars: individual (Vela X-1, 4U 1538-42, SMC X-1, LMC X-4, Cen X-3, Her X-1); stars: neutron; X-rays: binaries ID 4U 1538-52; VELA X-1; OPTICAL PHOTOMETRY; LIGHT-CURVE; SPECTROSCOPY; EVOLUTION; ASTRONOMY; COMPANION; HD-77581; VELOCITY AB We present an improved method for determining the mass of neutron stars in eclipsing X-ray pulsar binaries and apply the method to six systems, namely, Vela X-1, 4U 1538-52, SMC X-1, LMC X-4, Cen X-3, and Her X-1. In previous studies to determine neutron star mass, the X-ray eclipse duration has been approximated analytically by assuming that the companion star is spherical with an effective Roche lobe radius. We use a numerical code based on Roche geometry with various optimizers to analyze the published data for these systems, which we supplement with new spectroscopic and photometric data for 4U 1538-52. This allows us to model the eclipse duration more accurately and thus calculate an improved value for the neutron star mass. The derived neutron star mass also depends on the assumed Roche lobe filling factor beta of the companion star, where beta = 1 indicates a completely filled Roche lobe. In previous work a range of beta between 0.9 and 1.0 was usually adopted. We use optical ellipsoidal light-curve data to constrain beta. We find neutron star masses of 1.77 +/- 0.08 M-circle dot for Vela X-1, 0.87 +/- 0.07 M-circle dot for 4U 1538-52 (eccentric orbit), 1.00 +/- 0.10 M-circle dot for 4U 1538-52 (circular orbit), 1.04 +/- 0.09M(circle dot) for SMC X-1, 1.29 +/- 0.05 M-circle dot for LMC X-4, 1.49 +/- 0.08 M-circle dot for Cen X-3, and 1.07 +/- 0.36 M-circle dot for Her X-1. We discuss the limits of the approximations that were used to derive the earlier mass determinations, and we comment on the implications our new masses have for observationally refining the upper and lower bounds of the neutron star mass distribution. C1 [Rawls, Meredith L.; Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [McClintock, Jeffrey E.; Torres, Manuel A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bailyn, Charles D.; Buxton, Michelle M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. RP Rawls, ML (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. EM mrawls@sciences.sdsu.edu; orosz@sciences.sdsu.edu; jmcclintock@cfa.harvard.edu; mtorres@cfa.harvard.edu; bailyn@astro.yale.edu; michelle.buxton@yale.edu OI Rawls, Meredith/0000-0003-1305-7308 FU NSF [AST-0808145] FX M.L.R. and J.A.O. gratefully acknowledge the support of NSF grant AST-0808145. We also thank the anonymous referee who provided constructive feedback and encouraged us to include the full optical light curve analysis in this work. NR 39 TC 73 Z9 74 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 MAR 20 PY 2011 VL 730 IS 1 AR 25 DI 10.1088/0004-637X/730/1/25 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 735XI UT WOS:000288453600025 ER PT J AU Ross, AH Ubelaker, DH Kimmerle, EH AF Ross, A. H. Ubelaker, D. H. Kimmerle, E. H. TI Implications of dimorphism, population variation, and secular change in estimating population affinity in the Iberian Peninsula SO FORENSIC SCIENCE INTERNATIONAL LA English DT Article DE Craniofacial variation; Sexual dimorphism; Iberian Peninsula; Forensic Anthropology Population Data ID CRANIOFACIAL MORPHOLOGY; SEXUAL-DIMORPHISM; IDENTIFICATION; SKELETONS; HISTORY; CRANIA AB Morphometric cranial variation among Spanish samples was compared to a 19th century Portuguese sample using both traditional and three-dimensional approaches. The Spanish samples included the regional 19th century Oloriz collection and the local 16-17th century Villanubla and Vallolid sample from northwestern Spain. Results suggest moderate variation among the samples and suggest that varying patterns of regional variation, sexual dimorphism and secular change represent important factors to be considered in the evaluation of population affinity using craniometric approaches. (C) 2011 Elsevier Ireland Ltd. All rights reserved. C1 [Ross, A. H.] N Carolina State Univ, Dept Sociol & Anthropol, Raleigh, NC 27695 USA. [Ubelaker, D. H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kimmerle, E. H.] Univ S Florida, Dept Anthropol, Tampa, FL 33620 USA. RP Ross, AH (reprint author), N Carolina State Univ, Dept Sociol & Anthropol, 1911 Bldg,CB 8107, Raleigh, NC 27695 USA. EM ann_ross@ncsu.edu OI Ross, Ann/0000-0001-8780-1414 FU National Institute of Justice [2005-MU-BX-K078] FX We would like to thank Drs. Jose Prieto and Juan Carlos Prados for access and assistance with the Oloriz collection, Dr. Maria Dolores Garralda for access to the Wamba collection, and Craig Fishbough for assistance with data collection. This project was funded by a National Institute of Justice grant (# 2005-MU-BX-K078). NR 28 TC 3 Z9 3 U1 1 U2 14 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0379-0738 J9 FORENSIC SCI INT JI Forensic Sci.Int. PD MAR 20 PY 2011 VL 206 IS 1-3 AR 214.e1 DI 10.1016/j.forsciint.2011.01.003 PG 5 WC Medicine, Legal SC Legal Medicine GA 732PO UT WOS:000288200400062 PM 21288670 ER PT J AU Lee, C Martin, RV van Donkelaar, A Lee, H Dickerson, RR Hains, JC Krotkov, N Richter, A Vinnikov, K Schwab, JJ AF Lee, Chulkyu Martin, Randall V. van Donkelaar, Aaron Lee, Hanlim Dickerson, Russell R. Hains, Jennifer C. Krotkov, Nickolay Richter, Andreas Vinnikov, Konstantine Schwab, James J. TI SO2 emissions and lifetimes: Estimates from inverse modeling using in situ and global, space-based (SCIAMACHY and OMI) observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OZONE MONITORING INSTRUMENT; UNITED-STATES; SULFUR-DIOXIDE; RADIATIVE-TRANSFER; TROPOSPHERIC SULFATE; 3-DIMENSIONAL MODEL; PARTICULATE MATTER; NOX EMISSIONS; TRACE GAS; INTEX-B AB Top-down constraints on global sulfur dioxide (SO2) emissions are inferred through inverse modeling using SO2 column observations from two satellite instruments (SCIAMACHY and OMI). We first evaluated the SO2 column observations with surface SO2 measurements by applying local scaling factors from a global chemical transport model (GEOS-Chem) to SO2 columns retrieved from the satellite instruments. The resulting annual mean surface SO2 mixing ratios for 2006 exhibit a significant spatial correlation (r = 0.86, slope = 0.91 for SCIAMACHY and r = 0.80, slope = 0.79 for OMI) with coincident in situ measurements from monitoring networks throughout the United States and Canada. We evaluate the GEOS-Chem simulation of the SO2 lifetime with that inferred from in situ measurements to verify the applicability of GEOS-Chem for inversion of SO2 columns to emissions. The seasonal mean SO2 lifetime calculated with the GEOS-Chem model over the eastern United States is 13 h in summer and 48 h in winter, compared to lifetimes inferred from in situ measurements of 19 +/- 7 h in summer and 58 +/- 20 h in winter. We apply SO2 columns from SCIAMACHY and OMI to derive a top-down anthropogenic SO2 emission inventory over land by using the local GEOS-Chem relationship between SO2 columns and emissions. There is little seasonal variation in the top-down emissions (< 15%) over most major industrial regions providing some confidence in the method. Our global estimate for annual land surface anthropogenic SO2 emissions (52.4 Tg S yr(-1) from SCIAMACHY and 49.9 Tg S yr(-1) from OMI) closely agrees with the bottom-up emissions (54.6 Tg S yr(-1)) in the GEOS-Chem model and exhibits consistency in global distributions with the bottom-up emissions (r = 0.78 for SCIAMACHY, and r = 0.77 for OMI). However, there are significant regional differences. C1 [Lee, Chulkyu; Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Lee, Chulkyu] Korea Meteorol Adm, Natl Inst Meteorol Res, Seoul 156720, South Korea. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, Hanlim] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea. [Dickerson, Russell R.; Vinnikov, Konstantine] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Hains, Jennifer C.] Maryland Dept Environm, Baltimore, MD 21230 USA. [Krotkov, Nickolay] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Richter, Andreas] Univ Bremen, Inst Environm Phys & Remote Sensing, D-28334 Bremen, Germany. [Schwab, James J.] SUNY Albany, Atmospher Sci Res Ctr, Albany, NY 12203 USA. RP Lee, C (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. RI Richter, Andreas/C-4971-2008; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; Krotkov, Nickolay/E-1541-2012; Dickerson, Russell/F-2857-2010 OI Richter, Andreas/0000-0003-3339-212X; Martin, Randall/0000-0003-2632-8402; Krotkov, Nickolay/0000-0001-6170-6750; Dickerson, Russell/0000-0003-0206-3083 FU Health Canada; National Aeronautics and Space Administration (NASA); Maryland Department of the Environment FX We thank three anonymous reviewers for helpful comments. The publicly released Planetary Boundary Layer (PBL) OMI SO2 Level 2 VC products were obtained from GES Data and Information Service Center (http://disc.sci.gsfc.nasa.gov/). SO2 slant columns from SCIAMACHY were obtained from the Institute of Environmental Physics and Remote Sensing, University of Bremen, Germany (http://www.iup.uni-bremen.de/). This work was supported by Health Canada and by the National Aeronautics and Space Administration (NASA). Aircraft observations were supported by the Maryland Department of the Environment. NR 73 TC 77 Z9 78 U1 2 U2 39 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 18 PY 2011 VL 116 AR D06304 DI 10.1029/2010JD014758 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 737YK UT WOS:000288606300001 ER PT J AU Canning-Clode, J Fofonoff, P Riedel, GF Torchin, M Ruiz, GM AF Canning-Clode, Joao Fofonoff, Paul Riedel, Gerhardt F. Torchin, Mark Ruiz, Gregory M. TI The Effects of Copper Pollution on Fouling Assemblage Diversity: A Tropical-Temperate Comparison SO PLOS ONE LA English DT Article ID FUNCTIONAL-DIVERSITY; PROPAGULE PRESSURE; SPIRORBIDAE POLYCHAETA; BIOLOGICAL INVASIONS; MARINE COMMUNITIES; SPECIES RICHNESS; BUGULA-NERITINA; CHESAPEAKE BAY; REEF FISH; DISTURBANCE AB Background: The invasion of habitats by non-indigenous species (NIS) occurs at a global scale and can generate significant ecological, evolutionary, economic and social consequences. Estuarine and coastal ecosystems are particularly vulnerable to pollution from numerous sources due to years of human-induced degradation and shipping. Pollution is considered as a class of disturbance with anthropogenic roots and recent studies have concluded that high frequencies of disturbance may facilitate invasions by increasing the availability of resources. Methodology/Principal Findings: To examine the effects of heavy metal pollution as disturbance in shaping patterns of exotic versus native diversity in marine fouling communities we exposed fouling communities to different concentrations of copper in one temperate (Virginia) and one tropical (Panama) region. Diversity was categorized as total, native and nonindigenous and we also incorporated taxonomic and functional richness. Our findings indicate that total fouling diversity decreased with increasing copper pollution, whether taxonomic or functional diversity is considered. Both native and nonindigenous richness decreased with increasing copper concentrations at the tropical site whereas at the temperate site, non-indigenous richness was too low to detect any effect. Conclusions/Significance: Non-indigenous richness decreased with increasing metal concentrations, contradicting previous investigations that evaluate the influence of heavy metal pollution on diversity and invasibility of fouling assemblages. These results provide first insights on how the invasive species pool in a certain region may play a key role in the disturbance vs. non-indigenous diversity relationship. C1 [Canning-Clode, Joao; Fofonoff, Paul; Riedel, Gerhardt F.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Canning-Clode, Joao] Ctr Marine & Environm Res, CIIMAR, CIMAR, Oporto, Portugal. [Torchin, Mark] Smithsonian Trop Res Inst, Panama City, Panama. RP Canning-Clode, J (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM canning-clodej@si.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; Ruiz, Gregory/0000-0003-2499-441X FU Marine Science Network (MSN) FX The funding was provided by a Marine Science Network (MSN) fellowship award to JCC. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 80 TC 16 Z9 17 U1 3 U2 26 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 MAR 18 PY 2011 VL 6 IS 3 AR e18026 DI 10.1371/journal.pone.0018026 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 737CD UT WOS:000288545100063 PM 21437262 ER PT J AU Lamsal, LN Martin, RV Padmanabhan, A van Donkelaar, A Zhang, Q Sioris, CE Chance, K Kurosu, TP Newchurch, MJ AF Lamsal, L. N. Martin, R. V. Padmanabhan, A. van Donkelaar, A. Zhang, Q. Sioris, C. E. Chance, K. Kurosu, T. P. Newchurch, M. J. TI Application of satellite observations for timely updates to global anthropogenic NOx emission inventories SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID INTEX-B; NITROGEN-DIOXIDE; UNITED-STATES; TRANSPORT; INVERSION; OZONE; SPACE; SCIAMACHY; POLLUTION; AIRCRAFT AB Anthropogenic emissions of nitrogen oxides (NOx) can change rapidly due to economic growth or control measures. Bottom-up emissions estimated using source-specific emission factors and activity statistics require years to compile and can become quickly outdated. We present a method to use satellite observations of tropospheric NO2 columns to estimate changes in NOx emissions. We use tropospheric NO2 columns retrieved from the SCIAMACHY satellite instrument for 2003-2009, the response of tropospheric NO2 columns to changes in NOx emissions determined from a global chemical transport model (GEOS-Chem), and the bottom-up anthropogenic NOx emissions for 2006 to hindcast and forecast the inventories. We evaluate our approach by comparing bottom-up and hindcast emissions for 2003. The two inventories agree within 6.0% globally and within 8.9% at the regional scale with consistent trends in western Europe, North America, and East Asia. We go on to forecast emissions for 2009. During 2006-2009, anthropogenic NOx emissions over land increase by 9.2% globally and by 18.8% from East Asia. North American emissions decrease by 5.7%. Citation: Lamsal, L. N., R. V. Martin, A. Padmanabhan, A. van Donkelaar, Q. Zhang, C. E. Sioris, K. Chance, T. P. Kurosu, and M. J. Newchurch (2011), Application of satellite observations for timely updates to global anthropogenic NOx emission inventories, Geophys. Res. Lett., 38, L05810, doi: 10.1029/2010GL046476. C1 [Lamsal, L. N.; Martin, R. V.; Padmanabhan, A.; van Donkelaar, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, R. V.; Chance, K.; Kurosu, T. P.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Newchurch, M. J.] Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35805 USA. [Sioris, C. E.] Environm Canada, Toronto, ON M3H 5T4, Canada. [Zhang, Q.] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China. RP Lamsal, LN (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, James Dunn Bldg, Halifax, NS B3H 3J5, Canada. EM lok.lamsal@fizz.phys.dal.ca RI Zhang, Qiang/D-9034-2012; Lamsal, Lok/G-4781-2012; Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; OI Martin, Randall/0000-0003-2632-8402; Chance, Kelly/0000-0002-7339-7577 FU NASA; Environment Canada FX This work was supported by NASA's Atmospheric Composition Program and by Environment Canada. NR 33 TC 79 Z9 81 U1 3 U2 50 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 MAR 15 PY 2011 VL 38 AR L05810 DI 10.1029/2010GL046476 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 737XL UT WOS:000288603700001 ER PT J AU Fritz, U Schmidt, C Ernst, CH AF Fritz, Uwe Schmidt, Christian Ernst, Carl H. TI Competing generic concepts for Blanding's, Pacific and European pond turtles (Emydoidea, Actinemys and Emys)-Which is best? SO ZOOTAXA LA English DT Article DE Classification; Actinemys; Clemmys; Emydidae; Emydinae; Emydoidea; Emys; Glyptemys; Testudines ID MITOCHONDRIAL-DNA VARIATION; BUFO-VIRIDIS SUBGROUP; EMYS-ORBICULARIS; EMYDID TURTLES; TESTUDINES EMYDIDAE; CRYPTIC VARIATION; SHELL KINESIS; GENUS CLEMMYS; CRESTED NEWT; TREE FROGS AB We review competing taxonomic classifications and hypotheses for the phylogeny of emydine turtles. The formerly recognized genus Clemmys sensu lato clearly is paraphyletic. Two of its former species, now Glyptemys insculpta and G. muhlenbergii, constitute a well-supported basal clade within the Emydinae. However, the phylogenetic position of the other two species traditionally placed in Clemmys remains controversial. Mitochondrial data suggest a clade embracing Actinemys (formerly Clemmys) marmorata, Emydoidea and Emys and as its sister either another clade (Clemmys guttata + Terrapene) or Terrapene alone. In contrast, nuclear genomic data yield conflicting results, depending on which genes are used. Either Clemmys guttata is revealed as sister to ((Emydoidea + Emys) + Actinemys) + Terrapene or Clemmys guttata is sister to Actinemys marmorata and these two species together are the sister group of (Emydoidea + Emys); Terrapene appears then as sister to (Actinemys marmorata + Clemmys guttata) + (Emydoidea + Emys). The contradictory branching patterns depending from the selected loci are suggestive of lineage sorting problems. Ignoring the unclear phylogenetic position of Actinemys marmorata, one recently proposed classification scheme placed Actinemys marmorata, Emydoidea blandingii, Emys orbicularis, and Emys trinacris in one genus (Emys), while another classification scheme treats Actinemys, Emydoidea, and Emys as distinct genera. The inclusion of Actinemys in the same taxon as Emydoidea + Emys is unacceptable under a phylogenetic classification framework because there is evidence for the non-monophyly of this clade. Moreover, Actinemys, Emydoidea, and Emys are morphologically highly distinct. Their morphological divergence exceeds by far the differences that typically occur among species of the same genus, so that a continued usage of the distinct genera Actinemys, Emydoidea and Emys is recommended. C1 [Fritz, Uwe; Schmidt, Christian] Senckenberg Dresden, Museum Zool, D-01109 Dresden, Germany. [Ernst, Carl H.] Smithsonian Inst, MRC 162, Div Amphibians & Reptiles, Washington, DC 20013 USA. RP Fritz, U (reprint author), Senckenberg Dresden, Museum Zool, AB Meyer Bldg, D-01109 Dresden, Germany. EM uwe.fritz@senckenberg.de NR 48 TC 8 Z9 8 U1 1 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAR 15 PY 2011 IS 2791 BP 41 EP 53 PG 13 WC Zoology SC Zoology GA 734DV UT WOS:000288314300003 ER PT J AU Smith, DG AF Smith, David G. TI Joseph Schieser Nelson SO COPEIA LA English DT Editorial Material C1 Smithsonian Inst, Museum Support Ctr, Suitland, MD 20746 USA. RP Smith, DG (reprint author), Smithsonian Inst, Museum Support Ctr, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM smithd@si.edu NR 11 TC 0 Z9 0 U1 1 U2 2 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD MAR 14 PY 2011 IS 1 BP 169 EP 176 DI 10.1643/OT-10-155 PG 8 WC Zoology SC Zoology GA 741UA UT WOS:000288889400019 ER PT J AU Blackie, D Blackwell-Whitehead, R Stark, G Pickering, JC Smith, PL Rufus, J Thorne, AP AF Blackie, D. Blackwell-Whitehead, R. Stark, G. Pickering, J. C. Smith, P. L. Rufus, J. Thorne, A. P. TI High-resolution photoabsorption cross-section measurements of SO2 at 198 K from 213 to 325 nm SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID FOURIER-TRANSFORM SPECTROMETER; JET-COOLED SO2; SULFUR-DIOXIDE; FLUORESCENCE SPECTROSCOPY; TEMPERATURE-DEPENDENCE; ABSORPTION-SPECTRUM; VENUS ATMOSPHERE; REGION; UV; ULTRAVIOLET AB SO2 plays an important role in the atmospheric chemistry of the Earth, Venus, and Io. This paper presents photoabsorption cross sections of SO2 from 213 to 325 nm at 198 K, encompassing the (C) over tilde B-1(2) - (X) over tilde (1)A(1) and (B) over tilde B-1(1) - (X) over tilde (1)A(1) electronic bands. These measurements are part of a series of measurements over the 160 to 300 K temperature range between 190 and 325 nm. The cross sections have been measured at high resolution (lambda/Delta lambda approximate to 450,000) using Fourier transform spectrometry and are compared to other high-resolution measurements in the literature. C1 [Blackie, D.; Pickering, J. C.; Rufus, J.; Thorne, A. P.] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2AZ, England. [Blackwell-Whitehead, R.] Lund Observ, SE-22100 Lund, Sweden. [Smith, P. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stark, G.] Wellesley Coll, Dept Phys, Wellesley, MA 02481 USA. RP Blackie, D (reprint author), Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, Huxley Bldg, London SW7 2AZ, England. EM douglas.blackie01@imperial.ac.uk FU NASA [NNG05GA03G]; STFC (PPARC) (UK); Leverhulme Trust FX The authors would like to thank the following for their support of this work, NASA grant NNG05GA03G, STFC (PPARC) (UK), and the Leverhulme Trust. NR 62 TC 9 Z9 9 U1 3 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD MAR 12 PY 2011 VL 116 AR E03006 DI 10.1029/2010JE003707 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 734JC UT WOS:000288329400001 ER PT J AU Panova, M Blakeslee, AMH Miller, AW Makinen, T Ruiz, GM Johannesson, K Andre, C AF Panova, Marina Blakeslee, April M. H. Miller, A. Whitman Maekinen, Tuuli Ruiz, Gregory M. Johannesson, Kerstin Andre, Carl TI Glacial History of the North Atlantic Marine Snail, Littorina saxatilis, Inferred from Distribution of Mitochondrial DNA Lineages SO PLOS ONE LA English DT Article ID POSTGLACIAL COLONIZATION; POPULATION-STRUCTURE; INTERGLACIAL CYCLE; GENETIC DIVERSITY; LARVAL DISPERSAL; ENGLISH-CHANNEL; PHYLOGEOGRAPHY; REFUGIA; MIGRATION; GROWTH AB The North Atlantic intertidal gastropod, Littorina saxatilis (Olivi, 1792), exhibits extreme morphological variation between and within geographic regions and has become a model for studies of local adaptation; yet a comprehensive analysis of the species' phylogeography is lacking. Here, we examine phylogeographic patterns of the species' populations in the North Atlantic and one remote Mediterranean population using sequence variation in a fragment of the mitochondrial cytochrome b gene (607 bp). We found that, as opposed to many other rocky intertidal species, L. saxatilis has likely had a long and continuous history in the Northwest Atlantic, including survival during the last glacial maximum (LGM), possibly in two refugia. In the Northeast Atlantic, several areas likely harboured refugial populations that recolonized different parts of this region after glacial retreat, resulting in strong population structure. However, the outlying monomorphic Venetian population is likely a recent anthropogenic introduction from northern Europe and not a remnant of an earlier wider distribution in the Mediterranean Sea. Overall, our detailed phylogeography of L. saxatilis adds an important piece to the understanding of Pleistocene history in North Atlantic marine biota as well as being the first study to describe the species' evolutionary history in its natural range. The latter contribution is noteworthy because the snail has recently become an important model species for understanding evolutionary processes of speciation; thus our work provides integral information for such endeavours. C1 [Panova, Marina; Johannesson, Kerstin; Andre, Carl] Univ Gothenburg, Dept Marine Ecol Tjarno, Stromstad, Sweden. [Blakeslee, April M. H.; Miller, A. Whitman; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA. [Maekinen, Tuuli] S African Inst Aquat Biodivers, Grahamstown, South Africa. RP Panova, M (reprint author), Univ Gothenburg, Dept Marine Ecol Tjarno, Stromstad, Sweden. EM marina.panova@marecol.gu.se RI Andre, Carl/B-4237-2010; Johannesson, Kerstin/B-5528-2013; Panova, Marina/D-2633-2015; OI Johannesson, Kerstin/0000-0003-0176-7986; Panova, Marina/0000-0002-4147-6473; Ruiz, Gregory/0000-0003-2499-441X; Miller, Whitman/0000-0003-0484-182X FU Centre for Theoretical Biology at Gothenburg University; Swedish Royal Academy of Science; Swedish Research Council; Smithsonian Institution postdoctoral fellowship program; Helge Ax:son Johnson Foundation; Swedish Research Council VR; Swedish Research Council Formas FX Financial support was provided by the Centre for Theoretical Biology at Gothenburg University (MP, CA, KJ), the Swedish Royal Academy of Science (MP), the Swedish Research Council (KJ, CA), the Smithsonian Institution postdoctoral fellowship program (AMHB) and a grant from the Helge Ax:son Johnson Foundation (TM). This work was partly performed within the Linnaeus Centre for Marine Evolutionary Biology (http://www.cemeb.science.gu.se/) supported by a Linnaeus-grant from the Swedish Research Councils VR and Formas. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 60 TC 38 Z9 40 U1 1 U2 37 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 MAR 11 PY 2011 VL 6 IS 3 AR e17511 DI 10.1371/journal.pone.0017511 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 733FF UT WOS:000288247800009 PM 21412417 ER PT J AU Massaro, F Grindlay, JE AF Massaro, F. Grindlay, J. E. TI SPECTRAL EVOLUTION OF LONG GAMMA-RAY BURST PROMPT EMISSION: ELECTROSTATIC ACCELERATION AND ADIABATIC EXPANSION (pg 727, pg L1, 2011) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Massaro, F.; Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 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 NR 1 TC 0 Z9 0 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2011 VL 729 IS 2 AR L29 DI 10.1088/2041-8205/729/2/L29 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KG UT WOS:000293124700015 ER PT J AU Patnaude, DJ Vink, J Laming, JM Fesen, RA AF Patnaude, Daniel J. Vink, Jacco Laming, J. Martin Fesen, Robert A. TI A DECLINE IN THE NONTHERMAL X-RAY EMISSION FROM CASSIOPEIA A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; ISM: individual objects (Cassiopeia A); radiation mechanisms: non-thermal ID SUPERNOVA REMNANT CASSIOPEIA; PARTICLE-ACCELERATION; SYNCHROTRON EMISSION; MAGNETIC-FIELDS; SHOCK-WAVES; COSMIC-RAYS; SHELL; AMPLIFICATION; VARIABILITY; MORPHOLOGY AB We present new Chandra ACIS-S3 observations of Cassiopeia A which, when combined with earlier ACIS-S3 observations, show evidence for a steady similar to 1.5%-2% yr(-1) decline in the 4.2-6.0 keV X-ray emission between the years 2000 and 2010. The computed flux from exposure corrected images over the entire remnant showed a 17% decline over the entire remnant and a slightly larger (21%) decline from regions along the remnant's western limb. Spectral fits of the 4.2-6.0 keV emission across the entire remnant, forward shock filaments, and interior filaments indicate that the remnant's nonthermal spectral power-law index has steepened by about 10%, with interior filaments having steeper power-law indices. Since TeV electrons, which give rise to the observed X-ray synchrotron emission, are associated with the exponential cutoff portion of the electron distribution function, we have related our results to a change in the cutoff energy and conclude that the observed decline and steepening of the nonthermal X-ray emission is consistent with a deceleration of the remnant's similar or equal to 5000 km s(-1) forward shock of approximate to 30-70 km s(-1) yr(-1). C1 [Patnaude, Daniel J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Vink, Jacco] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. [Laming, J. Martin] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. RP Patnaude, DJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. FU Chandra GO program [GO0-11094X]; NASA [NAS8-03060]; Netherlands Scientific Organization (NWO) FX We thank Alexey Vikhlinin and Paul Plucinsky for useful discussions regarding the stability of the Chandra ACIS-S3 quantum efficiency. D.J.P. acknowledges support from the Chandra GO program through grant GO0-11094X as well as support from NASA contract NAS8-03060. J.V. is supported by a Vidi grant from the Netherlands Scientific Organization (NWO). NR 43 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 10 PY 2011 VL 729 IS 2 AR L28 DI 10.1088/2041-8205/729/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KG UT WOS:000293124700014 ER PT J AU Rea, N Jonker, PG Nelemans, G Pons, JA Kasliwal, MM Kulkarni, SR Wijnands, R AF Rea, N. Jonker, P. G. Nelemans, G. Pons, J. A. Kasliwal, M. M. Kulkarni, S. R. Wijnands, R. TI THE X-RAY QUIESCENCE OF SWIFT J195509.6+261406 (GRB 070610): AN OPTICAL BURSTING X-RAY BINARY? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: magnetic field; X-rays: individual (SWIFT J195509.6+261406); X-rays: stars ID ISOLATED NEUTRON-STARS; HOLE EVENT HORIZONS; BLACK-HOLE; TRANSIENT 1H-1905+000; GALACTIC MAGNETAR; VARIABILITY; ADVECTION; ACCRETION; PULSARS; CHANDRA AB We report on an similar to 63 ks Chandra observation of the X-ray transient Swift J195509.6+261406 discovered as the afterglow of what was first believed to be a long-duration gamma-ray burst (GRB 070610). The outburst of this source was characterized by unique optical flares on timescales of second or less, morphologically similar to the short X-ray bursts usually observed from magnetars. Our Chandra observation was performed similar to 2 years after the discovery of the optical and X-ray flaring activity of this source, catching it in its quiescent state. We derive stringent upper limits on the quiescent emission of Swift J195509.6+261406, which argues against the possibility of this object being a typical magnetar. Our limits show that the most viable interpretation on the nature of this peculiar bursting source is a binary system hosting a black hole or a neutron star with a low-mass companion star (<0.12 M-circle dot) and with an orbital period smaller than a few hours. C1 [Rea, N.] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Bellaterra 08193, Barcelona, Spain. [Jonker, P. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.; Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Kasliwal, M. M.; Kulkarni, S. R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Pons, J. A.] Univ Alacant, Dept Fis Aplicada, Alacant 03080, Spain. RP Rea, N (reprint author), Inst Ciencies Espai CSIC IEEC, Fac Ciencies, Campus UAB,Torre C5 Parell,2A Planta, Bellaterra 08193, Barcelona, Spain. EM rea@ieec.uab.es RI PONS, JOSE/D-4687-2012; Nelemans, Gijs/D-3177-2012; Rea, Nanda/I-2853-2015 OI PONS, JOSE/0000-0003-1018-8126; Nelemans, Gijs/0000-0002-0752-2974; Rea, Nanda/0000-0003-2177-6388 FU Consejo Superior de Investigaciones Cientficas; Netherlands Organization for Scientific Research; [AYA2009-07391]; [SGR2009-811] FX N.R. is supported by a Ramon y Cajal fellowship through Consejo Superior de Investigaciones Cientficas, by grants AYA2009-07391 and SGR2009-811, and thanks to P. Casella for useful discussions on the optical variability in black hole binaries. P.G.J. and G.N. acknowledge support from a VIDI grant from the Netherlands Organization for Scientific Research. NR 38 TC 11 Z9 11 U1 0 U2 3 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 MAR 10 PY 2011 VL 729 IS 2 AR L21 DI 10.1088/2041-8205/729/2/L21 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 797KG UT WOS:000293124700007 ER PT J AU Chatzopoulos, E Wheeler, JC Vinko, J Quimby, R Robinson, EL Miller, AA Foley, RJ Perley, DA Yuan, F Akerlof, C Bloom, JS AF Chatzopoulos, E. Wheeler, J. Craig Vinko, J. Quimby, R. Robinson, E. L. Miller, A. A. Foley, R. J. Perley, D. A. Yuan, F. Akerlof, C. Bloom, J. S. TI SN 2008am: A SUPER-LUMINOUS TYPE IIn SUPERNOVA SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; hydrodynamics; stars: evolution; supernovae: general; supernovae: individual (SN 2008am) ID RICH CIRCUMSTELLAR MEDIUM; CORE-COLLAPSE SUPERNOVAE; PAIR-INSTABILITY; LIGHT-CURVE; MASSIVE STARS; ELECTRON-SCATTERING; PHOTOMETRIC SYSTEM; ANALYTIC SOLUTIONS; TELESCOPE SYSTEM; SPACE-TELESCOPE AB We present observations and interpretation of the Type IIn supernova SN 2008am discovered by the ROTSE Supernova Verification Project (RSVP). SN 2008am peaked at approximately -22.3 mag at a redshift of z = 0.2338, giving it a peak luminosity of similar to 3 x 10(44) erg s(-1) and making it one of the most luminous supernovae ever observed. The total radiated energy is similar or equal to 2 x 10(51) erg. The host galaxy appears to be an SB1 of normal luminosity (M-r' similar to -20) with metallicity Z similar to 0.4Z(circle dot). ROTSE upper limits and detections constrain the rise time to be similar to 34 days in the rest frame, significantly shorter than similar events, SN 2006gy and SN 2006tf. Photometric observations in the ultraviolet, optical, and infrared bands (J, H, K-s) constrain the spectral energy distribution evolution. We obtained six optical spectra of the supernova, five on the early decline from maximum light and a sixth nearly a year later plus a very late time spectrum (similar to 2 yr) of the host galaxy. The spectra show no evidence for broad supernova photospheric features in either absorption or emission at any phase. The spectra of SN 2008am show strong Balmer-line and He I lambda 5876 emission with intermediate widths (similar to 25 angstrom) in the first similar to 40 days after optical maximum. The width formally corresponds to a velocity of similar to 1000 km s(-1). We examine a variety of models for the line wings and conclude that multiple scattering is most likely, implying that our spectra contain no specific information on the bulk flow velocity. We examine a variety of models for the ROTSE light curve subject to the rise time and the nature of the spectra, including radioactive decay, shocks in optically thick and optically thin circumstellar media (CSMs) and a magnetar. The most successful model is one for which the CSM is optically thick and in which diffusion of forward shock-deposited luminosity gives rise to the observed light curve. The model suggests strong mass loss and a greater contribution from the interaction of the forward shock with optically thick CSM than from the reverse shock. Diffusion of the shock-deposited energy from the forward shock is found to be important in accounting for the rising part of the light curve. Although there are differences in detail, SN 2008am appears to be closely related to other super-luminous Type IIn supernovae, SN 2006gy, SN 2006tf, and perhaps SN 2008iy, that may represent the deaths of very massive luminous-blue-variable-type progenitors and for which the luminosity is powered by the interaction of the ejecta with a dense CSM. C1 [Chatzopoulos, E.; Wheeler, J. Craig; Robinson, E. L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Vinko, J.] Univ Szeged, Dept Opt & Quantum Elect, Szeged, Hungary. [Quimby, R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Miller, A. A.; Perley, D. A.; Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yuan, F.; Akerlof, C.] Univ Michigan, Randall Lab Phys, Ann Arbor, MI 48109 USA. RP Chatzopoulos, E (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM manolis@astro.as.utexas.edu FU NSF [AST-0707669]; Texas Advanced Research Program [ASTRO-ARP-0094]; Propondis foundation of Piraeus, Greece; Hungarian OTKA [K76816] FX We are grateful to the anonymous referee for valuable guidance on style and science, and to Andy Howell and Milos Milosavljevic for useful discussions. This research is supported in part by NSF Grant AST-0707669 and by the Texas Advanced Research Program grant ASTRO-ARP-0094. E.C. thanks the Propondis foundation of Piraeus, Greece for its support of his studies. J.V. received support from Hungarian OTKA Grant K76816. NR 88 TC 39 Z9 39 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 MAR 10 PY 2011 VL 729 IS 2 AR 143 DI 10.1088/0004-637X/729/2/143 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737ZI UT WOS:000288608700066 ER PT J AU Cyganowski, CJ Brogan, CL Hunter, TR Churchwell, E Zhang, Q AF Cyganowski, C. J. Brogan, C. L. Hunter, T. R. Churchwell, E. Zhang, Q. TI BIPOLAR MOLECULAR OUTFLOWS AND HOT CORES IN GLIMPSE EXTENDED GREEN OBJECTS (EGOs) SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; infrared: stars; ISM: individual objects (G11.92-0.61, G19.01-0.03); ISM: jets and outflows; ISM: molecules; stars: formation; techniques: interferometric ID STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; ULTRACOMPACT HII-REGIONS; INFRARED ARRAY CAMERA; LOW-MASS PROTOSTARS; CO LINE FORMATION; METHANOL MASERS; GALACTIC PLANE; COLOGNE DATABASE AB We present high angular resolution Submillimeter Array and Combined Array for Research in Millimeter-wave Astronomy observations of two GLIMPSE Extended Green Objects (EGOs)-massive young stellar object (MYSO) outflow candidates identified based on their extended 4.5 mu m emission in Spitzer images. The millimeter observations reveal bipolar molecular outflows, traced by high-velocity (CO)-C-12(2-1) and HCO+(1-0) emission, coincident with the 4.5 mu m lobes in both sources. SiO(2-1) emission confirms that the extended 4.5 mu m emission traces active outflows. A single dominant outflow is identified in each EGO, with tentative evidence for multiple flows in one source (G11.92-0.61). The outflow driving sources are compact millimeter continuum cores, which exhibit hot core spectral line emission and are associated with 6.7 GHz Class II CH3OH masers. G11.92-0.61 is associated with at least three compact cores: the outflow driving source, and two cores that are largely devoid of line emission. In contrast, G19.01-0.03 appears as a single MYSO. The difference in multiplicity, the comparative weakness of its hot core emission, and the dominance of its extended envelope of molecular gas all suggest that G19.01-0.03 may be in an earlier evolutionary stage than G11.92-0.61. Modeling of the G19.01-0.03 spectral energy distribution suggests that a central (proto) star (M similar to 10 M-circle dot) has formed in the compact millimeter core (M-gas similar to 12-16 M-circle dot), and that accretion is ongoing at a rate of similar to 10-3 M-circle dot year(-1). Our observations confirm that these EGOs are young MYSOs driving massive bipolar molecular outflows and demonstrate that considerable chemical and evolutionary diversity are present within the EGO sample. C1 [Cyganowski, C. J.; Churchwell, E.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Cyganowski, C. J.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brogan, C. L.; Hunter, T. R.] NRAO, Charlottesville, VA 22903 USA. RP Cyganowski, CJ (reprint author), Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. EM ccyganowski@cfa.harvard.edu OI Hunter, Todd/0000-0001-6492-0090; Zhang, Qizhou/0000-0003-2384-6589 FU Smithsonian Institution; Academia Sinica; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; states of California, Illinois, and Maryland; National Science Foundation; CARMA partner universities 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.; Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. NR 88 TC 33 Z9 35 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 MAR 10 PY 2011 VL 729 IS 2 AR 124 DI 10.1088/0004-637X/729/2/124 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737ZI UT WOS:000288608700047 ER PT J AU Kim, HJ Evans, NJ Dunham, MM Chen, JH Lee, JE Bourke, TL Huard, TL Shirley, YL De Vries, C AF Kim, Hyo Jeong Evans, Neal J., II Dunham, Michael M. Chen, Jo-Hsin Lee, Jeong-Eun Bourke, Tyler L. Huard, Tracy L. Shirley, Yancy L. De Vries, Christopher TI THE SPITZER C2D SURVEY OF NEARBY DENSE CORES. XI. INFRARED AND SUBMILLIMETER OBSERVATIONS OF CB130 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: individual objects (CB130); stars: formation; stars: low-mass; submillimeter: ISM ID MASS STAR-FORMATION; MULTIBAND IMAGING PHOTOMETER; PRE-PROTOSTELLAR CORES; MOLECULAR CLOUD CORES; YOUNG STELLAR OBJECTS; LOW-LUMINOSITY OBJECT; 1ST HYDROSTATIC CORE; CLASS-I PROTOSTARS; ARRAY CAMERA IRAC; SPACE-TELESCOPE AB We present new observations of the CB130 region composed of three separate cores. Using the Spitzer Space Telescope, we detected a Class 0 and a Class II object in one of these, CB130-1. The observed photometric data from Spitzer and ground-based telescopes are used to establish the physical parameters of the Class 0 object. Spectral energy distribution fitting with a radiative transfer model shows that the luminosity of the Class 0 object is 0.14-0.16 L-circle dot, which is low for a protostellar object. In order to constrain the chemical characteristics of the core having the low-luminosity object, we compare our molecular line observations to models of lines including abundance variations. We tested both ad hoc step function abundance models and a series of self-consistent chemical evolution models. In the chemical evolution models, we consider a continuous accretion model and an episodic accretion model to explore how variable luminosity affects the chemistry. The step function abundance models can match observed lines reasonably well. The best-fitting chemical evolution model requires episodic accretion and the formation of CO2 ice from CO ice during the low-luminosity periods. This process removes C from the gas phase, providing a much improved fit to the observed gas-phase molecular lines and the CO2 ice absorption feature. Based on the chemical model result, the low luminosity of CB130-1 is explained better as a quiescent stage between episodic accretion bursts rather than being at the first hydrostatic core stage. C1 [Kim, Hyo Jeong; Evans, Neal J., II; Dunham, Michael M.; Chen, Jo-Hsin] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Dunham, Michael M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Chen, Jo-Hsin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lee, Jeong-Eun] Sejong Univ, Dept Astron & Space Sci, Astrophys Res Ctr Struct & Evolut Cosmos, Seoul 143747, South Korea. [Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huard, Tracy L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Shirley, Yancy L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [De Vries, Christopher] Calif State Univ Stanislaus, Turlock, CA 95382 USA. RP Kim, HJ (reprint author), Univ Texas Austin, Dept Astron, 1 Univ Stn,C1400, Austin, TX 78712 USA. EM hyojeong@astro.as.utexas.edu RI Lee , Jeong-Eun/E-2387-2013 FU NASA [1224608, 1288664, 1407, NNX07AJ72G, 1279198, 1288806, 1342425]; NSF [AST-0607793, AST-0708158]; Korea government (MEST) [2009-0062866]; Ministry of Education, Science and Technology [2010-0008704] FX We thank the Lorentz Center in Leiden for hosting several meetings that contributed to this paper. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608 and 1288664 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Support was also provided by NASA Origins grant NNX07AJ72G and NSF grant AST-0607793 to the University of Texas at Austin. This research was also supported by the National Research Foundation of Korea (NRF) grant funded by the Korea government (MEST; No. 2009-0062866) and by Basic Science Research Program through the NRF funded by the Ministry of Education, Science and Technology (No. 2010-0008704). T.L.B. was partially supported by NASA through contracts 1279198, 1288806, and 1342425 issued by the Jet Propulsion Laboratory, California Institute of Technology to the Smithsonian Astrophysical Observatory, and by the NSF through grant AST-0708158. NR 75 TC 16 Z9 16 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 MAR 10 PY 2011 VL 729 IS 2 AR 84 DI 10.1088/0004-637X/729/2/84 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737ZI UT WOS:000288608700007 ER PT J AU Liu, HB Zhang, QZ Ho, PTP AF Liu, Hauyu Baobab Zhang, Qizhou Ho, Paul T. P. TI AN OVERALL PICTURE OF THE GAS FLOW IN A MASSIVE CLUSTER-FORMING REGION: THE CASE OF G10.6-0.4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE evolution; H II regions; ISM: individual objects (G10.6-0.4); ISM: kinematics and dynamics; stars: formation; stars: massive ID ULTRACOMPACT HII-REGIONS; OUTFLOW-DRIVEN TURBULENCE; H-II REGIONS; STAR-FORMATION; ACCRETION FLOW; SUBMILLIMETER ARRAY; RADIATION PRESSURE; MOLECULAR CLOUDS; OB-CLUSTERS; CORE AB The massive clump G10.6-0.4 is an OB cluster-forming region, in which multiple ultracompact (UC) H II regions have been identified. In the present study, we report arcsecond resolution observations of the CS (1-0) transition, the NH3 (3,3) main hyperfine inversion transition, the CH3OH J=5 transitions, and the centimeter free-free continuum emissions in this region. The comparisons of the molecular line emissions with the free-free continuum emissions reveal a 0.5 pc scale massive molecular envelope which is being partially dispersed by the dynamically expanding bipolar ionized cavity. The massive envelope is rotationally flattened and has an enhanced molecular density in the mid-plane. In the center of this massive clump lies a compact (< 0.1 pc) hot (greater than or similar to 100 K) toroid, in which a cluster of O-type stars has formed. This overall geometry is analogous to the standard core collapse picture in a low-mass star-forming region, with a central (proto-) stellar object, a disk, an envelope, and a bipolar outflow and outflow cavity. However, G10.6-0.4 has a much larger physical size scale (<= 0.1 pc for typical low-mass star-forming core). Based on the observations, we propose a schematic picture of the OB cluster-forming region, which incorporates the various physical mechanisms. This model will be tested with the observations of other embedded OB clusters, and with numerical simulations. C1 [Liu, Hauyu Baobab; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Hauyu Baobab; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Liu, Hauyu Baobab; Ho, Paul T. P.] Natl Taiwan Univ, Dept Phys, Taipei, Taiwan. RP Liu, HB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hlu@cfa.havard.edu; qzhang@cfa.harvard.edu; pho@asiaa.sinica.edu.tw OI Zhang, Qizhou/0000-0003-2384-6589 NR 50 TC 18 Z9 18 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 MAR 10 PY 2011 VL 729 IS 2 AR 100 DI 10.1088/0004-637X/729/2/100 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737ZI UT WOS:000288608700023 ER PT J AU Mackay, DH Green, LM van Ballegooijen, A AF Mackay, Duncan H. Green, L. M. van Ballegooijen, Aad TI MODELING THE DISPERSAL OF AN ACTIVE REGION: QUANTIFYING ENERGY INPUT INTO THE CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; Sun: activity; Sun: corona ID FREE MAGNETIC-FIELDS; GLOBAL SOLAR CORONA; LARGE-SCALE CORONA; FILAMENT CHANNELS; EVOLUTION MODEL; MASS EJECTIONS; EMERGING FLUX; HELICITY; SUN; CHIRALITY AB In this paper, a new technique for modeling nonlinear force-free fields directly from line-of-sight magnetogram observations is presented. The technique uses sequences of magnetograms directly as lower boundary conditions to drive the evolution of coronal magnetic fields between successive force-free equilibria over long periods of time. It is illustrated by applying it to SOHO: MDI observations of a decaying active region, NOAA AR 8005. The active region is modeled during a four-day period around its central meridian passage. Over this time, the dispersal of the active region is dominated by random motions due to small-scale convective cells. Through studying the buildup of magnetic energy in the model, it is found that such small-scale motions may inject anywhere from (2.5-3) x 10(25) erg s(-1) of free magnetic energy into the coronal field. Most of this energy is stored within the center of the active region in the low corona, below 30 Mm. After four days, the buildup of free energy is 10% that of the corresponding potential field. This energy buildup is sufficient to explain the radiative losses at coronal temperatures within the active region. Small-scale convective motions therefore play an integral part in the energy balance of the corona. This new technique has wide ranging applications with the new high-resolution, high-cadence observations from the SDO:HMI and SDO:AIA instruments. C1 [Mackay, Duncan H.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. [Green, L. M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [van Ballegooijen, Aad] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mackay, DH (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. EM duncan@mcs.st-and.ac.uk; lmg@mssl.ucl.ac.uk; vanballe@cfa.harvard.edu OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU UK STFC; Royal Society; Leverhulme Trust FX D.H.M. thanks UK STFC for their financial support and the Royal Society for funding an 81 processor supercomputer under their Research Grants Scheme. L.M.G. thanks the Royal Society and Leverhulme Trust for financial support. We acknowledge the use of data provided by the SOHO/MDI instrument. The authors thank the referee for constructive comments which have improved this paper. NR 53 TC 26 Z9 26 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 2011 VL 729 IS 2 AR 97 DI 10.1088/0004-637X/729/2/97 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737ZI UT WOS:000288608700020 ER PT J AU Munoz, JA Loeb, A AF Munoz, J. A. Loeb, A. TI CONSTRAINING THE MINIMUM MASS OF HIGH-REDSHIFT GALAXIES AND THEIR CONTRIBUTION TO THE IONIZATION STATE OF THE INTERGALACTIC MEDIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; early universe; galaxies: formation; galaxies: high-redshift; stars: formation ID ULTRA-DEEP-FIELD; SIMILAR-TO 7; UV LUMINOSITY FUNCTIONS; COSMIC REIONIZATION; NONPARAMETRIC MODEL; HALO/SUBHALO MASS; FORMATION HISTORY; FORMING GALAXIES; MERGER RATES; L-ASTERISK AB We model the latest HST WFPC3/IR observations of greater than or similar to 100 galaxies at redshifts z = 7-8 in terms of a hierarchical galaxy formation model with starburst activity. Our model provides a distribution of UV luminosities per dark matter halo of a given mass and a natural explanation for the fraction of halos hosting galaxies. The observed luminosity function is best fit with a minimum halo mass per galaxy of 10(-0.9)(9.4)(+0.3) M-circle dot, corresponding to a virial temperature of 10(-0.7)(4.9)(+0.2) K. Extrapolating to faint, undetected galaxies, the total production rate of ionizing radiation depends critically on this minimum mass. Future measurements with JWST should determine whether the entire galaxy population can comfortably account for the UV background required to keep the intergalactic medium ionized. C1 [Munoz, J. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Munoz, J. A.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Munoz, JA (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RI Munoz, Joseph/A-3336-2013 OI Munoz, Joseph/0000-0003-1588-1296 FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX We thank Steve Furlanetto and Michele Trenti for useful comments and discussions. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A (for A.L.). NR 53 TC 52 Z9 52 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 MAR 10 PY 2011 VL 729 IS 2 AR 99 DI 10.1088/0004-637X/729/2/99 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737ZI UT WOS:000288608700022 ER PT J AU Rest, A Foley, RJ Gezari, S Narayan, G Draine, B Olsen, K Huber, ME Matheson, T Garg, A Welch, DL Becker, AC Challis, P Clocchiatti, A Cook, KH Damke, G Meixner, M Miknaitis, G Minniti, D Morelli, L Nikolaev, S Pignata, G Prieto, JL Smith, RC Stubbs, C Suntzeff, NB Walker, AR Wood-Vasey, WM Zenteno, A Wyrzykowski, L Udalski, A Szymanski, MK Kubiak, M Pietrzynski, G Soszynski, I Szewczyk, O Ulaczyk, K Poleski, R AF Rest, A. Foley, R. J. Gezari, S. Narayan, G. Draine, B. Olsen, K. Huber, M. E. Matheson, T. Garg, A. Welch, D. L. Becker, A. C. Challis, P. Clocchiatti, A. Cook, K. H. Damke, G. Meixner, M. Miknaitis, G. Minniti, D. Morelli, L. Nikolaev, S. Pignata, G. Prieto, J. L. Smith, R. C. Stubbs, C. Suntzeff, N. B. Walker, A. R. Wood-Vasey, W. M. Zenteno, A. Wyrzykowski, L. Udalski, A. Szymanski, M. K. Kubiak, M. Pietrzynski, G. Soszynski, I. Szewczyk, O. Ulaczyk, K. Poleski, R. TI PUSHING THE BOUNDARIES OF CONVENTIONAL CORE-COLLAPSE SUPERNOVAE: THE EXTREMELY ENERGETIC SUPERNOVA SN 2003ma SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; dust, extinction; supernovae: individual (SN 2003ma) ID LARGE-MAGELLANIC-CLOUD; QUANTITATIVE SPECTROSCOPIC ANALYSIS; GRAVITATIONAL LENSING EXPERIMENT; TIDAL DISRUPTION EVENTS; SPITZER SPACE TELESCOPE; CARBON-MONOXIDE; LUMINOUS SUPERNOVA; INFRARED-EMISSION; DUST FORMATION; II SUPERNOVAE AB We report the discovery of a supernova (SN) with the highest apparent energy output to date and conclude that it represents an extreme example of the Type IIn subclass. The SN, which was discovered behind the Large Magellanic Cloud at z = 0.289 by the SuperMACHO microlensing survey, peaked at M-R = -21.5 mag and only declined by 2.9 mag over 4.7 years after the peak. Over this period, SN 2003ma had an integrated bolometric luminosity of 4 x 10(51) erg, more than any other SN to date. The radiated energy is close to the limit allowed by conventional core-collapse explosions. Optical spectra reveal that SN 2003ma has persistent single-peaked intermediate-width hydrogen lines, a signature of interaction between the SN and a dense circumstellar medium. The light curves show further evidence for circumstellar interaction, including a long plateau with a shape very similar to the classic SN IIn 1988Z-however, SN 2003ma is 10 times more luminous at all epochs. The fast velocity measured for the intermediate-width H alpha component (similar to 6000 km s(-1)) points toward an extremely energetic explosion (> 10(52) erg), which imparts a faster blast-wave speed to the post-shock material and a higher luminosity from the interaction than is observed in typical SNe IIn. Mid-infrared observations of SN 2003ma suggest an infrared light echo is produced by normal interstellar dust at a distance similar to 0.5 pc from the SN. C1 [Rest, A.; Narayan, G.; Stubbs, C.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Foley, R. J.; Challis, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gezari, S.; Huber, M. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Draine, B.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Olsen, K.; Smith, R. C.; Walker, A. R.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. [Olsen, K.; Matheson, T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Garg, A.; Cook, K. H.; Nikolaev, S.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Welch, D. L.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Becker, A. C.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Clocchiatti, A.; Minniti, D.] Pontificia Univ Catolica Chile, Dept Astron, Santiago 22, Chile. [Damke, G.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Meixner, M.] STScI, Baltimore, MD 21218 USA. [Miknaitis, G.] Ctr Neighborhood Technol, Chicago, IL 60647 USA. [Morelli, L.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Prieto, J. L.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Prieto, J. L.] Carnegie Observ, Pasadena, CA 91101 USA. [Suntzeff, N. B.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Udalski, A.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Soszynski, I.; Szewczyk, O.; Ulaczyk, K.; Poleski, R.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland. [Pietrzynski, G.; Szewczyk, O.] Univ Concepcion, Dept Fis, Astron Grp, Concepcion, Chile. RP Rest, A (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM arest@physics.harvard.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Draine, Bruce/0000-0002-0846-936X; Narayan, Gautham/0000-0001-6022-0484 FU NOAO; National Science Foundation; STScI [GO-10583]; US Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; McDonnell Foundation; Harvard University; FONDAP [CFA 15010003]; Basal CATA [0609]; Padova University [CPDR061795/06]; Natural Sciences and Engineering Research Council of Canada (NSERC); EC [PERG04-GA-2008-234784]; Polish MNiSW [N20303032/4275]; [P06-045-F ICM-MIDEPLAN] FX We thank the referee for many insightful comments that helped to improve this paper. The SuperMACHO survey was undertaken under the auspices of the NOAO Survey Program. We are very grateful for the support provided to the Survey program from the NOAO and the National Science Foundation. We are particularly indebted to the scientists and staff at the Cerro Tololo Inter-American Observatory for their assistance in helping us carry out the survey. SuperMACHO is supported by the STScI Grant GO-10583. A.R. thanks the NOAO Goldberg Fellowship Program for its support. The work of A.G., K.H.C., M.E.H., and S.N. was performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. C. Stubbs thanks the McDonnell Foundation for its support through a Centennial Fellowship. C. Stubbs, A.G., and A.R. are also grateful for support from Harvard University. A.C. and G.P. acknowledge the support of grant P06-045-F ICM-MIDEPLAN. D.M., A.C., and G.P. are supported by grants FONDAP CFA 15010003 and Basal CATA 0609. L.M. is supported by grant (CPDR061795/06) from Padova University. D.L.W. acknowledges financial support in the form of a Discovery Grant from the Natural Sciences and Engineering Research Council of Canada (NSERC). L.W. acknowledges support by the EC FR7 grant PERG04-GA-2008-234784. Based on observations obtained as part of the GS-2003B-Q-12 science program at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the US National Science Foundation on behalf of the Gemini partnership: the NSF (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). The OGLE project is partially supported by the Polish MNiSW grant N20303032/4275. NR 103 TC 35 Z9 35 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 MAR 10 PY 2011 VL 729 IS 2 AR 88 DI 10.1088/0004-637X/729/2/88 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737ZI UT WOS:000288608700011 ER PT J AU Sand, DJ Graham, ML Bildfell, C Foley, RJ Pritchet, C Zaritsky, D Hoekstra, H Just, DW Herbert-Fort, S Sivanandam, S AF Sand, David J. Graham, Melissa L. Bildfell, Chris Foley, Ryan J. Pritchet, Chris Zaritsky, Dennis Hoekstra, Henk Just, Dennis W. Herbert-Fort, Stephane Sivanandam, Suresh TI INTRACLUSTER SUPERNOVAE IN THE MULTI-EPOCH NEARBY CLUSTER SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; supernovae: general ID DIGITAL SKY SURVEY; DIFFUSE OPTICAL LIGHT; REDSHIFT GALAXY CLUSTERS; IA SUPERNOVAE; VIRGO CLUSTER; LUMINOSITY FUNCTION; GLOBULAR-CLUSTERS; STAR-FORMATION; ELLIPTIC GALAXIES; K-CORRECTIONS AB The Multi-Epoch Nearby Cluster Survey has discovered 23 cluster Type Ia supernovae (SNe Ia) in the 58 X-ray-selected galaxy clusters (0.05 less than or similar to z less than or similar to 0.15) surveyed. Four of our SN Ia events have no host galaxy on close inspection, and are likely intracluster SNe. Although one of the candidates, Abell399_3_14_0, appears to be associated in projection with the outskirts of a nearby red sequence galaxy, its velocity offset of similar to 1000 km s(-1) indicates that it is unbound and therefore an intracluster SN. Another of our candidates, Abell85_6_08_0, has a spectrum consistent with an SN1991bg-like object, suggesting that at least some portion of intracluster stars belong to an old stellar population. Deep image stacks at the location of the candidate intracluster SNe put upper limits on the luminosities of faint hosts, with M-r greater than or similar to -13.0 mag and M-g greater than or similar to -12.5 mag in all cases. For such limits, the fraction of the cluster luminosity in faint dwarfs below our detection limit is less than or similar to 0.1%, assuming a standard cluster luminosity function. All four events occurred within similar to 600 kpc of the cluster center (projected), as defined by the position of the brightest cluster galaxy, and are more centrally concentrated than the cluster SN Ia population as a whole. After accounting for several observational biases that make intracluster SNe easier to discover and spectroscopically confirm, we calculate an intracluster stellar mass fraction of 0.16(-0.09)(+0.13) (68% confidence limit) for all objects within R-200. If we assume that the intracluster stellar population is exclusively old, and the cluster galaxies themselves have a mix of stellar ages, we derive an upper limit on the intracluster stellar mass fraction of < 0.47 (84% one-sided confidence limit). When combined with the intragroup SNe results of McGee & Balogh, we confirm the declining intracluster stellar mass fraction as a function of halo mass reported by Gonzalez and collaborators. C1 [Sand, David J.; Graham, Melissa L.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Sand, David J.; Graham, Melissa L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Graham, Melissa L.; Bildfell, Chris; Pritchet, Chris] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zaritsky, Dennis; Just, Dennis W.; Herbert-Fort, Stephane; Sivanandam, Suresh] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hoekstra, Henk] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. RP Sand, DJ (reprint author), Harvard Ctr Astrophys, Cambridge, MA USA. EM dsand@lcogt.net OI Hoekstra, Henk/0000-0002-0641-3231 FU NASA LTSA [NNG05GE82G]; NSF [AST-0307492]; Netherlands Organization for Scientific Research VIDI grant; Marie Curie International Reintegration Grant; Natural Sciences and Engineering Research Council of Canada; National Aeronautics and Space Administration FX Many thanks to Kathy Roth and Tom Matheson for ensuring that the Gemini observations were taken properly. We thank the CFHT queue observers and software team for acquiring excellent data and making it available to us in near real time. We thank Yan Gao for making us aware of the typographical error in Equation (1) of Sullivan et al. (2006). We are also grateful to Stephenson Yang for his patience and diligence regarding computer and network maintenance. D.J.S. thanks Nelson Caldwell for the use of his spectral templates, along with Greg Rudnick and Tommaso Treu for useful discussions. D.Z. acknowledges support from NASA LTSA award NNG05GE82G and NSF grant AST-0307492. H.H. acknowledges support from a Netherlands Organization for Scientific Research VIDI grant and a Marie Curie International Reintegration Grant. C.P. acknowledges the support of the Natural Sciences and Engineering Research Council of Canada. 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.; Based on observations obtained at the Gemini Observatory (under program IDs GN-2009A-Q-10 and GN-2008B-Q-3), 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 eTecnologia (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). NR 81 TC 26 Z9 27 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 MAR 10 PY 2011 VL 729 IS 2 AR 142 DI 10.1088/0004-637X/729/2/142 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 737ZI UT WOS:000288608700065 ER PT J AU Boeke, NL Marshall, JD Alvarez, S Chance, KV Fried, A Kurosu, TP Rappengluck, B Richter, D Walega, J Weibring, P Millet, DB AF Boeke, Nicholas L. Marshall, Julian D. Alvarez, Sergio Chance, Kelly V. Fried, Alan Kurosu, Thomas P. Rappenglueck, Bernhard Richter, Dirk Walega, James Weibring, Petter Millet, Dylan B. TI Formaldehyde columns from the Ozone Monitoring Instrument: Urban versus background levels and evaluation using aircraft data and a global model SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SATELLITE-OBSERVATIONS; EMISSION INVENTORIES; ISOPRENE EMISSIONS; NORTH-AMERICA; IN-SITU; SPACE; SCIAMACHY; MEXICO; TRANSPORT; CAMPAIGN AB We combine aircraft measurements (Second Texas Air Quality Study, Megacity Initiative: Local and Global Research Observations, Intercontinental Chemical Transport Experiment: Phase B) over the United States, Mexico, and the Pacific with a 3-D model (GEOS-Chem) to evaluate formaldehyde column (Omega(HCHO)) retrievals from the Ozone Monitoring Instrument (OMI) and assess the information they provide on HCHO across local to regional scales and urban to background regimes. OMI Omega(HCHO) correlates well with columns derived from aircraft measurements and GEOS-Chem (R = 0.80). For the full data ensemble, OMI's mean bias is -3% relative to aircraft-derived Omega(HCHO) (-17% where Omega(HCHO) > 5 x 10(15) molecules cm(-2)) and -8% relative to GEOS-Chem, within expected uncertainty for the retrieval. Some negative bias is expected for the satellite and model, given the plume sampling of many flights and averaging over the satellite and model footprints. Major axis regression for OMI versus aircraft and model columns yields slopes (95% confidence intervals) of 0.80 (0.62-1.03) and 0.98 (0.73-1.35), respectively, with no significant intercept. Aircraft measurements indicate that the normalized vertical HCHO distribution, required by the satellite retrieval, is well captured by GEOS-Chem, except near Mexico City. Using measured HCHO profiles in the retrieval algorithm does not improve satellite-aircraft agreement, suggesting that use of a global model to specify shape factors does not substantially degrade retrievals over polluted areas. While the OMI measurements show that biogenic volatile organic compounds dominate intra-annual and regional Omega(HCHO) variability across the United States, smaller anthropogenic Omega(HCHO) gradients are detectable at finer spatial scales (similar to 20-200 km) near many urban areas. C1 [Boeke, Nicholas L.; Marshall, Julian D.; Millet, Dylan B.] Univ Minnesota, Dept Civil Engn, Minneapolis, MN 55455 USA. [Alvarez, Sergio; Rappenglueck, Bernhard] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77004 USA. [Chance, Kelly V.; Kurosu, Thomas P.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Fried, Alan; Richter, Dirk; Walega, James; Weibring, Petter] Natl Ctr Atmospher Res, Earth Observing Lab, Boulder, CO 80307 USA. [Millet, Dylan B.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA. RP Boeke, NL (reprint author), Univ Minnesota, Dept Civil Engn, Minneapolis, MN 55455 USA. EM dbm@umn.edu RI Marshall, Julian/B-2998-2012; Millet, Dylan/G-5832-2012; Chem, GEOS/C-5595-2014; OI Chance, Kelly/0000-0002-7339-7577 FU University of Minnesota; NASA [NNX10AG65G]; NSF [0853467] FX This work was supported by the University of Minnesota, NASA (NNX10AG65G), and NSF (0853467). We thank NASA, KNMI, and SEDAC/CIESIN for data collection and processing and the INTEX-B, MILAGRO, and TexAQS II science teams. NR 47 TC 17 Z9 17 U1 3 U2 32 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 10 PY 2011 VL 116 AR D05303 DI 10.1029/2010JD014870 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 734HD UT WOS:000288324300003 ER PT J AU Erlandson, JM Rick, TC Braje, TJ Casperson, M Culleton, B Fulfrost, B Garcia, T Guthrie, DA Jew, N Kennett, DJ Moss, ML Reeder, L Skinner, C Watts, J Willis, L AF Erlandson, Jon M. Rick, Torben C. Braje, Todd J. Casperson, Molly Culleton, Brendan Fulfrost, Brian Garcia, Tracy Guthrie, Daniel A. Jew, Nicholas Kennett, Douglas J. Moss, Madonna L. Reeder, Leslie Skinner, Craig Watts, Jack Willis, Lauren TI Paleoindian Seafaring, Maritime Technologies, and Coastal Foraging on California's Channel Islands SO SCIENCE LA English DT Article ID NORTH-AMERICA; CLOVIS; ARCHAEOLOGY AB Three archaeological sites on California's Channel Islands show that Paleoindians relied heavily on marine resources. The Paleocoastal sites, dated between similar to 12,200 and 11,200 years ago, contain numerous stemmed projectile points and crescents associated with a variety of marine and aquatic faunal remains. At site CA-SRI-512 on Santa Rosa Island, Paleocoastal peoples used such tools to capture geese, cormorants, and other birds, along with marine mammals and finfish. At Cardwell Bluffs on San Miguel Island, Paleocoastal peoples collected local chert cobbles, worked them into bifaces and projectile points, and discarded thousands of marine shells. With bifacial technologies similar to those seen in Western Pluvial Lakes Tradition assemblages of western North America, the sites provide evidence for seafaring and island colonization by Paleoindians with a diversified maritime economy. C1 [Erlandson, Jon M.; Casperson, Molly; Garcia, Tracy; Jew, Nicholas; Moss, Madonna L.; Willis, Lauren] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Erlandson, Jon M.; Casperson, Molly; Culleton, Brendan; Garcia, Tracy; Jew, Nicholas; Kennett, Douglas J.; Moss, Madonna L.; Willis, Lauren] 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. [Braje, Todd J.] Humboldt State Univ, Dept Anthropol, Arcata, CA USA. [Fulfrost, Brian] San Francisco State Univ, Dept Geog, San Francisco, CA 94132 USA. [Guthrie, Daniel A.] Claremont Mckenna Coll, Joint Sci Dept, Claremont, CA 91711 USA. [Guthrie, Daniel A.] Scripps Coll, Joint Sci Dept, Claremont, CA 91711 USA. [Guthrie, Daniel A.] Pitzer Coll, Joint Sci Dept, Claremont, CA 91711 USA. [Reeder, Leslie] So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA. [Skinner, Craig] NW Res Obsidian Studies Lab, Corvallis, OR 97330 USA. [Watts, Jack] Univ Oxford, Kellogg Coll, Oxford OX2 6PN, England. RP Erlandson, JM (reprint author), Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. EM jerland@uoregon.edu RI Kennett, Douglas/I-7613-2015; OI Kennett, Douglas/0000-0001-5133-9010; Erlandson, Jon/0000-0002-4705-4319 FU NSF [EAR 0746314, BCS 0917677]; Channel Islands National Park; Watts Family Foundation FX Supported by NSF grants EAR 0746314 (J.M.E.) and BCS 0917677 (J.M.E. and T.C.R.), Channel Islands National Park, our home institutions, D. Dana, D. Easly, and the Watts Family Foundation. Work at SRI-512 was conducted under ARPA permit PWR-1979-09-CA-04. We thank A. Huston, K. Minas, M. Senning, and I. Williams of Channel Islands National Park for logistical support; D. L. Johnson, D. Muhs, N. Pinter, and T. Rockwell for insights into the geology of the area; C. Billings, C. Buell, T. Davis, N. Dwyer, E. Erlandson, B. Fernandes, K. Hamm, C. Lopez, P. Pugh, J. Rizzi, Q. Shup, and J. Southon for help in the field or lab; and the editors and anonymous reviewers for their constructive comments and editorial suggestions. NR 24 TC 90 Z9 91 U1 5 U2 34 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 MAR 4 PY 2011 VL 331 IS 6021 BP 1181 EP 1185 DI 10.1126/science.1201477 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 729SN UT WOS:000287971200039 PM 21385713 ER PT J AU Nandy, D Munoz-Jaramillo, A Martens, PCH AF Nandy, Dibyendu Munoz-Jaramillo, Andres Martens, Petrus C. H. TI The unusual minimum of sunspot cycle 23 caused by meridional plasma flow variations SO NATURE LA English DT Article ID MAGNETIC-FIELD; FLUX-TRANSPORT; SOLAR DYNAMO; MODEL; RECONSTRUCTION; OSCILLATION; CIRCULATION; MODULATION; STRENGTH; SUN AB Direct observations over the past four centuries(1) show that the number of sunspots observed on the Sun's surface varies periodically, going through successive maxima and minima. Following sunspot cycle 23, the Sun went into a prolonged minimum characterized by a very weak polar magnetic field(2,3) and an unusually large number of days without sunspots(4). Sunspots are strongly magnetized regions(5) generated by a dynamo mechanism(6) that recreates the solar polar field mediated through plasma flows(7). Here we report results from kinematic dynamo simulations which demonstrate that a fast meridional flow in the first half of a cycle, followed by a slower flow in the second half, reproduces both characteristics of the minimum of sunspot cycle 23. Our model predicts that, in general, very deep minima are associated with weak polar fields. Sunspots govern the solar radiative energy(8,9) and radio flux, and, in conjunction with the polar field, modulate the solar wind, the heliospheric open flux and, consequently, the cosmic ray flux at Earth(3,10,11). C1 [Nandy, Dibyendu] Indian Inst Sci Educ & Res, Dept Phys Sci, Mohanpur 741252, W Bengal, India. [Munoz-Jaramillo, Andres; Martens, Petrus C. H.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Munoz-Jaramillo, Andres; Martens, Petrus C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nandy, D (reprint author), Indian Inst Sci Educ & Res, Dept Phys Sci, Mohanpur 741252, W Bengal, India. EM dnandi@iiserkol.ac.in OI Munoz-Jaramillo, Andres/0000-0002-4716-0840 FU Government of India at the Indian Institute of Science Education and Research, Kolkata; NASA; Montana State University FX This work was supported through the Ramanujan Fellowship of the Government of India at the Indian Institute of Science Education and Research, Kolkata, and by a NASA Living With a Star grant to the Smithsonian Astrophysical Observatory and Montana State University. We are grateful to D. Hathaway for providing the observational data on days without sunspots; the analysis of these data is reported in Supplementary Fig. 1. NR 28 TC 77 Z9 78 U1 0 U2 9 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAR 3 PY 2011 VL 471 IS 7336 BP 80 EP 82 DI 10.1038/nature09786 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 729BY UT WOS:000287924100037 PM 21368827 ER PT J AU Opresko, DM AF Opresko, D. M. TI Nomenclatural note: Heteropathes (Cnidaria: Anthozoa: Antipatharia: Cladopathidae): A new name for Heliopathes Opresko, 2003 SO ZOOTAXA LA English DT Letter C1 Smithsonian Inst, US Natl Museum Nat Hist, Washington, DC 20560 USA. RP Opresko, DM (reprint author), Smithsonian Inst, US Natl Museum Nat Hist, Washington, DC 20560 USA. EM dmopresko@hotmail.com NR 10 TC 3 Z9 3 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 MAR 3 PY 2011 IS 2782 BP 67 EP 68 PG 2 WC Zoology SC Zoology GA 729GD UT WOS:000287935800004 ER PT J AU Forrest, LL Allen, NS Gudino, JA Korpelainen, H Long, DG AF Forrest, Laura L. Salazar Allen, Noris Gudino, Jose A. Korpelainen, Helena Long, David G. TI Molecular and morphological evidence for distinct species in Dumortiera (Dumortieraceae) SO BRYOLOGIST LA English DT Article DE phylogeography; liverwort species; Central America; rbcL; psbA-trnH; rpoC1; ITS ID LIVERWORT CONOCEPHALUM-CONICUM; LAND PLANTS; MARCHANTIOPHYTA; TAXA; DIVERGENCE; PHYLOGENY; COMPLEX; DNA AB Contemporary taxonomists usually recognize a single species in Dumortiera, which is widely distributed through tropical and subtropical regions and extends into some temperate regions. Two subspecies, D. hirsuta subsp hirsuta and subsp. nepalensis, may be recognized, and both of these were thought to occur in Central America. We sequenced four loci, the nuclear internal transcribed spacer region ITS, and three chloroplast loci (rbcL, psbA-trnH and rpoC1) from 50 samples of Dumortiera across its geographic range to test for phylogenetic structure within the species and its congruence to morphological and geographic patterns. We also used light and scanning electron microscopy to examine morphological differences between accessions from Central America. Phylogenetic inferences reveal two highly distinct lineages: the first apparently restricted to Central America, and the second distributed across all the geographic regions sampled. This widespread lineage could itself be subdivided into several genetically and geographically distinct clades. The restricted Central American lineage contains plants that have a light green velvety appearance, due to an abundance of papillae on their upper thallus surface. These can therefore be distinguished morphologically from sympatric accessions of the widespread lineage, which are dark green, with a wide range of papillae densities (absent, few or abundant) on the thallus and usually with abundant marginal hairs. However, the wider application of these characters to lineages outside the Central American region has not yet been confirmed. We conclude that Dumortiera contains at least two, if not more, distinct species. The Asian epithet nepalensis does not seem applicable to plants in Central America, as the papillate morphotypes to which this name has been applied form an exclusively new world lineage. A thorough morphological revision of the genus, and reinvestigation of type material, is required. C1 [Forrest, Laura L.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA. [Salazar Allen, Noris; Gudino, Jose A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Salazar Allen, Noris; Gudino, Jose A.] Univ Panama, Balboa, Ancon, Panama. [Korpelainen, Helena] Univ Helsinki, Dept Agr Sci, FI-00014 Helsinki, Finland. [Long, David G.] Royal Bot Garden, Edinburgh EH3 5LR, Midlothian, Scotland. RP Forrest, LL (reprint author), Univ Connecticut, Dept Ecol & Evolutionary Biol, 75 N Eagleville Rd,Unit 3043, Storrs, CT 06269 USA. EM laura.forrest@uconn.edu OI Forrest, Laura/0000-0002-0235-9506; Korpelainen, Helena/0000-0002-7046-6995 FU Smithsonian Tropical Research Institute; Royal Botanic Garden, Edinburgh; University of Helsinki; National Science Foundation [EF-0531557] FX We are grateful to the Smithsonian Tropical Research Institute, Royal Botanic Garden, Edinburgh, University of Helsinki and National Science Foundation grant EF-0531557 to Bernard Goffinet for financial support for field collection, morphological research and molecular sequencing. Colleagues from University of Costa Rica (particularly J. Carranza, M.I. Morales) and Instituto Nacional de Biodiversidad (E. Lepiz) provided logistic support, transport and laboratory space. Field and laboratory assistance from University of Panama students (including N. Rivera, A. Espinosa, M. Moya, A. Almendra, J.C. Villarreal, J.E. De Gracia, B. Arauz) is gratefully acknowledged, as is field help from students of graduate course MBV825, Autonomous University of Chiriqui (E. Rodriguez, A. Gomez, D. Gomez, R. Villarreal, R. Rodriguez). Comments from two anonymous reviewers, members of the Goffinet lab and the journal editor improved this paper. We are grateful to herbarium curators at E for arranging loans and to Panamanian Autoridad Nacional del Ambiente for collection and export permits. Finally, we dedicate this manuscript to Barbara Crandall-Stotler and Raymond Stotler, in appreciation of their painstaking and integrative contributions to hepaticology. NR 34 TC 8 Z9 13 U1 1 U2 9 PU AMER BRYOLOGICAL LICHENOLOGICAL SOC INC PI OMAHA PA C/O DR ROBERT S EGAN, SEC-TRES, ABLS, UNIV NEBRASKA OMAHA, DEPT BIOLOGY, OMAHA, NE 68182-0040 USA SN 0007-2745 J9 BRYOLOGIST JI Bryologist PD SPR PY 2011 VL 114 IS 1 BP 102 EP 115 DI 10.1639/0007-2745-114.1.102 PG 14 WC Plant Sciences SC Plant Sciences GA 764NR UT WOS:000290637900009 ER PT J AU Nadkarni, NM Parker, GG Lowman, MD AF Nadkarni, Nalini M. Parker, Geoffrey G. Lowman, Margaret D. TI Forest canopy studies as an emerging field of science SO ANNALS OF FOREST SCIENCE LA English DT Letter ID VASCULAR EPIPHYTES; CLIMATE-CHANGE; RAIN-FOREST; ECOLOGY; ATMOSPHERE; DIVERSITY C1 [Nadkarni, Nalini M.] Evergreen State Coll, Olympia, WA 98505 USA. [Parker, Geoffrey G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Lowman, Margaret D.] NC State Univ, NC Museum Nat Sci, Raleigh, NC 27601 USA. RP Nadkarni, NM (reprint author), Evergreen State Coll, Olympia, WA 98505 USA. EM nadkarnn@evergreen.edu; parker@si.edu; Canopymeg@gmail.com OI Parker, Geoffrey/0000-0001-7055-6491 NR 45 TC 10 Z9 14 U1 2 U2 38 PU SPRINGER FRANCE PI PARIS PA 22 RUE DE PALESTRO, PARIS, 75002, FRANCE SN 1286-4560 J9 ANN FOREST SCI JI Ann. For. Sci. PD MAR PY 2011 VL 68 IS 2 BP 217 EP 224 DI 10.1007/s13595-011-0046-6 PG 8 WC Forestry SC Forestry GA 762BT UT WOS:000290448000002 ER PT J AU Gedan, KB Bernhardt, J Bertness, MD Leslie, HM AF Gedan, Keryn B. Bernhardt, Joanna Bertness, Mark D. Leslie, Heather M. TI Substrate size mediates thermal stress in the rocky intertidal SO ECOLOGY LA English DT Article DE abiotic factors; barnacle; climate change; heterogeneity; Narragansett Bay, Rhode Island, USA; Semibalanus balanoides; temperature thermal refuge ID CLIMATE-CHANGE; NEW-ENGLAND; BODY-TEMPERATURE; TERRESTRIAL ECTOTHERMS; WAVE EXPOSURE; COMPETITION; ZONATION; CHTHAMALUS; BARNACLES; COMMUNITY AB Variation in physical factors, such as slope, orientation, and wind exposure, shapes thermal conditions. Variation in substrate size is common in many habitats, but its thermal consequences for organisms are not well characterized. Larger substrates should remain more thermally stable and act as thermal refuges for associated organisms during short, thermally stressful periods such as midday temperature peaks or tidal exposure. In observations and a transplant and thermal integration experiment, we found that larger rock substrates stayed cooler and facilitated greater survival of the barnacle Semibalanus balanoides in the high intertidal relative to small substrates during the hot summer months in southern New England, USA. However, in thermally benign northern New England, rock substrate size had no effect on barnacle distributions, indicating that the thermal effects of substrate size are mediated by regional climate. C1 [Gedan, Keryn B.; Bernhardt, Joanna; Bertness, Mark D.; Leslie, Heather M.] Brown Univ, Dept Ecol & Evolutionary, Providence, RI 02912 USA. [Leslie, Heather M.] Brown Univ, Ctr Environm Studies, Providence, RI 02912 USA. RP Gedan, KB (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM gedank@si.edu RI Gedan, Keryn/A-3575-2010; OI Gedan, Keryn/0000-0003-4020-5441; Leslie, Heather/0000-0003-4512-9417 FU NERR GRF; Brown University UTRA; NSF EPSCOR FX This research was funded by a NERR GRF to K. Gedan and by Brown University UTRA and NSF EPSCOR grants to J. Bernhardt. This research was part of J. Bernhardt's senior thesis work. We thank the Narragansett Bay NERR and Mt. Hope Farm for access and permission to conduct experiments on their properties and M. Cockrell for help in the field. NR 44 TC 24 Z9 24 U1 2 U2 33 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 MAR PY 2011 VL 92 IS 3 BP 576 EP 582 DI 10.1890/10-0717.1 PG 7 WC Ecology SC Environmental Sciences & Ecology GA 763CC UT WOS:000290529800007 PM 21608466 ER PT J AU Myers, JA Harms, KE AF Myers, Jonathan A. Harms, Kyle E. TI Seed arrival and ecological filters interact to assemble high-diversity plant communities SO ECOLOGY LA English DT Article DE community assembly; dispersal assembly; environmental filtering; fire disturbance intensity; niche assembly; resource availability; soil moisture; species diversity; species pool; species-rich longleaf pine savanna ID SPECIES RICHNESS; PINE SAVANNAS; RECRUITMENT LIMITATION; RESOURCE AVAILABILITY; FUNCTIONAL TRAITS; FIRE; PATTERNS; NEUTRALITY; FORESTS; NICHE AB Two prominent mechanisms proposed to structure biodiversity are niche-based ecological filtering and chance arrival of propagules from the species pool. Seed arrival is hypothesized to play a particularly strong role in high-diversity plant communities with large potential species pools and many rare species, but few studies have explored how seed arrival and local ecological filters interactively assemble species-rich communities in space and time. We experimentally manipulated seed arrival and multiple ecological filters in high-diversity, herbaceous-dominated groundcover communities in longleaf pine savannas, which contain the highest small-scale species richness in North America (up to >40 species/m(2)). We tested three hypotheses: (1) local communities constitute relatively open-membership assemblages, in which increased seed arrival from the species pool strongly increases species richness; (2) ecological filters imposed by local fire intensity and soil moisture influence recruitment and richness of immigrating species; and (3) ecological filters increase similarity in the composition of immigrating species. In a two-year factorial field experiment, we manipulated local fire intensity by increasing pre-fire fuel loads, soil moisture using rain shelters and irrigation, and seed arrival by adding seeds from the local species pool. Seed arrival increased species richness regardless of fire intensity and soil moisture but interacted with both ecological filters to influence community assembly. High-intensity fire decreased richness of resident species, suggesting an important abiotic filter. In contrast, high-intensity fire increased recruitment and richness of immigrating species, presumably by decreasing effects of other ecological filters (competition and resource limitation) in postfire environments. Drought decreased recruitment and richness of immigrating species, whereas wet soil conditions increased recruitment but decreased or had little effect on richness. Moreover, some ecological filters (wet soil conditions and, to a lesser extent, high-intensity fire) increased similarity in the composition of immigrating species, illustrating conditions that influence deterministic community assembly in species-rich communities. Our experiment provides insights into how dispersal-assembly mechanisms may interact with niche-assembly mechanisms in space (spatial variation in disturbance) and time (temporal variation in resource availability) to structure high-diversity communities and can help guide conservation of threatened longleaf pine ecosystems in the face of habitat fragmentation and environmental change. C1 [Myers, Jonathan A.; Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Div Systemat Ecol & Evolut, Baton Rouge, LA 70803 USA. [Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Myers, JA (reprint author), Washington Univ, Dept Biol, Campus Box 1137,1 Brookings Dr, St Louis, MO 63130 USA. EM jamyers@wustl.edu FU Torrey Botanical Society; Sigma Xi; Louisiana Office of Environmental Education; LSU Biological Sciences Graduate Student Association (BioGrads); National Science Foundation FX We thank Natalia Aristizabal, Adriana Bravo, Jane Carlson, Santiago Claramunt, Rae Crandall, Jim Cronin, Sandra Galeano, Paul Gagnon, Morgan Kerns, Metha Klock, Teresa Kurtz, John Morgan, Tim Paine, Heather Passmore, Bill Platt, Ellen Reid, and Richard Stevens for assistance and helpful suggestions throughout the course of the study; Erik Johnson for sharing unpublished data on seed densities in longleaf pine savannas; the Southeastern Girl Scout Council and Larry Ehrlich for access to the field site and for maintaining prescribed fires; and two anonymous reviewers for constructive comments on the manuscript. Financial support was provided by the Torrey Botanical Society, Sigma Xi, the Louisiana Office of Environmental Education, LSU Biological Sciences Graduate Student Association (BioGrads), and the National Science Foundation. NR 58 TC 41 Z9 41 U1 10 U2 114 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 MAR PY 2011 VL 92 IS 3 BP 676 EP 686 DI 10.1890/10-1001.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 763CC UT WOS:000290529800017 PM 21608476 ER PT J AU Ryder, TB Blake, JG Parker, PG Loiselle, BA AF Ryder, Thomas B. Blake, John G. Parker, Patricia G. Loiselle, Bette A. TI The composition, stability, and kinship of reproductive coalitions in a lekking bird SO BEHAVIORAL ECOLOGY LA English DT Article DE coordinated display; leks; manakins; relatedness; reproductive coalitions; social networks ID LONG-TAILED MANAKINS; LEK-BREEDING BIRD; SOCIAL-ORGANIZATION; MULTIVARIATE-ANALYSIS; CHIROXIPHIA-LINEARIS; GENETIC-MARKERS; MANACUS-MANACUS; MATING SUCCESS; SPATIAL SCALES; KIN SELECTION AB Male vertebrates often form reproductive coalitions to gain access to or defend females. One striking example occurs in the wire-tailed manakin (Pipra filicauda; Aves: Pipridae), where pairs of males form coalitions to display for females on leks. Here, we use data from a long-term study of the wire-tailed manakin to quantify the composition and stability of display coalitions, to examine how coalitions influence behavioral variation, and to determine if males gain indirect genetic benefits from coalition membership. Our data show that coalitions were most often formed between males of different status and that the presence of coalition partners increased a male's display rate via social facilitation. Display coalitions were nonrandom and varied in stability with male age. Moreover, our data suggest that both floaters and territorial males maintain multiple coalition partnerships through time. Maintenance of fixed partnerships for territorial males is hypothesized to have reproductive fitness benefits by increasing display synchronization and signal intensity. Finally, our data show that although males do not appear to gain indirect inclusive fitness benefits by joining display coalitions with relatives, the kin structuring observed within male social networks is likely a consequence of strong reproductive skew, short dispersal distances, and limited recruitment opportunities. C1 [Ryder, Thomas B.; Blake, John G.; Parker, Patricia G.; Loiselle, Bette A.] Univ Missouri, Dept Biol, Whitney Harris Ctr World Ecol, St Louis, MO 63121 USA. RP Ryder, TB (reprint author), Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, POB 37012,MRC 5503, Washington, DC 20013 USA. EM Pipridae@gmail.com RI Loiselle, Bette/O-7106-2016 OI Loiselle, Bette/0000-0003-1434-4173 FU International Center for Tropical Ecology; AFO [7113-01]; National Science Foundation [IBN 0235141, IOB 0508189, OISE 0513341] FX International Center for Tropical Ecology, AFO's Alexander Bergstrom Award, National Geographic Society (7113-01), and National Science Foundation (IBN 0235141, IOB 0508189, and OISE 0513341). NR 55 TC 14 Z9 14 U1 3 U2 38 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 MAR-APR PY 2011 VL 22 IS 2 BP 282 EP 290 DI 10.1093/beheco/arq213 PG 9 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 747DC UT WOS:000289299500014 ER PT J AU Stone, N Loeb, A AF Stone, Nicholas Loeb, Abraham TI Prompt tidal disruption of stars as an electromagnetic signature of supermassive black hole coalescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; gravitational waves; galaxies: nuclei ID GALACTIC NUCLEI; GALAXY MERGERS; MASS FUNCTION; GAS DISK; BINARY; FLARES; CLUSTER; RECOIL; RATES; EVOLUTION AB A precise electromagnetic measurement of the sky coordinates and redshift of a coalescing black hole binary holds the key for using its gravitational wave (GW) signal to constrain cosmological parameters and to test general relativity. Here we show that the merger of similar to 106-7 M-circle dot black holes is generically followed by electromagnetic flares from tidally disrupted stars. The sudden recoil imparted to the merged black hole by GW emission promptly fills its loss cone and results in a tidal disruption rate of stars as high as similar to 0.1 yr-1. The prompt disruption of a single star within a galaxy provides a unique electromagnetic flag of a recent black hole coalescence event, and sequential disruptions could be used on their own to calibrate the expected rate of GW sources for pulsar timing arrays or the proposed Laser Interferometer Space Antenna. C1 [Stone, Nicholas; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stone, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nstone@cfa.harvard.edu FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX We thank Matt Holman, Bence Kocsis, Ryan O'Leary, Hagai Perets and Alberto Sesana for helpful comments on the manuscript. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 66 TC 33 Z9 33 U1 0 U2 0 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 MAR PY 2011 VL 412 IS 1 BP 75 EP 80 DI 10.1111/j.1365-2966.2010.17880.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 734YC UT WOS:000288378100009 ER PT J AU Kocsis, B Tremaine, S AF Kocsis, Bence Tremaine, Scott TI Resonant relaxation and the warp of the stellar disc in the Galactic Centre SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE celestial mechanics; Galaxy: centre; Galaxy: nucleus ID MASSIVE BLACK-HOLE; TWISTED ACCRETION DISKS; N-BODY SIMULATIONS; SGR-A-ASTERISK; YOUNG STARS; MILKY-WAY; NGC 4258; S-STARS; SYSTEMS; EVOLUTION AB Observations of the spatial distribution and kinematics of young stars in the Galactic Centre can be interpreted as showing that the stars occupy one, or possibly two, discs of radii similar to 0.05-0.5 pc. The most prominent ('clockwise') disc exhibits a strong warp: the normals to the mean orbital planes in the inner and the outer third of the disc differ by similar to 60 degrees. Using an analytical model based on Laplace-Lagrange theory, we show that such warps arise naturally and inevitably through vector resonant relaxation between the disc and the surrounding old stellar cluster. C1 [Kocsis, Bence] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kocsis, Bence; Tremaine, Scott] Inst Adv Study, Princeton, NJ 08540 USA. RP Kocsis, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bkocsis@cfa.harvard.edu; tremaine@ias.edu RI Kocsis, Bence/C-3061-2013; Tremaine, Scott/M-4281-2015 OI Kocsis, Bence/0000-0002-4865-7517; Tremaine, Scott/0000-0002-0278-7180 FU NASA [NNX08AH24G]; NSF [AST-0807432]; Chandra X-ray Center [NAS8-03060]; OTKA [68228] FX We thank Yuri Levin for useful discussions and the anonymous referee for suggestions that substantially improved the paper. This research was supported, in part, by NASA grant NNX08AH24G and NSF grant AST-0807432. BK acknowledges support by NASA through Einstein Postdoctoral Fellowship grant number PF9-00063 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060, and partial support by OTKA grant 68228. NR 61 TC 39 Z9 39 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 MAR PY 2011 VL 412 IS 1 BP 187 EP 207 DI 10.1111/j.1365-2966.2010.17897.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 734YC UT WOS:000288378100018 ER PT J AU Rudert, S Brown, JL Ganslosser, U Mobius, G Songsasen, N AF Rudert, S. Brown, J. L. Ganslosser, U. Moebius, G. Songsasen, N. TI Activity Pattern, Reproductive Behaviors and Gonadal Hormones in the Raccoon Dog (Nyctereutes procyonoides) SO ZOO BIOLOGY LA English DT Article DE raccoon dog; reproduction; behaviors in enclosures; gonadal hormones; non-invasive hormone analysis; gender determination AB The objectives of this study were to (1) assess year-round behaviors and activity patterns of captive raccoon dogs (Nyctereutes procyonoides) and (2) characterize the species' reproductive endocrinology. Behaviors and activity patterns of 12 (5.7) animals were recorded over a 1-year period. During that time, fecal samples were collected 2-7 times/week from 16 (7.9) individuals (six of these were included in the behavioral study) for the analysis of testosterone, progesterone and estrogen metabolite concentrations. Activity pattern and excretion of gonadal steroids followed a seasonal pattern. Specifically, dogs were cathemeral in summer, and primarily nocturnal in winter. In the males, testosterone concentrations were at baseline from April through September, began to rise in October and reached peak concentrations in February (P<0.05). In the females, elevated estrogen (P<0.05) was observed in March followed by an increase in progestagen concentrations from March through May (P<0.05) in both pregnant and pseudopregnant animals. Gender significantly influenced monthly testosterone/estrogen ratio (P<0.01); values were higher in males than in females throughout the year with overall percentage of overlapping values between males and females being 28%. In summary, this study characterized cirannual fluctuations in behaviors and gonadal steroid metabolites in the raccoon dog maintained in captivity. Because there is no obvious sexual dimorphism, the differences in testosterone/estrogen ratio may be useful for gender differentiation (72% accuracy), especially among individuals living in the wild. Zoo Biol 30:134-148, 2011. (C) 2010 Wiley-Liss, Inc. C1 [Songsasen, N.] Smithsonians Natl Zool Pk, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA 22630 USA. [Rudert, S.; Ganslosser, U.] Zool Inst & Museum, Greifswald, Germany. [Rudert, S.; Moebius, G.] Univ Leipzig, Fac Vet Med, Inst Anim Hyg & Vet Publ Hlth, Leipzig, Germany. RP Songsasen, N (reprint author), Smithsonians Natl Zool Pk, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA 22630 USA. EM songsasenn@si.edu FU Smithsonian Institution; DAAD (German Academic Exchange Service) FX Grant sponsors: Smithsonian Institution; DAAD (German Academic Exchange Service). NR 16 TC 4 Z9 4 U1 2 U2 24 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 EI 1098-2361 J9 ZOO BIOL JI Zoo Biol. PD MAR-APR PY 2011 VL 30 IS 2 BP 134 EP 148 DI 10.1002/zoo.20315 PG 15 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 748CP UT WOS:000289367900002 PM 21462244 ER PT J AU Brown, M Ortner, DJ AF Brown, Matthew Ortner, Donald J. TI Childhood Scurvy in a Medieval Burial from Macvanska Mitrovica, Serbia SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY LA English DT Article DE osteology; paleopathology; scurvy ID INFANTILE SCURVY; ARCHAEOLOGICAL SITES; MANIFESTATIONS; BOY; SUBADULTS; INFANCY AB The type and distribution of abnormalities in the skeleton of a child 2 years of age indicates that the child likely suffered from scurvy at the time of death. The burial is from the archaeological site of Zidine, Macvanska Mitrovica, Serbia dated to the Medieval Period. Abnormal porosity and reactive woven bone formation are present affecting both the axial and appendicular skeleton. This case of scurvy is important because archaeological evidence of scurvy in this geographical location and at this time period is unknown. It is also important because the relative completeness of the skeleton and the widespread evidence of skeletal abnormalities provide additional insight regarding the skeletal manifestations of scurvy in young children. Copyright (c) 2009 John Wiley & Sons, Ltd. C1 [Brown, Matthew] CUNY Brooklyn Coll, Dept Anthropol & Archaeol, Zooarchaeol Lab, Brooklyn, NY 11210 USA. [Brown, Matthew] CUNY, Grad Sch, Dept Anthropol, New York, NY USA. [Brown, Matthew] CUNY, Univ Ctr, New York, NY 10021 USA. [Ortner, Donald J.] Smithsonian Inst, Dept Anthropol, Washington, DC 20013 USA. [Ortner, Donald J.] Univ Bradford, Dept Archaeol Sci, Bradford BD7 1DP, W Yorkshire, England. RP Brown, M (reprint author), CUNY Brooklyn Coll, Dept Anthropol & Archaeol, Zooarchaeol Lab, 2900 Bedford Ave, Brooklyn, NY 11210 USA. EM mbrown3@gc.cuny.edu NR 32 TC 18 Z9 18 U1 1 U2 12 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1047-482X J9 INT J OSTEOARCHAEOL JI Int. J. Osteoarchaeol. PD MAR-APR PY 2011 VL 21 IS 2 BP 197 EP 207 DI 10.1002/oa.1124 PG 11 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 741OD UT WOS:000288872100007 ER PT J AU Falcon-Lang, HJ Heckel, PH Dimichele, WA Blake, BM Easterday, CR Eble, CF Elrick, S Gastaldo, RA Greb, SF Martino, RL Nelson, WJ Pfefferkorn, HW Phillips, TL Rosscoe, SJ AF Falcon-Lang, Howard J. Heckel, Philip H. Dimichele, William A. Blake, Bascombe M., Jr. Easterday, Cary R. Eble, Cortland F. Elrick, Scott Gastaldo, Robert A. Greb, Stephen F. Martino, Ronald L. Nelson, W. John Pfefferkorn, Hermann W. Phillips, Tom L. Rosscoe, Steven J. TI NO MAJOR STRATIGRAPHIC GAP EXISTS NEAR THE MIDDLE-UPPER PENNSYLVANIAN (DESMOINESIAN-MISSOURIAN) BOUNDARY IN NORTH AMERICA SO PALAIOS LA English DT Article ID COAL-SWAMP VEGETATION; APPALACHIAN REGION; COLUMBIANA COUNTY; NORTHEASTERN OHIO; CLIMATE-CHANGE; 7-11 MINE; TRANSITION; MIDCONTINENT; EURAMERICA; PATTERNS AB Interregional correlation of the marine zones of major cyclothems between North America and eastern Europe does not support assertions that a major stratigraphic gap exists between the traditional regional Desmoinesian and Missourian stages in North America. Such a gap was previously proposed to explain an abrupt change in megafloral assemblages in the northern Appalachian Basin and by extension across all of North America. Conodont-based correlation from the essentially complete low-shelf Midcontinent succession (distal from the highstand shoreline), through the mid-shelf Illinois Basin, to the high shelf of the Appalachian Basin (proximal to highstand shoreline) demonstrates that all major similar to 400 kyr cyclothem groupings in the Midcontinent are recognizable in the Illinois Basin. In the Appalachian Basin, however, the grouping at the base of the Missourian is represented only by paleosols and localized coal. The immediately preceding grouping was removed very locally by paleovalley incision, as is evident at the 7-11 Mine, Columbiana County, Ohio, from which the original megafloral data were derived. At the few localities where incised paleodrainage exists, there may be a gap of similar to 1000 kyr, but a gap of no more than similar to 600 kyr occurs elsewhere in the Appalachian Basin at that level and its magnitude progressively decreases westward into the Illinois (similar to 300 kyr) and Midcontinent (< 200 kyr) Basins. Thus, while a gap is present near the Desmoinesian Missourian boundary in North America, it is typically more than an order of magnitude smaller than that originally proposed and is similar to the gaps inferred at sequence boundaries between cyclothems at many horizons in the Pennsylvanian of North America. C1 [Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. [Heckel, Philip H.] Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA. [Dimichele, William A.] Smithsonian Inst, Natl Museum Amer Hist, Dept Paleobiol, Washington, DC 20560 USA. [Blake, Bascombe M., Jr.] W Virginia Geol Survey, Morgantown, WV 26508 USA. [Easterday, Cary R.] NE Illinois Univ, Dept Earth Sci, Chicago, IL 60625 USA. [Eble, Cortland F.; Greb, Stephen F.] Univ Kentucky, Kentucky Geol Survey, Lexington, KY 40506 USA. [Elrick, Scott; Nelson, W. John] Illinois State Geol Survey, Champaign, IL 61820 USA. [Gastaldo, Robert A.] Colby Coll, Dept Geol, Waterville, ME 04901 USA. [Martino, Ronald L.] Marshall Univ, Dept Geol, Huntington, WV 25701 USA. [Pfefferkorn, Hermann W.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. [Phillips, Tom L.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Rosscoe, Steven J.] Hardin Simmons Univ, Dept Geol Sci, Abilene, TX 79698 USA. RP Falcon-Lang, HJ (reprint author), Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. EM h.falcon-lang@es.rhul.ac.uk RI Falcon-Lang, Howard/D-8465-2011; DiMichele, William/K-4301-2012 FU NERC [NE/F014120/2] FX HFL gratefully acknowledges receipt of a NERC Advanced Fellowship (NE/F014120/2) held at Royal Holloway, University of London. PHH thanks J.E. Barrick, D.M. Work, G.A. McComas, T.I. Nemyrovska, and A.S. Alekseev for valuable biostratigraphic information, T.R. Miller and E.R. Slucher for valuable stratigraphic information, and the John Swade Memorial Fund for departmental funding. WD thanks the Smithsonian Institution Small Grants and Endowment Funds for support of work related to this study. Helpful pre-review comments from Martin Gib ling (Dalhousie University), thorough reviews from Erwin Zodrow (Cape Breton College) and Charles Henderson (University of Calgary), and the meticulous editorial comments of Edie Taylor, greatly improved this manuscript. NR 118 TC 38 Z9 38 U1 1 U2 7 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD MAR-APR PY 2011 VL 26 IS 3-4 BP 125 EP 139 DI 10.2110/palo.2010.p10-049r PG 15 WC Geology; Paleontology SC Geology; Paleontology GA 744XY UT WOS:000289129700002 ER PT J AU Finnegan, S McClain, CM Kosnik, MA Payne, JL AF Finnegan, Seth McClain, Craig M. Kosnik, Matthew A. Payne, Jonathan L. TI Escargots through time: an energetic comparison of marine gastropod assemblages before and after the Mesozoic Marine Revolution SO PALEOBIOLOGY LA English DT Article ID DEEP-SEA GASTROPODS; END-PERMIAN EXTINCTION; BODY-SIZE; DEATH ASSEMBLAGES; METABOLIC-RATE; EUKARYOTIC PHYTOPLANKTON; MORPHOLOGICAL DISPARITY; BATHYMETRIC PATTERNS; FOSSIL ASSEMBLAGES; SPECIES RICHNESS AB The modern structure of marine benthic ecosystems was largely established during the Jurassic and Early Cretaceous (200-100 Ma), a transition that has been termed the Mesozoic Marine Revolution (MMR). Although it has been suggested that the MMR marks an increase in the average energy consumption of marine animal ecosystems, this hypothesis has not been evaluated quantitatively. In this study, we integrate body size and abundance data from the fossil record with physiological data from living representatives to estimate mean per capita metabolic rates of tropical to subtropical assemblages of shallow-marine gastropods-a major component of marine ecosystems throughout the Meso-Cenozoic-both before and after the MMR. We find that mean per capita metabolic rate rose by similar to 150% between the Late Triassic and Late Cretaceous and remained relatively stable thereafter. The most important factor governing the increase in metabolic rate was an increase in mean body size. In principle, this size increase could result from secular changes in sampling and taphonomic biases, but these biases are suggested to yield decreases rather than increases in mean size. Considering that post-MMR gastropod diversity is dominated by predators, the net primary production required to supply the energetic needs of the average individual increased by substantially more than 150%. These data support the hypothesis that benthic energy budgets increased during the MMR, possibly in response to rising primary productivity. C1 [Finnegan, Seth; Payne, Jonathan L.] Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA. [McClain, Craig M.] Natl Evolutionary Synth Ctr, Durham, NC 27705 USA. [Kosnik, Matthew A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Finnegan, S (reprint author), CALTECH, Div Geol & Planetary Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM sethf@caltech.edu RI Kosnik, Matthew/G-2312-2010; Payne, Jonathan/A-1240-2007; Payne, Jonathan/B-8088-2012; OI Kosnik, Matthew/0000-0001-5380-7041; Payne, Jonathan/0000-0002-9601-3310; McClain, Craig/0000-0003-0574-428X NR 103 TC 24 Z9 24 U1 1 U2 14 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 2011 VL 37 IS 2 BP 252 EP 269 PG 18 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 744ZA UT WOS:000289132500005 ER PT J AU Kosnik, MA Alroy, J Behrensmeyer, AK Fursich, FT Gastaldo, RA Kidwell, SM Kowalewski, M Plotnick, RE Rogers, RR Wagner, PJ AF Kosnik, Matthew A. Alroy, John Behrensmeyer, Anna K. Fuersich, Franz T. Gastaldo, Robert A. Kidwell, Susan M. Kowalewski, Michal Plotnick, Roy E. Rogers, Raymond R. Wagner, Peter J. TI Changes in shell durability of common marine taxa through the Phanerozoic: evidence for biological rather than taphonomic drivers SO PALEOBIOLOGY LA English DT Article ID FOSSIL RECORD; LARGE-SCALE; BODY-SIZE; ARAGONITE DISSOLUTION; SEAWATER CHEMISTRY; BIVALVE TAPHONOMY; SPECIES-DIVERSITY; MASS EXTINCTIONS; MOLLUSCAN SHELLS; MISSING MOLLUSKS AB Phanerozoic trends in shell and life habit traits linked to postmortem durability were evaluated for the most common fossil brachiopod, gastropod, and bivalve genera in order to test for changes in taphonomic bias. Using the Paleobiology Database, we tabulated occurrence frequencies of genera for 48 intervals of similar to 11 Myr duration. The most frequently occurring genera, cumulatively representing 40% of occurrences in each time bin, were scored for intrinsic durability on the basis of shell size, reinforcement (ribs, folds, and spines), life habit, and mineralogy. Shell durability is positively correlated with the number of genera in a time bin, but durability traits exhibit different temporal patterns across higher taxa, with notable offsets in the timing of changes in these traits. We find no evidence for temporal decreases in durability that would indicate taphonomic bias at the Phanerozoic scale among commonly occurring genera. Also, all three groups show a remarkable stability in mean shell size through the Phanerozoic, an unlikely pattern if strong size-filtering taphonomic megabiases were affecting the fossil record of shelly faunas. Moreover, small shell sizes are attained in the early Paleozoic in brachiopods and in the latest Paleozoic in gastropods but are steady in bivalves; unreinforced shells are common to all groups across the entire Phanerozoic; organophosphatic and aragonitic shells dominate only the oldest and youngest time bins; and microstructures having high organic content are most common in the oldest time bins. In most cases, the timing of changes in durability-related traits is inconsistent with a late Mesozoic Marine Revolution. The post-Paleozoic increase in mean gastropod reinforcement occurs in the early Triassic, suggesting either an earlier appearance and expansion of durophagous predators or other drivers. Increases in shell durability hypothesized to be the result of increased predation in the late Mesozoic are not evident in the common genera examined here. Infaunal life habit does increase in the late Mesozoic, but it does not become more common than levels already attained during the Paleozoic, and only among bivalves does the elevated late Mesozoic level persist through the Holocene. These temporal patterns suggest control on the occurrence of durability-related traits by individual evolutionary histories rather than taphonomic megabiases. Our findings do not mean taphonomic biases are absent from the fossil record, but rather that their effects apparently have had little net effect on the relative occurrence of shell traits generally thought to confer higher preservation potential over long time scales. C1 [Kosnik, Matthew A.; Behrensmeyer, Anna K.; Wagner, Peter J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Alroy, John] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. [Fuersich, Franz T.] Univ Erlangen Nurnberg, GeoZentrum Nordbayern, Fachgrp Palaoumwelt, D-91054 Erlangen, Germany. [Gastaldo, Robert A.] Colby Coll, Dept Geol, Waterville, ME 04901 USA. [Kidwell, Susan M.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Kowalewski, Michal] Virginia Polytech Inst & State Univ, Dept Geosci, Blacksburg, VA 24061 USA. [Plotnick, Roy E.] Univ Illinois, Dept Earth & Environm Sci, Chicago, IL 60607 USA. [Rogers, Raymond R.] Macalester Coll, Dept Geol, St Paul, MN 55105 USA. RP Kosnik, MA (reprint author), Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. EM matthew.kosnik@mq.edu.au; john.alroy@mq.edu.au; behrensa@si.edu; franz.fuersich@gzn.uni-erlangen.de; ragastal@colby.edu; skidwell@uchicago.edu; michalk@vt.edu; plotnick@uic.edu; rogers@macalester.edu; wagnerpj@si.edu RI Kowalewski, Michal/B-4263-2008; Alroy, John/B-4585-2009; Kosnik, Matthew/G-2312-2010 OI Kowalewski, Michal/0000-0002-8575-4711; Kosnik, Matthew/0000-0001-5380-7041 FU National Science Foundation (NSF) Division of Environmental Biology [DEB-0083983]; NSF [DEB-94-21535]; University of California at Santa Barbara; State of California FX The authors constitute the Taphonomy/Paleoecology Working Group of the Paleobiology Database, and all members of the Working Group contributed critical amounts of thought, time, and effort to this paper. This research was supported by the National Science Foundation (NSF) Division of Environmental Biology (grant DEB-0083983). This paper resulted from a series of workshops conducted at NCEAS, a center funded by NSF (grant DEB-94-21535), the University of California at Santa Barbara, and the State of California. We are deeply indebted to D. Erwin, G. Hunt, and J. Pojeta for helpful discussions and guidance, as well as A. Tomasovych and an anonymous reviewer for insightful comments to the manuscript. S.M.K. thanks A. Nutzel, A. Kaim, and J. Harasewych for advice on gastropod mineralogy. M.A.K. thanks James Cook University, the Wilson foundation, and the Smithsonian Institution for post-doctoral support; J. Thompson, T. Waller, M. Florence and others for access to and assistance with museum collections; and H. Street for assistance with data collection. This is Paleobiology Database contribution 125. NR 115 TC 19 Z9 19 U1 3 U2 19 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SPR PY 2011 VL 37 IS 2 BP 303 EP 331 PG 29 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 744ZA UT WOS:000289132500008 ER PT J AU Barro, G Perez-Gonzalez, PG Gallego, J Ashby, MLN Kajisawa, M Miyazaki, S Villar, V Yamada, T Zamorano, J AF Barro, Guillermo Perez-Gonzalez, P. G. Gallego, J. Ashby, M. L. N. Kajisawa, M. Miyazaki, S. Villar, V. Yamada, T. Zamorano, J. TI UV-TO-FIR ANALYSIS OF SPITZER/IRAC SOURCES IN THE EXTENDED GROTH STRIP. I. MULTI-WAVELENGTH PHOTOMETRY AND SPECTRAL ENERGY DISTRIBUTIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: high-redshift; galaxies: photometry; galaxies: starburst; infrared: galaxies ID INFRARED ARRAY CAMERA; DEEP FIELD-SOUTH; STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; YALE-CHILE MUSYC; MASSIVE GALAXIES; SPACE-TELESCOPE; NUMBER COUNTS; HIGH-REDSHIFT; STELLAR MASS AB We present an IRAC 3.6+4.5 mu m selected catalog in the Extended Groth Strip (EGS) containing photometry from the ultraviolet to the far-infrared and stellar parameters derived from the analysis of the multi-wavelength data. In this paper, we describe the method used to build coherent spectral energy distributions (SEDs) for all the sources. In a forthcoming companion paper, we analyze those SEDs to obtain robust estimations of stellar parameters such as photometric redshifts, stellar masses, and star formation rates. The catalog comprises 76,936 sources with [3.6] <= 23.75 mag (85% completeness level of the IRAC survey in the EGS) over 0.48 deg(2). For approximately 16% of this sample, we are able to deconvolve the IRAC data to obtain robust fluxes for the multiple counterparts found in ground-based optical images. Typically, the SEDs of the IRAC sources in our catalog count with more than 15 photometric data points, spanning from the ultraviolet wavelengths probed by GALEX to the far-infrared observed by Spitzer, and going through ground-and space-based optical and near-infrared data taken with 2-8 m class telescopes. Approximately 95% and 90% of all IRAC sources are detected in the deepest optical and near-infrared bands. These fractions are reduced to 85% and 70% for S/N > 5 detections in each band. Only 10% of the sources in the catalog have optical spectroscopy and redshift estimations. Almost 20% and 2% of the sources are detected by MIPS at 24 and 70 mu m, respectively. We also cross-correlate our catalog with public X-ray and radio catalogs. Finally, we present the Rainbow Navigator public Web interface utility, designed to browse all the data products resulting from this work, including images, spectra, photometry, and stellar parameters. C1 [Barro, Guillermo; Perez-Gonzalez, P. G.; Gallego, J.; Villar, V.; Zamorano, J.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain. [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kajisawa, M.; Yamada, T.] Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan. [Miyazaki, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan. RP Barro, G (reprint author), Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain. RI Zamorano, Jaime/K-7706-2014; Perez-Gonzalez, Pablo/J-2871-2016 OI Zamorano, Jaime/0000-0002-8993-5894; Perez-Gonzalez, Pablo/0000-0003-4528-5639 FU Spanish Programa Nacional de Astronomia y Astrofisica [AYA2009-10368]; Spanish Government; European Union; Spanish MICINN [CSD2006-00070]; NASA [1255094, 1407] FX We acknowledge support from the Spanish Programa Nacional de Astronomia y Astrofisica under grant AYA2009-10368. P. G. P.-G. acknowledges support from the Ramon y Cajal Program financed by the Spanish Government and the European Union. Partially funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. Support was also provided by NASA through contract no. 1255094 issued by JPL/Caltech. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, Caltech under NASA contract 1407. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. GALEX is a NASA Small Explorer launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation, and scientific analysis of the GALEX mission. 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. Based in part on data collected at Subaru Telescope and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. NR 66 TC 54 Z9 54 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 MAR PY 2011 VL 193 IS 1 DI 10.1088/0067-0049/193/1/13 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZF UT WOS:000289059000013 ER PT J AU Manoj, P Kim, KH Furlan, E McClure, MK Luhman, KL Watson, DM Espaillat, C Calvet, N Najita, JR D'Alessio, P Adame, L Sargent, BA Forrest, WJ Bohac, C Green, JD Arnold, LA AF Manoj, P. Kim, K. H. Furlan, E. McClure, M. K. Luhman, K. L. Watson, Dan M. Espaillat, C. Calvet, N. Najita, J. R. D'Alessio, P. Adame, L. Sargent, B. A. Forrest, W. J. Bohac, C. Green, J. D. Arnold, L. A. TI SPITZER INFRARED SPECTROGRAPH SURVEY OF YOUNG STARS IN THE CHAMAELEON I STAR-FORMING REGION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; infrared: stars; protoplanetary disks; stars: pre-main sequence ID T-TAURI STARS; MAIN-SEQUENCE STARS; LOW-MASS STARS; SPECTRAL ENERGY-DISTRIBUTIONS; NEARBY MOLECULAR CLOUDS; HERBIG AE/BE SYSTEMS; BROWN DWARF DISKS; ALL-SKY SURVEY; PROTOPLANETARY DISKS; GRAIN-GROWTH AB We present 5-36 mu m mid-infrared spectra of 82 young stars in the similar to 2 Myr old Chamaeleon I star-forming region, obtained with the Spitzer Infrared Spectrograph (IRS). We have classified these objects into various evolutionary classes based on their spectral energy distributions and the spectral features seen in the IRS spectra. We have analyzed the mid-IR spectra of Class II objects in Chamaeleon I in detail, in order to study the vertical and radial structure of the protoplanetary disks surrounding these stars. We find evidence for substantial dust settling in most protoplanetary disks in Chamaeleon I. We have identified several disks with altered radial structures in Chamaeleon I, among them transitional disk candidates which have holes or gaps in their disks. Analysis of the silicate emission features in the IRS spectra of Class II objects in Cha I shows that the dust grains in these disks have undergone significant processing (grain growth and crystallization). However, disks with radial holes/gaps appear to have relatively unprocessed grains. We further find the crystalline dust content in the inner (less than or similar to 1-2 AU) and the intermediate (less than or similar to 10 AU) regions of the protoplanetary disks to be tightly correlated. We also investigate the effects of accretion and stellar multiplicity on the disk structure and dust properties. Finally, we compare the observed properties of protoplanetary disks in Cha I with those in slightly younger Taurus and Ophiuchus regions and discuss the effects of disk evolution in the first 1-2 Myr. C1 [Manoj, P.; Kim, K. H.; Watson, Dan M.; Forrest, W. J.; Bohac, C.; Arnold, L. A.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Furlan, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [McClure, M. K.; Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Luhman, K. L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Luhman, K. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Espaillat, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Najita, J. R.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [D'Alessio, P.; Adame, L.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Sargent, B. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Green, J. D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Manoj, P (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. EM manoj@pas.rochester.edu OI McClure, Melissa/0000-0003-1878-327X; Adame, Lucia/0000-0002-6328-6099; Furlan, Elise/0000-0001-9800-6248 FU NASA [1407, 1257184]; JPL/Caltech, JPL [960803]; Cornell [31419-5714]; National Science Foundation [AST-0544588, 0901947]; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; PAPIIT-UNAM, Mexico FX 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 (Caltech), under NASA contract 1407. Support for this work was provided by NASA through contract no. 1257184 issued by JPL/Caltech, JPL contract 960803 to Cornell University, and Cornell subcontracts 31419-5714 to the University of Rochester. E. F. was partly supported by a NASA Postdoctoral Program Fellowship, administered by Oak Ridge Associated Universities through a contract with NASA, and partly supported by NASA through the Spitzer Space Telescope Fellowship Program, through a contract issued by JPL/Caltech under a contract with NASA. 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. C. E. was supported by the National Science Foundation under Award No. 0901947. P. D. acknowledges a grant from PAPIIT-UNAM, Mexico. This publication makes use of the SIMBAD and VizieR databases, operated at CDS (Strasbourg, France) and NASA's Astrophysics Data System Abstract Service. NR 131 TC 35 Z9 35 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 MAR PY 2011 VL 193 IS 1 DI 10.1088/0067-0049/193/1/11 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZF UT WOS:000289059000011 ER PT J AU Patel, NA Young, KH Gottlieb, CA Thaddeus, P Wilson, RW Menten, KM Reid, MJ McCarthy, MC Cernicharo, J He, JH Bruenken, S Trung, DV Keto, E AF Patel, Nimesh A. Young, Ken H. Gottlieb, Carl A. Thaddeus, Patrick Wilson, Robert W. Menten, Karl M. Reid, Mark J. McCarthy, Michael C. Cernicharo, Jose He, Jinhua Bruenken, Sandra Dinh-V. Trung Keto, Eric TI AN INTERFEROMETRIC SPECTRAL-LINE SURVEY OF IRC+10216 IN THE 345 GHz BAND SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrochemistry; line: identification; stars: AGB and post-AGB; stars: individual (IRC+10216, CW Leo); surveys ID GIANT BRANCH STARS; SUBMILLIMETER OBSERVATIONS; CIRCUMSTELLAR ENVELOPE; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; EVOLVED STARS; CARBON STAR; IRC +10216; EMISSION; MILLIMETER AB We report a spectral-line survey of the extreme carbon star IRC+10216 carried out between 293.9 and 354.8 GHz with the Submillimeter Array. A total of 442 lines were detected, more than 200 for the first time; 149 are unassigned. Maps at an angular resolution of similar to 3 '' were obtained for each line. A substantial new population of narrow lines with an expansion velocity of similar to 4 km s(-1) (i.e., approximate to 30% of the terminal velocity) was detected. Most of these are attributed to rotational transitions within vibrationally excited states, emitted from energy levels above the v = 0, J = 0 ground state with excitation energy of 1000-3000 K. Emission from these lines appears to be centered on the star with an angular extent of < 1 ''. We use multiple transitions detected in several molecules to derive physical conditions in this inner envelope of IRC+10216. C1 [Patel, Nimesh A.; Young, Ken H.; Gottlieb, Carl A.; Thaddeus, Patrick; Wilson, Robert W.; Reid, Mark J.; McCarthy, Michael C.; Keto, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, Karl M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Cernicharo, Jose] INTA CSIC, Lab Mol Astrophys, Dept Astrophys, CAB, Madrid 28850, Spain. [He, Jinhua] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China. [Bruenken, Sandra] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Dinh-V. Trung] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Patel, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM npatel@cfa.harvard.edu RI Brunken, Sandra/B-1880-2010; OI Brunken, Sandra/0000-0001-7175-4828; Wilson, Robert/0000-0001-5694-6725; McCarthy, Michael/0000-0001-9142-0008 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 41 TC 28 Z9 28 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 MAR PY 2011 VL 193 IS 1 DI 10.1088/0067-0049/193/1/17 PG 65 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 743ZF UT WOS:000289059000017 ER PT J AU Okamoto-Barth, S Moore, C Barth, J Subiaul, F Povinelli, DJ AF Okamoto-Barth, Sanae Moore, Chris Barth, Jochen Subiaul, Francys Povinelli, Daniel J. TI Carryover effect of joint attention to repeated events in chimpanzees and young children SO DEVELOPMENTAL SCIENCE LA English DT Article ID PAN-TROGLODYTES; VISUAL-ATTENTION; FOLLOW GAZE; SPECIES FOLLOW; HUMAN INFANTS; GREAT APES; COMMUNICATION; INDIVIDUALS; TROGIODYTES; MECHANISM AB Gaze following is a fundamental component of triadic social interaction which includes events and an object shared with other individuals and is found in both human and nonhuman primates. Most previous work has focused only on the immediate reaction after following another's gaze. In contrast, this study investigated whether gaze following is retained after the observation of the other's gaze shift, whether this retainment differs between species and age groups, and whether the retainment depends on the nature of the preceding events. In the social condition, subjects (1- and 2-year-old human children and chimpanzees) witnessed an experimenter who looked and pointed in the direction of a target lamp. In the physical condition, the target lamp blinked but the experimenter did not provide any cues. After a brief delay, we presented the same stimulus again without any cues. All subjects looked again to the target location after experiencing the social condition and thus showed a carryover effect. However, only 2-year-olds showed a carryover effect in the physical condition; 1-year-olds and chimpanzees did not. Additionally, only human children showed spontaneous interactive actions such as pointing. Our results suggest that the difference between the two age groups and chimpanzees is conceptual and not only quantitative. C1 [Okamoto-Barth, Sanae] Maastricht Univ, Fac Psychol & Neurosci, Dept Cognit Neurosci, NL-6200 MD Maastricht, Netherlands. [Okamoto-Barth, Sanae] Maastricht Univ, Dept Econ, NL-6200 MD Maastricht, Netherlands. [Moore, Chris] Dalhousie Univ, Dept Psychol, Halifax, NS B3H 3J5, Canada. [Subiaul, Francys] George Washington Univ, Dept Speech & Hearing Sci, Washington, DC 20052 USA. [Subiaul, Francys] Smithsonian Natl Zool Pk, Ape Mind Initiat, Washington, DC USA. RP Okamoto-Barth, S (reprint author), Maastricht Univ, Fac Psychol & Neurosci, Dept Cognit Neurosci, POB 616, NL-6200 MD Maastricht, Netherlands. EM s.barth@maastrichtuniversity.nl NR 38 TC 4 Z9 4 U1 0 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1363-755X J9 DEVELOPMENTAL SCI JI Dev. Sci. PD MAR PY 2011 VL 14 IS 2 BP 440 EP 452 DI 10.1111/j.1467-7687.2010.00996.x PG 13 WC Psychology, Developmental; Psychology, Experimental SC Psychology GA 723EQ UT WOS:000287489500028 PM 22213912 ER PT J AU Tani, K Fiske, RS Dunkley, DJ Ishizuka, O Oikawa, T Isobe, I Tatsumi, Y AF Tani, Kenichiro Fiske, Richard S. Dunkley, Daniel J. Ishizuka, Osamu Oikawa, Teruki Isobe, Ichiyo Tatsumi, Yoshiyuki TI The Izu Peninsula, Japan: Zircon geochronology reveals a record of intra-oceanic rear-arc magmatism in an accreted block of Izu-Bonin upper crust SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE zircon U-Pb ages; Izu Peninsula; Izu-Bonin arc; rear-arc; upper crust development ID TANZAWA PLUTONIC COMPLEX; PRECISION PB ISOTOPES; SHIRAHAMA GROUP; COLLISION-ZONE; MARIANA ARC; GEOCHEMICAL TRENDS; PYROCLASTIC DEBRIS; CONTINENTAL-CRUST; CONSTRAINTS; EVOLUTION AB The Izu Peninsula, central Japan, is situated in a zone where the active intra-oceanic Izu-Bonin arc has been colliding end-on with the mainland Honshu arc for the past 15 million years. As a result of this arc-arc collision, parts of the submarine Izu-Bonin upper crustal sequences have been accreted and uplifted to form the Izu Peninsula, exposing seafloor volcaniclastic deposits, associated lava flows, and coeval intrusive bodies. Parts of this sequence have been subjected to extensive hydrothermal alteration, and these altered rocks have previously been interpreted as representative of hypothetical widespread Middle Miocene basement that presumably underlay northern Izu-Bonin arc volcanoes. New zircon U-Pb ages presented here, however, show that both fresh and altered volcanic sequences exposed in Izu Peninsula are broadly contemporaneous and were products of the same Late Miocene to Pleistocene magmatism. Geochemical characteristics of these sequences show them to have formed in the Izu-Bonin rear-arc environment, providing an unusual opportunity to investigate in detail the growth and architecture of a rear-arc region in an active intra-oceanic arc. Moreover, zircon ages from altered basal units of Kozushima and Niijima. Quaternary volcanic islands in the northern Izu-Bonin rear-arc, show that these islands rest on units only slightly older (< 1 Ma) than the main body of these subaerial edifices, not, as previously believed, part of a regional older Miocene basement. The near-continuum growth of these arc volcanoes and their underlying successions, plus the absence of a distinctly older basement underlying the Izu Peninsula and northern Izu-Bonin arc, provide new insight into upper crust development in an intra-oceanic, convergent margin environment. (C) 2011 Elsevier B.V. All rights reserved. C1 [Tani, Kenichiro; Ishizuka, Osamu; Tatsumi, Yoshiyuki] Japan Agcy Marine Earth Sci & Technol, Inst Res Earth Evolut, Yokosuka, Kanagawa 2370061, Japan. [Fiske, Richard S.] Smithsonian Inst MRC 119, Washington, DC 20013 USA. [Dunkley, Daniel J.] Natl Inst Polar Res, Tokyo 1908518, Japan. [Ishizuka, Osamu; Oikawa, Teruki] Geol Survey Japan AIST, Inst Geol & Geoinformat, Higashi Ku, Tsukuba, Ibaraki 3058567, Japan. [Isobe, Ichiyo] Niijimamura Museum, Tokyo 1000402, Japan. RP Tani, K (reprint author), Japan Agcy Marine Earth Sci & Technol, Inst Res Earth Evolut, 2-15 Natsushimacho, Yokosuka, Kanagawa 2370061, Japan. EM kentani@jamstec.go.jp OI Tani, Kenichiro/0000-0003-3374-8608 NR 61 TC 11 Z9 11 U1 1 U2 10 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 MAR 1 PY 2011 VL 303 IS 3-4 BP 225 EP 239 DI 10.1016/j.epsl.2010.12.052 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 741RM UT WOS:000288881900007 ER PT J AU Christy, JS AF Christy, J. S. TI Timing of hatching in Brachyuran crabs: patterns and control SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2011 CL Salt Lake City, UT SP Soc Integrat & Comparat Biol C1 [Christy, J. S.] Smithsonian Trop Res Inst, Panama City, Panama. EM christyj@si.edu NR 0 TC 0 Z9 0 U1 1 U2 2 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 MAR PY 2011 VL 51 SU 1 BP E23 EP E23 PG 1 WC Zoology SC Zoology GA 733QP UT WOS:000288278100539 ER PT J AU Cohen, KL Seid, MA Rouben, CM Warkentin, KM AF Cohen, K. L. Seid, M. A. Rouben, C. M. Warkentin, K. M. TI The mechanism of rapid, plastic hatching in red-eyed treefrogs, Agalychnis callidryas SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2011 CL Salt Lake City, UT SP Soc Integrat & Comparat Biol C1 Boston Univ, Smithsonain Trop Res Inst, Boston, MA 02215 USA. Boston Univ, Smithsonian Trop Res Inst, Boston, MA 02215 USA. EM kcohen@bu.edu NR 0 TC 0 Z9 0 U1 2 U2 3 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 MAR PY 2011 VL 51 SU 1 BP E176 EP E176 PG 1 WC Zoology SC Zoology GA 733QP UT WOS:000288278100077 ER PT J AU Danner, RM Greenberg, R Walters, JR AF Danner, R. M. Greenberg, R. Walters, J. R. TI Winter food limits the body condition, survival, and molt of a migratory sparrow SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2011 CL Salt Lake City, UT SP Soc Integrat & Comparat Biol C1 [Danner, R. M.; Greenberg, R.; Walters, J. R.] Virginia Tech, Smithsonian Migratory Bird Ctr, Blacksburg, VA 24061 USA. EM rdanner@vt.edu RI Danner, Raymond/J-8350-2013 OI Danner, Raymond/0000-0002-3999-8141 NR 0 TC 0 Z9 0 U1 0 U2 2 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 MAR PY 2011 VL 51 SU 1 BP E180 EP E180 PG 1 WC Zoology SC Zoology GA 733QP UT WOS:000288278100093 ER PT J AU Farina, SC Song, J AF Farina, S. C. Song, J. TI Lateral line anatomy in deep-water benthic anglerfish, Chaunax suttkusi SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2011 CL Salt Lake City, UT SP Soc Integrat & Comparat Biol C1 [Farina, S. C.; Song, J.] Cornell Univ, Smithsonian Natl Museum Nat Hist, Ithaca, NY 14853 USA. EM stacy.farina@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 5 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 MAR PY 2011 VL 51 SU 1 BP E188 EP E188 PG 1 WC Zoology SC Zoology GA 733QP UT WOS:000288278100125 ER PT J AU Hopkins, WA Durant, SE Moser, WE AF Hopkins, W. A. Durant, S. E. Moser, W. E. TI Ectoparasitism, Innate Immunity, and Stress Physiology of Eastern Hellbenders (Cryptobranchus alleganiensis) from Stream Reaches with Differing Habitat Quality SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2011 CL Salt Lake City, UT SP Soc Integrat & Comparat Biol C1 Smithsonian Inst, Washington, DC 20560 USA. EM hopkinsw@vt.edu NR 0 TC 0 Z9 0 U1 4 U2 16 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 MAR PY 2011 VL 51 SU 1 BP E59 EP E59 PG 1 WC Zoology SC Zoology GA 733QP UT WOS:000288278100681 ER PT J AU Lessios, H AF Lessios, Harilaos TI What have DNA molecules told us about speciation in the sea? SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2011 CL Salt Lake City, UT SP Soc Integrat & Comparat Biol C1 [Lessios, Harilaos] Smithsonian Trop Res Inst, Panama City, Panama. EM Lessiosh@post.harvard.edu NR 0 TC 0 Z9 0 U1 0 U2 4 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 MAR PY 2011 VL 51 SU 1 BP E80 EP E80 PG 1 WC Zoology SC Zoology GA 733QP UT WOS:000288278101009 ER PT J AU Puebla, O Guichard, F Bermingham, E AF Puebla, Oscar Guichard, Frederic Bermingham, Eldredge TI Pairing dynamics and the origin of species SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2011 CL Salt Lake City, UT SP Soc Integrat & Comparat Biol C1 McGill Univ, Montreal, PQ H3A 2T5, Canada. Smithsonian Trop Res Inst, Panama City, Panama. EM oscar.puebla@mail.mcgill.ca RI Guichard, Frederic/B-6188-2015 OI Guichard, Frederic/0000-0002-7369-482X NR 0 TC 0 Z9 0 U1 0 U2 4 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 MAR PY 2011 VL 51 SU 1 BP E112 EP E112 PG 1 WC Zoology SC Zoology GA 733QP UT WOS:000288278101140 ER PT J AU Seaver, EC Boyle, MJ Meyer, NP AF Seaver, Elaine C. Boyle, Michael J. Meyer, Neva P. TI Evolution of the annelid body plan: developmental insights from the unsegmented sipunculan worm Themiste lageniformis SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2011 CL Salt Lake City, UT SP Soc Integrat & Comparat Biol C1 Univ Hawaii, Honolulu, HI 96822 USA. Smithsonian Marine Stn, Ft Pierce, FL USA. EM seaver@hawaii.edu NR 0 TC 0 Z9 0 U1 0 U2 1 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 MAR PY 2011 VL 51 SU 1 BP E125 EP E125 PG 1 WC Zoology SC Zoology GA 733QP UT WOS:000288278101191 ER PT J AU Williams, CK Marra, PP Ezenwa, VO Breuner, CW AF Williams, C. K. Marra, P. P. Ezenwa, V. O. Breuner, C. W. TI Parasite release in an urban colonizer SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2011 CL Salt Lake City, UT SP Soc Integrat & Comparat Biol C1 Univ Montana, Smithsonian Migratory Bird Ctr, Missoula, MT 59812 USA. Univ Georgia, Athens, GA 30602 USA. EM williams@umontana.edu NR 0 TC 0 Z9 0 U1 0 U2 2 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 MAR PY 2011 VL 51 SU 1 BP E151 EP E151 PG 1 WC Zoology SC Zoology GA 733QP UT WOS:000288278101294 ER PT J AU Mejia, LC Castlebury, LA Rossman, AY Sogonov, MV White, JF AF Mejia, L. C. Castlebury, L. A. Rossman, A. Y. Sogonov, M. V. White, J. F., Jr. TI A systematic account of the genus Plagiostoma (Gnomoniaceae, Diaporthales) based on morphology, host-associations, and a four-gene phylogeny SO STUDIES IN MYCOLOGY LA English DT Article DE Ascomycota; Betulaceae; epitypification; Fraxinus; new species; phylogeny; Salicaceae; Sordariomycetidae ID DISCULA-FRAXINEA; SP-NOV; ASH; FUNGUS AB Members of the genus Plagiostoma inhabit leaves, stems, twigs, and branches of woody and herbaceous plants predominantly in the temperate Northern Hemisphere. An account of all known species of Plagiostoma including Cryptodiaporthe is presented based on analyses of morphological, cultural, and DNA sequence data. Multigene phylogenetic analyses of DNA sequences from four genes (beta-tubulin, ITS, rpb2, and tef1-alpha) revealed eight previously undescribed phylogenetic species and an association between a clade composed of 11 species of Plagiostoma and the host family Salicaceae. In this paper these eight new species of Plagiostoma are described, four species are redescribed, and four new combinations are proposed. A key to the 25 accepted species of Plagiostoma based on host, shape, and size of perithecia, perithecial arrangement in the host, and microscopic characteristics of the asci and ascospores is provided. Disposition of additional names in Cryptodiaporthe and Plagiostoma is also discussed. C1 [Mejia, L. C.; Castlebury, L. A.; Rossman, A. Y.] ARS, Systemat Mycol & Microbiol Lab, USDA, Beltsville, MD 20705 USA. [Mejia, L. C.; White, J. F., Jr.] Rutgers State Univ, Dept Plant Biol & Pathol, New Brunswick, NJ 08901 USA. [Mejia, L. C.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Sogonov, M. V.] EMSL Analytical Inc, Beltsville, MD 20705 USA. RP Mejia, LC (reprint author), ARS, Systemat Mycol & Microbiol Lab, USDA, Rm 304,B010A,10300 Baltimore Ave, Beltsville, MD 20705 USA. EM MejiaLC@si.edu FU National Science Foundation [NSF 03-28364]; LCM through Rutgers University, New Brunswick, NJ; Neyra Fund; Department of Plant Biology and Pathology; Mycological Society of America FX This work was funded by the National Science Foundation Partnerships for Enhancing Expertise in Taxonomy (NSF 03-28364). Additional funding for field work by LCM was received through Rutgers University, New Brunswick, NJ, from the Neyra Fund, the Spencer Davis Research Award from the Department of Plant Biology and Pathology, A Special Study Support Award, and a Graduate School Travel Award and through the Backus Award from the Mycological Society of America. Much appreciation is extended to Lena Struwe for her valuable comments and insights during the course of this work. We acknowledge and appreciate Andrew Minnis for providing a specimen from which the new species Plagiostoma ovalisporum was described and for nomenclatural advice. Christian Feuillet kindly provided translations of the diagnoses into Latin. Tunesha Phipps and Sasha Allen are sincerely acknowledged for their technical expertise in the molecular laboratory. LCM appreciates the following people for graciously hosting visits for collecting and facilitating the shipment of specimens: Michael Giraurd, Adriana Hladki, Tina Hoffman, Christian Lethal, Christophe Lecuru, and Ralph Mangelsdorff. Special thanks to Zhu LiangYang for hosting LCM and providing superb logistical support during his collecting trip in China. NR 36 TC 17 Z9 17 U1 0 U2 4 PU CENTRAALBUREAU SCHIMMELCULTURE PI UTRECHT PA PO BOX 85167, 3508 AD UTRECHT, NETHERLANDS SN 0166-0616 EI 1872-9797 J9 STUD MYCOL JI Stud. Mycol. PD MAR PY 2011 IS 68 BP 211 EP 235 DI 10.3114/sim.2011.68.10 PG 25 WC Mycology SC Mycology GA 741AA UT WOS:000288834300011 PM 21523196 ER PT J AU Dell'Agnello, S Delle Monache, GO Currie, DG Vittori, R Cantone, C Garattini, M Boni, A Martini, M Lops, C Intaglietta, N Tauraso, R Arnold, DA Pearlman, MR Bianco, G Zerbini, S Maiello, M Berardi, S Porcelli, L Alley, CO McGarry, JF Sciarretta, C Luceri, V Zagwodzki, TW AF Dell'Agnello, S. Delle Monache, G. O. Currie, D. G. Vittori, R. Cantone, C. Garattini, M. Boni, A. Martini, M. Lops, C. Intaglietta, N. Tauraso, R. Arnold, D. A. Pearlman, M. R. Bianco, G. Zerbini, S. Maiello, M. Berardi, S. Porcelli, L. Alley, C. O. McGarry, J. F. Sciarretta, C. Luceri, V. Zagwodzki, T. W. TI Creation of the new industry-standard space test of laser retroreflectors for the GNSS and LAGEOS SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Galileo; GPS; SLR; New space test; Laser retroreflectors; Industry-standard; LAGEOS ID INTERNATIONAL GLONASS EXPERIMENT; SERVICE; PROSPECTS; GEODESY AB We built a new experimental apparatus (the "Satellite/lunar laser ranging Characterization Facility", SCF) and created a new test procedure (the SCF-Test) to characterize and model the detailed thermal behavior and the optical performance of cube corner laser retroreflectors in space for industrial and scientific applications. The primary goal of these innovative tools is to provide critical design and diagnostic capabilities for Satellites Laser Ranging (SLR) to Galileo and other GNSS (Global Navigation Satellite System) constellations. The capability will allow us to optimize the design of GNSS laser retroreflector payloads to maximize ranging efficiency, to improve signal-to-noise conditions in daylight and to provide pre-launch validation of retroreflector performance under laboratory-simulated space conditions. Implementation of new retroreflector designs being studied will help to improve GNSS orbits, which will then increase the accuracy, stability, and distribution of the International Terrestrial Reference Frame (ITRF), to provide better definition of the geocenter (origin) and the scale (length unit). Our key experimental innovation is the concurrent measurement and modeling of the optical Far Field Diffraction Pattern (FFDP) and the temperature distribution of the SLR retroreflector payload under thermal conditions produced with a close-match solar simulator. The apparatus includes infrared cameras for non-invasive thermometry, thermal control and real-time movement of the payload to experimentally simulate satellite orientation on orbit with respect to both solar illumination and laser interrogation beams. These unique capabilities provide experimental validation of the space segment for SLR and Lunar Laser Ranging (LLR). We used the SCF facility and the SCF-Test to perform a comprehensive, non-invasive space characterization of older generation, back-coated retroreflectors of the GIOVE-A and -B (Galileo In-Orbit Validation Elements) and the GPS-35 and -36 designs. First, using a full GPS flight model at laser wavelengths of 532 and 632 nm, we found its "effective optical cross section" in air, under isothermal conditions, to be six times lower than the Retrorefiector Standard for GNSS satellites (100 x 10(6) m(2) at 20,000 km altitude for GPS and 180 x 10(6) m(2) for Galileo at 23,200 km altitude), issued by the International Laser Ranging Service (ILRS). Under the simulated thermal and space conditions of the SCF, we also showed that in some space configurations the "effective optical cross section" is further reduced, by the thermal degradation of the FFDP. Using the same SCF-Test configuration on an individual GIOVE prototype cube, we measured severe thermal degradation in optical performance, which appears to be caused by the retroreflector metal coating and the non-optimized thermal conductance of the mounting. Uncoated retroreflectors with proper mounting can minimize thermal degradation and significantly increase the optical performance, and as such, are emerging as the recommended design for modern GNSS satellites. The COMPASS-MI, GLONASS-115 GNSS satellites use uncoated cubes. They provide better efficiency than those on GPS and GIOVE, including better daylight ranging performance. However, these retroreflectors were not characterized in the laboratory under space conditions prior to launch, so we have no basis to evaluate how well they were optimized for future GNSS satellites. SCF-Testing, under a non-disclosure agreement between INFN-LNF and the European Space Agency (ESA), of prototype uncoated cubes for the first four Galileo satellites to be launched (named "IOV", In-Orbit Validation satellites) is a major step forward. An SCF-Test performed on a LAGEOS (LAser GEOdynamics Satellite) engineering model retroreflector array provided by NASA, showed the good space performance on what is now a reference ILRS payload standard. The IOV and LAGEOS measurements demonstrated the effectiveness of the SCF-Test as an LRA diagnostic, optimization and validation tool in use by NASA, ESA and ASI. (C) 2010 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Dell'Agnello, S.; Delle Monache, G. O.; Cantone, C.; Garattini, M.; Boni, A.; Martini, M.; Lops, C.; Intaglietta, N.; Tauraso, R.; Maiello, M.; Berardi, S.; Porcelli, L.] Ist Nazl Fis Nucl, Lab Nazl Frascati, I-00044 Rome, Italy. [Currie, D. G.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Vittori, R.] Aeronaut Mil Italiana, I-00185 Rome, Italy. [Vittori, R.] ASI, I-00198 Rome, Italy. [Tauraso, R.] Univ Roma Tor Vergata, Dipartimento Matemat, I-00133 Rome, Italy. [Arnold, D. A.; Pearlman, M. R.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Bianco, G.; Sciarretta, C.; Luceri, V.] Ctr Geodesia Spaziale G Colombo ASI CGS, ASI, I-75100 Matera, Italy. [Zerbini, S.] Univ Bologna, Dept Phys, Sector Geophys, I-40127 Bologna, Italy. [McGarry, J. F.; Zagwodzki, T. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Dell'Agnello, S (reprint author), Ist Nazl Fis Nucl, Lab Nazl Frascati, Via E Fermi 40, I-00044 Rome, Italy. EM Simone.DellAgnello@lnf.infn.it OI Bianco, Giuseppe/0000-0002-4538-6467; Tauraso, Roberto/0000-0002-5619-3513; Martini, Manuele/0000-0001-6508-2930 NR 23 TC 17 Z9 17 U1 0 U2 12 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 MAR 1 PY 2011 VL 47 IS 5 BP 822 EP 842 DI 10.1016/j.asr.2010.10.022 PG 21 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 737SS UT WOS:000288589100006 ER PT J AU Robinson, H Funk, VA AF Robinson, Harold Funk, V. A. TI Stephanbeckia plumosa (Liabeae: Compositae): A new genus and species from southern Bolivia SO BRITTONIA LA English DT Article DE Asteraceae; new genus; southern Bolivia; Liabeae ID ASTERACEAE; ANDES AB Material from southern Bolivia, recently collected by Stephan Beck, is described as a new genus and species, Stephanbeckia plumosa (Compositae: Liabeae). Both morphological and molecular data place the genus in the broadly interpreted subtribe Paranepheliinae, but clearly distinct from other members. It differs morphologically by its small size, deciduous plumose pappus, lack of paleae, and compressed bicostate achenes. A key to the genera of the Liabeae is provided. C1 [Robinson, Harold; Funk, V. A.] Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, Washington, DC 20013 USA. RP Robinson, H (reprint author), Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, POB 37012, Washington, DC 20013 USA. EM robinsoh@si.edu; funkv@si.edu NR 33 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD MAR PY 2011 VL 63 IS 1 BP 75 EP 82 DI 10.1007/s12228-010-9136-2 PG 8 WC Plant Sciences SC Plant Sciences GA 738SK UT WOS:000288662200009 ER PT J AU Clark, JL Skog, LE AF Clark, John L. Skog, Laurence E. TI Novae Gesneriaceae Neotropicarum XVI: Cremosperma anisophyllum, a new species of Gesneriaceae from the Choco region of northern Ecuador and southern Colombia SO BRITTONIA LA English DT Article DE Beslerieae; Choco; Cremosperma; Ecuador; Gesneriaceae AB A new species of Cremosperma (Gesneriaceae, tribe Beslerieae) is described from the Choc floristic region of the western Andean slopes of northern Ecuador and southern Colombia. The dorsiventral shoots and strongly anisophyllous leaves differentiate Cremosperma anisophyllum from all other congeners. 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. RP Clark, JL (reprint author), Univ Alabama, Dept Biol Sci, Box 870345, Tuscaloosa, AL 35487 USA. EM jlc@ua.edu; skogl@si.edu FU Gesneriad Society; National Science Foundation [DEB 0841958]; Fulbright Graduate Study and Research Abroad Fellowship FX Support for this study was provided by The Gesneriad Society and the National Science Foundation (DEB 0841958). Fieldwork in 2003 was conducted while the first author was supported by a Fulbright Graduate Study and Research Abroad Fellowship. We are grateful to Alice Tangerini for preparing the illustration of the new species; to William Anderson (MICH) for providing the Latin diagnosis; and to Silvana Marten-Rodriguez (USJ) for the Spanish translation of the abstract. Herbaria MO, QCNE, and SEL are acknowledged for making their collections available to us. We thank John R. Clark (SEL) and Christian Feuillet (US) for providing helpful reviews and input to the manuscript. NR 16 TC 1 Z9 3 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD MAR PY 2011 VL 63 IS 1 BP 133 EP 138 DI 10.1007/s12228-010-9147-z PG 6 WC Plant Sciences SC Plant Sciences GA 738SK UT WOS:000288662200016 ER PT J AU del Hoyo-Melendez, JM Mecklenburg, MF Domenech-Carbo, MT AF del Hoyo-Melendez, Julio M. Mecklenburg, Marion F. Teresa Domenech-Carbo, Mara TI An evaluation of daylight distribution as an initial preventive conservation measure at two Smithsonian Institution Museums, Washington DC, USA SO JOURNAL OF CULTURAL HERITAGE LA English DT Article DE Illuminance measurements; Natural lighting; Data logging; Museum environment; Smithsonian American Art Museum; National Portrait Gallery AB This paper presents the results of a light levels survey conducted at the Donald W. Reynolds Center for American Art and Portraiture in Washington DC. The museum space is shared by the National Portrait Gallery and the Smithsonian American Art Museum. After six years of extensive renovations, the building reopened to the public in July 1, 2006. The structure was not originally designed to house a museum collection since it contains numerous openings such as windows, doors and skylights, which provide a path for natural radiation to enter the building and come in contact with the artworks. From a preventive conservation standpoint, this is an important problem since sensitive works of art in the collection may be subjected to damage caused by light exposure. Environmental data loggers installed throughout the museum were programmed to take successive measurements every 10 min for 24 h a day, 7 days a week and 52 weeks a year. This light levels assessment started in November 1, 2007 and finished in October 31, 2008. This study presents a new method for determining natural radiation exposures registered in exhibition spaces that rely on both electric lighting and natural lighting, considering the growing trend of using daylight illumination in museums. (C) 2010 Elsevier Masson SAS. All rights reserved. C1 [del Hoyo-Melendez, Julio M.; Mecklenburg, Marion F.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [del Hoyo-Melendez, Julio M.; Teresa Domenech-Carbo, Mara] Univ Politecn Valencia, Inst Univ Restaurac Patrimonio, Valencia Espana 46022, Spain. RP del Hoyo-Melendez, JM (reprint author), Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM judeho1@doctor.upv.es; mecklenburgm@si.edu; tdomenec@crbc.upv.es RI del Hoyo-Melendez, Julio/B-1395-2012 OI del Hoyo-Melendez, Julio/0000-0003-2163-2149 FU Smithsonian's Collections Care Pool Fund; Smithsonian Institution Office of Research and Training Services; Smithsonian American Art Museum; National Portrait Gallery; Museum Conservation Institute FX This research was supported by the Smithsonian's Collections Care Pool Fund, administered by the Smithsonian Collections Advisory Committee and through a predoctoral fellowship from the Smithsonian Institution Office of Research and Training Services. The work was jointly sponsored by the Smithsonian American Art Museum, the National Portrait Gallery and the Museum Conservation Institute. The authors would like to express their gratitude to staff from both museums for all their support, valuable discussions and recommendations concerning this work. NR 24 TC 5 Z9 5 U1 0 U2 12 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1296-2074 J9 J CULT HERIT JI J. Cult. Herit. PD MAR PY 2011 VL 12 IS 1 BP 54 EP 64 DI 10.1016/j.culher.2010.05.003 PG 11 WC Archaeology; Art; Chemistry, Analytical; Geosciences, Multidisciplinary; Materials Science, Multidisciplinary; Spectroscopy SC Archaeology; Art; Chemistry; Geology; Materials Science; Spectroscopy GA 722ZK UT WOS:000287474500007 ER PT J AU Schmidt, DA Barbiers, RB Ellersieck, MR Ball, RL Koutsos, EA Griffin, ME Grobler, D Citino, SB Bush, M AF Schmidt, Debra A. Barbiers, Robyn B. Ellersieck, Mark R. Ball, Ray L. Koutsos, Elizabeth A. Griffin, Mark E. Grobler, Douw Citino, Scott B. Bush, Mitchell TI SERUM CHEMISTRY COMPARISONS BETWEEN CAPTIVE AND FREE-RANGING GIRAFFES (GIRAFFA CAMELOPARDALIS) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Giraffe; Giraffa camelopardalis; glucose; serum chemistry; bilirubin; alanine aminotransferase ID BIGHORN SHEEP; AMINO-ACIDS; FATTY-ACIDS; LIPOPROTEINS; CANADENSIS; HEMATOLOGY; PARAMETERS; MORTALITY; ACIDOSIS; MINERALS AB Serum chemistry analyses were compared between captive and free-ranging giraffes (Giraffa camelopardalis) in an attempt to better understand some of the medical issues seen with captive giraffes. Illnesses, including peracute mortality, energy malnutrition, pancreatic disease, urolithiasis, hoof disease, and severe intestinal parasitism, may be related to zoo nutrition and management issues. Serum samples were collected from 20 captive giraffes at 10 United States institutions. Thirteen of the captive animal samples were collected from animals trained for blood collection; seven were banked samples obtained from a previous serum collection. These samples were compared with serum samples collected from 24 free-ranging giraffes in South Africa. Differences between captive and free-ranging giraffes, males and females, and adults and subadults were analyzed by using a 2 x 2 X 2 factorial and Fisher's least significant difference for mean separation; when necessary variables were ranked and analyzed via analysis of variance. Potassium and bilirubin concentrations and alanine aminotransferase (ALT) activities were different between captive and free-ranging giraffes, but all fell within normal bovid reference ranges. The average glucose concentration was significantly elevated in free-ranging giraffes (161 mg/dl) compared with captive giraffes (113 mg/dl). All giraffes in this study had glucose concentrations higher than bovine (42-75 mg/dl) and caprine (48-76 mg/dl) reference ranges. Differences were also seen in lipase, chloride, and magnesium though these findings are likely not clinically significant. There were no differences detected between sexes. Adults had higher concentrations of potassium, total protein, globulins, and chloride and higher gamma glutamyltransferase activities, whereas subadults had higher concentrations of phosphorus. Within the captive group, nonimmobilized animals had higher concentrations of total protein and globulins. Captive giraffe diets need further investigation to determine if the differences seen in this study, especially glucose and bilirubin concentrations and ALT activities, may result in some health problems often seen in captive giraffes. C1 [Ellersieck, Mark R.] Univ Missouri, Expt Stn Stat, Columbia, MO 65211 USA. [Ball, Ray L.] Busch Gardens, Tampa, FL 33612 USA. [Koutsos, Elizabeth A.; Griffin, Mark E.] Purina Mills LLC, St Louis, MO 63166 USA. [Grobler, Douw] Catchco Africa, Pretoria, South Africa. [Citino, Scott B.] White Oak Conservat Ctr, Yulee, FL 32097 USA. [Bush, Mitchell] Natl Zool Pk Conservat & Res Ctr, Front Royal, VA 22630 USA. [Schmidt, Debra A.; Barbiers, Robyn B.] Lincoln Pk Zoo, Chicago, IL 60614 USA. RP Schmidt, DA (reprint author), St Louis Zoo, 1 Govt Dr, St Louis, MO 63110 USA. EM schmidt@stlzoo.org FU Purina Mills, LLC; Daniel F. and Ada L. Rice Foundation FX The authors thank the giraffe keepers, managers, and veterinarians at Binder Park Zoo, Brookfield Zoo, Disney's Animal Kingdom, Houston Zoo, Indianapolis Zoo, Maryland Zoo in Baltimore, North Carolina Zoological Park, Oakland Zoo, Omaha's Henry Doorly Zoo, and Zoo New England Franklin Park Zoo for submitting serum samples from their giraffes. Gratitude is also extended to Annatjie Krige, Dr. Marius Smuts, Andriette de Jager, Corila Buitendag for their patience with the many questions relating to sample analyses. Phillip Cronje and Lorna Fuller were instrumental in acquiring the permit and receiving and routing the samples to the appropriate laboratories in South Africa. The authors are grateful to Purina Mills, LLC, and the Daniel F. and Ada L. Rice Foundation for funding this project. NR 35 TC 2 Z9 2 U1 5 U2 36 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 MAR PY 2011 VL 42 IS 1 BP 33 EP 39 PG 7 WC Veterinary Sciences SC Veterinary Sciences GA 736EC UT WOS:000288472400005 PM 22946367 ER PT J AU Halfar, J Hetzinger, S Adey, W Zack, T Gamboa, G Kunz, B Williams, B Jacob, DE AF Halfar, J. Hetzinger, S. Adey, W. Zack, T. Gamboa, G. Kunz, B. Williams, B. Jacob, D. E. TI Coralline algal growth-increment widths archive North Atlantic climate variability SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Coralline algae; Paleoclimate; North Atlantic; Atlantic Multidecadal Oscillation; Sclerochronology ID LIVED BIVALVE MOLLUSK; ARCTICA-ISLANDICA; SURFACE-TEMPERATURE; LABRADOR CURRENT; GEODUCK CLAMS; INDIAN-OCEAN; RED ALGAE; SEA; RESOLUTION; SHELLS AB Over the past decade coralline algae have increasingly been used as archives of paleoclimate information. Encrusting coralline algae, which deposit annual growth increments in a high Mg-calcite skeleton, are amongst the longest-lived shallow marine organisms. In fact, a live-collected plant has recently been shown to have lived for at least 850 years based on radiometric dating. While a number of investigations have successfully used geochemical information of coralline algal skeletons to reconstruct sea surface temperatures, less attention has been paid to employ growth increment widths as a temperature proxy. Here we explore the relationship between growth and environmental parameters in Clathromorphum compactum collected in the subarctic Northwestern Atlantic. Results indicate that growth-increment widths of individual plants are poorly correlated with instrumental sea surface temperatures (SST). However, an averaged record of multiple growth increment-width time series from a regional network of C. compactum specimens up to 800 km apart reveals strong correlations with annual instrumental SST since 1950. Hence, similar to methods applied in dendrochronology, averaging of multiple sclerochronological records of coralline algae provides accurate climate information. A 115-year growth-increment width master chronology created from modern-collected and museum specimens is highly correlated to multidecadal variability seen in North Atlantic sea surface temperatures. Positive changes in algal growth anomalies record the well-documented regime shift and warming in the northwestern Atlantic during the 1990s. Large positive changes in algal growth anomalies were also present in the 1920s and 1930s, indicating that the impact of a concurrent large-scale regime shift throughout the North Atlantic was more strongly felt in the subarctic Northwestern Atlantic than previously thought, and may have even exceeded the 1990s event with respect to the magnitude of the warming. (C) 2010 Elsevier B.V. All rights reserved. C1 [Halfar, J.; Hetzinger, S.; Gamboa, G.; Williams, B.] Univ Toronto, CPS Dept, Mississauga, ON L5L 1C6, Canada. [Adey, W.] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Zack, T.; Kunz, B.; Jacob, D. E.] Johannes Gutenberg Univ Mainz, Dept Geosci, Earth Syst Sci Res Ctr, D-55099 Mainz, Germany. RP Halfar, J (reprint author), Univ Toronto, CPS Dept, 3359 Mississauga Rd N, Mississauga, ON L5L 1C6, Canada. EM jochen.halfar@utoronto.ca; steffen.hetzinger@utoronto.ca; ADEYW@si.edu; zack@uni-mainz.de; gimy.gamboa@utoronto.ca; bkunz@students.uni-mainz.de; branwen.williams@utoronto.ca; jacobd@uni-mainz.de RI Zack, Thomas/C-6153-2009; Adey, Walter/G-2858-2011; Jacob, Dorrit/F-8617-2010; Halfar, Jochen/C-7317-2014; Zack, Thomas/K-7228-2013; Hetzinger, Steffen/B-5778-2016 OI Jacob, Dorrit/0000-0003-4744-6627; Zack, Thomas/0000-0003-4747-4134; FU Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Climate and Atmospheric Sciences [Gr-7004]; Alexander von Humboldt Foundation FX We thank Wade Saunders, Bob Hooper from Bonne Bay Marine Station and Philip Sargent from Memorial University of Newfoundland for logistical support and advice on sampling locations. Andreas Kronz at Universitat Gottingen, Germany, provided backscatter electron images. J.H. was supported by a Natural Sciences and Engineering Research Council of Canada Discovery Grant, and a Canadian Foundation for Climate and Atmospheric Sciences Grant (Gr-7004). S.H. acknowledges support from the Alexander von Humboldt Foundation (Feodor Lynen Fellowship). This is a Geocycles contribution. Two anonymous reviewers provided excellent input. NR 67 TC 26 Z9 27 U1 7 U2 38 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD MAR 1 PY 2011 VL 302 IS 1-2 SI SI BP 71 EP 80 DI 10.1016/j.palaeo.2010.04.009 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 740FJ UT WOS:000288776700008 ER PT J AU Hetzinger, S Halfar, J Zack, T Gamboa, G Jacob, DE Kunz, BE Kronz, A Adey, W Lebednik, PA Steneck, RS AF Hetzinger, S. Halfar, J. Zack, T. Gamboa, G. Jacob, D. E. Kunz, B. E. Kronz, A. Adey, W. Lebednik, P. A. Steneck, R. S. TI High-resolution analysis of trace elements in crustose coralline algae from the North Atlantic and North Pacific by laser ablation ICP-MS SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Coralline algae; Clathromorphum; Laser ablation; LA-ICP-MS; Trace element; Electron microprobe; North Pacific; North Atlantic; Proxy archive ID SEA-SURFACE TEMPERATURE; GREAT-BARRIER-REEF; ARCTICA-ISLANDICA; SR/CA RECORDS; RED ALGAE; MAGNESIUM; RECONSTRUCTIONS; GEOCHEMISTRY; THERMOMETRY; VARIABILITY AB We have investigated the trace elemental composition in the skeleta of two specimens of attached-living coralline algae of the species Clathromorphum compactum from the North Atlantic (Newfoundland) and Clathromorphum nereostratum from the North Pacific/Bering Sea region (Amchitka Island, Aleutians). Samples were analyzed using Laser Ablation-Inductively Coupled Plasma Mass Spectrometry (IA-ICP-MS) yielding for the first time continuous individual trace elemental records of up to 69 years in length. The resulting algal Mg/Ca, Sr/Ca, U/Ca, and Ba/Ca ratios are reproducible within individual sample specimens. Algal Mg/Ca ratios were additionally validated by electron microprobe analyses (Amchitka sample). Algal Sr/Ca, U/Ca, and Ba/Ca ratios were compared to algal Mg/Ca ratios, which previously have been shown to reliably record sea surface temperature (SST). Ratios of Sr/Ca from both Clathromorphum species show a strong positive correlation to temperature-dependent Mg/Ca ratios, implying that seawater temperature plays an important role in the incorporation of Sr into algal calcite. Linear Sr/Ca-SST regressions have provided positive, but weaker relationships as compared to Mg/Ca-SST relationships. Both, algal Mg/Ca and Sr/Ca display clear seasonal cycles. Inverse correlations were found between algal Mg/Ca and U/Ca, Ba/Ca, and correlations to SST are weaker than between Mg/Ca, Sr/Ca and SST. This suggests that the incorporation of U and Ba is influenced by other factors aside from temperature. (C) 2010 Elsevier B.V. All rights reserved. C1 [Hetzinger, S.; Halfar, J.; Gamboa, G.] Univ Toronto, CPS Dept, Mississauga, ON L5L 1C6, Canada. [Zack, T.; Jacob, D. E.; Kunz, B. E.] Johannes Gutenberg Univ Mainz, Dept Geosci, Earth Syst Sci Res Ctr, D-55099 Mainz, Germany. [Kronz, A.] Univ Gottingen, Geowissensch Zentrum, D-3400 Gottingen, Germany. [Adey, W.] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Lebednik, P. A.] ARCADIS, Walnut Creek, CA 94596 USA. [Steneck, R. S.] Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. RP Hetzinger, S (reprint author), Leibniz Inst Marine Sci, IFM GEOMAR, Wischhofstr 1-3, D-24148 Kiel, Germany. EM shetzinger@ifm-geomar.de; jochen.halfar@utoronto.ca; zack@uni-manz.de; gimy.gamboa@utoronto.ca; jacobd@uni-mainz.de; bkunz@students.uni-mainz.de; akronz@gwdg.de; adeyw@si.edu; phillip.lebednik@arcadis-us.com; steneck@maine.edu RI Hetzinger, Steffen/B-5778-2016; Zack, Thomas/C-6153-2009; Adey, Walter/G-2858-2011; Jacob, Dorrit/F-8617-2010; Halfar, Jochen/C-7317-2014; Zack, Thomas/K-7228-2013 OI Jacob, Dorrit/0000-0003-4744-6627; Zack, Thomas/0000-0003-4747-4134 FU Alexander von Humboldt Foundation; Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Climate and Atmospheric Sciences [Gr-7004] FX We would like to thank Wade Saunders and Bob Hooper from Bonne Bay Marine Station for the logistical support and advice on sampling locations, and Philip Sargent from Memorial University for the support during dive operations. The U.S. National Herbarium of the Smithsonian Institution, Washington DC, is kindly acknowledged for providing sample AM-KR-80 8-69-14B (AM1, Amchitka Island). S.H. acknowledges support from the Alexander von Humboldt Foundation (Feodor Lynen Fellowship). J.H. was supported by a Natural Sciences and Engineering Research Council of Canada Discovery Grant, and a Canadian Foundation for Climate and Atmospheric Sciences Grant (Gr-7004). Two anonymous reviewers are thanked for providing excellent comments. NR 54 TC 16 Z9 16 U1 3 U2 37 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD MAR 1 PY 2011 VL 302 IS 1-2 SI SI BP 81 EP 94 DI 10.1016/j.palaeo.2010.06.004 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 740FJ UT WOS:000288776700009 ER PT J AU Isler, ML Whitney, BM AF Isler, Morton L. Whitney, Bret M. TI SPECIES LIMITS IN ANTBIRDS (THAMNOPHILIDAE): THE SCALE-BACKED ANTBIRD (WILLISORNIS POECILINOTUS) COMPLEX SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article ID PASSERIFORMES AB The geographic range of the Scale-backed Antbird (Willisornis poecilinotus) encompasses Amazonia. Seven currently defined subspecies are distinguished from one another by diagnostic plumage characters except for one pair. Six pairs of subspecies are apparently parapatric and lack a known barrier to intergradation in at least a portion of their contact zone; yet confirmed hybrids are known only for one pair in one location. An analysis of > 350 recordings, however, found vocal differences among them insufficient to recommend elevating subspecies to the species level with one exception. Populations in southeastern Amazonia should be considered a distinct species, Willisornis vidua (Hellmayr), Xingu Scale-backed Antbird, on the basis of their distinct loudsongs, raspy call Series, and contact calls. Within the widespread Willisornis poecilinotus, Common Scale-backed Antbird, the remaining instances of parapatry without extensive intergradation provide a focus for future fieldwork to define interrelationships in contact zones and mechanisms of species recognition that may be sustaining them on independent evolutionary paths. Received 15 May 2010. Accepted 9 September 2010. C1 [Isler, Morton L.] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, MRC 116, Washington, DC 20013 USA. [Whitney, Bret M.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. RP Isler, ML (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, MRC 116, POB 37012, Washington, DC 20013 USA. EM antbird@cox.net NR 39 TC 10 Z9 13 U1 0 U2 9 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD MAR PY 2011 VL 123 IS 1 BP 1 EP 14 DI 10.1676/10-082.1 PG 14 WC Ornithology SC Zoology GA 734TB UT WOS:000288360100001 ER PT J AU Dove, CJ Snow, RW Rochford, MR Mazzotti, FJ AF Dove, Carla J. Snow, Ray W. Rochford, Michael R. Mazzotti, Frank J. TI BIRDS CONSUMED BY THE INVASIVE BURMESE PYTHON (PYTHON MOLURUS BIVITTATUS) IN EVERGLADES NATIONAL PARK, FLORIDA, USA SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article ID IDENTIFICATION; REMAINS AB We identified 25 species of birds representing nine avian Orders from remains in digestive tracts of 85 Burmese pythons (Python molurus bivittatus) collected in Everglades National Park, Florida, USA, from 2003 to 2008. Four species of birds identified in this study are of special concern in Florida and a fifth, the Wood Stork (Mycteria americana), is listed as federally endangered. This represents the first detailed analysis of the avian component of the diet of the introduced Burmese python, now established in Everglades National Park, Florida and highlights the potential for considerable negative impact of this invasive species on native bird populations. Received 9 June 2010. Accepted 27 September 2010, C1 [Dove, Carla J.] Smithsonian Inst, Div Birds, Washington, DC 20560 USA. [Snow, Ray W.] S Florida Nat Resources Ctr, Homestead, FL 33034 USA. [Rochford, Michael R.; Mazzotti, Frank J.] Univ Florida, Ft Lauderdale Res & Educ Ctr, Ft Lauderdale, FL 33314 USA. RP Dove, CJ (reprint author), Smithsonian Inst, Div Birds, NHB E-600,MRC 116, Washington, DC 20560 USA. EM dovec@si.edu FU U.S. Air Force; U.S. Navy; Federal Aviation Administration FX We are grateful to the many cooperators who collected and processed the samples that were analyzed in this study including Bob Hill, Mark Peyton, Jennifer Fells, Alex Wolf. Edward Lamivee, Rafael Crespo, and Brian Greeves. S. L. Olson (Smithsonian Institution) assisted with the identifications of osteological material. Marcy Heacker (Smithsonian Institution, Feather Identification Laboratory) presented these results to the Subcommittee on National Parks, Forests, and Public Lands of the House Committee on Natural Resources in Washington, D.C. Nancy Russell, South Florida Collection Management Center, Everglades and Dry Tortugas National parks coordinated shipping of samples and maintains the collections of ENP material. S. L. Olson, C. M. Milensky, R. W. McDiarmid (Smithsonian Institution), and two reviewers provided comments on the manuscript. The Feather Identification Laboratory is supported by interagency agreements with the U.S. Air Force, U.S. Navy, and Federal Aviation Administration. NR 20 TC 20 Z9 22 U1 30 U2 264 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 MAR PY 2011 VL 123 IS 1 BP 126 EP 131 DI 10.1676/10-092.1 PG 6 WC Ornithology SC Zoology GA 734TB UT WOS:000288360100016 ER PT J AU Grant, JA Irwin, RP Wilson, SA Buczkowski, D Siebach, K AF Grant, J. A. Irwin, R. P., III Wilson, S. A. Buczkowski, D. Siebach, K. TI A lake in Uzboi Vallis and implications for Late Noachian-Early Hesperian climate on Mars SO ICARUS LA English DT Article DE Mars; Mars, Surface; Geological processes ID MARGARITIFER SINUS; HOLDEN CRATER; EVOLUTION; CHANNELS; DEPOSITS; SYSTEMS; SCALE; WATER; EARTH AB Uzboi Vallis (centered at similar to 28 degrees S, 323 degrees E) is similar to 400 km long and comprises the southernmost segment of the northward-draining Uzboi-Ladon-Morava (ULM) meso-scale outflow system that emerges from Argyre basin. Bond and Holden craters blocked the valley to the south and north, respectively, forming a Late Noachian-to-Hesperian paleolake basin that exceeded 4000 km(3). Limited CRISM data suggest lake deposits in Uzboi and underlying basin floor incorporate relatively more Mg-clays and more Fe-clays, respectively. The short-lived lake overflowed and breached Holden crater's rim at an elevation of -350 m and rapidly drained into the crater. Fan deltas in Holden extend 25 km from the breach and incorporate meter-sized blocks, and longitudinal grooves along the Uzboi basin floor are hundreds of meters long and average 60 m wide, suggesting high-discharge drainage of the lake. Precipitation-derived runoff rather than regional groundwater or overflow from Argyre dominated contributions to the Uzboi lake. although the failure of most tributaries to respond to a lowering of base level indicates their incision largely ended when the lake drained. The Uzboi lake may have coincided with alluvial and/or lacustrine activity in Holden, Eberswalde, and other craters in southern Margaritifer Terra, where fluvial/lacustrine activity may have required widespread, synoptic precipitation (rain or snow), perhaps associated with an ephemeral, global hydrologic system during the Late Noachian into the Hesperian on Mars. Published by Elsevier Inc. C1 [Grant, J. A.; Wilson, S. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Irwin, R. P., III] Planetary Sci Inst, Tucson, AZ 85719 USA. [Buczkowski, D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Siebach, K.] Washington Univ, St Louis, MO 63130 USA. RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, 6th St,Independence Ave SW, Washington, DC 20560 USA. EM grantj@si.edu OI Siebach, Kirsten/0000-0002-6628-6297 FU NASA FX We thank the people at the University of Arizona, Ball Aerospace, and Lockheed Martin that built and operate the HiRISE camera and Mars Reconnaissance Orbiter spacecraft. Kevin Williams provided a constructive review that improved the manuscript. This work was supported by NASA. NR 49 TC 14 Z9 14 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD MAR PY 2011 VL 212 IS 1 BP 110 EP 122 DI 10.1016/j.icarus.2010.11.024 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 732KL UT WOS:000288183700008 ER PT J AU Pukazhenthi, BS Comizzoli, P Hagedorn, M AF Pukazhenthi, Budhan S. Comizzoli, Pierre Hagedorn, Mary TI FERTILITY CONSERVATION IN NON-DOMESTIC SPECIES: SUCCESSES, CHALLENGES AND LESSONS FOR HUMAN MEDICINE SO JOURNAL OF ANDROLOGY LA English DT Meeting Abstract CT 36th Annual Meeting of Genes and Harmones - State-of-the-Art Reproductive and Sexual Development CY APR 02-05, 2011 CL Hyatt Regency Montreal, Montreal, CANADA HO Hyatt Regency Montreal C1 [Pukazhenthi, Budhan S.; Comizzoli, Pierre; Hagedorn, Mary] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU AMER SOC ANDROLOGY, INC PI LAWRENCE PA C/O ALLEN PRESS, INC PO BOX 368, LAWRENCE, KS 66044 USA SN 0196-3635 J9 J ANDROL JI J. Androl. PD MAR-APR PY 2011 SU S BP 23 EP 23 PG 1 WC Andrology SC Endocrinology & Metabolism GA 724AZ UT WOS:000287549800003 ER PT J AU Cadena, CD Gutierrez-Pinto, N Davila, N Chesser, RT AF Daniel Cadena, Carlos Gutierrez-Pinto, Natalia Davila, Nicolas Chesser, R. Terry TI No population genetic structure in a widespread aquatic songbird from the Neotropics SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Andes; Amazonia; Chrysomus icterocephalus; Icteridae; Phylogeography; Yellow-hooded Blackbird ID HISTORICAL DIVERSIFICATION; LANDSCAPE EVOLUTION; FOREST BIRDS; DIFFERENTIATION; DIVERSITY; SOFTWARE; AMAZONIA; ECOLOGY; AVES AB Neotropical lowland organisms often show marked population genetic structure, suggesting restricted migration among populations. However, most phylogeographic studies have focused on species inhabiting humid forest interior. Little attention has been devoted to the study of species with ecologies conducive to dispersal, such as those of more open and variable environments associated with watercourses. Using mtDNA sequences, we examined patterns of genetic variation in a widely distributed Neotropical songbird of aquatic environments, the Yellow-hooded Blackbird (Icteridae, Chrysomus icterocephalus). In contrast to many forest species, Yellow-hooded Blackbirds showed no detectable genetic structure across their range, which includes lowland populations on both sides of the Andes, much of northeastern South America, Amazonia, as well as a phenotypically distinct highland population in Colombia. A coalescent-based analysis of the species indicated that its effective population size has increased considerably, suggesting a range expansion. Our results support the hypothesis that species occurring in open habitats and tracking temporally dynamic environments should show increased dispersal propensities (hence gene flow) relative to species from closed and more stable environments. The phenotypic and behavioral variation among populations of our study species appears to have arisen recently and perhaps in the face of gene flow. (C) 2010 Elsevier Inc. All rights reserved. C1 [Daniel Cadena, Carlos; Gutierrez-Pinto, Natalia; Davila, Nicolas] Univ Los Andes, Dept Ciencias Biol, Lab Biol Evolut Vertebrados, Bogota, Colombia. [Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. RP Cadena, CD (reprint author), Univ Los Andes, Dept Ciencias Biol, Lab Biol Evolut Vertebrados, Apartado 4976, Bogota, Colombia. EM ccadena@uniandes.edu.co; n.gutierrez126@uniandes.edu.co; nicodavila@hotmail.com; chessert@si.edu FU Facultad de Ciencias at Universidad de los Andes; National Science Foundation [DEB-0841729]; Office of Fellowships, Smithsonian Institution FX Financial support for this study was provided by the Facultad de Ciencias at Universidad de los Andes, the National Science Foundation (Grant DEB-0841729 to R. T. Brumfield), and the Office of Fellowships, Smithsonian Institution. We thank the American Museum of Natural History (J. Cracraft and P. Sweet), the Field Museum of Natural History (J. Bates and D. Willard), the Institut Nacional de Pesquisas de Amazonia (M. Cohn-Haft), and the Louisiana State University Museum of Natural Science (R. Brumfield and D. Dittmann) for tissue loans. Use of trade, product, or firm names does riot imply endorsement by the US Government. NR 33 TC 15 Z9 17 U1 0 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2011 VL 58 IS 3 BP 540 EP 545 DI 10.1016/j.ympev.2010.12.014 PG 6 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 731ZX UT WOS:000288151000012 PM 21195784 ER PT J AU Quenouille, B Hubert, N Bermingham, E Planes, S AF Quenouille, Brice Hubert, Nicolas Bermingham, Eldredge Planes, Serge TI Speciation in tropical seas: Allopatry followed by range change SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Phylogeny; Speciation; Sympatry; Competition; Co-existence; Marine species ID SPECIES-LEVEL PHYLOGENIES; CORAL-REEF FISHES; ECOLOGICAL SPECIATION; MOLECULAR SYSTEMATICS; GENETIC-DIVERGENCE; MARINE-SPECIATION; DNA-SEQUENCES; BIOGEOGRAPHY; DIVERSIFICATION; PHYLOGEOGRAPHY AB We investigated whether present distribution ranges in marine organisms are reliable indicators of the geographic pattern of past speciation events by assessing the level of geographic overlap (sympatric index) as a function of node age in four phylogenies of tropical marine species groups. The analyses led to remarkably similar results among the four groups examined with (1) most nodes associated with a sympatry index of either 0 (allopatry) or 1 (entire overlap) and (2) statistical support that sister species have an allopatric distribution significantly more frequently than sister clades (i.e. groups of species). Species divergences were expressed on a time scale and very similar times were needed for species range overlap to occur since sharp transitions from allopatry to sympatry occurred around 4 Ma in all groups. Present results supports that species range changes were not random as previous simulations results supports that species range probably evolve through occasional shifts of large amplitude. In front of the time needed for species range overlapping, our study suggests that species interaction and competitive exclusion can no longer be excluded as a driver of marine species distribution. (C) 2010 Elsevier Inc. All rights reserved. C1 [Quenouille, Brice; Planes, Serge] Univ Perpignan, USR 3278, Ctr Biol & Ecol Trop & Mediteraneenne, F-66860 Perpignan, France. [Hubert, Nicolas] Univ La Reunion, Fac Sci & Technol, Lab ECOMAR, St Denis 97715, Reunion. [Quenouille, Brice; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama. RP Planes, S (reprint author), Univ Perpignan, USR 3278, Ctr Biol & Ecol Trop & Mediteraneenne, Via Domitia,52 Ave Paul Alduy, F-66860 Perpignan, France. EM planes@univ-perp.fr FU "TOTAL Fundation"; PPF EPHE "Populations Franctionnees et Insulaires"; Smithsonian Tropical Research Institute FX Funded was jointly supported by the "TOTAL Fundation", the PPF EPHE "Populations Franctionnees et Insulaires", and the Smithsonian Tropical Research Institute's Molecular Systematics and Evolution program. We thank S. Thorrold, P. Doherty, L. Van Everden for discussion and reading previous versions of the manuscript. NR 48 TC 24 Z9 24 U1 2 U2 22 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2011 VL 58 IS 3 BP 546 EP 552 DI 10.1016/j.ympev.2010.12.009 PG 7 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 731ZX UT WOS:000288151000013 PM 21256237 ER EF